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RATAN-600

The RATAN-600 is a large radio telescope located at the Special Astrophysical Observatory in Zelenchukskaya, Karachay-Cherkess Republic, Russia, consisting of a 576-meter-diameter ring composed of 895 adjustable rectangular reflector panels that focus radio waves onto central subreflectors for high-sensitivity observations across a wide range of frequencies.^[1]^[2] Designed as a variable-profile antenna, it operates primarily in drift-scan mode to monitor celestial sources as they pass overhead, enabling detailed studies of variable radio emissions from objects like quasars, blazars, and the Sun.^[3]^[2] Construction of the RATAN-600 began in 1968 as part of a major Soviet astronomical initiative, alongside the 6-meter BTA optical telescope, with the north sector becoming operational in 1974—marking its first light on the quasar PKS 0521-36—and the full instrument officially opened in 1977.^[1]^[4] The telescope's innovative design features no structural links between its reflector elements, allowing for flexible reconfiguration into up to three independent subrings, each with its own subreflector on rails, to optimize for different observational needs.^[1]^[2] It covers wavelengths from 90 cm down to 0.8 cm (frequencies of 0.3 to 37.5 GHz), with a surface accuracy of approximately 0.3 mm and an angular resolution of about 1 arcminute in the horizontal plane, providing an effective collecting area of around 1,000 m² at 8 cm wavelength.^[1]^[3] Among its notable contributions, the RATAN-600 has conducted daily multi-frequency scans of solar radio emissions, compiled a catalog of over 1,700 blazars with flux densities at multiple bands,^[5] and contributed to searches for fast radio bursts, advancing research on transient astrophysical phenomena.^[3]^[6] It remains the largest radio telescope in Russia and continues active operations, including multifrequency monitoring of active galactic nuclei and galactic sources, underscoring its role in radio astronomy despite challenges like funding constraints in recent decades.^[1]^[7]

History and Development

Conception and Construction

The conceptual development of RATAN-600 originated in the early 1960s within Soviet radio astronomy circles, evolving as a short-wavelength adaptation of variable-profile antennas (VPA) pioneered at Pulkovo Observatory by S.E. Khaikin and N.L. Kaidanovskii, integrated with Kraus-type multi-element systems from the Shternberg Astronomical Institute.^[1] This hybrid approach addressed limitations in existing designs by enabling a large-scale, adjustable reflector for enhanced sensitivity at shorter wavelengths.^[8] By 1965, following deliberations by the Radio Astronomy Committee, the RATAN-600 project was prioritized over competing proposals like fixed paraboloids or arrays, marking it as an innovative step toward the world's first multi-element-reflector telescope without interconnecting structures.^[1] The technical plan received formal approval from Soviet authorities in 1967, greenlighting construction under the auspices of the newly established Special Astrophysical Observatory (SAO) of the Russian Academy of Sciences (RAS).^[1] Leadership fell to SAO, with significant contributions from engineers V.A. Korolkov, who advanced solar observation applications, and Yu.N. Pariiskii, who played a central role in overall project coordination and later scientific utilization.^[8] Pulkovo's radio astronomy team, transferred to SAO's Leningrad Branch in 1969, provided essential expertise during the build phase.^[1] Construction commenced with excavation and earth-moving in 1968 at the selected site in the North Caucasus mountains, a challenging endeavor due to the rugged terrain requiring extensive groundwork for stability.^[1] Reflector installation, involving the precise assembly of 895 independent elements without rigid linking frameworks, progressed through the 1970s amid logistical hurdles in material handling and alignment.^[9] The northern sector achieved first light on July 12, 1974, enabling initial observations, while full operational capability was realized in 1977 following completion of the entire ring structure.^[10]

