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mw-first-heading"><span class="mw-page-title-main">HD 5980</span></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. 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Spanish" lang="es" hreflang="es" data-title="HD 5980" data-language-autonym="Español" data-language-local-name="Spanish" class="interlanguage-link-target"><span>Español</span></a></li><li class="interlanguage-link interwiki-fa mw-list-item"><a href="https://fa.wikipedia.org/wiki/%D8%A7%DA%86%E2%80%8C%D8%AF%DB%8C_%DB%B5%DB%B9%DB%B8%DB%B0" title="اچ‌دی ۵۹۸۰ – Persian" lang="fa" hreflang="fa" data-title="اچ‌دی ۵۹۸۰" data-language-autonym="فارسی" data-language-local-name="Persian" class="interlanguage-link-target"><span>فارسی</span></a></li><li class="interlanguage-link interwiki-it mw-list-item"><a href="https://it.wikipedia.org/wiki/HD_5980" title="HD 5980 – Italian" lang="it" hreflang="it" data-title="HD 5980" data-language-autonym="Italiano" data-language-local-name="Italian" class="interlanguage-link-target"><span>Italiano</span></a></li><li class="interlanguage-link interwiki-hu mw-list-item"><a href="https://hu.wikipedia.org/wiki/HD_5980" title="HD 5980 – Hungarian" lang="hu" hreflang="hu" data-title="HD 5980" data-language-autonym="Magyar" data-language-local-name="Hungarian" class="interlanguage-link-target"><span>Magyar</span></a></li><li class="interlanguage-link interwiki-ja mw-list-item"><a href="https://ja.wikipedia.org/wiki/HD_5980" title="HD 5980 – Japanese" lang="ja" hreflang="ja" data-title="HD 5980" data-language-autonym="日本語" data-language-local-name="Japanese" class="interlanguage-link-target"><span>日本語</span></a></li><li class="interlanguage-link interwiki-ru mw-list-item"><a href="https://ru.wikipedia.org/wiki/HD_5980" title="HD 5980 – Russian" lang="ru" hreflang="ru" data-title="HD 5980" data-language-autonym="Русский" data-language-local-name="Russian" class="interlanguage-link-target"><span>Русский</span></a></li><li class="interlanguage-link interwiki-sv mw-list-item"><a href="https://sv.wikipedia.org/wiki/HD_5980" title="HD 5980 – Swedish" lang="sv" hreflang="sv" data-title="HD 5980" data-language-autonym="Svenska" 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bold">HD 5980 </caption><tbody><tr><td colspan="2" style="text-align:center;"><div style="text-align: center; margin-left:auto; margin-right:auto"><span typeof="mw:File"><a href="/wiki/File:Hd-5980-chadra.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/2/22/Hd-5980-chadra.jpg/280px-Hd-5980-chadra.jpg" decoding="async" width="280" height="280" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/2/22/Hd-5980-chadra.jpg 1.5x" data-file-width="350" data-file-height="350" /></a></span><br />X-ray image by <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra Observatory</a></div></td></tr> <tr> <th style="text-align: center; background-color: #FFFFC0;" colspan="2">Observation data<br /><a href="/wiki/Epoch_(astronomy)" title="Epoch (astronomy)">Epoch</a> J2000      <a href="/wiki/Equinox_(celestial_coordinates)" title="Equinox (celestial coordinates)">Equinox</a> J2000 </th></tr> <tr style="vertical-align:top"> <th style="text-align:left"><a href="/wiki/Constellation" title="Constellation">Constellation</a> </th> <td><a href="/wiki/Tucana" title="Tucana">Tucana</a> </td></tr> <tr style="vertical-align:top"> <th style="text-align:left"><span class="nowrap"><a href="/wiki/Right_ascension" title="Right ascension">Right ascension</a></span> </th> <td><span class="nowrap">00<sup>h</sup> 59<sup>m</sup> 26.569<sup>s</sup></span><sup id="cite_ref-tycho_1-0" class="reference"><a href="#cite_note-tycho-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> </td></tr> <tr style="vertical-align:top"> <th style="text-align:left"><a href="/wiki/Declination" title="Declination">Declination</a> </th> <td>−72° 09′ 53.91″<sup id="cite_ref-tycho_1-1" class="reference"><a href="#cite_note-tycho-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> </td></tr> <tr style="vertical-align:top"> <th style="text-align:left"><span class="nowrap"><a href="/wiki/Apparent_magnitude" title="Apparent magnitude">Apparent magnitude</a> (V)</span> </th> <td>8.8 - 11.9<sup id="cite_ref-vsx_2-0" class="reference"><a href="#cite_note-vsx-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> </td></tr> <tr> <th style="background-color: #FFFFC0; text-align: center;" colspan="2">Characteristics </th></tr> <tr style="vertical-align:top"> <th style="text-align:left"><a href="/wiki/Stellar_classification" title="Stellar classification">Spectral type</a> </th> <td>LBV + WN4 + OI<sup id="cite_ref-foellmi_3-0" class="reference"><a href="#cite_note-foellmi-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> </td></tr> <tr style="vertical-align:top"> <th style="text-align:left">U−B <a href="/wiki/Color_index" title="Color index">color index</a> </th> <td>−0.99<sup id="cite_ref-arp_4-0" class="reference"><a href="#cite_note-arp-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> </td></tr> <tr style="vertical-align:top"> <th style="text-align:left">B−V <a href="/wiki/Color_index" title="Color index">color index</a> </th> <td>−0.18<sup id="cite_ref-tycho2_5-0" class="reference"><a href="#cite_note-tycho2-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> </td></tr> <tr style="vertical-align:top"> <th style="text-align:left"><a href="/wiki/Variable_star" title="Variable star">Variable type</a> </th> <td><a href="/wiki/Luminous_blue_variable" title="Luminous blue variable">LBV</a><sup id="cite_ref-triple_6-0" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> and <a href="/wiki/Algol_variable" title="Algol variable">EA</a><sup id="cite_ref-foellmi_3-1" class="reference"><a href="#cite_note-foellmi-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> </td></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2"><a href="/wiki/Astrometry" title="Astrometry">Astrometry</a></th></tr><tr><th colspan="2" style="text-align: center"></th></tr><tr style="vertical-align:top;"><td><b><a href="/wiki/Radial_velocity" title="Radial velocity">Radial velocity</a> (R<sub>v</sub>)</b></td><td>−20<sup id="cite_ref-koenigsberger_7-0" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> km/s</td></tr><tr style="vertical-align:top;"><td><b><a href="/wiki/Proper_motion" title="Proper motion">Proper motion</a> (μ)</b></td><td> <abbr title="Right Ascension">RA:</abbr> −3.5<sup id="cite_ref-tycho_1-2" class="reference"><a href="#cite_note-tycho-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Milliarcsecond" class="mw-redirect" title="Milliarcsecond">mas</a>/<a href="/wiki/Year" title="Year">yr</a> <br /> <abbr title="Declination">Dec.:</abbr> −2.4<sup id="cite_ref-tycho_1-3" class="reference"><a href="#cite_note-tycho-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Milliarcsecond" class="mw-redirect" title="Milliarcsecond">mas</a>/<a href="/wiki/Year" title="Year">yr</a> </td></tr><tr style="vertical-align:top;"><td><b><a href="/wiki/Distance_(astronomy)" class="mw-redirect" title="Distance (astronomy)">Distance</a></b></td><td>200,000 <a href="/wiki/Light-year" title="Light-year">ly</a> <br />(64,000<sup