2014A&A...572A..37P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST15:10:09

2014A&A...572A..37P - Astronomy and Astrophysics, volume 572A, 37-37 (2014/12-1)

Modeling and predicting the shape of the far-infrared to submillimeter emission in ultra-compact HII regions and cold clumps.

PARADIS D., MENY C., NORIEGA-CRESPO A., PALADINI R., BERNARD J.-P., BOT C., CAMBRESY L., DEMYK K., GROMOV V., RIVERA-INGRAHAM A. and VENEZIANI M.

Abstract (from CDS):

Dust properties are very likely affected by the environment in which dust grains evolve. For instance, some analyses of cold clumps (7-17K) indicate that the aggregation process is favored in dense environments. However, studying warm (30-40 K) dust emission at long wavelength (λ>300µm has been limited because it is difficult to combine far infrared-to-millimeter (FIR-to-mm) spectral coverage and high angular resolution for observations of warm dust grains. Using Herschel data from 70 to 500µm, which are part of the Herschel infrared Galactic (Hi-GAL) survey combined with 1.1mm data from the Bolocam Galactic Plane Survey (BGPS), we compared emission in two types of environments: ultra-compact HII (UCHII) regions, and cold molecular clumps (denoted as cold clumps). With this comparison we tested dust emission models in the FIR-to-mm domain that reproduce emission in the diffuse medium, in these two environments (UCHII regions and cold clumps). We also investigated their ability to predict the dust emission in our Galaxy. We determined the emission spectra in twelve UCHII regions and twelve cold clumps, and derived the dust temperature (T) using the recent two-level system (TLS) model with three sets of parameters and the so-called T-β (temperature-dust emissivity index) phenomenological models, with β set to 1.5, 2 and 2.5. We tested the applicability of the TLS model in warm regions for the first time. This analysis indicates distinct trends in the dust emission between cold and warm environments that are visible through changes in the dust emissivity index. However, with the use of standard parameters, the TLS model is able to reproduce the spectral behavior observed in cold and warm regions, from the change of the dust temperature alone, whereas a T-β model requires β to be known.

Abstract Copyright:

Journal keyword(s): dust, extinction - infrared: ISM - submillimeter: ISM

Nomenclature: Table 1: [PMN2014] Cold clump NN (Nos 1-12).

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 962 3
2 NAME Heart Nebula HII 02 32.7 +61 27           ~ 281 1
3 IC 1848 OpC 02 51 06 +60 24.6   6.87 6.5     ~ 444 2
4 NAME Per Arm PoG 03 30 +45.0           ~ 1247 0
5 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
7 Ass Gem OB 1 As* 06 09.8 +21 35           ~ 166 0
8 [VMF94] 32 cor 12 25 35.6 -71 42 35           ~ 7 0
9 IRAS 17279-3350 HII 17 31 18.0 -33 52 50           ~ 23 0
10 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11533 0
11 NAME Sgr D HII HII 17 48 41.79 -28 01 41.3           ~ 62 1
12 IRAS 17577-2320 HII 18 00 49.6 -23 20 23           ~ 22 0
13 GAL 009.62+00.19 HII 18 06 13.9 -20 31 44           ~ 186 0
14 GAL 013.88+00.28 HII 18 14 35.2 -16 45 21           ~ 53 0
15 [PMN2014] Cold clump 4 smm 18 22 32 -12 59.3           ~ 1 0
16 [PMN2014] Cold clump 2 smm 18 23 21 -13 15.1           ~ 1 0
17 [PMN2014] Cold clump 1 smm 18 23 35 -13 19.7           ~ 1 0
18 [PMN2014] Cold clump 3 smm 18 24 11 -12 57.8           ~ 1 0
19 [PMN2014] Cold clump 8 smm 18 25 20 -12 50.1           ~ 1 0
20 [PMN2014] Cold clump 5 smm 18 25 22 -13 04.6           ~ 1 0
21 [PMN2014] Cold clump 6 smm 18 25 33 -13 01.8           ~ 1 0
22 [PMN2014] Cold clump 7 smm 18 26 22 -12 57.2           ~ 1 0
23 RAFGL 2194 Y*O 18 34 25.210 -07 54 45.06           ~ 19 2
24 [KC97c] G029.1+00.0 HII 18 44 39.4 -03 23 50           ~ 4 0
25 [L89b] 29.205-00.047 HII 18 44 48.0 -03 20 16           ~ 3 0
26 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 331 1
27 [PMN2014] Cold clump 9 smm 18 47 04 -02 43.6           ~ 1 0
28 GAL 031.40-00.26 HII 18 49 32.1 -01 29 04           ~ 41 0
29 RAFGL 5536 HII 18 50 30.8 -00 01 59           ~ 39 0
30 RAFGL 5541 Y*O 18 52 50.376 +00 55 26.48           ~ 16 1
31 [PMN2014] Cold clump 10 smm 19 07 26 +07 49.6           ~ 1 0
32 [PMN2014] Cold clump 11 smm 19 10 22 +08 45.4           ~ 1 0
33 [PMN2014] Cold clump 12 Y*O 19 26 45.310 +17 21 24.42           ~ 6 0
34 SH 2-87 HII 19 46 20.7 +24 35 15           ~ 152 2
35 SH 2-88 B HII 19 46 47.329 +25 12 45.62           ~ 152 2
36 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 618 1
37 IC 1396 OpC 21 39 00 +57 29.4           ~ 445 1
38 V* V733 Cep Or* 22 53 33.2582967602 +62 32 23.630788987     18.57   14.63 ~ 35 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-15:10:10

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