Abstract
Abstract We report on the coherent timing analysis of the 182 Hz accreting millisecond X-ray pulsar Swift J1756.9−2508 during its 2018 outburst as observed with the Neutron Star Interior Composition Explorer (NICER). Combining our NICER observations with Rossi X-ray Timing Explorer observations of the 2007 and 2009 outbursts, we also studied the long-term spin and orbital evolution of this source. We find that the binary system is well described by a constant orbital period model, with an upper limit on the orbital period derivative of ∣ P ˙ b ∣ < 7.4 × 10 − 13 s s−1. Additionally, we improve upon the source coordinates through astrometric analysis of the pulse arrival times, finding R.A. = 17h56m57.ˢ18 ± 0.ˢ08 and decl. = −25°06′27.″8 ± 3.″5, while simultaneously measuring the long-term spin frequency derivative as ν ˙ = − 7.3 × 10 − 16 Hz s−1. We briefly discuss the implications of these measurements in the context of the wider population of accreting millisecond pulsars.
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