Site Selection and Location

The RATAN-600 radio telescope is situated in Zelenchukskaya village, within the Karachay–Cherkess Republic, Russia, at coordinates 43°49′33″N 41°35′11″E and an elevation of 970 meters above sea level.^[11] This location places it in the North Caucasus mountains, approximately 20 kilometers northwest of the Special Astrophysical Observatory's (SAO) primary facilities.^[1] The site was chosen in 1967 based on several key criteria essential for radio astronomy operations, including low levels of radio frequency interference (RFI), stable weather patterns, and favorable terrain that supports large-scale installations.^[1]^[12] The remote mountainous setting in the North Caucasus was selected to minimize human-generated noise, as the area's isolation from urban centers and industrial activities provides a naturally radio-quiet environment.^[12] Additionally, the site's proximity to SAO's existing infrastructure facilitated logistical and operational integration.^[1] Environmental advantages of the location include the high altitude, which reduces atmospheric absorption and water vapor effects on radio signals, enhancing observational sensitivity at centimeter and millimeter wavelengths.^[11] The region's stable soil composition also ensures structural reliability for the telescope's expansive ring design.^[1] Zelenchukskaya, a traditional Cossack settlement, contributes to the area's low population density and reduced anthropogenic interference.^[13] Access to the site is provided by regional roads, positioning it about 1,800 kilometers southeast of Moscow, while its co-location with other SAO instruments, such as the BTA-6 optical telescope, enables coordinated multi-wavelength observations.^[1] Construction at this selected site commenced in 1968.^[1]

Design and Technical Specifications

Antenna Structure

The RATAN-600 features a large circular ring reflector with a diameter of 576 meters, nominally referred to as 600 meters, forming the primary antenna structure.^[14] This ring is composed of 895 independent rectangular reflector elements, each measuring 2 meters by 11.4 meters.^[15] The elements are arranged in a continuous circle without any structural links between them, which allows for a variable profile and enhances flexibility in shaping the reflector surface.^[9] Each reflector element is tiltable via motorized adjustments to achieve precise focusing and profile shaping for different observational requirements.^[15] The geometrical area of the full ring is approximately 20,000 square meters.^[16] The structure is divided into four independent sectors—North, South, East, and West—each comprising 225 elements, enabling partial use of the antenna for targeted configurations.^[14] The reflector panels are constructed from aluminum to ensure high reflectivity in the radio spectrum. Secondary reflectors are housed in four movable feed cabins positioned on a central rail system inside the ring, allowing them to be adjusted along the 576-meter circumference to direct the beam toward specific sky positions.^[14] Each cabin contains secondary mirrors designed to intercept and redirect signals from the primary ring to the receivers.^[14] A key innovation of the RATAN-600 is its design as the first radio telescope to employ multi-element reflectors without a central supporting structure, which facilitates the achievement of such a large scale while maintaining operational flexibility.^[9] This construction was completed in 1977.^[17]

Optical and Performance Specifications

The RATAN-600 radio telescope operates across a broad frequency range of 610 MHz to 30 GHz, corresponding to wavelengths from 49 cm to 1 cm, enabling detailed observations of radio emissions from solar, galactic, and extragalactic sources.^[15] The telescope's angular resolving power is approximately 1 arcminute at an 8 cm wavelength (3.75 GHz), providing sufficient detail for mapping extended structures like solar corona features or galactic filaments.^[18] At shorter wavelengths, the resolution improves significantly, reaching up to 2 arcseconds under optimal configurations, with the beam width varying based on the number of reflector elements illuminated and the observing elevation—typically around 40 arcseconds at average elevations for standard operations.^[15]^[16] This performance arises from the effective aperture synthesis of the ring structure, though it is constrained by the transit geometry. The reflector surface accuracy is approximately 0.3 mm.^[1] Sensitivity is enhanced by an effective area of up to 3,500 m² for the full ring or 700–1,500 m² for individual sectors, depending on wavelength and configuration, such as around 1,000 m² at 8 cm in sector mode, which supports detection of faint flux densities down to 0.5 mJy for continuum sources.^[15]^[1] The system noise temperature depends on frequency and receiver type, generally lower at centimeter wavelengths (e.g., around 80–100 K at 1–22 GHz), contributing to high brightness-temperature sensitivity on the order of 0.05 mK for absolute measurements.^[19]^[20] Gain varies with configuration but benefits from the large collecting area, enabling efficient spectral flux density measurements across multiple channels simultaneously. Pointing accuracy is maintained at 1–10 arcseconds, optimized for zenith-pointing in full-ring mode to maximize the illuminated aperture and minimize distortions from off-meridian observations.^[15] The telescope's fixed meridian orientation limits it to transit observations along the celestial meridian, though this is mitigated by the site's elevation of 970 m above sea level at Zelenchukskaya, which reduces atmospheric absorption and phase instabilities, particularly at higher frequencies.^[16]

