The miniJPAS survey: AGN and host galaxy coevolution of X-ray-selected sources^⋆

¹ Dipartimento di Fisica e Astronomia “Augusto Righi”, Università di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy
e-mail: ivanezequiel.lopez2@unibo.it
² INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, 40129 Bologna, Italy
³ Donostia International Physics Center (DIPC), Manuel Lardizabal Ibilbidea, 4, Donostia-San, Sebastián, Spain
⁴ IKERBASQUE, Basque Foundation for Science, 48013 Bilbao, Spain
⁵ School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ, UK
⁶ Institute for Astronomy & Astrophysics, National Observatory of Athens, V. Paulou & I. Metaxa, Athens 11532, Greece
⁷ Centre for Extragalactic Astronomy, Department of Physics, Durham University, Durham DH1 3LE, UK
⁸ Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München, Scheinerstr.1, 81679 München, Germany
⁹ Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85741 Garching, Germany
¹⁰ SISSA, Via Bonomea 265, 34136 Trieste, Italy
¹¹ Instituto de Astrofísica de Canarias, Calle Vía Láctea, s/n, 38205 La Laguna, Tenerife, Spain
¹² Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
¹³ Exzellenzcluster ORIGINS, Boltzmannstr. 2, 85748 Garching, Germany
¹⁴ Institut de Física d’Altes Energies, The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra, Barcelona, Spain
¹⁵ Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Rua do Matão, 1226, 05508-090 São Paulo, SP, Brazil
¹⁶ Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Unidad Asociada al CSIC, Plaza San Juan, 1, 44001 Teruel, Spain
¹⁷ Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, 18008 Granada, Spain
¹⁸ Astronomy and Astrophysics Research and Development Department, Entoto Observatory and Research Center (EORC), Space Science and Geospatial Institute (SSGI), PO Box 33679 Addis Ababa, Ethiopia
¹⁹ Physics Department, Faculty of Science, Mbarara University of Science and Technology (MUST), PO Box 1410 Mbarara, Uganda
²⁰ College of Astronomy and Space Sciences, University of the Chinese Academy of Sciences, Beijing 100049, PR China
²¹ Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, Sydney, NSW 2006, Australia
²² INAF – Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy
²³ Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, Rua do Matão, 1371, CEP 05508-090 São Paulo, Brazil
²⁴ Departamento de Astronomia, Instituto de Física, Universidade Federal do Rio Grande do Sul (UFRGS), Av. Bento Gonçalves, 9500 Porto Alegre, RS, Brazil
²⁵ CAS Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, Shanghai 200030, PR China
²⁶ Observatório Nacional, Rua General José Cristino, 77, São Cristóvão, 20921-400 Rio de Janeiro, RJ, Brazil
²⁷ Instituto de Física, Universidade Federal da Bahia, 40210-340 Salvador, BA, Brazil
²⁸ Instruments4, 4121 Pembury Place, La Canada Flintridge, CA 91011, USA

Received: 7 October 2022
Accepted: 31 January 2023

Abstract

Studies indicate strong evidence of a scaling relation in the local Universe between the supermassive black hole mass (M_BH) and the stellar mass of their host galaxies (M_⋆). They even show similar histories across cosmic times of their differential terms: the star formation rate (SFR) and black hole accretion rate (BHAR). However, a clear picture of this coevolution is far from being understood. We selected an X-ray sample of active galactic nuclei (AGN) up to z = 2.5 in the miniJPAS footprint. Their X-ray to infrared spectral energy distributions (SEDs) have been modeled with the CIGALE code, constraining the emission to 68 bands, from which 54 are the narrow filters from the miniJPAS survey. For a final sample of 308 galaxies, we derived their physical properties, such as their M_⋆, SFR, star formation history (SFH), and the luminosity produced by the accretion process of the central BH (L_AGN). For a subsample of 113 sources, we also fit their optical spectra to obtain the gas velocity dispersion from the broad emission lines and estimated the M_BH. We calculated the BHAR in physical units depending on two radiative efficiency regimes. We find that the Eddington ratios (λ_Edd) and its popular proxy (L_X/M_⋆) have a difference of 0.6 dex, on average, and a KS test indicates that they come from different distributions. Our sources exhibit a considerable scatter on the M_BH − M_⋆ scaling relation, which can explain the difference between λ_Edd and its proxy. We also modeled three evolution scenarios for each source to recover the integral properties at z = 0. Using the SFR and BHAR, we show a notable diminution in the scattering between M_BH − M_⋆. For the last scenario, we considered the SFH and a simple energy budget for the AGN accretion, and we retrieved a relation similar to the calibrations known for the local Universe. Our study covers ∼1 deg² in the sky and is sensitive to biases in luminosity. Nevertheless, we show that, for bright sources, the link between the differential values (SFR and BHAR) and their decoupling based on an energy limit is the key that leads to the local M_BH − M_⋆ scaling relation. In the future, we plan to extend this methodology to a thousand degrees of the sky using JPAS with an X-ray selection from eROSITA, to obtain an unbiased distribution of BHAR and Eddington ratios.