CDS

2008A&A...485..497S

Query : 2008A&A...485..497S

2008A&A...485..497S - Astronomy and Astrophysics, volume 485, 497-515 (2008/7-2)

Survey of intermediate/high mass star-forming regions at centimeter and millimeter wavelengths.

SANCHEZ-MONGE A., PALAU A., ESTALELLA R., BELTRAN M.T. and GIRART J.M.

Abstract (from CDS):

The goal of this work is to characterize the millimeter and centimeter properties of intermediate/high mass young stellar objects (YSOs) to search for any evolutionary trends.We carried out observations at 1.2mm with the IRAM 30m telescope, and at 3.6 and 1.3cm with the VLA toward a sample of 11 luminous (>103L☉) IRAS sources classified as high mass protostellar object candidates. The most promising regions additionally were observed at 7mm with the VLA. The 1.2mm emission, tracing the dust core in which the massive YSO is forming, shows a clear peak surrounded by some substructure in most cases, while in others it is very extended and weak. The masses from the 1.2mm data range from 10 to 140M☉. For all (but one) of the sources, we detected centimeter emission associated with the IRAS source, with spectral indices between 3.6 and 1.3cm typical of optically thin emission, and deconvolved sizes from <0.01 to 0.3pc, suggesting that the emission comes from compact or ultra-compact (UC) HII regions. The physical parameters of the UCHII regions indicate that the ionizing stars are early B-type. The 7mm emission is partially resolved for the four regions observed at this wavelength, and we estimated the contribution of the dust emission to the 7mm flux density, ranging from negligible to 45%. By combining our data with infrared surveys, we built the spectral energy distribution and fitted a modified blackbody law. We found dust temperatures between 25 and 35K, dust emissivity indices between 1.5 and 2.2, and masses similar to the masses derived from the 1.2mm continuum emission. In addition, we found a correlation between the degree of disruption of the natal cloud, estimated from the fraction of dust emission associated with the centimeter source relative to the total amount of dust in its surroundings, and the size of the centimeter source.From the correlation found, we established an evolutionary sequence in which sources with compact millimeter emission clearly associated with compact centimeter emission are younger than sources with the millimeter emission dispersed and with the centimeter emission extended. Such a sequence is consistent with the evolutionary stage expected from maser/outflow/dense gas emission reported in the literature, and with the infrared excess of the 2MASS sources associated with the centimeter source.

Abstract Copyright: ∼

Journal keyword(s): stars: formation - ISM: dust, extinction - ISM: HII regions - radio continuum: ISM

Nomenclature: Tables 6, 7: [SPE2008b] IRAS HHMMm+DDMM VLA N, [SPE2008b] NGC 7538 IRS9 VLA N, N=38. Table 8: [SPE2008b] IRAS 22187+5559 VLA Na (Nos 5a-5d).

CDS comments: Table 10 IRAS 18171-1845 is a probable misprint for IRAS 18171-1548. Table 3 IRAS 2344+010 is a misprint for IRAS 23448+6010.