id="cite_ref-triple_6-1" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Parsec" title="Parsec">pc</a>)</td></tr><tr style="vertical-align:top;"><td><b><a href="/wiki/Absolute_magnitude" title="Absolute magnitude">Absolute magnitude</a> (M<sub>V</sub>)</b></td><td>−8.1 <span class="nowrap">(−7.1/−6.8/−6.7)</span><sup id="cite_ref-shenar_8-0" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup></td></tr><tr><th colspan="2" style="text-align: center"></th></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2"><a href="/wiki/Orbit" title="Orbit">Orbit</a><sup id="cite_ref-koenigsberger_7-1" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup></th></tr><tr style="vertical-align:baseline;"><td><b>Primary</b></td><td>HD 5980 A</td></tr><tr style="vertical-align:baseline;"><td><b>Companion</b></td><td>HD 5980 B</td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Orbital_period" title="Orbital period">Period</a> (P)</b></td><td><span class="nowrap"><span data-sort-value="7006166454784000000♠"></span>19.2656<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.0009 d</span></td></tr><tr style="vertical-align:baseline;"><td><span class="nowrap"><b><a href="/wiki/Semi-major_axis" class="mw-redirect" title="Semi-major axis">Semi-major axis</a> (a)</b></span></td><td><span class="nowrap"><span data-sort-value="7011105050700000000♠"></span>151<span style="margin-left:0.3em;margin-right:0.15em;">±</span>4 <a href="/wiki/Solar_radius" title="Solar radius"><i>R</i><sub>☉</sub></a></span></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Eccentricity_(orbit)" class="mw-redirect" title="Eccentricity (orbit)">Eccentricity</a> (e)</b></td><td><span class="nowrap"><span data-sort-value="6999270000000000000♠"></span>0.27<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.02</span></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Inclination" class="mw-redirect" title="Inclination">Inclination</a> (i)</b></td><td>86°</td></tr><tr style="vertical-align:baseline;"><td><span class="nowrap"><b><a href="/wiki/Periastron" class="mw-redirect" title="Periastron">Periastron</a> <a href="/wiki/Epoch_(astronomy)" title="Epoch (astronomy)">epoch</a> (T)</b></span></td><td><span class="nowrap"><span data-sort-value="7006245142497000000♠"></span>2,451,424.97<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.25</span></td></tr><tr style="vertical-align:baseline;"><td><span class="nowrap"><b><a href="/wiki/Argument_of_periastron" class="mw-redirect" title="Argument of periastron">Argument of periastron</a> (ω)</b></span><br />(primary)</td><td><span class="nowrap"><span data-sort-value="7002134000000000000♠"></span>134<span style="margin-left:0.3em;margin-right:0.15em;">±</span>4</span>°</td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Semi-amplitude" class="mw-redirect" title="Semi-amplitude">Semi-amplitude</a></b> (K<sub>1</sub>)<br />(primary)</td><td><span class="nowrap"><span data-sort-value="7002214000000000000♠"></span>214<span style="margin-left:0.3em;margin-right:0.15em;">±</span>6</span> km/s</td></tr><tr style="vertical-align:baseline;"><td><b>Semi-amplitude</b> (K<sub>2</sub>)<br />(secondary)</td><td><span class="nowrap"><span data-sort-value="7002200000000000000♠"></span>200<span style="margin-left:0.3em;margin-right:0.15em;">±</span>6</span> km/s</td></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2"><a href="/wiki/Orbit" title="Orbit">Orbit</a><sup id="cite_ref-koenigsberger_7-2" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup></th></tr><tr style="vertical-align:baseline;"><td><b>Primary</b></td><td>HD 5980 C</td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Orbital_period" title="Orbital period">Period</a> (P)</b></td><td><span class="nowrap"><span data-sort-value="7006834278400000000♠"></span>96.56<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.01 d</span></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Eccentricity_(orbit)" class="mw-redirect" title="Eccentricity (orbit)">Eccentricity</a> (e)</b></td><td>0.815</td></tr><tr style="vertical-align:baseline;"><td><span class="nowrap"><b><a href="/wiki/Periastron" class="mw-redirect" title="Periastron">Periastron</a> <a href="/wiki/Epoch_(astronomy)" title="Epoch (astronomy)">epoch</a> (T)</b></span></td><td><span class="nowrap"><span data-sort-value="7006245118340000000♠"></span>2<span style="margin-left:.25em;">451</span><span style="margin-left:.25em;">183</span>.40<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.22</span></td></tr><tr style="vertical-align:baseline;"><td><span class="nowrap"><b><a href="/wiki/Argument_of_periastron" class="mw-redirect" title="Argument of periastron">Argument of periastron</a> (ω)</b></span><br />(primary)</td><td><span class="nowrap"><span data-sort-value="7002252000000000000♠"></span>252<span style="margin-left:0.3em;margin-right:0.15em;">±</span>3.3</span><sup id="cite_ref-koenigsberger_7-3" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup>°</td></tr><tr style="vertical-align:baseline;"><td><b>Semi-amplitude</b> (K<sub>2</sub>)<br />(secondary)</td><td><span class="nowrap"><span data-sort-value="7001810000000000000♠"></span>81<span style="margin-left:0.3em;margin-right:0.15em;">±</span>4</span> km/s</td></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2">Details</th></tr><tr><th colspan="2" style="text-align: center">A</th></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Stellar_mass" title="Stellar mass">Mass</a></b></td><td>61<sup id="cite_ref-shenar_8-1" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Solar_mass" title="Solar mass"><var>M</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Radius" title="Radius">Radius</a></b></td><td>24<sup id="cite_ref-shenar_8-2" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> (21<sup id="cite_ref-foellmi_3-2" class="reference"><a href="#cite_note-foellmi-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> – 280<sup id="cite_ref-drissen_9-0" class="reference"><a href="#cite_note-drissen-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup>) <a href="/wiki/Solar_radius" title="Solar radius"><var>R</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Luminosity" title="Luminosity">Luminosity</a></b></td><td>2,200,000<sup id="cite_ref-shenar_8-3" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> (2,000,000<sup id="cite_ref-pasemann_10-0" class="reference"><a href="#cite_note-pasemann-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup> – 10,000,000<sup id="cite_ref-drissen_9-1" class="reference"><a href="#cite_note-drissen-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup>) <a href="/wiki/Solar_luminosity" title="Solar luminosity"><var>L</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Effective_temperature" title="Effective temperature">Temperature</a></b></td><td>45,000<sup id="cite_ref-shenar_8-4" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <span class="nowrap">(21,000 – 53,000<sup id="cite_ref-foellmi_3-3" class="reference"><a href="#cite_note-foellmi-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup>)</span> <a href="/wiki/Kelvin" title="Kelvin">K</a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Metallicity" title="Metallicity">Metallicity</a></b> [Fe/H]</td><td>−1.0<sup