The Bolocam Galactic Plane Survey. XIII. Physical Properties And Mass Functions Of Dense Molecular Cloud Structures

dc.contributor.utaustinauthorEvans, Neal J.en_US
dc.creatorEllsworth-Bowers, Timothy P.en_US
dc.creatorGlenn, Jasonen_US
dc.creatorRiley, Allyssaen_US
dc.creatorRosolowsky, Eriken_US
dc.creatorGinsburg, Adamen_US
dc.creatorEvans, Neal J.en_US
dc.creatorBally, Johnen_US
dc.creatorBattersby, Caraen_US
dc.creatorShirley, Yancy L.en_US
dc.creatorMerello, Manuelen_US
dc.description.abstractWe use the distance probability density function formalism of Ellsworth-Bowers et al. to derive physical properties for the collection of 1,710 Bolocam Galactic Plane Survey (BGPS) version 2 sources with well-constrained distance estimates. To account for Malmquist bias, we estimate that the present sample of BGPS sources is 90% complete above 400 M-circle dot and 50% complete above 70 M-circle dot. The mass distributions for the entire sample and astrophysically motivated subsets are generally fitted well by a lognormal function, with approximately power-law distributions at high mass. Power-law behavior emerges more clearly when the sample population is narrowed in heliocentric distance (power-law index alpha = 2.0 +/- 0.1 for sources nearer than 6.5 kpc and alpha = 1.9 +/- 0.1 for objects between 2 and 10 kpc). The high-mass power-law indices are generally 1.85 <= alpha <= 2.05 for various subsamples of sources, intermediate between that of giant molecular clouds and the stellar initial mass function. The fit to the entire sample yields a high-mass power-law (alpha) over cap = 1.94(-0.10)(+0.34). Physical properties of BGPS sources are consistent with large molecular cloud clumps or small molecular clouds, but the fractal nature of the dense interstellar medium makes it difficult to map observational categories to the dominant physical processes driving the observed structure. The face-on map of the Galactic disk's mass surface density based on BGPS dense molecular cloud structures reveals the high-mass star-forming regions W43, W49, and W51 to be prominent mass concentrations in the first quadrant. Furthermore, we present a 0.25 kpc resolution map of the dense gas mass fraction across the Galactic disk that peaks around 5%.en_US
dc.description.sponsorshipNational Science Foundation AST-1008577, NSF, AST-0708403, AST-0540882, AST-0838261, AST-1109116, NSERC of Canadaen_US
dc.identifier.citationEllsworth-Bowers, Timothy P., Jason Glenn, Allyssa Riley, Erik Rosolowsky, Adam Ginsburg, Neal J. Evans II, John Bally, Cara Battersby, Yancy L. Shirley, and Manuel Merello. "The Bolocam Galactic Plane Survey. XIII. Physical Properties and Mass Functions of Dense Molecular Cloud Structures." The Astrophysical Journal, Vol. 805, No. 2 (Jun., 2015): 157.en_US
dc.relation.ispartofserialAstrophysical Journalen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectgalaxy: structureen_US
dc.subjectism: cloudsen_US
dc.subjectsubmillimeter: ismen_US
dc.subjectstars: formationen_US
dc.subjectstar-forming regionsen_US
dc.subjectdust continuum sourcesen_US
dc.subjectc2d legacy cloudsen_US
dc.subjectnearby galaxiesen_US
dc.subjectdark cloudsen_US
dc.subjectco surveyen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Bolocam Galactic Plane Survey. XIII. Physical Properties And Mass Functions Of Dense Molecular Cloud Structuresen_US

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