2021/02/28 by Yjan A. Gordon, Michelle M. Boyce, Christopher P. O’Dea +9 · 213 citations
Physics and Astronomy · #Angular resolution (graph drawing) #Astronomy and Astrophysical Research #Footprint #Galaxies: Formation, Evolution, Phenomena #LOFAR #Point source #Radio Astronomy Observations and Technology #Radio astronomy #Radio telescope #Sky #astro-ph.GA #astro-ph.HE #astro-ph.IM
paper · pdf · doi:10.3847/1538-4365/ac05c0
published in The Astrophysical Journal Supplement Series 255(2), 30 (Institute of Physics) · Accepted for publication in ApJS; 23 pages, 18 figures, 4 tables. Revised version includes new flux calibration (section 3.2) that results in VLASS fluxes being scaled by 15% in the presented analyses rather than the 10% used in the earlier version. Associated VLASS catalog data available at https://cirada.ca/catalogues
openalex created_date 2021/03/01 · arxiv created 2021/05/25 · openalex publication_date 2021/08/01 · arxiv updated 2021/08/25 · openalex updated_date 2026/08/05
Abstract The Very Large Array Sky Survey (VLASS) is observing the entire sky north of −40° in the S band (2 GHz < ν < 4 GHz), with the highest angular resolution (2.″5) of any all-sky radio continuum survey to date. VLASS will cover its entire footprint over three distinct epochs, the first of which has now been observed in full. Based on Quick Look images from this first epoch, we have created a catalog of 1.9 × 10 6 reliably detected radio components. Due to the limitations of the Quick Look images, component flux densities are underestimated by ∼15% at S peak > 3 mJy beam −1 and are often unreliable for fainter components. We use this catalog to perform statistical analyses of the ν ∼ 3 GHz radio sky. Comparisons with the Faint Images of the Radio Sky at Twenty-Centimeters (FIRST) survey show the typical 1.4–3 GHz spectral index, α , to be ∼−0.71. The radio color–color distribution of point and extended components is explored by matching with FIRST and the LOFAR Two-meter Sky Survey. We present the VLASS source counts, dN / dS , which are found to be consistent with previous observations at 1.4 and 3 GHz. Resolution improvements over FIRST result in excess power in the VLASS two-point correlation function at angular scales ≲7″, and in 18% of active galactic nuclei associated with a single FIRST component being split into multicomponent sources by VLASS.