Roman V. Baluev
Current Organizations / Institutes
The organizations/institutes from the scholar's latest article
Previous Organizations / Institutes
The organizations / institutes from the scholar's other articles in the past ten years
Research Subjects
Roman V. Baluev has a total of 215 co-authors. Here are the top co-authors by number of shared publications:
- Vakhit Sh. Shaidulin
St. Petersburg State University
5 shared publications Cristian Beaugé
Instituto de Astronomía Teórica y Experimental Observatorio Astronómico Universidad Nacional de Córdoba Laprida 854 (X5000BGR) Córdoba Argentina
4 shared publications- Gazinur Galazutdinov
Federal State Budget Scientific Institution Crimean Astrophysical Observatory of RAS 298409 Nauchny Crimea
3 shared publications A Ivanova
Space Research Institute, Russian Academy of Sciences , 84/32 Profsoyuznaya Str., Moscow 117997 , Russia
2 shared publicationsA Rzaev
Special Astrophysical Observatory, Russian Academy of Sciences , Nizhnij Arkhyz 369167 , Russia
2 shared publicationsA Tavrov
Space Research Institute, Russian Academy of Sciences , 84/32 Profsoyuznaya Str., Moscow 117997 , Russia
2 shared publications
Latest Publications
- 1 June 2026
- Published by Pleiades Publishing Ltd in Astrophysical Bulletin
- Vol. 81 (2) , 340-359
Effect of Spitzer/IRAC Systematic Noises on Secondary Eclipses of the Exoplanet HD 209458 b
We analyze infrared light curves for 13 secondary eclipses of the exoplanet HD 209458 b obtained by Spitzer/IRAC in the 3.6 \(\mu\)m channel. We find that in addition to the well-known effect of intra-pixel sensitivity variations, inducing quasiperiodic noise, these data also contain red noise which in turn consists of two subcomponents that differ by their correlation timescale, 10–20 s and 5–10 min. We also show that a global model of the intra-pixel sensitivity effect can be constructed such that it can fit all 13 light curves at once but uses only a few parameters (e.g., 12 or so). Finally, we tried to measure the systematic time shift of the exoplanetary secondary eclipse, which appeared consistent with zero, \(-4\pm 40\) s. This corresponds to a spatial shift of \(0.007\pm 0.060\) in units of planet radius, or to the orbital eccentricity \(e\cos\omega\) of \((-0.2\pm 2.1)\times 10^{-4}\).- 1 June 2026
- Published by Pleiades Publishing Ltd in Astrophysical Bulletin
- Vol. 81 (2) , 340-359
Effect of Spitzer/IRAC Systematic Noises on Secondary Eclipses of the Exoplanet HD 209458 b
We analyze infrared light curves for 13 secondary eclipses of the exoplanet HD 209458 b obtained by Spitzer/IRAC in the 3.6 \(\mu\)m channel. We find that in addition to the well-known effect of intra-pixel sensitivity variations, inducing quasiperiodic noise, these data also contain red noise which in turn consists of two subcomponents that differ by their correlation timescale, 10–20 s and 5–10 min. We also show that a global model of the intra-pixel sensitivity effect can be constructed such that it can fit all 13 light curves at once but uses only a few parameters (e.g., 12 or so). Finally, we tried to measure the systematic time shift of the exoplanetary secondary eclipse, which appeared consistent with zero, \(-4\pm 40\) s. This corresponds to a spatial shift of \(0.007\pm 0.060\) in units of planet radius, or to the orbital eccentricity \(e\cos\omega\) of \((-0.2\pm 2.1)\times 10^{-4}\).- 19 April 2026
- Published by Pleiades Publishing Ltd in Vestnik St. Petersburg University, Mathematics
- Vol. 59 (2) , 234-243
Application of Artificial Neural Networks in the Problem of Searching for Periodic Signals
- 19 April 2026
- Published by Pleiades Publishing Ltd in Vestnik St. Petersburg University, Mathematics
- Vol. 59 (2) , 234-243
Application of Artificial Neural Networks in the Problem of Searching for Periodic Signals
- 12 March 2026
- Published by Pleiades Publishing Ltd in Vestnik St. Petersburg University, Mathematics
- Vol. 59 (1) , 9-16
On the Errors in the Correlogram of a Time Series Modeled by a Gaussian Random Process
- 12 March 2026
- Published by Pleiades Publishing Ltd in Vestnik St. Petersburg University, Mathematics
- Vol. 59 (1) , 9-16
On the Errors in the Correlogram of a Time Series Modeled by a Gaussian Random Process
- 6 August 2025
- Published by Pleiades Publishing Ltd in Vestnik St. Petersburg University, Mathematics
- Vol. 58 (3) , 370-378
Multivariate Distribution Function for a Centered and Normalized Time Series with Gaussian White Noise
In this work, an explicit expression is obtained for the distribution function of a centered and normalized data vector containing a deterministic signal (or without a signal) and Gaussian white noise with constant variance. The obtained representation is exact and does not rely on any asymptotics for a large number of observations in particular; it is ultimately expressed through an error function and elementary functions and requires iterative calculations based on a recurrence formula.
