Single-pulse reanalysis of the 2024 Vela glitch and new observations of PSR~J0437−4715 and PSR~J1644−4559
Abstract
The Pulsar Monitoring in Argentina (PuMA) collaboration systematically monitors southern glitching pulsars, maintaining high-cadence single-pulse records of the Vela pulsar. We present a pulse-per-pulse reanalysis of the 2024 major glitch of Vela (PSR~J0835−4510) with the 400~MHz-bandwidth ROACH backend of the Argentine Institute of Radioastronomy, and extend our machine-learning single-pulse pipeline---Isolation Forest outlier rejection, β-Variational-AutoEncoder denoising, and Self-Organizing-Map clustering---to new observations of PSR~J1644−4559 and the millisecond pulsar PSR~J0437−4715. For Vela, the 4- and 6-cluster decompositions of the eight days bracketing the glitch reproduce, with seven times the previous bandwidth, the behavior found with the narrow-band ETTUS receivers: higher-amplitude clusters peak earlier in phase, are narrower, more skewed, and less populated. With the glitch jump and its two exponential recovery terms included in the timing solution, the mean profile is stable to 1\% across all eight days (width change −0.5±0.9\% from pre- to post-glitch); omitting the recovery terms would mimic a post-glitch broadening of up to 55\% through a folding-frequency error at the 10−7 level. The clusters of PSR~J1644−4559 differ almost exclusively in amplitude, as expected for a scattering-dominated profile. For PSR~J0437−4715, retaining the 10\% of pulses with the highest peak-dominance score doubles the signal-to-noise ratio, and a five-cluster decomposition yields narrow, phase-ordered groups a factor 3.6±0.4 narrower than the average profile, suggesting a ∼3.5-fold improvement in cluster-based timing precision for this pulsar-timing-array target, to be confirmed in a follow-up paper.
Related
- A multi-wavelength view of PSR J0437-4715 with NICER and other missions: Radius measurements from far-ultraviolet to hard X-ray pulse profile modeling
- A study of periodic single-pulse emission behavior in PSR J1819+1305 using L-band observations from the FAST
- Science Using Single-Pulse Exploration with Combined Telescopes: II. Pulse profile evolution and single-pulse modulation
- Is DESI Seeing Dynamical Dark Energy, or a Cosmic Glitch in Gravity?
- Discovery of Two Consecutive Profile Change Events in the Millisecond Pulsar PSR J0437-4715
BibTeX
@misc{lousto2026singlepulse,
title = {{Single-pulse reanalysis of the 2024 Vela glitch and new observations of PSR~J0437$-$4715 and PSR~J1644$-$4559}},
author = {Carlos O. Lousto and Ruby Shrestha and Ezequiel Zubieta and Susana B. Araujo Furlan and Guillermo Gancio and Federico García and Santiago del Palacio and Ryan Missel and Linwei Wang},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.03056},
eprint = {2609.03056},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.03056},
}
RIS
TY - UNPB
TI - Single-pulse reanalysis of the 2024 Vela glitch and new observations of PSR~J0437−4715 and PSR~J1644−4559
AU - Carlos O. Lousto
AU - Ruby Shrestha
AU - Ezequiel Zubieta
AU - Susana B. Araujo Furlan
AU - Guillermo Gancio
AU - Federico García
AU - Santiago del Palacio
AU - Ryan Missel
AU - Linwei Wang
PY - 2026
DA - 2026/09/02
PB - arXiv
DO - 10.48550/arxiv.2609.03056
UR - https://arxiv.org/abs/2609.03056
AB - The Pulsar Monitoring in Argentina (PuMA) collaboration systematically monitors southern glitching pulsars, maintaining high-cadence single-pulse records of the Vela pulsar. We present a pulse-per-pulse reanalysis of the 2024 major glitch of Vela (PSR~J0835−4510) with the 400~MHz-bandwidth ROACH backend of the Argentine Institute of Radioastronomy, and extend our machine-learning single-pulse pipeline---Isolation Forest outlier rejection, β-Variational-AutoEncoder denoising, and Self-Organizing-Map clustering---to new observations of PSR~J1644−4559 and the millisecond pulsar PSR~J0437−4715. For Vela, the 4- and 6-cluster decompositions of the eight days bracketing the glitch reproduce, with seven times the previous bandwidth, the behavior found with the narrow-band ETTUS receivers: higher-amplitude clusters peak earlier in phase, are narrower, more skewed, and less populated. With the glitch jump and its two exponential recovery terms included in the timing solution, the mean profile is stable to 1\% across all eight days (width change −0.5±0.9\% from pre- to post-glitch); omitting the recovery terms would mimic a post-glitch broadening of up to 55\% through a folding-frequency error at the 10^−7 level. The clusters of PSR~J1644−4559 differ almost exclusively in amplitude, as expected for a scattering-dominated profile. For PSR~J0437−4715, retaining the 10\% of pulses with the highest peak-dominance score doubles the signal-to-noise ratio, and a five-cluster decomposition yields narrow, phase-ordered groups a factor 3.6±0.4 narrower than the average profile, suggesting a ∼3.5-fold improvement in cluster-based timing precision for this pulsar-timing-array target, to be confirmed in a follow-up paper.
ER -