id="cite_ref-triple_6-2" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Decimal_exponent" class="mw-redirect" title="Decimal exponent">dex</a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Projected_rotational_velocity" class="mw-redirect" title="Projected rotational velocity">Rotational velocity</a> (<i>v</i> sin <i>i</i>)</b></td><td>250<sup id="cite_ref-gloria_11-0" class="reference"><a href="#cite_note-gloria-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> km/s</td></tr><tr><th colspan="2" style="text-align: center">B</th></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Stellar_mass" title="Stellar mass">Mass</a></b></td><td>66<sup id="cite_ref-shenar_8-5" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Solar_mass" title="Solar mass"><var>M</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Radius" title="Radius">Radius</a></b></td><td>22<sup id="cite_ref-shenar_8-6" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Solar_radius" title="Solar radius"><var>R</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b>Luminosity</b></td><td>1,800,000<sup id="cite_ref-shenar_8-7" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Solar_luminosity" title="Solar luminosity"><var>L</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Effective_temperature" title="Effective temperature">Temperature</a></b></td><td>45,000<sup id="cite_ref-shenar_8-8" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Kelvin" title="Kelvin">K</a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Metallicity" title="Metallicity">Metallicity</a></b> [Fe/H]</td><td>−1.0<sup id="cite_ref-triple_6-3" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Decimal_exponent" class="mw-redirect" title="Decimal exponent">dex</a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Projected_rotational_velocity" class="mw-redirect" title="Projected rotational velocity">Rotational velocity</a> (<i>v</i> sin <i>i</i>)</b></td><td><400<sup id="cite_ref-shenar_8-9" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> km/s</td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Star#Age_and_size_of_stars" title="Star">Age</a></b></td><td>2.6<sup id="cite_ref-shenar_8-10" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Megayear" class="mw-redirect" title="Megayear">Myr</a></td></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2"></th></tr><tr><th colspan="2" style="text-align: center">C</th></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Stellar_mass" title="Stellar mass">Mass</a></b></td><td>34<sup id="cite_ref-shenar_8-11" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Solar_mass" title="Solar mass"><var>M</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Radius" title="Radius">Radius</a></b></td><td>24<sup id="cite_ref-shenar_8-12" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Solar_radius" title="Solar radius"><var>R</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Luminosity" title="Luminosity">Luminosity</a></b></td><td>708,000<sup id="cite_ref-shenar_8-13" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Solar_luminosity" title="Solar luminosity"><var>L</var><sub>☉</sub></a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Effective_temperature" title="Effective temperature">Temperature</a></b></td><td>34,000<sup id="cite_ref-shenar_8-14" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Kelvin" title="Kelvin">K</a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Metallicity" title="Metallicity">Metallicity</a></b> [Fe/H]</td><td>≅ −0.7<sup id="cite_ref-triple_6-4" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Decimal_exponent" class="mw-redirect" title="Decimal exponent">dex</a></td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Projected_rotational_velocity" class="mw-redirect" title="Projected rotational velocity">Rotational velocity</a> (<i>v</i> sin <i>i</i>)</b></td><td>120<sup id="cite_ref-shenar_8-15" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> km/s</td></tr><tr style="vertical-align:baseline;"><td><b><a href="/wiki/Stellar_evolution" title="Stellar evolution">Age</a></b></td><td>3.1<sup id="cite_ref-koenigsberger_7-4" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> <a href="/wiki/Megayear" class="mw-redirect" title="Megayear">Myr</a></td></tr><tr><th colspan="2" style="text-align: center"></th></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2"><a href="/wiki/Star_catalogue" title="Star catalogue">Other designations</a></th></tr><tr><td colspan="2"><div style="width: 250px;"> <a href="/wiki/Henry_Draper_catalogue" class="mw-redirect" title="Henry Draper catalogue">HD</a> 5980, <a href="/wiki/Radcliffe_Observatory" title="Radcliffe Observatory">RMC</a> 14, <a href="/wiki/Nicholas_Sanduleak" title="Nicholas Sanduleak">Sk</a> 78, <a href="/wiki/AB_(star_catalogue)" class="mw-redirect" title="AB (star catalogue)">AB</a> 5, SMC WR5, <a href="/wiki/American_Association_of_Variable_Star_Observers" title="American Association of Variable Star Observers">AAVSO</a> 0056-72 </div></td></tr> <tr><th style="background-color: #FFFFC0; text-align: center;" colspan="2">Database references</th></tr><tr style="vertical-align: top;"><td><b><a href="/wiki/SIMBAD" title="SIMBAD">SIMBAD</a></b></td><td><a rel="nofollow" class="external text" href="https://simbad.cds.unistra.fr/simbad/sim-id?Ident=HD+5980">data</a></td></tr> </tbody></table> <p><b>HD 5980</b> is a <a href="/wiki/Multiple_star_system" class="mw-redirect" title="Multiple star system">multiple star system</a> on the outskirts of <a href="/wiki/NGC_346" title="NGC 346">NGC 346</a> in the <a href="/wiki/Small_Magellanic_Cloud" title="Small Magellanic Cloud">Small Magellanic Cloud</a> (SMC)<sup id="cite_ref-Nazé2002_12-0" class="reference"><a href="#cite_note-Nazé2002-12"><span class="cite-bracket">[</span>12<span class="cite-bracket">]</span></a></sup> and is one of the brightest stars in the SMC. </p><p>HD 5980 has at least three components among the <a href="/wiki/List_of_most_luminous_stars" title="List of most luminous stars">most luminous stars known</a>: the unusual primary has a <a href="/wiki/Wolf%E2%80%93Rayet_star" title="Wolf–Rayet star">Wolf–Rayet</a> spectrum and has produced a <a href="/wiki/Luminous_blue_variable" title="Luminous blue variable">luminous blue variable</a> (LBV) outburst; the secondary, also a Wolf–Rayet star, forms an eclipsing <a href="/wiki/Spectroscopic_binary" class="mw-redirect" title="Spectroscopic binary">spectroscopic binary</a> with the primary star; and a more distant <a href="/wiki/O-type_star" title="O-type star">O-type</a> <a href="/wiki/Supergiant" title="Supergiant">supergiant</a> is also likely to be a binary. </p> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Discovery">Discovery</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=HD_5980&action=edit&section=1" title="Edit section: Discovery"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:HD5980LightCurve.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/0/05/HD5980LightCurve.png/220px-HD5980LightCurve.png" decoding="async" width="220" height="143" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/05/HD5980LightCurve.png/330px-HD5980LightCurve.