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

Abstract

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 ~5 pc-long W43-MM1 ridge to determine its origin. 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 30 m 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. 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. 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.

13 pages, 9 figures, accepted by A&A

References in corpus (12)

• A Unified Representation of Gas-Phase Element Depletions in the Interstellar Medium
• The earliest phases of high-mass star formation: a 3 square degree millimeter continuum mapping of Cygnus X
• SiO line emission from C-type shock waves : interstellar jets and outflows
• Cooling, Gravity and Geometry: Flow-driven Massive Core Formation
• The dynamical properties of dense filaments in the infrared dark cloud G035.39-00.33
• Low velocity shocks: signatures of turbulent dissipation in diffuse irradiated gas
• The W43-MM1 mini-starburst ridge, a test for star formation efficiency models
• The formation of the W43 complex: constraining its atomic-to-molecular transition and searching for colliding clouds
• SiO emission from low- and high-velocity shocks in Cygnus-X massive dense clumps
• Shocks in dense clouds. IV. Effects of grain-grain processing on molecular line emission
• Impacts of pure shocks in the BHR71 bipolar outflow
• Water emission from the high-mass star-forming region IRAS 17233-3606. High water abundances at high velocities

Cited by in corpus (31)

• ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- I. Survey description and a first look at G9.62+0.19
• ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results
• Models of irradiated molecular shocks
• ALMA-IMF. V. Prestellar and protostellar core populations in the W43 cloud complex
• ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP) II. Survey overview: a first look at 1.3 mm continuum maps and molecular outflows
• ALMA-IMF VI -- Investigating the origin of stellar masses: Core mass function evolution in the W43-MM2&MM3 mini-starburst
• Cloud-cloud collision in the DR 21 cloud as a trigger of massive star formation
• A SiO J = 5 - 4 Survey Toward Massive Star Formation Regions
• HII regions and high-mass starless clump candidates II. Fragmentation and induced star formation at ~0.025 pc scale: An ALMA continuum study
• Molecular analysis of a high-mass prestellar core candidate in W43-MM1
• ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XII: Fragmentation and multi-scale gas kinematics in protoclusters G12.42+0.50 and G19.88-0.53
• Dense gas formation in the Musca filament due to the dissipation of a supersonic converging flow
• ALMA-IMF IV -- A comparative study of the main hot cores in W43-MM1: detection, temperature and molecular composition
• ALMA-IMF X -- The core population in the evolved W33-Main (G012.80) protocluster
• Large-scale Map of Millimeter-wavelength Hydrogen Radio Recombination Lines around a Young Massive Star Cluster
• ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- VI. On the formation of the "L" type filament in G286.21+0.17
• A survey of SiO $J=$ 1 -- 0 emission toward massive star-forming regions
• ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- VII. A catalogue of SiO clumps from ACA observations
• ALMA-IMF XVIII: The assembly of a star cluster: Dense N${}_2$H${}^{+}$ (1-0) kinematics in the massive G351.77 protocluster
• ALMAGAL IV. Morphological comparison of molecular and thermal dust emission using the histogram of oriented gradients (HOG) method
• Star Formation in Extreme Environments: A 200 pc High Velocity Gas Stream in the Galactic Centre
• Shaken or stirred: the diffuse interstellar medium with exceptionally high SiO abundance
• Bar-spiral interaction produces radial migration and star formation bursts
• Spatial distributions and kinematics of shocked and ionized gas in M17
• Confirmation of the outflow in L1451-mm: SiO line and CH${}_3$OH maser detections
• Surveys of clumps, cores, and condensations in Cygnus-X: SMA observations of SiO (5$-$4)
• Different molecular filament widths as tracers of accretion onto filaments
• ALMA observations of massive clouds in the central molecular zone: slim filaments tracing parsec-scale shocks
• ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XIX. The origin of SiO emission
• Origins of the shocks in high-mass starless clump candidates
• SiO emission in the filamentary Infrared Dark Cloud G035.39-00.33: An ALMA view