Interstellar matter and star formation in W5-E

A Herschel view^⋆,⋆⋆

¹ Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
e-mail: lise.deharveng@oamp.fr
² Physics Department, West Virginia University, Morgantown, WV 26506, USA
³ Laboratoire AIM Paris-Saclay, CEA/IRFU – CNRS/INSU – Université Paris Diderot, Service d’Astrophysique, Bât. 709, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France
⁴ Institut d’Astrophysique Spatiale, UMR 8617, CNRS, Université Paris-Sud 11, 91405 Orsay, France
⁵ CNRS/INSU, Laboratoire d’Astrophysique de Bordeaux, UMR 5804, BP 89, 33271 Floirac Cedex, France
⁶ Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France

Received: 28 February 2012
Accepted: 4 September 2012

Abstract

Aims. We identify the young stellar objects (YSOs) present in the vicinity of the W5-E H ii region, and study the influence of this H ii region on the star formation process in its surrounding molecular material.

Methods. W5-E has been observed with the Herschel-PACS and -SPIRE photometers, as part of the HOBYS key program; maps have been obtained at 100 μm, 160 μm, 250 μm, 350 μm, and 500 μm. The dust temperature and column density have been obtained by fitting spectral energy distributions (SEDs). Point sources have been detected and measured using PSF photometry with DAOPHOT.

Results. The dust temperature map shows a rather uniform temperature, in the range 17.5 K−20 K in the dense condensations or filaments, in the range 21 K−22 K in the photodissociation regions (PDRs), and in the range 24 K−31 K in the direction of the ionized regions. The values in the column density map are rather low, everywhere lower than 10²³ cm^-2, and of the order of a few 10²¹ cm^-2 in the PDRs. About 8000 M_⊙ of neutral material surrounds the ionized region, which is low with respect to the volume of this H ii region; we suggest that the exciting stars of the W5-E, W5-W, Sh 201, A and B H ii regions formed along a dense filament or sheet rather than inside a more spherical cloud. Fifty point sources have been detected at 100 μm. Most of them are Class 0/I YSOs. The SEDs of their envelopes have been fitted using a modified blackbody model. These envelopes are cold, with a mean temperature of 15.7 ± 1.8 K. Their masses are in the range 1.3 M_⊙–47 M_⊙. Eleven of these point sources are candidate Class 0 YSOs. Twelve of these point sources are possibly at the origin of bipolar outflows detected in this region. None of the YSOs contain a massive central object, but a few may form a massive star as they have both a massive envelope and also a high envelope accretion rate. Most of the Class 0/I YSOs are observed in the direction of high column density material, for example in the direction of the massive condensations present at the waist of the bipolar Sh 201 H ii region or enclosed by the bright-rimmed cloud BRC14. The overdensity of Class 0/I YSOs on the borders of the H ii regions present in the field strongly suggests that triggered star formation is at work in this region but, due to insufficient resolution, the exact processes at the origin of the triggering are difficult to determine.