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Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5

Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5
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 4.1x10^13 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
0004-637X
65-[10pp]
Ng, C. -Y.
a7854a32-33ee-44c3-b58d-6654da468894
Kaspi, Victoria M.
0bf2292a-964f-4795-a765-0c259c7fca19
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Weltevrede, Patrick
3df79187-6c73-4ff9-a96c-49df4c8f1448
Bogdanov, Slavko
39f20582-4d71-4b1a-ae2a-b266367341ef
Shannon, Ryan
4bfa267c-512a-405b-966a-86fc601b5502
Gonzalez, Marjorie E.
1b741593-7f36-4cc3-8bf1-d04012807a36
Ng, C. -Y.
a7854a32-33ee-44c3-b58d-6654da468894
Kaspi, Victoria M.
0bf2292a-964f-4795-a765-0c259c7fca19
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Weltevrede, Patrick
3df79187-6c73-4ff9-a96c-49df4c8f1448
Bogdanov, Slavko
39f20582-4d71-4b1a-ae2a-b266367341ef
Shannon, Ryan
4bfa267c-512a-405b-966a-86fc601b5502
Gonzalez, Marjorie E.
1b741593-7f36-4cc3-8bf1-d04012807a36

Ng, C. -Y., Kaspi, Victoria M., Ho, Wynn C.G., Weltevrede, Patrick, Bogdanov, Slavko, Shannon, Ryan and Gonzalez, Marjorie E. (2012) Deep X-ray observations of the young high-magnetic-field radio pulsar J1119-6127 and supernova remnant G292.2-0.5. Astrophysical Journal, 761 (1), 65-[10pp]. (doi:10.1088/0004-637X/761/1/65).

Record type: Article

Abstract

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 4.1x10^13 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

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Published date: 21 November 2012
Organisations: Applied Mathematics

Identifiers

Local EPrints ID: 345494
URI: http://eprints.soton.ac.uk/id/eprint/345494
ISSN: 0004-637X
PURE UUID: 1ef74993-1bd6-4d36-8486-492cf4aebf0a
ORCID for Wynn C.G. Ho: ORCID iD orcid.org/0000-0002-6089-6836

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Date deposited: 23 Nov 2012 14:28
Last modified: 14 Mar 2024 12:25

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Contributors

Author: C. -Y. Ng
Author: Victoria M. Kaspi
Author: Wynn C.G. Ho ORCID iD
Author: Patrick Weltevrede
Author: Slavko Bogdanov
Author: Ryan Shannon
Author: Marjorie E. Gonzalez

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