The VLA Galactic Plane Survey

By J. Stil, A. Taylor, J. Dickey, D. Kavars, P. G. Martin, T. A. Rothwell, A. Boothroyd, F. J. Lockman, N. McClure-Griffiths. 2006

292 citations recorded by the source corpus.

The VLA Galactic Plane Survey (VGPS) is a survey of H I and 21 cm continuum emission in the Galactic plane between longitude 18° and 67° with latitude coverage from |b| < 1.°3 to |b| < 2.°3. The survey area was observed with the Very Large Array in 990 pointings. Short-spacing information for the H I line emission was obtained by additional observations with the Green Bank Telescope. H I spectral line images are presented with a resolution of 1′ × 1′ × 1.56 km s-1 (FWHM) and an rms noise of 2 K per 0.824 km s-1 channel. Continuum images made from channels without H I line emission have 1′ (FWHM) resolution. The VGPS images reveal structures of atomic hydrogen and 21 cm continuum as large as several degrees with unprecedented resolution in this part of the Galaxy. With the completion of the VGPS, it is now possible for the first time to assess the consistency between arcminute-resolution surveys of Galactic H I emission. VGPS images are compared with images from the Canadian Galactic Plane Survey (CGPS) and the Southern Galactic Plane Survey (SGPS). In general, the agreement between these surveys is impressive, considering the differences in instrumentation and image-processing techniques used for each survey. The differences between VGPS and CGPS images are small, ≲6 K (rms) in channels in which the mean H I brightness temperature in the field exceeds 80 K. A similar degree of consistency is found between the VGPS and SGPS. The agreement we find between arcminute-resolution surveys of the Galactic plane is a crucial step toward combining these surveys into a single uniform data set that covers 90% of the Galactic disk: the International Galactic Plane Survey. The VGPS data will be made available on the World Wide Web through the Canadian Astronomy Data Centre.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Star Formation in the Milky Way and Nearby Galaxies (2012, background): “Surveys Recent and ongoing surveys of the Galactic Plane at multiple wavelengths are revitalizing the study of the MW as a galaxy.”
The second epoch Molonglo Galactic Plane Survey: compact source catalogue (2007, background): “It consists of three individual surveys: the Canadian Galactic Plane Survey (CGPS; Taylor et al. 2003), the VLA Galactic Plane Survey (VGPS; Stil et al. 2006) and the Southern Galactic Plane Survey (SGPS; McClure-Griffiths et al. 2005).”
Characterizing precursors to stellar clusters with Herschel (2011, background): “Additionally, this cloud shows no obvious HI self-absorption (Stil et al. 2006).”
The H2O Southern Galactic Plane Survey (HOPS) – I. Techniques and H2O maser data (2011, methodology): “Such surveys, as the International Galactic Plane Survey (Taylor et al. 2003; McClureGriffiths et al. 2005; Stil et al. 2006) in H I, as well as surveys of 12CO (Dame, Hartmann & Thaddeus 2001) and 13CO (Jackson et al. 2006), have been widely used in tracing out Galactic structure and E-mail:…”
A gallery of bubbles. The nature of the bubbles observed by Spitzer and what ATLASGAL tells us about the surrounding neutral material (2010, methodology): “For MAGPIS fields that are too noisy or not sensitive enough, we used the continuum data from the VLA Galactic Plane Survey at 21-cm (VGPS, Stil et al. 2006).”
The H i Distribution of the Milky Way (2009, methodology): “The data quality is excellent, as shown by Stil et al. (2006b) who made a few data checks and intercomparisons.”
