AustralieFrV1, PascalFrancis, Corpus, bibRecord, 003D03

Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud

Identifieur interne : 003D03 ( PascalFrancis/Corpus ); précédent : 003D02; suivant : 003D04

Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud

Auteurs : Eric Lagadec ; Albert A. Zijlstra ; G. C. Sloan ; Mikako Matsuura ; Peter R. Wood ; Jacco Th. Van Loon ; G. J. Harris ; J. A. D. L. Blommaert ; S. Hony ; M. A. T. Groenewegen ; M. W. Feast ; P. A. Whitelock ; J. W. Menzies ; M.-R. Cioni

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007.

RBID : Pascal:07-0188922

Descripteurs français

Pascal (Inist)
- Spectrométrie, Etoile carbone, Petit Nuage Magellan, Observation spectroscopique, Branche géante asymptotique, Grand Nuage Magellan, Galaxies, Matière interstellaire, Masse stellaire, Poussière circumstellaire, Epaisseur optique, Etoile centrale, Métallicité, Diagramme 2 couleurs, Couleur, Etoile C, Evolution thermique, Durée vie, Supergéante, Région H II compacte, Matière circumstellaire, Perte masse, Nuages Magellan, Etoile IR, Rapport carbone oxygène.

English descriptors

KwdEn :
- Asymptotic giant branch, C star, Carbon oxygen ratio, Carbon stars, Central stars, Circumstellar dust, Circumstellar matter, Color, Compact H II region, Galaxies, Infrared star, Interstellar matter, Large Magellanic Cloud, Lifetime, Magellanic Clouds, Mass loss, Metallicity, Optical thickness, Small Magellanic Cloud, Spectroscopical observation, Spectroscopy, Stellar mass, Supergiant stars, Thermal evolution, Two color diagram.

Abstract

We present Spitzer Space Telescope spectroscopic observations of 14 carbon-rich asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC). SiC dust is seen in most of the carbon-rich stars but it is weak compared to Large Magellanic Cloud (LMC) stars. The SiC feature is strong only for stars with significant dust excess, opposite to what is observed for Galactic stars. We argue that in the SMC, SiC forms at lower temperature than graphite dust, whereas in the Galaxy SiC and graphite condensate at more comparable temperatures. Dust input into the interstellar medium by AGB stars consists mostly of carbonaceous dust, with little SiC or silicate dust. Only the two coolest stars show a 30- μm band due to MgS dust. We suggest that this is due to the fact that, in the SMC, mass-losing AGB stars generally have low circumstellar (dust) optical depth and therefore effective heating of dust by the central star does not allow temperatures below the 650 K necessary for MgS to exist as a solid. Gas phase C₂H₂ bands are stronger in the SMC than in the LMC or Galaxy. This is attributed to an increasing C/O ratio at low metallicity. We present a colour-colour diagram based on Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) colours to discriminate between O- and C-rich stars. We show that AGB stars in the SMC become carbon stars early in the thermal-pulsing AGB evolution, and remain optically visible for ∼6 x 10⁵ yr. For the LMC, this lifetime is ∼3 x 10⁵ yr. The superwind phase traced with Spitzer lasts for ∼10⁴ yr. Spitzer spectra of a K supergiant and a compact H II region are also given.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A14	`10`			`@1 South African Astronomical Observatory, PO Box 9 @2 7935 Observatory @3 ZAF @Z 12 aut.`
A14	`11`			`@1 NASSP, Department of Mathematics & Applied Mathematics, University of Cape Town @2 7701 Rondebosch @3 ZAF @Z 12 aut.`
A14	`12`			`@1 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill @2 Edinburgh EH9 3HJ @3 GBR @Z 14 aut.`
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C01	`01`		`ENG`	@0 We present Spitzer Space Telescope spectroscopic observations of 14 carbon-rich asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC). SiC dust is seen in most of the carbon-rich stars but it is weak compared to Large Magellanic Cloud (LMC) stars. The SiC feature is strong only for stars with significant dust excess, opposite to what is observed for Galactic stars. We argue that in the SMC, SiC forms at lower temperature than graphite dust, whereas in the Galaxy SiC and graphite condensate at more comparable temperatures. Dust input into the interstellar medium by AGB stars consists mostly of carbonaceous dust, with little SiC or silicate dust. Only the two coolest stars show a 30- μm band due to MgS dust. We suggest that this is due to the fact that, in the SMC, mass-losing AGB stars generally have low circumstellar (dust) optical depth and therefore effective heating of dust by the central star does not allow temperatures below the 650 K necessary for MgS to exist as a solid. Gas phase C₂H₂ bands are stronger in the SMC than in the LMC or Galaxy. This is attributed to an increasing C/O ratio at low metallicity. We present a colour-colour diagram based on Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) colours to discriminate between O- and C-rich stars. We show that AGB stars in the SMC become carbon stars early in the thermal-pulsing AGB evolution, and remain optically visible for ∼6 x 10⁵ yr. For the LMC, this lifetime is ∼3 x 10⁵ yr. The superwind phase traced with Spitzer lasts for ∼10⁴ yr. Spitzer spectra of a K supergiant and a compact H II region are also given.
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C03	`06`	`3`	`FRE`	`@0 Grand Nuage Magellan @5 31`
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C03	`07`	`3`	`FRE`	`@0 Galaxies @5 32`
C03	`07`	`3`	`ENG`	`@0 Galaxies @5 32`
C03	`08`	`3`	`FRE`	`@0 Matière interstellaire @5 33`
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C03	`09`	`3`	`FRE`	`@0 Masse stellaire @5 34`
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C03	`10`	`X`	`FRE`	`@0 Poussière circumstellaire @5 35`
C03	`10`	`X`	`ENG`	`@0 Circumstellar dust @5 35`
C03	`10`	`X`	`SPA`	`@0 Polvo circunstelar @5 35`
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C03	`11`	`X`	`ENG`	`@0 Optical thickness @5 36`
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C03	`25`	`3`	`FRE`	`@0 Rapport carbone oxygène @4 CD @5 96`
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Format Inist (serveur)

