Timing of pulsars in the globular cluster Omega Centauri

S. Dai; S. Johnston; M. Kerr; J. Berteaud; B. Bhattacharyya; F. Camilo; E. Keane

doi:10.1093/mnras/stad704

Timing of pulsars in the globular cluster Omega Centauri

S. Dai, S. Johnston, M. Kerr, J. Berteaud, B. Bhattacharyya, F. Camilo, E. Keane

Western Sydney University

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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
Pages (from-to)	2616-2622
Number of pages	7
Journal	Monthly Notices of the Royal Astronomical Society
Volume	521
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stad704
Publication status	Published - 1 May 2023

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Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.

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10.1093/mnras/stad704

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title = "Timing of pulsars in the globular cluster Omega Centauri",

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.",

author = "S. Dai and S. Johnston and M. Kerr and J. Berteaud and B. Bhattacharyya and F. Camilo and E. Keane",

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doi = "10.1093/mnras/stad704",

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T1 - Timing of pulsars in the globular cluster Omega Centauri

AU - Dai, S.

AU - Johnston, S.

AU - Kerr, M.

AU - Berteaud, J.

AU - Bhattacharyya, B.

AU - Camilo, F.

AU - Keane, E.

PY - 2023/5/1

Y1 - 2023/5/1

N2 - 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.

AB - 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.

UR - https://hdl.handle.net/1959.7/uws:78198

U2 - 10.1093/mnras/stad704

DO - 10.1093/mnras/stad704

M3 - Article

SN - 0035-8711

VL - 521

SP - 2616

EP - 2622

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

Timing of pulsars in the globular cluster Omega Centauri

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