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Article: Origins of the thick disk as traced by the alpha elements of metal-poor giant stars selected from RAVE
Title | Origins of the thick disk as traced by the alpha elements of metal-poor giant stars selected from RAVE |
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Authors | Ruchti, Gregory R.Fulbright, Jon P.Wyse, Rosemary F GGilmore, Gerard F.Bienaymé, OlivierBinney, James J.Bland-Hawthorn, Joss BlandCampbell, Randy D.Freeman, Kenneth C.Gibson, Brad K.Grebel, Eva K.Helmi, AminaMunari, UlisseNavarro, Julio F.Parker, Quentin A.Reid, Warren A.Seabroke, George M.Siebert, ArnaudSiviero, AlessandroSteinmetz, MatthiasWatson, Fred G.Williams, Mary E KZwitter, Tomaž |
Keywords | Galaxy: abundances Stars: late-type Stars: abundances Galaxy: disk |
Issue Date | 2010 |
Citation | Astrophysical Journal Letters, 2010, v. 721, n. 2 PART 2, p. L92-L96 How to Cite? |
Abstract | Theories of thick-disk formation can be differentiated by measurements of stellar elemental abundances. We have undertaken a study of metal-poor stars selected from the RAVE spectroscopic survey of bright stars to establish whether or not there is a significant population of metal-poor thick-disk stars ([Fe/H] ≲ -1.0) and to measure their elemental abundances. In this Letter, we present abundances of four α-elements (Mg, Si, Ca, and Ti) and iron for a subsample of 212 red giant branch and 31 red clump/horizontal branch stars from this study. We find that the [α/Fe] ratios are enhanced, implying that enrichment proceeded by purely core-collapse supernovae. This requires that star formation in each star-forming region had a short duration. The relative lack of scatter in the [α/Fe] ratios implies good mixing in the interstellar medium prior to star formation. In addition, the ratios resemble that of the halo, indicating that the halo and thick disk share a similar massive star initial mass function. We conclude that the α-enhancement of the metal-poor thick disk implies that direct accretion of stars from dwarf galaxies similar to surviving dwarf galaxies today did not play a major role in the formation of the thick disk. © 2010 The American Astronomical Society. All rights reserved. |
Persistent Identifier | http://hdl.handle.net/10722/208914 |
ISSN | 2023 Impact Factor: 8.8 2023 SCImago Journal Rankings: 2.766 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Ruchti, Gregory R. | - |
dc.contributor.author | Fulbright, Jon P. | - |
dc.contributor.author | Wyse, Rosemary F G | - |
dc.contributor.author | Gilmore, Gerard F. | - |
dc.contributor.author | Bienaymé, Olivier | - |
dc.contributor.author | Binney, James J. | - |
dc.contributor.author | Bland-Hawthorn, Joss Bland | - |
dc.contributor.author | Campbell, Randy D. | - |
dc.contributor.author | Freeman, Kenneth C. | - |
dc.contributor.author | Gibson, Brad K. | - |
dc.contributor.author | Grebel, Eva K. | - |
dc.contributor.author | Helmi, Amina | - |
dc.contributor.author | Munari, Ulisse | - |
dc.contributor.author | Navarro, Julio F. | - |
dc.contributor.author | Parker, Quentin A. | - |
dc.contributor.author | Reid, Warren A. | - |
dc.contributor.author | Seabroke, George M. | - |
dc.contributor.author | Siebert, Arnaud | - |
dc.contributor.author | Siviero, Alessandro | - |
dc.contributor.author | Steinmetz, Matthias | - |
dc.contributor.author | Watson, Fred G. | - |
dc.contributor.author | Williams, Mary E K | - |
dc.contributor.author | Zwitter, Tomaž | - |
dc.date.accessioned | 2015-03-23T02:02:10Z | - |
dc.date.available | 2015-03-23T02:02:10Z | - |
dc.date.issued | 2010 | - |
dc.identifier.citation | Astrophysical Journal Letters, 2010, v. 721, n. 2 PART 2, p. L92-L96 | - |
dc.identifier.issn | 2041-8205 | - |
dc.identifier.uri | http://hdl.handle.net/10722/208914 | - |
dc.description.abstract | Theories of thick-disk formation can be differentiated by measurements of stellar elemental abundances. We have undertaken a study of metal-poor stars selected from the RAVE spectroscopic survey of bright stars to establish whether or not there is a significant population of metal-poor thick-disk stars ([Fe/H] ≲ -1.0) and to measure their elemental abundances. In this Letter, we present abundances of four α-elements (Mg, Si, Ca, and Ti) and iron for a subsample of 212 red giant branch and 31 red clump/horizontal branch stars from this study. We find that the [α/Fe] ratios are enhanced, implying that enrichment proceeded by purely core-collapse supernovae. This requires that star formation in each star-forming region had a short duration. The relative lack of scatter in the [α/Fe] ratios implies good mixing in the interstellar medium prior to star formation. In addition, the ratios resemble that of the halo, indicating that the halo and thick disk share a similar massive star initial mass function. We conclude that the α-enhancement of the metal-poor thick disk implies that direct accretion of stars from dwarf galaxies similar to surviving dwarf galaxies today did not play a major role in the formation of the thick disk. © 2010 The American Astronomical Society. All rights reserved. | - |
dc.language | eng | - |
dc.relation.ispartof | Astrophysical Journal Letters | - |
dc.subject | Galaxy: abundances | - |
dc.subject | Stars: late-type | - |
dc.subject | Stars: abundances | - |
dc.subject | Galaxy: disk | - |
dc.title | Origins of the thick disk as traced by the alpha elements of metal-poor giant stars selected from RAVE | - |
dc.type | Article | - |
dc.description.nature | link_to_subscribed_fulltext | - |
dc.identifier.doi | 10.1088/2041-8205/721/2/L92 | - |
dc.identifier.scopus | eid_2-s2.0-78649264102 | - |
dc.identifier.volume | 721 | - |
dc.identifier.issue | 2 PART 2 | - |
dc.identifier.spage | L92 | - |
dc.identifier.epage | L96 | - |
dc.identifier.eissn | 2041-8213 | - |
dc.identifier.isi | WOS:000282192200004 | - |
dc.identifier.issnl | 2041-8205 | - |