Journal Article

The properties of SCUBA cores in the Perseus molecular cloud: the bias of clump-finding algorithms

Emily I. Curtis and John S. Richer

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 402, issue 1, pages 603-619
Published in print February 2010 | ISSN: 0035-8711
Published online February 2010 | e-ISSN: 1365-2966 | DOI:
The properties of SCUBA cores in the Perseus molecular cloud: the bias of clump-finding algorithms

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We present a new analysis of the properties of star-forming cores in the Perseus molecular cloud, identified in SCUBA 850 μm data originally presented by Hatchell et al. 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., we separate these clumps into starless, Class 0 and Class I cores. Some trends are true for both populations: clumps become increasingly elongated over time; clumps are consistent with constant surface brightness objects (i.e. MR2), with an average brightness ≈4–10 times larger than the surrounding molecular cloud; the clump mass distribution (CMD) resembles the stellar initial mass function, with a slope α=−2.0 ± 0.1 for clfind and α=−3.15 ± 0.08 for gaussclumps, which straddle the Salpeter value (α=−2.35). The mass at which the slope shallows (similar for both algorithms at M≈ 6 M) implies a star-forming efficiency of between 10 and 20 per cent. Other trends reported elsewhere depend critically on the clump-finding technique: we find protostellar clumps are both smaller (for gaussclumps) and larger (for clfind) than their starless counterparts; the functional form, best fitting to the CMD, is different for the two algorithms. The gaussclumps CMD is best fitted with a log-normal distribution, whereas a broken power law is best for clfind; the reported lack of massive starless cores in previous studies can be seen in the clfind but not the gaussclumps data. Our approach, exploiting two extraction techniques, highlights similarities and differences between the clump populations, illustrating the caution that must be exercised when comparing results from different studies and interpreting the properties of samples of continuum cores.

Keywords: stars: formation; stars: evolution; ISM: clouds; dust, extinction; submillimetre; ISM: individual: Perseus

Journal Article.  11225 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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