Arecibo and FAST timing follow-up of 12 millisecond pulsars discovered in Commensal Radio Astronomy FAST Survey

Miao, Chenchen; Zhu, Weiwei; Li, Di; Freire, P. C. C.; Niu, Jiarui; Wang, P; Yuan, Jianping; Xue, Mengyao; Cameron, Andrew D.; Champion, D. J.; Cruces, M.; Chen, Y T; M, M; Cheng, Xiangming; Dang, S. J.; Ding, M.; Feng, Yi; Gan, Zhenye; Hobbs, G.; Krämer, M.; Liu, Z J; Li, Y X; Luo, Z K; Miao, Xueli; Meng, L.; Niu, Chenhui; Pan, Zhichen; Qian, Lei; Zhan, Sun; Wang, N; Wang, S Q; Wang, J B; Wu, Qingdong; Wang, Y B; Wang, C J; Wang, H F; Wang, S; Xie, Xiaoyao; Xie, Meng; Xiao, Yongmao; Yuan, Mao; Yue, Youling; Yao, Jumei; Yan, W. M.; You, Shijun; Yu, Xuhong; Zhao, Di; Zhao, Ru-Shuang; Zhang, L

doi:10.1093/mnras/stac1305

Cited by 13 publications

(8 citation statements)

References 68 publications

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“…Combining all pulsars discovered in the ongoing CRAFTS and the early FAST commission pilot survey, CRAFTS has confirmed the discovery of 188 new pulsars to date. 15 This includes 40 MSPs (Wang et al 2021;Wu et al 2023b;Miao et al 2023), two DNS systems (Wu et al 2023a and this work), one high-energy young pulsar with a γ-ray counterpart (Wang et al 2021), >20 binaries (Cruces et al 2021;Miao et al 2023), and >30 rotating radio transients (Chen et al 2022).…”

Section: Introductionmentioning

confidence: 90%

“…This increases the position uncertainty in the newly discovered pulsars (especially for single-pulse detection). With the rapid growth of pulsar candidates, we strive to swiftly follow up FAST discoveries through FAST and international collaborations (Cameron et al 2020;Cruces et al 2021;Miao et al 2023). Combining all pulsars discovered in the ongoing CRAFTS and the early FAST commission pilot survey, CRAFTS has confirmed the discovery of 188 new pulsars to date.…”

Section: Introductionmentioning

confidence: 99%

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A Relativistic Double Neutron Star Binary PSR J1846-0513

Zhao,

Wang,

Yuan

et al. 2024

ApJL

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We report the timing analysis of PSR J1846−0513, a pulsar discovered by the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in Commensal Radio Astronomy FAST Survey. The pulsar possesses a spin period of 23.36 ms and a spin-down rate ( P ̇ ) of 1.0106(3) × 10−18 s s−1, and it is located in an eccentric orbit (e ∼0.208) with an orbital period of 0.61 days. The characteristic age and surface magnetic field of the pulsar are found to be 366.62 Myr and 4.9178 × 109 G, respectively, indicating that it is a recycled pulsar. Using over two years of timing data, we measure the periastron advance ω ̇ = 0.8956(8) deg yr−1. By assuming that this effect is purely relativistic, we have estimated the total mass M = 2.6287(35)M ⊙ and obtained an upper limit for the pulsar mass and a lower limit for the companion’s mass. Our results indicate that this is a double neutron star system.

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Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

A Relativistic Double Neutron Star Binary PSR J1846-0513

Zhao,

Wang,

Yuan

et al. 2024

ApJL

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“…PSR J1720−0534 (Wang et al 2021) is a Galactic field BW pulsar with a spin period of 3.26 ms discovered in the Commensal Radio Astronomy FAST Survey (CRAFTS) (Li et al 2018;Cameron et al 2020;Cruces et al 2021;Miao et al 2023). The discovery of this BW pulsar and the presentation of pulse intensity variation with a modulation period of ∼22 s during the ingress of the eclipse have been reported (Wang et al 2021).…”

Section: Introductionmentioning

confidence: 98%

Reciprocating Magnetic Fields in the Pulsar Wind Observed from the Black Widow Pulsar J1720-0534

Miao

Zhu

et al. 2023

Res. Astron. Astrophys.

