Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM

Mochizuki, Yuto; Tsujimoto, Masahiro; Kelley, Richard L.; Vander Meulen, Bert; Enoto, Teruaki; Nagai, Yutaro; Done, Chris; Pradhan, Pragati; Hell, Natalie; Pottschmidt, Katja; Ebisawa, Ken; Behar, Ehud

doi:10.3847/2041-8213/ad946d

Title: Detection of the Orbital Modulation of Fe Kα Fluorescence Emission in Centaurus X-3 Using the High-resolution Spectrometer Resolve on board XRISM

Journal Article · 04 December 2024 · The Astrophysical Journal. Letters

DOI: https://doi.org/10.3847/2041-8213/ad946d · OSTI ID:2479946

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Abstract The Fe K α fluorescence line emission in X-ray spectra is a powerful diagnostic tool for various astrophysical objects to reveal the distribution of cold matter around photoionizing sources. The advent of the X-ray microcalorimeter on board the XRISM satellite will bring new constraints on the emission line. We present one of the first such results for the high-mass X-ray binary Centaurus X-3, which is composed of an O-type star and a neutron star (NS). We conducted a 155 ks observation covering an entire binary orbit. A weak Fe K α line was detected in all orbital phases at an equivalent width (EW) of 10–20 eV. We found for the first time that its radial velocity (RV) is sinusoidally modulated by the orbital phase. The RV amplitude is 248 ± 13 km s ⁻¹ , which is significantly smaller than the value (391 km s ⁻¹ ) expected if the emission is from the NS surface, but is consistent if the emission takes place at the O star surface. We discuss several possibilities of the line production site, including the NS surface, O star surface, O star wind, and accretion stream from the O star to the NS. We ran radiative transfer calculation for some of them assuming spherically symmetric density and velocity profiles and an isotropic distribution of X-ray emission from the NS. None of them explains the observed EW and velocity dispersion dependence on the orbital phase, suggesting that more elaborated modeling is needed. In other words, the present observational results have the capability to constrain deviations from these assumptions.

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Sponsoring Organization:: USDOE

Grant/Contract Number:: NONE; AC52-07NA27344

OSTI ID:: 2479946

Journal Information:: The Astrophysical Journal. Letters, Journal Name: The Astrophysical Journal. Letters Journal Issue: 1 Vol. 977; ISSN 2041-8205

Publisher:: American Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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