Broadband Spectral Properties of MAXI J1348–630 using AstroSat Observations

Mall, Gitika; Vadakkumthani, Jithesh; Misra, Ranjeev

doi:10.1088/1674-4527/aca505

Cited by 5 publications

(1 citation statement)

References 58 publications

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“…The analysis revealed several interesting characteristics of the source, including the flip-flop behaviour, different types of QPOs and energydependent behaviour of variability components (Jithesh et al 2021). The detailed broadband spectral study using the reflection models constrained the spin and inclination of the system and the values are > 0.97 and ∼ 33 • , respectively (Mall et al 2023). The studies mentioned above showcase the spectro-timing capabilities of AstroSat in broadband energy.…”

Section: Introductionmentioning

confidence: 70%

Spectral and temporal studies of Swift J1658.2–4242 using AstroSat observations with the JeTCAF model

Mondal

Jithesh

2023

Monthly Notices of the Royal Astronomical Society

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We present the X-ray spectral and temporal analysis of the black hole X-ray transient Swift J1658.2–4242 observed by AstroSat. Three epochs of data have been analysed using the JeTCAF model to estimate the mass accretion rates and to understand the geometry of the flow. The best-fit disc mass accretion rate ($\dot{m}_d$) varies between $0.90^{+0.02}_{-0.01}$ to $1.09^{+0.04}_{-0.03}$$\dot{M}_{\rm Edd}$ in these observations, while the halo mass accretion rate changes from $0.15^{+0.01}_{-0.01}$ to $0.25^{+0.02}_{-0.01}$$\dot{M}_{\rm Edd}$. We estimate the size of the dynamic corona, that varies substantially from $64.9^{+3.9}_{-3.1}$ to $34.5^{+2.0}_{-1.5}$rg and a moderately high jet/outflow collimation factor stipulates isotropic outflow. The inferred high disc mass accretion rate and bigger corona size indicate that the source might be in the intermediate to soft spectral state of black hole X-ray binaries. The mass of the black hole estimated from different model combinations is ∼14M⊙. In addition, we compute the quasi-periodic oscillation (QPO) frequencies from the model-fitted parameters, which match the observed QPOs. We further calculate the binary parameters of the system from the decay profile of the light curve and the spectral parameters. The estimated orbital period of the system is 4.0 ± 0.4 hr by assuming the companion as a mid or late K-type star. Our analysis using the JeTCAF model sheds light on the physical origin of the spectro-temporal behaviour of the source, and the observed properties are mainly due to the change in both the mass accretion rates and absorbing column density.

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Section: Introductionmentioning

confidence: 70%

Spectral and temporal studies of Swift J1658.2–4242 using AstroSat observations with the JeTCAF model

Mondal

Jithesh

2023

Monthly Notices of the Royal Astronomical Society

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A moderate spin for the black hole in X-ray binary MAXI J1348−630 revealed by Insight-HXMT

Wang

Sai

et al. 2023

Monthly Notices of the Royal Astronomical Society

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MAXI J1348-630 is a low-mass X-ray black hole binary located in the Galaxy and undergone the X-ray outburst in 2019. We analyzed the observation data in very soft state during the outburst between MJD 58588 and MJD 58596 based on the Insight-HXMT observations from 2 – 20 keV via the continuum fitting method to measure the spin of the stellar-mass black hole in MAXI J1348-630. The inner disk temperature and the apparent inner disk radius were found to be $0.47\pm 0.01 \rm keV$ and 5.33 ± 0.10 Rg from the observation data modeled by the multicolor disc blackbody model. Assuming the distance of the source $D\sim 3.4 \rm kpc$, the mass of the black hole M ∼ 11 M⊙, and the inclination of the system i ∼ 29.2○, the spin is determined to be a⋆ = 0.41 ± 0.03 for fixing hardening factor at 1.6 and $n_{H}=8.6\times 10^{21} \rm cm^{-2}$. Besides, considering the uncertainty of the parameters D, M, i of this system, with the Monte Carlo analysis, we still confirm the moderate spin of the black hole as $a_{\star }=0.42^{+0.13}_{-0.50}$. Some spectral parameters (e.g., column density and hardening factor) which could affect the measurements of the BH spin are also briefly discussed.

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A variable corona during the transition from type-C to type-B quasi-periodic oscillations in the black hole X-ray binary MAXI J1820+070

Méndez

García

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We analyze a Neutron Star Interior Composition Explorer (NICER) observation of the black hole X-ray binary MAXI J1820+070 during a transition from type-C to type-B quasi-periodic oscillations (QPOs). We find that below ∼2 keV, for the type-B QPOs the rms amplitude is lower and the magnitude of the phase lags is larger than for the type-C QPOs. Above that energy, the rms and phase-lag spectra of the type-B and type-C QPOs are consistent with being the same. We perform a joint fit of the time-averaged spectra of the source, and the rms and phase-lag spectra of the QPOs with the time-dependent Comptonization model vkompth to study the geometry of the corona during the transition. We find that the data can be well-fitted with a model consisting of a small and a large corona that are physically connected. The sizes of the small and large coronae increase gradually during the type-C QPO phase whereas they decrease abruptly at the transition to type-B QPO. At the same time, the inner radius of the disc moves inward at the QPO transition. Combined with simultaneous radio observations showing that discrete jet ejections happen around the time of the QPO transition, we propose that a corona that expands horizontally during the type-C QPO phase, from ∼104 km (∼800 Rg) to 105 km (∼8000 Rg) overlying the accretion disc, transforms into a vertical jet-like corona extending over ∼104 km (∼800 Rg) during the type-B QPO phase.

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Broadband Spectral Properties of MAXI J1348–630 using AstroSat Observations

Cited by 5 publications

References 58 publications

Spectral and temporal studies of Swift J1658.2–4242 using AstroSat observations with the JeTCAF model

Spectral and temporal studies of Swift J1658.2–4242 using AstroSat observations with the JeTCAF model

A moderate spin for the black hole in X-ray binary MAXI J1348−630 revealed by Insight-HXMT

A variable corona during the transition from type-C to type-B quasi-periodic oscillations in the black hole X-ray binary MAXI J1820+070

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