Properties of thick discs formed in clumpy galaxies
Abstract
We examine a possible formation scenario of galactic thick discs with numerical simulations. Thick discs have previously been argued to form in clumpy disc phase in the high-redshift Universe, which host giant clumps of ≲109 M⊙ in their highly gas-rich discs. We performed N-body/smoothed particle hydrodynamics simulations using isolated galaxy models for the purpose of verifying whether dynamical and chemical properties of the thick discs formed in such clumpy galaxies are compatible with observations. The results of our simulations seem nearly consistent with observations in dynamical properties such as radial and vertical density profiles, significant rotation velocity lag with height and distributions of orbital eccentricities. In addition, the thick discs in our simulations indicate nearly exponential dependence of σθ and σz with radius, nearly isothermal kinematics in vertical direction and negligible metallicity gradients in radial and vertical directions. However, our simulations cannot reproduce altitudinal dependence of eccentricities, metallicity relations with eccentricities or rotation velocities, which shows striking discrepancy from recent observations of the Galactic thick disc. From this result, we infer that the clumpy disc scenario for thick-disc formation would not be suitable at least for the Milky Way. Our study, however, cannot reject this scenario for external galaxies if not all galaxies form their thick discs by the same process. In addition, we found that a significant fraction of thick-disc stars forms in giant clumps.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- June 2014
- DOI:
- 10.1093/mnras/stu544
- arXiv:
- arXiv:1402.5986
- Bibcode:
- 2014MNRAS.441..243I
- Keywords:
-
- methods: numerical;
- Galaxy: disc;
- Galaxy: formation;
- galaxies: formation;
- Astrophysics - Astrophysics of Galaxies;
- Astrophysics - Cosmology and Nongalactic Astrophysics
- E-Print:
- 15 pages, 13 figures, 3 tables, accepted for publication in MNRAS