A Spitzer mid‐infrared spectral survey of mass‐losing carbon stars in the Large Magellanic Cloud
Identifieur interne : 001D89 ( Istex/Curation ); précédent : 001D88; suivant : 001D90A Spitzer mid‐infrared spectral survey of mass‐losing carbon stars in the Large Magellanic Cloud
Auteurs : Albert A. Zijlstra [Royaume-Uni] ; Mikako Matsuura [Royaume-Uni] ; Peter R. Wood [Australie] ; G. C. Sloan [États-Unis] ; Eric Lagadec [Royaume-Uni] ; Jacco Th. Van Loon ; M. A. T. Groenewegen [Belgique] ; M. W. Feast [Afrique du Sud] ; J. W. Menzies [Afrique du Sud] ; P. A. Whitelock [Afrique du Sud] ; J. A. D. L. Blommaert [Belgique] ; M. L. Cioni [Royaume-Uni] ; H. J. Habing [Pays-Bas] ; S. Hony [Belgique] ; C. Loup [France] ; L. B. F. M. Waters [Pays-Bas]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2006-08-21.
English descriptors
- KwdEn :
- 2mass, 2mass data, Absorption, Absorption bands, Absorption feature, Amorphous carbon dust, Aoki, Asymptotic giant branch, Average spectrum, Background emission, Background measurement, Best example, Blackbody, Blue carbon stars, Blue continuum, Blue edge, Blue spectra, Bluer colours, Bolometric, Bolometric magnitudes, Bottom panel, Broad absorption band, Broad component, Cape town, Carbon star, Carbon star sequence, Carbon stars, Carbonaceous dust, Carbonyl, Carbonyl group, Carbonyl groups, Central wavelength, Central wavelengths, Cernicharo, Colour, Colour range, Colours, Continuum, Continuum bands, Continuum colours, Continuum determination, Continuum temperatures, Crystalline silicate features, Current sample, Data points, Distance modulus, Dust bands, Dust continuum, Dust emission, Dust emission bands, Dust emission features, Dust enrichment, Dust features, Dust formation, Dust temperature, Dust temperatures, Dusty carbon stars, Dusty models, Dusty stars, Egan, Emission bands, Emission feature, Equivalent width, Equivalent widths, Error bars, Exposure times, Feature strength, Galactic, Galactic carbon stars, Galactic sample, Galactic stars, Goebel moseley, Groenewegen, Grrv, High rates, High ratio, Higher dust temperatures, Higher ratio, Hony, Initial masses, Interstellar medium, Ira, Iras iras iras, Iras source, Journal compilation, Large magellanic cloud, Large range, Larger number, Last star, Long sequence, Loon, Lower metallicity, Lter transmission curve, Magellanic, Magellanic clouds, Manchester system, Massloss rates, Matsuura, Metallicity, Middle panel, Millar, Mnras, Model carbon stars, Molecular absorption bands, Molecular bands, Naked carbon star, Naked carbon stars, Narrow band, Narrow bands, Narrow component, Narrow sequence, Open triangles, Optical depth, Other carbon stars, Other molecules, Other stars, Oxygen stars, Photometry, Photospheric, Photospheric temperatures, Planetary nebulae, Point sources, Progenitor masses, Redder stars, Silicate, Silicate feature, Small range, Spectral range, Spectral segments, Spectral types, Spectrum, Spitzer, Spitzer observations, Spitzer space telescope, Spitzer spectra, Star, Star iras, Stars fall, Stars show, Stellar, Stellar object, Superwind, Superwind phase, Technical report, Thick dust shells, Tielens, Tsuji ohnaka, Various silicates, Vassiliadis wood, Vertical line, Waters tielens, Wavelength, Wavelength range, Wavelength shift, Weak band, Whitelock, Zijlstra.
