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The MeerKAT Pulsar Timing Array: the 4.5-yr data release and the noise and stochastic signals of the millisecond pulsar populationстатья
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Дата последнего поиска статьи во внешних источниках: 8 октября 2025 г.
- Авторы: Miles Matthew T., Shannon Ryan M., Reardon Daniel J., Bailes Matthew, Champion David J., Geyer Marisa, Gitika Pratyasha, Grunthal Kathrin, Keith Michael J., Kramer Michael, Kulkarni Atharva D., Nathan Rowina S., Parthasarathy Aditya, Porayko Nataliya K., Singha Jaikhomba, Theureau Gilles, Abbate Federico, Buchner Sarah, Cameron Andrew D., Camilo Fernando, Moreschi Beatrice E., Shaifullah Golam, Shamohammadi Mohsen, Krishnan Vivek Venkatraman
- Журнал: Monthly Notices of the Royal Astronomical Society
- Том: 536
- Номер: 2
- Год издания: 2025
- Издательство: Oxford Journals, Oxford University Press
- Местоположение издательства: Oxford, UK, England
- Первая страница: 1467
- Последняя страница: 1488
- DOI: 10.1093/mnras/stae2572
- Аннотация: Pulsar timing arrays (PTAs) are ensembles of regularly observed millisecond pulsars timed to high precision. Each pulsar in an array could be affected by a suite of noise processes, most of which are astrophysically motivated. Analysing them carefully can be used to understand these physical processes. However, the primary purpose of these experiments is to detect signals that are common to all pulsars, in particular signals associated with a stochastic gravitational wave background. To detect this, it is paramount to appropriately characterize other signals that may otherwise impact array sensitivity or cause a spurious detection. Here, we describe the second data release and first detailed noise analysis of the pulsars in the MeerKAT Pulsar Timing Array, comprising high-cadence and high-precision observations of 83 millisecond pulsars over 4.5 yr. We use this analysis to search for a common signal in the data, finding a process with an amplitude of log10ACURN=−14.25+0.21−0.36 and spectral index γCURN=3.60+1.31−0.89 . Fixing the spectral index at the value predicted for a background produced by the inspiral of binary supermassive black holes, we measure the amplitude to be log10ACURN=−14.28+0.21−0.21 at a significance expressed as a Bayes factor of ln(B)=4.46 . Under both assumptions, the amplitude that we recover is larger than those reported by other PTA experiments. We use the results of this analysis to forecast our sensitivity to a gravitational wave background possessing the spectral properties of the common signal we have measured.
- Добавил в систему: Порайко Наталия Константиновна