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observations </div> </a> <ul id="toc-Ancient,_naked_eye_observations-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Telescopic_observations" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Telescopic_observations"> <div class="vector-toc-text"> 3.2 Telescopic observations </div> </a> <ul id="toc-Telescopic_observations-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Satellite_observations" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Satellite_observations"> <div class="vector-toc-text"> 3.3 Satellite observations </div> </a> <ul id="toc-Satellite_observations-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Astrography" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Astrography"> <div class="vector-toc-text"> 4 Astrography </div> </a> <button aria-controls="toc-Astrography-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> Toggle Astrography subsection </button> <ul id="toc-Astrography-sublist" class="vector-toc-list"> <li id="toc-Sun's_location_and_neighborhood" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Sun's_location_and_neighborhood"> <div class="vector-toc-text"> 4.1 Sun's location and neighborhood </div> </a> <ul id="toc-Sun's_location_and_neighborhood-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Galactic_quadrants" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Galactic_quadrants"> <div class="vector-toc-text"> 4.2 Galactic quadrants </div> </a> <ul id="toc-Galactic_quadrants-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Size_and_mass" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Size_and_mass"> <div class="vector-toc-text"> 5 Size and mass </div> </a> <button aria-controls="toc-Size_and_mass-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> Toggle Size and mass subsection </button> <ul id="toc-Size_and_mass-sublist" class="vector-toc-list"> <li id="toc-Size" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Size"> <div class="vector-toc-text"> 5.1 Size </div> </a> <ul id="toc-Size-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Mass" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Mass"> <div class="vector-toc-text"> 5.2 Mass </div> </a> <ul id="toc-Mass-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Contents" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Contents"> <div class="vector-toc-text"> 6 Contents </div> </a> <ul id="toc-Contents-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Structure" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Structure"> <div class="vector-toc-text"> 7 Structure </div> </a> <button aria-controls="toc-Structure-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> Toggle Structure subsection </button> <ul id="toc-Structure-sublist" class="vector-toc-list"> <li id="toc-Galactic_Center" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Galactic_Center"> <div class="vector-toc-text"> 7.1 Galactic Center </div> </a> <ul id="toc-Galactic_Center-sublist" class="vector-toc-list"> <li id="toc-Gamma_rays_and_x-rays" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Gamma_rays_and_x-rays"> <div class="vector-toc-text"> 7.1.1 Gamma rays and x-rays </div> </a> <ul id="toc-Gamma_rays_and_x-rays-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Spiral_arms" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Spiral_arms"> <div class="vector-toc-text"> 7.2 Spiral arms </div> </a> <ul id="toc-Spiral_arms-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Halo" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Halo"> <div class="vector-toc-text"> 7.3 Halo </div> </a> <ul id="toc-Halo-sublist" class="vector-toc-list"> <li id="toc-Gaseous_halo" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Gaseous_halo"> <div class="vector-toc-text"> 7.3.1 Gaseous halo </div> </a> <ul id="toc-Gaseous_halo-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Galactic_rotation" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Galactic_rotation"> <div class="vector-toc-text"> 7.4 Galactic rotation </div> </a> <ul id="toc-Galactic_rotation-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Formation" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Formation"> <div class="vector-toc-text"> 8 Formation </div> </a> <button aria-controls="toc-Formation-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> Toggle Formation subsection </button> <ul id="toc-Formation-sublist" class="vector-toc-list"> <li id="toc-History" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#History"> <div class="vector-toc-text"> 8.1 History </div> </a> <ul id="toc-History-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Age_and_cosmological_history" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Age_and_cosmological_history"> <div class="vector-toc-text"> 8.2 Age and cosmological history </div> </a> <ul id="toc-Age_and_cosmological_history-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Intergalactic_neighbourhood" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Intergalactic_neighbourhood"> <div class="vector-toc-text"> 9 Intergalactic neighbourhood </div> </a> <ul id="toc-Intergalactic_neighbourhood-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Velocity" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Velocity"> <div class="vector-toc-text"> 10 Velocity </div> </a> <ul id="toc-Velocity-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-See_also" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#See_also"> <div class="vector-toc-text"> 11 See also </div> </a> <ul id="toc-See_also-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Notes" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Notes"> <div class="vector-toc-text"> 12 Notes </div> </a> <ul id="toc-Notes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-References" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#References"> <div class="vector-toc-text"> 13 References </div> </a> <ul id="toc-References-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Further_reading" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Further_reading"> <div class="vector-toc-text"> 14 Further reading </div> </a> <ul id="toc-Further_reading-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-External_links" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#External_links"> <div class="vector-toc-text"> 15 External links </div> </a> <ul id="toc-External_links-sublist" class="vector-toc-list"> </ul> </li> </ul> </div> </div> </nav> </div> </div> <div class="mw-content-container"> <main id="content" class="mw-body"> <header class="mw-body-header vector-page-titlebar"> <nav aria-label="Contents" class="vector-toc-landmark"> <div id="vector-page-titlebar-toc" class="vector-dropdown vector-page-titlebar-toc vector-button-flush-left" > <input type="checkbox" id="vector-page-titlebar-toc-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-vector-page-titlebar-toc" class="vector-dropdown-checkbox " aria-label="Toggle the table of contents" > <label id="vector-page-titlebar-toc-label" for="vector-page-titlebar-toc-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--icon-only " aria-hidden="true" > Toggle the table of contents </label> <div class="vector-dropdown-content"> <div id="vector-page-titlebar-toc-unpinned-container" class="vector-unpinned-container"> </div> </div> </div> </nav> <h1 id="firstHeading" class="firstHeading mw-first-heading">Milky Way</h1> <div id="p-lang-btn" class="vector-dropdown mw-portlet mw-portlet-lang" > <input type="checkbox" id="p-lang-btn-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-p-lang-btn" class="vector-dropdown-checkbox mw-interlanguage-selector" aria-label="Go to an article in another language. Available in 187 languages" > <label id="p-lang-btn-label" for="p-lang-btn-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--action-progressive mw-portlet-lang-heading-187" aria-hidden="true" > 187 languages </label> <div class="vector-dropdown-content"> <div class="vector-menu-content"> <ul class="vector-menu-content-list"> <li class="interlanguage-link interwiki-kbd mw-list-item"><a href="https://kbd.wikipedia.org/wiki/%D0%A8%D1%8B%D1%85%D1%83%D0%BB%D1%8A%D0%B0%D0%B3%D1%8A%D1%83%D1%8D" title="Шыхулъагъуэ – Kabardian" lang="kbd" hreflang="kbd" data-title="Шыхулъагъуэ" data-language-autonym="Адыгэбзэ" data-language-local-name="Kabardian" class="interlanguage-link-target">Адыгэбзэ</a></li><li class="interlanguage-link interwiki-ady mw-list-item"><a href="https://ady.wikipedia.org/wiki/%D0%A8%D1%8B%D1%85%D1%83%D0%BB%D1%8A%D0%B0%D0%B3%D1%8A%D0%BE" title="Шыхулъагъо – Adyghe" lang="ady" hreflang="ady" data-title="Шыхулъагъо" data-language-autonym="Адыгабзэ" data-language-local-name="Adyghe" class="interlanguage-link-target">Адыгабзэ</a></li><li class="interlanguage-link interwiki-af badge-Q17437796 badge-featuredarticle mw-list-item" title="featured article badge"><a href="https://af.wikipedia.org/wiki/Melkweg" title="Melkweg – Afrikaans" lang="af" hreflang="af" data-title="Melkweg" data-language-autonym="Afrikaans" data-language-local-name="Afrikaans" class="interlanguage-link-target">Afrikaans</a></li><li class="interlanguage-link interwiki-als mw-list-item"><a href="https://als.wikipedia.org/wiki/Milchstra%C3%9Fe" title="Milchstraße – Alemannic" lang="gsw" hreflang="gsw" data-title="Milchstraße" data-language-autonym="Alemannisch" data-language-local-name="Alemannic" class="interlanguage-link-target">Alemannisch</a></li><li class="interlanguage-link interwiki-am mw-list-item"><a href="https://am.wikipedia.org/wiki/%E1%88%9A%E1%88%8D%E1%8A%AA_%E1%8B%8C%E1%8B%AD" title="ሚልኪ ዌይ – Amharic" lang="am" hreflang="am" data-title="ሚልኪ ዌይ" data-language-autonym="አማርኛ" data-language-local-name="Amharic" class="interlanguage-link-target">አማርኛ</a></li><li class="interlanguage-link interwiki-anp mw-list-item"><a href="https://anp.wikipedia.org/wiki/%E0%A4%86%E0%A4%95%E0%A4%BE%E0%A4%B6%E0%A4%97%E0%A4%82%E0%A4%97%E0%A4%BE" title="आकाशगंगा – Angika" lang="anp" hreflang="anp" data-title="आकाशगंगा" data-language-autonym="अंगिका" data-language-local-name="Angika" class="interlanguage-link-target">अंगिका</a></li><li class="interlanguage-link interwiki-ar mw-list-item"><a href="https://ar.wikipedia.org/wiki/%D8%AF%D8%B1%D8%A8_%D8%A7%D9%84%D8%AA%D8%A8%D8%A7%D9%86%D8%A9" title="درب التبانة – Arabic" lang="ar" hreflang="ar" data-title="درب التبانة" data-language-autonym="العربية" data-language-local-name="Arabic" class="interlanguage-link-target">العربية</a></li><li class="interlanguage-link interwiki-an mw-list-item"><a href="https://an.wikipedia.org/wiki/Carrera_de_Sant_Chaime" title="Carrera de Sant Chaime – Aragonese" lang="an" hreflang="an" data-title="Carrera de Sant Chaime" data-language-autonym="Aragonés" data-language-local-name="Aragonese" class="interlanguage-link-target">Aragonés</a></li><li class="interlanguage-link interwiki-hyw mw-list-item"><a href="https://hyw.wikipedia.org/wiki/%D4%BE%D5%AB%D6%80_%D4%BF%D5%A1%D5%A9%D5%AB%D5%B6" title="Ծիր Կաթին – Western Armenian" lang="hyw" hreflang="hyw" data-title="Ծիր Կաթին" data-language-autonym="Արեւմտահայերէն" data-language-local-name="Western Armenian" class="interlanguage-link-target">Արեւմտահայերէն</a></li><li class="interlanguage-link interwiki-as mw-list-item"><a href="https://as.wikipedia.org/wiki/%E0%A6%B9%E0%A6%BE%E0%A6%A4%E0%A7%80%E0%A6%AA%E0%A6%9F%E0%A6%BF" title="হাতীপটি – Assamese" lang="as" hreflang="as" data-title="হাতীপটি" data-language-autonym="অসমীয়া" data-language-local-name="Assamese" class="interlanguage-link-target">অসমীয়া</a></li><li class="interlanguage-link interwiki-ast mw-list-item"><a href="https://ast.wikipedia.org/wiki/Cam%C3%ADn_de_Santiago_(galaxa)" title="Camín de Santiago (galaxa) – Asturian" lang="ast" hreflang="ast" data-title="Camín de Santiago (galaxa)" data-language-autonym="Asturianu" data-language-local-name="Asturian" class="interlanguage-link-target">Asturianu</a></li><li class="interlanguage-link interwiki-gn mw-list-item"><a href="https://gn.wikipedia.org/wiki/Mborevi_Rape" title="Mborevi Rape – Guarani" lang="gn" hreflang="gn" data-title="Mborevi Rape" data-language-autonym="Avañe'ẽ" data-language-local-name="Guarani" class="interlanguage-link-target">Avañe'ẽ</a></li><li class="interlanguage-link interwiki-az mw-list-item"><a href="https://az.wikipedia.org/wiki/S%C3%BCd_Yolu" title="Süd Yolu – Azerbaijani" lang="az" hreflang="az" data-title="Süd Yolu" data-language-autonym="Azərbaycanca" data-language-local-name="Azerbaijani" class="interlanguage-link-target">Azərbaycanca</a></li><li class="interlanguage-link interwiki-azb mw-list-item"><a href="https://azb.wikipedia.org/wiki/%D8%B3%D8%A7%D9%85%D8%A7%D9%86_%DB%8C%D9%88%D9%84%D9%88" title="سامان یولو – South Azerbaijani" lang="azb" hreflang="azb" data-title="سامان یولو" data-language-autonym="تۆرکجه" data-language-local-name="South Azerbaijani" class="interlanguage-link-target">تۆرکجه</a></li><li class="interlanguage-link interwiki-bn mw-list-item"><a href="https://bn.wikipedia.org/wiki/%E0%A6%86%E0%A6%95%E0%A6%BE%E0%A6%B6%E0%A6%97%E0%A6%99%E0%A7%8D%E0%A6%97%E0%A6%BE_%E0%A6%9B%E0%A6%BE%E0%A6%AF%E0%A6%BC%E0%A6%BE%E0%A6%AA%E0%A6%A5" title="আকাশগঙ্গা ছায়াপথ – Bangla" lang="bn" hreflang="bn" data-title="আকাশগঙ্গা ছায়াপথ" data-language-autonym="বাংলা" data-language-local-name="Bangla" class="interlanguage-link-target">বাংলা</a></li><li class="interlanguage-link interwiki-zh-min-nan mw-list-item"><a href="https://zh-min-nan.wikipedia.org/wiki/H%C3%B4-khe" title="Hô-khe – Minnan" lang="nan" hreflang="nan" data-title="Hô-khe" data-language-autonym="閩南語 / Bân-lâm-gú" data-language-local-name="Minnan" class="interlanguage-link-target">閩南語 / Bân-lâm-gú</a></li><li class="interlanguage-link interwiki-ba mw-list-item"><a href="https://ba.wikipedia.org/wiki/%D2%A0%D0%BE%D1%88_%D1%8E%D0%BB%D1%8B" title="Ҡош юлы – Bashkir" lang="ba" hreflang="ba" data-title="Ҡош юлы" data-language-autonym="Башҡортса" data-language-local-name="Bashkir" class="interlanguage-link-target">Башҡортса</a></li><li class="interlanguage-link interwiki-be mw-list-item"><a href="https://be.wikipedia.org/wiki/%D0%9C%D0%BB%D0%B5%D1%87%D0%BD%D1%8B_%D0%A8%D0%BB%D1%8F%D1%85" title="Млечны Шлях – Belarusian" lang="be" hreflang="be" data-title="Млечны Шлях" data-language-autonym="Беларуская" data-language-local-name="Belarusian" class="interlanguage-link-target">Беларуская</a></li><li class="interlanguage-link interwiki-be-x-old mw-list-item"><a href="https://be-tarask.wikipedia.org/wiki/%D0%9C%D0%BB%D0%B5%D1%87%D0%BD%D1%8B_%D0%A8%D0%BB%D1%8F%D1%85" title="Млечны Шлях – Belarusian (Taraškievica orthography)" lang="be-tarask" hreflang="be-tarask" data-title="Млечны Шлях" data-language-autonym="Беларуская (тарашкевіца)" data-language-local-name="Belarusian (Taraškievica orthography)" class="interlanguage-link-target">Беларуская (тарашкевіца)</a></li><li class="interlanguage-link interwiki-bh mw-list-item"><a href="https://bh.wikipedia.org/wiki/%E0%A4%86%E0%A4%95%E0%A4%BE%E0%A4%B6%E0%A4%97%E0%A4%82%E0%A4%97%E0%A4%BE" title="आकाशगंगा – Bhojpuri" lang="bh" hreflang="bh" data-title="आकाशगंगा" data-language-autonym="भोजपुरी" data-language-local-name="Bhojpuri" class="interlanguage-link-target">भोजपुरी</a></li><li class="interlanguage-link interwiki-bcl mw-list-item"><a href="https://bcl.wikipedia.org/wiki/Milky_Way" title="Milky Way – Central Bikol" lang="bcl" hreflang="bcl" data-title="Milky Way" data-language-autonym="Bikol Central" data-language-local-name="Central Bikol" class="interlanguage-link-target">Bikol Central</a></li><li class="interlanguage-link interwiki-bg mw-list-item"><a href="https://bg.wikipedia.org/wiki/%D0%9C%D0%BB%D0%B5%D1%87%D0%B5%D0%BD_%D0%BF%D1%8A%D1%82" title="Млечен път – Bulgarian" lang="bg" hreflang="bg" data-title="Млечен път" data-language-autonym="Български" data-language-local-name="Bulgarian" class="interlanguage-link-target">Български</a></li><li class="interlanguage-link interwiki-bar mw-list-item"><a href="https://bar.wikipedia.org/wiki/Muichstrossn" title="Muichstrossn – Bavarian" lang="bar" hreflang="bar" data-title="Muichstrossn" data-language-autonym="Boarisch" data-language-local-name="Bavarian" class="interlanguage-link-target">Boarisch</a></li><li class="interlanguage-link interwiki-bs mw-list-item"><a href="https://bs.wikipedia.org/wiki/Mlije%C4%8Dni_put" title="Mliječni put – Bosnian" lang="bs" hreflang="bs" data-title="Mliječni put" data-language-autonym="Bosanski" data-language-local-name="Bosnian" class="interlanguage-link-target">Bosanski</a></li><li class="interlanguage-link interwiki-br mw-list-item"><a href="https://br.wikipedia.org/wiki/Hent_Sant-Jakez_(galaksienn)" title="Hent Sant-Jakez (galaksienn) – Breton" lang="br" hreflang="br" data-title="Hent Sant-Jakez (galaksienn)" data-language-autonym="Brezhoneg" data-language-local-name="Breton" class="interlanguage-link-target">Brezhoneg</a></li><li class="interlanguage-link interwiki-bxr mw-list-item"><a href="https://bxr.wikipedia.org/wiki/%D0%A2%D1%8D%D0%BD%D0%B3%D1%8D%D1%80%D0%B8%D0%B8%D0%BD_%D0%B7%D2%AF%D0%B9%D0%B4%D1%8D%D0%BB" title="Тэнгэриин зүйдэл – Russia Buriat" lang="bxr" hreflang="bxr" data-title="Тэнгэриин зүйдэл" data-language-autonym="Буряад" data-language-local-name="Russia Buriat" class="interlanguage-link-target">Буряад</a></li><li class="interlanguage-link interwiki-ca mw-list-item"><a href="https://ca.wikipedia.org/wiki/Via_L%C3%A0ctia" title="Via Làctia – Catalan" lang="ca" hreflang="ca" data-title="Via Làctia" data-language-autonym="Català" data-language-local-name="Catalan" class="interlanguage-link-target">Català</a></li><li class="interlanguage-link interwiki-cv mw-list-item"><a href="https://cv.wikipedia.org/wiki/%D0%A5%D1%83%D1%80%D0%BA%D0%B0%D0%B9%C4%83%D0%BA_%C3%87%D1%83%D0%BB%C4%95" title="Хуркайăк Çулĕ – Chuvash" lang="cv" hreflang="cv" data-title="Хуркайăк Çулĕ" data-language-autonym="Чӑвашла" data-language-local-name="Chuvash" class="interlanguage-link-target">Чӑвашла</a></li><li class="interlanguage-link interwiki-cs mw-list-item"><a href="https://cs.wikipedia.org/wiki/Galaxie_Ml%C3%A9%C4%8Dn%C3%A1_dr%C3%A1ha" title="Galaxie Mléčná dráha – Czech" lang="cs" hreflang="cs" data-title="Galaxie Mléčná dráha" data-language-autonym="Čeština" data-language-local-name="Czech" class="interlanguage-link-target">Čeština</a></li><li class="interlanguage-link interwiki-sn mw-list-item"><a href="https://sn.wikipedia.org/wiki/Gwara_raKurumbi" title="Gwara raKurumbi – Shona" lang="sn" hreflang="sn" data-title="Gwara raKurumbi" data-language-autonym="ChiShona" data-language-local-name="Shona" class="interlanguage-link-target">ChiShona</a></li><li class="interlanguage-link interwiki-co mw-list-item"><a href="https://co.wikipedia.org/wiki/Strada_di_Roma" title="Strada di Roma – Corsican" lang="co" hreflang="co" data-title="Strada di Roma" data-language-autonym="Corsu" data-language-local-name="Corsican" class="interlanguage-link-target">Corsu</a></li><li class="interlanguage-link interwiki-cy mw-list-item"><a href="https://cy.wikipedia.org/wiki/Galaeth_y_Llwybr_Llaethog" title="Galaeth y Llwybr Llaethog – Welsh" lang="cy" hreflang="cy" data-title="Galaeth y Llwybr Llaethog" data-language-autonym="Cymraeg" data-language-local-name="Welsh" class="interlanguage-link-target">Cymraeg</a></li><li class="interlanguage-link interwiki-da mw-list-item"><a href="https://da.wikipedia.org/wiki/M%C3%A6lkevejen" title="Mælkevejen – Danish" lang="da" hreflang="da" data-title="Mælkevejen" data-language-autonym="Dansk" data-language-local-name="Danish" class="interlanguage-link-target">Dansk</a></li><li class="interlanguage-link interwiki-ary mw-list-item"><a href="https://ary.wikipedia.org/wiki/%D9%85%D8%AC%D8%B1_%D9%84%D9%83%D8%A8%D8%B4" title="مجر لكبش – Moroccan Arabic" lang="ary" hreflang="ary" data-title="مجر لكبش" data-language-autonym="الدارجة" data-language-local-name="Moroccan Arabic" class="interlanguage-link-target">الدارجة</a></li><li class="interlanguage-link interwiki-de badge-Q17437798 badge-goodarticle mw-list-item" title="good article badge"><a href="https://de.wikipedia.org/wiki/Milchstra%C3%9Fe" title="Milchstraße – German" lang="de" hreflang="de" data-title="Milchstraße" data-language-autonym="Deutsch" data-language-local-name="German" class="interlanguage-link-target">Deutsch</a></li><li class="interlanguage-link interwiki-et mw-list-item"><a href="https://et.wikipedia.org/wiki/Linnutee" title="Linnutee – Estonian" lang="et" hreflang="et" data-title="Linnutee" data-language-autonym="Eesti" data-language-local-name="Estonian" class="interlanguage-link-target">Eesti</a></li><li class="interlanguage-link interwiki-el mw-list-item"><a href="https://el.wikipedia.org/wiki/%CE%93%CE%B1%CE%BB%CE%B1%CE%BE%CE%AF%CE%B1%CF%82" title="Γαλαξίας – Greek" lang="el" hreflang="el" data-title="Γαλαξίας" data-language-autonym="Ελληνικά" data-language-local-name="Greek" class="interlanguage-link-target">Ελληνικά</a></li><li class="interlanguage-link interwiki-es mw-list-item"><a href="https://es.wikipedia.org/wiki/V%C3%ADa_L%C3%A1ctea" title="Vía Láctea – Spanish" lang="es" hreflang="es" data-title="Vía Láctea" data-language-autonym="Español" data-language-local-name="Spanish" class="interlanguage-link-target">Español</a></li><li class="interlanguage-link interwiki-eo mw-list-item"><a href="https://eo.wikipedia.org/wiki/Lakta_Vojo" title="Lakta Vojo – Esperanto" lang="eo" hreflang="eo" data-title="Lakta Vojo" data-language-autonym="Esperanto" data-language-local-name="Esperanto" class="interlanguage-link-target">Esperanto</a></li><li class="interlanguage-link interwiki-eu mw-list-item"><a href="https://eu.wikipedia.org/wiki/Esne_Bidea" title="Esne Bidea – Basque" lang="eu" hreflang="eu" data-title="Esne Bidea" data-language-autonym="Euskara" data-language-local-name="Basque" class="interlanguage-link-target">Euskara</a></li><li class="interlanguage-link interwiki-fa mw-list-item"><a href="https://fa.wikipedia.org/wiki/%D8%B1%D8%A7%D9%87_%D8%B4%DB%8C%D8%B1%DB%8C" title="راه شیری – Persian" lang="fa" hreflang="fa" data-title="راه شیری" data-language-autonym="فارسی" data-language-local-name="Persian" class="interlanguage-link-target">فارسی</a></li><li class="interlanguage-link interwiki-hif mw-list-item"><a href="https://hif.wikipedia.org/wiki/Milky_Way" title="Milky Way – Fiji Hindi" lang="hif" hreflang="hif" data-title="Milky Way" data-language-autonym="Fiji Hindi" data-language-local-name="Fiji Hindi" class="interlanguage-link-target">Fiji Hindi</a></li><li class="interlanguage-link interwiki-fr badge-Q17437798 badge-goodarticle mw-list-item" title="good article badge"><a href="https://fr.wikipedia.org/wiki/Voie_lact%C3%A9e" title="Voie lactée – French" lang="fr" hreflang="fr" data-title="Voie lactée" data-language-autonym="Français" data-language-local-name="French" class="interlanguage-link-target">Français</a></li><li class="interlanguage-link interwiki-fy mw-list-item"><a href="https://fy.wikipedia.org/wiki/Molkewei" title="Molkewei – Western Frisian" lang="fy" hreflang="fy" data-title="Molkewei" data-language-autonym="Frysk" data-language-local-name="Western Frisian" class="interlanguage-link-target">Frysk</a></li><li class="interlanguage-link interwiki-ga mw-list-item"><a href="https://ga.wikipedia.org/wiki/Bealach_na_B%C3%B3_Finne" title="Bealach na Bó Finne – Irish" lang="ga" hreflang="ga" data-title="Bealach na Bó Finne" data-language-autonym="Gaeilge" data-language-local-name="Irish" class="interlanguage-link-target">Gaeilge</a></li><li class="interlanguage-link interwiki-gv mw-list-item"><a href="https://gv.wikipedia.org/wiki/Raad_Mooar_Gorree" title="Raad Mooar Gorree – Manx" lang="gv" hreflang="gv" data-title="Raad Mooar Gorree" data-language-autonym="Gaelg" data-language-local-name="Manx" class="interlanguage-link-target">Gaelg</a></li><li class="interlanguage-link interwiki-gd mw-list-item"><a href="https://gd.wikipedia.org/wiki/Slighe_Chloinn_Uisnich" title="Slighe Chloinn Uisnich – Scottish Gaelic" lang="gd" hreflang="gd" data-title="Slighe Chloinn Uisnich" data-language-autonym="Gàidhlig" data-language-local-name="Scottish Gaelic" class="interlanguage-link-target">Gàidhlig</a></li><li class="interlanguage-link interwiki-gl mw-list-item"><a href="https://gl.wikipedia.org/wiki/V%C3%ADa_L%C3%A1ctea" title="Vía Láctea – Galician" lang="gl" hreflang="gl" data-title="Vía Láctea" data-language-autonym="Galego" data-language-local-name="Galician" class="interlanguage-link-target">Galego</a></li><li class="interlanguage-link interwiki-gu mw-list-item"><a href="https://gu.wikipedia.org/wiki/%E0%AA%86%E0%AA%95%E0%AA%BE%E0%AA%B6%E0%AA%97%E0%AA%82%E0%AA%97%E0%AA%BE" title="આકાશગંગા – Gujarati" lang="gu" hreflang="gu" data-title="આકાશગંગા" data-language-autonym="ગુજરાતી" data-language-local-name="Gujarati" class="interlanguage-link-target">ગુજરાતી</a></li><li class="interlanguage-link interwiki-hak mw-list-item"><a href="https://hak.wikipedia.org/wiki/Ngi%C3%B9n-h%C3%B2" title="Ngiùn-hò – Hakka Chinese" lang="hak" hreflang="hak" data-title="Ngiùn-hò" data-language-autonym="客家語 / Hak-kâ-ngî" data-language-local-name="Hakka Chinese" class="interlanguage-link-target">客家語 / Hak-kâ-ngî</a></li><li class="interlanguage-link interwiki-ko mw-list-item"><a href="https://ko.wikipedia.org/wiki/%EC%9A%B0%EB%A6%AC_%EC%9D%80%ED%95%98" title="우리 은하 – Korean" lang="ko" hreflang="ko" data-title="우리 은하" data-language-autonym="한국어" data-language-local-name="Korean" class="interlanguage-link-target">한국어</a></li><li class="interlanguage-link interwiki-haw mw-list-item"><a href="https://haw.wikipedia.org/wiki/H%C5%8Dk%C5%ABnohoaupuni" title="Hōkūnohoaupuni – Hawaiian" lang="haw" hreflang="haw" data-title="Hōkūnohoaupuni" data-language-autonym="Hawaiʻi" data-language-local-name="Hawaiian" class="interlanguage-link-target">Hawaiʻi</a></li><li class="interlanguage-link interwiki-hy mw-list-item"><a href="https://hy.wikipedia.org/wiki/%D4%BE%D5%AB%D6%80_%D4%BF%D5%A1%D5%A9%D5%AB%D5%B6" title="Ծիր Կաթին – Armenian" lang="hy" hreflang="hy" data-title="Ծիր Կաթին" data-language-autonym="Հայերեն" data-language-local-name="Armenian" class="interlanguage-link-target">Հայերեն</a></li><li class="interlanguage-link interwiki-hi mw-list-item"><a href="https://hi.wikipedia.org/wiki/%E0%A4%86%E0%A4%95%E0%A4%BE%E0%A4%B6%E0%A4%97%E0%A4%82%E0%A4%97%E0%A4%BE" title="आकाशगंगा – Hindi" lang="hi" hreflang="hi" data-title="आकाशगंगा" data-language-autonym="हिन्दी" data-language-local-name="Hindi" class="interlanguage-link-target">हिन्दी</a></li><li class="interlanguage-link interwiki-hr mw-list-item"><a href="https://hr.wikipedia.org/wiki/Mlije%C4%8Dni_put" title="Mliječni put – Croatian" lang="hr" hreflang="hr" data-title="Mliječni put" data-language-autonym="Hrvatski" data-language-local-name="Croatian" class="interlanguage-link-target">Hrvatski</a></li><li class="interlanguage-link interwiki-io mw-list-item"><a href="https://io.wikipedia.org/wiki/Lakto-Voyo" title="Lakto-Voyo – Ido" lang="io" hreflang="io" data-title="Lakto-Voyo" data-language-autonym="Ido" data-language-local-name="Ido" class="interlanguage-link-target">Ido</a></li><li class="interlanguage-link interwiki-ilo mw-list-item"><a href="https://ilo.wikipedia.org/wiki/Nagririmpuok_a_Bitbituen" title="Nagririmpuok a Bitbituen – Iloko" lang="ilo" hreflang="ilo" data-title="Nagririmpuok a Bitbituen" data-language-autonym="Ilokano" data-language-local-name="Iloko" class="interlanguage-link-target">Ilokano</a></li><li class="interlanguage-link interwiki-id mw-list-item"><a href="https://id.wikipedia.org/wiki/Bima_Sakti" title="Bima Sakti – Indonesian" lang="id" hreflang="id" data-title="Bima Sakti" data-language-autonym="Bahasa Indonesia" data-language-local-name="Indonesian" class="interlanguage-link-target">Bahasa Indonesia</a></li><li class="interlanguage-link interwiki-ia mw-list-item"><a href="https://ia.wikipedia.org/wiki/Via_Lactee" title="Via Lactee – Interlingua" lang="ia" hreflang="ia" data-title="Via Lactee" data-language-autonym="Interlingua" data-language-local-name="Interlingua" class="interlanguage-link-target">Interlingua</a></li><li class="interlanguage-link interwiki-ie mw-list-item"><a href="https://ie.wikipedia.org/wiki/Via_Galactic" title="Via Galactic – Interlingue" lang="ie" hreflang="ie" data-title="Via Galactic" data-language-autonym="Interlingue" data-language-local-name="Interlingue" class="interlanguage-link-target">Interlingue</a></li><li class="interlanguage-link interwiki-os mw-list-item"><a href="https://os.wikipedia.org/wiki/%C3%86%D1%80%D1%84%C3%A6%D0%BD%D1%8B%D1%84%C3%A6%D0%B4" title="Æрфæныфæд – Ossetic" lang="os" hreflang="os" data-title="Æрфæныфæд" data-language-autonym="Ирон" data-language-local-name="Ossetic" class="interlanguage-link-target">Ирон</a></li><li class="interlanguage-link interwiki-zu mw-list-item"><a href="https://zu.wikipedia.org/wiki/UmZilafasimbe" title="UmZilafasimbe – Zulu" lang="zu" hreflang="zu" data-title="UmZilafasimbe" data-language-autonym="IsiZulu" data-language-local-name="Zulu" class="interlanguage-link-target">IsiZulu</a></li><li class="interlanguage-link interwiki-is mw-list-item"><a href="https://is.wikipedia.org/wiki/Vetrarbrautin" title="Vetrarbrautin – Icelandic" lang="is" hreflang="is" data-title="Vetrarbrautin" data-language-autonym="Íslenska" data-language-local-name="Icelandic" class="interlanguage-link-target">Íslenska</a></li><li class="interlanguage-link interwiki-it badge-Q17437796 badge-featuredarticle mw-list-item" title="featured article badge"><a href="https://it.wikipedia.org/wiki/Via_Lattea" title="Via Lattea – Italian" lang="it" hreflang="it" data-title="Via Lattea" data-language-autonym="Italiano" data-language-local-name="Italian" class="interlanguage-link-target">Italiano</a></li><li class="interlanguage-link interwiki-he mw-list-item"><a href="https://he.wikipedia.org/wiki/%D7%A9%D7%91%D7%99%D7%9C_%D7%94%D7%97%D7%9C%D7%91" title="שביל החלב – Hebrew" lang="he" hreflang="he" data-title="שביל החלב" data-language-autonym="עברית" data-language-local-name="Hebrew" class="interlanguage-link-target">עברית</a></li><li class="interlanguage-link interwiki-jv mw-list-item"><a href="https://jv.wikipedia.org/wiki/Bimasekti" title="Bimasekti – Javanese" lang="jv" hreflang="jv" data-title="Bimasekti" data-language-autonym="Jawa" data-language-local-name="Javanese" class="interlanguage-link-target">Jawa</a></li><li class="interlanguage-link interwiki-kbp mw-list-item"><a href="https://kbp.wikipedia.org/wiki/F%CA%8Awa_lak%C9%A9tee" title="Fʊwa lakɩtee – Kabiye" lang="kbp" hreflang="kbp" data-title="Fʊwa lakɩtee" data-language-autonym="Kabɩyɛ" data-language-local-name="Kabiye" class="interlanguage-link-target">Kabɩyɛ</a></li><li class="interlanguage-link interwiki-kn mw-list-item"><a href="https://kn.wikipedia.org/wiki/%E0%B2%95%E0%B3%8D%E0%B2%B7%E0%B3%80%E0%B2%B0%E0%B2%AA%E0%B2%A5" title="ಕ್ಷೀರಪಥ – Kannada" lang="kn" hreflang="kn" data-title="ಕ್ಷೀರಪಥ" data-language-autonym="ಕನ್ನಡ" data-language-local-name="Kannada" class="interlanguage-link-target">ಕನ್ನಡ</a></li><li class="interlanguage-link interwiki-pam mw-list-item"><a href="https://pam.wikipedia.org/wiki/Milky_Way" title="Milky Way – Pampanga" lang="pam" hreflang="pam" data-title="Milky Way" data-language-autonym="Kapampangan" data-language-local-name="Pampanga" class="interlanguage-link-target">Kapampangan</a></li><li class="interlanguage-link interwiki-krc mw-list-item"><a href="https://krc.wikipedia.org/wiki/%D0%9A%D1%8A%D0%BE%D0%B9_%D0%B4%D0%B6%D0%BE%D0%BB" title="Къой джол – Karachay-Balkar" lang="krc" hreflang="krc" data-title="Къой джол" data-language-autonym="Къарачай-малкъар" data-language-local-name="Karachay-Balkar" class="interlanguage-link-target">Къарачай-малкъар</a></li><li class="interlanguage-link interwiki-ka mw-list-item"><a href="https://ka.wikipedia.org/wiki/%E1%83%98%E1%83%A0%E1%83%9B%E1%83%98%E1%83%A1_%E1%83%9C%E1%83%90%E1%83%AE%E1%83%A2%E1%83%9D%E1%83%9B%E1%83%98" title="ირმის ნახტომი – Georgian" lang="ka" hreflang="ka" data-title="ირმის ნახტომი" data-language-autonym="ქართული" data-language-local-name="Georgian" class="interlanguage-link-target">ქართული</a></li><li class="interlanguage-link interwiki-kk mw-list-item"><a href="https://kk.wikipedia.org/wiki/%D2%9A%D2%B1%D1%81_%D0%B6%D0%BE%D0%BB%D1%8B" title="Құс жолы – Kazakh" lang="kk" hreflang="kk" data-title="Құс жолы" data-language-autonym="Қазақша" data-language-local-name="Kazakh" class="interlanguage-link-target">Қазақша</a></li><li class="interlanguage-link interwiki-kw mw-list-item"><a href="https://kw.wikipedia.org/wiki/Hyns_Sen_Jamys" title="Hyns Sen Jamys – Cornish" lang="kw" hreflang="kw" data-title="Hyns Sen Jamys" data-language-autonym="Kernowek" data-language-local-name="Cornish" class="interlanguage-link-target">Kernowek</a></li><li class="interlanguage-link interwiki-sw mw-list-item"><a href="https://sw.wikipedia.org/wiki/Njia_Nyeupe" title="Njia Nyeupe – Swahili" lang="sw" hreflang="sw" data-title="Njia Nyeupe" data-language-autonym="Kiswahili" data-language-local-name="Swahili" class="interlanguage-link-target">Kiswahili</a></li><li class="interlanguage-link interwiki-ht mw-list-item"><a href="https://ht.wikipedia.org/wiki/Vwa_lakte" title="Vwa lakte – Haitian Creole" lang="ht" hreflang="ht" data-title="Vwa lakte" data-language-autonym="Kreyòl ayisyen" data-language-local-name="Haitian Creole" class="interlanguage-link-target">Kreyòl ayisyen</a></li><li class="interlanguage-link interwiki-gcr mw-list-item"><a href="https://gcr.wikipedia.org/wiki/Vwa_lakt%C3%A9" title="Vwa lakté – Guianan Creole" lang="gcr" hreflang="gcr" data-title="Vwa lakté" data-language-autonym="Kriyòl gwiyannen" data-language-local-name="Guianan Creole" class="interlanguage-link-target">Kriyòl gwiyannen</a></li><li class="interlanguage-link interwiki-ku mw-list-item"><a href="https://ku.wikipedia.org/wiki/Kadiz" title="Kadiz – Kurdish" lang="ku" hreflang="ku" data-title="Kadiz" data-language-autonym="Kurdî" data-language-local-name="Kurdish" class="interlanguage-link-target">Kurdî</a></li><li class="interlanguage-link interwiki-ky mw-list-item"><a href="https://ky.wikipedia.org/wiki/%D0%A1%D0%B0%D0%BC%D0%B0%D0%BD%D1%87%D1%8B%D0%BD%D1%8B%D0%BD_%D0%B6%D0%BE%D0%BB%D1%83" title="Саманчынын жолу – Kyrgyz" lang="ky" hreflang="ky" data-title="Саманчынын жолу" data-language-autonym="Кыргызча" data-language-local-name="Kyrgyz" class="interlanguage-link-target">Кыргызча</a></li><li class="interlanguage-link interwiki-lld mw-list-item"><a href="https://lld.wikipedia.org/wiki/Strada_dl_lat" title="Strada dl lat – Ladin" lang="lld" hreflang="lld" data-title="Strada dl lat" data-language-autonym="Ladin" data-language-local-name="Ladin" class="interlanguage-link-target">Ladin</a></li><li class="interlanguage-link interwiki-lo mw-list-item"><a href="https://lo.wikipedia.org/wiki/%E0%BA%97%E0%BA%B2%E0%BA%87%E0%BA%8A%E0%BB%89%E0%BA%B2%E0%BA%87%E0%BB%80%E0%BA%9C%E0%BA%B7%E0%BA%AD%E0%BA%81" title="ທາງຊ້າງເຜືອກ – Lao" lang="lo" hreflang="lo" data-title="ທາງຊ້າງເຜືອກ" data-language-autonym="ລາວ" data-language-local-name="Lao" class="interlanguage-link-target">ລາວ</a></li><li class="interlanguage-link interwiki-la mw-list-item"><a href="https://la.wikipedia.org/wiki/Via_lactea" title="Via lactea – Latin" lang="la" hreflang="la" data-title="Via lactea" data-language-autonym="Latina" data-language-local-name="Latin" class="interlanguage-link-target">Latina</a></li><li class="interlanguage-link interwiki-lv mw-list-item"><a href="https://lv.wikipedia.org/wiki/Piena_Ce%C4%BC%C5%A1" title="Piena Ceļš – Latvian" lang="lv" hreflang="lv" data-title="Piena Ceļš" data-language-autonym="Latviešu" data-language-local-name="Latvian" class="interlanguage-link-target">Latviešu</a></li><li class="interlanguage-link interwiki-lb mw-list-item"><a href="https://lb.wikipedia.org/wiki/M%C3%ABllechstrooss" title="Mëllechstrooss – Luxembourgish" lang="lb" hreflang="lb" data-title="Mëllechstrooss" data-language-autonym="Lëtzebuergesch" data-language-local-name="Luxembourgish" class="interlanguage-link-target">Lëtzebuergesch</a></li><li class="interlanguage-link interwiki-lez mw-list-item"><a href="https://lez.wikipedia.org/wiki/%D0%9A%D0%B0%D1%80%D0%B2%D0%B0%D0%BD%D0%B4_%D0%A0%D0%B5%D1%85%D1%8A" title="Карванд Рехъ – Lezghian" lang="lez" hreflang="lez" data-title="Карванд Рехъ" data-language-autonym="Лезги" data-language-local-name="Lezghian" class="interlanguage-link-target">Лезги</a></li><li class="interlanguage-link interwiki-lt mw-list-item"><a href="https://lt.wikipedia.org/wiki/Pauk%C5%A1%C4%8Di%C5%B3_Takas" title="Paukščių Takas – Lithuanian" lang="lt" hreflang="lt" data-title="Paukščių Takas" data-language-autonym="Lietuvių" data-language-local-name="Lithuanian" class="interlanguage-link-target">Lietuvių</a></li><li class="interlanguage-link interwiki-li mw-list-item"><a href="https://li.wikipedia.org/wiki/M%C3%A8lkweeg" title="Mèlkweeg – Limburgish" lang="li" hreflang="li" data-title="Mèlkweeg" data-language-autonym="Limburgs" data-language-local-name="Limburgish" class="interlanguage-link-target">Limburgs</a></li><li class="interlanguage-link interwiki-lfn mw-list-item"><a href="https://lfn.wikipedia.org/wiki/Via_Letin" title="Via Letin – Lingua Franca Nova" lang="lfn" hreflang="lfn" data-title="Via Letin" data-language-autonym="Lingua Franca Nova" data-language-local-name="Lingua Franca Nova" class="interlanguage-link-target">Lingua Franca Nova</a></li><li class="interlanguage-link interwiki-lmo mw-list-item"><a href="https://lmo.wikipedia.org/wiki/Via_L%C3%A0tea" title="Via Làtea – Lombard" lang="lmo" hreflang="lmo" data-title="Via Làtea" data-language-autonym="Lombard" data-language-local-name="Lombard" class="interlanguage-link-target">Lombard</a></li><li class="interlanguage-link interwiki-hu mw-list-item"><a href="https://hu.wikipedia.org/wiki/Tej%C3%BAtrendszer" title="Tejútrendszer – Hungarian" lang="hu" hreflang="hu" data-title="Tejútrendszer" data-language-autonym="Magyar" data-language-local-name="Hungarian" class="interlanguage-link-target">Magyar</a></li><li class="interlanguage-link interwiki-mk mw-list-item"><a href="https://mk.wikipedia.org/wiki/%D0%9C%D0%BB%D0%B5%D1%87%D0%B5%D0%BD_%D0%9F%D0%B0%D1%82" title="Млечен Пат – Macedonian" lang="mk" hreflang="mk" data-title="Млечен