Millimeter-wave Receiver Optics for Korean VLBI Network

Over the past several years the millimeter wave VLBI (Very Long Baseline Interferometry) observations have been intensively performed. However phase fluctuation due to troposphere is one of the key issue in terms of degradation of sensitivity and limits imaging capability in millimeter wave VLBI observations. We describe the details of designed receiver optics for the Korean VLBI Network to calibrate tropospheric phase fluctuation for the millimeter wave VLBI observation. These optics guide beams from one position on sky to 22, 43, 86, and 129 GHz-band receivers simultaneously. Several topics, such as the design principles of imaging and power loss due to phase errors on common ellipsoidal mirrors are discussed.     

Spacecraft Doppler tracking with a VLBI antenna

Summary Accurate measurements of the Doppler shift of the Voyager 2 spacecraft (26 A. U.) have been performed in the period 23/7/88-12/8/88 with the 32m VLBI antenna at Medicina (BO). The device which allows the use of VLBI instrumentation for precision Doppler tracking is basically an open-loop receiver and is called digital tone extractor (DTE). Simultaneous measurements were performed at NASA's Deep Space Network (DSN) stations of the Madrid complex, using a different technique (closed loop). In the most interesting tracking configuration, the signal was transmitted inS-band (2.1 GHz) from the 70 m DSN station at Canberra (Australia), retransmitted back coherently from the spacecraft inX-band (8.4 GHz–19 W) and received 7h 6min later at Medicina and Madrid. The main purpose of the experiment was to test the capabilities of this new system and to characterize its performances. This taks has been successfully accomplished with the acquisition of high-quality data, which are presently under analysis. We plan also to compare and correlate the data with the ones acquired at Madrid stations, in order to separate out different noise contributions to the measured signal. The use of Medicina antenna as a listen-only station is planned for the gravitational wave experiment of the Ulysses spacecraft (ESA), in 1992. To speed up publication, the proofs were not sent to the authors and were supervised by the Scientific Committee.     

On the monitoring model of reference point of VLBI antenna

Some insights and analysis are presented concerning the monitoring model of the VLBI(Very Long Baseline Interferometry) antenna,settings of parameters and selection of constraints to the observation equation,which are verified via data simulation analysis to be reasonable and effective.The effects of the number of targets and antenna orientations,the precision of target positioning observations,the observation outliers detection and deletion on the determination precision of antenna parameters are also analyzed,and some preliminary conclusions are given.     

Applications of same-beam VLBI in the orbit determination of multi-spacecrafts in a lunar sample-return mission

Same-beam VLBI means that two spacecrafts with small separation angles that transmit multi-frequency signals specially designed are observed simultaneously through the main beam of receiving antennas. In same-beam VLBI,the differential phase delay between the two spacecrafts and the two receiving antennas can be obtained within a small error of several picoseconds. As a successful application,the short-arc orbit determination of several hours for Rstar and Vstar,which are two small sub-spacecrafts of SELENE,has been much improved by using the same-beam VLBI data together with the Doppler and range data. The long-arc orbit determination of several days has also been accomplished within an error of about 10 m with the same-beam VLBI data incorporated. These results show the value of the same-beam VLBI for the orbit determination of multi-spacecrafts. This paper introduces the same-beam VLBI and Doppler observations of SELENE and the orbit determination results. In addition,this paper introduces how to use the same-beam VLBI for a lunar sample-return mission,which usually consists of an orbiter,a lander and a return unit. The paper also offers the design for the onboard radio sources in the lunar sample-return mission,and introduces applications of S-band multi-frequency same-beam VLBI in lunar gravity exploration and applications during all stages in the position/orbit determinations such as orbiting,landing,sampling,ascending,and docking.     

Relative position determination of a lunar rover using high-accuracy multi-frequency same-beam VLBI

Multi-frequency same-beam VLBI means that two explorers with a small separation angle are simultaneously observed with the main beam of receiving antennas. In the same-beam VLBI, the differential phase delay between two explorers and two receiving telescopes can be obtained with a small error of several picoseconds. The differential phase delay, as the observable of the same-beam VLBI, gives the separation angular information of the two explorers in the celestial sphere. The two-dimensional relative position on the plane-of-sky can thus be precisely determined with an error of less than 1 m for a distance of 3.8×105 km far away from the earth, by using the differential phase delay obtained with the four Chinese VLBI stations. The relative position of a lunar rover on the lunar surface can be determined with an error of 10 m by using the differential phase delay data and the range data for the lander when the lunar topography near the rover and the lander can be determined with an error of 10 m.     

