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|Title:||Structure and kinematics of shocked gas in Sgr B2: further evidence of a cloud–cloud collision from SiO emission maps|
|Authors:||Armijos Abendaño, J.|
Banda Barragán, W. E.
Martín Pintado, J.
Requeña Torres, M. A.
|Keywords:||Methods: numerical;ISM: clouds;ISM: molecules;Galaxy: centre|
|Publisher:||Oxford Academics: Oxford University Press|
|Citation:||Monthly Notices of the Royal Astronomical Society 499(4): 4918–4939(2020)|
|Abstract:||We present SiO J = 2-1 maps of the Sgr B2 molecular cloud, which show shocked gas with a turbulent substructure comprising at least three cavities at velocities of [10, 40] km s(-1) and an arc at velocities of [-20, 10] km s(-1). The spatial anticorrelation of shocked gas at low and high velocities, and the presence of bridging features in position-velocity diagrams suggest that these structures formed in a cloud-cloud collision. Some of the known compact HII regions spatially overlap with sites of strong SiO emission at velocities of [40, 85] km s(-1), and are between or along the edges of SiO gas features at [100, 120] km s(-1), suggesting that the stars responsible for ionizing the compact HII regions formed in compressed gas due to this collision. We find gas densities and kinetic temperatures of the order of n(H2) similar to 10(5) cm(-3) and similar to 30 K, respectively, towards three positions of Sgr B2. The average values of the SiO relative abundances, integrated line intensities, and line widths are similar to 10(-9), similar to 11 K kms(-1), and similar to 31 km s(-1), respectively. These values agree with those obtained with chemical models that mimic grain sputtering by C-type shocks. A comparison of our observations with hydrodynamical simulations shows that a cloud-cloud collision that took place less than or similar to 0.5 Myr ago can explain the density distribution with a mean column density of (N) over bar (H2) greater than or similar to 5 x 10(22) cm(-2), and the morphology and kinematics of shocked gas in different velocity channels. Colliding clouds are efficient at producing internal shocks with velocities similar to 5-50 km s(-1). High-velocity shocks are produced during the early stages of the collision and can readily ignite star formation, while moderate- and low-velocity shocks are important over longer time-scales and can explain the widespread SiO emission in Sgr B2.|
|Appears in Collections:||(CAB) Artículos|
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