New and updated timing models for seven young energetic X-ray pulsars, including the Big Glitcher PSR J0537-6910

TL;DR

This paper provides updated and comprehensive timing models for seven young energetic X-ray pulsars, including glitch detections and spectral data, enhancing their utility for multi-energy and gravitational wave studies.

Contribution

The paper introduces new and extended timing models for seven pulsars, including the first glitch detections for some, covering multi-year NICER, NuSTAR, and Chandra observations.

Findings

23 glitches detected in PSR J0537-6910

First three glitches observed in PSR J0058-7218

Largest glitch measured in PSR J1849-0001

Abstract

We present new timing models and update our previous ones for the rotational evolution of seven young energetic pulsars, including four of the top five in spin-down luminosity Edot among all known pulsars. For each of the six pulsars that were monitored on a regular basis by NICER, their rotation phase-connected timing model covers the entire period of NICER observations, in many cases from 2017-2025. For PSR J0058-7218, which was only identified in 2021, we extend the baseline of its timing model by 3 years and report detections of its first three glitches. The timing model for PSR J0537-6910 over the entire 8 years of NICER monitoring is presented, including a total of 23 glitches; we also report its spin frequency and pulsed spectrum from a 2016 NuSTAR observation. For PSR B0540-69, its complete timing model from 2015-2025 is provided, including a braking index evolution from near 0 to 1.6 during this period. The 8-year timing model for PSR J1412+7922 (also known as Calvera) is reported, which includes a position that is consistent with that measured from imaging. For PSR J1811-1925, we present its 3.5-year timing model. For PSR J1813-1749, its incoherent timing model is extended through early 2025 using new Chandra observations. For PSR J1849-0001, its 7-year timing model is provided, including a position that is consistent with and more accurate than its imaging position and its first glitch that is one of the largest ever measured. Our timing models of these seven X-ray pulsars enable their study at other energies and in gravitational wave data.