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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742881.0, MPI für Astronomie / Publikationen_mpia
Stellar dynamics and star formation histories of z ˜ 1 radio-loud galaxies
Authors:Barišić, I.; van der Wel, A.; Bezanson, R.; Pacifici, C.; Noeske, K.; Muñoz-Mateos, J. C.; Franx, M.; Smolčić, V.; Bell, E. F.; Brammer, G.; Calhau, J.; Chauké, P.; van Dokkum, P. G.; van Houdt, J.; Gallazzi, A.; Labbé, I.; Maseda, M. V.; Muzzin, A.; Sobral, D.; Straatman, C.; Wu, P.-F.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:The Astrophysical Journal
Volume:847
Issue / Number:1
Start Page:id. 72 (9 pp)
Audience:Not Specified
Abstract / Description:We investigate the stellar kinematics and stellar populations of 58 radio-loud galaxies of intermediate luminosities (L 3 GHz > 1023 W Hz-1) at 0.6 < z < 1. This sample is constructed by cross-matching galaxies from the deep VLT/VIMOS LEGA-C spectroscopic survey with the VLA 3 GHz data set. The LEGA-C continuum spectra reveal for the first time stellar velocity dispersions and age indicators of z ˜ 1 radio galaxies. We find that z ˜ 1 radio-loud active galactic nucleus (AGN) occur exclusively in predominantly old galaxies with high velocity dispersions: σ * > 175 km s-1, corresponding to black hole masses in excess of 108 M . Furthermore, we confirm that at a fixed stellar mass the fraction of radio-loud AGN at z ˜ 1 is five to 10 times higher than in the local universe, suggesting that quiescent, massive galaxies at z ˜ 1 switch on as radio AGN on average once every Gyr. Our results strengthen the existing evidence for a link between high black hole masses, radio loudness, and quiescence at z ˜ 1.
Free Keywords:galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: jets; galaxies: star formation
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X
URL:http://adsabs.harvard.edu/abs/2017ApJ...847...72B
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