The VIMOS Ultra Deep Survey: The reversal of the star-formation rate $-$ density relation at $2 < z < 5$
B. C. Lemaux, O. Cucciati, O. Le Fèvre, G. Zamorani, L. M. Lubin, N. Hathi, O. Ilbert, D. Pelliccia, R. Amorín, S. Bardelli, P. Cassata, R. R. Gal, B. Garilli, … 展开作者
B. C. Lemaux, O. Cucciati, O. Le Fèvre, G. Zamorani, L. M. Lubin, N. Hathi, O. Ilbert, D. Pelliccia, R. Amorín, S. Bardelli, P. Cassata, R. R. Gal, B. Garilli, L. Guaita, M. Giavalisco, D. Hung, A. Koekemoer, D. Maccagni, L. Pentericci, B. Ribeiro, D. Schaerer, E. Shah, L. Shen, P. Staab, M. Talia, R. Thomas, A. R. Tomczak, L. Tresse, E. Vanzella, D. Vergani, E. Zucca
备注：
v2, 24 pages, nine figures, accepted to A&A after minor changes to language and formatting
Utilizing spectroscopic observations taken for the VIMOS Ultra-Deep Survey (VUDS), new observations from Keck/DEIMOS, and publicly available observations of large samples of star-forming galaxies, we report here on the relationship between the star formation rate (SFR) and the local environment ($δ_{gal}$) of galaxies in the early universe ($2<z<5$). Unlike what is observed at lower redshifts ($z<2$), we observe a definite, nearly monotonic increase in the average SFR with increasing galaxy overdensity over more than an order of magnitude in $δ_{gal}$. The robustness of this trend is quantified by accounting for both uncertainties in our measurements and galaxy populations that are either underrepresented or not present in our sample and find that the trend remains significant under all circumstances. This trend appears to be primarily driven by the fractional increase of galaxies in high density environments that are more massive in their stellar content and are forming stars at a higher rate than their less massive counterparts. We find that, even after stellar mass effects are accounted for, there remains a weak but significant SFR-$δ_{gal}$ trend in our sample implying that additional environmentally-related processes are helping to drive this trend. We also find clear evidence that the average SFR of galaxies in the densest environments increases with increasing redshift. These results lend themselves to a picture in which massive gas-rich galaxies coalesce into proto-cluster environments at $z\sim3$, interact with other galaxies or with a forming large-scale medium, subsequently using or losing most of their gas in the process, and begin to seed the nascent red sequence that is present in clusters at slightly lower redshifts.
New constraints on the average escape fraction of Lyman continuum radiation in z~4 galaxies from the VIMOS Ultra Deep Survey (VUDS)
确定逃离高红移星系的莱曼连续谱（LyC）光子的平均分数对于理解z>6宇宙中的再电离是如何进行的至关重要。我们希望测量来自Chandra Deep Field South（CDFS）和COSMOS领域的源样本的LyC信号，其中超深VIMOS光谱学以及多波长哈勃太空望远镜（HST）成像可用。我们从VIMOS超深巡天（VUDS）数据库中选择了46个$z\sim 4$星系的样本，使得VUDS光谱包含光谱的LyC部分，即静止帧范围$880-910Å$。利用HST成像，我们应用了仔细的清洗程序，并拒绝了所有显示附近具有不同颜色的团块的源，这些团块可能是低红移的闯入者。经过这个过程，样本减少到33个星系。我们测量所有单个源的电离通量（$895Å$处的LyC）和非电离发射（$\sim 1500 Å$处）之间的比率。我们还产生了所有源的归一化堆叠光谱。假设固有平均$L_ν(1470)/L_ν(895)$为3，我们估计个体和平均相对逃逸分数。我们没有检测到来自任何单独来源的电离辐射，虽然我们确定了一个可能的LyC发射极具有非常高的Ly $α$等效宽度（EW）。从堆叠的光谱并假设样品的平均透射率，我们测量相对逃逸分数$f_{esc}^{rel}=0.09\pm0.04$。我们还寻找LyC通量极限与源属性之间的相关性，并发现LyC通量与Ly $α$发射线EW之间的初步相关性。我们的研究结果意味着，在z $…
The UV and Ly$α$ Luminosity Functions of galaxies and the Star Formation Rate Density at the end of HI reionization from the VIMOS Ultra-Deep Survey (VUDS)
The VIMOS Ultra Deep Survey. Luminosity and stellar mass dependence of galaxy clustering at z~3
我们提出的依赖于星系团的光度和恒星质量的红移范围2 $<$ z $<$ 3.5使用3236星系的VIMOS超深巡天（VUDS）强大的光谱红移的研究。我们测量两点实空间相关函数$w_p(r_p)$为四个体积有限的恒星质量和四个光度，M $_{UV}$绝对星等选择，子样本。我们发现，尺度相关的聚类幅度$r_0$显着增加光度和恒星质量表明一个强大的星系聚类依赖于这些属性。这对应于$Δ$ b/b $^*$ =0.43的这两个子样本之间的强相对偏倚。拟合一个5参数的HOD模型，我们发现最明亮和质量最大的星系占据最大质量的暗物质晕，$\langle$ M $_h$ $\rangle$ = 10 $^{12.30}$ h $^{-1}$ M $_{\odot}$ .类似于在较低的红移观察到的趋势，最小晕质量M $_{min}$取决于光度和星系的恒星质量，并从M $_{min}$ =10 $^{9.73}$ h $^{-1}$ M $_{\odot}$到M $_{min}$ =10 $^{11.58}$ h $^{-1}$ M $_{\odot}$，分别从我们的星系样本中最暗到最亮。我们发现这些晕质量之间的差异要明显得多，比观察到的本地星系类似的属性。此外，在z~3，我们观察到，在晕主机，平均而言，一个卫星和一个中心星系的质量是M $_1$ $\approx$ 4 M $_{min}$在所有光度范…
