2005A&A...432..921F

Query : 2005A&A...432..921F

2005A&A...432..921F - Astronomy and Astrophysics, volume 432, 921-935 (2005/3-4)

Search for massive protostellar candidates in the southern hemisphere. I. Association with dense gas.

FONTANI F., BELTRAN M.T., BRAND J., CESARONI R., TESTI L., MOLINARI S. and WALMSLEY C.M.

Abstract (from CDS):

We have observed two rotational transitions of both CS and C17O, and the 1.2 mm continuum emission towards a sample of 130 high-mass protostellar candidates with δ←30°. This work represents the first step of the extension to the southern hemisphere of a project started more than a decade ago aimed at the identification of massive protostellar candidates. Following the same approach adopted for sources with δ≥-30°, we have selected from the IRAS Point Source Catalogue 429 sources which potentially are compact molecular clouds on the basis of their IR colours. The sample has then been divided into two groups according to the colour indices [25-12] and [60-12]: the 298 sources with [25-12]≥0.57 and [60-12]≥1.30 have been called High sources, the remaining 131 have been called Low sources. In this paper, we check the association with dense gas and dust in 130 Low sources. We have obtained a detection rate of ∼85% in CS, demonstrating a tight association of the sources with dense molecular clumps. Among the sources detected in CS, ∼76% have also been detected in C17O and ∼93% in the 1.2mm continuum. Millimeter-continuum maps show the presence of clumps with diameters in the range 0.2-2 pc and masses from a few M☉ to 105M☉; H2 volume densities computed from CS line ratios lie between ∼104.5 and 105.5cm–3. The bolometric luminosities of the sources, derived from IRAS data, are in the range 103-106L☉, consistent with embedded high-mass objects. Based on our results and those found in the literature for other samples of high-mass young stellar objects, we conclude that our sources are massive objects in a very early evolutionary stage, probably prior to the formation of an HII region. We propose a scenario in which High and Low sources are both made of a massive clump hosting a high-mass protostellar candidate and a nearby stellar cluster. The difference might be due to the fact that the 12µm IRAS flux, the best discriminant between the two groups, is dominated by the emission from the cluster in Lows and from the massive protostellar object in Highs.

Abstract Copyright: ∼

Journal keyword(s): stars: formation - radio lines: ISM - ISM: molecules

VizieR on-line data: <Available at CDS (J/A+A/432/921): tablea1.dat tablea2.dat tablea3.dat tablea4.dat tablea5.dat tablea6.dat>

