The Bolocam Galactic Plane Survey (BGPS) is a 1.1 mm continuum survey of the Galactic Plane made using Bolocam on the Caltech Submillimeter Observatory. Millimeter-wavelength thermal dust emission reveals the repositories of the densest molecular gas, ranging in scale from cores to whole clouds. By pinpointing these regions, the connection of this gas to nascent and ongoing star formation may be explored. The BGPS coverage totals 170 square degrees (with 33" FWHM effective resolution). The survey is contiguous over the range -10.5 ≤ l ≤ 90.5, |b| ≤ 0.5. Towards the Cygnus X spiral arm, the coverage was flared to |b| ≤ 1.5 for 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 of this section is 133 square degrees. With the exception of the increase in latitude, no pre-selection criteria were applied to the coverage in this region. In addition to the contiguous region, four targeted regions in the outer Galaxy were observed: IC1396 (9 square degrees, 97.5 ≤ l ≤ 100.5, 2.25 ≤ l ≤ 5.25), a region towards the Perseus Arm (4 square degrees centered on l = 111, b=0 near NGC7538), W3/4/5 (18 square degrees, 132.5 ≤ l ≤ 138.5) and Gem OB1 (6 square degrees, 187.5 ≤ l ≤ 193.5). The survey has detected approximately 8,400 sources, to an rms noise level in the maps ranging from 30 to 60 mJy beam-1. The BGPS survey and catalog provide an important database for sub/millimeter observations with the Herschel Space Observatory, ALMA, SCUBA-2, APEX, and others.
The BOLOCAM GPS coverage is overlayed on the all-sky ISSA image above. Data from the v1 release are shown in blue, additional data from the v2 release are shown in red. You can get cutouts of BOLOCAM mosaics by clicking on any area on the above image, or by typing a coordinate below.
Use the search form below to request data - search results will show cutout images of the requested search size. Use Catalog Search to perform advanced searching on the BOLOCAM GPS catalog. To bypass searching and go directly to the data download locations, follow these links for images and catalogs.
The Version 2.1 release (hereafter v2) of the BGPS data includes images and a catalog. It is described in Ginsburg et al (2013).
The new images have improved fidelity and more uniform noise. The fields include all those in the original v1 release and some new data. There are new fields included in the BGPS v2 release, primarily in the outer galaxy but including some expansions in the inner galaxy. These include M17, IRAS 22172, a significant expansion in l and b around the l=110 region, Mon R2, NGC 2264, parts of the Orion A and B clouds, Sharpless 235, and scattered IRAS+CO selected fields at longitude 119, 123, 126, 129, 154, 169, 181, 182, 195, 201, and 217. IRSA provides a coverage map.
There is a new catalog associated with the v2 images. The sources were extracted using Bolocat with parameters set in the same way as for the v1 catalog. There are many sources in v1 that are not in v2 and vice-versa. These discrepancies occur primarily for faint sources with low signal-to-noise. Objects in both catalogs are likely to be real since catalog parameters were selected to minimize false positives. Changing the quality of the images and the structure of the noise highlights some new objects and obscures others. The v2 catalog has about a 75% overlap with the v1 catalog. The differences are explored in more detail in Ginsburg et al (2013).
The flux calibration offset identified in the version 1 data is now understood. The version 2 data are brighter, on average, by approximately a factor 1.5, but the factor varies from source to source. The v2 catalog should be used instead of the v1 catalog. The source of the error was the incorrect application of a flux calibration solution.
Contreras (2013) noted a 4.7 arcsecond offset between the BGPS v1 catalog and the ATLASGAL catalog. We believe this is caused by an offset of that magnitude (~3-4 arcseconds) in a few fields that have an inordinate number of sources extracted; the pointing accuracy in the vast majority of the BGPS fields, based on a comparison to Herschel Hi-Gal images, is better than 4 arcseconds, but the mean offset is within 2 arcseconds of zero.
For full details about the BGPS version 1 data, please see the BGPS v1 Documentation. The BGPS data pipeline is available online at
The Caltech Submillimeter Observatory is operated by Caltech under a contract from the NSF. We would like to acknowledge the staff and day crew of the CSO for their assistance over the many years of this project.

The BGPS team:

James Aguirre, John Bally, Cara Battersby, Eric Todd Bradley, Richard Chamberlin, Claudia Cyganowski, Darren Dowell, Meredith Drosback, Miranda Dunham, Timothy Ellsworth-Bowers, Neal Evans, Adam Ginsburg, Jason Glenn, Paul Harvey, Manuel Merello, Erik Rosolowsky, Wayne Schlingman, Yancy Shirley, Guy Stringfellow, Josh Walawender, and Jonathan Williams

For additional information on the BGPS data, please contact Adam Ginsburg
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 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

Support for the development of Bolocam was provided by NSF grants AST-9980846 and AST-0206158.

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