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Micro-second Timing of PSR B1821-24 with Chandra/HRC-S | | Robert E. Rutledge
; Derek W. Fox
; S. R. Kulkarni
; Bryan A. Jacoby
; I. Cognard
; D. C. Backer
; Stephen S. Murray
; | | Date: |
22 Dec 2002 | | Journal: | Astrophys.J. 613 (2004) 522-531 | | Subject: | astro-ph | | Affiliation: | Caltech), I. Cognard (Nancay), D. C. Backer (UCB), and Stephen S. Murray (CfA | | Abstract: | We perform absolute timing of PSR B1821-24 in M28, using a 50 ksec observation with Chandra/HRC-S. We have obtained the highest signal-to-noise X-ray pulsed lightcurve of this source to date, detecting two X-ray pulses, as well as significant non-pulsed emission -- a persistent X-ray flux which comprises 15+/-3% of the total X-ray flux of the pulsar. The Gaussian width of the sharp X-ray peak is 34+/-3 micro-sec in time, implying a size of the X-ray beam as it crosses the line of sight of 4.0+/-0.4 deg. We find evidence for a significant trailing component in both X-ray peaks of the pulse profile. Including three RXTE/PCA observations in our analysis, and tying the phases together using a radio ephemeris obtained at Nancay, we find the absolute phases in the X-ray wander with respect to this radio ephemeris by up to 60 micro-sec, likely due to the variable dispersion measure, which changes the pulse arrival time in the radio band but not the X-ray band. The present analysis makes clear that study of pulsar timing noise properties in millisecond pulsars such as PSR B1821-24 -- hitherto only studied at radio wavelengths, where variable dispersion measure requires a significant correction -- can be studied at X-ray wavelengths, where the effect of variable dispersion measure is negligible. We also examine the known uncertainties in the absolute Chandra/HRC-S timing accuracy, which amount to +/-12 microsec. We limit the amount of linear drift in the relative timing accuracy of HRC-S to <3e-10 s s-1. | | Source: | arXiv, astro-ph/0301453 | | Services: | Forum | Review | PDF | Favorites | |
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