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We report the radio observations of the eclipsing black widow pulsar J1720−0534, a 3.26 ms pulsar in orbit with a low mass companion of mass 0.029 to 0.034 M⊙. We obtain the phase-connected timing ephemeris and polarization profile of this millisecond pulsar (MSP) using the Five-hundred-meter Aperture Spherical Radio Telescope (FAST), the Green Bank Telescope (GBT), and the Parkes Telescope. For the first time from such a system, an oscillatory polarisation angle change was observed from a particular eclipse egress with partial depolarization, indicating 10-milliGauss-level reciprocating magnetic fields oscillating in a length scale of 5×103 km (assuming an orbital inclination angle of 90 degrees) outside the companion’s magnetosphere. The dispersion measure variation observed during the ingresses and egresses shows the rapid raising of the electron density in the shock boundary between the companion’s magnetosphere and the surrounding pulsar wind. We suggest that the observed oscillatory magnetic fields originate from the pulsar wind outside the companion’s magnetosphere.

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“…<66°in drift-scan mode (Cruces et al 2021) using the FAST 19-beam receiver with a total bandwidth of 1.05-1.45 GHz and a center frequency of 1.25 GHz (Jiang et al 2020). Currently, the CRAFTS survey has discovered about 179 new pulsars, 15 57 of which have their timing solutions reported from earlier studies (Cameron et al 2020;Cruces et al 2021;Miao et al 2023;Wu et al 2023). About 11% of the known pulsars are in binary systems (ATNF Pulsar Catalogue v1.69; Manchester et al 2005), with the majority (∼84%) being millisecond pulsars (MSPs) with spin period P < 20 ms. MSPs are proposed to be formed from the evolution of low-mass X-ray binaries (Bhattacharya & van den Heuvel 1991).…”

Section: Introductionmentioning

confidence: 99%

PSR J2150+3427: A Possible Double Neutron Star System

Wu,

Wang,

Yuan

et al. 2023

ApJL

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PSR J2150+3427 is a 0.654 s pulsar discovered by the Commensal Radio Astronomy FAST Survey. From the follow-up observations, we find that the pulsar is in a highly eccentric orbit (e = 0.601) with an orbital period of 10.592 days and a projected semimajor axis of 25.488 lt-s. Using 2.7 yr of timing data, we also measured the rate of periastron advance ω ̇ = 0.0115(4) deg yr−1. An estimate for the total mass of the system using the ω ̇ gives M tot = 2.59(13)M ⊙, which is consistent with most of the known double neutron star (DNS) systems and one neutron star (NS)–white dwarf (WD) system named B2303+46. Combining ω ̇ with the mass function of the system gives the masses of M p < 1.67 and M c > 0.98 M ⊙ for the pulsar and the companion star, respectively. This constraint, along with the spin period and orbital parameters, suggests that it is possibly a DNS system, and we cannot entirely rule out the possibility of an NS–WD system. Future timing observations will vastly improve the uncertainty in ω ̇ , and are likely to allow the detection of additional relativistic effects, which can be used to modify the values of M p and M c . With a spin-down luminosity of E ̇ = 5.07(6) × 1029 erg s−1, PSR J2150+3427 is a very low-luminosity pulsar, with only the binary pulsar J2208+4610 having a smaller E ̇ .

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Arecibo and FAST timing follow-up of 12 millisecond pulsars discovered in Commensal Radio Astronomy FAST Survey

Cited by 13 publications

References 68 publications

A Relativistic Double Neutron Star Binary PSR J1846-0513

A Relativistic Double Neutron Star Binary PSR J1846-0513

Reciprocating Magnetic Fields in the Pulsar Wind Observed from the Black Widow Pulsar J1720-0534

PSR J2150+3427: A Possible Double Neutron Star System

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