Marat Mingaliev | Kazan Federal University (original) (raw)

Papers by Marat Mingaliev

Astrophysical Bulletin, 2015

Astrophysical Bulletin, 2015

We study the synchrotron component of the spectral energy distribution (SED) on the sample of 877... more We study the synchrotron component of the spectral energy distribution (SED) on the sample of 877 blazars using the ASDC SED Builder Tool with available broadband data from the literature. Our sample includes 423 flat-spectrum radio sources (FSRQs), 361 BL Lac objects and candidates, and 93 blazars of uncertain type. We have made an estimation of the synchrotron peak frequency (ν s peak) for the 875 objects and further classified them as high, intermediate and low synchrotron peaked sources (HSPs/ISPs/LSPs). There are 42 HSPs with ν s peak > 10 16.5 Hz, 222 ISPs with 10 14.5 < ν s peak < 10 16.5 Hz, and 611 LSPs with ν s peak < 10 14.5 Hz in our sample. We have calculated an average value of ν s peak to be 10 13.4±1.0 Hz for FSRQs and 10 14.6±1.4 Hz for BL Lacs. We found out that ν s peak and the flux density at 4.8 GHz have a different distribution (as indicated by Kolmogorov-Smirnov test at significance level 0.05) for the FSRQ and BL Lac blazars, and for the RBL and XBL types of BL Lacs. Distribution of ν s peak values is broader for BL Lacs, than for FSRQs. There are no ultra-high energy peaked objects (with ν s peak > 10 19 Hz) in our BL Lac sample according to our estimations. The significant part of FSRQs (41%) and small part of BL Lacs (9%) in our sample could be considered as candidates to the very-low synchrotron peaked blazars (with ν s peak < 10 13 Hz). Our foundations confirm results of the previous studies made on samples with significantly smaller number of objects.

Monthly Notices of the Royal Astronomical Society, 2015

We study the correlation between gamma-ray and radio band radiation for 123 blazars, using the Fe... more We study the correlation between gamma-ray and radio band radiation for 123 blazars, using the Fermi-LAT first source catalog (1FGL) and the RATAN-600 data obtained at the same period of time (within a few months). We found an apparent positive correlation for BL Lac and flat-spectrum radio quasar (FSRQ) sources from our sample through testing the value of the Pearson product-moment correlation coefficient. The BL Lac objects show higher values of the correlation coefficient than FSRQs at all frequencies, except 21.7 GHz, and at all bands, except 10 − 100 GeV, typically at high confidence level (> 99 %). At higher gammaray energies the correlation weakens and even becomes negative for BL Lacs and FSRQs. For BL Lac blazars, the correlation of the fluxes appeared to be more sensitive to the considered gamma-ray energy band, than to the frequency, while for FSRQ sources the correlation changed notably both with the considered radio frequency and gamma-ray energy band. We used a data randomization method to quantify the significance of the computed correlation coefficients. We find that the statistical significance of the correlations we obtained between the flux densities at all frequencies and the photon flux in all gamma-ray bands below 3 GeV is high for BL Lacs (chance probability ∼ 10 −3 − 10 −7). The correlation coefficient is high and significant for the 0.1 − 0.3 GeV band and low and insignificant for the 10 − 100 GeV band for both types of blazars for all considered frequencies.

Astronomy Reports, 1999

Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are prese... more Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7, 3.9, 7.6, 13,

Simultaneous multifrequency radio spectra have been obtained for the source 3C 84 (the Seyfert ga... more Simultaneous multifrequency radio spectra have been obtained for the source 3C 84 (the Seyfert galaxy NGC 1275) with the RATAN-600 radio telescope at two epochs, 1979.5 and 1980.0. The energy of the particles and field is confirmed to be growing at a rate of about 15% annually.