Пат" data-language-autonym="Македонски" data-language-local-name="Macedonian" class="interlanguage-link-target">Македонски</a></li><li class="interlanguage-link interwiki-ml mw-list-item"><a href="https://ml.wikipedia.org/wiki/%E0%B4%86%E0%B4%95%E0%B4%BE%E0%B4%B6%E0%B4%97%E0%B4%82%E0%B4%97" title="ആകാശഗംഗ – Malayalam" lang="ml" hreflang="ml" data-title="ആകാശഗംഗ" data-language-autonym="മലയാളം" data-language-local-name="Malayalam" class="interlanguage-link-target">മലയാളം</a></li><li class="interlanguage-link interwiki-mt mw-list-item"><a href="https://mt.wikipedia.org/wiki/Triq_ta%27_Sant%27Anna" title="Triq ta' Sant'Anna – Maltese" lang="mt" hreflang="mt" data-title="Triq ta' Sant'Anna" data-language-autonym="Malti" data-language-local-name="Maltese" class="interlanguage-link-target">Malti</a></li><li class="interlanguage-link interwiki-mr mw-list-item"><a href="https://mr.wikipedia.org/wiki/%E0%A4%86%E0%A4%95%E0%A4%BE%E0%A4%B6%E0%A4%97%E0%A4%82%E0%A4%97%E0%A4%BE" title="आकाशगंगा – Marathi" lang="mr" hreflang="mr" data-title="आकाशगंगा" data-language-autonym="मराठी" data-language-local-name="Marathi" class="interlanguage-link-target">मराठी</a></li><li class="interlanguage-link interwiki-xmf mw-list-item"><a href="https://xmf.wikipedia.org/wiki/%E1%83%9B%E1%83%94%E1%83%A8%E1%83%AE%E1%83%A3%E1%83%A0%E1%83%94%E1%83%A8_%E1%83%A8%E1%83%90%E1%83%A0%E1%83%90" title="მეშხურეშ შარა – Mingrelian" lang="xmf" hreflang="xmf" data-title="მეშხურეშ შარა" data-language-autonym="მარგალური" data-language-local-name="Mingrelian" class="interlanguage-link-target">მარგალური</a></li><li class="interlanguage-link interwiki-arz mw-list-item"><a href="https://arz.wikipedia.org/wiki/%D8%AF%D8%B1%D8%A8_%D8%A7%D9%84%D9%84%D8%A8%D8%A7%D9%86%D9%87" title="درب اللبانه – Egyptian Arabic" lang="arz" hreflang="arz" data-title="درب اللبانه" data-language-autonym="مصرى" data-language-local-name="Egyptian Arabic" class="interlanguage-link-target">مصرى</a></li><li class="interlanguage-link interwiki-ms mw-list-item"><a href="https://ms.wikipedia.org/wiki/Bima_Sakti" title="Bima Sakti – Malay" lang="ms" hreflang="ms" data-title="Bima Sakti" data-language-autonym="Bahasa Melayu" data-language-local-name="Malay" class="interlanguage-link-target">Bahasa Melayu</a></li><li class="interlanguage-link interwiki-min mw-list-item"><a href="https://min.wikipedia.org/wiki/Bima_Sakti" title="Bima Sakti – Minangkabau" lang="min" hreflang="min" data-title="Bima Sakti" data-language-autonym="Minangkabau" data-language-local-name="Minangkabau" class="interlanguage-link-target">Minangkabau</a></li><li class="interlanguage-link interwiki-cdo mw-list-item"><a href="https://cdo.wikipedia.org/wiki/Ti%C4%95ng-%C3%B2%CC%A4" title="Tiĕng-ò̤ – Mindong" lang="cdo" hreflang="cdo" data-title="Tiĕng-ò̤" data-language-autonym="閩東語 / Mìng-dĕ̤ng-ngṳ̄" data-language-local-name="Mindong" class="interlanguage-link-target">閩東語 / Mìng-dĕ̤ng-ngṳ̄</a></li><li class="interlanguage-link interwiki-mwl mw-list-item"><a href="https://mwl.wikipedia.org/wiki/Carril_de_Santiago" title="Carril de Santiago – Mirandese" lang="mwl" hreflang="mwl" data-title="Carril de Santiago" data-language-autonym="Mirandés" data-language-local-name="Mirandese" class="interlanguage-link-target">Mirandés</a></li><li class="interlanguage-link interwiki-mn mw-list-item"><a href="https://mn.wikipedia.org/wiki/%D0%A2%D1%8D%D0%BD%D0%B3%D1%8D%D1%80%D0%B8%D0%B9%D0%BD_%D0%B7%D0%B0%D0%B0%D0%B4%D0%B0%D1%81" title="Тэнгэрийн заадас – Mongolian" lang="mn" hreflang="mn" data-title="Тэнгэрийн заадас" data-language-autonym="Монгол" data-language-local-name="Mongolian" class="interlanguage-link-target">Монгол</a></li><li class="interlanguage-link interwiki-my mw-list-item"><a href="https://my.wikipedia.org/wiki/%E1%80%94%E1%80%82%E1%80%AB%E1%80%B8%E1%80%84%E1%80%BD%E1%80%B1%E1%80%B7%E1%80%90%E1%80%94%E1%80%BA%E1%80%B8_%E1%80%82%E1%80%9A%E1%80%BA%E1%80%9C%E1%80%80%E1%80%BA%E1%80%86%E1%80%AE" title="နဂါးငွေ့တန်း ဂယ်လက်ဆီ – Burmese" lang="my" hreflang="my" data-title="နဂါးငွေ့တန်း ဂယ်လက်ဆီ" data-language-autonym="မြန်မာဘာသာ" data-language-local-name="Burmese" class="interlanguage-link-target">မြန်မာဘာသာ</a></li><li class="interlanguage-link interwiki-nah mw-list-item"><a href="https://nah.wikipedia.org/wiki/Citlalin_icue" title="Citlalin icue – Nahuatl" lang="nah" hreflang="nah" data-title="Citlalin icue" data-language-autonym="Nāhuatl" data-language-local-name="Nahuatl" class="interlanguage-link-target">Nāhuatl</a></li><li class="interlanguage-link interwiki-fj mw-list-item"><a href="https://fj.wikipedia.org/wiki/Maliwa_sucusucuya" title="Maliwa sucusucuya – Fijian" lang="fj" hreflang="fj" data-title="Maliwa sucusucuya" data-language-autonym="Na Vosa Vakaviti" data-language-local-name="Fijian" class="interlanguage-link-target">Na Vosa Vakaviti</a></li><li class="interlanguage-link interwiki-nl mw-list-item"><a href="https://nl.wikipedia.org/wiki/Melkweg_(sterrenstelsel)" title="Melkweg (sterrenstelsel) – Dutch" lang="nl" hreflang="nl" data-title="Melkweg (sterrenstelsel)" data-language-autonym="Nederlands" data-language-local-name="Dutch" class="interlanguage-link-target">Nederlands</a></li><li class="interlanguage-link interwiki-nds-nl mw-list-item"><a href="https://nds-nl.wikipedia.org/wiki/Melkweg_(sternstelsel)" title="Melkweg (sternstelsel) – Low Saxon" lang="nds-NL" hreflang="nds-NL" data-title="Melkweg (sternstelsel)" data-language-autonym="Nedersaksies" data-language-local-name="Low Saxon" class="interlanguage-link-target">Nedersaksies</a></li><li class="interlanguage-link interwiki-ne mw-list-item"><a href="https://ne.wikipedia.org/wiki/%E0%A4%86%E0%A4%95%E0%A4%BE%E0%A4%B6%E0%A4%97%E0%A4%99%E0%A5%8D%E0%A4%97%E0%A4%BE" title="आकाशगङ्गा – Nepali" lang="ne" hreflang="ne" data-title="आकाशगङ्गा" data-language-autonym="नेपाली" data-language-local-name="Nepali" class="interlanguage-link-target">नेपाली</a></li><li class="interlanguage-link interwiki-new mw-list-item"><a href="https://new.wikipedia.org/wiki/%E0%A4%AE%E0%A4%BF%E0%A4%B2%E0%A5%8D%E0%A4%95%E0%A5%80_%E0%A4%B5%E0%A5%87" title="मिल्की वे – Newari" lang="new" hreflang="new" data-title="मिल्की वे" data-language-autonym="नेपाल भाषा" data-language-local-name="Newari" class="interlanguage-link-target">नेपाल भाषा</a></li><li class="interlanguage-link interwiki-ja mw-list-item"><a href="https://ja.wikipedia.org/wiki/%E9%8A%80%E6%B2%B3%E7%B3%BB" title="銀河系 – Japanese" lang="ja" hreflang="ja" data-title="銀河系" data-language-autonym="日本語" data-language-local-name="Japanese" class="interlanguage-link-target">日本語</a></li><li class="interlanguage-link interwiki-ce mw-list-item"><a href="https://ce.wikipedia.org/wiki/%D0%A7%D0%B0%D1%82%D0%B0%D0%BA%D1%85%D0%B8%D0%B9%D0%BD%D0%B0_%D1%82%D0%B0%D1%87%D0%B0" title="Чатакхийна тача – Chechen" lang="ce" hreflang="ce" data-title="Чатакхийна тача" data-language-autonym="Нохчийн" data-language-local-name="Chechen" class="interlanguage-link-target">Нохчийн</a></li><li class="interlanguage-link interwiki-frr mw-list-item"><a href="https://frr.wikipedia.org/wiki/Moolkstruat" title="Moolkstruat – Northern Frisian" lang="frr" hreflang="frr" data-title="Moolkstruat" data-language-autonym="Nordfriisk" data-language-local-name="Northern Frisian" class="interlanguage-link-target">Nordfriisk</a></li><li class="interlanguage-link interwiki-no mw-list-item"><a href="https://no.wikipedia.org/wiki/Melkeveien" title="Melkeveien – Norwegian Bokmål" lang="nb" hreflang="nb" data-title="Melkeveien" data-language-autonym="Norsk bokmål" data-language-local-name="Norwegian Bokmål" class="interlanguage-link-target">Norsk bokmål</a></li><li class="interlanguage-link interwiki-nn mw-list-item"><a href="https://nn.wikipedia.org/wiki/Mj%C3%B8lkevegen" title="Mjølkevegen – Norwegian Nynorsk" lang="nn" hreflang="nn" data-title="Mjølkevegen" data-language-autonym="Norsk nynorsk" data-language-local-name="Norwegian Nynorsk" class="interlanguage-link-target">Norsk nynorsk</a></li><li class="interlanguage-link interwiki-nrm mw-list-item"><a href="https://nrm.wikipedia.org/wiki/C%27m%C3%AEns_d%27Saint_Jacques" title="C'mîns d'Saint Jacques – Norman" lang="nrf" hreflang="nrf" data-title="C'mîns d'Saint Jacques" data-language-autonym="Nouormand" data-language-local-name="Norman" class="interlanguage-link-target">Nouormand</a></li><li class="interlanguage-link interwiki-nov mw-list-item"><a href="https://nov.wikipedia.org/wiki/Milke-vie" title="Milke-vie – Novial" lang="nov" hreflang="nov" data-title="Milke-vie" data-language-autonym="Novial" data-language-local-name="Novial" class="interlanguage-link-target">Novial</a></li><li class="interlanguage-link interwiki-oc mw-list-item"><a href="https://oc.wikipedia.org/wiki/Via_Lact%C3%A8a" title="Via Lactèa – Occitan" lang="oc" hreflang="oc" data-title="Via Lactèa" data-language-autonym="Occitan" data-language-local-name="Occitan" class="interlanguage-link-target">Occitan</a></li><li class="interlanguage-link interwiki-mhr mw-list-item"><a href="https://mhr.wikipedia.org/wiki/%D0%9A%D0%B0%D0%B9%D1%8B%D0%BA%D0%BA%D0%BE%D0%BC%D0%B1%D0%BE_%D0%9A%D0%BE%D1%80%D0%BD%D0%BE" title="Кайыккомбо Корно – Eastern Mari" lang="mhr" hreflang="mhr" data-title="Кайыккомбо Корно" data-language-autonym="Олык марий" data-language-local-name="Eastern Mari" class="interlanguage-link-target">Олык марий</a></li><li class="interlanguage-link interwiki-or mw-list-item"><a href="https://or.wikipedia.org/wiki/%E0%AC%86%E0%AC%95%E0%AC%BE%E0%AC%B6%E0%AC%97%E0%AC%99%E0%AD%8D%E0%AC%97%E0%AC%BE" title="ଆକାଶଗଙ୍ଗା – Odia" lang="or" hreflang="or" data-title="ଆକାଶଗଙ୍ଗା" data-language-autonym="ଓଡ଼ିଆ" data-language-local-name="Odia" class="interlanguage-link-target">ଓଡ଼ିଆ</a></li><li class="interlanguage-link interwiki-om mw-list-item"><a href="https://om.wikipedia.org/wiki/Xurree_Aannannoo" title="Xurree Aannannoo – Oromo" lang="om" hreflang="om" data-title="Xurree Aannannoo" data-language-autonym="Oromoo" data-language-local-name="Oromo" class="interlanguage-link-target">Oromoo</a></li><li class="interlanguage-link interwiki-uz mw-list-item"><a href="https://uz.wikipedia.org/wiki/Somon_yo%CA%BBli" title="Somon yoʻli – Uzbek" lang="uz" hreflang="uz" data-title="Somon yoʻli" data-language-autonym="Oʻzbekcha / ўзбекча" data-language-local-name="Uzbek" class="interlanguage-link-target">Oʻzbekcha / ўзбекча</a></li><li class="interlanguage-link interwiki-pa mw-list-item"><a href="https://pa.wikipedia.org/wiki/%E0%A8%AE%E0%A8%BF%E0%A8%B2%E0%A8%95%E0%A9%80_%E0%A8%B5%E0%A9%87" title="ਮਿਲਕੀ ਵੇ – Punjabi" lang="pa" hreflang="pa" data-title="ਮਿਲਕੀ ਵੇ" data-language-autonym="ਪੰਜਾਬੀ" data-language-local-name="Punjabi" class="interlanguage-link-target">ਪੰਜਾਬੀ</a></li><li class="interlanguage-link interwiki-pnb mw-list-item"><a href="https://pnb.wikipedia.org/wiki/%DA%86%D9%B9%D8%A7_%D8%B1%D8%A7%DB%81" title="چٹا راہ – Western Punjabi" lang="pnb" hreflang="pnb" data-title="چٹا راہ" data-language-autonym="پنجابی" data-language-local-name="Western Punjabi" class="interlanguage-link-target">پنجابی</a></li><li class="interlanguage-link interwiki-ps mw-list-item"><a href="https://ps.wikipedia.org/wiki/%D8%AF_%D8%B4%DB%8C%D8%AF%D9%88_%D9%84%D8%A7%D8%B1" title="د شیدو لار – Pashto" lang="ps" hreflang="ps" data-title="د شیدو لار" data-language-autonym="پښتو" data-language-local-name="Pashto" class="interlanguage-link-target">پښتو</a></li><li class="interlanguage-link interwiki-jam mw-list-item"><a href="https://jam.wikipedia.org/wiki/Milki_Wie" title="Milki Wie – Jamaican Creole English" lang="jam" hreflang="jam" data-title="Milki Wie" data-language-autonym="Patois" data-language-local-name="Jamaican Creole English" class="interlanguage-link-target">Patois</a></li><li class="interlanguage-link interwiki-km mw-list-item"><a href="https://km.wikipedia.org/wiki/%E1%9E%80%E1%9E%96%E1%9F%92%E1%9E%85%E1%9E%BB%E1%9F%86%E1%9E%B6%E1%9E%95%E1%9F%92%E1%9E%80%E1%9E%B6%E1%9E%99%E1%9E%87%E1%9E%BE%E1%9E%84%E1%9E%97%E1%9F%92%E1%9E%93%E1%9E%B6%E1%9E%99" title="កព្ចុំាផ្កាយជើងភ្នាយ – Khmer" lang="km" hreflang="km" data-title="កព្ចុំាផ្កាយជើងភ្នាយ" data-language-autonym="ភាសាខ្មែរ" data-language-local-name="Khmer" class="interlanguage-link-target">ភាសាខ្មែរ</a></li><li class="interlanguage-link interwiki-pcd mw-list-item"><a href="https://pcd.wikipedia.org/wiki/Voe_lact%C3%A9e" title="Voe lactée – Picard" lang="pcd" hreflang="pcd" data-title="Voe lactée" data-language-autonym="Picard" data-language-local-name="Picard" class="interlanguage-link-target">Picard</a></li><li class="interlanguage-link interwiki-pms mw-list-item"><a href="https://pms.wikipedia.org/wiki/Stra_%C3%ABd_San_Giaco" title="Stra ëd San Giaco – Piedmontese" lang="pms" hreflang="pms" data-title="Stra ëd San Giaco" data-language-autonym="Piemontèis" data-language-local-name="Piedmontese" class="interlanguage-link-target">Piemontèis</a></li><li class="interlanguage-link interwiki-nds mw-list-item"><a href="https://nds.wikipedia.org/wiki/Melkstraat" title="Melkstraat – Low German" lang="nds" hreflang="nds" data-title="Melkstraat" data-language-autonym="Plattdüütsch" data-language-local-name="Low German" class="interlanguage-link-target">Plattdüütsch</a></li><li class="interlanguage-link interwiki-pl mw-list-item"><a href="https://pl.wikipedia.org/wiki/Droga_Mleczna" title="Droga Mleczna – Polish" lang="pl" hreflang="pl" data-title="Droga Mleczna" data-language-autonym="Polski" data-language-local-name="Polish" class="interlanguage-link-target">Polski</a></li><li class="interlanguage-link interwiki-pt badge-Q17437796 badge-featuredarticle mw-list-item" title="featured article badge"><a href="https://pt.wikipedia.org/wiki/Via_L%C3%A1ctea" title="Via Láctea – Portuguese" lang="pt" hreflang="pt" data-title="Via Láctea" data-language-autonym="Português" data-language-local-name="Portuguese" class="interlanguage-link-target">Português</a></li><li class="interlanguage-link interwiki-crh mw-list-item"><a href="https://crh.wikipedia.org/wiki/K%C3%A2be_yolu" title="Kâbe yolu – Crimean Tatar" lang="crh" hreflang="crh" data-title="Kâbe yolu" data-language-autonym="Qırımtatarca" data-language-local-name="Crimean Tatar" class="interlanguage-link-target">Qırımtatarca</a></li><li class="interlanguage-link interwiki-ksh mw-list-item"><a href="https://ksh.wikipedia.org/wiki/Melechstroa%C3%9F" title="Melechstroaß – Colognian" lang="ksh" hreflang="ksh" data-title="Melechstroaß" data-language-autonym="Ripoarisch" data-language-local-name="Colognian" class="interlanguage-link-target">Ripoarisch</a></li><li class="interlanguage-link interwiki-ro mw-list-item"><a href="https://ro.wikipedia.org/wiki/Calea_Lactee" title="Calea Lactee – Romanian" lang="ro" hreflang="ro" data-title="Calea Lactee" data-language-autonym="Română" data-language-local-name="Romanian" class="interlanguage-link-target">Română</a></li><li class="interlanguage-link interwiki-rmy mw-list-item"><a href="https://rmy.wikipedia.org/wiki/Pharnovon" title="Pharnovon – Vlax Romani" lang="rmy" hreflang="rmy" data-title="Pharnovon" data-language-autonym="Romani čhib" data-language-local-name="Vlax Romani" class="interlanguage-link-target">Romani čhib</a></li><li class="interlanguage-link interwiki-qu mw-list-item"><a href="https://qu.wikipedia.org/wiki/Qullqaquyllur" title="Qullqaquyllur – Quechua" lang="qu" hreflang="qu" data-title="Qullqaquyllur" data-language-autonym="Runa Simi" data-language-local-name="Quechua" class="interlanguage-link-target">Runa Simi</a></li><li class="interlanguage-link interwiki-rue mw-list-item"><a href="https://rue.wikipedia.org/wiki/%D0%9C%D0%BE%D0%BB%D0%BE%D1%87%D0%BD%D0%B0_%D0%B4%D0%BE%D1%80%D0%BE%D0%B3%D0%B0" title="Молочна дорога – Rusyn" lang="rue" hreflang="rue" data-title="Молочна дорога" data-language-autonym="Русиньскый" data-language-local-name="Rusyn" class="interlanguage-link-target">Русиньскый</a></li><li class="interlanguage-link interwiki-ru badge-Q17437796 badge-featuredarticle mw-list-item" title="featured article badge"><a href="https://ru.wikipedia.org/wiki/%D0%9C%D0%BB%D0%B5%D1%87%D0%BD%D1%8B%D0%B9_%D0%9F%D1%83%D1%82%D1%8C" title="Млечный Путь – Russian" lang="ru" hreflang="ru" data-title="Млечный Путь" data-language-autonym="Русский" data-language-local-name="Russian" class="interlanguage-link-target">Русский</a></li><li class="interlanguage-link interwiki-sah mw-list-item"><a href="https://sah.wikipedia.org/wiki/%D0%A5%D0%B0%D0%BB%D0%BB%D0%B0%D0%B0%D0%BD_%D0%A1%D0%B8%D0%B8%D0%B3%D1%8D" title="Халлаан Сиигэ – Yakut" lang="sah" hreflang="sah" data-title="Халлаан Сиигэ" data-language-autonym="Саха тыла" data-language-local-name="Yakut" class="interlanguage-link-target">Саха тыла</a></li><li class="interlanguage-link interwiki-sa mw-list-item"><a href="https://sa.wikipedia.org/wiki/%E0%A4%95%E0%A5%8D%E0%A4%B7%E0%A5%80%E0%A4%B0%E0%A4%AA%E0%A4%A5-%E0%A4%86%E0%A4%95%E0%A4%BE%E0%A4%B6%E0%A4%97%E0%A4%99%E0%A5%8D%E0%A4%97%E0%A4%BE" title="क्षीरपथ-आकाशगङ्गा – Sanskrit" lang="sa" hreflang="sa" data-title="क्षीरपथ-आकाशगङ्गा" data-language-autonym="संस्कृतम्" data-language-local-name="Sanskrit" class="interlanguage-link-target">संस्कृतम्</a></li><li class="interlanguage-link interwiki-sat mw-list-item"><a href="https://sat.wikipedia.org/wiki/%E1%B1%9B%E1%B1%B3%E1%B1%A3%E1%B1%9F_%E1%B1%B0%E1%B1%9F%E1%B1%A6%E1%B1%9F%E1%B1%A8" title="ᱛᱳᱣᱟ ᱰᱟᱦᱟᱨ – Santali" lang="sat" hreflang="sat" data-title="ᱛᱳᱣᱟ ᱰᱟᱦᱟᱨ" data-language-autonym="ᱥᱟᱱᱛᱟᱲᱤ" data-language-local-name="Santali" class="interlanguage-link-target">ᱥᱟᱱᱛᱟᱲᱤ</a></li><li class="interlanguage-link interwiki-sc mw-list-item"><a href="https://sc.wikipedia.org/wiki/Camminu_de_paza" title="Camminu de paza – Sardinian" lang="sc" hreflang="sc" data-title="Camminu de paza" data-language-autonym="Sardu" data-language-local-name="Sardinian" class="interlanguage-link-target">Sardu</a></li><li class="interlanguage-link interwiki-sco mw-list-item"><a href="https://sco.wikipedia.org/wiki/Vatlant_Streit" title="Vatlant Streit – Scots" lang="sco" hreflang="sco" data-title="Vatlant Streit" data-language-autonym="Scots" data-language-local-name="Scots" class="interlanguage-link-target">Scots</a></li><li class="interlanguage-link interwiki-stq mw-list-item"><a href="https://stq.wikipedia.org/wiki/Molkstr%C3%A4ite" title="Molksträite – Saterland Frisian" lang="stq" hreflang="stq" data-title="Molksträite" data-language-autonym="Seeltersk" data-language-local-name="Saterland Frisian" class="interlanguage-link-target">Seeltersk</a></li><li class="interlanguage-link interwiki-sq mw-list-item"><a href="https://sq.wikipedia.org/wiki/Hyjplimja" title="Hyjplimja – Albanian" lang="sq" hreflang="sq" data-title="Hyjplimja" data-language-autonym="Shqip" data-language-local-name="Albanian" class="interlanguage-link-target">Shqip</a></li><li class="interlanguage-link interwiki-scn mw-list-item"><a href="https://scn.wikipedia.org/wiki/Jolu_di_San_J%C3%A0bbucu" title="Jolu di San Jàbbucu – Sicilian" lang="scn" hreflang="scn" data-title="Jolu di San Jàbbucu" data-language-autonym="Sicilianu" data-language-local-name="Sicilian" class="interlanguage-link-target">Sicilianu</a></li><li class="interlanguage-link interwiki-si mw-list-item"><a href="https://si.wikipedia.org/wiki/%E0%B6%9A%E0%B7%8A%E0%B7%82%E0%B7%93%E0%B6%BB_%E0%B6%B4%E0%B6%AE%E0%B6%BA" title="ක්ෂීර පථය – Sinhala" lang="si" hreflang="si" data-title="ක්ෂීර පථය" data-language-autonym="සිංහල" data-language-local-name="Sinhala" class="interlanguage-link-target">සිංහල</a></li><li class="interlanguage-link interwiki-simple mw-list-item"><a href="https://simple.wikipedia.org/wiki/Milky_Way" title="Milky Way – Simple English" lang="en-simple" hreflang="en-simple" data-title="Milky Way" data-language-autonym="Simple English" data-language-local-name="Simple English" class="interlanguage-link-target">Simple English</a></li><li class="interlanguage-link interwiki-sd mw-list-item"><a href="https://sd.wikipedia.org/wiki/%DA%A9%D9%8A%D8%B1%D8%A7%D8%A6%D9%8A%D9%86_%D9%88%D8%A7%D9%BD_%DA%AA%D9%87%DA%AA%D8%B4%D8%A7%D9%86" title="کيرائين واٽ ڪهڪشان – Sindhi" lang="sd" hreflang="sd" data-title="کيرائين واٽ ڪهڪشان" data-language-autonym="سنڌي" data-language-local-name="Sindhi" class="interlanguage-link-target">سنڌي</a></li><li class="interlanguage-link interwiki-sk badge-Q17437798 badge-goodarticle mw-list-item" title="good article badge"><a href="https://sk.wikipedia.org/wiki/Galaxia_(Mlie%C4%8Dna_cesta)" title="Galaxia (Mliečna cesta) – Slovak" lang="sk" hreflang="sk" data-title="Galaxia (Mliečna cesta)" data-language-autonym="Slovenčina" data-language-local-name="Slovak" class="interlanguage-link-target">Slovenčina</a></li><li class="interlanguage-link interwiki-sl mw-list-item"><a href="https://sl.wikipedia.org/wiki/Rimska_cesta_(galaksija)" title="Rimska cesta (galaksija) – Slovenian" lang="sl" hreflang="sl" data-title="Rimska cesta (galaksija)" data-language-autonym="Slovenščina" data-language-local-name="Slovenian" class="interlanguage-link-target">Slovenščina</a></li><li class="interlanguage-link interwiki-ckb mw-list-item"><a href="https://ckb.wikipedia.org/wiki/%DA%95%DB%8E%DA%AF%D8%A7%DB%8C_%D8%B4%DB%8C%D8%B1%DB%8C" title="ڕێگای شیری – Central Kurdish" lang="ckb" hreflang="ckb" data-title="ڕێگای شیری" data-language-autonym="کوردی" data-language-local-name="Central Kurdish" class="interlanguage-link-target">کوردی</a></li><li class="interlanguage-link interwiki-sr mw-list-item"><a href="https://sr.wikipedia.org/wiki/%D0%9C%D0%BB%D0%B5%D1%87%D0%BD%D0%B8_%D0%BF%D1%83%D1%82" title="Млечни пут – Serbian" lang="sr" hreflang="sr" data-title="Млечни пут" data-language-autonym="Српски / srpski" data-language-local-name="Serbian" class="interlanguage-link-target">Српски / srpski</a></li><li class="interlanguage-link interwiki-sh mw-list-item"><a href="https://sh.wikipedia.org/wiki/Mlije%C4%8Dna_staza" title="Mliječna staza – Serbo-Croatian" lang="sh" hreflang="sh" data-title="Mliječna staza" data-language-autonym="Srpskohrvatski / српскохрватски" data-language-local-name="Serbo-Croatian" class="interlanguage-link-target">Srpskohrvatski / српскохрватски</a></li><li class="interlanguage-link interwiki-su mw-list-item"><a href="https://su.wikipedia.org/wiki/Bima_Sakti" title="Bima Sakti – Sundanese" lang="su" hreflang="su" data-title="Bima Sakti" data-language-autonym="Sunda" data-language-local-name="Sundanese" class="interlanguage-link-target">Sunda</a></li><li class="interlanguage-link interwiki-fi badge-Q17559452 badge-recommendedarticle mw-list-item" title="recommended article"><a href="https://fi.wikipedia.org/wiki/Linnunrata" title="Linnunrata – Finnish" lang="fi" hreflang="fi" data-title="Linnunrata" data-language-autonym="Suomi" data-language-local-name="Finnish" class="interlanguage-link-target">Suomi</a></li><li class="interlanguage-link interwiki-sv mw-list-item"><a href="https://sv.wikipedia.org/wiki/Vintergatan" title="Vintergatan – Swedish" lang="sv" hreflang="sv" data-title="Vintergatan" data-language-autonym="Svenska" data-language-local-name="Swedish" class="interlanguage-link-target">Svenska</a></li><li class="interlanguage-link interwiki-tl mw-list-item"><a href="https://tl.wikipedia.org/wiki/Ariwanas" title="Ariwanas – Tagalog" lang="tl" hreflang="tl" data-title="Ariwanas" data-language-autonym="Tagalog" data-language-local-name="Tagalog" class="interlanguage-link-target">Tagalog</a></li><li class="interlanguage-link interwiki-ta mw-list-item"><a href="https://ta.wikipedia.org/wiki/%E0%AE%AA%E0%AE%BE%E0%AE%B2%E0%AF%8D_%E0%AE%B5%E0%AE%B4%E0%AE%BF" title="பால் வழி – Tamil" lang="ta" hreflang="ta" data-title="பால் வழி" data-language-autonym="தமிழ்" data-language-local-name="Tamil" class="interlanguage-link-target">தமிழ்</a></li><li class="interlanguage-link interwiki-kab mw-list-item"><a href="https://kab.wikipedia.org/wiki/Asif_n_igenwan" title="Asif n igenwan – Kabyle" lang="kab" hreflang="kab" data-title="Asif n igenwan" data-language-autonym="Taqbaylit" data-language-local-name="Kabyle" class="interlanguage-link-target">Taqbaylit</a></li><li class="interlanguage-link interwiki-tt mw-list-item"><a href="https://tt.wikipedia.org/wiki/%D0%9A%D0%B8%D0%B5%D0%BA_%D0%9A%D0%B0%D0%B7_%D0%AE%D0%BB%D1%8B" title="Киек Каз Юлы – Tatar" lang="tt" hreflang="tt" data-title="Киек Каз Юлы" data-language-autonym="Татарча / tatarça" data-language-local-name="Tatar" class="interlanguage-link-target">Татарча / tatarça</a></li><li class="interlanguage-link interwiki-te mw-list-item"><a href="https://te.wikipedia.org/wiki/%E0%B0%AA%E0%B0%BE%E0%B0%B2%E0%B0%AA%E0%B1%81%E0%B0%82%E0%B0%A4" title="పాలపుంత – Telugu" lang="te" hreflang="te" data-title="పాలపుంత" data-language-autonym="తెలుగు" data-language-local-name="Telugu" class="interlanguage-link-target">తెలుగు</a></li><li class="interlanguage-link interwiki-th mw-list-item"><a href="https://th.wikipedia.org/wiki/%E0%B8%97%E0%B8%B2%E0%B8%87%E0%B8%8A%E0%B9%89%E0%B8%B2%E0%B8%87%E0%B9%80%E0%B8%9C%E0%B8%B7%E0%B8%AD%E0%B8%81" title="ทางช้างเผือก – Thai" lang="th" hreflang="th" data-title="ทางช้างเผือก" data-language-autonym="ไทย" data-language-local-name="Thai" class="interlanguage-link-target">ไทย</a></li><li class="interlanguage-link interwiki-din mw-list-item"><a href="https://din.wikipedia.org/wiki/Akeu" title="Akeu – Dinka" lang="din" hreflang="din" data-title="Akeu" data-language-autonym="Thuɔŋjäŋ" data-language-local-name="Dinka" class="interlanguage-link-target">Thuɔŋjäŋ</a></li><li class="interlanguage-link interwiki-tg mw-list-item"><a href="https://tg.wikipedia.org/wiki/%D0%A0%D0%BE%D2%B3%D0%B8_%D0%9A%D0%B0%D2%B3%D0%BA%D0%B0%D1%88%D0%BE%D0%BD" title="Роҳи Каҳкашон – Tajik" lang="tg" hreflang="tg" data-title="Роҳи Каҳкашон" data-language-autonym="Тоҷикӣ" data-language-local-name="Tajik" class="interlanguage-link-target">Тоҷикӣ</a></li><li class="interlanguage-link interwiki-tr mw-list-item"><a href="https://tr.wikipedia.org/wiki/Samanyolu" title="Samanyolu – Turkish" lang="tr" hreflang="tr" data-title="Samanyolu" data-language-autonym="Türkçe" data-language-local-name="Turkish" class="interlanguage-link-target">Türkçe</a></li><li class="interlanguage-link interwiki-tk mw-list-item"><a href="https://tk.wikipedia.org/wiki/Akma%C3%BDany%C5%88_%C3%BDoly" title="Akmaýanyň ýoly – Turkmen" lang="tk" hreflang="tk" data-title="Akmaýanyň ýoly" data-language-autonym="Türkmençe" data-language-local-name="Turkmen" class="interlanguage-link-target">Türkmençe</a></li><li class="interlanguage-link interwiki-tyv mw-list-item"><a href="https://tyv.wikipedia.org/wiki/%D0%94%D1%8D%D1%8D%D1%80_%D0%BE%D1%80%D1%83%D1%83" title="Дээр оруу – Tuvinian" lang="tyv" hreflang="tyv" data-title="Дээр оруу" data-language-autonym="Тыва дыл" data-language-local-name="Tuvinian" class="interlanguage-link-target">Тыва дыл</a></li><li class="interlanguage-link interwiki-udm mw-list-item"><a href="https://udm.wikipedia.org/wiki/%D3%9E%D0%B0%D0%B7%D0%B5%D0%B3%D1%81%D1%8E%D1%80%D0%B5%D1%81" title="Ӟазегсюрес – Udmurt" lang="udm" hreflang="udm" data-title="Ӟазегсюрес" data-language-autonym="Удмурт" data-language-local-name="Udmurt" class="interlanguage-link-target">Удмурт</a></li><li class="interlanguage-link interwiki-uk mw-list-item"><a href="https://uk.wikipedia.org/wiki/%D0%A7%D1%83%D0%BC%D0%B0%D1%86%D1%8C%D0%BA%D0%B8%D0%B9_%D0%A8%D0%BB%D1%8F%D1%85" title="Чумацький Шлях – Ukrainian" lang="uk" hreflang="uk" data-title="Чумацький Шлях" data-language-autonym="Українська" data-language-local-name="Ukrainian" class="interlanguage-link-target">Українська</a></li><li class="interlanguage-link interwiki-ur mw-list-item"><a href="https://ur.wikipedia.org/wiki/%D9%85%D9%84%DA%A9%DB%8C_%D9%88%DB%92" title="ملکی وے – Urdu" lang="ur" hreflang="ur" data-title="ملکی وے" data-language-autonym="اردو" data-language-local-name="Urdu" class="interlanguage-link-target">اردو</a></li><li class="interlanguage-link interwiki-ug mw-list-item"><a href="https://ug.wikipedia.org/wiki/%D8%B3%D8%A7%D9%85%D8%A7%D9%86%D9%8A%D9%88%D9%84%D9%89_%D8%B3%D9%89%D8%B3%D8%AA%D9%89%D9%85%DB%90%D8%B3%D9%89" title="سامانيولى سىستىمېسى – Uyghur" lang="ug" hreflang="ug" data-title="سامانيولى سىستىمېسى" data-language-autonym="ئۇيغۇرچە / Uyghurche" data-language-local-name="Uyghur" class="interlanguage-link-target">ئۇيغۇرچە / Uyghurche</a></li><li class="interlanguage-link interwiki-za mw-list-item"><a href="https://za.wikipedia.org/wiki/Dahmbwn" title="Dahmbwn – Zhuang" lang="za" hreflang="za" data-title="Dahmbwn" data-language-autonym="Vahcuengh" data-language-local-name="Zhuang" class="interlanguage-link-target">Vahcuengh</a></li><li class="interlanguage-link interwiki-vep mw-list-item"><a href="https://vep.wikipedia.org/wiki/Maidte" title="Maidte – Veps" lang="vep" hreflang="vep" data-title="Maidte" data-language-autonym="Vepsän kel’" data-language-local-name="Veps" class="interlanguage-link-target">Vepsän kel’</a></li><li class="interlanguage-link interwiki-vi mw-list-item"><a href="https://vi.wikipedia.org/wiki/Ng%C3%A2n_H%C3%A0" title="Ngân Hà – Vietnamese" lang="vi" hreflang="vi" data-title="Ngân Hà" data-language-autonym="Tiếng Việt" data-language-local-name="Vietnamese" class="interlanguage-link-target">Tiếng Việt</a></li><li class="interlanguage-link interwiki-fiu-vro mw-list-item"><a href="https://fiu-vro.wikipedia.org/wiki/Tsirgurada" title="Tsirgurada – Võro" lang="vro" hreflang="vro" data-title="Tsirgurada" data-language-autonym="Võro" data-language-local-name="Võro" class="interlanguage-link-target">Võro</a></li><li class="interlanguage-link interwiki-wa mw-list-item"><a href="https://wa.wikipedia.org/wiki/Voye_Sint-Dj%C3%A5ke_(sitoelreye)" title="Voye Sint-Djåke (sitoelreye) – Walloon" lang="wa" hreflang="wa" data-title="Voye Sint-Djåke (sitoelreye)" data-language-autonym="Walon" data-language-local-name="Walloon" class="interlanguage-link-target">Walon</a></li><li class="interlanguage-link interwiki-zh-classical mw-list-item"><a href="https://zh-classical.wikipedia.org/wiki/%E9%8A%80%E6%B2%B3" title="銀河 – Literary Chinese" lang="lzh" hreflang="lzh" data-title="銀河" data-language-autonym="文言" data-language-local-name="Literary Chinese" class="interlanguage-link-target">文言</a></li><li class="interlanguage-link interwiki-vls mw-list-item"><a href="https://vls.wikipedia.org/wiki/Melkweg" title="Melkweg – West Flemish" lang="vls" hreflang="vls" 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For other uses, see <a href="/wiki/Milky_Way_(disambiguation)" class="mw-disambig" title="Milky Way (disambiguation)">Milky Way (disambiguation)</a>.</div> <style data-mw-deduplicate="TemplateStyles:r1257001546">.mw-parser-output .infobox-subbox{padding:0;border:none;margin:-3px;width:auto;min-width:100%;font-size:100%;clear:none;float:none;background-color:transparent}.mw-parser-output .infobox-3cols-child{margin:auto}.mw-parser-output .infobox .navbar{font-size:100%}@media screen{html.skin-theme-clientpref-night .mw-parser-output .infobox-full-data:not(.notheme)>div:not(.notheme)[style]{background:#1f1f23!important;color:#f8f9fa}}@media screen and (prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .infobox-full-data:not(.notheme) div:not(.notheme){background:#1f1f23!important;color:#f8f9fa}}@media(min-width:640px){body.skin--responsive .mw-parser-output .infobox-table{display:table!important}body.skin--responsive .mw-parser-output .infobox-table>caption{display:table-caption!important}body.skin--responsive .mw-parser-output .infobox-table>tbody{display:table-row-group}body.skin--responsive .mw-parser-output .infobox-table tr{display:table-row!important}body.skin--responsive .mw-parser-output .infobox-table th,body.skin--responsive .mw-parser-output .infobox-table td{padding-left:inherit;padding-right:inherit}}</style><table class="infobox"><tbody><tr><th colspan="2" class="infobox-above" style="background: #ddd;">Milky Way</th></tr><tr><td colspan="2" class="infobox-image"><a href="/wiki/File:ESO-VLT-Laser-phot-33a-07.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/43/ESO-VLT-Laser-phot-33a-07.jpg/290px-ESO-VLT-Laser-phot-33a-07.jpg" decoding="async" width="290" height="193" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/43/ESO-VLT-Laser-phot-33a-07.jpg/435px-ESO-VLT-Laser-phot-33a-07.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/43/ESO-VLT-Laser-phot-33a-07.jpg/580px-ESO-VLT-Laser-phot-33a-07.jpg 2x" data-file-width="3888" data-file-height="2583" /></a><div class="infobox-caption"><div style="display: inline-block; line-height: 1.2em; padding: .1em 0; padding: 4px 0;">The <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a> as seen from <a href="/wiki/Earth" title="Earth">Earth</a>'s night sky (featuring the telescope's <a href="/wiki/Laser_guide_star" title="Laser guide star">laser guide star</a>). Listed below is Galactic Center's information.</div></div></td></tr><tr><th colspan="2" class="infobox-header" style="background: #ddd;">Observation data (<a href="/wiki/Epoch_(astronomy)#Julian_years_and_J2000" title="Epoch (astronomy)">J2000</a> <a href="/wiki/Epoch_(astronomy)" title="Epoch (astronomy)">epoch</a>)</th></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Constellation" title="Constellation">Constellation</a></th><td class="infobox-data"><a href="/wiki/Sagittarius_(constellation)" title="Sagittarius (constellation)">Sagittarius</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Right_ascension" title="Right ascension">Right ascension</a></th><td class="infobox-data">17h 45m 40.03599s<a href="#cite_note-Petrov-1">[1]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Declination" title="Declination">Declination</a></th><td class="infobox-data">−29° 00′ 28.1699″<a href="#cite_note-Petrov-1">[1]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Cosmic_distance_ladder" title="Cosmic distance ladder">Distance</a></th><td class="infobox-data">7.935–8.277 <a href="/wiki/Parsec#Parsecs_and_kiloparsecs" title="Parsec">kpc</a> (25,881–26,996 <a href="/wiki/Light-year" title="Light-year">ly</a>)<a href="#cite_note-ehtc_6-2">[2]</a><a href="#cite_note-idrani-3">[3]</a><a href="#cite_note-gravity_2019-4">[4]</a><a href="#cite_note-distance-5">[a]</a></td></tr><tr><th colspan="2" class="infobox-header" style="background: #ddd;">Characteristics</th></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Galaxy_morphological_classification" title="Galaxy morphological classification">Type</a></th><td class="infobox-data">Sb; Sbc; SB(rs)bc<a href="#cite_note-ssr100_1_129-6">[5]</a><a href="#cite_note-7">[6]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Mass" title="Mass">Mass</a></th><td class="infobox-data">1.15×1012<a href="#cite_note-SA-20190308-8">[7]</a><a href="#cite_note-ARX-20190208-9">[8]</a><a href="#cite_note-Kafle2012-10">[9]</a> <a href="/wiki/Solar_mass" title="Solar mass"><var>M</var>☉</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Number of stars</th><td class="infobox-data">100–400 billion ((1–4)×1011)<a href="#cite_note-frommert_kronberg2005-14">[12]</a><a href="#cite_note-wethington2010-15">[13]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Size</th><td class="infobox-data">26.8 ± 1.1 <a href="/wiki/Parsec#Parsecs_and_kiloparsecs" title="Parsec">kpc</a> (87,400 ± 3,600 <a href="/wiki/Light-year" title="Light-year">ly</a>) (diameter; <a href="/wiki/Galaxy#Isophotal_diameter" title="Galaxy">D25 isophote</a>)<a href="#cite_note-Goodwin-11">[10]</a><a href="#cite_note-Disk-13">[b]</a></td></tr><tr><td colspan="2" class="infobox-full-data"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1257001546"></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Thickness of <a href="/wiki/Thin_disk" title="Thin disk">thin disk</a></th><td class="infobox-data">220–450 pc (718–1,470 ly)<a href="#cite_note-bland-16">[14]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Thickness of <a href="/wiki/Thick_disk" title="Thick disk">thick disk</a></th><td class="infobox-data">2.6 ± 0.5 kpc (8,500 ± 1,600 ly)<a href="#cite_note-bland-16">[14]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Angular momentum</th><td class="infobox-data">~1×1067 J s<a href="#cite_note-17">[15]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Sun's <a href="/wiki/Galactic_year" title="Galactic year">Galactic rotation period</a></th><td class="infobox-data">212 Myr<a href="#cite_note-newview-18">[16]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Density_wave_theory" title="Density wave theory">Spiral pattern rotation period</a></th><td class="infobox-data">220–360 Myr<a href="#cite_note-rotation_pattern_speeds-19">[17]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;"><a href="/wiki/Barred_spiral_galaxy" title="Barred spiral galaxy">Bar pattern</a> rotation period</th><td class="infobox-data">160–180 Myr<a href="#cite_note-structure-20">[18]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Speed relative to <a href="/wiki/Cosmic_microwave_background" title="Cosmic microwave background">CMB</a> <a href="/wiki/Rest_frame" title="Rest frame">rest frame</a></th><td class="infobox-data">552.2±5.5 km/s<a href="#cite_note-COBE1993-21">[19]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Escape velocity at Sun's position</th><td class="infobox-data">550 km/s<a href="#cite_note-Kafle2014-22">[20]</a></td></tr><tr><th scope="row" class="infobox-label" style="background: inherit;">Dark matter density at Sun's position</th><td class="infobox-data">0.0088+0.0024 −0.0018 <a href="/wiki/Solar_mass" title="Solar mass"><var>M</var>☉</a>pc−3 (0.35+0.08 −0.07 GeV cm−3)<a href="#cite_note-Kafle2014-22">[20]</a></td></tr><tr style="display:none"><td colspan="2"> </td></tr></tbody></table> The Milky Way<a href="#cite_note-context-28">[c]</a> is the <a href="/wiki/Galaxy" title="Galaxy">galaxy</a> that includes the <a href="/wiki/Solar_System" title="Solar System">Solar System</a>, with the name describing the galaxy's appearance from <a href="/wiki/Earth" title="Earth">Earth</a>: a hazy band of light seen in the <a href="/wiki/Night_sky" title="Night sky">night sky</a> formed from stars that cannot be individually distinguished by the <a href="/wiki/Naked_eye" title="Naked eye">naked eye</a>. The Milky Way is a <a href="/wiki/Barred_spiral_galaxy" title="Barred spiral galaxy">barred spiral galaxy</a> with a <a href="/wiki/Galaxy#Isophotal_diameter" title="Galaxy">D25 isophotal diameter</a> estimated at 26.8 ± 1.1 <a href="/wiki/Parsec#Parsecs_and_kiloparsecs" title="Parsec">kiloparsecs</a> (87,400 ± 3,600 <a href="/wiki/Light-year" title="Light-year">light-years</a>),<a href="#cite_note-Goodwin-11">[10]</a> but only about 1,000 light-years thick at the spiral arms (more at the bulge). Recent simulations suggest that a <a href="/wiki/Dark_matter" title="Dark matter">dark matter</a> area, also containing some visible stars, may extend up to a diameter of almost 2 million light-years (613 kpc).