Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5
High-magnetic-field radio pulsars are important transition objects for understanding the connection between magnetars and conventional radio pulsars. We present a detailed study of the young radio pulsar J1119-6127, which has a characteristic age of 1900 yr and a spin-down-inferred magnetic field of...
| Main Authors: | , , , , , , |
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| Format: | Journal Article |
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Institute of Physics Publishing
2012
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| Online Access: | http://hdl.handle.net/20.500.11937/35806 |
| _version_ | 1848754596568104960 |
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| author | Ng, C. Kaspi, V. Ho, W. Weltevrede, P. Bogdanov, S. Shannon, Ryan Gonzalez, M. |
| author_facet | Ng, C. Kaspi, V. Ho, W. Weltevrede, P. Bogdanov, S. Shannon, Ryan Gonzalez, M. |
| author_sort | Ng, C. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | High-magnetic-field radio pulsars are important transition objects for understanding the connection between magnetars and conventional radio pulsars. We present a detailed study of the young radio pulsar J1119-6127, which has a characteristic age of 1900 yr and a spin-down-inferred magnetic field of 4.1 × 1013 G, and its associated supernova remnant G292.2-0.5, using deep XMM-Newton and Chandra X-ray Observatory exposures of over 120 ks from each telescope. The pulsar emission shows strong modulation below 2.5 keV with a single-peaked profile and a large pulsed fraction of 0.48 ± 0.12. Employing a magnetic, partially ionized hydrogen atmosphere model, we find that the observed pulse profile can be produced by a single hot spot of temperature 0.13 keV covering about one-third of the stellar surface, and we place an upper limit of 0.08 keV for an antipodal hot spot with the same area. The non-uniform surface temperature distribution could be the result of anisotropic heat conduction under a strong magnetic field, and a single-peaked profile seems common among high-B radio pulsars. For the associated remnant G292.2-0.5, its large diameter could be attributed to fast expansion in a low-density wind cavity, likely formed by a Wolf-Rayet progenitor, similar to two other high-B radio pulsars. |
| first_indexed | 2025-11-14T08:42:56Z |
| format | Journal Article |
| id | curtin-20.500.11937-35806 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T08:42:56Z |
| publishDate | 2012 |
| publisher | Institute of Physics Publishing |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-358062023-02-22T06:24:17Z Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 Ng, C. Kaspi, V. Ho, W. Weltevrede, P. Bogdanov, S. Shannon, Ryan Gonzalez, M. High-magnetic-field radio pulsars are important transition objects for understanding the connection between magnetars and conventional radio pulsars. We present a detailed study of the young radio pulsar J1119-6127, which has a characteristic age of 1900 yr and a spin-down-inferred magnetic field of 4.1 × 1013 G, and its associated supernova remnant G292.2-0.5, using deep XMM-Newton and Chandra X-ray Observatory exposures of over 120 ks from each telescope. The pulsar emission shows strong modulation below 2.5 keV with a single-peaked profile and a large pulsed fraction of 0.48 ± 0.12. Employing a magnetic, partially ionized hydrogen atmosphere model, we find that the observed pulse profile can be produced by a single hot spot of temperature 0.13 keV covering about one-third of the stellar surface, and we place an upper limit of 0.08 keV for an antipodal hot spot with the same area. The non-uniform surface temperature distribution could be the result of anisotropic heat conduction under a strong magnetic field, and a single-peaked profile seems common among high-B radio pulsars. For the associated remnant G292.2-0.5, its large diameter could be attributed to fast expansion in a low-density wind cavity, likely formed by a Wolf-Rayet progenitor, similar to two other high-B radio pulsars. 2012 Journal Article http://hdl.handle.net/20.500.11937/35806 10.1088/0004-637X/761/1/65 Institute of Physics Publishing unknown |
| spellingShingle | Ng, C. Kaspi, V. Ho, W. Weltevrede, P. Bogdanov, S. Shannon, Ryan Gonzalez, M. Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 |
| title | Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 |
| title_full | Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 |
| title_fullStr | Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 |
| title_full_unstemmed | Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 |
| title_short | Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5 |
| title_sort | deep x-ray observations of the young high-magnetic-field radio pulsar j1119-6127 and supernova remnant g292.2-0.5 |
| url | http://hdl.handle.net/20.500.11937/35806 |