PSR J2222−0137

Guo, Y.; Freire, P. C. C.; Guillemot, L.; Krämer, M.; Zhu, Weiwei; Wex, Norbert; McKee, James W.; Deller, Adam T.; Ding, Hao; Kaplan, David L.; Stappers, B. W.; Cognard, I.; Miao, Xueli; Haase, Lorenz Matthias; Keith, Michael; Ransom, Scott M.; Theureau, G.

doi:10.1051/0004-6361/202141450

Cited by 42 publications

(29 citation statements)

References 58 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For this reason, it is important to take into account kinematic contributions to this quantity, in order to obtain an estimate of the intrinsic spin period derivatives, P int  . To do this, we follow the analytic equations and quantities used in Section 7 of Guo et al (2021). In the case of PSR J1828+0625, we can estimate the intrinsic spindown since we know the proper motion.…”

Section: Timing Studymentioning

confidence: 99%

Serendipitous Discovery of Three Millisecond Pulsars with the GMRT in Fermi-directed Survey and Follow-up Radio Timing

Bhattacharyya

Roy

Freire

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

We report the discovery of three millisecond pulsars (MSPs): PSRs J1120−3618, J1646−2142, and J1828+0625 with the Giant Metrewave Radio Telescope (GMRT) at a frequency of 322 MHz using a 32 MHz observing bandwidth. These sources were discovered serendipitously while conducting the deep observations to search for millisecond radio pulsations in the directions of unidentified Fermi Large Area Telescope (LAT) γ-ray sources. We also present phase coherent timing models for these MSPs using ∼5 yr of observations with the GMRT. PSR J1120−3618 has a 5.5 ms spin period and is in a binary system with an orbital period of 5.6 days and minimum companion mass of 0.18 M ⊙, PSR J1646−2142 is an isolated object with a spin period of 5.8 ms, and PSR J1828+0625 has a spin period of 3.6 ms and is in a binary system with an orbital period of 77.9 days and minimum companion mass of 0.27 M ⊙. The two binaries have very low orbital eccentricities, in agreement with expectations for MSP-helium white dwarf systems. Using the GMRT 607 MHz receivers having a 32 MHz bandwidth, we have also detected PSR J1646−2142 and PSR J1828+0625, but not PSR J1120−3618. PSR J1646−2142 has a wide profile, with significant evolution between 322 and 607 MHz, whereas PSR J1120−3618 exhibits a single peaked profile at 322 MHz and PSR J1828+0625 exhibits a single peaked profile at both the observing frequencies. These MSPs do not have γ-ray counterparts, indicating that these are not associated with the target Fermi LAT pointing emphasizing the significance of deep blind searches for MSPs.

show abstract

Section: Timing Studymentioning

confidence: 99%

Serendipitous Discovery of Three Millisecond Pulsars with the GMRT in Fermi-directed Survey and Follow-up Radio Timing

Bhattacharyya

Roy

Freire

et al. 2022

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Recently, despite the overall difficulty in describing the position angles of recycled pulsars with RVMs, a number of cases have been presented where the orbital inclination angle determined from RVM fits was indeed in very good agreement with the value inferred from pulsar timing (see e.g. Guo et al 2021 andKramer et al 2021b). Motivated by these previous findings, and with the described caveats in mind, we investigate whether the difference between ζ and i could also be due to our assumption of spin-orbit alignment.…”

Section: Geometry Of Psr J0955−6150 From Pulse Structure Datamentioning

confidence: 92%

The eccentric millisecond pulsar, PSR J0955−6150

Serylak

Krishnan

Freire

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Context. PSR J0955−6150 is a member of an enigmatic class of eccentric millisecond pulsar (MSP) and helium white dwarf (He WD) systems (eMSPs), whose binary evolution is poorly understood and believed to be strikingly different to that of traditional MSP+He WD systems in circular orbits. Aims. Measuring the masses of the stars in this system is important for testing the different hypotheses for the formation of eMSPs. Methods. We carried out timing observations of this pulsar with the Parkes radio telescope using the 20 cm multibeam and ultra-wide bandwidth low-frequency (UWL) receivers, and the L-band receiver of the MeerKAT radio telescope. The pulse profiles were flux and polarisation calibrated, and a rotating-vector model (RVM) was fitted to the position angle of the linear polarisation of the combined MeerKAT data. Pulse times of arrival (ToAs) were obtained from these using standard pulsar analysis techniques and analysed using the TEMPO2 timing software. Results. Our observations reveal a strong frequency evolution of this MSP’s intensity, with a flux density spectral index (α) of −3.13(2). The improved sensitivity of MeerKAT resulted in a greater than tenfold improvement in the timing precision obtained compared to our older Parkes observations. This, combined with the eight-year timing baseline, has allowed precise measurements of a very small proper motion and three orbital post-Keplerian parameters, namely the rate of advance of periastron, ω̇ = 0.00152(1) deg yr−1, and the orthometric Shapiro delay parameters, h3 = 0.89(7) μs and ς = 0.88(2). Assuming general relativity, we obtain Mp = 1.71(2) M⊙ for the mass of the pulsar and Mc = 0.254(2) M⊙ for the mass of the companion; the orbital inclination is 83.2(4) degrees. Crucially, assuming that the position angle of the linear polarisation follows the RVM, we find that the spin axis has a misalignment relative to the orbital angular momentum of > 4.8deg at 99% confidence level. Conclusions. While the value of Mp falls well within the wide range observed in eMSPs, Mc is significantly smaller than expected from several formation hypotheses proposed, which are therefore unlikely to be correct and can be ruled out; Mc is also significantly different from the expected value for an ideal low mass X-ray binary evolution scenario. If the misalignment between the spin axis of the pulsar and the orbital angular momentum is to be believed, it suggests that the unknown process that created the orbital eccentricity of the binary was also capable of changing its orbital orientation, an important evidence for understanding the origin of eMSPs.

