Ward-Thompson, D.; Kirk, J. M.; André, P.; Saraceno, P.; Didelon, P.; Könyves, V.; Schneider, N.; Abergel, A.; Baluteau, J.-P.; Bernard, J.-Ph.; Bontemps, S.; Cambrésy, L.; Cox, P.; Di Francesco, J.; Di Giorgio, A. M.; Griffin, M.; Hargrave, P.; Huang, M.; Li, J. Z.; Martin, P.; Men'shchikov, A.; Minier, V.; Molinari, S.; Motte, F.; Olofsson, G.; Pezzuto, S.; Russeil, D.; Sauvage, M.; Sibthorpe, B.; Spinoglio, L.; Testi, L.; White, G.; Wilson, C.; Woodcraft, A. and Zavagno, A.
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|DOI (Digital Object Identifier) Link:||https://doi.org/10.1051/0004-6361/201014618|
|Google Scholar:||Look up in Google Scholar|
The Polaris Flare cloud region contains a great deal of extended emission. It is at high declination and high Galactic latitude. It was previously seen strongly in IRAS Cirrus emission at 100 microns. We have detected it with both PACS and SPIRE on Herschel. We see filamentary and low-level structure. We identify the five densest cores within this structure. We present the results of a temperature, mass and density analysis of these cores. We compare their observed masses to their virial masses, and see that in all cases the observed masses lie close to the lower end of the range of estimated virial masses. Therefore, we cannot say whether they are gravitationally bound prestellar cores. Nevertheless, these are the best candidates to be potential prestellar cores in the Polaris cloud region.
|Item Type:||Journal Article|
|Copyright Holders:||2010 ESO|
|Extra Information:||5 pp.|
|Keywords:||stellar formation; galactic clouds; galactic dust|
|Academic Unit/School:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Mairi Harding|
|Date Deposited:||07 Dec 2010 16:45|
|Last Modified:||30 Nov 2016 21:28|
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