2003A&A...405..639P


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.25CEST10:22:21

2003A&A...405..639P - Astronomy and Astrophysics, volume 405, 639-654 (2003/7-2)

N2H+(1-0) survey of massive molecular cloud cores.

PIROGOV L., ZINCHENKO I., CASELLI P., JOHANSSON L.E.B. and MYERS P.C.

Abstract (from CDS):

We present the results of N2H+(1-0) observations of 35 dense molecular cloud cores from the northern and southern hemispheres where massive stars and star clusters are formed. Line emission has been detected in 33 sources, for 28 sources detailed maps have been obtained. Peak N2H+ column densities lie in the range: 3.6x1012-1.5x1014mc–2. Intensity ratios of (01-12) to (23-12) hyperfine components are slightly higher than the LTE value. The optical depth of (23-12) component toward peak intensity positions of 10 sources is ∼0.2-1. In many cases the cores have elongated or more complex structures with several emission peaks. In total, 47 clumps have been revealed in 26 sources. Their sizes lie in the range 0.3-2.1pc, the range of virial masses is ∼30-3000M. Mean N2H+ abundance for 36 clumps is 5x10–10. Integrated intensity maps with axial ratios <2 have been fitted with a power-law radial distribution ∼r–p convolved with the telescope beam. Mean power-law index for 25 clumps is close to 1.3. For reduced maps where positions of low intensity are rejected mean power-law index is close to unity corresponding to the ∼r–2 density profile provided N2H+ excitation conditions do not vary inside these regions. In those cases where we have relatively extensive and high quality maps, line widths of the cores either decrease or stay constant with distance from the center, implying an enhanced dynamical activity in the center. There is a correlation between total velocity gradient direction and elongation angle of the cores. However, the ratio of rotational to gravitational energy is too low (4x10–4-7.1x10–2) for rotation to play a significant role in the dynamics of the cores. A correlation between mean line widths and sizes of clumps has been found. A comparison with physical parameters of low-mass cores is given.

Abstract Copyright:

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

Simbad objects: 56

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Number of rows : 56

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 46.41432 +63 28 56.2224           ~ 84 0
2 LDN 1287 DNe 00 36 47.5 +63 29 02           ~ 83 0
3 GM 1-33 HH 00 36 47.5 +63 29 02           ~ 112 0
4 NGC 281 HII 00 52 25.1 +56 33 54           ~ 229 1
5 GAL 123.07-06.31 reg 00 52 25.2 +56 33 53           ~ 14 0
6 LBN 126.70-00.80 HII 01 22 58.00 +61 48 16.0           ~ 80 3
7 GAL 133.69+01.22 HII 02 25 28.23 +62 06 57.7           ~ 5 0
8 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 967 3
9 IC 1848 OpC 02 51 06 +60 24.6   6.87 6.5     ~ 447 2
10 NAME W 5 East MoC 03 01 32 +60 29.2           ~ 121 2
11 SH 2-201 HII 03 03 17.9 +60 27 52           ~ 112 0
12 [BE83] Maser 138.50+01.64 Mas 03 03 19.7 +60 27 56           ~ 6 0
13 HHL 5 HII 03 07 24.2 +58 30 45           ~ 143 0
14 RAFGL 490 Y*O 03 27 38.7928323987 +58 47 00.017662871           ~ 341 0
15 GAL 142.00+01.83 ~ 03 27 40.65 +58 47 16.8           ~ 2 0
16 [LMG94] Per 4 PoC 03 29 18.0 +31 27 31           ~ 10 0
17 NGC 1579 HII 04 30 11 +35 16.7           ~ 73 1
18 EM* LkHA 101 Em* 04 30 14.438 +35 16 24.03   17.91 15.71 13.33   F 298 1
19 SH 2-231 HII 05 39 12.9 +35 45 54           ~ 120 0
20 GAL 173.48+02.45 ~ 05 39 12.91 +35 45 54.0           ~ 4 0
21 IRAS 05361+3539 Y*O 05 39 28.64016 +35 40 36.9588           ~ 35 0
22 LBN 189.02+00.91 HII 06 08.5 +21 36           ~ 64 0
23 RAFGL 6366S HII 06 08 41.0 +21 31 01           ~ 82 0
24 SH 2-257 HII 06 12 44 +17 59.3           ~ 122 1
25 NAME SH 2-255 IRS 1 Y*O 06 12 54.0060 +17 59 22.958           ~ 319 0
26 IC 2162 HII 06 13 04.1 +17 58 44           ~ 339 2
27 EM* LkHA 25 Ae* 06 40 44.6381481431 +09 48 02.146205543 12.745 13.03 12.88 12.545 12.386 B4Ve 131 0
28 RAFGL 4519S IR 06 40 45.7 +09 46 33           ~ 8 0
29 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1597 1
30 GAL 264.28+01.48 Mas 08 56 27.8 -43 05 05           ~ 7 0
31 Caswell H2O 267.94-01.06 Mas 08 59 03.6 -47 30 47           ~ 13 0
32 Caswell H2O 265.14+01.45 Mas 08 59 24.7 -43 45 22           ~ 9 0
33 [BSG89] 268.42-0.85 Mas 09 01 54.3 -47 43 59           ~ 7 0
34 [BE83] Maser 269.11-01.12 Mas 09 03 26 -48 25.9           ~ 4 0
35 [BE83] Maser 270.26+00.83 Mas 09 16 43 -47 56.6           ~ 7 0
36 Caswell OH 285.26-00.05 Mas 10 31 30.0 -58 02 07           ~ 21 0
37 NGC 3576 HII 11 11 49.8 -61 18 14           ~ 228 2
38 [BSG89] 294.97-1.73 Mas 11 39 13.94 -63 29 04.6           ~ 13 0
39 Caswell OH 305.36+00.15 Mas 13 12 33.9 -62 37 38           ~ 12 0
40 OH 316.77 -0.02 Mas 14 44 58.8 -59 48 09           ~ 10 0
41 IRAS 16533-4009 HII 16 56 45.58 -40 14 32.4           ~ 46 0
42 GAL 345.2+01.0 HII 16 59 40 -40 11.4           ~ 25 0
43 OH 345.4 -0.9 Mas 17 09 33.8 -41 35 30           ~ 18 0
44 RCW 117 HII 17 09 34.0 -41 36 12           ~ 65 3
45 NAME NGC 6334-I Cl* 17 20 53.35 -35 47 01.5           ~ 274 0
46 NAME NGC 6334F (C) HII 17 20 53.45 -35 47 02.6           ~ 206 1
47 GAL 040.49-02.54 HII 18 56 10.43 +07 53 14.1           ~ 6 0
48 SH 2-76 E SFR 18 56 12 +07 53.4           ~ 32 0
49 SH 2-88 B HII 19 46 47.329 +25 12 45.62           ~ 153 2
50 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 947 0
51 NAME Cyg X FIR 36 Rad 20 39 01.6 +42 22 47           ~ 107 1
52 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 634 2
53 IRAS 22176+6303 Y*O 22 19 17.978 +63 18 52.92           ~ 590 0
54 LDN 1204 DNe 22 26.7 +63 15           ~ 85 1
55 [TW96] T4 PoC 22 28 05.5 +75 13 22           ~ 4 0
56 LBN 108.78-01.01 HII 22 58 37 +58 46.8           ~ 52 0

    Equat.    Gal    SGal    Ecl

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2020.09.25-10:22:21

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