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/05/HD5980LightCurve.png/440px-HD5980LightCurve.png 2x" data-file-width="1500" data-file-height="975" /></a><figcaption>A <a href="/wiki/Photometric_system#Photometric_letters" title="Photometric system">visual band</a> <a href="/wiki/Light_curve" title="Light curve">light curve</a> for HD 5980, adapted from Perrier <i>et al.</i> (2009)<sup id="cite_ref-Perrier_13-0" class="reference"><a href="#cite_note-Perrier-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup></figcaption></figure> <p>HD 5980 was first recorded in 1901 as the first object in a list of southern sky objects having peculiar spectra. It was described as "Type V", referring to the <a href="/wiki/Stellar_classification#Secchi_classes" title="Stellar classification">Secchi class</a> for stars with emission lines.<sup id="cite_ref-pickering_14-0" class="reference"><a href="#cite_note-pickering-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup> </p><p>It was formally named HD 5980 in the first <a href="/wiki/Henry_Draper_Catalogue" title="Henry Draper Catalogue">Henry Draper Catalogue</a> where it was given the spectral type of Oa indicating strong emission bands.<sup id="cite_ref-hd_15-0" class="reference"><a href="#cite_note-hd-15"><span class="cite-bracket">[</span>15<span class="cite-bracket">]</span></a></sup> The spectral type was later refined to Wa when the emission line "O" stars were recognised as a separate class.<sup id="cite_ref-payne_16-0" class="reference"><a href="#cite_note-payne-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup> </p><p>Later observations detected spectral and brightness variations<sup id="cite_ref-feast_17-0" class="reference"><a href="#cite_note-feast-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup>and eclipses,<sup id="cite_ref-hoffman_18-0" class="reference"><a href="#cite_note-hoffman-18"><span class="cite-bracket">[</span>18<span class="cite-bracket">]</span></a></sup> but it was thought to be a simple WR/OB binary. Absorption lines in the spectrum that did not move during the binary orbit eventually led to the conclusion that HD 5980 was a triple system with a close eclipsing binary and a more distant class O supergiant.<sup id="cite_ref-niemela_19-0" class="reference"><a href="#cite_note-niemela-19"><span class="cite-bracket">[</span>19<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-Koenigsberger_20-0" class="reference"><a href="#cite_note-Koenigsberger-20"><span class="cite-bracket">[</span>20<span class="cite-bracket">]</span></a></sup> </p><p>In 1993, the spectrum began to change and the brightness increased, beginning a dramatic change that has been interpreted as a unique type of LBV eruption.<sup id="cite_ref-gloria_11-1" class="reference"><a href="#cite_note-gloria-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> Since then the star has been intensively observed and modelled.<sup id="cite_ref-triple_6-5" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Components">Components</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=HD_5980&action=edit&section=2" title="Edit section: Components"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:NGC_346_in_Small_magellanic_cloud.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/NGC_346_in_Small_magellanic_cloud.jpg/260px-NGC_346_in_Small_magellanic_cloud.jpg" decoding="async" width="260" height="277" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/NGC_346_in_Small_magellanic_cloud.jpg/390px-NGC_346_in_Small_magellanic_cloud.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4c/NGC_346_in_Small_magellanic_cloud.jpg/520px-NGC_346_in_Small_magellanic_cloud.jpg 2x" data-file-width="6555" data-file-height="6995" /></a><figcaption><a href="/wiki/NGC_346" title="NGC 346">NGC 346</a>. HD 5980 is the brightest star on the left, just above centre.</figcaption></figure> <p>HD 5980 is visually a single star, but the spectrum reveals three hot <a href="/wiki/Luminosity" title="Luminosity">luminous</a> components. The physical parameters of the three stars are uncertain because of the difficulties of resolving their spectra, the partial <a href="/wiki/Eclipses" class="mw-redirect" title="Eclipses">eclipses</a>, apparent intrinsic variations with the orbital phase, and the strong variability of at least one component. The calibration of spectral features to physical characters such as temperature has historically been complicated by the low <a href="/wiki/Metallicity" title="Metallicity">metallicity</a> of objects in the SMC.<sup id="cite_ref-triple_6-6" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> </p><p>The primary star, <i>HD 5980 A</i>, is visually the brightest component of the three. It was apparently a hydrogen-poor <a href="/wiki/Wolf%E2%80%93Rayet_star#Classification" title="Wolf–Rayet star">WN3</a>-type until about 1990, but then underwent an LBV-type outburst that saw its radius increase ten-fold and its temperature drop dramatically so that it appeared as a B hypergiant with prominent hydrogen spectral lines. Since then it has returned to near its original brightness and temperature. The emission line spectrum is produced in the dense <a href="/wiki/Stellar_wind" title="Stellar wind">stellar wind</a> and little is known about the underlying <a href="/wiki/Photosphere" title="Photosphere">photosphere</a>.<sup id="cite_ref-koenigsberger_7-5" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> </p><p>The secondary, <i>HD 5980 B</i>, is also a Wolf–Rayet star. It forms a spectroscopic double with the primary A and they orbit each other every 19.3 days. The orbital parameters indicate that the two stars are approximately equally massive, within the margin of error. The orbit is inclined at 86° to us, and partial eclipses occur twice per orbit, with timings that indicate an <a href="/wiki/Orbital_eccentricity" title="Orbital eccentricity">eccentricity</a> of 0.27. The eclipses only produce a 0.2 magnitude change in the total system brightness, but the shape of the light curve and line profile changes during the eclipses allow both a stellar core and a dense wind region about twice the width of the star to be identified.<sup id="cite_ref-foellmi_3-4" class="reference"><a href="#cite_note-foellmi-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> HD 5980 B is generally classified as WN4. The spectrum can only be distinguished from HD 5980 A on the basis of variations in the profile of some broad emission lines during the orbit. Some hydrogen lines are seen in emission but generally combined with or hidden by other broad emission. Narrow hydrogen absorption lines are not generally considered to originate from this component and do not show the same radial velocity variations.