arXiv subjects

A. N. Burenkov

Publications and source records attributed to A. N. Burenkov.

At least 19 recordsLinked to original sources

arXiv2025

Photometric Stability of an EMCCD Camera at 1-s Exposures

We present the results of testing an iXonUltra 888 EMCCDcamera to determine the operating parameters for short-exposure photometry of stars. As a result of the testing, those camera modes were selected in which the temporal instability of the electron multiplication charge does not significantly affect the light curves. In addition, the photometry of the eclipsing variable star ZTFJ 0038+2030, obtained with the Zeiss-1000 telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences, is presented. We have shown the advantages and disadvantages of 1-s exposures for studying variable stars.

astro-ph.IM↗

arXiv2024

Investigation of the Nature of the B[e] Star CI Cam in the Optical Range

We report the results of 24 years of photometric and spectroscopic monitoring of CI Cam since its outburst in 1998. In the early years of our research, we identified a system component responsible for the emission of the He II 4686 line, which moves in an elliptical orbit with a period of 19.407 days and an eccentricity from 0.44 to 0.49. Variations in optical brightness with the same period were observed, with an average amplitude of 0.04 magnitudes. The total amplitude of the He II radial velocity variations was approximately 380 kilometers per second. The equivalent width of the line varied on timescales of tens of minutes as well as with the orbital period, reaching maximum values when the companion passed the descending node of the orbit. The intensity of the He II 4686 emission has gradually increased over time. Our photometric monitoring revealed pulsations of the main B component of the CI Cam system. Between 2005 and 2009, the B star exhibited multiperiodic pulsations, however, since 2012, it pulsated in a single mode. We interpret the pulsations from 2005 to 2009 as a resonance of radial modes, with the residual stable mode being the first overtone. The pulsations are coherent over several months, with average amplitudes from 0.02 to 0.04 magnitudes in the V band. The pulsation data constrain the spectral type of the primary component of B0 to B2 III, the distance to the system from 2.5 to 4.5 kpc. The classification of the main component of CI Cam as a supergiant is ruled out due to the observed pulsation periods. CI Cam is likely in the stage after the first mass exchange and may belong to the FS CMa-type objects.

astro-ph.SR↗

arXiv2024

Monitoring of DDO68 'Northern Ring' SF regions during years 2016-2023

DDO68 is a star-forming (SF) dwarf galaxy residing in a nearby void. Its gas metallicity is among the lowest known in the local Universe, with parameter 12+log(O/H) in the range of 6.96-7.3 dex. Six of its SF regions are located in or near the so-called 'Northern Ring', in which the Hubble Space Telescope (HST) images reveal many luminous young stars. We present for these SF regions (Knots) the results of optical monitoring in 35 epochs during the years 2016--2023. The data was acquired with the 6m (BTA) and the 1m telescopes of the Special Astrophysical Observatory and the 2.5m telescope of the MSU Caucasian Mountain Observatory. We complement the above results with the archive data from 10 other telescopes for 11 epochs during the years 1988-2013 and with 3 our BTA observations between 2005 and 2015. Our goal is to search for variability of these Knots and to relate it to the probable light variations of their brightest stars. One of them, DDO68-V1 (in Knot 3), was identified in 2008 with a luminous blue variable (LBV) star, born in the lowest metallicity environments. For Knot 3, variations of its integrated light in the previous epochs reached ~0.8 mag. In the period since 2016, the amplitude of variations of Knot 3 reached ~0.3 mag. For the rest Knots, due to the lower amplitudes, the manifestation of variability is less pronounced. We examine the presence of variability via the criterion chi^{2} and the Robust Median Statistics and discuss the robustness of the detected variations. The variability is detected according to the both criteria in the lightcurves of all Knots with the chi^{2} confidence level of alpha = 0.0005. The peak-to-peak amplitudes of variations are ~0.09, ~0.13, ~0.11, ~0.08 and ~0.16 mag for Knots 1, 2, 4, 5 and 6, respectively. The amplitudes of the related variations of the brightest supergiants in these regions can reach of ~3.0 mag.

