VIPERS Multi-Lambda调查。II。从z = 1.5开始在22平方度内与大质量星系一起潜水
The VIPERS Multi-Lambda Survey. II. Diving with massive galaxies in 22 square degrees since z = 1.5
摘要：
我们研究了一个$K_{AB}$ <22-选定的具有高度可靠的光度红移的样本的星系恒星质量函数（SMF）和恒星质量密度从红移z=0.2到z=1.5的演化。我们的研究是基于近红外观测进行了WIRCam在CFHT的足迹的VIPERS光谱调查，并受益于高品质的光学光度测量CFHTLS和紫外线观测与GALEX卫星。我们的测光红移的精度为$σ_z$ < 0.03和0.05的明亮（$i_{AB}$ <22.5）和暗淡（$i_{AB}$ >22.5）的样品，分别。SMF是用~ 760，000个直到$K_s$ =22的星系和~22.4 deg $^2$的有效区域测量的，后者大大降低了统计不确定性（即泊松误差和宇宙方差）。我们指出的测光校准，其影响迅速成为主导时，统计不确定性降低，这将是未来一代的宇宙学调查，例如EUCLID或LSST的一个主要问题，仔细控制的重要性。通过探索静息帧（NUV-r）与（r- $K_s$）色-色图区分恒星形成星系和静止星系，（1）我们发现超大质量星系的密度（$M_*/ M_{\odot}$）> 11.5的星系主要由静止星系主导，并且从z~1到z~0.2增加了2倍，这允许通过干合并进行额外的质量组装，（2）我们证实了一种恒星形成活动在恒星质量对数以上受到阻碍的情况。（$M^*_{SF} / M_{\odot}$）= 10.64 $\pm$ 0.01，该值在0.2 < z < 1.5时非常稳定，（3）讨论了存在一个主猝灭通道，之后是大质量恒星形成星系，最后（4）我们提出了另一种猝灭机制，用以解释在低红移观测到的明显过量的低质量静止星系。
英文摘要：
We investigate the evolution of the galaxy stellar mass function (SMF) and stellar mass density from redshift z=0.2 to z=1.5 of a $K_{AB}$<22-selected sample with highly reliable photometric redshifts and over an unprecedentedly large area. Our study is based on NIR observations carried out with WIRCam at CFHT over the footprint of the VIPERS spectroscopic survey and benefits from the high quality optical photometry from the CFHTLS and UV observations with the GALEX satellite. The accuracy of our photometric redshifts is $σ_z$ < 0.03 and 0.05 for the bright ($i_{AB}$<22.5) and faint ($i_{AB}$>22.5) samples, respectively. The SMF is measured with ~760,000 galaxies down to $K_s$=22 and over an effective area of ~22.4 deg$^2$, the latter of which drastically reduces the statistical uncertainties (i.e. Poissonian error & cosmic variance). We point out the importance of a careful control of the photometric calibration, whose impact becomes quickly dominant when statistical uncertainties are reduced, which will be a major issue for future generation of cosmological surveys with, e.g. EUCLID or LSST. By exploring the rest-frame (NUV-r) vs (r-$K_s$) color-color diagram separating star-forming and quiescent galaxies, (1) we find that the density of very massive log($M_*/ M_{\odot}$) > 11.5 galaxies is largely dominated by quiescent galaxies and increases by a factor 2 from z~1 to z~0.2, which allows for additional mass assembly via dry mergers, (2) we confirm a scenario where star formation activity is impeded above a stellar mass log($M^*_{SF} / M_{\odot}$) = 10.64$\pm$0.01, a value that is found to be very stable at 0.2 < z < 1.5, (3) we discuss the existence of a main quenching channel that is followed by massive star-forming galaxies, and finally (4) we characterise another quenching mechanism required to explain the clear excess of low-mass quiescent galaxies observed at low redshift.
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