2018A&A...612A..71J


Query : 2018A&A...612A..71J

2018A&A...612A..71J - Astronomy and Astrophysics, volume 612A, 71-71 (2018/4-1)

Herschel and SCUBA-2 observations of dust emission in a sample of Planck cold clumps.

JUVELA M., HE J., PATTLE K., LIU T., BENDO G., EDEN D.J., FEHER O., MICHEL F., FULLER G., HIRANO N., KIM K.-T., LI D., LIU S.-Y., MALINEN J., MARSHALL D.J., PARADIS D., PARSONS H., PELKONEN V.-M., RAWLINGS M.G., RISTORCELLI I., SAMAL M.R., TATEMATSU K., THOMPSON M., TRAFICANTE A., WANG K., WARD-THOMPSON D., WU Y., YI H.-W. and YOO H.

Abstract (from CDS):


Context. Analysis of all-sky Planck submillimetre observations and the IRAS 100µm data has led to the detection of a population of Galactic cold clumps. The clumps can be used to study star formation and dust properties in a wide range of Galactic environments.
Aims. Our aim is to measure dust spectral energy distribution (SED) variations as a function of the spatial scale and the wavelength.
Methods. We examined the SEDs at large scales using IRAS, Planck, and Herschel data. At smaller scales, we compared JCMT/SCUBA-2 850µm maps with Herschel data that were filtered using the SCUBA-2 pipeline. Clumps were extracted using the Fellwalker method, and their spectra were modelled as modified blackbody functions.
Results. According to IRAS and Planck data, most fields have dust colour temperatures TC∼14-18K and opacity spectral index values of β=1.5-1.9. The clumps and cores identified in SCUBA-2 maps have T∼13K and similar β values. There are some indications of the dust emission spectrum becoming flatter at wavelengths longer than 500µm. In fits involving Planck data, the significance is limited by the uncertainty of the corrections for CO line contamination. The fits to the SPIRE data give a median β value that is slightly above 1.8. In the joint SPIRE and SCUBA-2 850µm fits, the value decreases to β∼1.6. Most of the observed T-β anticorrelation can be explained by noise.
Conclusions. The typical submillimetre opacity spectral index β of cold clumps is found to be ∼1.7. This is above the values of diffuse clouds, but lower than in some previous studies of dense clumps. There is only tentative evidence of a T-β anticorrelation and β decreasing at millimetre wavelengths.

Abstract Copyright: © ESO 2018

Journal keyword(s): ISM: clouds - Infrared: ISM - Submillimetre: ISM - dust, extinction - Stars: formation - Stars: protostars

Simbad objects: 45

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Number of rows : 45
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 LDN 1340A PoC 02 28 36 +72 35.9           ~ 6 1
2 LDN 1340C PoC 02 31 43 +72 38.9           ~ 6 1
3 LDN 1457 DNe 02 55.9 +19 35           ~ 85 1
4 LDN 1454 DNe 02 56.8 +20 12           ~ 26 0
5 MBM 12 MoC 02 56 50 +19 32.0           ~ 224 1
6 LDN 1455 DNe 03 28 00.6480 +30 07 58.800           ~ 186 1
7 LDN 1452 DNe 03 28.1 +30 40           ~ 13 0
8 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1363 0
9 LDN 1434 DNe 03 36.1 +37 41           ~ 12 0
10 LDN 1471 DNe 03 48.0 +32 54           ~ 329 0
11 LDN 1443 DNe 04 00.4 +40 48           ~ 9 0
12 LDN 1459 DNe 04 08.4 +39 38           ~ 16 0
13 LDN 1501 DNe 04 15.0 +25 07           ~ 6 0
14 LDN 1394 DNe 04 17.0 +55 17           ~ 7 0
15 LDN 1495 DNe 04 18.1 +27 37           ~ 366 1
16 LDN 1400H DNe 04 18 13.0 +55 13 05           ~ 4 0
17 LDN 1506 DNe 04 20.0 +25 17           ~ 78 0
18 Barnard 213 DNe 04 20 51 +27 16.3           ~ 217 0
19 LDN 1478 DNe 04 23.3 +37 07           ~ 22 0
20 LDN 1399 DNe 04 24.0 +55 04           ~ 19 0
21 LDN 1400 DNe 04 25.0 +54 57           ~ 22 0
22 LDN 1543 DNe 04 27.4 +18 52           ~ 13 0
23 MBM 107 MoC 04 27.4 +18 52           ~ 4 0
24 LDN 1524 DNe 04 27 57.7 +24 39 18           ~ 83 0
25 LDN 1407 DNe 04 29 59 +54 16.5           ~ 30 0
26 NAME Kutner's Cloud MoC 04 32 44.6 +24 23 13           ~ 272 0
27 LDN 1521 DNe 04 33.1 +26 06           ~ 60 0
28 LDN 1536 DNe 04 33 24.6 +22 43 29           ~ 111 0
29 LDN 1642 MoC 04 35 18 -14 13.9           ~ 153 0
30 LDN 1483 DNe 04 35 19 +36 26.1           ~ 11 0
31 IRAS 04325+2402 Y*O 04 35 35.39160 +24 08 19.4244           ~ 159 0
32 LDN 1528 DNe 04 37.1 +25 46           ~ 10 0
33 LDN 1532 DNe 04 40.1 +25 46           ~ 5 0
34 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4412 0
35 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1673 0
36 LDN 1534 DNe 04 41 46 +25 41.4           ~ 45 0
37 LDN 1426 DNe 04 47.0 +53 05           ~ 8 0
38 LDN 1652 DNe 06 26.4 -10 02           ~ 17 0
39 MBM 148 MoC 16 48.3 -11 05           ~ 3 0
40 LDN 234 DNe 16 48.8 -11 05           ~ 12 0
41 LDN 841 DNe 20 11.0 +33 09           ~ 4 0
42 LDN 1228 DNe 20 57 13 +77 35.8           ~ 128 0
43 MBM 162 MoC 20 59.0 +77 32           ~ 2 0
44 LDN 1241 DNe 21 50.0 +76 44           ~ 19 0
45 NAME Cepheus Flare MoC 23 34 +72.0           ~ 128 0

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