astro-ph.GA↗

arXiv2024

Spectroscopic and photometric study of the new eclipsing polar Gaia23cer

We present the results of the optical study of the new eclipsing polar Gaia23cer. We analyzed the brightness variability of the polar in high ($\langle r \rangle \approx 16.5\mathrm{\,mag}$) and low ($\langle r \rangle \approx 19.2\mathrm{\,mag}$) states. The system has an orbital period $P_{orb} = 102.0665 \pm 0.0015$ min and exhibits deep eclipses with a duration $Δt_{ecl} = 401.30 \pm 0.81$ s. The spectra have a red cyclotron continuum with the Zeeman H$α$ absorption triplet forming in a magnetic field with a strength of $15.2 \pm 1.1$ MG. The source of emission lines has a high radial velocity semiamplitude ($K\approx 450$km/s) and its eclipse lags behind the eclipse of the white dwarf. The mass $M_1=0.79 \pm 0.03 M_{\odot}$ and temperature $T=11350 \pm 650 K$ of the white dwarf have been found by modelling the spectral energy distribution. The eclipse duration corresponds to a donor mass $M_2 = 0.10-0.13M_{\odot}$ and an orbital inclination $i=84.3-87.0^{\circ}$. The donor temperature was estimated to be $T\approx 2900K$ by modelling the elliptical variability and eclipse depth.

astro-ph.HE↗

arXiv2023

SDSS J085414.02+390537.3 -- a new asynchronous polar

The asynchrony of the polar SDSS~J085414.02+390537.3 was revealed using the data of ZTF photometric survey. The light curves show a beat period $P_{beat} = 24.6 \pm 0.1$~days. During this period the system changes its brightness by $\sim 3^m$. The periodograms show power peaks at the white dwarf's rotation period $P_{spin} = 113.197 \pm 0.001$~min and orbital period $P_{orb} = 113.560 \pm 0.001$~min with the corresponding polar asynchrony $1-P_{orb}/P_{spin} = 0.3\%$. The photometric behavior of the polar indicates a change of the main accreting pole during the beat period. Based on the Zeeman splitting of the H$β$ line, an estimate of the mean magnetic field strength of the white dwarf is found to be $B = 28.5\pm 1.5$~MG. The magnetic field strength $B \approx 34$~MG near the magnetic pole was found by modeling cyclotron spectra. Doppler tomograms in the H$β$ line demonstrate the distribution of emission sources typical for polars.

astro-ph.HE↗

arXiv2023

Optical study of the polar BM CrB in low accretion state

This paper presents a spectral and photometric study of the poorly studied polar BM CrB. Three states of the polar brightness and signs of transition from one-pole to two-pole accretion mode were found by an analysis of ZTF data. It is shown that the transition from the low state to the high state changes the longitude of the main accretion spot (by $\approx 17^{\circ}$) and increases its elongation (by $\approx 10^{\circ}$). The spectra contain Zeeman absorptions of the H$α$ line which are formed at a magnetic field strength of $15.5\pm1$ MG. These absorptions are likely produced by a cold halo extending from the accretion spot at $\approx {^1/_4}$ of the white dwarf radius. Modeling of the behavior of the H$α$ emission line shows that the main source of emission is the part of the accretion stream near the Lagrangian point L$_1$, which is periodically eclipsed by the donor star. The spectra exhibit a cyclotron component formed in the accretion spot. Its modeling by a simple accretion spot model gives constraints on the magnetic field strength $B=15-40$ MG and the temperature $T_e\gtrsim15$ keV.

astro-ph.HE↗

arXiv2022

Local Volume dwarf KK242: radial velocity, SF region, and metallicity

KK242 is a LV dwarf of transition type residing in the void environment. Koda et al. present clear indications on its connection with Scd galaxy NGC6503. This implies the distance to KK242 of ~6.3 Mpc and its M_B = -10.5 mag. Its radial velocity, known from the Effelsberg radio telescope \HI\ observations, reveals, however, the difference with that of NGC6503, dV ~ 400 km/s. If real, this fact implies the substantial constraints on its origin. To clear-up the issue of KK242 radial velocity, we obtained with the SAO 6-m telescope spectra of its faint star-forming (SF) complex. H-alpha and H-beta emission is detected in two adjacent compact regions, the southern and northern, separated by ~2" (~60 pc). Their mean radial velocity is V_hel = -66 km/s, ~100 km/s lower than that of NGC6503. We use the HST Legacy Archive images and photometry of individual stars from the Extragalactic Distance Database, available for KK242, to identify in the SF complex the exciting hot stars, the probable BHeB and RHeB stars and a supernova remnant. We address, based on the possible range of its gas metallicity, the probable evolutionary paths of KK242. Using package Cloudy and parameters of the exciting B0V stars, we conclude that the observed flux ratio of [Sii] doublet to H-alpha is consistent with the value of 12+log(O/H) ~7.35+/-0.18 dex, expected for a stripped void dIrr galaxy.