Simbad objects: 134

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Number of rows : 134
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 IRAS 08211-4158 IR 08 22 52.08 -42 07 53.7           ~ 25 0
2 IRAS 08247-4223 IR 08 26 27.6 -42 33 05           ~ 12 1
3 IRAS 08477-4359 cor 08 49 32.3 -44 10 46           ~ 20 0
4 TGU H1699 DNe 08 50 38.683 -45 08 20.80           G3V 9 0
5 IRAS 08563-4225 Cl* 08 58 12.5 -42 37 34           ~ 12 0
6 IRAS 09014-4736 Y*? 09 03 09.4897804392 -47 48 27.703882296           ~ 23 1
7 IRAS 09026-4842 IR 09 04 22.145 -48 54 21.28           ~ 7 0
8 IRAS 09131-4723 IR 09 14 55.5 -47 36 13           ~ 8 1
9 IRAS 09166-4813 IR 09 18 26.6 -48 26 26           ~ 5 1
10 IRAS 09209-5143 * 09 22 34.6 -51 56 23           M0V: 4 0
11 IRAS 10088-5730 IR 10 10 38.8 -57 45 32           ~ 1 0
12 2MASX J10111502-5858084 G 10 11 15.026 -58 58 08.43           ~ 8 0
13 IRAS 10102-5706 IR 10 12 03.7 -57 21 26           ~ 2 0
14 IRAS 10123-5727 IR 10 14 08.8 -57 42 12           ~ 9 0
15 IRAS 10156-5804 IR 10 17 26.8 -58 19 46           ~ 1 0
16 IRAS 10277-5730 IR 10 29 35.4 -57 45 34           ~ 6 0
17 IRAS 10308-6122 IR 10 32 39.8 -61 37 33           ~ 7 0
18 IRAS 10317-5936 IR 10 33 38.1 -59 51 54           ~ 3 0
19 IRAS 10439-5941 HII 10 45 54.0 -59 57 03           ~ 12 0
20 IRAS 10521-6031 IR 10 54 10.1 -60 47 30           ~ 2 0
21 IRAS 10537-5930 IR 10 55 49.0 -59 46 47           ~ 6 0
22 IRAS 10545-6244 IR 10 56 32.7880242624 -63 00 33.492111480           ~ 4 0
23 IRAS 10548-5929 IR 10 56 52.0 -59 45 13           ~ 3 0
24 IRAS 10554-6237 Ae? 10 57 24.2600129736 -62 53 13.240645908 15.21 15.35 14.45     B1 12 0
25 IRAS 10555-5949 IR 10 57 36.9 -60 05 35           ~ 3 0
26 IRAS 10572-6018 IR 10 59 19.4 -60 34 04           ~ 2 0
27 ESO 128-25 PN? 10 59 40.499 -59 01 10.56           ~ 14 1
28 IRAS 10591-5934 IR 11 01 15.8 -59 51 01           ~ 12 1
29 IRAS 11265-6158 MIR 11 28 51.59040 -62 15 06.1236           ~ 4 0
30 IRAS 11294-6257 IR 11 31 46.5 -63 14 25           ~ 5 0
31 IRAS 11380-6311 IR 11 40 27.6 -63 27 56           ~ 4 0
32 IRAS 11396-6202 IR 11 42 01.6 -62 19 24           ~ 3 0
33 IRAS 11404-6215 IR 11 42 48.0 -62 32 20           ~ 2 0
34 IRAS 11476-6435 IR 11 50 08.0 -64 52 20           ~ 4 0
35 IRAS 12102-6133 Cld 12 12 57.49680 -61 50 17.4300           ~ 6 0
36 IRAS 12295-6224 IR 12 32 22.7 -62 41 25           ~ 3 0
37 IRAS 12377-6237 IR 12 40 42.1536173592 -62 54 09.114408396           ~ 2 0
38 IRAS 12434-6355 IR 12 46 24.6 -64 11 26           ~ 6 0
39 IRAS 13023-6213 IR 13 05 30.7 -62 29 58           ~ 1 0
40 IRAS 13039-6108 MIR 13 07 06.4 -61 24 29           ~ 10 0
41 IRAS 13078-6247 IR 13 11 04.9721258352 -63 03 49.126319064           ~ 3 0
42 IRAS 13106-6050 Y*O 13 13 49.14120 -61 06 29.8368           ~ 6 0
43 RAFGL 4902S IR 13 36 45.7 -62 49 36           ~ 4 0
