2014A&A...570A...1D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST08:20:18

2014A&A...570A...1D - Astronomy and Astrophysics, volume 570A, 1-1 (2014/10-1)

SiO emission from low- and high-velocity shocks in Cygnus-X massive dense clumps.

DUARTE-CABRAL A., BONTEMPS S., MOTTE F., GUSDORF A., CSENGERI T., SCHNEIDER N. and LOUVET F.

Abstract (from CDS):

The SiO molecule is formed through interstellar shocks and is often used as a tracer of high-velocity shocks from protostellar outflows. However, recent studies have suggested that low-velocity shocks in the interstellar medium can be responsible for a significant amount of SiO emission observed in star-forming regions. We aim to investigate the existence of SiO emission that may or may not be associated with outflow shocks, within several massive dense clumps (MDCs), and explore how the SiO luminosities compare with the outflow properties estimated using CO. We used observations of SiO (2-1) from the Plateau de Bure Interferometre, towards a sample of six MDCs in Cygnus-X, and compared them to the CO high-velocity outflow emission, and to the velocity shears found in these regions. We find that most molecular outflows are detected in both SiO and CO, although there are some cases of CO outflows with no SiO counterpart. The data also shows narrow line SiO emission (σv≲1.5km/s) which, in some cases, appears to be unrelated to outflows. The kinematics of this narrow emission often differs from those found by other high-density tracers such as H13CO+, and its extent varies from rather compact (∼0.03pc) to widespread (∼0.2pc). We find that the least centrally concentrated clumps with the least massive protostellar cores have the most widespread narrow SiO emission. The fraction of the total SiO luminosity that is not associated with outflows is highly variable in the different MDCs (from 10% to 90%); this might be a problem when extrapolating outflow properties from SiO luminosities without resolving individual outflows. In line with previous evidence of SiO emission associated with low-velocity shocks, we propose an evolutionary picture to explain the existence and distribution of narrow SiO line profiles. In this scenario, the least centrally condensed MDCs are at an early stage where the SiO emission traces shocks from the large-scale collapse of material onto the MDC. This could be the case of CygX-N40, a MDC with a low-mass protostar at its centre, a weak outflow, and where 90% of the SiO emission is narrow and arises from the outskirts. As the MDC collapses, the SiO emission becomes more confined to the close surroundings of cores, tracing the post-shock material from the infalling MDC against the dense cores, such as in the small-scale converging flows of CygX-N3, N12, and N48. At later stages, when single massive protostars are formed, as for instance in CygX-N53 and N63, the SiO luminosity is largely dominated by powerful outflows, and the weaker narrow component shows perhaps the last remnants of the initial collapse.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: protostars - stars: massive - ISM: jets and outflows - ISM: kinematics and dynamics - ISM: molecules

Status at CDS:   Examining the need for a new acronym.

CDS comments: Table 3 [BMC2010] CygX-N40 MM2 not existing in the original table from Bontemps et al. 2010A&A...524A..18B

Simbad objects: 23

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Number of rows : 23

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 MSXDC G028.23-0.19 DNe 18 43 31.3 -04 13 18           ~ 23 0
2 QSO J2015+371 BLL 20 15 28.72976962 +37 10 59.5148505     21.82 21.4   ~ 243 2
3 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 619 1
4 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 707 0
5 [MBS2007c] CygX-N3 mm 20 35 34.10 +42 20 05.0           ~ 7 0
6 [BMC2010] CygX-N3 MM2 mm 20 35 34.41 +42 20 07.0           ~ 3 0
7 [BMC2010] CygX-N3 MM1 mm 20 35 34.63 +42 20 08.8           ~ 3 0
8 [MBS2007c] CygX-N12 mm 20 36 57.40 +42 11 27.5           ~ 7 0
9 [BMC2010] CygX-N12 MM2 mm 20 36 57.51 +42 11 31.2           ~ 3 0
10 [BMC2010] CygX-N12 MM1 mm 20 36 57.65 +42 11 30.2           ~ 3 0
11 [BMC2010] CygX-N40 MM1 mm 20 38 59.54 +42 23 43.6           ~ 4 0
12 [MBS2007c] CygX-N40 mm 20 38 59.8 +42 23 43           ~ 6 0
13 NAME DR 21(OH) N1 PoC 20 39 00.0 +42 23 24           ~ 4 0
14 [BMC2010] CygX-N48 MM2 mm 20 39 01.10 +42 22 08.3           ~ 6 0
15 [BMC2010] CygX-N48 MM1 mm 20 39 01.34 +42 22 04.9           ~ 5 0
16 [MBS2007c] CygX-N48 IR 20 39 01.36 +42 22 06.7           ~ 14 0
17 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 944 0
18 2MASS J20390285+4222001 ERO 20 39 02.85 +42 22 00.2           ~ 5 0
19 [BMC2010] CygX-N53 MM1 mm 20 39 02.96 +42 25 51.0           ~ 6 0
20 [MBS2007c] CygX-N53 mm 20 39 03.2 +42 25 49           ~ 12 0
21 [BMC2010] CygX-N53 MM2 mm 20 39 03.22 +42 25 51.2           ~ 11 0
22 [MBS2007c] CygX-N63 mm 20 40 05.2 +41 32 13           ~ 14 0
23 [BMC2010] CygX-N63 MM1 mm 20 40 05.39 +41 32 13.1           ~ 3 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-08:20:18

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