Work

The pulsar population of Omega Centauri: New TRAPUM searches, timing, and cluster dynamics with MeerKAT and Parkes

Year: 2026
Type: article
Abstract: -3 $. We updated the timing solutions for pulsars A--E, obtained the first timing solutions for G, H, and K, and updated the orbital parameters for I, L, N, and Q. The latter three, I, N, and Q, have significantly longer orbital periods (P_ =1--7,days) than previously reported. Pulsars B, G, H, K, and L are black widows (P_ =2--4,hours); I is a wide-orbit (P_ =3.50,days) MSP with a light ∼0.05,M_⊙ companion; N and Q have ∼0.25,M_⊙ companions; and N shows a significant orbital eccentricity (e = 0.093). We folded Fermi-LAT and NICER photons to search for high-energy pulsations, but failed to detect them from individual MSPs. Significant spin period derivatives were measured for eight MSPs and interpreted as arising from the cluster gravitational potential. The inferred line-of-sight accelerations are consistent with a King-model gravitational potential, and allow us to set an upper central black hole mass limit of M_ <8 ,M$_⊙ at 90% confidence. The high fraction of isolated MSPs (58%) and black widow systems (63% of binaries), and possibly the eccentricity of N, are difficult to reconcile with MSP population predictions based solely on encounter rates. Instead, these properties require alternative formation channels or reflect the complex evolutionary history of Omega Centauri, with part of its MSP population having formed in denser environments than those observed today. b b b BH 4
Language: English
Open Access status: gold
Estimated APC paid: $1,865
OpenAlex ID: W7140190147
FWCI: 2.463
Cites: 6
Cited by: 3
Related to: 3