black hole physics; catalogs; galaxies: active; galaxies: nuclei; quasars: supermassive black holes; surveys; Active galactic nuclei; Black Hole physics; Catalog; Galaxies active; Galaxies:Nuclei; Optical-; Quasar: supermassive black hole; Spectral energy distribution; Supermassive black holes; X-ray emission; Astronomy and Astrophysics; Space and Planetary Science
Abstract :
[en] We present one of the largest multiwavelength studies of simultaneous optical-to-X-ray spectral energy distributions (SEDs) of unobscured (NH < 1022 cm−2) active galactic nuclei (AGN) in the local Universe. Using a representative sample of hard-X-ray-selected AGN from the 70-month Swift/BAT catalog, with optical/UV photometric data from Swift/UVOT and X-ray spectral data from Swift/XRT, we constructed broadband SEDs of 236 nearby AGN (0.001 < z < 0.3). We employed GALFIT to estimate host galaxy contamination in the optical/UV and determine the intrinsic AGN fluxes. We used an absorbed power law with a reflection component to model the X-ray spectra and a dust-reddened multi-temperature blackbody to fit the optical/UV SED. We calculated intrinsic luminosities at multiple wavelengths, total bolometric luminosities (Lbol), optical-to-X-ray spectral indices (αox), and multiple bolometric corrections (κλ) in the optical, UV, and X-rays. We used black hole masses obtained by reverberation mapping and the virial method to estimate Eddington ratios (λEdd) for all our AGN. We confirm the tight correlation (scatter = 0.45 dex) between UV (2500 Å) and X-ray (2 keV) luminosity for our sample. We observe a significant decrease in αox with Lbol and λEdd, suggesting that brighter sources emit more UV photons per X-rays. We report a second-order regression relation (scatter = 0.15 dex) between the 2–10 keV bolometric correction (κ2−10) and αox, which is useful to compute Lbol in the absence of multiband SEDs. We also investigate the dependence of optical/UV bolometric corrections on the physical properties of AGN and obtain a significant increase in the UV bolometric corrections (κW2 and κM2) with Lbol and λEdd, unlike those in the optical (κV and κB), which are constant across five orders of Lbol and λEdd. We obtain significant dispersions (∼0.1–1 dex) in all bolometric corrections, and hence recommend using appropriate relations with observed quantities while including the reported scatter, instead of their median values.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Gupta, Kriti Kamal ; Université de Liège - ULiège > Unités de recherche interfacultaires > Space sciences, Technologies and Astrophysics Research (STAR) ; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Santiago, Chile ; Sterrenkundig Observatorium, Universiteit Gent, Gent, Belgium
Ricci, Claudio ; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Santiago, Chile ; Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China
Temple, Matthew J. ; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Santiago, Chile
Tortosa, Alessia ; INAF – Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy
Koss, Michael J. ; Eureka Scientific, Oakland, United States ; Space Science Institute, Boulder, United States
Assef, Roberto J.; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Santiago, Chile
Bauer, Franz E.; Instituto de Astrofísica, Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, Campus San Joaquin, Santiago, Chile ; Millennium Institute of Astrophysics, Santiago, Chile
Mushotzy, Richard ; Department of Astronomy, Joint Space-Science Institute, University of Maryland, College Park, United States
Ricci, Federica; INAF – Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy ; Dipartimento di Matematica e Fisica, Universita Roma Tre, Roma, Italy
Ueda, Yoshihiro; Department of Astronomy, Kyoto University, Kyoto, Japan
Rojas, Alejandra F. ; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Santiago, Chile ; Centro de Astronomía (CITEVA), Universidad de Antofagasta, Antofagasta, Chile
Trakhtenbrot, Benny ; School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
Chang, Chin-Shin; Joint ALMA Observatory, Santiago, Chile
Oh, Kyuseok; Korea Astronomy & Space Science institute, Daejeon, South Korea
Li, Ruancun; Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China ; Department of Earth and Space Science, Graduate School of Science, Osaka University, Osaka, Japan
Kawamuro, Taiki ; 6 RIKEN Cluster for Pioneering Research, Wako, Japan
Diaz, Yaherlyn ; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Santiago, Chile
Powell, Meredith C. ; Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, United States ; Department of Physics, Stanford University, Stanford, United States
Stern, Daniel; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, United States
Urry, C. Megan ; Yale Center for Astronomy & Astrophysics, Physics Department, New Haven, United States
Harrison, Fiona; Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, United States
Cenko, Brad ; Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, United States
We would like to thank the anonymous referee for their useful suggestions that helped improve this manuscript. This work made use of data from the NASA/IPAC Infrared Science Archive and NASA/IPAC Extragalactic Database (NED), which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research also made use of photutils , an Astropy package for the detection and photometry of astronomical sources (Bradley et al. 2021). We acknowledge financial support from: a 2018 grant from the ESO-Government of Chile Joint Committee (KKG); the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Programme of the European Space Agency (KKG); ANID CATA-BASAL project FB210003 (CR, RJA, FEB); ANID FONDECYT Regular grant #1230345 (CR), #1231718 (RJA), and #1200495 (FEB); NASA ADAP award 80NSSC19K0749 (MJK); ANID Millennium Science Initiative Program - ICN12_009 (FEB); ANID FONDECYT Postdoctorado grant #3220516 (MJT), #3210157 (AFR), and #3230310 (YD); the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation program, grant agreement #950533 (BT); the Israel Science Foundation, grant #1849/19 (BT); the Korea Astronomy and Space Science Institute under the R&D program supervised by the Ministry of Science and ICT, Project #2024-1-831-01 (KO); the National Research Foundation of Korea, NRF-2020R1C1C1005462 (KO).We would like to thank the anonymous referee for their useful suggestions that helped improve this manuscript. This work made use of data from the NASA/IPAC Infrared Science Archive and NASA/IPAC Extragalactic Database (NED), which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research also made use of photutils, an Astropy package for the detection and photometry of astronomical sources (Bradley et al. 2021). We acknowledge financial support from: a 2018 grant from the ESO-Government of Chile Joint Committee (KKG); the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Pro-gramme of the European Space Agency (KKG); ANID CATA-BASAL project FB210003 (CR, RJA, FEB); ANID FONDECYT Regular grant #1230345 (CR), #1231718 (RJA), and #1200495 (FEB); NASA ADAP award 80NSSC19K0749 (MJK); ANID Millennium Science Initiative Program - ICN12_009 (FEB); ANID FONDECYT Postdoctorado grant #3220516 (MJT), #3210157 (AFR), and #3230310 (YD); the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation program, grant agreement #950533 (BT); the Israel Science Foundation, grant #1849/19 (BT); the Korea Astronomy and Space Science Institute under the R&D program supervised by the Ministry of Science and ICT, Project #2024-1-831-01 (KO); the National Research Foundation of Korea, NRF-2020R1C1C1005462 (KO).