- 6 August 2025
- Published by Pleiades Publishing Ltd in Vestnik St. Petersburg University, Mathematics
- Vol. 58 (3) , 370-378
Multivariate Distribution Function for a Centered and Normalized Time Series with Gaussian White Noise
In this work, an explicit expression is obtained for the distribution function of a centered and normalized data vector containing a deterministic signal (or without a signal) and Gaussian white noise with constant variance. The obtained representation is exact and does not rely on any asymptotics for a large number of observations in particular; it is ultimately expressed through an error function and elementary functions and requires iterative calculations based on a recurrence formula.
- Open Access
- 6 January 2025
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 537 (1) , 171-184
Cleaning WASP-33 b transits from the host star photometric variability: analysis of TESS data from two sectors
Based on TESS observations of a $\delta$ Scuti variable WASP-33 obtained in 2019 and 2022, we thoroughly investigate the power spectrum of this target photometric flux and construct a statistically exhaustive model for its variability. This model contains 30 robustly justified harmonics detected in both the TESS sectors simultaneously, 13 less robust harmonics detected in a single TESS sector, a red noise, and a quasi-periodic noise term. This allowed us to greatly improve the accuracy of the exoplanet WASP-33 b transit timings, reducing the TTV residuals r.m.s. drastically, by a factor of 3.5, from 63 to 18 s. Finally, our analysis does not confirm existence of a detectable orbital phase variation claimed previously based on WASP-33 TESS photometry of 2019.- 6 January 2025
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 537 (1) , 171-184
Open AccessCleaning WASP-33 b transits from the host star photometric variability: analysis of TESS data from two sectors
Based on TESS observations of a $\delta$ Scuti variable WASP-33 obtained in 2019 and 2022, we thoroughly investigate the power spectrum of this target photometric flux and construct a statistically exhaustive model for its variability. This model contains 30 robustly justified harmonics detected in both the TESS sectors simultaneously, 13 less robust harmonics detected in a single TESS sector, a red noise, and a quasi-periodic noise term. This allowed us to greatly improve the accuracy of the exoplanet WASP-33 b transit timings, reducing the TTV residuals r.m.s. drastically, by a factor of 3.5, from 63 to 18 s. Finally, our analysis does not confirm existence of a detectable orbital phase variation claimed previously based on WASP-33 TESS photometry of 2019. - Open Access
- 27 December 2024
- Published by Special Astrophysical Observatory of the Russian Academy of Sciences
- p. 687-692
Cleaning the TESS observations of WASP-33 b transits from the host star photometric variability
Based on the TESS observations of a $\delta$ Scuti variable WASP-33 obtained in 2019 and 2022, we thoroughly investigate the power spectrum of its photometric flux and construct a statistically exhaustive model for its variation. This model contains 30 robustly justified harmonics, the red noise, and quasiperiodic noise components. This compound model allows us to greatly improve the transit timing accuracy of the exoplanet WASP-33 b. The rms of its transit timing variation residuals is drastically reduced by a factor of 3.5, from 63 s to 18 s.- 27 December 2024
- Published by Special Astrophysical Observatory of the Russian Academy of Sciences
- p. 687-692
Open AccessCleaning the TESS observations of WASP-33 b transits from the host star photometric variability
Based on the TESS observations of a $\delta$ Scuti variable WASP-33 obtained in 2019 and 2022, we thoroughly investigate the power spectrum of its photometric flux and construct a statistically exhaustive model for its variation. This model contains 30 robustly justified harmonics, the red noise, and quasiperiodic noise components. This compound model allows us to greatly improve the transit timing accuracy of the exoplanet WASP-33 b. The rms of its transit timing variation residuals is drastically reduced by a factor of 3.5, from 63 s to 18 s. - Open Access
- 27 December 2024
- Published by Special Astrophysical Observatory of the Russian Academy of Sciences
- p. 698-703
Investigation of the infrared profiles of exoplanet HD 209458 b secondary eclipses
In this work we process infrared light curves for 13 secondary eclipses of the exoplanet HD 209458 b, obtained with the Spitzer Space Telescope. The objective of the study was to identify any discrepancies that might be attributed to the inhomogeneity of the planet's surface brightness or a difference of the planet's shape from a sphere. Firstly, an attempt was made to ascertain whether the observed midpoint of the secondary eclipse exhibited a shift from the ephemeris moment. This could indicate the presence of a hot spot on the planet's surface that is shifted from the central meridian. The analysis allowed for the correlated noise that remained in the IRAC detector data after aperture photometry by approximating the noise with a Gaussian random process. As a result, we detected two components of red noise with different time scales: $\sim\!10$ s and $\sim\!5$ min. In addition, we constructed a unified model of the effect of inhomogeneous pixel sensitivity as a periodic function of the brightness centroid coordinates, which works well for all the analyzed eclipses. According to the results, the main parameters of the HD 209458 b eclipse coincided with those obtained by other authors: a depth of $0.125 \pm 0.004$% and a shift of the observed midpoint of $-0.53 \pm 0.61$ min.- 27 December 2024
