Structure of an Absorbing Medium in the Nucleus of the Galaxy Mrk 417 Based on NuSTAR and Swift/Bat Data

Kompaniiets, O.V.; Vasylenko, A. A.

doi:10.1007/s10511-020-09636-1

Cited by 2 publications

(2 citation statements)

References 27 publications

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“…Multiwavelength properties of several galaxies from this sample of low redshift galaxies were already provided, including properties in the X-ray spectral range [22,26,50,52]. It was noted that all these objects are very faint in X-ray in comparison with the AGNs in a more dense environment [1,9,11,23,25,35,49]. A part of these galaxies has a reflection component in X-ray spectra with different reflection fractions in addition to the primary power-law continuum [38,45].…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength Properties of the Low-Redshift Isolated Galaxies With Active Nuclei Modelled With Cigale

KOMPANIIETS

2023

Kosm. nauka tehnol.

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Using the CIGALE software, we present the preliminary results of a multiwavelength analysis of eighteen low-redshift isolated galaxies with active nuclei (isolated AGNs). This sample was formed by cross-matching the 2MIG isolated AGNs sample with the SDSS DR9 catalog. The host galaxies of this sample have not undergone a merger for at least three billion years, making them a unique laboratory for studying interactions between various astrophysical processes without the complicating factors of merging with other galaxies or the effects of a denser environment. In addition, the study of isolated AGNs can provide valuable information about the evolution and activity of galaxies in the broader context of the distribution of large-scale structures of the Universe. First, we seek to understand how the environment affects the physical processes involved in the accretion of matter onto supermassive black holes in these galaxies. Secondly, to what extent do processes of star formation or degeneration of nuclei activity continue the evolution of these galaxies? Third, how does the localization of isolated AGNs in voids or filaments of a large-scale structure determine the properties of this envi- ronment at the low redshifts? Using observable fluxes from UV to the radio ranges from archival databases of space-born and ground-based observatories (GALEX, SDSS, 2MASS, Spitzer, Hershel, IRAS, WISE, VLA), we estimated the contribution from the emission of an active nucleus to the galaxy’s total emission, the stellar mass, and the star formation rate. The mass of the stellar component falls from 1010 MSun and 1011 MSun. The star formation rate for most galaxies (except UGC 10120) does not exceed 3 MSun per year. The best SED fittings (with χ2 values less than 5) are obtained for the galaxies CGCG248-019 (χ2 = 1.6), CGCG179-005 (χ2 = 1.6), CGCG243-024 (χ2 = 2.6), IC0009 (χ2 = 2.8), MCG+09-25-022 (χ2 = 3.1), UGC10244 (χ2 = 4.1)

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Section: Introductionmentioning

confidence: 99%

Multiwavelength Properties of the Low-Redshift Isolated Galaxies With Active Nuclei Modelled With Cigale

KOMPANIIETS

2023

Kosm. nauka tehnol.

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“…Except for SMBH, the AGN also contains major components such as the accretion disk around the BH and molecular torus (e.g. Ricci et al 2014;Vasylenko 2018;Gröbner et al 2020;Kompaniiets & Vasylenko 2020). Accretion onto SMBH is accompanied by converting the gravitational potential energy to the observed radiation, spanning the entire electromagnetic spectrum.…”

Section: Introductionmentioning

confidence: 99%

NGC 6240 supermassive black hole binary dynamical evolution based on Chandra data

Sobolenko

Kompaniiets

Berczik

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The main idea of our research is to estimate the physical coalescence time of the double supermassive black hole (SMBH) system in the centre of NGC 6240 based on the X-ray observations from the Chandra space observatory. The spectra of the Northern and Southern nuclei were fitted by spectral models from Sherpa and both presented the narrow component of the Fe Kα emission line. It enabled us to apply the spectral model to these lines and to find relative offset ≈0.02 keV. The enclosed dynamical mass of the central region of NGC 6240 with radius 1 kpc was estimated $\approx 2.04\times 10^{11} \rm \,\, M_{\odot }$. These data allowed us to carry on the high resolution direct N-body simulations with Newtonian and post-Newtonian (up to $2.5\mathcal {PN}$ correction) dynamics for this particular double SMBH system. As a result, from our numerical models we approximated the central SMBH binary merging time for the different binary eccentricities. In our numerical parameters range the upper limit for the merging time, even for the very small eccentricities, is still below ≈70 Myr. Gravitational waveforms and amplitude-frequency pictures from such events can be detected using Pulsar Timing Array (PTA) projects at the last merging phase.

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Structure of an Absorbing Medium in the Nucleus of the Galaxy Mrk 417 Based on NuSTAR and Swift/Bat Data

Cited by 2 publications

References 27 publications

Multiwavelength Properties of the Low-Redshift Isolated Galaxies With Active Nuclei Modelled With Cigale

Multiwavelength Properties of the Low-Redshift Isolated Galaxies With Active Nuclei Modelled With Cigale

NGC 6240 supermassive black hole binary dynamical evolution based on Chandra data

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