Deep Extragalactic VIsible Legacy Survey (DEVILS): identification of AGN through SED fitting and the evolution of the bolometric AGN luminosity function

Author:

Thorne Jessica E12ORCID,Robotham Aaron S G12ORCID,Davies Luke J M1ORCID,Bellstedt Sabine1ORCID,Brown Michael J I3ORCID,Croom Scott M24ORCID,Delvecchio Ivan5ORCID,Groves Brent1ORCID,Jarvis Matt J67ORCID,Shabala Stanislav S28ORCID,Seymour Nick9ORCID,Whittam Imogen H67ORCID,Bravo Matias1ORCID,Cook Robin H W1ORCID,Driver Simon P1ORCID,Holwerda Benne10ORCID,Phillipps Steven11ORCID,Siudek Malgorzata1213ORCID

Affiliation:

1. ICRAR, The University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia

2. ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia

3. School of Physics and Astronomy, Monash University, VIC 3800, Australia

4. Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, Sydney, NSW 2006, Australia

5. INAF – Osservatorio Astronomico di Brera, Via Brera 28, 20121 Milano, Italy

6. Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK

7. Department of Physics and Astronomy, University of the Western Cape, Robert Sobukwe Road, Bellville 7535, South Africa

8. School of Natural Sciences, University of Tasmania, Private Bag 37, Hobart, TAS 7001, Australia

9. ICRAR, Curtin University, Bentley, WA 6102, Australia

10. Department of Physics and Astronomy, University of Louisville, 102 Natural Science Building, Louisville, KY 40292, USA

11. Astrophysics Group, School of Physics, University of Bristol, Bristol BS8 1TL, UK

12. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, 08193 Bellaterra, Barcelona, Spain

13. National Centre for Nuclear Research, ul. Pasteura 7, PL-02-093 Warsaw, Poland

Abstract

ABSTRACT Active galactic nuclei (AGN) are typically identified through radio, mid-infrared, or X-ray emission or through the presence of broad and/or narrow emission lines. AGN can also leave an imprint on a galaxy’s spectral energy distribution (SED) through the re-processing of photons by the dusty torus. Using the SED fitting code ProSpect with an incorporated AGN component, we fit the far-ultraviolet to far-infrared SEDs of ∼494 000 galaxies in the D10-COSMOS field and ∼230 000 galaxies from the GAMA survey. By combining an AGN component with a flexible star formation and metallicity implementation, we obtain estimates for the AGN luminosities, stellar masses, star formation histories, and metallicity histories for each of our galaxies. We find that ProSpect can identify AGN components in 91 per cent of galaxies pre-selected as containing AGN through narrow-emission line ratios and the presence of broad lines. Our ProSpect-derived AGN luminosities show close agreement with luminosities derived for X-ray selected AGN using both the X-ray flux and previous SED fitting results. We show that incorporating the flexibility of an AGN component when fitting the SEDs of galaxies with no AGN has no significant impact on the derived galaxy properties. However, in order to obtain accurate estimates of the stellar properties of AGN host galaxies, it is crucial to include an AGN component in the SED fitting process. We use our derived AGN luminosities to map the evolution of the AGN luminosity function for 0 < z < 2 and find good agreement with previous measurements and predictions from theoretical models.

Funder

Australian Research Council

ESO

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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