AustralieFrV1, PascalFrancis, Corpus, bibRecord, 004C62

Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy

Identifieur interne : 004C62 ( PascalFrancis/Corpus ); précédent : 004C61; suivant : 004C63

Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy

Auteurs : D. L. Block ; K. C. Freeman ; T. H. Jarrett ; I. Puerari ; G. Worthey ; F. Combes ; R. Groess

Source :

Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2004.

RBID : Pascal:04-0541978

Descripteurs français

Pascal (Inist)
- Etoile carbone, Galaxies spirales, Masse stellaire, Luminosité, Age, Nuages Magellan, Observation IR, Photométrie IR, Accrétion, Métallicité, Evolution galaxies.

English descriptors

KwdEn :
- Accretion, Age, Carbon stars, Galaxy evolution, Infrared observation, Infrared photometry, Luminosity, Magellanic Clouds, Metallicity, Spiral galaxies, Stellar mass.

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.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A08	`01`	`1`	`ENG`	`@1 Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy`
A11	`01`	`1`		`@1 BLOCK (D. L.)`
A11	`02`	`1`		`@1 FREEMAN (K. C.)`
A11	`03`	`1`		`@1 JARRETT (T. H.)`
A11	`04`	`1`		`@1 PUERARI (I.)`
A11	`05`	`1`		`@1 WORTHEY (G.)`
A11	`06`	`1`		`@1 COMBES (F.)`
A11	`07`	`1`		`@1 GROESS (R.)`
A14	`01`			`@1 School of Computational and Applied Mathematics, University of Witwatersrand, Private Bag 3 @2 WITS 2050 @3 ZAF @Z 1 aut. @Z 7 aut.`
A14	`02`			`@1 Mount Stromlo and Siding Spring Observatories, Research School of Astronomy and Astrophysics, Australian National University @3 AUS @Z 2 aut.`
A14	`03`			`@1 Infrared Processing and Analysis Centre, 100-22, CALTECH, 770 South Wilson Ave @2 Pasadena, CA 91125 @3 USA @Z 3 aut.`
A14	`04`			`@1 Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1 @2 72840 Tonantzintla, Puebla @3 MEX @Z 4 aut.`
A14	`05`			`@1 Washington State University, 1245 Webster Hall @2 Pullman, WA 99163-2814 @3 USA @Z 5 aut.`
A14	`06`			`@1 Observatoire de Paris, LERMA, 61 Av. de l'Observatoire @2 75014 Paris @3 FRA @Z 6 aut.`
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A23	`01`			`@0 ENG`
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A44				`@0 0000 @1 © 2004 INIST-CNRS. All rights reserved.`
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C01	`01`		`ENG`	@0 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.
C02	`01`	`3`		`@0 001E03`
C03	`01`	`3`	`FRE`	`@0 Etoile carbone @2 NO @5 26`
C03	`01`	`3`	`ENG`	`@0 Carbon stars @2 NO @5 26`
C03	`02`	`3`	`FRE`	`@0 Galaxies spirales @5 27`
C03	`02`	`3`	`ENG`	`@0 Spiral galaxies @5 27`
C03	`03`	`3`	`FRE`	`@0 Masse stellaire @5 28`
C03	`03`	`3`	`ENG`	`@0 Stellar mass @5 28`
C03	`04`	`3`	`FRE`	`@0 Luminosité @5 29`
C03	`04`	`3`	`ENG`	`@0 Luminosity @5 29`
C03	`05`	`X`	`FRE`	`@0 Age @5 30`
C03	`05`	`X`	`ENG`	`@0 Age @5 30`
C03	`05`	`X`	`SPA`	`@0 Edad @5 30`
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C03	`06`	`3`	`ENG`	`@0 Magellanic Clouds @5 31`
C03	`07`	`X`	`FRE`	`@0 Observation IR @5 32`
C03	`07`	`X`	`ENG`	`@0 Infrared observation @5 32`
C03	`07`	`X`	`SPA`	`@0 Observación IR @5 32`
C03	`08`	`X`	`FRE`	`@0 Photométrie IR @5 33`
C03	`08`	`X`	`ENG`	`@0 Infrared photometry @5 33`
C03	`08`	`X`	`SPA`	`@0 Fotometría IR @5 33`
C03	`09`	`3`	`FRE`	`@0 Accrétion @5 34`
C03	`09`	`3`	`ENG`	`@0 Accretion @5 34`
C03	`10`	`X`	`FRE`	`@0 Métallicité @5 35`
C03	`10`	`X`	`ENG`	`@0 Metallicity @5 35`
C03	`10`	`X`	`SPA`	`@0 Metalicidad @5 35`
C03	`11`	`3`	`FRE`	`@0 Evolution galaxies @4 CD @5 96`
C03	`11`	`3`	`ENG`	`@0 Galaxy evolution @4 CD @5 96`
C03	`11`	`3`	`SPA`	`@0 Evolución galaxias @4 CD @5 96`
N21				`@1 306`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 04-0541978 INIST
ET :	Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy
AU :	BLOCK (D. L.); FREEMAN (K. C.); JARRETT (T. H.); PUERARI (I.); WORTHEY (G.); COMBES (F.); GROESS (R.)
AF :	School of Computational and Applied Mathematics, University of Witwatersrand, Private Bag 3/WITS 2050/Afrique du Sud (1 aut., 7 aut.); Mount Stromlo and Siding Spring Observatories, Research School of Astronomy and Astrophysics, Australian National University/Australie (2 aut.); Infrared Processing and Analysis Centre, 100-22, CALTECH, 770 South Wilson Ave/Pasadena, CA 91125/Etats-Unis (3 aut.); Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1/72840 Tonantzintla, Puebla/Mexique (4 aut.); Washington State University, 1245 Webster Hall/Pullman, WA 99163-2814/Etats-Unis (5 aut.); Observatoire de Paris, LERMA, 61 Av. de l'Observatoire/75014 Paris/France (6 aut.)
DT :	Publication en série; Lettre à l'éditeur; Niveau analytique
SO :	Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2004; Vol. 425; No. 3; L37-L40; Bibl. 18 ref.
LA :	Anglais
EA :	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.
CC :	001E03
FD :	Etoile carbone; Galaxies spirales; Masse stellaire; Luminosité; Age; Nuages Magellan; Observation IR; Photométrie IR; Accrétion; Métallicité; Evolution galaxies
ED :	Carbon stars; Spiral galaxies; Stellar mass; Luminosity; Age; Magellanic Clouds; Infrared observation; Infrared photometry; Accretion; Metallicity; Galaxy evolution
SD :	Edad; Observación IR; Fotometría IR; Metalicidad; Evolución galaxias
LO :	INIST-14176.354000114213110010
ID :	04-0541978

