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PINT: Maximum-likelihood estimation of pulsar timing noise parameters

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arxiv 2405.01977 v2 pith:MRLLHOIU submitted 2024-05-03 astro-ph.IM astro-ph.HE

Abhimanyu Susobhanan , David Kaplan , Anne Archibald , Jing Luo , Paul Ray , Timothy Pennucci , Scott Ransom , Gabriella Agazie
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William Fiore Bjorn Larsen Patrick O'Neill Rutger van Haasteren Akash Anumarlapudi Matteo Bachetti Deven Bhakta Chloe Champagne H. Thankful Cromartie Paul Demorest Ross Jennings Matthew Kerr Sasha Levina Alexander McEwen Brent Shapiro-Albert Joseph Swiggum
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PINT is a pure-Python framework for high-precision pulsar timing developed on top of widely used and well-tested Python libraries, supporting both interactive and programmatic data analysis workflows. We present a new frequentist framework within PINT to characterize the single-pulsar noise processes present in pulsar timing datasets. This framework enables the parameter estimation for both uncorrelated and correlated noise processes as well as the model comparison between different timing and noise models in a computationally inexpensive way. We demonstrate the efficacy of the new framework by applying it to simulated datasets as well as a real dataset of PSR B1855+09. We also describe the new features implemented in PINT since it was first described in the literature.

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Forward citations

Cited by 5 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. PSRDISP: A novel approach to modeling dispersive processes in single-pulsar noise analysis using epoch-wise dispersion measures

    astro-ph.IM 2026-07 unverdicted novelty 6.0 of 10

    PSRDISP is a Gaussian-process framework that fits dispersion-measure and solar-wind noise directly to epoch-wise dispersion measures, recovering injected signals in simulated pulsar data.

  2. Regularizing the Pulsar Timing Array likelihood: A path towards Fourier Space

    astro-ph.IM 2024-12 conditional novelty 6.0 of 10

    A ridge-regularized Gaussian form of the PTA likelihood lets pulsars be analyzed individually first and then combined globally for a gravitational-wave background search, reproducing standard ENTERPRISE results on EPT...

  3. A Lower Mass Estimate for PSR J0348+0432 Based on CHIME/Pulsar Precision Timing

    astro-ph.HE 2024-12 conditional novelty 6.0 of 10

    Extended pulsar timing lowers the mass of J0348+0432 to 1.806(37) solar masses, about 10% below the widely cited 2.01 value.

  4. \texttt{GWBird}: a toolkit for the characterization of the Stochastic Gravitational Wave Background for Ground, Space, and Pulsar Timing Array detectors

    astro-ph.IM 2025-07 conditional novelty 5.0 of 10

    A new, unified Python package computes overlap reduction functions, power-law integrated sensitivity curves, and angular sensitivity curves for ground, space, and pulsar timing array detectors across all gravitational...

  5. Pulse Profile Variability of PSR J1022+1001 in NANOGrav Data

    astro-ph.HE 2024-12 conditional novelty 5.0 of 10

    PSR J1022+1001's pulse profile variability survives rigorous MEM and METM polarization calibration and is consistent across frequency, favoring an intrinsic pulsar origin.

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