- Teeft :
- 2mass, 2mass data, Absorption, Absorption bands, Absorption feature, Amorphous carbon dust, Aoki, Asymptotic giant branch, Average spectrum, Background emission, Background measurement, Best example, Blackbody, Blue carbon stars, Blue continuum, Blue edge, Blue spectra, Bluer colours, Bolometric, Bolometric magnitudes, Bottom panel, Broad absorption band, Broad component, Cape town, Carbon star, Carbon star sequence, Carbon stars, Carbonaceous dust, Carbonyl, Carbonyl group, Carbonyl groups, Central wavelength, Central wavelengths, Cernicharo, Colour, Colour range, Colours, Continuum, Continuum bands, Continuum colours, Continuum determination, Continuum temperatures, Crystalline silicate features, Current sample, Data points, Distance modulus, Dust bands, Dust continuum, Dust emission, Dust emission bands, Dust emission features, Dust enrichment, Dust features, Dust formation, Dust temperature, Dust temperatures, Dusty carbon stars, Dusty models, Dusty stars, Egan, Emission bands, Emission feature, Equivalent width, Equivalent widths, Error bars, Exposure times, Feature strength, Galactic, Galactic carbon stars, Galactic sample, Galactic stars, Goebel moseley, Groenewegen, Grrv, High rates, High ratio, Higher dust temperatures, Higher ratio, Hony, Initial masses, Interstellar medium, Ira, Iras iras iras, Iras source, Journal compilation, Large magellanic cloud, Large range, Larger number, Last star, Long sequence, Loon, Lower metallicity, Lter transmission curve, Magellanic, Magellanic clouds, Manchester system, Massloss rates, Matsuura, Metallicity, Middle panel, Millar, Mnras, Model carbon stars, Molecular absorption bands, Molecular bands, Naked carbon star, Naked carbon stars, Narrow band, Narrow bands, Narrow component, Narrow sequence, Open triangles, Optical depth, Other carbon stars, Other molecules, Other stars, Oxygen stars, Photometry, Photospheric, Photospheric temperatures, Planetary nebulae, Point sources, Progenitor masses, Redder stars, Silicate, Silicate feature, Small range, Spectral range, Spectral segments, Spectral types, Spectrum, Spitzer, Spitzer observations, Spitzer space telescope, Spitzer spectra, Star, Star iras, Stars fall, Stars show, Stellar, Stellar object, Superwind, Superwind phase, Technical report, Thick dust shells, Tielens, Tsuji ohnaka, Various silicates, Vassiliadis wood, Vertical line, Waters tielens, Wavelength, Wavelength range, Wavelength shift, Weak band, Whitelock, Zijlstra.
Abstract
We present a Spitzer Space Telescope spectroscopic survey of mass‐losing carbon stars (and one oxygen‐rich star) in the Large Magellanic Cloud (LMC). The stars represent the superwind phase on the asymptotic giant branch (AGB), which forms a major source of dust for the interstellar medium (ISM) in galaxies. Bolometric magnitudes indicate progenitor masses of 1.5–2.5 M⊙. The spectra cover the wavelength range 5–38 μm. They show varying combinations of dust continuum, dust emission features (SiC, MgS) and molecular absorption bands (C2H2, HCN). A 10‐μm absorption feature is attributed to C3. A weak band at 5.8 μm is suggestive of carbonyl. The circumstellar 7.5‐μm C2H2 band is found to be stronger at lower metallicity, explained by higher C/O ratios at low metallicity. The J−K versus K−A colours, used to select the sample, are shown to be relatively insensitive in separating carbon versus oxygen‐rich AGB stars. The predominance of carbon stars therefore indicates that in the range 1.5–2.5 M⊙, LMC AGB stars become carbon‐rich before onset of the superwind. A set of four narrow bands, dubbed the Manchester system, is used to define the infrared continuum for dusty carbon stars. We investigate the strength and central wavelength of the SiC and MgS dust bands as a function of colour and metallicity. The line‐to‐continuum ratio of these bands shows some indication of being lower at low metallicity. The MgS band is only seen at dust temperatures below 600 K. Metal‐poor carbon stars can form amorphous carbon dust from self‐produced carbon. The formation efficiency of oxygen‐rich dust depends more strongly on metallicity. In lower‐metallicity environments, the dust input into the ISM by AGB stars may be strongly biased towards carbonaceous dust.