- Published by Special Astrophysical Observatory of the Russian Academy of Sciences
- p. 698-703
Open AccessInvestigation of the infrared profiles of exoplanet HD 209458 b secondary eclipses
In this work we process infrared light curves for 13 secondary eclipses of the exoplanet HD 209458 b, obtained with the Spitzer Space Telescope. The objective of the study was to identify any discrepancies that might be attributed to the inhomogeneity of the planet's surface brightness or a difference of the planet's shape from a sphere. Firstly, an attempt was made to ascertain whether the observed midpoint of the secondary eclipse exhibited a shift from the ephemeris moment. This could indicate the presence of a hot spot on the planet's surface that is shifted from the central meridian. The analysis allowed for the correlated noise that remained in the IRAC detector data after aperture photometry by approximating the noise with a Gaussian random process. As a result, we detected two components of red noise with different time scales: $\sim\!10$ s and $\sim\!5$ min. In addition, we constructed a unified model of the effect of inhomogeneous pixel sensitivity as a periodic function of the brightness centroid coordinates, which works well for all the analyzed eclipses. According to the results, the main parameters of the HD 209458 b eclipse coincided with those obtained by other authors: a depth of $0.125 \pm 0.004$% and a shift of the observed midpoint of $-0.53 \pm 0.61$ min. - Open Access
- 27 December 2024
- Published by Special Astrophysical Observatory of the Russian Academy of Sciences
- p. 681-686
Doppler confirmation of TESS planet candidate TOI-1408.01: updated analysis and fitting
Based on the Doppler observations from the FFOREST spectrograph of the 6-meter telescope (BTA) and on the photometric observations from the TESS spacecraft, we provide an updated analysis for TOI-1408, an F-type main sequence star, located 140 pc away, that hosts exoplanet TOI-1408.01. We confirm the qualitative conclusions from our initial paper: (1) a grazing transit geometry such that the planet obscures its host star by only a portion of the visible disc,(2) unreliably fitted planet radius, (3) which nonetheless has a lower bound constraint of $\sim\!1~R_{\rm Jup}$, (4) unexpectedly large planet mass of $\simeq\!1.7~M_{\rm Jup}$, and (5) significant evidence in favor of a moderately eccentric orbit with $e\simeq0.27$. This solution may suggest that the planet is likely to experience a high tidal eccentricity migration at the stage of intense orbital rounding or may indicate the possible presence of other unseen companions in the system, yet to be detected.- 27 December 2024
- Published by Special Astrophysical Observatory of the Russian Academy of Sciences
- p. 681-686
Open AccessDoppler confirmation of TESS planet candidate TOI-1408.01: updated analysis and fitting
Based on the Doppler observations from the FFOREST spectrograph of the 6-meter telescope (BTA) and on the photometric observations from the TESS spacecraft, we provide an updated analysis for TOI-1408, an F-type main sequence star, located 140 pc away, that hosts exoplanet TOI-1408.01. We confirm the qualitative conclusions from our initial paper: (1) a grazing transit geometry such that the planet obscures its host star by only a portion of the visible disc,(2) unreliably fitted planet radius, (3) which nonetheless has a lower bound constraint of $\sim\!1~R_{\rm Jup}$, (4) unexpectedly large planet mass of $\simeq\!1.7~M_{\rm Jup}$, and (5) significant evidence in favor of a moderately eccentric orbit with $e\simeq0.27$. This solution may suggest that the planet is likely to experience a high tidal eccentricity migration at the stage of intense orbital rounding or may indicate the possible presence of other unseen companions in the system, yet to be detected. - Open Access
- 29 March 2024
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society: Letters
- Vol. 531 (1) , L33
Erratum: Doppler confirmation of TESS planet candidate TOI1408.01: grazing transit and likely eccentric orbit
The paper ‘Doppler confirmation of TESS planet candidate TOI1408.01: grazing transit and likely eccentric orbit’ was published in Mon. Not. R. Astron. Soc. Letters 526, L111-L115 (2023). Here we notice that by a mistake there were multiple duplicated transit lightcurves among the 96 ones used in the analysis (see Section 2.1 of the paper). It was unnoticed that TESS data archive contains results from multiple DVT pipeline runs, including same observations reprocessed with a slightly different output. We performed a reanalysis of the correct dataset, including just the latest processing available for a given lightcurve, and it appeared that there are mostly insignificant changes to the results from the original paper. Here we provide the corrected Table 3, based on 58 unique transit lightcurves. Most of estimates remain within the two-sigma range of the original ones, and only the orbital period changed more remarkably. The changes to the figures from the paper are entirely insignificant.
