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134 results on '"Castander F.J."'

1. CosmoHub: Interactive exploration and distribution of astronomical data on Hadoop

Author: Tallada, P., Carretero, J., Casals, J., Acosta-Silva, C., Serrano, S., Caubet, M., Castander, F.J., César, E., Crocce, M., Delfino, M., Eriksen, M., Fosalba, P., Gaztañaga, E., Merino, G., Neissner, C., and Tonello, N.
Published: 2020
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2. The PAU Survey: Operation and orchestration of multi-band survey data

Author: Tonello, N., Tallada, P., Serrano, S., Carretero, J., Eriksen, M., Folger, M., Neissner, C., Sevilla-Noarbe, I., Castander, F.J., Delfino, M., De Vicente, J., Fernandez, E., Garcia-Bellido, J., Gaztanaga, E., Padilla, C., Sanchez, E., and Tortorelli, L.
Published: 2019
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3. DES science portal: Computing photometric redshifts

Author: Gschwend, J., Rossel, A.C., Ogando, R.L.C., Neto, A.F., Maia, M.A.G., da Costa, L.N., Lima, M., Pellegrini, P., Campisano, R., Singulani, C., Adean, C., Benoist, C., Aguena, M., Carrasco Kind, M., Davis, T.M., de Vicente, J., Hartley, W.G., Hoyle, B., Palmese, A., Sadeh, I., Abbott, T.M.C., Abdalla, F.B., Allam, S., Annis, J., Asorey, J., Brooks, D., Calcino, J., Carollo, D., Castander, F.J., D’Andrea, C.B., Desai, S., Evrard, A.E., Fosalba, P., Frieman, J., García-Bellido, J., Glazebrook, K., Gerdes, D.W., Gruendl, R.A., Gutierrez, G., Hinton, S., Hollowood, D.L., Honscheid, K., Hoormann, J.K., James, D.J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G., Lidman, C., Lin, H., Macaulay, E., Marshall, J., Melchior, P., Miquel, R., Möller, A., Plazas, A.A., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R.H., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Sommer, N.E., Suchyta, E., Swanson, M.E.C., Tarle, G., Tucker, B.E., Tucker, D.L., Uddin, S., and Walker, A.R.
Published: 2018
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4. Skip Nav Destination The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Author: Kelsey, L., Sullivan, M., Smith, M., Wiseman, P., Brout, D., Davis, T.M., Frohmaier, C., Galbany, L., Grayling, M., Gutiérrez, C.P., Hinton, S.R., Kessler, R., Lidman, C., Möller, A., Sako, M., Scolnic, D., Uddin, S.A., Vincenzi, M., Abbott, T.M.C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Brooks, D., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Costanzi, M., Da Costa, L.N., Desai, S., Diehl, H.T., Doel, P., Everett, S., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., García-Bellido, J., Gerdes, D.W., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Hollowood, D.L., Honscheid, K., James, D.J., Kim, A.G., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J.L., Martini, P., Menanteau, F., Miquel, R., Morgan, R., Ogando, R.L.C., Palmese, A., Paz-Chinchón, F., Plazas, A.A., Romer, A.K., Sánchez, C., Sanchez, E., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T.N., Walker, A.R., Wilkinson, R.D., Laboratoire de Physique de Clermont (LPC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), DES, and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS)
Subjects: surveys, supernovae: general, cosmology: observations, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; Analyses of Type Ia supernovae (SNe Ia) have found puzzling correlations between their standardized luminosities and host galaxy properties: SNe Ia in high-mass, passive hosts appear brighter than those in lower mass, star-forming hosts. We examine the host galaxies of SNe Ia in the Dark Energy Survey 3-yr spectroscopically confirmed cosmological sample, obtaining photometry in a series of ‘local’ apertures centred on the SN, and for the global host galaxy. We study the differences in these host galaxy properties, such as stellar mass and rest-frame U − R colours, and their correlations with SN Ia parameters including Hubble residuals. We find all Hubble residual steps to be >3σ in significance, both for splitting at the traditional environmental property sample median and for the step of maximum significance. For stellar mass, we find a maximal local step of 0.098 ± 0.018 mag; ∼0.03 mag greater than the largest global stellar mass step in our sample (0.070 ± 0.017 mag). When splitting at the sample median, differences between local and global U − R steps are small, both ∼0.08 mag, but are more significant than the global stellar mass step (0.057 ± 0.017 mag). We split the data into sub-samples based on SN Ia light-curve parameters: stretch (x_1) and colour (c), finding that redder objects (c > 0) have larger Hubble residual steps, for both stellar mass and U − R, for both local and global measurements, of ∼0.14 mag. Additionally, the bluer (star-forming) local environments host a more homogeneous SN Ia sample, with local U − R rms scatter as low as 0.084 ± 0.017 mag for blue (c < 0) SNe Ia in locally blue U − R environments.
Published: 2021
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5. Erratum. Euclid preparation. VI. Verifying the performance of cosmic shear experiments

Author: Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V.F., Cropper, M., Duncan, C.A.J., Kannawadi Jayaraman, A., Miller, L., Aussel, H., Conti, I.F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castander, F.J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H.M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P.G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B.R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C.C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P.B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R.B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R.C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sánchez, A.G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J.-L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., and Zucca, E.
Abstract: This article is an erratum for:[https://doi.org/10.1051/0004-6361/201936980]
Published: 2020

6. Euclid: the selection of quiescent and star-forming galaxies using observed colours

Author: Bisigello, L., Kuchner, U., Conselice, C.J., Andreon, S., Bolzonella, M., Duc, P-A, Garilli, B., Humphrey, A., Maraston, C., Moresco, M., Pozzetti, L., Tortora, C., Zamorani, G., Auricchio, N., Brinchmann, J., Capobianco, V., Carretero, J., Castander, F.J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Corcione, L., Cropper, M.S., Dusini, S., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Hormuth, F., Israel, H., Jahnke, K., Kermiche, S., Kitching, T., Kohley, R., Kubik, B., Kunz, M., Ligori, S., Lilje, P.B., Lloro, I., Maiorano, E., Marggraf, O., Massey, R., Masters, D.C., Mei, S., Mellier, Y., Meylan, G., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Raison, F., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Sauvage, M., Schneider, P., Secroun, A., Serrano, S., Sureau, F., Taylor, A.N., Tereno, I., Toledo-Moreo, R., Valenziano, L., Wang, Y, Wetzstein, M., and Zoubian, J.
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Abstract: The Euclid mission will observe well over a billion galaxies out to z ∼ 6 and beyond. This will offer an unrivalled opportunity to investigate several key questions for understanding galaxy formation and evolution. The first step for many of these studies will be the selection of a sample of quiescent and star-forming galaxies, as is often done in the literature by using well-known colour techniques such as the ‘UVJ’ diagram. However, given the limited number of filters available for the Euclid telescope, the recovery of such rest-frame colours will be challenging. We therefore investigate the use of observed Euclid colours, on their own and together with ground-based u-band observations, for selecting quiescent and star-forming galaxies. The most efficient colour combination, among the ones tested in this work, consists of the (u − VIS) and (VIS − J) colours. We find that this combination allows users to select a sample of quiescent galaxies complete to above ∼70 per cent and with less than 15 per cent contamination at redshifts in the range 0.75 < z < 1. For galaxies at high-z or without the u-band complementary observations, the (VIS − Y) and (J − H) colours represent a valid alternative, with >65 per cent completeness level and contamination below 20 per cent at 1 < z < 2 for finding quiescent galaxies. In comparison, the sample of quiescent galaxies selected with the traditional UVJ technique is only ∼20 per cent complete at z < 3, when recovering the rest-frame colours using mock Euclid observations. This shows that our new methodology is the most suitable one when only Euclid bands, along with u-band imaging, are available.
Published: 2020

7. Euclid preparation

Author: Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V.F., Cropper, M., Duncan, C.A.J., Kannawadi Jayaraman, A., Miller, L., Aussel, H., Conti, I.F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castander, F.J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H.M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P.G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B.R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C.C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P.B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R.B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R.C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sánchez, A.G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J.-L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., Zucca, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique Nucléaire de Lyon (IPNL), 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), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Euclid, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), 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), 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 de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astronomy Centre, University of Sussex, Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Astronomie (MPIA), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, European Project: 617656,EC:FP7:ERC,ERC-2013-CoG,THEMODS(2014), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), University of Helsinki, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut national de recherches archéologiques préventives (Inrap), Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-CY Cergy Paris Université (CY)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Particle Physics and Astrophysics, Department of Physics, Helsinki Institute of Physics, Science and Technology Facilities Council (UK), Royal Society (UK), Dutch Research Council, Netherlands Organization for Scientific Research, UK Space Agency, Swiss National Science Foundation, European Commission, Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V. F., Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Conti, I. F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B. R., Giocoli, C., Gracia-Carpio, J., Grupp, F., Hormuth, F., Ilic, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P. B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sanchez, A. G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Sureau, F., Tallada-Crespi, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., Zucca, E., Da Silva, A., Graciá-Carpio, J., Ilić, S., Sánchez, A. G., Starck, J.-L., and Tallada-Crespí, P.
Subjects: Point spread function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ComputerSystemsOrganization_COMPUTERSYSTEMIMPLEMENTATION, Pipeline (computing), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Residual, 7. Clean energy, 01 natural sciences, gravitational lensing: weak, 0103 physical sciences, Statistical physics, 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, CALIBRATION, CHARGE-TRANSFER INEFFICIENCY, COSMIC cancer database, 010308 nuclear & particles physics, Computer Science::Information Retrieval, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 115 Astronomy, Space science, Galaxy, Shear (sheet metal), CHALLENGE LIGHTCONE SIMULATION, BIAS, Space and Planetary Science, astro-ph.CO, Dark energy, DARK ENERGY, SENSITIVITY, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], REQUIREMENTS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. Our aim is to quantify the impact of systematic effects on the inference of cosmological parameters from cosmic shear. Methods. We present an "end-to-end" approach that introduces sources of bias in a modelled weak lensing survey on a galaxy-by-galaxy level. We propagated residual biases through a pipeline from galaxy properties at one end to cosmic shear power spectra and cosmological parameter estimates at the other end. We did this to quantify how imperfect knowledge of the pipeline changes the maximum likelihood values of dark energy parameters. Results. We quantify the impact of an imperfect correction for charge transfer inefficiency and modelling uncertainties of the point spread function for Euclid, and find that the biases introduced can be corrected to acceptable levels., PP is supported by an STFC consolidated grant. CW is supported by an STFC urgency grant. TDK is supported by a Royal Society University Research Fellowship. HH acknowledges support from Vici grant 639.043.512 and an NWO-G grant financed by the Netherlands Organization for Scientific Research. LM and CD are supported by UK Space Agency grant ST/N001796/1. VFC is funded by Italian Space Agency (ASI) through contract Euclid – IC (I/031/10/0) and acknowledges financial contribution from the agreement ASI/INAF/I/023/12/0. We would like to thank Jérome Amiaux, Koryo Okumura, Samuel Ronayette for running the ZEMAX simulations. AP is a UK Research and Innovation Future Leaders Fellow, grant MR/S016066/1, and also acknowledges support from the UK Science & Technology Facilities Council through grant ST/S000437/1. MK and FL acknowledge financial support from the Swiss National Science Foundation. SI acknowledges financial support from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007–2013)/ERC Grant Agreement No. 617656 “Theories and Models of the Dark Sector: Dark Matter, Dark Energy and Gravity”.
Published: 2020
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8. The Future Landscape of High-Redshift Galaxy Cluster Science

Author: Mantz, A., Allen, S.W., Battaglia, N., Benson, B., Canning, R., Ettori, S., Evrard, A., Linden, A., McDonald, M., Abidi, M., Ahmed, Z., Amin, Mustafa.A., Ansarinejad, B., Armstrong, R., Avestruz, C., Baccigalupi, C., Bandura, K., Barkhouse, W., Basu, K., Bavdhankar, C., Bender, A.N., Bernardis, P., Bischoff, C., Biviano, A., Bleem, L., Bocquet, S., Bond, J., Borgani, S., Borrill, J., Boutigny, D., Frye, B., Bruggen, M., Cai, Z., Carlstrom, J.E., Castander, F.J., Challinor, A., Clowe, D., Cohn, J.D., Comparat, J., Cooray, A., Coulton, W., Cyr-Racine, F., Daddi, E., Delabrouille, J., Dell'antonio, I., Demarteau, M., Donahue, M., Dunkley, J., Escoffier, S., Essinger-Hileman, T., Fabbian, G., Fabjan, D., Farahi, A., Foreman, S., Fraisse, A.A., Garcia, L., Gaspari, M., Gerbino, M., Gitti, M., Gluscevic, V., Gonzalez, A., Górski, K.M., Gruen, D., Gudmundsson, J.E., Gupta, N., Haan, T., Hernquist, L., Hirata, C.M., Hlozek, R., Jeltema, T., Cohen-Tanugi, J., Johnson, B., Kadota, K., Kamionkowski, M., Khatri, R., Kisner, T., Kneib, J., Knox, L., Kovetz, E.D., Krause, E., Lattanzi, M., Lau, Erwin.T., Liguori, M., Lovisari, L., Macorra, A., Masi, S., Masui, K., Maughan, B., Maurogordato, S., McMahon, J., McNamara, B., Melchior, P., Mertens, J., Meyers, J., Mirbabayi, M., More, S., Motloch, P., Moustakas, J., Mroczkowski, T., Mukherjee, S., Nagai, D., Nagy, J., Naselsky, P., Nati, F., Newburgh, L., Niemack, M.D., Nomerotski, A., Noordeh, E., Ntampaka, M., Ota, N., Page, L., Palmese, A., Penna-Lima, M., Piacentni, F., Pierpaoli, E., Plazas, A.A., Pogosian, L., Pointecouteau, E., Prakash, A., Pratt, G., Prescod-Weinstein, C., Pryke, C., Puglisi, G., Rapetti, D., Raveri, M., Reichardt, C.L., Reiprich, Thomas.H., Remazeilles, M., Rhodes, J., Ricci, M., Rocha, G., Rose, B., Rozo, E., Ruhl, J., Sadun, A., Saliwanchik, B., Schaan, E., Schmidt, R., Fromenteau, S., Sehgal, N., Senatore, L., Seo, H., Sereno, M., Shafieloo, A., Shan, H., Shandera, S., Sherwin, B.D., Simon, S., Sridhar, S., Staggs, S., Stern, D., Suzuki, A., Tsai, Y., Turriziani, S., Umilta, C., Vazza, F., Vieregg, A., Vikhlinin, A., Walker, S.A., Watson, S., Weeren, R.J. van, Weller, J., Werner, N., Whitehorn, N., Wong, K., Wright, A., Wu, W.L.K., Xu, Z., Yasini, S., Zemcov, M., Zhang, Y., Zhao, G., Zheng, Y., Zhu, N., Zhuravleva, I., Zuntz, J., Hickox, R., Churazov, E., Nulsen, P., Jones, W.C., Wang, L., and Desai, S.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We describe the opportunities for galaxy cluster science in the high- redshift regime where massive, virialized halos first formed and where star formation and AGN activity peaked. New observing facilities from radio to X-ray wavelengths, combining high spatial/spectral resolution with large collecting areas, are poised to uncover this population.
Published: 2019

9. Dark Energy Survey Year 1 Results: Cross-correlation between Dark Energy Survey Y1 galaxy weak lensing and South Pole Telescope +Planck CMB weak lensing

Author: Omori, Y., Baxter, E.J., Kirk, D., Alarcon, A., Bernstein, G.M., Bleem, L.E., Cawthon, R., Choi, A., Chown, R., Crawford, T.M., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T.F., Fosalba, P., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Gruen, D., Hartley, W.G., Holder, G.P., Hoyle, B., Huterer, D., Jain, B., Jarvis, M., Krause, E., MacCrann, N., Miquel, R., Prat, J., Rau, M.M., Reichardt, C.L., ROZO, E., Samuroff, S., Sánchez, C., Secco, L.F., Sheldon, E., Simard, G., Troxel, M.A., Vielzeuf, P., Wechsler, R.H., Zuntz, J., Abbott, T.M.C., Abdalla, F.B., Allam, S., Annis, J., Avila, S., Aylor, K., Benson, B.A., Bertin, E., Bridle, S.L., Brooks, D., Burke, D.L., Carlstrom, J.E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Chang, C.L., Cho, H-M., Crites, A.T., Crocce, M., Cunha, C.E., Da Costa, L.N., De Haan, T., Desai, S., Diehl, H.T., Dietrich, J.P., Dobbs, M.A., Everett, W.B., Fernandez, E., Flaugher, B., Frieman, J., García-Bellido, J., George, E.M., Gruendl, R.A., Gutierrez, G., Halverson, N.W., Harrington, N.L., Hollowood, D.L., Honscheid, K., Holzapfel, W.L., Hou, Z., Hrubes, J.D., James, D.J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Lee, A.T., Leitch, E.M., Luong-Van, D., Maia, M.A.G., Manzotti, A., Marrone, D.P., Marshall, J.L., Martini, P., McMahon, J.J., Melchior, P., Menanteau, F., Meyer, S.S., Mocanu, L.M., Mohr, J.J., Natoli, T., Ogando, R.L.C., Padin, S., Plazas, A.A., Pryke, C., Romer, A.K., Roodman, A., Ruhl, J.E., Rykoff, E.S., Sanchez, E., Scarpine, V., Schaffer, K.K., Schindler, R., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R.C., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A.A., Story, K.T., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J.D., Vikram, V., Walker, A.R., Weller, J., Williamson, R., Wu, W.L.K., Zahn, O., 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), DES, and SPT
Subjects: Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmology
Abstract: International audience; We cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg2. With the combined measurements from four source galaxy redshift bins, we obtain a detection significance of 5.8σ. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial ΛCDM model, finding A=0.99±0.17. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the ΛCDM model, we obtain the marginalized constraints of Ωm=0.261-0.051+0.070 and S8≡σ8Ωm/0.3=0.660-0.100+0.085. These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT, and Planck data.
Published: 2019
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10. Three new VHS–DES quasars at 6.7 < z < 6.9 and emission line properties at z > 6.5