<a href="#cite_note-croswell2020-29">[26]</a><a href="#cite_note-dearson2020-30">[27]</a> The Milky Way has several <a href="/wiki/List_of_Milky_Way%27s_satellite_galaxies" class="mw-redirect" title="List of Milky Way's satellite galaxies">satellite galaxies</a> and is part of the <a href="/wiki/Local_Group" title="Local Group">Local Group</a> of galaxies, which form part of the <a href="/wiki/Virgo_Supercluster" title="Virgo Supercluster">Virgo Supercluster</a>, which is itself a component of the <a href="/wiki/Laniakea_Supercluster" title="Laniakea Supercluster">Laniakea Supercluster</a>.<a href="#cite_note-31">[28]</a><a href="#cite_note-32">[29]</a> It is estimated to contain 100–400 billion stars<a href="#cite_note-33">[30]</a><a href="#cite_note-34">[31]</a> and at least that number of <a href="/wiki/Planet" title="Planet">planets</a>.<a href="#cite_note-Nature-20120111-35">[32]</a><a href="#cite_note-Space-20130102-36">[33]</a> The Solar System is located at a radius of about 27,000 light-years (8.3 kpc) from the <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a>,<a href="#cite_note-Gillessen2016-37">[34]</a> on the inner edge of the <a href="/wiki/Orion_Arm" title="Orion Arm">Orion Arm</a>, one of the spiral-shaped concentrations of gas and dust. The stars in the innermost 10,000 light-years form a <a href="/wiki/Bulge_(astronomy)" class="mw-redirect" title="Bulge (astronomy)">bulge</a> and one or more bars that radiate from the bulge. The Galactic Center is an intense radio source known as <a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a>, a <a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">supermassive black hole</a> of 4.100 (± 0.034) million <a href="/wiki/Solar_mass" title="Solar mass">solar masses</a>.<a href="#cite_note-NYT-20220131-38">[35]</a><a href="#cite_note-ARX-20220128-39">[36]</a> The oldest stars in the Milky Way are nearly as old as the Universe itself and thus probably formed shortly after the <a href="/wiki/Chronology_of_the_universe#Dark_Ages" title="Chronology of the universe">Dark Ages</a> of the <a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a>.<a href="#cite_note-HD_140283_(arXiv)-40">[37]</a> <a href="/wiki/Galileo_Galilei" title="Galileo Galilei">Galileo Galilei</a> first resolved the band of light into individual stars with his telescope in 1610. Until the early 1920s, most astronomers thought that the Milky Way contained all the stars in the <a href="/wiki/Universe" title="Universe">Universe</a>.<a href="#cite_note-41">[38]</a> Following the 1920 <a href="/wiki/Great_Debate_(astronomy)" title="Great Debate (astronomy)">Great Debate</a> between the astronomers <a href="/wiki/Harlow_Shapley" title="Harlow Shapley">Harlow Shapley</a> and <a href="/wiki/Heber_Doust_Curtis" title="Heber Doust Curtis">Heber Doust Curtis</a>,<a href="#cite_note-shapley_curtis-42">[39]</a> observations by <a href="/wiki/Edwin_Hubble" title="Edwin Hubble">Edwin Hubble</a> showed that the Milky Way is just one of many galaxies. <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Etymology_and_mythology">Etymology and mythology</h2></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Milky_Way_(mythology)" title="Milky Way (mythology)">Milky Way (mythology)</a></div> In the <a href="/wiki/Babylonia" title="Babylonia">Babylonian</a> epic poem <a href="/wiki/En%C5%ABma_Eli%C5%A1" title="Enūma Eliš">Enūma Eliš</a>, the Milky Way is created from the severed tail of the primeval salt water <a href="/wiki/Dragon" title="Dragon">dragoness</a> <a href="/wiki/Tiamat" title="Tiamat">Tiamat</a>, set in the sky by <a href="/wiki/Marduk" title="Marduk">Marduk</a>, the Babylonian <a href="/wiki/National_god" title="National god">national god</a>, after slaying her.<a href="#cite_note-43">[40]</a><a href="#cite_note-44">[41]</a> This story was once thought to have been based on an older <a href="/wiki/Sumer" title="Sumer">Sumerian</a> version in which Tiamat is instead slain by <a href="/wiki/Enlil" title="Enlil">Enlil</a> of <a href="/wiki/Nippur" title="Nippur">Nippur</a>,<a href="#cite_note-45">[42]</a><a href="#cite_note-Lambert1964-46">[43]</a> but is now thought to be purely an invention of Babylonian propagandists with the intention to show Marduk as superior to the Sumerian deities.<a href="#cite_note-Lambert1964-46">[43]</a> In <a href="/wiki/Greek_mythology" title="Greek mythology">Greek mythology</a>, <a href="/wiki/Zeus" title="Zeus">Zeus</a> places his son born by a mortal woman, the infant <a href="/wiki/Heracles" title="Heracles">Heracles</a>, on <a href="/wiki/Hera" title="Hera">Hera</a>'s breast while she is asleep so the baby will drink <a href="/wiki/Milk_of_Hera" title="Milk of Hera">her divine milk</a> and become immortal. Hera wakes up while breastfeeding and then realizes she is nursing an unknown baby: she pushes the baby away, some of her milk spills, and it produces the band of light known as the Milky Way. In another Greek story, the abandoned Heracles is given by <a href="/wiki/Athena" title="Athena">Athena</a> to Hera for feeding, but Heracles' forcefulness causes Hera to rip him from her breast in pain.<a href="#cite_note-47">[44]</a><a href="#cite_note-Leeming-48">[45]</a><a href="#cite_note-Pache-49">[46]</a> Llys Dôn (literally "The Court of <a href="/wiki/D%C3%B4n" title="Dôn">Dôn</a>") is the traditional Welsh name for the constellation <a href="/wiki/Cassiopeia_(constellation)" title="Cassiopeia (constellation)">Cassiopeia</a>. At least three of Dôn's children also have astronomical associations: Caer Gwydion ("The fortress of <a href="/wiki/Gwydion" title="Gwydion">Gwydion</a>") is the traditional Welsh name for the Milky Way,<a href="#cite_note-50">[47]</a><a href="#cite_note-51">[48]</a> and Caer Arianrhod ("The Fortress of <a href="/wiki/Arianrhod" title="Arianrhod">Arianrhod</a>") being the constellation of <a href="/wiki/Corona_Borealis" title="Corona Borealis">Corona Borealis</a>.<a href="#cite_note-52">[49]</a><a href="#cite_note-53">[50]</a> In Western culture, the name "Milky Way" is derived from its appearance as a dim un-resolved "milky" glowing band arching across the night sky. The term is a translation of the <a href="/wiki/Classical_Latin" title="Classical Latin">Classical Latin</a> via lactea, in turn derived from the <a href="/wiki/Hellenistic_Greek" class="mw-redirect" title="Hellenistic Greek">Hellenistic Greek</a> γαλαξίας, short for γαλαξίας κύκλος (galaxías kýklos), meaning "milky circle". The <a href="/wiki/Ancient_Greek" title="Ancient Greek">Ancient Greek</a> γαλαξίας (galaxias) – from root γαλακτ-, γάλα ("milk") + -ίας (forming adjectives) – is also the root of "galaxy", the name for our, and later all such, collections of stars.<a href="#cite_note-eo_galaxy-54">[51]</a><a href="#cite_note-jankowski2010-55">[52]</a><a href="#cite_note-oxford-56">[53]</a> The Milky Way, or "milk circle", was just one of 11 "circles" the Greeks identified in the sky, others being the <a href="/wiki/Zodiac" title="Zodiac">zodiac</a>, the <a href="/wiki/Meridian_(astronomy)" title="Meridian (astronomy)">meridian</a>, the <a href="/wiki/Horizon" title="Horizon">horizon</a>, the <a href="/wiki/Equator" title="Equator">equator</a>, the <a href="/wiki/Tropics_of_Cancer_and_Capricorn" class="mw-redirect" title="Tropics of Cancer and Capricorn">tropics of Cancer and Capricorn</a>, the <a href="/wiki/Arctic_Circle" title="Arctic Circle">Arctic Circle</a> and the <a href="/wiki/Antarctic_Circle" title="Antarctic Circle">Antarctic Circle</a>, and two <a href="/wiki/Colure" title="Colure">colure</a> circles passing through both poles.<a href="#cite_note-eratosthenes1997-57">[54]</a> <div class="mw-heading mw-heading3"><h3 id="Common_names">Common names</h3></div> <ul><li>"Birds' Path" is used in several <a href="/wiki/Uralic_languages" title="Uralic languages">Uralic</a> and <a href="/wiki/Turkic_languages" title="Turkic languages">Turkic languages</a> and in the <a href="/wiki/Baltic_languages" title="Baltic languages">Baltic languages</a>. Northern peoples observed that <a href="/wiki/Migratory_birds" class="mw-redirect" title="Migratory birds">migratory birds</a> follow the course of the galaxy<a href="#cite_note-58">[55]</a> while migrating at the Northern Hemisphere. The name "Birds' Path" (in Finnish, Estonian, Latvian, Lithuanian, Bashkir and Kazakh) has some variations in other languages, e.g. "Way of the grey (wild) goose" in Chuvash, Mari and Tatar and "Way of the Crane" in Erzya and Moksha.</li> <li>House river: The <a href="/wiki/Kaurna_people" class="mw-redirect" title="Kaurna people">Kaurna people</a> of the <a href="/wiki/Adelaide_Plains" title="Adelaide Plains">Adelaide Plains</a> of South Australia called the Milky Way wodliparri in the <a href="/wiki/Kaurna_language" title="Kaurna language">Kaurna language</a>, meaning "house river".<a href="#cite_note-59">[56]</a></li> <li>Emu in the Sky: The <a href="/wiki/Gamilaraay" title="Gamilaraay">Gomeroi people</a> between <a href="/wiki/New_South_Wales" title="New South Wales">New South Wales</a> and <a href="/wiki/Queensland" title="Queensland">Queensland</a> called the Milky Way Dhinawan, the giant <a href="/wiki/Emu" title="Emu">Emu in the Sky</a> that it stretches across the night sky.<a href="#cite_note-60">[57]</a></li> <li>Milky Way: Many European languages have borrowed, directly or indirectly, the Greek name for the Milky Way, including English and Latin.</li> <li>Road to Santiago: the Milky Way was traditionally used as a guide by <a href="/wiki/Pilgrims" class="mw-redirect" title="Pilgrims">pilgrims</a> traveling to the holy site at <a href="/wiki/Santiago_de_Compostela" title="Santiago de Compostela">Compostela</a>, hence the use of "The Road to Santiago" as a name for the Milky Way.<a href="#cite_note-Fiona-61">[58]</a> Curiously, La Voje Ladee "The Milky Way" was also used to refer to the pilgrimage road.<a href="#cite_note-62">[59]</a></li> <li>River Ganga of the Sky: this Sanskrit name (आकाशगंगा Ākāśagaṃgā) is used in many Indian languages following a Hindu belief .</li> <li>Silver River: this Chinese name "Silver River" (銀河) is used throughout East Asia, including Korea and Vietnam. In Japan and Korea, "Silver River" (<a href="/wiki/Japanese_language" title="Japanese language">Japanese</a>: 銀河, <a href="/wiki/Romanization_of_Japanese" title="Romanization of Japanese">romanized</a>: ginga; <a href="/wiki/Korean_language" title="Korean language">Korean</a>: 은하; <a href="/wiki/Revised_Romanization_of_Korean" title="Revised Romanization of Korean">RR</a>: eunha) means galaxies in general.</li> <li>River of Heaven: The Japanese name for the Milky Way is the "River of Heaven" (天の川, Amanokawa), as well as an alternative name in Chinese (<a href="/wiki/Chinese_language" title="Chinese language">Chinese</a>: 天河; <a href="/wiki/Pinyin" title="Pinyin">pinyin</a>: Tiānhé).</li> <li>Straw Way:In West Asia, Central Asia and parts of the Balkans the name for the Milky Way is related to the word for <a href="/wiki/Straw" title="Straw">straw</a>. Today, Persians, Pakistanis, and Turks use it in addition to Arabs. It has been suggested that the term was spread by medieval <a href="/wiki/Arab" class="mw-redirect" title="Arab">Arabs</a> who in turn borrowed it from Armenians.<a href="#cite_note-63">[60]</a></li> <li>Walsingham Way: In England the Milky Way was called the Walsingham Way in reference to the shrine of <a href="/wiki/Our_Lady_of_Walsingham" title="Our Lady of Walsingham">Our Lady of Walsingham</a> which is in <a href="/wiki/Norfolk" title="Norfolk">Norfolk</a>, England. It was understood to be either a guide to the pilgrims who flocked there, or a representation of the pilgrims themselves.<a href="#cite_note-64">[61]</a></li> <li>Winter Street: Scandinavian peoples, such as Swedes, have called the galaxy Winter Street (Vintergatan) as the galaxy is most clearly visible during the winter at the northern hemisphere, especially at high latitudes where the <a href="/wiki/Midnight_sun" title="Midnight sun">glow of the Sun late at night</a> can obscure it during the summer.</li></ul> <div class="mw-heading mw-heading2"><h2 id="Appearance">Appearance</h2></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Milky_Way_Night_Sky_Black_Rock_Desert_Nevada.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c6/Milky_Way_Night_Sky_Black_Rock_Desert_Nevada.jpg/220px-Milky_Way_Night_Sky_Black_Rock_Desert_Nevada.jpg" decoding="async" width="220" height="308" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c6/Milky_Way_Night_Sky_Black_Rock_Desert_Nevada.jpg/330px-Milky_Way_Night_Sky_Black_Rock_Desert_Nevada.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c6/Milky_Way_Night_Sky_Black_Rock_Desert_Nevada.jpg/440px-Milky_Way_Night_Sky_Black_Rock_Desert_Nevada.jpg 2x" data-file-width="2912" data-file-height="4078" /></a><figcaption>The Milky Way as seen from a dark site with little <a href="/wiki/Light_pollution" title="Light pollution">light pollution</a></figcaption></figure><style data-mw-deduplicate="TemplateStyles:r1251242444">.mw-parser-output .ambox{border:1px solid #a2a9b1;border-left:10px solid #36c;background-color:#fbfbfb;box-sizing:border-box}.mw-parser-output .ambox+link+.ambox,.mw-parser-output .ambox+link+style+.ambox,.mw-parser-output .ambox+link+link+.ambox,.mw-parser-output .ambox+.mw-empty-elt+link+.ambox,.mw-parser-output .ambox+.mw-empty-elt+link+style+.ambox,.mw-parser-output .ambox+.mw-empty-elt+link+link+.ambox{margin-top:-1px}html body.mediawiki .mw-parser-output .ambox.mbox-small-left{margin:4px 1em 4px 0;overflow:hidden;width:238px;border-collapse:collapse;font-size:88%;line-height:1.25em}.mw-parser-output .ambox-speedy{border-left:10px solid #b32424;background-color:#fee7e6}.mw-parser-output .ambox-delete{border-left:10px solid #b32424}.mw-parser-output .ambox-content{border-left:10px solid #f28500}.mw-parser-output .ambox-style{border-left:10px solid #fc3}.mw-parser-output .ambox-move{border-left:10px solid #9932cc}.mw-parser-output .ambox-protection{border-left:10px solid #a2a9b1}.mw-parser-output .ambox .mbox-text{border:none;padding:0.25em 0.5em;width:100%}.mw-parser-output .ambox .mbox-image{border:none;padding:2px 0 2px 0.5em;text-align:center}.mw-parser-output .ambox .mbox-imageright{border:none;padding:2px 0.5em 2px 0;text-align:center}.mw-parser-output .ambox .mbox-empty-cell{border:none;padding:0;width:1px}.mw-parser-output .ambox .mbox-image-div{width:52px}@media(min-width:720px){.mw-parser-output .ambox{margin:0 10%}}@media print{body.ns-0 .mw-parser-output .ambox{display:none!important}}</style><table class="box-More_citations_needed_section plainlinks metadata ambox ambox-content ambox-Refimprove" role="presentation"><tbody><tr><td class="mbox-image"><div class="mbox-image-div"><a href="/wiki/File:Question_book-new.svg" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/99/Question_book-new.svg/50px-Question_book-new.svg.png" decoding="async" width="50" height="39" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/99/Question_book-new.svg/75px-Question_book-new.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/99/Question_book-new.svg/100px-Question_book-new.svg.png 2x" data-file-width="512" data-file-height="399" /></a></div></td><td class="mbox-text"><div class="mbox-text-span">This section needs additional citations for <a href="/wiki/Wikipedia:Verifiability" title="Wikipedia:Verifiability">verification</a>. Please help <a href="/wiki/Special:EditPage/Milky_Way" title="Special:EditPage/Milky Way">improve this article</a> by <a href="/wiki/Help:Referencing_for_beginners" title="Help:Referencing for beginners">adding citations to reliable sources</a> in this section. Unsourced material may be challenged and removed. (June 2024) (<a href="/wiki/Help:Maintenance_template_removal" title="Help:Maintenance template removal">Learn how and when to remove this message</a>)</div></td></tr></tbody></table> The Milky Way is visible as a hazy band of white light, some 30° wide, arching the <a href="/wiki/Night_sky" title="Night sky">night sky</a>.<a href="#cite_note-pasachoff1994-65">[62]</a> Although all the individual naked-eye stars in the entire sky are part of the Milky Way Galaxy, the term "Milky Way" is limited to this band of light.<a href="#cite_note-66">[63]</a><a href="#cite_note-67">[64]</a> The light originates from the accumulation of <a href="/wiki/Angular_resolution" title="Angular resolution">unresolved</a> stars and other material located in the direction of the <a href="/wiki/Galactic_plane" title="Galactic plane">galactic plane</a>. Brighter regions around the band appear as soft visual patches known as <a href="/wiki/Star_cloud" class="mw-redirect" title="Star cloud">star clouds</a>. The most conspicuous of these is the <a href="/wiki/Large_Sagittarius_Star_Cloud" title="Large Sagittarius Star Cloud">Large Sagittarius Star Cloud</a>, a portion of the central <a href="/wiki/Galactic_bulge" title="Galactic bulge">bulge</a> of the galaxy.<a href="#cite_note-68">[65]</a> Dark regions within the band, such as the <a href="/wiki/Great_Rift_(astronomy)" title="Great Rift (astronomy)">Great Rift</a> and the <a href="/wiki/Coalsack_Nebula" title="Coalsack Nebula">Coalsack</a>, are areas where <a href="/wiki/Interstellar_dust" class="mw-redirect" title="Interstellar dust">interstellar dust</a> blocks light from distant stars. Peoples of the southern hemisphere, including the <a href="/wiki/Coricancha#Inca_astronomy" title="Coricancha">Inca</a> and <a href="/wiki/Australian_Aboriginal_astronomy#Emu_in_the_sky" title="Australian Aboriginal astronomy">Australian aborigines</a>, identified these regions as <a href="/wiki/Dark_cloud_constellation" class="mw-redirect" title="Dark cloud constellation">dark cloud constellations</a>.<a href="#cite_note-69">[66]</a> The area of sky that the Milky Way obscures is called the <a href="/wiki/Zone_of_Avoidance" title="Zone of Avoidance">Zone of Avoidance</a>.<a href="#cite_note-70">[67]</a> The Milky Way has a relatively low <a href="/wiki/Surface_brightness" title="Surface brightness">surface brightness</a>. Its visibility can be greatly reduced by background light, such as <a href="/wiki/Light_pollution" title="Light pollution">light pollution</a> or moonlight. The sky needs to be darker than about 20.2 <a href="/wiki/Magnitude_(astronomy)" title="Magnitude (astronomy)">magnitude</a> per square arcsecond in order for the Milky Way to be visible.<a href="#cite_note-71">[68]</a> It should be visible if the <a href="/wiki/Limiting_magnitude" title="Limiting magnitude">limiting magnitude</a> is approximately +5.1 or better and shows a great deal of detail at +6.1.<a href="#cite_note-steinicke_sakiel2007-72">[69]</a> This makes the Milky Way difficult to see from brightly lit urban or suburban areas, but very prominent when viewed from <a href="/wiki/Rural_area" title="Rural area">rural areas</a> when the Moon is below the horizon.<a href="#cite_note-bortle-73">[d]</a> Maps of artificial night sky brightness show that more than one-third of Earth's population cannot see the Milky Way from their homes due to light pollution.<a href="#cite_note-74">[70]</a> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Via_l%C3%A1ctea_sobre_el_Sajama.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/9c/Via_l%C3%A1ctea_sobre_el_Sajama.jpg/220px-Via_l%C3%A1ctea_sobre_el_Sajama.jpg" decoding="async" width="220" height="147" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/9c/Via_l%C3%A1ctea_sobre_el_Sajama.jpg/330px-Via_l%C3%A1ctea_sobre_el_Sajama.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/9c/Via_l%C3%A1ctea_sobre_el_Sajama.jpg/440px-Via_l%C3%A1ctea_sobre_el_Sajama.jpg 2x" data-file-width="5184" data-file-height="3456" /></a><figcaption>The Milky Way as seen from <a href="/wiki/Sajama_National_Park" title="Sajama National Park">Sajama National Park</a> in <a href="/wiki/Bolivia" title="Bolivia">Bolivia</a>, an area with little light pollution.</figcaption></figure> As viewed from Earth, the visible region of the Milky Way's <a href="/wiki/Galactic_plane" title="Galactic plane">galactic plane</a> occupies an area of the sky that includes 30 <a href="/wiki/Constellation" title="Constellation">constellations</a>.<a href="#cite_note-const-75">[e]</a> The <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a> lies in the direction of <a href="/wiki/Sagittarius_(constellation)" title="Sagittarius (constellation)">Sagittarius</a>, where the Milky Way is brightest. From Sagittarius, the hazy band of white light appears to pass around to the <a href="/wiki/Galactic_anticenter" title="Galactic anticenter">galactic anticenter</a> in <a href="/wiki/Auriga_(constellation)" class="mw-redirect" title="Auriga (constellation)">Auriga</a>. The band then continues the rest of the way around the sky, back to Sagittarius, dividing the sky into two roughly equal <a href="/wiki/Celestial_sphere" title="Celestial sphere">hemispheres</a>.<a href="#cite_note-76">[71]</a> The galactic plane is inclined by about 60° to the <a href="/wiki/Ecliptic" title="Ecliptic">ecliptic</a> (the plane of <a href="/wiki/Earth%27s_orbit" title="Earth's orbit">Earth's orbit</a>). Relative to the <a href="/wiki/Celestial_equator" title="Celestial equator">celestial equator</a>, it passes as far north as the constellation of <a href="/wiki/Cassiopeia_(constellation)" title="Cassiopeia (constellation)">Cassiopeia</a> and as far south as the constellation of <a href="/wiki/Crux" title="Crux">Crux</a>, indicating the high inclination of Earth's <a href="/wiki/Equator" title="Equator">equatorial</a> plane and the plane of the ecliptic, relative to the galactic plane. The north galactic pole is situated at <a href="/wiki/Right_ascension" title="Right ascension">right ascension</a> 12h 49m, <a href="/wiki/Declination" title="Declination">declination</a> +27.4° (<a href="/wiki/B1950" class="mw-redirect" title="B1950">B1950</a>) near <a href="/wiki/Beta_Comae_Berenices" title="Beta Comae Berenices">β Comae Berenices</a>, and the south galactic pole is near <a href="/wiki/Alpha_Sculptoris" title="Alpha Sculptoris">α Sculptoris</a>. Because of this high inclination, depending on the time of night and year, the Milky Way arch may appear relatively low or relatively high in the sky. For observers from latitudes approximately 65° north to 65° south, the Milky Way passes <a href="/wiki/Zenith" title="Zenith">directly overhead</a> twice a day.[<a href="/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed">citation needed</a>] <div class="mw-heading mw-heading2"><h2 id="Astronomical_history">Astronomical history</h2></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">See also: <a href="/wiki/Galaxy#Observation_history" title="Galaxy">Galaxy § Observation history</a></div> <div class="mw-heading mw-heading3"><h3 id="Ancient,_naked_eye_observations">Ancient, naked eye observations</h3></div> In <a href="/wiki/Meteorology_(Aristotle)" title="Meteorology (Aristotle)">Meteorologica</a>, <a href="/wiki/Aristotle" title="Aristotle">Aristotle</a> (384–322 BC) states that the <a href="/wiki/Greek_philosophy" class="mw-redirect" title="Greek philosophy">Greek philosophers</a> <a href="/wiki/Anaxagoras" title="Anaxagoras">Anaxagoras</a> (<abbr title="circa">c.</abbr> 500–428 BC) and <a href="/wiki/Democritus" title="Democritus">Democritus</a> (460–370 BC) proposed that the Milky Way is the glow of stars not directly visible due to Earth's shadow, while other stars receive their light from the Sun, but have their glow obscured by solar rays.<a href="#cite_note-77">[72]</a> Aristotle himself believed that the Milky Way was part of the Earth's upper atmosphere, along with the stars, and that it was a byproduct of stars burning that did not dissipate because of its outermost location in the atmosphere, composing its <a href="/wiki/Great_circle" title="Great circle">great circle</a>. He said that the milky appearance of the Milky Way <a href="/wiki/Galaxy" title="Galaxy">Galaxy</a> is due to the refraction of the Earth's atmosphere.<a href="#cite_note-What_does_your_image_show-78">[73]</a><a href="#cite_note-Montada-79">[74]</a><a href="#cite_note-80">[75]</a> The <a href="/wiki/Neoplatonism" title="Neoplatonism">Neoplatonist</a> philosopher <a href="/wiki/Olympiodorus_the_Younger" title="Olympiodorus the Younger">Olympiodorus the Younger</a> (c. 495–570 AD) criticized this view, arguing that if the Milky Way were <a href="/wiki/Sublunary" class="mw-redirect" title="Sublunary">sublunary</a>, it should appear different at different times and places on Earth, and that it should have <a href="/wiki/Parallax" title="Parallax">parallax</a>, which it does not. In his view, the Milky Way is celestial. This idea would be influential later in the <a href="/wiki/Muslim_world" title="Muslim world">Muslim world</a>.<a href="#cite_note-heidarzadeh2008-81">[76]</a> The <a href="/wiki/Persian_people" class="mw-redirect" title="Persian people">Persian</a> astronomer <a href="/wiki/Al-Biruni" title="Al-Biruni">Al-Biruni</a> (973–1048) proposed that the Milky Way is "a collection of countless fragments of the nature of <a href="/wiki/Nebula" title="Nebula">nebulous</a> stars".<a href="#cite_note-mactutor_albirundi-82">[77]</a> The <a href="/wiki/Al-Andalus" title="Al-Andalus">Andalusian</a> astronomer <a href="/wiki/Avempace" title="Avempace">Avempace</a> (<abbr title="died">d</abbr> 1138) proposed that the Milky Way was made up of many stars but appeared to be a continuous image in the Earth's atmosphere, citing his observation of a <a href="/wiki/Conjunction_(astronomy_and_astrology)" class="mw-redirect" title="Conjunction (astronomy and astrology)">conjunction</a> of Jupiter and Mars in 1106 or 1107 as evidence.<a href="#cite_note-Montada-79">[74]</a> The Persian astronomer <a href="/wiki/Nasir_al-Din_al-Tusi" title="Nasir al-Din al-Tusi">Nasir al-Din al-Tusi</a> (1201–1274) in his Tadhkira wrote: "The Milky Way, i.e. the Galaxy, is made up of a very large number of small, tightly clustered stars, which, on account of their concentration and smallness, seem to be cloudy patches. Because of this, it was likened to milk in color."<a href="#cite_note-ragep1993-83">[78]</a> <a href="/wiki/Ibn_Qayyim_al-Jawziyya" title="Ibn Qayyim al-Jawziyya">Ibn Qayyim al-Jawziyya</a> (1292–1350) proposed that the Milky Way is "a myriad of tiny stars packed together in the sphere of the fixed stars".<a href="#cite_note-Livingston-84">[79]</a> <div class="mw-heading mw-heading3"><h3 id="Telescopic_observations">Telescopic observations</h3></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Herschel-Galaxy.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/b/ba/Herschel-Galaxy.png/220px-Herschel-Galaxy.png" decoding="async" width="220" height="66" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/ba/Herschel-Galaxy.png/330px-Herschel-Galaxy.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/ba/Herschel-Galaxy.png/440px-Herschel-Galaxy.png 2x" data-file-width="668" data-file-height="200" /></a><figcaption>The shape of the Milky Way as deduced from star counts by <a href="/wiki/William_Herschel" title="William Herschel">William Herschel</a> in 1785. The <a href="/wiki/Solar_System" title="Solar System">Solar System</a> was assumed to be near the center</figcaption></figure>Proof of the Milky Way consisting of many stars came in 1610 when <a href="/wiki/Galileo_Galilei" title="Galileo Galilei">Galileo Galilei</a> used a <a href="/wiki/Optical_telescope" title="Optical telescope">telescope</a> to study the Milky Way and discovered that it is composed of a huge number of faint stars. Galileo also concluded that the appearance of the Milky Way was due to <a href="/wiki/Refraction" title="Refraction">refraction</a> of the Earth's atmosphere.<a href="#cite_note-85">[80]</a><a href="#cite_note-oconnor_robertson2002-86">[81]</a><a href="#cite_note-What_does_your_image_show-78">[73]</a> In a treatise in 1755, <a href="/wiki/Immanuel_Kant" title="Immanuel Kant">Immanuel Kant</a>, drawing on earlier work by <a href="/wiki/Thomas_Wright_(astronomer)" title="Thomas Wright (astronomer)">Thomas Wright</a>,<a href="#cite_note-87">[82]</a> speculated (correctly) that the Milky Way might be a rotating body of a huge number of stars, held together by <a href="/wiki/Gravitation" class="mw-redirect" title="Gravitation">gravitational</a> forces akin to the Solar System but on much larger scales.<a href="#cite_note-88">[83]</a> The resulting disk of stars would be seen as a band on the sky from our perspective inside the disk. Wright and Kant also conjectured that some of the <a href="/wiki/Nebula" title="Nebula">nebulae</a> visible in the night sky might be separate "galaxies" themselves, similar to our own. Kant referred to both the Milky Way and the "extragalactic nebulae" as "island universes", a term still current up to the 1930s.<a href="#cite_note-89">[84]</a><a href="#cite_note-our_galaxy-90">[85]</a><a href="#cite_note-91">[86]</a> The first attempt to describe the shape of the Milky Way and the position of the Sun within it was carried out by <a href="/wiki/William_Herschel" title="William Herschel">William Herschel</a> in 1785 by carefully counting the number of stars in different regions of the visible sky. He produced a diagram of the shape of the Milky Way with the Solar System close to the center.<a href="#cite_note-92">[87]</a> In 1845, <a href="/wiki/William_Parsons,_3rd_Earl_of_Rosse" title="William Parsons, 3rd Earl of Rosse">Lord Rosse</a> constructed a new telescope and was able to distinguish between elliptical and spiral-shaped nebulae. He also managed to make out individual point sources in some of these nebulae, lending credence to Kant's earlier conjecture.<a href="#cite_note-abbey-93">[88]</a><a href="#cite_note-94">[89]</a> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Pic_iroberts1.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/5/51/Pic_iroberts1.jpg/220px-Pic_iroberts1.jpg" decoding="async" width="220" height="143" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/51/Pic_iroberts1.jpg/330px-Pic_iroberts1.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/51/Pic_iroberts1.jpg/440px-Pic_iroberts1.jpg 2x" data-file-width="569" data-file-height="371" /></a><figcaption>Photograph of the "Great Andromeda Nebula" from 1899, later identified as the <a href="/wiki/Andromeda_Galaxy" title="Andromeda Galaxy">Andromeda Galaxy</a></figcaption></figure> In 1904, studying the <a href="/wiki/Proper_motion" title="Proper motion">proper motions</a> of stars, <a href="/wiki/Jacobus_Kapteyn" title="Jacobus Kapteyn">Jacobus Kapteyn</a> reported that these were not random, as it was believed in that time; stars could be divided into two streams, moving in nearly opposite directions.<a href="#cite_note-95">[90]</a> It was later realized that Kapteyn's data had been the first evidence of the rotation of our galaxy,<a href="#cite_note-96">[91]</a> which ultimately led to the finding of galactic rotation by <a href="/wiki/Bertil_Lindblad" title="Bertil Lindblad">Bertil Lindblad</a> and <a href="/wiki/Jan_Oort" title="Jan Oort">Jan Oort</a>.[<a href="/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed">citation needed</a>] In 1917, <a href="/wiki/Heber_Doust_Curtis" title="Heber Doust Curtis">Heber Doust Curtis</a> had observed the nova <a href="/wiki/S_Andromedae" class="mw-redirect" title="S Andromedae">S Andromedae</a> within the <a href="/wiki/Great_Andromeda_Nebula" class="mw-redirect" title="Great Andromeda Nebula">Great Andromeda Nebula</a> (<a href="/wiki/Messier_object" title="Messier object">Messier object</a> 31). Searching the photographic record, he found 11 more <a href="/wiki/Nova" title="Nova">novae</a>. Curtis noticed that these novae were, on average, 10 <a href="/wiki/Magnitude_(astronomy)" title="Magnitude (astronomy)">magnitudes</a> fainter than those that occurred within the Milky Way. As a result, he was able to come up with a distance estimate of 150,000 parsecs. He became a proponent of the "island universes" hypothesis, which held that the spiral nebulae were independent galaxies.<a href="#cite_note-97">[92]</a><a href="#cite_note-pasp100_6-98">[93]</a> In 1920 the <a href="/wiki/Great_Debate_(astronomy)" title="Great Debate (astronomy)">Great Debate</a> took place between <a href="/wiki/Harlow_Shapley" title="Harlow Shapley">Harlow Shapley</a> and Heber Curtis, concerning the nature of the Milky Way, spiral nebulae, and the dimensions of the Universe. To support his claim that the Great Andromeda Nebula is an external galaxy, Curtis noted the appearance of dark lanes resembling the dust clouds in the Milky Way, as well as the significant <a href="/wiki/Doppler_effect" title="Doppler effect">Doppler shift</a>.<a href="#cite_note-weaver-99">[94]</a> The controversy was conclusively settled by <a href="/wiki/Edwin_Hubble" title="Edwin Hubble">Edwin Hubble</a> in the early 1920s using the Mount Wilson observatory <a href="/wiki/Hooker_telescope" class="mw-redirect" title="Hooker telescope">2.5 m (100 in) Hooker telescope</a>. With the <a href="/wiki/Light-gathering_power" class="mw-redirect" title="Light-gathering power">light-gathering power</a> of this new telescope, he was able to produce <a href="/wiki/Astrophotography" title="Astrophotography">astronomical photographs</a> that resolved the outer parts of some spiral nebulae as collections of individual stars. He was also able to identify some <a href="/wiki/Cepheid_variable" title="Cepheid variable">Cepheid variables</a> that he could use as a <a href="https://en.wiktionary.org/wiki/benchmark" class="extiw" title="wikt:benchmark">benchmark</a> to estimate the distance to the nebulae. He found that the Andromeda Nebula is 275,000 parsecs from the Sun, far too distant to be part of the Milky Way.<a href="#cite_note-jrasc83_6-100">[95]</a><a href="#cite_note-apj69_103-101">[96]</a> <div class="mw-heading mw-heading3"><h3 id="Satellite_observations">Satellite observations</h3></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1251242444"><table class="box-Update plainlinks metadata ambox ambox-content ambox-Update" role="presentation"><tbody><tr><td class="mbox-image"><div class="mbox-image-div"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/53/Ambox_current_red_Americas.svg/42px-Ambox_current_red_Americas.svg.png" decoding="async" width="42" height="34" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/53/Ambox_current_red_Americas.svg/63px-Ambox_current_red_Americas.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/53/Ambox_current_red_Americas.svg/84px-Ambox_current_red_Americas.svg.png 2x" data-file-width="360" data-file-height="290" /></div></td><td class="mbox-text"><div class="mbox-text-span">This section needs to be updated. The reason given is: It is now 2024, so the article should reflect the status of the ESA's "four planned releases of maps in 2016, 2018...". Please help update this article to reflect recent events or newly available information. (August 2024)</div></td></tr></tbody></table> <figure typeof="mw:File/Thumb"><a href="/wiki/File:Galaxymap.com,_map_5000_parsecs_(2022).png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/f/f3/Galaxymap.com%2C_map_5000_parsecs_%282022%29.png/300px-Galaxymap.com%2C_map_5000_parsecs_%282022%29.png" decoding="async" width="300" height="300" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/f/f3/Galaxymap.com%2C_map_5000_parsecs_%282022%29.png/450px-Galaxymap.com%2C_map_5000_parsecs_%282022%29.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/f/f3/Galaxymap.com%2C_map_5000_parsecs_%282022%29.png/600px-Galaxymap.com%2C_map_5000_parsecs_%282022%29.png 2x" data-file-width="2160" data-file-height="2160" /></a><figcaption>Map of stars cataloged by the Gaia release in 2021, displayed as density mesh in the diagram</figcaption></figure> The <a href="/wiki/European_Space_Agency" title="European Space Agency">ESA</a> spacecraft <a href="/wiki/Gaia_(spacecraft)" title="Gaia (spacecraft)">Gaia</a> provides distance estimates by determining the <a href="/wiki/Parallax" title="Parallax">parallax</a> of a billion stars and is mapping the Milky Way with four planned releases of maps in 2016, 2018, 2021 and 2024.<a href="#cite_note-102">[97]</a><a href="#cite_note-103">[98]</a> Data from Gaia has been described as "transformational". It has been estimated that Gaia has expanded the number of observations of stars from about 2 million stars as of the 1990s to 2 billion. It has expanded the measurable volume of space by a factor of 100 in radius and a factor of 1,000 in precision.<a href="#cite_note-Skibba-104">[99]</a> A study in 2020 concluded that Gaia detected a wobbling motion of the galaxy, which might be caused by "<a href="/wiki/Torques" class="mw-redirect" title="Torques">torques</a> from a misalignment of the disc's rotation axis with respect to the principal axis of a non-spherical halo, or from <a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">accreted</a> matter in the halo acquired during late infall, or from nearby, interacting satellite galaxies and their consequent tides".<a href="#cite_note-105">[100]</a> In April 2024, initial studies (and related maps) involving the <a href="/wiki/Magnetic_field" title="Magnetic field">magnetic fields</a> of the Milky Way were reported.<a href="#cite_note-NYT-20240419-106">[101]</a> <div class="mw-heading mw-heading2"><h2 id="Astrography">Astrography</h2></div> <div class="mw-heading mw-heading3"><h3 id="Sun's_location_and_neighborhood">Sun's location and neighborhood</h3></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">See also: <a href="/wiki/Location_of_Earth" title="Location of Earth">Location of Earth</a></div> <figure typeof="mw:File/Thumb"><a href="/wiki/File:Galaxymap.com,_map_12000_parsecs_(2022).png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/40/Galaxymap.com%2C_map_12000_parsecs_%282022%29.png/300px-Galaxymap.com%2C_map_12000_parsecs_%282022%29.png" decoding="async" width="300" height="300" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/40/Galaxymap.com%2C_map_12000_parsecs_%282022%29.png/450px-Galaxymap.com%2C_map_12000_parsecs_%282022%29.