The radio-optical correlation in steep-spectrum quasars

Serjeant, S.; Rawlings, Steve; Maddox, S. J.; Baker, Joanne; Clements, D. L.; Lacy, Mark; Lilje, P. B.

doi:10.1046/j.1365-8711.1998.01303.x

Cited by 75 publications

(113 citation statements)

References 42 publications

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“…The result is consistent with other authors (e.g. Rawlings & Saunders 1991;Falcke & Biermann 1995;Serjeant, Rawlings & Maddox 1998;Cao & Jiang 1999;Wang, Luo & Ho 2004;Liu, Jiang & Gu 2006;Xie et al 2007;Ghisellini, Tavecchio & Ghirlanda 2009a;Ghisellini et al 2009bGhisellini et al , 2010Ghisellini et al , 2011Gu, Cao & Jiang 2009;Sbarrato et al 2012). Linear regression is applied to analyze the correlation between broad line luminosity and jet power, and we obtain log LBLR ∼ (0.94 ± 0.12) log Pjet for Fermi blazars and log LBLR ∼ (0.39 ± 0.12) log Pjet for non-Fermi blazars.…”

Section: The Basic Properties Of Fermi Blazarssupporting

confidence: 93%

Basic properties of Fermi blazars and the ‘blazar sequence’

Xiong

Zhang

Bai

et al. 2015

Monthly Notices of the Royal Astronomical Society

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By statistically analyzing a large sample which includes blazars of Fermi detection (FBs) and non-Fermi detection (NFBs), we find that there are significant differences between FBs and NFBs for redshift, black hole mass, jet kinetic power from "cavity" power, broad-line luminosity, and ratio of core luminosity to absolute V-band magnitude (R v ), but not for ratio of radio core to extended flux (R c ) and Eddington ratio. Compared with NFBs, FBs have larger mean jet power, R c and R v while smaller mean redshift, black hole mass, broad-line luminosity. These results support that the beaming effect is main reason for differences between FBs and NFBs, and that FBs are likely to have a more powerful jet. For both Fermi and non-Fermi blazars, there are significant correlations between jet power and the accretion rate (traced by the broad-emission-lines luminosity), between jet power and black hole mass; for Fermi blazars, the black hole mass does not have significant influence on jet power while for non-Fermi blazars, both accretion rate and black hole mass have contributions to the jet power. Our results support the "blazar sequence" and show that synchrotron peak frequency (ν peak ) is associated with accretion rate but not with black hole mass.

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Section: The Basic Properties Of Fermi Blazarssupporting

confidence: 93%

Basic properties of Fermi blazars and the ‘blazar sequence’

Xiong

Zhang

Bai

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…A positive correlation between the radio and optical luminosities of SSQs is observed, confirming a result of Serjeant et al (1998). We are able to rule out this correlation being due to selection effects or biases in our combined sample.…”

Section: Introductionsupporting

confidence: 84%

“…The z-dependence of the RLF follows a one-tailed gaussian which peaks at z = 1.7 ± 0.2. We find no evidence for a decline in the co-moving space density of RLQs at higher redshifts.A positive correlation between the radio and optical luminosities of SSQs is observed, confirming a result of Serjeant et al (1998). We are able to rule out this correlation being due to selection effects or biases in our combined sample.…”

supporting

confidence: 84%

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The radio luminosity function of radio-loud quasars from the 7C Redshift Survey

Rawlings

Blundell

Lacy

1998

Monthly Notices of the Royal Astronomical Society

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We present a complete sample of 24 radio-loud quasars (RLQs) from the new 7C Redshift Survey. Every quasar with a low-frequency (151 MHz) radio flux-density S 151 > 0.5 Jy in two regions of the sky covering 0.013 sr is included; 23 of these have sufficient extended flux to meet the selection criteria, 18 of these have steep radio spectra (hereafter denoted as SSQs). The key advantage of this sample over most samples of RLQs is the lack of an optical magnitude limit. By combining the 7C and 3CRR samples, we have investigated the properties of RLQs as a function of redshift z and radio luminosity L 151 .We derive the radio luminosity function (RLF) of RLQs and find that the data are well fitted by a single power-law with slope α 1 = 1.9 ± 0.1 (for H • = 50 km s −1 Mpc −1 , Ω M = 1, Ω Λ = 0). We find that there must be a break in the RLQ RLF at log 10 (L 151 / W Hz −1 sr −1 ) < ∼ 27, in order for the models to be consistent with the 7C and 6C source counts. The z-dependence of the RLF follows a one-tailed gaussian which peaks at z = 1.7 ± 0.2. We find no evidence for a decline in the co-moving space density of RLQs at higher redshifts.A positive correlation between the radio and optical luminosities of SSQs is observed, confirming a result of Serjeant et al. (1998). We are able to rule out this correlation being due to selection effects or biases in our combined sample. The radiooptical correlation and best-fit model RLF enable us to estimate the distribution of optical magnitudes of quasars in samples selected at low radio frequencies. We conclude that for samples with S 151 < ∼ 1 Jy one must use optical data significantly deeper than the POSS-I limit (R ≈ 20), in order to avoid severe incompleteness.

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“…This type of relation between galaxy mass and radio power is also found to exist in high-redshift quasars (Browne & Murphy 1987;Carballo et al 1998;Serjeant et al 1998;Willott et al 1998;Sánchez & González-Serrano 2003) and in radio galaxies (Yates et al 1986;van Velzen et al 2015). Galaxies have to be massive enough to be powerful radio sources.…”

Section: Relation Between Radio Power and Host Galaxy Properties 43mentioning

confidence: 69%

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Vaddi

O’Dea

Baum

et al. 2016

ApJ

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We address the relation between star formation and active galactic nucleus (AGN) activity in a sample of 231 nearby (0.0002 < z < 0.0358) early-type galaxies by carrying out a multi-wavelength study using archival observations in the UV, IR, and radio. Our results indicate that early-type galaxies in the current epoch are rarely powerful AGNs, with P 10 WHz 22 1 < -for a majority of the galaxies. Only massive galaxies are capable of hosting powerful radio sources while less massive galaxies are hosts to lower radio power sources. Evidence of ongoing star formation is seen in approximately 7% of the sample. The star formation rate (SFR) of these galaxies is less than 0.1 M e yr −1 . They also tend to be radio faint (P 10 WHzThere is a nearly equal fraction of star-forming galaxies in radio faint (P 10 WHz 22 1 < -) and radio bright galaxies (P 10 WHz 22 1  -) suggesting that both star formation and radio mode feedback are constrained to be very low in our sample. We notice that our galaxy sample and the Brightest Cluster Galaxies follow similar trends in radio power versus SFR. This may be produced if both radio power and SFR are related to stellar mass.

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The radio-optical correlation in steep-spectrum quasars

Cited by 75 publications

References 42 publications

Basic properties of Fermi blazars and the ‘blazar sequence’

Basic properties of Fermi blazars and the ‘blazar sequence’

The radio luminosity function of radio-loud quasars from the 7C Redshift Survey

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

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