[astro-ph/0203110] Mass distribution in our Galaxy

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A new luminosity model consistent with the COBE NIR data and the apparent magnitude distributions of bulge clump giant stars has bulge/bar length of $\simeq 3.5\kpc$, axis ratios of 1:(0.3-0.4):0.3, and short disk scale-length ($\simeq 2.1\kpc$). Gas-dynamical flows in the potential of this model with constant M/L fit the terminal velocities in $10掳\le |l| \le 50掳$ very well. The luminous mass distribution with this M/L is consistent with the surface density of known matter near the Sun, but still underpredicts the microlensing optical depth towards the bulge. Together, these facts argue strongly for a massive, near-maximal disk in our $\sim L^\ast$, Sbc spiral Galaxy. While the outer rotation curve and global mass distribution are not as readily measured as in similar spiral galaxies, the dark halo mass estimated from satellite velocities is consistent with a flat rotation curve continuing on from the luminous mass distribution."/> <meta name="twitter:site" content="@arxiv"/> <meta name="twitter:card" content="summary"/> <meta name="twitter:title" content="Mass distribution in our Galaxy"/> <meta name="twitter:description" content="This article summarizes recent work on the luminosity and mass distribution of the Galactic bulge and disk, and on the mass of the Milky Way's dark halo. A new luminosity model consistent with the..."/> <meta name="twitter:image" content="https://static.arxiv.org/icons/twitter/arxiv-logo-twitter-square.png"/> <meta name="twitter:image:alt" content="arXiv logo"/> <link rel="stylesheet" media="screen" type="text/css" href="/static/browse/0.3.4/css/tooltip.css"/><link rel="stylesheet" media="screen" type="text/css" href="https://static.arxiv.org/js/bibex-dev/bibex.css?20200709"/> <script src="/static/browse/0.3.4/js/mathjaxToggle.min.js" type="text/javascript"></script> <script src="//code.jquery.com/jquery-latest.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/js-cookie@2/src/js.cookie.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/dompurify@2.3.5/dist/purify.min.js"></script> <script src="/static/browse/0.3.4/js/toggle-labs.js?20241022" type="text/javascript"></script> <script src="/static/browse/0.3.4/js/cite.js" type="text/javascript"></script><meta name="citation_title" content="Mass distribution in our Galaxy" /><meta name="citation_author" content="Gerhard, Ortwin" /><meta name="citation_doi" content="10.1023/A:1015818111633" /><meta name="citation_date" content="2002/03/07" /><meta name="citation_online_date" content="2002/03/07" /><meta name="citation_pdf_url" content="http://arxiv.org/pdf/astro-ph/0203110" /><meta name="citation_arxiv_id" content="astro-ph/0203110" /><meta name="citation_abstract" content=" This article summarizes recent work on the luminosity and mass distribution of the Galactic bulge and disk, and on the mass of the Milky Way's dark halo. A new luminosity model consistent with the COBE NIR data and the apparent magnitude distributions of bulge clump giant stars has bulge/bar length of $\simeq 3.5\kpc$, axis ratios of 1:(0.3-0.4):0.3, and short disk scale-length ($\simeq 2.1\kpc$). Gas-dynamical flows in the potential of this model with constant M/L fit the terminal velocities in $10\deg\le |l| \le 50\deg$ very well. The luminous mass distribution with this M/L is consistent with the surface density of known matter near the Sun, but still underpredicts the microlensing optical depth towards the bulge. Together, these facts argue strongly for a massive, near-maximal disk in our $\sim L^\ast$, Sbc spiral Galaxy. While the outer rotation curve and global mass distribution are not as readily measured as in similar spiral galaxies, the dark halo mass estimated from satellite velocities is consistent with a flat rotation curve continuing on from the luminous mass distribution." /> </head> <body class="with-cu-identity"> <aside class="slider-wrapper bps-banner special-color"> <div class="columns"> <div class="copy-donation bps-banner"> <h2>Change to arXiv's privacy policy</h2> <p>The <a target="_blank" href="https://info.arxiv.org/help/policies/privacy_policy.html">arXiv Privacy Policy</a> has changed. 