NO :	PASCAL 07-0188922 INIST
ET :	Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud
AU :	LAGADEC (Eric); ZIJLSTRA (Albert A.); SLOAN (G. C.); MATSUURA (Mikako); WOOD (Peter R.); VAN LOON (Jacco Th.); HARRIS (G. J.); BLOMMAERT (J. A. D. L.); HONY (S.); GROENEWEGEN (M. A. T.); FEAST (M. W.); WHITELOCK (P. A.); MENZIES (J. W.); CIONI (M.-R.)
AF :	University of Manchester School of Physics & Astronomy, PO Box 88/Manchester M60 1QD/Royaume-Uni (1 aut., 2 aut., 4 aut.); Department of Astronomy, Cornell University, 108 Space Sciences Building/Ithaca, NY 14853-6801/Etats-Unis (3 aut.); Division of Optical and IR Astronomy, National Astronomical Observatory of Japan, Osawa 2-21-1/Mitaka, Tokyo 181-8588/Japon (4 aut.); Research School of Astronomy and Astrophysics, Australian National University, Cotter Road/Weston Creek, ACT 2611/Australie (5 aut.); Astrophysics Group, School of Physical & Geographical Sciences, Keele University/Staffordshire ST5 5BG/Royaume-Uni (6 aut.); Department of Physics and Astronomy, University College London, Gower Street/London WC1E 6BT/Royaume-Uni (7 aut.); Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200 D/3001 Leuven/Belgique (8 aut., 10 aut.); CEA, DSM, DAPNIA, Service d'Astrophysique, C.E. Saclay/91191 Gif-sur-Yvette/France (9 aut.); Department of Astronomy, University of Cape Town/7701 Rondebosch/Afrique du Sud (11 aut., 12 aut., 13 aut.); South African Astronomical Observatory, PO Box 9/7935 Observatory/Afrique du Sud (12 aut.); NASSP, Department of Mathematics & Applied Mathematics, University of Cape Town/7701 Rondebosch/Afrique du Sud (12 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (14 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2007; Vol. 376; No. 3; Pp. 1270-1284; Bibl. 3/4 p.
LA :	Anglais
EA :	We present Spitzer Space Telescope spectroscopic observations of 14 carbon-rich asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC). SiC dust is seen in most of the carbon-rich stars but it is weak compared to Large Magellanic Cloud (LMC) stars. The SiC feature is strong only for stars with significant dust excess, opposite to what is observed for Galactic stars. We argue that in the SMC, SiC forms at lower temperature than graphite dust, whereas in the Galaxy SiC and graphite condensate at more comparable temperatures. Dust input into the interstellar medium by AGB stars consists mostly of carbonaceous dust, with little SiC or silicate dust. Only the two coolest stars show a 30- μm band due to MgS dust. We suggest that this is due to the fact that, in the SMC, mass-losing AGB stars generally have low circumstellar (dust) optical depth and therefore effective heating of dust by the central star does not allow temperatures below the 650 K necessary for MgS to exist as a solid. Gas phase C₂H₂ bands are stronger in the SMC than in the LMC or Galaxy. This is attributed to an increasing C/O ratio at low metallicity. We present a colour-colour diagram based on Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) colours to discriminate between O- and C-rich stars. We show that AGB stars in the SMC become carbon stars early in the thermal-pulsing AGB evolution, and remain optically visible for ∼6 x 10⁵ yr. For the LMC, this lifetime is ∼3 x 10⁵ yr. The superwind phase traced with Spitzer lasts for ∼10⁴ yr. Spitzer spectra of a K supergiant and a compact H II region are also given.
CC :	001E03
FD :	Spectrométrie; Etoile carbone; Petit Nuage Magellan; Observation spectroscopique; Branche géante asymptotique; Grand Nuage Magellan; Galaxies; Matière interstellaire; Masse stellaire; Poussière circumstellaire; Epaisseur optique; Etoile centrale; Métallicité; Diagramme 2 couleurs; Couleur; Etoile C; Evolution thermique; Durée vie; Supergéante; Région H II compacte; Matière circumstellaire; Perte masse; Nuages Magellan; Etoile IR; Rapport carbone oxygène
ED :	Spectroscopy; Carbon stars; Small Magellanic Cloud; Spectroscopical observation; Asymptotic giant branch; Large Magellanic Cloud; Galaxies; Interstellar matter; Stellar mass; Circumstellar dust; Optical thickness; Central stars; Metallicity; Two color diagram; Color; C star; Thermal evolution; Lifetime; Supergiant stars; Compact H II region; Circumstellar matter; Mass loss; Magellanic Clouds; Infrared star; Carbon oxygen ratio
SD :	Observación espectroscópica; Rama gigante asintótica; Polvo circunstelar; Espesor óptico; Metalicidad; Diagrama 2 colores; Estrella C; Evolución térmica; Región H II compacta; Estrella IR; Relación carbono oxígeno
LO :	INIST-2067.354000147122370300
ID :	07-0188922