44 IRAS 13384-6152 IR 13 41 54.3593801472 -62 07 34.384826568           ~ 4 0
45 RAFGL 4176 Y*O 13 43 01.70352 -62 08 51.2304           ~ 152 0
46 [GGB2012] G308.9176+00.1231 HII 13 43 02.1 -62 08 52           ~ 59 0
47 IRAS 13438-6203 IR 13 47 21.9 -62 18 41           ~ 6 0
48 IRAS 13481-6124 Y*O 13 51 37.85568 -61 39 07.5168           ~ 52 0
49 IRAS 13558-6159 IR 13 59 27.0 -62 13 40           ~ 3 0
50 IRAS 13560-6133 IR 13 59 35.3 -61 48 17           ~ 3 0
51 IRAS 14000-6104 IR 14 03 38.0 -61 17 56           ~ 11 0
52 IRAS 14131-6126 IR 14 16 48.5095062552 -61 40 25.762901448           ~ 3 0
53 IRAS 14166-6118 IR 14 20 19.5 -61 31 53           ~ 4 0
54 IRAS 14183-6050 IR 14 22 03.6 -61 04 22           ~ 6 0
55 IRAS 14198-6115 LP? 14 23 32.0950205040 -61 28 47.725841532           ~ 8 0
56 IRAS 14201-6044 IR 14 23 54.53 -60 57 48.6           ~ 3 0
57 IRAS 14395-5941 IR 14 43 20.9 -59 53 54           ~ 2 0
58 IRAS 14412-5948 IR 14 45 04.1 -60 01 14           ~ 2 0
59 IRAS 14425-6023 MIR 14 46 23.37 -60 35 45.6           ~ 10 0
60 IRAS 14591-5843 IR 15 02 58.8 -58 55 06           ~ 2 0
61 IRAS 15038-5828 MIR 15 07 45.0218180184 -58 40 00.805611468           ~ 2 0
62 IRAS 15072-5855 IR 15 11 07.9 -59 06 30           ~ 2 0
63 IRAS 15100-5903 IR 15 14 00.1 -59 15 09           ~ 4 0
64 IRAS 15178-5641 IR 15 21 45.4 -56 52 42           ~ 2 0
65 IRAS 15219-5658 IR 15 25 48.7 -57 09 11           ~ 2 0
66 IRAS 15239-5538 IR 15 27 49.3 -55 48 42           ~ 2 0
67 IRAS 15246-5612 IR 15 28 32.7 -56 23 00           ~ 11 0
68 IRAS 15262-5541 IR 15 30 05.6 -55 52 01           ~ 2 0
69 IRAS 15347-5518 IR 15 38 36.0 -55 28 07           ~ 5 0
70 IRAS 15371-5458 MIR 15 40 59.22360 -55 08 17.1852           ~ 1 0
71 IRAS 15470-5419 IR 15 50 55.2 -54 28 22           ~ 2 0
72 IRAS 15506-5325 IR 15 54 32.2 -53 33 53           ~ 4 0
73 IRAS 15519-5430 IR 15 55 50.4667609152 -54 38 59.656961040           ~ 13 0
74 GRS G328.59 -00.52 bub 15 59 28.4 -53 44 57           ~ 43 1
75 IRAS 15557-5337 MIR 15 59 36.64 -53 45 53.3           ~ 19 0
76 IRAS 15571-5218 IR 16 01 00.4 -52 27 13           ~ 1 0
77 OH 329.2-00.3 Mas 16 01 47.01 -53 11 43.3           ~ 34 0
78 IRAS 15579-5303 of? 16 01 47.18424 -53 11 44.1780           ~ 36 0
79 IRAS 15579-5347 IR 16 01 52.54 -53 56 28.3           ~ 6 0
80 IRAS 15583-5314 IR 16 02 10.1 -53 22 35           ~ 2 0
81 IRAS 16061-5048 Cld 16 09 57.3 -50 56 45           ~ 5 0
82 IRAS 16082-5031 IR 16 12 03.2 -50 39 16           ~ 6 0
83 IRAS 16093-5015 IR 16 13 05.2 -50 23 05           ~ 6 0
84 IRAS 16093-5128 IR 16 13 09.2 -51 36 26           ~ 2 0
85 IRAS 16106-5048 IR 16 14 26.8 -50 56 12           ~ 2 0
86 IRAS 16107-4956 IR 16 14 29.4 -50 03 51           ~ 2 0
87 IRAS 16148-5011 SFR 16 18 37.104 -50 18 58.32           ~ 12 0
88 IRAS 16153-5016 * 16 19 07.0731110208 -50 24 11.920048272           ~ 7 0
