The Structure of Four Molecular Cloud Complexes in the BU-FCRAO Milky Way Galactic Ring Survey

By R. Simon, J. Jackson, D. Clemens, T. Bania, M. Heyer. 2001

195 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/bce9fa62608043c2c1581433fcde6d9660f8c7ab

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In Astronomy and Astrophysics

Citations in the corpus

The Resolved Properties of Extragalactic Giant Molecular Clouds (2008, unknown): “15−0.30 (Simon et al. 2001).”
GLIMPSE. I. An SIRTF Legacy Project to Map the Inner Galaxy (2003, methodology): “…this is a large-scale 13CO J = 1 → 0 molecular line survey of the inner Galaxy between latitudes −1◦ to +1◦ and longitudes 18◦ and 52◦, with an angular resolution of 22′′ and a velocity resolution of 0.3 km s−1 (Simon et al. 2001) It is available through the GRS website: www.bu.edu/grs.”
2MASS wide field extinction maps. I. The Pipe nebula (2006, background): “…of entire Send offprint requests to: M. Lombardi Correspondence to: mlombard@eso.org molecular cloud complexes are now available (Heyer et al. 1998; Simon et al. 2001), maps with sufficient resolution and dynamic range to identify not only dense molecular cores but also their extended environment…”
Interstellar Turbulence I: Observations and Processes (2004, background): “However other surveys using a variety of tracers and scales yield little correlation (e.g., Plume et al. 1997, Kawamura et al. 1998, Peng et al. 1998, Brand et al. 2001, Simon et al. 2001, Tachihara et al. 2002), or yield correlations dominated by scatter (Heyer et al. 2001).”
Molecular Clouds in the Milky Way (2015, methodology): “…when applied to real data, the Larson relationships are not so readily produced by these analyses, as the dynamic range of clump size is typically less than 10 and the scatter of properties is large (Carr 1987, Stutzki & Guesten 1990, Simon et al. 2001, Schneider & Brooks 2004, Wong et al. 2011).”
RESOLUTION OF THE DISTANCE AMBIGUITY FOR GALACTIC H ii REGIONS (2008, methodology): “Using the conversions of Simon et al. (2001): N (H2) = 4.92 × 1020 T13CO Δv 5 × 1020 W13CO, (5) a W13CO value of ∼10 K km s−1 is required to produce measurable H i SA from cold H i in a molecular cloud.”
The Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey (2005, methodology): “This paper describes a catalog of molecular clouds and clumps identified using 13CO data from the GRS which provides a new, homogeneous database for the study of the large- and small-scale structure of molecular gas throughout the inner Milky Way (e.g., Simon et al. 2001).”
Infrared Dark Clouds: Precursors to Star Clusters (2004, unknown): “Within the errors, this power-law index is the same as that for the stellar IMF for high-mass stars (α ∼ 2.35; Salpeter 1955) and also to that of the clump mass spectrum for molecular clouds (α ∼ 1.8; Kramer et al. 1998; Simon et al. 2001).”
A Catalog of Midcourse Space Experiment Infrared Dark Cloud Candidates (2006, background): “0 Galactic Ring Survey data (GRS; Simon et al. 2001; Jackson et al. 2006).”
PHYSICAL PROPERTIES AND GALACTIC DISTRIBUTION OF MOLECULAR CLOUDS IDENTIFIED IN THE GALACTIC RING SURVEY (2010, background): “A mean molecular weight of 2.72 accounts for the presence of both H2 and He (Allen 1973; Simon et al. 2001).”