2011ApJ...730..142R

Query : 2011ApJ...730..142R

2011ApJ...730..142R - Astrophys. J., 730, 142 (2011/April-1)

Deconvolution of images from BLAST 2005: insight into the K3-50 and IC 5146 star-forming regions.

ROY A., ADE P.A.R., BOCK J.J., BRUNT C.M., CHAPIN E.L., DEVLIN M.J., DICKER S.R., FRANCE K., GIBB A.G., GRIFFIN M., GUNDERSEN J.O., HALPERN M., HARGRAVE P.C., HUGHES D.H., KLEIN J., MARSDEN G., MARTIN P.G., MAUSKOPF P., NETTERFIELD C.B., OLMI L., PATANCHON G., REX M., SCOTT D., SEMISCH C., TRUCH M.D.P., TUCKER C., TUCKER G.S., VIERO M.P. and WIEBE D.V.

Abstract (from CDS):

We present an implementation of the iterative flux-conserving Lucy-Richardson (L-R) deconvolution method of image restoration for maps produced by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST). Compared to the direct Fourier transform method of deconvolution, the L-R operation restores images with better-controlled background noise and increases source detectability. Intermediate iterated images are useful for studying extended diffuse structures, while the later iterations truly enhance point sources to near the designed diffraction limit of the telescope. The L-R method of deconvolution is efficient in resolving compact sources in crowded regions while simultaneously conserving their respective flux densities. We have analyzed its performance and convergence extensively through simulations and cross-correlations of the deconvolved images with available high-resolution maps. We present new science results from two BLAST surveys, in the Galactic regions K3-50 and IC 5146, further demonstrating the benefits of performing this deconvolution. We have resolved three clumps within a radius of 4'.5 inside the star-forming molecular cloud containing K3-50. Combining the well-resolved dust emission map with available multi-wavelength data, we have constrained the spectral energy distributions (SEDs) of five clumps to obtain masses (M), bolometric luminosities (L), and dust temperatures (T). The L-M diagram has been used as a diagnostic tool to estimate the evolutionary stages of the clumps. There are close relationships between dust continuum emission and both 21 cm radio continuum and 12CO molecular line emission. The restored extended large-scale structures in the Northern Streamer of IC 5146 have a strong spatial correlation with both SCUBA and high-resolution extinction images. A dust temperature of 12 K has been obtained for the central filament. We report physical properties of ten compact sources, including six associated protostars, by fitting SEDs to multi-wavelength data. All of these compact sources are still quite cold (typical temperature below ∼ 16 K) and are above the critical Bonner-Ebert mass. They have associated low-power young stellar objects. Further evidence for starless clumps has also been found in the IC 5146 region.

Abstract Copyright: ∼

Journal keyword(s): stars: formation - submillimeter: general - techniques: image processing

Nomenclature: Table 1, col(1): [RAB2011] KN (Nos K1-K5) = Table 1, col(2): BLAST JHHMMSS+DDMMSS N=5. Table 2, col(1): [RAB2011] ICNN (Nos IC1-IC10) = Table 2, col(2): BLAST JHHMMSS+DDMMSS N=10. Fig. 10: [RAB2011] GLL.ll+B.bb N=3.

Simbad objects: 36

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Number of rows : 36
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 NAME Per Arm PoG 03 30 +45.0           ~ 1672 0
2 NAME Aql Region reg 18 31.1 -02 10           ~ 456 0
3 [RAB2011] K1 smm 20 00 54.0 +33 30 55           ~ 1 0
4 [RAB2011] K2 smm 20 01 12.0 +33 38 02           ~ 1 0
5 GAL 070.33+01.63 Rad 20 01 33.0 +33 35 36           ~ 4 0
6 [RAB2011] K3 smm 20 01 37.0 +33 34 54           ~ 1 0
7 IRAS 19597+3327A Y*O 20 01 37.354 +33 35 28.23           ~ 9 1
8 CTB 82 Mas 20 01.7 +33 33           ~ 40 0
9 GAL 070.31+01.66 Rad 20 01 44.0 +33 35 42           ~ 5 0
10 NAME K 3-50A HII 20 01 45.6 +33 32 42           ~ 85 0
11 W 58a HII 20 01 45.8 +33 32 43           ~ 294 4
12 [RAB2011] K4 smm 20 01 46.0 +33 32 14           ~ 1 0
13 NGC 6857 HII 20 01 47.71 +33 31 33.4           ~ 88 3
14 [RAB2011] K5 smm 20 01 54.0 +33 33 43           ~ 1 0
15 OH 070.33+01.59 Y*? 20 01 54.03 +33 34 14.2           ~ 35 0
16 [W69] C Rad 20 01 54.2 +33 34 15           ~ 18 0
17 W 58c2 Y*? 20 01 55.21 +33 34 17.5           ~ 10 0
18 NAME Cyg X Cld 20 30 04.7973633 +40 51 36.002197           ~ 962 1
19 [RAB2011] G93.43-4.28 smm 21 44.5 +47 36           ~ 1 0
20 IRAS 21428+4732 IR 21 44 43.9 +47 46 45           ~ 9 0
21 [RAB2011] G93.48-4.30 smm 21 44.8 +47 37           ~ 1 0
22 NAME HHL 73 IRS 1 Y*? 21 44 52.01 +47 40 30.8           ~ 20 0
23 IRAS 21433+4719 IR 21 45 08.1 +47 33 05           ~ 3 0
24 [RAB2011] G93.54-4.33 smm 21 45.2 +47 38           ~ 1 0
25 [RAB2011] IC5 smm 21 45 33.6 +47 35 59           ~ 1 0
26 [RAB2011] IC7 smm 21 45 55.8 +47 35 32           ~ 1 0
27 [RAB2011] IC1 smm 21 45 59.2 +47 18 12           ~ 1 0
28 LDN 1031 DNe 21 46.3 +47 18           ~ 13 0
29 [RAB2011] IC3 smm 21 46 23.9 +47 17 59           ~ 1 0
30 LDN 1030 DNe 21 46.5 +47 06           ~ 7 0
31 [RAB2011] IC8 smm 21 47 07.3 +47 32 42           ~ 1 0
32 V* V1735 Cyg Or* 21 47 20.6628414360 +47 32 03.857457372           ~ 170 0
33 [RAB2011] IC10 smm 21 47 58.8 +47 36 43           ~ 1 0
34 IC 5146 OpC 21 53 29.3 +47 14 46           ~ 507 2
35 NAME Cas A SNR 23 23 26.0 +58 48 41     14.30     ~ 3033 1
36 NAME Vulpecula Region reg ~ ~           ~ 30 0

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