Operating Modes and Capabilities

Transit Telescope Operations

The RATAN-600 operates primarily as a transit telescope, leveraging Earth's rotation to scan the sky across its fixed meridian focus without requiring alt-azimuth tracking mechanisms. In this mode, radio sources crossing the zenith are observed as they drift through the telescope's beam, enabling efficient monitoring of celestial objects along the meridian plane. The antenna's 576-meter diameter ring reflector consists of 895 adjustable rectangular elements that are tilted to form a cylindrical parabolic profile in the radial direction, concentrating signals toward a linear focal line at the center. A movable secondary mirror, shaped as a parabolic cylinder with its generatrix parallel to the horizon, is positioned at this focus to redirect and collimate the incoming waves into receiver feeds located in one of several feed cabins along a central rail.^[14]^[21] Multi-channel receivers allow simultaneous observations across a broad frequency range from 610 MHz to 30 GHz, with typical setups using bands such as 1.2, 2.3, 4.7, 8.2, 11.2, and 22.3 GHz for quasi-simultaneous spectral measurements. The observation procedure involves drift scans where data are recorded continuously as sources transit the beam, typically lasting 1 to 5 minutes per pass depending on the source's declination and the selected sector (north or south, each comprising about 225 elements). Automated systems, including the FADPS data processing software, handle real-time calibration, flux density extraction, and polarization analysis during these scans, often employing a sliding regime with integration times of 60 to 100 seconds for enhanced signal-to-noise ratios.^[22]^[23]^[14] This transit configuration provides high sensitivity to flux variations and brightness temperatures, making it ideal for long-term monitoring programs such as solar transits and variable source catalogs, and it accounts for the majority of the telescope's operational time since its commissioning in 1974. The method's efficiency stems from the fixed beam pattern, which simplifies mechanical demands and supports rapid multi-frequency data acquisition without repositioning the main reflector. Representative resolving power in the meridian plane reaches approximately 40 arcseconds.^[16]^[22]

Multi-Mirror Configurations

The RATAN-600 radio telescope employs multi-mirror configurations to enable non-transit observations, allowing for off-meridian pointing and source tracking beyond the limitations of Earth's rotation. In the two-mirror mode, a single perimeter sector of the ring reflector, typically comprising 225 elements, is paired with one secondary mirror to focus incoming radiation onto receivers. This setup facilitates basic off-zenith pointing with azimuthal coverage of approximately ±15°, enabling observations of sources at fixed elevations while the secondary mirror adjusts position along an arc-shaped track. The configuration achieves an effective area of around 1000 m² at centimeter wavelengths, with beam patterns exhibiting a knife-edge profile and sidelobe levels suppressed through precise reflector profiling to minimize diffraction effects.^[1]^[16]^[24] The three-mirror mode extends flexibility by combining a perimeter sector with two secondary mirrors, including a flat periscope reflector (Kraus-type) to redirect radiation from off-axis directions. This arrangement provides wider azimuthal coverage of ±30°, permitting continuous tracking of cosmic sources at arbitrary angles over intervals of 3-4 hours with up to 15 positional settings. The triple-reflector system, utilizing a parabolic or circular main mirror with a focal length of 131.8 m, supports multi-beam operations where feeds are positioned along the focal line, enhancing sensitivity for continuum and spectral observations. Beam patterns in this mode are computed using multilevel physical optics algorithms, revealing power distributions that account for diffraction and achieve sidelobe suppression via optimized mirror curvatures.^[24]^[1]^[25] For zenith-only high-sensitivity observations, the full-ring mode activates the entire 576 m diameter ring with all 895 reflector elements and a conical secondary mirror positioned near the zenith. This configuration maximizes the collecting area to 22,000 m², yielding angular resolutions of approximately 40 arcseconds and enabling simultaneous multi-frequency monitoring across bands from 0.6 to 30 GHz. It is restricted to declinations between 38° and 49° (zenith distance ±6°), ideal for detailed studies of bright sources passing overhead. Post-2010 upgrades have integrated focal phased arrays into these modes, supporting multibeam reception with up to 100 channels for improved field-of-view coverage. As of 2024, further enhancements include automation for improved tracking modes, new low-noise radiometric modules, cryogenic systems, and data processing pipelines like RatanSunPy, expanding capabilities for solar and transient observations.^[16]^[26]^[22]^[27]^[28]^[29] Recent enhancements include the West Sector mode, introduced in 2017, which utilizes a dedicated 225-element sector for drift scans of point sources with a static antenna configuration. This mode employs a large secondary mirror and asymmetric primary radiation patterns, allowing blind surveys at 4.7 GHz with effective areas of 1200 m² and beam patterns calculated to optimize flux density measurements outside the central cross-section. Sidelobe suppression in sector-based operations, such as the West Sector, relies on reflector element profiling to reduce interference, with experimental validations confirming accuracy in source positioning to 3-10". These configurations collectively expand the telescope's capabilities for targeted, non-transit sky coverage.^[30]^[14]^[31]

