2010MNRAS.401..204B

Query : 2010MNRAS.401..204B

2010MNRAS.401..204B - Mon. Not. R. Astron. Soc., 401, 204-222 (2010/January-1)

The JCMT legacy survey of the Gould belt: a first look at Orion B with HARP.

BUCKLE J.V., CURTIS E.I., ROBERTS J.F., WHITE G.J., HATCHELL J., BRUNT C., BUTNER H.M., CAVANAGH B., CHRYSOSTOMOU A., DAVIS C.J., DUARTE-CABRAL A., ETXALUZE M., DI FRANCESCO J., FRIBERG P., FRIESEN R., FULLER G.A., GRAVES S., GREAVES J.S., HOGERHEIJDE M.R., JOHNSTONE D., MATTHEWS B., MATTHEWS H., NUTTER D., RAWLINGS J.M.C., RICHER J.S., SADAVOY S., SIMPSON R.J., TOTHILL N.F.H., TSAMIS Y.G., VITI S., WARD-THOMPSON D., WOUTERLOOT J.G.A. and YATES J.

Abstract (from CDS):

The Gould Belt Legacy Survey will survey nearby star-forming regions (within 500 pc), using Heterodyne Array Receiver Programme (HARP), Submillimetre Common-User Bolometer Array 2 and Polarimeter 2 on the James Clerk Maxwell Telescope. This paper describes the initial data obtained using HARP to observe 12CO, 13CO and C18O J = 3 ⟶ 2 towards two regions in Orion B, NGC 2024 and NGC 2071. We describe the physical characteristics of the two clouds, calculating temperatures and opacities utilizing all the three isotopologues. We find good agreement between temperatures calculated from CO and from dust emission in the dense, energetic regions. We determine the mass and energetics of the clouds, and of the high-velocity material seen in 12CO emission, and compare the relative energetics of the high- and low-velocity material in the two clouds. We present a clumpfind analysis of the 13CO condensations. The slope of the condensation mass functions, at the high-mass ends, is similar to the slope of the initial mass function.

Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS

Journal keyword(s): molecular data - stars: formation - ISM: kinematics and dynamics - submillimetre

Simbad objects: 18

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Number of rows : 18
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 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 657 1
2 [MCK88] NGC 2024 FIR 1 FIR 05 41 41.40 -01 53 47.0           ~ 37 0
3 [MCK88] NGC 2024 FIR 2 Y*? 05 41 42.50 -01 54 06.0           ~ 38 0
4 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1498 0
5 [MCK88] NGC 2024 FIR 3 Y*O 05 41 43.00 -01 54 24.0           ~ 52 0
6 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1198 1
7 [MCK88] NGC 2024 FIR 4 Y*O 05 41 44.00 -01 54 42.0           ~ 55 0
8 [MCK88] NGC 2024 FIR 5 cor 05 41 44.6 -01 55 38           ~ 98 0
9 [MCK88] NGC 2024 FIR 7 cor 05 41 44.90 -01 56 15.0           ~ 33 0
10 [MCK88] NGC 2024 FIR 6 IR 05 41 45.00 -01 56 01.0           ~ 56 0
11 LBS 2-23 PoC 05 46 07.5 -00 10 24           ~ 14 0
12 HH 24 HH 05 46 09 -00 10.2           ~ 163 1
13 M 78 RNe 05 46 45.8 +00 04 45   8.0       ~ 397 0
14 NAME NGC 2071 IR SFR 05 47 04.4 +00 21 49           ~ 75 0
15 [PGS81] IRS 3 IR 05 47 04.63 +00 21 47.9           ~ 57 0
16 [PGS81] IRS 1 Y*O 05 47 04.78 +00 21 42.8           ~ 88 0
17 NGC 2071 RNe 05 47 10 +00 18.0           ~ 661 1
18 NAME Gould Belt PoG ~ ~           ~ 956 1

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