期刊
ASTRONOMY & ASTROPHYSICS
卷 547, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201219501
关键词
stars: protostars; stars: individual: [HKM99] B1-bS; stars: individual: [HKM99] B1-bN; stars: individual: [EYG2006] Bolo 81; stars: individual: [EDJ2009] 295
资金
- ASI [I/038/08/0, I/005/11/0]
- BMVIT (Austria)
- ESA-PRODEX (Belgium)
- CEA/CNES (France)
- DLR (Germany)
- ASI/INAF (Italy)
- CICYT/MCYT (Spain)
- CSA (Canada)
- NAOC (China)
- CEA (France)
- CNES (France)
- CNRS (France)
- ASI (Italy)
- MCINN (Spain)
- SNSB (Sweden)
- STFC (UK)
- UKSA (UK)
- NASA (USA)
- STFC [ST/G002533/1, ST/K002708/1, PP/D000963/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K002708/1, PP/D000963/1, ST/G002533/1] Funding Source: researchfish
We report far-infrared Herschel observations obtained between 70 mu m and 500 mu m of two star-forming dusty condensations, [HKM99] B1-bS and [HKM99] B1-bN, in the B1 region of the Perseus star-forming cloud. In the western part of the Perseus cloud, B1-bS is the only source detected in all six PACS and SPIRE photometric bands, but it is not visible in the Spitzer map at 24 mu m. B1-bN is clearly detected between 100 mu m and 250 mu m. We have fitted the spectral energy distributions of these sources to derive their physical properties, and find that a simple greybody model fails to reproduce the observed spectral energy distributions. At least a two-component model is required, consisting of a central source surrounded by a dusty envelope. The properties derived from the fit, however, suggest that the central source is not a Class 0 object. We then conclude that while B1-bS and B1-bN appear to be more evolved than a pre-stellar core, the best-fit models suggest that their central objects are younger than a Class 0 source. Hence, they may be good candidates to be examples of the first hydrostatic core phase. The projected distance between B1-bS and B1-bN is a few Jeans lengths. If their physical separation is close to this value, this pair would allow studying the mutual interactions between two forming stars at a very early stage of their evolution.
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