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/40/Galaxymap.com%2C_map_12000_parsecs_%282022%29.png/600px-Galaxymap.com%2C_map_12000_parsecs_%282022%29.png 2x" data-file-width="2160" data-file-height="2160" /></a><figcaption>Map of stars cataloged by the Gaia release in 2021, overlay on top of artist's conception of the Milky Way overall shape</figcaption></figure> The <a href="/wiki/Sun" title="Sun">Sun</a> is near the inner rim of the <a href="/wiki/Orion_Arm" title="Orion Arm">Orion Arm</a>, within the <a href="/wiki/Local_Fluff" class="mw-redirect" title="Local Fluff">Local Fluff</a> of the <a href="/wiki/Local_Bubble" title="Local Bubble">Local Bubble</a>, between the <a href="/wiki/Radcliffe_wave" title="Radcliffe wave">Radcliffe wave</a> and Split linear structures (formerly <a href="/wiki/Gould_Belt" title="Gould Belt">Gould Belt</a>).<a href="#cite_note-Alves_Zucker_Goodman_Speagle_2020-107">[102]</a> Based upon studies of stellar orbits around Sgr A* by Gillessen et al. (2016), the Sun lies at an estimated distance of 27.14 ± 0.46 kly (8.32 ± 0.14 kpc)<a href="#cite_note-Gillessen2016-37">[34]</a> from the Galactic Center. Boehle et al. (2016) found a smaller value of 25.64 ± 0.46 kly (7.86 ± 0.14 kpc), also using a star orbit analysis.<a href="#cite_note-boehle2016-108">[103]</a> The Sun is currently 5–30 parsecs (16–98 ly) above, or north of, the central plane of the Galactic disk.<a href="#cite_note-majaess2009-109">[104]</a> The distance between the local arm and the next arm out, the <a href="/wiki/Perseus_Arm" title="Perseus Arm">Perseus Arm</a>, is about 2,000 parsecs (6,500 ly).<a href="#cite_note-fn9-110">[105]</a> The Sun, and thus the Solar System, is located in the Milky Way's <a href="/wiki/Galactic_habitable_zone" title="Galactic habitable zone">galactic habitable zone</a>.<a href="#cite_note-mullen-2001-111">[106]</a><a href="#cite_note-sundin-2006-112">[107]</a> There are about 208 stars brighter than <a href="/wiki/Absolute_magnitude" title="Absolute magnitude">absolute magnitude</a> 8.5 within a sphere with a radius of 15 parsecs (49 ly) from the Sun, giving a density of one star per 69 cubic parsecs, or one star per 2,360 cubic light-years (from <a href="/wiki/List_of_nearest_bright_stars" title="List of nearest bright stars">List of nearest bright stars</a>). On the other hand, there are 64 known stars (of any magnitude, not counting 4 <a href="/wiki/Brown_dwarf" title="Brown dwarf">brown dwarfs</a>) within 5 parsecs (16 ly) of the Sun, giving a density of about one star per 8.2 cubic parsecs, or one per 284 cubic light-years (from <a href="/wiki/List_of_nearest_stars" title="List of nearest stars">List of nearest stars</a>). This illustrates the fact that there are far more faint stars than bright stars: in the entire sky, there are about 500 stars brighter than <a href="/wiki/Apparent_magnitude" title="Apparent magnitude">apparent magnitude</a> 4 but 15.5 million stars brighter than apparent magnitude 14.<a href="#cite_note-113">[108]</a> The apex of the Sun's way, or the <a href="/wiki/Solar_apex" title="Solar apex">solar apex</a>, is the direction that the Sun travels through space in the Milky Way. The general direction of the Sun's Galactic motion is towards the star <a href="/wiki/Vega" title="Vega">Vega</a> near the constellation of <a href="/wiki/Hercules_(constellation)" title="Hercules (constellation)">Hercules</a>, at an angle of roughly 60 sky degrees to the direction of the Galactic Center. The Sun's orbit about the Milky Way is expected to be roughly elliptical with the addition of perturbations due to the Galactic spiral arms and non-uniform mass distributions. In addition, the Sun passes through the Galactic plane approximately 2.7 times per orbit.<a href="#cite_note-114">[109]</a> [<a href="/wiki/Wikipedia:Reliable_sources" title="Wikipedia:Reliable sources">unreliable source?</a>] This is very similar to how a <a href="/wiki/Simple_harmonic_oscillator" class="mw-redirect" title="Simple harmonic oscillator">simple harmonic oscillator</a> works with no drag force (damping) term. These oscillations were until recently thought to coincide with <a href="/wiki/Mass_extinction" class="mw-redirect" title="Mass extinction">mass lifeform extinction</a> periods on Earth.<a href="#cite_note-extinction-115">[110]</a> A reanalysis of the effects of the Sun's transit through the spiral structure based on CO data has failed to find a correlation.<a href="#cite_note-overholt_etal-116">[111]</a> It takes the Solar System about 240 million years to complete one orbit of the Milky Way (a <a href="/wiki/Galactic_year" title="Galactic year">galactic year</a>),<a href="#cite_note-sparke_gallagher-117">[112]</a> so the Sun is thought to have completed 18–20 orbits during its lifetime and 1/1250 of a revolution since the <a href="/wiki/Origin_of_humans" class="mw-redirect" title="Origin of humans">origin of humans</a>. The <a href="/wiki/Orbital_speed" title="Orbital speed">orbital speed</a> of the Solar System about the center of the Milky Way is approximately 220 km/s (490,000 mph) or 0.073% of the <a href="/wiki/Speed_of_light" title="Speed of light">speed of light</a>. The Sun moves through the heliosphere at 84,000 km/h (52,000 mph). At this speed, it takes around 1,400 years for the Solar System to travel a distance of 1 light-year, or 8 days to travel 1 AU (<a href="/wiki/Astronomical_unit" title="Astronomical unit">astronomical unit</a>).<a href="#cite_note-garlick2002-118">[113]</a> The Solar System is headed in the direction of the zodiacal constellation <a href="/wiki/Scorpius" title="Scorpius">Scorpius</a>, which follows the ecliptic.<a href="#cite_note-119">[114]</a> <div class="mw-heading mw-heading3"><h3 id="Galactic_quadrants">Galactic quadrants</h3></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Galactic_quadrant" title="Galactic quadrant">Galactic quadrant</a></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Galactic_longitude.JPG" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/3/30/Galactic_longitude.JPG/300px-Galactic_longitude.JPG" decoding="async" width="300" height="284" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/3/30/Galactic_longitude.JPG/450px-Galactic_longitude.JPG 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/3/30/Galactic_longitude.JPG/600px-Galactic_longitude.JPG 2x" data-file-width="1200" data-file-height="1134" /></a><figcaption>A diagram of the Sun's location in the Milky Way, the angles represent longitudes in the <a href="/wiki/Galactic_coordinate_system" title="Galactic coordinate system">galactic coordinate system</a></figcaption></figure> A galactic quadrant, or quadrant of the Milky Way, refers to one of four circular sectors in the division of the Milky Way. In astronomical practice, the delineation of the galactic quadrants is based upon the <a href="/wiki/Galactic_coordinate_system" title="Galactic coordinate system">galactic coordinate system</a>, which places the <a href="/wiki/Sun" title="Sun">Sun</a> as the <a href="/wiki/Polar_coordinate_system" title="Polar coordinate system">origin of the mapping system</a>.<a href="#cite_note-120">[115]</a> Quadrants are described using <a href="/wiki/Ordinal_number_(linguistics)" class="mw-redirect" title="Ordinal number (linguistics)">ordinals</a> – for example, "1st galactic quadrant",<a href="#cite_note-toolsofradio-121">[116]</a> "second galactic quadrant",<a href="#cite_note-NASAAD131K-122">[117]</a> or "third quadrant of the Milky Way".<a href="#cite_note-Lampton1997-123">[118]</a> Viewing from the <a href="/wiki/North_galactic_pole" class="mw-redirect" title="North galactic pole">north galactic pole</a> with 0° <a href="/wiki/Degree_(angle)" title="Degree (angle)">(zero degrees)</a> as the <a href="/wiki/Ray_(geometry)" class="mw-redirect" title="Ray (geometry)">ray</a> that runs starting from the Sun and through the Galactic Center, the quadrants are: <dl><dd><dl><dd><table> <tbody><tr> <th>Galactic quadrant   </th> <th>Galactic longitude <a href="/wiki/Galactic_longitude" class="mw-redirect" title="Galactic longitude">(ℓ)</a> </th> <th>  Reference   </th></tr> <tr> <th align="center">1st </th> <td align="right">0° ≤ ℓ ≤ 90°   </td> <td align="center"><a href="#cite_note-vanWoerden-Strom-2006-124">[119]</a> </td></tr> <tr> <th align="center">2nd </th> <td align="right">  90° ≤ ℓ ≤ 180° </td> <td align="center"><a href="#cite_note-NASAAD131K-122">[117]</a> </td></tr> <tr> <th align="center">3rd </th> <td align="right">180° ≤ ℓ ≤ 270° </td> <td align="center"><a href="#cite_note-Lampton1997-123">[118]</a> </td></tr> <tr> <th align="center">4th   </th> <td align="right">270° ≤ ℓ ≤ 360° (360° ≅ 0°) </td> <td align="center"><a href="#cite_note-toolsofradio-121">[116]</a>   </td></tr></tbody></table></dd></dl></dd></dl> with the galactic longitude <a href="/wiki/Galactic_longitude" class="mw-redirect" title="Galactic longitude">(ℓ)</a> increasing in the counter-clockwise direction (<a href="/wiki/Angle#Positive_and_negative_angles" title="Angle">positive rotation</a>) as viewed from <a href="/wiki/Galactic_north" class="mw-redirect" title="Galactic north">north</a> of the <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a> (a view-point several hundred thousand <a href="/wiki/Light-year" title="Light-year">light-years</a> distant from Earth in the direction of the constellation <a href="/wiki/Coma_Berenices" title="Coma Berenices">Coma Berenices</a>); if viewed from south of the Galactic Center (a view-point similarly distant in the constellation <a href="/wiki/Sculptor_(constellation)" title="Sculptor (constellation)">Sculptor</a>), <a href="/wiki/Galactic_longitude" class="mw-redirect" title="Galactic longitude">ℓ</a> would increase in the clockwise direction (<a href="/wiki/Angle#Positive_and_negative_angles" title="Angle">negative rotation</a>). <div class="mw-heading mw-heading2"><h2 id="Size_and_mass">Size and mass</h2></div> <div class="mw-heading mw-heading3"><h3 id="Size">Size</h3></div> <figure class="mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:Local_Group_Galaxies_Comparison.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/a/a2/Local_Group_Galaxies_Comparison.png/300px-Local_Group_Galaxies_Comparison.png" decoding="async" width="300" height="186" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/a/a2/Local_Group_Galaxies_Comparison.png/450px-Local_Group_Galaxies_Comparison.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/a/a2/Local_Group_Galaxies_Comparison.png/600px-Local_Group_Galaxies_Comparison.png 2x" data-file-width="3480" data-file-height="2160" /></a><figcaption>A size comparison of the six largest galaxies of the <a href="/wiki/Local_Group" title="Local Group">Local Group</a>, including the Milky Way</figcaption></figure> The Milky Way is one of the two largest galaxies in the <a href="/wiki/Local_Group" title="Local Group">Local Group</a> (the other being the <a href="/wiki/Andromeda_Galaxy" title="Andromeda Galaxy">Andromeda Galaxy</a>), although the size for its <a href="/wiki/Galactic_disc" title="Galactic disc">galactic disc</a> and how much it defines the isophotal diameter is not well understood.<a href="#cite_note-Lopez2018-12">[11]</a> It is estimated that the significant bulk of stars in the galaxy lies within the 26 kiloparsecs (80,000 light-years) diameter, and that the number of stars beyond the outermost disc dramatically reduces to a very low number, with respect to an extrapolation of the exponential disk with the scale length of the inner disc.<a href="#cite_note-arxiv0909.3857-125">[120]</a><a href="#cite_note-Lopez2018-12">[11]</a> There are several methods being used in astronomy in defining the size of a galaxy, and each of them can yield different results with respect to one another. The most commonly employed method is the <a href="/wiki/Galaxy#Isophotal_diameter" title="Galaxy">D25 standard</a> – the <a href="/wiki/Isophote" title="Isophote">isophote</a> where the photometric brightness of a galaxy in the B-band (445 nm wavelength of light, in the blue part of the <a href="/wiki/Visible_spectrum" title="Visible spectrum">visible spectrum</a>) reaches 25 mag/arcsec2.<a href="#cite_note-Dimensions-126">[121]</a> An estimate from 1997 by Goodwin and others compared the distribution of <a href="/wiki/Cepheid_variable" title="Cepheid variable">Cepheid variable</a> stars in 17 other spiral galaxies to the ones in the Milky Way, and modelling the relationship to their surface brightnesses. This gave an <a href="/wiki/Isophotal_diameter" class="mw-redirect" title="Isophotal diameter">isophotal diameter</a> for the Milky Way at 26.8 ± 1.1 kiloparsecs (87,400 ± 3,600 light-years), by assuming that the galactic disc is well represented by an exponential disc and adopting a central surface brightness of the galaxy (μ0) of 22.1±0.3 B-mag/arcsec−2 and a disk scale length (h) of 5.0 ± 0.5 kpc (16,300 ± 1,600 ly).<a href="#cite_note-Average-127">[122]</a><a href="#cite_note-Goodwin-11">[10]</a><a href="#cite_note-Castro-128">[123]</a> This is significantly smaller than the Andromeda Galaxy's isophotal diameter, and slightly below the mean isophotal sizes of the galaxies being at 28.3 kpc (92,000 ly).<a href="#cite_note-Goodwin-11">[10]</a> The paper concludes that the Milky Way and Andromeda Galaxy were not overly large spiral galaxies, nor were among the <a href="/wiki/List_of_largest_galaxies" title="List of largest galaxies">largest known</a> (if the former not being the largest) as previously widely believed, but rather average ordinary spiral galaxies.<a href="#cite_note-Goodwin_Hubble-129">[124]</a> To compare the relative physical scale of the Milky Way, if the <a href="/wiki/Solar_System" title="Solar System">Solar System</a> out to <a href="/wiki/Neptune" title="Neptune">Neptune</a> were the size of a <a href="/wiki/Quarter_(United_States_coin)" title="Quarter (United States coin)">US quarter</a> (24.3 mm (0.955 in)), the Milky Way would be approximately at least the greatest north–south line of the <a href="/wiki/Contiguous_United_States" title="Contiguous United States">contiguous United States</a>.<a href="#cite_note-130">[125]</a> An even older study from 1978 gave a lower diameter for Milky Way about 23 kpc (75,000 ly).<a href="#cite_note-Goodwin-11">[10]</a> A 2015 paper discovered that there is a ring-like filament of stars called Triangulum–Andromeda Ring (TriAnd Ring) rippling above and below the relatively flat <a href="/wiki/Galactic_plane" title="Galactic plane">galactic plane</a>, which alongside <a href="/wiki/Monoceros_Ring" title="Monoceros Ring">Monoceros Ring</a> were both suggested to be primarily the result of disk oscillations and wrapping around the Milky Way, at a diameter of at least 50 kpc (160,000 ly),<a href="#cite_note-131">[126]</a> which may be part of the Milky Way's outer disk itself, hence making the stellar disk larger by increasing to this size.<a href="#cite_note-rpi2015-132">[127]</a> A more recent 2018 paper later somewhat ruled out this hypothesis, and supported a conclusion that the Monoceros Ring, <a href="/w/index.php?title=A13_(stellar_overdensity)&action=edit&redlink=1" class="new" title="A13 (stellar overdensity) (page does not exist)">A13</a> and TriAnd Ring were stellar overdensities rather kicked out from the main stellar disk, with the velocity dispersion of the RR Lyrae stars found to be higher and consistent with halo membership.<a href="#cite_note-allyson-133">[128]</a> Another 2018 study revealed the very probable presence of disk stars at 26–31.5 kpc (84,800–103,000 ly) from the Galactic Center or perhaps even farther, significantly beyond approximately 13–20 kpc (40,000–70,000 ly), in which it was once believed to be the abrupt drop-off of the stellar density of the disk, meaning that few or no stars were expected to be above this limit, save for stars that belong to the old population of the galactic halo.<a href="#cite_note-Lopez2018-12">[11]</a><a href="#cite_note-nbcnews1-134">[129]</a><a href="#cite_note-135">[130]</a> A 2020 study predicted the edge of the Milky Way's <a href="/wiki/Dark_matter_halo" title="Dark matter halo">dark matter halo</a> being around 292 ± 61 <a href="/wiki/Parsec#Parsecs_and_kiloparsecs" title="Parsec">kpc</a> (952,000 ± 199,000 <a href="/wiki/Light-year" title="Light-year">ly</a>), which translates to a diameter of 584 ± 122 <a href="/wiki/Parsec#Parsecs_and_kiloparsecs" title="Parsec">kpc</a> (1.905 ± 0.3979 <a href="/wiki/Light-year#Definitions" title="Light-year">Mly</a>).<a href="#cite_note-croswell2020-29">[26]</a><a href="#cite_note-dearson2020-30">[27]</a> The Milky Way's stellar disk is also estimated to be approximately up to 1.35 kpc (4,000 ly) thick.<a href="#cite_note-ask-astro-136">[131]</a><a href="#cite_note-Rix_Bovy-137">[132]</a> <div class="mw-heading mw-heading3"><h3 id="Mass">Mass</h3></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Milky_way_profile.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c3/Milky_way_profile.svg/260px-Milky_way_profile.svg.png" decoding="async" width="260" height="272" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c3/Milky_way_profile.svg/390px-Milky_way_profile.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c3/Milky_way_profile.svg/520px-Milky_way_profile.svg.png 2x" data-file-width="1681" data-file-height="1760" /></a><figcaption>A schematic profile of the Milky Way. Abbreviations: GNP/GSP: Galactic North and South Poles</figcaption></figure>The Milky Way is approximately 890 billion to 1.54 trillion times the mass of the <a href="/wiki/Sun" title="Sun">Sun</a> in total (8.9×1011 to 1.54×1012 solar masses),<a href="#cite_note-SA-20190308-8">[7]</a><a href="#cite_note-ARX-20190208-9">[8]</a><a href="#cite_note-Kafle2012-10">[9]</a> although stars and planets make up only a small part of this. Estimates of the mass of the Milky Way vary, depending upon the method and data used. The low end of the estimate range is 5.8×1011 <a href="/wiki/Solar_mass" title="Solar mass">solar masses</a> (<var>M</var>☉), somewhat less than that of the <a href="/wiki/Andromeda_Galaxy" title="Andromeda Galaxy">Andromeda Galaxy</a>.<a href="#cite_note-Karachentsevetal2006-138">[133]</a><a href="#cite_note-mass-139">[134]</a><a href="#cite_note-galmass-140">[135]</a> Measurements using the <a href="/wiki/Very_Long_Baseline_Array" title="Very Long Baseline Array">Very Long Baseline Array</a> in 2009 found velocities as large as 254 km/s (570,000 mph) for stars at the outer edge of the Milky Way.<a href="#cite_note-nrao20090105-141">[136]</a> Because the orbital velocity depends on the total mass inside the orbital radius, this suggests that the Milky Way is more massive, roughly equaling the mass of Andromeda Galaxy at 7×1011 <var>M</var>☉ within 160,000 ly (49 kpc) of its center.<a href="#cite_note-reid2009-142">[137]</a> In 2010, a measurement of the radial velocity of halo stars found that the mass enclosed within 80 kilo<a href="/wiki/Parsec" title="Parsec">parsecs</a> is 7×1011 <var>M</var>☉.<a href="#cite_note-gnedin2010-143">[138]</a> In a 2014 study, the mass of the entire Milky Way is estimated to be 8.5×1011 <var>M</var>☉,<a href="#cite_note-Jorge_Peñarrubia2014-144">[139]</a> but this is only half the mass of the Andromeda Galaxy.<a href="#cite_note-Jorge_Peñarrubia2014-144">[139]</a> A recent 2019 mass estimate for the Milky Way is 1.29×1012 <var>M</var>☉.<a href="#cite_note-145">[140]</a> Much of the mass of the Milky Way seems to be <a href="/wiki/Dark_matter" title="Dark matter">dark matter</a>, an unknown and invisible form of matter that interacts gravitationally with ordinary matter. A <a href="/wiki/Dark_matter_halo" title="Dark matter halo">dark matter halo</a> is conjectured to spread out relatively uniformly to a distance beyond one hundred kiloparsecs (kpc) from the Galactic Center. Mathematical models of the Milky Way suggest that the mass of dark matter is 1–1.5×1012 <var>M</var>☉.<a href="#cite_note-McMillan2011-146">[141]</a><a href="#cite_note-McMillan2016-147">[142]</a><a href="#cite_note-148">[143]</a> 2013 and 2014 studies indicate a range in mass, as large as 4.5×1012 <var>M</var>☉<a href="#cite_note-149">[144]</a> and as small as 8×1011 <var>M</var>☉.<a href="#cite_note-150">[145]</a> By comparison, the total mass of all the stars in the Milky Way is estimated to be between 4.6×1010 <var>M</var>☉<a href="#cite_note-Licquia2013-151">[146]</a> and 6.43×1010 <var>M</var>☉.<a href="#cite_note-McMillan2011-146">[141]</a> In addition to the stars, there is also interstellar gas, comprising 90% <a href="/wiki/Hydrogen" title="Hydrogen">hydrogen</a> and 10% <a href="/wiki/Helium" title="Helium">helium</a> by mass,<a href="#cite_note-ism1-152">[147]</a> [<a href="/wiki/Wikipedia:Reliable_sources" title="Wikipedia:Reliable sources">unreliable source?</a>] with two thirds of the hydrogen found in the <a href="/wiki/Neutral_hydrogen" class="mw-redirect" title="Neutral hydrogen">atomic form</a> and the remaining one-third as <a href="/wiki/Molecular_hydrogen" class="mw-redirect" title="Molecular hydrogen">molecular hydrogen</a>.<a href="#cite_note-ism2-153">[148]</a> The mass of the Milky Way's interstellar gas is equal to between 10%<a href="#cite_note-ism2-153">[148]</a> and 15%<a href="#cite_note-ism1-152">[147]</a> of the total mass of its stars. <a href="/wiki/Interstellar_dust" class="mw-redirect" title="Interstellar dust">Interstellar dust</a> accounts for an additional 1% of the total mass of the gas.<a href="#cite_note-ism1-152">[147]</a> In March 2019, astronomers reported that the <a href="/wiki/Virial_mass" title="Virial mass">virial mass</a> of the Milky Way Galaxy is 1.54 trillion <a href="/wiki/Solar_mass" title="Solar mass">solar masses</a> within a <a href="/wiki/Radius" title="Radius">radius</a> of about 39.5 kpc (130,000 ly), over twice as much as was determined in earlier studies, suggesting that about 90% of the mass of the galaxy is <a href="/wiki/Dark_matter" title="Dark matter">dark matter</a>.<a href="#cite_note-SA-20190308-8">[7]</a><a href="#cite_note-ARX-20190208-9">[8]</a> In September 2023, astronomers reported that the <a href="/wiki/Virial_mass" title="Virial mass">virial mass</a> of the Milky Way Galaxy is only 2.06 1011 <a href="/wiki/Solar_mass" title="Solar mass">solar masses</a>, only a 10th of the mass of previous studies. The mass was determined from data of the <a href="/wiki/Gaia_(spacecraft)" title="Gaia (spacecraft)">Gaia spacecraft</a>.<a href="#cite_note-aA-20230927-154">[149]</a> <div style="clear:both;" class=""></div> <div class="mw-heading mw-heading2"><h2 id="Contents">Contents</h2></div> The Milky Way contains between 100 and 400 billion stars<a href="#cite_note-frommert_kronberg2005-14">[12]</a><a href="#cite_note-wethington2010-15">[13]</a> and at least that many planets.<a href="#cite_note-villard20120111-155">[150]</a> An exact figure would depend on counting the number of very-low-mass stars, which are difficult to detect, especially at distances of more than 300 ly (90 pc) from the Sun. As a comparison, the neighboring Andromeda Galaxy contains an estimated one trillion (1012) stars.<a href="#cite_note-young2006-156">[151]</a> The Milky Way may contain ten billion <a href="/wiki/White_dwarf" title="White dwarf">white dwarfs</a>, a billion <a href="/wiki/Neutron_star" title="Neutron star">neutron stars</a>, and a hundred million stellar <a href="/wiki/Black_hole" title="Black hole">black holes</a>.<a href="#cite_note-number-159">[f]</a><a href="#cite_note-160">[154]</a><a href="#cite_note-161">[155]</a> Filling the space between the stars is a disk of gas and dust called the <a href="/wiki/Interstellar_medium" title="Interstellar medium">interstellar medium</a>. This disk has at least a comparable extent in radius to the stars,<a href="#cite_note-science312_1773-162">[156]</a> whereas the thickness of the gas layer ranges from hundreds of light-years for the colder gas to thousands of light-years for warmer gas.<a href="#cite_note-araa28_215-163">[157]</a><a href="#cite_note-apj702_1472-164">[158]</a> The disk of stars in the Milky Way does not have a sharp edge beyond which there are no stars. Rather, the concentration of stars decreases with distance from the center of the Milky Way. Beyond a radius of roughly 40,000 light years (13 kpc) from the center, the number of stars per cubic <a href="/wiki/Parsec" title="Parsec">parsec</a> drops much faster with radius.<a href="#cite_note-arxiv0909.3857-125">[120]</a> Surrounding the galactic disk is a spherical <a href="/wiki/Galactic_halo" title="Galactic halo">galactic halo</a> of stars and <a href="/wiki/Globular_cluster" title="Globular cluster">globular clusters</a> that extends farther outward, but is limited in size by the orbits of two Milky Way satellites, the Large and Small <a href="/wiki/Magellanic_Clouds" title="Magellanic Clouds">Magellanic Clouds</a>, whose <a href="/wiki/Apsis" title="Apsis">closest approach</a> to the Galactic Center is about 180,000 ly (55 kpc).<a href="#cite_note-mnras371_1_108-165">[159]</a> At this distance or beyond, the orbits of most halo objects would be disrupted by the Magellanic Clouds. Hence, such objects would probably be ejected from the vicinity of the Milky Way. The integrated <a href="/wiki/Absolute_visual_magnitude" class="mw-redirect" title="Absolute visual magnitude">absolute visual magnitude</a> of the Milky Way is estimated to be around −20.9.<a href="#cite_note-coffey-166">[160]</a><a href="#cite_note-Karachentsev2004-167">[161]</a><a href="#cite_note-milky_way_mag-168">[g]</a> Both <a href="/wiki/Gravitational_microlensing" title="Gravitational microlensing">gravitational microlensing</a> and planetary transit observations indicate that there may be at least as many planets bound to stars as there are stars in the Milky Way,<a href="#cite_note-Nature-20120111-35">[32]</a><a href="#cite_note-borenstein2011-169">[162]</a> and microlensing measurements indicate that there are more <a href="/wiki/Rogue_planet" title="Rogue planet">rogue planets</a> not bound to host stars than there are stars.<a href="#cite_note-170">[163]</a><a href="#cite_note-nasa20110526-171">[164]</a> The Milky Way contains an average of at least one planet per star, resulting in 100–400 billion planets, according to a January 2013 study of the five-planet star system <a href="/wiki/Kepler-32" title="Kepler-32">Kepler-32</a> by the <a href="/wiki/Kepler_(spacecraft)" class="mw-redirect" title="Kepler (spacecraft)">Kepler</a> space observatory.<a href="#cite_note-Space-20130102-36">[33]</a> A different January 2013 analysis of Kepler data estimated that at least 17 billion <a href="/wiki/Terrestrial_planet" title="Terrestrial planet">Earth-sized</a> <a href="/wiki/Exoplanet" title="Exoplanet">exoplanets</a> reside in the Milky Way.<a href="#cite_note-Space-Billions-172">[165]</a> In November 2013, astronomers reported, based on <a href="/wiki/Kepler_(spacecraft)" class="mw-redirect" title="Kepler (spacecraft)">Kepler space mission</a> data, that there could be as many as 40 billion Earth-sized <a href="/wiki/Extrasolar_planet" class="mw-redirect" title="Extrasolar planet">planets</a> orbiting in the <a href="/wiki/Habitable_zone" title="Habitable zone">habitable zones</a> of <a href="/wiki/Solar_analog" title="Solar analog">Sun-like stars</a> and <a href="/wiki/Red_dwarf" title="Red dwarf">red dwarfs</a> within the Milky Way.<a href="#cite_note-NYT-20131104-173">[166]</a><a href="#cite_note-PNAS-20131031-174">[167]</a><a href="#cite_note-nov2013_planet_estimate-175">[168]</a> 11 billion of these estimated planets may be orbiting Sun-like stars.<a href="#cite_note-LATimes-20131104-176">[169]</a> The nearest exoplanet may be 4.2 light-years away, orbiting the <a href="/wiki/Red_dwarf" title="Red dwarf">red dwarf</a> <a href="/wiki/Proxima_Centauri" title="Proxima Centauri">Proxima Centauri</a>, according to a 2016 study.<a href="#cite_note-Planet-Alpha-Centauri-177">[170]</a> Such Earth-sized planets may be more numerous than gas giants,<a href="#cite_note-Nature-20120111-35">[32]</a> though harder to detect at great distances given their small size. Besides exoplanets, "<a href="/wiki/Exocomet" title="Exocomet">exocomets</a>", <a href="/wiki/Comet" title="Comet">comets</a> beyond the Solar System, have also been detected and may be common in the Milky Way.<a href="#cite_note-Space-Exocomets-178">[171]</a> More recently, in November 2020, over 300 million habitable exoplanets are estimated to exist in the Milky Way Galaxy.<a href="#cite_note-NYT-20201105-179">[172]</a> When compared to other more distant galaxies in the universe, the Milky Way galaxy has a below average amount of <a href="/w/index.php?title=Neutrino_luminosity&action=edit&redlink=1" class="new" title="Neutrino luminosity (page does not exist)">neutrino luminosity</a> making our galaxy a "<a href="/w/index.php?title=Neutrino_desert&action=edit&redlink=1" class="new" title="Neutrino desert (page does not exist)">neutrino desert</a>".<a href="#cite_note-180">[173]</a> <div class="mw-heading mw-heading2"><h2 id="Structure">Structure</h2></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Milky_Way_side_view.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/1/19/Milky_Way_side_view.png/300px-Milky_Way_side_view.png" decoding="async" width="300" height="300" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/1/19/Milky_Way_side_view.png/450px-Milky_Way_side_view.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/1/19/Milky_Way_side_view.png/600px-Milky_Way_side_view.png 2x" data-file-width="4200" data-file-height="4200" /></a><figcaption>Overview of different elements of the overall structure of the Milky Way</figcaption></figure> The Milky Way consists of a bar-shaped core region surrounded by a warped disk of <a href="/wiki/Interstellar_medium" title="Interstellar medium">gas, dust</a> and stars.<a href="#cite_note-181">[174]</a><a href="#cite_note-182">[175]</a> The mass distribution within the Milky Way closely resembles the type Sbc in the <a href="/wiki/Hubble_sequence" title="Hubble sequence">Hubble classification</a>, which represents spiral galaxies with relatively loosely wound arms.<a href="#cite_note-ssr100_1_129-6">[5]</a> Astronomers first began to conjecture that the Milky Way is a <a href="/wiki/Barred_spiral_galaxy" title="Barred spiral galaxy">barred spiral galaxy</a>, rather than an ordinary <a href="/wiki/Spiral_galaxy" title="Spiral galaxy">spiral galaxy</a>, in the 1960s.<a href="#cite_note-183">[176]</a><a href="#cite_note-184">[177]</a><a href="#cite_note-185">[178]</a> These conjectures were confirmed by the <a href="/wiki/Spitzer_Space_Telescope" title="Spitzer Space Telescope">Spitzer Space Telescope</a> observations in 2005 that showed the Milky Way's central bar to be larger than previously thought.<a href="#cite_note-fn3-186">[179]</a> <div class="mw-heading mw-heading3"><h3 id="Galactic_Center">Galactic Center</h3></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main articles: <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a> and <a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a></div> <style data-mw-deduplicate="TemplateStyles:r1237032888/mw-parser-output/.tmulti">.mw-parser-output .tmulti .multiimageinner{display:flex;flex-direction:column}.mw-parser-output .tmulti .trow{display:flex;flex-direction:row;clear:left;flex-wrap:wrap;width:100%;box-sizing:border-box}.mw-parser-output .tmulti .tsingle{margin:1px;float:left}.mw-parser-output .tmulti .theader{clear:both;font-weight:bold;text-align:center;align-self:center;background-color:transparent;width:100%}.mw-parser-output .tmulti .thumbcaption{background-color:transparent}.mw-parser-output .tmulti .text-align-left{text-align:left}.mw-parser-output .tmulti .text-align-right{text-align:right}.mw-parser-output .tmulti .text-align-center{text-align:center}@media all and (max-width:720px){.mw-parser-output .tmulti .thumbinner{width:100%!important;box-sizing:border-box;max-width:none!important;align-items:center}.mw-parser-output .tmulti .trow{justify-content:center}.mw-parser-output .tmulti .tsingle{float:none!important;max-width:100%!important;box-sizing:border-box;text-align:center}.mw-parser-output .tmulti .tsingle .thumbcaption{text-align:left}.mw-parser-output .tmulti .trow>.thumbcaption{text-align:center}}@media screen{html.skin-theme-clientpref-night .mw-parser-output .tmulti .multiimageinner img{background-color:white}}@media screen and (prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .tmulti .multiimageinner img{background-color:white}}</style><div class="thumb tmulti tright"><div class="thumbinner multiimageinner" style="width:392px;max-width:392px"><div class="trow"><div class="tsingle" style="width:194px;max-width:194px"><div class="thumbimage" style="height:192px;overflow:hidden"><a href="/wiki/File:EHT_Saggitarius_A_black_hole.tif" class="mw-file-description"><img alt="A dark spot surrounded by doughnut shaped orange-yellow ring" src="//upload.wikimedia.org/wikipedia/commons/thumb/9/96/EHT_Saggitarius_A_black_hole.tif/lossy-page1-192px-EHT_Saggitarius_A_black_hole.tif.jpg" decoding="async" width="192" height="192" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/96/EHT_Saggitarius_A_black_hole.tif/lossy-page1-288px-EHT_Saggitarius_A_black_hole.tif.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/96/EHT_Saggitarius_A_black_hole.tif/lossy-page1-384px-EHT_Saggitarius_A_black_hole.tif.jpg 2x" data-file-width="4076" data-file-height="4076" /></a></div><div class="thumbcaption"><a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">Supermassive black hole</a> <a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a> imaged by the <a href="/wiki/Event_Horizon_Telescope" title="Event Horizon Telescope">Event Horizon Telescope</a> in radio waves. The central dark spot is the black hole's shadow, which is larger than the <a href="/wiki/Event_horizon" title="Event horizon">event horizon</a>.</div></div><div class="tsingle" style="width:194px;max-width:194px"><div class="thumbimage" style="height:192px;overflow:hidden"><a href="/wiki/File:X-RayFlare-BlackHole-MilkyWay-20140105.jpg" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/8/85/X-RayFlare-BlackHole-MilkyWay-20140105.jpg/192px-X-RayFlare-BlackHole-MilkyWay-20140105.jpg" decoding="async" width="192" height="192" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/85/X-RayFlare-BlackHole-MilkyWay-20140105.jpg/288px-X-RayFlare-BlackHole-MilkyWay-20140105.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/85/X-RayFlare-BlackHole-MilkyWay-20140105.jpg/384px-X-RayFlare-BlackHole-MilkyWay-20140105.jpg 2x" data-file-width="1200" data-file-height="1200" /></a></div><div class="thumbcaption">Bright <a href="/wiki/X-ray" title="X-ray">X-ray</a> flares from Sagittarius A* (inset) in the center of the Milky Way, as detected by the <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a>.<a href="#cite_note-NASA-20150105-187">[180]</a></div></div></div></div></div> The Sun is 25,000–28,000 ly (7.7–8.6 kpc) from the Galactic Center. This value is estimated using <a href="/wiki/Geometric" class="mw-redirect" title="Geometric">geometric</a>-based methods or by measuring selected astronomical objects that serve as <a href="/wiki/Standard_candles" class="mw-redirect" title="Standard candles">standard candles</a>, with different techniques yielding various values within this approximate range.<a href="#cite_note-apj692_2_1075-188">[181]</a><a href="#cite_note-boehle2016-108">[103]</a><a href="#cite_note-Gillessen2016-37">[34]</a><a href="#cite_note-ReideaSgrb2009-189">[182]</a><a href="#cite_note-vanhollebeke09-190">[183]</a><a href="#cite_note-majaess10-191">[184]</a> In the inner few kiloparsecs (around 10,000 light-years radius) is a dense concentration of mostly old stars in a roughly spheroidal shape called <a href="/wiki/Bulge_(astronomy)" class="mw-redirect" title="Bulge (astronomy)">the bulge</a>.<a href="#cite_note-Galactic_bulge-192">[185]</a> It has been proposed that the Milky Way lacks a <a href="/wiki/Galactic_bulge#Classical_bulges" title="Galactic bulge">bulge</a> due to a <a href="/wiki/Galactic_merger" class="mw-redirect" title="Galactic merger">collision and merger between previous galaxies</a>, and that instead it only has a <a href="/wiki/Galactic_bulge#Disk-like_Bulges" title="Galactic bulge">pseudobulge</a> formed by its central bar.<a href="#cite_note-apjl_1_l72-193">[186]</a> However, confusion in the literature between the (peanut shell)-shaped structure created by instabilities in the bar, versus a possible bulge with an expected half-light radius of 0.5 kpc, abounds.<a href="#cite_note-194">[187]</a> The Galactic Center is marked by an intense <a href="/wiki/Radio_astronomy" title="Radio astronomy">radio source</a> named <a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a> (pronounced Sagittarius A-star). The motion of material around the center indicates that Sagittarius A* harbors a massive, compact object.<a href="#cite_note-Jones2004-195">[188]</a> This concentration of mass is best explained as a <a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">supermassive black hole</a><a href="#cite_note-chandra2003-196">[h]</a><a href="#cite_note-apj692_2_1075-188">[181]</a><a href="#cite_note-apj689_2_1044-197">[189]</a> (SMBH) with an estimated mass of 4.1–4.5 million times the <a href="/wiki/Solar_mass" title="Solar mass">mass of the Sun</a>.<a href="#cite_note-apj689_2_1044-197">[189]</a> The rate of accretion of the SMBH is consistent with an <a href="/wiki/Active_galactic_nucleus" title="Active galactic nucleus">inactive galactic nucleus</a>, being estimated at 1×10−5 <var>M</var>☉ per year.<a href="#cite_note-wang13-198">[190]</a> Observations indicate that there are SMBHs located near the center of most normal galaxies.