2007/04/11 by P. Esposito, A. Tiengo, A. De Luca +1
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1051/0004-6361:20077480
published as Astronomy and Astrophysics, Volume 467, Issue 2, May IV 2007, pp.L45-L48 · Revised version (minor changes in text and figures). Accepted for publication on Astronomy and Astrophysics Letters on 10/04/2007
arxiv created 2007/04/11 · openalex publication_date 2007/04/24 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We present the first X-ray detection of the very young pulsar PSR J1357-6429 (characteristic age of 7.3 kyr) using data from the XMM-Newton and Chandra satellites. We find that the spectrum is well described by a power-law plus blackbody model, with photon index and blackbody temperature eV. For the estimated distance of 2.5 kpc, this corresponds to a 2–10 keV luminosity of ~1.2 1032 erg s-1, thus the fraction of the spin-down energy channeled by PSR J1357-6429 into X-ray emission is one of the lowest observed. The Chandra data confirm the positional coincidence with the radio pulsar and allow to set an upper limit of 3 1031 erg s-1 on the 2–10 keV luminosity of a compact pulsar wind nebula. We do not detect any pulsed emission from the source and determine an upper limit of 30% for the modulation amplitude of the X-ray emission at the radio frequency of the pulsar.