2014/06/09 by P. Arumugasamy, Prakash Arumugasamy, George G. Pavlov +3
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysical Phenomena and Observations #High-pressure geophysics and materials #Pulsars and Gravitational Waves Research #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/790/2/103
10 pages, 13 figures; accepted by ApJ
arxiv created 2014/06/09 · openalex publication_date 2014/07/10 · arxiv updated 2015/06/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We report on XMM-Newton EPIC observations of the young pulsar J2022+3842, with a characteristic age of 8.9 kyr. We detected X-ray pulsations and found the pulsation period P ≈ 48.6 ms, and its derivative , which is two times larger than previously reported values. The pulsar exhibits two very narrow (FWHM ∼1.2 ms) X-ray pulses each rotation, separated by ≈0.48 of the period, with a pulsed fraction of ≈0.8. Using the correct values of P and , we calculate the pulsar's spin-down power erg s −1 and magnetic field B = 2.1 × 10 12 G. The pulsar spectrum is well modeled with a hard power-law (PL) model (photon index Γ = 0.9 ± 0.1, hydrogen column density n H = (2.3 ± 0.3) × 10 22 cm −2 ). We detect a weak off-pulse emission, which can be modeled with a softer PL (Γ ≈ 1.7 ± 0.7), that is poorly constrained because of contamination in the EPIC-pn timing mode data. The pulsar's X-ray efficiency in the 0.5–8 keV energy band, , is similar to those of other pulsars. The XMM-Newton observation did not detect extended emission around the pulsar. Our re-analysis of Chandra X-ray Observatory archival data shows a hard, Γ ≈ 0.9 ± 0.5, spectrum and a low efficiency, η PWN ∼ 2 × 10 −5 ( D /10 kpc) 2 , for the compact pulsar wind nebula, unresolved in the XMM-Newton images.