Radio Sources and Star Formation in the Local Universe

By J. Condon, W. Cotton, J. Broderick. 2002

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Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4000188a9cd682ee32cb1ebd009dd0a431d3f0ab

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The Very Large Array Low-frequency Sky Survey Redux (VLSSr) (2014, background): “For large N , the uncertainty on the source count is given by σdN = dFi −1 [ N ∑ j=1 ( 1 Amax )2 j ]1/2 (2) (Windhorst et al. 1985; Condon et al. 2002).”
THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, methodology): “…are treated as potential AGN contaminants and thus removed from our sample.32 Studies of the radio luminosity function (e.g. Sadler et al. 2002; Condon et al. 2002) agree that radio- 30 Here the absolute magnitudes were inferred from the observed magnitudes not accounting for dust reddening.”
LARGE AREA SURVEY FOR z = 7 GALAXIES IN SDF AND GOODS-N: IMPLICATIONS FOR GALAXY FORMATION AND COSMIC REIONIZATION (2009, background): “…in various wavelength including Hα (Glazebrook et al. 1999; Tresse et al. 2002; Hanish et al. 2006), midinfrared (Flores et al. 1999; Pérez-González et al. 2005), submm (Barger et al. 2000; Hughes et al. 1998), radio (Condon et al. 2002; Serjeant et al. 2002), and Xray (Georgakakis et al. 2003).”
Radio and millimeter continuum surveys and their astrophysical implications (2009, methodology): “A frequently-used criterion (Condon et al. 2002) is that galaxies with radio to far-IR flux ratio more than three times higher than the mean for star-forming galaxies are classified as AGN-powered.”
DETERMINING STAR FORMATION RATES FOR INFRARED GALAXIES (2008, methodology): “We used primarily radio data from Condon et al. (1996) and Condon et al. (1998), augmented in a few cases by Condon et al. (1983), Condon et al. (1991), Condon et al. (2002), Iono et al. (2005), and Baan & Klöckner (2006).”
The Cosmic Energy Inventory (2004, background): “At close to zero redshift the integral over the luminosity function gives luminosity densities Lg = 1.5 × 10 19W Hz−1 Mpc−3, La = 3.7 × 10 19 W Hz−1 Mpc−3, (112) at 1.4 GHz (Condon et al. 2002).”
The physical properties of star-forming galaxies in the low-redshift universe (2003, background): “It is clear that radio determinations (Haarsma et al. 2000; Condon et al. 2002; Serjeant et al. 2002) typically give the highest estimates, although alternative calibrations might bring these down somewhat (Hopkins et al. 2003).”
RESOLVING THE RADIO SOURCE BACKGROUND: DEEPER UNDERSTANDING THROUGH CONFUSION (2012, background): “…these luminosity functions are similar to more modern luminosity functions in which the FIR/radio correlation and/or optical line spectra are used to distinguish radio sources primarily powered by AGN from those primarily powered by recently formed stars (Condon et al. 2002; Mauch & Sadler 2007).”
A semi-empirical simulation of the extragalactic radio continuum sky for next generation radio telescopes (2008, background): “However, other determinations of the luminosity function with higher degrees of faint end completeness (e.g. Mauch & Sadler 2007, Condon et al. 2002) show instead that theluminosity function just flattens below log L1.”
Spitzer Power-Law Active Galactic Nucleus Candidates in the Chandra Deep Field-North (2007, background): “In the local universe, galaxies with logLradio (W Hz−1)> 23 tend to be AGNdominated (Condon et al. 2002; Yun et al. 2001).”
STAR FORMATION AND DUST OBSCURATION AT z ≈ 2: GALAXIES AT THE DAWN OF DOWNSIZING (2009, background): “In the local Universe it is usually assumed, based on radio luminosity function studies (e.g. Sadler et al. 2002; Condon et al. 2002), that 1.4GHz radio luminosities greater than ≈2×1023 W/Hz are mostly produced by AGNs, while below this luminosity star formation has a dominant role in producing…”
Outflows in Infrared-Luminous Starbursts at z < 0.5. I. Sample, Na I D Spectra, and Profile Fitting (2005, background): “However, Condon et al. (2002) classify it as a starburst on the basis of (1) the radio/FIR flux ratio, (2) the 25 m/60 m flux ratio, and (3) a lack of extended radio structures.”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, methodology): “…Hα: James et al. 2008 Hα: Perez et al. 2003 Hα: Gallego et al. 1995 10 100 Distance [Mpc] 10 -3 10 -2 10 -1 Lo ca l S F R [M y r-1 M pc -3 ] radio: Serjeant et al. 2002 radio: Condon et al. 2002 FIR: Yun et al. 2001 UV+IR: Martin et al. 2005 UV+IR: Bothwell et al. 2011 Cosmic extrapolation FIG.”
Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly (2009, neutral): “…0.0511 0.0022 0.0067 submm Pascale et al. (2009) 0.824 0.239 0.0785 0.0073 0.0086 submm Pascale et al. (2009) 2.281 1.219 0.1104 0.0092 0.0140 submm Pascale et al. (2009) 0.005 0.005 0.0109 0.0007 0.0008 radio Condon et al. (2002); Hopkins (2004) 0.080 0.080 0.0187 0.0035 0.0038 radio Sadler et…”
Radio sources in the 6dFGS: local luminosity functions at 1.4 GHz for star-forming galaxies and radio-loud AGN (2006, methodology): “We have corrected the measured RLF for galaxy clustering at a distance s centred on our own Galaxy using ρP ρ = 1 + 3 3 − γs ( s0 s )γs (4) (Peebles 1980), as discussed by Condon et al. (2002).”