MAMBO: An empirical galaxy and AGN mock catalogue for the exploitation of future surveys

¹ INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero Gobetti 93/3, 40129 Bologna, Italy
² Dipartimento di Fisica e Astronomia, Università di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy
³ Max-Planck-Institut für extraterrestrische Physik, Giessenbachstr. 1, 85748 Garching, Germany
⁴ Exzellenzcluster ORIGINS, Boltzmannstr. 2, 85748 Garching, Germany
⁵ INAF, Istituto di Radioastronomia, Via Piero Gobetti 101, 40129 Bologna, Italy
⁶ Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova, Via Marzolo 8, 35131 Padova, Italy
⁷ INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy
⁸ INAF – Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monteporzio Catone, Italy
⁹ Department of Physics and Helsinki Institute of Physics, Gustaf Hällströmin katu 2, 00014 University of Helsinki, Finland
¹⁰ INAF – Osservartorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy
¹¹ Independent researcher, Bologna, Italy
¹² Sorbonne Université, CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, France
¹³ Dipartimento di Matematica e Fisica, Università degli Studi Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy
¹⁴ IBEX Innovations, Sedgefield, Stockton-on-Tees TS21 3FF, UK

^★ Corresponding author; xavier.lopezlopez2@unibo.it

Received: 15 July 2024
Accepted: 6 September 2024

Abstract

Context. Current and future large surveys will produce unprecedented amounts of data. Realistic simulations have become essential for the design and development of these surveys, as well as for the interpretation of the results.

Aims. We present MAMBO, a flexible and efficient workflow to build empirical galaxy and active galactic nucleus (AGN) mock catalogues that reproduce the physical and observational properties of these sources.

Methods. We started with simulated dark matter (DM) haloes, to preserve the link with the cosmic web, and we populated them with galaxies and AGN using abundance matching techniques. We followed an empirical methodology, using stellar mass functions, host galaxy AGN mass functions, and AGN accretion rate distribution functions studied at different redshifts to assign, among other properties, stellar masses, the fraction of quenched galaxies, or the AGN activity (demography, obscuration, multiwavelength emission, etc.).

Results. As a proof test, we applied the method to a Millennium DM lightcone of 3.14 deg2 up to a redshift of z = 10 and down to stellar masses of ℳ ≳ 1075 M_⊙. We show that the AGN population from the mock lightcone presented here reproduces with good accuracy various observables, such as state-of-the-art luminosity functions in the X-ray up to z~7 and in the ultraviolet up to z~5, optical/near-infrared colour-colour diagrams, and narrow emission line diagnostic diagrams. Finally, we demonstrate how this catalogue can be used to make useful predictions for large surveys. Using Euclid as a case example, we compute, among other forecasts, the expected surface densities of galaxies and AGN detectable in the Euclid H_E band. We find that Euclid might observe (on H_E only) about 107 and 8 × 107 type 1 and 2 AGN, respectively, and 2 × 109 galaxies at the end of its 14 679 deg2 Wide survey, in good agreement with other published forecasts.