SiO emission as a probe of cloud–cloud collisions in infrared dark clouds

  • G Cosentino
    Space, Earth and Environment Department, Chalmers University of Technology, SE-412 96 Gothenburg, Sweden
  • I Jiménez-Serra
    Centro de Astrobiología (CSIC/INTA), Ctra. de Torrejón a Ajalvir km 4, E-28850 Madrid, Spain
  • J D Henshaw
    Max Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
  • P Caselli
    Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse 1, D-85748 Garching bei München, Germany
  • S Viti
    Department of Physics and Astronomy, University College London, Gower Street, London WC1E6BT, UK
  • A T Barnes
    Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany
  • J C Tan
    Space, Earth and Environment Department, Chalmers University of Technology, SE-412 96 Gothenburg, Sweden
  • F Fontani
    INAF Osservatorio Astronomico di Arcetri, Largo E. Fermi 5, I-50125 Florence, Italy
  • B Wu
    National Astronomical Observatory of Japan, Yubinbango 181-8588 Tokio, Mitaka, Osawa 2-21-1, Japan

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<jats:title>ABSTRACT</jats:title> <jats:p>Infrared dark clouds (IRDCs) are very dense and highly extincted regions that host the initial conditions of star and stellar cluster formation. It is crucial to study the kinematics and molecular content of IRDCs to test their formation mechanism and ultimately characterize these initial conditions. We have obtained high-sensitivity Silicon Monoxide, SiO(2–1), emission maps towards the six IRDCs, G018.82–00.28, G019.27+00.07, G028.53–00.25, G028.67+00.13, G038.95–00.47, and G053.11+00.05 (cloud A, B, D, E, I, and J, respectively), using the 30-m antenna at the Instituto de Radioastronomía Millimétrica (IRAM30m). We have investigated the SiO spatial distribution and kinematic structure across the six clouds to look for signatures of cloud–cloud collision events that may have formed the IRDCs and triggered star formation within them. Towards clouds A, B, D, I, and J, we detect spatially compact SiO emission with broad-line profiles that are spatially coincident with massive cores. Towards the IRDCs A and I, we report an additional SiO component that shows narrow-line profiles and that is widespread across quiescent regions. Finally, we do not detect any significant SiO emission towards cloud E. We suggest that the broad and compact SiO emission detected towards the clouds is likely associated with ongoing star formation activity within the IRDCs. However, the additional narrow and widespread SiO emission detected towards cloud A and I may have originated from the collision between the IRDCs and flows of molecular gas pushed towards the clouds by nearby H ii regions.</jats:p>

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