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DOI: 10.1111/j.1365-2966.2006.10623.x
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Jacco Th. Van Loon<affiliation><mods:affiliation>Astrophysics Group, School of Physical & Geographical Sciences, Keele University, Staffordshire ST5 5BG</mods:affiliation><wicri:noCountry code="subField">5BG</wicri:noCountry></affiliation>Le document en format XML
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Habing</name><affiliation wicri:level="1"><mods:affiliation>Sterrewacht Leiden, Niels Bohrweg 2, 2333 RA Leiden, the Netherlands</mods:affiliation><country xml:lang="fr" wicri:curation="lc">Pays-Bas</country><wicri:regionArea>Sterrewacht Leiden, Niels Bohrweg 2, 2333 RA Leiden</wicri:regionArea></affiliation></author><author><name sortKey="Hony, S" sort="Hony, S" uniqKey="Hony S" first="S." last="Hony">S. Hony</name><affiliation wicri:level="1"><mods:affiliation>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven, Belgium</mods:affiliation><country xml:lang="fr">Belgique</country><wicri:regionArea>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven</wicri:regionArea></affiliation></author><author><name sortKey="Loup, C" sort="Loup, C" uniqKey="Loup C" first="C." last="Loup">C. Loup</name><affiliation wicri:level="1"><mods:affiliation>Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, 75014 Paris, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, 75014 Paris</wicri:regionArea></affiliation></author><author><name sortKey="Waters, L B F M" sort="Waters, L B F M" uniqKey="Waters L" first="L. B. F. M." last="Waters">L. B. F. M. Waters</name><affiliation wicri:level="1"><mods:affiliation>Astronomical Institute, 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, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam</wicri:regionArea></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:9D813BE4DB11A8D90A64912E9E1E3EA06A25D8AD</idno><date when="2006" year="2006">2006</date><idno type="doi">10.1111/j.1365-2966.2006.10623.x</idno><idno type="url">https://api.istex.fr/document/9D813BE4DB11A8D90A64912E9E1E3EA06A25D8AD/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001D89</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001D89</idno><idno type="wicri:Area/Istex/Curation">001D89</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">A <hi rend="italic">Spitzer</hi> mid‐infrared spectral survey of mass‐losing carbon stars in the Large Magellanic Cloud</title><author><name sortKey="Zijlstra, Albert A" sort="Zijlstra, Albert A" uniqKey="Zijlstra A" first="Albert A." last="Zijlstra">Albert A. Zijlstra</name><affiliation wicri:level="4"><mods:affiliation>University of Manchester, School of Physics & Astronomy, PO Box 88, Manchester M60 1QD</mods:affiliation><orgName type="university">Université de Manchester</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Manchester</settlement><region type="nation">Angleterre</region><region nuts="2" type="region">Grand Manchester</region></placeName></affiliation><affiliation wicri:level="1"><mods:affiliation>E-mail: a.zijlstra@manchester.ac.uk</mods:affiliation><country wicri:rule="url">Royaume-Uni</country></affiliation></author><author><name sortKey="Matsuura, Mikako" sort="Matsuura, Mikako" uniqKey="Matsuura M" first="Mikako" last="Matsuura">Mikako Matsuura</name><affiliation wicri:level="4"><mods:affiliation>University of Manchester, School of Physics & Astronomy, PO Box 88, Manchester M60 1QD</mods:affiliation><orgName type="university">Université de Manchester</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Manchester</settlement><region type="nation">Angleterre</region><region nuts="2" type="region">Grand Manchester</region></placeName></affiliation><affiliation><mods:affiliation>Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast BT7 1NN</mods:affiliation></affiliation></author><author><name sortKey="Wood, Peter R" sort="Wood, Peter R" uniqKey="Wood P" first="Peter R." last="Wood">Peter R. Wood</name><affiliation wicri:level="1"><mods:affiliation>Research School of Astronomy and Astrophysics, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Research