J/MNRAS/402/603 Properties of SCUBA cores in Perseus mol. cloud (Curtis+, 2010)
The properties of SCUBA cores in the Perseus molecular cloud:
the bias of clump-finding algorithms.
Curtis E.I., Richer J.S.
<Mon. Not. R. Astron. Soc., 402, 603-619 (2010)>
=2010MNRAS.402..603C 2010MNRAS.402..603C
ADC_Keywords: Molecular clouds; Photometry, millimetric/submm
Keywords: stars: formation - stars: evolution - ISM: clouds - dust, extinction -
submillimetre - ISM: individual: Perseus
Abstract:
We present a new analysis of the properties of star-forming cores in
the Perseus molecular cloud, identified in SCUBA 850um data
originally presented by Hatchell et al. (2005, Cat. J/A+A/440/151).
Our goal is to determine which core properties can be robustly
identified and which depend on the extraction technique. Four regions
in the cloud are examined: NGC 1333, IC348/HH211, L1448 and L1455. We
identify clumps of dust emission using two popular automated
algorithms, clfind and gaussclumps, finding 85 and 122 clumps in
total, respectively. Using the catalogues of Hatchell et al. (2005,
Cat. J/A+A/440/151), we separate these clumps into starless, Class 0
and Class I cores.
Description:
We extracted fully calibrated and reduced SCUBA 850um maps across the
four regions in Perseus we observed with HARP from the data presented
by Hatchell et al. (2005, Cat. J/A+A/440/151), where we refer the
reader for details of the observations and processing. In short, the
data were taken during 20 nights between 1999 and 2003.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 57 85 Properties of SCUBA clumps found with CLFIND
tablea2.dat 57 122 Properties of SCUBA clumps found with GAUSSCLUMPS
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See also:
J/A+A/440/151 : Observations at 850um in Perseus clusters (Hatchell+, 2005)
J/ApJ/638/293 : 1.1mm sources in the Perseus Molecular Cloud (Enoch+, 2006)
J/ApJ/646/1009 : Structures of dust in Perseus molecular cloud (Kirk+, 2006)
J/A+A/468/1009 : Star formation in Perseus. II. (Hatchell+, 2007)
J/A+A/472/187 : 12CO outflows towards submm cores in Perseus (Hatchell+, 2007)
J/ApJ/668/1042 : Dense cores in Perseus molecular cloud (Kirk+, 2007)
J/ApJ/683/822 : Star formation in Ophiuchus and Perseus II. (Jorgensen+, 2008)
J/ApJS/175/509 : Ammonia spectral atlas in Perseus (Rosolowsky+, 2008)
J/ApJ/696/298 : Dense cores in Perseus (Foster+, 2009)
Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- sub-reg Sub-region name: IC348, L1448, L1455 or NGC1333
9- 10 I2 --- Clump [1/65] Clump number, within the sub-region
and the table
12- 13 I2 h RAh Right ascension (J2000) of peak clump flux
15- 16 I2 min RAm Right ascension (J2000) of peak clump flux
18- 22 F5.2 s RAs Right ascension (J2000) of peak clump flux
24 A1 --- DE- Declination sign (J2000) of peak clump flux
25- 26 I2 deg DEd Declination (J2000) of peak clump flux
28- 29 I2 arcmin DEm Declination (J2000) of peak clump flux
31- 34 F4.1 arcsec DEs Declination (J2000) of peak clump flux
36- 40 F5.3 pc Reff Clump effective radius (1)
42- 45 F4.2 Jy Speak Clump peak flux at 850um (in Jy/beam)
47- 51 F5.2 Jy S850 Clump total flux at 850um
53- 57 F5.2 Msun M850 Clump mass derived from the total flux assuming
optically thin, isothermal dust at 12K
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Note (1): the effective radius is computed as the geometric mean of the
clump major/minor 'sizes' (sqrt(Size1+Size2)). Each size is formed
from the standard deviation of the clump co-ordinates about the
centroid position, weighted by the pixel data values.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-May-2013