HAL: hal-00523477, version 1

arXiv: 1005.3118

ADS Bibliographic id: 2010A&A...518L..84H

DOI: 10.1051/0004-6361/201014629

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Astronomy & Astrophysics 518 (2010) L84

Herschel observations of embedded protostellar clusters in the Rosette Molecular Cloud

M. Hennemann 1, F. Motte 2, 3, S. Bontemps 4, 5, 6, 7, N. Schneider 1, T. Csengeri 1, Z. Balog 8, J. Di Francesco 9, A. Zavagno 10, 11, Ph. André 1, A. Men'shchikov 1, A. Abergel 12, B. Ali, J. -P. Baluteau 10, J. -Ph. Bernard 13, P. Cox, P. Didelon 1, A. -M. di Giorgio, M. Griffin 14, P. Hargrave, T. Hill 1, B. Horeau 15, M. Huang 16, J. Kirk 17, S. Leeks 18, J. Z. Li 16, A. Marston, P. Martin 19, S. Molinari 20, Q. Nguyen Luong, G. Olofsson 21, P. Persi 20, S. Pezzuto 20, D. Russeil 10, P. Saraceno 20, M. Sauvage 1, B. Sibthorpe 22, L. Spinoglio 23, L. Testi 24, D. Ward-Thompson 14, G. White 18, C. Wilson 25, A. Woodcraft 22

(2010)

The Herschel OB young stellar objects survey (HOBYS) has observed the Rosette molecular cloud, providing an unprecedented view of its star formation activity. These new far-infrared data reveal a population of compact young stellar objects whose physical properties we aim to characterise. We compiled a sample of protostars and their spectral energy distributions that covers the near-infrared to submillimetre wavelength range. These were used to constrain key properties in the protostellar evolution, bolometric luminosity, and envelope mass and to build an evolutionary diagram. Several clusters are distinguished including the cloud centre, the embedded clusters in the vicinity of luminous infrared sources, and the interaction region. The analysed protostellar population in Rosette ranges from 0.1 to about 15 Msun with luminosities between 1 and 150 Lsun, which extends the evolutionary diagram from low-mass protostars into the high-mass regime. Some sources lack counterparts at near- to mid-infrared wavelengths, indicating extreme youth. The central cluster and the Phelps & Lada 7 cluster appear less evolved than the remainder of the analysed protostellar population. For the central cluster, we find indications that about 25% of the protostars classified as Class I from near- to mid-infrared data are actually candidate Class 0 objects. As a showcase for protostellar evolution, we analysed four protostars of low- to intermediate-mass in a single dense core, and they represent different evolutionary stages from Class 0 to Class I. Their mid- to far-infrared spectral slopes flatten towards the Class I stage, and the 160 to 70um flux ratio is greatest for the presumed Class 0 source. This shows that the Herschel observations characterise the earliest stages of protostellar evolution in detail.

1:	Astrophysique Interactions Multi-échelles (AIM)
	CNRS : UMR7158 – INSU – Université Paris VII - Paris Diderot – CEA : DSM/IRFU
2:	Laboratoire AIM (AIM)
	CEA – Université Paris VII - Paris Diderot
3:	Institut de Recherches sur les lois Fondamentales de l'Univers (ex DAPNIA) (IRFU)
	CEA : DSM/IRFU
4:	Laboratoire d'Astrophysique de Bordeaux (LAB)
	CNRS : UMR5804 – INSU – Université Sciences et Technologies - Bordeaux I
5:	Observatoire aquitain des sciences de l'univers (OASU)
	CNRS : UMS2567 – INSU – Université Sciences et Technologies - Bordeaux I
6:	Université Sciences et Technologies - Bordeaux 1
	Université Sciences et Technologies - Bordeaux I
7:	Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB)
	CNRS : UMR5804 – INSU – Université Sciences et Technologies - Bordeaux I
8:	Max Planck Institut für Astronomie (MPIA)
	Max Planck Institut für Astronomie
9:	National Research Council of Canada, Herzberg Institute of Astrophysics
	Herzberg Institute of Astrophysics
10:	Laboratoire d'Astrophysique de Marseille (LAM)
	CNRS : UMR6110 – INSU – Université de Provence - Aix-Marseille I
11:	Observatoire Astronomique de Marseille Provence (OAMP)
	INSU – Université de Provence - Aix-Marseille I – CNRS : UMR6110
12:	Institut d'astrophysique spatiale (IAS)
	CNRS : UMR8617 – INSU – Université Paris XI - Paris Sud
13:	Centre d'étude spatiale des rayonnements (CESR)
	CNRS : UMR5187 – Observatoire Midi-Pyrénées – INSU – Université Paul Sabatier [UPS] - Toulouse III
14:	School of Physics & Astronomy
	Cardiff University
15:	Service d'Astrophysique (SAp)
	CEA : DSM/IRFU
16:	National Astronomical Observatories
	Chinese Academy of Sciences
17:	School of Physis & Astronomy
	Cardiff University
18:	Rutherford Appleton Laboratory - Didcot (RAL)
	Science & Technologie Facilities Council
19:	CITA
	University of Toronto
20:	Interplanetary Space Physics Institute (IFSI) (IFSI-INAF)
	Interplanetary Space Physics Institute
21:	Stockholm University
	Stockholm University
22:	Royal Observatory Edinburgh
	Royal Observatory Edinburgh
23:	Antarctic Research a European Network for Astrophysics (ARENA)
	CEA
24:	European Southern Observatory (ESO)
	ESO
25:	University of Exeter
	University of Nottingham

Subject

:

Sciences of the Universe/Astrophysics/Solar and Stellar Astrophysics Physics/Astrophysics/Solar and Stellar Astrophysics

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From: Marie-Paule Pomies <>

Submitted on: Tuesday, 5 October 2010 13:16:54

Updated on: Wednesday, 5 January 2011 15:00:49