The Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey

By J. Jackson, J. Rathborne, R. Shah, R. Simon, T. Bania, D. Clemens, E. Chambers, A. Johnson, M. Dormody, R. Lavoie and 1 more. 2005

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The Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey is a new survey of Galactic 13CO J = 1 → 0 emission. The survey used the SEQUOIA multipixel array on the Five College Radio Astronomy Observatory 14 m telescope to cover a longitude range of l = 18°-55.°7 and a latitude range of |b| < 1°, a total of 75.4 deg2. Using both position-switching and On-The-Fly mapping modes, we achieved an angular sampling of 22'', better than half of the telescope's 46'' angular resolution. The survey's velocity coverage is -5 to 135 km s-1 for Galactic longitudes l ≤ 40° and -5 to 85 km s-1 for Galactic longitudes l > 40°. At the velocity resolution of 0.21 km s-1, the typical rms sensitivity is σ(T) ~ 0.13 K. The survey comprises a total of 1,993,522 spectra. We show integrated intensity images (zeroth moment maps), channel maps, position-velocity diagrams, and an average spectrum of the completed survey data set. We also discuss the telescope and instrumental parameters, the observing modes, the data reduction processes, and the emission and noise characteristics of the data set. The Galactic Ring Survey data are available to the community online or in DVD form by request.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/733e01f0fc0a2e25095fabe1f9b9ba0441a708b9

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Citations in the corpus

The RMS survey : Galactic distribution of massive star formation (2013, background): “Similar features have also been reported in the Galactocentric distribution of methanol masers (Green & McClure-Griffiths 2011), H II regions (Paladini, Davies & De Zotti 2004; Anderson & Bania 2009), thermal dust emission (Dunham et al. 2011) and molecular gas (Rathborne et al. 2009).”
The observed spiral structure of the Milky Way (2014, background): “First of all, a large number of new spiral tracers have been Article number, page 1 of 22 detected (e.g., Rathborne et al. 2009; Anderson et al. 2011; Green & McClure-Griffiths 2011; García et al. 2014).”
STAR FORMATION EFFICIENCIES AND LIFETIMES OF GIANT MOLECULAR CLOUDS IN THE MILKY WAY (2010, methodology): “The number of clouds follows a power law with indexα≈ 1.5−1.6 (Casoli et al. 1984; Dame et al. 1986; Digel et al. 1996; Rathborne et al. 2009).”
The H2O Southern Galactic Plane Survey (HOPS) – I. Techniques and H2O maser data (2011, background): “Previous observations of the Galactic plane in continuum (Schuller et al. 2009), thermal line (Dame et al. 2001; Jackson et al. 2006) and methanol maser emission (Walsh et al. 1998; Green et al. 2009) indicate that molecular material is concentrated in a region within about 30◦ in the Galactic…”
RESOLUTION OF THE DISTANCE AMBIGUITY FOR GALACTIC H ii REGIONS (2008, methodology): “◦3) using the BUAO H i survey (Kuchar & Bania 1993) and the Boston University-Five College Radio Astronomy Observatory (BUFCRAO) 13CO Galactic Ring Survey data2 (GRS; Jackson et al. 2006).”
LIFTING THE DUSTY VEIL WITH NEAR- AND MID-INFRARED PHOTOMETRY. I. DESCRIPTION AND APPLICATIONS OF THE RAYLEIGH–JEANS COLOR EXCESS METHOD (2011, methodology): “This publication also makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS).”
THE BOLOCAM GALACTIC PLANE SURVEY: SURVEY DESCRIPTION AND DATA REDUCTION (2010, methodology): “This result is in contrast to CO filling factors which are ∼1 for l 40 (Dame et al. 2001; Jackson et al. 2006).”
Characterizing precursors to stellar clusters with Herschel (2011, background): “The faint decrement at 8 µm can be morphologically matched with a molecular cloud in 13CO (Jackson et al. 2006, from the Galactic Ring Survey) at about 104 km s−1.”
ATLASGAL — towards a complete sample of massive star forming clumps ⋆ (2014, result): “Moore et al. 2012 compared Lbol/M13CO ratios for RMS sources matched with molecular clouds identified by the Galactic Ring Survey (Jackson et al. 2006) and found a ratio for W51 similar to that estimated in this paper from the submillimetre continuum (7.6 ± 2.3 L /M ).”
FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) I: Project Overview and Initial Results (2017, methodology): “The Galactic Ring Survey (GRS) in 13CO (J=1−0) was made with the Five College Radio Astronomy Observatory 14 m telescope (Jackson et al. 2006) and Rathborne et al. (2009) cataloged 829 clouds and 6124 clumps using the data.”
CHEMISTRY IN INFRARED DARK CLOUD CLUMPS: A MOLECULAR LINE SURVEY AT 3 mm (2011, methodology): “They carried out a morphological matching of theMSXmid–infrared extinction with the 13CO J = 1 → 0 molecular line emission from the Boston University-Five College Radio Astronomy Observatory (BU-FCRAO) Galactic Ring Survey (GRS; Jackson et al. 2006).”
Turbulent molecular clouds (2012, background): “Since then, several 12CO(1–0) (May et al. 1988, 1993, Sanders et al. 1986, Clemens et al. 1986) and 13CO(1–0) (Jackson et al. 2006) surveys have further broadened the view of molecular gas and clouds throughout the Galaxy, beyond the neighborhood of star–forming regions.”
PHYSICAL PROPERTIES OF MOLECULAR CLOUDS FOR THE ENTIRE MILKY WAY DISK (2016, methodology): “Their data sets (available in 12CO and in 13CO; Clemens et al. 1986; Sanders et al. 1986; Heyer et al. 1998; Jackson et al. 2006) cover a smaller area on the sky but at higher angular resolution (46”).”
STAR FORMATION IN DISK GALAXIES. I. FORMATION AND EVOLUTION OF GIANT MOLECULAR CLOUDS VIA GRAVITATIONAL INSTABILITY AND CLOUD COLLISIONS (2008, background): “…to smaller scales (∼ 100 pc) we see, based mostly on surveys of CO emission in the Milky 2 Way (Solomon et al. 1987; Dame, Hartmann & Thaddeus 2001; Jackson et al. 2006) that most of the dense, cold, potentially star-forming gas is organized into giant molecular clouds (GMCs) with masses ∼ 106 M⊙…”
THE DARK MOLECULAR GAS (2010, background): “…the Large Magellanic Clouds (LMC; Dufour 1984); the Z ′ = 1.9 case is appropriate for clouds in the Galactic Molecular Ring at a Galactocentric radius of 4.5 kpc (Rathborne et al. 2009), based on an exponential scale length for the metallicity in the Galaxy of HZR = 6.2 kpc (Wolfire et al. 2003).”