期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 444, 期 2, 页码 1475-1485出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu1444
关键词
galaxies: evolution; galaxies: formation; galaxies: interactions; galaxies: kinematics and dynamics
资金
- National Science Foundation [AST-0909237]
- Department of Energy
- ERC European Research Council [267399-Momentum]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1010033] Funding Source: National Science Foundation
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.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据