School of Astronomy and Astrophysics, Australian National University, Cotter Road, Weston Creek, ACT 2611</wicri:regionArea></affiliation></author><author><name sortKey="Sloan, G C" sort="Sloan, G C" uniqKey="Sloan G" first="G. C." last="Sloan">G. C. Sloan</name><affiliation wicri:level="1"><mods:affiliation>Department of Astronomy, Cornell University, 108 Space Sciences Building, Ithaca, NY 14853‐6801, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Astronomy, Cornell University, 108 Space Sciences Building, Ithaca, NY 14853‐6801</wicri:regionArea></affiliation></author><author><name sortKey="Lagadec, Eric" sort="Lagadec, Eric" uniqKey="Lagadec E" first="Eric" last="Lagadec">Eric Lagadec</name><affiliation wicri:level="4"><mods:affiliation>University of Manchester, School of Physics & Astronomy, PO Box 88, Manchester M60 1QD</mods:affiliation><orgName type="university">Université de Manchester</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Manchester</settlement><region type="nation">Angleterre</region><region nuts="2" type="region">Grand Manchester</region></placeName></affiliation></author><author><name sortKey="Van Loon, Jacco Th" sort="Van Loon, Jacco Th" uniqKey="Van Loon J" first="Jacco Th." last="Van Loon">Jacco Th. Van Loon</name><affiliation><mods:affiliation>Astrophysics Group, School of Physical & Geographical Sciences, Keele University, Staffordshire ST5 5BG</mods:affiliation><wicri:noCountry code="subField">5BG</wicri:noCountry></affiliation></author><author><name sortKey="Groenewegen, M A T" sort="Groenewegen, M A T" uniqKey="Groenewegen M" first="M. A. T." last="Groenewegen">M. A. T. Groenewegen</name><affiliation wicri:level="1"><mods:affiliation>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven, Belgium</mods:affiliation><country xml:lang="fr">Belgique</country><wicri:regionArea>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven</wicri:regionArea></affiliation></author><author><name sortKey="Feast, M W" sort="Feast, M W" uniqKey="Feast M" first="M. W." last="Feast">M. W. Feast</name><affiliation wicri:level="1"><mods:affiliation>Department of Astronomy and University of Cape Town, 7701 Rondebosch, South Africa</mods:affiliation><country xml:lang="fr">Afrique du Sud</country><wicri:regionArea>Department of Astronomy and University of Cape Town, 7701 Rondebosch</wicri:regionArea></affiliation></author><author><name sortKey="Menzies, J W" sort="Menzies, J W" uniqKey="Menzies J" first="J. W." last="Menzies">J. W. Menzies</name><affiliation wicri:level="1"><mods:affiliation>Department of Mathematics and Applied Mathematics, University of Cape Town, Private Bag, Rondebosch 7701, South Africa</mods:affiliation><country xml:lang="fr">Afrique du Sud</country><wicri:regionArea>Department of Mathematics and Applied Mathematics, University of Cape Town, Private Bag, Rondebosch 7701</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>Department of Astronomy and University of Cape Town, 7701 Rondebosch, South Africa</mods:affiliation><country xml:lang="fr">Afrique du Sud</country><wicri:regionArea>Department of Astronomy and University of Cape Town, 7701 Rondebosch</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>Department of Mathematics and Applied Mathematics, University of Cape Town, Private Bag, Rondebosch 7701, South Africa</mods:affiliation><country xml:lang="fr">Afrique du Sud</country><wicri:regionArea>Department of Mathematics and Applied Mathematics, University of Cape Town, Private Bag, Rondebosch 7701</wicri:regionArea></affiliation></author><author><name sortKey="Blommaert, J A D L" sort="Blommaert, J A D L" uniqKey="Blommaert J" first="J. A. D. L." last="Blommaert">J. A. D. L. Blommaert</name><affiliation wicri:level="1"><mods:affiliation>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven, Belgium</mods:affiliation><country xml:lang="fr">Belgique</country><wicri:regionArea>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven</wicri:regionArea></affiliation></author><author><name sortKey="Cioni, M L" sort="Cioni, M L" uniqKey="Cioni M" first="M. L." last="Cioni">M. L. Cioni</name><affiliation