VLBI studies at the Radiophysical Research Institute

We consider the state-of-the-art of research in the field of very long baseline interferometry (VLBI) at the Radiophysical Research Institute (Nizhny Novgorod, Russia). In the past decade, the team of the VLBI Laboratory at this institute used the extensive methodological and instrument basis and the accumulated experience of radio-interferometric observations to continue experimental and theoretical studies along several research lines including the studies of the solar wind and radio emission of the Sun, radar studies of the bodies in the solar system, and navigational measurements. We present the main experimental results obtained for the analyzed problems. __________ Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 50, No. 7, pp. 577–592, July 2007.     

Very Long Baseline Interferometry — a high precision tool for geodesy and astrometry

Very Long Baseline Interferometry is able to provide a direct geometrical tie to the extragalactic radio sources which represent the best possible realization of an inertial system. By this token, VLBI can measure Earth rotation and orientation as well as precise station positions and their velocities without involving the gravity field of the Earth. In the broader context of Earth observation and the monitoring of geodynamic processes, this one and many more unique features have allowed the VLBI technique to achieve pioneering feats such as the determination of present-day plate tectonic motions, post glacial rebound, sub-daily Earth rotation variations and parameters of general relativity. In this contribution, a brief outline of the VLBI technique and the models used in geodetic data analysis will be given before some of the most important achievements to date will be passed in review and future developments will be indicated.     

Orbit determination for Chang’E-2 lunar probe and evaluation of lunar gravity models

The Unified S-Band (USB) ranging/Doppler system and the Very Long Baseline Interferometry (VLBI) system as the ground tracking system jointly supported the lunar orbit capture of both Chang’E-2 (CE-2) and Chang’E-1 (CE-1) missions. The tracking system is also responsible for providing precise orbits for scientific data processing. New VLBI equipment and data processing strategies have been proposed based on CE-1 experiences and implemented for CE-2. In this work the role VLBI tracking data played was reassessed through precision orbit determination (POD) experiments for CE-2. Significant improvement in terms of both VLBI delay and delay rate data accuracy was achieved with the noise level of X-band band-width synthesis delay data reaching 0.2–0.3 ns. Short-arc orbit determination experiments showed that the combination of only 15 min’s range and VLBI data was able to improve the accuracy of 3 h’s orbit using range data only by a 1–1.5 order of magnitude, confirming a similar conclusion for CE-1. Moreover, because of the accuracy improvement, VLBI data was able to contribute to CE-2’s long-arc POD especially in the along-track and orbital normal directions. Orbital accuracy was assessed through the orbital overlapping analysis (2 h arc overlapping for 18 h POD arc). Compared with about 100 m position error of CE-1’s 200 km×200 km lunar orbit, for CE-2’s 100 km×100 km lunar orbit, the position errors were better than 31 and 6 m in the radial direction, and for CE-2’s 15 km×100 km orbit, the position errors were better than 45 and 12 m in the radial direction. In addition, in trying to analyze the Delta Differential One-Way Ranging (ΔDOR) experiments data we concluded that the accuracy of ΔDOR delay was dramatically improved with the noise level better than 0.1 ns and systematic errors better calibrated, and the Short-arc POD tests with ΔDOR data showed excellent results. Although unable to support the development of an independent lunar gravity model, the tracking data of CE-2 provided evaluations of different lunar gravity models through POD. It is found that for the 100 km×100 km lunar orbit, with a degree and order expansion up to 165, JPL’s gravity model LP165P did not show noticeable improvement over Japan’s SGM series models (100×100), but for the 15 km×100 km lunar orbit, a higher degree-order model can significantly improve the orbit accuracy.

     

The first geodetic VLBI experiment with the Bologna radio telescope

Summary The results of the first geodetic experiment with the Bologna VLBI radiotelescope are presented, giving a decimeter level determination of the radio telescope position.     

