Abstract
We present the timing of the first five millisecond pulsars discovered in the globular cluster Omega Centauri and the discovery of a pulsar with a spin period of 3.68 ms. With a timing baseline of ∼3.5 yr we are able to measure the derivative of the spin frequency (υ·) for the first five pulsars. Upper limits on the pulsar line-of-sight acceleration are estimated and compared with predictions based on analytical models of the cluster. We find that PSRs J1326-4728B and D show large negative accelerations, which are in tension with the minimum acceleration predicted by analytical models. We searched for pulsed γ-ray signals using 14.3 yr of data from the Fermi Large Area Telescope. Although we found no evidence for γ-ray pulsations, PSRs J1326-4728A, B, C, and E are associated with X-ray sources. This suggests that the observed γ-ray emission from Omega Centauri is likely caused by the emission of the ensemble of MSPs.
Original language | English |
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Pages (from-to) | 2616-2622 |
Number of pages | 7 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 521 |
Issue number | 2 |
DOIs | |
Publication status | Published - 1 May 2023 |