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href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gerhard,+O" rel="nofollow">Ortwin Gerhard</a> (Astronom. Institut, Univ. Basel, Switzerland)</div> <div id="download-button-info" hidden>View a PDF of the paper titled Mass distribution in our Galaxy, by Ortwin Gerhard (Astronom. Institut and 2 other authors</div> <a class="mobile-submission-download" href="/pdf/astro-ph/0203110">View PDF</a> <blockquote class="abstract mathjax"> <span class="descriptor">Abstract:</span> This article summarizes recent work on the luminosity and mass distribution of the Galactic bulge and disk, and on the mass of the Milky Way's dark halo. A new luminosity model consistent with the COBE NIR data and the apparent magnitude distributions of bulge clump giant stars has bulge/bar length of $\simeq 3.5\kpc$, axis ratios of 1:(0.3-0.4):0.3, and short disk scale-length ($\simeq 2.1\kpc$). Gas-dynamical flows in the potential of this model with constant M/L fit the terminal velocities in $10掳\le |l| \le 50掳$ very well. The luminous mass distribution with this M/L is consistent with the surface density of known matter near the Sun, but still underpredicts the microlensing optical depth towards the bulge. Together, these facts argue strongly for a massive, near-maximal disk in our $\sim L^\ast$, Sbc spiral Galaxy. While the outer rotation curve and global mass distribution are not as readily measured as in similar spiral galaxies, the dark halo mass estimated from satellite velocities is consistent with a flat rotation curve continuing on from the luminous mass distribution. </blockquote>  <div class="metatable"> <table summary="Additional metadata"> <tr> <td class="tablecell label">Comments:</td> <td class="tablecell comments mathjax">To appear in: Matter in the Universe, eds. Jetzer P., Pretzl K., von Steiger R., Space Science Reviews, Kluwer. 10 pages, LaTeX, 5 figures</td> </tr> <tr> <td class="tablecell label">Subjects:</td> <td class="tablecell subjects"> <span class="primary-subject">Astrophysics (astro-ph)</span></td> </tr> <tr> <td class="tablecell label">Report number:</td> <td class="tablecell jref">Basel Preprint Ser. 132</td> </tr> <tr> <td class="tablecell label">Cite as:</td> <td class="tablecell arxivid"><span class="arxivid"><a href="https://arxiv.org/abs/astro-ph/0203110">arXiv:astro-ph/0203110</a></span></td> </tr> <tr> <td class="tablecell label"> </td> <td class="tablecell arxividv">(or <span class="arxivid"> <a href="https://arxiv.org/abs/astro-ph/0203110v1">arXiv:astro-ph/0203110v1</a></span> for this version) </td> </tr> <tr> <td class="tablecell label"> </td> <td class="tablecell arxivdoi"> <a href="https://doi.org/10.48550/arXiv.astro-ph/0203110" id="arxiv-doi-link">https://doi.org/10.48550/arXiv.astro-ph/0203110</a><div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button>  <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> arXiv-issued DOI via DataCite</div> </div> </td> </tr> <tr> <td class="tablecell label"> <abbr title="Digital Object Identifier">Related DOI</abbr>: </td> <td class="tablecell doi"><a href="https://doi.org/10.1023/A%3A1015818111633" data-doi="10.1023/A:1015818111633" class="link-https link-external" rel="external noopener nofollow">https://doi.org/10.1023/A%3A1015818111633</a>  <div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button>  <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> DOI(s) linking to related resources </div> </div> </td> </tr> </table> </div> </div> </div> <div class="submission-history"> <h2>Submission history</h2> From: Ortwin Gerhard [<a href="/show-email/868f50c3/astro-ph/0203110" rel="nofollow">view email</a>] <br/> <strong>[v1]</strong> Thu, 7 Mar 2002 15:58:53 UTC (234 KB)<br/> </div> </div>  <div class="extra-services"> <div class="full-text"> <a name="other"></a> <span class="descriptor">Full-text links:</span> <h2>Access Paper:</h2> <ul> <div id="download-button-info" hidden> View a PDF of the paper titled Mass distribution in our Galaxy, by Ortwin Gerhard (Astronom. 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[astro-ph/0203110] Mass distribution in our Galaxy