Author: Reed, S.L., Banerji, M., Becker, G.D., Hewett, P.C., Martini, P., Mcmahon, R.G., Pons, E., Rauch, M., Abbott, T.M.C., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Cunha, C.E., D'Andrea, C.B., Da Costa, L.N., De Vicente, J., Desai, S., Diehl, H.T., Doel, P., Evrard, A.E., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hollowood, D.L., Honscheid, K., Hoyle, B., James, D.J., Kuehn, K., Lahav, O., Lima, M., Maia, M.A.G., Marshall, J.L., Miquel, R., Ogando, R.L.C., Plazas, A.A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Tucker, D.L., Vikram, V., 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), and DES
Subjects: galaxies: high-redshift, quasars: individual: VDES J0224−4711, quasars: individual: VDES J0244−5008, first stars, galaxies: active, quasars: individual: VDES J0020−3653, reionization, galaxies: formation, quasars: individual: VDES J0246−5219, dark ages, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the results from a search for z > 6.5 quasars using the Dark Energy Survey (DES) Year 3 dataset combined with the VISTA Hemisphere Survey (VHS) and WISE All-Sky Survey. Our photometric selection method is shown to be highly efficient in identifying clean samples of high-redshift quasars leading to spectroscopic confirmation of three new quasars - VDESJ 0244-5008 (z=6.724), VDESJ 0020-3653 (z=6.834) and VDESJ 0246-5219 (z=6.90) - which were selected as the highest priority candidates in the survey data without any need for additional follow-up observations. The new quasars span the full range in luminosity covered by other z>6.5 quasar samples (J AB = 20.2 to 21.3; M1450 = -25.6 to -26.6). We have obtained spectroscopic observations in the near infrared for VDESJ 0244-5008 and VDESJ 0020-3653 as well as our previously identified quasar, VDESJ 0224-4711 at z=6.50 from Reed et al. (2017). We use the near infrared spectra to derive virial black-hole masses from the full-width-half-maximum of the MgII line. These black-hole masses are ~ 1 - 2 x 10$^9$M$_\odot$. Combining with the bolometric luminosities of these quasars of L$_{\rm{bol}}\simeq$ 1 - 3 x 10$^{47}$implies that the Eddington ratios are high - $\simeq$0.6-1.1. We consider the C\textrm{\textsc{IV}} emission line properties of the sample and demonstrate that our high-redshift quasars do not have unusual C\textrm{\textsc{IV}} line properties when compared to carefully matched low-redshift samples. Our new DES+VHS $z>6.5$ quasars now add to the growing census of luminous, rapidly accreting supermassive black-holes seen well into the epoch of reionisation., Comment: 12 pages, 9 figures
Published: 2019
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11. Dark Energy Survey Year 1 Results: Tomographic cross-correlations between Dark Energy Survey galaxies and CMB lensing from South Pole Telescope+Planck

Author: Omori, Y., Giannantonio, T., Porredon, A., Baxter, E.J., Crocce, M., Fosalba, P., Alarcon, A., Banik, N., Blazek, J., Bleem, L.E., Bridle, S.L., Cawthon, R., Choi, A., Chown, R., Crawford, T., Dodelson, S., Drlica-Wagner, A., Eifler, T.F., Elvin-Poole, J., Friedrich, O., Gruen, D., Holder, G.P., Huterer, D., Jain, B., Jarvis, M., Kirk, D., Kokron, N., Krause, E., MacCrann, N., Muir, J., Prat, J., Reichardt, C.L., Ross, A.J., ROZO, E., Rykoff, E.S., Sánchez, C., Secco, L.F., Simard, G., Wechsler, R.H., Zuntz, J., Abbott, T.M.C., Abdalla, F.B., Allam, S., Avila, S., Aylor, K., Benson, B.A., Bernstein, G.M., Bertin, E., Bianchini, F., Brooks, D., Buckley-Geer, E., Burke, D.L., Carlstrom, J.E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Chang, C.L., Cho, H-M., Crites, A.T., Cunha, C.E., Da Costa, L.N., De Haan, T., Davis, C., De Vicente, J., Desai, S., Diehl, H.T., Dietrich, J.P., Dobbs, M.A., Everett, W.B., Doel, P., Estrada, J., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., George, E.M., Gruendl, R.A., Gschwend, J., Gutierrez, G., Halverson, N.W., Harrington, N.L., Hartley, W.G., Hollowood, D.L., Holzapfel, W.L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J.D., James, D.J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lee, A.T., Leitch, E.M., Lima, M., Luong-Van, D., Manzotti, A., Marrone, D.P., Marshall, J.L., McMahon, J.J., Melchior, P., Menanteau, F., Meyer, S.S., Miller, C.J., Miquel, R., Mocanu, L.M., Mohr, J.J., Natoli, T., Padin, S., Plazas, A.A., Pryke, C., Romer, A.K., Roodman, A., Ruhl, J.E., Sanchez, E., Scarpine, V., Schaffer, K.K., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A.A., Story, K.T., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Troxel, M.A., Vanderlinde, K., Vieira, J.D., Walker, A.R., Wu, W.L.K., Zahn, O., 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), DES, SPT, and UAM. Departamento de Física Teórica
Subjects: Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, 0103 physical sciences, media_common.cataloged_instance, European union, 010306 general physics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), STFC, ComputingMilieux_MISCELLANEOUS, QC, media_common, Physics, 010308 nuclear & particles physics, European research, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Física, GALÁXIAS, Cosmology, South Pole Telescope, 13. Climate action, Research council, Fundamental physics, Christian ministry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Kavli Foundation; Natural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Canada Research Chairs program; U.S. Department of Energy [DE-SC0007901]; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-1125897]; Australian Research Council Future Fellowship [FT150100074]; Fermi Research Alliance, LLC [De-AC02-07CH11359]; United States Department of Energy; National Science Foundation [OCI-0725070, ACI-1238993]; NSF Physics Frontier Center [PHY-0114422]; Kavli Institute of Cosmological Physics at the University of Chicago; Gordon and Betty Moore Foundation; GBMF [947]; National Aeronautics and Space Administration; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; University of California at Santa Cruz; University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Ludwig-Maximilians Universitat Munchen; University of Portsmouth; OzDES Membership Consortium; Association of Universities for Research in Astronomy (AURA); MINECO [AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509]; ERDF; European Union - CERCA program of the Generalitat de Catalunya; European Research Council under the European Union [240672, 291329, 306478]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq) [De-AC02-07CH11359, 465376/2014-2]; U.S. Department of Energy, Office of Science, Office of High Energy Physics - Canada Foundation for Innovation (CFI); ministere de l'Economie, de la science et de l'innovation du Quebec (MESI); Fonds de recherche du Quebec-Nature et technologies (FRQ-NT); state of Illinois; University of Illinois at Urbana-Champaign [49,70, MATPLOTLIB [75], 76,77]
Published: 2019
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12. Improving Weak Lensing Mass Map Reconstructions using Gaussian and Sparsity Priors: Application to DES SV

Author: Jeffrey, N., Abdalla, F.B., Lahav, O., Lanusse, F., Starck, J.-L., Leonard, A., Kirk, D., Chang, C., Baxter, E., Kacprzak, T., Seitz, S., Vikram, V., Whiteway, L., Abbott, T.M.C., Allam, S., Avila, S., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D'Andrea, C.B., Da Costa, L.N., Davis, C., De Vicente, J., Desai, S., Doel, P., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D.W., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Hartley, W.G., Honscheid, K., Hoyle, B., James, D.J., Jarvis, M., Kuehn, K., Lima, M., Lin, H., March, M., Melchior, P., Menanteau, F., Miquel, R., Plazas, A.A., Reil, K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Walker, A.R., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), DES, 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 AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational lensing: weak, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Mapping the underlying density field, including non-visible dark matter, using weak gravitational lensing measurements is now a standard tool in cosmology. Due to its importance to the science results of current and upcoming surveys, the quality of the convergence reconstruction methods should be well understood. We compare three methods: Kaiser-Squires (KS), Wiener filter, and GLIMPSE. KS is a direct inversion, not accounting for survey masks or noise. The Wiener filter is well-motivated for Gaussian density fields in a Bayesian framework. GLIMPSE uses sparsity, aiming to reconstruct non-linearities in the density field. We compare these methods with several tests using public Dark Energy Survey (DES) Science Verification (SV) data and realistic DES simulations. The Wiener filter and GLIMPSE offer substantial improvements over smoothed KS with a range of metrics. Both the Wiener filter and GLIMPSE convergence reconstructions show a 12 per cent improvement in Pearson correlation with the underlying truth from simulations. To compare the mapping methods' abilities to find mass peaks, we measure the difference between peak counts from simulated {\Lambda}CDM shear catalogues and catalogues with no mass fluctuations (a standard data vector when inferring cosmology from peak statistics); the maximum signal-to-noise of these peak statistics is increased by a factor of 3.5 for the Wiener filter and 9 for GLIMPSE. With simulations we measure the reconstruction of the harmonic phases; the phase residuals' concentration is improved 17 per cent by GLIMPSE and 18 per cent by the Wiener filter. The correlation between reconstructions from data and foreground redMaPPer clusters is increased 18 per cent by the Wiener filter and 32 per cent by GLIMPSE., Comment: 19 pages, 10 figures, MNRAS published: 15 May 2018
Published: 2018
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13. Evidence for Dynamically Driven Formation of the GW170817 Neutron Star Binary in NGC 4993

Author: Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, galaxies: structure – gravitational waves, galaxies: individual (NGC 4993), Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: We present a study of NGC 4993, the host galaxy of the GW170817 gravitational-wave event, the GRB 170817A short gamma-ray burst (sGRB), and the AT 2017gfo kilonova. We use Dark Energy Camera imaging, AAT spectra, and publicly available data, relating our findings to binary neutron star (BNS) formation scenarios and merger delay timescales. NGC 4993 is a nearby early-type galaxy, with an i-band Sérsic index n = 4.0 and low asymmetry (A = 0.04 ± 0.01). These properties are unusual for sGRB hosts. However, NGC 4993 presents shell-like structures and dust lanes indicative of a recent galaxy merger, with the optical transient located close to a shell. We constrain the star formation history (SFH) of the galaxy assuming that the galaxy merger produced a star formation burst, but find little to no ongoing star formation in either spatially resolved broadband SED or spectral fitting. We use the best-fit SFH to estimate the BNS merger rate in this type of galaxy, as ${R}_{\mathrm{NSM}}^{\mathrm{gal}}={5.7}_{-3.3}^{+0.57}\times {10}^{-6}{\mathrm{yr}}^{-1}$. If star formation is the only considered BNS formation scenario, the expected number of BNS mergers from early-type galaxies detectable with LIGO during its first two observing seasons is ${0.038}_{-0.022}^{+0.004}$, as opposed to ~0.5 from all galaxy types. Hypothesizing that the binary formed due to dynamical interactions during the galaxy merger, the subsequent time elapsed can constrain the delay time of the BNS coalescence. By using velocity dispersion estimates and the position of the shells, we find that the galaxy merger occurred t mer lesssim 200 Myr prior to the BNS coalescence.
Published: 2017

14. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Discovery of the Optical Counterpart Using the Dark Energy Camera

Author: Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., Butler, R. E., Palmese, A., Doctor, Z., Diehl, H.T., Frieman, J., Yanny, B., Lin, H., Scolnic, D., Cowperthwaite, P., Neilsen, E., Marriner, J., Kuropatkin, N., Hartley, W.G., Alexander, K.D., Balbinot, E., Blanchard, P., Brown, D.A., Carlin, J.L., Conselice, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., Finley, D.A., Foley, R.J., Fong, W., Fryer, C.L., Gill, M.S.S., Gruendl, R.A., Hanna, C., Kasen, D., Li, T.S., Lopes, P.A.A., Margutti, R., Marshall, J.L., Matheson, T., Medina, G.E., Metzger, B.D., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D.J., Secco, L.F., Sobreira, F., Stebbins, A., Villar, V.A., Vivas, K., Walker, A.R., Wester, W., Williams, P.K.G., Zenteno, A., Zhang, Y., Abbott, T.M.C., Abdalla, F.B., Banerji, M., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D.L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., Costa, L.N. da, Davis, C., Desai, S., Dietrich, J.P., Doel, P., Eifler, T.F., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Goldstein, D.A., Gruen, D., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M.A.G., March, M., McMahon, R.G., Menanteau, F., Miquel, R., Mohr, J.J., Nichol, R.C., Nord, B., Ogando, R.L C., Petravick, D., Plazas, A.A., Romer, A.K., Roodman, A., Rykoff, E.S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Troxel, M.A., Vikram, V., Wechsler, R.H., and Weller, J.
Subjects: binaries: close— catalogs— gravitational waves — stars: neutron— surveys
Abstract: We present the Dark Energy Camera (DECam) discovery of the optical counterpart of the first binary neutron star merger detected through gravitational wave emission, GW170817. Our observations commenced 10.5 hours post-merger, as soon as the localization region became accessible from Chile. We imaged 70 deg2 in the i and z bands, covering 93% of the initial integrated localization probability, to a depth necessary to identify likely optical counterparts (e.g., a kilonova). At 11.4 hours post-merger we detected a bright optical transient located 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -15.7, in the luminosity range expected for a kilonova. We identified 1,500 potential transient candidates. Applying simple selection criteria aimed at rejecting background events such as supernovae, we find the transient associated with NGC4993 as the only remaining plausible counterpart, and reject chance coincidence at the 99.5% confidence level. We therefore conclude that the optical counterpart we have identified near NGC4993 is associated with GW170817. This discovery ushers in the era of multi-messenger astronomy with gravitational waves, and demonstrates the power of DECam to identify the optical counterparts of gravitational-wave sources.
Published: 2017

15. Optical and near-infrared observations of the afterglow of GRB 980329 from 15 hours to 10 days

Author: Quashnock, J.M., Castander, F.J., Lamb, D.Q., Cooray, A.R., Rhoads, J.E., Reichart, D.E., Cole, D.M., Fruchter, A.S., Klose, S., Metzger, M.R., and Vanden Berk, D.E.
Abstract: We report I-band observations of the GRB 980329 field made on 1998 March 29 with the 1.34 m Tautenberg Schmidt telescope, R-, J- and K-band observations made on 1998 April 1 with the APO 3.5 m telescope, R- and I-band observations made on 1998 April 3 with the Mayall 4 m telescope at KPNO, and J- and K-band observations made 1998 April 6-8 with the Keck-I 10 m telescope. We show that these and other reported measurements are consistent with a power-law fading of the optical/near-infrared source that is coincident with the variable radio source VLA J0702+3850. This firmly establishes that this source is the afterglow of GRB 980329.
Published: 1999
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16. A deficit of high-redshift, high-luminosity X-ray clusters: Evidence for a high value of Ωm?

Author: Nichol, R.C., Reichart, D.E., Castander, F.J., Collins, C.A., Romer, A.K., Ulmer, M.P., Burke, D.J., and Holden, B.P.
Abstract: From the Press-Schechter mass function and the empirical X-ray cluster luminosity-temperature (L-T) relation, we construct an X-ray cluster luminosity function that can be applied to the growing number of high-redshift, X-ray cluster luminosity catalogs to constrain cosmological parameters. In this paper, we apply this luminosity function to the Einstein Medium Sensitivity Survey (EMSS) and the ROSAT Brightest Cluster Sample (BCS) luminosity function to constrain the value of Ωm. In the case of the EMSS, we find a factor of 4-5 fewer X-ray clusters at redshifts above z = 0.4 than below this redshift at luminosities above LX = 7 × 1044 ergs s-1 (0.3-3.5 keV), which suggests that the X-ray cluster luminosity function has evolved above L(Black star). At lower luminosities, this luminosity function evolves only minimally, if at all. Using Bayesian inference, we find that the degree of evolution at high luminosities suggests that Ωm = 0.96+0.36-0.32, given the best-fit L-T relation of Reichart, Castander, & Nichol. When we account for the uncertainty in how the empirical L-T relation evolves with redshift, we find that Ωm ≈ 1.0 ± 0.4. However, it is unclear to what degree systematic effects may affect this and similarly obtained results.
Published: 1999
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17. The PAU Survey and Euclid: Improving broadband photometric redshifts with multi-task learning.