<sup id="cite_ref-triple_6-7" class="reference"><a href="#cite_note-triple-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> </p><p>Component C is a distant hydrogen-rich star identified from narrow absorption lines which do not show the same strong radial velocity variations as the broad emission lines from the A/B pair. Higher resolution spectra show smaller slower radial velocity variations and it is assumed that C itself also has a companion. The primary is a hot conventional star, most likely an early O-type supergiant. A period of 96.5 days has been derived from the radial velocity variations. This is five times the period of the A/B system, suggesting the four stars form a gravitational trapezium system although it cannot be ruled out that it is an unrelated chance alignment.<sup id="cite_ref-koenigsberger_7-6" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> </p><p>Pulsations and brightness variations have been interpreted as those of a <a href="/wiki/Heartbeat_star" title="Heartbeat star">heartbeat star</a>, probably the A/B pair. This would be the most massive such system. It is also possible that the C/D pair also develops heartbeat pulsations during <a href="/wiki/Periastron" class="mw-redirect" title="Periastron">periastron</a>.<sup id="cite_ref-ks2021_21-0" class="reference"><a href="#cite_note-ks2021-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Luminous_blue_variable">Luminous blue variable</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=HD_5980&action=edit&section=3" title="Edit section: Luminous blue variable"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:Lbvstar.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/9a/Lbvstar.png/330px-Lbvstar.png" decoding="async" width="330" height="202" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/9a/Lbvstar.png/495px-Lbvstar.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/9a/Lbvstar.png/660px-Lbvstar.png 2x" data-file-width="1669" data-file-height="1024" /></a><figcaption>H-R Diagram showing the location of HD 5980A in relation to the S Doradus Instability Strip and a number of more conventional LBVs. The likely location of HD 5980A during its outburst is also shown.</figcaption></figure> <p>Prior to 1990, HD 5980 had not been observed to show significant variation beyond the regular eclipses. At that time it was known only as a WN+OB binary, but later analysis shows that the primary HD 5980A showed a spectrum similar to a WN3 star. The system had an apparent visual magnitude around 11.7 and the primary is calculated to be slightly the brightest of the three known components.<sup id="cite_ref-moffat_22-0" class="reference"><a href="#cite_note-moffat-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup> </p><p>By November 1993, the spectral type was WN6 and the brightness had increased to around magnitude 10.9. The absorption lines in the spectrum were no longer detectable. The brightness increased for several weeks at the end of 1993, to above 10th magnitude, and the spectral type reached WN8, before the brightness dropped rapidly close to 11th magnitude.<sup id="cite_ref-moffat_22-1" class="reference"><a href="#cite_note-moffat-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup> In June 1994, the star started to cool and become brighter again. It peaked at magnitude 8.6 in September and was comfortably the brightest star in the SMC, but there are no spectra at this exact time. Very shortly after the peak it was classified as WN11.<sup id="cite_ref-Heydari_23-0" class="reference"><a href="#cite_note-Heydari-23"><span class="cite-bracket">[</span>23<span class="cite-bracket">]</span></a></sup> In November the spectrum was considered to be B1.5Ia<sup>+</sup>, a blue hypergiant with strong hydrogen and ionised metal lines in emission or with <a href="/wiki/P_Cygni_profile" class="mw-redirect" title="P Cygni profile">P Cygni profiles</a>. B1.5Ia<sup>+</sup> is a very similar spectral type to WN11, with lower ionisation levels and stronger P Cygni profile absorption in some lines, indicating a slightly lower temperature with changes to the stellar wind. A month later the brightness had decreased slightly and the spectrum indicated an increase in temperature. Within a year the brightness had dropped to 11th magnitude and the spectrum was back to WN6.<sup id="cite_ref-Sahade_24-0" class="reference"><a href="#cite_note-Sahade-24"><span class="cite-bracket">[</span>24<span class="cite-bracket">]</span></a></sup> </p><p>Since the outburst, the brightness has dropped to about magnitude 11.3 and HD 5980 A shows a WN4/5 spectrum. One study suggests an increase of 3–6 times in luminosity to <span class="nowrap"><span data-sort-value="7007100000000000000♠"></span>10,000,000</span> times that of the Sun (<var>L</var><sub>☉</sub>) at its peak,<sup id="cite_ref-drissen_9-2" class="reference"><a href="#cite_note-drissen-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> but this may simply be due to different analysis techniques and others find a fairly consistent luminosity of a few million <var>L</var><sub>☉</sub>.<sup id="cite_ref-wind_25-0" class="reference"><a href="#cite_note-wind-25"><span class="cite-bracket">[</span>25<span class="cite-bracket">]</span></a></sup> </p><p>An earlier outburst may have occurred around 1960 and a 40-year cycle is proposed. Micro-variations with a 30-minute timescale have also been observed when HD 5980A is in its quiescent phase. The causes of the large-amplitude variations and eruptions are not understood, but it is speculated that the large eruptions are triggered when the star expands sufficiently during a normal LBV outburst to force violent interaction with a close binary companion.<sup id="cite_ref-gloria_11-2" class="reference"><a href="#cite_note-gloria-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> </p><p>Although HD 5980 is treated as an LBV, it does not follow the normal pattern which would be an effective temperature during outburst of around 8,500K and an A type spectrum. It is speculated that the close companion causes this particular star to exhibit the LBV-type instability at much higher temperatures. <a href="/wiki/Romano%27s_star" class="mw-redirect" title="Romano's star">Romano's star</a> and <a href="/wiki/Var_83" title="Var 83">Var 83</a> may be similar, and the little-studied <a href="/w/index.php?title=Var_2&action=edit&redlink=1" class="new" title="Var 2 (page does not exist)">Var 2</a> is even hotter, all of them in <a href="/wiki/Messier_33" class="mw-redirect" title="Messier 33">M33</a>. </p> <div class="mw-heading mw-heading2"><h2 id="Evolution">Evolution</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=HD_5980&action=edit&section=4" title="Edit section: Evolution"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Small_Magellanic_Cloud_(Digitized_Sky_Survey_2).jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/7/7a/Small_Magellanic_Cloud_%28Digitized_Sky_Survey_2%29.jpg/310px-Small_Magellanic_Cloud_%28Digitized_Sky_Survey_2%29.jpg" decoding="async" width="310" height="322" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/7/7a/Small_Magellanic_Cloud_%28Digitized_Sky_Survey_2%29.jpg/465px-Small_Magellanic_Cloud_%28Digitized_Sky_Survey_2%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/7/7a/Small_Magellanic_Cloud_%28Digitized_Sky_Survey_2%29.jpg/620px-Small_Magellanic_Cloud_%28Digitized_Sky_Survey_2%29.jpg 2x" data-file-width="13096" data-file-height="13616" /></a><figcaption>Small Magellanic Cloud. NGC 346 the brightest red patch near the centre (the very bright object at the bottom of the frame is <a href="/wiki/NGC_362" title="NGC 362">NGC 362</a>).