Linear algorithms of multi-frequency image processing for VLBI

We consider linear algorithms of multi-frequency image synthesis and analysis for very-long baseline interferometry (VLBI). Compared with the existing algorithms of multi-frequency synthesis, the developed algorithm allows one to obtain the spectral-index map simultaneously with the map of a radio source for any value of the reference frequency within a given frequency band. In addition, there exists an opportunity to obtain a spectral estimate for any given part of the image. Some examples of the multi-frequency image retrieval for the quasar 3C84 are presented. __________ Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 49, No. 7, pp. 553–560, July 2006.     

用于"萤火1号"火星轨道器的开环电测技术

中国首个火星探测器"萤火1号"计划于2011年和俄罗斯的火卫一采样探测器一道发射升空."萤火1号"将探测火星的空间环境,并验证深空导航测控与通信技术.与常规的火星探测任务不同,该探测器的轨道与位置测量主要利用天文甚长基线干涉测量技术、开环跟踪测量技术、差分单程测距测速技术、同波束干涉测量技术以及单程多普勒(Doppler)测速技术.     

Possibilities of VLBI observation of solar spike-like events

Modern theoretical and experimental investigations of energy release fragmentation in solar flares show the necessity of observations with high space and time resolution. In this paper, we analyze earlier interferometric observations of solar radio spikes and discuss the first results of the Radiophysical Research Institute of Nizhny Novgorod (NIRFI) in this field. We describe the NIRFI's receiving and analyzing equipment, which is part of the measuring complex for solarflare investigation with high space and time resolution and enables one to analyze the form of the interference signal and its amplitude spectrum with time and frequency resolutions of up to 16.7 sec and 100 Hz, respectively. The prospects for VLBI observation of solar flares with high space resolution are discussed.Radiophysical Research Institute, Nizhny Novgorod. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 38, No. 10, pp. 1046–1056, October, 1995.     

VLBI studies of the solar-wind plasma irregularities at 18 and 92 CM wavelengths in 1994–1996

We discuss the capabilities of VLBI studies of irregularities of the solar-wind plasma using multi-element radio interferometric facilities. We analyze the data obtained during international VLBI experiments at decimeter wavelengths (92 and 18 cm) in 1994–1996 and supposed that the irregularities have a “stream” structure. The “streams” are strongly elongated in the solar-wind direction (longitudinal size of about a few hundred thousand kilometers) and have the transverse size of about 0.5–2.0 thousand kilometers. The irregularities inside a single “stream” are almost isotropic. We discuss the restrictions imposed on operation of decimeter VLBI systems due to effects of the interplanetary medium. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 43, No. 3, pp. 197–206, March, 2000     

Determination of Structure Corrections using Geodetic VLBI Observations of Fiducial Extragalactic Radio Sources

We present the further development of the mathematical technique for calculating the structure corrections using VLBI images of fiducial extragalactic radio sources entering the celestial reference frame. In contrast to techniques described in the literature, the proposed approach can be applied to arbitrary images rather than to images which can be represented by a few Gaussian or delta functions. This is especially topical in view of the appearance of new sophisticated and high-precision image-reconstruction techniques different from the conventional CLEAN procedure or model fitting. The calculation efficiency of the structure corrections is ensured by using the algorithm of fast Fourier transform. We apply the proposed method to analyze a sufficiently representative sample of 36 fiducial extragalactic sources entering the celestial reference frame and illustrate its use for four sources, 1357+769, 0229+131, 2201+315, and 2200+420, each of them belonging to one of the four structure-index classes.     

Theoretical analysis on phase-locking properties of a laser diode array facing an external cavity

External coupling model has been used to describe the output field of a laser diode array (LDA) phase-locked with an external cavity. The analytical solution for the coupling matrix equation of the phase-locked system has been obtained. The dependencies of the threshold gain, g_j of the system mode on the residue reflection of the front facet, r_f and round trip external cavity lengths, L have been discussed. The working lengths of the external cavity for stably phase-locking the LDA of different residual reflectivities have been calculated.     

