The mass of the central body of the galaxy Ark 120 and the orbits of objects in its gravitational field

Denissyuk, E. K.; Валиуллин, Р. Р.; Gaisina, V. N.

doi:10.1134/s106377291412004x

Cited by 8 publications

(5 citation statements)

References 8 publications

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“…Other direct methods to determine the mass exist and have been applied to Ark 120. Recently, Denissyuk et al (2015) used the radial velocities of emission features to infer a BH mass for Ark 120 of 1.675 ± 0.028 × 10 8 M , similar to that found by Peterson et al (2004) and Ho & Kim (2015). Another method is based on polarisation of the broad emission lines (e.g.…”

Section: Black Hole Mass Valuementioning

confidence: 76%

A deep X-ray view of the bare AGN Ark 120

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Reeves

et al. 2019

A&A

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Context. The spin of supermassive black holes (SMBH) in active galactic nuclei (AGN) can be determined from spectral signature(s) of relativistic reflection such as the X-ray iron Kα line profile, but this can be rather uncertain when the line of sight intersects the so-called warm absorber and/or other wind components as these distort the continuum shape. Therefore, AGN showing no (or very weak) intrinsic absorption along the line-of-sight such as Ark 120, a so-called bare AGN, are the ideal targets for SMBH spin measurements. However, in our previous work on Ark 120, we found that its 2014 X-ray spectrum is dominated by Comptonisation, while the relativistic reflection emission only originates at tens of gravitational radii from the SMBH. As a result, we could not constrain the SMBH spin from disc reflection alone. Aims. Our aim is to determine the SMBH spin in Ark 120 from an alternative technique based on the global energetics of the disc-corona system. Indeed, the mass accretion rate (Ṁ) through the outer disc can be measured from the optical-UV emission, while the bolometric luminosity (Lbol) can be fairly well constrained from the optical to hard X-rays spectral energy distribution, giving access to the accretion efficiency η = Lbol/(Ṁc2) which depends on the SMBH spin. Methods. The spectral analysis uses simultaneous XMM-Newton (OM and pn) and NuSTAR observations on 2014 March 22 and 2013 February 18. We applied the OPTXCONV model (based on OPTXAGNF) to self consistently reproduce the emission from the inner corona (warm and hot thermal Comptonisation) and the outer disc (colour temperature corrected black body), taking into account both the disc inclination angle and relativistic effects. For self-consistency, we modelled the mild relativistic reflection of the incident Comptonisation components using the XILCONV convolution model. Results. We infer a SMBH spin of 0.83+0.05−0.03, adopting the SMBH reverberation mass of 1.50 × 108 M⊙. In addition, we find that the coronal radius decreases with increasing flux (by about a factor of two), from 85+13−10Rg in 2013 to 14 ± 3 Rg in 2014. Conclusions. This is the first time that such a constraint is obtained for a SMBH spin from this technique, thanks to the bare properties of Ark 120, its well determined SMBH reverberation mass, and the presence of a mild relativistic reflection component in 2014 which allows us to constrain the disc inclination angle. We caution that these results depend on the detailed disc-corona structure, which is not yet fully established. However, the realistic parameter values (e.g. Lbol/LEdd, disc inclination angle) found suggest that this is a promising method to determine spin in moderate-Ṁ AGN.

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Section: Black Hole Mass Valuementioning

confidence: 76%

A deep X-ray view of the bare AGN Ark 120

Porquet

Done

Reeves

et al. 2019

A&A

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“…More details of the spectral decomposition were described in Bon et al (2014Bon et al ( , 2016. Furthermore, Denissyuk et al (2015) collected spectroscopic monitoring data of Ark 120 over 1976-2013 using a 70-cm telescope. We use 16 of their spectra between 2005 and 2011.…”

Section: Hβ Profile Variationsmentioning

confidence: 99%

A Possible ∼20 yr Periodicity in Long-term Optical Photometric and Spectral Variations of the Nearby Radio-quiet Active Galactic Nucleus Ark 120

