Time lags of the type-B QPO in MAXI J1348-630

TL;DR

This study analyzes the timing and spectral properties of type-B QPOs in MAXI J1348-630, revealing energy-dependent phase lags and rms behavior below 2 keV, providing new insights into the inner accretion flow and jet connection.

Contribution

First detailed analysis of phase lags and rms at energies below 2 keV for type-B QPOs in a black-hole binary, using NICER data.

Findings

Fractional rms decreases from >10% at 9 keV to 0.6% at 1.5 keV.

All energies show a hard lag relative to 2-3 keV.

Results support a Comptonization origin for the phase lags.

Abstract

The fast variability observed in the X-ray emission from black-hole binaries has a very complex phenomenology, but offers the possibility to investigate directly the properties of the inner accretion flow. In particular, type-B oscillations in the 2-8 Hz range, observed in the Soft-Intermediate state, have been associated to the emission from a relativistic jet. We present the results of the timing and spectral analysis of a set of observations of the bright transient MAXI J1348-630 made with the NICER telescope. The observations are in the brightest part of the outburst and all feature a strong type-B QPO at ~4.5 Hz. We compute the energy dependence of the fractional rms and the phase lags at the QPO frequency, obtaining high signal-to-noise data and sampling for the first time at energies below 2 keV. The fractional rms decreases from more than 10% at 9 keV to 0.6% at 1.5 keV, and is constant below that energy. Taking the 2-3 keV band as reference, photons at all energies show a hard lag, increasing with the distance from the reference band. The behaviour below 2 keV has never been observed before, due to the higher energy bandpass of previous timing instruments. The energy spectrum can be fitted with a standard model for this state, consisting of a thin disc component and a harder power law, plus an emission line between 6 and 7 keV. We discuss the results, concentrating on the phase lags, and show that they can be interpreted within a Comptonization model.