XMM-Newton observation of the very old pulsar J0108-1431
We report on an X-ray observation of the 166 Myr old radio pulsar J0108–1431 with XMM-Newton. The X-ray spectrum can be described by a power-law model with a relatively steep photon index Γ ≈ 3 or by a combination of thermal and non-thermal components, e.g., a power-law component with fixed photon i...
| Main Authors: | , , , , , |
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| Format: | Journal Article |
| Published: |
2012
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| Online Access: | http://hdl.handle.net/20.500.11937/7206 |
| _version_ | 1848745301114880000 |
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| author | Posselt, B. Arumugasamy, P. Pavlov, G. Manchester, R. Shannon, Ryan Kargaltsev, O. |
| author_facet | Posselt, B. Arumugasamy, P. Pavlov, G. Manchester, R. Shannon, Ryan Kargaltsev, O. |
| author_sort | Posselt, B. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | We report on an X-ray observation of the 166 Myr old radio pulsar J0108–1431 with XMM-Newton. The X-ray spectrum can be described by a power-law model with a relatively steep photon index Γ ≈ 3 or by a combination of thermal and non-thermal components, e.g., a power-law component with fixed photon index Γ = 2 plus a blackbody component with a temperature of kT = 0.11 keV. The two-component model appears more reasonable considering different estimates for the hydrogen column density N H. The non-thermal X-ray efficiency in the single power-law model is η PL1-10keV/E ~ 0.003, higher than in most other X-ray-detected pulsars. In the case of the combined model, the non-thermal and thermal X-ray efficiencies are even higher, η PL1-10keV ~ ηbbPC ~ 0.006. We detected X-ray pulsations at the radio period of P ≈ 0.808 s with significance of ≈7σ. The pulse shape in the folded X-ray light curve (0.15-2 keV) is asymmetric, with statistically significant contributions from up to five leading harmonics. Pulse profiles at two different energy ranges differ slightly: the profile is asymmetric at low energies, 0.15-1 keV, while at higher energies, 1-2 keV, it has a nearly sinusoidal shape. The radio pulse peak leads the 0.15-2 keV X-ray pulse peak by Δ ø = 0.06 ± 0.03. |
| first_indexed | 2025-11-14T06:15:11Z |
| format | Journal Article |
| id | curtin-20.500.11937-7206 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T06:15:11Z |
| publishDate | 2012 |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-72062017-09-13T14:38:34Z XMM-Newton observation of the very old pulsar J0108-1431 Posselt, B. Arumugasamy, P. Pavlov, G. Manchester, R. Shannon, Ryan Kargaltsev, O. We report on an X-ray observation of the 166 Myr old radio pulsar J0108–1431 with XMM-Newton. The X-ray spectrum can be described by a power-law model with a relatively steep photon index Γ ≈ 3 or by a combination of thermal and non-thermal components, e.g., a power-law component with fixed photon index Γ = 2 plus a blackbody component with a temperature of kT = 0.11 keV. The two-component model appears more reasonable considering different estimates for the hydrogen column density N H. The non-thermal X-ray efficiency in the single power-law model is η PL1-10keV/E ~ 0.003, higher than in most other X-ray-detected pulsars. In the case of the combined model, the non-thermal and thermal X-ray efficiencies are even higher, η PL1-10keV ~ ηbbPC ~ 0.006. We detected X-ray pulsations at the radio period of P ≈ 0.808 s with significance of ≈7σ. The pulse shape in the folded X-ray light curve (0.15-2 keV) is asymmetric, with statistically significant contributions from up to five leading harmonics. Pulse profiles at two different energy ranges differ slightly: the profile is asymmetric at low energies, 0.15-1 keV, while at higher energies, 1-2 keV, it has a nearly sinusoidal shape. The radio pulse peak leads the 0.15-2 keV X-ray pulse peak by Δ ø = 0.06 ± 0.03. 2012 Journal Article http://hdl.handle.net/20.500.11937/7206 10.1088/0004-637X/761/2/117 unknown |
| spellingShingle | Posselt, B. Arumugasamy, P. Pavlov, G. Manchester, R. Shannon, Ryan Kargaltsev, O. XMM-Newton observation of the very old pulsar J0108-1431 |
| title | XMM-Newton observation of the very old pulsar J0108-1431 |
| title_full | XMM-Newton observation of the very old pulsar J0108-1431 |
| title_fullStr | XMM-Newton observation of the very old pulsar J0108-1431 |
| title_full_unstemmed | XMM-Newton observation of the very old pulsar J0108-1431 |
| title_short | XMM-Newton observation of the very old pulsar J0108-1431 |
| title_sort | xmm-newton observation of the very old pulsar j0108-1431 |
| url | http://hdl.handle.net/20.500.11937/7206 |