Euclid preparation XXX. Performance assessment of the NISP red grism through spectroscopic simulations for the wide and deep surveys

被引：7

作者：

Gabarra, L. ^{[1
,2
]}

Mancini, C.

Rodriguez Munoz, L.

Rodighiero, G. ^{[1
,4
]}

Sirignano, C. ^{[1
,2
]}

Scodeggio, M. ^{[3
]}

Talia, M. ^{[6
]}

Dusini, S. ^{[2
]}

Gillard, W. ^{[7
]}

Granett, B. R. ^{[8
]}

Maiorano, E. ^{[6
]}

Moresco, M. ^{[5
,6
]}

Paganin, L. ^{[9
,10
]}

Palazzi, E. ^{[6
]}

Pozzetti, L. ^{[6
]}

Renzi, A. ^{[1
,2
]}

Rossetti, E. ^{[11
]}

Vergani, D. ^{[6
]}

Allevato, V. ^{[12
]}

Bisigello, L. ^{[1
,4
]}

Castignani, G. ^{[5
,6
]}

De Caro, B. ^{[1
]}

Fumana, M. ^{[3
]}

Ganga, K. ^{[13
]}

Garilli, B. ^{[3
]}

Hirschmann, M. ^{[14
]}

La Franca, F. ^{[16
]}

Laigle, C. ^{[17
]}

Passalacqua, F. ^{[2
]}

Schirmer, M. ^{[18
]}

Stanco, L.

Troja, A. ^{[1
]}

Yung, L. Y. A. ^{[19
]}

Zamorani, G. ^{[6
]}

Zoubian, J. ^{[7
]}

Anselmi, S. ^{[1
,2
]}

Oppizzi, F. ^{[1
,2
]}

Verza, G. ^{[1
]}

Aghanim, N. ^{[20
]}

Amara, A. ^{[21
]}

Auricchio, N. ^{[6
]}

Baldi, M. ^{[5
,22
]}

Bender, R. ^{[23
,24
]}

Bodendorf, C. ^{[23
]}

Bonino, D. ^{[25
]}

Branchini, E. ^{[9
,26
]}

Brescia, M. ^{[27
,28
]}

Brinchmann, J.

Camera, S. ^{[25
,29
,30
]}

Capobianco, V. ^{[25
]}

机构：

[1] Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy

[2] INFN Padova, Via Marzolo 8, I-35131 Padua, Italy

[3] INAF IASF Milano, Via Alfonso Corti 12, I-20133 Milan, Italy

[4] INAF Osservatorio Astronom Padova, Via Osservatorio 5, I-35122 Padua, Italy

[5] Univ Bologna, Dipartimento Fis & Astron, Augusto Righi Alma Mater Studiorum, Via Piero Gobetti 93-2, I-40129 Bologna, Italy

[6] INAF Osservat Astrofis & Sci Spazio Bologna, Via Piero Gobetti 93-3, I-40129 Bologna, Italy

[7] Aix Marseille Univ, CNRS, IN2P3, CPPM, Marseille, France

[8] INAF Osserv Astronom Brera, Via Brera 28, I-20122 Milan, Italy

[9] Univ Genoa, Dipartimento Fis, Via Dodecaneso 33, I-16146 Genoa, Italy

[10] INFN, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy

[11] Univ Bologna, Dipartimento Fis & Astron, Via Gobetti 93 2, I-40129 Bologna, Italy

[12] INAF Osserv Astronom Capodimonte, Via Moiariello 16, I-80131 Naples, Italy

[13] Univ Paris Cite, CNRS, Astroparticule & Cosmol, F-75013 Paris, France

[14] Ecole Poly Tech Federale Lausanne, Inst Phys, Lab Galaxy Evolut, Observ Sauverny, CH-1290 Versoix, Switzerland

[15] INAF Osserv Astronom Trieste, Via G B Tiepolo 11, I-34143 Trieste, Italy

[16] Roma Tre Univ, Dept Math & Phys, Via Vasca Navale 84, I-00146 Rome, Italy

[17] Sorbonne Univ, Inst Astrophys Paris, UMR 7095, CNRS, F-75014 Paris, France

[18] Max Planck Inst Astronom, Konigstuhl 17, D-69117 Heidelberg, Germany

[19] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[20] Univ Paris Saclay, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France

[21] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[22] INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy

[23] Max Planck Inst Extraterrestrial Phys, Giessenbachstr 1, D-85748 Garching, Germany

[24] Ludwig Maximilians Univ Munchen, Univ Sternwarte Munchen, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany

[25] INAF Osserv Astrofis Torino, Via Osserv 20, I-10025 Pino Torinese, TO, Italy

[26] INFN, Sez Roma Tre, Via Vasca Navale 84, I-00146 Rome, Italy

[27] Univ Federico II, Dept Phys E Pancini, Via Cinthia 6, I-80126 Naples, Italy

[28] Univ Porto, Inst Astrofis Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal

[29] Univ Torino, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy

[30] INFN, Sez Torino, Via P Giuria 1, I-10125 Turin, Italy

[31] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, Bellaterra 08193, Barcelona, Spain

[32] Port Informacio Cient, Campus UAB,C Albareda S-N, Bellaterra 08193, Spain

[33] Inst Estudis Espacials Catalunya IEEC, Carrer Gran Capita 2-4, Barcelona 08034, Spain

[34] CSIC, Inst Space Sci ICE, Campus UAB, Carrer Can Magrans,S-N, Barcelona 08193, Spain

[35] INAF Osserv Astronom Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy

[36] INFN sect Naples, Via Cinthia 6, I-80126 Naples, Italy

[37] Ctr Natl Etudes Spati Ctr Spatial Toulouse, 18 Ave Edouard Belin, F-31401 Toulouse, France

[38] Inst Natl Phys Nucl & Phys Particules, 3 Rue Michel Ange, F-75794 Paris, France

[39] Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland

[40] Univ Manchester, Dept Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Oxford M13 9PL, England

[41] ESAC ESA, Camino Bajo Castillo S-N, Madrid, Spain

[42] European Space Agcy ESRIN, Largo Galileo Galilei 1, I-00044 Frascati, Italy

[43] Univ Claude Bernard Lyon 1, Univ Lyon, CNRS, IP2I Lyon,UMR 5822,IN2P3, Lyon, France

[44] Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France

[45] Ecole Polytech Federale Lausanne EPFL, Inst Phys, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland

[46] Univ Lisbon, Dept Fis, Fac Ciencias, Edificio C8, Lisbon, Portugal

[47] Univ Lisbon, Inst Astrofis & Ciencias Espaco, Fac Ciencias, Lisbon, Portugal

[48] Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland

[49] Univ Paris Cite, Univ Paris Saclay, CNRS, CEA,Astrophys,Instrumentat & Modelisat Paris Sacl, F-91191 Gif Sur Yvette, France

[50] Ist Nazl Fis Nucl, Sez Bologna, Via Irnerio 46, I-40126 Bologna, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 676卷

基金：

美国国家航空航天局; 芬兰科学院;

关键词：

surveys; Galaxy; evolution; galaxies; formation; star formation; techniques; spectroscopic; instrumentation; detectors; STAR-FORMING GALAXIES; FMOS-COSMOS SURVEY; MASS-METALLICITY RELATION; SPIRAL GALAXIES; FORMATION RATES; MAIN-SEQUENCE; HIGH-REDSHIFT; STRONG LINES; EMISSION; EVOLUTION;

D O I：

10.1051/0004-6361/202346177

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This work focusses on the pilot run of a simulation campaign aimed at investigating the spectroscopic capabilities of the Euclid NearInfrared Spectrometer and Photometer (NISP), in terms of continuum and emission line detection in the context of galaxy evolutionary studies. To this purpose, we constructed, emulated, and analysed the spectra of 4992 star-forming galaxies at 0:3 <= z <= 2:5 using the NISP pixel-level simulator. We built the spectral library starting from public multi-wavelength galaxy catalogues, with value-added information on spectral energy distribution (SED) fitting results, and stellar population templates from Bruzual & Charlot (2003, MNRAS, 344, 1000). Rest-frame optical and near-IR nebular emission lines were included using empirical and theoretical relations. Dust attenuation was treated using the Calzetti extinction law accounting for the differential attenuation in line-emitting regions with respect to the stellar continuum. The NISP simulator was configured including instrumental and astrophysical sources of noise such as the dark current, read-out noise, zodiacal background, and out-of-field stray light. In this preliminary study, we avoided contamination due to the overlap of the slitless spectra. For this purpose, we located the galaxies on a grid and simulated only the first order spectra. We inferred the 3.5 sigma NISP red grism spectroscopic detection limit of the continuum measured in the H band for star-forming galaxies with a median disk half-light radius of 0 :00 4 at magnitude H = 19:5 +/- 0:2ABmag for the Euclid Wide Survey and at H = 20:8 +/- 0:6ABmag for the Euclid Deep Survey. We found a very good agreement with the red grism emission line detection limit requirement for the Wide and Deep surveys. We characterised the effect of the galaxy shape on the detection capability of the red grism and highlighted the degradation of the quality of the extracted spectra as the disk size increased. In particular, we found that the extracted emission line signal-to-noise ratio (S/N) drops by similar to 45% when the disk size ranges from 0".25 to 1". These trends lead to a correlation between the emission line S/N and the stellar mass of the galaxy and we demonstrate the effect in a stacking analysis unveiling emission lines otherwise too faint to detect.

引用

页数：24

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