astro-ph.GA↗

arXiv2021

XMP gas-rich dwarfs in nearby voids: results of BTA spectroscopy

We present the second part of results of the on-going project of searching for and studying eXtremely Metal-Poor (XMP, adopted as those with Z(gas) <~ Zo/30, or with 12+log(O/H) <~ 7.21~dex) very gas-rich blue dwarfs in voids.They were first identified in course of the 'unbiased' study of galaxy population in the nearby Lynx-Cancer void. These very rare and unusual galaxies seem to be the best proxies of so-called Very Young Galaxies (VYGs) defined recently in model simulations by Tweed et al. To date, for 16 preselected void XMP candidates, we obtained with the SAO 6-m telescope (BTA) spectra suitable for determination of O/H. For majority of the observed galaxies, the principal line [OIII]4363 used for the direct classical T_e method of O/H determination, is undetected. Therefore, to estimate O/H, we use a new 'Strong-lines' method by Izotov et al. This appears the most accurate empirical O/H estimator for the range of 12+log(O/H) < 7.4-7.5. For higher O/H objects, we use the semi-empirical method by Izotov and Thuan with our modification accounting for variance of the excitation parameter O32. Six of those 16 candidates are found to be the confident XMP dwarfs. In addition, eight studied galaxies are somewhat less metal-poor, with 12+log(O/H) = 7.24-7.33. They also can fall into the category of VYG candidates. With account of the recently published by us and previously known (9 prototype galaxies) XMP gas-rich void objects, the new findings increase the number of this type galaxies to the total of 19.

astro-ph.GA↗

arXiv2019

Two epoch spectro-imagery of FS Tau B outflow system

Herbig-Haro (HH) flows exhibit a large variety of morphological and kinematical structures such as bow shocks, Mach disks, and deflection shocks. Both proper motion (PM) and radial velocity investigations are essential to understand the physical nature of such structures. We investigate the kinematics and PM of spectrally separated structures in the FS~Tau~B HH flow. Collating these data makes it possible to understand the origin of these structures and to explain the unusual behavior of the jet. On the other hand, the study of emission profiles in the associated reflection nebulae allows us to consider the source of the outflow both from edge-on and pole-on points of view. We present the observational results obtained with the 6 m telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences using the SCORPIO multimode focal reducer with a scanning Fabry-Perot interferometer. Two epochs of the observations of the FS~Tau~B region in H$α$ emission (2001 and 2012) allowed us to measure the PM of the spectrally separated inner structures of the jet. In addition to already known emission structures in the FS~Tau~B system, we discover new features in the extended part of the jet and in the counter-jet. Moreover, we reveal a new HH knot in the HH~276 independent outflow system and point out its presumable source. In the terminal working surface of the jet, structures with different radial velocities have PMs of the same value. This result can be interpreted as the direct observation of bow-shock and Mach disk regions. A bar-like structure, located southwest from the source demonstrates zero PM and can be considered as one more example of deflection shock. An analysis of H$α$ profiles in the reflection nebulae R1 and R3 indicates the uniqueness of this object, which can be studied in pole-on and edge-on directions simultaneously.

astro-ph.SR↗

arXiv2019

Long-term optical spectral monitoring of a changing-look AGN NGC 3516 I: Continuum and broad-line flux variability

Here we present the long-term optical spectral monitoring of a changing-look active galactic nuclei (AGN) NGC 3516 that covers 22 years (from 1996 to 2018). We explore a variability in the broad lines and continuum, finding that the continuum is changing by more than a factor of 2, while the broad lines are varying by more than a factor of 10. The minimum of activity is observed in 2014, when the broad lines almost disappeared. We confirm that NGC 3516 is a changing-look AGN, and the absorption seen in the UV and X-ray may indicate that there is an obscuring region which is responsible for this. The line profiles are also changing. The mean profiles of the broad Halpha and Hbeta lines show shoulder-like structure in the wings, and enhanced peak, that may indicate a complex BLR. The rms-profiles of both lines seem to have the same shape and width of around 4200 km/s, indicating practically the same kinematics in the Halpha and Hbeta emitting regions. Measured time-lags between the continuum and Halpha and Hbeta broad-line variability are ~15 and 17 days, respectively, that in combination with the broad lines width allows us to estimate the NGC 3516 central black hole mass. We find that the black hole mass is 4.73+-1.40 x 10^7M_sun which is in agreement with previous estimates.

