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J/ApJ/646/1009   Structures of dust in Perseus molecular cloud    (Kirk+, 2006)

The large- and small-scale structures of dust in the star-forming Perseus molecular cloud. Kirk H., Johnstone D., Di Francesco J. <Astrophys. J., 646, 1009-1023 (2006)> =2006ApJ...646.1009K
ADC_Keywords: Molecular clouds ; Millimetric/submm sources Keywords: ISM: clouds - stars: formation Abstract: We present an analysis of 3.5deg2 of submillimeter continuum and extinction data of the Perseus molecular cloud. We identify 58 clumps in the submillimeter map, and we identify 39 structures (cores) and 11 associations of structures (super cores) in the extinction map. The cumulative mass distributions of the submillimeter clumps and extinction cores have steep slopes (alpha∼2 and 1.5-2, respectively), steeper than the Salpeter initial mass function (IMF; alpha=1.35), while the distribution of extinction super cores has a shallow slope (alpha∼1). Most of the submillimeter clumps are well fit by stable Bonnor-Ebert spheres with 10K<T<19K and 5.5<log10(Pext/k)<0.6. The clumps are found only in the highest column density regions (AV>5-7mag), although Bonnor-Ebert models suggest that we should have been able to detect them at lower column densities if they exist. Description: Submillimeter data at 850um of the Perseus molecular cloud were obtained using the Submillimeter Common User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT) on Mauna Kea.4 The data we present here are a combination of our own observations (∼1.3deg2) with publicly available archival data for a total of 3.5deg2. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 85 58 Properties of Submillimeter Clumps in Perseus table2.dat 59 39 Properties of Extinction Cores in Perseus table3.dat 49 11 Properties of Extinction Super Cores in Perseus
See also: J/ApJ/638/293 : 1.1mm sources in the Perseus Molecular Cloud (Enoch+, 2006) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 12 A12 --- SMM Name from J2000 positions (HHMMSS+DDMMm) [KJD2006] SMM JHHMMmm+DDMMm in Simbad 14- 15 I2 h RAh Peak flux right ascension (J2000) (1) 17- 18 I2 min RAm Peak flux right ascension (J2000) (1) 20- 23 F4.1 s RAs Peak flux right ascension (J2000) (1) 25 A1 --- DE- Peak flux declination sign (J2000) (1) 26- 27 I2 deg DEd Peak flux declination (J2000) (1) 29- 30 I2 arcmin DEm Peak flux declination (J2000) (1) 32- 35 F4.1 arcsec DEs Peak flux declination (J2000) (1) 37- 41 F5.2 Jy f0 Peak flux at 850um (in Jy/beam) 43- 47 F5.2 Jy S850um Total flux at 850um (2) 49- 52 F4.1 arcsec Reff Radius derived from clfind (Williams et al. 1994, Cat. J/ApJ/428/693) 54- 56 F3.1 solMass Mass Mass derived from the total flux assuming Td=15K and k850=0.02cm2/g, d=250pc 58- 61 F4.2 --- Conc Concentration from Bonnor-Ebert modeling 63- 66 F4.1 K Temp Temperature from Bonnor-Ebert modeling 68- 71 F4.2 solMass MBE Mass from Bonnor-Ebert modeling 73- 75 F3.1 [cm-3] logNc Central number density from Bonnor-Ebert modeling 77- 79 F3.1 [cm-3.K] logP/k External pressure derived from Bonnor-Ebert modeling, log(Pext/k) 81- 82 I2 --- [HRF2005] ? Best corresponding submillimeter clump in Hatchell et al. (2005, Cat. J/A+A/440/151) number (3) 84- 85 I2 --- EC Closest corresponding extinction core number, [KJD2006] EC NN in Simbad, in table2
Note (1): Position of peak flux within clump (accurate to 6"). Note (2): Note a beam size of 19.9" is used for the peak flux. Note (3): More clumps were identified in their survey, as discussed in Section 4.1.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 I2 --- EC Identification number, [KJD2006] EC NN in Simbad 4- 5 I2 h RAh Peak flux right ascension (J2000) (1) 7- 8 I2 min RAm Peak flux right ascension (J2000) (1) 10- 13 F4.1 s RAs Peak flux right ascension (J2000) (1) 15 A1 --- DE- Peak flux declination sign (J2000) (1) 16- 17 I2 deg DEd Peak flux declination (J2000) (1) 19- 20 I2 arcmin DEm Peak flux declination (J2000) (1) 22- 25 F4.1 arcsec DEs Peak flux declination (J2000) (1) 27- 29 F3.1 --- AVpeak Peak extinction (2) 31- 33 F3.1 --- AVbg Background extinction (2) 35- 39 F5.1 solMass Mass Mass (2) 41- 45 F5.1 arcsec sigmax sigma_x_ (2) 47- 51 F5.1 arcsec sigmay sigma_y_ (2) 53- 56 F4.1 10+3cm-3 <n> Mean number density (2) 58- 59 I2 --- ESC Associated extinction super core, [KJD2006] ESC NN in Simbad, in table3
Note (1): Position of peak extinction within core (accurate to 2.5'). Note (2): From results of Gaussian fitting
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 2 I2 --- ESC Identification number, [KJD2006] ESC NN in Simbad 4- 5 I2 h RAh Peak flux right ascension (J2000) (1) 7- 8 I2 min RAm Peak flux right ascension (J2000) (1) 10- 13 F4.1 s RAs Peak flux right ascension (J2000) (1) 15 A1 --- DE- Peak flux declination sign (J2000) (1) 16- 17 I2 deg DEd Peak flux declination (J2000) (1) 19- 20 I2 arcmin DEm Peak flux declination (J2000) (1) 22- 25 F4.1 arcsec DEs Peak flux declination (J2000) (1) 27- 30 F4.1 --- AVpeak Peak extinction (2) 32- 37 F6.1 solMass Mass Mass from results (2) 39- 44 F6.1 arcsec Reff Effective radius (2) 46- 49 F4.1 10+3cm-3 <n> Mean number density (2)
Note (1): Position of peak extinction within core (accurate to 2.5'). Note (2): Derived from Clumpfind (Williams et al. 1994, Cat. J/ApJ/428/693) with several clumps further separated.
History: From electronic version of the journal Tables 1 and 2 are taken from erratum Vol. 669, p. 657 (2007).
(End) Patricia Vannier [CDS] 09-May-2008
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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