VERY LARGE ARRAY 1.4 GHz OBSERVATIONS OF THE GOODS-NORTH FIELD: DATA REDUCTION AND ANALYSIS

By G. Morrison, F. Owen, Mark Dickinson, R. Ivison, E. Ibar. 2010

134 citations recorded by the source corpus.

We describe deep, new, wide-field radio continuum observations of the Great Observatories Origins Deep Survey-North field. The resulting map has a synthesized beam size of ∼1.″7 and an rms noise level of ∼3.9 μJy beam−1 near its center and ∼8 μJy beam−1 at 15′ from phase center. We have cataloged 1230 discrete radio emitters, within a 40′ × 40′ region, above a 5σ detection threshold of ∼20 μJy at the field center. New techniques, pioneered by Owen & Morrison, have enabled us to achieve a dynamic range of 6800:1 in a field that has significantly strong confusing sources. We compare the 1.4 GHz (20 cm) source counts with those from other published radio surveys. Our differential counts are nearly Euclidean below 100 μJy with a median source diameter of ∼1.″2. This adds to the evidence presented by Owen & Morrison that the natural confusion limit may lie near 1 μJy. If the Euclidean slope of the counts continues down to the natural confusion limit as an extrapolation of our log N–log S, this indicates that the cutoff must be fairly sharp below 1 μJy else the cosmic microwave background temperature would increase above 2.7 K at 1.4 GHz.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/393cc9015cebaa35356dc9a9c4619f338a8a761e

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Citations in the corpus

GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, methodology): “…correlation: the contribution of old stellar populations to the FIR Taking advantage of the deep 1.4 GHz map available in the GOODS-N field (Morrison et al. 2010), we perform a stacking analysis of the radio continuum in the same bins of mass and redshift as done in the FIRHerschel bands…”
The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, unknown): “…2011), optical (Giavalisco et al. 2004), near-infrared (CANDELS; Grogin et al. 2011), mid-infrared (GOODS-Spitzer; PI: M. Dickinson; see Magnelli et al. 2011), (sub)mm (e.g., Oliver et al. 2012; Borys et al. 2003; Weiß et al. 2009) and radio (Morrison et al. 2010; Miller et al. 2008) observations.”
GOODS-HERSCHEL MEASUREMENTS OF THE DUST ATTENUATION OF TYPICAL STAR-FORMING GALAXIES AT HIGH REDSHIFT: OBSERVATIONS OF ULTRAVIOLET-SELECTED GALAXIES AT z ∼ 2 (2011, methodology): “We supplement these data with deep Very Large Array (VLA) 1.4GHz continuum imaging in the GOODS-North field (Morrison et al. 2010).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “…with the QUIRC camera on the University of Hawaii 2.2 m telescope (Capak et al. 2004), additional mid-IR imaging with Spitzer/IRAC (3.6–8.0µM) from the SEDS program and Spitzer/MIPS (24µm) from the FIDEL survey and deep radio imaging (1.4 GHz) from the Very Large Array (VLA; Morrison et al. 2010).”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, background): “…Photometer for Spitzer (MIPS; Rieke et al. 2004); submillimeter from the Submillimetre Common-User Bolometer Array (SCUBA; Holland et al. 1999) maps of Borys et al. (2003) and Pope et al. (2005); and radio from Very Large Array (VLA) observations taken from an early Morrison et al. (2010) catalog.”
Tracing the molecular gas in distant submillimetre galaxies via CO(1-0) imaging with the EVLA (2010, methodology): “2 The ELAIS N2 continuum image was recreated from the raw data (programmes AI91 and AD432) to avoid the astrometric issue described by Morrison et al. (2010).”
The far-infrared/radio correlation as probed by Herschel (2010, methodology): “GOODS-N has also been observed with the VLA at 1.4 GHz (1.7′′ FWHM – Biggs & Ivison 2006; Morrison et al. 2010) and Spitzer at 24, 70 and 160 μm; we make use of these data, as well as the 850-, 1100- and 1250-μm images of Borys et al. (2003), Perera et al. (2008) and Greve et al. (2008).”
EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, methodology): “Some of the fields from which the samples are drawn have VLA 20 cm radio catalogs from VLA-COSMOS (Schinnerer et al. 2010), AEGIS-20 (Ivison et al. 2007), GOODS-N (Morrison et al. 2010), ECDF-S (Miller et al. 2013), and SXDF (Simpson et al. 2006).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY—THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS, AND MOSAICS (2011, methodology): “For GOODS-North, the astrometry is based on the Subaru/Suprime-Cam R-band imaging (Capak et al. 2004), whose absolute astrometric reference frame has been registered to SDSS, 2MASS, and the new deep VLA 20 cm survey of the field (Morrison et al. 2010).”
EMU: Evolutionary Map of the Universe (2011, background): “…Chandra, COSMOS and Phoenix deep fields (Huynh et al. 2005; Miller et al. 2008; Schinnerer et al. 2007; Hopkins et al. 2003; Biggs & Ivison 2006; Morrison et al. 2010), with a further 7 deg2 expected in the immediate future as part of the ATLAS survey (Norris et al. 2006; Middelberg et al.…”
THE 2 Ms CHANDRA DEEP FIELD-NORTH SURVEY AND THE 250 Ks EXTENDED CHANDRA DEEP FIELD-SOUTH SURVEY: IMPROVED POINT-SOURCE CATALOGS (2016, methodology): “The VLA 1.4 GHz GOODS-N radio catalog (denoted as “VLA”; Morrison et al. 2010), with a 5σ detection threshold of m»20 Jy at the field center.”
THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE z = 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS (2012, background): “Hence, we use a reduced set of priors based primarily on Very Large Array (VLA) radio detections, resulting in flux uncertainties consistent with the confusion noise at the IR wavelengths.”