<a href="#cite_note-blandford1999-199">[191]</a><a href="#cite_note-frolov_zelnikov2011-200">[192]</a> The nature of the Milky Way's bar is actively debated, with estimates for its half-length and orientation spanning from 1 to 5 kpc (3,000–16,000 ly) and 10–50 degrees relative to the line of sight from Earth to the Galactic Center.<a href="#cite_note-vanhollebeke09-190">[183]</a><a href="#cite_note-majaess10-191">[184]</a><a href="#cite_note-Cabrera-Lavers08-201">[193]</a> Certain authors advocate that the Milky Way features two distinct bars, one nestled within the other.<a href="#cite_note-nishiyama06-202">[194]</a> However, <a href="/wiki/RR_Lyrae_variable" title="RR Lyrae variable">RR Lyrae-type</a> stars do not trace a prominent Galactic bar.<a href="#cite_note-majaess10-191">[184]</a><a href="#cite_note-alcock98-203">[195]</a><a href="#cite_note-kunder08-204">[196]</a> The bar may be surrounded by a ring called the "5 kpc ring" that contains a large fraction of the molecular hydrogen present in the Milky Way, as well as most of the Milky Way's <a href="/wiki/Star_formation" title="Star formation">star formation</a> activity. Viewed from the <a href="/wiki/Andromeda_Galaxy" title="Andromeda Galaxy">Andromeda Galaxy</a>, it would be the brightest feature of the Milky Way.<a href="#cite_note-fn14-205">[197]</a> X-ray emission from the core is aligned with the massive stars surrounding the central bar<a href="#cite_note-wang13-198">[190]</a> and the <a href="/wiki/Galactic_ridge" title="Galactic ridge">Galactic ridge</a>.<a href="#cite_note-nature318_267-206">[198]</a> In June 2023, astronomers reported using a new cascade neutrino technique<a href="#cite_note-207">[199]</a> to detect, for the first time, the release of <a href="/wiki/Neutrino" title="Neutrino">neutrinos</a> from the <a href="/wiki/Galactic_plane" title="Galactic plane">galactic plane</a> of the Milky Way <a href="/wiki/Galaxy" title="Galaxy">galaxy</a>, creating the first neutrino view of the Milky Way.<a href="#cite_note-NYT-20230629-208">[200]</a><a href="#cite_note-SCI-20230629-209">[201]</a> <div class="mw-heading mw-heading4"><h4 id="Gamma_rays_and_x-rays">Gamma rays and x-rays</h4></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:SRG-eROSITA_all-sky_image.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/43/SRG-eROSITA_all-sky_image.jpg/350px-SRG-eROSITA_all-sky_image.jpg" decoding="async" width="350" height="178" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/43/SRG-eROSITA_all-sky_image.jpg/525px-SRG-eROSITA_all-sky_image.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/43/SRG-eROSITA_all-sky_image.jpg/700px-SRG-eROSITA_all-sky_image.jpg 2x" data-file-width="3770" data-file-height="1915" /></a><figcaption>All-sky x-ray image</figcaption></figure> Since 1970, various gamma-ray detection missions have discovered 511-<a href="/wiki/KeV" class="mw-redirect" title="KeV">keV</a> <a href="/wiki/Gamma_rays" class="mw-redirect" title="Gamma rays">gamma rays</a> coming from the general direction of the Galactic Center. These gamma rays are produced by <a href="/wiki/Positrons" class="mw-redirect" title="Positrons">positrons</a> (antielectrons) annihilating with <a href="/wiki/Electron" title="Electron">electrons</a>. In 2008 it was found that the distribution of the sources of the gamma rays resembles the distribution of low-mass <a href="/wiki/X-ray_binaries" class="mw-redirect" title="X-ray binaries">X-ray binaries</a>, seeming to indicate that these X-ray binaries are sending positrons (and electrons) into interstellar space where they slow down and annihilate.<a href="#cite_note-210">[202]</a><a href="#cite_note-NASA-2008-211">[203]</a><a href="#cite_note-212">[204]</a> The observations were both made by <a href="/wiki/NASA" title="NASA">NASA</a> and <a href="/wiki/European_Space_Agency" title="European Space Agency">ESA</a>'s satellites. In 1970 gamma ray detectors found that the emitting region was about 10,000 light-years across with a luminosity of about 10,000 suns.<a href="#cite_note-NASA-2008-211">[203]</a> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:800_nasa_structure_renderin2.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5a/800_nasa_structure_renderin2.jpg/300px-800_nasa_structure_renderin2.jpg" decoding="async" width="300" height="169" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5a/800_nasa_structure_renderin2.jpg/450px-800_nasa_structure_renderin2.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5a/800_nasa_structure_renderin2.jpg/600px-800_nasa_structure_renderin2.jpg 2x" data-file-width="2896" data-file-height="1629" /></a><figcaption>Illustration of the two gigantic <a href="/wiki/X-ray" title="X-ray">X-ray</a>/<a href="/wiki/Gamma-ray" class="mw-redirect" title="Gamma-ray">gamma-ray</a> bubbles (blue-violet) of the Milky Way (center)</figcaption></figure> In 2010, two gigantic spherical bubbles of high energy gamma-emission were detected to the north and the south of the Milky Way core, using data from the <a href="/wiki/Fermi_Gamma-ray_Space_Telescope" title="Fermi Gamma-ray Space Telescope">Fermi Gamma-ray Space Telescope</a>. The diameter of each of the bubbles is about 25,000 light-years (7.7 kpc) (or about 1/4 of the galaxy's estimated diameter); they stretch up to <a href="/wiki/Grus_(constellation)" title="Grus (constellation)">Grus</a> and to <a href="/wiki/Virgo_(constellation)" title="Virgo (constellation)">Virgo</a> on the night-sky of the southern hemisphere.<a href="#cite_note-overbye2010-213">[205]</a><a href="#cite_note-sz2010-214">[206]</a> Subsequently, observations with the <a href="/wiki/Parkes_Telescope" class="mw-redirect" title="Parkes Telescope">Parkes Telescope</a> at radio frequencies identified polarized emission that is associated with the Fermi bubbles. These observations are best interpreted as a magnetized outflow driven by star formation in the central 640 ly (200 pc) of the Milky Way.<a href="#cite_note-215">[207]</a> Later, on January 5, 2015, <a href="/wiki/NASA" title="NASA">NASA</a> reported observing an <a href="/wiki/X-ray" title="X-ray">X-ray</a> flare 400 times brighter than usual, a record-breaker, from Sagittarius A*. The unusual event may have been caused by the breaking apart of an <a href="/wiki/Asteroid" title="Asteroid">asteroid</a> falling into the black hole or by the entanglement of <a href="/wiki/Magnetic_field_lines" class="mw-redirect" title="Magnetic field lines">magnetic field lines</a> within gas flowing into Sagittarius A*.<a href="#cite_note-NASA-20150105-187">[180]</a> <div class="mw-heading mw-heading3"><h3 id="Spiral_arms">Spiral arms</h3></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Further information: <a href="/wiki/Spiral_galaxy" title="Spiral galaxy">Spiral galaxy</a></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Milky_Way_Arms.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/1/1d/Milky_Way_Arms.svg/320px-Milky_Way_Arms.svg.png" decoding="async" width="320" height="302" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/1/1d/Milky_Way_Arms.svg/480px-Milky_Way_Arms.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/1/1d/Milky_Way_Arms.svg/640px-Milky_Way_Arms.svg.png 2x" data-file-width="614" data-file-height="580" /></a><figcaption>Observed (normal lines) and extrapolated (dotted lines) structure of the spiral arms of the Milky Way, viewed from north of the galaxy – the galaxy rotates clockwise in this view. The gray lines radiating from the Sun's position (upper center) list the three-letter abbreviations of the corresponding constellations</figcaption></figure>Outside the gravitational influence of the Galactic bar, the structure of the interstellar medium and stars in the disk of the Milky Way is organized into four spiral arms.<a href="#cite_note-churchwell09-216">[208]</a> Spiral arms typically contain a higher density of interstellar gas and dust than the Galactic average as well as a greater concentration of star formation, as traced by <a href="/wiki/H_II_region" title="H II region">H II regions</a><a href="#cite_note-TaylorCordes-217">[209]</a><a href="#cite_note-russeil03-218">[210]</a> and <a href="/wiki/Molecular_cloud" title="Molecular cloud">molecular clouds</a>.<a href="#cite_note-219">[211]</a> The Milky Way's spiral structure is uncertain, and there is currently no consensus on the nature of the Milky Way's arms.<a href="#cite_note-two_arms-220">[212]</a> Perfect logarithmic spiral patterns only crudely describe features near the Sun,<a href="#cite_note-russeil03-218">[210]</a><a href="#cite_note-majaess09b-221">[213]</a> because galaxies commonly have arms that branch, merge, twist unexpectedly, and feature a degree of irregularity.<a href="#cite_note-majaess10-191">[184]</a><a href="#cite_note-majaess09b-221">[213]</a><a href="#cite_note-lepine10-222">[214]</a> The possible scenario of the Sun within a spur / Local arm<a href="#cite_note-russeil03-218">[210]</a> emphasizes that point and indicates that such features are probably not unique, and exist elsewhere in the Milky Way.<a href="#cite_note-majaess09b-221">[213]</a> Estimates of the pitch angle of the arms range from about 7° to 25°.<a href="#cite_note-science312_1773-162">[156]</a><a href="#cite_note-Drimmel2000-223">[215]</a> There are thought to be four spiral arms that all start near the Milky Way Galaxy's center.<a href="#cite_note-224">[216]</a> These are named as follows, with the positions of the arms shown in the image: <table class="wikitable"> <tbody><tr> <th>Color </th> <th>Arm(s) </th></tr> <tr> <td style="background:#28c7b4;">turquoise </td> <td><a href="/wiki/Near_3_kpc_Arm" title="Near 3 kpc Arm">Near 3 kpc</a> and <a href="/wiki/Perseus_Arm" title="Perseus Arm">Perseus Arm</a> </td></tr> <tr> <td style="background:#928bff;">blue </td> <td><a href="/wiki/Norma_Arm" title="Norma Arm">Norma</a> and <a href="/wiki/Outer_arm" class="mw-redirect" title="Outer arm">Outer arm</a> (Along with extension discovered in 2004<a href="#cite_note-mcclure-griffiths-225">[217]</a>) </td></tr> <tr> <td style="background:#07c459;">green </td> <td><a href="/wiki/Far_3_kpc_Arm" title="Far 3 kpc Arm">Far 3 kpc</a> and <a href="/wiki/Scutum%E2%80%93Centaurus_Arm" title="Scutum–Centaurus Arm">Scutum–Centaurus Arm</a> </td></tr> <tr> <td style="background:#ff6c6c;">red </td> <td><a href="/wiki/Carina%E2%80%93Sagittarius_Arm" title="Carina–Sagittarius Arm">Carina–Sagittarius Arm</a> </td></tr> <tr> <td colspan="2" style="text-align:center;">There are at least two smaller arms or spurs, including: </td></tr> <tr> <td style="background:#ff9b00;">orange </td> <td><a href="/wiki/Orion%E2%80%93Cygnus_Arm" class="mw-redirect" title="Orion–Cygnus Arm">Orion–Cygnus Arm</a> (which contains the Sun and Solar System) </td></tr></tbody></table> Two spiral arms, the Scutum–Centaurus arm and the Carina–Sagittarius arm, have tangent points inside the Sun's orbit about the center of the Milky Way. If these arms contain an overdensity of stars compared to the average density of stars in the Galactic disk, it would be detectable by counting the stars near the tangent point. Two surveys of near-infrared light, which is sensitive primarily to red giants and not affected by dust extinction, detected the predicted overabundance in the Scutum–Centaurus arm but not in the Carina–Sagittarius arm: the Scutum–Centaurus Arm contains approximately 30% more <a href="/wiki/Red_giant" title="Red giant">red giants</a> than would be expected in the absence of a spiral arm.<a href="#cite_note-Drimmel2000-223">[215]</a><a href="#cite_note-Benjamin2005-226">[218]</a> This observation suggests that the Milky Way possesses only two major stellar arms: the Perseus arm and the Scutum–Centaurus arm. The rest of the arms contain excess gas but not excess old stars.<a href="#cite_note-two_arms-220">[212]</a> In December 2013, astronomers found that the distribution of young stars and star-forming regions matches the four-arm spiral description of the Milky Way.<a href="#cite_note-227">[219]</a><a href="#cite_note-228">[220]</a><a href="#cite_note-urquart2013-229">[221]</a> Thus, the Milky Way appears to have two spiral arms as traced by old stars and four spiral arms as traced by gas and young stars. The explanation for this apparent discrepancy is unclear.<a href="#cite_note-urquart2013-229">[221]</a> The <a href="/wiki/Near_3_kpc_Arm" title="Near 3 kpc Arm">Near 3 kpc Arm</a> (also called the Expanding 3 kpc Arm or simply the 3 kpc Arm) was discovered in the 1950s by astronomer van Woerden and collaborators through <a href="/wiki/Hydrogen_line" title="Hydrogen line">21 centimeter</a> radio measurements of HI (<a href="/wiki/Atomic_hydrogen" class="mw-redirect" title="Atomic hydrogen">atomic hydrogen</a>).<a href="#cite_note-230">[222]</a><a href="#cite_note-Dame-231">[223]</a> It was found to be expanding away from the central bulge at more than 50 <a href="/wiki/Kilometer_per_second" class="mw-redirect" title="Kilometer per second">km/s</a>. It is located in the fourth galactic quadrant at a distance of about 5.2 <a href="/wiki/Parsec" title="Parsec">kpc</a> from the <a href="/wiki/Sun" title="Sun">Sun</a> and 3.3 kpc from the <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a>. The Far 3 kpc Arm was discovered in 2008 by astronomer Tom Dame (<a href="/wiki/Harvard%E2%80%93Smithsonian_Center_for_Astrophysics" title="Harvard–Smithsonian Center for Astrophysics">Center for Astrophysics | Harvard & Smithsonian</a>). It is located in the first galactic quadrant at a distance of 3 <a href="/wiki/Parsec" title="Parsec">kpc</a> (about 10,000 <a href="/wiki/Light_year" class="mw-redirect" title="Light year">ly</a>) from the Galactic Center.<a href="#cite_note-Dame-231">[223]</a><a href="#cite_note-232">[224]</a> A simulation published in 2011 suggested that the Milky Way may have obtained its spiral arm structure as a result of repeated collisions with the <a href="/wiki/Sagittarius_Dwarf_Elliptical_Galaxy" class="mw-redirect" title="Sagittarius Dwarf Elliptical Galaxy">Sagittarius Dwarf Elliptical Galaxy</a>.<a href="#cite_note-233">[225]</a> It has been suggested that the Milky Way contains two different spiral patterns: an inner one, formed by the Sagittarius arm, that rotates fast and an outer one, formed by the Carina and Perseus arms, whose rotation velocity is slower and whose arms are tightly wound. In this scenario, suggested by numerical simulations of the dynamics of the different spiral arms, the outer pattern would form an outer <a href="/wiki/Galaxy_morphological_classification#De_Vaucouleurs_system" title="Galaxy morphological classification">pseudoring</a>,<a href="#cite_note-pseudoring2-234">[226]</a> and the two patterns would be connected by the Cygnus arm.<a href="#cite_note-pseudoring-235">[227]</a> Outside of the major spiral arms is the <a href="/wiki/Monoceros_Ring" title="Monoceros Ring">Monoceros Ring</a> (or Outer Ring), a ring of gas and stars torn from other galaxies billions of years ago. However, several members of the scientific community recently restated their position affirming the Monoceros structure is nothing more than an over-density produced by the flared and warped <a href="/wiki/Thick_disk" title="Thick disk">thick disk</a> of the Milky Way.<a href="#cite_note-236">[228]</a> The structure of the Milky Way's disk is warped along an <a href="/wiki/Sigmoid_function" title="Sigmoid function">"S" curve</a>.<a href="#cite_note-237">[229]</a> <div class="mw-heading mw-heading3"><h3 id="Halo">Halo</h3></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Galactic_halo" title="Galactic halo">Galactic halo</a></div> The Galactic disk is surrounded by a <a href="/wiki/Galactic_spheroid" class="mw-redirect" title="Galactic spheroid">spheroidal halo</a> of old stars and <a href="/wiki/Globular_cluster" title="Globular cluster">globular clusters</a>, of which 90% lie within 100,000 light-years (30 kpc) of the Galactic Center.<a href="#cite_note-harris2003-238">[230]</a> However, a few globular clusters have been found farther, such as PAL 4 and AM 1 at more than 200,000 light-years from the Galactic Center. About 40% of the Milky Way's clusters are on <a href="/wiki/Retrograde_orbit" class="mw-redirect" title="Retrograde orbit">retrograde orbits</a>, which means they move in the opposite direction from the Milky Way rotation.<a href="#cite_note-aaa313_119-239">[231]</a> The globular clusters can follow <a href="/wiki/Rosette_orbit" class="mw-redirect" title="Rosette orbit">rosette orbits</a> about the Milky Way, in contrast to the <a href="/wiki/Elliptical_orbit" class="mw-redirect" title="Elliptical orbit">elliptical orbit</a> of a planet around a star.<a href="#cite_note-apj522-240">[232]</a> Although the disk contains dust that obscures the view in some wavelengths, the halo component does not. Active <a href="/wiki/Star_formation" title="Star formation">star formation</a> takes place in the disk (especially in the spiral arms, which represent areas of high density), but does not take place in the halo, as there is little cool gas to collapse into stars.<a href="#cite_note-sparke_gallagher-117">[112]</a> <a href="/wiki/Open_cluster" title="Open cluster">Open clusters</a> are also located primarily in the disk.<a href="#cite_note-aj108-241">[233]</a> Discoveries in the early 21st century have added dimension to the knowledge of the Milky Way's structure. With the discovery that the disk of the Andromeda Galaxy (M31) extends much farther than previously thought,<a href="#cite_note-fn5-242">[234]</a> the possibility of the disk of the Milky Way extending farther is apparent, and this is supported by evidence from the discovery of the Outer Arm extension of the <a href="/wiki/Cygnus_Arm" class="mw-redirect" title="Cygnus Arm">Cygnus Arm</a><a href="#cite_note-mcclure-griffiths-225">[217]</a><a href="#cite_note-fn6-243">[235]</a> and of a similar extension of the <a href="/wiki/Scutum%E2%80%93Centaurus_Arm" title="Scutum–Centaurus Arm">Scutum–Centaurus Arm</a>.<a href="#cite_note-244">[236]</a> With the discovery of the <a href="/wiki/Sagittarius_Dwarf_Elliptical_Galaxy" class="mw-redirect" title="Sagittarius Dwarf Elliptical Galaxy">Sagittarius Dwarf Elliptical Galaxy</a> came the discovery of a ribbon of galactic debris as the polar orbit of the dwarf and its interaction with the Milky Way tears it apart. Similarly, with the discovery of the <a href="/wiki/Canis_Major_Dwarf_Galaxy" class="mw-redirect" title="Canis Major Dwarf Galaxy">Canis Major Dwarf Galaxy</a>, it was found that a ring of galactic debris from its interaction with the Milky Way encircles the Galactic disk.[<a href="/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed">citation needed</a>] The <a href="/wiki/Sloan_Digital_Sky_Survey" title="Sloan Digital Sky Survey">Sloan Digital Sky Survey</a> of the northern sky shows a huge and diffuse structure (spread out across an area around 5,000 times the size of a full moon) within the Milky Way that does not seem to fit within current models. The collection of stars rises close to perpendicular to the plane of the spiral arms of the Milky Way. The proposed likely interpretation is that a <a href="/wiki/Dwarf_galaxy" title="Dwarf galaxy">dwarf galaxy</a> is merging with the Milky Way. This galaxy is tentatively named the <a href="/wiki/Virgo_Stellar_Stream" title="Virgo Stellar Stream">Virgo Stellar Stream</a> and is found in the direction of Virgo about 30,000 light-years (9 kpc) away.<a href="#cite_note-apj673_2_864-245">[237]</a> <div class="mw-heading mw-heading4"><h4 id="Gaseous_halo">Gaseous halo</h4></div> In addition to the stellar halo, the <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a>, <a href="/wiki/XMM-Newton" title="XMM-Newton">XMM-Newton</a>, and <a href="/wiki/Suzaku_(satellite)" title="Suzaku (satellite)">Suzaku</a> have provided evidence that there is also a gaseous halo containing a large amount of hot gas. This halo extends for hundreds of thousands of light-years, much farther than the stellar halo and close to the distance of the Large and Small <a href="/wiki/Magellanic_Clouds" title="Magellanic Clouds">Magellanic Clouds</a>. The mass of this hot halo is nearly equivalent to the mass of the Milky Way itself.<a href="#cite_note-chandra_hotgas-246">[238]</a><a href="#cite_note-247">[239]</a><a href="#cite_note-248">[240]</a> The temperature of this halo gas is between 1 and 2.5 million K (1.8 and 4.5 million °F).<a href="#cite_note-249">[241]</a> Observations of distant galaxies indicate that the Universe had about one-sixth as much <a href="/wiki/Baryon" title="Baryon">baryonic</a> (ordinary) matter as dark matter when it was just a few billion years old. However, only about half of those baryons are accounted for in the modern Universe based on observations of nearby galaxies like the Milky Way.<a href="#cite_note-Harrington_feature-250">[242]</a> If the finding that the mass of the halo is comparable to the mass of the Milky Way is confirmed, it could be the identity of the missing baryons around the Milky Way.<a href="#cite_note-Harrington_feature-250">[242]</a> <div class="mw-heading mw-heading3"><h3 id="Galactic_rotation">Galactic rotation</h3></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Rotation_curve_(Milky_Way).svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/7/73/Rotation_curve_%28Milky_Way%29.svg/220px-Rotation_curve_%28Milky_Way%29.svg.png" decoding="async" width="220" height="154" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/7/73/Rotation_curve_%28Milky_Way%29.svg/330px-Rotation_curve_%28Milky_Way%29.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/7/73/Rotation_curve_%28Milky_Way%29.svg/440px-Rotation_curve_%28Milky_Way%29.svg.png 2x" data-file-width="562" data-file-height="393" /></a><figcaption><a href="/wiki/Galaxy_rotation_curve" title="Galaxy rotation curve">Galaxy rotation curve</a> for the Milky Way – vertical axis is speed of rotation about the galactic center; horizontal axis is distance from the galactic center in kpcs; the sun is marked with a yellow ball; the observed curve of speed of rotation is blue; the predicted curve based upon stellar mass and gas in the Milky Way is red; scatter in observations roughly indicated by gray bars, the difference is due to dark matter<a href="#cite_note-Koupelis_Kuhn2007-251">[243]</a><a href="#cite_note-Schneider-252">[244]</a><a href="#cite_note-Jones1-253">[245]</a></figcaption></figure> The stars and gas in the Milky Way rotate about its center <a href="/wiki/Differential_rotation" title="Differential rotation">differentially</a>, meaning that the rotation period varies with location. As is typical for spiral galaxies, the orbital speed of most stars in the Milky Way does not depend strongly on their distance from the center. Away from the central bulge or outer rim, the typical stellar orbital speed is between 210 ± 10 km/s (470,000 ± 22,000 mph).<a href="#cite_note-254">[246]</a> Hence the <a href="/wiki/Orbital_period" title="Orbital period">orbital period</a> of the typical star is directly proportional only to the length of the path traveled. This is unlike the situation within the Solar System, where two-body gravitational dynamics dominate, and different orbits have significantly different velocities associated with them. The rotation curve (shown in the figure) describes this rotation. Toward the center of the Milky Way the orbit speeds are too low, whereas beyond 7 kpcs the speeds are too high to match what would be expected from the universal law of gravitation.[<a href="/wiki/Wikipedia:Citation_needed" title="Wikipedia:Citation needed">citation needed</a>] If the Milky Way contained only the mass observed in stars, gas, and other baryonic (ordinary) matter, the rotational speed would decrease with distance from the center. However, the observed curve is relatively flat, indicating that there is additional mass that cannot be detected directly with electromagnetic radiation. This inconsistency is attributed to dark matter.<a href="#cite_note-Koupelis_Kuhn2007-251">[243]</a> The rotation curve of the Milky Way agrees with the <a href="/wiki/Universal_rotation_curve" class="mw-redirect" title="Universal rotation curve">universal rotation curve</a> of spiral galaxies, the best evidence for the existence of <a href="/wiki/Dark_matter" title="Dark matter">dark matter</a> in galaxies. Alternatively, a minority of astronomers propose that a <a href="/wiki/MOND" class="mw-redirect" title="MOND">modification of the law of gravity</a> may explain the observed rotation curve.<a href="#cite_note-Schneider_p413-255">[247]</a> <div class="mw-heading mw-heading2"><h2 id="Formation">Formation</h2></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Galaxy_formation_and_evolution" title="Galaxy formation and evolution">Galaxy formation and evolution</a></div> <div class="mw-heading mw-heading3"><h3 id="History">History</h3></div> <figure typeof="mw:File/Thumb"><a href="/wiki/File:Galaxy_color-magnitude_diagram-en.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/96/Galaxy_color-magnitude_diagram-en.svg/224px-Galaxy_color-magnitude_diagram-en.svg.png" decoding="async" width="224" height="203" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/96/Galaxy_color-magnitude_diagram-en.svg/336px-Galaxy_color-magnitude_diagram-en.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/96/Galaxy_color-magnitude_diagram-en.svg/448px-Galaxy_color-magnitude_diagram-en.svg.png 2x" data-file-width="671" data-file-height="609" /></a><figcaption>A <a href="/wiki/Galaxy_color%E2%80%93magnitude_diagram" title="Galaxy color–magnitude diagram">galaxy color–magnitude diagram</a> showing the red sequence (old galaxies, typically elliptical galaxies), the green valley (where the Milky Way is believed to be in), and the blue cloud (young galaxies, typically spiral galaxies).</figcaption></figure> The Milky Way began as one or several small overdensities in the mass distribution in the <a href="/wiki/Universe" title="Universe">Universe</a> shortly after the <a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a> 13.61 billion years ago.<a href="#cite_note-PHYS-20170727-256">[248]</a><a href="#cite_note-borah-257">[249]</a><a href="#cite_note-legassick-258">[250]</a> Some of these overdensities were the seeds of globular clusters in which the oldest remaining stars in what is now the Milky Way formed. Nearly half the matter in the Milky Way may have come from other distant galaxies.<a href="#cite_note-PHYS-20170727-256">[248]</a> These stars and clusters now comprise the stellar halo of the Milky Way. Within a few billion years of the birth of the first stars, the mass of the Milky Way was large enough so that it was spinning relatively quickly. Due to <a href="/wiki/Conservation_of_angular_momentum" class="mw-redirect" title="Conservation of angular momentum">conservation of angular momentum</a>, this led the gaseous interstellar medium to collapse from a roughly spheroidal shape to a disk. Therefore, later generations of stars formed in this spiral disk. Most younger stars, including the Sun, are observed to be in the disk.<a href="#cite_note-ut20090527-259">[251]</a><a href="#cite_note-Buser-260">[252]</a> Since the first stars began to form, the Milky Way has grown through both <a href="/wiki/Galaxy_merger" title="Galaxy merger">galaxy mergers</a> (particularly early in the Milky Way's growth) and accretion of gas directly from the Galactic halo.<a href="#cite_note-Buser-260">[252]</a> The Milky Way is currently accreting material from several small galaxies, including two of its largest satellite galaxies, the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large</a> and <a href="/wiki/Small_Magellanic_Cloud" title="Small Magellanic Cloud">Small</a> Magellanic Clouds, through the <a href="/wiki/Magellanic_Stream" title="Magellanic Stream">Magellanic Stream</a>. Direct accretion of gas is observed in <a href="/wiki/High-velocity_cloud" title="High-velocity cloud">high-velocity clouds</a> like the <a href="/wiki/Smith_Cloud" class="mw-redirect" title="Smith Cloud">Smith Cloud</a>.<a href="#cite_note-araa35_217-261">[253]</a><a href="#cite_note-apj679_L21-262">[254]</a> Cosmological simulations indicate that, 11 billion years ago, it merged with a particularly large galaxy that has been labeled the <a href="/wiki/Kraken_galaxy" title="Kraken galaxy">Kraken</a>.<a href="#cite_note-263">[255]</a><a href="#cite_note-264">[256]</a> Properties of the Milky Way such as stellar mass, <a href="/wiki/Angular_momentum" title="Angular momentum">angular momentum</a>, and <a href="/wiki/Metallicity" title="Metallicity">metallicity</a> in its outermost regions suggest it has undergone no mergers with large galaxies in the last 10 billion years. This lack of recent major mergers is unusual among similar spiral galaxies. Its neighbour the Andromeda Galaxy appears to have a more typical history shaped by more recent mergers with relatively large galaxies.<a href="#cite_note-265">[257]</a><a href="#cite_note-266">[258]</a> According to recent studies, the Milky Way as well as the Andromeda Galaxy lie in what in the <a href="/wiki/Galaxy_color%E2%80%93magnitude_diagram" title="Galaxy color–magnitude diagram">galaxy color–magnitude diagram</a> is known as the "green valley", a region populated by galaxies in transition from the "blue cloud" (galaxies actively forming new stars) to the "red sequence" (galaxies that lack star formation). Star-formation activity in green valley galaxies is slowing as they run out of star-forming gas in the interstellar medium. In simulated galaxies with similar properties, star formation will typically have been extinguished within about five billion years from now, even accounting for the expected, short-term increase in the rate of star formation due to the collision between both the Milky Way and the Andromeda Galaxy.<a href="#cite_note-267">[259]</a> Measurements of other galaxies similar to the Milky Way suggest it is among the reddest and brightest spiral galaxies that are still forming new stars and it is just slightly bluer than the bluest red sequence galaxies.<a href="#cite_note-268">[260]</a> <div class="mw-heading mw-heading3"><h3 id="Age_and_cosmological_history">Age and cosmological history</h3></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Early_Milky_Way.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Early_Milky_Way.jpg/290px-Early_Milky_Way.jpg" decoding="async" width="290" height="363" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Early_Milky_Way.jpg/435px-Early_Milky_Way.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Early_Milky_Way.jpg/580px-Early_Milky_Way.jpg 2x" data-file-width="960" data-file-height="1200" /></a><figcaption>Comparison of the night sky with the night sky of a hypothetical planet within the Milky Way 10 billion years ago, at an age of about 3.6 billion years and 5 billion years before the Sun formed.<a href="#cite_note-269">[261]</a></figcaption></figure> Globular clusters are among the oldest objects in the Milky Way, which thus set a lower limit on the age of the Milky Way. The ages of individual stars in the Milky Way can be estimated by measuring the abundance of long-lived <a href="/wiki/Radioactive_element" class="mw-redirect" title="Radioactive element">radioactive elements</a> such as <a href="/wiki/Thorium-232" title="Thorium-232">thorium-232</a> and <a href="/wiki/Uranium-238" title="Uranium-238">uranium-238</a>, then comparing the results to estimates of their original abundance, a technique called <a href="/wiki/Nucleocosmochronology" title="Nucleocosmochronology">nucleocosmochronology</a>. These yield values of about 12.5 ± 3 billion years for <a href="/wiki/Cayrel%27s_Star" title="Cayrel's Star">CS 31082-001</a><a href="#cite_note-270">[262]</a> and 13.8 ± 4 billion years for <a href="/wiki/BD_%2B17%C2%B0_3248" class="mw-redirect" title="BD +17° 3248">BD +17° 3248</a>.<a href="#cite_note-271">[263]</a> Once a <a href="/wiki/White_dwarf" title="White dwarf">white dwarf</a> is formed, it begins to undergo radiative cooling and the surface temperature steadily drops. By measuring the temperatures of the coolest of these white dwarfs and comparing them to their expected initial temperature, an age estimate can be made. With this technique, the age of the globular cluster M4 was estimated as 12.7 ± 0.7 billion years. Age estimates of the oldest of these clusters gives a best fit estimate of 12.6 billion years, and a 95% confidence upper limit of 16 billion years.<a href="#cite_note-science299_5603_65-272">[264]</a> In November 2018, astronomers reported the discovery of one of the oldest stars in the universe. About 13.5 billion-years-old, <a href="/wiki/2MASS_J18082002-5104378_B" class="mw-redirect" title="2MASS J18082002-5104378 B">2MASS J18082002-5104378 B</a> is a tiny ultra metal-poor (UMP) star made almost entirely of materials released from the <a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a>, and is possibly one of the first stars. The discovery of the star in the Milky Way <a href="/wiki/Galaxy" title="Galaxy">Galaxy</a> suggests that the galaxy may be at least 3 billion years older than previously thought.<a href="#cite_note-EA-20181105-273">[265]</a><a href="#cite_note-JHU-20181105-274">[266]</a><a href="#cite_note-ApJ-20181105-275">[267]</a> Several individual stars have been found in the Milky Way's halo with measured ages very close to the 13.80-billion-year <a href="/wiki/Age_of_the_Universe" class="mw-redirect" title="Age of the Universe">age of the Universe</a>. In 2007, a star in the galactic halo, <a href="/wiki/HE_1523-0901" title="HE 1523-0901">HE 1523-0901</a>, was estimated to be about 13.2 billion years old. As the oldest known object in the Milky Way at that time, this measurement placed a lower limit on the age of the Milky Way.<a href="#cite_note-frebel-276">[268]</a> This estimate was made using the UV-Visual Echelle Spectrograph of the <a href="/wiki/Very_Large_Telescope" title="Very Large Telescope">Very Large Telescope</a> to <a href="/wiki/Measurement" title="Measurement">measure</a> the relative strengths of <a href="/wiki/Spectral_line" title="Spectral line">spectral lines</a> caused by the presence of <a href="/wiki/Thorium" title="Thorium">thorium</a> and other <a href="/wiki/Chemical_element" title="Chemical element">elements</a> created by the <a href="/wiki/R-process" title="R-process">R-process</a>. The line strengths yield abundances of different elemental <a href="/wiki/Isotope" title="Isotope">isotopes</a>, from which an estimate of the age of the star can be derived using <a href="/wiki/Nucleocosmochronology" title="Nucleocosmochronology">nucleocosmochronology</a>.<a href="#cite_note-frebel-276">[268]</a> Another star, <a href="/wiki/HD_140283" title="HD 140283">HD 140283</a>, has been estimated at 14.5 ± 0.7 billion years old.<a href="#cite_note-HD_140283_(arXiv)-40">[37]</a><a href="#cite_note-277">[269]</a>[<a href="/wiki/Category:All_self-contradictory_articles" title="Category:All self-contradictory articles">contradictory</a>] According to observations utilizing <a href="/wiki/Adaptive_optics" title="Adaptive optics">adaptive optics</a> to correct for Earth's atmospheric distortion, stars in the galaxy's bulge date to about 12.8 billion years old.<a href="#cite_note-278">[270]</a> The age of stars in the galactic <a href="/wiki/Thin_disk" title="Thin disk">thin disk</a> has also been estimated using nucleocosmochronology. Measurements of thin disk stars yield an estimate that the thin disk formed 8.8 ± 1.7 billion years ago. These measurements suggest there was a hiatus of almost 5 billion years between the formation of the <a href="/wiki/Galactic_halo" title="Galactic halo">galactic halo</a> and the thin disk.<a href="#cite_note-del_Peloso-279">[271]</a> Recent analysis of the chemical signatures of thousands of stars suggests that stellar formation might have dropped by an order of magnitude at the time of disk formation, 10 to 8 billion years ago, when interstellar gas was too hot to form new stars at the same rate as before.<a href="#cite_note-280">[272]</a> The satellite galaxies surrounding the Milky Way are not randomly distributed but seem to be the result of a breakup of some larger system producing a ring structure 500,000 light-years in diameter and 50,000 light-years wide.<a href="#cite_note-281">[273]</a> Close encounters between galaxies, like that expected in 4 billion years with the Andromeda Galaxy, can rip off huge tails of gas, which, over time can coalesce to form dwarf galaxies in a ring at an arbitrary angle to the main disc.<a href="#cite_note-282">[274]</a> <div class="mw-heading mw-heading2"><h2 id="Intergalactic_neighbourhood">Intergalactic neighbourhood</h2></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1237032888/mw-parser-output/.tmulti"><div class="thumb tmulti tright"><div class="thumbinner multiimageinner" style="width:224px;max-width:224px"><div class="trow"><div class="tsingle" style="width:222px;max-width:222px"><div class="thumbimage"><a href="/wiki/File:06-Local_Group_(LofE06240).png" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/9/90/06-Local_Group_%28LofE06240%29.png/220px-06-Local_Group_%28LofE06240%29.png" decoding="async" width="220" height="161" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/90/06-Local_Group_%28LofE06240%29.png/330px-06-Local_Group_%28LofE06240%29.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/90/06-Local_Group_%28LofE06240%29.png/440px-06-Local_Group_%28LofE06240%29.png 2x" data-file-width="5172" data-file-height="3786" /></a></div><div class="thumbcaption">A diagram of the galaxies in the <a href="/wiki/Local_Group" title="Local Group">Local Group</a> relative to the Milky Way</div></div></div><div class="trow"><div class="tsingle" style="width:222px;max-width:222px"><div class="thumbimage"><a href="/wiki/File:07-Laniakea_(LofE07240).png" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/8/81/07-Laniakea_%28LofE07240%29.png/220px-07-Laniakea_%28LofE07240%29.png" decoding="async" width="220" height="161" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/81/07-Laniakea_%28LofE07240%29.png/330px-07-Laniakea_%28LofE07240%29.