Astronomy Letters, 2016

The results of observations of the quasar J0530+1331 (B0528+134) with the radio telescopes RATAN-... more The results of observations of the quasar J0530+1331 (B0528+134) with the radio telescopes RATAN-600 at frequencies of 4.6, 8.2, 11.2, 21.7 GHz and RT-32 at the Zelenchukskaya and Badary observatories of the Quasar network of the Institute of Applied Astronomy, the Russian Academy of Sciences, at frequencies of 4.84 and 8.57 GHz in 2014–2015 are presented. A strong variability on a timescale of 20 days at 4.6–11.2 GHz has been detected over three months of daily RATAN-600 observations; the variability indices are V = dS/〈S〉; = 0.65−0.39. The spectrum of the variable component is falling toward high frequencies with an index α = −0.76. The structure and autocorrelation functions at 4.6 GHz show an additional process on a timescale of 7 days. No delay of the main process has been detected between 11.2 and 8.2 GHz; the delay between 8.2 and 4.6 GHz does not exceed two days. The most likely cause of the observed variability is the scattering by inhomogeneities of the interstellar medium. The variability has been obtained at theminimum activity phase of the source. The intraday variability (IDV) has been searched for at both RT-32 telescopes since April 2014. Out of 38 successful observing sessions for the source, only three have shown a variability on a timescale of four hours or more at a significance level no higher than 0.1%. This confirms our conclusion drawn from the previous IDV measurements for other sources that the IDV is observed mainly at the maximum phases of long-term variability of the sources.

PROCEEDINGS OF SPIE, 2020

We are presenting the results of astroclimatic studies in the North Caucasus started on our Febru... more We are presenting the results of astroclimatic studies in the North Caucasus started on our February 2020 expedition. The main objective of the studies is to compare millimeter-wave optical depth characteristics of four North Caucasus sites: BTA-6, RATAN-600, CMO of GAISh, and the Terskol Observatory. The opacity was studied by the atmospheric dip method in the 3 mm and 2 mm atmospheric windows. The astroclimate conditions of these four sites are compared through statistically processed data. This astroclimatic analysis has been performed with the view to selecting a site for radio astronomical observations in the millimeter bandwidth.

Astronomische Nachrichten

Proceedings of RFI mitigation workshop — PoS(RFI2010)

During several recent years the interference situation at RATAN-600 deteriorated sharply. The ana... more During several recent years the interference situation at RATAN-600 deteriorated sharply. The analysis of electromagnetic interference at the RATAN-600 radio telescope is presented. The practical experience of radio frequency interference mitigation is discussed.

Proceedings of RFI mitigation workshop — PoS(RFI2010)

The "Octave" project seeks to modernize the RATAN-600 continuum radiometers. The implementation o... more The "Octave" project seeks to modernize the RATAN-600 continuum radiometers. The implementation of the first stage was started for the 13, 31 and 49 cm wavelength of the decimeter range. The second stage concentrates on the rest of the centimeter range. Using the method presented in this report, it is possible to produce radiometers hat have the ability to react quickly to the changing interference environment (and to retune the receivers to an adjacent band).

International Astronomical Union Colloquium, 1998

The preliminary results of monitoring of simultaneous spectra of a sample of extragalactic source... more The preliminary results of monitoring of simultaneous spectra of a sample of extragalactic sources are given. Eight sets of observations were done at the RATAN-600 radio telescope in 1995-1996 at six frequencies (0.96, 2.3, 3.9, 7.7, 11.2, and 22 GHz). The light curves as well as the variability parameters are given

Astrophysical Bulletin, 2015

During thirteen-year monitoring of the source J0010+1058, four bursts have been observed with an ... more During thirteen-year monitoring of the source J0010+1058, four bursts have been observed with an amplitude greater than 1 Jy on a frequency of 21.7 GHz. Using autocorrelation functions, we determined the average characteristic burst time τ acf ≈ 1.55 ± 0.1 yr (max-min), identical at five frequencies: 2.3, 4.8, 7.7, 11.2, and 21.7 GHz, which provides the linear sizes of the emission region R ≈ c τ acf ≈ 0.48 pc, and the angular ones-0.28 mas; the brightness temperature is 0.6-6.5 × 10 11 K at the frequencies 21.7-2.3 GHz. Moreover, at frequencies higher than 2.3 GHz, there is one more characteristic time τ ≈ 0.6 yr. We estimated the average lag time of the bursts in relation to a frequency of 21.7 GHz as 150, 210, 270, and 390 days at 11.2, 7.7, 4.8, and 2.3 GHz respectively, and some other source characteristics. Spectra obtained in different periods of source activity confirm the model of the burst development as a result of the evolution of a shock wave propagating along the radio source jet.