89 IRAS 16170-5053 IR 16 20 53.2 -51 00 14           ~ 6 0
90 IRAS 16187-4932 Cld 16 22 29.3 -49 39 02           ~ 2 0
91 IRAS 16194-4934 IR 16 23 13.2 -49 40 59           ~ 2 0
92 IRAS 16204-4916 IR 16 24 12.3 -49 23 34           ~ 1 0
93 IRAS 16204-4943 IR 16 24 15.5 -49 50 05           ~ 2 0
94 IRAS 16218-4931 IR 16 25 37.9 -49 38 20           ~ 2 0
95 2MASS J16254034-4855155 Y*? 16 25 40.35 -48 55 15.6           ~ 6 0
96 IRAS 16231-4819 IR 16 26 49.1 -48 25 49           ~ 3 0
97 LEDA 101328 G 16 27 03.3 -49 23 59   18.0       ~ 11 0
98 IRAS 16252-4853 IR 16 29 01.6 -48 59 48           ~ 2 0
99 IRAS 16254-4844 IR 16 29 09.0 -48 51 27           ~ 1 0
100 IRAS 16344-4605 mul 16 38 08.6 -46 11 10           ~ 3 0
101 IRAS 16358-4614 IR 16 39 29.4 -46 20 44           ~ 1 0
102 IRAS 16363-4645 mul 16 40 00.5 -46 51 32           ~ 9 0
103 IRAS 16369-4810 MIR 16 40 38.463 -48 16 02.78           ~ 2 0
104 IRAS 16403-4614 IR 16 44 01.5 -46 20 27           ~ 3 0
105 IRAS 16404-4518 IR 16 44 05.9 -45 23 53           ~ 1 0
106 IRAS 16417-4445 IR 16 45 19.9 -44 51 00           ~ 3 0
107 IRAS 16419-4602 IR 16 45 37.9 -46 07 49           ~ 3 0
108 IRAS 16428-4109 IR 16 46 22.6 -41 14 58           ~ 3 0
109 IRAS 16464-4359 HII 16 50 01.0 -44 05 03           ~ 5 0
110 IRAS 16501-4314 mul 16 53 41.0 -43 19 22           ~ 7 0
111 IRAS 16535-4300 IR 16 57 05.5 -43 05 20           ~ 4 0
112 IRAS 16573-4214 IR 17 00 54.3 -42 19 10           ~ 6 0
113 IRAS 16581-4212 IR 17 01 38.8 -42 17 05           ~ 1 0
114 IRAS 17033-4035 IR 17 06 49.3 -40 39 51           ~ 5 0
115 IRAS 17036-4033 IR 17 07 08.9 -40 37 08           ~ 3 0
116 IRAS 17040-3959 IR 17 07 33.7 -40 03 04           ~ 2 0
117 IRAS 17082-4114 IR 17 11 46.2 -41 18 03           ~ 3 0
118 IRAS 17114-3804 IR 17 14 52.2 -38 07 26           ~ 2 0
119 IRAS 17140-3747 IR 17 17 28.1 -37 51 06           ~ 1 0
120 IRAS 17141-3606 IR 17 17 28.2 -36 09 38           ~ 1 0
121 IRAS 17156-3607 IR 17 19 01.2 -36 10 12           ~ 1 0
122 IRAS 17211-3537 Y*O 17 24 27.60888 -35 40 09.3000           ~ 15 0
123 IRAS 17218-3704 IR 17 25 14.0 -37 07 29           ~ 1 0
124 IRAS 17225-3426 IR 17 25 50.3 -34 29 21           ~ 3 0
125 IRAS 17230-3531 IR 17 26 26.3 -35 33 35           ~ 2 0
126 IRAS 17256-3631 HII 17 29 01.1 -36 33 38           ~ 10 0
127 IRAS 17285-3346 IR 17 31 48.1 -33 48 23           ~ 3 0
128 GAL 357.46+00.60 CGb 17 37 03.9 -30 46 17           ~ 5 0
129 IRAS 17355-3241 LP? 17 38 50.4236908608 -32 43 33.592917468           ~ 6 0
130 IRAS 17368-3057 HII 17 40 05.69664 -30 58 56.4060           ~ 12 1
131 IRAS 17377-3109 IR 17 40 57.21 -31 10 58.2           ~ 6 0
132 IRAS 17410-3019 IR 17 44 14.9 -30 20 42           ~ 2 0
133 IRAS 17419-3207 IR 17 45 10.4 -32 08 48           ~ 4 0
134 IRAS 17425-3017 IR 17 45 45.1 -30 18 51           ~ 2 0

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