X-ray Time Lag Evaluation of MAXI J1820+070 with a Differential Cross-correlation Analysis

• Published in: The Astrophysical journal Vol. 945; no. 2; pp. 92 - 101
• Main Authors: Omama, Tomoki, Tsujimoto, Masahiro, Ebisawa, Ken, Mizumoto, Misaki
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.03.2023; IOP Publishing
• Subjects: Accretion; Accretion disks; Astrophysics; Astrostatistics; Astrostatistics tools; Black holes; Blackbody; Circular orbits; Configurations; Correlation analysis; Cross correlation; Emission; Fourier analysis; Low-mass x-ray binary stars; Orbital stability; Shot noise; Stellar accretion disks; Time lag; X ray telescopes; X-ray astronomy; X-rays
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/acba00

Abstract MAXI J1820+070 is a transient black hole binary discovered on 2018 March 11. The unprecedented rich statistics brought by the NICER X-ray telescope allow detailed timing analyses up to ∼1 kHz uncompromised by photon shot noise. To estimate the time lags, a Fourier analysis was applied, which led to two different conclusions for the system configuration: one supporting a lamp-post configuration with a stable accretion disk extending close to the innermost stable circular orbit and the other supporting a truncated accretion disk contracting with time. Using the same data set, we present the results based on the cross-correlation function (CCF). The CCF is calculated between two different X-ray bands where one side is subtracted from the other side, which we call the differential CCF (dCCF). Soft and hard lags of ∼0.03 and 3 s, respectively, are clearly identified without being diluted by the spectral mixture, demonstrating the effectiveness of the dCCF analysis. The evolution of these lags is tracked, along with spectral changes for the first 120 days since discovery. Both the dCCF and spectral fitting results are interpreted as the soft lag being a reverberation lag between the Comptonized emission and the soft excess emission, and that the hard lag is between the disk blackbody emission and the Comptonized emission. The evolutions of these lags are in line with the picture of a truncated disk contracting with time.