Astronomy Reports, 2000

Simultaneous observations on the RATAN-600 radio telescope at 0.97, 2.3, 3.9, 7.7, 11.1, and 21.7... more Simultaneous observations on the RATAN-600 radio telescope at 0.97, 2.3, 3.9, 7.7, 11.1, and 21.7 GHz during the period from January 3 to February 25, 1998, revealed variability of 0524 + 034 on time scales not exceeding 10 days. The variations are correlated at all frequencies where the parameters of the variability could be determined, including in the optically thick part of the spectrum. The mean spectrum of the variable component was derived and is in agreement with the spectrum of a homogeneous, spherically symmetrical source. In the optically thin part of the spectrum, the spectral index of the variable component is α =-0.2, reflecting the initial energy distribution of the relativistic electrons. It is argued that the variable emission is associated with the acceleration of electrons and amplification of the magnetic field and that adiabatic expansion can be neglected. It is proposed that the observed variability is due to illumination of inhomogeneities in the jet by a shock front passing through them and that the light curve reflects the distribution and characteristic sizes of these inhomogeneities (0.14-0.5 pc for angles to the line of sight not exceeding 10° , Lorentz factor γ = 10, and adopted redshift z = 0.5). In 0524 + 034, in addition to the rapidly variable component, there are two slowly varying components, one of which has α =-0.7 in the optically thin part of the spectrum.

Astronomy & Astrophysics, 2011

Radiophysics and Quantum Electronics, 2007

We develop a high-sensitivity matrix radiometer which will be used on the large altazimuth telesc... more We develop a high-sensitivity matrix radiometer which will be used on the large altazimuth telescope BTA of the Special Astrophysical Observatory (SAO) of the Russian Academy of Sciences ( for performing astronomical observations in atmospheric transparency windows in the poorly explored frequency range from 0.13 to 0.38 THz (wavelengths from 2.3 to 0.8 mm). Mounting of the radiometer at the focal point of the 6-m BTA telescope will enhance the capability of the SAO in the transparency windows of the Earth's atmosphere from the UV range (wavelengths about 3000Å) up to the ultimate wavelength of the RATAN-600 telescope (about 0.5 m). This will make it possible to perform unique comprehensive multifrequency studies in one observatory. The radiometer is presumed to be used with other radio and optical telescopes, both in the above-mentioned and higher-frequency intervals of the terahertz range.

Millimeter and Submillimeter Detectors and Instrumentation for Astronomy IV, 2008

We describe design of two-polarization imaging array of 7 antenna-coupled TES-bolometers. The fab... more We describe design of two-polarization imaging array of 7 antenna-coupled TES-bolometers. The fabrication procedure involves both electron beam lithography and convenient optical lithography resulting in submicron definition of TES absorber films (down to ~ 0.2 µm) integrated within planar submm-wave antenna. Concept of matching optics between the long-focus optical telescope and lens-antenna TES bolometer array is described. Two-mirror short-focusing beam concentrator in combination with image rotator provides signal coupling to immersion lenses of the array. Each TES bolometer is coupled via microstrip transmission line to only one polarization of two-polarization crossed double-slot lens-antenna. Design of cryogenic 0.3-K system accommodating the matching optics is presented. We describe multiplexing readout scheme, which combines tomography, rotational scanning of the image and frequency domain division methods that drastically reduce the amount of wiring and substantially increase the final image resolution, especially for low-dimension arrays.

Symposium - International Astronomical Union, 2001

Astrophysical Bulletin, 2013

Radiophysics and Quantum Electronics, 2004

This paper is devoted to the development of capabilities of the RATAN-600 radio telescope by putt... more This paper is devoted to the development of capabilities of the RATAN-600 radio telescope by putting the regime of multi-azimuth observations at the southern sector with periscope reflector into regular operation. This method makes it possible to study the dynamics of variable radio sources on temporal scales down to a few minutes and increase by one order of magnitude the number of variable sources observed during sky surveys. To date, over ten series of observations of the Sun were performed in the new regime using the multi-wavelength receiver complex, and new astrophysical results were obtained. The software for multi-wavelength mapping of the Sun and wavelet analysis of time series is developed. The following characteristics of the regime are achieved: a temporal resolution of 4 min during a time interval of up to 4.5 h for observations at azimuth angles in the interval from 30 • to −30

