2016ApJ...826...95C

Query : 2016ApJ...826...95C

2016ApJ...826...95C - Astrophys. J., 826, 95-95 (2016/July-3)

The JCMT Gould belt survey: evidence for dust grain evolution in Perseus star-forming clumps.

CHEN M.C.-Y., DI FRANCESCO J., JOHNSTONE D., SADAVOY S., HATCHELL J., MOTTRAM J.C., KIRK H., BUCKLE J., BERRY D.S., BROEKHOVEN-FIENE H., CURRIE M.J., FICH M., JENNESS T., NUTTER D., PATTLE K., PINEDA J.E., QUINN C., SALJI C., TISI S., HOGERHEIJDE M.R., WARD-THOMPSON D., BASTIEN P., BRESNAHAN D., BUTNER H., CHRYSOSTOMOU A., COUDE S., DAVIS C.J., DRABEK-MAUNDER E., DUARTE-CABRAL A., FIEGE J., FRIBERG P., FRIESEN R., FULLER G.A., GRAVES S., GREAVES J., GREGSON J., HOLLAND W., JONCAS G., KIRK J.M., KNEE L.B.G., MAIRS S., MARSH K., MATTHEWS B.C., MORIARTY-SCHIEVEN G., MOWAT C., PEZZUTO S., RAWLINGS J., RICHER J., ROBERTSON D., ROSOLOWSKY E., RUMBLE D., SCHNEIDER-BONTEMPS N., THOMAS H., TOTHILL N., VITI S., WHITE G.J., WOUTERLOOT J., YATES J. and ZHU M.

Abstract (from CDS):

The dust emissivity spectral index, β, is a critical parameter for deriving the mass and temperature of star-forming structures and, consequently, their gravitational stability. The β value is dependent on various dust grain properties, such as size, porosity, and surface composition, and is expected to vary as dust grains evolve. Here we present β, dust temperature, and optical depth maps of the star-forming clumps in the Perseus Molecular Cloud determined from fitting spectral energy distributions to combined Herschel and JCMT observations in the 160, 250, 350, 500, and 850 µm bands. Most of the derived β and dust temperature values fall within the ranges of 1.0-2.7 and 8-20 K, respectively. In Perseus, we find the β distribution differs significantly from clump to clump, indicative of grain growth. Furthermore, we also see significant localized β variations within individual clumps and find low-β regions correlate with local temperature peaks, hinting at the possible origins of low-β grains. Throughout Perseus, we also see indications of heating from B stars and embedded protostars, as well evidence of outflows shaping the local landscape.

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

Journal keyword(s): dust, extinction - ISM: clouds - stars: formation - stars: low-mass - stars: protostars

Simbad objects: 20

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Number of rows : 20
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 V* VX Cas Ae* 00 31 30.6818495040 +61 58 50.984946300 11.83 11.59 10.50 11.19 10.94 A0Vep 139 0
2 LDN 1448 DNe 03 22.5 +30 35           ~ 546 0
3 HH 197 HH 03 25 36.7 +30 44 00           ~ 10 0
4 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 371 0
5 LDN 1451 DNe 03 26.1 +30 10           ~ 60 0
6 LDN 1455 DNe 03 28 00.6480 +30 07 58.800           ~ 198 1
7 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 173 1
8 BD+30 547 Y*O 03 28 57.2114503248 +31 14 19.076151444   10.73 9.98 9.1   G4V 117 1
9 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 357 0
10 NGC 1333 OpC 03 29 09.2 +31 20 59           ~ 1575 1
11 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 770 1
12 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 489 0
13 BD+30 549 Or* 03 29 19.7773614209 +31 24 57.044926178 10.81 10.95 10.47 10.587   B8/9V 129 0
14 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 350 0
15 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1553 0
16 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 296 0
17 IC 348 OpC 03 44 31.1 +32 10 02           ~ 1476 1
18 LDN 1471 DNe 03 48.0 +32 54           ~ 349 0
19 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1227 1
20 V* FU Dra SB* 15 34 45.2133432432 +62 16 44.333175900   11.16 10.55 10.182 9.817 G0: 145 1

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