Euclid preparation. XVIII. The NISP photometric system
Euclid Collaboration, M. Schirmer, K. Jahnke, G. Seidel, H. Aussel, C. Bodendorf, F. Grupp, F. Hormuth, S. Wachter, P. N. Appleton, R. Barbier, J. Brinchmann, J… 展开作者
Euclid Collaboration, M. Schirmer, K. Jahnke, G. Seidel, H. Aussel, C. Bodendorf, F. Grupp, F. Hormuth, S. Wachter, P. N. Appleton, R. Barbier, J. Brinchmann, J. M. Carrasco, F. J. Castander, J. Coupon, F. De Paolis, A. Franco, K. Ganga, P. Hudelot, E. Jullo, A. Lancon, A. A. Nucita, S. Paltani, G. Smadja, L. M. G. Venancio, F. Strafella, M. Weiler, A. Amara, T. Auphan, N. Auricchio, A. Balestra, R. Bender, D. Bonino, E. Branchini, M. Brescia, V. Capobianco, C. Carbone, J. Carretero, R. Casas, M. Castellano, S. Cavuoti, A. Cimatti, R. Cledassou, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, L. Corcione, A. Costille, F. Courbin, A. Da Silva, H. Degaudenzi, M. Douspis, F. Dubath, X. Dupac, S. Dusini, A. Ealet, S. Farrens, S. Ferriol, P. Fosalba, M. Frailis, E. Franceschi, P. Franzetti, M. Fumana, B. Garilli, W. Gillard, B. Gillis, C. Giocoli, A. Grazian, L. Guzzo, S. V. H. Haugan, H. Hoekstra, W. Holmes, A. Hornstrup, S. Kermiche, A. Kiessling, M. Kilbinger, T. Kitching, R. Kohley, M. Kümmel, M. Kunz, H. Kurki-Suonio, R. Laureijs, S. Ligori, P. B. Lilje, I. Lloro, T. Maciaszek, E. Maiorano, O. Mansutti, O. Marggraf, K. Markovic, F. Marulli, R. Massey, S. Maurogordato, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, M. Moresco, L. Moscardini, E. Munari, R. Nakajima, R. C. Nichol, S. M. Niemi, C. Padilla, F. Pasian, K. Pedersen, W. J. Percival, V. Pettorino, S. Pires, M. Poncet, L. Popa, L. Pozzetti, E. Prieto, F. Raison, J. Rhodes, H. -W. Rix, M. Roncarelli, E. Rossetti, R. Saglia, B. Sartoris, R. Scaramella, P. Schneider, A. Secroun, S. Serrano, C. Sirignano, G. Sirri, L. Stanco, P. Tallada-Crespí, A. N. Taylor, H. I. Teplitz, I. Tereno, R. Toledo-Moreo, F. Torradeflot, M. Trifoglio, E. A. Valentijn, L. Valenziano, Y. Wang, J. Weller, G. Zamorani, J. Zoubian, S. Andreon, S. Bardelli, A. Boucaud, S. Camera, R. Farinelli, J. Graciá-Carpio, D. Maino, E. Medinaceli, S. Mei, N. Morisset, G. Polenta, A. Renzi, E. Romelli, M. Tenti, T. Vassallo, A. Zacchei, E. Zucca, C. Baccigalupi, A. Balaguera-Antolínez, A. Biviano, A. Blanchard, S. Borgani, E. Bozzo, C. Burigana, R. Cabanac, A. Cappi, C. S. Carvalho, S. Casas, G. Castignani, C. Colodro-Conde, A. R. Cooray, H. M. Courtois, M. Crocce, J. -G. Cuby, S. Davini, S. de la Torre, D. Di Ferdinando, J. A. Escartin, M. Farina, P. G. Ferreira, F. Finelli, S. Fotopoulou, S. Galeotta, J. Garcia-Bellido, E. Gaztanaga, K. George, G. Gozaliasl, I. M. Hook, S. Ilić, V. Kansal, A. Kashlinsky, E. Keihanen, C. C. Kirkpatrick, V. Lindholm, G. Mainetti, R. Maoli, M. Martinelli, N. Martinet, M. Maturi, N. Mauri, H. J. McCracken, R. B. Metcalf, P. Monaco, G. Morgante, J. Nightingale, L. Patrizii, A. Peel, V. Popa, C. Porciani, D. Potter, P. Reimberg, G. Riccio, A. G. Sánchez, D. Sapone, V. Scottez, E. Sefusatti, R. Teyssier, I. Tutusaus, C. Valieri, J. Valiviita, M. Viel, H. Hildebrandt
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33 pages, 25 figures, accepted for publication in A&A
