Baade's window and APOGEE: Metallicities, ages, and chemical abundances

M. Schultheis, A. Rojas-Arriagada, A. E. García Pérez, H. Jönsson, M. Hayden, G. Nandakumar, K. Cunha, C. Allende Prieto, J. A. Holtzman, T. C. Beers, D. Bizyaev, J. Brinkmann, R. Carrera, R. E. Cohen, D. Geisler, F. R. Hearty, J. G. Fernandez-Tricado, C. Maraston, D. Minnitti, C. NitschelmA. Roman-Lopes, D. P. Schneider, B. Tang, S. Villanova, G. Zasowski, S. R. Majewski

Resultado de la investigación: Article

31 Citas (Scopus)

Resumen

Context. Baade's window (BW) is one of the most observed Galactic bulge fields in terms of chemical abundances. Owing to its low and homogeneous interstellar absorption it is considered the perfect calibration field for Galactic bulge studies. Aims. In the era of large spectroscopic surveys, calibration fields such as BW are necessary for cross calibrating the stellar parameters and individual abundances of the APOGEE survey. Methods. We use the APOGEE BW stars to derive the metallicity distribution function (MDF) and individual abundances for α-and iron-peak elements of the APOGEE ASPCAP pipeline (DR13), as well as the age distribution for stars in BW. Results. We determine the MDF of APOGEE stars in BW and find a remarkable agreement with that of the Gaia-ESO survey (GES). Both exhibit a clear bimodal distribution. We also find that the Mg-metallicity planes of the two surveys agree well, except for the metal-rich part ([Fe/H] > 0.1), where APOGEE finds systematically higher Mg abundances with respect to the GES. The ages based on the [C/N] ratio reveal a bimodal age distribution, with a major old population at ~ 10 Gyr, with a decreasing tail towards younger stars. A comparison of stellar parameters determined by APOGEE and those determined by other sources reveals detectable systematic offsets, in particular for spectroscopic surface gravity estimates. In general, we find a good agreement between individual abundances of O, Na, Mg, Al, Si, K, Ca, Cr, Mn, Co, and Ni from APOGEE with that of literature values. Conclusions. We have shown that in general APOGEE data show a good agreement in terms of MDF and individual chemical abundances with respect to literature works. Using the [C/N] ratio we found a significant fraction of young stars in BW.

Idioma originalEnglish
Número de artículoA14
PublicaciónAstronomy and Astrophysics
Volumen600
DOI
EstadoPublished - 1 abr 2017

Huella dactilar

metallicity
stars
galactic bulge
distribution functions
European Southern Observatory
age structure
calibration
calibrating
chemical
gravity
gravitation
iron
distribution
metal
estimates
metals
parameter
young

