An X-ray characterization of the central region of the supernova remnant G332.5-5.6

We present an X-ray analysis of the central region of supernova remnant (SNR) G332.5-5.6 through an exhaustive analysis of XMM-Netwon observations with complementary infrared observations. We characterize and discuss the origin of the observed X-ray morphology, which presents a peculiar plane edge o...

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Detalles Bibliográficos
Publicado: 2015
Materias:
ISM: individual objects: G332.5-5.6
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
Collisional plasmas
Neon
Spectrum analysis
Supernovae
X ray analysis
X ray scattering
Infrared observations
ISM: individual objects
Spectral properties
X rays: ISM
X-ray characterization
XMM-Newton observations
Electromagnetic wave emission
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v583_n_p_Suarez
http://hdl.handle.net/20.500.12110/paper_00046361_v583_n_p_Suarez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00046361_v583_n_p_Suarez
record_format dspace
spelling paper:paper_00046361_v583_n_p_Suarez2023-06-08T14:28:11Z An X-ray characterization of the central region of the supernova remnant G332.5-5.6 ISM: individual objects: G332.5-5.6 ISM: supernova remnants Radiation mechanisms: thermal X-rays: ISM Collisional plasmas Neon Spectrum analysis Supernovae X ray analysis X ray scattering Infrared observations ISM: individual objects ISM: supernova remnants Radiation mechanisms: thermal Spectral properties X rays: ISM X-ray characterization XMM-Newton observations Electromagnetic wave emission We present an X-ray analysis of the central region of supernova remnant (SNR) G332.5-5.6 through an exhaustive analysis of XMM-Netwon observations with complementary infrared observations. We characterize and discuss the origin of the observed X-ray morphology, which presents a peculiar plane edge over the west side of the central region. Methods. The morphology and spectral properties of the X-ray SNR were studied using a single full frame XMM-Newton observation in the 0.3 to 10.0 keV energy band. Archival infrared WISE observations at 8, 12 and 24 μm were also used to investigate the properties of the source and its surroundings at different wavelengths. Results. The results show that the extended X-ray emission is predominantly soft (0.3-1.2 keV) and peaks around 0.5 keV, which shows that it is an extremely soft SNR. X-ray emission correlates very well with central regions of bright radio emission. On the west side the radio/X-ray emission displays a plane-like feature with a terminal wall where strong infrared emission is detected. Our spatially resolved X-ray spectral analysis confirms that the emission is dominated by weak atomic emission lines of N, O, Ne, and Fe, all of them undetected in previous X-ray studies. These characteristics suggest that the X-ray emission is originated in an optically thin thermal plasma, whose radiation is well fitted by a non-equilibrium ionization collisional plasma (VNEI) X-ray emission model. Our study favors a scenario where G332.5-5.6 is expanding in a medium with an abrupt density change (the wall), likely a dense infrared emitting region of dust on the western side of the source. © 2015 ESO. 2015 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v583_n_p_Suarez http://hdl.handle.net/20.500.12110/paper_00046361_v583_n_p_Suarez
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: individual objects: G332.5-5.6
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
Collisional plasmas
Neon
Spectrum analysis
Supernovae
X ray analysis
X ray scattering
Infrared observations
ISM: individual objects
ISM: supernova remnants
Radiation mechanisms: thermal
Spectral properties
X rays: ISM
X-ray characterization
XMM-Newton observations
Electromagnetic wave emission
spellingShingle ISM: individual objects: G332.5-5.6
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
Collisional plasmas
Neon
Spectrum analysis
Supernovae
X ray analysis
X ray scattering
Infrared observations
ISM: individual objects
ISM: supernova remnants
Radiation mechanisms: thermal
Spectral properties
X rays: ISM
X-ray characterization
XMM-Newton observations
Electromagnetic wave emission
An X-ray characterization of the central region of the supernova remnant G332.5-5.6
topic_facet ISM: individual objects: G332.5-5.6
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
Collisional plasmas
Neon
Spectrum analysis
Supernovae
X ray analysis
X ray scattering
Infrared observations
ISM: individual objects
ISM: supernova remnants
Radiation mechanisms: thermal
Spectral properties
X rays: ISM
X-ray characterization
XMM-Newton observations
Electromagnetic wave emission
description We present an X-ray analysis of the central region of supernova remnant (SNR) G332.5-5.6 through an exhaustive analysis of XMM-Netwon observations with complementary infrared observations. We characterize and discuss the origin of the observed X-ray morphology, which presents a peculiar plane edge over the west side of the central region. Methods. The morphology and spectral properties of the X-ray SNR were studied using a single full frame XMM-Newton observation in the 0.3 to 10.0 keV energy band. Archival infrared WISE observations at 8, 12 and 24 μm were also used to investigate the properties of the source and its surroundings at different wavelengths. Results. The results show that the extended X-ray emission is predominantly soft (0.3-1.2 keV) and peaks around 0.5 keV, which shows that it is an extremely soft SNR. X-ray emission correlates very well with central regions of bright radio emission. On the west side the radio/X-ray emission displays a plane-like feature with a terminal wall where strong infrared emission is detected. Our spatially resolved X-ray spectral analysis confirms that the emission is dominated by weak atomic emission lines of N, O, Ne, and Fe, all of them undetected in previous X-ray studies. These characteristics suggest that the X-ray emission is originated in an optically thin thermal plasma, whose radiation is well fitted by a non-equilibrium ionization collisional plasma (VNEI) X-ray emission model. Our study favors a scenario where G332.5-5.6 is expanding in a medium with an abrupt density change (the wall), likely a dense infrared emitting region of dust on the western side of the source. © 2015 ESO.
title An X-ray characterization of the central region of the supernova remnant G332.5-5.6
title_short An X-ray characterization of the central region of the supernova remnant G332.5-5.6
title_full An X-ray characterization of the central region of the supernova remnant G332.5-5.6
title_fullStr An X-ray characterization of the central region of the supernova remnant G332.5-5.6
title_full_unstemmed An X-ray characterization of the central region of the supernova remnant G332.5-5.6
title_sort x-ray characterization of the central region of the supernova remnant g332.5-5.6
publishDate 2015
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v583_n_p_Suarez
http://hdl.handle.net/20.500.12110/paper_00046361_v583_n_p_Suarez
_version_ 1768545765513232384

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