A sample of radio-loud active galactic nuclei in the Sloan Digital Sky Survey

By P. Best, G. Kauffmann, T. Heckman, Željko Ivezic´. 2005

233 citations recorded by the source corpus.

A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9 per cent reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000-A break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5 mJy at 1.4 GHz. A full catalogue of positions and radio properties is provided for these sources. The local radio luminosity function is then derived both for radio-loud AGN and for star-forming galaxies and is found to be in agreement with previous studies. By using the radio to far-infrared (FIR) correlation, the radio luminosity function of star-forming galaxies is also compared to the luminosity function derived in the FIR. It is found to agree well at high luminosities but less so at lower luminosities, confirming that the linearity of the radio to FIR correlation breaks down below about 10 22 W Hz -1 at 1.4GHz.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

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Citations in the corpus

A UNIFIED CATALOG OF RADIO OBJECTS DETECTED BY NVSS, FIRST, WENSS, GB6, AND SDSS (2008, methodology): “Best et al. (2005) crosscorrelated the SDSS spectroscopic galaxies sample with both FIRST and NVSS, and found that AGN dominate radio counts down to 5 mJy at 20 cm.”
The Relationship of Hard X-Ray and Optical Line Emission in Low-Redshift Active Galactic Nuclei (2005, background): “For example, radio-selected AGNs in the SDSS are associated with a very different population (themost massive black holes and giant elliptical galaxies; Best et al. 2005a, 2005b).”
On the prevalence of radio‐loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows (2006, methodology): “Best et al. (2005b) identified the radio-emitting galaxies within the main spectroscopic sample of the SDSS DR2, by cross-comparing C© 2007 The Authors.”
How special are Brightest Group and Cluster Galaxies (2006, methodology): “Best et al. (2005a) identified the radio–emitting galaxies within the main spectroscopic sample of the SDSS DR2, by cross–comparing these galaxies with a combination of the National Radio Astronomy Observatory (NRAO) Very Large Array (VLA) Sky Survey (NVSS; Condon et al. 1998) and the Faint Images…”
Radio sources in the 6dFGS: local luminosity functions at 1.4 GHz for star-forming galaxies and radio-loud AGN (2006, methodology): “More recently Best et al. (2005a) used the SDSS–NVSS/FIRST sample of 2215 galaxies to calculate accurate bivariate radio luminosity-mass functions, from both host-galaxy mass and black hole mass.”
Radio and millimeter continuum surveys and their astrophysical implications (2009, methodology): “Spectacular progress has been recently achieved combining large-area spectroscopic surveys (Las Campanas, SDSS, 2dF and 6dF) with the NVSS and FIRST surveys (Machalski & Godlowski 2000; Magliocchetti et al. 2002; Sadler et al. 2002; Best et al. 2005; Mauch & Sadler 2007).”
Predicting dust extinction from the stellar mass of a galaxy (2010, methodology): “Journal compilation C© 2010 RAS, MNRAS 409, 421–432 Downloaded from https://academic.oup.com/mnras/article-abstract/409/1/421/1026333 by guest on 26 July 2018 described in Best et al. (2005).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, methodology): “…such as the 1.4 GHz National Radio Astronomy Observatory (NRAO) VLA Sky Survey (NVSS; Condon et al. 1998) by Sadler et al. (2002) and Mauch & Sadler (2007) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST; Becker et al. 1995) survey by Best et al. (2005) and Best & Heckman (2012).”
The faint radio sky: radio astronomy becomes mainstream (2016, methodology): “4 G H z/M plane Best et al. (2005a) used the location of sources on the D4000 − P1.4 GHz/M plane, where D4000 is the strength of the 4000 Å break (a proxy for the mean stellar age of a galaxy) to separate SFGs from RL AGN. As for the FIR–radio correlation, this method singles out “radio excess” sour”
Grand unification of AGN activity in the ΛCDM cosmology (2009, background): “12 we show the predictions of the BZ jet model for the radio luminosity function in both the prolonged and chaotic acretion cases and compare with the estimates from the Two-degreeField Galaxy Redshift Survey (2dFGRS; Sadler et al. 2002) and from the SDSS (Best et al. 2005)5.”
AGN-controlled cooling in elliptical galaxies (2006, methodology): “Best et al. (2005a) found that the occurrence of low luminosity radio–loud AGN activity was completely independent of that of optical (emission–line)AGN activity, and therefore argued that radio–loud AGN were fuelled by the accretion of hot gas (as opposed to the cold gas which fuels optical AGN…”
On the fundamental dichotomy in the local radio-AGN population (2012, methodology): “These galaxies were cross-matched with the NVSS and FIRST radio sources following the method of Best et al. (2005a), but adopting the improvement described by Donoso et al. (2009) for identification of sources without FIRST counterparts.”