A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Modelling polarized X-ray pulses from accreting millisecond pulsars with X-PSI, using different hot spot locations and shapes
Tekijät: Salmi, Tuomo; Dorsman, Bas; Watts, Anna L.; Bobrikova, Anna; Di Marco, Alessandro; Loktev, Vladislav; Papitto, Alessandro; Pilia, Maura; Poutanen, Juri; Rankin, John
Kustantaja: OXFORD UNIV PRESS
Kustannuspaikka: OXFORD
Julkaisuvuosi: 2025
Journal: Monthly Notices of the Royal Astronomical Society
Tietokannassa oleva lehden nimi: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Lehden akronyymi: MON NOT R ASTRON SOC
Vuosikerta: 538
Numero: 4
Aloitussivu: 2562
Lopetussivu: 2568
Sivujen määrä: 7
ISSN: 0035-8711
eISSN: 1365-2966
DOI: https://doi.org/10.1093/mnras/staf441
Verkko-osoite: https://academic.oup.com/mnras/article/538/4/2562/8082125
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/491839382
We present an analysis of polarized X-ray pulses based on simulated data for accreting millisecond pulsars (AMPs). We used the open-source X-ray Pulse Simulation and Inference code (previously applied to NICER observations), which we upgraded to allow polarization analysis. We provide estimates of how well neutron star (NS) parameters can be constrained for the Imaging X-ray Polarimetry Explorer (IXPE) and find that strong limits on the hot region geometries can be hard to obtain if the emitting hot region is large and the number of polarized photons relatively small. However, if the star is bright enough and the hot regions are small and located so that polarization degree is higher, the observer inclination and hot spot colatitude can be constrained to a precision of within a few degrees. We also found that the shape of the hot region, whether a circle or a ring, cannot be distinguished in our most optimistic scenario. Nevertheless, future X-ray polarization missions are expected to improve the constraints, and already the recent AMP polarization detections by IXPE should help to infer the NS mass and radius when combined with modelling of X-ray pulse data sets that do not contain polarization information.
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TS, BD, and ALW acknowledge support from European Research Council (ERC) Consolidator Grant (CoG) No. 865768 AEONS (PI: Watts). ADM is supported by the Italian Space Agency (Agenzia Spaziale Italiana, ASI) through contract ASI-INAF-2022-19-HH.0. JP was supported by the Ministry of Science and Higher Education grant 075-15-2024-647. AP acknowledges support supported by INAF 2022 Research Grant FANS (PI: Papitto), Italian Ministry for Universities and Research PRIN 2020 Grant 2020BRP57Z, (PI: Astone), and Fondazione Cariplo/CDP, grant no. 2023–2560 (PI: Papitto). The use of the national computer facilities in this research was subsidized by NWO Domain Science. This work used the Dutch national e-infrastructure with the support of the SURF Cooperative using grant no. EINF-8005.
