MENGUJI KEBERADAAN INTERMEDIATE-MASS BLACK HOLE PADA ESO 243-49 HLX-1 MENGGUNAKAN MODEL STANDAR PIRINGAN AKRESI YANG DITERAPKAN PADA DATA SWIFT/XRT

• Main Author: Wulandari Sholikhah, Shinta
• Format: Final Project
• Language: Indonesia
• Online Access: https://digilib.itb.ac.id/gdl/view/47970
• Institution: Institut Teknologi Bandung

Hyperluminous X-ray Source (HLX) is a non-nuclear extragalactic X-ray source which appears to a point-like source in X-ray image and generates X-ray luminosity Lx 1041 erg/s. In order to explain the very high luminosity of a point-like source, the scenario of accretion process involving compact object is needed. If the observed luminosity of HLX does not exceed the Eddington luminosity, it is required the presence of a 1000 M compact object. Hence, HLX currently provides the strongest candidate for the existence of intermediate-mass black hole. One of the HLXs that has been well studied is ESO 243-49 HLX-1. This study describes the X-ray spectral variability of ESO 243-49 HLX-1. The data were taken from Swift observations in 2008 to 2020. Due to the short duration of Swift observations (around thousands of second), the spectra were merged. The analysis of X-ray spectrum using several simple models shows that all spectra are dominated by thermal component in which the disk luminosity appears to scale with the fourth power of the inner disk temperature. Continuum tting method which requires thermal spectrum, has been implemented to estimate the black hole mass in ESO 243-49 HLX-1. In this work, the mass of the black hole of (6; 383; 86)103 M to (3; 11 4; 03) 106 M can be derived. This value is lied in the range of mass for intermediate-mass black hole. Besides, the study of spectral evolution found several similar behaviours between ESO 243-49 HLX-1 and Galactic black hole binaries, particularly sub-Eddington sources. Thus, this result suggests the presence of intermediate-mass black hole in ESO 243-49 HLX-1.