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J/ApJ/639/259  Sub-mm clumps in Orion B South molecular cloud (Johnstone+, 2006)

Large area mapping at 850 µm. IV. Analysis of the clump distribution in the Orion B South molecular cloud. Johnstone D., Matthews H., Mitchell G.F. <Astrophys. J., 639, 259-274 (2006)> =2006ApJ...639..259J
ADC_Keywords: Infrared sources ; Millimetric/submm sources ; Molecular clouds ; Interstellar medium Keywords: infrared: ISM - ISM: clouds - ISM: individual (B33, NGC 2023, NGC 2024, Orion B South) - ISM: structure - stars: formation Abstract: We present results from a survey of a 1300arcmin2 region of the Orion B South molecular cloud, including NGC 2024, NGC 2023, and the Horsehead Nebula (B33), obtained using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). Submillimeter continuum observations at 450 and 850µm are discussed. Using an automated algorithm, 57 discrete emission features ("clumps") are identified in the 850µm map. Description: The data covering Orion B South were obtained between 1997 and 2000 using SCUBA at the JCMT. The JCMT archive, hosted by the CADC was used to find all relevant observations toward the region. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 73 57 Clump properties in Orion B South derived from 850µm data table2.dat 28 57 Submillimeter wavelength properties of clumps in Orion B South
See also: J/ApJ/559/307 : Sub-mm mapping in Orion B molecular cloud (Johnstone+, 2001) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 12 A12 --- SMMJ Clump name (HHMMmm+DDMMm) (G1) 14- 15 I2 h RAh Hour of Right Ascension (J2000.0) (1) 17- 18 I2 min RAm Minute of Right Ascension (J2000.0) (1) 20- 23 F4.1 s RAs Second of Right Ascension (J2000.0) (1) 25 A1 --- DE- Sign of the Declination (J2000.0) (1) 26- 27 I2 deg DEd Degree of Declination (J2000.0) (1) 29- 30 I2 arcmin DEm Arcminute of Declination (J2000.0) (1) 32- 33 I2 arcsec DEs Arcsecond of Declination (J2000.0) (1) 35- 40 F6.2 Jy S850 Total flux density at 850µm (2) 42- 46 F5.2 Jy Sp850 Peak flux at 850µm, in units of Jy/beam (2) 48- 49 I2 10+3AU Reff Effective radius (2) 51- 54 F4.2 --- C Degree of concentration (3) 56- 57 I2 K Td Dust temperature (3) 59- 61 F3.1 [K/cm+3] log(P/k) Bounding pressure (3) 63- 67 F5.2 solMass M1 Mass derived from Bonnor-Ebert analysis (3) 69- 73 F5.2 solMass M2 Derived mass, assuming Td=20K (4)
Note (1): Position of peak surface brightness within clump (accurate to 3"). Note (2): Radius, peak flux, and total flux are derived from clfind (Williams et al. 1994, Cat. J/ApJ/428/693). The peak flux and total flux have uncertainties of about 20%, mostly due to absolute flux calibration. The radius has not been deconvolved from the telescope beam. Note (3): Quantity derived from Bonnor-Ebert analysis. Note (4): Mass derived from the total flux assuming Td=20K and κ850=0.02cm2/g.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 12 A12 --- SMMJ Clump name (HHMMmm+DDMMm) (G1) 14- 17 F4.1 --- FRt Total flux ratio (S450um/S850um) (1) 19- 22 F4.1 --- FRp Peak flux ratio (Sp450um/Sp850um) (1) 24- 25 I2 K Td1 Dust temperature derived from Bonnor-Ebert analysis 27- 28 I2 K Td2 Dust temperature derived from spectral energy distribution (2)
Note (1): The 850 and 450µm peak flux and total flux are derived from CLFIND (Williams et al. 1994, Cat. J/ApJ/428/693) after convolution to an identical beam size. Note (2): Quantity derived from spectral energy fit to 450 and 850{um}m integrated fluxes.
Global Notes: Note (G1): [JMM2006] SMM JHHMMmm+DDMMm in Simbad.
History: From electronic version of the journal References: Johnstone et al., Paper I 2000ApJS..131..505J Johnstone et al., Paper II 2000ApJ...545..327J Johnstone et al., Paper III 2001ApJ...559..307J, Cat. J/ApJ/559/307
(End) Marianne Brouty [CDS] 19-Jul-2007
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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