Stanford, S. A. and Masters, D. and Darvish, B. and Stern, D. and Cohen, J. G. and Capak, P. and Hernitschek, N. and Davidzon, I. and Rhodes, J. and Sanders, D. B. and Mobasher, B. and Castander, F. J. and Paltani, S. and Aghanim, N. and Amara, A. and Auricchio, N. and Balestra, A. and Bender, R. and Bodendorf, C. and Bonino, D. and Branchini, E. and Brinchmann, J. and Capobianco, V. and Carbone, C. and Carretero, J. and Casas, R. and Castellano, M. and Cavuoti, S. and Cimatti, A. and Cledassou, R. and Conselice, C. J. and Corcione, L. and Costille, A. and Cropper, M. and Degaudenzi, H. and Douspis, M. and Dubath, F. and Dusini, S. and Fosalba, P. and Frailis, M. and Franceschi, E. and Franzetti, P. and Fumana, M. and Garilli, B. and Giocoli, C. and Grupp, F. and Haugan, S. V. H. and Hoekstra, H. and Holmes, W. and Hormuth, F. and Hudelot, P. and Jahnke, K. and Kiessling, A. and Kilbinger, M. and Kitching, T. and Kubik, B. and Kümmel, M. and Kunz, M. and Kurki-Suonio, H. and Laureijs, R. and Ligori, S. and Lilje, P. B. and Lloro, I. and Maiorano, E. and Marggraf, O. and Markovic, K. and Massey, R. and Meneghetti, M. and Meylan, G. and Moscardini, L. and Niemi, S. M. and Padilla, C. and Pasian, F. and Pedersen, K. and Pettorino, V. and Pires, S. and Poncet, M. and Popa, L. and Pozzetti, L. and Raison, F. and Roncarelli, M. and Rossetti, E. and Saglia, R. and Scaramella, R. and Schneider, P. and Secroun, A. and Seidel, G. and Serrano, S. and Sirignano, C. and Sirri, G. and Taylor, A. N. and Teplitz, H. I. and Tereno, I. and Toledo-Moreo, R. and Valentijn, E. A. and Valenziano, L. and Verdoes Kleijn, G. A. and Wang, Y. and Zamorani, G. and Zoubian, J. and Brescia, M. and Congedo, G. and Conversi, L. and Copin, Y. and Kermiche, S. and Kohley, R. and Medinaceli, E. and Mei, S. and Moresco, M. and Morin, B. and Munari, E. and Polenta, G. and Sureau, F. and Tallada Crespí, P. and Vassallo, T. and Zacchei, A. and Andreon, S. and Aussel, H. and Baccigalupi, C. and Balaguera-Antolínez, A. and Baldi, M. and Bardelli, S. and Biviano, A. and Borsato, E. and Bozzo, E. and Burigana, C. and Cabanac, R. and Camera, S. and Cappi, A. and Carvalho, C. S. and Casas, S. and Castignani, G. and Colodro-Conde, C. and Coupon, J. and Courtois, H. M. and Cuby, J.-G. and Da Silva, A. and de la Torre, S. and Di Ferdinando, D. and Duncan, C. A. J. and Dupac, X. and Fabricius, M. and Farina, M. and Farrens, S. and Ferreira, P. G. and Finelli, F. and Flose-Reimberg, P. and Fotopoulou, S. and Galeotta, S. and Ganga, K. and Gillard, W. and Gozaliasl, G. and Graciá-Carpio, J. and Keihanen, E. and Kirkpatrick, C. C. and Lindholm, V. and Mainetti, G. and Maino, D. and Martinet, N. and Marulli, F. and Maturi, M. and Maurogordato, S. and Metcalf, R. B. and Nakajima, R. and Neissner, C. and Nightingale, J. W. and Nucita, A. A. and Patrizii, L. and Potter, D. and Renzi, A. and Riccio, G. and Romelli, E. and Sánchez, A. G. and Sapone, D. and Schirmer, M. and Schultheis, M. and Scottez, V. and Stanco, L. and Tenti, M. and Teyssier, R. and Torradeflot, F. and Valiviita, J. and Viel, M. and Whittaker, L. and Zucca, E. (2021) Euclid Preparation. XIV. The Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Data Release 3. Astrophysical Journal Supplement Series, 256 (1). Art. No. 9. ISSN 0067-0049. doi:10.3847/1538-4365/ac0833. https://resolver.caltech.edu/CaltechAUTHORS:20210914-225403874
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Abstract
The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of i ∼ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage iv dark energy projects, particularly Euclid and the Nancy Grace Roman Space Telescope (Roman), which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B–2019B semesters using the DEIMOS, LRIS, and MOSFIRE multiobject spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 < z_p < 2.6 range of interest for the Euclid cosmological goals, then with the current data release, C3R2 has increased the spectroscopic redshift coverage of the Euclid color space from 51% (as reported by Masters et al.) to the current 91%. Once completed and combined with extensive data collected by other spectroscopic surveys, C3R2 should provide the spectroscopic calibration set needed to enable photometric redshifts to meet the cosmology requirements for Euclid, and make significant headway toward solving the problem for Roman.
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| Additional Information: | © 2021. The American Astronomical Society. Received 2021 March 11; revised 2021 May 24; accepted 2021 May 26; published 2021 August 31. A significant portion of the research and manuscript preparation took place during the COVID-19 global pandemic. The authors would like to thank all of those who risked their lives as essential workers in order for us to safely continue our work from home. The authors also thank the referee whose comments helped improve the clarity and presentation of our results. The research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was enabled by a NASA Keck grant. F.J.C. acknowledges support from grant ESP2017-89838 ad H2020 European Commission grant 776247. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. | ||||||||||
| Group: | Astronomy Department, Infrared Processing and Analysis Center (IPAC) | ||||||||||
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| Subject Keywords: | Galaxy spectroscopy | ||||||||||
| Issue or Number: | 1 | ||||||||||
| Classification Code: | Unified Astronomy Thesaurus concepts: Galaxy spectroscopy (2171) | ||||||||||
| DOI: | 10.3847/1538-4365/ac0833 | ||||||||||
| Record Number: | CaltechAUTHORS:20210914-225403874 | ||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20210914-225403874 | ||||||||||
| Official Citation: | S. A. Stanford et al 2021 ApJS 256 9 | ||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||
| ID Code: | 110898 | ||||||||||
| Collection: | CaltechAUTHORS | ||||||||||
| Deposited By: | George Porter | ||||||||||
| Deposited On: | 17 Sep 2021 16:54 | ||||||||||
| Last Modified: | 17 Sep 2021 16:54 |
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