show abstract

“…Moreover, recently, despite the overall difficulty in describing the position angles of recycled pulsars with RVMs, a number of cases has been presented where the orbital inclination angle determined from RVM-fits was indeed in very good agreement with the value inferred from pulsar timing (see e.g. Guo et al 2021 andKramer et al 2021b). Motivated by these previous findings, and with the described caveats in mind, we investigate if the difference between ζ and i could also be due to our assumption of spin-orbit alignment.…”

Section: Geometry Of Psr J0955−6150 From Pulse Structure Datamentioning

confidence: 97%

The eccentric millisecond pulsar, PSR J0955$-$6150 I: Pulse profile analysis, mass measurements and constraints on binary evolution

Serylak,

Krishnan,

Freire

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

Context. PSR J0955−6150 is a member of an enigmatic class of eccentric MSP+He WD systems (eMSPs), whose binary evolution is poorly understood and believed to be strikingly different to that of traditional MSP+He WD systems in circular orbits. Aims. Measuring the masses of the stars in this system is important for testing the different hypotheses for the formation of eMSPs. Methods. We have carried out timing observations of this pulsar with the Parkes radio telescope using the 20-cm multibeam and ultra-wide bandwidth low-frequency (UWL) receivers, and the L-band receiver of the MeerKAT radio telescope. The pulse profiles were flux and polarisation calibrated, and a Rotating Vector Model (RVM) was fitted to the position angle of the linear polarisation of the combined MeerKAT data. Pulse times of arrival (ToAs) were obtained from these using standard pulsar analysis techniques and analysed using the tempo2 timing software. Results. Our observations reveal a strong frequency evolution of this millisecond pulsar's intensity, with a flux density spectral index (α) of −3.13(2). The improved sensitivity of MeerKAT has resulted in a > 10-fold improvement in the timing precision obtained compared to our older Parkes observations. This, combined with the 8-year timing baseline, has allowed precise measurements of a very small proper motion and three orbital "post-Keplerian" parameters, namely the rate of advance of periastron, ω = 0.00152(1) deg yr −1 and the orthometric Shapiro delay parameters: h 3 = 0.89(7) µs and ς = 0.88(2). Assuming general relativity, we obtain M p = 1.71(2) M for the mass of the pulsar and M c = 0.254(2) M for the mass of the companion; the orbital inclination is 83.2(4) degrees. Crucially, assuming that the position angle of the linear polarisation follows the rotating vector model, we find that the spin axis has a misalignment relative to the orbital angular momentum of > 4.8 deg at 99% CI. Conclusions. While the value of M p falls well within the wide range observed in eMSPs, M c is significantly smaller than expected by several formation hypotheses proposed, which are therefore unlikely to be correct and can be ruled out. M c is also significantly different from the expected value for an ideal low mass X-ray binary evolution scenario. If the misalignment between the spin axis of the pulsar and the orbital angular momentum is to be believed, it suggests that the unknown process that created the orbital eccentricity of the binary was also capable of changing its orbital orientation, an important evidence for understanding the origin of eMSPs.

show abstract

PSR J2222−0137

Cited by 42 publications

References 58 publications

Serendipitous Discovery of Three Millisecond Pulsars with the GMRT in Fermi-directed Survey and Follow-up Radio Timing

Serendipitous Discovery of Three Millisecond Pulsars with the GMRT in Fermi-directed Survey and Follow-up Radio Timing

The eccentric millisecond pulsar, PSR J0955−6150

The eccentric millisecond pulsar, PSR J0955$-$6150 I: Pulse profile analysis, mass measurements and constraints on binary evolution

Contact Info

Product

Resources

About