A NICER Discovery of a Low-Frequency Quasi-Periodic Oscillation in the Soft-Intermediate State of MAXI J1535-571

TL;DR

This paper reports the first detection of a low-frequency QPO in MAXI J1535-571's soft-intermediate state, revealing properties similar to Type A/B QPOs and suggesting a jet-like corona origin based on lag-energy analysis.

Contribution

First identification of a low-frequency QPO in MAXI J1535-571, with detailed timing and spectral analysis indicating a possible jet corona origin.

Findings

Detected a ~5.7 Hz QPO with Q≈2 and 1.9% rms.

QPO shows increasing soft lags at lower energies, up to 50 ms at 1 keV.

QPO characteristics resemble Type A/B QPOs in other black hole binaries.

Abstract

We present the discovery of a low-frequency $\approx 5.7$ Hz quasi-periodic oscillation (QPO) feature in observations of the black hole X-ray binary MAXI J1535-571 in its soft-intermediate state, obtained in September-October 2017 by the Neutron Star Interior Composition Explorer (NICER). The feature is relatively broad (compared to other low-frequency QPOs; quality factor $Q\approx 2$) and weak (1.9% rms in 3-10 keV), and is accompanied by a weak harmonic and low-amplitude broadband noise. These characteristics identify it as a weak Type A/B QPO, similar to ones previously identified in the soft-intermediate state of the transient black hole X-ray binary XTE J1550-564. The lag-energy spectrum of the QPO shows increasing soft lags towards lower energies, approaching 50 ms at 1 keV (with respect to a 3-10 keV continuum). This large phase shift has similar amplitude but opposite sign to that seen in Rossi X-ray Timing Explorer data for a Type B QPO from the transient black hole X-ray binary GX 339-4. Previous phase-resolved spectroscopy analysis of the Type B QPO in GX 339-4 pointed towards a precessing jet-like corona illuminating the accretion disk as the origin of the QPO signal. We suggest that this QPO in MAXI J1535-571 may have the same origin, with the different lag sign depending on the scale height of the emitting region and the observer inclination angle.