Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy
Identifieur interne : 00AA11 ( Main/Exploration ); précédent : 00AA10; suivant : 00AA12Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy
Auteurs : D. L. Block [Afrique du Sud] ; K. C. Freeman [Australie] ; T. H. Jarrett [États-Unis] ; I. Puerari [Mexique] ; G. Worthey [États-Unis] ; F. Combes [France] ; R. Groess [Afrique du Sud]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2004.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
Abstract
Stars with masses in the range from about 1.3 to 3.5 M◦. pass through an evolutionary stage where they become carbon stars. In this stage, which lasts a few Myr, these stars are extremely luminous pulsating giants. They are so luminous in the near-infrared that just a few of them can double the integrated luminosity of intermediate-age (0.6 to 2 Gyr) Magellanic Cloud clusters at 2.2 microns. Astronomers routinely use such near-infrared observations to minimize the effects of dust extinction, but it is precisely in this band that carbon stars can contribute hugely. The actual contribution of carbon stars to the outer disk light of evolving spiral galaxies has not previously been morphologically investigated. Here we report new and very deep near-IR images of the Triangulum spiral galaxy M 33 = NGC 598, delineating spectacular arcs of carbon stars in its outer regions. It is these arcs which dominate the near-infrared m = 2 Fourier spectra of M 33. We present near-infrared photometry with the Hale 5-m reflector, and propose that the arcs are the signature of accretion of low metallicity gas in the outer disk of M 33.
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Freeman</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Mount Stromlo and Siding Spring Observatories, Research School of Astronomy and Astrophysics, Australian National University</s1><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Mount Stromlo and Siding Spring Observatories, Research School of Astronomy and Astrophysics, Australian National University</wicri:noRegion></affiliation></author><author><name sortKey="Jarrett, T H" sort="Jarrett, T H" uniqKey="Jarrett T" first="T. H." last="Jarrett">T. H. Jarrett</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Infrared Processing and Analysis Centre, 100-22, CALTECH, 770 South Wilson Ave</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>3 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Pasadena, CA 91125</wicri:noRegion></affiliation></author><author><name sortKey="Puerari, I" sort="Puerari, I" uniqKey="Puerari I" first="I." last="Puerari">I. 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L." last="Block">D. L. Block</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Computational and Applied Mathematics, University of Witwatersrand, Private Bag 3</s1><s2>WITS 2050</s2><s3>ZAF</s3><sZ>1 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Afrique du Sud</country><wicri:noRegion>WITS 2050</wicri:noRegion></affiliation></author><author><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Mount Stromlo and Siding Spring Observatories, Research School of Astronomy and Astrophysics, Australian National University</s1><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Mount Stromlo and Siding Spring Observatories, Research School of Astronomy and Astrophysics, Australian National University</wicri:noRegion></affiliation></author><author><name sortKey="Jarrett, T H" sort="Jarrett, T H" uniqKey="Jarrett T" first="T. 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Groess</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Computational and Applied Mathematics, University of Witwatersrand, Private Bag 3</s1><s2>WITS 2050</s2><s3>ZAF</s3><sZ>1 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Afrique du Sud</country><wicri:noRegion>WITS 2050</wicri:noRegion></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2004">2004</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accretion</term><term>Age</term><term>Carbon stars</term><term>Galaxy evolution</term><term>Infrared observation</term><term>Infrared photometry</term><term>Luminosity</term><term>Magellanic Clouds</term><term>Metallicity</term><term>Spiral galaxies</term><term>Stellar mass</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Etoile carbone</term><term>Galaxies spirales</term><term>Masse stellaire</term><term>Luminosité</term><term>Age</term><term>Nuages Magellan</term><term>Observation IR</term><term>Photométrie IR</term><term>Accrétion</term><term>Métallicité</term><term>Evolution galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Stars with masses in the range from about 1.3 to 3.5 M<sub>◦.</sub> pass through an evolutionary stage where they become carbon stars. In this stage, which lasts a few Myr, these stars are extremely luminous pulsating giants. They are so luminous in the near-infrared that just a few of them can double the integrated luminosity of intermediate-age (0.6 to 2 Gyr) Magellanic Cloud clusters at 2.2 microns. Astronomers routinely use such near-infrared observations to minimize the effects of dust extinction, but it is precisely in this band that carbon stars can contribute hugely. The actual contribution of carbon stars to the outer disk light of evolving spiral galaxies has not previously been morphologically investigated. Here we report new and very deep near-IR images of the Triangulum spiral galaxy M 33 = NGC 598, delineating spectacular arcs of carbon stars in its outer regions. It is these arcs which dominate the near-infrared m = 2 Fourier spectra of M 33. We present near-infrared photometry with the Hale 5-m reflector, and propose that the arcs are the signature of accretion of low metallicity gas in the outer disk of M 33.</div></front></TEI><affiliations><list><country><li>Afrique du Sud</li><li>Australie</li><li>France</li><li>Mexique</li><li>États-Unis</li></country><region><li>Île-de-France</li></region><settlement><li>Paris</li></settlement></list><tree><country name="Afrique du Sud"><noRegion><name sortKey="Block, D L" sort="Block, D L" uniqKey="Block D" first="D. L." last="Block">D. L. Block</name></noRegion><name sortKey="Groess, R" sort="Groess, R" uniqKey="Groess R" first="R." last="Groess">R. Groess</name></country><country name="Australie"><noRegion><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name></noRegion></country><country name="États-Unis"><noRegion><name sortKey="Jarrett, T H" sort="Jarrett, T H" uniqKey="Jarrett T" first="T. H." last="Jarrett">T. H. Jarrett</name></noRegion><name sortKey="Worthey, G" sort="Worthey, G" uniqKey="Worthey G" first="G." last="Worthey">G. Worthey</name></country><country name="Mexique"><noRegion><name sortKey="Puerari, I" sort="Puerari, I" uniqKey="Puerari I" first="I." last="Puerari">I. Puerari</name></noRegion></country><country name="France"><region name="Île-de-France"><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name></region></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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