Scientific Applications and Discoveries

Solar and Heliospheric Studies

Since its operational inception in 1974, the RATAN-600 radio telescope has played a primary role in dedicated solar observations, particularly probing the corona and chromosphere at centimeter wavelengths (roughly 1-20 cm) to investigate plasma dynamics and magnetic structures.^[32] These observations leverage the telescope's high angular resolution, up to 15-30 arcseconds, to map thermal and non-thermal emissions from solar active regions, revealing flux variations associated with evolving sunspots and magnetic loops.^[33] For instance, studies have quantified brightness temperature fluctuations in active regions, linking them to underlying magnetic field strengths of 40-200 Gauss derived from polarization measurements.^[33] Key investigations using RATAN-600 have focused on coronal mass ejections (CMEs) and associated radio bursts, capturing their microwave signatures during solar cycles, including the 23rd and 24th.^[34] Observations of type III and microflares have documented impulsive energy releases, with radio flux enhancements correlating to particle acceleration in the low corona.^[35] In preparation for the 24th solar cycle, 2011 upgrades introduced the Spectral and Polarization High-Resolution Solar Research System (SPHRS), featuring multi-octave analyzers and new receivers for enhanced burst detection sensitivity across 1-18 GHz, enabling regular multi-frequency monitoring of dynamic events.^[36] These modifications improved spectral resolution to 1-2% and polarization accuracy, facilitating precise tracking of radio burst evolution.^[37] Data acquisition relies on multi-frequency drift scans conducted daily at approximately 50 frequencies in the 3-17 GHz range, providing one-dimensional scans of solar emission with temporal resolution of seconds.^[38] This transit mode is particularly suited for continuous solar monitoring, integrating RATAN-600 data into networks like those involving SPOT and STOP for coordinated space weather forecasting.^[39] Notable outcomes include high-resolution maps of solar radio emission, such as those from joint VLA-RATAN observations, which reveal inhomogeneous coronal plasma distributions above active regions.^[40] Furthermore, these maps have established strong correlations between microwave fluxes and X-ray flares, with radio peaks often preceding or coinciding with GOES soft X-ray enhancements during eruptive events.^[41] Observations have continued into the 25th solar cycle (as of 2025), with over 30,000 archived scans analyzed using tools like RatanSunPy for enhanced preprocessing.^[42]

