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FAST discovery of an extremely radio-faint millisecond pulsar from the Fermi-LAT unassociated source 3FGL J0318.1+0252

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Abstract

High sensitivity radio searches of unassociated γ-ray sources have proven to be an effective way of finding new pulsars. Using the Five-hundred-meter Aperture Spherical radio Telescope (FAST) during its commissioning phase, we have carried out a number of targeted deep searches of Fermi Large Area Telescope (LAT) γ-ray sources. On February 27, 2018 we discovered an isolated millisecond pulsar (MSP), PSR J0318+0253, coincident with the unassociated γ-ray source 3FGL J0318.1+0252. PSR J0318+0253 has a spin period of 5.19 ms, a dispersion measure (DM) of 26 pc cm−3 corresponding to a DM distance of about 1.3 kpc, and a period-averaged flux density of (∼11±2) µJy at L-band (1.05–1.45 GHz). Among all high energy MSPs, PSR J0318+0253 is the faintest ever detected in radio bands, by a factor of at least ∼4 in terms of L-band fluxes. With the aid of the radio ephemeris, an analysis of 9.6 years of Fermi-LAT data revealed that PSR J0318+0253 also displays strong γ-ray pulsations. Follow-up observations carried out by both Arecibo and FAST suggest a likely spectral turn-over around 350 MHz. This is the first result from the collaboration between FAST and the Fermi-LAT teams as well as the first confirmed new MSP discovery by FAST, raising hopes for the detection of many more MSPs. Such discoveries will make a significant contribution to our understanding of the neutron star zoo while potentially contributing to the future detection of gravitational waves, via pulsar timing array (PTA) experiments.

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Authors and Affiliations

  1. CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China

    Pei Wang, Di Li, Weiwei Zhu, Lei Qian, Youling Yue, Zhichen Pan, Jumei Yao, Jun Yan & Chengmin Zhang

  2. University of Chinese Academy of Sciences, Beijing, 100049, China

    Di Li

  3. Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, University of Manchester, Manchester, M13 9PL, UK

    Colin J. Clark

  4. Department of Physics and Laboratory for Space Research, University of Hong Kong, Hong Kong, 999077, China

    Pablo M. Saz Parkinson & Kwok Lung Fan

  5. Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, CA, 95064, USA

    Pablo M. Saz Parkinson

  6. Yunnan Observatories, Chinese Academy of Sciences, Kunming, 650216, China

    Xian Hou

  7. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, 650216, China

    Xian Hou

  8. School of Computer Science and Technology, Key Laboratory of Information and Computing Guizhou Province, Guizhou Normal University, Guiyang, 550001, China

    Zhijie Liu, Xuhong Yu, Shanping You, Xiaoyao Xie & Hui Zhang

  9. School of Physics and Electronic Science, Guizhou Normal University, Guiyang, 550001, China

    Qijun Zhi

  10. Physics Department, Stanford University, Stanford, CA, 94305, USA

    Peter F. Michelson

  11. UMCP/CRESST/GSFC, NASA, Greenbelt, Maryland MD, 20771, USA

    Elizabeth C. Ferrara

  12. GSFC, NASA, Greenbelt, Maryland MD, 20771, USA

    David J. Thompson

  13. Centre d’Études Nucléaires de Bordeaux Gradignan, IN2P3/CNRS, Université Bordeaux, Gradignan, 33175, France

    David A. Smith

  14. Space Science Division, U.S. Naval Research Laboratory, Washington DC, 20375-5352, USA

    Paul S. Ray & Matthew Kerr

  15. Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, 200030, China

    Zhiqiang Shen

  16. Xinjiang Astronomical Observatory, Urumqi, 830011, China

    Na Wang

  17. Department of Physics, University of Maryland, College Park, MD, 20742, USA

    Kwok Lung Fan

  18. NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban, 4000, South Africa

    Colin J. Clark

Authors
  1. Pei Wang
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  2. Di Li
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  3. Colin J. Clark
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  6. Weiwei Zhu
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  9. Zhichen Pan
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  17. Jun Yan
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  18. Chengmin Zhang
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  19. Kwok Lung Fan
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  20. Paul S. Ray
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  21. Matthew Kerr
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  27. Na Wang
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Consortia

FAST & Fermi-LAT Collaboration

Corresponding authors

Correspondence to Pei Wang or Di Li.

Additional information

This work was supported by the National Natural Science Foundation of China (Grant Nos. 11988101, 11690024, 11743002, 11873067, U1631132, U1831131, U1731238, U1938103, 11703047, 11773041, and 11673060), the National Key R&D Program of China (Grant No. 2017YFA0402600), the Chinese Academy of Sciences (CAS) Key Laboratory of FAST, NAOC, Chinese Academy of Sciences, the National Basic Research Program of China (Grant No. 2015CB857100), the CAS Strategic Priority Research Program (Grant No. XDB23000000), the CAS International Partnership Program (Grant No. 114A11KYSB20160008), the Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences and Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing, Guizhou Normal University. Pei Wang acknowledges support by the Youth Innovation Promotion Association CAS (Grant No. 2021055), the CAS Project for Young Scientists in Basic Reasearch (Grant No. YSBR-006), and the Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS. Zhichen Pan and Xian Hou are supported by the CAS “Light of West China” Program. FAST is a Chinese national mega-science facility, built and operated by the National Astronomical Observatories, Chinese Academy of Sciences (NAOC). We appreciate all of the people in the FAST group for their support and assistance during the observations. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515. This work was partially supported by the Fermi Guest Observer Program, administered by NASA (Grant No. 80NSSC18K1731). Colin J. Clark acknowledges support from the ERC under the European Union’s Horizon 2020 Research and Innovation Programme (Grant No. 715051; Spiders). Fermi LAT work at NRL is supported by NASA.

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Wang, P., Li, D., Clark, C.J. et al. FAST discovery of an extremely radio-faint millisecond pulsar from the Fermi-LAT unassociated source 3FGL J0318.1+0252. Sci. China Phys. Mech. Astron. 64, 129562 (2021). https://doi.org/10.1007/s11433-021-1757-5

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