1999A&A...348..600P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.31CET12:12:14

1999A&A...348..600P - Astronomy and Astrophysics, volume 348, 600-613 (1999/8-2)

J=1-0 HCN toward bright far-infrared sources in the outer Galaxy.

PIROGOV L.

Abstract (from CDS):

Result. of the J=1-0 HCN observations toward 34 bright far-infrared sources selected from the IRAS Point Source Catalog are reported. Together with 17 sources observed in this line earlier (Pirogov et al., 1996, A&A Transactions 11, 287) they form a complete sample of the sources with flux densities S(100µm)>500 Jy and δ> 0° in the outer Galaxy. The HCN data are compared with the HCO+, NH3, CS and CO data taken from literature. Prominent correlations with nearly similar slopes of ∼1 are revealed between line integrated intensities of the molecules known to be high density tracers (HCN, HCO+, NH3 and CS). The correlations become higher after adding the data for dark clouds, small globules and cirrus cores implying similar excitation and formation mechanisms of the considered molecules. Collisional excitation in regions with different densities as well as different molecular abundances and velocity dispersions in different types of cores seem to be important in producing these correlations. The following relations hold on the average over ∼3 orders of magnitude of integrated intensities: I(HCN)>I(HCO+)∼I(CS)>I(NH3) where ammonia integrated intensities are several times lower than HCN ones. Correlations are also found between HCN and CO integrated intensities for the sample sources as well as between HCN line widths and those of other species. The HCN lines have the same widths as the HCO+ ones and are larger than CS and especially NH3 line widths. Weak correlations are found between HCN line widths and luminosities of IRAS sources as well as between HCN integrated intensities, IRAS flux densities at 100µm and luminosities of IRAS sources divided by distance squared. The sources with most intense HCN lines have associated water masers and molecular outflows while the lack of associated maser and outflow implies weak or no HCN emission. In order to reproduce the anomalies of the J=1-0 HCN hyperfine structure (R12<0.6) detected in several sources together with suprathermal line widths the model calculations are performed. Two models have been considered: a microturbulent one with a smooth density distribution and a clumpy model. It is found that in the parameter space explored a clumpy model is preferable in comparison with a microturbulent one due to the absence of self-reversals on calculated profiles and the possibility of reproducing HCN profile anomalies and suprathermal line widths. Detailed clumpy model simulations have been performed to fit the observed HCN and H13CN spectra toward S140 IRS1. The best fit model parameters are calculated, including radial dependencies of clump density and volume filling factor.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: clouds - ISM: molecules - radio lines: ISM - ISM: individual objects: S 140