wicri:level="4"><mods:affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</mods:affiliation><orgName type="university">Université d'Édimbourg</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Édimbourg</settlement><region type="country">Écosse</region></placeName></affiliation></author><author><name sortKey="Habing, H J" sort="Habing, H J" uniqKey="Habing H" first="H. J." last="Habing">H. J. Habing</name><affiliation wicri:level="1"><mods:affiliation>Sterrewacht Leiden, Niels Bohrweg 2, 2333 RA Leiden, the Netherlands</mods:affiliation><country xml:lang="fr" wicri:curation="lc">Pays-Bas</country><wicri:regionArea>Sterrewacht Leiden, Niels Bohrweg 2, 2333 RA Leiden</wicri:regionArea></affiliation></author><author><name sortKey="Hony, S" sort="Hony, S" uniqKey="Hony S" first="S." last="Hony">S. Hony</name><affiliation wicri:level="1"><mods:affiliation>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven, Belgium</mods:affiliation><country xml:lang="fr">Belgique</country><wicri:regionArea>Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, B‐3001 Leuven</wicri:regionArea></affiliation></author><author><name sortKey="Loup, C" sort="Loup, C" uniqKey="Loup C" first="C." last="Loup">C. Loup</name><affiliation wicri:level="1"><mods:affiliation>Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, 75014 Paris, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, 75014 Paris</wicri:regionArea></affiliation></author><author><name sortKey="Waters, L B F M" sort="Waters, L B F M" uniqKey="Waters L" first="L. B. F. M." last="Waters">L. B. F. M. Waters</name><affiliation wicri:level="1"><mods:affiliation>Astronomical Institute, 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, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam</wicri:regionArea></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">370</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="1961">1961</biblScope><biblScope unit="page" to="1978">1978</biblScope><biblScope unit="page-count">18</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2006-08-21">2006-08-21</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>2mass</term><term>2mass data</term><term>Absorption</term><term>Absorption bands</term><term>Absorption feature</term><term>Amorphous carbon dust</term><term>Aoki</term><term>Asymptotic giant branch</term><term>Average spectrum</term><term>Background emission</term><term>Background measurement</term><term>Best example</term><term>Blackbody</term><term>Blue carbon stars</term><term>Blue continuum</term><term>Blue edge</term><term>Blue spectra</term><term>Bluer colours</term><term>Bolometric</term><term>Bolometric magnitudes</term><term>Bottom panel</term><term>Broad absorption band</term><term>Broad component</term><term>Cape town</term><term>Carbon star</term><term>Carbon star sequence</term><term>Carbon stars</term><term>Carbonaceous dust</term><term>Carbonyl</term><term>Carbonyl group</term><term>Carbonyl groups</term><term>Central wavelength</term><term>Central wavelengths</term><term>Cernicharo</term><term>Colour</term><term>Colour range</term><term>Colours</term><term>Continuum</term><term>Continuum bands</term><term>Continuum colours</term><term>Continuum determination</term><term>Continuum temperatures</term><term>Crystalline silicate features</term><term>Current sample</term><term>Data points</term><term>Distance modulus</term><term>Dust bands</term><term>Dust continuum</term><term>Dust emission</term><term>Dust emission bands</term><term>Dust emission features</term><term>Dust enrichment</term><term>Dust features</term><term>Dust formation</term><term>Dust temperature</term><term>Dust temperatures</term><term>Dusty carbon stars</term><term>Dusty models</term><term>Dusty stars</term><term>Egan</term><term>Emission bands</term><term>Emission feature</term><term>Equivalent width</term><term>Equivalent widths</term><term>Error bars</term><term>Exposure times</term><term>Feature strength</term><term>Galactic</term><term>Galactic carbon stars</term><term>Galactic sample</term><term>Galactic stars</term><term>Goebel moseley</term><term>Groenewegen</term><term>Grrv</term><term>High rates</term><term>High