2020/12/18 by K. Sysoliatina, A. Just
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Disc #Galaxy #Galaxy formation and evolution #Gamma-ray bursts and supernovae #Globular cluster #Halo #Metallicity #Milky Way #Physics #Star formation #Stars #Stellar mass #Stellar, planetary, and galactic studies #Thick disk #Thin disk #astro-ph.GA
paper · pdf · doi:10.1051/0004-6361/202038840
published as A&A 647, A39 (2021) · 29 pages, 16 figures, 4 tables. Accepted for publication in Astronomy&Astrophysics on December 1, 2020
openalex publication_date 2020/12/18 · arxiv created 2021/02/18 · openalex created_date 2021/03/01 · arxiv updated 2021/03/10 · openalex updated_date 2026/08/05
Aims. We present an updated version of the semi-analytic Just-Jahrei (JJ) model of the Galactic disk and constrain its parameters in the Solar neighbourhood. Methods. The new features of the JJ model include a simple two-component gaseous disk, a star-formation rate (SFR) function of the thick disk that has been extended in time, and a correlation between the kinematics of molecular gas and thin-disk populations. Here, we study the vertical number density profiles and W -velocity distributions determined from ∼2 × 10 6 local stars of the second Gaia data release (DR2). We also investigate an apparent Hess diagram of the Gaia DR2 stars selected in a conic volume towards the Galactic poles. Using a stellar evolution library, we synthesise stellar populations with a four-slope broken power-law initial mass function, the SFR, and an age-metallicity relation. The latter is consistently derived with the observed metallicity distribution of the local Red Clump giants from the Apache Point Observatory Galactic Evolution Experiment (APOGEE). Working within a Bayesian approach, we sample the posterior probability distribution in a multidimensional parameter space using the Markov chain Monte Carlo method. Results. We find that the spatial distribution and motion of the Gaia DR2 stars imply two recent SF bursts centered at ages of ∼0.5 Gyr and ∼3 Gyr and characterised by a ∼30% and ∼55% SF enhancement, respectively, relative to a monotonously declining SFR continuum. The stellar populations associated with this SF excess are found to be dynamically hot for their age: they have W -velocity dispersions of ∼12.5 km s −1 and ∼26 km s −1 . The new JJ model is able to reproduce the local star counts with an accuracy of ∼5%. Conclusions. Using Gaia DR2 data, we self-consistently constrained 22 parameters of the updated JJ model. Our optimised model predicts two SF bursts within the last ∼4 Gyr, which may point to recent episodes of gas infall.