</figcaption></figure> <p>The current evolutionary states and future development of the HD 5980 stars is highly uncertain. The stars cannot be separated visually and their spectra are largely blended so that the exact chemical and physical properties of the stars are subject to wide margins of error. Stars in the Small Magellanic Cloud have low metallicity and this affects the process of stellar evolution, especially for massive stars. Low metallicity reduces mass loss rates. One effect of this is that Wolf–Rayet stars are uncommon, with a higher proportion of massive stars exploding as supernovae before losing enough mass to become a Wolf–Rayet star. Only stars more massive than 45 <var>M</var><sub>☉</sub> (or higher<sup id="cite_ref-georgy_26-0" class="reference"><a href="#cite_note-georgy-26"><span class="cite-bracket">[</span>26<span class="cite-bracket">]</span></a></sup>) are predicted to become WR stars in the SMC, while in the Milky Way those above 25 <var>M</var><sub>☉</sub> do so.<sup id="cite_ref-foellmi2003_27-0" class="reference"><a href="#cite_note-foellmi2003-27"><span class="cite-bracket">[</span>27<span class="cite-bracket">]</span></a></sup> Only 12 WR stars are known in the SMC, 11 WN type and 1 WO, all of them massive and luminous compared to Milky Way Wolf–Rayets, and over half have massive companions.<sup id="cite_ref-pasemann_10-1" class="reference"><a href="#cite_note-pasemann-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup> SMC WR stars have relatively early spectral types for their temperatures, again as a result of the low metallicity. Other than HD 5980, the latest Wolf–Rayet spectral type in the SMC is WN4. All SMC Wolf–Rayets, with one exception, show some absorption in their spectrum, indicative of an O-type star of similar temperature to the Wolf–Rayet. In some cases, an O companion does exists, but it is speculated that Wolf–Rayet stellar winds are sufficiently weak at SMC metallicities for some photospheric absorption to be seen in the spectrum.<sup id="cite_ref-massey_28-0" class="reference"><a href="#cite_note-massey-28"><span class="cite-bracket">[</span>28<span class="cite-bracket">]</span></a></sup> </p><p>Component C is most likely a relatively normal O-type star. It has been variously classified from O4 to O7, tentatively as a supergiant. Thus it is only slightly evolved from the main sequence, most likely still fusing hydrogen at the core, and may follow a fairly typical single star evolutionary track. Its companion is unknown, but currently too distant to be a strong influence on its evolution.<sup id="cite_ref-foellmi_3-5" class="reference"><a href="#cite_note-foellmi-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> </p><p>The current evolutionary state of the WR binary components is less clear. They are in a close orbit but fully detached, although it is possible that mass transfer has taken place in the past when one or other star was expanded. The LBV was estimated to be larger than the orbital separation at the peak of its outburst, although that is effectively just a pseudo-photosphere formed by ejected material. The early WN classification with little hydrogen in the spectrum is generally associated with highly evolved low mass helium burning stars nearing the end of their lives, but the HD 5980 components are massive luminous stars. The spectral types displayed by low metallicity Wolf–Rayet stars such as those in the SMC are not directly comparable to higher-metallicity stars and this complicates interpretation of their evolutionary state. Quasi-chemically homogeneous evolution of very massive stars can approximately reproduce the state of the A and B components as stars just evolving away from the main sequence, but at SMC metallicity this requires near-critical rotation to force sufficient mixing.<sup id="cite_ref-koenigsberger_7-7" class="reference"><a href="#cite_note-koenigsberger-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-yoon_29-0" class="reference"><a href="#cite_note-yoon-29"><span class="cite-bracket">[</span>29<span class="cite-bracket">]</span></a></sup> </p><p>There are two binary evolution models that have been developed that reproduce the current system state. In the first model, two stars of initial masses 90 <var>M</var><sub>☉</sub> and 80 <var>M</var><sub>☉</sub> were evolved with an initial orbital period of 12 days and initial rotation velocity of 500 km/s. After ~3.1 million years, the stars were found to have an orbital period of 19.2d, and masses and luminosity similar to those that are derived from recent observations.<sup id="cite_ref-gk_30-0" class="reference"><a href="#cite_note-gk-30"><span class="cite-bracket">[</span>30<span class="cite-bracket">]</span></a></sup> No mass transfer has occurred because the stars follow a quasi-chemically evolutionary computation. In the second model, the initial masses of the two stars were 150 <var>M</var><sub>☉</sub> and 75 <var>M</var><sub>☉</sub> in a 16-day orbit 160 <var>R</var><sub>☉</sub> apart. After 2.3 million years, the more massive star starts to overflow its <a href="/wiki/Roche_lobe" title="Roche lobe">roche lobe</a> and quickly transfers 25 <var>M</var><sub>☉</sub> to the smaller star. We observe the system after 2.6 million years. Details of the model are obviously uncertain due to the highly unstable behaviour of the primary observed over the last century.<sup id="cite_ref-shenar_8-16" class="reference"><a href="#cite_note-shenar-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> </p><p>Wolf–Rayet stars explode as type Ib/c core collapse <a href="/wiki/Supernova" title="Supernova">supernovae</a> when they have fused elements all the way to iron. Depending on the mass of the core at the time of collapse they will leave a black hole or neutron star remnant. SMC Wolf–Rayet stars are expected to be relatively massive and relatively short-lived, leaving behind black holes. They are also good candidates for <a href="/wiki/Gamma-ray_burst" title="Gamma-ray burst">gamma-ray bursts</a> if they are rotating quickly enough.<sup id="cite_ref-yoon_29-1" class="reference"><a href="#cite_note-yoon-29"><span class="cite-bracket">[</span>29<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="See_also">See also</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=HD_5980&action=edit&section=5" title="Edit section: See also"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a href="/wiki/WR_25" title="WR 25">WR 25</a>, a similar star in the <a href="/wiki/Carina_Nebula" title="Carina Nebula">Carina Nebula</a></li> <li><a href="/wiki/List_of_most_massive_stars" title="List of most massive stars">List of most massive stars</a></li></ul> <div class="mw-heading mw-heading2"><h2 id="References">References</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=HD_5980&action=edit&section=6" title="Edit section: References"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></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"> <div class="mw-references-wrap mw-references-columns"><ol class="references"> <li id="cite_note-tycho-1"><span class="mw-cite-backlink">^ <a href="#cite_ref-tycho_1-0"><sup><i><b>a</b></i></sup></a> <a href="#cite_ref-tycho_1-1"><sup><i><b>b</b></i></sup></a> <a href="#cite_ref-tycho_1-2"><sup><i><b>c</b></i></sup></a> <a href="#cite_ref-tycho_1-3"><sup><i><b>d</b></i></sup></a></span> <span class="reference-text"><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 id="CITEREFHogKuzminBastianFabricius1998" class="citation journal cs1">Hog, E.; Kuzmin, A.; Bastian, U.; Fabricius, C.; Kuimov, K.; Lindegren, L.; Makarov, V. 