Extragalactic Radio Astronomy and SETI

The RATAN-600 telescope has significantly contributed to extragalactic radio astronomy through its high-sensitivity, multi-frequency monitoring capabilities, particularly for active galactic nuclei (AGN) such as blazars and BL Lacertae objects. Operating at frequencies from 1 to 22 GHz, it enables quasi-simultaneous spectral observations that reveal variability in radio flux densities, aiding in the study of jet physics and emission mechanisms in these distant sources. For instance, the telescope's long-term monitoring program has compiled multi-frequency data for over 300 BL Lac objects between 2006 and 2014, expanding the sample size by more than threefold and facilitating analyses of spectral indices and flux variability patterns.^[43] Key discoveries include detailed flux measurements of extended components in giant radio galaxies, where RATAN-600 observations at centimeter wavelengths have helped characterize their large-scale structures and emission properties. In one study, flux densities were measured for thirteen such galaxies, providing insights into their morphological and energetic evolution across cosmic distances.^[44] Additionally, the telescope has played a pivotal role in investigating neutrino-associated blazars, such as TXS 0506+056 linked to the IceCube-170922A event; 72 instantaneous spectra from 1–22 GHz over 20 years, combined with space-based data from RadioAstron, revealed synchrotron self-absorption and jet variability consistent with high-energy particle acceleration.^[45] RATAN-600's broadband monitoring has also cataloged over 1,600 blazars, supporting investigations into correlations between radio and gamma-ray emissions, as well as fast radio burst (FRB) searches using neural network algorithms on archival data.^[3]^[46] Recent monitoring (as of 2025) includes detection of a giant flare from microquasar Cygnus X-3 in March 2024 and a blazar PMN J0606-0724 flare in March 2025.^[47]^[48] These efforts emphasize the telescope's strength in detecting transient phenomena and establishing radio properties of high-redshift quasars (z > 3), contributing to broader understandings of supermassive black hole feedback and cosmic evolution. In the realm of the Search for Extraterrestrial Intelligence (SETI), RATAN-600 has conducted targeted radio observations since the early 2010s, leveraging its large collecting area—thousands of square meters—for high-sensitivity searches at 2.7 cm and 6.3 cm wavelengths. Between 2015 and 2016, the telescope monitored approximately 30 Sun-like stars and two metal-rich globular clusters (47 Tucanae and M13) for artificial signals, using methods such as single-signal detection, temporal flux averaging, and frequency correlation analysis. No stationary or flare-like emissions indicative of extraterrestrial technology were detected, setting power limits of 10¹⁶–10²⁰ W for averaged signals and 10¹⁷–10²¹ W for single observations, with effective isotropic radiated power constraints below 2 × 10⁹–2 × 10¹³ W.^[49]^[50] A notable event occurred on May 15, 2015, when RATAN-600 detected a transient ~750 mJy signal at 11.1 GHz from the direction of HD 164595, a G2V star 28.9 parsecs away hosting a Neptune-mass planet. This narrowband signal, with a signal-to-noise ratio suggesting potential technosignature origin, prompted international follow-up, including observations by the Green Bank Telescope under the Breakthrough Listen initiative. Subsequent analyses, however, attributed the detection to likely radio frequency interference or an instrumental artifact, as no corroborating emission was found, and the transient's characteristics mismatched expected astrophysical rates. These SETI efforts underscore RATAN-600's utility in generating candidate lists for periodic monitoring while establishing stringent limits on nearby extraterrestrial transmitters.^[51]

