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Horizon-AGN virtual observatory – 1. SED-fitting performance and forecasts for future imaging surveys

Laigle, C. and Davidzon, I. and Ilbert, O. and Devriendt, J. and Kashino, D. and Pichon, C. and Capak, P. and Arnouts, S. and de la Torre, S and Dubois, Y. and Gozaliasl, G. and Le Borgne, D. and Lilly, S. and McCracken, H. J. and Salvato, M. and Slyz, A. (2019) Horizon-AGN virtual observatory – 1. SED-fitting performance and forecasts for future imaging surveys. Monthly Notices of the Royal Astronomical Society, 486 (4). pp. 5104-5123. ISSN 0035-8711. doi:10.1093/mnras/stz1054.

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Using the light-cone from the cosmological hydrodynamical simulation HORIZON-AGN, we produced a photometric catalogue over 0 < z < 4 with apparent magnitudes in COSMOS, Dark Energy Survey, Large Synoptic Survey Telescope (LSST)-like, and Euclid-like filters at depths comparable to these surveys. The virtual photometry accounts for the complex star formation history (SFH) and metal enrichment of HORIZON-AGN galaxies, and consistently includes magnitude errors, dust attenuation, and absorption by intergalactic medium. The COSMOS-like photometry is fitted in the same configuration as the COSMOS2015 catalogue. We then quantify random and systematic errors of photometric redshifts, stellar masses, and star formation rates (SFR). Photometric redshifts and redshift errors capture the same dependencies on magnitude and redshift as found in COSMOS2015, excluding the impact of source extraction. COSMOS-like stellar masses are well recovered with a dispersion typically lower than 0.1 dex. The simple SFHs and metallicities of the templates induce a systematic underestimation of stellar masses at z < 1.5 by at most 0.12 dex. SFR estimates exhibit a dust-induced bimodality combined with a larger scatter (typically between 0.2 and 0.6 dex). We also use our mock catalogue to predict photometric redshifts and stellar masses in future imaging surveys. We stress that adding Euclid near-infrared photometry to the LSST-like baseline improves redshift accuracy especially at the faint end and decreases the outlier fraction by a factor ∼2. It also considerably improves stellar masses, reducing the scatter up to a factor 3. It would therefore be mutually beneficial for LSST and Euclid to work in synergy.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Davidzon, I.0000-0002-2951-7519
Ilbert, O.0000-0002-7303-4397
Devriendt, J.0000-0002-8140-0422
Kashino, D.0000-0001-9044-1747
Capak, P.0000-0003-3578-6843
de la Torre, S0000-0002-0839-2884
Gozaliasl, G.0000-0002-0236-919X
Lilly, S.0000-0002-6423-3597
McCracken, H. J.0000-0002-9489-7765
Salvato, M.0000-0001-7116-9303
Additional Information:© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model ( Accepted 2019 April 5. Received 2019 March 26; in original form 2018 December 31. Published: 13 April 2019. CL is supported by a Beecroft Fellowship, and thanks the Korean Astronomy and Space Science Institute for hospitality when this work was finalized. ID was supported in part by NASA ROSES grant 12-EUCLID12-0004. OI acknowledges the funding of the French Agence Nationale de la Recherche for the project ‘SAGACE’. JD and AS acknowledge funding support from Adrian Beecroft, the Oxford Martin School and the STFC. HJMCC acknowledges support from the Programme national cosmologie et galaxies (PNCG) and the Domaine d’intérêt majeur en astrophysique et conditions d’apparition de la vie (DIM–ACAV +). The authors thank A. L. Serra for her suggestions to improve graphic rendering of the figures. This research was supported in part by the National Science Foundation under Grant No. NSF PHY-1748958. This work relied on the HPC resources of CINES (Jade) under the allocation 2013047012 and c2014047012 made by GENCI and on the Horizon and CANDIDE clusters hosted by Institut d’Astrophysique de Paris. We warmly thank S. Rouberol for maintaining these clusters on which the simulation was post-processed. This research is part of Spin(e) (ANR-13-BS05-0005,, ERC grant 670193 and HORIZON-UK. This research is also partly supported by the Centre National dEtudes Spatiales (CNES). This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Beecroft FellowshipUNSPECIFIED
Agence Nationale de la Recherche (ANR)UNSPECIFIED
Adrian BeecroftUNSPECIFIED
Oxford Martin SchoolUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Programme National Cosmologie et Galaxies (PNCG)UNSPECIFIED
Domaine d’intérêt majeur en astrophysique et conditions d’apparition de la vie (DIM–ACAV +)UNSPECIFIED
European Research Council (ERC)670193
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Subject Keywords:methods: observational – techniques: photometric – galaxies: evolution – galaxies: formation
Issue or Number:4
Record Number:CaltechAUTHORS:20190801-093834016
Persistent URL:
Official Citation:C Laigle, I Davidzon, O Ilbert, J Devriendt, D Kashino, C Pichon, P Capak, S Arnouts, S de la Torre, Y Dubois, G Gozaliasl, D Le Borgne, S Lilly, H J McCracken, M Salvato, A Slyz, Horizon-AGN virtual observatory – 1. SED-fitting performance and forecasts for future imaging surveys, Monthly Notices of the Royal Astronomical Society, Volume 486, Issue 4, July 2019, Pages 5104–5123,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97580
Deposited By: Tony Diaz
Deposited On:01 Aug 2019 16:49
Last Modified:16 Nov 2021 17:32

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