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/81/07-Laniakea_%28LofE07240%29.png/440px-07-Laniakea_%28LofE07240%29.png 2x" data-file-width="5172" data-file-height="3786" /></a></div><div class="thumbcaption">The position of the Local Group within the <a href="/wiki/Laniakea_Supercluster" title="Laniakea Supercluster">Laniakea Supercluster</a></div></div></div></div></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Local_Group" title="Local Group">Local Group</a></div> The Milky Way and the <a href="/wiki/Andromeda_Galaxy" title="Andromeda Galaxy">Andromeda Galaxy</a> are a <a href="/wiki/Binary_system_(astronomy)" class="mw-redirect" title="Binary system (astronomy)">binary system</a> of giant spiral galaxies belonging to a group of 50 closely bound galaxies known as the <a href="/wiki/Local_Group" title="Local Group">Local Group</a>, surrounded by a Local Void, itself being part of the <a href="/wiki/Local_Sheet" title="Local Sheet">Local Sheet</a><a href="#cite_note-apj676_1_184-283">[275]</a> and in turn the <a href="/wiki/Virgo_Supercluster" title="Virgo Supercluster">Virgo Supercluster</a>. Surrounding the Virgo Supercluster are a number of voids, devoid of many galaxies, the Microscopium Void to the "north", the Sculptor Void to the "left", the <a href="/wiki/Bo%C3%B6tes_Void" title="Boötes Void">Boötes Void</a> to the "right" and the Canes-Major Void to the "south". These voids change shape over time, creating filamentous structures of galaxies. The Virgo Supercluster, for instance, is being drawn towards the <a href="/wiki/Great_Attractor" title="Great Attractor">Great Attractor</a>,<a href="#cite_note-284">[276]</a> which in turn forms part of a greater structure, called <a href="/wiki/Laniakea_Supercluster" title="Laniakea Supercluster">Laniakea</a>.<a href="#cite_note-285">[277]</a> Two smaller galaxies and a number of <a href="/wiki/Dwarf_galaxy" title="Dwarf galaxy">dwarf galaxies</a> in the Local Group orbit the Milky Way. The largest of these is the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a> with a diameter of 32,200 light-years.<a href="#cite_note-RC3-286">[278]</a> It has a close companion, the <a href="/wiki/Small_Magellanic_Cloud" title="Small Magellanic Cloud">Small Magellanic Cloud</a>. The <a href="/wiki/Magellanic_Stream" title="Magellanic Stream">Magellanic Stream</a> is a stream of neutral <a href="/wiki/Hydrogen" title="Hydrogen">hydrogen</a> gas extending from these two small galaxies across 100° of the sky. The stream is thought to have been dragged from the Magellanic Clouds in tidal interactions with the Milky Way.<a href="#cite_note-287">[279]</a> Some of the <a href="/wiki/Milky_Way%27s_satellite_galaxies" class="mw-redirect" title="Milky Way's satellite galaxies">dwarf galaxies orbiting the Milky Way</a> are <a href="/wiki/Canis_Major_Dwarf" class="mw-redirect" title="Canis Major Dwarf">Canis Major Dwarf</a> (the closest), <a href="/wiki/Sagittarius_Dwarf_Elliptical_Galaxy" class="mw-redirect" title="Sagittarius Dwarf Elliptical Galaxy">Sagittarius Dwarf Elliptical Galaxy</a>, <a href="/wiki/Ursa_Minor_Dwarf" title="Ursa Minor Dwarf">Ursa Minor Dwarf</a>, <a href="/wiki/Sculptor_Dwarf" class="mw-redirect" title="Sculptor Dwarf">Sculptor Dwarf</a>, <a href="/wiki/Sextans_Dwarf" class="mw-redirect" title="Sextans Dwarf">Sextans Dwarf</a>, <a href="/wiki/Fornax_Dwarf" title="Fornax Dwarf">Fornax Dwarf</a>, and <a href="/wiki/Leo_I_Dwarf" class="mw-redirect" title="Leo I Dwarf">Leo I Dwarf</a>.<a href="#cite_note-Koposov2015-288">[280]</a> The smallest dwarf galaxies of the Milky Way are only 500 light-years in diameter. These include <a href="/wiki/Carina_Dwarf" class="mw-redirect" title="Carina Dwarf">Carina Dwarf</a>, <a href="/wiki/Draco_Dwarf" title="Draco Dwarf">Draco Dwarf</a>, and <a href="/wiki/Leo_II_(dwarf_galaxy)" title="Leo II (dwarf galaxy)">Leo II Dwarf</a>. There may still be undetected dwarf galaxies that are dynamically bound to the Milky Way, which is supported by the detection of nine new satellites of the Milky Way in a relatively small patch of the night sky in 2015.<a href="#cite_note-Koposov2015-288">[280]</a> There are some dwarf galaxies that have already been absorbed by the Milky Way, such as the progenitor of <a href="/wiki/Omega_Centauri" title="Omega Centauri">Omega Centauri</a>.<a href="#cite_note-289">[281]</a> In 2005<a href="#cite_note-290">[282]</a> with further confirmation in 2012<a href="#cite_note-291">[283]</a> researchers reported that most satellite galaxies of the Milky Way lie in a very large disk and orbit in the same direction. This came as a surprise: according to standard cosmology, the satellite galaxies should form in dark matter halos, and they should be widely distributed and moving in random directions. This discrepancy is still not explained.<a href="#cite_note-292">[284]</a> In January 2006, researchers reported that the heretofore unexplained warp in the disk of the Milky Way has now been mapped and found to be a ripple or vibration set up by the Large and Small Magellanic Clouds as they orbit the Milky Way, causing vibrations when they pass through its edges. Previously, these two galaxies, at around 2% of the mass of the Milky Way, were considered too small to influence the Milky Way. However, in a computer model, the movement of these two galaxies creates a dark matter wake that amplifies their influence on the larger Milky Way.<a href="#cite_note-berkeley20060109-293">[285]</a> Current measurements suggest the Andromeda Galaxy is approaching the Milky Way at 100 to 140 km/s (220,000 to 310,000 mph). In 4.3 billion years, there may be an <a href="/wiki/Andromeda%E2%80%93Milky_Way_collision" title="Andromeda–Milky Way collision">Andromeda–Milky Way collision</a>, depending on the importance of unknown lateral components to the galaxies' relative motion. If they collide, the chance of individual <a href="/wiki/Stellar_collision" title="Stellar collision">stars colliding</a> with each other is extremely low,<a href="#cite_note-wong20000414-294">[286]</a> but instead the two galaxies will merge to form a single <a href="/wiki/Elliptical_galaxy" title="Elliptical galaxy">elliptical galaxy</a> or perhaps a large <a href="/wiki/Disk_galaxy" class="mw-redirect" title="Disk galaxy">disk galaxy</a><a href="#cite_note-Ueda2014-295">[287]</a> over the course of about six billion years.<a href="#cite_note-Schiavi-296">[288]</a> <div class="mw-heading mw-heading2"><h2 id="Velocity">Velocity</h2></div> Although <a href="/wiki/Special_relativity" title="Special relativity">special relativity</a> states that there is no "preferred" <a href="/wiki/Inertial_frame_of_reference" title="Inertial frame of reference">inertial frame of reference</a> in space with which to compare the Milky Way, the Milky Way does have a velocity with respect to cosmological <a href="/wiki/Frames_of_reference" class="mw-redirect" title="Frames of reference">frames of reference</a>. One such frame of reference is the <a href="/wiki/Hubble_flow" class="mw-redirect" title="Hubble flow">Hubble flow</a>, the apparent motions of galaxy clusters due to the <a href="/wiki/Expansion_of_space" class="mw-redirect" title="Expansion of space">expansion of space</a>. Individual galaxies, including the Milky Way, have <a href="/wiki/Peculiar_velocities" class="mw-redirect" title="Peculiar velocities">peculiar velocities</a> relative to the average flow. Thus, to compare the Milky Way to the Hubble flow, one must consider a volume large enough so that the expansion of the Universe dominates over local, random motions. A large enough volume means that the mean motion of galaxies within this volume is equal to the Hubble flow. Astronomers believe the Milky Way is moving at approximately 630 km/s (1,400,000 mph) with respect to this local co-moving frame of reference.<a href="#cite_note-297">[289]</a><a href="#cite_note-298">[290]</a> The Milky Way is moving in the general direction of the <a href="/wiki/Great_Attractor" title="Great Attractor">Great Attractor</a> and other <a href="/wiki/Galaxy_cluster" title="Galaxy cluster">galaxy clusters</a>, including the <a href="/wiki/Shapley_Supercluster" title="Shapley Supercluster">Shapley Supercluster</a>, behind it.<a href="#cite_note-299">[291]</a> The Local Group, a cluster of gravitationally bound galaxies containing, among others, the Milky Way and the Andromeda Galaxy, is part of a <a href="/wiki/Supercluster" title="Supercluster">supercluster</a> called the <a href="/wiki/Local_Supercluster" class="mw-redirect" title="Local Supercluster">Local Supercluster</a>, centered near the <a href="/wiki/Virgo_Cluster" title="Virgo Cluster">Virgo Cluster</a>: although they are moving away from each other at 967 km/s (2,160,000 mph) as part of the Hubble flow, this velocity is less than would be expected given the 16.8 million pc distance due to the gravitational attraction between the Local Group and the Virgo Cluster.<a href="#cite_note-300">[292]</a> Another reference frame is provided by the <a href="/wiki/Cosmic_microwave_background" title="Cosmic microwave background">cosmic microwave background</a> (CMB), in which the CMB temperature is least distorted by Doppler shift (zero dipole moment). The Milky Way is moving at 552 ± 6 km/s (1,235,000 ± 13,000 mph)<a href="#cite_note-COBE1993-21">[19]</a> with respect to this frame, toward 10.5 right ascension, −24° declination (<a href="/wiki/J2000" class="mw-redirect" title="J2000">J2000</a> epoch, near the center of <a href="/wiki/Hydra_(constellation)" title="Hydra (constellation)">Hydra</a>). This motion is observed by satellites such as the <a href="/wiki/Cosmic_Background_Explorer" title="Cosmic Background Explorer">Cosmic Background Explorer</a> (COBE) and the <a href="/wiki/Wilkinson_Microwave_Anisotropy_Probe" title="Wilkinson Microwave Anisotropy Probe">Wilkinson Microwave Anisotropy Probe</a> (WMAP) as a dipole contribution to the CMB, as photons in equilibrium in the CMB frame get <a href="/wiki/Doppler_effect" title="Doppler effect">blue-shifted</a> in the direction of the motion and <a href="/wiki/Redshift" title="Redshift">red-shifted</a> in the opposite direction.<a href="#cite_note-COBE1993-21">[19]</a> <div class="mw-heading mw-heading2"><h2 id="See_also">See also</h2></div> <style data-mw-deduplicate="TemplateStyles:r1239009302">.mw-parser-output .portalbox{padding:0;margin:0.5em 0;display:table;box-sizing:border-box;max-width:175px;list-style:none}.mw-parser-output .portalborder{border:1px solid var(--border-color-base,#a2a9b1);padding:0.1em;background:var(--background-color-neutral-subtle,#f8f9fa)}.mw-parser-output .portalbox-entry{display:table-row;font-size:85%;line-height:110%;height:1.9em;font-style:italic;font-weight:bold}.mw-parser-output .portalbox-image{display:table-cell;padding:0.2em;vertical-align:middle;text-align:center}.mw-parser-output .portalbox-link{display:table-cell;padding:0.2em 0.2em 0.2em 0.3em;vertical-align:middle}@media(min-width:720px){.mw-parser-output .portalleft{clear:left;float:left;margin:0.5em 1em 0.5em 0}.mw-parser-output .portalright{clear:right;float:right;margin:0.5em 0 0.5em 1em}}</style><ul role="navigation" aria-label="Portals" class="noprint portalbox portalborder portalright"> <li class="portalbox-entry"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Solar_system.jpg/22px-Solar_system.jpg" decoding="async" width="22" height="28" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Solar_system.jpg/34px-Solar_system.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/83/Solar_system.jpg/45px-Solar_system.jpg 2x" data-file-width="4500" data-file-height="5600" /><a href="/wiki/Portal:Solar_system" class="mw-redirect" title="Portal:Solar system">solar system portal</a></li><li class="portalbox-entry"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5c/Earth-moon.jpg/32px-Earth-moon.jpg" decoding="async" width="32" height="26" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5c/Earth-moon.jpg/48px-Earth-moon.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5c/Earth-moon.jpg/64px-Earth-moon.jpg 2x" data-file-width="3000" data-file-height="2400" /><a href="/wiki/Portal:Outer_space" title="Portal:Outer space">outer space portal</a></li><li class="portalbox-entry"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/28px-Crab_Nebula.jpg" decoding="async" width="28" height="28" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/42px-Crab_Nebula.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/56px-Crab_Nebula.jpg 2x" data-file-width="3864" data-file-height="3864" /><a href="/wiki/Portal:Astronomy" title="Portal:Astronomy">astronomy portal</a></li></ul> <ul><li><a href="/wiki/Baade%27s_Window" title="Baade's Window">Baade's Window</a></li> <li><a href="/wiki/Galactic_astronomy" title="Galactic astronomy">Galactic astronomy</a></li> <li><a href="/wiki/Galactic_Center_GeV_excess" title="Galactic Center GeV excess">Galactic Center GeV excess</a></li> <li><a href="/wiki/Oort_constants" title="Oort constants">Oort constants</a></li></ul> <div class="mw-heading mw-heading2"><h2 id="Notes">Notes</h2></div> <style data-mw-deduplicate="TemplateStyles:r1239543626">.mw-parser-output .reflist{margin-bottom:0.5em;list-style-type:decimal}@media screen{.mw-parser-output .reflist{font-size:90%}}.mw-parser-output .reflist .references{font-size:100%;margin-bottom:0;list-style-type:inherit}.mw-parser-output .reflist-columns-2{column-width:30em}.mw-parser-output .reflist-columns-3{column-width:25em}.mw-parser-output .reflist-columns{margin-top:0.3em}.mw-parser-output .reflist-columns ol{margin-top:0}.mw-parser-output .reflist-columns li{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .reflist-upper-alpha{list-style-type:upper-alpha}.mw-parser-output .reflist-upper-roman{list-style-type:upper-roman}.mw-parser-output .reflist-lower-alpha{list-style-type:lower-alpha}.mw-parser-output .reflist-lower-greek{list-style-type:lower-greek}.mw-parser-output .reflist-lower-roman{list-style-type:lower-roman}</style><div class="reflist reflist-lower-alpha"> <div class="mw-references-wrap"><ol class="references"> <li id="cite_note-distance-5"><a href="#cite_ref-distance_5-0">^</a> The distance towards its <a href="/wiki/Galactic_Center" title="Galactic Center">center</a> (<a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a>). </li> <li id="cite_note-Disk-13"><a href="#cite_ref-Disk_13-0">^</a> This is the diameter measured using the D25 standard. It has been recently suggested that there is a presence of disk stars beyond this diameter, although it is not clear how much of this influences the surface brightness profile.<a href="#cite_note-Lopez2018-12">[11]</a> </li> <li id="cite_note-context-28"><a href="#cite_ref-context_28-0">^</a> Some authors use the term Milky Way to refer exclusively to the band of light that the galaxy forms in the night sky, while the galaxy receives the full name Milky Way Galaxy. See for example Laustsen et al.,<a href="#cite_note-23">[21]</a> Pasachoff,<a href="#cite_note-24">[22]</a> Jones,<a href="#cite_note-25">[23]</a> van der Kruit,<a href="#cite_note-26">[24]</a> and Hodge et al.<a href="#cite_note-27">[25]</a> </li> <li id="cite_note-bortle-73"><a href="#cite_ref-bortle_73-0">^</a> See also <a href="/wiki/Bortle_Dark-Sky_Scale" class="mw-redirect" title="Bortle Dark-Sky Scale">Bortle Dark-Sky Scale</a>. </li> <li id="cite_note-const-75"><a href="#cite_ref-const_75-0">^</a> The bright center of the galaxy is located in the constellation <a href="/wiki/Sagittarius_(constellation)" title="Sagittarius (constellation)">Sagittarius</a>. From Sagittarius, the hazy band of white light appears to pass westward through the constellations of <a href="/wiki/Scorpius" title="Scorpius">Scorpius</a>, <a href="/wiki/Ara_(constellation)" title="Ara (constellation)">Ara</a>, <a href="/wiki/Norma_(constellation)" title="Norma (constellation)">Norma</a>, <a href="/wiki/Triangulum_Australe" title="Triangulum Australe">Triangulum Australe</a>, <a href="/wiki/Circinus" title="Circinus">Circinus</a>, <a href="/wiki/Centaurus" title="Centaurus">Centaurus</a>, <a href="/wiki/Musca" title="Musca">Musca</a>, <a href="/wiki/Crux" title="Crux">Crux</a>, <a href="/wiki/Carina_(constellation)" title="Carina (constellation)">Carina</a>, <a href="/wiki/Vela_(constellation)" title="Vela (constellation)">Vela</a>, <a href="/wiki/Puppis" title="Puppis">Puppis</a>, <a href="/wiki/Canis_Major" title="Canis Major">Canis Major</a>, <a href="/wiki/Monoceros" title="Monoceros">Monoceros</a>, <a href="/wiki/Orion_(constellation)" title="Orion (constellation)">Orion</a> and <a href="/wiki/Gemini_(constellation)" title="Gemini (constellation)">Gemini</a>, <a href="/wiki/Taurus_(constellation)" title="Taurus (constellation)">Taurus</a>, to the <a href="/wiki/Galactic_anticenter" title="Galactic anticenter">galactic anticenter</a> in <a href="/wiki/Auriga_(constellation)" class="mw-redirect" title="Auriga (constellation)">Auriga</a>. From there, it passes through <a href="/wiki/Perseus_(constellation)" title="Perseus (constellation)">Perseus</a>, <a href="/wiki/Andromeda_(constellation)" title="Andromeda (constellation)">Andromeda</a>, <a href="/wiki/Cassiopeia_(constellation)" title="Cassiopeia (constellation)">Cassiopeia</a>, <a href="/wiki/Cepheus_(constellation)" title="Cepheus (constellation)">Cepheus</a> and <a href="/wiki/Lacerta" title="Lacerta">Lacerta</a>, <a href="/wiki/Cygnus_(constellation)" title="Cygnus (constellation)">Cygnus</a>, <a href="/wiki/Vulpecula" title="Vulpecula">Vulpecula</a>, <a href="/wiki/Sagitta" title="Sagitta">Sagitta</a>, <a href="/wiki/Aquila_(constellation)" title="Aquila (constellation)">Aquila</a>, <a href="/wiki/Ophiuchus" title="Ophiuchus">Ophiuchus</a>, <a href="/wiki/Scutum_(constellation)" title="Scutum (constellation)">Scutum</a>, and back to <a href="/wiki/Sagittarius_(constellation)" title="Sagittarius (constellation)">Sagittarius</a>. </li> <li id="cite_note-number-159"><a href="#cite_ref-number_159-0">^</a> These estimates are very uncertain, as most non-star objects are difficult to detect; for example, black hole estimates range from ten million to one billion.<a href="#cite_note-157">[152]</a><a href="#cite_note-158">[153]</a> </li> <li id="cite_note-milky_way_mag-168"><a href="#cite_ref-milky_way_mag_168-0">^</a> Karachentsev et al. give a blue absolute magnitude of −20.8. Combined with a <a href="/wiki/Color_index" title="Color index">color index</a> of 0.55 estimated <a rel="nofollow" class="external text" href="http://adsabs.harvard.edu/abs/2014MNRAS.440..405M">here</a>, an absolute visual magnitude of −21.35 (−20.8 − 0.55 = −21.35) is obtained. Determining the absolute magnitude of the Milky Way is very difficult, because Earth is inside it. </li> <li id="cite_note-chandra2003-196"><a href="#cite_ref-chandra2003_196-0">^</a> For a photo see: <style data-mw-deduplicate="TemplateStyles:r1238218222">.mw-parser-output cite.citation{font-style:inherit;word-wrap:break-word}.mw-parser-output .citation q{quotes:"\"""\"""'""'"}.mw-parser-output .citation:target{background-color:rgba(0,127,255,0.133)}.mw-parser-output .id-lock-free.id-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/6/65/Lock-green.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-limited.id-lock-limited a,.mw-parser-output .id-lock-registration.id-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/d/d6/Lock-gray-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-subscription.id-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/a/aa/Lock-red-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .cs1-ws-icon a{background:url("//upload.wikimedia.org/wikipedia/commons/4/4c/Wikisource-logo.svg")right 0.1em center/12px no-repeat}body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-free a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-limited a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-registration a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-subscription a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .cs1-ws-icon a{background-size:contain;padding:0 1em 0 0}.mw-parser-output .cs1-code{color:inherit;background:inherit;border:none;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;color:var(--color-error,#d33)}.mw-parser-output .cs1-visible-error{color:var(--color-error,#d33)}.mw-parser-output .cs1-maint{display:none;color:#085;margin-left:0.3em}.mw-parser-output .cs1-kern-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right{padding-right:0.2em}.mw-parser-output .citation .mw-selflink{font-weight:inherit}@media screen{.mw-parser-output .cs1-format{font-size:95%}html.skin-theme-clientpref-night .mw-parser-output .cs1-maint{color:#18911f}}@media screen and (prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .cs1-maint{color:#18911f}}</style><cite class="citation web cs1"><a rel="nofollow" class="external text" href="http://chandra.harvard.edu/photo/2003/0203long/">"Sagittarius A*: Milky Way monster stars in cosmic reality show"</a>. Chandra X-ray Observatory. Center for Astrophysics | Harvard & Smithsonian. January 6, 2003. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20080317061809/http://chandra.harvard.edu/photo/2003/0203long/">Archived</a> from the original on March 17, 2008. Retrieved May 20, 2012.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Chandra+X-ray+Observatory&rft.atitle=Sagittarius+A%2A%3A+Milky+Way+monster+stars+in+cosmic+reality+show&rft.date=2003-01-06&rft_id=http%3A%2F%2Fchandra.harvard.edu%2Fphoto%2F2003%2F0203long%2F&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> </ol></div></div> <div class="mw-heading mw-heading2"><h2 id="References">References</h2></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239543626"><div class="reflist"> <div class="mw-references-wrap mw-references-columns"><ol class="references"> <li id="cite_note-Petrov-1">^ <a href="#cite_ref-Petrov_1-0">a</a> <a href="#cite_ref-Petrov_1-1">b</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFPetrovKovalevFomalontGordon2011" class="citation journal cs1">Petrov, L.; Kovalev, Y. Y.; Fomalont, E. 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Retrieved May 5, 2022.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=snowdonia-npa.gov.uk&rft.atitle=Eryri+%E2%80%93+Snowdonia&rft_id=https%3A%2F%2Fwww.snowdonia-npa.gov.uk%2Flooking-after%2Fdark-skies%2Fglossary&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-53"><a href="#cite_ref-53">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHarris2011" class="citation book cs1">Harris, Mike (2011). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=7dU2kfUVUaQC&dq=Caer+Arianrhod++Corona+Borealis&pg=PA145">Awen: The Quest of the Celtic Mysteries</a>. Skylight Press. p. 144. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-1-908011-36-7" title="Special:BookSources/978-1-908011-36-7"><bdi>978-1-908011-36-7</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230326142938/https://books.google.com/books?id=7dU2kfUVUaQC&dq=Caer+Arianrhod++Corona+Borealis&pg=PA145">Archived</a> from the original on March 26, 2023. Retrieved May 13, 2022. <q>The stars of the Corona Borealis, the Caer Arianrhod, as it is called in Welsh, whose shape is remembered in certain Bronze Age circles</q></cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Awen%3A+The+Quest+of+the+Celtic+Mysteries&rft.pages=144&rft.pub=Skylight+Press&rft.date=2011&rft.isbn=978-1-908011-36-7&rft.aulast=Harris&rft.aufirst=Mike&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3D7dU2kfUVUaQC%26dq%3DCaer%2BArianrhod%2B%2BCorona%2BBorealis%26pg%3DPA145&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-eo_galaxy-54"><a href="#cite_ref-eo_galaxy_54-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHarper" class="citation web cs1">Harper, Douglas. <a rel="nofollow" class="external text" href="http://www.etymonline.com/index.php?term=galaxy">"galaxy"</a>. <a href="/wiki/Online_Etymology_Dictionary" title="Online Etymology Dictionary">Online Etymology Dictionary</a>. <a rel="nofollow" class="external text" href="https://archive.today/20120527/http://www.etymonline.com/index.php?term=galaxy">Archived</a> from the original on May 27, 2012. Retrieved May 20, 2012.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Online+Etymology+Dictionary&rft.atitle=galaxy&rft.aulast=Harper&rft.aufirst=Douglas&rft_id=http%3A%2F%2Fwww.etymonline.com%2Findex.php%3Fterm%3Dgalaxy&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-jankowski2010-55"><a href="#cite_ref-jankowski2010_55-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFJankowski2010" class="citation book cs1">Jankowski, Connie (2010). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=Wp6E3y-58LkC&pg=PT6">Pioneers of Light and Sound</a>. Compass Point Books. p. 6. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-7565-4306-8" title="Special:BookSources/978-0-7565-4306-8"><bdi>978-0-7565-4306-8</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120142012/https://books.google.com/books?id=Wp6E3y-58LkC&pg=PT6">Archived</a> from the original on November 20, 2016.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Pioneers+of+Light+and+Sound&rft.pages=6&rft.pub=Compass+Point+Books&rft.date=2010&rft.isbn=978-0-7565-4306-8&rft.aulast=Jankowski&rft.aufirst=Connie&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DWp6E3y-58LkC%26pg%3DPT6&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-oxford-56"><a href="#cite_ref-oxford_56-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSimpsonWeiner1989" class="citation book cs1">Simpson, John; Weiner, Edmund, eds. (March 30, 1989). The Oxford English Dictionary (2nd ed.). Oxford University Press. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-19-861186-8" title="Special:BookSources/978-0-19-861186-8"><bdi>978-0-19-861186-8</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=The+Oxford+English+Dictionary&rft.edition=2nd&rft.pub=Oxford+University+Press&rft.date=1989-03-30&rft.isbn=978-0-19-861186-8&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> See the entries for "Milky Way" and "galaxy". </li> <li id="cite_note-eratosthenes1997-57"><a href="#cite_ref-eratosthenes1997_57-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFEratosthenes1997" class="citation book cs1">Eratosthenes (1997). Condos, Theony (ed.). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=4Sp8CaA5HI0C&pg=PA110">Star Myths of the Greeks and Romans: A Sourcebook Containing the Constellations of Pseudo-Eratosthenes and the Poetic Astronomy of Hyginus</a>. Red Wheel/Weiser. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-1-890482-93-0" title="Special:BookSources/978-1-890482-93-0"><bdi>978-1-890482-93-0</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120164810/https://books.google.com/books?id=4Sp8CaA5HI0C&pg=PA110">Archived</a> from the original on November 20, 2016.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Star+Myths+of+the+Greeks+and+Romans%3A+A+Sourcebook+Containing+the+Constellations+of+Pseudo-Eratosthenes+and+the+Poetic+Astronomy+of+Hyginus&rft.pub=Red+Wheel%2FWeiser&rft.date=1997&rft.isbn=978-1-890482-93-0&rft.au=Eratosthenes&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3D4Sp8CaA5HI0C%26pg%3DPA110&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-58"><a href="#cite_ref-58">^</a> ^ Sauer, EGF (July 1971). "Celestial Rotation and Stellar Orientation in Migratory Warblers". Science 30: 459–461. </li> <li id="cite_note-59"><a href="#cite_ref-59">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="https://web.archive.org/web/20190712144216/https://www.adelaide.edu.au/kwp/placenames/council/areas/map_kwp.html">"Reconciliation"</a>. Adelaide City Council. Archived from <a rel="nofollow" class="external text" href="https://www.adelaide.edu.au/kwp/placenames/council/areas/map_kwp.html">the original</a> on July 12, 2019. Retrieved February 26, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Adelaide+City+Council&rft.atitle=Reconciliation&rft_id=https%3A%2F%2Fwww.adelaide.edu.au%2Fkwp%2Fplacenames%2Fcouncil%2Fareas%2Fmap_kwp.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-60"><a href="#cite_ref-60">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMandow2021" class="citation web cs1">Mandow, Rami (May 3, 2021). <a rel="nofollow" class="external text" href="https://spaceaustralia.com/news/moonhack-coding-story-emu-sky">"Moonhack – Coding the Story of the Emu in the Sky"</a>. Space Australia. Retrieved June 5, 2022.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Space+Australia&rft.atitle=Moonhack+%E2%80%93+Coding+the+Story+of+the+Emu+in+the+Sky&rft.date=2021-05-03&rft.aulast=Mandow&rft.aufirst=Rami&rft_id=https%3A%2F%2Fspaceaustralia.com%2Fnews%2Fmoonhack-coding-story-emu-sky&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-Fiona-61"><a href="#cite_ref-Fiona_61-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMacleod1911" class="citation book cs1"><a href="/wiki/William_Sharp_(writer)" title="William Sharp (writer)">Macleod, Fiona</a> (1911). <a rel="nofollow" class="external text" href="https://web.archive.org/web/20070217215638/http://www.sundown.pair.com/SundownShores/Volume_VI/ForestMurmers/milky%20way.htm">Where the forest murmurs</a>. New York: Duffield & Company. Chapter 21: Milky Way. Archived from <a rel="nofollow" class="external text" href="http://www.sundown.pair.com/SundownShores/Volume_VI/ForestMurmers/milky%20way.htm">the original</a> on February 17, 2007.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Where+the+forest+murmurs&rft.place=New+York&rft.pages=Chapter+21%3A+%27%27Milky+Way%27%27&rft.pub=Duffield+%26+Company&rft.date=1911&rft.aulast=Macleod&rft.aufirst=Fiona&rft_id=http%3A%2F%2Fwww.sundown.pair.com%2FSundownShores%2FVolume_VI%2FForestMurmers%2Fmilky%2520way.htm&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-62"><a href="#cite_ref-62">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="https://web.archive.org/web/20061217160109/http://dspace.dial.pipex.com/telegraph/04camino/04000001.htm">"The Pilgrim's Way: El Camino de Santiago"</a>. Archived from <a rel="nofollow" class="external text" href="http://dspace.dial.pipex.com/telegraph/04camino/04000001.htm">the original</a> on December 17, 2006. Retrieved January 6, 2007.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=The+Pilgrim%27s+Way%3A+El+Camino+de+Santiago&rft_id=http%3A%2F%2Fdspace.dial.pipex.com%2Ftelegraph%2F04camino%2F04000001.htm&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-63"><a href="#cite_ref-63">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHarutyunyan2003" class="citation journal cs1">Harutyunyan, Hayk (August 29, 2003). <a rel="nofollow" class="external text" href="https://web.archive.org/web/20060429194053/http://www.aras.am/ARASNEWS/arasnews06.html">"The Armenian name of the Milky Way"</a>. ArAS News. 6. Armenian Astronomical Society (ArAS). Archived from <a rel="nofollow" class="external text" href="http://www.aras.am/ArasNews/arasnews06.html">the original</a> on April 29, 2006. Retrieved August 10, 2009.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=ArAS+News&rft.atitle=The+Armenian+name+of+the+Milky+Way&rft.volume=6&rft.date=2003-08-29&rft.aulast=Harutyunyan&rft.aufirst=Hayk&rft_id=http%3A%2F%2Fwww.aras.am%2FArasNews%2Farasnews06.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-64"><a href="#cite_ref-64">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFBogle2011" class="citation web cs1">Bogle, Joanna (September 16, 2011). <a rel="nofollow" class="external text" href="http://www.ncregister.com/site/article/a-pilgrimage-to-walsingham-englands-nazareth">"A Pilgrimage to Walsingham, 'England's Nazareth'"</a>. National Catholic Register. EWTN. Retrieved November 13, 2013.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=National+Catholic+Register&rft.atitle=A+Pilgrimage+to+Walsingham%2C+%27England%27s+Nazareth%27&rft.date=2011-09-16&rft.aulast=Bogle&rft.aufirst=Joanna&rft_id=http%3A%2F%2Fwww.ncregister.com%2Fsite%2Farticle%2Fa-pilgrimage-to-walsingham-englands-nazareth&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-pasachoff1994-65"><a href="#cite_ref-pasachoff1994_65-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFPasachoff1994" class="citation book cs1"><a href="/wiki/Jay_Pasachoff" title="Jay Pasachoff">Pasachoff, Jay M.</a> (1994). Astronomy: From the Earth to the Universe. Harcourt School. p. 500. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-03-001667-7" title="Special:BookSources/978-0-03-001667-7"><bdi>978-0-03-001667-7</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Astronomy%3A+From+the+Earth+to+the+Universe&rft.pages=500&rft.pub=Harcourt+School&rft.date=1994&rft.isbn=978-0-03-001667-7&rft.aulast=Pasachoff&rft.aufirst=Jay+M.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-66"><a href="#cite_ref-66">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFRey1976" class="citation book cs1">Rey, H. A. (1976). <a rel="nofollow" class="external text" href="https://archive.org/details/stars00hare/page/145">The Stars</a>. Houghton Mifflin Harcourt. p. <a rel="nofollow" class="external text" href="https://archive.org/details/stars00hare/page/145">145</a>. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-395-24830-0" title="Special:BookSources/978-0-395-24830-0"><bdi>978-0-395-24830-0</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=The+Stars&rft.pages=145&rft.pub=Houghton+Mifflin+Harcourt&rft.date=1976&rft.isbn=978-0-395-24830-0&rft.aulast=Rey&rft.aufirst=H.+A.&rft_id=https%3A%2F%2Farchive.org%2Fdetails%2Fstars00hare%2Fpage%2F145&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-67"><a href="#cite_ref-67">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFPasachoffFilippenko2013" class="citation book cs1">Pasachoff, Jay M.; Filippenko, Alex (2013). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=tZsoAAAAQBAJ&pg=PA384">The Cosmos: Astronomy in the New Millennium</a>. Cambridge University Press. p. 384. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-1-107-68756-1" title="Special:BookSources/978-1-107-68756-1"><bdi>978-1-107-68756-1</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230326142950/https://books.google.com/books?id=tZsoAAAAQBAJ&pg=PA384">Archived</a> from the original on March 26, 2023. Retrieved December 18, 2016.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=The+Cosmos%3A+Astronomy+in+the+New+Millennium&rft.pages=384&rft.pub=Cambridge+University+Press&rft.date=2013&rft.isbn=978-1-107-68756-1&rft.aulast=Pasachoff&rft.aufirst=Jay+M.&rft.au=Filippenko%2C+Alex&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DtZsoAAAAQBAJ%26pg%3DPA384&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-68"><a href="#cite_ref-68">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFCrossen2013" class="citation journal cs1">Crossen, Craig (July 2013). "Observing the Milky Way, part I: Sagittarius & Scorpius". Sky & Telescope. 126 (1): 24. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2013S&T...126a..24C">2013S&T...126a..24C</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Sky+%26+Telescope&rft.atitle=Observing+the+Milky+Way%2C+part+I%3A+Sagittarius+%26+Scorpius&rft.volume=126&rft.issue=1&rft.pages=24&rft.date=2013-07&rft_id=info%3Abibcode%2F2013S%26T...126a..24C&rft.aulast=Crossen&rft.aufirst=Craig&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-69"><a href="#cite_ref-69">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFUrton1981" class="citation book cs1"><a href="/wiki/Gary_Urton" title="Gary Urton">Urton, Gary</a> (1981). At the Crossroads of the Earth and the Sky: An Andean Cosmology. Latin American Monographs. Vol. 55. Austin: Univ. of Texas Pr. pp. 102–4, 109–11. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/0-292-70349-X" title="Special:BookSources/0-292-70349-X"><bdi>0-292-70349-X</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=At+the+Crossroads+of+the+Earth+and+the+Sky%3A+An+Andean+Cosmology&rft.place=Austin&rft.series=Latin+American+Monographs&rft.pages=102-4%2C+109-11&rft.pub=Univ.+of+Texas+Pr.&rft.date=1981&rft.isbn=0-292-70349-X&rft.aulast=Urton&rft.aufirst=Gary&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-70"><a href="#cite_ref-70">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFStarr2020" class="citation web cs1">Starr, Michelle (July 14, 2020). <a rel="nofollow" class="external text" href="https://www.sciencealert.com/a-giant-wall-of-galaxies-has-been-found-stretching-across-the-universe">"A Giant 'Wall' of Galaxies Has Been Found Stretching Across The Universe"</a>. ScienceAlert. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210205141100/https://www.sciencealert.com/a-giant-wall-of-galaxies-has-been-found-stretching-across-the-universe">Archived</a> from the original on February 5, 2021. Retrieved May 5, 2022.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=ScienceAlert&rft.atitle=A+Giant+%27Wall%27+of+Galaxies+Has+Been+Found+Stretching+Across+The+Universe&rft.date=2020-07-14&rft.aulast=Starr&rft.aufirst=Michelle&rft_id=https%3A%2F%2Fwww.sciencealert.com%2Fa-giant-wall-of-galaxies-has-been-found-stretching-across-the-universe&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-71"><a href="#cite_ref-71">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFCrumey2014" class="citation journal cs1">Crumey, Andrew (2014). <a rel="nofollow" class="external text" href="https://doi.org/10.1093%2Fmnras%2Fstu992">"Human contrast threshold and astronomical visibility"</a>. Monthly Notices of the Royal Astronomical Society. 442 (3): 2600–2619. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/1405.4209">1405.4209</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2014MNRAS.442.2600C">2014MNRAS.442.2600C</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1093%2Fmnras%2Fstu992">10.1093/mnras/stu992</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:119210885">119210885</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Monthly+Notices+of+the+Royal+Astronomical+Society&rft.atitle=Human+contrast+threshold+and+astronomical+visibility&rft.volume=442&rft.issue=3&rft.pages=2600-2619&rft.date=2014&rft_id=info%3Aarxiv%2F1405.4209&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A119210885%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1093%2Fmnras%2Fstu992&rft_id=info%3Abibcode%2F2014MNRAS.442.2600C&rft.aulast=Crumey&rft.aufirst=Andrew&rft_id=https%3A%2F%2Fdoi.org%2F10.1093%252Fmnras%252Fstu992&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-steinicke_sakiel2007-72"><a href="#cite_ref-steinicke_sakiel2007_72-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSteinickeJakiel2007" class="citation book cs1">Steinicke, Wolfgang; Jakiel, Richard (2007). <a rel="nofollow" class="external text" href="https://archive.org/details/galaxieshowtoobs0000stei">Galaxies and how to observe them</a>. Astronomers' observing guides. Springer. p. <a rel="nofollow" class="external text" href="https://archive.org/details/galaxieshowtoobs0000stei/page/94">94</a>. