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J/ApJ/710/1247        Dense cores in Gould Belt clouds        (Sadavoy+, 2010)

The mass distribution of starless and protostellar cores in Gould Belt clouds. Sadavoy S.I., Di Francesco J., Bontemps S., Megeath S.T., Rebull L.M., Allgaier E., Carey S., Gutermuth R., Hora J., Huard T., McCabe C.-E., Muzerolle J., Noriega-Crespo A., Padgett D., Terebey S. <Astrophys. J., 710, 1247-1270 (2010)> =2010ApJ...710.1247S
ADC_Keywords: Molecular clouds ; YSOs ; Millimetric/submm sources Keywords: dust, extinction - ISM: clouds - stars: formation - stars: luminosity function, mass function - stars: protostars Abstract: Using data from the SCUBA Legacy Catalogue (850um) and Spitzer Space Telescope (3.6-70um), we explore dense cores in the Ophiuchus, Taurus, Perseus, Serpens, and Orion molecular clouds. We develop a new method to discriminate submillimeter cores found by Submillimeter Common-User Bolometer Array (SCUBA) as starless or protostellar, using point source photometry from Spitzer wide field surveys. First, we identify infrared sources with red colors associated with embedded young stellar objects (YSOs). Second, we compare the positions of these YSO candidates to our submillimeter cores. With these identifications, we construct new, self-consistent starless and protostellar core mass functions (CMFs) for the five clouds. We find best-fit slopes to the high-mass end of the CMFs of -1.26±0.20, -1.22±0.06, -0.95±0.20, and -1.67±0.72 for Ophiuchus, Taurus, Perseus, and Orion, respectively. Description: We obtained our submillimeter data from the SCUBA Legacy Catalogue (SLC; see Di Francesco et al. 2008, Cat. J/ApJS/175/277), which is an archive of all 850um and 450um mapping observations from SCUBA on the James Clerk Maxwell Telescope (JCMT). We used the "Molecular Cores to Planet Forming Disks" (c2d; Evans et al. 2003PASP..115..965E, 2009, Cat. J/ApJS/181/321) Legacy Project data for the Ophiuchus, Perseus, and Serpens molecular clouds. The Taurus data came from Guest Observer (GO) observations for the Taurus Legacy Project (D. L. Padgett et al. 2010, in preparation), and the Orion data are from Guaranteed Time Observations (GTO) for the Spitzer Orion Survey (S. T. Megeath et al. 2010, in preparation). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table10.dat 71 559 List of starless cores table11.dat 71 185 List of protostellar cores
See also: J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009) J/ApJ/692/973 : Protostars in Perseus, Serpens and Ophiuchus (Enoch+, 2009) J/ApJS/175/277 : Submillimeter-Continuum SCUBA detections (Di Francesco+, 2008) J/ApJ/677/401 : Xray properties of protostars in ONC (Prisinzano+, 2008) J/ApJ/663/1149 : Spitzer survey of Serpens YSO population (Harvey+, 2007) J/A+A/447/609 : 1.2mm continuum observations in rho Oph cloud (Stanke+, 2006) http://irsa.ipac.caltech.edu/data/SPITZER/C2D/ : C2D Spitzer data http://irsa.ipac.caltech.edu/data/SPITZER/Taurus/ : Taurus Spitzer data Byte-by-byte Description of file: table1[01].dat
Bytes Format Units Label Explanations
1- 9 A9 --- Cloud Cloud 11- 17 A7 --- --- [JCMTSF_] 18- 33 A16 --- JCMTSF Core name (JHHMMSS.s+DDMMSS) 35- 39 F5.2 mag AV V band extinction (1) 41- 46 F6.2 Jy SPeak SCUBA 850 micron peak flux at the source position in Jy/beam 48- 53 F6.2 Jy S850 SCUBA total 850 micron flux (2) 55- 62 F8.3 Msun Mass Mass (3) 64- 71 E8.2 pc Reff Effective radius (4)
Note (1): Extinction measured towards the location of peak SCUBA 850 micron flux. Note (2): Within the core, where the core was defined by Clumpfind with a threshold of 90mJy/beam. Note (3): Derived from total 850 micron SCUBA flux using Equation 3. Note (4): Of the core determined by the Clumpfind area, A, where Reff=sqrt(A/π) for a Clumpfind threshold of 90mJy/beam.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 16-Mar-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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