Euclid preparation. XXXI. The effect of the variations in photometric passbands on photometric-redshift accuracy

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Author(s): Paltani, S; Coupon, J; Hartley, W.G; Alvarez-Ayllon, A; Dubath, F; Mohr, J.J; Schirmer, M; Cuillandre, J.-C; Desprez, G; Ilbert, O; Kuijken, K; Aghanim, N; Altieri, B; Amara, A; Auricchio, N; Baldi, M; Bender, R; Bodendorf, C; Bonino, D; Branchini, E; Brescia, M; Brinchmann, J; Camera, S; Capobianco, V; Carbone, C; Cardone, V.F; Carretero, J; Castander, F.J; Castellano, M; Cavuoti, S; Cledassou, R; Congedo, G; Conselice, C.J; Conversi, L; Copin, Y; Corcione, L; Courbin, F; Cropper, M; da Silva, A; Degaudenzi, H; Dinis, J; Douspis, M; Dupac, X; Dusini, S; Farrens, S; Ferriol, S; Fosalba, P; Frailis, M; Franceschi, E; Franzetti, P; Galeotta, S; Garilli, B; Gillard, W; Gillis, B; Giocoli, C; Grazian, A; Haugan, S.V; Hoekstra, H; Hornstrup, A; Hudelot, P; Jahnke, K; Kümmel, M; Kermiche, S; Kiessling, A; Kilbinger, M; Kitching, T; Kohley, R; Kubik, B; Kunz, M; Kurki-Suonio, H; Ligori, S; Lilje, P.B; Lloro, I; Maiorano, E; Mansutti, O; Marggraf, O; Markovic, K; Marulli, F; Massey, R; Masters, D.C; Maurogordato, S; Mccracken, H.J; Medinaceli, E; Mei, S; Melchior, M; Meneghetti, M; Merlin, E; Meylan, G; Moresco, M; Moscardini, L; Munari, E; Niemi, S.-M; Nightingale, J; Padilla, C; Pasian, F; Pedersen, K; Percival, W.J; Pettorino, V; Polenta, G; Poncet, M; Popa, L.A; Raison, F; Rebolo, R; Renzi, A; Rhodes, J; Riccio, G; Romelli, E; Roncarelli, M; Rossetti, E; Saglia, R; Sapone, D; Sartoris, B; Schneider, P; Secroun, A; Sirignano, C; Sirri, G; Skottfelt, J; Stanco, L; Starck, J.-L; Surace, C; Tallada-Crespí, P; Tereno, I; Toledo-Moreo, R; Torradeflot, F; Tutusaus, I; Valentijn, E.A; Valenziano, L; Vassallo, T; Wang, Y; Zamorani, G; Zoubian, J; Andreon, S; Aussel, H; Bardelli, S; Bolzonella, M; Boucaud, A; Di Ferdinando, D; Farina, M; Graciá-Carpio, J; Lindholm, V; Maino, D; Mauri, N; Neissner, C; Scottez, V; Zucca, E; Baccigalupi, C; Ballardini, M; Biviano, A; Blanchard, A; Borgani, S; Borlaff, A.S; Burigana, C; Cabanac, R; Cappi, A; Carvalho, C.S; Casas, S; Castignani, G; Chambers, K; Cooray, A.R; Courtois, H.M; Cucciati, O; Davini, S; de Lucia, G; Dole, H; Escartin, J.A; Escoffier, S; Finelli, F; Fotopoulou, S; Ganga, K; George, K; Gozaliasl, G; Hildebrandt, H; Hook, I; Muñoz, A. Jimenez; Joachimi, B; Kansal, V; Keihanen, E; Kirkpatrick, C.C; Loureiro, A; Macias-Perez, J; Maggio, G; Magliocchetti, M; Maoli, R; Marcin, S; Martinelli, M; Martinet, N; Matthew, S; Maurin, L; Metcalf, R.B; Monaco, P; Morgante, G; Nadathur, S; Nucita, A.A; Patrizii, L; Pollack, J.E; Popa, V; Porciani, C; Potter, D; Pourtsidou, A; Pozzetti, L; Pöntinen, M; Reimberg, P; Sánchez, A.G; Sakr, Z; Sefusatti, E; Sereno, M; Mancini, A. Spurio; Stadel, J; Steinwagner, J; Teyssier, R; Valieri, C; Valiviita, J; van Mierlo, S.E; Veropalumbo, A; Viel, M; Weaver, J.R
Source:
ISSN: 0004-6361.
Subject Terms:
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Document Type:
article in journal/newspaper
Language:
English

