Timing of pulsars in the globular cluster omega centauri

被引：4
作者：
Dai, S. [1 ,2 ]
Johnston, S. [2 ]
Kerr, M. [3 ]
Berteaud, J. [4 ,5 ]
Bhattacharyya, B. [6 ]
Camilo, F. [7 ]
Keane, E. [8 ]
机构：
[1] Western Sydney Univ, Sch Sci, Locked Bag 1797, Penrith, NSW 2751, Australia
[2] Australia Telescope Natl Facil, CSIRO, Space & Astron, POB 76, Epping, NSW 1710, Australia
[3] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA
[4] USMB, CNRS, LAPTh, F-74940 Annecy, France
[5] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France
[6] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, India
[7] South African Radio Astron Observ, 2 Fir St, ZA-7925 Observatory, South Africa
[8] Trinity Coll Dublin, Sch Phys, 2 Coll Green, Dublin D02PN40, Ireland
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 521卷 / 02期
基金：
澳大利亚研究理事会; 美国国家航空航天局;
关键词：
pulsars: general; globular clusters: individual: Omega Centauri; Gamma-rays: stars; LONG-TERM OBSERVATIONS; MASS BLACK-HOLES; 47; TUCANAE; MILLISECOND PULSARS; STAR-CLUSTERS; DARK-MATTER; MILKY-WAY; GAIA EDR3; CONSTRAINTS; PROFILES;
D O I：
10.1093/mnras/stad704
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present the timing of the first five millisecond pulsars disco v ered in the globular cluster Omega Centauri and the disco v ery of a pulsar with a spin period of 3.68 ms. With a timing baseline of similar to 3.5 yr we are able to measure the deri v ati ve of the spin frequency (nu) 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 ne gativ e accelerations, which are in tension with the minimum acceleration predicted by analytical models. We searched for pulsed gamma-ray signals using 14.3 yr of data from the Fermi Large Area Telescope. Although we found no evidence for gamma-ray pulsations, PSRs J1326-4728A, B, C, and E are associated with X-ray sources. This suggests that the observed gamma-ray emission from Omega Centauri is likely caused by the emission of the ensemble of MSPs. Finally, the linearly polarized emission from PSR J1326 -4728A yields a rotation measure of -18 +/- 8 rad m(-2).
引用
收藏
页码：2616 / 2622
页数：7
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