Simulating multiple merger pathways to the central kinematics of early-type galaxies

被引:48
作者
Moody, Christopher E. [1 ]
Romanowsky, Aaron J. [2 ,3 ]
Cox, Thomas J. [4 ]
Novak, G. S. [5 ]
Primack, Joel R. [1 ]
机构
[1] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA
[2] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA
[3] Univ Calif Observ, Santa Cruz, CA 95064 USA
[4] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA
[5] CNRS, Observ Paris, LERMA, F-75014 Paris, France
基金
欧洲研究理事会; 美国国家科学基金会;
关键词
galaxies: evolution; galaxies: formation; galaxies: interactions; galaxies: kinematics and dynamics; SIGHT VELOCITY DISTRIBUTIONS; DARK-MATTER HALOS; ELLIPTIC GALAXIES; MAJOR MERGERS; ANGULAR-MOMENTUM; ATLAS(3D) PROJECT; ISOPHOTE SHAPES; SAURON PROJECT; MINOR MERGERS; SLOW ROTATORS;
D O I
10.1093/mnras/stu1444
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Two-dimensional integral field surveys such as ATLAS(3D) are producing rich observational data sets yielding insights into galaxy formation. These new kinematic observations have highlighted the need to understand the evolutionary mechanisms leading to a spectrum of fast rotators and slow rotators in early-type galaxies. We address the formation of slow and fast rotators through a series of controlled, comprehensive hydrodynamical simulations, sampling idealized galaxy merger scenarios constructed from model spiral galaxies. Idealized and controlled simulations of this sort complement the more 'realistic' cosmological simulations by isolating and analysing the effects of specific parameters, as we do in this paper. We recreate minor and major binary mergers, binary merger trees with multiple progenitors, and multiple sequential mergers. Within each of these categories of formation history, we correlate progenitor gas fraction, mass ratio, orbital pericentre, orbital ellipticity, and spin with remnant kinematic properties. We create kinematic profiles of these 95 simulations comparable to ATLAS3D data. By constructing remnant profiles of the projected specific angular momentum (lambda(R) = < R vertical bar V vertical bar > / < R root V-2 + sigma(2) >), triaxiality, and measuring the incidences of kinematic twists and kinematically decoupled cores, we distinguish between varying formation scenarios. We find that binary mergers nearly always form fast rotators. Slow rotators can be formed from zero initial angular momentum configurations and gas-poor mergers, but are not as round as the ATLAS(3D) galaxies. Remnants of binary merger trees are triaxial slow rotators. Sequential mergers form round slow rotators that most resemble the ATLAS(3D) rotators.
引用
收藏
页码:1475 / 1485
页数:11
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