Astrophysical Bulletin, 2015

Astrophysical Bulletin, 2015

We study the synchrotron component of the spectral energy distribution (SED) on the sample of 877... more We study the synchrotron component of the spectral energy distribution (SED) on the sample of 877 blazars using the ASDC SED Builder Tool with available broadband data from the literature. Our sample includes 423 flat-spectrum radio sources (FSRQs), 361 BL Lac objects and candidates, and 93 blazars of uncertain type. We have made an estimation of the synchrotron peak frequency (ν s peak) for the 875 objects and further classified them as high, intermediate and low synchrotron peaked sources (HSPs/ISPs/LSPs). There are 42 HSPs with ν s peak > 10 16.5 Hz, 222 ISPs with 10 14.5 < ν s peak < 10 16.5 Hz, and 611 LSPs with ν s peak < 10 14.5 Hz in our sample. We have calculated an average value of ν s peak to be 10 13.4±1.0 Hz for FSRQs and 10 14.6±1.4 Hz for BL Lacs. We found out that ν s peak and the flux density at 4.8 GHz have a different distribution (as indicated by Kolmogorov-Smirnov test at significance level 0.05) for the FSRQ and BL Lac blazars, and for the RBL and XBL types of BL Lacs. Distribution of ν s peak values is broader for BL Lacs, than for FSRQs. There are no ultra-high energy peaked objects (with ν s peak > 10 19 Hz) in our BL Lac sample according to our estimations. The significant part of FSRQs (41%) and small part of BL Lacs (9%) in our sample could be considered as candidates to the very-low synchrotron peaked blazars (with ν s peak < 10 13 Hz). Our foundations confirm results of the previous studies made on samples with significantly smaller number of objects.

Monthly Notices of the Royal Astronomical Society, 2015

We study the correlation between gamma-ray and radio band radiation for 123 blazars, using the Fe... more We study the correlation between gamma-ray and radio band radiation for 123 blazars, using the Fermi-LAT first source catalog (1FGL) and the RATAN-600 data obtained at the same period of time (within a few months). We found an apparent positive correlation for BL Lac and flat-spectrum radio quasar (FSRQ) sources from our sample through testing the value of the Pearson product-moment correlation coefficient. The BL Lac objects show higher values of the correlation coefficient than FSRQs at all frequencies, except 21.7 GHz, and at all bands, except 10 − 100 GeV, typically at high confidence level (> 99 %). At higher gammaray energies the correlation weakens and even becomes negative for BL Lacs and FSRQs. For BL Lac blazars, the correlation of the fluxes appeared to be more sensitive to the considered gamma-ray energy band, than to the frequency, while for FSRQ sources the correlation changed notably both with the considered radio frequency and gamma-ray energy band. We used a data randomization method to quantify the significance of the computed correlation coefficients. We find that the statistical significance of the correlations we obtained between the flux densities at all frequencies and the photon flux in all gamma-ray bands below 3 GeV is high for BL Lacs (chance probability ∼ 10 −3 − 10 −7). The correlation coefficient is high and significant for the 0.1 − 0.3 GeV band and low and insignificant for the 10 − 100 GeV band for both types of blazars for all considered frequencies.

Astronomy Reports, 1999

Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are prese... more Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7, 3.9, 7.6, 13,

Simultaneous multifrequency radio spectra have been obtained for the source 3C 84 (the Seyfert ga... more Simultaneous multifrequency radio spectra have been obtained for the source 3C 84 (the Seyfert galaxy NGC 1275) with the RATAN-600 radio telescope at two epochs, 1979.5 and 1980.0. The energy of the particles and field is confirmed to be growing at a rate of about 15% annually.