Author: Cabayol, L., Eriksen, M., Carretero, J., Casas, R., Castander, F. J., Fernández, E., Garcia-Bellido, J., Gaztanaga, E., Hildebrandt, H., Hoekstra, H., Joachimi, B., Miquel, R., Padilla, C., Pocino, A., Sanchez, E., Serrano, S., Sevilla, I., Siudek, M., Tallada-Crespí, P., and Aghanim, N.
Subjects: EXPANDING universe, GALACTIC redshift, PHOTOMETRY, UNIVERSE, REDSHIFT, GALAXIES
Abstract: Current and future imaging surveys require photometric redshifts (photo-zs) to be estimated for millions of galaxies. Improving the photo-z quality is a major challenge but is needed to advance our understanding of cosmology. In this paper we explore how the synergies between narrow-band photometric data and large imaging surveys can be exploited to improve broadband photometric redshifts. We used a multi-task learning (MTL) network to improve broadband photo-z estimates by simultaneously predicting the broadband photo-z and the narrow-band photometry from the broadband photometry. The narrow-band photometry is only required in the training field, which also enables better photo-z predictions for the galaxies without narrow-band photometry in the wide field. This technique was tested with data from the Physics of the Accelerating Universe Survey (PAUS) in the COSMOS field. We find that the method predicts photo-zs that are 13% more precise down to magnitude iAB< 23; the outlier rate is also 40% lower when compared to the baseline network. Furthermore, MTL reduces the photo-z bias for high-redshift galaxies, improving the redshift distributions for tomographic bins with z > 1. Applying this technique to deeper samples is crucial for future surveys such as Euclid or LSST. For simulated data, training on a sample with iAB < 23, the method reduces the photo-z scatter by 16% for all galaxies with iAB < 25. We also studied the effects of extending the training sample with photometric galaxies using PAUS high-precision photo-zs, which reduces the photo-z scatter by 20% in the COSMOS field. [ABSTRACT FROM AUTHOR]
Published: 2023
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18. Exploring the selection of galaxy clusters and groups: an optical survey for X-ray dark clusters.

Author: Gilbank, David G., Bower, Richard G., Castander, F.J., and Ziegler, B.L.
Subjects: STAR clusters, GALAXIES, METAPHYSICAL cosmology, SUPERCLUSTERS, ASTROPHYSICS, ASTRONOMY
Abstract: Data from a new, wide-field, coincident optical and X-ray survey, the X-ray Dark Cluster Survey (XDCS), are presented. This survey comprises simultaneous and independent searches for clusters of galaxies in the optical and X-ray passbands. Optical cluster detection algorithms implemented on the data are detailed. Two distinct optically selected catalogues are constructed, one based on I-band overdensity, the other on overdensities of colour-selected galaxies. The superior accuracy of the colour-selection technique over that of the single-passband method is demonstrated, via internal consistency checks and comparison with external spectroscopic redshift information. This is compared with an X-ray-selected cluster catalogue. In terms of gross numbers, the survey yields 185 I-band-selected, 290 colour-selected and 15 X-ray-selected systems, residing in ∼11 deg2 of optical + X-ray imaging. The relationship between optical richness/luminosity and X-ray luminosity is examined, by measuring X-ray luminosities at the positions of our 290 colour-selected systems. Power-law correlations between the optical richness/luminosity and X-ray luminosity are fitted, both exhibiting approximately 0.2 dex of intrinsic scatter. Interesting outliers in these correlations are discussed in greater detail. Spectroscopic follow-up of a subsample of X-ray underluminous systems confirms their reality. [ABSTRACT FROM AUTHOR]
Published: 2004
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19. The Purport of Space Telescopes in Supernova Research.

Author: Vinkó, József, Szalai, Tamás, and Könyves-Tóth, Réka
Subjects: SPACE telescopes, COSMIC dust, STELLAR evolution, ASTROPHYSICS, SCIENTIFIC community
Abstract: The violent stellar explosions known as supernovae have received especially strong attention in both the research community and the general public recently. With the advent of space telescopes, the study of these extraordinary events has switched gears and it has become one of the leading fields in modern astrophysics. In this paper, we review some of the recent developments, focusing mainly on studies related to space-based observations. [ABSTRACT FROM AUTHOR]
Published: 2023
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20. The scientific performance of the microchannel X-ray telescope on board the SVOM mission.

Author: Götz, D., Boutelier, M., Burwitz, V., Chipaux, R., Cordier, B., Feldman, C., Ferrando, P., Fort, A., Gonzalez, F., Gros, A., Hussein, S., Le Duigou, J.-M., Meidinger, N., Mercier, K., Meuris, A., Pearson, J., Renault-Tinacci, N., Robinet, F., Schneider, B., and Willingale, R.
Subjects: X-ray telescopes, FOCAL length, ASTROPHYSICS, SPACE telescopes, OPTICS
Abstract: The Microchannel X-ray Telescope (MXT) will be the first focusing X-ray telescope based on a narrow field "Lobster-Eye" optical design to be flown on a satellite, namely the Sino-French mission SVOM. SVOM will be dedicated to the study of Gamma-Ray Bursts and more generally time-domain astrophysics. The MXT telescope is a compact (focal length ∼ 1.15 m) and light (< 42 kg) instrument, sensitive in the 0.2–10 keV energy range. It is composed of an optical system, based on micro-pore optics (MPOs) of 40 μ m pore size, coupled to a low-noise pnCDD X-ray detector. In this paper we describe the expected scientific performance of the MXT telescope, based on the End-to-End calibration campaign performed in fall 2021, before the integration of the SVOM payload on the satellite. [ABSTRACT FROM AUTHOR]
Published: 2023
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21. CATCH: chasing all transients constellation hunters space mission.

Author: Li, Panping, Yin, Qian-Qing, Li, Zhengwei, Tao, Lian, Wen, Xiangyang, Zhang, Shuang-Nan, Qi, Liqiang, Zhang, Juan, Zhao, Donghua, Li, Dalin, Yu, Xizheng, Bu, Qingcui, Chen, Wen, Chen, Yupeng, Huang, Yiming, Huang, Yue, Jin, Ge, Li, Gang, Liu, Hongbang, and Liu, Xiaojing
Subjects: MICROSPACECRAFT, INTELLIGENT control systems, FOCAL length, ARTIFICIAL satellites
Abstract: In time-domain astronomy, a substantial number of transients will be discovered by multi-wavelength and multi-messenger observatories, posing a great challenge for follow-up capabilities. We have thus proposed an intelligent X-ray constellation, the Chasing All Transients Constellation Hunters (CATCH) space mission. Consisting of 126 micro-satellites in three types, CATCH will have the capability to perform follow-up observations for a large number of different types of transients simultaneously. Each satellite in the constellation will carry lightweight X-ray optics and use a deployable mast to increase the focal length. The combination of different optics and detector systems enables different types of satellites to have multiform observation capabilities, including timing, spectroscopy, imaging, and polarization. Controlled by the intelligent system, different satellites can cooperate to perform uninterrupted monitoring, all-sky follow-up observations, and scanning observations with a flexible field of view (FOV) and multi-dimensional observations. Therefore, CATCH will be a powerful mission to study the dynamic universe. Here, we present the current design of the spacecraft, optics, detector system, constellation configuration and observing modes, as well as the development plan. [ABSTRACT FROM AUTHOR]
Published: 2023
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22. Quasar Identification Using Multivariate Probability Density Estimated from Nonparametric Conditional Probabilities.

Author: Farmer, Jenny, Allen, Eve, and Jacobs, Donald J.
Subjects: MAXIMUM entropy method, NONPARAMETRIC estimation, QUASARS, CONDITIONAL probability, ORDER statistics, PROBABILITY theory, DENSITY
Abstract: Nonparametric estimation for a probability density function that describes multivariate data has typically been addressed by kernel density estimation (KDE). A novel density estimator recently developed by Farmer and Jacobs offers an alternative high-throughput automated approach to univariate nonparametric density estimation based on maximum entropy and order statistics, improving accuracy over univariate KDE. This article presents an extension of the single variable case to multiple variables. The univariate estimator is used to recursively calculate a product array of one-dimensional conditional probabilities. In combination with interpolation methods, a complete joint probability density estimate is generated for multiple variables. Good accuracy and speed performance in synthetic data are demonstrated by a numerical study using known distributions over a range of sample sizes from 100 to 10 6 for two to six variables. Performance in terms of speed and accuracy is compared to KDE. The multivariate density estimate developed here tends to perform better as the number of samples and/or variables increases. As an example application, measurements are analyzed over five filters of photometric data from the Sloan Digital Sky Survey Data Release 17. The multivariate estimation is used to form the basis for a binary classifier that distinguishes quasars from galaxies and stars with up to 94% accuracy. [ABSTRACT FROM AUTHOR]
Published: 2023
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23. Observational constraints on Tsallis holographic dark energy with Ricci horizon cutoff.

Author: Feizi Mangoudehi, Zahra
Subjects: DARK energy, PHASE transitions, COSMOLOGICAL constant, EQUATIONS of state, ACCELERATION (Mechanics)
Abstract: In this research, we are interested in constraining the nonlinear interacting and noninteracting Tsallis holographic dark energy (THDE) with Ricci horizon cutoff by employing three observational datasets. To this aim, the THDE with Ricci horizon considering the noninteraction and nonlinear interaction terms will be fitted by the SNe Ia, SNe Ia+H(z), and SNe Ia+H(z)+GRB samples to investigate the Hubble (H (z) ), dark-energy equation of state ( ω D E ), effective equation of state ( ω e f f ), and deceleration (q ) parameters. Investigating the H (z) parameter illustrates that our models are in good consistency with respect to observations. Also, it can reveal the turning point for both noninteracting and nonlinear interacting THDE with Ricci cutoff in the late-time era. Next, the analysis of the ω D E for our models displays that the dark energy can experience the phantom state at the current time. However, this lies in the quintessence regime in the early era and approaches the cosmological constant in the late-time epoch. Similar results will be given for the ω e f f parameter with the difference that the ω e f f will experience the quintessence region at the current redshift. In addition to the mentioned parameters, the study of the q parameter indicates that the models satisfy an acceptable transition phase from the matter- to the dark energy-dominated era. After that, the classical stability ( v s 2 ) will be analyzed for our models. The v s 2 shows that the noninteracting and nonlinear interacting THDE with Ricci cutoff will be stable in the past era but unstable in the present and progressive epochs. Then, we will employ the J e r k (J ) and O M parameters to distinguish between our models and the Λ C D M model. Finally, we will calculate the age of the Universe for the THDE and nonlinear interacting THDE with Ricci as the IR cutoff. [ABSTRACT FROM AUTHOR]
Published: 2022
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24. The Diffraction-Limited Near-Infrared Spectropolarimeter (DL-NIRSP) of the Daniel K. Inouye Solar Telescope (DKIST).

Author: Jaeggli, Sarah A., Lin, Haosheng, Onaka, Peter, Yamada, Hubert, Anan, Tetsu, Bonnet, Morgan, Ching, Gregory, Huang, Xiao-Pei, Kramar, Maxim, McGregor, Helen, Nitta, Garry, Rae, Craig, Robertson, Louis, Schad, Thomas A., Toyama, Paul, Young, Jessica, Berst, Chris, Harrington, David M., Liang, Mary, and Puentes, Myles
Subjects: SOLAR telescopes, SCIENTIFIC apparatus & instruments, SPECTRAL lines, OPTICS, SPECTROGRAPHS, WAVELENGTHS
Abstract: The Diffraction-Limited Near-Infrared Spectropolarimeter (DL-NIRSP) is one of the first-light instruments for the National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST). DL-NIRSP is an integral-field, dual-beam spectropolarimeter intended for studying magnetically sensitive spectral lines in the Sun's photosphere, chromosphere, and corona with high spectral resolution and polarimetric accuracy. Two novel fiber-optic integral-field units (IFUs), paired with selectable feed optics and a field-scanning mirror provide great flexibility in spatial sampling ( 0.03 ″ , 0.08 ″ , and 0.5 ″ ) and field coverage ( 2 ′ × 2 ′ ). The IFUs allow DL-NIRSP to record all the spectra from a 2D field of view simultaneously, enabling the instrument to study the evolution of highly dynamic events. The spectrograph is an all-reflecting, near-Littrow design, which achieves a resolving power of approximately 125,000. Multiple wavelengths can be observed simultaneously using three spectral arms: one for visible wavelengths (500 – 900 nm) and two for infrared wavelengths (900 – 1350 nm and 1350 – 1800 nm). Each supporting camera sub-system is capable of a 30-Hz frame rate, making it possible to track dynamic phenomena on the Sun. [ABSTRACT FROM AUTHOR]
Published: 2022
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25. The Role of Cross-Correlations in the Multi-Tracer Area.

Author: Blanchard, Alain
Subjects: NOISE, PHYSICAL cosmology
Abstract: Mapping the same volume of space with different tracers allows us to obtain information through estimated quantities exploiting the multi-tracer technique. Indeed, the cross-correlation of different probes provides information that cannot be otherwise obtained. In addition, some estimated quantities are not sensitive to the noise produced by the sampling variance but are only limited by the shot (or Poisson) noise, an attractive perspective. A simple example is the ratio between the (cross)-correlations, measuring the ratio of the bias parameters. Multi-tracer approaches can thereby provide additional information that cannot be extracted from independent volumes. [ABSTRACT FROM AUTHOR]
Published: 2022
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26. A Short Review on the Latest Neutrinos Mass and Number Constraints from Cosmological Observables.

Author: Sakr, Ziad
Subjects: HUBBLE constant, NUMBERS of species, NEUTRINO mass, SPECIES distribution, NEUTRINOS, PHYSICAL cosmology
Abstract: We review the neutrino science, focusing on its impact on cosmology along with the latest constraints on its mass and number of species. We also discuss its status as a possible solution to some of the recent cosmological tensions, such as the Hubble constant or the matter fluctuation parameter. We end by showing forecasts from next-generation planned or candidate surveys, highlighting their constraining power, alone or in combination, but also the limitations in determining neutrino mass distribution among its species. [ABSTRACT FROM AUTHOR]
Published: 2022
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27. How the Big Bang Ends Up Inside a Black Hole.

Author: Gaztanaga, Enrique
Subjects: BLACK holes, DARK matter, GRAVITATIONAL collapse, PHYSICAL cosmology, QUANTUM states, INFLATIONARY universe, DARK energy
Abstract: The standard model of cosmology assumes that our Universe began 14 Gyrs (billion years) ago from a singular Big Bang creation. This can explain a vast range of different astrophysical data from a handful of free cosmological parameters. However, we have no direct evidence or fundamental understanding of some key assumptions: Inflation, Dark Matter and Dark Energy. Here we review the idea that cosmic expansion originates instead from gravitational collapse and bounce. The collapse generates a Black Hole (BH) of mass M ≃ 5 × 10 22 M ⊙ that formed 25 Gyrs ago. As there is no pressure support, the cold collapse can continue inside in free fall until it reaches atomic nuclear saturation (GeV), when is halted by Quantum Mechanics, as two particles cannot occupy the same quantum state. The collapse then bounces like a core-collapse supernovae, producing the Big Bang expansion. Cosmic acceleration results from the BH event horizon. During collapse, perturbations exit the horizon to re-enter during expansion, giving rise to the observed universe without the need for Inflation or Dark Energy. Using Ockham's razor, this makes the BH Universe (BHU) model more compelling than the standard singular Big Bang creation. [ABSTRACT FROM AUTHOR]
Published: 2022
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28. Astronomical big data processing using machine learning: A comprehensive review.

Author: Sen, Snigdha, Agarwal, Sonali, Chakraborty, Pavan, and Singh, Krishna Pratap
Subjects: MACHINE learning, ELECTRONIC data processing, BIG data, ASTRONOMERS, ASTRONOMY
Abstract: Astronomy, being one of the oldest observational sciences, has collected a lot of data over the ages. In recent times, it is experiencing a huge data surge due to advancements in telescopic technologies with automated digital outputs. The main driver behind this article is to present various relevant Machine Learning (ML) algorithms and big data frameworks or tools being applied and can be employed in large astronomical data-set analysis to assist astronomers in solving multiple vital intriguing problems. Throughout this survey, we attempt to review, evaluate and summarize diverse astronomical data sources, gain knowledge of structure, the complexity of the data, and challenges in the data processing. Additionally, we discuss ample technologies being developed to handle and process this voluminous data. We also look at numerous activities being carried out all over the world enriching this domain. While going through existing literature, we perceived a limited number of comprehensive studies reported so far analyzing astronomy data-sets from the viewpoint of parallel processing and machine learning collectively. This motivated us to pursue this extensive literature review task by outlining up-to-date contributions and opportunities available in this area. Besides, this article also discusses briefly a cloud-based machine learning approach to estimate the extra-galactic object redshifts considering photometric data as input features. As the intersection of big data, machine learning and astronomy is a quite new paradigm, this article will create a strong awareness among interested young scientists for future research and provide an appropriate insight on how these algorithms and tools are becoming inevitable to the astronomy community day by day. [ABSTRACT FROM AUTHOR]
Published: 2022
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29. Confidence Limits of Evolutionary Synthesis Models.

Author: Cerviño, Miguel and Luridiana, Valentina
Abstract: The probabilistic nature of the IMF in stellar systems implies that clusters of the same mass and age do not present the same unique values of their observed parameters. Instead they follow a distribution. We address the study of such distributions in terms of their confidence limits that can be obtained by evolutionary synthesis models. These confidence limits can be understood as the inherent uncertainties of synthesis models. We will compare such confidence limits arising from the discreteness of the number of stars obtained with Monte Carlo simulations with the dispersion resulting from an analytical formalism. We give some examples of the effects on the kinetic energy, V–K, EW(Hβ) and multiwavelength continuum. [ABSTRACT FROM AUTHOR]
Published: 2002
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30. Gravitation and the Universe from large scale-structures: The GAUSS mission concept Mapping the cosmic web up to the reionization era.