astro-ph.GA↗

arXiv2017

Long-term optical spectral monitoring of NGC 7469

We present the results of the long-term (20-year period, from 1996 to 2015) optical spectral monitoring of the Seyfert 1 galaxy NGC 7469. The variation in the light-curves of the broad He II λ4686A Hβ and Hα lines, and the continuum at 5100A and 6300A have been explored. The maximum of activity was in 1998, and the variability in the continuum and lines seems to have two periods of around 1200 and 2600 days, however these periodicities should be taken with caution because of the red-noise. Beside these periods, there are several short-term (1-5 days) flare-like events in the light-curves. There are good correlations between the continuum fluxes and Hα and Hβ line fluxes, but significantly smaller correlation between the He II and continuum. We found that the time-lags between the continuum and broad lines are different for Hβ (~20 l.d.) and Hα (~3 l.d.), and that He II also has a smaller lag (~2-3 l.d.). The Hα and Hβ line profiles show a slight red asymmetry, and the broad line profiles did not changed in the 20-year period. Using the lags and widths of Hα and Hβ we estimated the central black hole mass and found that it is ~(1-6)x$10^7 M_{\odot}$, which is in agreement with previous reverberation estimates.

astro-ph.GA↗

arXiv2016

Evidence for periodicity in 43 year-long monitoring of NGC 5548

We present an analysis of 43 years (1972 to 2015) of spectroscopic observations of the Seyfert 1 galaxy NGC 5548. This includes 12 years of new unpublished observations (2003 to 2015). We compiled about 1600 H$β$ spectra and analyzed the long-term spectral variations of the 5100 Å continuum and the H$β$ line. Our analysis is based on standard procedures including the Lomb-Scargle method, which is known to be rather limited to such heterogeneous data sets, and new method developed specifically for this project that is more robust and reveals a $\sim$5700 day periodicity in the continuum light curve, the H$β$ light curve and the radial velocity curve of the red wing of the H$β$ line. The data are consistent with orbital motion inside the broad emission line region of the source. We discuss several possible mechanisms that can explain this periodicity, including orbiting dusty and dust-free clouds, a binary black hole system, tidal disruption events, and the effect of an orbiting star periodically passing through an accretion disc.

astro-ph.HE↗

arXiv2016

Polarization angle swings in blazars: The case of 3C 279

Over the past few years, several occasions of large, continuous rotations of the electric vector position angle (EVPA) of linearly polarized optical emission from blazars have been reported. These events are often coincident with high energy gamma-ray flares and they have attracted considerable attention, as they could allow one to probe the magnetic field structure in the gamma-ray emitting region of the jet. The flat-spectrum radio quasar 3C279 is one of the most prominent examples showing this behaviour. Our goal is to study the observed EVPA rotations and to distinguish between a stochastic and a deterministic origin of the polarization variability. We have combined multiple data sets of R-band photometry and optical polarimetry measurements of 3C279, yielding exceptionally well-sampled flux density and polarization curves that cover a period of 2008-2012. Several large EVPA rotations are identified in the data. We introduce a quantitative measure for the EVPA curve smoothness, which is then used to test a set of simple random walk polarization variability models against the data. 3C279 shows different polarization variation characteristics during an optical low-flux state and a flaring state. The polarization variation during the flaring state, especially the smooth approx. 360 degrees rotation of the EVPA in mid-2011, is not consistent with the tested stochastic processes. We conclude that during the two different optical flux states, two different processes govern the polarization variation, possibly a stochastic process during the low-brightness state and a deterministic process during the flaring activity.

astro-ph.HE↗

arXiv2016

First long-term optical spectro-photometric monitoring of a binary black hole candidate E1821+643: I. Variability of spectral lines and continuum

We report the results of the first long-term (1990-2014) optical spectro-photometric monitoring of a binary black hole candidate QSO E1821+643, a low-redshift high-luminosity radio-quiet quasar. In the monitored period the continua and H$γ$ fluxes changed for around two times, while the H$β$ flux changed around 1.4 times. We found the periodical variations in the photometric flux with the periods of 1200, 1850 and 4000 days, and 4500 days periodicity in the spectroscopic variations. However, the periodicity of 4000-4500 days covers only one cycle of variation and should be confirmed with a longer monitoring campaign. There is an indication of the period around 1300 days in the spectroscopic light curves, but with small significance level, while the 1850 days period could not be clearly identified in the spectroscopic light curves. The line profiles have not significantly changed, showing an important red asymmetry and broad line peak redshifted around +1000 km s$^{-1}$. However, H$β$ shows broader mean profile and has a larger time-lag ($τ\sim120$ days) than H$γ$ ($τ\sim60$ days). We estimate that the mass of the black hole is $\sim2.6\times10^9\rm M_\odot$. The obtained results are discussed in the frame of the binary black hole hypothesis. To explain the periodicity in the flux variability and high redshift of broad lines we discuss a scenario where dense gas-rich cloudy-like structures are orbiting around a recoiling black hole.

