The VLA Low-Frequency Sky Survey

By A. Cohen, W. Lane, N. Kassim, T. Lazio, W. Cotton, Richard Perley, J. Condon, W. Erickson. 2005

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The VLA Low-frequency Sky Survey (VLSS) has imaged 95% of the 3π sr of sky north of δ = -30° at a frequency of 74 MHz (4 m wavelength). The resolution is 80″ (FWHM) throughout, and the typical rms noise level is ⟨σ⟩ ≈ 0.1 Jy beam-1. The typical point-source detection limit is 0.7 Jy beam-1, and so far nearly 70,000 sources have been cataloged. This survey used the 74 MHz system added to the VLA in 1998. It required new imaging algorithms to remove the large ionospheric distortions at this very low frequency throughout the entire ∼11.9° field of view. This paper describes the observation and data reduction methods used for the VLSS and presents the survey images and source catalog. All of the calibrated images and the source catalog are available from the VLSS Web site for use by the astronomical community.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/15002778629d489117255fd962b7562542b943cc

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Citations in the corpus

The Very Large Array Low-frequency Sky Survey Redux (VLSSr) (2014, methodology): “The reported errors in the catalog also include the errors introduced by the Gaussian fits, described in detail in (Cohen et al. 2007).”
What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample (2009, background): “…(Giovannini & Feretti 2000), three (A85, A133 and A4038) are small scale (a few tens of kpc) relics associated with nearby radio galaxies (e.g Slee et al. 2001a) and one (MKW8) as identified as a possible relic as seen in the VLA Low-Frequency Sky Survey (VLSS) at 74 MHz (Cohen et al. 2007).”
LOFAR 150-MHz observations of the Boötes field: catalogue and source counts (2016, background): “…178, 151, and 151 MHz, respectively (Edge et al. 1959; Bennett 1962; Pilkington & Scott 1965; Gower, Scott & Wills 1967; Hales, Baldwin & Warner 1988; Hales et al. 2007), the UTR-2 sky survey between 10 and 25 MHz (Braude et al. 2002), and the VLSS at 74 MHz (Cohen et al. 2007; Lane et al. 2014).”
wsclean: an implementation of a fast, generic wide-field imager for radio astronomy (2014, methodology): “…Haarlem et al. 2013); the Amsterdam–ASTRON Radio Transients Facility and Analysis Centre (AARTFAAC) project4; The VLA Low-Frequency Sky Survey (VLSS, Cohen et al. 2007); The MeerKAT; and the lowfrequency Phase 1 aperture arrays of the Square-Kilometre Array (SKA), with the full core (3 km) and…”
An Overview of CHIME, the Canadian Hydrogen Intensity Mapping Experiment (2022, methodology): “We construct a model of this sky using catalogs of source spectra measured by the VLA Low-frequency Sky Survey (VLSS; Cohen et al. 2007), the Westerbork Northern Sky Survey (WENSS; Rengelink et al. 1997), the NRAO VLA Sky Survey (NVSS; Condon et al. 1998), and the Green Bank survey (GB6; Gregory et…”
Ionospheric calibration of low frequency radio interferometric observations using the peeling scheme I. Method description and first results (2009, methodology): “In each test case, SPAM is used for ionospheric phase calibration and imaging of a VLSS visibility data set (Cohen et al. 2007), following the steps described in Sect.”
Cosmology at low frequencies: The 21 cm transition and the high-redshift Universe (2006, methodology): “For convenience, a useful conversion between observed angular scale ∆θ and comoving size at z & 10 is rcom ≈ 1.9 ( ∆θ 1′ ) ( 1 + z 10 )0.2 h−1 Mpc. (3) A similar approximation for the relation between observed bandwidth ∆ν and the radial distance is rcom ≈ 1.7 ( ∆ν 0.1 MHz )( 1 + z 10 )1/2 ( Ωmh 2 0”
The LOFAR Two-metre Sky Survey. I. Survey description and preliminary data release (2016, background): “The target data were then phase calibrated with a calibration time interval of 32 seconds against a sky model generated from the VLA Low-Frequency Sky Survey (VLSSr; Lane et al. 2012), Westerbork Northern Sky Survey (WENSS; Rengelink et al. 1997) and the NRAO/VLA Sky Survey (NVSS; Condon et al. 1998”
LOFAR: The LOw-Frequency ARray (2013, methodology): “In order to estimate σc, we first adopt a parameterization for N(S ) determined from the VLSS sky survey at 74 MHz (Cohen et al. 2007; Lane et al. 2012) and given by N(> S ) = A S β ( λ λ0 )αβ = 1.14 S −1.30 ( λ 4 m )0.91 (5) where β represents the intrinsic slope of the underlying source…”
Radio and millimeter continuum surveys and their astrophysical implications (2009, background): “Other large-area, low-frequency surveys: – the VLA Low-Frequency Sky Survey (VLSS; Cohen et al. 2007) is a 74-MHz con- tinuum survey covering the entire sky North of δ = −30◦ to a typical point-source detection limit of 0.7 Jy; 14 – the Cambridge 6C survey at 151 MHz (Hales et al. 1993, and…”
Distant radio galaxies and their environments (2008, background): “The most appropriate surveys are the 74 MHz VLA Low-frequency Sky Survey (VLSS; Cohen et al. 2007) and the 1.”
The GMRT 150 MHz all-sky radio survey - First alternative data release TGSS ADR1 (2016, background): “…low-frequency radio catalogs, namely NVSS at 1400 MHz (Condon et al. 1998), WENSS at 327 MHz (Rengelink et al. 1997), WISH at 352 MHz (De Breuck et al. 2002), VLSSr at 74 MHz (Cohen et al. 2007; Lane et al. 2012, 2014), and SUMSS and MGPS-2 at 843 MHz (Mauch et al. 2003; Murphy et al. 2007).”