ratio</term><term>Higher dust temperatures</term><term>Higher ratio</term><term>Hony</term><term>Initial masses</term><term>Interstellar medium</term><term>Ira</term><term>Iras iras iras</term><term>Iras source</term><term>Journal compilation</term><term>Large magellanic cloud</term><term>Large range</term><term>Larger number</term><term>Last star</term><term>Long sequence</term><term>Loon</term><term>Lower metallicity</term><term>Lter transmission curve</term><term>Magellanic</term><term>Magellanic clouds</term><term>Manchester system</term><term>Massloss rates</term><term>Matsuura</term><term>Metallicity</term><term>Middle panel</term><term>Millar</term><term>Mnras</term><term>Model carbon stars</term><term>Molecular absorption bands</term><term>Molecular bands</term><term>Naked carbon star</term><term>Naked carbon stars</term><term>Narrow band</term><term>Narrow bands</term><term>Narrow component</term><term>Narrow sequence</term><term>Open triangles</term><term>Optical depth</term><term>Other carbon stars</term><term>Other molecules</term><term>Other stars</term><term>Oxygen stars</term><term>Photometry</term><term>Photospheric</term><term>Photospheric temperatures</term><term>Planetary nebulae</term><term>Point sources</term><term>Progenitor masses</term><term>Redder stars</term><term>Silicate</term><term>Silicate feature</term><term>Small range</term><term>Spectral range</term><term>Spectral segments</term><term>Spectral types</term><term>Spectrum</term><term>Spitzer</term><term>Spitzer observations</term><term>Spitzer space telescope</term><term>Spitzer spectra</term><term>Star</term><term>Star iras</term><term>Stars fall</term><term>Stars show</term><term>Stellar</term><term>Stellar object</term><term>Superwind</term><term>Superwind phase</term><term>Technical report</term><term>Thick dust shells</term><term>Tielens</term><term>Tsuji ohnaka</term><term>Various silicates</term><term>Vassiliadis wood</term><term>Vertical line</term><term>Waters tielens</term><term>Wavelength</term><term>Wavelength range</term><term>Wavelength shift</term><term>Weak band</term><term>Whitelock</term><term>Zijlstra</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>2mass</term><term>2mass data</term><term>Absorption</term><term>Absorption bands</term><term>Absorption feature</term><term>Amorphous carbon dust</term><term>Aoki</term><term>Asymptotic giant branch</term><term>Average spectrum</term><term>Background emission</term><term>Background measurement</term><term>Best example</term><term>Blackbody</term><term>Blue carbon stars</term><term>Blue continuum</term><term>Blue edge</term><term>Blue spectra</term><term>Bluer colours</term><term>Bolometric</term><term>Bolometric magnitudes</term><term>Bottom panel</term><term>Broad absorption band</term><term>Broad component</term><term>Cape town</term><term>Carbon star</term><term>Carbon star sequence</term><term>Carbon stars</term><term>Carbonaceous dust</term><term>Carbonyl</term><term>Carbonyl group</term><term>Carbonyl groups</term><term>Central wavelength</term><term>Central wavelengths</term><term>Cernicharo</term><term>Colour</term><term>Colour range</term><term>Colours</term><term>Continuum</term><term>Continuum bands</term><term>Continuum colours</term><term>Continuum determination</term><term>Continuum temperatures</term><term>Crystalline silicate features</term><term>Current sample</term><term>Data points</term><term>Distance modulus</term><term>Dust bands</term><term>Dust continuum</term><term>Dust emission</term><term>Dust emission bands</term><term>Dust emission features</term><term>Dust enrichment</term><term>Dust features</term><term>Dust formation</term><term>Dust temperature</term><term>Dust temperatures</term><term>Dusty carbon stars</term><term>Dusty models</term><term>Dusty stars</term><term>Egan</term><term>Emission bands</term><term>Emission feature</term><term>Equivalent width</term><term>Equivalent widths</term><term>Error bars</term><term>Exposure times</term><term>Feature strength</term><term>Galactic</term><term>Galactic carbon stars</term><term>Galactic sample</term><term>Galactic stars</term><term>Goebel