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Schultheis, M., Rojas-Arriagada, A., García Pérez, A. E., Jönsson, H., Hayden, M., Nandakumar, G., ... Majewski, S. R. (2017). Baade's window and APOGEE: Metallicities, ages, and chemical abundances. Astronomy and Astrophysics, 600, [A14]. https://doi.org/10.1051/0004-6361/201630154
Schultheis, M. ; Rojas-Arriagada, A. ; García Pérez, A. E. ; Jönsson, H. ; Hayden, M. ; Nandakumar, G. ; Cunha, K. ; Allende Prieto, C. ; Holtzman, J. A. ; Beers, T. C. ; Bizyaev, D. ; Brinkmann, J. ; Carrera, R. ; Cohen, R. E. ; Geisler, D. ; Hearty, F. R. ; Fernandez-Tricado, J. G. ; Maraston, C. ; Minnitti, D. ; Nitschelm, C. ; Roman-Lopes, A. ; Schneider, D. P. ; Tang, B. ; Villanova, S. ; Zasowski, G. ; Majewski, S. R. / Baade's window and APOGEE : Metallicities, ages, and chemical abundances. En: Astronomy and Astrophysics. 2017 ; Vol. 600.
@article{78b98dd9d82c4f13989acdc58bc0179c,
title = "Baade's window and APOGEE: Metallicities, ages, and chemical abundances",
abstract = "Context. Baade's window (BW) is one of the most observed Galactic bulge fields in terms of chemical abundances. Owing to its low and homogeneous interstellar absorption it is considered the perfect calibration field for Galactic bulge studies. Aims. In the era of large spectroscopic surveys, calibration fields such as BW are necessary for cross calibrating the stellar parameters and individual abundances of the APOGEE survey. Methods. We use the APOGEE BW stars to derive the metallicity distribution function (MDF) and individual abundances for α-and iron-peak elements of the APOGEE ASPCAP pipeline (DR13), as well as the age distribution for stars in BW. Results. We determine the MDF of APOGEE stars in BW and find a remarkable agreement with that of the Gaia-ESO survey (GES). Both exhibit a clear bimodal distribution. We also find that the Mg-metallicity planes of the two surveys agree well, except for the metal-rich part ([Fe/H] > 0.1), where APOGEE finds systematically higher Mg abundances with respect to the GES. The ages based on the [C/N] ratio reveal a bimodal age distribution, with a major old population at ~ 10 Gyr, with a decreasing tail towards younger stars. A comparison of stellar parameters determined by APOGEE and those determined by other sources reveals detectable systematic offsets, in particular for spectroscopic surface gravity estimates. In general, we find a good agreement between individual abundances of O, Na, Mg, Al, Si, K, Ca, Cr, Mn, Co, and Ni from APOGEE with that of literature values. Conclusions. We have shown that in general APOGEE data show a good agreement in terms of MDF and individual chemical abundances with respect to literature works. Using the [C/N] ratio we found a significant fraction of young stars in BW.",
keywords = "Galaxy: bulge, Galaxy: stellar content, Infrared: stars, Stars: abundances, Stars: fundamental parameters",
author = "M. Schultheis and A. Rojas-Arriagada and {Garc{\'i}a P{\'e}rez}, {A. E.} and H. J{\"o}nsson and M. Hayden and G. Nandakumar and K. Cunha and {Allende Prieto}, C. and Holtzman, {J. A.} and Beers, {T. C.} and D. Bizyaev and J. Brinkmann and R. Carrera and Cohen, {R. E.} and D. Geisler and Hearty, {F. R.} and Fernandez-Tricado, {J. G.} and C. Maraston and D. Minnitti and C. Nitschelm and A. Roman-Lopes and Schneider, {D. P.} and B. Tang and S. Villanova and G. Zasowski and Majewski, {S. R.}",
year = "2017",
month = "4",
day = "1",
doi = "10.1051/0004-6361/201630154",
language = "English",
volume = "600",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

Schultheis, M, Rojas-Arriagada, A, García Pérez, AE, Jönsson, H, Hayden, M, Nandakumar, G, Cunha, K, Allende Prieto, C, Holtzman, JA, Beers, TC, Bizyaev, D, Brinkmann, J, Carrera, R, Cohen, RE, Geisler, D, Hearty, FR, Fernandez-Tricado, JG, Maraston, C, Minnitti, D, Nitschelm, C, Roman-Lopes, A, Schneider, DP, Tang, B, Villanova, S, Zasowski, G & Majewski, SR 2017, 'Baade's window and APOGEE: Metallicities, ages, and chemical abundances', Astronomy and Astrophysics, vol. 600, A14. https://doi.org/10.1051/0004-6361/201630154

Baade's window and APOGEE : Metallicities, ages, and chemical abundances. / Schultheis, M.; Rojas-Arriagada, A.; García Pérez, A. E.; Jönsson, H.; Hayden, M.; Nandakumar, G.; Cunha, K.; Allende Prieto, C.; Holtzman, J. A.; Beers, T. C.; Bizyaev, D.; Brinkmann, J.; Carrera, R.; Cohen, R. E.; Geisler, D.; Hearty, F. R.; Fernandez-Tricado, J. G.; Maraston, C.; Minnitti, D.; Nitschelm, C.; Roman-Lopes, A.; Schneider, D. P.; Tang, B.; Villanova, S.; Zasowski, G.; Majewski, S. R.

En: Astronomy and Astrophysics, Vol. 600, A14, 01.04.2017.

Resultado de la investigación: Article

TY - JOUR

T1 - Baade's window and APOGEE

T2 - Metallicities, ages, and chemical abundances

AU - Schultheis, M.

AU - Rojas-Arriagada, A.

AU - García Pérez, A. E.

AU - Jönsson, H.

AU - Hayden, M.

AU - Nandakumar, G.

AU - Cunha, K.

AU - Allende Prieto, C.

AU - Holtzman, J. A.

AU - Beers, T. C.

AU - Bizyaev, D.

AU - Brinkmann, J.

AU - Carrera, R.

