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The pulsar population of Omega Centauri: New TRAPUM searches, timing, and cluster dynamics with MeerKAT and Parkes
High Energy Astrophysical Phenomena · Submitted 23 Mar 2026 · Published version
abstract compiled · 2026-11-02 · no language-model review
The authors' main claim 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.
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The abstract, sentence by sentence
Millisecond pulsars (MSPs) are probes of globular clusters, tracing their stellar evolution, cluster dynamics, and gravitational potential. We searched for and timed MSPs in the Omega Centauri, then investigated their high-energy emission, the cluster potential, and MSP demographics. We performed Fourier-domain acceleration and jerk searches on MeerKAT observations, followed by pulsar timing using MeerKAT and Parkes Murriyang data spanning 2021-2025. We discovered the new isolated MSP PSR J1326-4728S (PSR S, Ps=4.538 ms and DM=96.24 pc/cm3. We updated the timing solutions for PSRs 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 (Pb=1-7 days) than previously reported. Pulsars B, G, H, K, and L are black widows (Pb=2-4 hours); I is a wide-orbit (Pb=3.50 days) MSP with a light ~0.05 Mo companion; N and Q have ~0.25 Mo 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 Mbh<8e4 Mo 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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Millisecond pulsars (MSPs) are probes of globular clusters, tracing their stellar evolution, cluster dynamics, and gravitational potential. | background 1.00 | 0.05 | 0.03 | asserted 1.00 |
| s1 | We searched for and timed MSPs in the Omega Centauri, then investigated their high-energy emission, the cluster potential, and MSP demographics. | contribution 1.00 | 0.96 | 0.05 | asserted 0.91 |
| s2 | We performed Fourier-domain acceleration and jerk searches on MeerKAT observations, followed by pulsar timing using MeerKAT and Parkes Murriyang data spanning 2021-2025. | method 1.00 | 0.98 | 0.02 | asserted 1.00 |
| s3 | We discovered the new isolated MSP PSR J1326-4728S (PSR S, Ps=4.538 ms and DM=96.24 pc/cm3. | result 0.96 | 0.97 | 0.03 | asserted 1.00 |
| s4 | We updated the timing solutions for PSRs A-E, obtained the first timing solutions for G, H, and K, and updated the orbital parameters for I, L, N, and Q. | result 0.61 | 0.97 | 0.03 | asserted 1.00 |
| s5 | The latter three, I, N, and Q, have significantly longer orbital periods (Pb=1-7 days) than previously reported. | result 1.00 | 0.86 | 0.04 | asserted 1.00 |
| s6 | Pulsars B, G, H, K, and L are black widows (Pb=2-4 hours); I is a wide-orbit (Pb=3.50 days) MSP with a light ~0.05 Mo companion; N and Q have ~0.25 Mo companions; and N shows a significant orbital eccentricity (e=0.093). | result 1.00 | 0.91 | 0.05 | asserted 1.00 |
| s7 | We folded Fermi-LAT and NICER photons to search for high-energy pulsations, but failed to detect them from individual MSPs. | result 0.92 | 0.97 | 0.02 | asserted 1.00 |
| s8 | Significant spin period derivatives were measured for eight MSPs and interpreted as arising from the cluster gravitational potential. | result 0.75 | 0.96 | 0.08 | asserted 0.97 |
| s9 | 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 Mbh<8e4 Mo at 90% confidence. | result 0.91 | 0.95 | 0.21 | hedged possibility 0.65 |
| s10 | 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. | interpretation 0.79 | 0.85 | 0.29 | asserted 0.61 |
| s11 | 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. | interpretation 1.00 | 0.48 | 0.63 | asserted 0.66 |
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The paper
Original abstract
Millisecond pulsars (MSPs) are probes of globular clusters, tracing their stellar evolution, cluster dynamics, and gravitational potential. We searched for and timed MSPs in the Omega Centauri, then investigated their high-energy emission, the cluster potential, and MSP demographics. We performed Fourier-domain acceleration and jerk searches on MeerKAT observations, followed by pulsar timing using MeerKAT and Parkes Murriyang data spanning 2021-2025. We discovered the new isolated MSP PSR J1326-4728S (PSR S, Ps=4.538 ms and DM=96.24 pc/cm3. We updated the timing solutions for PSRs 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 (Pb=1-7 days) than previously reported. Pulsars B, G, H, K, and L are black widows (Pb=2-4 hours); I is a wide-orbit (Pb=3.50 days) MSP with a light ~0.05 Mo companion; N and Q have ~0.25 Mo 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 Mbh<8e4 Mo 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.
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