HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS

Deep Chandra ACIS observations of the region around the putative pulsar, CXOU J061705.3+222127, in the supernova remnant (SNR) IC 443 reveal an ∼5″ radius ring-like structure surrounding the pulsar and a jet-like feature oriented roughly north-south across the ring and through the pulsar's loca...

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Detalles Bibliográficos
Publicado: 2015
Materias:
ISM: individual objects (G189.22+2.90 IC 443)
ISM: supernova remnants
stars: neutron
X-rays: individual (CXOU J061705.3+222127)
X-rays: ISM
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v808_n1_p_Swartz
http://hdl.handle.net/20.500.12110/paper_0004637X_v808_n1_p_Swartz
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v808_n1_p_Swartz
record_format dspace
spelling paper:paper_0004637X_v808_n1_p_Swartz2023-06-08T14:29:14Z HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS ISM: individual objects (G189.22+2.90 IC 443) ISM: supernova remnants stars: neutron X-rays: individual (CXOU J061705.3+222127) X-rays: ISM Deep Chandra ACIS observations of the region around the putative pulsar, CXOU J061705.3+222127, in the supernova remnant (SNR) IC 443 reveal an ∼5″ radius ring-like structure surrounding the pulsar and a jet-like feature oriented roughly north-south across the ring and through the pulsar's location at 06 h 17 m 5.200 + 2221′27.″52 (J2000.0 coordinates). The observations further confirm that (1) the spectrum and flux of the central object are consistent with a rotation-powered pulsar, (2) the non-thermal spectrum and morphology of the surrounding nebula are consistent with a pulsar wind, and (3) the spectrum at greater distances is consistent with thermal emission from the SNR. The cometary shape of the nebula, suggesting motion toward the southwest, appears to be subsonic: There is no evidence either spectrally or morphologically for a bow shock or contact discontinuity; the nearly circular ring is not distorted by motion through the ambient medium; and the shape near the apex of the nebula is narrow. Comparing this observation with previous observations of the same target, we set a 99% confidence upper limit to the proper motion of CXOU J061705.3+222127 to be less than 44 mas yr -1 (310 km s -1 for a distance of 1.5 kpc), with the best-fit (but not statistically significant) projected direction toward the west. © 2015. The American Astronomical Society. All rights reserved.. 2015 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v808_n1_p_Swartz http://hdl.handle.net/20.500.12110/paper_0004637X_v808_n1_p_Swartz
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 (G189.22+2.90 IC 443)
ISM: supernova remnants
stars: neutron
X-rays: individual (CXOU J061705.3+222127)
X-rays: ISM
spellingShingle ISM: individual objects (G189.22+2.90 IC 443)
ISM: supernova remnants
stars: neutron
X-rays: individual (CXOU J061705.3+222127)
X-rays: ISM
HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS
topic_facet ISM: individual objects (G189.22+2.90 IC 443)
ISM: supernova remnants
stars: neutron
X-rays: individual (CXOU J061705.3+222127)
X-rays: ISM
description Deep Chandra ACIS observations of the region around the putative pulsar, CXOU J061705.3+222127, in the supernova remnant (SNR) IC 443 reveal an ∼5″ radius ring-like structure surrounding the pulsar and a jet-like feature oriented roughly north-south across the ring and through the pulsar's location at 06 h 17 m 5.200 + 2221′27.″52 (J2000.0 coordinates). The observations further confirm that (1) the spectrum and flux of the central object are consistent with a rotation-powered pulsar, (2) the non-thermal spectrum and morphology of the surrounding nebula are consistent with a pulsar wind, and (3) the spectrum at greater distances is consistent with thermal emission from the SNR. The cometary shape of the nebula, suggesting motion toward the southwest, appears to be subsonic: There is no evidence either spectrally or morphologically for a bow shock or contact discontinuity; the nearly circular ring is not distorted by motion through the ambient medium; and the shape near the apex of the nebula is narrow. Comparing this observation with previous observations of the same target, we set a 99% confidence upper limit to the proper motion of CXOU J061705.3+222127 to be less than 44 mas yr -1 (310 km s -1 for a distance of 1.5 kpc), with the best-fit (but not statistically significant) projected direction toward the west. © 2015. The American Astronomical Society. All rights reserved..
title HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS
title_short HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS
title_full HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS
title_fullStr HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS
title_full_unstemmed HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY of the IC 443 PULSAR WIND NEBULA and ENVIRONS
title_sort high spatial resolution x-ray spectroscopy of the ic 443 pulsar wind nebula and environs
publishDate 2015
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v808_n1_p_Swartz
http://hdl.handle.net/20.500.12110/paper_0004637X_v808_n1_p_Swartz
_version_ 1768543875577675776

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