Wang

Zhang

et al. 2019

ApJS

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We study the long-term variability in the optical monitoring database of Ark 120, a nearby radio-quiet active galactic nucleus (AGN) at a distance of 143 Mpc (z = 0.03271). We compiled the historical archival photometric and spectroscopic data since 1974 and conducted a new two-year monitoring campaign in 2015-2017, resulting in a total temporal baseline over four decades. The long-term variations in the optical continuum exhibit a wave-like pattern and the Hβ integrated flux series varies with a similar behaviour. The broad Hβ profiles have asymmetric double peaks, which change strongly with time and tend to merge into a single peak during some epochs. The period in the optical continuum determined from various period-search methods is about 20 years and the estimated false alarm probability with null hypothesis simulations is about 1 × 10 −3 . The overall variations of the broad Hβ profiles also follow the same period. However, the present database only covers two cycles of the suggested period, which strongly encourages continued monitoring to track more cycles and confirm the periodicity. Nevertheless, in light of the possible periodicity and the complicated Hβ profile, Ark 120 is one candidate of the nearest radio-quiet AGNs with possible periodic variability and it is thereby a potential candidate host for a sub-parsec supermassive black hole binary. (15) the All-Sky Automated Survey for Supernovae database (Shappee et al. 2014; Kochanek et al. 2017). a The flux of [O III] λ5007 used for absolute calibration of spectra in the dataset. b The photometric data of all the datasets are at V -band, except for dataset M79 at B-band.c This dataset has no temporal overlap with the other datasets so that it is impossible to do intercalibration. We simply adjust the fluxes to make the mean and standard deviation to be at the same scales as those of the other datasets. We do not use this dataset for periodicity analysis.d This dataset includes 15 additional observations (50,863-52,282) that have not been public.e There is a large flux difference with respect to the other datasets. We offset the fluxes by −20.0 × 10 −15 erg s −1 cm −2 Å −1 before performing intercalibration.f This dataset has a poor temporal overlap with the other datasets and we simply fix ϕ = 1.

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“…After processing the observational data, the parameters of Keplerian orbits were obtained for three bodies emitting these emissions. The parameters of these three orbits are published in Denissyuk et al (2015). A common parameter of these orbits is the central mass of this galaxy.…”

Section: Seyfert Galaxy Mrk 1095 = Ark 120mentioning

confidence: 99%

Studies of Seyfert galaxies in Fesenkov Astrophysical Institute

Denissyuk

Валиуллин

Omarov

et al. 2020

ComBAO

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This article provides an overview of the main research results of a large group of Seyfert galaxies, carried out at Fesenkov Astrophysical Institute (FAI) over the past 50 years. Spectral observations have been performed since 1970. At an early stage, a three cascade image-tube (UM-92) was used as a radiation receiver. In the 1990s, the equipment was modernized, and at present, the modern CCD cameras are used as radiation detectors at the output of spectrographs. The results of observations were used to determine the absolute fluxes of the emission lines and to study their profiles. Several additional emission features were detected on the wings of the broad emission lines Hα in the spectra of two galaxies NGC 4151 and Ark 120. These features are emitted by compact ionized objects, rotating in the field of Central Body (CB). Photometric observations of Seyfert galaxies have been carried out at FAI since 2010. Light curves of more than 20 Seyfert galaxies have been obtained. In particular, the light curves of the galaxy NGC 4151, obtained last years, shows that an active stage of its nucleus took place in 2015-2016, when the brightness increased by 0m.5 in the V filter, and by almost 2m in the R filter. Then, in 2018-2019 there was a rather sharp decline of brightness, and B V R magnitudes returned to their minimal values.

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The mass of the central body of the galaxy Ark 120 and the orbits of objects in its gravitational field

Cited by 8 publications

References 8 publications

A deep X-ray view of the bare AGN Ark 120

A deep X-ray view of the bare AGN Ark 120

A Possible ∼20 yr Periodicity in Long-term Optical Photometric and Spectral Variations of the Nearby Radio-quiet Active Galactic Nucleus Ark 120

Studies of Seyfert galaxies in Fesenkov Astrophysical Institute

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