Euclid Preparation. XIV. The Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Data Release 3

Creators: Stanford, S. A.; Masters, D.; Darvish, B.; Stern, D.; Cohen, J. G.; Capak, P.; Hernitschek, N.; Davidzon, I.; Rhodes, J.; Sanders, D. B.; Mobasher, B.; Castander, F. J.; Paltani, S.; Aghanim, N.; Amara, A.; Auricchio, N.; Balestra, A.; Bender, R.; Bodendorf, C.; Bonino, D.; Branchini, E.; Brinchmann, J.; Capobianco, V.; Carbone, C.; Carretero, J.; Casas, R.; Castellano, M.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Conselice, C. J.; Corcione, L.; Costille, A.; Cropper, M.; Degaudenzi, H.; Douspis, M.; Dubath, F.; Dusini, S.; Fosalba, P.; Frailis, M.; Franceschi, E.; Franzetti, P.; Fumana, M.; Garilli, B.; Giocoli, C.; Grupp, F.; Haugan, S. V. H.; Hoekstra, H.; Holmes, W.; Hormuth, F.; Hudelot, P.; Jahnke, K.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kubik, B.; Kümmel, M.; Kunz, M.; Kurki-Suonio, H.; Laureijs, R.; Ligori, S.; Lilje, P. B.; Lloro, I.; Maiorano, E.; Marggraf, O.; Markovic, K.; Massey, R.; Meneghetti, M.; Meylan, G.; Moscardini, L.; Niemi, S. M.; Padilla, C.; Pasian, F.; Pedersen, K.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Pozzetti, L.; Raison, F.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Scaramella, R.; Schneider, P.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Taylor, A. N.; Teplitz, H. I.; Tereno, I.; Toledo-Moreo, R.; Valentijn, E. A.; Valenziano, L.; Verdoes Kleijn, G. A.; Wang, Y.; Zamorani, G.; Zoubian, J.; Brescia, M.; Congedo, G.; Conversi, L.; Copin, Y.; Kermiche, S.; Kohley, R.; Medinaceli, E.; Mei, S.; Moresco, M.; Morin, B.; Munari, E.; Polenta, G.; Sureau, F.; Tallada Crespí, P.; Vassallo, T.; Zacchei, A.; Andreon, S.; Aussel, H.; Baccigalupi, C.; Balaguera-Antolínez, A.; Baldi, M.; Bardelli, S.; Biviano, A.; Borsato, E.; Bozzo, E.; Burigana, C.; Cabanac, R.; Camera, S.; Cappi, A.; Carvalho, C. S.; Casas, S.; Castignani, G.; Colodro-Conde, C.; Coupon, J.; Courtois, H. M.; Cuby, J.-G.; Da Silva, A.; de la Torre, S.; Di Ferdinando, D.; Duncan, C. A. J.; Dupac, X.; Fabricius, M.; Farina, M.; Farrens, S.; Ferreira, P. G.; Finelli, F.; Flose-Reimberg, P.; Fotopoulou, S.; Galeotta, S.; Ganga, K.; Gillard, W.; Gozaliasl, G.; Graciá-Carpio, J.; Keihanen, E.; Kirkpatrick, C. C.; Lindholm, V.; Mainetti, G.; Maino, D.; Martinet, N.; Marulli, F.; Maturi, M.; Maurogordato, S.; Metcalf, R. B.; Nakajima, R.; Neissner, C.; Nightingale, J. W.; Nucita, A. A.; Patrizii, L.; Potter, D.; Renzi, A.; Riccio, G.; Romelli, E.; Sánchez, A. G.; Sapone, D.; Schirmer, M.; Schultheis, M.; Scottez, V.; Stanco, L.; Tenti, M.; Teyssier, R.; Torradeflot, F.; Valiviita, J.; Viel, M.; Whittaker, L.; Zucca, E.

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.

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.

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