dc.identifier.citation | Franco , M , Elbaz , D , Zhou , L , Magnelli , B , Schreiber , C , Ciesla , L , Dickinson , M , Nagar , N , Magdis , G , Alexander , D M , Béthermin , M , Demarco , R , Daddi , E , Wang , T , Mullaney , J , Inami , H , Shu , X , Bournaud , F , Chary , R , Coogan , R T , Ferguson , H , Finkelstein , S L , Giavalisco , M , Gómez-Guijarro , C , Iono , D , Juneau , S , Lagache , G , Lin , L , Motohara , K , Okumura , K , Pannella , M , Papovich , C , Pope , A , Rujopakarn , W , Silverman , J & Xiao , M 2020 , ' GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies ' , Astronomy & Astrophysics , vol. 643 , A53 . https://doi.org/10.1051/0004-6361/202038310 | |
dc.description.abstract | In this paper, we extend the source detection in the GOODS-ALMA field (69 arcmin$^2$, rms sensitivity $\sigma$ $\simeq$ 0.18 mJy.beam$^{-1}$), to deeper levels than presented in Franco et al. (2018). Using positional information at 3.6 and 4.5 $\mu$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-$\sigma$ 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$\sigma$ 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. | en |