XMM-Newton and Chandra observations of the candidate Fermi-LAT pulsar 4FGL J1015.5-6030

Abstract

4FGL J1015.5-6030 is an unidentified Fermi-LAT source hosting a bright, extended X-ray source whose X-ray spectrum is consistent with that of a young pulsar, yet no pulsations have been found. Here we report on XMM-Newton timing and Chandra imaging observations of the X-ray counterpart of 4FGL J1015.5-6030. We find no significant periodicity from the source and place a 3$\sigma$ upper-limit on its pulsed fraction of 34$\%$. The Chandra observations resolve the point source from the extended emission. We find that the point source's spectrum is well fit by a blackbody model, with temperature $kT=0.205\pm 0.009$ keV, plus a weak power-law component, which is consistent with a thermally emitting neutron star with a magnetospheric component. The extended emission spans angular scales of a few arcseconds up to about 30${}^{\prime \prime }$ from the point source and its spectrum is well fit by a power-law model with a photon index $\Gamma =1.70\pm 0.05$. The extended emission's spectrum and 0.5-10 keV luminosity of 4$\times 10^{32}$ erg s${}^{-1}$ (at a plausible distance of 2 kpc) are consistent with that of a pulsar wind nebula. Based on a comparison to other GeV and X-ray pulsars, we find that this putative pulsar is likely a middle-aged (i.e., $\tau \sim 0.1$--1 Myr) radio-quiet pulsar with $\dot{E}\sim 10^{34}-10^{35}$ erg s${}^{-1}$.

Accepted for publication in ApJ

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