The VLA Low-frequency Sky Survey

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dc.creatorCohen, A. S.
dc.creatorLane, W. M.
dc.creatorCotton, W. D.
dc.creatorKassim, N. E.
dc.creatorLazio, T. J. W.
dc.creatorPerley, R. A.
dc.creatorCondon, J. J.
dc.creatorErickson, W. C.
dc.date2007-06-08
dc.date.accessioned2026-07-07T11:16:43Z
dc.date.available2026-07-07T11:16:43Z
dc.descriptionThe Very Large Array (VLA) Low-frequency Sky Survey (VLSS) has imaged 95% of the 3*pi sr of sky north of declination = -30 degrees at a frequency of 74 MHz (4 meter wavelength). The resolution is 80" (FWHM) throughout, and the typical RMS noise level is ~0.1 Jy/beam. The typical point-source detection limit is 0.7 Jy/beam and so far nearly 70,000 sources have been catalogued. 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 degree 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 online (http://lwa.nrl.navy.mil/VLSS) for use by the astronomical community.
dc.description53 pages, including 3 tables and 15 figures. Has been accepted for publication in the Astronomical Journal
dc.identifierhttps://arxiv.org/abs/0706.1191
dc.identifierhttp://arxiv.org/abs/0706.1191
dc.identifierAstron.J.134:1245-1262,2007
dc.identifierdoi:10.1086/520719
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/192769
dc.subjectAstrophysics
dc.titleThe VLA Low-frequency Sky Survey
dc.typetext

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