Author: Blanchard, Alain, Aubourg, Éric, Brax, Philippe, Castander, Francisco J., Codis, Sandrine, Escoffier, Stéphanie, Dournac, Fabien, Ferté, Agnès, Finelli, Fabio, Fosalba, Pablo, Gangler, Emmanuel, Gontcho, Satya Gontcho A, Hawken, Adam, Ilić, Stéphane, Kneib, Jean-Paul, Kunz, Martin, Lavaux, Guilhem, Le Fèvre, Olivier, Lesgourgues, Julien, and Mellier, Yannick
Subjects: INFLATIONARY universe, CONCEPT mapping, DARK energy, PROPERTIES of matter, UNIVERSE, GRAVITATION
Abstract: Today, thanks in particular to the results of the ESA Planck mission, the concordance cosmological model appears to be the most robust to describe the evolution and content of the Universe from its early to late times. It summarizes the evolution of matter, made mainly of dark matter, from the primordial fluctuations generated by inflation around 10− 30 second after the Big Bang to galaxies and clusters of galaxies, 13.8 billion years later, and the evolution of the expansion of space, with a relative slowdown in the matter-dominated era and, since a few billion years, an acceleration powered by dark energy. But we are far from knowing the pillars of this model which are inflation, dark matter and dark energy. Comprehending these fundamental questions requires a detailed mapping of our observable Universe over the whole of cosmic time. The relic radiation provides the starting point and galaxies draw the cosmic web. JAXA's LiteBIRD mission will map the beginning of our Universe with a crucial test for inflation (its primordial gravity waves), and the ESA Euclid mission will map the most recent half part, crucial for dark energy. The mission concept GAUSS, described in this White Paper, aims at being a mission to fully map the cosmic web up to the reionization era, linking early and late evolution, to tackle and disentangle the crucial degeneracies persisting after the Euclid era between dark matter and inflation properties, dark energy, structure growth and gravitation at large scale. [ABSTRACT FROM AUTHOR]
Published: 2021
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31. Optical-Ultraviolet Tidal Disruption Events.

Author: van Velzen, Sjoert, Holoien, Thomas W.-S., Onori, Francesca, Hung, Tiara, and Arcavi, Iair
Abstract: The existence of optical-ultraviolet Tidal Disruption Events (TDEs) could be considered surprising because their electromagnetic output was originally predicted to be dominated by X-ray emission from an accretion disk. Yet over the last decade, the growth of optical transient surveys has led to the identification of a new class of optical transients occurring exclusively in galaxy centers, many of which are considered to be TDEs. Here we review the observed properties of these events, identified based on a shared set of both photometric and spectroscopic properties. We present a homogeneous analysis of 33 sources that we classify as robust TDEs, and which we divide into classes. The criteria used here to classify TDEs will possibly get updated as new samples are collected and potential additional diversity of TDEs is revealed. We also summarize current measurements of the optical-ultraviolet TDE rate, as well as the mass function and luminosity function. Many open questions exist regarding the current sample of events. We anticipate that the search for answers will unlock new insights in a variety of fields, from accretion physics to galaxy evolution. [ABSTRACT FROM AUTHOR]
Published: 2020
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32. Detection of short high-energy transients in the local universe with SVOM/ECLAIRs.

Author: Arcier, B., Atteia, J. L., Godet, O., Mate, S., Guillot, S., Dagoneau, N., Rodriguez, J., Gotz, D., Schanne, S., and Bernardini, M. G.
Abstract: The coincidental detection of the gravitational wave event GW 170817 and the gamma-ray burst GRB 170817A marked the advent of multi-messenger astronomy and represented a milestone in the study of GRBs. Significant progress in this field is expected in the coming years with the increased sensitivity of gravitational waves detectors and the launch of new facilities for the high-energy survey of the sky. In this context, the launch of SVOM in mid-2022, with its two wide-field high-energy instruments ECLAIRs and GRM, will foster the possibilities of coincidental transient detection with gravitational waves and gamma-rays events. The purpose of this paper is to assess the ability of SVOM/ECLAIRs to detect and quickly characterize high-energy transients in the local Universe (z ≤ 0.3), and to discuss the contribution of this instrument to multi-messenger astronomy and to gamma-ray burst (GRB) astrophysics in the 2020’s. A list of local HE transients, along with their main characteristics, is constructed through an extensive literature survey. This list includes 41 transients: 24 long GRBs, 10 short GRBs and 7 SGR Giant Flares. The detectability of these transients with ECLAIRs is assessed with detailed simulations using tools developed for the SVOM mission, including a GEANT4 simulation of the energy response and a simulated trigger algorithm representative of the onboard trigger algorithm. SVOM/ECLAIRs would have been able to detect 88% of the short high-energy transients in our list: 22 out of 24 long GRBs, 8 out of 10 short GRBs and 6 out of 7 SGR Giant Flares. The SNR for almost all detections will be sufficiently high to allow the on-board ECLAIRs trigger algorithm to derive the localisation of the transient, transmitting it to the SVOM satellite and ground-based instruments. Coupled with the anti-solar pointing strategy of SVOM, this will enable an optimal follow-up of the events, allowing the observation of their afterglows, supernovae/kilonovae counterparts, and host galaxies. We conclude the paper with a discussion of the unique contribution expected from SVOM and of the possibility of simultaneous GW detection for each type of transient in our sample. [ABSTRACT FROM AUTHOR]
Published: 2020
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33. Characterizing some Gaia Alerts with LAMOST and SDSS.

Author: Huo, Z., Dennefeld, M., Liu, X., Pursimo, T., and Zhang, T.
Subjects: EMISSION-line galaxies, SUPERNOVAE, GALAXY spectra, QUASARS, GALAXIES
Abstract: The ESA-Gaia satellite is regularly producing Alerts on objects where photometric variability has been detected after several passages over the same region of the sky. The physical nature of these objects has often to be determined with the help of complementary observations from ground-based facilities. We have compared the list of Gaia Alerts (from the beginning in 2014 to Nov. 1st, 2018) with archival LAMOST and SDSS spectroscopic data. A search radius of 3″ has been adopted. In using survey data, the date of the ground-based observation rarely corresponds to the date of the Alert, but this allows at least the identification of the source if it is persistent, or the host galaxy if the object was only transient like a supernova (SN). Some of the objects have several LAMOST observations, and we complemented this search by adding also SDSS DR15 data in order to look for long-term variability. A list of Gaia Nuclear Transients (GNT) from Kostrzewa-Rutkowska et al. (Mon. Not. R. Astron. Soc. 481(1):307, 2018) has been included in this search also. We found 26 Gaia Alerts with spectra in LAMOST+SDSS labelled as stars, among which 12 have multi-epoch spectra. A majority of them are Cataclysmic Variables (CVs). Similarly, 206 Gaia Alerts have associated spectra labelled as galaxies, among which 49 have multi-epoch spectra. Those spectra were generally obtained on a date widely different from the Alert date, and are mostly emission-line galaxies with no particularity (except a few Seyferts), leading to the suspicion that most of the Alerts were due to a SN. As for the GNT list, we found 55 associated spectra labelled as galaxies, among them 13 with multi-epoch spectra. In these two galaxy samples, in only two cases, Gaia17aal and GNTJ170213+2543, was the date of the spectroscopic observation close enough to the Alert date: we find a trace of the SN itself in their LAMOST spectrum, both being now classified here as a type Ia SN. Compared to the galaxy sample from the Gaia alerts, the GNT sample has a higher proportion of AGNs, suggesting that some of the detected variations are also due to the AGN itself. Similarly for Quasars, we found only 30 Gaia Alerts but 68 GNT cases associated with single epoch quasar spectra in the databases. In addition to those, 12 plus 23 are quasars where multi-epoch spectra are available. For ten out of these 35, their multi-epoch spectra show appearance or disappearance of the broad Balmer lines and also variations in the continuum, qualifying them as "Changing Look Quasars" and therefore significantly increasing the available sample of such objects. [ABSTRACT FROM AUTHOR]
Published: 2020
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34. The Host Galaxies of Tidal Disruption Events.

Author: French, K. Decker, Wevers, Thomas, Law-Smith, Jamie, Graur, Or, and Zabludoff, Ann I.
Subjects: STELLAR black holes, GALAXIES, STAR formation, STELLAR populations, BLACK holes
Abstract: Recent studies of Tidal Disruption Events (TDEs) have revealed unexpected correlations between the TDE rate and the large-scale properties of the host galaxies. In this review, we present the host galaxy properties of all TDE candidates known to date and quantify their distributions. We consider throughout the differences between observationally-identified types of TDEs and differences from spectroscopic control samples of galaxies. We focus here on the black hole and stellar masses of TDE host galaxies, their star formation histories and stellar populations, the concentration and morphology of the optical light, the presence of AGN activity, and the extra-galactic environment of the TDE hosts. We summarize the state of several possible explanations for the links between the TDE rate and host galaxy type. We present estimates of the TDE rate for different host galaxy types and quantify the degree to which rate enhancement in some types results in rate suppression in others. We discuss the possibilities for using TDE host galaxies to assist in identifying TDEs in upcoming large transient surveys and possibilities for TDE observations to be used to study their host galaxies. [ABSTRACT FROM AUTHOR]
Published: 2020
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35. Cosmological N-body simulations: a challenge for scalable generative models.

Author: Perraudin, Nathanaël, Srivastava, Ankit, Lucchi, Aurelien, Kacprzak, Tomasz, Hofmann, Thomas, and Réfrégier, Alexandre
Subjects: MACHINE learning, GENERATIVE adversarial networks, PHYSICAL cosmology
Abstract: Deep generative models, such as Generative Adversarial Networks (GANs) or Variational Autoencoders (VAs) have been demonstrated to produce images of high visual quality. However, the existing hardware on which these models are trained severely limits the size of the images that can be generated. The rapid growth of high dimensional data in many fields of science therefore poses a significant challenge for generative models. In cosmology, the large-scale, three-dimensional matter distribution, modeled with N-body simulations, plays a crucial role in understanding the evolution of structures in the universe. As these simulations are computationally very expensive, GANs have recently generated interest as a possible method to emulate these datasets, but they have been, so far, mostly limited to two dimensional data. In this work, we introduce a new benchmark for the generation of three dimensional N-body simulations, in order to stimulate new ideas in the machine learning community and move closer to the practical use of generative models in cosmology. As a first benchmark result, we propose a scalable GAN approach for training a generator of N-body three-dimensional cubes. Our technique relies on two key building blocks, (i) splitting the generation of the high-dimensional data into smaller parts, and (ii) using a multi-scale approach that efficiently captures global image features that might otherwise be lost in the splitting process. We evaluate the performance of our model for the generation of N-body samples using various statistical measures commonly used in cosmology. Our results show that the proposed model produces samples of high visual quality, although the statistical analysis reveals that capturing rare features in the data poses significant problems for the generative models. We make the data, quality evaluation routines, and the proposed GAN architecture publicly available at https://github.com/nperraud/3DcosmoGAN. [ABSTRACT FROM AUTHOR]
Published: 2019
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36. Superluminous Supernovae.

Author: Moriya, Takashi J., Sorokina, Elena I., and Chevalier, Roger A.
Abstract: Superluminous supernovae are a new class of supernovae that were recognized about a decade ago. Both observational and theoretical progress has been significant in the last decade. In this review, we first briefly summarize the observational properties of superluminous supernovae. We then introduce the three major suggested luminosity sources to explain the huge luminosities of superluminous supernovae, i.e., the nuclear decay of 56Ni, the interaction between supernova ejecta and dense circumstellar media, and the spin down of magnetars. We compare these models and discuss their strengths and weaknesses. [ABSTRACT FROM AUTHOR]
Published: 2018
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37. Astronomical Distance Determination in the Space Age.

Author: Czerny, Bożena, Beaton, Rachael, Bejger, Michał, Cackett, Edward, Dall'Ora, Massimo, Holanda, R. F. L., Jensen, Joseph B., Jha, Saurabh W., Lusso, Elisabeta, Minezaki, Takeo, Risaliti, Guido, Salaris, Maurizio, Toonen, Silvia, and Yoshii, Yuzuru
Abstract: The formal division of the distance indicators into primary and secondary leads to difficulties in description of methods which can actually be used in two ways: with, and without the support of the other methods for scaling. Thus instead of concentrating on the scaling requirement we concentrate on all methods of distance determination to extragalactic sources which are designated, at least formally, to use for individual sources. Among those, the Supernovae Ia is clearly the leader due to its enormous success in determination of the expansion rate of the Universe. However, new methods are rapidly developing, and there is also a progress in more traditional methods. We give a general overview of the methods but we mostly concentrate on the most recent developments in each field, and future expectations. [ABSTRACT FROM AUTHOR]
Published: 2018
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38. Euclid preparation - XVII. Cosmic Dawn Survey: Spitzer Space Telescope observations of the Euclid deep fields and calibration fields

Author: Euclid Collaboration, Moneti, A., McCracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Pires, S., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Chary, R., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Taylor, A. N., Cuby, J., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., ANDREON, Stefano, BARDELLI, Sandro, Faisst, A. L., Camera, S., Graciá-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, Erik, Sureau, F., Tenti, M., Vassallo, T., ZACCHEI, Andrea, Masters, D. C., ZUCCA, Elena, Baccigalupi, C., Balaguera-Antolínez, A., Bernardeau, F., BIVIANO, ANDREA, BOLZONELLA, MICOL, Bozzo, E., BURIGANA, CARLO, Cabanac, R., CAPPI, Alberto, McPartland, C., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., FARINA, Maria, FINELLI, FABIO, Flose-Reimberg, P., Mobasher, B., Fotopoulou, S., GALEOTTA, Samuele, Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Sanders, D. B., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., MORGANTE, GIANLUCA, SCARAMELLA, Roberto, Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., RICCIO, GIUSEPPE, Sánchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Stern, D., Scottez, V., SEFUSATTI, Emiliano, Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., VIEL, MATTEO, Hildebrandt, H., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., AURICCHIO, NATALIA, Bodendorf, C., BONINO, Donata, Branchini, Enzo, Brau-Nogue, S., BRESCIA, Massimo, Brinchmann, J., Capobianco, Vito, CARBONE, Carmelita, Carretero, J., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., FRAILIS, Marco, FRANCESCHI, ENRICO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillis, B., GIOCOLI, Carlo, Granett, B. R., GRAZIAN, Andrea, Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MAIORANO, Elisabetta, MANSUTTI, Oriana, Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., MENEGHETTI, MASSIMO, MERLIN, Emiliano, Meylan, G., Moresco, M., Moscardini, L., Munari, Emiliano, Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., 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), 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 National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), 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), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), 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), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, Moneti, A., Mccracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Chary, R., Cuby, J., Faisst, A. L., Masters, D. C., Mcpartland, C., Mobasher, B., Sanders, D. B., Scaramella, R., Stern, D., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., Auricchio, N., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillis, B., Giocoli, C., Granett, B. R., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., K??mmel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Cresp??, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Camera, S., Graci??-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Sureau, F., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antol??nez, A., Bernardeau, F., Biviano, A., Bolzonella, M., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., Farina, M., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., S??nchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., Viel, M., Hildebrandt, H., Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, UAM. Departamento de Física Teórica, Moneti A., Mccracken H.J., Shuntov M., Kauffmann O.B., Capak P., Davidzon I., Ilbert O., Scarlata C., Toft S., Weaver J., Chary R., Cuby J., Faisst A.L., Masters D.C., Mcpartland C., Mobasher B., Sanders D.B., Scaramella R., Stern D., Szapudi I., Teplitz H., Zalesky L., Amara A., Auricchio N., Bodendorf C., Bonino D., Branchini E., Brau-Nogue S., Brescia M., Brinchmann J., Capobianco V., Carbone C., Carretero J., Castander F.J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Douspis M., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Farrens S., Ferriol S., Fosalba P., Frailis M., Franceschi E., Fumana M., Garilli B., Gillis B., Giocoli C., Granett B.R., Grazian A., Grupp F., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kilbinger M., Kitching T., Kohley R., Kummel M., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Marulli F., Massey R., Maurogordato S., Meneghetti M., Merlin E., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Rix H., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Andreon S., Bardelli S., Camera S., Gracia-Carpio J., Medinaceli E., Mei S., Polenta G., Romelli E., Sureau F., Tenti M., Vassallo T., Zacchei A., Zucca E., Baccigalupi C., Balaguera-Antolinez A., Bernardeau F., Biviano A., Bolzonella M., Bozzo E., Burigana C., Cabanac R., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Di Ferdinando D., Farina M., Finelli F., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Garcia-Bellido J., Gaztanaga E., Gozaliasl G., Hook I., Joachimi B., Kansal V., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Maoli R., Martinelli M., Martinet N., Maturi M., Metcalf R.B., Morgante G., Morisset N., Nucita A., Patrizii L., Potter D., Renzi A., Riccio G., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Sefusatti E., Teyssier R., Tubio O., Tutusaus I., Valiviita J., Viel M., Hildebrandt H., Kummel, M., Tallada-Crespi, P., Gracia-Carpio, J., Balaguera-Antolinez, A., and Sanchez, A. G.
Subjects: SAMPLE, Large-scale structure of Universe, DATA RELEASE, Formation, Surveys, observations, Dark energy, Dark matter, Galaxy: formation, Large-scale structure of Universe, Surveys [Cosmology], kosmologia, Astrophysics, Cosmology: observation, dark matter, galaksijoukot, pimeä aine, surveys, Dark energy, Dark matter, observations [Cosmology], dark energy, Observations, LEGACY SURVEY, Astrophysics of Galaxies, Física, Astronomy and Astrophysics, 115 Astronomy, Space science, EVOLUTION, Cosmology, galaksit, GALAXIES, Cosmology: observations, Galaxy: formation, Galaxy, formation [Galaxy], Space and Planetary Science, cosmology: observations, large-scale structure of Universe, pimeä energia, Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Artículo escrito por un elevado núnmero de autores, sólo se referencian el qque aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere, We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer Space Telescope's Infrared Array Camera (IRAC). We combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11 % of the total Spitzer Space Telescope mission time. The resulting mosaics cover a total of approximately 71.5 deg2 in the 3.6 and 4.5 μm bands, and approximately 21.8 deg2 in the 5.8 and 8 μm bands. They reach at least 24 AB magnitude (measured to 5σ, in a 2″.5 aperture) in the 3.6 μm band and up to ∼5 mag deeper in the deepest regions. The astrometry is tied to the Gaia astrometric reference system, and the typical astrometric uncertainty for sources with 16 "< "[3.6]< 19 is ≲ 0″.15. The photometric calibration is in excellent agreement with previous WISE measurements. We extracted source number counts from the 3.6 μm band mosaics, and they are in excellent agreement with previous measurements. Given that the Spitzer Space Telescope has now been decommissioned, these mosaics are likely to be the definitive reduction of these IRAC data. This survey therefore represents an essential first step in assembling multi-wavelength data on the Euclid deep fields, which are set to become some of the premier fields for extragalactic astronomy in the 2020s
Published: 2022
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39. Euclid preparation. XVI. Exploring the ultra-low surface brightness Universe with Euclid/VIS

