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The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way

Published online by Cambridge University Press:  02 August 2018

T. Bensby ,
S. Feltzing ,
A. Gould ,
J. C. Yee ,
J. A. Johnson ,
M. Asplund ,
J. Meléndez Open the ORCID record for J. Meléndez [Opens in a new window] ,
S. Lucatello  and
L. M. Howes Open the ORCID record for L. M. Howes [Opens in a new window]
T. Bensby
Affiliation:
Lund Observatory, Box 43, SE-221 00 Lund, Sweden
S. Feltzing
Affiliation:
Lund Observatory, Box 43, SE-221 00 Lund, Sweden
A. Gould
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany Korea Astronomy and Space Science Institute Institute, Daejon 305-348, Republic of Korea Dept of Astronomy, Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210, USA
J. C. Yee
Affiliation:
Smithsonian Astrophysical Observatory, 60 Garden St., Cambridge, MA 02138, USA
J. A. Johnson
Affiliation:
Dept of Astronomy, Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210, USA
M. Asplund
Affiliation:
Research School of Astronomy & Astrophysics, ANU, Canberra, Australia
J. Meléndez
Affiliation:
Departamento de Astronomia do IAG/USP, Universidade de São Paulo, São Paulo, Brasil
S. Lucatello
Affiliation:
INAF-Astronomical Observatory of Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
L. M. Howes
Affiliation:
Lund Observatory, Box 43, SE-221 00 Lund, Sweden
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Abstract

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The four main findings about the age and abundance structure of the Milky Way bulge based on microlensed dwarf and subgiant stars are: (1) a wide metallicity distribution with distinct peaks at [Fe/H] = -1.09, -0.63, -0.20, +0.12, +0.41; (2) a high fraction of intermediate-age to young stars where at [Fe/H] > 0 more than 35 % are younger than 8 Gyr, (3) several episodes of significant star formation in the bulge 3, 6, 8, and 11 Gyr ago; (4) the ‘knee’ in the α-element abundance trends of the sub-solar metallicity bulge appears to be located at a slightly higher [Fe/H] (about 0.05 to 0.1 dex) than in the local thick disk.

Keywords

Galaxy: diskGalaxy: evolutionGalaxy: structureGalaxy: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 86 - 89
Copyright
Copyright © International Astronomical Union 2018 

References

Alves-Brito, A., Meléndez, J., Asplund, M., Ramírez, I., & Yong, D., 2010, A&A, 513, A35Google Scholar
Bensby, T., Adén, D., Meléndez, J., et al. 2011, A&A, 533, A134Google Scholar
Bensby, T., Feltzing, S., Gould, A., et al. 2017, A&A, 605, A89Google Scholar
Bensby, T., Feltzing, S., Johnson, J. A., et al. 2010, A&A, 512, A41Google Scholar
Bensby, T., Feltzing, S., & Oey, M. S., 2014, A&A, 562, A71Google Scholar
Bensby, T., Johnson, J. A., Cohen, J., et al. 2009, A&A, 499, 737Google Scholar
Bensby, T., Yee, J. C., Feltzing, S., et al. 2013, A&A, 549, A147Google Scholar
Cohen, J. G., Huang, W., Udalski, A., Gould, A., & Johnson, J. A., 2008, ApJ, 682, 1029Google Scholar
Cohen, J. G., Thompson, I. B., Sumi, T., et al. 2009, ApJ, 699, 66Google Scholar
Dwek, E., Arendt, R. G., Hauser, M. G., et al. 1995, ApJ, 445, 716Google Scholar
Edvardsson, B., Andersen, J., Gustafsson, B., et al. 1993, A&A, 275, 101Google Scholar
Epstein, C. R., Johnson, J. A., Dong, S., et al. 2010, ApJ, 709, 447Google Scholar
Fuhrmann, K., 1998, A&A, 338, 161Google Scholar
Fulbright, J. P., McWilliam, A., & Rich, R. M., 2007, ApJ, 661, 1152Google Scholar
Hill, V., Lecureur, A., Gómez, A., et al. 2011, A&A, 534, A80Google Scholar
Johnson, J. A., Gal-Yam, A., Leonard, D. C., et al. 2007, ApJ, 655, L33Google Scholar
Johnson, J. A., Gaudi, B. S., Sumi, T., Bond, I. A., & Gould, A., 2008, ApJ, 685, 508Google Scholar
Kormendy, J. & Kennicutt, R. C., 2004, ARA&A, 42, 603Google Scholar
Kunder, A., Koch, A., Rich, R. M., et al. 2012, AJ, 143, 57Google Scholar
McWilliam, A. & Rich, R. M., 1994, ApJ, 91, 749Google Scholar
Ness, M., Freeman, K., Athanassoula, E., et al. 2013, MNRAS, 430, 836Google Scholar
Rojas-Arriagada, A., Recio-Blanco, A., de Laverny, P., et al. 2017, A&A, 601, A140Google Scholar
Wegg, C. & Gerhard, O., 2013, MNRAS, 435, 1874Google Scholar
White, S. D. M. & Rees, M. J., 1978, MNRAS, 183, 341Google Scholar
Zoccali, M., Vasquez, S., Gonzalez, O. A., et al. 2017, A&A, 599, A12Google Scholar