An X-ray study of the supernova remnant G20.0-0.2 and its surroundings
Aims. We study the supernova remnant G20.0-0.2 and its surroundings to look for the high-energy counterpart of the radio nebula and to find evidence of interaction between the shock front and the interstellar medium. Methods. We used Chandra archival observations to analyze the X-ray emission from t...
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2013
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v554_n_p_Petriella http://hdl.handle.net/20.500.12110/paper_00046361_v554_n_p_Petriella |
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paper:paper_00046361_v554_n_p_Petriella2023-06-08T14:28:02Z An X-ray study of the supernova remnant G20.0-0.2 and its surroundings ISM: clouds ISM: supernova remnants Pulsars: general Stars: formation Galactic plane surveys Interstellar mediums ISM : clouds ISM: supernova remnants Pulsars: general Star-forming region Stars: formation Young stellar objects Electromagnetic wave emission Shock waves Surveys X ray scattering X rays Stars Aims. We study the supernova remnant G20.0-0.2 and its surroundings to look for the high-energy counterpart of the radio nebula and to find evidence of interaction between the shock front and the interstellar medium. Methods. We used Chandra archival observations to analyze the X-ray emission from the supernova remnant. The surrounding gas was investigated using data extracted from the Galactic Ring Survey, the VLA Galactic Plane Survey, the Galactic Legacy Infrared Midplane Survey Extraordinaire, and the Bolocam Galactic Plane Survey. Results. G20.0-0.2 shows diffuse X-ray emission from the central region of the radio remnant. Although the current data do not allow us to distinguish between a thermal or non-thermal origin for the X-ray diffuse emission, based on the radio properties we suggest a synchrotron origin as the most favorable. The hard X-ray point source CXO J182807.4-113516 appears located at the geometrical center of the remnant and is a potential candidate to be the pulsar powering the nebula. We found a molecular cloud adjacent to the flattest border of G20.0-0.2, indicating a probable interaction between the shock front of the remnant and the molecular gas. Several young stellar object candidates are found located in the brightest region of the molecular emission, as well as over a millimeter continuum source and a dark cloud. This distribution is an indication of an active star-forming region around the supernova remnant. © 2013 ESO. 2013 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v554_n_p_Petriella http://hdl.handle.net/20.500.12110/paper_00046361_v554_n_p_Petriella |
| 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: supernova remnants Pulsars: general Stars: formation Galactic plane surveys Interstellar mediums ISM : clouds ISM: supernova remnants Pulsars: general Star-forming region Stars: formation Young stellar objects Electromagnetic wave emission Shock waves Surveys X ray scattering X rays Stars |
| spellingShingle |
ISM: clouds ISM: supernova remnants Pulsars: general Stars: formation Galactic plane surveys Interstellar mediums ISM : clouds ISM: supernova remnants Pulsars: general Star-forming region Stars: formation Young stellar objects Electromagnetic wave emission Shock waves Surveys X ray scattering X rays Stars An X-ray study of the supernova remnant G20.0-0.2 and its surroundings |
| topic_facet |
ISM: clouds ISM: supernova remnants Pulsars: general Stars: formation Galactic plane surveys Interstellar mediums ISM : clouds ISM: supernova remnants Pulsars: general Star-forming region Stars: formation Young stellar objects Electromagnetic wave emission Shock waves Surveys X ray scattering X rays Stars |
| description |
Aims. We study the supernova remnant G20.0-0.2 and its surroundings to look for the high-energy counterpart of the radio nebula and to find evidence of interaction between the shock front and the interstellar medium. Methods. We used Chandra archival observations to analyze the X-ray emission from the supernova remnant. The surrounding gas was investigated using data extracted from the Galactic Ring Survey, the VLA Galactic Plane Survey, the Galactic Legacy Infrared Midplane Survey Extraordinaire, and the Bolocam Galactic Plane Survey. Results. G20.0-0.2 shows diffuse X-ray emission from the central region of the radio remnant. Although the current data do not allow us to distinguish between a thermal or non-thermal origin for the X-ray diffuse emission, based on the radio properties we suggest a synchrotron origin as the most favorable. The hard X-ray point source CXO J182807.4-113516 appears located at the geometrical center of the remnant and is a potential candidate to be the pulsar powering the nebula. We found a molecular cloud adjacent to the flattest border of G20.0-0.2, indicating a probable interaction between the shock front of the remnant and the molecular gas. Several young stellar object candidates are found located in the brightest region of the molecular emission, as well as over a millimeter continuum source and a dark cloud. This distribution is an indication of an active star-forming region around the supernova remnant. © 2013 ESO. |
| title |
An X-ray study of the supernova remnant G20.0-0.2 and its surroundings |
| title_short |
An X-ray study of the supernova remnant G20.0-0.2 and its surroundings |
| title_full |
An X-ray study of the supernova remnant G20.0-0.2 and its surroundings |
| title_fullStr |
An X-ray study of the supernova remnant G20.0-0.2 and its surroundings |
| title_full_unstemmed |
An X-ray study of the supernova remnant G20.0-0.2 and its surroundings |
| title_sort |
x-ray study of the supernova remnant g20.0-0.2 and its surroundings |
| publishDate |
2013 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v554_n_p_Petriella http://hdl.handle.net/20.500.12110/paper_00046361_v554_n_p_Petriella |
| _version_ |
1768545030363938816 |