Simbad objects: 85

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Number of rows : 85

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 V* V710 Cas Or* 00 36 45.9929553151 +63 28 52.968310752           ~ 84 0
2 GM 1-33 HH 00 36 47.5 +63 29 02           ~ 112 0
3 NGC 281 HII 00 52 25.1 +56 33 54           ~ 229 1
4 RAFGL 205 IR 01 22 48.6 +61 52 15           ~ 14 1
5 LBN 126.70-00.80 HII 01 22 58.00 +61 48 16.0           ~ 80 3
6 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 330 0
7 NAME W 3 North HII 02 26 51.14 +62 15 47.2           ~ 89 0
8 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 947 2
9 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 968 3
10 IRAS 02244+6117 Y*O 02 28 07.32 +61 30 36.8           ~ 13 0
11 NAME Heart Nebula HII 02 32.7 +61 27           ~ 285 1
12 IC 1805 OpC 02 32 42 +61 27.0   7.03 6.5     ~ 475 2
13 IC 1848 OpC 02 51 06 +60 24.6   6.87 6.5     ~ 448 2
14 NAME AFGL 4029 IRS 1 Y*O 03 01 29.2 +60 29 12           ~ 109 1
15 SH 2-201 HII 03 03 17.9 +60 27 52           ~ 112 0
16 87GB 030326.8+581839 HII 03 07 19 +58 30.2           ~ 9 0
17 HHL 5 HII 03 07 24.2 +58 30 45           ~ 143 0
18 IRAS 03064+5638 HII 03 10 15.3 +56 50 18           ~ 25 0
19 87GB 032059.1+544556 HII 03 24 46 +54 56.5           ~ 20 0
20 IRAS 03211+5446 HII 03 24 59.1 +54 57 25           ~ 27 0
21 RAFGL 490 Y*O 03 27 38.7928323987 +58 47 00.017662871           ~ 341 0
22 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 333 0
23 LZK 12 Y*O 03 29 10.4138336046 +31 21 59.070333199   16.06 14.25     B5:V+F2: 128 0
24 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1231 1
25 NGC 1491 HII 04 03 15.9 +51 18 54           ~ 107 1
26 SH 2-209 HII 04 11 06.7 +51 09 44           ~ 91 0
27 NGC 1579 HII 04 30 11 +35 16.7           ~ 73 1
28 EM* LkHA 101 Em* 04 30 14.438 +35 16 24.03   17.91 15.71 13.33   F 301 1
29 IRAS 04324+5106 Y*O 04 36 21.0058242720 +51 12 55.236611700           ~ 40 1
30 IRAS 04329+5047 IR 04 36 48.5 +50 53 25           ~ 8 0
31 LBN 154.69+02.43 HII 04 36 57 +50 52.6           ~ 40 0
32 LBN 784 HII 05 13 25.5 +37 27 01           ~ 73 0
33 SH 2-230 HII 05 22.5 +34 08           ~ 15 0
34 IRAS 05197+3355 HII 05 23 10.0 +33 58 14           ~ 21 1
35 GAL 174.20-00.08 Cld 05 30 45.9 +33 47 56           ~ 184 2
36 NGC 1931 BNe 05 31 23 +34 14.0     10.1     ~ 116 0
37 NGC 1985 RNe 05 37 47.8 +31 59 24           ~ 130 2
38 CPM 18 Y*O 05 38 47.2 +30 41 28           ~ 24 0
39 IRAS 05358+3543 mul 05 39 10.4 +35 45 19           ~ 136 1
40 NAME SH 2-233 IR Cl* 05 39 10.4 +35 45 19           ~ 93 0
41 SH 2-231 HII 05 39 12.9 +35 45 54           ~ 121 0
42 SH 2-235 B HII 05 40 52.366 +35 41 29.43   17       ~ 172 1
43 BFS 46 HII 05 40 52.90 +35 42 16.7           ~ 50 0
44 SH 2-235 HII 05 41.1 +35 50           ~ 191 0
45 IRAS 05377+3548 mul 05 41 08.5 +35 49 55           ~ 20 0
46 NGC 2071 RNe 05 47 10 +00 18.0           ~ 610 1
47 BFS 48 HII 05 51 07.8 +25 45 36           ~ 12 0
48 IRAS 05480+2544 IR 05 51 07.8 +25 45 36           ~ 12 0
49 IRAS 05480+2545 HII 05 51 10.8 +25 46 14           ~ 24 0
50 LBN 182.30+00.07 HII 05 51 54 +27 01.9           ~ 47 1
51 IRAS 05490+2658 Y*O 05 52 12.9 +26 59 33           ~ 49 0
52 GAL 192.16-03.82 HII 05 58 13.4 +16 32 00           ~ 135 1
53 IRAS 06006+3015 IR 06 03 54.1 +30 14 55           ~ 16 0
54 SH 2-241 HII 06 04.1 +30 15           ~ 55 1
55 LBN 180.71+04.30 RNe 06 04 34.3 +30 30 40           ~ 24 0
56 LBN 189.02+00.91 HII 06 08.5 +21 36           ~ 64 0
57 IRAS 06055+2039 ISM 06 08 32.1 +20 39 18           ~ 54 0
58 SH 2-252 A HII 06 08 33 +20 39.3           ~ 73 0
59 RAFGL 6366S HII 06 08 41.0 +21 31 01           ~ 82 0
60 RAFGL 5180 SFR 06 08 54.1 +21 38 25           ~ 110 0
61 IRAS 06061+2151 SFR 06 09 07.8 +21 50 39           ~ 81 0
62 RAFGL 5183 HII 06 09 21.9 +20 39 28           ~ 40 0
63 NGC 2175 OpC 06 09 39 +20 29.2   7.0 6.8     ~ 248 3
64 RAFGL 5184 IR 06 09 51.7 +20 30 04           ~ 38 0
65 LBN 196.79-03.15 HII 06 10 12.5179825916 +12 48 48.261812212   16.65 15.79     ~ 60 0
66 SH 2-257 HII 06 12 44 +17 59.3           ~ 122 1
67 NAME SH 2-255 IRS 1 Y*O 06 12 54.0060 +17 59 22.958           ~ 319 0
68 IC 2162 HII 06 13 04.1 +17 58 44           ~ 339 2
69 SH 2-258 HII 06 13 28 +17 55.5           ~ 69 0
70 IRAS 06105+1756 HII 06 13 28.338 +17 55 33.02           ~ 29 0
71 LEDA 136208 G 06 14 24.1 +17 44 39           ~ 37 0
72 IRAS 06117+1350 HII 06 14 37.2 +13 49 34           ~ 50 0
73 LBN 196.49-01.60 HII 06 14 38.40 +13 49 44.7           ~ 162 1
74 IRAS 06155+2319A HII 06 18 35.2 +23 18 11           ~ 27 0
75 BFS 51 HII 06 18.7 +23 22           ~ 11 0
76 NGC 2244 OpC 06 31 55 +04 56.5   5.26 4.8     ~ 566 4
77 IRAS 06308+0402 Y*O 06 33 31.1 +04 00 07           ~ 47 1
78 RNO 73 ISM 06 33 31.1 +04 00 07           ~ 19 0
79 RAFGL 961 Y*O 06 34 37.741 +04 12 44.20           ~ 236 1
80 RAFGL 4519S IR 06 40 45.7 +09 46 33           ~ 8 0
81 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1602 1
82 RAFGL 989 Y*O 06 41 10.1592954288 +09 29 33.635497596   17.4 16.8 18.26 17.28 B2 243 0
83 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 635 2
84 IRAS 22176+6303 Y*O 22 19 17.978 +63 18 52.92           ~ 590 0
85 NAME SH 2-140 IRS 1 Y*O 22 19 18.277 +63 18 45.82           ~ 192 0

    Equat.    Gal    SGal    Ecl

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2020.10.31-12:12:14

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