Euclid will be the first space mission to survey most of the extragalactic sky in the 0.95-2.02 $μ$m range, to a 5$σ$ point-source median depth of 24.4 AB mag. This unique photometric data set will find wide use beyond Euclid's core science. In this paper, we present accurate computations of the Euclid Y_E, J_E and H_E passbands used by the Near-Infrared Spectrometer and Photometer (NISP), and the associated photometric system. We pay particular attention to passband variations in the field of view, accounting among others for spatially variable filter transmission, and variations of the angle of incidence on the filter substrate using optical ray tracing. The response curves' cut-on and cut-off wavelengths - and their variation in the field of view - are determined with 0.8 nm accuracy, essential for the photometric redshift accuracy required by Euclid. After computing the photometric zeropoints in the AB mag system, we present linear transformations from and to common ground-based near-infrared photometric systems, for normal stars, red and brown dwarfs, and galaxies separately. A Python tool to compute accurate magnitudes for arbitrary passbands and spectral energy distributions is provided. We discuss various factors from space weathering to material outgassing that may slowly alter Euclid's spectral response. At the absolute flux scale, the Euclid in-flight calibration program connects the NISP photometric system to Hubble Space Telescope spectrophotometric white dwarf standards; at the relative flux scale, the chromatic evolution of the response is tracked at the milli-mag level. In this way, we establish an accurate photometric system that is fully controlled throughout Euclid's lifetime.
To characterise the NISP (Near-Infrared Spectrometer and Photometer) instrument optical capability before the launch of the \Euclid telescope to orbit, foreseen in 2023, data analysis of ground-based tests and Monte Carlo simulations that mimic the expected NISP performance were carried out. Pre-launch test data were analysed to assess the fulfilment of the mission specifications in terms of Point Spread Function (PSF), set at EE50(PSF)$\,\leq 0.3$ arcseconds, and with a spectral resolution below 16 angstroms per pixel. We also provide a first comparison between real images from the ground-bas…
ESA EUCLID mission will be launched in 2020 to understand the nature of the dark energy responsible of the accelerated expansion of the Universe and to map the geometry of the dark matter. The map will investigate the distanceredshift relationship and the evolution of cosmic structures thanks to two instruments: the NISP and the VIS. The NISP (Near Infrared Spectro-Photometer) is operating in the near-IR spectral range (0.9-2$μ$m) with two observing modes: the photometric mode for the acquisition of images with broad band filters, and the spectroscopic mode for the acquisition of slitless disp…
The Euclid satellite, to be launched by ESA in 2022, will be a major instrument for cosmology for the next decades. \Euclid\ is composed of two instruments: the Visible (VIS) instrument and the Near Infrared Spectromete and Photometer (NISP). In this work we estimate the implications of correlated readout noise in the NISP detectors for the final in-flight flux measurements. Considering the multiple accumulated (MACC) readout mode, for which the UTR (Up The Ramp) exposure frames are averaged in groups, we derive an analytical expression for the noise covariance matrix between groups in the pre…
Euclid Near Infrared Spectro-Photometer: spatial considerations on H2RG detectors interpixel capacitance and IPC corrected conversion gain from on-ground characterization
Euclid. Properties and performance of the NISP signal estimator
