Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays
We introduce a distinct method for performing spatially resolved spectral analysis of astronomical sources with highly structured X-ray emission. The method measures the surface brightness of neighboring pixels to adaptively size and shape each region, thus the spectra from the bright and faint fila...
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2016
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v590_n_p_Luna http://hdl.handle.net/20.500.12110/paper_00046361_v590_n_p_Luna |
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paper:paper_00046361_v590_n_p_Luna2023-06-08T14:28:14Z Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays ISM: individual objects: Puppis A ISM: supernova remnants X-rays: ISM Magnesium Neon Spectroscopic analysis Spectrum analysis Supernovae Astronomical sources Elemental abundance Filamentary structures ISM: individual objects ISM: supernova remnants Spatially resolved spectroscopy X rays: ISM X-ray emitting plasmas Atmospheric optics We introduce a distinct method for performing spatially resolved spectral analysis of astronomical sources with highly structured X-ray emission. The method measures the surface brightness of neighboring pixels to adaptively size and shape each region, thus the spectra from the bright and faint filamentary structures evident in the broadband images can be extracted. As a test case, we present the spectral analysis of the complete X-ray emitting plasma in the supernova remnant Puppis A observed with XMM-Newton and Chandra. Given the angular size of Puppis A, many pointings with different observational configurations have to be combined, presenting a challenge to any method of spatially resolved spectroscopy. From the fit of a plane-parallel shocked plasma model we find that temperature, absorption column, ionization time scale, emission measure, and elemental abundances of O, Ne, Mg, Si, S, and Fe, are smoothly distributed in the remnant. Some regions with overabundances of O, Ne, and Mg previously characterized as ejecta material, were automatically selected by our method, proving the excellent response of the technique. This method is an advantageous tool for the exploitation of archival X-ray data. © ESO 2016. 2016 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v590_n_p_Luna http://hdl.handle.net/20.500.12110/paper_00046361_v590_n_p_Luna |
| 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: Puppis A ISM: supernova remnants X-rays: ISM Magnesium Neon Spectroscopic analysis Spectrum analysis Supernovae Astronomical sources Elemental abundance Filamentary structures ISM: individual objects ISM: supernova remnants Spatially resolved spectroscopy X rays: ISM X-ray emitting plasmas Atmospheric optics |
| spellingShingle |
ISM: individual objects: Puppis A ISM: supernova remnants X-rays: ISM Magnesium Neon Spectroscopic analysis Spectrum analysis Supernovae Astronomical sources Elemental abundance Filamentary structures ISM: individual objects ISM: supernova remnants Spatially resolved spectroscopy X rays: ISM X-ray emitting plasmas Atmospheric optics Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays |
| topic_facet |
ISM: individual objects: Puppis A ISM: supernova remnants X-rays: ISM Magnesium Neon Spectroscopic analysis Spectrum analysis Supernovae Astronomical sources Elemental abundance Filamentary structures ISM: individual objects ISM: supernova remnants Spatially resolved spectroscopy X rays: ISM X-ray emitting plasmas Atmospheric optics |
| description |
We introduce a distinct method for performing spatially resolved spectral analysis of astronomical sources with highly structured X-ray emission. The method measures the surface brightness of neighboring pixels to adaptively size and shape each region, thus the spectra from the bright and faint filamentary structures evident in the broadband images can be extracted. As a test case, we present the spectral analysis of the complete X-ray emitting plasma in the supernova remnant Puppis A observed with XMM-Newton and Chandra. Given the angular size of Puppis A, many pointings with different observational configurations have to be combined, presenting a challenge to any method of spatially resolved spectroscopy. From the fit of a plane-parallel shocked plasma model we find that temperature, absorption column, ionization time scale, emission measure, and elemental abundances of O, Ne, Mg, Si, S, and Fe, are smoothly distributed in the remnant. Some regions with overabundances of O, Ne, and Mg previously characterized as ejecta material, were automatically selected by our method, proving the excellent response of the technique. This method is an advantageous tool for the exploitation of archival X-ray data. © ESO 2016. |
| title |
Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays |
| title_short |
Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays |
| title_full |
Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays |
| title_fullStr |
Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays |
| title_full_unstemmed |
Feature-tailored spectroscopic analysis of the supernova remnant Puppis A in X-rays |
| title_sort |
feature-tailored spectroscopic analysis of the supernova remnant puppis a in x-rays |
| publishDate |
2016 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v590_n_p_Luna http://hdl.handle.net/20.500.12110/paper_00046361_v590_n_p_Luna |
| _version_ |
1768546655909445632 |