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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

ALMA Observations of the Massive Molecular Outflow G331.512-0.103. II. Physical Properties, Kinematics, and Geometry Modeling

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Author(s):
Hervias-Caimapo, Carlos [1, 2] ; Merello, Manuel [3] ; Bronfman, Leonardo [1] ; Ake-Nyman, Lars [4] ; Garay, Guido [1] ; Lo, Nadia [1] ; Evans, II, Neal J. ; Lopez-Calderon, Cristian [4] ; Mendoza, Edgar [3]
Total Authors: 9
Affiliation:
[1] Univ Chile, Dept Astron, Casilla 36-D, Santiago - Chile
[2] Univ Manchester, Ctr Astrophys, Sch Phys & Astron, Jodrell Bank, Oxford Rd, Manchester M13 9PL, Lancs - England
[3] Univ Sao Paulo, IAG Rua Matao 1226, Cidade Univ, BR-05508090 Sao Paulo - Brazil
[4] Joint ALMA Observ JAO, Alonso de Cordova 3107, Santiago - Chile
Total Affiliations: 4
Document type: Journal article
Source: ASTROPHYSICAL JOURNAL; v. 872, n. 2 FEB 20 2019.
Web of Science Citations: 0
Abstract

We present observations and analysis of the massive molecular outflow G331.512-0.103, obtained with Atacama Large Millimeter/submillimeter Array band 7, continuing the work from Merello et al. Several lines were identified in the observed bandwidth, consisting of two groups: lines with narrow profiles, tracing the emission from the core ambient medium; and lines with broad velocity wings, tracing the outflow and shocked gas emission. The physical and chemical conditions, such as density, temperature, and fractional abundances are calculated. The ambient medium, or core, has a mean density of similar to 5 x 10(6) cm(-3) and a temperature of similar to 70 K. The SiO and SO2 emission trace the very dense and hot part of the shocked outflow, with values of n(H2) similar to 10(9) cm(-3) and T similar to 160-200 K. The interpretation of the molecular emission suggests an expanding cavity geometry powered by stellar winds from a newborn UCHII region, alongside a massive and high-velocity molecular outflow. This scenario, along with the estimated physical conditions, is modeled using the 3D geometry radiative transfer code MOLLIE for the SiO(J = 8 - 7) molecular line. The main features of the outflow and the expanding shell are reproduced by the model. (AU)

FAPESP's process: 17/23708-0 - 183 GHz H2O Megamaser galaxies and intensity Calibrations
Grantee:Manuel Antonio Merello Ferrada
Support type: Scholarships in Brazil - Post-Doctorate
FAPESP's process: 14/22095-6 - ACHEMOS: astrochemistry of our origins, a comprehensive study of the prebiotic chemistry in pre-stellar regions
Grantee:Edgar Fabián Mendoza Rodríguez
Support type: Scholarships in Brazil - Post-Doctorate