Correlations between age, kinematics, and chemistry as seen by the RAVE survey
(2018) In Monthly Notices of the Royal Astronomical Society 477(4). p.5612-5624- Abstract
We explore the connections between stellar age, chemistry, and kinematics across a Galactocentric distance of 7.5 < R(kpc) < 9.0, using a sample of ~12 000 intermediate-mass (FGK) turn-offstars observed with the RAdial Velocity Experiment (RAVE) survey. The kinematics of this sample are determined using radial velocity measurements from RAVE, and parallax and proper motion measurements from the Tycho-Gaia Astrometric Solution (TGAS). In addition, ages for RAVE stars are determined using a Bayesian method, taking TGAS parallaxes as a prior. We divide our sample into young (0 < τ < 3 Gyr) and old (8 < τ < 13 Gyr) populations, and then consider different metallicity bins for each of these... (More)
(Less)
We explore the connections between stellar age, chemistry, and kinematics across a Galactocentric distance of 7.5 < R(kpc) < 9.0, using a sample of ~12 000 intermediate-mass (FGK) turn-offstars observed with the RAdial Velocity Experiment (RAVE) survey. The kinematics of this sample are determined using radial velocity measurements from RAVE, and parallax and proper motion measurements from the Tycho-Gaia Astrometric Solution (TGAS). In addition, ages for RAVE stars are determined using a Bayesian method, taking TGAS parallaxes as a prior. We divide our sample into young (0 < τ < 3 Gyr) and old (8 < τ < 13 Gyr) populations, and then consider different metallicity bins for each of these age groups. We find significant differences in kinematic trends of young and old, metal-poor and metal-rich, stellar populations. In particular, we find a strong metallicity dependence in the mean Galactocentric radial velocity as a function of radius (∂V
R
/∂R) for young stars, with metal-rich stars having a much steeper gradient than metal-poor stars. For ∂V
Φ
/∂R, young, metal-rich stars significantly lag the LSR with a slightly positive gradient, while metal-poor stars show a negative gradient above the LSR. We interpret these findings as correlations between metallicity and the relative contributions of the non-axisymmetries in the Galactic gravitational potential (the spiral arms and the bar) to perturb stellar orbits.
- author
- organization
- publishing date
- 2018-07-11
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Galaxy: kinematics and dynamics, Galaxy: structure, Solar neighbourhood
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 477
- issue
- 4
- pages
- 13 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:85050153787
- ISSN
- 0035-8711
- DOI
- 10.1093/mnras/sty1016
- language
- English
- LU publication?
- yes
- id
- 8f4dbc89-b126-4fd1-b827-48b9520c7e74
- date added to LUP
- 2019-04-29 13:32:32
- date last changed
- 2024-03-19 05:37:20
@article{8f4dbc89-b126-4fd1-b827-48b9520c7e74, abstract = {{<p><br> We explore the connections between stellar age, chemistry, and kinematics across a Galactocentric distance of 7.5 < R(kpc) < 9.0, using a sample of ~12 000 intermediate-mass (FGK) turn-offstars observed with the RAdial Velocity Experiment (RAVE) survey. The kinematics of this sample are determined using radial velocity measurements from RAVE, and parallax and proper motion measurements from the Tycho-Gaia Astrometric Solution (TGAS). In addition, ages for RAVE stars are determined using a Bayesian method, taking TGAS parallaxes as a prior. We divide our sample into young (0 < τ < 3 Gyr) and old (8 < τ < 13 Gyr) populations, and then consider different metallicity bins for each of these age groups. We find significant differences in kinematic trends of young and old, metal-poor and metal-rich, stellar populations. In particular, we find a strong metallicity dependence in the mean Galactocentric radial velocity as a function of radius (∂V<br> <sub>R</sub><br> /∂R) for young stars, with metal-rich stars having a much steeper gradient than metal-poor stars. For ∂V<br> <sub>Φ</sub><br> /∂R, young, metal-rich stars significantly lag the LSR with a slightly positive gradient, while metal-poor stars show a negative gradient above the LSR. We interpret these findings as correlations between metallicity and the relative contributions of the non-axisymmetries in the Galactic gravitational potential (the spiral arms and the bar) to perturb stellar orbits.<br> </p>}}, author = {{Wojno, Jennifer and Kordopatis, Georges and Steinmetz, Matthias and McMillan, Paul and Binney, James and Famaey, Benoit and Monari, Giacomo and Minchev, Ivan and Wyse, Rosemary F.G. and Antoja, Teresa and Siebert, Arnaud and Carrillo, Ismael and Bland-Hawthorn, Joss and Grebel, Eva K. and Zwitter, Tomaž and Bienaymé, Olivier and Gibson, Brad and Kunder, Andrea and Munari, Ulisse and Navarro, Julio and Parker, Quentin and Reid, Warren and Seabroke, George}}, issn = {{0035-8711}}, keywords = {{Galaxy: kinematics and dynamics; Galaxy: structure; Solar neighbourhood}}, language = {{eng}}, month = {{07}}, number = {{4}}, pages = {{5612--5624}}, publisher = {{Oxford University Press}}, series = {{Monthly Notices of the Royal Astronomical Society}}, title = {{Correlations between age, kinematics, and chemistry as seen by the RAVE survey}}, url = {{http://dx.doi.org/10.1093/mnras/sty1016}}, doi = {{10.1093/mnras/sty1016}}, volume = {{477}}, year = {{2018}}, }