Author: Euclid Collaboration, Borlaff, A. S., Gómez-Alvarez, P., Altieri, B., Marcum, P. M., Vavrek, R., Laureijs, R., Kohley, R., Buitrago, F., Cuillandre, J. -C., Duc, P. -A., Gaspar Venancio, L. M., Amara, A., Andreon, S., Auricchio, N., Azzollini, R., Baccigalupi, C., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Bozzo, E., Branchini, E., Brescia, M., Brinchmann, J., Burigana, C., Cabanac, R., Camera, S., Candini, G. P., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, S., Castander, F. J., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Coupon, J., Courtois, H. M., Cropper, M., Da Silva, A., Degaudenzi, H., Di Ferdinando, D., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Fabricius, M., Farina, M., Farrens, S., Ferreira, P. G., Ferriol, S., Finelli, F., Flose-Reimberg, P., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., Ganga, K., Garilli, B., Gillis, B., Giocoli, C., Gozaliasl, G., Graciá-Carpio, J., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kilbinger, M., Kirkpatrick, C. C., Kitching, T., Knapen, J. H., Kubik, B., Kümmel, M., Kunz, M., Kurki-Suonio, H., Liebing, P., Ligori, S., Lilje, P. B., Lindholm, V., Lloro, I., Mainetti, G., Maino, D., Mansutti, O., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Martínez-Delgado, D., Marulli, F., Massey, R., Maturi, M., Maurogordato, S., Medinaceli, E., Mei, S., Meneghetti, M., Merlin, E., Metcalf, R. B., Meylan, G., Moresco, M., Morgante, G., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Niemi, S. M., Nightingale, J. W., Nucita, A., Padilla, C., Paltani, S., Pasian, F., Patrizii, L., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rosset, C., Rossetti, E., Saglia, R., Sánchez, A. G., Sapone, D., Sauvage, M., Schneider, P., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Skottfelt, J., Stanco, L., Starck, J. L., Sureau, F., Tallada-Crespí, P., Taylor, A. N., Tenti, M., Tereno, I., Teyssier, R., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Weller, J., Whittaker, L., Zacchei, A., Zamorani, G., Zucca, E., Euclid, Collaboration, Borlaff, A. S., Gómez-Alvarez, P., Altieri, B., Marcum, P. M., Vavrek, R., Laureijs, R., Kohley, R., Buitrago, F., Cuillandre, J. -C., Duc, P. -A., Gaspar Venancio, L. M., Amara, A., Andreon, S., Auricchio, N., Azzollini, R., Baccigalupi, C., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Bozzo, E., Branchini, E., Brescia, M., Brinchmann, J., Burigana, C., Cabanac, R., Camera, S., Candini, G. P., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, S., Castander, F. J., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Coupon, J., Courtois, H. M., Cropper, M., Da Silva, A., Degaudenzi, H., Di Ferdinando, D., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Fabricius, M., Farina, M., Farrens, S., Ferreira, P. G., Ferriol, S., Finelli, F., Flose-Reimberg, P., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., Ganga, K., Garilli, B., Gillis, B., Giocoli, C., Gozaliasl, G., Graciá-Carpio, J., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kilbinger, M., Kirkpatrick, C. C., Kitching, T., Knapen, J. H., Kubik, B., Kümmel, M., Kunz, M., Kurki-Suonio, H., Liebing, P., Ligori, S., Lilje, P. B., Lindholm, V., Lloro, I., Mainetti, G., Maino, D., Mansutti, O., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Martínez-Delgado, D., Marulli, F., Massey, R., Maturi, M., Maurogordato, S., Medinaceli, E., Mei, S., Meneghetti, M., Merlin, E., Metcalf, R. B., Meylan, G., Moresco, M., Morgante, G., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Niemi, S. M., Nightingale, J. W., Nucita, A., Padilla, C., Paltani, S., Pasian, F., Patrizii, L., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rosset, C., Rossetti, E., Saglia, R., Sánchez, A. G., Sapone, D., Sauvage, M., Schneider, P., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Skottfelt, J., Stanco, L., Starck, J. L., Sureau, F., Tallada-Crespí, P., Taylor, A. N., Tenti, M., Tereno, I., Teyssier, R., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Weller, J., Whittaker, L., Zacchei, A., Zamorani, G., Zucca, E., European Commission, Ministerio de Ciencia e Innovación (España), Borlaff A.S., Gomez-Alvarez P., Altieri B., Marcum P.M., Vavrek R., Laureijs R., Kohley R., Buitrago F., Cuillandre J.-C., Duc P.-A., Gaspar Venancio L.M., Amara A., Andreon S., Auricchio N., Azzollini R., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Bozzo E., Branchini E., Brescia M., Brinchmann J., Burigana C., Cabanac R., Camera S., Candini G.P., Capobianco V., Cappi A., Carbone C., Carretero J., Carvalho C.S., Casas S., Castander F.J., Castellano M., Castignani G., Cavuoti S., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Coupon J., Courtois H.M., Cropper M., Da Silva A., Degaudenzi H., Di Ferdinando D., Douspis M., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Ealet A., Fabricius M., Farina M., Farrens S., Ferreira P.G., Ferriol S., Finelli F., Flose-Reimberg P., Fosalba P., Frailis M., Franceschi E., Fumana M., Galeotta S., Ganga K., Garilli B., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grazian A., Grupp F., Haugan S.V.H., Holmes W., Hormuth F., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kilbinger M., Kirkpatrick C.C., Kitching T., Knapen J.H., Kubik B., Kummel M., Kunz M., Kurki-Suonio H., Liebing P., Ligori S., Lilje P.B., Lindholm V., Lloro I., Mainetti G., Maino D., Mansutti O., Marggraf O., Markovic K., Martinelli M., Martinet N., Martinez-Delgado D., Marulli F., Massey R., Maturi M., Maurogordato S., Medinaceli E., Mei S., Meneghetti M., Merlin E., Metcalf R.B., Meylan G., Moresco M., Morgante G., Moscardini L., Munari E., Nakajima R., Neissner C., Niemi S.M., Nightingale J.W., Nucita A., Padilla C., Paltani S., Pasian F., Patrizii L., Pedersen K., Percival W.J., Pettorino V., Pires S., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Rebolo R., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Rosset C., Rossetti E., Saglia R., Sanchez A.G., Sapone D., Sauvage M., Schneider P., Scottez V., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Skottfelt J., Stanco L., Starck J.L., Sureau F., Tallada-Crespi P., Taylor A.N., Tenti M., Tereno I., Teyssier R., Toledo-Moreo R., Torradeflot F., Tutusaus I., Valentijn E.A., Valenziano L., Valiviita J., Vassallo T., Viel M., Wang Y., Weller J., Whittaker L., Zacchei A., Zamorani G., Zucca E., Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gomez-Alvarez, P., Balaguera-Antolinez, A., Gracia-Carpio, J., Kummel, M., Martinez-Delgado, D., Sanchez, A. G., Tallada-Crespi, P., Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-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), Astronomy, 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), 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), 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), 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), 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), 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), 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), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Research Program in Systems Oncology, and Helsinki Institute of Physics
Subjects: diffuse light, stellar haloes, FOS: Physical sciences, Galaxies: general, Instrumentation: detectors, Methods: observational, Space vehicles: instruments, Techniques: image processing, Techniques: photometric, virgo cluster, techniques: image processing, Astrophysics::Cosmology and Extragalactic Astrophysics, Space vehicles: instrument, 01 natural sciences, 7. Clean energy, instruments [Space vehicles], techniques: photometric, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, spiral galaxies, image processing [Techniques], observational [Methods], space vehicles: instruments, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, detectors [Instrumentation], Astrophysics::Galaxy Astrophysics, data release, Instrumentation: detector, substructure, 010308 nuclear & particles physics, instrumentation: detectors, photometric [Techniques], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, general [Galaxies], 115 Astronomy, Space science, calibration, Astrophysics - Astrophysics of Galaxies, galaxies: general, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), deep, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, tidal features, tracing galaxy formation
Abstract: Full list of authors: Borlaff, A. S.; Gómez-Alvarez, P.; Altieri, B.; Marcum, P. M.; Vavrek, R.; Laureijs, R.; Kohley, R.; Buitrago, F.; Cuillandre, J. -C.; Duc, P. -A.; Gaspar Venancio, L. M.; Amara, A.; Andreon, S.; Auricchio, N.; Azzollini, R.; Baccigalupi, C.; Balaguera-Antolínez, A.; Baldi, M.; Bardelli, S.; Bender, R.; Biviano, A.; Bodendorf, C.; Bonino, D.; Bozzo, E.; Branchini, E.; Brescia, M.; Brinchmann, J.; Burigana, C.; Cabanac, R.; Camera, S.; Candini, G. P.; Capobianco, V.; Cappi, A.; Carbone, C.; Carretero, J.; Carvalho, C. S.; Casas, S.; Castander, F. J.; Castellano, M.; Castignani, G.; Cavuoti, S.; Cimatti, A.; Cledassou, R.; Colodro-Conde, C.; Congedo, G.; Conselice, C. J.; Conversi, L.; Copin, Y.; Corcione, L.; Coupon, J.; Courtois, H. M.; Cropper, M.; Da Silva, A.; Degaudenzi, H.; Di Ferdinando, D.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Dusini, S.; Ealet, A.; Fabricius, M.; Farina, M. ; Farrens, S.; Ferreira, P. G.; Ferriol, S.; Finelli, F.; Flose-Reimberg, P.; Fosalba, P.; Frailis, M.; Franceschi, E.; Fumana, M.; Galeotta, S.; Ganga, K.; Garilli, B.; Gillis, B.; Giocoli, C.; Gozaliasl, G.; Graciá-Carpio, J.; Grazian, A.; Grupp, F.; Haugan, S. V. H.; Holmes, W.; Hormuth, F.; Jahnke, K.; Keihanen, E.; Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kirkpatrick, C. C.; Kitching, T.; Knapen, J. H.; Kubik, B.; Kümmel, M.; Kunz, M.; Kurki-Suonio, H.; Liebing, P.; Ligori, S.; Lilje, P. B.; Lindholm, V.; Lloro, I.; Mainetti, G.; Maino, D.; Mansutti, O.; Marggraf, O.; Markovic, K.; Martinelli, M.; Martinet, N.; Martínez-Delgado, D.; Marulli, F.; Massey, R.; Maturi, M.; Maurogordato, S.; Medinaceli, E.; Mei, S.; Meneghetti, M.; Merlin, E.; Metcalf, R. B.; Meylan, G.; Moresco, M.; Morgante, G.; Moscardini, L.; Munari, E.; Nakajima, R.; Neissner, C.; Niemi, S. M.; Nightingale, J. W.; Nucita, A.; Padilla, C.; Paltani, S.; Pasian, F.; Patrizii, L.; Pedersen, K.; Percival, W. J.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L.; Potter, D.; Pozzetti, L.; Raison, F.; Rebolo, R.; Renzi, A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Rosset, C.; Rossetti, E.; Saglia, R.; Sánchez, A. G.; Sapone, D.; Sauvage, M.; Schneider, P.; Scottez, V.; Secroun, A.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Skottfelt, J.; Stanco, L.; Starck, J. L.; Sureau, F.; Tallada-Crespí, P.; Taylor, A. N.; Tenti, M.; Tereno, I.; Teyssier, R.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valentijn, E. A.; Valenziano, L.; Valiviita, J.; Vassallo, T.; Viel, M.; Wang, Y.; Weller, J.; Whittaker, L.; Zacchei, A.; Zamorani, G.; Zucca, E.; Euclid Collaboration., Context. While Euclid is an ESA mission specifically designed to investigate the nature of dark energy and dark matter, the planned unprecedented combination of survey area (∼15 000 deg2), spatial resolution, low sky-background, and depth also make Euclid an excellent space observatory for the study of the low surface brightness Universe. Scientific exploitation of the extended low surface brightness structures requires dedicated calibration procedures that are yet to be tested. Aims. We investigate the capabilities of Euclid to detect extended low surface brightness structure by identifying and quantifying sky-background sources and stray-light contamination. We test the feasibility of generating sky flat-fields to reduce large-scale residual gradients in order to reveal the extended emission of galaxies observed in the Euclid survey. Methods. We simulated a realistic set of Euclid/VIS observations, taking into account both instrumental and astronomical sources of contamination, including cosmic rays, stray-light, zodiacal light, interstellar medium, and the cosmic infrared background, while simulating the effects of background sources in the field of view. Results. We demonstrate that a combination of calibration lamps, sky flats, and self-calibration would enable recovery of emission at a limiting surface brightness magnitude of μlim = 29.5−0.27+0.08 mag arcsec−2 (3σ, 10 × 10 arcsec2) in the Wide Survey, and it would reach regions deeper by 2 mag in the Deep Surveys. Conclusions.Euclid/VIS has the potential to be an excellent low surface brightness observatory. Covering the gap between pixel-to-pixel calibration lamp flats and self-calibration observations for large scales, the application of sky flat-fielding will enhance the sensitivity of the VIS detector at scales larger than 1″, up to the size of the field of view, enabling Euclid to detect extended surface brightness structures below μlim = 31 mag arcsec−2 and beyond. © ESO 2022., A. B. was supported by an appointment to the NASA Postdoctoral Program at the NASA Ames Research Center, administered by Universities Space Research Association under contract with NASA, and the European Space Agency (ESA), through the European Space Astronomy Center Faculty. We acknowledge a number of agencies and institutes that have supported the development of Euclid, in particular the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the Centre National d’Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Romanian Space Agency, the State Secretariat for Education, Research and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid website (http://www.euclid-ec.org). This work has made use of data from the ESA mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research made use of NumPy (Van Der Walt et al. 2011), Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration 2013). All of the figures on this publication were generated using Matplotlib (Hunter 2007). This work was partly done using GNU Astronomy Utilities (Gnuastro, ascl.net/1801.009) version 0.11.22-dc86., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
Published: 2022
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40. Euclid preparation: XIII. Forecasts for galaxy morphology with the Euclid Survey using Deep Generative Models

