2016A&A...595A.122L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST23:12:34

2016A&A...595A.122L - Astronomy and Astrophysics, volume 595A, 122-122 (2016/11-1)

Tracing extended low-velocity shocks through SiO emission. Case study of the W43-MM1 ridge.

LOUVET F., MOTTE F., GUSDORF A., NGUYEN LUONG Q., LESAFFRE P., DUARTE-CABRAL A., MAURY A., SCHNEIDER N., HILL T., SCHILKE P. and GUETH F.

Abstract (from CDS):

Aims. Previous literature suggests that the densest structures in the interstellar medium form through colliding flows, but patent evidence of this process is still missing. Recent literature proposes using SiO line emission to trace low-velocity shocks associated with cloud formation through collision. In this paper we investigate the bright and extended SiO(2-1) emission observed along the ∼5pc-long W43-MM1 ridge to determine its origin.
Methods. We used high angular resolution images of the SiO(2-1) and HCN(1-0) emission lines obtained with the IRAM plateau de Bure (PdBI) interferometer and combined with data from the IRAM 30m radiotelescope. These data were complemented by a Herschel column density map of the region. We performed spectral analysis of SiO and HCN emission line profiles to identify protostellar outflows and spatially disentangle two velocity components associated with low- and high-velocity shocks. Then, we compared the low-velocity shock component to a dedicated grid of one-dimensional (1D) radiative shock models.
Results. We find that the SiO emission originates from a mixture of high-velocity shocks caused by bipolar outflows and low-velocity shocks. Using SiO and HCN emission lines, we extract seven bipolar outflows associated with massive dense cores previously identified within the W43-MM1 mini-starburst cluster. Comparing observations with dedicated Paris-Durham shock models constrains the velocity of the low-velocity shock component from 7 to 12km/s.
Conclusions. The SiO arising from low-velocity shocks spreads along the complete length of the ridge. Its contribution represents at least 45% and up to 100% of the total SiO emission depending on the area considered. The low-velocity component of SiO is most likely associated with the ridge formation through colliding flows or cloud-cloud collision.

Abstract Copyright: © ESO, 2016

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

Simbad objects: 13

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Number of rows : 13

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 QSO J0217+0144 QSO 02 17 48.9547510 +01 44 49.698899   16.74 16.09 18.51 13.29 ~ 371 1
2 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 119 0
3 ICRF J183005.9+061915 QSO 18 30 05.9399600344 +06 19 15.947596681       19.5   ~ 71 1
4 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 437 0
5 [LMH2014] N4 MDC cor 18 47 44.6 -01 54 40           ~ 2 0
6 [LMH2014] N6 MDC cor 18 47 44.9 -01 54 44           ~ 2 0
7 [LMH2014] N2 MDC cor 18 47 46.4 -01 54 32           ~ 3 0
8 [LMH2014] N7 MDC cor 18 47 46.5 -01 54 21           ~ 2 0
9 [MSL2003] W43-MM1 cor 18 47 47.0 -01 54 28           ~ 95 0
10 [LMH2014] N1 MDC cor 18 47 47.0 -01 54 26           ~ 2 0
11 [LMH2014] N12 dense core cor 18 47 49.6 -01 54 00           ~ 2 0
12 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 707 0
13 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2506 2

    Equat.    Gal    SGal    Ecl

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2020.07.13-23:12:34

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