In the thick of it: metal-poor disc stars in RAVE
By selecting in the Radial Velocity Experiment-fourth data release (RAVE-DR4) survey the stars located between 1 and 2 kpc above the Galactic plane, we question the consistency of the simplest three-component model (thin disc, thick disc and halo) for the Milky Way. We confirm that the metallicity a...
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| Veröffentlicht in: | Monthly Notices of the Royal Astronomical Society 2013-12, Vol.436 (4), p.3231-3246 |
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| creator | Kordopatis, G. Gilmore, G. Wyse, R. F. G. Steinmetz, M. Siebert, A. Bienaymé, O. McMillan, P. J. Minchev, I. Zwitter, T. Gibson, B. K. Seabroke, G. Grebel, E. K. Bland-Hawthorn, J. Boeche, C. Freeman, K. C. Munari, U. Navarro, J. F. Parker, Q. Reid, W. A. Siviero, A. |
| description | By selecting in the Radial Velocity Experiment-fourth data release (RAVE-DR4) survey the stars located between 1 and 2 kpc above the Galactic plane, we question the consistency of the simplest three-component model (thin disc, thick disc and halo) for the Milky Way. We confirm that the metallicity and azimuthal velocity distribution functions of the thick disc are not Gaussian. In particular, we find that the thick disc has an extended metallicity tail going at least down to [M/H] = -2 dex, contributing roughly 3 per cent of the entire thick disc population and having a shorter scalelength compared to the canonical thick disc. The mean azimuthal velocity of these metal-poor stars allows us to estimate the correlation between the metallicity ([M/H]) and the orbital velocity (V...), which is an important constraint on the formation mechanisms of the Galactic thick disc. Given our simple approach, we find ... 50 km s... dex..., which is in very good agreement with previous literature values. We complete the study with a brief discussion on the implications of the formation scenarios for the thick disc and suggest that given the above-mentioned characteristics, a thick disc mainly formed by radial migration mechanisms seems unlikely. (ProQuest: ... denotes formulae/symbols omitted.) |
| doi_str_mv | 10.1093/mnras/stt1804 |
| format | Article |
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F. G. ; Steinmetz, M. ; Siebert, A. ; Bienaymé, O. ; McMillan, P. J. ; Minchev, I. ; Zwitter, T. ; Gibson, B. K. ; Seabroke, G. ; Grebel, E. K. ; Bland-Hawthorn, J. ; Boeche, C. ; Freeman, K. C. ; Munari, U. ; Navarro, J. F. ; Parker, Q. ; Reid, W. A. ; Siviero, A.</creator><creatorcontrib>Kordopatis, G. ; Gilmore, G. ; Wyse, R. F. G. ; Steinmetz, M. ; Siebert, A. ; Bienaymé, O. ; McMillan, P. J. ; Minchev, I. ; Zwitter, T. ; Gibson, B. K. ; Seabroke, G. ; Grebel, E. K. ; Bland-Hawthorn, J. ; Boeche, C. ; Freeman, K. C. ; Munari, U. ; Navarro, J. F. ; Parker, Q. ; Reid, W. A. ; Siviero, A.</creatorcontrib><description>By selecting in the Radial Velocity Experiment-fourth data release (RAVE-DR4) survey the stars located between 1 and 2 kpc above the Galactic plane, we question the consistency of the simplest three-component model (thin disc, thick disc and halo) for the Milky Way. 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A.</creatorcontrib><creatorcontrib>Siviero, A.</creatorcontrib><title>In the thick of it: metal-poor disc stars in RAVE</title><title>Monthly Notices of the Royal Astronomical Society</title><description>By selecting in the Radial Velocity Experiment-fourth data release (RAVE-DR4) survey the stars located between 1 and 2 kpc above the Galactic plane, we question the consistency of the simplest three-component model (thin disc, thick disc and halo) for the Milky Way. We confirm that the metallicity and azimuthal velocity distribution functions of the thick disc are not Gaussian. In particular, we find that the thick disc has an extended metallicity tail going at least down to [M/H] = -2 dex, contributing roughly 3 per cent of the entire thick disc population and having a shorter scalelength compared to the canonical thick disc. The mean azimuthal velocity of these metal-poor stars allows us to estimate the correlation between the metallicity ([M/H]) and the orbital velocity (V...), which is an important constraint on the formation mechanisms of the Galactic thick disc. Given our simple approach, we find ... 