APOLLO-Timing: Annealed Phase - Orbit Lattice Linking across Observations for Binary Pulsar Timing
Abstract
Sparse observations of binary pulsars can leave the orbit and the pulse count across observing gaps uncertain. We present APOLLO-Timing, a Bayesian phase-orbit lattice method that fits timing parameters together with integer pulse offsets between observing sessions. PINT checks the candidate connections at fixed pulse numbers. For PSR J1912-1215, a preliminary Keplerian fit to variations in the apparent spin period and its derivative did not phase-connect 96 times of arrival (TOAs) spanning 1438.07 days in 23 sessions. Starting from its position, spin frequency F0, and first time derivative F1 estimated in that fit, with dispersion measure fixed, APOLLO-Timing recovers the orbit and a unique best-supported phase-connected solution without supplied orbital parameters. A repeat full-data blind search recovers the same pulse counts in 914.0 s, including the final fit. Setting the initial F1 to zero in the 17, 18, and 19 session subsets also recovers the reference path. The solution gives Pb = 17.526 days, x = 23.448 light-seconds, e = 2.65e-5, chi-square = 188.01, and a weighted rms residual of 5.08 microseconds. For a pulsar mass of 1.4 solar masses and inclination of 60 degrees, the inferred companion mass is 0.67 solar masses, favoring a CO/ONeMg white dwarf.
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BibTeX
@misc{wen2026apollotiming,
title = {{APOLLO-Timing: Annealed Phase - Orbit Lattice Linking across Observations for Binary Pulsar Timing}},
author = {Y. R. Wen and D. Zhao and N. Wang and J. P. Yuan and W. M. Yan and J. B. Wang and J. T. Bai and Z. H. Chen},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.06640},
eprint = {2611.06640},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.06640},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - APOLLO-Timing: Annealed Phase - Orbit Lattice Linking across Observations for Binary Pulsar Timing
AU - Y. R. Wen
AU - D. Zhao
AU - N. Wang
AU - J. P. Yuan
AU - W. M. Yan
AU - J. B. Wang
AU - J. T. Bai
AU - Z. H. Chen
PY - 2026
DA - 2026/11/04
PB - arXiv
DO - 10.48550/arxiv.2611.06640
UR - https://arxiv.org/abs/2611.06640
AB - Sparse observations of binary pulsars can leave the orbit and the pulse count across observing gaps uncertain. We present APOLLO-Timing, a Bayesian phase-orbit lattice method that fits timing parameters together with integer pulse offsets between observing sessions. PINT checks the candidate connections at fixed pulse numbers. For PSR J1912-1215, a preliminary Keplerian fit to variations in the apparent spin period and its derivative did not phase-connect 96 times of arrival (TOAs) spanning 1438.07 days in 23 sessions. Starting from its position, spin frequency F0, and first time derivative F1 estimated in that fit, with dispersion measure fixed, APOLLO-Timing recovers the orbit and a unique best-supported phase-connected solution without supplied orbital parameters. A repeat full-data blind search recovers the same pulse counts in 914.0 s, including the final fit. Setting the initial F1 to zero in the 17, 18, and 19 session subsets also recovers the reference path. The solution gives Pb = 17.526 days, x = 23.448 light-seconds, e = 2.65e-5, chi-square = 188.01, and a weighted rms residual of 5.08 microseconds. For a pulsar mass of 1.4 solar masses and inclination of 60 degrees, the inferred companion mass is 0.67 solar masses, favoring a CO/ONeMg white dwarf.
ER -