Alma Mater Studiorum Università di Bologna（博洛尼亚大学）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚国家天体物理研究所天文与空间科学观测站）；Université Claude Bernard Lyon 1（里昂第一大学）；CNRS/IN2P3, IP2I Lyon（法国国家科学研究中心/法国国家核子与粒子物理研究所，里昂粒子与宇宙学物理研究所）；INFN-Bologna（博洛尼亚意大利国家核物理研究所）；Université Paris-Saclay（巴黎萨克雷大学）；Institut d’astrophysique spatiale（太空天体物理研究所）；ESAC/ESA（欧洲空间应用中心/欧洲空间局）；INAF-Osservatorio Astronomico di Brera（布雷拉天文台）
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；CEA Saclay, DFR/IRFU, Service d’Astrophysique（法国原子能和替代能源委员会萨克雷研究中心核物理与核工程研究所天体物理部）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Université Paris-Saclay, CNRS, Institut d’astrophysique spatiale（巴黎-萨克雷大学、法国国家科学研究中心空间天体物理研究所）；ESAC/ESA（欧洲空间应用中心/欧洲空间局）；School of Mathematics and Physics, University of Surrey（萨里大学数学与物理学院）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；INFN, Sezione di Trieste（意大利国家核物理研究院的里雅斯特分部）；SISSA, International School for Advanced Studies（国际高等研究学院）；Dipartimento di Fisica e Astronomia, Università di Bologna（博洛尼亚大学物理与天文学系）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间天体物理学与天体物理观测站）；INFN-Sezione di Bologna（意大利国家核物理研究院博洛尼亚分部）
Euclid preparation: The NISP spectroscopy channel, on ground performance and calibration
Aix-Marseille Université（艾克斯-马赛大学）；CNRS/IN2P3, CPPM（法国国家科学研究中心/欧洲粒子物理研究所，马普核物理研究所）；Centre National d’Etudes Spatiales – Centre spatial de Toulouse（法国国家空间研究中心 - 图卢兹航天中心）；CNES, LAM（法国国家空间研究中心，拉格朗日天体物理实验室）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理学研究所）；Universitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-Universität München（慕尼黑大学天文台，物理学院，路德维希-马克西米利安大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；INFN-Padova（意大利国家核物理研究所帕多瓦分部）；Dipartimento di Fisica e Astronomia "G. Galilei", Università di Padova（帕多瓦大学伽利略物理与天文学系）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间科学与天体物理观测站）；INAF-Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）
The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments. It operates in the near-IR spectral region (950-2020nm) as a photometer and spectrometer. The instrument is composed of: a cold (135 K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly, a filter wheel mechanism, a grism wheel mechanism, a calibration unit, and a thermal control system, a detection system based on a mosaic of 16 H2RG with their front-end readout electronic, and a warm electronic system (290 K) composed of a data processing / detector control unit and…
Euclid preparation. First investigation of the impact of cross-contamination on spectroscopic redshift measurements with pixel-level simulations
Università di Padova（帕多瓦大学）；INFN-Padova（意大利国家核物理研究所帕多瓦分部）；Laboratoire Univers et Théorie, Observatoire de Paris, Université PSL, Université Paris Cité, CNRS（巴黎天文台宇宙与理论实验室，巴黎文理研究大学，巴黎西岱大学，法国国家科学研究中心）；Università di Trieste（的里雅斯特大学）；INAF-Osservatorio Astronomico di Trieste（的里雅斯特天文台）；INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Aix-Marseille Université（艾克斯-马赛大学）；CNRS/IN2P3, CPPM（法国国家科学研究中心/欧洲粒子物理研究所，普罗旺斯粒子与天体物理中心）；INAF-IASF Milano（米兰空间天体物理学研究所）
The ESA Euclid mission will provide high-quality imaging for about 1.5 billion galaxies. A software pipeline to automatically process and analyse such a huge amount of data in real time is being developed by the Science Ground Segment of the Euclid Consortium; this pipeline will include a model-fitting algorithm, which will provide photometric and morphological estimates of paramount importance for the core science goals of the mission and for legacy science. The Euclid Morphology Challenge is a comparative investigation of the performance of five model-fitting software packages on simulated E…
Euclid: High-precision imaging astrometry and photometry from Early Release Observations. I. Internal kinematics of NGC 6397 by combining Euclid and Gaia data