moseley</term><term>Groenewegen</term><term>Grrv</term><term>High rates</term><term>High ratio</term><term>Higher dust temperatures</term><term>Higher ratio</term><term>Hony</term><term>Initial masses</term><term>Interstellar medium</term><term>Ira</term><term>Iras iras iras</term><term>Iras source</term><term>Journal compilation</term><term>Large magellanic cloud</term><term>Large range</term><term>Larger number</term><term>Last star</term><term>Long sequence</term><term>Loon</term><term>Lower metallicity</term><term>Lter transmission curve</term><term>Magellanic</term><term>Magellanic clouds</term><term>Manchester system</term><term>Massloss rates</term><term>Matsuura</term><term>Metallicity</term><term>Middle panel</term><term>Millar</term><term>Mnras</term><term>Model carbon stars</term><term>Molecular absorption bands</term><term>Molecular bands</term><term>Naked carbon star</term><term>Naked carbon stars</term><term>Narrow band</term><term>Narrow bands</term><term>Narrow component</term><term>Narrow sequence</term><term>Open triangles</term><term>Optical depth</term><term>Other carbon stars</term><term>Other molecules</term><term>Other stars</term><term>Oxygen stars</term><term>Photometry</term><term>Photospheric</term><term>Photospheric temperatures</term><term>Planetary nebulae</term><term>Point sources</term><term>Progenitor masses</term><term>Redder stars</term><term>Silicate</term><term>Silicate feature</term><term>Small range</term><term>Spectral range</term><term>Spectral segments</term><term>Spectral types</term><term>Spectrum</term><term>Spitzer</term><term>Spitzer observations</term><term>Spitzer space telescope</term><term>Spitzer spectra</term><term>Star</term><term>Star iras</term><term>Stars fall</term><term>Stars show</term><term>Stellar</term><term>Stellar object</term><term>Superwind</term><term>Superwind phase</term><term>Technical report</term><term>Thick dust shells</term><term>Tielens</term><term>Tsuji ohnaka</term><term>Various silicates</term><term>Vassiliadis wood</term><term>Vertical line</term><term>Waters tielens</term><term>Wavelength</term><term>Wavelength range</term><term>Wavelength shift</term><term>Weak band</term><term>Whitelock</term><term>Zijlstra</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present a Spitzer Space Telescope spectroscopic survey of mass‐losing carbon stars (and one oxygen‐rich star) in the Large Magellanic Cloud (LMC). The stars represent the superwind phase on the asymptotic giant branch (AGB), which forms a major source of dust for the interstellar medium (ISM) in galaxies. Bolometric magnitudes indicate progenitor masses of 1.5–2.5 M⊙. The spectra cover the wavelength range 5–38 μm. They show varying combinations of dust continuum, dust emission features (SiC, MgS) and molecular absorption bands (C2H2, HCN). A 10‐μm absorption feature is attributed to C3. A weak band at 5.8 μm is suggestive of carbonyl. The circumstellar 7.5‐μm C2H2 band is found to be stronger at lower metallicity, explained by higher C/O ratios at low metallicity. The J−K versus K−A colours, used to select the sample, are shown to be relatively insensitive in separating carbon versus oxygen‐rich AGB stars. The predominance of carbon stars therefore indicates that in the range 1.5–2.5 M⊙, LMC AGB stars become carbon‐rich before onset of the superwind. A set of four narrow bands, dubbed the Manchester system, is used to define the infrared continuum for dusty carbon stars. We investigate the strength and central wavelength of the SiC and MgS dust bands as a function of colour and metallicity. The line‐to‐continuum ratio of these bands shows some indication of being lower at low metallicity. The MgS band is only seen at dust temperatures below 600 K. Metal‐poor carbon stars can form amorphous carbon dust from self‐produced carbon. The formation efficiency of oxygen‐rich dust depends more strongly on metallicity. In lower‐metallicity environments, the dust input into the ISM by AGB stars may be strongly biased towards carbonaceous dust.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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