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The nearest neutron star candidate in a binary revealed by optical time-domain surveys

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Abstract

The near-Earth (within ∼100 pc) supernova explosions in the past several million years can cause the global deposition of radioactive elements (e.g., 60Fe) on Earth. The remnants of such supernovae are too old to be easily identified. It is therefore of great interest to search for million-year-old near-Earth neutron stars or black holes, the products of supernovae. However, neutron stars and black holes are challenging to find even in our Solar neighbourhood if they are not radio pulsars or X-ray/γ-ray emitters. Here we report the discovery of one of the nearest (127.7 ± 0.3 pc) neutron star candidates in a detached single-lined spectroscopic binary LAMOST J235456.73+335625.9 (hereafter J2354). Utilizing the time-resolved ground-based spectroscopy and space photometry, we find that J2354 hosts an unseen compact object with Minv being 1.4–1.6 M⊙. The follow-up Swift ultraviolet (UV) and X-ray observations suggest that the UV and X-ray emission is produced by the visible star rather than the compact object. Hence, J2354 probably harbours a neutron star rather than a hot ultramassive white dwarf. Two-hour exceptionally sensitive radio follow-up observations with Five-hundred-meter Aperture Spherical radio Telescope fail to reveal any pulsating radio signals at the 6σ flux upper limit of 12.5 µJy. Therefore, the neutron star candidate in J2354 can only be revealed via our time-resolved observations. Interestingly, the distance between J2354 and our Earth can be as close as ∼ 50 pc around 2.5 million years (Myrs) ago, as revealed by the Gaia kinematics. Our discovery demonstrates a promising way to unveil the hidden near-Earth neutron stars in binaries by exploring the optical time domain, thereby facilitating understanding of the metal-enrichment history in our Solar neighbourhood.

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  1. These authors contributed equally to this work.

Authors and Affiliations

  1. Department of Astronomy, Xiamen University, Xiamen, 361005, China

    Ling-Lin Zheng, Mouyuan Sun, Wei-Min Gu, Tuan Yi, Zhi-Xiang Zhang, Junfeng Wang, Jianfeng Wu, Sen-Yu Qi & Jin-Bo Fu

  2. National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China

    Pei Wang, Song Wang, Chun-Qian Li, Jian-Rong Shi, Fan Yang, Zhongrui Bai, Yu Bai, Haotong Zhang & Jifeng Liu

  3. Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing, 102206, China

    Pei Wang

  4. Department of Physics, Institute of Theoretical Physics, Nanjing Normal University, Nanjing, 210023, China

    Shan-Shan Weng

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

    Jia Zhang

  6. College of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China

    Jian-Rong Shi & Jifeng Liu

  7. School of Astronomy and Space Science, Nanjing University, Nanjing, 210023, China

    Yong Shao & Xiang-Dong Li

  8. Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Nanjing, 210023, China

    Yong Shao & Xiang-Dong Li

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Corresponding authors

Correspondence to Wei-Min Gu, Zhi-Xiang Zhang or Jifeng Liu.

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Conflict of interest The authors declare that they have no conflict of interest.

Additional information

We thank Hong-Gang Yang, Yi-Han Song, Xuan Fang, Shuai Liu, and Yi-Ze Dong for beneficial discussions. Wei-Min Gu was supported by the National Key R&D Program of China (Grant No. 2021YFA1600401), and the National Natural Science Foundation of China (NSFC) (Grant Nos. 11925301, and 12033006). Mouyuan Sun was supported by the NSFC (Grant Nos. 11973002, and 12322303). Zhi-Xiang Zhang was supported by the NSFC (Grant No. 12103041). Jifeng Liu was supported by the NSFC (Grant Nos. 11988101, and 11933004). Pei Wang was supported by the NSFC (Grant No. U2031117). Junfeng Wang was supported by the NSFC (Grant No. 12033004). Jianfeng Wu was supported by the NSFC (Grant No. 12273029). Wei-Min Gu, Junfeng Wang, and Jianfeng Wu were supported by the NSFC (Grant No. 12221003). Jia Zhang was supported by the NSFC (Grant No. 11933008). Jian-Rong Shi was supported by the NSFC (Grant No. 12090044). Xiang-Dong Li was supported by the NSFC (Grant Nos. 12041301, and 12121003). This work used the LAMOST spectra. Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences. This work included public data collected by the TESS mission, the NASA Galaxy Evolution Explorer (GALEX), SDSS, the Pan-STARRS1 Surveys (PS1), the Two Micron All Sky Survey (2MASS), the Wide-field Infrared Survey Explorer (WISE), the Zwicky Transient Facility (ZTF) project, ASAS-SN, the European Space Agency (ESA) mission Gaia, TESS, and the APASS database. This work used data obtained through the Telescope Access Program (TAP), which had been funded by the TAP member institutes. This work made use of the data from FAST. FAST is a Chinese national mega-science facility, operated by National Astronomical Observatories, Chinese Academy of Sciences. This work used data from Swift Target of Opportunity observations.

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Zheng, LL., Sun, M., Gu, WM. et al. The nearest neutron star candidate in a binary revealed by optical time-domain surveys. Sci. China Phys. Mech. Astron. 66, 129512 (2023). https://doi.org/10.1007/s11433-023-2247-x

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  • DOI: https://doi.org/10.1007/s11433-023-2247-x