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"The TYCHO Reference Catalogue". <i>Astronomy and Astrophysics</i>. <b>335</b>: L65. <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/1998A&A...335L..65H">1998A&A...335L..65H</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomy+and+Astrophysics&rft.atitle=The+TYCHO+Reference+Catalogue&rft.volume=335&rft.pages=L65&rft.date=1998&rft_id=info%3Abibcode%2F1998A%26A...335L..65H&rft.aulast=Hog&rft.aufirst=E.&rft.au=Kuzmin%2C+A.&rft.au=Bastian%2C+U.&rft.au=Fabricius%2C+C.&rft.au=Kuimov%2C+K.&rft.au=Lindegren%2C+L.&rft.au=Makarov%2C+V.+V.&rft.au=Roeser%2C+S.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AHD+5980" class="Z3988"></span></span> </li> <li id="cite_note-vsx-2"><span class="mw-cite-backlink"><b><a href="#cite_ref-vsx_2-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="https://www.aavso.org/vsx/index.php?view=detail.top&oid=236169">"HD 5980"</a>. <i>International Variable Star Index</i>. <a href="/wiki/AAVSO" class="mw-redirect" title="AAVSO">AAVSO</a><span class="reference-accessdate">. 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"Evolution of rapidly rotating metal-poor massive stars towards gamma-ray bursts". <i>Astronomy and Astrophysics</i>. <b>443</b> (2): 643–648. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0508242">astro-ph/0508242</a></span>. <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/2005A&A...443..643Y">2005A&A...443..643Y</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1051%2F0004-6361%3A20054030">10.1051/0004-6361:20054030</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:16528030">16528030</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomy+and+Astrophysics&rft.atitle=Evolution+of+rapidly+rotating+metal-poor+massive+stars+towards+gamma-ray+bursts&rft.volume=443&rft.issue=2&rft.pages=643-648&rft.date=2005&rft_id=info%3Aarxiv%2Fastro-ph%2F0508242&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A16528030%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1051%2F0004-6361%3A20054030&rft_id=info%3Abibcode%2F2005A%26A...443..643Y&rft.aulast=Yoon&rft.aufirst=S.-C.&rft.au=Langer%2C+N.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AHD+5980" class="Z3988"></span></span> </li> <li id="cite_note-gk-30"><span class="mw-cite-backlink"><b><a href="#cite_ref-gk_30-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFKoenigsbergerMorrellHillierGamen2014" class="citation journal cs1">Koenigsberger, G.; Morrell, N.; Hillier, D.J.; Gamen, R.; Schneider, F.; González-Jiménez, N.; Langer, N.; Barbá, R. (2014). "The HD 5980 Multiple System: Masses and Evolutionary Status". <i>The Astronomical Journal</i>. <b>148</b> (4): 13. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/1408.0556">1408.0556</a></span>. <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/2014AJ....148...62K">2014AJ....148...62K</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%2F0004-6256%2F148%2F4%2F62">10.1088/0004-6256/148/4/62</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:118348677">118348677</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astronomical+Journal&rft.atitle=The+HD+5980+Multiple+System%3A+Masses+and+Evolutionary+Status&rft.volume=148&rft.issue=4&rft.pages=13&rft.date=2014&rft_id=info%3Aarxiv%2F1408.0556&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A118348677%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1088%2F0004-6256%2F148%2F4%2F62&rft_id=info%3Abibcode%2F2014AJ....148...62K&rft.aulast=Koenigsberger&rft.aufirst=G.&rft.au=Morrell%2C+N.&rft.au=Hillier%2C+D.J.&rft.au=Gamen%2C+R.&rft.au=Schneider%2C+F.&rft.au=Gonz%C3%A1lez-Jim%C3%A9nez%2C+N.&rft.au=Langer%2C+N.&rft.au=Barb%C3%A1%2C+R.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AHD+5980" class="Z3988"></span></span> </li> </ol></div></div> <div class="mw-heading mw-heading2"><h2 id="External_links">External links</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=HD_5980&action=edit&section=7" title="Edit section: External links"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a rel="nofollow" class="external text" href="https://apod.nasa.gov/apod/ap030214.html">NASA Astronomy Picture of the Day: The Heart in NGC 346 (14 February 2003)</a></li> <li><a rel="nofollow" class="external text" href="https://heasarc.gsfc.nasa.gov/docs/objects/heapow/archive/stars/hd5980_chandra.html">Chandra X-Ray Image</a></li> <li><a rel="nofollow" class="external text" href="http://www.solstation.com/x-objects/hd5980ab.htm">Solstation (many images)</a></li></ul> <div class="navbox-styles"><style data-mw-deduplicate="TemplateStyles:r1129693374">.mw-parser-output .hlist dl,.mw-parser-output .hlist ol,.mw-parser-output .hlist ul{margin:0;padding:0}.mw-parser-output .hlist dd,.mw-parser-output .hlist dt,.mw-parser-output .hlist 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navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Tucana" title="Template:Tucana"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Tucana" title="Template talk:Tucana"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Tucana" title="Special:EditPage/Template:Tucana"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Constellation_of_Tucana" style="font-size:114%;margin:0 4em"><a href="/wiki/Tucana_(constellation)" class="mw-redirect" title="Tucana (constellation)">Constellation of Tucana</a></div></th></tr><tr><td class="navbox-abovebelow" colspan="2" style="text-align: center;"><div> <ul><li><a href="/wiki/List_of_stars_in_Tucana" title="List of stars in Tucana">List of stars in Tucana</a></li> <li><a href="/wiki/Tucana_in_Chinese_astronomy" title="Tucana in Chinese astronomy">Tucana in Chinese astronomy</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:55px"><a href="/wiki/Star" title="Star">Stars</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="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:70px"><a href="/wiki/Bayer_designation" title="Bayer designation">Bayer</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Alpha_Tucanae" title="Alpha Tucanae">α</a></li> <li><a href="/wiki/Beta_Tucanae" title="Beta Tucanae">β<sup>1</sup></a></li> <li><a href="/wiki/Beta_Tucanae" title="Beta Tucanae">β<sup>2</sup></a></li> <li><a href="/wiki/Beta_Tucanae" title="Beta Tucanae">β<sup>3</sup></a></li> <li><a href="/wiki/Gamma_Tucanae" title="Gamma Tucanae">γ</a></li> <li><a href="/wiki/Delta_Tucanae" title="Delta Tucanae">δ</a></li> <li><a href="/wiki/Epsilon_Tucanae" title="Epsilon Tucanae">ε</a></li> <li><a href="/wiki/Zeta_Tucanae" title="Zeta Tucanae">ζ</a></li> <li><a href="/wiki/Eta_Tucanae" title="Eta Tucanae">η</a></li> <li><a href="/wiki/Theta_Tucanae" title="Theta Tucanae">θ</a></li> <li><a