4.6 Article

The bright end of the infrared luminosity functions and the abundance of hyperluminous infrared galaxies

Journal

ASTRONOMY & ASTROPHYSICS
Volume 648, Issue -, Pages -

Publisher

EDP SCIENCES S A
DOI: 10.1051/0004-6361/202038811

Keywords

galaxies: abundances; galaxies: high-redshift; infrared: galaxies; radio continuum: galaxies; galaxies: luminosity function; mass function; galaxies: evolution

Funding

  1. Center for Information Technology of the University of Groningen
  2. UK Science and Technology Facilities Council [ST/R000905/1]
  3. National Science Centre [UMO-2018/30/E/ST9/00082]
  4. STFC [ST/P000096/1, ST/R505146/1]
  5. Science and Technology Facilities Council (STFC) [ST/R504737/1]
  6. INAF under PRIN SKA/CTA FORECaST
  7. Ministero degli Affari Esteri della Cooperazione Internazionale - Direzione Generale per la Promozione del Sistema Paese Progetto di Grande Rilevanza [ZA18GR02]
  8. INAF under the SKA/CTA PRINFORECaST project
  9. INAF under PRIN MAIN STREAM SAuROS project
  10. UK STFC [ST/R000972/1]
  11. Italian Ministry of Foreign Affairs and International Cooperation (MAECI) [ZA18GR02]
  12. South African Department of Science and Technology's National Research Foundation (DST-NRF), ISARP RADIOSKY2020 Joint Research Scheme [113121]
  13. European Commission Research Executive Agency [FP7-SPACE-2013-1, 607254]
  14. CNRS-INSU, France
  15. Observatoire de Paris, France
  16. Universite d'Orleans, France
  17. BMBF, Germany
  18. MIWF-NRW, Germany
  19. MPG, Germany
  20. Science Foundation Ireland (SFI), Department of Business, Enterprise and Innovation (DBEI), Ireland
  21. NWO, The Netherlands
  22. The Science and Technology Facilities Council, UK
  23. Ministry of Science and Higher Education, Poland
  24. Gauss Centre for Supercomputing e.V through the John von Neumann Institute for Computing (NIC) [CHTB00]
  25. SURF Cooperative [e-infra 180169]
  26. LOFAR e-infra group
  27. STFC [ST/R000972/1] Funding Source: UKRI

Ask authors/readers for more resources

By cross-matching Herschel sources and LOFAR sources, this study provides the most accurate estimate to date of the bright end of the infrared luminosity functions and the abundance of hyperluminous IR galaxies with IR luminosities >10(13)L(circle dot). The results show a good agreement with previous studies and indicate that the population of HLIRGs has surface densities with variations due to a combination of the applied flux limit and cosmic variance.
Aims. We provide the most accurate estimate yet of the bright end of the infrared (IR) luminosity functions (LFs) and the abundance of hyperluminous IR galaxies (HLIRGs) with IR luminosities >10(13)L(circle dot), thanks to the combination of the high sensitivity, angular resolution, and large area of the LOFAR Deep Fields, which probes an unprecedented dynamic range of luminosity and volume.Methods. We cross-match Herschel sources and LOFAR sources in Bootes (8.63 deg(2)), Lockman Hole (10.28 deg(2)), and ELAIS-N1 (6.74 deg(2)) with rms sensitivities of similar to 32, 22, and 20 mu Jy beam(-1), respectively. We divide the matched samples into unique and multiple categories. For the multiple matches, we de-blend the Herschel fluxes using the LOFAR positions and the 150-MHz flux densities as priors. We perform spectral energy distribution fitting, combined with multi-wavelength counterpart identifications and photometric redshift estimates, to derive IR luminosities.Results. The depth of the LOFAR data allows us to identify highly complete (similar to 92% completeness) samples of bright Herschel sources with a simple selection based on the 250 mu m flux density (45, 40, and 35 mJy in Bootes, Lockman Hole, and ELAIS-N1, respectively). Most of the bright Herschel sources fall into the unique category (i.e. a single LOFAR counterpart). For the multiple matches, there is excellent correspondence between the radio emission and the far-IR emission. We find a good agreement in the IR LFs with a previous study out to z similar to 6 which used de-blended Herschel data. Our sample gives the strongest and cleanest indication to date that the population of HLIRGs has surface densities of similar to 5 to similar to 18/deg(2) (with variations due to a combination of the applied flux limit and cosmic variance) and an uncertainty of a factor of less than or similar to 2. In comparison, the GALFORM semi-analytic model significantly under-predicts the abundance of HLIRGs.

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