Herschel observations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud

Pezzuto, S., Elia, D., Schisano, E., Strafella, F., Di Francesco, J., Sadavoy, S., Andre, P., Benedettini, M., Bernard, J. P., di Giorgio, A. M., Facchini, A., Hennemann, M., Hill, T., Koenyves, V., Molinari, S., Motte, F., Nguyen-Luong, Q., Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Pestalozzi, M., Polychroni, D., Rygl, K. L. J., Saraceno, P., Schneider, N., Spinoglio, L., Testi, L., Ward-Thompson, Derek ORCID: https://orcid.org/0000-0003-1140-2761 and White, G. J. 2012. Herschel observations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud. Astronomy and Astrophysics 547 , A54. 10.1051/0004-6361/201219501

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Abstract

We report far-infrared Herschel observations obtained between 70 μm and 500 μm 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 μm. B1-bN is clearly detected between 100 μm and 250 μm. 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.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	stars: protostars / stars: individual: [HKM99] B1-bS / stars: individual: [HKM99] B1-bN / stars: individual: [EYG2006] Bolo 81 / stars: individual: [EDJ2009] 295
Additional Information:	Pdf uploaded in accordance with publisher's policy at http://www.sherpa.ac.uk/romeo/issn/0004-6361/ (accessed 16/04/2014)
Publisher:	EDP Sciences
ISSN:	0004-6361
Date of First Compliant Deposit:	30 March 2016
Last Modified:	23 May 2023 15:06
URI:	https://orca.cardiff.ac.uk/id/eprint/56256

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