href="/wiki/Iota_Tucanae" title="Iota Tucanae">ι</a></li> <li><a href="/wiki/Kappa_Tucanae" title="Kappa Tucanae">κ</a></li> <li><a href="/wiki/Lambda1_Tucanae" title="Lambda1 Tucanae">λ<sup>1</sup></a></li> <li><a href="/wiki/Lambda2_Tucanae" title="Lambda2 Tucanae">λ<sup>2</sup></a></li> <li><a href="/wiki/Mu_Tucanae" class="mw-redirect" title="Mu Tucanae">μ</a></li> <li><a href="/wiki/Nu_Tucanae" title="Nu Tucanae">ν</a></li> <li><a href="/wiki/Pi_Tucanae" title="Pi Tucanae">π</a></li> <li><a href="/wiki/Rho_Tucanae" title="Rho Tucanae">ρ</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:70px"><a href="/wiki/Variable_star_designation" class="mw-redirect" title="Variable star designation">Variable</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/DS_Tucanae" title="DS Tucanae">DS</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:70px"><a href="/wiki/Bright_Star_Catalogue" title="Bright Star Catalogue">HR</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/HD_219077" title="HD 219077">8829</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:70px"><a href="/wiki/Henry_Draper_Catalogue" title="Henry Draper Catalogue">HD</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/HD_4308" title="HD 4308">4308</a></li> <li><a class="mw-selflink selflink">5980</a></li> <li><a href="/wiki/HD_7199" title="HD 7199">7199 (Emiw)</a></li> <li><a href="/wiki/HD_215497" title="HD 215497">215497</a></li> <li><a href="/wiki/HD_221287" title="HD 221287">221287 (Poerava)</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:70px">Other</th><td class="navbox-list-with-group navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/AB7" title="AB7">AB7</a></li> <li><a href="/wiki/Gliese_54" title="Gliese 54">Gliese 54</a></li> <li><a href="/wiki/HV_2112" title="HV 2112">HV 2112</a></li> <li><a href="/wiki/HV_11417" title="HV 11417">HV 11417</a></li> <li><a href="/wiki/HV_11423" title="HV 11423">HV 11423</a></li> <li><a href="/wiki/L_168-9" title="L 168-9">L 168-9</a></li> <li><a href="/wiki/PMMR_62" class="mw-redirect" title="PMMR 62">PMMR 62</a></li> <li><a href="/wiki/SMC_018136" class="mw-redirect" title="SMC 018136">SMC 018136</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><td colspan="2" class="navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th id="Exoplanets" scope="row" class="navbox-group" style="width:151px;background: #ddddff;"><a href="/wiki/Exoplanet" title="Exoplanet">Exoplanets</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/DS_Tucanae_Ab" class="mw-redirect" title="DS Tucanae Ab">DS Tucanae Ab</a></li> <li><a href="/wiki/HD_4308_b" title="HD 4308 b">HD 4308 b</a></li> <li><a href="/wiki/HD_7199_b" class="mw-redirect" title="HD 7199 b">HD 7199 b (Hairu)</a></li> <li><a href="/wiki/HD_215497_b" title="HD 215497 b">HD 215497 b</a></li> <li><a href="/wiki/HD_215497_c" title="HD 215497 c">c</a></li> <li><a href="/wiki/HD_219077_b" class="mw-redirect" title="HD 219077 b">HD 219077 b</a></li> <li><a href="/wiki/HD_221287_b" title="HD 221287 b">HD 221287 b (Pipitea)</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:55px"><a href="/wiki/Star_cluster" title="Star cluster">Star<br />clusters</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="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:70px"><a href="/wiki/New_General_Catalogue" title="New General Catalogue">NGC</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/NGC_121" title="NGC 121">121</a></li> <li><a href="/wiki/NGC_152" title="NGC 152">152</a></li> <li><a href="/wiki/NGC_176" title="NGC 176">176</a></li> <li><a href="/wiki/NGC_220" title="NGC 220">220</a></li> <li><a href="/wiki/NGC_222" title="NGC 222">222</a></li> <li><a href="/wiki/NGC_231" title="NGC 231">231</a></li> <li><a href="/wiki/NGC_241" title="NGC 241">241</a></li> <li><a href="/wiki/NGC_256" title="NGC 256">256</a></li> <li><a href="/wiki/NGC_265" title="NGC 265">265</a></li> <li><a href="/wiki/NGC_267" title="NGC 267">267</a></li> <li><a href="/wiki/NGC_269" title="NGC 269">269</a></li> <li><a href="/wiki/NGC_290" title="NGC 290">290</a></li> <li><a href="/wiki/NGC_294" title="NGC 294">294</a></li> <li><a href="/wiki/NGC_299" title="NGC 299">299</a></li> <li><a href="/wiki/NGC_306" title="NGC 306">306</a></li> <li><a href="/wiki/NGC_330" title="NGC 330">330</a></li> <li><a href="/wiki/NGC_339" title="NGC 339">339</a></li> <li><a href="/wiki/NGC_346" title="NGC 346">346</a></li> <li><a href="/wiki/NGC_361" title="NGC 361">361</a></li> <li><a href="/wiki/NGC_362" title="NGC 362">362</a></li> <li><a href="/wiki/NGC_371" title="NGC 371">371</a></li> <li><a href="/wiki/NGC_376" title="NGC 376">376</a></li> <li><a href="/wiki/NGC_395" title="NGC 395">395</a></li> <li><a href="/wiki/NGC_411" title="NGC 411">411</a></li> <li><a href="/wiki/NGC_416" title="NGC 416">416</a></li> <li><a href="/wiki/NGC_419" title="NGC 419">419</a></li> <li><a href="/wiki/NGC_422" title="NGC 422">422</a></li> <li><a href="/wiki/NGC_456" title="NGC 456">456</a></li> <li><a href="/wiki/NGC_458" title="NGC 458">458</a></li> <li><a href="/wiki/NGC_460" title="NGC 460">460</a></li> <li><a href="/wiki/NGC_465" title="NGC 465">465</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:70px">Other</th><td class="navbox-list-with-group navbox-list navbox-even" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/47_Tucanae" title="47 Tucanae">ξ (47)</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><td colspan="2" class="navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th id="Nebulae" scope="row" class="navbox-group" style="width:151px;background: #ddddff;"><a href="/wiki/Nebula" title="Nebula">Nebulae</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/E0102" title="E0102">E0102</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:55px"><a href="/wiki/Galaxy" title="Galaxy">Galaxies</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="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:70px">NGC</th><td class="navbox-list-with-group navbox-list navbox-even" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/NGC_53" title="NGC 53">53</a></li> <li><a href="/wiki/NGC_360" title="NGC 360">360</a></li> <li><a href="/wiki/NGC_406" title="NGC 406">406</a></li> <li><a href="/wiki/NGC_432" title="NGC 432">432</a></li> <li><a href="/wiki/NGC_434" title="NGC 434">434</a></li> <li><a href="/wiki/NGC_440" title="NGC 440">440</a></li> <li><a href="/wiki/NGC_466" title="NGC 466">466</a></li> <li><a href="/wiki/NGC_484" title="NGC 484">484</a></li> <li><a href="/wiki/NGC_7329" title="NGC 7329">7329</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:70px">Other</th><td class="navbox-list-with-group navbox-list navbox-odd" style="padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/ESO_148-2" title="ESO 148-2">ESO 148-2</a></li> <li><a href="/wiki/ISOHDFS_27" title="ISOHDFS 27">ISOHDFS 27</a></li> <li><a href="/wiki/Tucana_Dwarf" title="Tucana Dwarf">Tucana Dwarf</a></li> <li><a href="/wiki/Small_Magellanic_Cloud" title="Small Magellanic Cloud">Small Magellanic Cloud</a> (partly in <a href="/wiki/Hydrus" title="Hydrus">Hydrus</a>)</li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><td 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