Population III X-ray binaries and their impact on the early universe

• Verfasst von: Sanches Sartorio, Nina [VerfasserIn]
• Verfasst von: Fialkov, A [VerfasserIn]
• Verfasst von: Hartwig, T [VerfasserIn]
• Verfasst von: Mirouh, G M [VerfasserIn]
• Verfasst von: Izzard, R G [VerfasserIn]
• Verfasst von: Magg, Mattis [VerfasserIn]
• Verfasst von: Klessen, Ralf S. [VerfasserIn]
• Verfasst von: Glover, Simon [VerfasserIn]
• Verfasst von: Chen, Li-Hsin [VerfasserIn]
• Verfasst von: Tarumi, Y [VerfasserIn]
• Verfasst von: Hendriks, D D [VerfasserIn]
• Titel: Population III X-ray binaries and their impact on the early universe
• Verf.angabe: Nina S. Sartorio, A. Fialkov, T. Hartwig, G.M. Mirouh, R.G. Izzard, M. Magg, R.S. Klessen, S.C.O. Glover, L. Chen, Y. Tarumi and D.D. Hendriks
• E-Jahr: 2023
• Jahr: 10 March 2023
• Umfang: 17 S.
• Fussnoten: Gesehen am 05.07.2023
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2023
• Band/Heft Quelle: 521(2023), 3 vom: März, Seite 4039-4055
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stad697
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1851801456

Abstract

The first population of X-ray binaries (XRBs) is expected to affect the thermal and ionization states of the gas in the early Universe. Although these X-ray sources are predicted to have important implications for high-redshift observable signals, such as the hydrogen 21-cm signal from cosmic dawn and the cosmic X-ray background, their properties are poorly explored, leaving theoretical models largely uninformed. In this paper we model a population of X-ray binaries arising from zero metallicity stars. We explore how their properties depend on the adopted initial mass function (IMF) of primordial stars, finding a strong effect on their number and X-ray production efficiency. We also present scaling relations between XRBs and their X-ray emission with the local star formation rate, which can be used in sub-grid models in numerical simulations to improve the X-ray feedback prescriptions. Specifically, we find that the uniformity and strength of the X-ray feedback in the intergalactic medium is strongly dependant on the IMF. Bottom-heavy IMFs result in a smoother distribution of XRBs, but have a luminosity orders of magnitude lower than more top-heavy IMFs. Top-heavy IMFs lead to more spatially uneven, albeit strong, X-ray emission. An intermediate IMF has a strong X-ray feedback while sustaining an even emission across the intergalactic medium. These differences in X-ray feedback could be probed in the future with measurements of the cosmic dawn 21-cm line of neutral hydrogen, which offers us a new way of constraining population III IMF.