Configuration interaction study including the effects of spin–orbit coupling for the electronic states of the LiX molecules (X = C,Si, Ge,Sn)

Ab initio multireference configuration interaction calculations including spin–orbit coupling effects have been carried out for four LiX molecules (X?=?C, Si, Ge and Sn). Potential energy curves of the ground and low-lying excited states have been obtained in each case as well as the corresponding spectroscopic constants. Transition moments have also been computed in order to give estimates of the radiative lifetimes of the excited states for each system. Trends in a variety of quantities such as T _e values, spin–orbit splittings, equilibrium bond lengths and vibrational frequencies for this series of molecules are discussed in detail and comparison with the corresponding data reported earlier for the PbLi system is also made.     

Orientational order and molecular parameters of two nematogenic mixtures from X-ray studies: confirmation of electro-optical results

This study entails the report of X-ray studies conducted on two nematogenic mixtures (code names ZLI 1221 and ZLI 1291) containing identical moieties: phenyl cyclohexane, biphenyl cyclohexane and cyclohexyl benzoate, but exhibiting different mesogenic ranges and properties. X-ray studies have been undertaken with a view to investigate the difference in the mesogenic behaviour of the said mixtures at the molecular level. The average apparent molecular length ‘l?’ and intermolecular distance ‘D’ of the two mixtures and their variations with temperature have been determined from X-ray data. The orientational order parameters ?P ₂? and ?P ₄? and their thermal variations have also been obtained. Comparison has been made with the ?P ₂? values obtained from X-ray study with those obtained from optical study. The average apparent molecular lengths of the two mixtures corroborate the findings regarding the relative molecular weights of the two samples obtained from optical and dielectric data.     

The structure factor for liquid nitrogen and liquid oxygen by neutron scattering

The structure factor S(Q) has been measured for liquid nitrogen at 77 K by neutron diffraction at four wavelengths. The effects of Placzek corrections on the self [1, 2] and interference [3] components of the observed differential scattering cross-sections at 0·35, 0·7, 0·84 and 1·06 Å [4] have been investigated. Effective molecular masses and internuclear bond lengths have been obtained by fitting a modified Placzek model to the observed data. It is concluded that after correction the different structure factors agree satisfactorily within the statistical errors of the measurements and the internuclear bond length is close to that measured in the gas phase.     

Results of theoretical and experimental studies of solar wind and active galactic nuclei on LFVN VLBI network using S2 recording system

We discuss the results of two sessions of observations at the Low-Frequency VLBI Network (LFVN), carried out in 1999 (INTAS99.4) and 2000 (INTAS00.3) at a wavelength of 18 cm using the S2 recording system and processed using the correlator system in Pentictone, Canada. In different configurations of the experiments on studying the solar wind and active galactic nuclei, the antennas at the following sites were employed: Medvezhji Ozera (RT-64, Special Engineering Bureau of Moscow Power Engineering Institute, Russia), Pushchino (RT-22, Pushchino Radio Astronomy Observatory, Russia), Hartebeesthoek (RT-25, South Africa), Noto (RT-32, Italy), Shanghai (RT-25, China), Pune (RT-45, India), Svetloe (RT-32, Institute of Applied Astronomy RAS, Russia). The work resulted in successful testing of the method of radio probing of the solar-wind plasma by radiation of extragalactic sources, supplemented with the method of radio interferometric reception. Spectral analysis of the obtained data allowed us to estimate the index of spatial spectrum of the electron number density.uctuations and the transfer velocity of the solar-wind inhomogeneities on the sounding path. We present and discuss the retrieved images of STA-102 quasar and the BL Lacertae object 1418+546 with millisecond angular resolution and demonstrate the results of modeling the structure of these sources. __________ Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 50, No. 4, pp. 275–299, April 2007     

Observations of deterministic chaos in financial time series by recurrence plots, can one control chaotic economy?

Several economical time series such as exchange rates US$/British Pound, USA Treasure Bonds rates and Warsaw Stock Index WIG have been investigated using the method of recurrence plots. The percentage of recurrence REC and the percentage of determinism DET have been calculated for the original and for shuffled data. We have found that in some cases the values of REC and DET parameters are about 20% lower for the surrogate data which indicates the presence of unstable periodical orbits in the considered data. A similar result has been obtained for the chaotic Lorenz model contaminated by noise. Our investigations suggest that real economical dynamics is a mixture of deterministic and stochastic chaos. We show how a simple chaotic economic model can be controlled by appropriate influence of time-delayed feedback. Received 13 October 2000