Analysis and calibration of Ca ii triplet spectroscopy of red giant branch stars from VLT/FLAMES observations
Identifieur interne : 000844 ( Main/Corpus ); précédent : 000843; suivant : 000845Analysis and calibration of Ca ii triplet spectroscopy of red giant branch stars from VLT/FLAMES observations
Auteurs : G. Battaglia ; M. Irwin ; E. Tolstoy ; V. Hill ; A. Helmi ; B. Letarte ; P. JablonkaSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008-01-01.
Abstract
We demonstrate that low-resolution Ca ii triplet (CaT) spectroscopic estimates of the overall metallicity ([Fe/H]) of individual red giant branch (RGB) stars in two nearby dwarf spheroidal galaxies (dSphs) agree to ±0.1–0.2 dex with detailed high-resolution spectroscopic determinations for the same stars over the range −2.5 < [Fe/H] < −0.5. For this study, we used a sample of 129 stars observed in low- and high-resolution modes with VLT/FLAMES in the Sculptor and Fornax dSphs. We also present the data-reduction steps we used in our low-resolution analysis and show that the typical accuracy of our velocity and CaT [Fe/H] measurement is ∼2 km s−1 and 0.1 dex, respectively. We conclude that CaT–[Fe/H] relations calibrated on globular clusters can be applied with confidence to RGB stars in composite stellar populations over the range −2.5 < [Fe/H] < −0.5.
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DOI: 10.1111/j.1365-2966.2007.12532.x
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Jablonka</name><affiliation><mods:affiliation>Observatoire de Genève, Laboratoire d'Astrophysique de l'Ecole Polytechnique Fédérale de Lausanne (EPFL), CH-1290 Sauverny, Switzerland</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbrev">Monthly Notices of the Royal Astronomical Society</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2008-01-01">2008-01-01</date><biblScope unit="volume">383</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="183">183</biblScope><biblScope unit="page" to="199">199</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">11EE6D493CCBDE6D91621C48CEBADB9F0AB7EAC1</idno><idno type="DOI">10.1111/j.1365-2966.2007.12532.x</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract">We demonstrate that low-resolution Ca ii triplet (CaT) spectroscopic estimates of the overall metallicity ([Fe/H]) of individual red giant branch (RGB) stars in two nearby dwarf spheroidal galaxies (dSphs) agree to ±0.1–0.2 dex with detailed high-resolution spectroscopic determinations for the same stars over the range −2.5 < [Fe/H] < −0.5. For this study, we used a sample of 129 stars observed in low- and high-resolution modes with VLT/FLAMES in the Sculptor and Fornax dSphs. We also present the data-reduction steps we used in our low-resolution analysis and show that the typical accuracy of our velocity and CaT [Fe/H] measurement is ∼2 km s−1 and 0.1 dex, respectively. We conclude that CaT–[Fe/H] relations calibrated on globular clusters can be applied with confidence to RGB stars in composite stellar populations over the range −2.5 < [Fe/H] < −0.5.</div></front></TEI><istex><corpusName>oup</corpusName><author><json:item><name>G. Battaglia</name><affiliations><json:string>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</json:string><json:string>E-mail: gbattagl@astro.rug.nl</json:string></affiliations></json:item><json:item><name>M. 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For this study, we used a sample of 129 stars observed in low- and high-resolution modes with VLT/FLAMES in the Sculptor and Fornax dSphs. We also present the data-reduction steps we used in our low-resolution analysis and show that the typical accuracy of our velocity and CaT [Fe/H] measurement is ∼2 km s−1 and 0.1 dex, respectively. 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For this study, we used a sample of 129 stars observed in low- and high-resolution modes with VLT/FLAMES in the Sculptor and Fornax dSphs. We also present the data-reduction steps we used in our low-resolution analysis and show that the typical accuracy of our velocity and CaT [Fe/H] measurement is ∼2 km s−1 and 0.1 dex, respectively. We conclude that CaT–[Fe/H] relations calibrated on globular clusters can be applied with confidence to RGB stars in composite stellar populations over the range −2.5 < [Fe/H] < −0.5.