z~3长带隙的物理和形态特性：Lyalpha线发射的依赖性
Physical and morphological properties of z~3 LBGs: dependence on Lyalpha line emission
摘要：
我们调查的物理和形态学性质的LBG在z ~2.5 ~3.5，以确定它们是否以及如何依赖于Lyalpha发射的性质和强度。我们选择了U-辍学星系从z检测的GOODS MUSIC目录，通过适应经典的莱曼破裂准则的GOODS过滤器集。我们只保留了那些光谱确认的星系，主要来自VIMOS和FORS的公共观测。使用全多波长14波段测光，我们确定了星系的物理性质，通过一个标准的光谱能量分布与更新的Charlot & Bruzual（2009）模板拟合。我们还增加了其他相关的观测，即斯皮策/MIPS的24 μ m观测和2毫秒钱德拉X射线观测。最后，利用非参数诊断法（Gini、浓度、不对称性、M_20和椭圆率），对星系的静止坐标系UV形态进行了表征。然后，我们分析了这些物理和形态学特性如何与光谱中Lyalpha线的存在相关。我们发现，与在较高的红移，物理性质的依赖Lyalpha线是温和的：星系没有Lyalpha的发射往往是更大的质量和尘埃比其余的样品，但所有其他参数，年龄，SFR，X射线发射以及紫外线形态不强烈依赖于线发射的存在。在一个简单的场景中，所有的LBG都具有固有的高Lyalpha发射，但尘埃和中性氢含量（形成Lyalpha的最终外观）取决于星系的质量，能够再现z~3处的大部分观测特性。一些修改可能需要考虑到所观察到的这些属性与宇宙时代的演变，这也进行了讨论。
英文摘要：
We investigate the physical and morphological properties of LBGs at z ~2.5 to ~3.5, to determine if and how they depend on the nature and strength of the Lyalpha emission. We selected U-dropout galaxies from the z-detected GOODS MUSIC catalog, by adapting the classical Lyman Break criteria on the GOODS filter set. We kept only those galaxies with spectroscopic confirmation, mainly from VIMOS and FORS public observations. Using the full multi-wavelength 14-bands photometry, we determined the physical properties of the galaxies, through a standard spectral energy distribution fitting with the updated Charlot & Bruzual (2009) templates. We also added other relevant observations, i.e. the 24mu m observations from Spitzer/MIPS and the 2 MSec Chandra X-ray observations. Finally, using non parametric diagnostics (Gini, Concentration, Asymmetry, M_20 and ellipticity), we characterized the rest-frame UV morphology of the galaxies. We then analyzed how these physical and morphological properties correlate with the presence of the Lyalpha line in the optical spectra. We find that, unlike at higher redshift, the dependence of physical properties on the Lyalpha line is milder: galaxies without Lyalpha in emission tend to be more massive and dustier than the rest of the sample, but all other parameters, ages, SFRs, X-ray emission as well as UV morphology do not depend strongly on the presence of the line emission. A simple scenario where all LBGs have intrinsically high Lyalpha emission, but where dust and neutral hydrogen content (which shape the final appearance of the Lyalpha) depend on the mass of the galaxies, is able to reproduce the majority of the observed properties at z~3. Some modification might be needed to account for the observed evolution of these properties with cosmic epoch, which is also discussed.
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