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

Journal Article · · Astronomy and Astrophysics
 [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [9];  [10];  [11];  [12];  [13];  [14];  [15];  [15];  [14];  [14];  [16];  [17] more »;  [18];  [19];  [20];  [21];  [14];  [22];  [15];  [15];  [21];  [15];  [15];  [15];  [20];  [15];  [20];  [23];  [15];  [15] « less
  1. Università di Bologna (Italy); Istituto Nazionale di Astrofisica (INAF), San Sebastián (Italy)
  2. Università di Bologna (Italy); Istituto Nazionale di Astrofisica (INAF), Bologna (Italy)
  3. Donostia International Physics Center (DIPC), San Sebastian (Spain); Basque Foundation for Science, Bilbao (Spain). IKERBASQUE
  4. Univ. of Southampton (United Kingdom)
  5. Donostia International Physics Center (DIPC), San Sebastian (Spain)
  6. National Observatory of Athens (Greece); Durham Univ. (United Kingdom)
  7. Ludwig Maximilian Univ. of Munich, Munich (Germany); Max Planck Institute for Astrophysics, Garching (Germany)
  8. National Observatory of Athens (Greece)
  9. International School for Advanced Studies (SISSA), Trieste (Italy)
  10. Instituto de Astrofísica de Canarias, La Laguna (Spain); Univ. of La Laguna, San Cristobal de La Laguna (Spain)
  11. Max Planck Institute for Astrophysics, Garching (Germany); Exzellenzcluster ORIGINS, Garching (Germany)
  12. Donostia International Physics Center (DIPC), San Sebastian (Spain); Barcelona Institute of Science and Technology (BIST), Barcelona (Spain)
  13. Univ. of Sao Paulo (Brazil); Unidad Asociada al CSIC, Teruel (Spain). Centro de Estudios de Física del Cosmos de Aragón (CEFCA)
  14. Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada (Spain)
  15. Unidad Asociada al CSIC, Teruel (Spain). Centro de Estudios de Física del Cosmos de Aragón (CEFCA)
  16. Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada (Spain); Entoto Observatory and Research Center (EORC), Addis Ababa (Ethiopia); Mbarara University of Science and Technology (MUST) (Uganda)
  17. University of the Chinese Academy of Sciences, Beijing (China); Univ. of Sydney, NSW (Australia); Istituto Nazionale di Astrofisica (INAF), Turin (Italy)
  18. Univ. of Sao Paulo (Brazil); Universidade Federal do Rio Grande do Sul (UFRGS), Porto Alegre, RS (Brazil)
  19. Chinese Academy of Sciences (CAS), Shanghai (China). Shanghai Astronomical Observatory
  20. Univ. of Sao Paulo (Brazil)
  21. Observatório Nacional, Rio de Janeiro (Brazil)
  22. Universidade Federal da Bahia, Salvador, BA (Brazil)
  23. Instruments4, La Canada Flintridge, CA (United States)
Studies indicate strong evidence of a scaling relation in the local Universe between the supermassive black hole mass (MBH) 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 (LAGN). 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 MBH. We calculated the BHAR in physical units depending on two radiative efficiency regimes. We find that the Eddington ratios (λEdd) and its popular proxy (LX/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 MBH - M* scaling relation, which can explain the difference between λEdd 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 MBH - 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 MBH - 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.
Research Organization:
US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
Sponsoring Organization:
Marie Sklodowska-Curie Grant; USDOE
Contributing Organization:
Sloan Digital Sky Survey (SDSS)
OSTI ID:
2425350
Journal Information:
Astronomy and Astrophysics, Journal Name: Astronomy and Astrophysics Vol. 672; ISSN 0004-6361
Publisher:
EDP SciencesCopyright Statement
Country of Publication:
United States
Language:
English

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