Author: Euclid Collaboration, Bretonnière, H., Huertas-Company, M., Boucaud, A., Lanusse, F., Jullo, E., MERLIN, Emiliano, Tuccillo, D., CASTELLANO, MARCO, Brinchmann, J., Conselice, C. J., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Dole, H., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Cabanac, R., Torradeflot, F., Valentijn, E. A., VALENZIANO, LUCA, Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Baldi, M., BARDELLI, Sandro, Courtois, H. M., Camera, S., FARINELLI, Ruben, Medinaceli, E., Mei, S., Polenta, G., Romelli, Erik, Tenti, M., Vassallo, T., ZACCHEI, Andrea, ZUCCA, Elena, Castander, F. J., Baccigalupi, C., Balaguera-Antolínez, A., BIVIANO, ANDREA, BORGANI, STEFANO, Bozzo, E., BURIGANA, CARLO, CAPPI, Alberto, Carvalho, C. S., Casas, S., Castignani, G., Duc, P. A., Colodro-Conde, C., Coupon, J., de la Torre, S., Fabricius, M., FARINA, Maria, Ferreira, P. G., Flose-Reimberg, P., Fotopoulou, S., GALEOTTA, Samuele, Ganga, K., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I. M., Joachimi, B., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Guinet, D., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., McCracken, H. J., Metcalf, R. B., MORGANTE, GIANLUCA, Morisset, N., Nightingale, J., Kruk, S., Nucita, A., Patrizii, L., Potter, D., Renzi, A., RICCIO, GIUSEPPE, Sánchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Kuchner, U., SEFUSATTI, Emiliano, Teyssier, R., Tutusaus, I., Valiviita, J., VIEL, MATTEO, Whittaker, L., Knapen, J. H., Serrano, S., Soubrie, E., Tramacere, A., Wang, L., Amara, A., AURICCHIO, NATALIA, Bender, R., Bodendorf, C., BONINO, Donata, Branchini, Enzo, Brau-Nogue, S., BRESCIA, Massimo, Capobianco, Vito, CARBONE, Carmelita, Carretero, J., CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., FRAILIS, Marco, FRANCESCHI, ENRICO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillard, W., Gillis, B., GIOCOLI, Carlo, GRAZIAN, Andrea, Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MAIORANO, Elisabetta, MANSUTTI, Oriana, Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Melchior, M., MENEGHETTI, MASSIMO, Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, Emiliano, Nakajima, R., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Cosmologie et Statistiques (LCS - COSMOSTAT), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Lanusse, Francois, UAM. Departamento de Física Teórica, Bretonniere, H., Huertas-Company, M., Boucaud, A., Lanusse, F., Jullo, E., Merlin, E., Tuccillo, D., Castellano, M., Brinchmann, J., Conselice, C. J., Dole, H., Cabanac, R., Courtois, H. M., Castander, F. J., Duc, P. A., Fosalba, P., Guinet, D., Kruk, S., Kuchner, U., Serrano, S., Soubrie, E., Tramacere, A., Wang, L., Amara, A., Auricchio, N., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Capobianco, V., Carbone, C., Carretero, J., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kummel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Melchior, M., Meneghetti, M., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Tallada-Crespi, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Valenziano, L., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Baldi, M., Bardelli, S., Camera, S., Farinelli, R., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antolinez, A., Biviano, A., Borgani, S., Bozzo, E., Burigana, C., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., De La Torre, S., Fabricius, M., Farina, M., Ferreira, P. G., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I. M., Joachimi, B., Kansal, V., Kashlinsky, A., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Mccracken, H. J., Metcalf, R. B., Morgante, G., Morisset, N., Nightingale, J., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., Sanchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tutusaus, I., Valiviita, J., Viel, M., Whittaker, L., Knapen, J. H., Bretonniere H., Huertas-Company M., Boucaud A., Lanusse F., Jullo E., Merlin E., Tuccillo D., Castellano M., Brinchmann J., Conselice C.J., Dole H., Cabanac R., Courtois H.M., Castander F.J., Duc P.A., Fosalba P., Guinet D., Kruk S., Kuchner U., Serrano S., Soubrie E., Tramacere A., Wang L., Amara A., Auricchio N., Bender R., Bodendorf C., Bonino D., Branchini E., Brau-Nogue S., Brescia M., Capobianco V., Carbone C., Carretero J., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Douspis M., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Farrens S., Ferriol S., Frailis M., Franceschi E., Fumana M., Garilli B., Gillard W., Gillis B., Giocoli C., Grazian A., Grupp F., Haugan S.V.H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kilbinger M., Kitching T., Kohley R., Kummel M., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Marulli F., Massey R., Maurogordato S., Melchior M., Meneghetti M., Meylan G., Moresco M., Morin B., Moscardini L., Munari E., Nakajima R., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Pettorino V., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Seidel G., Sirignano C., Sirri G., Stanco L., Starck J.-L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Valentijn E.A., Valenziano L., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Baldi M., Bardelli S., Camera S., Farinelli R., Medinaceli E., Mei S., Polenta G., Romelli E., Tenti M., Vassallo T., Zacchei A., Zucca E., Baccigalupi C., Balaguera-Antolinez A., Biviano A., Borgani S., Bozzo E., Burigana C., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., De La Torre S., Fabricius M., Farina M., Ferreira P.G., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Garcia-Bellido J., Gaztanaga E., Gozaliasl G., Hook I.M., Joachimi B., Kansal V., Kashlinsky A., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Maoli R., Martinelli M., Martinet N., McCracken H.J., Metcalf R.B., Morgante G., Morisset N., Nightingale J., Nucita A., Patrizii L., Potter D., Renzi A., Riccio G., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Sefusatti E., Teyssier R., Tutusaus I., Valiviita J., Viel M., Whittaker L., Knapen J.H., Astronomy, Bretonniere, H, Huertas-Company, M, Boucaud, A, Lanusse, F, Jullo, E, Merlin, E, Tuccillo, D, Castellano, M, Brinchmann, J, Conselice, Cj, Dole, H, Cabanac, R, Courtois, Hm, Castander, Fj, Duc, Pa, Fosalba, P, Guinet, D, Kruk, S, Kuchner, U, Serrano, S, Soubrie, E, Tramacere, A, Wang, L, Amara, A, Auricchio, N, Bender, R, Bodendorf, C, Bonino, D, Branchini, E, Brau-Nogue, S, Brescia, M, Capobianco, V, Carbone, C, Carretero, J, Cavuoti, S, Cimatti, A, Cledassou, R, Congedo, G, Conversi, L, Copin, Y, Corcione, L, Costille, A, Cropper, M, Da Silva, A, Degaudenzi, H, Douspis, M, Dubath, F, Duncan, Caj, Dupac, X, Dusini, S, Farrens, S, Ferriol, S, Frailis, M, Franceschi, E, Fumana, M, Garilli, B, Gillard, W, Gillis, B, Giocoli, C, Grazian, A, Grupp, F, Haugan, Svh, Holmes, W, Hormuth, F, Hudelot, P, Jahnke, K, Kermiche, S, Kiessling, A, Kilbinger, M, Kitching, T, Kohley, R, Kummel, M, Kunz, M, Kurki-Suonio, H, Ligori, S, Lilje, Pb, Lloro, I, Maiorano, E, Mansutti, O, Marggraf, O, Markovic, K, Marulli, F, Massey, R, Maurogordato, S, Melchior, M, Meneghetti, M, Meylan, G, Moresco, M, Morin, B, Moscardini, L, Munari, E, Nakajima, R, Niemi, Sm, Padilla, C, Paltani, S, Pasian, F, Pedersen, K, Pettorino, V, Pires, S, Poncet, M, Popa, L, Pozzetti, L, Raison, F, Rebolo, R, Rhodes, J, Roncarelli, M, Rossetti, E, Saglia, R, Schneider, P, Secroun, A, Seidel, G, Sirignano, C, Sirri, G, Stanco, L, Starck, Jl, Tallada-Crespi, P, Taylor, An, Tereno, I, Toledo-Moreo, R, Torradeflot, F, Valentijn, Ea, Valenziano, L, Wang, Y, Welikala, N, Weller, J, Zamorani, G, Zoubian, J, Baldi, M, Bardelli, S, Camera, S, Farinelli, R, Medinaceli, E, Mei, S, Polenta, G, Romelli, E, Tenti, M, Vassallo, T, Zacchei, A, Zucca, E, Baccigalupi, C, Balaguera-Antolinez, A, Biviano, A, Borgani, S, Bozzo, E, Burigana, C, Cappi, A, Carvalho, C, Casas, S, Castignani, G, Colodro-Conde, C, Coupon, J, de la Torre, S, Fabricius, M, Farina, M, Ferreira, Pg, Flose-Reimberg, P, Fotopoulou, S, Galeotta, S, Ganga, K, Garcia-Bellido, J, Gaztanaga, E, Gozaliasl, G, Hook, Im, Joachimi, B, Kansal, V, Kashlinsky, A, Keihanen, E, Kirkpatrick, Cc, Lindholm, V, Mainetti, G, Maino, D, Maoli, R, Martinelli, M, Martinet, N, Mccracken, Hj, Metcalf, Rb, Morgante, G, Morisset, N, Nightingale, J, Nucita, A, Patrizii, L, Potter, D, Renzi, A, Riccio, G, Sanchez, Ag, Sapone, D, Schirmer, M, Schultheis, M, Scottez, V, Sefusatti, E, Teyssier, R, Tutusaus, I, Valiviita, J, Viel, M, Whittaker, L, Knapen, Jh, Department of Physics, Research Program in Systems Oncology, and Helsinki Institute of Physics
Subjects: INFORMATION, structure [Galaxies], FOS: Physical sciences, Techniques: image processing, Morphology (biology), observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Cosmology: observation, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, DEPENDENCE, Galaxies: structure, galaxies, evolution, 0103 physical sciences, image processing [Techniques], structure, Survey, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, COSMOS, Physics, 010308 nuclear & particles physics, galaxie, Cosmology: observations, [PHYS.ASTR.GA] Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galaxies: evolution, Física, Astronomy and Astrophysics, technique, 115 Astronomy, Space science, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, techniques, image processing, surveys, cosmology, observations, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), SIMULATION, Generative grammar
Abstract: Artículo escrito por un elevado número de autores, sólo se referencian el que aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere., We present a machine learning framework to simulate realistic galaxies for the Euclid Survey, producing more complex and realistic galaxies than the analytical simulations currently used in Euclid. The proposed method combines a control on galaxy shape parameters offered by analytic models with realistic surface brightness distributions learned from real Hubble Space Telescope observations by deep generative models. We simulate a galaxy field of 0.4 deg2 as it will be seen by the Euclid visible imager VIS, and we show that galaxy structural parameters are recovered to an accuracy similar to that for pure analytic Sérsic profiles. Based on these simulations, we estimate that the Euclid Wide Survey (EWS) will be able to resolve the internal morphological structure of galaxies down to a surface brightness of 22.5 mag arcsec-2, and the Euclid Deep Survey (EDS) down to 24.9 mag arcsec-2. This corresponds to approximately 250 million galaxies at the end of the mission and a 50% complete sample for stellar masses above 1010.6 M (resp. 109.6 M) at a redshift z ∼ 0.5 for the EWS (resp. EDS). The approach presented in this work can contribute to improving the preparation of future high-precision cosmological imaging surveys by allowing simulations to incorporate more realistic galaxies
Published: 2021

41. Euclid preparation. XII. Optimizing the photometric sample of the Euclid survey for galaxy clustering and galaxy-galaxy lensing analyses

Author: Martin Crocce, Chiara Sirignano, O. Mansutti, L. Whittaker, Massimo Meneghetti, I. Ferrero, Alina Kiessling, Edwin A. Valentijn, Gianluca Castignani, S. Maurogordato, Giuseppe Riccio, P. B. Lilje, Carlo Burigana, Rafael Toledo-Moreo, B. Gillis, Davide Maino, Felix Hormuth, G. Sirri, F. Sureau, W. A. Holmes, Marco Baldi, Richard Massey, Knud Jahnke, K. Pedersen, A. Da Silva, Enrico Bozzo, E. Romelli, Simona Mei, C. Bodendorf, Jussi Valiviita, L. Popa, R. Cledassou, Luigi Guzzo, Andrea Cimatti, A. Pocino, F. Raison, Hélène M. Courtois, M. Tenti, Jarle Brinchmann, Robert C. Nichol, M. Poncet, Massimo Brescia, D. Di Ferdinando, Ghassem Gozaliasl, G. Meylan, D. Bonino, C. Neissner, C. S. Carvalho, Anne Costille, C. A. J. Duncan, M. Viel, A. Balaguera-Antolínez, Valeria Pettorino, Leonardo Corcione, S. Serrano, X. Dupac, Jean Coupon, C. Baccigalupi, R. Benton Metcalf, S. Farrens, Lauro Moscardini, V. Scottez, Yu Wang, Marco Castellano, G. Zamorani, Roberto P. Saglia, Andrea Biviano, Martin Kunz, F. Grupp, S. Casas, S. M. Niemi, J. Nightingale, Enzo Branchini, A. Secroun, N. Martinet, Mark Cropper, G. Seidel, Ismael Tereno, L. Stanco, L. Conversi, E. Medinaceli, Doug Potter, Stefano Cavuoti, Lucia Pozzetti, A. Cappi, F. J. Castander, C. C. Kirkpatrick, G. Congedo, R. Nakajima, Emanuel Rossetti, B. Morin, Fabio Finelli, F. Lacasa, Y. Copin, C. Padilla, Andrea Tramacere, W. Gillard, M. Martinelli, E. Keihänen, S. Kermiche, Mauro Roncarelli, Domenico Sapone, B. Garilli, I. Lloro, E. Munari, Sotiria Fotopoulou, Ariel G. Sánchez, Julien Zoubian, T. Vassallo, Romain Teyssier, Stefano Camera, Ole Marggraf, S. de la Torre, Z. Sakr, V. Capobianco, L. Patrizii, Carlo Giocoli, Stefano Andreon, S. Dusini, M. Frailis, A. Balestra, Ralf Bender, Pedro G. Ferreira, A. Boucaud, Jason Rhodes, Luca Valenziano, E. Zucca, F. Dubath, S. Bardelli, G. Polenta, Pablo Fosalba, Peter Schneider, Elisabetta Maiorano, Fabio Pasian, Hannu Kurki-Suonio, Jean-Gabriel Cuby, N. Welikala, Natalia Auricchio, Thomas D. Kitching, A. Porredon, V. F. Cardone, C. Colodro-Conde, Michele Moresco, Andy Taylor, Will J. Percival, Alkistis Pourtsidou, Christopher J. Conselice, S. Paltani, E. Franceschi, Sebastiano Ligori, Roberto Scaramella, Javier Graciá-Carpio, A. Renzi, Remi A. Cabanac, S. Galeotta, S. Pires, Federico Marulli, Andrea Zacchei, I. Tutusaus, Astronomy, Pocino, A., Tutusaus, I., Castander, F. J., Fosalba, P., Crocce, M., Porredon, A., Camera, S., Cardone, V., Casas, S., Kitching, T., Lacasa, F., Martinelli, M., Pourtsidou, A., Sakr, Z., Andreon, S., Auricchio, N., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Balestra, A., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Boucaud, A., Bozzo, E., Branchini, E., Brescia, M., Brinchmann, J., Burigana, C., Cabanac, R., Capobianco, V., Cappi, A., Carvalho, C. S., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Coupon, J., Courtois, H. M., Cropper, M., Cuby, J. -G., Da Silva, A., De La Torre, S., Di Ferdinando, D., Dubath, F., Duncan, C., Dupac, X., Dusini, S., Farrens, S., Ferreira, P. G., Ferrero, I., Finelli, F., Fotopoulou, S., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gozaliasl, G., Gracia-Carpio, J., Grupp, F., Guzzo, L., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kirkpatrick, C. C., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Mansutti, O., Marggraf, O., Martinet, N., Marulli, F., Massey, R., Maurogordato, S., Medinaceli, E., Mei, S., Meneghetti, M., Benton Metcalf, R., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Nichol, R. C., Niemi, S., Nightingale, J., Padilla, C., Paltani, S., Pasian, F., Patrizii, L., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sanchez, A. G., Sapone, D., Scaramella, R., Schneider, P., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Sureau, F., Taylor, A. N., Tenti, M., Tereno, I., Teyssier, R., Toledo-Moreo, R., Tramacere, A., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Welikala, N., Whittaker, L., Zacchei, A., Zamorani, G., Zoubian, J., Zucca, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-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 de Paris (UP), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), 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), Euclid, 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), 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, Pocino A., Tutusaus I., Castander F.J., Fosalba P., Crocce M., Porredon A., Camera S., Cardone V., Casas S., Kitching T., Lacasa F., Martinelli M., Pourtsidou A., Sakr Z., Andreon S., Auricchio N., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Balestra A., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Boucaud A., Bozzo E., Branchini E., Brescia M., Brinchmann J., Burigana C., Cabanac R., Capobianco V., Cappi A., Carvalho C.S., Castellano M., Castignani G., Cavuoti S., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Coupon J., Courtois H.M., Cropper M., Cuby J.-G., Da Silva A., De La Torre S., Di Ferdinando D., Dubath F., Duncan C., Dupac X., Dusini S., Farrens S., Ferreira P.G., Ferrero I., Finelli F., Fotopoulou S., Frailis M., Franceschi E., Galeotta S., Garilli B., Gillard W., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grupp F., Guzzo L., Holmes W., Hormuth F., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kirkpatrick C.C., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Mansutti O., Marggraf O., Martinet N., Marulli F., Massey R., Maurogordato S., Medinaceli E., Mei S., Meneghetti M., Benton Metcalf R., Meylan G., Moresco M., Morin B., Moscardini L., Munari E., Nakajima R., Neissner C., Nichol R.C., Niemi S., Nightingale J., Padilla C., Paltani S., Pasian F., Patrizii L., Pedersen K., Percival W.J., Pettorino V., Pires S., Polenta G., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Rossetti E., Saglia R., Sanchez A.G., Sapone D., Scaramella R., Schneider P., Scottez V., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Sureau F., Taylor A.N., Tenti M., Tereno I., Teyssier R., Toledo-Moreo R., Tramacere A., Valentijn E.A., Valenziano L., Valiviita J., Vassallo T., Viel M., Wang Y., Welikala N., Whittaker L., Zacchei A., Zamorani G., Zoubian J., and Zucca E.
Subjects: luminous red galaxies, Cosmological parameter, Astrophysics, Surveys, 01 natural sciences, Cosmology, techniques: photometric, galaxies, Galaxies: distances and redshift, distances and redshifts, Survey, 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, Redshift survey, lsst, astro-ph.CO, galaxies: distances and redshifts, constraints, Astrophysics - Cosmology and Nongalactic Astrophysics, redshift survey, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, photometric, Settore FIS/05 - Astronomia e Astrofisica, surveys, 0103 physical sciences, distances and redshifts [Galaxies], cosmological parameters, Spurious relationship, Cluster analysis, dark energy survey, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, photometric [Techniques], Astronomy and Astrophysics, space, 115 Astronomy, Space science, Redshift, Galaxy, Space and Planetary Science, Galaxies: distances and redshifts, Techniques: photometric, techniques, Focus (optics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, cosmic shear, intrinsic alignments
Abstract: Pocino, A., et al. (Euclid Collaboration), Photometric redshifts (photo-zs) are one of the main ingredients in the analysis of cosmological probes. Their accuracy particularly affects the results of the analyses of galaxy clustering with photometrically selected galaxies (GCph) and weak lensing. In the next decade, space missions such as Euclid will collect precise and accurate photometric measurements for millions of galaxies. These data should be complemented with upcoming ground-based observations to derive precise and accurate photo-zs. In this article we explore how the tomographic redshift binning and depth of ground-based observations will affect the cosmological constraints expected from the Euclid mission. We focus on GCph and extend the study to include galaxy-galaxy lensing (GGL). We add a layer of complexity to the analysis by simulating several realistic photo-z distributions based on the Euclid Consortium Flagship simulation and using a machine learning photo-z algorithm. We then use the Fisher matrix formalism together with these galaxy samples to study the cosmological constraining power as a function of redshift binning, survey depth, and photo-z accuracy. We find that bins with an equal width in redshift provide a higher figure of merit (FoM) than equipopulated bins and that increasing the number of redshift bins from ten to 13 improves the FoM by 35% and 15% for GCph and its combination with GGL, respectively. For GCph, an increase in the survey depth provides a higher FoM. However, when we include faint galaxies beyond the limit of the spectroscopic training data, the resulting FoM decreases because of the spurious photo-zs. When combining GCph and GGL, the number density of the sample, which is set by the survey depth, is the main factor driving the variations in the FoM. Adding galaxies at faint magnitudes and high redshift increases the FoM, even when they are beyond the spectroscopic limit, since the number density increase compensates for the photo-z degradation in this case. We conclude that there is more information that can be extracted beyond the nominal ten tomographic redshift bins of Euclid and that we should be cautious when adding faint galaxies into our sample since they can degrade the cosmological constraints.
Published: 2021
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42. Euclid Preparation. XIV. The Complete Calibration of the Color–Redshift Relation (C3R2) Survey: Data Release 3

