1999A&A...343..585C


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.11CEST10:37:56

1999A&A...343..585C - Astronomy and Astrophysics, volume 343, 585-598 (1999/3-2)

Low and high velocity SiO emission around young stellar objects.

CODELLA C., BACHILLER R. and REIPURTH B.

Abstract (from CDS):

We present a multiline mm-wave survey of SiO emission towards a sample of star-forming regions associated with molecular and Herbig-Haro outflows. The sample includes sources in the northern and southern hemispheres. We extensively mapped some particularly interesting objects (IRAS 00338+6312, HH 7-11 and Cep A). The high detection rate in the sample (52%) confirms that the SiO emission is closely associated with outflows. There exists a trend so that the more intense SiO sources are associated with higher luminosities, with an average LSiO/LIR ratio of 1.8x10–10. The SiO lines exhibit a variety of profiles, ranging from narrow lines (1-3km/s width) at ambient velocities to broad profiles (10-20km/s), with complex profiles consisting of a blend of low and high velocity components as intermediate stages. In the regions where SiO was mapped, the low velocity SiO emission comes from regions definitely offset from the position where the high velocity emission is present, indicating that the low and high velocity SiO emissions trace two distinct regimes. The SiO abundances are different in those two regimes: we estimate that typical SiO abundances are ≃10–9-10–8 in the high velocity components, but they decrease by two orders of magnitude (10–11-10–10) when SiO is detected at low velocities. The hydrogen volume densities estimated from the multiline SiO observations are in the range 105 to fews 106cm–3, in both the low and the high velocity regimes, indicating that all the SiO emission arises in shock-compressed regions. We argue that the different observed SiO profiles could be caused by an evolutionary effect: the SiO molecules produced at high velocities could be slowed down because of their interaction with the surrounding gas before they stick onto the dust grains. However, the possibility that the low velocity SiO emission is due to slow shocks cannot be ruled out, but this would require the presence of a small amount of silicon compounds on the dust grain mantles.

Abstract Copyright:

Journal keyword(s): ISM: clouds - ISM: jets and outflows - ISM: molecules - radio lines: ISM

Simbad objects: 41

goto View the reference in ADS

Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 LDN 1287 DNe 00 36 47.5 +63 29 02           ~ 86 0
2 GM 1-33 HH 00 36 47.5 +63 29 02           ~ 115 0
3 LDN 1448 DNe 03 22.5 +30 35           ~ 480 0
4 IRAS 03222+3034 Y*O 03 25 22.32 +30 45 13.9           ~ 128 0
5 NAME LDN 1455 IRS 1 cor 03 27 39.08 +30 13 03.1           ~ 146 0
6 HH 12 HH 03 28 59.4 +31 20 11           ~ 118 1
7 V* V512 Per Or* 03 29 03.7567945196 +31 16 03.959183877           ~ 359 0
8 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 336 0
9 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1261 1
10 IRAS 03282+3035 cor 03 31 20.98 +30 45 30.1           ~ 164 0
11 HH 366W1 HH 03 46 59.12 +32 45 19.8           ~ 3 0
12 HH 366E1 HH 03 48 32.01 +32 55 34.6           ~ 3 0
13 HH 300A HH 04 25 23.0 +24 23 20           ~ 5 0
14 HH 300C HH 04 25 38.6 +24 26 46           ~ 4 0
15 NAME LDN 1551-4W ? 04 31 17.7 +18 07 46           ~ 2 0
16 LDN 1551 DNe 04 31 30.0 +18 12 30           ~ 780 1
17 RAFGL 5123 Y*O 04 31 34.07736 +18 08 04.9020           K3V/M3III 821 0
18 NAME LDN 1551-2E ? 04 31 42 +18 08.1           ~ 2 0
19 NAME Horsehead Nebula DNe 05 40 59.0 -02 27 30           ~ 458 0
20 LDN 1630 DNe 05 45.5 -00 59           ~ 358 0
21 2MASS J05460363-0014493 Y*O 05 46 03.63 -00 14 49.3           ~ 50 0
22 IRAS 05435-0015 Y*O 05 46 04.775 -00 14 16.51           ~ 60 0
23 HH 26 HH 05 46 05.1 -00 14 17           ~ 94 1
24 M 78 RNe 05 46 45.8 +00 04 45   8.0       ~ 352 0
25 NGC 2071 RNe 05 47 10 +00 18.0           ~ 616 1
26 HH 47C HH 08 25 32.96 -51 01 37.4           ~ 42 0
27 NAME HH 46-47 HH 08 25 43.6 -51 00 36           ~ 186 2
28 2MASS J08254384-5100326 Y*O 08 25 43.85 -51 00 32.7           ~ 299 1
29 HH 47 HH 08 25 44.30 -51 00 26.2           ~ 242 0
30 HH 47D HH 08 26 02 -50 59.4           ~ 47 1
31 HH 56 HH 16 32 29.32 -44 54 57.5           ~ 41 0
32 HH 57 HH 16 32 31.96 -44 55 37.2           ~ 68 1
33 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 243 2
34 HH 100 HH 19 01 49.1 -36 58 16           ~ 79 0
35 IRAS 20050+2720 Y*O 20 07 06.549 +27 28 49.10           ~ 100 0
36 NAME IRAS 20050+2720 Cluster Cl* 20 07 06.7 +27 28 53           ~ 83 0
37 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 508 0
38 RNO 129 Y*O 20 59 14.08512 +78 23 04.0020       15.30   G:e 46 1
39 IRAS 21334+5039 Y*O 21 35 09.10944 +50 53 09.6072           ~ 39 0
40 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 708 2
41 IRAS 22543+6145 HII 22 56 19.1 +62 01 57           ~ 71 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 1999A&A...343..585C and select 'bookmark this link' or equivalent in the popup menu


2021.05.11-10:37:56

© Université de Strasbourg/CNRS

    • Contact