References

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Cold: The RATAN-600 Radio Telescope
This radio telescope was a short-wavelength version of a VPA combined with a Kraus-type system and was named the RATAN-600. At the same time, a committee was ...
[2]
Bill Keel's Telescope Tourism - RATAN-600
This radio telescope takes the form of a 600-meter ring of adjustable reflecting panels, which can be angled to direct the radiation from a point in the sky to ...
[3]
RATAN-600 is a radio telescope with a variable-profile circular ...
RATAN-600 is a radio telescope with a variable-profile circular antenna of 600 m in diameter, the largest Russian telescope.
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Antenna RATAN-600 and techniques of observations
BTA and RATAN-600 are largest optical and radio telescopes in Russia. RATAN has seen 'first light' from source PKS 0521-36 12 July 1974 .Missing: date | Show results with:date
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https://rat.sao.ru/en/scientific-results/the-ratan-600-multi-frequency-catalogue-of-blazars-blcat/
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[PDF] RATAN-600: past, present, future - Yu. N. Parijskij
1976 completion of construction of the. RATAN-600. It will not be too overstated to say that without advances in Pulkovo, without actual astrophysical re- sults ...
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RATAN-600 - The world's biggest reflector at the 'cross roads'
The RATAN-600 is the first multielement reflector radio telescope without any structure linking the surface elements.
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RATAN-600 - 45 years of the first observation
Jul 25, 2019 · The first observations at RATAN-600 were on July 12, 1974. The first years included research on the Sun, planets, and lunar soil.Missing: timeline light
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[PDF] Technical and operational characteristics of radio astronomy ... - ITU
As illustrated in Fig. 1, the atmospheric attenuation at the geographic locations selected as sites of millimetre and sub-millimetre radio telescopes is ...
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[PDF] Selection of radio astronomical observation sites and its ...
Russia, Ratan-600. 600. 18. Russia, RT-7.5. 7.5. 155. United States, GBT. 100. 17 ... site selection criteria (Abidin et al. 2013). 2 METHODOLOGY. There are ...
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Jul 29, 2015 · The RATAN-600 is the world's first multi-element-reflector radio telescope without any structure linking the surface elements.
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BTA and RATAN-600 are largest optical and radio telescopes in Russia. RATAN has seen 'first light' from source PKS 0521-36 12 July 1974 . Since more 50000 ...
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Technicality RATAN-600
Number of antenna elements, 895 ; Size of an element, 11.4 x 2 m ; Geometrical area, 15000 m ; Effective area of full circle, 3500 m ; Wavelength range, 1 - 50 cm.Missing: structure design specifications
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The Soviet RATAN-600 Radio Telescope - ADS
The RATAN-600 telescope, located near Zelenchukskaya in the Northern Caucasus, designed for short-wavelength operation, is described. The 576-meters ...Missing: selection criteria Karachay- Cherkess Republic
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63 Ratan 600 Royalty-Free Images, Stock Photos & Pictures
... panel array. Flat sector. Reflector antenna with movable shields made of aluminum. Zelenchukskaya, Karachay-Cherkessia, Russia - June 05, 2024: The RATAN-600.
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RATAN-600 multi-frequency data for the BL Lacertae objects
The RATAN-600 data are available in the form of radio continuum spectra and light curves (Fig. 2), flux density tables with the date of observation in the “Data ...
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RATAN-600
RATAN-600. (Radio Astronomical Telescope Academy Nauk 600). (ring-shaped radio telescope in Russia). RATAN-600 ... arcminute angular resolution. at a 10-cm ...
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Telescope
RATAN-600 is a open access instrument with the status of a "unique ... Geometric area. 22000 m2. Frequencies. 1.25, 2.25, 4.7, 8.2, 11.2, 14.4 and 22.3 ...Missing: total | Show results with:total
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Category:RATAN 600 - Wikimedia Commons
Jun 19, 2018 · Category:RATAN 600 ; construction (1968–1977) · 576 m (primary mirror) · 1.38 cm; 2.7 cm; 3.9 cm; 7.6 cm; 13 cm; 31.1 cm · 12,000 m² (31 cm) · 970 m.
[21]
A search for 1404-MHz H2 + line emission in the atmosphere of ...
... RATAN-600 radio telescope (Esepkina et al. 1979) with an automated radio ... 1986); the system noise temperature at this frequency is 80 K. The spectra ...
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Multi-feed System for a Variable Profile Antenna
... RATAN-600 radio telescope is discussed. A multi-channel receiving system ... The system noise temperature is 100 K: this corresponds to a fluctuation ...
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Illumination of the Main(a) and Secondary (b) mirrors of RATAN-600 ...
The secondary mirror having the shape of a parabolic cylindrical surface, whose generatrix is parallel to the horizon, focuses the wave in the vertical ...
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[PDF] RATAN-600 and PLANCK Mission - arXiv