Astronomy Letters, 2016

The results of observations of the quasar J0530+1331 (B0528+134) with the radio telescopes RATAN-... more The results of observations of the quasar J0530+1331 (B0528+134) with the radio telescopes RATAN-600 at frequencies of 4.6, 8.2, 11.2, 21.7 GHz and RT-32 at the Zelenchukskaya and Badary observatories of the Quasar network of the Institute of Applied Astronomy, the Russian Academy of Sciences, at frequencies of 4.84 and 8.57 GHz in 2014–2015 are presented. A strong variability on a timescale of 20 days at 4.6–11.2 GHz has been detected over three months of daily RATAN-600 observations; the variability indices are V = dS/〈S〉; = 0.65−0.39. The spectrum of the variable component is falling toward high frequencies with an index α = −0.76. The structure and autocorrelation functions at 4.6 GHz show an additional process on a timescale of 7 days. No delay of the main process has been detected between 11.2 and 8.2 GHz; the delay between 8.2 and 4.6 GHz does not exceed two days. The most likely cause of the observed variability is the scattering by inhomogeneities of the interstellar medium. The variability has been obtained at theminimum activity phase of the source. The intraday variability (IDV) has been searched for at both RT-32 telescopes since April 2014. Out of 38 successful observing sessions for the source, only three have shown a variability on a timescale of four hours or more at a significance level no higher than 0.1%. This confirms our conclusion drawn from the previous IDV measurements for other sources that the IDV is observed mainly at the maximum phases of long-term variability of the sources.

PROCEEDINGS OF SPIE, 2020

We are presenting the results of astroclimatic studies in the North Caucasus started on our Febru... more We are presenting the results of astroclimatic studies in the North Caucasus started on our February 2020 expedition. The main objective of the studies is to compare millimeter-wave optical depth characteristics of four North Caucasus sites: BTA-6, RATAN-600, CMO of GAISh, and the Terskol Observatory. The opacity was studied by the atmospheric dip method in the 3 mm and 2 mm atmospheric windows. The astroclimate conditions of these four sites are compared through statistically processed data. This astroclimatic analysis has been performed with the view to selecting a site for radio astronomical observations in the millimeter bandwidth.

Astronomische Nachrichten

Proceedings of RFI mitigation workshop — PoS(RFI2010)

During several recent years the interference situation at RATAN-600 deteriorated sharply. The ana... more During several recent years the interference situation at RATAN-600 deteriorated sharply. The analysis of electromagnetic interference at the RATAN-600 radio telescope is presented. The practical experience of radio frequency interference mitigation is discussed.

Proceedings of RFI mitigation workshop — PoS(RFI2010)

The "Octave" project seeks to modernize the RATAN-600 continuum radiometers. The implementation o... more The "Octave" project seeks to modernize the RATAN-600 continuum radiometers. The implementation of the first stage was started for the 13, 31 and 49 cm wavelength of the decimeter range. The second stage concentrates on the rest of the centimeter range. Using the method presented in this report, it is possible to produce radiometers hat have the ability to react quickly to the changing interference environment (and to retune the receivers to an adjacent band).

International Astronomical Union Colloquium, 1998

The preliminary results of monitoring of simultaneous spectra of a sample of extragalactic source... more The preliminary results of monitoring of simultaneous spectra of a sample of extragalactic sources are given. Eight sets of observations were done at the RATAN-600 radio telescope in 1995-1996 at six frequencies (0.96, 2.3, 3.9, 7.7, 11.2, and 22 GHz). The light curves as well as the variability parameters are given

Astrophysical Bulletin, 2015

During thirteen-year monitoring of the source J0010+1058, four bursts have been observed with an ... more During thirteen-year monitoring of the source J0010+1058, four bursts have been observed with an amplitude greater than 1 Jy on a frequency of 21.7 GHz. Using autocorrelation functions, we determined the average characteristic burst time τ acf ≈ 1.55 ± 0.1 yr (max-min), identical at five frequencies: 2.3, 4.8, 7.7, 11.2, and 21.7 GHz, which provides the linear sizes of the emission region R ≈ c τ acf ≈ 0.48 pc, and the angular ones-0.28 mas; the brightness temperature is 0.6-6.5 × 10 11 K at the frequencies 21.7-2.3 GHz. Moreover, at frequencies higher than 2.3 GHz, there is one more characteristic time τ ≈ 0.6 yr. We estimated the average lag time of the bursts in relation to a frequency of 21.7 GHz as 150, 210, 270, and 390 days at 11.2, 7.7, 4.8, and 2.3 GHz respectively, and some other source characteristics. Spectra obtained in different periods of source activity confirm the model of the burst development as a result of the evolution of a shock wave propagating along the radio source jet.