Simbad objects: 63

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Number of rows : 63
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023 		#notes
1 [SPE2008b] IRAS 00117+6412 VLA 1 Rad 00 14 22.26 +64 28 28.7           ~ 1 0
2 IRAS 00117+6412 HII 00 14 26.61 +64 28 30.3           ~ 38 0
3 [SPE2008b] IRAS 00117+6412 VLA 3 HII 00 14 28.12 +64 28 46.2           ~ 2 0
4 [SPE2008b] IRAS 00117+6412 VLA 2 HII 00 14 28.12 +64 28 46.2           ~ 1 0
5 3C 48 QSO 01 37 41.2996631208 +33 09 35.080388820   16.62 16.20     ~ 2750 2
6 IRAS 04579+4703 Y*O 05 01 39.661 +47 07 21.92           ~ 49 0
7 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4217 2
8 IRAS 15502-5302 HII 15 54 07.2 -53 11 20           ~ 45 0
9 MSX6C G332.1544-00.4487 HII 16 16 40.776 -51 17 06.36           ~ 35 1
10 [SPE2008b] IRAS 18123-1203 VLA 1 Rad 18 15 01.36 -12 01 43.2           ~ 1 0
11 IRAS 18123-1203 HII 18 15 07.3 -12 02 42           ~ 14 0
12 [SPE2008b] IRAS 18123-1203 VLA 2 Rad 18 15 07.55 -12 01 43.3           ~ 1 0
13 [SPE2008b] IRAS 18123-1203 VLA 3 Rad 18 15 08.01 -12 05 10.0           ~ 1 0
14 [SPE2008b] IRAS 18123-1203 VLA 4 Rad 18 15 08.05 -12 01 58.0           ~ 1 0
15 [SPE2008b] IRAS 18123-1203 VLA 5 Rad 18 15 08.12 -12 01 38.0           ~ 1 0
16 [SPE2008b] IRAS 18123-1203 VLA 6 Rad 18 15 08.75 -12 01 58.0           ~ 1 0
17 [SPE2008b] IRAS 18123-1203 VLA 7 Rad 18 15 14.42 -11 59 32.0           ~ 1 0
18 IRAS 18172-1548 IR 18 20.1 -15 47           ~ 4 0
19 [SPE2008b] IRAS 18171-1548 VLA 1 HII 18 20 06.40 -15 46 44.1           ~ 2 0
20 IRAS 18171-1548 MIR 18 20 06.400 -15 46 43.91           ~ 7 0
21 IRAS 18212-1320 IR 18 24 04.7 -13 19 16           ~ 11 0
22 [SPE2008b] IRAS 19045+0813 VLA 1 Rad 19 06 50.61 +08 19 20.6           ~ 1 0
23 [SPE2008b] IRAS 19045+0813 VLA 2 Rad 19 06 58.64 +08 18 58.3           ~ 1 0
24 [SPE2008b] IRAS 19045+0813 VLA 3 Rad 19 06 59.34 +08 18 56.7           ~ 1 0
25 [SPE2008b] IRAS 19045+0813 VLA 4 Rad 19 06 59.63 +08 19 08.9           ~ 1 0
26 [SPE2008b] IRAS 19045+0813 VLA 5 Rad 19 06 59.77 +08 19 19.1           ~ 1 0
27 [SPE2008b] IRAS 19045+0813 VLA 6 Rad 19 07 00.12 +08 19 09.9           ~ 1 0
28 [SPE2008b] IRAS 19045+0813 VLA 7 HII 19 07 00.45 +08 18 44.5           ~ 2 0
29 [BNM96] 042.096+0.354 Y*O 19 07 00.527 +08 18 44.48           ~ 16 0
30 [SPE2008b] IRAS 20293+4007 VLA 1 Rad 20 31 07.17 +40 17 20.9           ~ 1 0
31 [SPE2008b] IRAS 20293+4007 VLA 2 HII 20 31 07.19 +40 17 27.1           ~ 1 0
32 IRAS 20293+4007 Cld 20 31 07.9 +40 17 23           ~ 9 0
33 [SPE2008b] IRAS 20293+4007 VLA 3 Rad 20 31 19.11 +40 18 09.7           ~ 1 0
34 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 653 2
35 IRAS 22176+6303 Y*O 22 19 17.978 +63 18 52.92           ~ 592 0
36 LDN 1204G cor 22 19 19.1 +63 18 51           ~ 10 0
37 [SPE2008b] IRAS 22187+5559 VLA 1 Rad 22 20 32.01 +56 14 53.5           ~ 1 0
38 [SPE2008b] IRAS 22187+5559 VLA 2 Rad 22 20 33.45 +56 15 01.5           ~ 1 0
39 [SPE2008b] IRAS 22187+5559 VLA 3 cor 22 20 33.67 +56 14 26.4           ~ 2 0
40 [SPE2008b] IRAS 22187+5559 VLA 4 Rad 22 20 34.51 +56 14 57.6           ~ 1 0
41 IRAS 22187+5559 IR 22 20 34.9 +56 14 39           ~ 15 0
42 [SPE2008b] IRAS 22187+5559 VLA 5a Rad 22 20 35.27 +56 14 36.2           ~ 1 0
43 [SPE2008b] IRAS 22187+5559 VLA 5b Rad 22 20 35.56 +56 14 45.4           ~ 1 0
44 JCMTSE J222036.6+561450 cor 22 20 35.58 +56 14 45.3           ~ 3 0
45 [SPE2008b] IRAS 22187+5559 VLA 5c Rad 22 20 36.10 +56 14 41.7           ~ 1 0
46 [SPE2008b] IRAS 22187+5559 VLA 5d Rad 22 20 36.27 +56 14 38.1           ~ 1 0
47 LDN 1204A DNe 22 21 22.5 +63 51 13           ~ 104 0
48 [SPE2008b] IRAS 22198+6336 VLA 1 Rad 22 21 24.48 +63 52 20.2           ~ 1 0
49 [SPE2008b] IRAS 22198+6336 VLA 2 HII 22 21 26.68 +63 51 38.2           ~ 3 0
50 NGC 7538 OpC 23 13 37 +61 30.0           ~ 859 1
51 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 404 3
52 [SPE2008b] NGC 7538 IRS9 VLA 1 Rad 23 13 45.47 +61 28 19.7           ~ 1 0
53 [TGJ91] NGC 7538 IRS 9 Peak A1 HII 23 14 01.10 +61 27 18.8           ~ 3 0
54 [SPE2008b] NGC 7538 IRS9 VLA 3 HII 23 14 01.79 +61 27 20.0           ~ 1 0
55 IRAS 23118+6110 Y*O 23 14 02.09473 +61 27 18.8460           ~ 369 0
56 [SPE2008b] IRAS 23448+6010 VLA 1 HII 23 47 16.29 +60 27 13.6           ~ 1 0
57 IRAS 23448+6010 SFR 23 47 19.8 +60 27 23           ~ 17 0
58 [SPE2008b] IRAS 23448+6010 VLA 2 HII 23 47 20.08 +60 27 22.8           ~ 1 0
59 [SPE2008b] IRAS 23448+6010 VLA 4 Rad 23 47 21.97 +60 27 48.3           ~ 1 0
60 [SPE2008b] IRAS 23448+6010 VLA 5 Rad 23 47 22.47 +60 27 12.7           ~ 1 0
61 [SPE2008b] IRAS 23448+6010 VLA 6 Rad 23 47 23.21 +60 27 33.8           ~ 1 0
62 NAME LDN 1204/SH 2-140 Complex ? ~ ~           ~ 4 0
63 [SPE2008b] IRAS 23448+6010 VLA 3 HII ~ ~           ~ 1 0

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2023.06.09-23:01:50

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