Author: P. Tallada Crespí, Alina Kiessling, L. Stanco, Y. Copin, E. Zucca, Edwin A. Valentijn, L. Moscardini, C. A. J. Duncan, F. Torradeflot, G. Sirri, Bahram Mobasher, F. J. Castander, Harry I. Teplitz, F. Pasian, H. Degaudenzi, Marian Douspis, Santiago Serrano, E. Munari, Henk Hoekstra, Stefano Cavuoti, C. Sirignano, Jean Coupon, G. Mainetti, Massimo Brescia, S. Bardelli, Ariel G. Sánchez, Stefano Camera, Matteo Viel, Pablo Fosalba, V. Scottez, A. Balaguera-Antolínez, D. Di Ferdinando, G. Polenta, R. B. Metcalf, J. Nightingale, Andrea Zacchei, G. A. Verdoes Kleijn, Jason Rhodes, V. Capobianco, Enrico Bozzo, Gianluca Castignani, Florent Sureau, Natalia Auricchio, L. Patrizii, Ivan Lloro, L. Whittaker, Doug Potter, C. S. Carvalho, B. Kubik, S. Casas, M. Fabricius, R. Cledassou, Andrea Biviano, J. Valiviita, Nabila Aghanim, E. Borsato, Peter Schneider, K. Pedersen, M. Frailis, Carlo Baccigalupi, Lucia Pozzetti, I. Davidzon, Sandrine Pires, Andrea Cimatti, Domenico Sapone, Eugenio Maiorano, Massimo Meneghetti, C. C. Kirkpatrick, S. de la Torre, J. Carretero, S. Dusini, Roberto Scaramella, M. Farina, R. Nakajima, G. Congedo, Ralf Bender, Pedro G. Ferreira, David B. Sanders, B. Morin, Ole Marggraf, Peter Capak, Martin Kunz, P. Flose-Reimberg, Luca Conversi, Giuseppe Riccio, A. Balestra, Stéphane Paltani, M. Tenti, W. Gillard, Luca Valenziano, M. Schultheis, Carlo Giocoli, Martin Kilbinger, Carlo Burigana, P. B. Lilje, P. Hudelot, Ken Ganga, Marco Baldi, A. Da Silva, P. Franzetti, D. Masters, S. Kermiche, N. Hernitschek, F. Raison, Anne Costille, S. A. Stanford, C. Bodendorf, Leonardo Corcione, Daniel Stern, Frank Grupp, Romain Teyssier, Stefano Andreon, Herve Aussel, Mischa Schirmer, Cristobal Padilla, Adam Amara, E. Romelli, Ghassem Gozaliasl, Yu Wang, Marco Castellano, Enzo Branchini, N. Martinet, Mark Cropper, M. Poncet, Sami-Matias Niemi, G. Seidel, Ismael Tereno, F. Dubath, Hélène M. Courtois, C. J. Conselice, Katarina Markovic, Davide Maino, Felix Hormuth, A. Cappi, S. Maurogordato, D. Bonino, Roberto P. Saglia, Simona Mei, V. Lindholm, E. Keihänen, Richard Massey, Knud Jahnke, Georges Meylan, Mauro Roncarelli, S. Farrens, Sotiria Fotopoulou, A. N. Taylor, Matteo Maturi, W. Holmes, A. Renzi, Federico Marulli, M. Fumana, Ricard Casas, C. Colodro-Conde, Bianca Garilli, Michele Moresco, Jarle Brinchmann, G. Zamorani, M. Kümmel, R. Kohley, Sebastiano Ligori, E. Franceschi, Rafael Toledo-Moreo, Achille A. Nucita, X. Dupac, Stein Vidar Hagfors Haugan, L. Popa, Javier Graciá-Carpio, C. Neissner, Remi A. Cabanac, Hannu Kurki-Suonio, S. Galeotta, Jean-Gabriel Cuby, Thomas D. Kitching, Behnam Darvish, Emanuel Rossetti, Julien Zoubian, T. Vassallo, A. Secroun, E. Medinaceli, J. G. Cohen, Valeria Pettorino, Carmelita Carbone, René J. Laureijs, Fabio Finelli, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), 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 de Paris (UP), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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., Kummel, 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 Crespi, P., Vassallo, T., Zacchei, A., Andreon, S., Aussel, H., Baccigalupi, C., Balaguera-Antolinez, 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., Gracia-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., Sanchez, 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., Astronomy, 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., Kummel 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 Crespi P., Vassallo T., Zacchei A., Andreon S., Aussel H., Baccigalupi C., Balaguera-Antolinez 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., Gracia-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., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Stanco L., Tenti M., Teyssier R., Torradeflot F., Valiviita J., Viel M., Whittaker L., and Zucca E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Calibration (statistics), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Color space, 01 natural sciences, Cosmology, Large-scale structure, 010309 optics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxy, spectroscopy, Settore FIS/05 - Astronomia e Astrofisica, Spitzer Space Telescope, 0103 physical sciences, DISTRIBUTIONS, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, Hardware_MEMORYSTRUCTURES, Astrophysics::Instrumentation and Methods for Astrophysics, Euclid, Astronomy and Astrophysics, Redshift, Galaxy, Space and Planetary Science, Galaxy spectroscopy, Dark energy, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Stanford, S. A., et al., 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 < zp < 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.
Published: 2021
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43. Euclid preparation: XI. Mean redshift determination from galaxy redshift probabilities for cosmic shear tomography

Author: C. Colodro-Conde, Marco Baldi, K. Pedersen, F. Sureau, Sebastiano Ligori, M. Fabricius, F. Torradeflot, Chiara Sirignano, L. Whittaker, Michele Moresco, J. Valiviita, Sandrine Pires, Christopher J. Conselice, Andrea Zacchei, Natalia Auricchio, A. Renzi, Peter Schneider, M. Tenti, E. Romelli, Elisabetta Maiorano, P. Tallada Crespa, A. Ealet, Eric Jullo, Yu Wang, Marco Castellano, Hendrik Hildebrandt, S. Paltani, K. Markovic, Fabio Pasian, Hélène M. Courtois, E. Franceschi, Enzo Branchini, A. Secroun, N. Martinet, Mark Cropper, Stein Vidar Hagfors Haugan, Adam Amara, Ghassem Gozaliasl, D. Masters, Martin Kunz, G. Seidel, Ismael Tereno, A. Cappi, Leonardo Corcione, Emanuel Rossetti, Ralf Bender, Pedro G. Ferreira, Giuseppe Riccio, Massimo Brescia, D. Di Ferdinando, G. Zamorani, Stefano Borgani, D. Bonino, X. Dupac, Lauro Moscardini, C. Baccigalupi, B. Morin, Rafael Toledo-Moreo, Federico Marulli, C. Padilla, A. Boucaud, Jason Rhodes, F. Dubath, Javier Graciá-Carpio, Remi A. Cabanac, S. Casas, Roberto P. Saglia, F. Grupp, S. Galeotta, Enrico Bozzo, V. Scottez, Luca Valenziano, B. Gillis, Alina Kiessling, L. Popa, R. Cledassou, V. Capobianco, L. Patrizii, Julien Zoubian, Iary Davidzon, Carlo Burigana, Hannu Kurki-Suonio, Jean Coupon, L. Conversi, H. J. McCracken, Lucia Pozzetti, T. Vassallo, Edwin A. Valentijn, G. Sirri, Jean-Gabriel Cuby, N. Welikala, S. Dusini, R. Nakajima, Matteo Maturi, H. Degaudenzi, P. Franzetti, A. Balestra, Stefano Cavuoti, Ole Marggraf, C. S. Carvalho, S. Bardelli, Ruyman Azzollini, W. Gillard, E. Keihänen, A. Da Silva, R. Benton Metcalf, G. Polenta, Gianluca Castignani, S. Maurogordato, M. Poncet, O. Ilbert, Stefano Andreon, Richard Massey, Knud Jahnke, E. Zucca, E. Medinaceli, Mauro Roncarelli, S. Farrens, C. A. J. Duncan, C. Neissner, Doug Potter, Andrea Tramacere, Jochen Weller, Sotiria Fotopoulou, F. J. Castander, J. Carretero, S. Serrano, Pablo Fosalba, Andrea Cimatti, E. Munari, R. Pello, Anne Costille, Tim Schrabback, Stefano Camera, Y. Copin, L. Stanco, W. A. Holmes, Domenico Sapone, I. Lloro, Harry I. Teplitz, B. Garilli, Clotilde Laigle, Ariel G. Sánchez, Luigi Guzzo, F. Raison, N. Mauri, P. B. Lilje, C. Bodendorf, A. Balaguera-Antolínez, Valeria Pettorino, Carmelita Carbone, Fabio Finelli, Andrea Biviano, Angus H. Wright, J. Nightingale, S. de la Torre, S. Niemi, Carlo Giocoli, G. Congedo, S. Kermiche, C. C. Kirkpatrick, Davide Maino, Felix Hormuth, Simona Mei, Astronomy, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of New South Wales [Sydney] (UNSW), 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), California Institute of Technology (CALTECH), University of Copenhagen = Københavns Universitet (KU), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), 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 de Paris (UP), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - 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CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), University of Bordeaux, CNRS, UMR 5805 EPOC, Pessac, France, Recherche en Pharmaco-épidémiologie et Recours aux Soins (REPERES), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-École des Hautes Études en Santé Publique [EHESP] (EHESP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Fondation FondaMental [Créteil], Université Paris-Sorbonne - Paris 4 - École des hautes études en sciences de l'information et de la communication (UP4 CELSA), Université Paris-Sorbonne (UP4), Laboratoire Européen Performance Santé Altitude (LEPSA), Université de Perpignan Via Domitia (UPVD), Wuhan University [China], Euclid Collaboration, Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, Ilbert, O., De La Torre, S., Martinet, N., Wright, A. H., Paltani, S., Laigle, C., Davidzon, I., Jullo, E., Hildebrandt, H., Masters, D. C., Amara, A., Conselice, C. J., Andreon, S., Auricchio, N., Azzollini, R., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Balestra, A., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Borgani, S., Boucaud, A., Bozzo, E., Branchini, E., Brescia, M., Burigana, C., Cabanac, R., Camera, S., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, S., Castander, F. J., Castellano, M., Castignani, G., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Costille, A., Coupon, J., Courtois, H. M., Cropper, M., Cuby, J., Da Silva, A., Degaudenzi, H., Di Ferdinando, D., Dubath, F., Duncan, C., Dupac, X., Dusini, S., Ealet, A., Fabricius, M., Farrens, S., Ferreira, P. G., Finelli, F., Fosalba, P., Fotopoulou, S., Franceschi, E., Franzetti, P., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gozaliasl, G., Gracia-Carpio, J., Grupp, F., Guzzo, L., Haugan, S. V. H., Holmes, W., Hormuth, F., Jahnke, K., Keihanen, E., Kermiche, S., Kiessling, A., Kirkpatrick, C. C., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maturi, M., Mauri, N., Maurogordato, S., Mccracken, H. J., Medinaceli, E., Mei, S., Benton Metcalf, R., Moresco, M., Morin, B., Moscardini, L., Munari, E., Nakajima, R., Neissner, C., Niemi, S., Nightingale, J., Padilla, C., Pasian, F., Patrizii, L., Pedersen, K., Pello, R., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sanchez, A. G., Sapone, D., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Sureau, F., Tallada Crespa, P., Tenti, M., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tramacere, A., Valentijn, E. A., Valenziano, L., Valiviita, J., Vassallo, T., Wang, Y., Welikala, N., Weller, J., Whittaker, L., Zacchei, A., Zamorani, G., Zoubian, J., Zucca, E., 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), University of Copenhagen = Københavns Universitet (UCPH), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), Université de Genève = University of Geneva (UNIGE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA (UMR_8112)), 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), University of Zurich, Ilbert, O, Ilbert O., De La Torre S., Martinet N., Wright A.H., Paltani S., Laigle C., Davidzon I., Jullo E., Hildebrandt H., Masters D.C., Amara A., Conselice C.J., Andreon S., Auricchio N., Azzollini R., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Balestra A., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Borgani S., Boucaud A., Bozzo E., Branchini E., Brescia M., Burigana C., Cabanac R., Camera S., Capobianco V., Cappi A., Carbone C., Carretero J., Carvalho C.S., Casas S., Castander F.J., Castellano M., Castignani G., Cavuoti S., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conversi L., Copin Y., Corcione L., Costille A., Coupon J., Courtois H.M., Cropper M., Cuby J., Da Silva A., Degaudenzi H., Di Ferdinando D., Dubath F., Duncan C., Dupac X., Dusini S., Ealet A., Fabricius M., Farrens S., Ferreira P.G., Finelli F., Fosalba P., Fotopoulou S., Franceschi E., Franzetti P., Galeotta S., Garilli B., Gillard W., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grupp F., Guzzo L., Haugan S.V.H., Holmes W., Hormuth F., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kirkpatrick C.C., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Marggraf O., Markovic K., Marulli F., Massey R., Maturi M., Mauri N., Maurogordato S., McCracken H.J., Medinaceli E., Mei S., Benton Metcalf R., Moresco M., Morin B., Moscardini L., Munari E., Nakajima R., Neissner C., Niemi S., Nightingale J., Padilla C., Pasian F., Patrizii L., Pedersen K., Pello R., Pettorino V., Pires S., Polenta G., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Rossetti E., Saglia R., Sanchez A.G., Sapone D., Schneider P., Schrabback T., Scottez V., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Sureau F., Tallada Crespa P., Tenti M., Teplitz H.I., Tereno I., Toledo-Moreo R., Torradeflot F., Tramacere A., Valentijn E.A., Valenziano L., Valiviita J., Vassallo T., Wang Y., Welikala N., Weller J., Whittaker L., Zacchei A., Zamorani G., Zoubian J., Zucca E., German Research Foundation, European Commission, Centre National D'Etudes Spatiales (France), and Duncan, C
Subjects: statistical [Methods], IMPACT, UNIVERSE, Astrophysics, 01 natural sciences, Dark energy, Galaxies: distances and redshift, dark energy, PHOTOMETRIC REDSHIFTS, 010303 astronomy & astrophysics, Weak gravitational lensing, Photometric redshift, media_common, Physics, distances and redshift [Galaxies], Galaxies: distances and redshifts, Methods: statistical, SIMULATION, astro-ph.CO, 3103 Astronomy and Astrophysics, Probability distribution, Spectral energy distribution, galaxies: distances and redshifts, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 530 Physics, astro-ph.GA, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 1912 Space and Planetary Science, 0103 physical sciences, distances and redshifts [Galaxies], DISTRIBUTIONS, methods: statistical, 010308 nuclear & particles physics, Astronomy and Astrophysics, PERFORMANCE, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Galaxy, Universe, Redshift, STELLAR, RESOLUTION, Space and Planetary Science, 10231 Institute for Computational Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Ilbert, O., et al. (Euclid Collaboration), The analysis of weak gravitational lensing in wide-field imaging surveys is considered to be a major cosmological probe of dark energy. Our capacity to constrain the dark energy equation of state relies on an accurate knowledge of the galaxy mean redshift ⟨ z⟩. We investigate the possibility of measuring ⟨ z»with an accuracy better than 0.002(1 + z) in ten tomographic bins spanning the redshift interval 0.2 99.8%. The zPDF approach can also be successful if the zPDF is de-biased using a spectroscopic training sample. This approach requires deep imaging data but is weakly sensitive to spectroscopic redshift failures in the training sample. We improve the de-biasing method and confirm our finding by applying it to real-world weak-lensing datasets (COSMOS and KiDS+VIKING-450)., H. Hildebrandt is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1) as well as an ERC Consolidator Grant (No. 770935). A.H. Wright is supported by the ERC Consolidator Grant (No. 770935). This work relied on the HPC resources of CINES (Jade) under the allocation 2013047012 and c2014047012 made by GENCI and on the Horizon Cluster hosted by Institut d’Astrophysique de Paris. ID acknowledges that he received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 896225. We warmly thank S. Rouberol for running the cluster on which the simulation was post-processed. This research is also partly supported by the Centre National d’Etudes Spatiales (CNES). We would also like to recognise the contributions from all of the members of the COSMOS team who helped in obtaining and reducing the large amount of multi-wavelength and spectroscopic data. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, 177.A-3018, 179.A-2004, and on data products produced by the KiDS consortium. The KiDS production team acknowledges support from: Deutsche Forschungsgemeinschaft, ERC, NOVA and NWO-M grants; Target; the University of Padova, and the University Federico II (Naples). SA thank the support PRIN MIUR2015 “Cosmology and Fundamental Physics: Illuminating the Dark Universe with Euclid”.
Published: 2021
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44. X-ray Galaxy Clusters & Cosmology.

