The FAST Discovery of Three Radio Pulsars Coincident with Fermi-LAT Gamma-ray Sources

ATel #17384; Jianhua Fang(ZL), Pei Wang(NAOC), Dengke Zhou(ZL), Huaxi Chen(ZL), Yi Feng(ZL), Kuang Mao(ZL), Qi Wang(ZL), Zhaorong Tang(ZL), Qiuhong Pan(ZL), Dantong Jin(ZL), Di Li(THU/NAOC)
on 11 Sep 2025; 06:52 UT
Credential Certification: Pei Wang (wangpei@nao.cas.cn)

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We report the FAST (Five-hundred-meter Aperture Spherical radio Telescope, [1]) discovery of three new radio pulsars coincident with previously unassociated Fermi-LAT gamma-ray sources from the Fourth Fermi-LAT catalog (4FGL, [2][3]).
The pulsar PSR J1904-0708, associated with 4FGL J1904.7-0708, was first detected in FAST data taken on 23 March 2025. It was detected in this single epoch with a dispersion measure (DM) of 87.15 pc cm^-3 and a spin period of P=2.06 ms. Archival Swift-XRT observations of the region revealed an X-ray counterpart with a count rate of (1.0 ± 0.2) × 10^-2 counts/s, based on 34 photons. Previous analysis combining Fermi gamma-ray data and machine learning identified this source as a high-probability pulsar candidate [4].
The pulsar PSR J1730-0359, associated with 4FGL J1730.4-0359, was first detected in FAST observations on 28 March 2025. It was observed in this single epoch with a dispersion measure of 22.45 pc cm^-3 and a spin period of P = 5.09 ms.
The pulsar PSR J1827+1141, associated with 4FGL J1827.5+1141, was first detected in FAST observations on 31 March 2025. It was detected in this single epoch with a dispersion measure of 45.10 pc cm^-3 and a spin period of P = 2.66 ms. This source had previously been identified by the MeerKAT TRAPUM survey as a high-confidence gamma-ray pulsar candidate (random forest probability 0.96), with imaging sensitivity in the range of 59-111 μJy [5].
We have proposed further FAST observations to conduct phase-connected timing and to better constrain the rotational and emission properties of these pulsars. We also encourage more target observations with multi-band facilities.
References:
[1] Nan et al. 2011, IJMPD, 20, 989, doi:10.1142/S0218271811019335arXiv: 1105.3794
[2] Ballet et al. 2023, arXiv:2307.12546
[3]Smith et al. 2023, ApJ, 958, 191, doi:10.3847/1538-4357/acee67, arXiv: 2307.11132
[4] Kaur et al. 2019, ApJ, 887, 18, doi:10.3847/1538-4357/ab4ceb
[5] Clark et al. 2023, MNRAS, 519, 5590, arXiv:2212.08528