- 29 March 2024
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society: Letters
- Vol. 531 (1) , L33
Open AccessErratum: Doppler confirmation of TESS planet candidate TOI1408.01: grazing transit and likely eccentric orbit
The paper ‘Doppler confirmation of TESS planet candidate TOI1408.01: grazing transit and likely eccentric orbit’ was published in Mon. Not. R. Astron. Soc. Letters 526, L111-L115 (2023). Here we notice that by a mistake there were multiple duplicated transit lightcurves among the 96 ones used in the analysis (see Section 2.1 of the paper). It was unnoticed that TESS data archive contains results from multiple DVT pipeline runs, including same observations reprocessed with a slightly different output. We performed a reanalysis of the correct dataset, including just the latest processing available for a given lightcurve, and it appeared that there are mostly insignificant changes to the results from the original paper. Here we provide the corrected Table 3, based on 58 unique transit lightcurves. Most of estimates remain within the two-sigma range of the original ones, and only the orbital period changed more remarkably. The changes to the figures from the paper are entirely insignificant.
- 9 August 2023
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society: Letters
- Vol. 526 (1) , L111-L115
Doppler confirmation of TESS planet candidate TOI−1408.01: grazing transit and likely eccentric orbit
We report an independent Doppler confirmation of the TESS planet candidate orbiting an F-type main sequence star TOI-1408 located 140 pc away. We present a set of radial velocities obtained with a high-resolution fiber-optic spectrograph FFOREST mounted at the SAO RAS 6-m telescope (BTA-6). Our self- consistent analysis of these Doppler data and TESS photometry suggests a grazing transit such that the planet obscures its host star by only a portion of the visible disc. Because of this degeneracy, the radius of TOI-1408.01 appears ill-determined with lower limit about ∼1 RJup, significantly larger than in the current TESS solution. We also derive the planet mass of 1.69 ± 0.20 MJup and the orbital period ∼4.425 days, thus making this object a typical hot Jupiter, but with a significant orbital eccentricity of 0.259 ± 0.026. Our solution may suggest the planet is likely to experience a high tidal eccentricity migration at the stage of intense orbital rounding, or may indicate possible presence of other unseen companions in the system, yet to be detected.
- 9 August 2023
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society: Letters
- Vol. 526 (1) , L111-L115
Doppler confirmation of TESS planet candidate TOI−1408.01: grazing transit and likely eccentric orbit
We report an independent Doppler confirmation of the TESS planet candidate orbiting an F-type main sequence star TOI-1408 located 140 pc away. We present a set of radial velocities obtained with a high-resolution fiber-optic spectrograph FFOREST mounted at the SAO RAS 6-m telescope (BTA-6). Our self- consistent analysis of these Doppler data and TESS photometry suggests a grazing transit such that the planet obscures its host star by only a portion of the visible disc. Because of this degeneracy, the radius of TOI-1408.01 appears ill-determined with lower limit about ∼1 RJup, significantly larger than in the current TESS solution. We also derive the planet mass of 1.69 ± 0.20 MJup and the orbital period ∼4.425 days, thus making this object a typical hot Jupiter, but with a significant orbital eccentricity of 0.259 ± 0.026. Our solution may suggest the planet is likely to experience a high tidal eccentricity migration at the stage of intense orbital rounding, or may indicate possible presence of other unseen companions in the system, yet to be detected.