About 1000 objects were observed more the. 100 times, and high pixel sensitivity was accumulated in about 1000 sq. deg. total area. This approach reminds the ...
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RATAN-600 Radio Telescope: Observing Programs and Outlook
The observations were made in the RATAN transit mode, and the multi-frequency broad-band radio spectra were obtained at the five above-mentioned frequencies ...
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RATAN-600 and RadioAstron reveal the neutrino-associated blazar ...
Jan 15, 2020 · It is operated mostly in transit mode for measuring broad-band spectra. The 1–22 GHz instantaneous spectrum of TXS 0506+056 was first ...
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[PDF] Analysis of RATAN-600 Radiation Patterns in New Operation ... - HAL
The following extensions of the original MLPO scheme have been developed to facilitate the analysis of multi-reflector antenna systems such as the RATAN-600 ...
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About 1% of the total number of elements of the main surf th can be used for formation of the spot. The simplest method is the combined manner transposition ...Missing: challenges | Show results with:challenges
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RATAN-600 Beam Pattern and Drift Scans of Radio Sources in the ...
Nov 7, 2023 · This paper presents the results of calculating the BP in the operation mode of the RATAN-600 radio telescope with the West Sector. This mode is ...
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RATAN-600 Beam Pattern and Drift Scans of Radio Sources in the ...
The paper presents results of calculating the RATAN-600 beam pattern (BP) and BP drift scans of point radio sources in the West Sector radio telescope ...Missing: three- | Show results with:three-
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Diagnostics of the Solar Plasma Using Radio Observations with the ...
... of the solar atmosphere from the chromosphere to the outer corona, as based on the observations with a 600-meter radio telescope the RATAN-600 (1975-1989).
[33]
Radio Measurements of the Magnetic Field in the Solar ... - Frontiers
Still, in a recent work, Bogod et al. (2015) reported polarization of 1.4–7% and magnetic field in the range of 40–200 G from RATAN-600 observations of the ...
[34]
Solar Microwave Emission Associated with Coronal Mass Ejections ...
The connection between Coronal Mass Ejections (CME) and radio burst has been discovered especially at lower frequencies (< 2 GHz).
[35]
About the nature of long‐term microflare energy release in solar ...
Nov 1, 2001 · Abstract. In this paper we compare the long-term impulsive microflares (mi- crobursts (MB) in the range 1000 MHz) using RATAN-600 ...
[36]
RATAN-600 radio telescope in the 24th solar-activity cycle. I. New ...
May 24, 2011 · The upgrade included the improvement of the parameters of the multi-octave solar spectral and polarization analyzer, realization of regular ...
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RATAN-600 radio telescope in the 24th solar-activity cycle. II. Multi ...
... sensitivity of radio telescopes, a detailed spectral analysis over a wide frequency range, high temporal resolution and a broad coverage range in time. We ...Missing: specifications | Show results with:specifications
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The solar radio emission during the minimum between the 23–24 ...
Nov 15, 2016 · RATAN-600 solar observations are daily made at about 50 frequencies in the 3.3–17 GHz range. The fan beam of the antenna pattern of RATAN-600 ...Missing: upgrades | Show results with:upgrades
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[PDF] Solar Service by SPOT, STOP, and RATAN-600
This paper briefly introduces the solar patrol optical telescope (SPOT) · and solar telescope for operational prognoses (STOP) as two important · systems which ...
[40]
[PDF] High-Resolution Microwave Observations of the Sun - DTIC
VLA-RATAN 600 SOLAR MAPS AT THE TIME OF THE JULY 22 SOLAR ECLIPSE ... of the radio and soft X-ray emissions is typical for such flares ... the hard X-ray emission ...
[41]
[PDF] SOURCES OF TYPE III SOLAR MICROWAVE BURSTS
The authors show that RATAN-600 and. BBMS observed the SSP simultaneously. They analyzed the correlation between curves of radio fluxes,. X-ray fluxes, ...
[42]
A study of giant radio galaxies at RATAN-600 - ADS
We report the results of flux density measurements in the extended components of thirteen giant radio galaxies, made with the RATAN-600 in the centimeter ...
[43]
[PDF] Radio properties of radio-loud high-redshift quasars at z>3
RATAN-600 blazar monitoring program. • RATAN-600 radio telescope stands out for its capability of obtaining six-frequency measurements (1–22 GHz) ...
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Observations within the Framework of SETI Program on RATAN-600 Telescope in 2015 and 2016 | Request PDF
### Summary of RATAN-600 SETI Observations (2015–2016)
[45]
SETI - SAO RAS
Aug 30, 2016 · Such observations at RATAN-600 are made possible owing to its large collecting area of thousands of square meters, and this high sensibility ...
[46]
[PDF] Breakthrough Listen Follow-up of a Transient Signal from the ...
May 15, 2015 · While we await with interest a formal write-up of the RATAN-600 result, the claim that the detection could be a signal from an extraterrestrial ...Missing: low North Caucasus SAO