Anti-glitches in the Ultraluminous Accreting Pulsar NGC 300 ULX-1 Observed with NICER

Research output: Contribution to journalJournal article – Annual report year: 2019Researchpeer-review

DOI

  • Author: Ray, Paul S.

    U.S. Naval Research Laboratory , United States

  • Author: Guillot, Sebastien

    Universite de Toulouse, France

  • Author: Ho, Wynn C. G.

    University of Southampton, United Kingdom

  • Author: Kerr, Matthew

    U.S. Naval Research Laboratory , United States

  • Author: Enoto, Teruaki

    Kyoto University, Japan

  • Author: Gendreau, Keith C.

    NASA Goddard Space Flight Center, United States

  • Author: Arzoumanian, Zaven

    NASA Goddard Space Flight Center, United States

  • Author: Altamirano, Diego

    University of Southampton, United Kingdom

  • Author: Bogdanov, Slavko

    Columbia University, United States

  • Author: Campion, Robert

    Chesapeake Aerospace , United States

  • Author: Chakrabarty, Deepto

    Massachusetts Institute of Technology, United States

  • Author: Deneva, Julia S.

    George Mason University, United States

  • Author: Jaisawal, Gaurava K.

    Astrophysics and Atmospheric Physics, National Space Institute, Technical University of Denmark, Elektrovej, 2800, Kgs. Lyngby, Denmark

  • Author: Kozon, Robert P.

    NASA Goddard Space Flight Center, United States

  • Author: Malacaria, Christian

    NASA Marshall Space Flight Center, United States

  • Author: Strohmayer, Tod E.

    NASA Goddard Space Flight Center, United States

  • Author: Wolff, Michael T.

    U.S. Naval Research Laboratory , United States

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We present evidence for three spin-down glitches (or “anti-glitches”) in the ultraluminous accreting X-ray pulsar NGC 300 ULX-1, in timing observations made with the Neutron Star Interior Composition Explorer. Our timing analysis reveals three sudden spin-down events of magnitudes Δν = −23, −30, and −43 μHz (fractional amplitudes Δν/ν = −4.4, −5.5, and −7.7 × 10−4). We determined fully phase-coherent timing solutions through the first two glitches, giving us high confidence in their detection, while the third candidate glitch is somewhat less secure. These are larger in magnitude (and opposite in sign) than any known radio pulsar glitch. This may be caused by the prolonged rapid spin up of the pulsar, causing a sudden transfer of angular momentum between the superfluid and non-superfluid components of the star. We find no evidence for profile or spectral changes at the epochs of the glitches, supporting the conclusion that these are due to the same process as in normal pulsar glitches, but in reverse.
Original languageEnglish
Article number130
JournalAstrophysical Journal
Volume879
Issue number2
Number of pages11
ISSN0004-637X
DOIs
Publication statusPublished - 2019
CitationsWeb of Science® Times Cited: No match on DOI

ID: 186183241