Cold dust clumps in dynamically hot gas
Author
- Kim, S.;
- Kwon, E.;
- Madden, S. C.;
- Meixner, M.;
- Hony, S.;
- Panuzzo, P.;
- Sauvage, M.;
- Roman Duval, Julia;
- Gordon, K. D.;
- Engelbracht, C.;
- Israel, F. P.;
- Misselt, K.;
- Okumura, K.;
- Li, A.;
- Bolatto, Alberto;
- Skibba, R.;
- Galliano, F.;
- Matsuura, M.;
- Bernard, J. P.;
- Bot, Caroline;
- Galametz, M.;
- Hughes, A.;
- Kawamura, A.;
- Onishi, T.;
- Paradis, D.;
- Poglitsch, A.;
- Reach, W. T.;
- Robitaille, T.;
- Rubio López, Mónica;
- Tielens, A. G. G. M.;
Abstract
Aims. We present clumps of dust emission from Herschel observations of the Large Magellanic Cloud (LMC) and their physical and statistical
properties. We catalog cloud features seen in the dust emission from Herschel observations of the LMC, the Magellanic type irregular galaxy
closest to the Milky Way, and compare these features with Hi catalogs from the ATCA+Parkes Hi survey.
Methods. Using an automated cloud-finding algorithm, we identify clouds and clumps of dust emission and examine the cumulative mass distribution
of the detected dust clouds. The mass of cold dust is determined from physical parameters that we derive by performing spectral energy distribution
fits to 250, 350, and 500 μm emission from SPIRE observations using dust grain size distributions for graphite/silicate in low-metallicity
extragalactic environments.
Results. The dust cloud mass spectrum follows a power law distribution with an exponent of γ = −1.8 for clumps larger than 4 × 102 M and is
similar to the Hi mass distribution. This is expected from the theory of ISM structure in the vicinity of star formation.
General note
Artículo de publicación ISI.
Patrocinador
We acknowledge financial support from the NASA
Herschel Science Center, JPL contracts # 1381522 & 1381650. We thank the
contributions and support from the European Space Agency (ESA), the PACS
and SPIRE teams, the Herschel Science Center and the NASA Herschel Science
Center (esp. A. Barbar and K. Xu) and the PACS and SPIRE instrument control
centers, without which none of this work would be possible. We thank the referee
for his/her very important comments on the manuscript. S.K. and E.K. were
supported by Basic Science Research Program through the National Research
Foundation of Korea (NRF) funded by the Ministry of Education, Science and
Technology 2009-0066892. M.R. is supported by FONDECYT No. 1080335 and
FONDAP No. 15010003.
Identifier
URI: https://repositorio.uchile.cl/handle/2250/126205
DOI: doi: 10.1051/0004-6361/201014645
Quote Item
A&A 518, L75 (2010)
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