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FältnamnIndikatorerMetadata
00006072naa a2200589 4500
001oai:research.chalmers.se:e8822c61-2cf8-41ca-ac18-0361c8f96ea0
003SwePub
008201107s2020 | |||||||||||000 ||eng|
0247 a https://research.chalmers.se/publication/5201752 URI
0247 a https://doi.org/10.1051/0004-6361/2019367762 DOI
040 a (SwePub)cth
041 a engb eng
042 9 SwePub
072 7a art2 swepub-publicationtype
072 7a ref2 swepub-contenttype
1001 a Ceraj, L.u Sveučilište u Zagrebu,University of Zagreb4 aut
2451 0a The XXL Survey: XLIII. The quasar radio loudness dichotomy exposed via radio luminosity functions obtained by combining results from COSMOS and XXL-S X-ray selected quasars
264 c 2020-10-13
264 1b EDP Sciences,c 2020
338 a electronic2 rdacarrier
520 a We studied a sample of 274 radio and X-ray selected quasars (XQSOs) detected in the COSMOS and XXL-S radio surveys at 3 GHz and 2.1 GHz, respectively. This sample was identified by adopting a conservative threshold in X-ray luminosity, LX [2-10 keV] ≥ 1044 erg s-1, selecting only the most powerful quasars. A number of previous studies on the origin of radio emission in type-1 quasars have focused on the radio loudness distributions, some claiming to have found evidence for bimodality, pointing toward the existence of two physically different mechanisms for the radio emission. Using available multiwavelength data, we examined various criteria for the selection of radio-loud (RL) and radio-quiet (RQ) XQSOs and found that the number of RL/RQ XQSOs changes significantly depending on the chosen criterion. This discrepancy arises due to the different criteria tracing different physical processes and due to the fact that our sample was selected from flux-limited radio and X-ray surveys. Another approach to study the origin of radio emission in XQSOs is via their radio luminosity functions (RLF). We constructed the XQSO 1.4 GHz RLFs in six redshift bins at 0:5 ≤ z ≤ 3:75. The lower-1.4 GHz luminosity end shows a higher normalization than expected only from AGN contribution in all studied redshift bins. We found that the so-called "bump"is mostly dominated by emission due to star-forming processes within the host galaxies of XQSOs. As expected, AGN-related radio emission is the dominant contribution at the higher-luminosity end of RLF. To study the evolution of the XQSO RLF, we used a combination of analytic forms from the literature to constrain the "bump"due to star formation and the higher-luminosity AGN part of the RLF. We defined two 1.4 GHz luminosity thresholds, Lth;SF and Lth;AGN, below and above which more than 80% of sources contributing to the RLF are dominated by star formation and AGN-related activity, respectively. The two thresholds evolve with redshift, which is most likely driven by the strong evolution of star formation rates of the XQSO host galaxies. We found that both the lower and higher luminosity ends evolve significantly in density, while their luminosity evolution parameters are consistent with being constant. We found that the lower-luminosity end evolves both in density and luminosity, while the higher-luminosity end evolves significantly only in density. Our results expose the dichotomy of the origin of radio emission: while the higher-luminosity end of the XQSO RLF is dominated by AGN activity, the lower-luminosity end is dominated by the star formation-related processes.
650 7a NATURVETENSKAPx Kemix Oorganisk kemi0 (SwePub)104042 hsv//swe
650 7a NATURAL SCIENCESx Chemical Sciencesx Inorganic Chemistry0 (SwePub)104042 hsv//eng
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
650 7a NATURVETENSKAPx Fysikx Annan fysik0 (SwePub)103992 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Other Physics Topics0 (SwePub)103992 hsv//eng
653 a Galaxies: high-redshift
653 a Galaxies: evolution
653 a Galaxies: active
653 a Quasars: general
7001 a Smolcic, V.u Sveučilište u Zagrebu,University of Zagreb4 aut
7001 a Delvecchio, I.u Université Paris-Saclay,University Paris-Saclay4 aut
7001 a Butler, A.u University of Western Australia4 aut
7001 a Tisanić, K.u Sveučilište u Zagrebu,University of Zagreb4 aut
7001 a Delhaize, J.u University of Cape Town4 aut
7001 a Horellou, Cathy,d 1967u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)horellou
7001 a Kartaltepe, Jeyhan S.u Rochester Institute of Technology4 aut
7001 a Kolokythas, K.u North-West University4 aut
7001 a Leslie, S.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Marchesi, S.u Clemson University4 aut
7001 a Novak, M.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Pierre, M.u Université Paris-Saclay,University Paris-Saclay4 aut
7001 a Plionis, M.u National Observatory of Athens4 aut
7001 a Vardoulaki, E.u Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)4 aut
7001 a Zamorani, G.u Istituto nazionale di astrofisica (INAF)4 aut
7102 a Sveučilište u Zagrebub Université Paris-Saclay4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 642q 642x 0004-6361x 1432-0746
8564 u https://research.chalmers.se/publication/520175/file/520175_Fulltext.pdfx primaryx freey FULLTEXT
8564 u https://www.aanda.org/articles/aa/pdf/2020/10/aa36776-19.pdf
8564 8u https://research.chalmers.se/publication/520175
8564 8u https://doi.org/10.1051/0004-6361/201936776

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