50 km s... dex..., which is in very good agreement with previous literature values. We complete the study with a brief discussion on the implications of the formation scenarios for the thick disc and suggest that given the above-mentioned characteristics, a thick disc mainly formed by radial migration mechanisms seems unlikely. (ProQuest: ... denotes formulae/symbols omitted.)</description><subject>Accretion disks</subject><subject>Astronomi, astrofysik och kosmologi</subject><subject>Astronomy, Astrophysics and Cosmology</subject><subject>Fysik</subject><subject>Galaxy: abundances, Galaxy: disc, Galaxy: kinematics and dynamics, Galaxy: stellar content, Galaxy: structure</subject><subject>Milky Way</subject><subject>Natural Sciences</subject><subject>Naturvetenskap</subject><subject>Physical Sciences</subject><subject>Star & galaxy formation</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNo9kM9Lw0AQhRdRsFaP3hc8x-5kNpOst1KqFgqCqNdlsz8wtW3iboL43xtt8fCYy-N7zMfYNYhbEApnu300aZb6HiohT9gEkIosV0SnbCIEFllVApyzi5Q2QgiJOU0YrPa8f_djGvvB28Cb_o7vfG-2Wde2kbsmWZ56ExNv9vx5_ra8ZGfBbJO_Ot4pe71fviwes_XTw2oxX2cWS-wza4M1UpGngOjqSpEVVAjKkWxRlFYYV3tApAqCyqX3ZY7grPEGrK1I4pStD9z05buh1l1sdiZ-69Y0ejt0Y-oxOnntbO2Ug1JD6SotEZVWEkjL4GtQoQCp6hF3c8B1sf0cfOr1ph3ifvxAgyQiLEhUYys7tGxsU4o-_M-C0L-S9Z9kfZSMP0v9bys</recordid><startdate>20131221</startdate><enddate>20131221</enddate><creator>Kordopatis, G.</creator><creator>Gilmore, G.</creator><creator>Wyse, R. 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J. ; Minchev, I. ; Zwitter, T. ; Gibson, B. K. ; Seabroke, G. ; Grebel, E. K. ; Bland-Hawthorn, J. ; Boeche, C. ; Freeman, K. C. ; Munari, U. ; Navarro, J. F. ; Parker, Q. ; Reid, W. 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A.</au><au>Siviero, A.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>In the thick of it: metal-poor disc stars in RAVE</atitle><jtitle>Monthly Notices of the Royal Astronomical Society</jtitle><date>2013-12-21</date><risdate>2013</risdate><volume>436</volume><issue>4</issue><spage>3231</spage><epage>3246</epage><pages>3231-3246</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>By selecting in the Radial Velocity Experiment-fourth data release (RAVE-DR4) survey the stars located between 1 and 2 kpc above the Galactic plane, we question the consistency of the simplest three-component model (thin disc, thick disc and halo) for the Milky Way. We confirm that the metallicity and azimuthal velocity distribution functions of the thick disc are not Gaussian. In particular, we find that the thick disc has an extended metallicity tail going at least down to [M/H] = -2 dex, contributing roughly 3 per cent of the entire thick disc population and having a shorter scalelength compared to the canonical thick disc. The mean azimuthal velocity of these metal-poor stars allows us to estimate the correlation between the metallicity ([M/H]) and the orbital velocity (V...), which is an important constraint on the formation mechanisms of the Galactic thick disc. Given our simple approach, we find ... 50 km s... dex..., which is in very good agreement with previous literature values. We complete the study with a brief discussion on the implications of the formation scenarios for the thick disc and suggest that given the above-mentioned characteristics, a thick disc mainly formed by radial migration mechanisms seems unlikely. (ProQuest: ... denotes formulae/symbols omitted.)</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stt1804</doi><tpages>16</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Accretion disks Astronomi, astrofysik och kosmologi Astronomy, Astrophysics and Cosmology Fysik Galaxy: abundances, Galaxy: disc, Galaxy: kinematics and dynamics, Galaxy: stellar content, Galaxy: structure Milky Way Natural Sciences Naturvetenskap Physical Sciences Star & galaxy formation |
| title | In the thick of it: metal-poor disc stars in RAVE |
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