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J/ApJ/721/137      The Bolocam Galactic Plane Survey (BGPS)       (Bally+, 2010)

The Bolocam Galactic Plane Survey: λ = 1.1 and 0.35mm dust continuum emission in the Galactic center region. Bally J., Aguirre J., Battersby C., Bradley E.T., Cyganowski C., Dowell D., Drosback M., Dunham M.K., Evans II N.J., Ginsburg A., Glenn J., Harvey P., Mills E., Merello M., Rosolowsky E., Schlingman W., Shirley Y.L., Stringfellow G.S., Walawender J., Williams J. <Astrophys. J., 721, 137-163 (2010)> =2010ApJ...721..137B
ADC_Keywords: Interstellar medium ; Galactic plane ; Millimetric/submm sources Keywords: dust, extinction - Galaxy: center - ISM: clouds - stars: formation - surveys Abstract: The Bolocam Galactic Plane Survey (BGPS) data for a 6deg2 region of the Galactic plane containing the Galactic center are analyzed and compared to infrared and radio continuum data. The BGPS 1.1mm emission consists of clumps interconnected by a network of fainter filaments surrounding cavities, a few of which are filled with diffuse near-IR emission indicating the presence of warm dust or with radio continuum characteristic of HII regions or supernova remnants. New 350um images of the environments of the two brightest regions, Sgr A and B, are presented. Sgr B2 is the brightest millimeter-emitting clump in the Central Molecular Zone (CMZ) and may be forming the closest analog to a super star cluster in the Galaxy. The CMZ contains the highest concentration of millimeter- and submillimeter-emitting dense clumps in the Galaxy. Most 1.1mm features at positive longitudes are seen in silhouette against the 3.6-24um background observed by the Spitzer Space Telescope. However, only a few clumps at negative longitudes are seen in absorption, confirming the hypothesis that positive longitude clumps in the CMZ tend to be on the near side of the Galactic center, consistent with the suspected orientation of the central bar in our Galaxy. The Bolocat catalog of 1.1mm clumps contains 1428 entries in the Galactic center between l=358.5° and l=4.5° of which about 80% are likely to be within about 500pc of the center. Description: The observations reported here were obtained with Bolocam between 2005 June and 2007 July on the CSO 10m diameter telescope. SHARC-II observations were obtained during the best weather on these observing runs and in 2008 April. All data were obtained with a 45GHz bandwidth filter centered at 268GHz (1.1mm). Each bolometer has an effective Gaussian beam with an FWHM diameter of 31", but the maps presented here have an effective resolution of 33" due to beam-smearing by the scanning strategy, data sampling rate, and data reduction as discussed by Aguirre et al. (2011ApJS..192....4A). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 109 1428 1.1mm masses, column densities, and densities for 1428 Bolocat clumps
See also: J/ApJS/195/14 : The Bolocam Galactic Plane Survey. V. (Schlingman+, 2011) J/ApJS/188/123 : The Bolocam Galactic Plane Survey. II. (Rosolowsky+, 2010) J/AJ/138/1380 : Dust clumps in the Galactic Plane (Matthews+, 2009) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Seq Bolocat Galactic Plane Survey clump number (1) 6- 12 F7.3 deg GLON Galactic longitude 14- 19 F6.3 deg GLAT Galactic latitude 21- 27 F7.3 deg RAdeg Right Ascension in decimal degrees (J2000) 29- 35 F7.3 deg DEdeg Declination in decimal degrees (J2000) 37- 43 F7.1 Msun M40 Mass estimate from 40" aperture (2) 45- 51 E7.2 cm-2 N40 H2 column density from 40" aperture (2) 53- 60 F8.1 cm-3 n40 H2 volume number density from 40" aperture (2) 62- 69 F8.1 Msun Mr Mass estimate from effective beam-deconvolved area (2) 71- 75 F5.1 arcsec r Effective clump radius 77- 83 E7.2 cm-2 Nr H2 column density from effective beam-deconvolved area (2) 85- 92 F8.1 cm-3 nr H2 volume number density from effective beam-deconvolved area (2) 94-101 F8.1 Msun M120 Mass estimate from 120" aperture (2) 103-109 F7.1 Msun Mgrad Mass estimate from 40" aperture assuming a temperature gradient (3)
Note (1): From Bolocat V1.0 released in June via the IPAC website at As "Seq" number in Paper II: Rosolowsky et al., 2010, Cat. J/ApJS/188/123; <BGPS GLLL.lll+BB.bbb> in Simbad. Note (2): Assuming a dust temperature of 20K. Note (3): Temperature gradient that declines as a power-law with distance from Sgr A*. The power-law has a slope γg=0.2 and is normalized to have T=50K at a distance of 10pc from Sgr A*. This power-law implies T=27.5K at d=200pc from Sgr A*, 15.5K at d=3kpc, and 12.5K at d=8.5kpc. See discussion in Section 3.1.
History: From electronic version of the journal References: Aguirre et al. Paper I. 2011ApJS..192....4A Rosolowsky et al. Paper II. 2010ApJS..188..123R Cat. J/ApJS/188/123 Dunham et al. Paper III. 2010ApJ...717.1157D Schlingman et al. Paper V. 2011ApJS..195...14S Cat. J/ApJS/195/14 Dunham et al. Paper VI. 2011ApJ...731...90D Cat. J/ApJ/731/90 Dunham et al. Paper VII. 2011ApJ...741..110D Cat. J/ApJ/741/110 Ellsworth-Bowers et al. Paper VIII. 2013ApJ...770...39E Ginsburg et al. Paper IX. 2013ApJS..208...14G Shirley et al. Paper X. 2013ApJS..209....2S Cat. J/ApJS/209/2 Merello et al. Paper XI. 2015ApJS..218....1M Cat. J/ApJS/218/1 Ellsworth-Bowers et al. Paper XII. 2015ApJ...799...29E Cat. J/ApJ/799/29 Ellsworth-Bowers et al. Paper XIII. 2015ApJ...805..157E Cat. J/ApJ/805/157 Svoboda et al. Paper XIV. 2016ApJ...822...59S Cat. J/ApJ/822/59
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 05-Jul-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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