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Spitzer observations of acetylene bands in carbon-rich asymptotic giant branch stars in the Large Magellanic Cloud

Identifieur interne : 000928 ( Istex/Curation ); précédent : 000927; suivant : 000929

Spitzer observations of acetylene bands in carbon-rich asymptotic giant branch stars in the Large Magellanic Cloud

Auteurs : M. Matsuura [Royaume-Uni, Japon] ; P. R. Wood [Australie] ; G. C. Sloan [États-Unis] ; A. A. Zijlstra [Royaume-Uni] ; J. Th. Van Loon ; M. A. T. Groenewegen [Belgique] ; J. A. D. L. Blommaert [Belgique] ; M.-R. L. Cioni [Royaume-Uni] ; M. W. Feast [Afrique du Sud] ; H. J. Habing [Pays-Bas] ; S. Hony [Belgique] ; E. Lagadec [Royaume-Uni] ; C. Loup [France] ; J. W. Menzies [Afrique du Sud] ; L. B. F. M. Waters [Belgique, Pays-Bas] ; P. A. Whitelock [Afrique du Sud]

Source :

RBID : ISTEX:3069AFB278002056B5714EDFEBC47026C848B163

Abstract

We investigate the molecular bands in carbon-rich asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), using the Infrared Spectrograph (IRS) onboard the Spitzer Space Telescope (SST) over the 5–38 μm range. All 26 low-resolution spectra show acetylene (C2H2) bands at 7 and 14 μm. The hydrogen cyanide (HCN) bands at these wavelengths are very weak or absent. This is consistent with low nitrogen abundances in the LMC. The observed 14 μm C2H2  band is reasonably reproduced by an excitation temperature of 500 K. There is no clear dilution of the 14 μm C2H2  band by circumstellar dust emission. This 14-μm band originates from molecular gas in the circumstellar envelope in these high mass-loss rate stars, in agreement with previous findings for Galactic stars. The C2H2 column density, derived from the 13.7 μm band, shows a gas mass-loss rate in the range 3 × 10−6 to 5 × 10−5 M⊙ yr−1. This is comparable with the total mass-loss rate of these stars estimated from the spectral energy distribution. Additionally, we compare the line strengths of the 13.7 μm C2H2  band of our LMC sample with those of a Galactic sample. Despite the low metallicity of the LMC, there is no clear difference in the C2H2  abundance among LMC and Galactic stars. This reflects the effect of the third dredge-up bringing self-produced carbon to the surface, leading to high carbon-to-oxygen ratio at low metallicity.

Url:
DOI: 10.1111/j.1365-2966.2006.10664.x

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ISTEX:3069AFB278002056B5714EDFEBC47026C848B163

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J. Th. Van Loon
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<mods:affiliation>Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium</mods:affiliation>
<country xml:lang="fr">Belgique</country>
<wicri:regionArea>Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200B, 3001 Leuven</wicri:regionArea>
</affiliation>
<affiliation wicri:level="1">
<mods:affiliation>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, the Netherlands</mods:affiliation>
<country xml:lang="fr" wicri:curation="lc">Pays-Bas</country>
<wicri:regionArea>Astronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam</wicri:regionArea>
</affiliation>
</author>
<author>
<name sortKey="Whitelock, P A" sort="Whitelock, P A" uniqKey="Whitelock P" first="P. A." last="Whitelock">P. A. Whitelock</name>
<affiliation wicri:level="1">
<mods:affiliation>Astronomy Department, University of Cape Town, 7701 Rondebosch, South Africa</mods:affiliation>
<country xml:lang="fr">Afrique du Sud</country>
<wicri:regionArea>Astronomy Department, University of Cape Town, 7701 Rondebosch</wicri:regionArea>
</affiliation>
<affiliation wicri:level="1">
<mods:affiliation>South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa</mods:affiliation>
<country xml:lang="fr">Afrique du Sud</country>
<wicri:regionArea>South African Astronomical Observatory, PO Box 9, 7935 Observatory</wicri:regionArea>
</affiliation>
<affiliation wicri:level="1">
<mods:affiliation>NASSP, Department of Mathematics and Applied Mathematics, University of Cape Town, 7701 Rondebosch, South Africa</mods:affiliation>
<country xml:lang="fr">Afrique du Sud</country>
<wicri:regionArea>NASSP, Department of Mathematics and Applied Mathematics, University of Cape Town, 7701 Rondebosch</wicri:regionArea>
</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="2006-09-01">2006-09-01</date>
<biblScope unit="volume">371</biblScope>
<biblScope unit="issue">1</biblScope>
<biblScope unit="page" from="415">415</biblScope>
<biblScope unit="page" to="420">420</biblScope>
</imprint>
<idno type="ISSN">0035-8711</idno>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt>
<idno type="ISSN">0035-8711</idno>
</seriesStmt>
</fileDesc>
<profileDesc>
<textClass></textClass>
</profileDesc>
</teiHeader>
<front>
<div type="abstract">We investigate the molecular bands in carbon-rich asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), using the Infrared Spectrograph (IRS) onboard the Spitzer Space Telescope (SST) over the 5–38 μm range. All 26 low-resolution spectra show acetylene (C2H2) bands at 7 and 14 μm. The hydrogen cyanide (HCN) bands at these wavelengths are very weak or absent. This is consistent with low nitrogen abundances in the LMC. The observed 14 μm C2H2  band is reasonably reproduced by an excitation temperature of 500 K. There is no clear dilution of the 14 μm C2H2  band by circumstellar dust emission. This 14-μm band originates from molecular gas in the circumstellar envelope in these high mass-loss rate stars, in agreement with previous findings for Galactic stars. The C2H2 column density, derived from the 13.7 μm band, shows a gas mass-loss rate in the range 3 × 10−6 to 5 × 10−5 M⊙ yr−1. This is comparable with the total mass-loss rate of these stars estimated from the spectral energy distribution. Additionally, we compare the line strengths of the 13.7 μm C2H2  band of our LMC sample with those of a Galactic sample. Despite the low metallicity of the LMC, there is no clear difference in the C2H2  abundance among LMC and Galactic stars. This reflects the effect of the third dredge-up bringing self-produced carbon to the surface, leading to high carbon-to-oxygen ratio at low metallicity.</div>
</front>
</TEI>
</record>

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