SAURON项目- XIX。邻近椭圆星系、透镜星系和Sa星系的光学和近红外标度关系
The SAURON Project - XIX. Optical and near-infrared scaling relations of nearby elliptical, lenticular and Sa galaxies
摘要：
本文介绍了SAURON巡天72个代表星系的MDM V波段和Spitzer/IRAC 3.6 μ m波段的地面测光观测结果。结合在有效半径（se）内测量的SAURON恒星速度色散，这使我们能够探索我们的星系在主要标度关系中的位置。我们调查的依赖这些关系，我们最近的运动学分类的早型星系（即慢/快旋转）和恒星星族。慢旋转和快旋转E/S 0星系在标度关系中并不占据不同的位置，尽管慢旋转星系显示出较小的内在散射。令人惊讶的是，在我们的样本中，非常年轻的物体并没有显示出最蓝的（V-[3.6]）颜色，这在光学颜色中通常是这样的。这可以在TP-AGB恒星对红外线的巨大贡献的背景下理解，即使对于年轻的恒星群体，也会导致非常紧密的（V-[3.6]）- se关系，这反过来又使我们能够定义金属丰度和速度色散之间的强相关性。许多Sa星系似乎遵循E/S 0星系定义的基本平面。星系团出现偏离的关系，主要对应的对象与非常年轻的人口，与正在进行的，扩展的恒星形成的迹象。我们在基本平面中校正了这种效应，通过使用恒星质光比的估计用恒星质量代替光度，使所有星系都是紧密的单一关系的一部分。新的估计系数是一致的，在两个光度带，并建议在恒星星族的差异占约一半的观察到的倾斜相对于维里预测。经过这些校正后，慢旋转器系列在最佳拟合的基本平面周围几乎没有固有的散射。
英文摘要：
[Abridged] We present ground-based MDM V-band and Spitzer/IRAC 3.6um-band photometric observations of the 72 representative galaxies of the SAURON Survey. In combination with the SAURON stellar velocity dispersion measured within an effective radius (se), this allows us to explore the location of our galaxies in the main scaling relations. We investigate the dependence of these relations on our recent kinematical classification of early-type galaxies (i.e. Slow/Fast Rotators) and the stellar populations. Slow Rotator and Fast Rotator E/S0 galaxies do not populate distinct locations in the scaling relations, although Slow Rotators display a smaller intrinsic scatter. Surprisingly, extremely young objects do not display the bluest (V-[3.6]) colours in our sample, as is usually the case in optical colours. This can be understood in the context of the large contribution of TP-AGB stars to the infrared, even for young populations, resulting in a very tight (V-[3.6]) - se relation that in turn allows us to define a strong correlation between metallicity and velocity dispersion. Many Sa galaxies appear to follow the Fundamental Plane defined by E/S0 galaxies. Galaxies that appear offset from the relations correspond mostly to objects with extremely young populations, with signs of on-going, extended star formation. We correct for this effect in the Fundamental Plane, by replacing luminosity with stellar mass using an estimate of the stellar mass-to-light ratio, so that all galaxies are part of a tight, single relation. The new estimated coefficients are consistent in both photometric bands and suggest that differences in stellar populations account for about half of the observed tilt with respect to the virial prediction. After these corrections, the Slow Rotator family shows almost no intrinsic scatter around the best-fit Fundamental Plane.
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