Sökning: WFRF:(Dye L) > The mean star forma...
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000 | 04272naa a2200613 4500 | |
001 | oai:research.chalmers.se:47ed38e7-365f-49ef-9357-b3b853dfdd3c | |
003 | SwePub | |
008 | 171108s2017 | |||||||||||000 ||eng| | |
024 | 7 | a https://research.chalmers.se/publication/2529952 URI |
024 | 7 | a https://research.chalmers.se/publication/5048252 URI |
024 | 7 | a https://doi.org/10.1093/MNRAS/STX21212 DOI |
024 | 7 | a https://doi.org/10.1093/mnras/stx21212 DOI |
040 | a (SwePub)cth | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a art2 swepub-publicationtype |
072 | 7 | a ref2 swepub-contenttype |
100 | 1 | a Stanley, Flora,d 1990u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)floras |
245 | 1 0 | a The mean star formation rates of unobscured QSOs: searching for evidence of suppressed or enhanced star formation |
264 | c 2017-08-17 | |
264 | 1 | b Oxford University Press (OUP),c 2017 |
338 | a electronic2 rdacarrier | |
520 | a We investigate the mean star formation rates (SFRs) in the host galaxies of similar to 3000 optically selected quasi-stellar objects (QSOs) from the Sloan Digital Sky Survey within the Herschel-ATLAS fields, and a radio-luminous subsample covering the redshift range of z = 0.2-2.5. Using Wide-field Infrared Survey Explorer (WISE) and Herschel photometry (12-500 mu m) we construct composite spectral energy distributions (SEDs) in bins of redshift and active galactic nucleus (AGN) luminosity. We perform SED fitting to measure the mean infrared luminosity due to star formation, removing the contamination from AGN emission. We find that the mean SFRs show a weak positive trend with increasing AGN luminosity. However, we demonstrate that the observed trend could be due to an increase in black hole (BH) mass (and a consequent increase of inferred stellar mass) with increasing AGN luminosity. We compare to a sample of X-ray selected AGN and find that the two populations have consistent mean SFRs when matched in AGN luminosity and redshift. On the basis of the available virial BH masses, and the evolving BH mass to stellar mass relationship, we find that the mean SFRs of our QSO sample are consistent with those of main sequence star-forming galaxies. Similarly the radio-luminous QSOs have mean SFRs that are consistent with both the overall QSO sample and with star-forming galaxies on the main sequence. In conclusion, on average QSOs reside on the main sequence of star-forming galaxies, and the observed positive trend between the mean SFRs and AGN luminosity can be attributed to BH mass and redshift dependencies. | |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
653 | a galaxies: active | |
653 | a galaxies: star formation | |
653 | a galaxies: evolution | |
653 | a quasars: general | |
700 | 1 | a Alexander, D. M.4 aut |
700 | 1 | a Harrison, C. M.4 aut |
700 | 1 | a Rosario, D. J.4 aut |
700 | 1 | a Wang, L.4 aut |
700 | 1 | a Aird, J. A.4 aut |
700 | 1 | a Bourne, N.4 aut |
700 | 1 | a Dunne, L.4 aut |
700 | 1 | a Dye, S.4 aut |
700 | 1 | a Eales, S.4 aut |
700 | 1 | a Knudsen, Kirsten Kraiberg,d 1976u Chalmers tekniska högskola,Chalmers University of Technology4 aut0 (Swepub:cth)kraiberg |
700 | 1 | a Michalowski, M. J.4 aut |
700 | 1 | a Valiante, E.4 aut |
700 | 1 | a De Zotti, G.4 aut |
700 | 1 | a Furlanetto, C.4 aut |
700 | 1 | a Ivison, R. J.4 aut |
700 | 1 | a Maddox, S.4 aut |
700 | 1 | a Smith, M. W. L.4 aut |
710 | 2 | a Chalmers tekniska högskola4 org |
773 | 0 | t Monthly Notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 472:2, s. 2221-2240q 472:2<2221-2240x 0035-8711x 1365-2966 |
856 | 4 | u http://publications.lib.chalmers.se/records/fulltext/252995/local_252995.pdfx primaryx freey FULLTEXT |
856 | 4 | u http://dro.dur.ac.uk/23390/1/23390.pdf |
856 | 4 8 | u https://research.chalmers.se/publication/252995 |
856 | 4 8 | u https://research.chalmers.se/publication/504825 |
856 | 4 8 | u https://doi.org/10.1093/MNRAS/STX2121 |
856 | 4 8 | u https://doi.org/10.1093/mnras/stx2121 |
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