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Pascal:07-0188922

Le document en format XML

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<author><name sortKey="Whitelock, P A" sort="Whitelock, P A" uniqKey="Whitelock P" first="P. A." last="Whitelock">P. A. Whitelock</name>
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<affiliation><inist:fA14 i1="09"><s1>Department of Astronomy, University of Cape Town</s1>
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<sZ>11 aut.</sZ>
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<affiliation><inist:fA14 i1="09"><s1>Department of Astronomy, University of Cape Town</s1>
<s2>7701 Rondebosch</s2>
<s3>ZAF</s3>
<sZ>11 aut.</sZ>
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</affiliation>
<affiliation><inist:fA14 i1="10"><s1>South African Astronomical Observatory, PO Box 9</s1>
<s2>7935 Observatory</s2>
<s3>ZAF</s3>
<sZ>12 aut.</sZ>
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<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Asymptotic giant branch</term>
<term>C star</term>
<term>Carbon oxygen ratio</term>
<term>Carbon stars</term>
<term>Central stars</term>
<term>Circumstellar dust</term>
<term>Circumstellar matter</term>
<term>Color</term>
<term>Compact H II region</term>
<term>Galaxies</term>
<term>Infrared star</term>
<term>Interstellar matter</term>
<term>Large Magellanic Cloud</term>
<term>Lifetime</term>
<term>Magellanic Clouds</term>
<term>Mass loss</term>
<term>Metallicity</term>
<term>Optical thickness</term>
<term>Small Magellanic Cloud</term>
<term>Spectroscopical observation</term>
<term>Spectroscopy</term>
<term>Stellar mass</term>
<term>Supergiant stars</term>
<term>Thermal evolution</term>
<term>Two color diagram</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Spectrométrie</term>
<term>Etoile carbone</term>
<term>Petit Nuage Magellan</term>
<term>Observation spectroscopique</term>
<term>Branche géante asymptotique</term>
<term>Grand Nuage Magellan</term>
<term>Galaxies</term>
<term>Matière interstellaire</term>
<term>Masse stellaire</term>
<term>Poussière circumstellaire</term>
<term>Epaisseur optique</term>
<term>Etoile centrale</term>
<term>Métallicité</term>
<term>Diagramme 2 couleurs</term>
<term>Couleur</term>
<term>Etoile C</term>
<term>Evolution thermique</term>
<term>Durée vie</term>
<term>Supergéante</term>
<term>Région H II compacte</term>
<term>Matière circumstellaire</term>
<term>Perte masse</term>
<term>Nuages Magellan</term>
<term>Etoile IR</term>
<term>Rapport carbone oxygène</term>
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<front><div type="abstract" xml:lang="en">We present Spitzer Space Telescope spectroscopic observations of 14 carbon-rich asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC). SiC dust is seen in most of the carbon-rich stars but it is weak compared to Large Magellanic Cloud (LMC) stars. The SiC feature is strong only for stars with significant dust excess, opposite to what is observed for Galactic stars. We argue that in the SMC, SiC forms at lower temperature than graphite dust, whereas in the Galaxy SiC and graphite condensate at more comparable temperatures. Dust input into the interstellar medium by AGB stars consists mostly of carbonaceous dust, with little SiC or silicate dust. Only the two coolest stars show a 30- μm band due to MgS dust. We suggest that this is due to the fact that, in the SMC, mass-losing AGB stars generally have low circumstellar (dust) optical depth and therefore effective heating of dust by the central star does not allow temperatures below the 650 K necessary for MgS to exist as a solid. Gas phase C<sub>2</sub>
H<sub>2</sub>
