Type-A quasi-periodic oscillation in the black hole transient MAXI J1348-630

TL;DR

This paper analyzes a 7-Hz type-A QPO in the black hole binary MAXI J1348-630, revealing energy-dependent rms and phase-lag spectra, and models the variability with a vertically extended Comptonised region.

Contribution

First detailed rms and phase-lag spectra for a type-A QPO in a black hole binary, modeled with a time-dependent Comptonisation framework.

Findings

RMS amplitude increases with energy from below 1% to 3%.

QPO variability is driven by the Comptonised region.

Phase lags are consistently soft at the QPO frequency.

Abstract

We present a detailed analysis of the spectral and timing characteristics of a 7-Hz type-A quasi-periodic oscillation (QPO) detected in NICER observations of the black hole X-ray binary MAXI J1348-630 during its high-soft state. The QPO is broad and weak, with an integrated fractional rms amplitude of 0.9 per cent in the 0.5-10 keV band. Thanks to the large effective area of NICER, combined with the high flux of the source and a relatively long accumulative exposure time, we construct the first rms and phase-lag spectra for a type-A QPO. Our analysis reveals that the fractional rms amplitude of the QPO increases with energy from below 1 per cent at 1 keV to 3 per cent at 6 keV. The shape of the QPO spectrum is similar to that of the Comptonised component, suggesting that the Comptonised region is driving the variability. The phase lags at the QPO frequency are always soft taking the lowest energy as reference. By jointly fitting the time-averaged spectrum of the source and the rms and phase-lag spectra of the QPO with the time-dependent Comptonisation model vkompthdk, we find that the radiative properties of the type-A QPO can be explained by a vertically extended Comptonised region with a size of 2300 km.