The origin of the mue-MB and Kormendy relations in dwarf elliptical galaxies
The origin of the mue-MB and Kormendy relations in dwarf elliptical galaxies
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DOI：
10.1051/0004-6361:200809546
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发表时间：
2008-07
影响因子：
6.5
通讯作者：
A. Boselli;S. Boissier;L. Cortese;G. Gavazzi
中科院分区：
文献类型：
--
作者：
A. Boselli;S. Boissier;L. Cortese;G. Gavazzi
目标。本工作的目的是研究不同类型和亮度的星系沿不同结构尺度关系的分布，以确定大质量和矮小椭圆星系是否由相同的形成过程形成。方法：研究方法。这项工作是通过比较处女座星系团、大质量和矮小椭圆形星系以及恒星形成星系在B波段的有效表面亮度和有效半径与绝对星等关系以及Kormendy关系与追踪冲压剥离对进入星系团环境的盘状星系和星系骚扰的影响的模型预测的关系来完成的。结果。矮星椭圆体可能是由最近进入星系团的低光度、晚型螺旋体形成的，由于冲压剥离事件而失去了气体，停止了它们的恒星形成。恒星形成活动的突然减少所引起的扰动足以将盘状星系的结构性质改变为矮小椭圆形星系的结构性质。星系的扰动会导致盘状结构的截断，并且通常会增加扰动星系的有效表面亮度。缺乏对广泛光度范围内的扰动星系的动力学模拟，使我们无法就处女座星系团中的低表面亮度矮小椭圆星系群可能是由骚扰引起的起源得出任何确定的结论。结论。虽然观测到的标度关系与椭圆星系沿上述标度关系的分布是由Sersic指数n的光度逐渐变化所致的观点一致，但与模型的比较表明，矮小椭圆形可能是由与巨型椭圆形完全不同的过程形成的。
Aims. The present work is aimed at studying the distribution of galaxies of different types and luminosities along different structural scaling relations to see whether massive and dwarf ellipticals have been shaped by the same formation process. Methods. This exercise is done by comparing the distribution of Virgo cluster massive and dwarf ellipticals and star forming galaxies along the B band effective surface brightness and effective radius vs. absolute magnitude relations and the Kormendy relation to the predictions of models tracing the effects of ram-pressure stripping on disc galaxies entering the cluster environment and galaxy harassment. Results. Dwarf ellipticals might have been formed from low luminosity, late-type spirals that recently entered into the cluster and lost their gas because of a ram-pressure stripping event, stopping their star formation. The perturbations induced by the abrupt decrease of the star formation activity are sufficient to modify the structural properties of disc galaxies into those of dwarf ellipticals. Galaxy harassment induces a truncation of the disc and generally an increase of the effective surface brightness of the perturbed galaxies. The lack of dynamical simulations of perturbed galaxies spanning a wide range in luminosity prevents us from deriving any firm conclusion on a possible harassment-induced origin of the low surface brightness dwarf elliptical galaxy population inhabiting the Virgo cluster. Conclusions. Although the observed scaling relations are consistent with the idea that the distribution of elliptical galaxies along the mentioned scaling relation is due to a gradual variation with luminosity of the Sersic index n, the comparison with models indicates that dwarf ellipticals might have been formed by a totally different process to giant ellipticals.