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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.)

Sulphur-bearing and complex organic molecules in an infrared cold core

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Beaklini, Pedro P. B. [1] ; Mendoza, Edgar [1] ; Canelo, Carla M. [1] ; Aleman, Isabel [1, 2] ; Merello, Manuel [1] ; Kong, Shuo [3] ; Navarete, Felipe [1] ; Janot-Pacheco, Eduardo [1] ; Abraham, Zulema [1] ; Lepine, Jacques R. D. [1] ; de Almeida, Amaury A. [1] ; Friaca, Amancio C. S. [1]
Total Authors: 12
[1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226, BR-05508090 Sao Paulo, SP - Brazil
[2] Univ Fed Itajuba, UNIFEI, Inst Fis & Quim, Av BPS 1303 Pinheirinho, BR-37500903 Itajuba, MG - Brazil
[3] Yale Univ, Dept Astron, New Haven, CT 06511 - USA
Total Affiliations: 3
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 491, n. 1, p. 427-439, JAN 2020.
Web of Science Citations: 0

Since the start of ALMA (Atacama Large Millimeter Array) observatory operation, new and important chemistry of infrared cold core was revealed. Molecular transitions at millimetre range are being used to identify and to characterize these sources. We have investigated the 231 GHz ALMA archive observations of the infrared dark cloud region C9, focusing on the brighter source that we called as IRDC-C9 Main. We report the existence of two substructures on the continuum map of this source: a compact bright spot with high chemistry diversity that we labelled as core, and a weaker and extended one, that we labelled as tail. In the core, we have identified lines of the molecules OCS(19-18), (CS)-C-13(5-4), and CH3CH2CN, several lines of CH3CHO and the k-ladder emission of (CH3CN)-C-13. We report two different temperature regions, while the rotation diagram of CH3CHO indicates a temperature of 25 K, the rotation diagram of (CH3CN)-C-13 indicates a warmer phase at temperature of similar to 450 K. In the tail, only the OCS(19-18) and (CS)-C-13(5-4) lines were detected. We used the NAUTILUS and the RADEX codes to estimate the column densities and the abundances. The existence of hot gas in the core of IRDC-C9 Main suggests the presence of a protostar, which is not present in the tail. (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: 17/18191-8 - High-mass star formation: the mass of the central sources and the physics of the accretion process
Grantee:Felipe Donizeti Teston Navarete
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
FAPESP's process: 14/07460-0 - Targets for LLAMA: study of variability of radio sources at 43 GHz (band 1) and search for correlation with interferometric images
Grantee:Pedro Paulo Bonetti Beaklini
Support type: Scholarships in Brazil - Post-Doctorate
FAPESP's process: 09/54006-4 - A computer cluster for the Astronomy Department of the University of São Paulo Institute of Astronomy, Geophysics and Atmospheric Sciences and for the Cruzeiro do Sul University Astrophysics Center
Grantee:Elisabete Maria de Gouveia Dal Pino
Support type: Multi-user Equipment Program