2007MNRAS.382.1213G


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.31CET11:44:15

2007MNRAS.382.1213G - Mon. Not. R. Astron. Soc., 382, 1213-1224 (2007/December-2)

A survey of SiO 5 ⟶ 4 emission towards outflows from massive young stellar objects.

GIBB A.G., DAVIS C.J. and MOORE T.J.T.

Abstract (from CDS):

Result. are presented of a survey of SiO 5 ⟶ 4 emission observed with the James Clerk Maxwell Telescope towards a sample of outflows from massive young stellar objects. The sample is drawn from a single-distance study by Ridge & Moore and allows the reasons that govern the detectability of SiO to be explored without the bias introduced by observing sources at different distances. This is the first such unbiased survey of SiO emission from massive outflows. In a sample of 12 sources, the 5 ⟶ 4 line was detected in five, a detection rate of 42 per cent. This detection rate is higher than that found for a sample of low-luminosity outflow sources, although for sources of comparable luminosity, it is in good agreement with the results of a previous survey of high-luminosity sources. For most of the detected sources, the 5 ⟶ 4 emission is compact or slightly extended along the direction of the outflow. NGC6334I shows a clear bipolar flow in the 5 ⟶ 4 line. Additional data were obtained for W3-IRS5, AFGL5142 and W75N for the 2 ⟶ 1 transition of SiO using the Berkeley-Illinois-Maryland Association millimetre interferometer. There is broad agreement between the appearance of the SiO emission in both lines, though there are some minor differences. The 2 ⟶ 1 emission in AFGL5142 is resolved into two outflow lobes which are spatially coincident on the sky, in good agreement with previous observations. In general, the SiO emission is clearly associated with the outflow. Simple analysis and radiative transfer modelling of the detected sources yields similar SiO column densities. The abundance of SiO is ∼0.1-7.0x10–9, and the H2 number density is within a factor of 2 of 105/cm3. However, the temperature is not constrained over the range 50-150K. The primary indicator of SiO 5 ⟶ 4 detectability is the outflow velocity, that is, the presence of SiO is an indicator of a high-velocity outflow. This result is consistent with the existence of a critical shock velocity required to disrupt dust grains and subsequent SiO formation in post-shock gas. There is also weak evidence that higher luminosity sources and denser outflows are more likely to be detected.

Abstract Copyright: 2007 The Authors. Journal compilation © 2007 RAS

Journal keyword(s): stars: formation - ISM: abundances - ISM: jets and outflows - ISM: molecules - radio lines: ISM

CDS comments: G34.3 not identified.

Simbad objects: 28

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Number of rows : 28

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 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 330 0
2 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 947 2
3 HHL 5 HII 03 07 24.2 +58 30 45           ~ 143 0
4 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3582 3
5 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 304 0
6 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 242 1
7 NAME HH 211-mm Y*O 03 43 56.816 +32 00 50.06           ~ 56 1
8 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 862 1
9 GAL 174.20-00.08 Cld 05 30 45.9 +33 47 56           ~ 184 2
10 NGC 1985 RNe 05 37 47.8 +31 59 24           ~ 130 2
11 GAL 192.16-03.82 HII 05 58 13.4 +16 32 00           ~ 135 1
12 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1058 1
13 [KRL2007b] 236 AGN 17 20 21.81 -35 52 48.2           ~ 101 0
14 NAME NGC 6334-I Cl* 17 20 53.35 -35 47 01.5           ~ 277 0
15 NAME NGC 6334F (C) HII 17 20 53.45 -35 47 02.6           ~ 209 1
16 NAME HH 80-81 HH 18 19 06 -20 51.4           ~ 195 0
17 NAME HH 80-81 IRS HII 18 19 11.8 -20 47 35           ~ 134 0
18 GAL 035.2-00.74 MoC 18 58 13 +01 40.6           ~ 153 0
19 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 92 0
20 IRAS 18556+0136 mul 18 58 13.1 +01 40 35           ~ 133 0
21 [MSM95] G35.20 FIR 1 FIR 18 58 13.2 +01 40 26           ~ 8 0
22 SH 2-88 B HII 19 46 47.329 +25 12 45.62           ~ 153 2
23 IRAS 19550+3248 HII 19 56 56.0 +32 56 34           ~ 11 0
24 LBN 077.61+01.59 HII 20 20 39.3 +39 37 52           ~ 74 0
25 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 634 1
26 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 710 0
27 NAME Cyg X FIR 33 Y*O 20 38 35.9 +42 37 22           B1.5 360 1
28 [S2001] MM 1 mm 20 38 36.39 +42 37 34.1           ~ 11 0

    Equat.    Gal    SGal    Ecl

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2020.10.31-11:44:15

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