Chandra X-ray Observations of 12 Millisecond Pulsars in the Globular Cluster M28
van den Berg, Maureen
Heinke, Craig O.
Grindlay, Jonathan E.
Stairs, Ingrid H.
Ransom, Scott M.
Freire, Paulo C. C.
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CitationBogdanov, Slavko, Maureen van den Berg, Mathieu Servillat, Craig O. Heinke, Jonathan E. Grindlay, Ingrid H. Stairs, Scott M. Ransom, Paulo C. C. Freire, Steve Bégin, and Werner Becker. 2011. “CHANDRAX-RAY OBSERVATIONS OF 12 MILLISECOND PULSARS IN THE GLOBULAR CLUSTER M28.” The Astrophysical Journal 730 (2): 81. https://doi.org/10.1088/0004-637x/730/2/81.
AbstractWe present a Chandra X-ray Observatory investigation of the millisecond pulsars in the globular cluster M28 (NGC 6626). In what is one of the deepest X-ray observations of a globular cluster, we firmly detect seven and possibly detect two of the 12 known M28 pulsars. With the exception of PSRs B1821-24 and J1824-2452H, the detected pulsars have relatively soft spectra, with X-ray luminosities 10(30)-10(31) erg s(-1) (0.3-8 keV), similar to most "recycled" pulsars in 47 Tucanae and the field of the Galaxy, implying thermal emission from the pulsar magnetic polar caps. We present the most detailed X-ray spectrum to date of the energetic PSR B1821-24. It is well described by a purely non-thermal spectrum with spectral photon index Gamma = 1.23 and luminosity 1.4x10(33)Theta (D/5.5 kpc)(2) erg s(-1) (0.3-8 keV), where Theta is the fraction of the sky covered by the X-ray emission beam(s). We find no evidence for the previously reported line emission feature around 3.3 keV, most likely as a consequence of improvements in instrument calibration. The X-ray spectrum and pulse profile of PSR B1821-24 suggest that the bulk of unpulsed emission from this pulsar is not of thermal origin, and is likely due to low-level non-thermal magnetospheric radiation, an unresolved pulsar wind nebula, and/or small-angle scattering of the pulsed X-rays by interstellar dust grains. The peculiar binary PSR J1824-2452H shows a relatively hard X-ray spectrum and possible variability at the binary period, indicative of an intrabinary shock formed by interaction between the relativistic pulsar wind and matter from its non-degenerate companion star.
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