Links to Exploration step

Pascal:04-0541978

Le document en format XML

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<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>
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<fC01 i1="01" l="ENG"><s0>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.</s0>
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<fC03 i1="01" i2="3" l="FRE"><s0>Etoile carbone</s0>
<s2>NO</s2>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Carbon stars</s0>
<s2>NO</s2>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="3" l="FRE"><s0>Galaxies spirales</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="3" l="ENG"><s0>Spiral galaxies</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Masse stellaire</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Stellar mass</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE"><s0>Luminosité</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG"><s0>Luminosity</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="X" l="FRE"><s0>Age</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="ENG"><s0>Age</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA"><s0>Edad</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Nuages Magellan</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Magellanic Clouds</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Observation IR</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Infrared observation</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Observación IR</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="X" l="FRE"><s0>Photométrie IR</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="ENG"><s0>Infrared photometry</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="SPA"><s0>Fotometría IR</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Accrétion</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Accretion</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Métallicité</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="ENG"><s0>Metallicity</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="SPA"><s0>Metalicidad</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Evolution galaxies</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Galaxy evolution</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fC03 i1="11" i2="3" l="SPA"><s0>Evolución galaxias</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fN21><s1>306</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 04-0541978 INIST</NO>
<ET>Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy</ET>
<AU>BLOCK (D. L.); FREEMAN (K. C.); JARRETT (T. H.); PUERARI (I.); WORTHEY (G.); COMBES (F.); GROESS (R.)</AU>
<AF>School of Computational and Applied Mathematics, University of Witwatersrand, Private Bag 3/WITS 2050/Afrique du Sud (1 aut., 7 aut.); Mount Stromlo and Siding Spring Observatories, Research School of Astronomy and Astrophysics, Australian National University/Australie (2 aut.); Infrared Processing and Analysis Centre, 100-22, CALTECH, 770 South Wilson Ave/Pasadena, CA 91125/Etats-Unis (3 aut.); Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1/72840 Tonantzintla, Puebla/Mexique (4 aut.); Washington State University, 1245 Webster Hall/Pullman, WA 99163-2814/Etats-Unis (5 aut.); Observatoire de Paris, LERMA, 61 Av. de l'Observatoire/75014 Paris/France (6 aut.)</AF>
<DT>Publication en série; Lettre à l'éditeur; Niveau analytique</DT>
<SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2004; Vol. 425; No. 3; L37-L40; Bibl. 18 ref.</SO>
<LA>Anglais</LA>
<EA>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.</EA>
<CC>001E03</CC>
<FD>Etoile carbone; Galaxies spirales; Masse stellaire; Luminosité; Age; Nuages Magellan; Observation IR; Photométrie IR; Accrétion; Métallicité; Evolution galaxies</FD>
<ED>Carbon stars; Spiral galaxies; Stellar mass; Luminosity; Age; Magellanic Clouds; Infrared observation; Infrared photometry; Accretion; Metallicity; Galaxy evolution</ED>
<SD>Edad; Observación IR; Fotometría IR; Metalicidad; Evolución galaxias</SD>
<LO>INIST-14176.354000114213110010</LO>
<ID>04-0541978</ID>
</server>
</inist>
</record>

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Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy

Very luminous carbon stars in the outer disk of the Triangulum spiral galaxy

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