The Bolocam Northern Galactic Plane Survey



The BGPS has officially been released via IPAC as of June 22, 2009.


The Bolocam Galactic Plane Survey I. Survey Description and Data Reduction ADS arXiv
The Bolocam Galactic Plane Survey II. Catalog of the Image Data arXiv
The Bolocam Galactic Plane Survey III. Characterizing Physical Properties of Massive Star-Forming Regions in the Gemini OB1 Molecular Cloud arXiv
The Bolocam Galactic Plane Survey IV: λ = 1.1 and 0.35 mm Dust Continuum Emission in the Galactic Center Region
The Bolocam Galactic Plane Survey V: HCO+ and N2H+ Spectroscopy of 1.1 mm Dust Continuum Sources
The Bolocam Galactic Plane Survey VI: A Mid-infrared Census of Star Formation Activity in Bolocam Galactic Plane Survey Sources
The Bolocam Galactic Plane Survey. VII. Characterizing the Properties of Massive Star-Forming Regions
The Bolocam Galactic Plane Survey. VIII. A Mid-Infrared Kinematic Distance Discrimination Method
The Bolocam Galactic Plane Survey. IX. Data Release 2 and Outer Galaxy Extension




The Galactic Center as seen by Bolocam (orange), the VLA at 20 GHz (purple), and Spitzer at 8 microns (cyan)






The Bolocam Galactic Plane Survey is a 1.1mm continuum survey of 170 square degrees of the galactic plane visible from the northern hemisphere. It is one of the first large-area, systematic surveys of the Galactic Plane in the millimeter continuum without pre-selected targets. The survey is contiguous over the range -10.5 < l < 90.5, |b| < 0.5. Towards the Cygnus X region, the coverage was flared to |b| < 1.5 over the range 75.5 < l < 87.5. In addition, cross-cuts to |b| < 1.5 were made at l=3,15,30, and 31. The total area covered in the first quadrant is 133 square degrees. Four targeted regions in the outer galaxy were also observed, covering l=111 near NGC 7538, the W3/4/5 complex, IC1396, and the Gem OB1 complex.

The survey has detected approximately 8400 sources to a limiting non-uniform 1-sigma noise level in the range 30 to 60 mJy/beam. The BGPS source catalog (Bolocat) is presented in a paper by Rosolowsky et al. (2010). A custom pipeline was written to reduce the large data set from the BGPS and is described in detail in Aguirre et al., (2011) and in Ginsburg et al (in progress).

Follow-up work is under way to determine radial velocities from which kinematic distances can be determined. Observations in the CS 5-4, HCO+ 3-2, and N2H+ 3-2 transitions have detected a significant fraction of the BGPS sources.







The BGPS team:
John Bally (PI), James Aguirre, Cara Battersby, Eric Todd Bradley,
Richard Chamberlin, Claudia Cyganowski, Darren Dowell, Meredith Drosback,
Neal Evans, Adam Ginsburg, Jason Glenn, Paul Harvey,
Miranda Dunham, Erik Rosolowsky, Wayne Schlingman, Yancy Shirley,
Guy Stringfellow, Josh Walawender, and Jonathan Williams

The Bolocam team:
Peter A.R. Ade, Mihail Amarie, James J. Bock, Samantha F. Edgington,
Jason Glenn, Alexey Goldin, Sunil Golwala, Douglas Haig,
Andrew E. Lange, Glenn Laurent, Philip D. Mauskopf,
Minhee Yun, and Hien Nguyen

The BGPS project is supported by the National Science Foundation through NSF grant AST-0708403. J.A. was supported by a Jansky Fellowship from the National Radio Astronomy Observatory (NRAO). The first observing runs for BGPS were supported by travel funds provided by NRAO. Team support was provided in part by NSF grant AST-0607793 to the University of Texas at Austin. The BGPS is made possible by Bolocam and the Caltech Submillimeter Observatory.
BGPS v2 is coming!