 bands are stronger in the SMC than in the LMC or Galaxy. This is attributed to an increasing C/O ratio at low metallicity. We present a colour-colour diagram based on Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) colours to discriminate between O- and C-rich stars. We show that AGB stars in the SMC become carbon stars early in the thermal-pulsing AGB evolution, and remain optically visible for ∼6 x 10<sup>5</sup>
 yr. For the LMC, this lifetime is ∼3 x 10<sup>5</sup>
 yr. The superwind phase traced with Spitzer lasts for ∼10<sup>4</sup>
 yr. Spitzer spectra of a K supergiant and a compact H II region are also given.</div>
</front>
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<fA08 i1="01" i2="1" l="ENG"><s1>Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud</s1>
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<sZ>6 aut.</sZ>
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<s2>3001 Leuven</s2>
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<sZ>8 aut.</sZ>
<sZ>10 aut.</sZ>
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<fA14 i1="08"><s1>CEA, DSM, DAPNIA, Service d'Astrophysique, C.E. Saclay</s1>
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<sZ>9 aut.</sZ>
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<fA14 i1="09"><s1>Department of Astronomy, University of Cape Town</s1>
<s2>7701 Rondebosch</s2>
<s3>ZAF</s3>
<sZ>11 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
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<fA14 i1="10"><s1>South African Astronomical Observatory, PO Box 9</s1>
<s2>7935 Observatory</s2>
<s3>ZAF</s3>
<sZ>12 aut.</sZ>
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<fA14 i1="11"><s1>NASSP, Department of Mathematics & Applied Mathematics, University of Cape Town</s1>
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<s3>ZAF</s3>
<sZ>12 aut.</sZ>
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<fA14 i1="12"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1>
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H<sub>2</sub>
 bands are stronger in the SMC than in the LMC or Galaxy. This is attributed to an increasing C/O ratio at low metallicity. We present a colour-colour diagram based on Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) colours to discriminate between O- and C-rich stars. We show that AGB stars in the SMC become carbon stars early in the thermal-pulsing AGB evolution, and remain optically visible for ∼6 x 10<sup>5</sup>
 yr. For the LMC, this lifetime is ∼3 x 10<sup>5</sup>
 yr. The superwind phase traced with Spitzer lasts for ∼10<sup>4</sup>
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<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Masse stellaire</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Stellar mass</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Poussière circumstellaire</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="ENG"><s0>Circumstellar dust</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="SPA"><s0>Polvo circunstelar</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="X" l="FRE"><s0>Epaisseur optique</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="X" l="ENG"><s0>Optical thickness</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="X" l="SPA"><s0>Espesor óptico</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="3" l="FRE"><s0>Etoile centrale</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="3" l="ENG"><s0>Central stars</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="X" l="FRE"><s0>Métallicité</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="ENG"><s0>Metallicity</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="SPA"><s0>Metalicidad</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE"><s0>Diagramme 