The time evolution of the Milky Way's oxygen abundance gradient

Autor(es)

Molla, M. ^[1] ; Diaz, A. I. ^{[2, 3]} ; Cavichia, O. ^[4] ; Gibson, B. K. ^{[5, 6]} ; Maciel, W. J. ^[7] ; Costa, R. D. D. ^[7] ; Ascasibar, Y. ^{[2, 3]} ; Few, C. G. ^{[5, 6]}

Afiliação do(s) autor(es)

^[1] CIEMAT, Dept Invest Basica, Avda Complutense 40, E-28040 Madrid - Spain

^[2] Univ Autonoma Madrid, Dept Fis Teor, Cantoblanco, E-28049 Madrid - Spain

^[3] Univ Autonoma Madrid, Unidad Asociada CSIC, AstroUW, E-28049 Madrid - Spain

^[4] Univ Fed Itajuba, Inst Fis & Quim, Ave BPS 1303, BR-37500903 Itajuba, MG - Brazil

^[5] Univ Hull, EA Milne Ctr Astrophys, Kingston Upon Hull HU6 7RX, N Humberside - England

^[6] Michigan State Univ, JINA CEE, 640 S Shaw Lane, E Lansing, MI 48824 - USA

^[7] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao, BR-05508900 Sao Paulo, SP - Brazil

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 482, n. 3, p. 3071-3088, JAN 2019.
• Citações Web of Science: 5

Resumo

We study the evolution of oxygen abundance radial gradients as a function of time for the Milky Way Galaxy obtained with our MULCHEM chemical evolution model. We review the recent data of abundances for different objects observed in our Galactic disc. We analyse with our models the role of the growth of the stellar disc, as well as the effect of infall rate and star formation prescriptions, or the pre-enrichment of the infall gas, on the time evolution of the oxygen abundance radial distribution. We compute the radial gradient of abundances within the disc, and its corresponding evolution, taking into account the disc growth along time. We compare our predictions with the data compilation, showing a good agreement. Our models predict a very smooth evolution when the radial gradient is measured within the optical disc with a slight flattening of the gradient from similar to -0.057 dex kpc(-1) at z = 4 until values around similar to-0.015 dex kpc(-1) at z = 1 and basically the same gradient until the present, with small differences between models. Moreover, some models show a steepening at the last times, from z = 1 until z = 0 in agreement with data which give a variation of the gradient in a range from -0.02 to -0.04 dex kpc(-1) from t = 10 Gyr until now. The gradient measured as a function of the normalized radius R/R-eff is in good agreement with findings by CALIFA and MUSE, and its evolution with redshift falls within the error bars of cosmological simulations. (AU)

• Processo FAPESP: 18/04562-7 - IAU Symposium 343: Why Galaxies Care About AGB Stars
• Beneficiário: Walter Junqueira Maciel
• Modalidade de apoio: Auxílio à Pesquisa - Reunião - Exterior