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Chemical gradients in the Milky Way from the RAVE data

Authors :
Boeche, C.
Siebert, A.
Piffl, T.
Just, A.
Steinmetz, M.
Sharma, S.
Kordopatis, G.
Gilmore, G.
Chiappini, C.
Williams, M.
Grebel, E. K.
Bland-Hawthorn, J.
Gibson, Bradley Kenneth
Munari, U.
Siviero, A.
Bienaymé, O.
Navarro, J. F.
Parker, Q. A.
Reid, W.
Seabroke, G. M.
Watson, F. G.
Wyse, R. F. G.
Zwitter, T.
Boeche, C.
Siebert, A.
Piffl, T.
Just, A.
Steinmetz, M.
Sharma, S.
Kordopatis, G.
Gilmore, G.
Chiappini, C.
Williams, M.
Grebel, E. K.
Bland-Hawthorn, J.
Gibson, Bradley Kenneth
Munari, U.
Siviero, A.
Bienaymé, O.
Navarro, J. F.
Parker, Q. A.
Reid, W.
Seabroke, G. M.
Watson, F. G.
Wyse, R. F. G.
Zwitter, T.
Publication Year :
2013

Abstract

Aims. We aim at measuring the chemical gradients of the elements Mg, Al, Si, and Fe along the Galactic radius to provide new constraints on the chemical evolution models of the Galaxy and Galaxy models such as the Besancon model. Thanks to the large number of stars of our RAVE sample we can study how the gradients vary as function of the distance from the Galactic plane. Methods. We analysed three different samples selected from three independent datasets: a sample of 19 962 dwarf stars selected from the RAVE database, a sample of 10 616 dwarf stars selected from the Geneva-Copenhagen Survey (GCS) dataset, and a mock sample (equivalent to the RAVE sample) created by using the GALAXIA code, which is based on the Besancon model. The three samples were analysed by using the very same method for comparison purposes. We integrated the Galactic orbits and obtained the guiding radii (R-g) and the maximum distances from the Galactic plane reached by the stars along their orbits (Z(max)). We measured the chemical gradients as functions of R-g at different Z(max). Results. We found that the chemical gradients of the RAVE and GCS samples are negative and show consistent trends, although they are not equal: at Z(max) < 0.4 kpc and 4.5 < R-g(kpc) < 9.5, the iron gradient for the RAVE sample is d[Fe/H]/dR(g) = -0.065 dex kpc(-1), whereas for the GCS sample it is d[Fe/H]/dR(g) = -0.043 dex kpc(-1) with internal errors of +/-0.002 and +/-0.004 dex kpc(-1), respectively. The gradients of the RAVE and GCS samples become flatter at larger Z(max). Conversely, the mock sample has a positive iron gradient of d[Fe/H]/dR(g) = +0.053 +/- 0.003 dex kpc(-1) at Z(max) < 0.4 kpc and remains positive at any Z(max). These positive and unrealistic values originate from the lack of correlation between metallicity and tangential velocity in the Besancon model. In addition, the low metallicity and asymmetric drift of the thick disc causes a shift of the stars towards lower R-g and metallicity which

Details

Database :
OAIster
Notes :
application/pdf, English
Publication Type :
Electronic Resource
Accession number :
edsoai.on1137479774
Document Type :
Electronic Resource