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Spectro-polarimetric study to constrain accretion-ejection properties of MCG-5-23-16 using IXPE and NuSTAR observations

Published online by Cambridge University Press:  22 October 2024

Santanu Mondal Open the ORCID record for Santanu Mondal [Opens in a new window] ,
Rwitika Chatterjee ,
Vivek K. Agrawal  and
Anuj Nandi
Santanu Mondal*
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bengaluru, India
Rwitika Chatterjee
Affiliation:
Space Astronomy Group, ISITE Campus, U. R. Rao Satellite Center, ISRO, Bengaluru, India
Vivek K. Agrawal
Affiliation:
Space Astronomy Group, ISITE Campus, U. R. Rao Satellite Center, ISRO, Bengaluru, India
Anuj Nandi
Affiliation:
Space Astronomy Group, ISITE Campus, U. R. Rao Satellite Center, ISRO, Bengaluru, India
*
Corresponding authors: S. Mondal, Emails: [email protected], [email protected].
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Abstract

We conducted a study on the X-ray polarisation properties of MCG-5-23-16 by analysing long-term monitoring data from NuSTAR jointly with IXPE observations made in May and November 2022. The re-analysis of IXPE data gives model-dependent polarisation degree, PD (%) = $1.08\pm0.66$ in the energy band 2–8 keV, which agrees with previous studies within error bars. The model-independent analysis of PD poses an upper limit of $\leq3.8$ ($1\sigma$ level) for the same energy band. The observed upper limit of PD, along with broadband spectral analysis (2–79 keV) using an accretion-ejection based model, allowed us to derive the corona geometry (i.e. radius and height) and the accretion disc inclination ($\sim33^\circ$). Additional NuSTAR observations were also analysed to gain insights into the accretion flow properties of the source and to estimate the expected polarisation during those epochs with PD $\sim 4.3\%$. The radius and height of the corona varies between $28.2\pm3.1 - 39.8\pm4.6$ r$_s$ and $14.3\pm1.7-21.4\pm1.9$ r$_s$ respectively, with a mass outflow rate from the corona measuring $0.14\pm0.03-0.2\pm0.03$ Eddington rate ($\dot m_{\mathrm{Edd}}$). The estimated PD values were nearly constant up to a certain radial distance and height of the corona and then decreased for increasing corona geometry. The spectral analysis further provided an estimate for the mass of the central black hole $\sim2\times 10^7$ M$_\odot$ and the velocity of the outflowing gas $\sim0.16-0.19c$. A comparative broadband spectral study using reflection-based models estimates the disc inclination between $\sim 31^\circ\pm8^\circ-45^\circ\pm7^\circ$, and yields an expected PD of 3.4–6.0%. We also found a weak reflection fraction and a less ionised distant reflecting medium. The expected PD measured using accretion-ejection and reflection models is less compared to the expected PD measured for a given disc inclination of $45^\circ$. Our modelling of the disc-corona-outflows and polarisation connection can be extended and validated with data from the recently launched XPoSat, India’s first X-ray Polarimeter Satellite, offering potential applications to other sources.

Keywords

Accretion discgalaxies:activegalaxies: SeyfertpolarisationX-rays: individual: MCG-5-23-16
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 41 , 2024 , e072
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Copyright
© Indian Institute of Astrophysics, 2024. Published by Cambridge University Press on behalf of Astronomical Society of Australia

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