</p></abstract><textClass><keywords scheme="keyword"><list><item><term>Papers</term></item></list></keywords></textClass><textClass><keywords scheme="keyword"><list><head>keywords</head><item><term>techniques: spectroscopic</term></item><item><term>stars: abundances</term></item><item><term>galaxies: dwarf</term></item><item><term>galaxies: star clusters</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2007-12-06">Created</change><change when="2008-01-01">Published</change><change xml:id="refBibs-istex" who="#ISTEX-API" when="2016-10-14">References added</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/11EE6D493CCBDE6D91621C48CEBADB9F0AB7EAC1/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="corpus oup" wicri:toSee="no header"><istex:xmlDeclaration>version="1.0" encoding="utf-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//NLM//DTD Journal Publishing DTD v2.3 20070202//EN" URI="journalpublishing.dtd" name="istex:docType"></istex:docType><istex:document><article article-type="research-article"><front><journal-meta><journal-id journal-id-type="hwp">mnras</journal-id><journal-id journal-id-type="publisher-id">mnras</journal-id><journal-title>Monthly Notices of the Royal Astronomical Society</journal-title><abbrev-journal-title>Monthly Notices of the Royal Astronomical Society</abbrev-journal-title><issn pub-type="ppub">0035-8711</issn><issn pub-type="epub">1365-2966</issn><publisher><publisher-name>Blackwell Publishing Ltd</publisher-name><publisher-loc>Oxford, UK</publisher-loc></publisher></journal-meta><article-meta><article-id pub-id-type="doi">10.1111/j.1365-2966.2007.12532.x</article-id><article-categories><subj-group><subject>Papers</subject></subj-group></article-categories><title-group><article-title>Analysis and calibration of Ca <sc>ii</sc> triplet spectroscopy of red giant branch stars from VLT/FLAMES observations</article-title></title-group><contrib-group><contrib contrib-type="author"><name><surname>Battaglia</surname><given-names>G.</given-names></name><xref ref-type="aff" rid="a1">1</xref><xref ref-type="corresp" rid="c1">*</xref></contrib><contrib contrib-type="author"><name><surname>Irwin</surname><given-names>M.</given-names></name><xref ref-type="aff" rid="a2">2</xref></contrib><contrib contrib-type="author"><name><surname>Tolstoy</surname><given-names>E.</given-names></name><xref ref-type="aff" rid="a1">1</xref></contrib><contrib contrib-type="author"><name><surname>Hill</surname><given-names>V.</given-names></name><xref ref-type="aff" rid="a3">3</xref></contrib><contrib contrib-type="author"><name><surname>Helmi</surname><given-names>A.</given-names></name><xref ref-type="aff" rid="a1">1</xref></contrib><contrib contrib-type="author"><name><surname>Letarte</surname><given-names>B.</given-names></name><xref ref-type="aff" rid="a1">1</xref><xref ref-type="aff" rid="a4">4</xref></contrib><contrib contrib-type="author"><name><surname>Jablonka</surname><given-names>P.</given-names></name><xref ref-type="aff" rid="a5">5</xref></contrib></contrib-group><aff id="a1"><label>1</label>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</aff><aff id="a2"><label>2</label>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</aff><aff id="a3"><label>3</label>GEPI, Observatoire de Paris, CNRS, Universit Paris Diderot; Place Jules Janssen 92190 Meudon, France</aff><aff id="a4"><label>4</label>Caltech Astronomy, MC105-24, Pasadena, CA 91125, USA</aff><aff id="a5"><label>5</label>Observatoire de Genève, Laboratoire d'Astrophysique de l'Ecole Polytechnique Fédérale de Lausanne (EPFL), CH-1290 Sauverny, Switzerland</aff><author-notes><corresp id="c1">*E-mail: <email>gbattagl@astro.rug.nl</email></corresp></author-notes><pub-date pub-type="ppub"><day>01</day><month>01</month><year>2008</year></pub-date><pub-date pub-type="epub"><day>06</day><month>12</month><year>2007</year></pub-date><volume>383</volume><issue>1</issue><fpage>183</fpage><lpage>199</lpage><history><date date-type="received"><day>25</day><month>09</month><year>2007</year></date><date date-type="accepted"><day>28</day><month>09</month><year>2007</year></date></history><copyright-statement>© 2007 The Authors. Journal compilation © 2007 RAS</copyright-statement><copyright-year>2007</copyright-year><abstract><p>We demonstrate that low-resolution Ca <sc>ii</sc> triplet (CaT) spectroscopic estimates of the overall metallicity ([Fe/H]) of individual red giant branch (RGB) stars in two nearby dwarf spheroidal galaxies (dSphs) agree to ±0.1–0.2 dex with detailed high-resolution spectroscopic determinations for the same stars over the range −2.5 < [Fe/H] < −0.5. For this study, we used a sample of 129 stars observed in low- and high-resolution modes with VLT/FLAMES in the Sculptor and Fornax dSphs. We also present the data-reduction steps we used in our low-resolution analysis and show that the typical accuracy of our velocity and CaT [Fe/H] measurement is ∼2 km s<sup>−1</sup> and 0.1 dex, respectively. We conclude that CaT–[Fe/H] relations calibrated on globular clusters can be applied with confidence to RGB stars in composite stellar populations over the range −2.5 < [Fe/H] < −0.5.