THE WISE CATALOG OF GALACTIC H ii REGIONS (2013, background): “Anderson (2010) measured the integrated MIPSGAL flux and 21 cm Very Large Array (VLA) Galactic Plane Survey (VGPS; Stil et al. 2006) continuum emission from a large sample of 301 first quadrant Galactic H ii regions.”
GASS: THE PARKES GALACTIC ALL-SKY SURVEY. I. SURVEY DESCRIPTION, GOALS, AND INITIAL DATA RELEASE (2009, background): “While high angular resolution Galactic Plane surveys (Taylor et al. 2003; McClure-Griffiths et al. 2005; Stil et al. 2006) have allowed us to carefully explore Galactic H i emission in the disk, they are not very sensitive (σ TB ∼ 1 K) and are restricted to a few degrees around the Galactic Plane,…”
THE BOLOCAM GALACTIC PLANE SURVEY: SURVEY DESCRIPTION AND DATA REDUCTION (2010, methodology): “The BGPS maps in the first quadrant overlap with the VLA Galactic Plane Survey (VGPS) in H i and radio continuum (Stil et al. 2006), the Spitzer-GLIMPSE and GLIMPSE-II fields (Benjamin et al. 2003), MIPSGAL (Carey et al. 2009), the BU-FCRAO 13CO J = 1 → 0 Galactic Ring Survey (Jackson et al. 2006),…”
ATLASGAL - properties of a complete sample of Galactic clumps (2017, methodology): “We have extracted HI spectra from the Southern Galactic Plane Survey (SGPS; McClure-Griffiths et al. 2005) and the VLA Galactic Plane Survey (VGPS; Stil et al. 2006) archives towards all ATLASGAL clump.”
KINEMATIC DISTANCES TO MOLECULAR CLOUDS IDENTIFIED IN THE GALACTIC RING SURVEY (2009, methodology): “The HISA analysis was performed using the VGPS (Stil et al. 2006).”
THE GALFA-Hi SURVEY: DATA RELEASE 1 (2011, background): “The International Galactic Plane Survey (IGPS; Taylor et al. 2003, Stil et al. 2006, and McClure-Griffiths et al. 2005) is a compilation of relatively high resolution (∼ 1′) interferometric observations of the Galactic plane.”
A revised catalogue of 294 Galactic supernova remnants (2019, background): “More recently Anderson et al. (2017) have identified many candidate SNRs in the region 17◦.5 < l < 67◦.4, |b| ≤ 1◦.25, from THOR (e.g. Beuther et al. 2016) and VGPS (e.g. Stil et al. 2006) radio continuum observations at 1.4 GHz and mid-IR surveys.”
EMU: Evolutionary Map of the Universe (2011, background): “…cover an area,100 deg2 at an angular resolution of 1–6 arcsec, while the International Galactic Plane Survey consists of a number of studies over several hundred deg2 at a typical resolution of ,1 arcmin (McClure-Griffiths et al. 2005; Taylor et al. 2003; Stil et al. 2006; Haverkorn et al. 2006).”
Molecular Clouds in the Milky Way (2015, methodology): “Most important are the high-resolution interferometric 21-cm surveys that now cover the inner Galaxy in the first quadrant [the Very Large Array (VLA) Galactic Plane Survey or VGPS; Stil et al. 2006] and the fourth quadrant (Southern Galactic Plane Survey or SGPS; McClure-Griffiths et al. 2005).”
A Herschel [C ii] Galactic plane survey - I. The global distribution of ISM gas components (2013, methodology): “We used supplementary H i 21 cm data taken from the Southern Galactic Plane Survey (SGPS; McClure-Griffiths et al. 2005), the Canadian Galactic Plane Survey (CGPS; Taylor et al. 2003), and the VLA Galactic Plane Survey (VGPS; Stil et al. 2006).”
RESOLUTION OF THE DISTANCE AMBIGUITY FOR GALACTIC H ii REGIONS (2008, methodology): “For the H i E/A analysis we use data from the VLA 21 cm H i Galactic Plane Survey (VGPS; Stil et al. 2006).”
THE GREEN BANK TELESCOPE H ii REGION DISCOVERY SURVEY. II. THE SOURCE CATALOG (2011, background): “…list from the following multi-frequency, large solid angle Galac- tic surveys: the NRAO VLA Galactic Plane Survey at 21 cm H I and continuum (VGPS: Stil et al. 2006), the NRAO VLA Sky Survey at 20 cm continuum (NVSS: Condon et al. 1998), the Southern Galactic Plane Survey at 21 cm H I and…”