Abundances of disk and bulge giants from high-resolution optical spectra: V. Molybdenum: The p-process element
Research output: Contribution to journal › Journal article › Research › peer-review
Standard
Abundances of disk and bulge giants from high-resolution optical spectra : V. Molybdenum: The p-process element. / Forsberg, R.; Ryde, N.; Jönsson, H.; Rich, R. M.; Johansen, A.
In: Astronomy & Astrophysics, Vol. 666, A125, 2022.Research output: Contribution to journal › Journal article › Research › peer-review
Harvard
APA
Vancouver
Author
Bibtex
}
RIS
TY - JOUR
T1 - Abundances of disk and bulge giants from high-resolution optical spectra
T2 - V. Molybdenum: The p-process element
AU - Forsberg, R.
AU - Ryde, N.
AU - Jönsson, H.
AU - Rich, R. M.
AU - Johansen, A.
PY - 2022
Y1 - 2022
N2 - Aims. In this work, we aim to make a differential comparison of the neutron-capture and p-process element molybdenum (Mo) in the stellar populations in the local disk(s) and the bulge, focusing on minimising possible systematic effects in the analysis.Methods. The stellar sample consists of 45 bulge and 291 local disk K-giants observed with high-resolution optical spectra. The abundances are determined by fitting synthetic spectra using the Spectroscopy Made Easy (SME) code. The disk sample is separated into thin and thick disk components using a combination of abundances and kinematics. The cosmic origin of Mo is investigated and discussed by comparing with published abundances of Mo and the neutron-capture elements cerium (Ce) and europium (Eu).Results. We determine reliable Mo abundances for 35 bulge and 282 disk giants with a typical uncertainty of [Mo/Fe] similar to 0.2 and similar to 0.1 dex for the bulge and disk, respectively.Conclusions. We find that the bulge is possibly enhanced in [Mo/Fe] compared to the thick disk, which we do not observe in either [Ce/Fe] or [Eu/Fe]. This might suggest a higher past star-formation rate in the bulge; however, as we do not observe the bulge to be enhanced in [Eu/Fe], the origin of the molybdenum enhancement is yet to be constrained. Although the scatter is large, we may be observing evidence of the p-process contributing to the heavy element production in the chemical evolution of the bulge.
AB - Aims. In this work, we aim to make a differential comparison of the neutron-capture and p-process element molybdenum (Mo) in the stellar populations in the local disk(s) and the bulge, focusing on minimising possible systematic effects in the analysis.Methods. The stellar sample consists of 45 bulge and 291 local disk K-giants observed with high-resolution optical spectra. The abundances are determined by fitting synthetic spectra using the Spectroscopy Made Easy (SME) code. The disk sample is separated into thin and thick disk components using a combination of abundances and kinematics. The cosmic origin of Mo is investigated and discussed by comparing with published abundances of Mo and the neutron-capture elements cerium (Ce) and europium (Eu).Results. We determine reliable Mo abundances for 35 bulge and 282 disk giants with a typical uncertainty of [Mo/Fe] similar to 0.2 and similar to 0.1 dex for the bulge and disk, respectively.Conclusions. We find that the bulge is possibly enhanced in [Mo/Fe] compared to the thick disk, which we do not observe in either [Ce/Fe] or [Eu/Fe]. This might suggest a higher past star-formation rate in the bulge; however, as we do not observe the bulge to be enhanced in [Eu/Fe], the origin of the molybdenum enhancement is yet to be constrained. Although the scatter is large, we may be observing evidence of the p-process contributing to the heavy element production in the chemical evolution of the bulge.
KW - stars: abundances
KW - Galaxy: abundances
KW - Galaxy: bulge
KW - Galaxy: disk
KW - Galaxy: evolution
KW - solar neighborhood
KW - NEUTRON-CAPTURE ELEMENTS
KW - GALACTIC CHEMICAL EVOLUTION
KW - R-PROCESS
KW - S-PROCESS
KW - HEAVY-ELEMENTS
KW - STAR MERGERS
KW - PROCESS NUCLEOSYNTHESIS
KW - MASSIVE STARS
KW - SOLAR
KW - ORIGIN
U2 - 10.1051/0004-6361/202244013
DO - 10.1051/0004-6361/202244013
M3 - Journal article
VL - 666
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
M1 - A125
ER -
ID: 325009979