The Stability of Galaxy Disks

被引:0
作者
Westfall, Kyle B. [1 ]
Andersen, David R. [2 ]
Bershady, Matthew A. [3 ]
Martinsson, Thomas P. K. [4 ]
Swaters, Robert A. [5 ]
Verheijen, Marc A. W. [1 ]
机构
[1] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands
[2] NRC Herzberg Inst Astrophys, Victoria, BC, Canada
[3] Univ Wisconsin Madison, Dept Astron, Madison, WI USA
[4] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands
[5] Natl Opt Astron Observ, Victoria, BC, Canada
来源
STRUCTURE AND DYNAMICS OF DISK GALAXIES | 2014年 / 480卷
关键词
STAR-FORMATION; SPIRAL GALAXIES; DARK-MATTER; SCHMIDT LAW; EFFICIENCY;
D O I
暂无
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We calculate the stellar surface mass density (E.) and two -component (gas+stars) disk stability (Q(Rw)) for 25 late-type galaxies from the DiskMass Survey. These calculations are based on fits of a dynamical model to our ionized-gas and stellar kinematic data performed using a Markov Chain Monte Carlo sampling of the Bayesian posterior. Marginalizing over all galaxies, we find a median value of QRw = 2.0 +/- 0.9 at 1.5 scale lengths. We also find that QRw is anti-correlated with the star-formation rate surface density (E.), which can be predicted using a closed. set of empirical scaling relations. Finally, we find that the star-formation efficiency (overdot (Sigma)(*)/Sigma(g)) is correlated with E. and weakly anti-correlated with QRw. The former is consistent with an equilibrium prediction of E-*/E-g cc proportional to Sigma(1/2)(*). Despite its order-of-magnitude range, we find no correlation of overdot (Sigma)/Sigma g Sigma(1/2)(*) with any other physical quantity derived by our study.
引用
收藏
页码:93 / 96
页数:4
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