</p></abstract><kwd-group><kwd>techniques: spectroscopic</kwd><kwd>stars: abundances</kwd><kwd>galaxies: dwarf</kwd><kwd>galaxies: star clusters</kwd></kwd-group></article-meta></front></article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo><title>Analysis and calibration of Ca ii triplet spectroscopy of red giant branch stars from VLT/FLAMES observations</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>Analysis and calibration of Ca ii triplet spectroscopy of red giant branch stars from VLT/FLAMES observations</title></titleInfo><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Battaglia</namePart><affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</affiliation><affiliation>E-mail: gbattagl@astro.rug.nl</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Irwin</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E.</namePart><namePart type="family">Tolstoy</namePart><affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">V.</namePart><namePart type="family">Hill</namePart><affiliation>GEPI, Observatoire de Paris, CNRS, Universit Paris Diderot; Place Jules Janssen 92190 Meudon, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Helmi</namePart><affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">B.</namePart><namePart type="family">Letarte</namePart><affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</affiliation><affiliation>Caltech Astronomy, MC105-24, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Jablonka</namePart><affiliation>Observatoire de Genève, Laboratoire d'Astrophysique de l'Ecole Polytechnique Fédérale de Lausanne (EPFL), CH-1290 Sauverny, Switzerland</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="research-article" displayLabel="research-article"></genre><subject><topic>Papers</topic></subject><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2008-01-01</dateIssued><dateCreated encoding="w3cdtf">2007-12-06</dateCreated><copyrightDate encoding="w3cdtf">2008</copyrightDate></originInfo><language><languageTerm type="code" authority="iso639-2b">eng</languageTerm><languageTerm type="code" authority="rfc3066">en</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType></physicalDescription><abstract>We demonstrate that low-resolution Ca ii triplet (CaT) spectroscopic estimates of the overall metallicity ([Fe/H]) of individual red giant branch (RGB) stars in two nearby dwarf spheroidal galaxies (dSphs) agree to ±0.1–0.2 dex with detailed high-resolution spectroscopic determinations for the same stars over the range −2.5 < [Fe/H] < −0.5. For this study, we used a sample of 129 stars observed in low- and high-resolution modes with VLT/FLAMES in the Sculptor and Fornax dSphs. We also present the data-reduction steps we used in our low-resolution analysis and show that the typical accuracy of our velocity and CaT [Fe/H] measurement is ∼2 km s−1 and 0.1 dex, respectively. We conclude that CaT–[Fe/H] relations calibrated on globular clusters can be applied with confidence to RGB stars in composite stellar populations over the range −2.5 < [Fe/H] < −0.5.</abstract><subject><genre>keywords</genre><topic>techniques: spectroscopic</topic><topic>stars: abundances</topic><topic>galaxies: dwarf</topic><topic>galaxies: star clusters</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><titleInfo type="abbreviated"><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="PublisherID">mnras</identifier><identifier type="PublisherID-hwp">mnras</identifier><part><date>2008</date><detail type="volume"><caption>vol.</caption><number>383</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>183</start><end>199</end></extent></part></relatedItem><identifier type="istex">11EE6D493CCBDE6D91621C48CEBADB9F0AB7EAC1</identifier><identifier type="DOI">10.1111/j.1365-2966.2007.12532.x</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2007 The Authors. 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