CO observations toward supernova remnants with associated OH 1720 MHz masers

The environs of three supernova remnants (SNRs) with associated OH 1720 MHz masers, G349.7 + 0.2, CTB 37A, and G16.7 + 0.1, have been surveyed in the CO J = 1-0 transition with the 12 Meter Telescope of the NRAO, using the on-the-fly technique. These observations have revealed a number of molecular...

Descripción completa

Guardado en:
Detalles Bibliográficos
Publicado: 2000
Materias:
ISM: clouds
ISM: molecules
Masers
Supernova remnants
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v545_n2PART1_p874_Reynoso
http://hdl.handle.net/20.500.12110/paper_0004637X_v545_n2PART1_p874_Reynoso
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v545_n2PART1_p874_Reynoso
record_format dspace
spelling paper:paper_0004637X_v545_n2PART1_p874_Reynoso2023-06-08T14:28:43Z CO observations toward supernova remnants with associated OH 1720 MHz masers ISM: clouds ISM: molecules Masers Supernova remnants The environs of three supernova remnants (SNRs) with associated OH 1720 MHz masers, G349.7 + 0.2, CTB 37A, and G16.7 + 0.1, have been surveyed in the CO J = 1-0 transition with the 12 Meter Telescope of the NRAO, using the on-the-fly technique. These observations have revealed a number of molecular clouds interacting with the SNR shock fronts. Most of the OH 1720 MHz masers have been found to lie over CO concentrations, and the maser velocities are coincident with the CO peak velocities to an accuracy better than 2 km s-1. The present data trace the interstellar medium (ISM) structures interacting with the SNRs; however, to probe the shocked molecular gas in which the OH 1720 MHz emission originates, higher excitation transitions and more complex species should be observed. In CTB 37A, where the shock velocity into the molecular cloud could be determined, it has been found to be of C-type, in agreement with theoretical predictions. Part of the rim of G16.7 + 0.1 appears to be flattened by a dense external cloud, yet the only associated OH 1720 MHz maser lies near the opposite region of the remnant. This behavior, also observed in IC 443 and 3C 391, seems to contradict the suggestion that OH 1720 MHz maser emission occurs mainly for transverse shocks. 2000 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v545_n2PART1_p874_Reynoso http://hdl.handle.net/20.500.12110/paper_0004637X_v545_n2PART1_p874_Reynoso
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic ISM: clouds
ISM: molecules
Masers
Supernova remnants
spellingShingle ISM: clouds
ISM: molecules
Masers
Supernova remnants
CO observations toward supernova remnants with associated OH 1720 MHz masers
topic_facet ISM: clouds
ISM: molecules
Masers
Supernova remnants
description The environs of three supernova remnants (SNRs) with associated OH 1720 MHz masers, G349.7 + 0.2, CTB 37A, and G16.7 + 0.1, have been surveyed in the CO J = 1-0 transition with the 12 Meter Telescope of the NRAO, using the on-the-fly technique. These observations have revealed a number of molecular clouds interacting with the SNR shock fronts. Most of the OH 1720 MHz masers have been found to lie over CO concentrations, and the maser velocities are coincident with the CO peak velocities to an accuracy better than 2 km s-1. The present data trace the interstellar medium (ISM) structures interacting with the SNRs; however, to probe the shocked molecular gas in which the OH 1720 MHz emission originates, higher excitation transitions and more complex species should be observed. In CTB 37A, where the shock velocity into the molecular cloud could be determined, it has been found to be of C-type, in agreement with theoretical predictions. Part of the rim of G16.7 + 0.1 appears to be flattened by a dense external cloud, yet the only associated OH 1720 MHz maser lies near the opposite region of the remnant. This behavior, also observed in IC 443 and 3C 391, seems to contradict the suggestion that OH 1720 MHz maser emission occurs mainly for transverse shocks.
title CO observations toward supernova remnants with associated OH 1720 MHz masers
title_short CO observations toward supernova remnants with associated OH 1720 MHz masers
title_full CO observations toward supernova remnants with associated OH 1720 MHz masers
title_fullStr CO observations toward supernova remnants with associated OH 1720 MHz masers
title_full_unstemmed CO observations toward supernova remnants with associated OH 1720 MHz masers
title_sort co observations toward supernova remnants with associated oh 1720 mhz masers
publishDate 2000
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v545_n2PART1_p874_Reynoso
http://hdl.handle.net/20.500.12110/paper_0004637X_v545_n2PART1_p874_Reynoso
_version_ 1768542343306149888

Ejemplares similares