AU - Cohen, R. E.

AU - Geisler, D.

AU - Hearty, F. R.

AU - Fernandez-Tricado, J. G.

AU - Maraston, C.

AU - Minnitti, D.

AU - Nitschelm, C.

AU - Roman-Lopes, A.

AU - Schneider, D. P.

AU - Tang, B.

AU - Villanova, S.

AU - Zasowski, G.

AU - Majewski, S. R.

PY - 2017/4/1

Y1 - 2017/4/1

N2 - Context. Baade's window (BW) is one of the most observed Galactic bulge fields in terms of chemical abundances. Owing to its low and homogeneous interstellar absorption it is considered the perfect calibration field for Galactic bulge studies. Aims. In the era of large spectroscopic surveys, calibration fields such as BW are necessary for cross calibrating the stellar parameters and individual abundances of the APOGEE survey. Methods. We use the APOGEE BW stars to derive the metallicity distribution function (MDF) and individual abundances for α-and iron-peak elements of the APOGEE ASPCAP pipeline (DR13), as well as the age distribution for stars in BW. Results. We determine the MDF of APOGEE stars in BW and find a remarkable agreement with that of the Gaia-ESO survey (GES). Both exhibit a clear bimodal distribution. We also find that the Mg-metallicity planes of the two surveys agree well, except for the metal-rich part ([Fe/H] > 0.1), where APOGEE finds systematically higher Mg abundances with respect to the GES. The ages based on the [C/N] ratio reveal a bimodal age distribution, with a major old population at ~ 10 Gyr, with a decreasing tail towards younger stars. A comparison of stellar parameters determined by APOGEE and those determined by other sources reveals detectable systematic offsets, in particular for spectroscopic surface gravity estimates. In general, we find a good agreement between individual abundances of O, Na, Mg, Al, Si, K, Ca, Cr, Mn, Co, and Ni from APOGEE with that of literature values. Conclusions. We have shown that in general APOGEE data show a good agreement in terms of MDF and individual chemical abundances with respect to literature works. Using the [C/N] ratio we found a significant fraction of young stars in BW.

AB - Context. Baade's window (BW) is one of the most observed Galactic bulge fields in terms of chemical abundances. Owing to its low and homogeneous interstellar absorption it is considered the perfect calibration field for Galactic bulge studies. Aims. In the era of large spectroscopic surveys, calibration fields such as BW are necessary for cross calibrating the stellar parameters and individual abundances of the APOGEE survey. Methods. We use the APOGEE BW stars to derive the metallicity distribution function (MDF) and individual abundances for α-and iron-peak elements of the APOGEE ASPCAP pipeline (DR13), as well as the age distribution for stars in BW. Results. We determine the MDF of APOGEE stars in BW and find a remarkable agreement with that of the Gaia-ESO survey (GES). Both exhibit a clear bimodal distribution. We also find that the Mg-metallicity planes of the two surveys agree well, except for the metal-rich part ([Fe/H] > 0.1), where APOGEE finds systematically higher Mg abundances with respect to the GES. The ages based on the [C/N] ratio reveal a bimodal age distribution, with a major old population at ~ 10 Gyr, with a decreasing tail towards younger stars. A comparison of stellar parameters determined by APOGEE and those determined by other sources reveals detectable systematic offsets, in particular for spectroscopic surface gravity estimates. In general, we find a good agreement between individual abundances of O, Na, Mg, Al, Si, K, Ca, Cr, Mn, Co, and Ni from APOGEE with that of literature values. Conclusions. We have shown that in general APOGEE data show a good agreement in terms of MDF and individual chemical abundances with respect to literature works. Using the [C/N] ratio we found a significant fraction of young stars in BW.

KW - Galaxy: bulge

KW - Galaxy: stellar content

KW - Infrared: stars

KW - Stars: abundances

KW - Stars: fundamental parameters

UR - http://www.scopus.com/inward/record.url?scp=85016164325&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201630154

DO - 10.1051/0004-6361/201630154

M3 - Article

AN - SCOPUS:85016164325

VL - 600

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A14

ER -

Schultheis M, Rojas-Arriagada A, García Pérez AE, Jönsson H, Hayden M, Nandakumar G y otros. Baade's window and APOGEE: Metallicities, ages, and chemical abundances. Astronomy and Astrophysics. 2017 abr 1;600. A14. https://doi.org/10.1051/0004-6361/201630154