论文标题
缪斯群体的观察结果A2744：z $ \ sim $ 3-7的LBG和LAE种群之间的交集
MUSE observations towards the lensing cluster A2744: Intersection between the LBG and LAE populations at z $\sim$ 3-7
论文作者
论文摘要
We present a study of the intersection between the populations of star forming galaxies (SFGs) selected as either Lyman break galaxies (LBGs) or Lyman-alpha emitters (LAEs) in the redshift range 2.9 - 6.7, within the same volume of universe sampled by the Multi-Unit Spectroscopic Explorer (MUSE) behind the Hubble Frontier Fields lensing cluster A2744.我们定义了三个形成星系的样本：具有LAE对应物（92个星系）的LBG星系，没有LAE的LBG星系（408个星系）（408个星系）和没有LBG的LAE星系（46个星系）。由于样品的镜头性质（MUV $ \ ge $ -20.5），所有这些星系在本质上都是微弱的。所有选定的SFG中LAES的一部分随红移时增加到Z $ \ sim $ 6，并且减少了更高的红移。 LAE/LBG种群具有紫外线幅度和Lya亮度的演变表明，LAE选择能够识别具有MUV $ \ ge $ -15的本质上的紫外线，通常在最深的镜头光度测试中错过了$ \ ge $ -15。 LBG人口似乎公平地代表了SFG的总人口，降至MUV $ \ sim $ -15。带有MUV $ <-17 $的星系往往具有Sfrlya $ <$ SFRUV，而在我们的样品中观察到相反的趋势，对于MUV $> -17 $的微弱星系，包括仅由Lya发射检测到的星系，并具有较大的散射。这些趋势以前在其他SFG样本中以高$ Z $的方式观察到，在这里以非常微弱的MUV $ \ sim -15 $星系的方式看到了这些趋势，比以前的研究中得以愚蠢。基于目前的结果，没有明确的证据表明选择为LBG和/或LAE的两个种群的特性固有差异。观察到的趋势可以通过几个事实的结合来解释，例如存在不同的恒星形成方案，灰尘含量，灰尘和恒星的相对分布和形态，或恒星种群
We present a study of the intersection between the populations of star forming galaxies (SFGs) selected as either Lyman break galaxies (LBGs) or Lyman-alpha emitters (LAEs) in the redshift range 2.9 - 6.7, within the same volume of universe sampled by the Multi-Unit Spectroscopic Explorer (MUSE) behind the Hubble Frontier Fields lensing cluster A2744. We define three samples of star-forming galaxies: LBG galaxies with an LAE counterpart (92 galaxies), LBG galaxies without LAE counterpart (408 galaxies) and LAE galaxies without an LBG counterpart (46 galaxies). All these galaxies are intrinsically faint due to the lensing nature of the sample (Muv $\ge$ -20.5). The fraction of LAEs among all selected SFGs increases with redshift up to z $\sim$ 6 and decreases for higher redshifts. The evolution of LAE/LBG populations with UV magnitude and Lya luminosity shows that the LAE selection is able to identify intrinsically UV faint galaxies with Muv $\ge$ -15 that are typically missed in the deepest lensing photometric surveys. The LBG population seems to fairly represent the total population of SFGs down to Muv$\sim$-15. Galaxies with Muv$<-17$ tend to have SFRLya$<$SFRuv, whereas the opposite trend is observed within our sample for faint galaxies with Muv$>-17$, including galaxies only detected by their Lya emission, with a large scatter. These trends, previously observed in other samples of SFGs at high-$z$, are seen here for very faint Muv$\sim -15$ galaxies, much fainter than in previous studies. There is no clear evidence, based on the present results, for an intrinsic difference on the properties of the two populations selected as LBG and/or LAE. The observed trends could be explained by a combination of several facts, like the existence of different star-formation regimes, the dust content, the relative distribution and morphology of dust and stars, or the stellar populations