Author: Ettori, Stefano
Subjects: X-rays, GALAXY clusters, METAPHYSICAL cosmology, LECTURES & lecturing, GASES, DARK energy, SCALING laws (Nuclear physics), PLASMA gases
Abstract: I present a summary of the four lectures given on these topics: (i) Galaxy Clusters in a cosmological context: an introduction; (ii) Galaxy Clusters in X-ray: how and what we observe, limits and prospects; (iii) X-ray Galaxy Clusters and Cosmology: total mass, gas mass & systematics; (iv) Properties of the ICM: scaling laws and metallicity. [ABSTRACT FROM AUTHOR]
Published: 2011
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45. Observations and Morphology of the Cosmic Web.

Author: van de Weygaert, Rien and Bond, J. R.
Published: 2008
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46. Cosmology with Clusters of Galaxies.

Author: Borgani, S.
Published: 2008
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47. Weak Gravitational Lensing.

Author: Schneider, Peter, Kochanek, Christopher S., Wambsganss, Joachim, and Schneider, P.
Published: 2006
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48. Formation and Evolution of Supermassive Black Holes in Galactic Centers: Observational Constraints.

Author: Hasinger, Günther
Subjects: SUPERMASSIVE black holes, SUPERMASSIVE stars, GALACTIC center
Abstract: Deep X-ray surveys have shown that the cosmic X-ray background (XRB) is largely due to the accretion onto supermassive black holes, integrated over the cosmic time. These surveys have resolved more than 80% of the 0.1-10 keV X-ray background into discrete sources. Optical spectroscopic identifications show that the sources producing the bulk of the X-ray background are a mixture of obscured (type-1) and unobscured (type-2) AGNs, as predicted by the XRB population synthesis models. A class of highly luminous type-2 AGN, so called QSO-2s, has been detected in the deepest Chandra and XMM-Newton surveys. The new Chandra AGN redshift distribution peaks at much lower redshifts (z ≈ 0.7) than that based on ROSAT data, indicating that Seyfert galaxies peak at significantly lower redshifts than QSOs. [ABSTRACT FROM AUTHOR]
Published: 2003

49. Deep ROSAT Surveys & the contribution of AGNs to the soft X-ray background.

Author: Lehmann, I., Hasinger, G., Schmidt, M., Gunn, J. E., Schneider, D. P., Giacconi, R., McCaughrean, M., Tru¨mper, J., and Zamorani, G.
Subjects: ACTIVE galactic nuclei, GALACTIC X-ray sources
Abstract: The ROSAT Deep Surveys in the Lockman Hole have revealed that AGNs are the main contributors (∼75 %) to the soft X-ray background in the 1-2 keV band. Using new optical/infrared and radio observations we have obtained a nearly complete identification (93 %) of the 91 X-ray sources down to a limiting flux of 1.2 · 10[sup -15] erg cm[sup -2] s[sup -1] in the 0.5-2.0 keV band. We present the optical colours and the emission line properties of our AGNs in comparison with other X-ray selected AGN samples. Furthermore we discuss the fraction of red AGNs found in the ROSAT Deep Surveys. From the ROSAT Deep Surveys we see no evidence for a new class of X-ray bright galaxies, which significantly contributes to the soft X-ray background. [ABSTRACT FROM AUTHOR]
Published: 2001

50. Euclid preparation: VII. Forecast validation for Euclid cosmological probes

Author: Ivan Lloro, Peter Schneider, S. Ilić, Elisabetta Maiorano, Andrea Zacchei, E. Franceschi, A. Balaguera-Antolinez, M. Frailis, Fabio Pasian, S. Kermiche, S. Paltani, B. Gillis, S. Casas, Ralf Bender, Jason Rhodes, Javier Graciá-Carpio, Luca Valenziano, R. Kohley, Franck Ducret, Mauro Roncarelli, S. Farrens, Sotiria Fotopoulou, Remi A. Cabanac, V. F. Cardone, Jean Coupon, Paula Gomez-Alvarez, Herve Aussel, S. Galeotta, Alain Blanchard, Lucia Pozzetti, Jean-Luc Starck, F. Torradeflot, P. B. Lilje, Ole Marggraf, S. Bardelli, Massimo Brescia, L. Stanco, J. Carretero, Rafael Toledo-Moreo, G. A. Verdoes Kleijn, S. Yahia-Cherif, Richard Massey, Knud Jahnke, G. Polenta, Michele Moresco, Enrico Bozzo, M. Poncet, Stefano Cavuoti, S. Brau-Nogue, G. Sirri, Stefano Andreon, Elisabetta Majerotto, D. Tavagnacco, Isaac Tutusaus, Valeria Pettorino, Carmelita Carbone, D. Di Ferdinando, Davide Maino, Felix Hormuth, Sebastien Clesse, F. Dubath, Simona Mei, A. Boucaud, F. J. Castander, C. A. J. Duncan, R. Cledassou, Z. Sakr, E. Romelli, Robert C. Nichol, E. Munari, Henk Hoekstra, V. Capobianco, Hélène M. Courtois, Stefano Camera, B. Kubik, E. Medinaceli, J. J. Metge, M. H. Fabricius, P. Tallada-Crespí, Matteo Viel, S. Dusini, Andrea Cimatti, Emanuel Rossetti, Yannick Mellier, D. Bonino, C. Padilla, Benjamin J. Metcalf, K. Markovic, Andrea Biviano, Andy Taylor, F. Lacasa, E. Zucca, P. Franzetti, S. de la Torre, A. Da Silva, Julien Zoubian, W. Gillard, Carlo Burigana, Marco Baldi, Martin Kilbinger, L. Conversi, Will J. Percival, T. Vassallo, Yu Wang, Marco Castellano, C. C. Kirkpatrick, V. Yankelevich, Giuseppe D. Racca, Y. Copin, S. Niemi, Domenico Sapone, Pablo Fosalba, G. Congedo, N. Fourmanoit, F. Raison, Enzo Branchini, A. Secroun, N. Martinet, M. Martinelli, Mark Cropper, Ismael Tereno, M. Tenti, A. Cappi, Sandrine Pires, C. J. Conselice, Eric V. Linder, Giulio Fabbian, H. Israel, G. Meylan, Alkistis Pourtsidou, Leonardo Corcione, X. Dupac, Lauro Moscardini, Carlo Giocoli, E. Keihänen, Roberto P. Saglia, F. Grupp, Luigi Guzzo, Ricard Casas, Ariel G. Sánchez, A. Renzi, V. Scottez, Martin Kunz, Federico Marulli, M. Fumana, C. Colodro-Conde, F. Sureau, Sebastiano Ligori, Achille A. Nucita, Hannu Kurki-Suonio, Thomas D. Kitching, Jarle Brinchmann, C. S. Carvalho, 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), Eurecat, Ctr Tecnol Catalunya, Placa Ciencia 2, Manresa 08242, Spain, Corporate technology Siemens, Siemens AG [Munich], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), Centre Jean Perrin [Clermont-Ferrand] (UNICANCER/CJP), UNICANCER, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Ludwig-Maximilians-Universität München (LMU), 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), INAF - Osservatorio Astronomico di Capodimonte (OAC), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique Nucléaire de Lyon (IPNL), 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), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Durham University, Université de Genève = University of Geneva (UNIGE), 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), Dipartimento di Fisica (Milano), Università degli Studi di Milano = University of Milan (UNIMI), Department of Surgical Oncology, University of Groningen [Groningen], Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Centre International de Recherches Médicales de Franceville (CIRMF), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Department of Biogeochemical Integration [Jena], Max Planck Institute for Biogeochemistry (MPI-BGC), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Euclid Collaboration, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Euclid, Blanchard A., Camera S., Carbone C., Cardone V.F., Casas S., Clesse S., Ilic S., Kilbinger M., Kitching T., Kunz M., Lacasa F., Linder E., Majerotto E., Markovic K., Martinelli M., Pettorino V., Pourtsidou A., Sakr Z., Sanchez A.G., Sapone D., Tutusaus I., Yahia-Cherif S., Yankelevich V., Andreon S., Aussel H., Balaguera-Antolinez A., Baldi M., Bardelli S., Bender R., Biviano A., Bonino D., Boucaud A., Bozzo E., Branchini E., Brau-Nogue S., Brescia M., Brinchmann J., Burigana C., Cabanac R., Capobianco V., Cappi A., Carretero J., Carvalho C.S., Casas R., Castander F.J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Coupon J., Courtois H.M., Cropper M., Da Silva A., De La Torre S., Di Ferdinando D., Dubath F., Ducret F., Duncan C.A.J., Dupac X., Dusini S., Fabbian G., Fabricius M., Farrens S., Fosalba P., Fotopoulou S., Fourmanoit N., Frailis M., Franceschi E., Franzetti P., Fumana M., Galeotta S., Gillard W., Gillis B., Giocoli C., Gomez-Alvarez P., Gracia-Carpio J., Grupp F., Guzzo L., Hoekstra H., Hormuth F., Israel H., Jahnke K., Keihanen E., Kermiche S., Kirkpatrick C.C., Kohley R., Kubik B., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Marggraf O., Martinet N., Marulli F., Massey R., Medinaceli E., Mei S., Mellier Y., Metcalf B., Metge J.J., Meylan G., Moresco M., Moscardini L., Munari E., Nichol R.C., Niemi S., Nucita A.A., Padilla C., Paltani S., Pasian F., Percival W.J., Pires S., Polenta G., Poncet M., Pozzetti L., Racca G.D., Raison F., Renzi A., Rhodes J., Romelli E., Roncarelli M., Rossetti E., Saglia R., Schneider P., Scottez V., Secroun A., Sirri G., Stanco L., Starck J.-L., Sureau F., Tallada-Crespi P., Tavagnacco D., Taylor A.N., Tenti M., Tereno I., Toledo-Moreo R., Torradeflot F., Valenziano L., Vassallo T., Verdoes Kleijn G.A., Viel M., Wang Y., Zacchei A., Zoubian J., Zucca E., Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Academy of Finland, European Commission, Agenzia Spaziale Italiana, Belgian Science Policy Office, Canadian Euclid Consortium, Centre National D'Etudes Spatiales (France), Danish Space Research Institute, German Centre for Air and Space Travel, Fundação para a Ciência e a Tecnologia (Portugal), Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), Netherlands Research School for Astronomy, Norwegian Space Agency, Romanian Space Agency, State Secretariat for Education, Research and Innovation (Switzerland), Swiss Space Office, UK Space Agency, Ministero dell'Istruzione, dell'Università e della Ricerca, California Institute of Technology, Ministerio de Ciencia, Innovación y Universidades (España), International Max Planck Research Schools, Swiss National Science Foundation, Blanchard, A., Camera, S., Carbone, C., Cardone, V. F., Casas, S., Clesse, S., Ilić, S., Kilbinger, M., Kitching, T., Kunz, M., Lacasa, F., Linder, E., Majerotto, E., Markovič, K., Martinelli, M., Pettorino, V., Pourtsidou, A., Sakr, Z., Sánchez, A. G., Sapone, D., Tutusaus, I., Yahia-Cherif, S., Yankelevich, V., Andreon, S., Aussel, H., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Bender, R., Biviano, A., Bonino, D., Boucaud, A., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Cabanac, R., Capobianco, V., Cappi, A., Carretero, J., Carvalho, C. S., Casas, R., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Coupon, J., Courtois, H. M., Cropper, M., Da, Silva, de la, Torre, Di, Ferdinando, D., Dubath, F., Ducret, F., Duncan, C. A. J., Dupac, X., Dusini, S., Fabbian, G., Fabriciu, M., Farren, S., Fosalba, P., Fotopoulou, S., Fourmanoit, N., Fraili, M., Franceschi, E., Franzetti, P., Fumana, M., Galeotta, S., Gillard, W., Gilli, B., Giocoli, C., Gómez-Alvarez, P., Graciá-Carpio, J., Grupp, F., Guzzo, L., Hoekstra, H., Hormuth, F., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kirkpatrick, C. C., Kohley, R., Kubik, B., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Marggraf, O., Martinet, N., Marulli, F., Massey, R., Medinaceli, E., Mei, S., Mellier, Y., Metcalf, B., Metge, J. J., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Nichol, R. C., Niemi, S., Nucita, A. A., Padilla, C., Paltani, S., Pasian, F., Percival, W. J., Pire, S., Polenta, G., Poncet, M., Pozzetti, L., Racca, G. D., Raison, F., Renzi, A., Rhode, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Scottez, V., Secroun, A., Sirri, G., Stanco, L., Starck, J., -L., Sureau, F., Tallada-Crespí, P., Tavagnacco, D., Taylor, A. N., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valenziano, L., Vassallo, T., Verdoes, Kleijn, G. A., Viel, M., Wang, Y., Zacchei, A., Zoubian, J., Zucca, Ilic, S., Markovic, K., Sanchez, A. G., Balaguera-Antolinez, A., Da Silva, A., De La Torre, S., Di Ferdinando, D., Dubath, F., Ducret, F., Duncan, C. A. J., Dupac, X., Dusini, S., Fabbian, G., Fabricius, M., Farrens, S., Fosalba, P., Fotopoulou, S., Fourmanoit, N., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Galeotta, S., Gillard, W., Gillis, B., Giocoli, C., Gomez-Alvarez, P., Gracia-Carpio, J., Grupp, F., Guzzo, L., Hoekstra, H., Hormuth, F., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kirkpatrick, C. C., Kohley, R., Kubik, B., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Marggraf, O., Martinet, N., Marulli, F., Massey, R., Medinaceli, E., Mei, S., Mellier, Y., Metcalf, B., Metge, J. J., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Nichol, R. C., Niemi, S., Nucita, A. A., Padilla, C., Paltani, S., Pasian, F., Percival, W. J., Pires, S., Polenta, G., Poncet, M., Pozzetti, L., Racca, G. D., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Scottez, V., Secroun, A., Sirri, G., Stanco, L., Starck, J. -L., Tallada-Crespi, P., Verdoes Kleijn, G. A., Viel, M., Wang, Y., Zacchei, A., Zoubian, J., Zucca, E., Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of Geneva [Switzerland], Università degli Studi di Milano [Milano] (UNIMI), Institut Régional de Médecine Physique et de Réadaptation Louis Pierquin [Nancy] (IRR Louis Pierquin), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Department of Physics, Helsinki Institute of Physics, and Astronomy
Subjects: cosmology: observations / cosmological parameters / cosmology: theory, Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), DARK ENERGY CONSTRAINTS, IMPACT, ANGULAR POWER SPECTRA, Cosmological parameters, Cosmology: observations, Cosmology: theory, FOS: Physical sciences, observation [Cosmology], GALAXY REDSHIFT SURVEYS, Astrophysics, Cosmological constant, Astrophysics::Cosmology and Extragalactic Astrophysics, ACOUSTIC-OSCILLATIONS, 01 natural sciences, Measure (mathematics), Cosmology: observation, PRIMORDIAL NON-GAUSSIANITY, Set (abstract data type), INFORMATION-CONTENT, HALO-MODEL, theory [Cosmology], cosmology: theory, 0103 physical sciences, cosmological parameters, observations [Cosmology], Cluster analysis, 010303 astronomy & astrophysics, Astrophysique, Weak gravitational lensing, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Astronomy and Astrophysics, INTRINSIC ALIGNMENTS, 115 Astronomy, Space science, MASSIVE NEUTRINOS, Space and Planetary Science, cosmology: observations, astro-ph.CO, Dark energy, Baryon acoustic oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. The Euclid space telescope will measure the shapes and redshifts of galaxies to reconstruct the expansion history of the Universe and the growth of cosmic structures. The estimation of the expected performance of the experiment, in terms of predicted constraints on cosmological parameters, has so far relied on various individual methodologies and numerical implementations, which were developed for different observational probes and for the combination thereof. In this paper we present validated forecasts, which combine both theoretical and observational ingredients for different cosmological probes. This work is presented to provide the community with reliable numerical codes and methods for Euclid cosmological forecasts. Methods. We describe in detail the methods adopted for Fisher matrix forecasts, which were applied to galaxy clustering, weak lensing, and the combination thereof. We estimated the required accuracy for Euclid forecasts and outline a methodology for their development. We then compare and improve different numerical implementations, reaching uncertainties on the errors of cosmological parameters that are less than the required precision in all cases. Furthermore, we provide details on the validated implementations, some of which are made publicly available, in different programming languages, together with a reference training-set of input and output matrices for a set of specific models. These can be used by the reader to validate their own implementations if required. Results. We present new cosmological forecasts for Euclid. We find that results depend on the specific cosmological model and remaining freedom in each setting, for example flat or non-flat spatial cosmologies, or different cuts at non-linear scales. The numerical implementations are now reliable for these settings. We present the results for an optimistic and a pessimistic choice for these types of settings. We demonstrate that the impact of cross-correlations is particularly relevant for models beyond a cosmological constant and may allow us to increase the dark energy figure of merit by at least a factor of three., 0, info:eu-repo/semantics/published
Published: 2020
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