The most complete and detailed X-ray view of the SNR Puppis A

Aims. With the purpose of producing the first detailed full view of Puppis A in X-rays, we carried out new XMM-Newton observations covering the missing regions in the southern half of the supernova remnant (SNR) and combined them with existing XMM-Newton and Chandra data. Methods. Two pointings towa...

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Publicado:	2013
Materias:	ISM: individual objects: Puppis A ISM: supernova remnants X-rays: ISM Germanium compounds Infrared imaging Luminance Supernovae Accelerated particles Interstellar mediums ISM: individual objects Magnetic field strengths Spectral energy distribution X rays: ISM XMM-Newton observations Gamma rays
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v555_n_p_Dubner http://hdl.handle.net/20.500.12110/paper_00046361_v555_n_p_Dubner
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

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spelling	paper:paper_00046361_v555_n_p_Dubner2023-06-08T14:28:04Z The most complete and detailed X-ray view of the SNR Puppis A ISM: individual objects: Puppis A ISM: supernova remnants X-rays: ISM Germanium compounds Infrared imaging Luminance Supernovae Accelerated particles Interstellar mediums ISM: individual objects ISM: supernova remnants Magnetic field strengths Spectral energy distribution X rays: ISM XMM-Newton observations Gamma rays Aims. With the purpose of producing the first detailed full view of Puppis A in X-rays, we carried out new XMM-Newton observations covering the missing regions in the southern half of the supernova remnant (SNR) and combined them with existing XMM-Newton and Chandra data. Methods. Two pointings toward the south and southwest of Puppis A were observed with XMM-Newton. We combined these data with archival XMM-Newton and Chandra data and produced images in the 0.3-0.7, 0.7-1.0, and 1.0-8.0 energy bands. Results. We present the first sensitive complete X-ray image of Puppis A. We investigated its morphology in detail, carried out a multiwavelength analysis, and estimated the flux density and luminosity of the whole SNR. The complex structure observed across the remnant confirms that Puppis A evolves in an inhomogeneous, probably knotty interstellar medium. The southwestern corner includes filaments that perfectly correlate with radio features suggested to be associated with shock/cloud interaction. In the northern half of Puppis A the comparison with Spitzer infrared images shows an excellent correspondence between X-rays and 24 and 70 μm emission features, while to the south there are some matched and other unmatched features. X-ray flux densities of 12.6 × 10-9,6.2 × 10-9, and 2.8 × 10-9 erg cm-2 s-1 were derived for the 0.3-0.7, 0.7-1.0, and 1.0-8.0 keV bands, respectively. At the assumed distance of 2.2 kpc, the total X-ray luminosity between 0.3 and 8.0 keV is 1.2 × 1037 erg s-1. We also collected and updated the broad-band data of Puppis A between radio and GeV γ-ray range, producing its spectral energy distribution. To provide constraints to the high-energy emission models, we re-analyzed radio data, estimating the energy content in accelerated particles to be Umin = 4.8 × 1049 erg and the magnetic field strength B ∼ 26 μG. © 2013 ESO. 2013 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v555_n_p_Dubner http://hdl.handle.net/20.500.12110/paper_00046361_v555_n_p_Dubner
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 Germanium compounds Infrared imaging Luminance Supernovae Accelerated particles Interstellar mediums ISM: individual objects ISM: supernova remnants Magnetic field strengths Spectral energy distribution X rays: ISM XMM-Newton observations Gamma rays
spellingShingle	ISM: individual objects: Puppis A ISM: supernova remnants X-rays: ISM Germanium compounds Infrared imaging Luminance Supernovae Accelerated particles Interstellar mediums ISM: individual objects ISM: supernova remnants Magnetic field strengths Spectral energy distribution X rays: ISM XMM-Newton observations Gamma rays The most complete and detailed X-ray view of the SNR Puppis A
topic_facet	ISM: individual objects: Puppis A ISM: supernova remnants X-rays: ISM Germanium compounds Infrared imaging Luminance Supernovae Accelerated particles Interstellar mediums ISM: individual objects ISM: supernova remnants Magnetic field strengths Spectral energy distribution X rays: ISM XMM-Newton observations Gamma rays
description	Aims. With the purpose of producing the first detailed full view of Puppis A in X-rays, we carried out new XMM-Newton observations covering the missing regions in the southern half of the supernova remnant (SNR) and combined them with existing XMM-Newton and Chandra data. Methods. Two pointings toward the south and southwest of Puppis A were observed with XMM-Newton. We combined these data with archival XMM-Newton and Chandra data and produced images in the 0.3-0.7, 0.7-1.0, and 1.0-8.0 energy bands. Results. We present the first sensitive complete X-ray image of Puppis A. We investigated its morphology in detail, carried out a multiwavelength analysis, and estimated the flux density and luminosity of the whole SNR. The complex structure observed across the remnant confirms that Puppis A evolves in an inhomogeneous, probably knotty interstellar medium. The southwestern corner includes filaments that perfectly correlate with radio features suggested to be associated with shock/cloud interaction. In the northern half of Puppis A the comparison with Spitzer infrared images shows an excellent correspondence between X-rays and 24 and 70 μm emission features, while to the south there are some matched and other unmatched features. X-ray flux densities of 12.6 × 10-9,6.2 × 10-9, and 2.8 × 10-9 erg cm-2 s-1 were derived for the 0.3-0.7, 0.7-1.0, and 1.0-8.0 keV bands, respectively. At the assumed distance of 2.2 kpc, the total X-ray luminosity between 0.3 and 8.0 keV is 1.2 × 1037 erg s-1. We also collected and updated the broad-band data of Puppis A between radio and GeV γ-ray range, producing its spectral energy distribution. To provide constraints to the high-energy emission models, we re-analyzed radio data, estimating the energy content in accelerated particles to be Umin = 4.8 × 1049 erg and the magnetic field strength B ∼ 26 μG. © 2013 ESO.
title	The most complete and detailed X-ray view of the SNR Puppis A
title_short	The most complete and detailed X-ray view of the SNR Puppis A
title_full	The most complete and detailed X-ray view of the SNR Puppis A
title_fullStr	The most complete and detailed X-ray view of the SNR Puppis A
title_full_unstemmed	The most complete and detailed X-ray view of the SNR Puppis A
title_sort	most complete and detailed x-ray view of the snr puppis a
publishDate	2013
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v555_n_p_Dubner http://hdl.handle.net/20.500.12110/paper_00046361_v555_n_p_Dubner
_version_	1768545765327634432

The most complete and detailed X-ray view of the SNR Puppis A

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