Phase-resolved spectroscopy of a quasi-periodic oscillation in the black hole X-ray binary GRS 1915+105 with NICER and NuSTAR. Issue 1 (4th January 2022)

• Record Type: Journal Article
• Authors: Nathan, Edward; Ingram, Adam; Homan, Jeroen; Huppenkothen, Daniela; Uttley, Phil; van der Klis, Michiel; Motta, Sara; Altamirano, Diego; Middleton, Matthew
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 511:Issue 1(2022)
• Page Start: 255
• Page End: 279
• Publication Date: 2022-01-04
• Subjects: accretion, accretion discs -- black hole physics -- methods: data analysis -- X-rays: binaries -- X-rays: individual: GRS 1915+105; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab3803
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Quasi-periodic oscillations (QPOs) are often present in the X-ray flux from accreting stellar-mass black holes (BHs). If they are due to relativistic (Lense–Thirring) precession of an inner accretion flow which is misaligned with the disc, the iron emission line caused by irradiation of the disc by the inner flow will rock systematically between red and blue shifted during each QPO cycle. Here, we conduct phase-resolved spectroscopy of an ∼2.2 Hz type-C QPO from the BH X-ray binary GRS 1915+105, observed simultaneously with NICER and NuSTAR . We apply a tomographic model in order to constrain the QPO phase-dependent illumination profile of the disc. We detect the predicted QPO phase-dependent shifts of the iron line centroid energy, with our best fit featuring an asymmetric illumination profile (>2σ confidence). The observed line energy shifts can alternatively be explained by the spiral density waves of the accretion-ejection instability model. However, we additionally measure a significant (>3σ) modulation in reflection fraction, strongly favouring a geometric QPO origin. We infer that the disc is misaligned with previously observed jet ejections, which is consistent with the model of a truncated disc with an inner precessing hot flow. However, our inferred disc inner radius is small ( r in ∼ 1.4 GM / c 2 ). For this disc inner radius, Lense–Thirring precession cannot reproduce the observed QPO frequency. In fact, this disc inner radius is incompatible with the predictions of all well-studied QPO models in the literature.