2 couleurs</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="ENG"><s0>Two color diagram</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="SPA"><s0>Diagrama 2 colores</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="3" l="FRE"><s0>Couleur</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="3" l="ENG"><s0>Color</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="X" l="FRE"><s0>Etoile C</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="ENG"><s0>C star</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="SPA"><s0>Estrella C</s0>
<s5>41</s5>
</fC03>
<fC03 i1="17" i2="X" l="FRE"><s0>Evolution thermique</s0>
<s5>42</s5>
</fC03>
<fC03 i1="17" i2="X" l="ENG"><s0>Thermal evolution</s0>
<s5>42</s5>
</fC03>
<fC03 i1="17" i2="X" l="SPA"><s0>Evolución térmica</s0>
<s5>42</s5>
</fC03>
<fC03 i1="18" i2="3" l="FRE"><s0>Durée vie</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="3" l="ENG"><s0>Lifetime</s0>
<s5>43</s5>
</fC03>
<fC03 i1="19" i2="3" l="FRE"><s0>Supergéante</s0>
<s5>44</s5>
</fC03>
<fC03 i1="19" i2="3" l="ENG"><s0>Supergiant stars</s0>
<s5>44</s5>
</fC03>
<fC03 i1="20" i2="X" l="FRE"><s0>Région H II compacte</s0>
<s5>45</s5>
</fC03>
<fC03 i1="20" i2="X" l="ENG"><s0>Compact H II region</s0>
<s5>45</s5>
</fC03>
<fC03 i1="20" i2="X" l="SPA"><s0>Región H II compacta</s0>
<s5>45</s5>
</fC03>
<fC03 i1="21" i2="3" l="FRE"><s0>Matière circumstellaire</s0>
<s5>46</s5>
</fC03>
<fC03 i1="21" i2="3" l="ENG"><s0>Circumstellar matter</s0>
<s5>46</s5>
</fC03>
<fC03 i1="22" i2="3" l="FRE"><s0>Perte masse</s0>
<s5>47</s5>
</fC03>
<fC03 i1="22" i2="3" l="ENG"><s0>Mass loss</s0>
<s5>47</s5>
</fC03>
<fC03 i1="23" i2="3" l="FRE"><s0>Nuages Magellan</s0>
<s5>48</s5>
</fC03>
<fC03 i1="23" i2="3" l="ENG"><s0>Magellanic Clouds</s0>
<s5>48</s5>
</fC03>
<fC03 i1="24" i2="X" l="FRE"><s0>Etoile IR</s0>
<s5>49</s5>
</fC03>
<fC03 i1="24" i2="X" l="ENG"><s0>Infrared star</s0>
<s5>49</s5>
</fC03>
<fC03 i1="24" i2="X" l="SPA"><s0>Estrella IR</s0>
<s5>49</s5>
</fC03>
<fC03 i1="25" i2="3" l="FRE"><s0>Rapport carbone oxygène</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fC03 i1="25" i2="3" l="ENG"><s0>Carbon oxygen ratio</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fC03 i1="25" i2="3" l="SPA"><s0>Relación carbono oxígeno</s0>
<s4>CD</s4>
<s5>96</s5>
</fC03>
<fN21><s1>128</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 07-0188922 INIST</NO>
<ET>Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud</ET>
<AU>LAGADEC (Eric); ZIJLSTRA (Albert A.); SLOAN (G. C.); MATSUURA (Mikako); WOOD (Peter R.); VAN LOON (Jacco Th.); HARRIS (G. J.); BLOMMAERT (J. A. D. L.); HONY (S.); GROENEWEGEN (M. A. T.); FEAST (M. W.); WHITELOCK (P. A.); MENZIES (J. W.); CIONI (M.-R.)</AU>
<AF>University of Manchester School of Physics & Astronomy, PO Box 88/Manchester M60 1QD/Royaume-Uni (1 aut., 2 aut., 4 aut.); Department of Astronomy, Cornell University, 108 Space Sciences Building/Ithaca, NY 14853-6801/Etats-Unis (3 aut.); Division of Optical and IR Astronomy, National Astronomical Observatory of Japan, Osawa 2-21-1/Mitaka, Tokyo 181-8588/Japon (4 aut.); Research School of Astronomy and Astrophysics, Australian National University, Cotter Road/Weston Creek, ACT 2611/Australie (5 aut.); Astrophysics Group, School of Physical & Geographical Sciences, Keele University/Staffordshire ST5 5BG/Royaume-Uni (6 aut.); Department of Physics and Astronomy, University College London, Gower Street/London WC1E 6BT/Royaume-Uni (7 aut.); Instituut voor Sterrenkunde, K. U. Leuven, Celestijnenlaan 200 D/3001 Leuven/Belgique (8 aut., 10 aut.); CEA, DSM, DAPNIA, Service d'Astrophysique, C.E. Saclay/91191 Gif-sur-Yvette/France (9 aut.); Department of Astronomy, University of Cape Town/7701 Rondebosch/Afrique du Sud (11 aut., 12 aut., 13 aut.); South African Astronomical Observatory, PO Box 9/7935 Observatory/Afrique du Sud (12 aut.); NASSP, Department of Mathematics & Applied Mathematics, University of Cape Town/7701 Rondebosch/Afrique du Sud (12 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (14 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2007; Vol. 376; No. 3; Pp. 1270-1284; Bibl. 3/4 p.</SO>
