Astronomy and Astrophysics, volume 546A, 74-74 (2012/10-1)
Interstellar matter and star formation in W5-E. A Herschel view.
DEHARVENG L., ZAVAGNO A., ANDERSON L.D., MOTTE F., ABERGEL A., ANDRE P., BONTEMPS S., LELEU G., ROUSSEL H. and RUSSEIL D.
Abstract (from CDS):
We identify the young stellar objects (YSOs) present in the vicinity of the W5-E HII region, and study the influence of this HII region on the star formation process in its surrounding molecular material. W5-E has been observed with the Herschel-PACS and -SPIRE photometers, as part of the HOBYS key program; maps have been obtained at 100µm, 160µm, 250µm, 350µm, and 500µm. 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. The dust temperature map shows a rather uniform temperature, in the range 17.5K-20K in the dense condensations or filaments, in the range 21K-22K in the photodissociation regions (PDRs), and in the range 24K-31K in the direction of the ionized regions. The values in the column density map are rather low, everywhere lower than 1023cm–2, and of the order of a few 1021cm–2 in the PDRs. About 8000M☉ of neutral material surrounds the ionized region, which is low with respect to the volume of this HII region; we suggest that the exciting stars of the W5-E, W5-W, Sh 201, A and B HII regions formed along a dense filament or sheet rather than inside a more spherical cloud. Fifty point sources have been detected at 100µm. 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±1.8K. Their masses are in the range 1.3M☉-47M☉. 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 HII region or enclosed by the bright-rimmed cloud BRC14. The overdensity of Class 0/I YSOs on the borders of the HII 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.
stars: formation - stars: early-type - dust, extinction - HII regions - ISM: individual objects: W5-E - ISM: individual objects: Sh201
Tables 2,3,5,6,A.1,B.1,B.2,C.1,C.2,D.1 : [DZA2012] BRCNN aN,[DZA2012] BRCNN N,[DZA2012] Sh201 aN,[DZA2012] Sh201 N,[DZA2012] IB aN,[DZA2012] IB N,[DZA2012] IB exN,[DZA2012] Isolated NN,[DZA2012] Isolated 14bis N=13+5+19+13+20+15
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