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We present a Chandra X-ray Observatory investigation of the millisecondpulsars (MSPs) in the globular cluster M28 (NGC 6626). In what is one of thedeepest X-ray observations of a globular cluster, we firmly detect seven andpossibly detect two of the twelve known M28 pulsars. With the exception of PSRsB1821-24 and J1824-2452H, the detected pulsars have relatively soft spectra,with X-ray luminosities 10^30-31 ergs s^-1 (0.3-8 keV),similar to most"recycled" pulsars in 47 Tucanae and the field of the Galaxy, implying thermalemission from the pulsar magnetic polar caps. We present the most detailedX-ray spectrum to date of the energetic PSR B1821-24. It is well described by apurely non-thermal spectrum with spectral photon index 1.23 and luminosity1.4x10^33Theta(D/5.5 kpc)^2 ergs s^-1 (0.3-8 keV), where Theta is the fractionof the sky covered by the X-ray emission beam(s). We find no evidence for thepreviously reported line emission feature around 3.3 keV, most likely as aconsequence of improvements in instrument calibration. The X-ray spectrum andpulse profile of PSR B1821--24 suggest that the bulk of unpulsed emission fromthis pulsar is not of thermal origin, and is likely due to low-levelnon-thermal magnetospheric radiation, an unresolved pulsar wind nebula, and/orsmall-angle scattering of the pulsed X-rays by interstellar dust grains. Thepeculiar binary PSR J1824-2452H shows a relatively hard X-ray spectrum andpossible variability at the binary period, indicative of an intrabinary shockformed by interaction between the relativistic pulsar wind and matter from itsnon-degenerate companion star.

Chandra X-ray Observations of 12 Millisecond Pulsars in the Globular Cluster M28