Additional Information
- Contributors:
  Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)); Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS); Laboratoire d'Astrophysique de Marseille (LAM); Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales Toulouse (CNES)-Centre National de la Recherche Scientifique (CNRS); Institut d'astrophysique spatiale (IAS); Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales Paris (CNES); Centre National d'Études Spatiales Toulouse (CNES); Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3); Institut de Physique des 2 Infinis de Lyon (IP2I Lyon); Université Claude Bernard Lyon 1 (UCBL); Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS); Centre de Physique des Particules de Marseille (CPPM); Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS); Institut d'Astrophysique de Paris (IAP); Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS); Joseph Louis LAGRANGE (LAGRANGE); Université Nice Sophia Antipolis (1965 - 2019) (UNS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur; Université Côte d'Azur (UniCA)-Université Côte d'Azur (UniCA)-Centre National de la Recherche Scientifique (CNRS); AstroParticule et Cosmologie (APC (UMR_7164)); Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris; Université Paris Sciences et Lettres (PSL)-Université Paris Sciences et Lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité); Institut de recherche en astrophysique et planétologie (IRAP); Université Toulouse III - Paul Sabatier (UT3); Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP); Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3); Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales Toulouse (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales Toulouse (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France-Centre National de la Recherche Scientifique (CNRS); Evaluation des technologies de santé et des pratiques médicales - ULR 2694 (METRICS); Université de Lille-Centre Hospitalier Régional Universitaire CHU Lille (CHRU Lille); Laboratoire de Physique Subatomique et de Cosmologie (LPSC); Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ); Université Grenoble Alpes (UGA); Euclid
- Publication Information:
  HAL CCSD
  EDP Sciences
- Publication Date:
  2024
- Collection:
  LillOA (HAL Lille Open Archive, Université de Lille)
- Abstract:
  International audience ; The technique of photometric redshifts has become essential for the exploitation of multi-band extragalactic surveys. While the requirements on photo-zs for the study of galaxy evolution mostly pertain to the precision and to the fraction of outliers, the most stringent requirement in their use in cosmology is on the accuracy, with a level of bias at the sub-percent level for the Euclid cosmology mission. A separate, and challenging, calibration process is needed to control the bias at this level of accuracy. The bias in photo-zs has several distinct origins that may not always be easily overcome. We identify here one source of bias linked to the spatial or time variability of the passbands used to determine the photometric colours of galaxies. We first quantified the effect as observed on several well-known photometric cameras, and found in particular that, due to the properties of optical filters, the redshifts of off-axis sources are usually overestimated. We show using simple simulations that the detailed and complex changes in the shape can be mostly ignored and that it is sufficient to know the mean wavelength of the passbands of each photometric observation to correct almost exactly for this bias; the key point is that this mean wavelength is independent of the spectral energy distribution of the source. We use this property to propose a correction that can be computationally efficiently implemented in some photo-z algorithms, in particular template-fitting. We verified that our algorithm, implemented in the new photo-z code Phosphoros, can effectively reduce the bias in photo-zs on real data using the CFHTLS T007 survey, with an average measured bias Delta z over the redshift range 0.4
- Relation:
  info:eu-repo/semantics/altIdentifier/arxiv/2310.14716; hal-04268683; https://hal.science/hal-04268683; https://hal.science/hal-04268683/document; https://hal.science/hal-04268683/file/aa46993-23.pdf; ARXIV: 2310.14716; INSPIRE: 2713505
- Accession Number:
  10.1051/0004-6361/202346993
- Online Access:
  https://doi.org/10.1051/0004-6361/202346993
  https://hal.science/hal-04268683
  https://hal.science/hal-04268683/document
  https://hal.science/hal-04268683/file/aa46993-23.pdf
- Rights:
  info:eu-repo/semantics/OpenAccess
- Accession Number:
  edsbas.A7C66188

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