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-1-85233-752-0" title="Special:BookSources/978-1-85233-752-0"><bdi>978-1-85233-752-0</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Galaxies+and+how+to+observe+them&rft.series=Astronomers%27+observing+guides&rft.pages=94&rft.pub=Springer&rft.date=2007&rft.isbn=978-1-85233-752-0&rft.aulast=Steinicke&rft.aufirst=Wolfgang&rft.au=Jakiel%2C+Richard&rft_id=https%3A%2F%2Farchive.org%2Fdetails%2Fgalaxieshowtoobs0000stei&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-74"><a href="#cite_ref-74">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFFalchiCinzanoDuriscoeKyba2016" class="citation journal cs1">Falchi, Fabio; Cinzano, Pierantonio; Duriscoe, Dan; Kyba, Christopher C. M.; Elvidge, Christopher D.; Baugh, Kimberly; Portnov, Boris A.; Rybnikova, Nataliya A.; Furgoni, Riccardo (June 1, 2016). <a rel="nofollow" class="external text" href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC4928945">"The new world atlas of artificial night sky brightness"</a>. Science Advances. 2 (6): e1600377. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/1609.01041">1609.01041</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2016SciA....2E0377F">2016SciA....2E0377F</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1126%2Fsciadv.1600377">10.1126/sciadv.1600377</a>. <a href="/wiki/ISSN_(identifier)" class="mw-redirect" title="ISSN (identifier)">ISSN</a> <a rel="nofollow" class="external text" href="https://search.worldcat.org/issn/2375-2548">2375-2548</a>. <a href="/wiki/PMC_(identifier)" class="mw-redirect" title="PMC (identifier)">PMC</a> <a rel="nofollow" class="external text" href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC4928945">4928945</a>. <a href="/wiki/PMID_(identifier)" class="mw-redirect" title="PMID (identifier)">PMID</a> <a rel="nofollow" class="external text" href="https://pubmed.ncbi.nlm.nih.gov/27386582">27386582</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Science+Advances&rft.atitle=The+new+world+atlas+of+artificial+night+sky+brightness&rft.volume=2&rft.issue=6&rft.pages=e1600377&rft.date=2016-06-01&rft_id=https%3A%2F%2Fwww.ncbi.nlm.nih.gov%2Fpmc%2Farticles%2FPMC4928945%23id-name%3DPMC&rft_id=info%3Abibcode%2F2016SciA....2E0377F&rft_id=info%3Aarxiv%2F1609.01041&rft.issn=2375-2548&rft_id=info%3Adoi%2F10.1126%2Fsciadv.1600377&rft_id=info%3Apmid%2F27386582&rft.aulast=Falchi&rft.aufirst=Fabio&rft.au=Cinzano%2C+Pierantonio&rft.au=Duriscoe%2C+Dan&rft.au=Kyba%2C+Christopher+C.+M.&rft.au=Elvidge%2C+Christopher+D.&rft.au=Baugh%2C+Kimberly&rft.au=Portnov%2C+Boris+A.&rft.au=Rybnikova%2C+Nataliya+A.&rft.au=Furgoni%2C+Riccardo&rft_id=https%3A%2F%2Fwww.ncbi.nlm.nih.gov%2Fpmc%2Farticles%2FPMC4928945&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-76"><a href="#cite_ref-76">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMiller2015" class="citation web cs1">Miller, James (November 14, 2015). <a rel="nofollow" class="external text" href="https://www.astronomytrek.com/which-constellation-can-be-seen-along-the-milky-way/">"Which Constellations Can Be Seen Along The Milky Way?"</a>. Retrieved August 13, 2024.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Which+Constellations+Can+Be+Seen+Along+The+Milky+Way%3F&rft.date=2015-11-14&rft.aulast=Miller&rft.aufirst=James&rft_id=https%3A%2F%2Fwww.astronomytrek.com%2Fwhich-constellation-can-be-seen-along-the-milky-way%2F&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-77"><a href="#cite_ref-77">^</a> Aristotle with W. D. Ross, ed., The Works of Aristotle ... (Oxford, England: Clarendon Press, 1931), vol. III, Meteorologica, E. W. Webster, trans., Book 1, Part 8, <a rel="nofollow" class="external text" href="https://archive.org/stream/workstranslatedi03arisuoft#page/n37/mode/2up/">pp. 39–40</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20160411091135/https://archive.org/stream/workstranslatedi03arisuoft">Archived</a> April 11, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>: "(2) Anaxagoras, Democritus, and their schools say that the milky way is the light of certain stars ... shaded by the earth from the sun's rays." </li> <li id="cite_note-What_does_your_image_show-78">^ <a href="#cite_ref-What_does_your_image_show_78-0">a</a> <a href="#cite_ref-What_does_your_image_show_78-1">b</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="http://mo-www.harvard.edu/microobs/guestobserverportal/Galileo/ThenNow/Milky%20Way/mObsMilkyWayweb.htm">"What does your image show"</a>. mo-www.harvard.edu. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230315164805/http://mo-www.harvard.edu/microobs/guestobserverportal/Galileo/ThenNow/Milky%20Way/mObsMilkyWayweb.htm">Archived</a> from the original on March 15, 2023. Retrieved October 20, 2022.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=mo-www.harvard.edu&rft.atitle=What+does+your+image+show&rft_id=http%3A%2F%2Fmo-www.harvard.edu%2Fmicroobs%2Fguestobserverportal%2FGalileo%2FThenNow%2FMilky%2520Way%2FmObsMilkyWayweb.htm&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-Montada-79">^ <a href="#cite_ref-Montada_79-0">a</a> <a href="#cite_ref-Montada_79-1">b</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMontada2007" class="citation encyclopaedia cs1">Montada, Josep Puig (September 28, 2007). <a rel="nofollow" class="external text" href="http://plato.stanford.edu/entries/ibn-bajja">"Ibn Bajja"</a>. <a href="/wiki/Stanford_Encyclopedia_of_Philosophy" title="Stanford Encyclopedia of Philosophy">Stanford Encyclopedia of Philosophy</a>. <a rel="nofollow" class="external text" href="https://archive.today/20120728/http://plato.stanford.edu/entries/ibn-bajja">Archived</a> from the original on July 28, 2012. Retrieved July 11, 2008.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=bookitem&rft.atitle=Ibn+Bajja&rft.btitle=Stanford+Encyclopedia+of+Philosophy&rft.date=2007-09-28&rft.aulast=Montada&rft.aufirst=Josep+Puig&rft_id=http%3A%2F%2Fplato.stanford.edu%2Fentries%2Fibn-bajja&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-80"><a href="#cite_ref-80">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFAristotle1931" class="citation book cs1">Aristotle (1931). <a rel="nofollow" class="external text" href="http://archive.org/details/workstranslatedi03arisuoft">Works</a>. Translated by Ross, William David; Smith, John Alexander. Oxford: Clarendon Press. p. 345.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Works&rft.place=Oxford&rft.pages=345&rft.pub=Clarendon+Press&rft.date=1931&rft.au=Aristotle&rft_id=http%3A%2F%2Farchive.org%2Fdetails%2Fworkstranslatedi03arisuoft&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-heidarzadeh2008-81"><a href="#cite_ref-heidarzadeh2008_81-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHeidarzadeh2008" class="citation book cs1">Heidarzadeh, Tofigh (2008). <a rel="nofollow" class="external text" href="https://archive.org/details/historyphysicalt00heid_599">A history of physical theories of comets, from Aristotle to Whipple</a>. Springer. pp. <a rel="nofollow" class="external text" href="https://archive.org/details/historyphysicalt00heid_599/page/n33">23</a>–25. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-1-4020-8322-8" title="Special:BookSources/978-1-4020-8322-8"><bdi>978-1-4020-8322-8</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=A+history+of+physical+theories+of+comets%2C+from+Aristotle+to+Whipple&rft.pages=23-25&rft.pub=Springer&rft.date=2008&rft.isbn=978-1-4020-8322-8&rft.aulast=Heidarzadeh&rft.aufirst=Tofigh&rft_id=https%3A%2F%2Farchive.org%2Fdetails%2Fhistoryphysicalt00heid_599&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-mactutor_albirundi-82"><a href="#cite_ref-mactutor_albirundi_82-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFO'ConnorRobertson" class="citation cs2">O'Connor, John J.; <a href="/wiki/Edmund_F._Robertson" title="Edmund F. Robertson">Robertson, Edmund F.</a>, <a rel="nofollow" class="external text" href="https://mathshistory.st-andrews.ac.uk/Biographies/Al-Biruni.html">"Abu Rayhan Muhammad ibn Ahmad al-Biruni"</a>, <a href="/wiki/MacTutor_History_of_Mathematics_Archive" title="MacTutor History of Mathematics Archive">MacTutor History of Mathematics Archive</a>, <a href="/wiki/University_of_St_Andrews" title="University of St Andrews">University of St Andrews</a></cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=bookitem&rft.atitle=Abu+Rayhan+Muhammad+ibn+Ahmad+al-Biruni&rft.btitle=MacTutor+History+of+Mathematics+Archive&rft.pub=University+of+St+Andrews&rft.aulast=O%27Connor&rft.aufirst=John+J.&rft.au=Robertson%2C+Edmund+F.&rft_id=https%3A%2F%2Fmathshistory.st-andrews.ac.uk%2FBiographies%2FAl-Biruni.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988">[<a href="/wiki/Wikipedia:Reliable_sources" title="Wikipedia:Reliable sources">unreliable source?</a>] </li> <li id="cite_note-ragep1993-83"><a href="#cite_ref-ragep1993_83-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFRagep1993" class="citation book cs1">Ragep, Jamil (1993). Nasir al-Din al-Tusi's Memoir on Astronomy (al-Tadhkira fi 'ilm al-hay' a). New York: Springer-Verlag. p. 129.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Nasir+al-Din+al-Tusi%27s+Memoir+on+Astronomy+%28al-Tadhkira+fi+%27ilm+al-hay%27+a%29&rft.place=New+York&rft.pages=129&rft.pub=Springer-Verlag&rft.date=1993&rft.aulast=Ragep&rft.aufirst=Jamil&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-Livingston-84"><a href="#cite_ref-Livingston_84-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFLivingston1971" class="citation journal cs1">Livingston, John W. (1971). "Ibn Qayyim al-Jawziyyah: A Fourteenth Century Defense against Astrological Divination and Alchemical Transmutation". Journal of the American Oriental Society. 91 (1): 96–103 [99]. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.2307%2F600445">10.2307/600445</a>. <a href="/wiki/JSTOR_(identifier)" class="mw-redirect" title="JSTOR (identifier)">JSTOR</a> <a rel="nofollow" class="external text" href="https://www.jstor.org/stable/600445">600445</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Journal+of+the+American+Oriental+Society&rft.atitle=Ibn+Qayyim+al-Jawziyyah%3A+A+Fourteenth+Century+Defense+against+Astrological+Divination+and+Alchemical+Transmutation&rft.volume=91&rft.issue=1&rft.pages=96-103+99&rft.date=1971&rft_id=info%3Adoi%2F10.2307%2F600445&rft_id=https%3A%2F%2Fwww.jstor.org%2Fstable%2F600445%23id-name%3DJSTOR&rft.aulast=Livingston&rft.aufirst=John+W.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-85"><a href="#cite_ref-85">^</a> Galileo Galilei, Sidereus Nuncius (Venice: Thomas Baglioni, 1610), <a rel="nofollow" class="external text" href="https://archive.org/stream/Sidereusnuncius00Gali#page/n37/mode/2up">pp. 15–16</a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20160316173644/https://archive.org/stream/Sidereusnuncius00Gali">Archived</a> March 16, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a> English translation: Galileo Galilei with Edward Stafford Carlos, trans., The Sidereal Messenger (London: Rivingtons, 1880), <a rel="nofollow" class="external text" href="https://archive.org/stream/siderealmessenge80gali#page/42/mode/2up/">pp. 42–43</a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20121202215542/https://archive.org/stream/siderealmessenge80gali">Archived</a> December 2, 2012, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a> </li> <li id="cite_note-oconnor_robertson2002-86"><a href="#cite_ref-oconnor_robertson2002_86-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFO'ConnorRobertson2002" class="citation web cs1">O'Connor, J. J.; Robertson, E. F. (November 2002). <a rel="nofollow" class="external text" href="http://www-gap.dcs.st-and.ac.uk/~history/Biographies/Galileo.html">"Galileo Galilei"</a>. University of St. Andrews. <a rel="nofollow" class="external text" href="https://archive.today/20120530/http://www-gap.dcs.st-and.ac.uk/~history/Biographies/Galileo.html">Archived</a> from the original on May 30, 2012. Retrieved January 8, 2007.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Galileo+Galilei&rft.pub=University+of+St.+Andrews&rft.date=2002-11&rft.aulast=O%27Connor&rft.aufirst=J.+J.&rft.au=Robertson%2C+E.+F.&rft_id=http%3A%2F%2Fwww-gap.dcs.st-and.ac.uk%2F~history%2FBiographies%2FGalileo.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-87"><a href="#cite_ref-87">^</a> Thomas Wright, An Original Theory or New Hypothesis of the Universe (London, England: H. Chapelle, 1750). <ul><li><a rel="nofollow" class="external text" href="https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA57">On page 57</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120195004/https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA57">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>, Wright stated that despite their mutual gravitational attraction, the stars in the constellations do not collide because they are in orbit, so centrifugal force keeps them separated: "centrifugal force, which not only preserves them in their orbits, but prevents them from rushing all together, by the common universal law of gravity, ..."</li> <li><a rel="nofollow" class="external text" href="https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA48">On page 48</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120194825/https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA48">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>, Wright stated that the form of the Milky Way is a ring: "the stars are not infinitely dispersed and distributed in a promiscuous manner throughout all the mundane space, without order or design, ... this phænomenon [is] no other than a certain effect arising from the observer's situation, ... To a spectator placed in an indefinite space, ... it [i.e. the Milky Way (Via Lactea)] [is] a vast ring of stars ..."</li> <li><a rel="nofollow" class="external text" href="https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA65">On page 65</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120174208/https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA65">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>, Wright speculated that the central body of the Milky Way, around which the rest of the galaxy revolves, might not be visible to us: "the central body A, being supposed as incognitum [i.e. an unknown], without [i.e. outside of] the finite view; ..."</li> <li><a rel="nofollow" class="external text" href="https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA73">On page 73</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120194830/https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA73">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>, Wright called the Milky Way the Vortex Magnus (the great whirlpool) and estimated its diameter to be 8.64×1012 miles (13.9×1012 km).</li> <li><a rel="nofollow" class="external text" href="https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA33">On page 33</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120172753/https://books.google.com/books?id=80VZAAAAcAAJ&pg=PA33">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>, Wright speculated that there are a vast number of inhabited planets in the galaxy: "therefore we may justly suppose, that so many radiant bodies [i.e. stars] were not created barely to enlighten an infinite void, but to ... display an infinite shapeless universe, crowded with myriads of glorious worlds, all variously revolving round them; and ... with an inconceivable variety of beings and states, animate ..."</li></ul> </li> <li id="cite_note-88"><a href="#cite_ref-88">^</a> Immanuel Kant, <a rel="nofollow" class="external text" href="https://books.google.com/books?id=nCcaAQAAMAAJ&pg=PP9">Allgemeine Naturgeschichte und Theorie des Himmels</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120195036/https://books.google.com/books?id=nCcaAQAAMAAJ&pg=PP9">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a> [General Natural History and Theory of Heaven], (Koenigsberg and Leipzig, (Germany): Johann Friederich Petersen, 1755). On pages 2–3, Kant acknowledged his debt to Thomas Wright: "Dem Herrn Wright von Durham, einen Engeländer, war es vorbehalten, einen glücklichen Schritt zu einer Bemerkung zu thun, welche von ihm selber zu keiner gar zu tüchtigen Absicht gebraucht zu seyn scheinet, und deren nützliche Anwendung er nicht genugsam beobachtet hat. Er betrachtete die Fixsterne nicht als ein ungeordnetes und ohne Absicht zerstreutes Gewimmel, sondern er fand eine systematische Verfassung im Ganzen, und eine allgemeine Beziehung dieser Gestirne gegen einen Hauptplan der Raume, die sie einnehmen." ("To Mr. Wright of Durham, an Englishman, it was reserved to take a happy step towards an observation, which seemed, to him and to no one else, to be needed for a clever idea, the exploitation of which he has not studied sufficiently. He regarded the fixed stars not as a disorganized swarm that was scattered without a design; rather, he found a systematic shape in the whole, and a general relation between these stars and the principal plane of the space that they occupy.") </li> <li id="cite_note-89"><a href="#cite_ref-89">^</a> Kant (1755), <a rel="nofollow" class="external text" href="https://books.google.com/books?id=nCcaAQAAMAAJ&pg=PP49">pages xxxiii–xxxvi of the Preface (Vorrede)</a>: <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120231151/https://books.google.com/books?id=nCcaAQAAMAAJ&pg=PP49">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>: "Ich betrachtete die Art neblichter Sterne, deren Herr von Maupertuis in der Abhandlung von der Figur der Gestirne gedenket, und die die Figur von mehr oder weniger offenen Ellipsen vorstellen, und versicherte mich leicht, daß sie nichts anders als eine Häufung vieler Fixsterne seyn können. Die jederzeit abgemessene Rundung dieser Figuren belehrte mich, daß hier ein unbegreiflich zahlreiches Sternenheer, und zwar um einen gemeinschaftlichen Mittelpunkt, müste geordnet seyn, weil sonst ihre freye Stellungen gegen einander, wohl irreguläre Gestalten, aber nicht abgemessene Figuren vorstellen würden. Ich sahe auch ein: daß sie in dem System, darinn sie sich vereinigt befinden, vornemlich auf eine Fläche beschränkt seyn müßten, weil sie nicht zirkelrunde, sondern elliptische Figuren abbilden, und daß sie wegen ihres blassen Lichts unbegreiflich weit von uns abstehen." ("I considered the type of nebulous stars, which Mr. de Maupertuis considered in his treatise on the shape of stars, and which present the figures of more or less open ellipses, and I readily assured myself, that they could be nothing else than a cluster of fixed stars. That these figures always measured round informed me that here an inconceivably numerous host of stars, [which were clustered] around a common center, must be orderly, because otherwise their free positions among each other would probably present irregular forms, not measurable figures. I also realized: that in the system in which they find themselves bound, they must be restricted primarily to a plane, because they display not circular, but elliptical figures, and that on account of their faint light, they are located inconceivably far from us.") </li> <li id="cite_note-our_galaxy-90"><a href="#cite_ref-our_galaxy_90-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFEvans1998" class="citation web cs1">Evans, J. C. (November 24, 1998). <a rel="nofollow" class="external text" href="http://physics.gmu.edu/~jevans/astr103/CourseNotes/ECText/ch20_txt.htm">"Our Galaxy"</a>. George Mason University. <a rel="nofollow" class="external text" href="https://archive.today/20120630/http://physics.gmu.edu/~jevans/astr103/CourseNotes/ECText/ch20_txt.htm">Archived</a> from the original on June 30, 2012. Retrieved January 4, 2007.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Our+Galaxy&rft.pub=George+Mason+University&rft.date=1998-11-24&rft.aulast=Evans&rft.aufirst=J.+C.&rft_id=http%3A%2F%2Fphysics.gmu.edu%2F~jevans%2Fastr103%2FCourseNotes%2FECText%2Fch20_txt.htm&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-91"><a href="#cite_ref-91">^</a> The term Weltinsel (world island) appears nowhere in Kant's book of 1755. The term first appeared in 1850, in the third volume of von Humboldt's Kosmos: Alexander von Humboldt, Kosmos, vol. 3 (Stuttgart & Tübingen, (Germany): J. G. Cotta, 1850), pp. 187, 189. <a rel="nofollow" class="external text" href="https://books.google.com/books?id=Su0iAQAAMAAJ&pg=PA187">From p. 187</a>: <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120174304/https://books.google.com/books?id=Su0iAQAAMAAJ&pg=PA187">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a> "Thomas Wright von Durham, Kant, Lambert und zuerst auch William Herschel waren geneigt die Gestalt der Milchstraße und die scheinbare Anhäufung der Sterne in derselben als eine Folge der abgeplatteten Gestalt und ungleichen Dimensionen der Weltinsel (Sternschict) zu betrachten, in welche unser Sonnensystem eingeschlossen ist." ("Thomas Wright of Durham, Kant, Lambert and at first also William Herschel were inclined to regard the shape of the Milky Way and the apparent clustering of stars in it as a consequence of the oblate shape and unequal dimensions of the world island (star stratum), in which our solar system is included.) In the English translation – Alexander von Humboldt with <a href="/wiki/E._C._Ott%C3%A9" class="mw-redirect" title="E. C. Otté">E. C. Otté</a>, trans., Cosmos ... (New York City: Harper & Brothers, 1897), vols. 3–5. see <a rel="nofollow" class="external text" href="http://babel.hathitrust.org/cgi/pt?id=njp.32101057350447;view=1up;seq=157">p. 147</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20181106181344/https://babel.hathitrust.org/cgi/pt?id=njp.32101057350447;view=1up;seq=157">Archived</a> November 6, 2018, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>. </li> <li id="cite_note-92"><a href="#cite_ref-92">^</a> William Herschel (1785), "On the Construction of the Heavens", Philosophical Transactions of the Royal Society of London, 75: 213–266. Herschel's diagram of the Milky Way appears immediately after the article's last page. See: <ul><li><a rel="nofollow" class="external text" href="https://books.google.com/books?id=IU9FAAAAcAAJ&pg=PA213">Google Books</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20161120170623/https://books.google.com/books?id=IU9FAAAAcAAJ&pg=PA213">Archived</a> November 20, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a></li> <li><a rel="nofollow" class="external text" href="http://rstl.royalsocietypublishing.org/content/75/213.full.pdf+html">The Royal Society of London</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20160406132029/http://rstl.royalsocietypublishing.org/content/75/213.full.pdf%20html">Archived</a> April 6, 2016, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a></li></ul> </li> <li id="cite_note-abbey-93"><a href="#cite_ref-abbey_93-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFAbbey" class="citation web cs1">Abbey, Lenny. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20130519124426/http://labbey.com/Telescopes/Parsontown.html">"The Earl of Rosse and the Leviathan of Parsontown"</a>. The Compleat Amateur Astronomer. Archived from <a rel="nofollow" class="external text" href="http://labbey.com/Telescopes/Parsontown.html">the original</a> on May 19, 2013. Retrieved January 4, 2007.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=The+Earl+of+Rosse+and+the+Leviathan+of+Parsontown&rft.pub=The+Compleat+Amateur+Astronomer&rft.aulast=Abbey&rft.aufirst=Lenny&rft_id=http%3A%2F%2Flabbey.com%2FTelescopes%2FParsontown.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-94"><a href="#cite_ref-94">^</a> See: <ul><li>Rosse revealed the spiral structure of <a href="/wiki/Whirlpool_Galaxy" title="Whirlpool Galaxy">Whirlpool Galaxy</a> (M51) at the 1845 meeting of the British Association for the Advancement of Science. Rosse's illustration of M51 was reproduced in J. P. Nichol's book of 1846. <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFRosse1846" class="citation journal cs1">Rosse, Earl of (1846). <a rel="nofollow" class="external text" href="https://babel.hathitrust.org/cgi/pt?id=njp.32101049356890&view=1up&seq=402">"On the nebula 25 Herschel, or 61 [should read: 51] of Messier's catalogue"</a>. Report of the Fifteenth Meeting of the British Association for the Advancement of Science; Held at Cambridge in June 1845 § Notices and Abstracts of Miscellaneous Communications to the Sections. Report of the ... Meeting of the British Association for the Advancement of Science (1833): 4. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210310235347/https://babel.hathitrust.org/cgi/pt?id=njp.32101049356890&view=1up&seq=402">Archived</a> from the original on March 10, 2021. Retrieved February 17, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Report+of+the+Fifteenth+Meeting+of+the+British+Association+for+the+Advancement+of+Science%3B+Held+at+Cambridge+in+June+1845+%C2%A7+Notices+and+Abstracts+of+Miscellaneous+Communications+to+the+Sections&rft.atitle=On+the+nebula+25+Herschel%2C+or+61+%5Bshould+read%3A+51%5D+of+Messier%27s+catalogue&rft.pages=4&rft.date=1846&rft.aulast=Rosse&rft.aufirst=Earl+of&rft_id=https%3A%2F%2Fbabel.hathitrust.org%2Fcgi%2Fpt%3Fid%3Dnjp.32101049356890%26view%3D1up%26seq%3D402&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFNichol1846" class="citation book cs1">Nichol, John Pringle (1846). <a rel="nofollow" class="external text" href="https://babel.hathitrust.org/cgi/pt?id=uc2.ark%3A%2F13960%2Ft9k360k8b&view=1up&seq=65">Thoughts on Some Important Points Relating to the System of the World</a>. Edinburgh, Scotland: William Tait. p. 23. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210308094837/https://babel.hathitrust.org/cgi/pt?id=uc2.ark%3A%2F13960%2Ft9k360k8b&view=1up&seq=65">Archived</a> from the original on March 8, 2021. Retrieved February 17, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Thoughts+on+Some+Important+Points+Relating+to+the+System+of+the+World&rft.place=Edinburgh%2C+Scotland&rft.pages=23&rft.pub=William+Tait&rft.date=1846&rft.aulast=Nichol&rft.aufirst=John+Pringle&rft_id=https%3A%2F%2Fbabel.hathitrust.org%2Fcgi%2Fpt%3Fid%3Duc2.ark%253A%252F13960%252Ft9k360k8b%26view%3D1up%26seq%3D65&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> Rosse's illustration of the Whirlpool Galaxy appears on the plate that immediately precedes p. 23.</li></ul></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSouth1846" class="citation journal cs1 cs1-prop-foreign-lang-source">South, James (1846). <a rel="nofollow" class="external text" href="https://babel.hathitrust.org/cgi/pt?id=pst.000055399548&view=1up&seq=279&size=125">"Auszug aus einem Berichte über Lord Rosse's grosses Telescop, den Sir James South in The Times, Nr. 18899, 1845 April 16 bekannt gemacht hat"</a> [Excerpt from a report about Lord Rosse's great telescope, which Sir James South made known in The Times [of London], no. 18,899, 1845 April 16]. Astronomische Nachrichten (in German). 23 (536): 113–118. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1002%2Fasna.18460230802">10.1002/asna.18460230802</a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210308145128/https://babel.hathitrust.org/cgi/pt?id=pst.000055399548&view=1up&seq=279&size=125">Archived</a> from the original on March 8, 2021. Retrieved February 17, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomische+Nachrichten&rft.atitle=Auszug+aus+einem+Berichte+%C3%BCber+Lord+Rosse%27s+grosses+Telescop%2C+den+Sir+James+South+in+The+Times%2C+Nr.+18899%2C+1845+April+16+bekannt+gemacht+hat&rft.volume=23&rft.issue=536&rft.pages=113-118&rft.date=1846&rft_id=info%3Adoi%2F10.1002%2Fasna.18460230802&rft.aulast=South&rft.aufirst=James&rft_id=https%3A%2F%2Fbabel.hathitrust.org%2Fcgi%2Fpt%3Fid%3Dpst.000055399548%26view%3D1up%26seq%3D279%26size%3D125&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> On March 5, 1845, Rosse observed M51, the <a href="/wiki/Whirlpool_Galaxy" title="Whirlpool Galaxy">Whirlpool Galaxy</a>. From column 115: "The most popularly known nebulæ observed this night were the ring nebulæ in the Canes Venatici, or the 51st of Messier's catalogue, which was resolved into stars with a magnifying power of 548".</li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFRobinson1845" class="citation journal cs1">Robinson, T. R. (1845). <a rel="nofollow" class="external text" href="https://www.biodiversitylibrary.org/item/46714#page/132/mode/1up">"On Lord Rosse's telescope"</a>. Proceedings of the Royal Irish Academy. 3 (50): 114–133. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20200610193425/https://www.biodiversitylibrary.org/item/46714#page/132/mode/1up">Archived</a> from the original on June 10, 2020. Retrieved February 17, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Proceedings+of+the+Royal+Irish+Academy&rft.atitle=On+Lord+Rosse%27s+telescope&rft.volume=3&rft.issue=50&rft.pages=114-133&rft.date=1845&rft.aulast=Robinson&rft.aufirst=T.+R.&rft_id=https%3A%2F%2Fwww.biodiversitylibrary.org%2Fitem%2F46714%23page%2F132%2Fmode%2F1up&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> Rosse's early observations of nebulae and galaxies are discussed on pp. 127–130.</li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFRosse1850" class="citation journal cs1">Rosse, The Earl of (1850). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=BlFFAAAAcAAJ&pg=PA499">"Observations on the nebulae"</a>. Philosophical Transactions of the Royal Society of London. 140: 499–514. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1098%2Frstl.1850.0026">10.1098/rstl.1850.0026</a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230326142957/https://books.google.com/books?id=BlFFAAAAcAAJ&pg=PA499">Archived</a> from the original on March 26, 2023. Retrieved February 17, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Philosophical+Transactions+of+the+Royal+Society+of+London&rft.atitle=Observations+on+the+nebulae&rft.volume=140&rft.pages=499-514&rft.date=1850&rft_id=info%3Adoi%2F10.1098%2Frstl.1850.0026&rft.aulast=Rosse&rft.aufirst=The+Earl+of&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DBlFFAAAAcAAJ%26pg%3DPA499&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> Rosse's illustrations of nebulae and galaxies appear on the plates that immediately precede the article.</li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFBaileyButlerMcFarland2005" class="citation journal cs1">Bailey, M. E.; Butler, C. J.; McFarland, J. (April 2005). <a rel="nofollow" class="external text" href="https://doi.org/10.1111%2Fj.1468-4004.2005.46226.x">"Unwinding the discovery of spiral nebulae"</a>. Astronomy & Geophysics. 46 (2): 2.26–2.28. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1111%2Fj.1468-4004.2005.46226.x">10.1111/j.1468-4004.2005.46226.x</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomy+%26+Geophysics&rft.atitle=Unwinding+the+discovery+of+spiral+nebulae&rft.volume=46&rft.issue=2&rft.pages=2.26-2.28&rft.date=2005-04&rft_id=info%3Adoi%2F10.1111%2Fj.1468-4004.2005.46226.x&rft.aulast=Bailey&rft.aufirst=M.+E.&rft.au=Butler%2C+C.+J.&rft.au=McFarland%2C+J.&rft_id=https%3A%2F%2Fdoi.org%2F10.1111%252Fj.1468-4004.2005.46226.x&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li></ul> </li> <li id="cite_note-95"><a href="#cite_ref-95">^</a> See: <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFKapteyn1906" class="citation book cs1">Kapteyn, Jacobus Cornelius (1906). <a rel="nofollow" class="external text" href="https://babel.hathitrust.org/cgi/pt?id=hvd.32044103057121&view=1up&seq=412">"Statistical methods in stellar astronomy"</a>. In Rogers, Howard J. (ed.). Congress of Arts and Science, Universal Exposition, St. Louis, 1904. Vol. 4. Boston and New York: Houghton, Mifflin and Co. pp. 396–425. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210308053515/https://babel.hathitrust.org/cgi/pt?id=hvd.32044103057121&view=1up&seq=412">Archived</a> from the original on March 8, 2021. Retrieved February 6, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=bookitem&rft.atitle=Statistical+methods+in+stellar+astronomy&rft.btitle=Congress+of+Arts+and+Science%2C+Universal+Exposition%2C+St.+Louis%2C+1904&rft.place=Boston+and+New+York&rft.pages=396-425&rft.pub=Houghton%2C+Mifflin+and+Co.&rft.date=1906&rft.aulast=Kapteyn&rft.aufirst=Jacobus+Cornelius&rft_id=https%3A%2F%2Fbabel.hathitrust.org%2Fcgi%2Fpt%3Fid%3Dhvd.32044103057121%26view%3D1up%26seq%3D412&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> From pp. 419–420: "It follows that the one set of the stars must have a systematic motion relative to the other. ... these two main directions of motion must be in reality diametrically opposite."</li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFKapteyn1905" class="citation journal cs1">Kapteyn, J. C. (1905). <a rel="nofollow" class="external text" href="https://babel.hathitrust.org/cgi/pt?id=njp.32101076796737&view=1up&seq=399">"Star streaming"</a>. Report of the Seventy-fifth Meeting of the British Association for the Advancement of Science, South Africa. Report of the ... Meeting of the British Association for the Advancement of Science (1833): 257–265. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210308042552/https://babel.hathitrust.org/cgi/pt?id=njp.32101076796737&view=1up&seq=399">Archived</a> from the original on March 8, 2021. Retrieved February 6, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Report+of+the+Seventy-fifth+Meeting+of+the+British+Association+for+the+Advancement+of+Science%2C+South+Africa&rft.atitle=Star+streaming&rft.pages=257-265&rft.date=1905&rft.aulast=Kapteyn&rft.aufirst=J.+C.&rft_id=https%3A%2F%2Fbabel.hathitrust.org%2Fcgi%2Fpt%3Fid%3Dnjp.32101076796737%26view%3D1up%26seq%3D399&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li></ul> </li> <li id="cite_note-96"><a href="#cite_ref-96">^</a> See: <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSchwarzschild1907" class="citation journal cs1 cs1-prop-foreign-lang-source">Schwarzschild, K. (1907). <a rel="nofollow" class="external text" href="https://babel.hathitrust.org/cgi/pt?id=mdp.39015048391208&view=1up&seq=654">"Ueber die Eigenbewegungen der Fixsterne"</a> [On the proper motions of the fixed stars]. Nachrichten von der Königlichen Gesellschaft der Wissenschaften zu Göttingen (Reports of the Royal Society of Science at Göttingen) (in German). 5: 614–632. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1907NWGot...5..614S">1907NWGot...5..614S</a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210308142441/https://babel.hathitrust.org/cgi/pt?id=mdp.39015048391208&view=1up&seq=654">Archived</a> from the original on March 8, 2021. Retrieved February 6, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Nachrichten+von+der+K%C3%B6niglichen+Gesellschaft+der+Wissenschaften+zu+G%C3%B6ttingen+%28Reports+of+the+Royal+Society+of+Science+at+G%C3%B6ttingen%29&rft.atitle=Ueber+die+Eigenbewegungen+der+Fixsterne&rft.volume=5&rft.pages=614-632&rft.date=1907&rft_id=info%3Abibcode%2F1907NWGot...5..614S&rft.aulast=Schwarzschild&rft.aufirst=K.&rft_id=https%3A%2F%2Fbabel.hathitrust.org%2Fcgi%2Fpt%3Fid%3Dmdp.39015048391208%26view%3D1up%26seq%3D654&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSchwarzschild1908" class="citation journal cs1 cs1-prop-foreign-lang-source">Schwarzschild, K. (1908). <a rel="nofollow" class="external text" href="https://babel.hathitrust.org/cgi/pt?id=mdp.39015048391554&view=1up&seq=209">"Ueber die Bestimmung von Vertex und Apex nach der Ellipsoidhypothese aus einer geringeren Anzahl beobachteter Eigenbewegungen"</a> [On the determination, according to the ellipsoid hypothesis, of the vertex and apex from a small number of observed proper motions]. Nachrichten von der Königlichen Gesellschaft der Wissenschaften zu Göttingen (in German): 191–200. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210308024321/https://babel.hathitrust.org/cgi/pt?id=mdp.39015048391554&view=1up&seq=209">Archived</a> from the original on March 8, 2021. Retrieved February 6, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Nachrichten+von+der+K%C3%B6niglichen+Gesellschaft+der+Wissenschaften+zu+G%C3%B6ttingen&rft.atitle=Ueber+die+Bestimmung+von+Vertex+und+Apex+nach+der+Ellipsoidhypothese+aus+einer+geringeren+Anzahl+beobachteter+Eigenbewegungen&rft.pages=191-200&rft.date=1908&rft.aulast=Schwarzschild&rft.aufirst=K.&rft_id=https%3A%2F%2Fbabel.hathitrust.org%2Fcgi%2Fpt%3Fid%3Dmdp.39015048391554%26view%3D1up%26seq%3D209&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li></ul> </li> <li id="cite_note-97"><a href="#cite_ref-97">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFCurtis1917" class="citation journal cs1">Curtis, Heber D. (1917). <a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F122632">"Novae in spiral nebulae and the island universe theory"</a>. Publications of the Astronomical Society of the Pacific. 29 (171): 206–207. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1917PASP...29..206C">1917PASP...29..206C</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F122632">10.1086/122632</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Publications+of+the+Astronomical+Society+of+the+Pacific&rft.atitle=Novae+in+spiral+nebulae+and+the+island+universe+theory&rft.volume=29&rft.issue=171&rft.pages=206-207&rft.date=1917&rft_id=info%3Adoi%2F10.1086%2F122632&rft_id=info%3Abibcode%2F1917PASP...29..206C&rft.aulast=Curtis&rft.aufirst=Heber+D.&rft_id=https%3A%2F%2Fdoi.org%2F10.1086%252F122632&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-pasp100_6-98"><a href="#cite_ref-pasp100_6_98-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFCurtis1988" class="citation journal cs1"><a href="/wiki/Heber_Doust_Curtis" title="Heber Doust Curtis">Curtis, H. 