论文标题
商品 - alma：使用IRAC和VLA探测毫无用处的毫米星系
GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies
论文作者
论文摘要
在本文中，我们将源检测扩展到商品 - alma字段（69 arcmin $^2 $，RMS敏感性$σ$ $ $ $ \ simeq $ 0.18 mjy.beam $^{ - 1} $），比Franco等人更深的水平。 （2018）。使用3.6和4.5 $μ$ m（来自Spitzer-IRAC）的位置信息，我们探索了以1.1 mm检测到的星系的存在，而ALMA低于我们的原始盲目检测极限，为4.8- $σ$，而虚假来源的数量开始占主导地位。在此补充目录中，我们发现总共16个星系，包括2个星系，在HST图像（也称为光向星系）中没有对应的星系，至5 $σ$限制H = 28.2 AB（HST/WFC3 F160W）。这将商品 - alma 1.1 mm源的总样本带到了35个星系。 Galaxies in the new sample cover a wider dynamic range in redshift ($z$ = 0.65 - 4.73), are on average twice as large (1.3 vs 0.65 kpc) and and have lower stellar mass (M$_{\star}^{\rm SC}$ = 7.6$\times$10$^{10}$M$_\odot$ vs m $ _ {\ star}^{\ rm mc} $ = 1.2 $ \ times $ 10 $^{11} $ m $ _ \ odot $）。尽管表现出较大的物理尺寸，但这些星系的尺寸仍然比从光学发射中推断出的远红外尺寸明显更紧凑。我们表明，HST图像的天文测量不仅遭受了全球天文学的影响，正如先前论文中已经讨论过的那样，而且还遭受了本地变化的影响。这些扭曲是在构建商品 - 南HST图像的镶嵌过程中人为引入的。通过比较HST，Pan-Starrs和Alma检测到的近400个星系的位置，我们创建了一个失真图，可用于校正这些星体问题。
In this paper, we extend the source detection in the GOODS-ALMA field (69 arcmin$^2$, rms sensitivity $σ$ $\simeq$ 0.18 mJy.beam$^{-1}$), to deeper levels than presented in Franco et al. (2018). Using positional information at 3.6 and 4.5 $μ$m (from Spitzer-IRAC), we explore the presence of galaxies detected at 1.1 mm with ALMA below our original blind detection limit of 4.8-$σ$ at which the number of spurious sources starts to dominate over that of real sources. In this Supplementary Catalog, we find a total of 16 galaxies, including 2 galaxies with no counterpart in HST images (also known as optically-dark galaxies) down to a 5$σ$ limiting depth of H = 28.2 AB (HST/WFC3 F160W). This brings the total sample of GOODS-ALMA 1.1 mm sources to 35 galaxies. Galaxies in the new sample cover a wider dynamic range in redshift ($z$ = 0.65 - 4.73), are on average twice as large (1.3 vs 0.65 kpc) and and have lower stellar mass (M$_{\star}^{\rm SC}$ = 7.6$\times$10$^{10}$M$_\odot$ vs M$_{\star}^{\rm MC}$ = 1.2$\times$10$^{11}$M$_\odot$). Although exhibiting larger physical sizes, these galaxies have still far-infrared sizes significantly more compact than inferred from their optical emission. We show that the astrometry of the HST image does not only suffer from a global astrometric shift, as already discussed in previous papers, but also from local shifts. These distortions were artificially introduced in the process of building the mosaic of the GOODS-South HST image. By comparing the positions of almost 400 galaxies detected by HST, Pan-STARRS and ALMA, we create a distortion map which can be used to correct for these astrometric issues.