Astronomy Reports, 2000

Simultaneous observations on the RATAN-600 radio telescope at 0.97, 2.3, 3.9, 7.7, 11.1, and 21.7... more Simultaneous observations on the RATAN-600 radio telescope at 0.97, 2.3, 3.9, 7.7, 11.1, and 21.7 GHz during the period from January 3 to February 25, 1998, revealed variability of 0524 + 034 on time scales not exceeding 10 days. The variations are correlated at all frequencies where the parameters of the variability could be determined, including in the optically thick part of the spectrum. The mean spectrum of the variable component was derived and is in agreement with the spectrum of a homogeneous, spherically symmetrical source. In the optically thin part of the spectrum, the spectral index of the variable component is α =-0.2, reflecting the initial energy distribution of the relativistic electrons. It is argued that the variable emission is associated with the acceleration of electrons and amplification of the magnetic field and that adiabatic expansion can be neglected. It is proposed that the observed variability is due to illumination of inhomogeneities in the jet by a shock front passing through them and that the light curve reflects the distribution and characteristic sizes of these inhomogeneities (0.14-0.5 pc for angles to the line of sight not exceeding 10° , Lorentz factor γ = 10, and adopted redshift z = 0.5). In 0524 + 034, in addition to the rapidly variable component, there are two slowly varying components, one of which has α =-0.7 in the optically thin part of the spectrum.

Astronomy & Astrophysics, 2011

Radiophysics and Quantum Electronics, 2007

We develop a high-sensitivity matrix radiometer which will be used on the large altazimuth telesc... more We develop a high-sensitivity matrix radiometer which will be used on the large altazimuth telescope BTA of the Special Astrophysical Observatory (SAO) of the Russian Academy of Sciences ( for performing astronomical observations in atmospheric transparency windows in the poorly explored frequency range from 0.13 to 0.38 THz (wavelengths from 2.3 to 0.8 mm). Mounting of the radiometer at the focal point of the 6-m BTA telescope will enhance the capability of the SAO in the transparency windows of the Earth's atmosphere from the UV range (wavelengths about 3000Å) up to the ultimate wavelength of the RATAN-600 telescope (about 0.5 m). This will make it possible to perform unique comprehensive multifrequency studies in one observatory. The radiometer is presumed to be used with other radio and optical telescopes, both in the above-mentioned and higher-frequency intervals of the terahertz range.

Millimeter and Submillimeter Detectors and Instrumentation for Astronomy IV, 2008

We describe design of two-polarization imaging array of 7 antenna-coupled TES-bolometers. The fab... more We describe design of two-polarization imaging array of 7 antenna-coupled TES-bolometers. The fabrication procedure involves both electron beam lithography and convenient optical lithography resulting in submicron definition of TES absorber films (down to ~ 0.2 µm) integrated within planar submm-wave antenna. Concept of matching optics between the long-focus optical telescope and lens-antenna TES bolometer array is described. Two-mirror short-focusing beam concentrator in combination with image rotator provides signal coupling to immersion lenses of the array. Each TES bolometer is coupled via microstrip transmission line to only one polarization of two-polarization crossed double-slot lens-antenna. Design of cryogenic 0.3-K system accommodating the matching optics is presented. We describe multiplexing readout scheme, which combines tomography, rotational scanning of the image and frequency domain division methods that drastically reduce the amount of wiring and substantially increase the final image resolution, especially for low-dimension arrays.

Symposium - International Astronomical Union, 2001

Astrophysical Bulletin, 2013

Radiophysics and Quantum Electronics, 2004

This paper is devoted to the development of capabilities of the RATAN-600 radio telescope by putt... more This paper is devoted to the development of capabilities of the RATAN-600 radio telescope by putting the regime of multi-azimuth observations at the southern sector with periscope reflector into regular operation. This method makes it possible to study the dynamics of variable radio sources on temporal scales down to a few minutes and increase by one order of magnitude the number of variable sources observed during sky surveys. To date, over ten series of observations of the Sun were performed in the new regime using the multi-wavelength receiver complex, and new astrophysical results were obtained. The software for multi-wavelength mapping of the Sun and wavelet analysis of time series is developed. The following characteristics of the regime are achieved: a temporal resolution of 4 min during a time interval of up to 4.5 h for observations at azimuth angles in the interval from 30 • to −30