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Publications of the Astronomical Society of the Pacific. 100: 6–7. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1988PASP..100....6C">1988PASP..100....6C</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F132128">10.1086/132128</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Publications+of+the+Astronomical+Society+of+the+Pacific&rft.atitle=Novae+in+spiral+nebulae+and+the+Island+Universe+Theory&rft.volume=100&rft.pages=6-7&rft.date=1988&rft_id=info%3Adoi%2F10.1086%2F132128&rft_id=info%3Abibcode%2F1988PASP..100....6C&rft.aulast=Curtis&rft.aufirst=H.+D.&rft_id=https%3A%2F%2Fdoi.org%2F10.1086%252F132128&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-weaver-99"><a href="#cite_ref-weaver_99-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFWeaver" class="citation web cs1">Weaver, Harold F. <a rel="nofollow" class="external text" href="http://www.nap.edu/readingroom/books/biomems/rtrumpler.html">"Robert Julius Trumpler"</a>. National Academy of Sciences. <a rel="nofollow" class="external text" href="https://archive.today/20120604/http://www.nap.edu/readingroom/books/biomems/rtrumpler.html">Archived</a> from the original on June 4, 2012. Retrieved January 5, 2007.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Robert+Julius+Trumpler&rft.pub=National+Academy+of+Sciences&rft.aulast=Weaver&rft.aufirst=Harold+F.&rft_id=http%3A%2F%2Fwww.nap.edu%2Freadingroom%2Fbooks%2Fbiomems%2Frtrumpler.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-jrasc83_6-100"><a href="#cite_ref-jrasc83_6_100-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSandage1989" class="citation journal cs1"><a href="/wiki/Allan_Sandage" title="Allan Sandage">Sandage, Allan</a> (1989). 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The Astrophysical Journal. 69: 103–158. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1929ApJ....69..103H">1929ApJ....69..103H</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F143167">10.1086/143167</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astrophysical+Journal&rft.atitle=A+spiral+nebula+as+a+stellar+system%2C+Messier+31&rft.volume=69&rft.pages=103-158&rft.date=1929&rft_id=info%3Adoi%2F10.1086%2F143167&rft_id=info%3Abibcode%2F1929ApJ....69..103H&rft.aulast=Hubble&rft.aufirst=E.+P.&rft_id=https%3A%2F%2Fdoi.org%2F10.1086%252F143167&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-102"><a href="#cite_ref-102">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="https://web.archive.org/web/20160915183426/http://news.nationalgeographic.com/2016/09/gaia-milky-way-maps-billion-stars-atlas-space-science/">"New Milky Way Map Is a Spectacular Billion-Star Atlas"</a>. September 14, 2016. Archived from <a rel="nofollow" class="external text" href="http://news.nationalgeographic.com/2016/09/gaia-milky-way-maps-billion-stars-atlas-space-science">the original</a> on September 15, 2016. Retrieved September 15, 2016.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=New+Milky+Way+Map+Is+a+Spectacular+Billion-Star+Atlas&rft.date=2016-09-14&rft_id=http%3A%2F%2Fnews.nationalgeographic.com%2F2016%2F09%2Fgaia-milky-way-maps-billion-stars-atlas-space-science&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-103"><a href="#cite_ref-103">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="http://www.cosmos.esa.int/web/gaia/dr1">"Gaia > Gaia DR1"</a>. www.cosmos.esa.int. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20160915091251/http://www.cosmos.esa.int/web/gaia/dr1">Archived</a> from the original on September 15, 2016. 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Brooke Boen. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20121023023929/http://www.nasa.gov/mission_pages/chandra/news/H-12-331.html">Archived</a> from the original on October 23, 2012. Retrieved October 28, 2012.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=NASA%27s+Chandra+Shows+Milky+Way+is+Surrounded+by+Halo+of+Hot+Gas&rft.pub=Brooke+Boen&rft.aulast=Boen&rft.aufirst=Brooke&rft_id=http%3A%2F%2Fwww.nasa.gov%2Fmission_pages%2Fchandra%2Fnews%2FH-12-331.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-247"><a href="#cite_ref-247">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGuptaMathurKrongoldNicastro2012" class="citation journal cs1">Gupta, A.; Mathur, S.; Krongold, Y.; Nicastro, F.; Galeazzi, M. (2012). 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The Astrophysical Journal. 756 (1): L8. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/1205.5037">1205.5037</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2012ApJ...756L...8G">2012ApJ...756L...8G</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1088%2F2041-8205%2F756%2F1%2FL8">10.1088/2041-8205/756/1/L8</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:118567708">118567708</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astrophysical+Journal&rft.atitle=A+Huge+Reservoir+of+Ionized+Gas+Around+the+Milky+Way%3A+Accounting+for+the+Missing+Mass%3F&rft.volume=756&rft.issue=1&rft.pages=L8&rft.date=2012&rft_id=info%3Aarxiv%2F1205.5037&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A118567708%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1088%2F2041-8205%2F756%2F1%2FL8&rft_id=info%3Abibcode%2F2012ApJ...756L...8G&rft.aulast=Gupta&rft.aufirst=A.&rft.au=Mathur%2C+S.&rft.au=Krongold%2C+Y.&rft.au=Nicastro%2C+F.&rft.au=Galeazzi%2C+M.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-248"><a href="#cite_ref-248">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="http://chandra.si.edu/photo/2012/halo/">"Galactic Halo: Milky Way is Surrounded by Huge Halo of Hot Gas"</a>. 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September 24, 2012. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20121029155611/http://chandra.si.edu/photo/2012/halo/">Archived</a> from the original on October 29, 2012.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Smithsonian+Astrophysical+Observatory&rft.atitle=Galactic+Halo%3A+Milky+Way+is+Surrounded+by+Huge+Halo+of+Hot+Gas&rft.date=2012-09-24&rft_id=http%3A%2F%2Fchandra.si.edu%2Fphoto%2F2012%2Fhalo%2F&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-249"><a href="#cite_ref-249">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFCommunications" class="citation web cs1">Communications, Discovery. <a rel="nofollow" class="external text" href="http://news.discovery.com/space/massive-pocket-of-hot-gas-envelopes-milky-way-120924.html">"Our Galaxy Swims Inside a Giant Pool of Hot Gas"</a>. Discovery Communications. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20121029004855/http://news.discovery.com/space/massive-pocket-of-hot-gas-envelopes-milky-way-120924.html">Archived</a> from the original on October 29, 2012. Retrieved October 28, 2012.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Our+Galaxy+Swims+Inside+a+Giant+Pool+of+Hot+Gas&rft.pub=Discovery+Communications&rft.aulast=Communications&rft.aufirst=Discovery&rft_id=http%3A%2F%2Fnews.discovery.com%2Fspace%2Fmassive-pocket-of-hot-gas-envelopes-milky-way-120924.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-Harrington_feature-250">^ <a href="#cite_ref-Harrington_feature_250-0">a</a> <a href="#cite_ref-Harrington_feature_250-1">b</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFJ.D._HarringtonJanet_AndersonPeter_Edmonds2012" class="citation news cs1">J.D. Harrington; Janet Anderson; Peter Edmonds (September 24, 2012). <a rel="nofollow" class="external text" href="https://www.nasa.gov/mission_pages/chandra/news/H-12-331.html">"NASA's Chandra Shows Milky Way is Surrounded by Halo of Hot Gas"</a>. NASA. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20121023023929/http://www.nasa.gov/mission_pages/chandra/news/H-12-331.html">Archived</a> from the original on October 23, 2012.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=NASA&rft.atitle=NASA%27s+Chandra+Shows+Milky+Way+is+Surrounded+by+Halo+of+Hot+Gas&rft.date=2012-09-24&rft.au=J.D.+Harrington&rft.au=Janet+Anderson&rft.au=Peter+Edmonds&rft_id=http%3A%2F%2Fwww.nasa.gov%2Fmission_pages%2Fchandra%2Fnews%2FH-12-331.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-Koupelis_Kuhn2007-251">^ <a href="#cite_ref-Koupelis_Kuhn2007_251-0">a</a> <a href="#cite_ref-Koupelis_Kuhn2007_251-1">b</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFKoupelisKuhn2007" class="citation book cs1">Koupelis, Theo; Kuhn, Karl F. (2007). <a rel="nofollow" class="external text" href="https://archive.org/details/inquestofunivers00koup">In Quest of the Universe</a>. Jones & Bartlett Publishers. p. <a rel="nofollow" class="external text" href="https://archive.org/details/inquestofunivers00koup/page/492">492</a>, Fig. 16–13. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-7637-4387-1" title="Special:BookSources/978-0-7637-4387-1"><bdi>978-0-7637-4387-1</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=In+Quest+of+the+Universe&rft.pages=492%2C+Fig.+16-13&rft.pub=Jones+%26+Bartlett+Publishers&rft.date=2007&rft.isbn=978-0-7637-4387-1&rft.aulast=Koupelis&rft.aufirst=Theo&rft.au=Kuhn%2C+Karl+F.&rft_id=https%3A%2F%2Farchive.org%2Fdetails%2Finquestofunivers00koup&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-Schneider-252"><a href="#cite_ref-Schneider_252-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFPeter_Schneider2006" class="citation book cs1">Peter Schneider (2006). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=uP1Hz-6sHaMC&q=rotation+Milky+way&pg=PA100">Extragalactic Astronomy and Cosmology</a>. Springer. page 4, Fig. 1.4. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-3-540-33174-2" title="Special:BookSources/978-3-540-33174-2"><bdi>978-3-540-33174-2</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230326143010/https://www.google.com/books/edition/Extragalactic_Astronomy_and_Cosmology/uP1Hz-6sHaMC?hl=en&gbpv=1&bsq=rotation+Milky+way&pg=PA100&printsec=frontcover">Archived</a> from the original on March 26, 2023. Retrieved October 27, 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Extragalactic+Astronomy+and+Cosmology&rft.pages=page-4%2C+Fig.-1.4&rft.pub=Springer&rft.date=2006&rft.isbn=978-3-540-33174-2&rft.au=Peter+Schneider&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DuP1Hz-6sHaMC%26q%3Drotation%2BMilky%2Bway%26pg%3DPA100&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-Jones1-253"><a href="#cite_ref-Jones1_253-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFJonesLambourneAdams2004" class="citation book cs1">Jones, Mark H.; Lambourne, Robert J.; Adams, David John (2004). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=36K1PfetZegC&q=Milky+Way+%22rotation+curve%22&pg=PA20">An Introduction to Galaxies and Cosmology</a>. Cambridge University Press. p. 21; Fig. 1.13. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-521-54623-2" title="Special:BookSources/978-0-521-54623-2"><bdi>978-0-521-54623-2</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230326143523/https://books.google.com/books?id=36K1PfetZegC&q=Milky+Way+%22rotation+curve%22&pg=PA20">Archived</a> from the original on March 26, 2023. 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Springer. p. 413. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-3-540-33174-2" title="Special:BookSources/978-3-540-33174-2"><bdi>978-3-540-33174-2</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230326143010/https://www.google.com/books/edition/Extragalactic_Astronomy_and_Cosmology/uP1Hz-6sHaMC?hl=en&gbpv=1&bsq=rotation+Milky+way&pg=PA100&printsec=frontcover">Archived</a> from the original on March 26, 2023. 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Wired UK. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20190106104313/https://www.wired.co.uk/article/dipole-repeller-milky-way">Archived</a> from the original on January 6, 2019. Retrieved May 5, 2022.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Wired+UK&rft.atitle=The+Milky+Way+is+being+pushed+through+space+by+a+void+called+the+Dipole+Repeller&rft_id=https%3A%2F%2Fwww.wired.co.uk%2Farticle%2Fdipole-repeller-milky-way&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-299"><a href="#cite_ref-299">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFKocevskiEbeling2006" class="citation journal cs1">Kocevski, D. D.; Ebeling, H. (2006). "On the origin of the Local Group's peculiar velocity". The Astrophysical Journal. 645 (2): 1043–1053. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0510106">astro-ph/0510106</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2006ApJ...645.1043K">2006ApJ...645.1043K</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F503666">10.1086/503666</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:2760455">2760455</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astrophysical+Journal&rft.atitle=On+the+origin+of+the+Local+Group%27s+peculiar+velocity&rft.volume=645&rft.issue=2&rft.pages=1043-1053&rft.date=2006&rft_id=info%3Aarxiv%2Fastro-ph%2F0510106&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A2760455%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1086%2F503666&rft_id=info%3Abibcode%2F2006ApJ...645.1043K&rft.aulast=Kocevski&rft.aufirst=D.+D.&rft.au=Ebeling%2C+H.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> <li id="cite_note-300"><a href="#cite_ref-300">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFPeirani,_SDefreitaspacheco2006" class="citation journal cs1">Peirani, S; Defreitaspacheco, J (2006). "Mass determination of groups of galaxies: Effects of the cosmological constant". New Astronomy. 11 (4): 325–330. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0508614">astro-ph/0508614</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2006NewA...11..325P">2006NewA...11..325P</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1016%2Fj.newast.2005.08.008">10.1016/j.newast.2005.08.008</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:685068">685068</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=New+Astronomy&rft.atitle=Mass+determination+of+groups+of+galaxies%3A+Effects+of+the+cosmological+constant&rft.volume=11&rft.issue=4&rft.pages=325-330&rft.date=2006&rft_id=info%3Aarxiv%2Fastro-ph%2F0508614&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A685068%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1016%2Fj.newast.2005.08.008&rft_id=info%3Abibcode%2F2006NewA...11..325P&rft.au=Peirani%2C+S&rft.au=Defreitaspacheco%2C+J&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"> </li> </ol></div></div> <div class="mw-heading mw-heading2"><h2 id="Further_reading">Further reading</h2></div> <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFDambeck2008" class="citation journal cs1">Dambeck, Thorsten (March 2008). "Gaia's Mission to the Milky Way". <a href="/wiki/Sky_%26_Telescope" title="Sky & Telescope">Sky & Telescope</a>: 36–39.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Sky+%26+Telescope&rft.atitle=Gaia%27s+Mission+to+the+Milky+Way&rft.pages=36-39&rft.date=2008-03&rft.aulast=Dambeck&rft.aufirst=Thorsten&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFChiappini2001" class="citation journal cs1">Chiappini, Cristina (November–December 2001). <a rel="nofollow" class="external text" href="http://www.astro.caltech.edu/~george/ay20/Chiappini-MilkyWay.pdf">"The Formation and Evolution of the Milky Way"</a> (PDF). <a href="/wiki/American_Scientist" title="American Scientist">American Scientist</a>. 89 (6): 506–515. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1511%2F2001.40.745">10.1511/2001.40.745</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=American+Scientist&rft.atitle=The+Formation+and+Evolution+of+the+Milky+Way&rft.volume=89&rft.issue=6&rft.pages=506-515&rft.date=2001-11%2F2001-12&rft_id=info%3Adoi%2F10.1511%2F2001.40.745&rft.aulast=Chiappini&rft.aufirst=Cristina&rft_id=http%3A%2F%2Fwww.astro.caltech.edu%2F~george%2Fay20%2FChiappini-MilkyWay.pdf&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMcTier2022" class="citation book cs1">McTier, Moiya (August 16, 2022). The Milky Way. Grand Central Publishing. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-1-5387-5415-3" title="Special:BookSources/978-1-5387-5415-3"><bdi>978-1-5387-5415-3</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=The+Milky+Way&rft.pub=Grand+Central+Publishing&rft.date=2022-08-16&rft.isbn=978-1-5387-5415-3&rft.aulast=McTier&rft.aufirst=Moiya&rfr_id=info%3Asid%2Fen.wikipedia.org%3AMilky+Way" class="Z3988"></li> <li><a href="/wiki/Phil_Plait" title="Phil Plait">Plait, Phil</a>, "The Milky Way's Secrets: Our galaxy's night-sky spectacle sparked <a href="/wiki/Scientific_revolution" class="mw-redirect" title="Scientific revolution">scientific revolutions</a>", <a href="/wiki/Scientific_American" title="Scientific American">Scientific American</a>, vol. 329, no. 4 (November 2023), pp. 86–87.</li></ul> <div class="mw-heading mw-heading2"><h2 id="External_links">External links</h2></div> <style data-mw-deduplicate="TemplateStyles:r1235681985">.mw-parser-output .side-box{margin:4px 0;box-sizing:border-box;border:1px solid #aaa;font-size:88%;line-height:1.25em;background-color:var(--background-color-interactive-subtle,#f8f9fa);display:flow-root}.mw-parser-output .side-box-abovebelow,.mw-parser-output .side-box-text{padding:0.25em 0.9em}.mw-parser-output .side-box-image{padding:2px 0 2px 0.9em;text-align:center}.mw-parser-output .side-box-imageright{padding:2px 0.9em 2px 0;text-align:center}@media(min-width:500px){.mw-parser-output .side-box-flex{display:flex;align-items:center}.mw-parser-output .side-box-text{flex:1;min-width:0}}@media(min-width:720px){.mw-parser-output .side-box{width:238px}.mw-parser-output .side-box-right{clear:right;float:right;margin-left:1em}.mw-parser-output .side-box-left{margin-right:1em}}</style><style data-mw-deduplicate="TemplateStyles:r1237033735">@media print{body.ns-0 .mw-parser-output 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href="http://www.sky-map.org/?ra=12.0593794293245&de=-20.27239516216098&zoom=0&show_grid=1&show_constellation_lines=1&show_constellation_boundaries=1&show_const_names=0&show_galaxies=1&img_source=HALPHA">Milky Way – H-Alpha survey</a> – wikisky.org</li> <li><a rel="nofollow" class="external text" href="https://asd.gsfc.nasa.gov/archive/mwmw/mmw_sci.html">Multiwavelength Milky Way</a> – Images and <a href="/wiki/VRML" title="VRML">VRML</a> models (NASA)</li> <li><a rel="nofollow" class="external text" href="http://www.360pano.eu/show/?id=736">Milky Way – Panorama (9 billion pixels)</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20170806131326/http://www.360pano.eu/show/?id=736">Archived</a> August 6, 2017, at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a>.</li> <li><a rel="nofollow" class="external text" href="http://messier.seds.org/more/mw.html">Milky Way</a> – SEDS Messier website</li> <li><a rel="nofollow" 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a>abbr{text-decoration:inherit}.mw-parser-output .navbar-mini abbr{font-variant:small-caps;border-bottom:none;text-decoration:none;cursor:inherit}.mw-parser-output .navbar-ct-full{font-size:114%;margin:0 7em}.mw-parser-output .navbar-ct-mini{font-size:114%;margin:0 4em}html.skin-theme-clientpref-night .mw-parser-output .navbar li a abbr{color:var(--color-base)!important}@media(prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .navbar li a abbr{color:var(--color-base)!important}}@media print{.mw-parser-output .navbar{display:none!important}}</style><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Milky_Way" title="Template:Milky Way"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Milky_Way" title="Template talk:Milky Way"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Milky_Way" title="Special:EditPage/Template:Milky Way"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Milky_Way" style="font-size:114%;margin:0 4em"><a class="mw-selflink selflink">Milky Way</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Location</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0;line-height:1.3em;"><div style="padding:0 0.25em"><a class="mw-selflink selflink">Milky Way</a> → <a href="/wiki/Satellite_galaxies_of_the_Milky_Way" title="Satellite galaxies of the Milky Way">Milky Way subgroup</a> → <a href="/wiki/Local_Group" title="Local Group">Local Group</a> → <a href="/wiki/Local_Sheet" title="Local Sheet">Local Sheet</a> → <a href="/wiki/Virgo_Supercluster" title="Virgo Supercluster">Virgo Supercluster</a> → <a href="/wiki/Laniakea_Supercluster" title="Laniakea Supercluster">Laniakea Supercluster</a> → <a href="/wiki/Local_Hole" title="Local Hole">Local Hole</a> → <a href="/wiki/Observable_universe" title="Observable universe">Observable universe</a> → <a href="/wiki/Universe" title="Universe">Universe</a> Each arrow (→) may be read as "within" or "part of".</div></td><td class="noviewer navbox-image" rowspan="4" style="width:1px;padding:0 0 0 2px"><div><figure class="mw-halign-right" typeof="mw:File"><a href="/wiki/File:Artist%E2%80%99s_impression_of_the_Milky_Way.jpg" class="mw-file-description" title="The Milky Way Galaxy"><img alt="The Milky Way Galaxy" src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4f/Artist%E2%80%99s_impression_of_the_Milky_Way.jpg/85px-Artist%E2%80%99s_impression_of_the_Milky_Way.jpg" decoding="async" width="85" height="85" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4f/Artist%E2%80%99s_impression_of_the_Milky_Way.jpg/128px-Artist%E2%80%99s_impression_of_the_Milky_Way.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4f/Artist%E2%80%99s_impression_of_the_Milky_Way.jpg/170px-Artist%E2%80%99s_impression_of_the_Milky_Way.jpg 2x" data-file-width="5600" data-file-height="5600" /></a><figcaption>The Milky Way Galaxy</figcaption></figure></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Structure</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Sagittarius_A" title="Sagittarius A">Sagittarius A</a></li> <li><a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a> <ul><li><a href="/wiki/Fermi_bubble" class="mw-redirect" title="Fermi bubble">Fermi bubbles</a></li></ul></li> <li><a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">Supermassive black hole</a></li> <li><a href="/wiki/Galactic_Center_filament" title="Galactic Center filament">Galactic Center filaments</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Galactic_disc#Structure_of_the_Milky_Way_Disc" title="Galactic disc">Disk</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Carina%E2%80%93Sagittarius_Arm" title="Carina–Sagittarius Arm">Carina–Sagittarius</a></li> <li><a href="/wiki/Norma_Arm" title="Norma Arm">Norma–Cygnus</a></li> <li><a href="/wiki/Orion_Arm" title="Orion Arm">Orion–Cygnus</a></li> <li><a href="/wiki/Perseus_Arm" title="Perseus Arm">Perseus</a></li> <li><a href="/wiki/Scutum%E2%80%93Centaurus_Arm" title="Scutum–Centaurus Arm">Scutum–Centaurus</a></li> <li><a href="/wiki/Near_3_kpc_Arm" title="Near 3 kpc Arm">Near 3 kpc Arm</a></li> <li><a href="/wiki/Far_3_kpc_Arm" title="Far 3 kpc Arm">Far 3 kpc Arm</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Galactic_halo" title="Galactic halo">Halo</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Aquarius_Stream" title="Aquarius Stream">Aquarius Stream</a></li> <li><a href="/wiki/Fimbulthul_stream" title="Fimbulthul stream">Fimbulthul stream</a></li> <li><a href="/wiki/Gaia_Sausage" title="Gaia Sausage">Gaia Sausage</a></li> <li><a href="/wiki/Helmi_stream" title="Helmi stream">Helmi stream</a></li> <li><a href="/wiki/Magellanic_Stream" title="Magellanic Stream">Magellanic Stream</a></li> <li><a href="/wiki/Monoceros_Ring" title="Monoceros Ring">Monoceros Ring</a></li> <li><a href="/wiki/Palomar_5" title="Palomar 5">Palomar 5</a> stream</li> <li><a href="/wiki/Pisces-Eridanus_stellar_stream" class="mw-redirect" title="Pisces-Eridanus stellar stream">Pisces-Eridanus stream</a></li> <li><a href="/wiki/Sagittarius_Stream" title="Sagittarius Stream">Sagittarius Stream</a></li> <li><a href="/wiki/Virgo_Stellar_Stream" title="Virgo Stellar Stream">Virgo Stream</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Satellite_galaxies_of_the_Milky_Way" title="Satellite galaxies of the Milky Way">Satellite galaxies</a></th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Magellanic_Clouds" title="Magellanic Clouds">Magellanic Clouds</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a></li> <li><a href="/wiki/Small_Magellanic_Cloud" title="Small Magellanic Cloud">Small Magellanic Cloud</a></li> <li><a href="/wiki/Magellanic_Bridge" title="Magellanic Bridge">Magellanic Bridge</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Dwarf_galaxy" title="Dwarf galaxy">Dwarfs</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Antlia_II" title="Antlia II">Antlia II</a></li> <li><a href="/wiki/Bo%C3%B6tes_I" title="Boötes I">Boötes I</a></li> <li><a href="/wiki/Bo%C3%B6tes_II" title="Boötes II">Boötes II</a></li> <li><a href="/wiki/Bo%C3%B6tes_III" title="Boötes III">Boötes III</a></li> <li><a href="/wiki/Canes_Venatici_I" title="Canes Venatici I">Canes Venatici I</a></li> <li><a href="/wiki/Canes_Venatici_II" title="Canes Venatici II">Canes Venatici II</a></li> <li><a href="/wiki/Canis_Major_Overdensity" title="Canis Major Overdensity">Canis Major</a></li> <li><a href="/wiki/Carina_Dwarf_Spheroidal_Galaxy" title="Carina Dwarf Spheroidal Galaxy">Carina</a></li> <li><a href="/wiki/Coma_Berenices_(dwarf_galaxy)" title="Coma Berenices (dwarf galaxy)">Coma Berenices</a></li> <li><a href="/wiki/Crater_2_Dwarf" title="Crater 2 Dwarf">Crater 2</a></li> <li><a href="/wiki/Draco_Dwarf" title="Draco Dwarf">Draco</a></li> <li><a href="/wiki/Eridanus_II" title="Eridanus II">Eridanus II</a></li> <li><a href="/wiki/Fornax_Dwarf" title="Fornax Dwarf">Fornax</a></li> <li><a href="/wiki/Hercules_(dwarf_galaxy)" title="Hercules (dwarf galaxy)">Hercules</a></li> <li><a href="/wiki/Leo_I_(dwarf_galaxy)" title="Leo I (dwarf galaxy)">Leo I</a></li> <li><a href="/wiki/Leo_II_(dwarf_galaxy)" title="Leo II (dwarf galaxy)">Leo II</a></li> <li><a href="/wiki/Leo_IV_(dwarf_galaxy)" title="Leo IV (dwarf galaxy)">Leo IV</a></li> <li><a href="/wiki/Leo_V_(dwarf_galaxy)" title="Leo V (dwarf galaxy)">Leo V</a></li> <li><a href="/wiki/Leo_T" title="Leo T">Leo T</a></li> <li><a href="/wiki/Phoenix_Dwarf" title="Phoenix Dwarf">Phoenix</a></li> <li><a href="/wiki/Pisces_Overdensity" title="Pisces Overdensity">Pisces Overdensity</a></li> <li><a href="/wiki/Pisces_II" title="Pisces II">Pisces II</a></li> <li><a href="/wiki/Reticulum_II" title="Reticulum II">Reticulum II</a></li> <li><a href="/wiki/Sagittarius_Dwarf_Spheroidal_Galaxy" title="Sagittarius Dwarf Spheroidal Galaxy">Sagittarius Spheroidal</a></li> <li><a href="/wiki/Segue_1" title="Segue 1">Segue 1</a></li> <li><a href="/wiki/Segue_2" title="Segue 2">Segue 2</a></li> <li><a href="/wiki/Sculptor_Dwarf_Galaxy" title="Sculptor Dwarf Galaxy">Sculptor</a></li> <li><a href="/wiki/Sextans_Dwarf_Spheroidal" title="Sextans Dwarf Spheroidal">Sextans</a></li> <li><a href="/wiki/Triangulum_II" title="Triangulum II">Triangulum II</a></li> <li><a href="/wiki/Ursa_Major_I_Dwarf" title="Ursa Major I Dwarf">Ursa Major I</a></li> <li><a href="/wiki/Ursa_Major_II_Dwarf" title="Ursa Major II Dwarf">Ursa Major II</a></li> <li><a href="/wiki/Ursa_Major_III" title="Ursa Major III">Ursa Major III</a></li> <li><a href="/wiki/Ursa_Minor_Dwarf" title="Ursa Minor Dwarf">Ursa Minor</a></li> <li><a href="/wiki/Virgo_I" title="Virgo I">Virgo I</a></li> <li><a href="/wiki/Willman_1" title="Willman 1">Willman 1</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/List_of_names_for_the_Milky_Way" class="mw-redirect" title="List of names for the Milky Way">Alternate names</a></li> <li><a href="/wiki/Andromeda%E2%80%93Milky_Way_collision" title="Andromeda–Milky Way collision">Andromeda–Milky Way collision</a></li> <li><a href="/wiki/Baade%27s_Window" title="Baade's Window">Baade's Window</a></li> <li><a href="/wiki/Milky_Way_(mythology)" title="Milky Way (mythology)">In mythology</a></li> <li><a href="/wiki/Zone_of_Avoidance" title="Zone of Avoidance">Zone of Avoidance</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow hlist" colspan="3"><div> <ul><li><a href="/wiki/File:Symbol_portal_class.svg" class="mw-file-description" title="Portal"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/16px-Symbol_portal_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/23px-Symbol_portal_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/31px-Symbol_portal_class.svg.png 2x" data-file-width="180" data-file-height="185" /></a> <a href="/wiki/Portal:Astronomy" title="Portal:Astronomy">Astronomy portal</a></li> <li><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /> <a href="/wiki/Category:Milky_Way" title="Category:Milky Way">Category</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="Location_of_Earth" style="padding:3px"><table class="nowraplinks hlist mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="2"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Earth%27s_location" title="Template:Earth's location"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Earth%27s_location" title="Template talk:Earth's location"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Earth%27s_location" title="Special:EditPage/Template:Earth's location"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Location_of_Earth" style="font-size:114%;margin:0 4em"><a href="/wiki/Location_of_Earth" title="Location of Earth">Location of Earth</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Included</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"><a href="/wiki/Earth" title="Earth">Earth</a> → <a href="/wiki/Solar_System" title="Solar System">Solar System</a> → <a href="/wiki/Local_Interstellar_Cloud" title="Local Interstellar Cloud">Local Interstellar Cloud</a> → <a href="/wiki/Local_Bubble" title="Local Bubble">Local Bubble</a> → <a href="/wiki/Gould_Belt" title="Gould Belt">Gould Belt</a> → <a href="/wiki/Orion_Arm" title="Orion Arm">Orion Arm</a> → <a class="mw-selflink selflink">Milky Way</a> → <a href="/wiki/Satellite_galaxies_of_the_Milky_Way" title="Satellite galaxies of the Milky Way">Milky Way subgroup</a> → <a href="/wiki/Local_Group" title="Local Group">Local Group</a> → <a href="/wiki/Local_Sheet" title="Local Sheet">Local Sheet</a> → <a href="/wiki/Virgo_Supercluster" title="Virgo Supercluster">Virgo Supercluster</a> → <a href="/wiki/Laniakea_Supercluster" title="Laniakea Supercluster">Laniakea Supercluster</a> → <a href="/wiki/Local_Hole" title="Local Hole">Local Hole</a> → <a href="/wiki/Observable_universe" title="Observable universe">Observable universe</a> → <a href="/wiki/Universe" title="Universe">Universe</a> Each arrow (→) may be read as "within" or "part of".</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Cosmic_View" title="Cosmic View">Cosmic View (1957 book)</a></li> <li><a href="/wiki/To_the_Moon_and_Beyond" title="To the Moon and Beyond">To the Moon and Beyond (1964 film)</a></li> <li><a href="/wiki/Cosmic_Zoom" title="Cosmic Zoom">Cosmic Zoom (1968 film)</a></li> <li><a href="/wiki/Powers_of_Ten_(film)" title="Powers of Ten (film)">Powers of Ten (1968 and 1977 films)</a></li> <li><a href="/wiki/Cosmic_Voyage_(1996_film)" title="Cosmic Voyage (1996 film)">Cosmic Voyage (1996 documentary)</a></li> <li><a href="/wiki/Cosmic_Eye" title="Cosmic Eye">Cosmic Eye (2012)</a></li> <li><a href="/wiki/History_of_the_center_of_the_Universe" title="History of the center of the Universe">History of the center of the Universe</a></li> <li><a href="/wiki/Order_of_magnitude" title="Order of magnitude">Order of magnitude</a></li> <li><a href="/wiki/Pisces%E2%80%93Cetus_Supercluster_Complex" title="Pisces–Cetus Supercluster Complex">Pisces–Cetus Supercluster Complex</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><a href="/wiki/File:Symbol_portal_class.svg" class="mw-file-description" title="Portal"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/16px-Symbol_portal_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/23px-Symbol_portal_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/31px-Symbol_portal_class.svg.png 2x" data-file-width="180" data-file-height="185" /></a> <a href="/wiki/Portal:Astronomy" title="Portal:Astronomy">Astronomy portal</a></li> <li><a href="/wiki/File:Symbol_portal_class.svg" class="mw-file-description" title="Portal"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/16px-Symbol_portal_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/23px-Symbol_portal_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/31px-Symbol_portal_class.svg.png 2x" data-file-width="180" data-file-height="185" /></a> <a href="/wiki/Portal:Space" class="mw-redirect" title="Portal:Space">Space portal</a></li></ul> </div></td></tr></tbody></table></div> <style data-mw-deduplicate="TemplateStyles:r1130092004">.mw-parser-output .portal-bar{font-size:88%;font-weight:bold;display:flex;justify-content:center;align-items:baseline}.mw-parser-output .portal-bar-bordered{padding:0 2em;background-color:#fdfdfd;border:1px solid #a2a9b1;clear:both;margin:1em auto 0}.mw-parser-output .portal-bar-related{font-size:100%;justify-content:flex-start}.mw-parser-output .portal-bar-unbordered{padding:0 1.7em;margin-left:0}.mw-parser-output .portal-bar-header{margin:0 1em 0 0.5em;flex:0 0 auto;min-height:24px}.mw-parser-output .portal-bar-content{display:flex;flex-flow:row wrap;flex:0 1 auto;padding:0.15em 0;column-gap:1em;align-items:baseline;margin:0;list-style:none}.mw-parser-output .portal-bar-content-related{margin:0;list-style:none}.mw-parser-output .portal-bar-item{display:inline-block;margin:0.15em 0.2em;min-height:24px;line-height:24px}@media screen and (max-width:768px){.mw-parser-output .portal-bar{font-size:88%;font-weight:bold;display:flex;flex-flow:column wrap;align-items:baseline}.mw-parser-output .portal-bar-header{text-align:center;flex:0;padding-left:0.5em;margin:0 auto}.mw-parser-output .portal-bar-related{font-size:100%;align-items:flex-start}.mw-parser-output .portal-bar-content{display:flex;flex-flow:row wrap;align-items:center;flex:0;column-gap:1em;border-top:1px solid #a2a9b1;margin:0 auto;list-style:none}.mw-parser-output .portal-bar-content-related{border-top:none;margin:0;list-style:none}}.mw-parser-output .navbox+link+.portal-bar,.mw-parser-output .navbox+style+.portal-bar,.mw-parser-output .navbox+link+.portal-bar-bordered,.mw-parser-output .navbox+style+.portal-bar-bordered,.mw-parser-output .sister-bar+link+.portal-bar,.mw-parser-output .sister-bar+style+.portal-bar,.mw-parser-output .portal-bar+.navbox-styles+.navbox,.mw-parser-output .portal-bar+.navbox-styles+.sister-bar{margin-top:-1px}</style><div class="portal-bar noprint metadata noviewer portal-bar-bordered" role="navigation" aria-label="Portals"><a href="/wiki/Wikipedia:Contents/Portals" title="Wikipedia:Contents/Portals">Portals</a>:<ul class="portal-bar-content"><li class="portal-bar-item"><a href="/wiki/File:He1523a.jpg" class="mw-file-description"><img alt="icon" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/16px-He1523a.jpg" decoding="async" width="16" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/25px-He1523a.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/33px-He1523a.jpg 2x" data-file-width="180" data-file-height="207" /></a> <a href="/wiki/Portal:Star" class="mw-redirect" title="Portal:Star">Star</a></li><li class="portal-bar-item"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Solar_system.jpg/15px-Solar_system.jpg" decoding="async" width="15" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Solar_system.jpg/23px-Solar_system.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/83/Solar_system.jpg/30px-Solar_system.jpg 2x" data-file-width="4500" data-file-height="5600" /> <a href="/wiki/Portal:Solar_System" title="Portal:Solar System">Solar System</a></li><li class="portal-bar-item"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/RocketSunIcon.svg/19px-RocketSunIcon.svg.png" decoding="async" width="19" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/RocketSunIcon.svg/29px-RocketSunIcon.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/d/d6/RocketSunIcon.svg/38px-RocketSunIcon.svg.png 2x" data-file-width="128" data-file-height="128" /> <a href="/wiki/Portal:Spaceflight" title="Portal:Spaceflight">Spaceflight</a></li><li class="portal-bar-item"><a 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srcset="//upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Stylised_atom_with_three_Bohr_model_orbits_and_stylised_nucleus.svg/26px-Stylised_atom_with_three_Bohr_model_orbits_and_stylised_nucleus.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Stylised_atom_with_three_Bohr_model_orbits_and_stylised_nucleus.svg/34px-Stylised_atom_with_three_Bohr_model_orbits_and_stylised_nucleus.svg.png 2x" data-file-width="530" data-file-height="600" /></a> <a href="/wiki/Portal:Physics" title="Portal:Physics">Physics</a></li><li class="portal-bar-item"><a href="/wiki/File:Noun-technology.svg" class="mw-file-description"><img alt="icon" src="//upload.wikimedia.org/wikipedia/commons/thumb/a/a9/Noun-technology.svg/19px-Noun-technology.svg.png" decoding="async" width="19" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/a/a9/Noun-technology.svg/30px-Noun-technology.svg.png 1.5x, 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/></a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">International</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"><ul><li><a rel="nofollow" class="external text" href="https://viaf.org/viaf/170343872">VIAF</a></li><li><a rel="nofollow" class="external text" href="http://id.worldcat.org/fast/1240104/">FAST</a></li></ul></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">National</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"><ul><li><a rel="nofollow" class="external text" href="https://d-nb.info/gnd/4169926-9">Germany</a></li><li><a rel="nofollow" class="external text" href="https://id.loc.gov/authorities/sh85085376">United States</a></li><li><a rel="nofollow" class="external text" href="https://catalogue.bnf.fr/ark:/12148/cb11978895z">France</a></li><li><a rel="nofollow" class="external 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