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GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies

Franco, M. and Elbaz, D. and Zhou, L. and Magnelli, B. and Schreiber, C. and Ciesla, L. and Dickinson, M. and Nagar, N. and Magdis, G. and Alexander, D. M. and Béthermin, M. and Demarco, R. and Daddi, E. and Wang, T. and Mullaney, J. and Inami, H. and Shu, X. and Bournaud, F. and Chary, R. and Ferguson, H. and Finkelstein, S. and Giavalisco, M. and Gómez-Guijarro, C. and Iono, D. and Juneau, S. and Lagache, G. and Lin, L. and Motohara, K. and Okumura, K. and Pannella, M. and Papovich, C. and Pope, A. and Rujopakarn, W. and Silverman, J. and Xiao, M. (2020) GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies. Astronomy and Astrophysics, 643 . Art. No. A53. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20200916-112916561

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Abstract

In this paper, we extend the source detection in the GOODS-ALMA field (69 arcmin², 1σ ≃ 0.18 mJy beam⁻¹) to deeper levels than presented in our previous work. Using positional information at 3.6 and 4.5 μm (from Spitzer-IRAC) as well as the Very Large Array (VLA) at 3 GHz, 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 order to ensure the most reliable counterpart association possible, we have investigated the astrometry differences between different instruments in the GOODS–South field. In addition to a global offset between the Atacama Large Millimeter/submillimeter Array (ALMA) and the Hubble Space Telescope (HST) already discussed in previous studies, we have highlighted a local offset between ALMA and the HST that was artificially introduced in the process of building the mosaic of the GOODS–South image. We created a distortion map that can be used to correct for these astrometric issues. In this Supplementary Catalog, we find a total of 16 galaxies, including two galaxies with no counterpart in HST images (also known as optically dark galaxies), down to a 5σ 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 have lower stellar masses (M⋆^(SC) = 7.6 × 10¹⁰ M_⊙ vs M⋆^(MC) = 1.2 × 10¹¹ M_⊙). Although exhibiting larger physical sizes, these galaxies still have far-infrared sizes that are significantly more compact than inferred from their optical emission.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/202038310DOIArticle
https://arxiv.org/abs/2005.03040arXivDiscussion Paper
ORCID:
AuthorORCID
Franco, M.0000-0002-3560-8599
Elbaz, D.0000-0002-7631-647X
Magnelli, B.0000-0002-6777-6490
Schreiber, C.0000-0003-0942-5198
Nagar, N.0000-0001-6920-662X
Magdis, G.0000-0002-4872-2294
Alexander, D. M.0000-0002-5896-6313
Béthermin, M.0000-0002-3915-2015
Demarco, R.0000-0003-3921-2177
Daddi, E.0000-0002-3331-9590
Mullaney, J.0000-0002-3126-6712
Inami, H.0000-0003-4268-0393
Shu, X.0000-0002-7020-4290
Bournaud, F.0000-0002-5743-0250
Chary, R.0000-0001-7583-0621
Ferguson, H.0000-0001-7113-2738
Finkelstein, S.0000-0001-8519-1130
Giavalisco, M.0000-0002-7831-8751
Gómez-Guijarro, C.0000-0002-4085-9165
Iono, D.0000-0002-2364-0823
Juneau, S.0000-0002-0000-2394
Lagache, G.0000-0003-1492-2519
Motohara, K.0000-0002-0724-9146
Pannella, M.0000-0003-3738-3976
Papovich, C.0000-0001-7503-8482
Pope, A.0000-0001-8592-2706
Rujopakarn, W.0000-0002-0303-499X
Silverman, J.0000-0002-0000-6977
Additional Information:© M. Franco et al. 2020. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Received 30 April 2020; Accepted 7 August 2020; Published online 02 November 2020. We thank the anonymous referee for the insightful comments and suggestions that improved the clarity and quality of this work. M.F. acknowledges support from the UK Science and Technology Facilities Council (STFC) (grant number ST/R000905/1). B.M. acknowledges support from the Collaborative Research Centre 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG) – project ID 184018867. L.Z. acknowledges the support from the National Key R&D Program of China (No. 2017YFA0402704, No. 2018YFA0404502), the National Natural Science Foundation of China (NSFC grants 11825302, 11733002 and 11773013) and China Scholarship Council (CSC). R.D. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) BASAL grant AFB-17000. GEM acknowledges support from the Villum Fonden research grant 13160 “Gas to stars, stars to dust: tracing star formation across cosmic time”, the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation and the ERC Consolidator Grant funding scheme (project ConTExt, grant number No. 648179). MP is supported by the ERC-StG “ClustersXCosmo”, grant agreement 71676. DMA acknowledges support from the Science and Technology Facilities Council (ST/P000541/1; ST/T000244/1). This work was supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00543.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)ST/R000905/1
Deutsche Forschungsgemeinschaft (DFG)956/A1
National Key Research and Development Program of China2017YFA0402704
National Key Research and Development Program of China2018YFA0404502
National Natural Science Foundation of China11825302
National Natural Science Foundation of China11733002
National Natural Science Foundation of China11773013
China Scholarship CouncilUNSPECIFIED
BASAL-CATAAFB-170002
VILLUM FONDEN13160
European Research Council (ERC)648179
European Research Council (ERC)71676
Science and Technology Facilities Council (STFC)ST/P000541/1
Science and Technology Facilities Council (STFC)ST/T000244/1
Programme National Cosmology et Galaxies (PNCG)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Institut national des sciences de l'Univers (INSU)UNSPECIFIED
Institut National du Patrimoine (INP)UNSPECIFIED
Institut National de Physique Nucléaire et de Physique des Particules (IN2P3)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)184018867
Subject Keywords:galaxies: high-redshift – galaxies: evolution – galaxies: star formation – galaxies: photometry – galaxies: fundamental parameters – submillimeter: galaxies
Record Number:CaltechAUTHORS:20200916-112916561
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200916-112916561
Official Citation:GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies. M. Franco, D. Elbaz, L. Zhou, B. Magnelli, C. Schreiber, L. Ciesla, M. Dickinson, N. Nagar, G. Magdis, D. M. Alexander, M. Béthermin, R. Demarco, E. Daddi, T. Wang, J. Mullaney, H. Inami, X. Shu, F. Bournaud, R. Chary, R. T. Coogan, H. Ferguson, S. L. Finkelstein, M. Giavalisco, C. Gómez-Guijarro, D. Iono, S. Juneau, G. Lagache, L. Lin, K. Motohara, K. Okumura, M. Pannella, C. Papovich, A. Pope, W. Rujopakarn, J. Silverman and M. Xiao. A&A, 643 (2020) A53; DOI: https://doi.org/10.1051/0004-6361/202038310
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105419
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:17 Sep 2020 21:25
Last Modified:05 Nov 2020 17:49

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