<LA>Anglais</LA>
<EA>We present Spitzer Space Telescope spectroscopic observations of 14 carbon-rich asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC). SiC dust is seen in most of the carbon-rich stars but it is weak compared to Large Magellanic Cloud (LMC) stars. The SiC feature is strong only for stars with significant dust excess, opposite to what is observed for Galactic stars. We argue that in the SMC, SiC forms at lower temperature than graphite dust, whereas in the Galaxy SiC and graphite condensate at more comparable temperatures. Dust input into the interstellar medium by AGB stars consists mostly of carbonaceous dust, with little SiC or silicate dust. Only the two coolest stars show a 30- μm band due to MgS dust. We suggest that this is due to the fact that, in the SMC, mass-losing AGB stars generally have low circumstellar (dust) optical depth and therefore effective heating of dust by the central star does not allow temperatures below the 650 K necessary for MgS to exist as a solid. Gas phase C<sub>2</sub>
H<sub>2</sub>
 bands are stronger in the SMC than in the LMC or Galaxy. This is attributed to an increasing C/O ratio at low metallicity. We present a colour-colour diagram based on Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) colours to discriminate between O- and C-rich stars. We show that AGB stars in the SMC become carbon stars early in the thermal-pulsing AGB evolution, and remain optically visible for ∼6 x 10<sup>5</sup>
 yr. For the LMC, this lifetime is ∼3 x 10<sup>5</sup>
 yr. The superwind phase traced with Spitzer lasts for ∼10<sup>4</sup>
 yr. Spitzer spectra of a K supergiant and a compact H II region are also given.</EA>
<CC>001E03</CC>
<FD>Spectrométrie; Etoile carbone; Petit Nuage Magellan; Observation spectroscopique; Branche géante asymptotique; Grand Nuage Magellan; Galaxies; Matière interstellaire; Masse stellaire; Poussière circumstellaire; Epaisseur optique; Etoile centrale; Métallicité; Diagramme 2 couleurs; Couleur; Etoile C; Evolution thermique; Durée vie; Supergéante; Région H II compacte; Matière circumstellaire; Perte masse; Nuages Magellan; Etoile IR; Rapport carbone oxygène</FD>
<ED>Spectroscopy; Carbon stars; Small Magellanic Cloud; Spectroscopical observation; Asymptotic giant branch; Large Magellanic Cloud; Galaxies; Interstellar matter; Stellar mass; Circumstellar dust; Optical thickness; Central stars; Metallicity; Two color diagram; Color; C star; Thermal evolution; Lifetime; Supergiant stars; Compact H II region; Circumstellar matter; Mass loss; Magellanic Clouds; Infrared star; Carbon oxygen ratio</ED>
<SD>Observación espectroscópica; Rama gigante asintótica; Polvo circunstelar; Espesor óptico; Metalicidad; Diagrama 2 colores; Estrella C; Evolución térmica; Región H II compacta; Estrella IR; Relación carbono oxígeno</SD>
<LO>INIST-2067.354000147122370300</LO>
<ID>07-0188922</ID>
</server>
</inist>
</record>

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Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud

Spitzer spectroscopy of carbon stars in the Small Magellanic Cloud

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