astro-ph.GA↗

arXiv2015

Line shape variability in a sample of AGN with broad lines

The spectral variability of active galactic nuclei (AGN) is one of their key features that enables us to study in more details the structure of AGN emitting regions. Especially, the broad line profiles, that vary both in flux and shape, give us invaluable information about the kinematics and geometry of the broad line region (BLR) where these lines are originating from. We give here a comparative review of the line shape variability in a sample of five type 1 AGN, those with broad emission lines in their spectra, of the data obtained from the international long-term optical monitoring campaign coordinated by the Special Astrophysical Observatory of the Russian Academy of Science. The main aim of this campaign is to study the physics and kinematics of the BLR on a uniform data set, focusing on the problems of the photoionization heating of the BLR and its geometry, where in this paper we give for a first time a comparative analysis of the variabilty of five type 1 AGN, discussing their complex BLR physics and geometry in the framework of the estimates of the supermassive black hole mass in AGN.

astro-ph.GA↗

arXiv2014

Spectral monitoring of AGNs: Preliminary results for Ark 564 and Arp 102B

We present preliminary results of the long term spectral monitoring of two active galactic nuclei with different broad line shapes: Ark 564 and Arp 102B. Ark 564 is a bright nearby narrow line Syfert 1 (NLS1) galaxy with relatively narrow permitted optical emission lines and a high FeII/H$β$ ratio, while Arp 102B is a nearby broad-line radio galaxy with broad double-peaked Balmer emission lines. The spectra of Ark 564 were observed during 11-year period (1999-2009) and the spectra of Arp 102B in the 12-year period (1998-2009), with SAO 6-m and 1-m telescopes (Russia) and the GHAO 2.1-m telescope (Cananea, Mexico).

astro-ph.CO↗

arXiv2014

Spectral optical monitoring of the double peaked emission line AGN Arp 102B: II. Variability of the broad line properties

We investigate a long-term (26 years, from 1987 to 2013) variability in the broad spectral line properties of the radio galaxy Arp 102B, an active galaxy with broad double-peaked emission lines. We use observations presented in Paper I (Shapovalova et al. 2013) in the period from 1987 to 2011, and a new set of observations performed in 2012--2013. To explore the BLR geometry, and clarify some contradictions about the nature of the BLR in Arp 102B we explore variations in the H$α$ and H$β$ line parameters during the monitored period. We fit the broad lines with three broad Gaussian functions finding the positions and intensities of the blue and red peaks in H$α$ and H$β$. Additionally we fit averaged line profiles with the disc model. We find that the broad line profiles are double-peaked and have not been changed significantly in shapes, beside an additional small peak that, from time to time can be seen in the blue part of the H$α$ line. The positions of the blue and red peaks { have not changed significantly during the monitored period. The H$β$ line is broader than H$α$ line in the monitored period. The disc model is able to reproduce the H$β$ and H$α$ broad line profiles, however, observed variability in the line parameters are not in a good agreement with the emission disc hypothesis. It seems that the BLR of Arp 102B has a disc-like geometry, but the role of an outflow can also play an important role in observed variation of the broad line properties.

astro-ph.GA↗

arXiv2014

Time Series Analysis of Active Galactic Nuclei: The case of Arp 102B, 3C 390.3, NGC 5548 and NGC 4051

We used the Z-transformed Discrete Correlation Function (ZDCF) and the Stochastic Process Estimation for AGN Reverberation (SPEAR) methods for the time series analysis of the continuum and the H$α$ and H$β$ line fluxes of a sample of well known type 1 active galactic nuclei (AGNs): Arp 102B, 3C 390.3, NGC 5548, and NGC 4051, where the first two objects are showing double-peaked emission line profiles. The aim of this work is to compare the time lag measurements from these two methods, and check if there is a connection with other emission line properties. We found that the obtained time lags from H$β$ are larger than those derived from the H$α$ analysis for Arp 102B, 3C 390.3 and NGC 5548. This may indicate that the H$β$ line originates at larger radii in these objects. Moreover, we found that the ZDCF and SPEAR time lags are highly correlated ($r \sim0.87$), and that the error ranges of both ZDCF and SPEAR time lags are correlated with the FWHM of used emission lines ($r\sim 0.7$). This increases the uncertainty of the black hole mass estimates using the virial theorem for AGNs with broader lines.

astro-ph.GA↗