Methodology for the observation of radio sources using Ku‐band compact radio telescopes

2021 ◽  
Author(s):  
David Galeano ◽  
Edwin A. Quintero ◽  
Miguel A. Salazar
Keyword(s):  
Radio Sources ◽  
Radio Telescopes ◽  
Ku Band

scholarly journals Search for molecular bremsstrahlung radiation signals in Ku band with coincidental operations of radio telescopes with air shower detectors

2013 ◽  
Vol 53 ◽  
pp. 08007
Author(s):  
Shoichi Ogio ◽  
Tokonatsu Yamamoto ◽  
Kazuyuki Kuramoto ◽  
Takashi Iijima ◽  
Hidetoshi Akimune ◽  
...  
Keyword(s):  
Radio Telescopes ◽  
Bremsstrahlung Radiation ◽  
Air Shower ◽  
Ku Band

scholarly journals Use of the Long Baseline Array in Australia for Precise Geodesy and Absolute Astrometry

2009 ◽  
Vol 26 (1) ◽  
pp. 75-84 ◽  
Author(s):  
Leonid Petrov ◽  
Chris Phillips ◽  
Alessandra Bertarini ◽  
Adam Deller ◽  
Sergei Pogrebenko ◽  
...  
Keyword(s):  
Data Analysis ◽  
Heterogeneous Network ◽  
Radio Sources ◽  
Radio Telescopes ◽  
Geodetic Vlbi ◽  
Novel Technique ◽  
Long Baseline ◽  
Better Than

AbstractWe report the results of a successful 12-hour 22-GHz VLBI experiment using a heterogeneous network that includes radio telescopes of the Long Baseline Array (LBA) in Australia and several VLBI stations that regularly observe in geodetic VLBI campaigns. We have determined positions of three VLBI stations, atca-104, ceduna and mopra, with an accuracy of 4–30 mm using a novel technique of data analysis. These stations have never before participated in geodetic experiments. We observed 105 radio sources, and amongst them 5 objects which have not previously been observed with VLBI. We have determined positions of these new sources with the accuracy of 2–5 mas. We make the conclusion that the LBA network is capable of conducting absolute astrometry VLBI surveys with an accuracy better than 5 mas.

scholarly journals Gain Measurements of Large Aerials Used in Interferometer and Cross?Type Radio Telescopes

1958 ◽  
Vol 11 (1) ◽  
pp. 70 ◽  
Author(s):  
AG Little
Keyword(s):  
Radio Telescope ◽  
Radio Sources ◽  
Radio Telescopes ◽  
Discrete Radio Sources ◽  
Cross Type

A method has been developed for measuring the gain of large interferometer and cross-type radio telescope aerials. Use is made of the strong discrete radio sources, whose intensity need not be known, to allow comparison of the gains of the aerials with that of a standard.

scholarly journals An overview of jet-mode AGN feedback and the prospects for studying its cosmic evolution with LOFAR

2014 ◽  
Vol 10 (S313) ◽  
pp. 251-259
Author(s):  
L. Bîrzan ◽  
D. A. Rafferty ◽  
M. Brüggen ◽  
Keyword(s):  
Star Formation ◽  
Strong Coupling ◽  
Direct Measurement ◽  
Relativistic Plasma ◽  
Scaling Relations ◽  
Radio Sources ◽  
Radio Telescopes ◽  
Radio Data ◽  
Cosmic Evolution ◽  
Radio Power

AbstractChandra revealed cavities in the hot atmospheres of many nearby clusters. These cavities are tracers of a strong coupling between the relativistic plasma in radio sources and the cooling, thermal gas in clusters. They demonstrate clearly that the AGN affects the cooling gas that leads to star formation and galaxy growth and allow a direct measurement of the bulk of the AGN's power. Together with radio data, the cavities allow us to derive scaling relations between mechanical (cavity) and radio power that can be used to estimate the AGN feedback power when direct measurement of the cavities is not possible. We review the importance of such relations for extending current studies of feedback with new and upcoming radio telescopes such as LOFAR and SKA.

40. Radio Astronomy

1982 ◽  
Vol 18 (1) ◽  
pp. 529-549
Author(s):  
G. Swarup
Keyword(s):  
Data Processing ◽  
Radio Astronomy ◽  
Present Report ◽  
Source Parameters ◽  
Radio Sources ◽  
Radio Telescopes ◽  
New Developments

This report covers surveys of radio sources, basic measurements of source parameters and new developments in radio telescopes, instrumental techniques and data processing. The period covered is approximately late 1978 to about August 1981. The results and conclusions of astronomical investigations based on measurements made through the radio window are included in the reports of other commissions, as relevant. Following the practice adopted in 1979, a circular was sent to the Presidents of 18 IAU Commissions and to all members of Commission 40 describing the proposed format of the present report and also identifying contact persons who could be consulted to avoid duplication and to ensure that radio astronomical results are adequately covered by various commissions. I am grateful to all concerned for providing the necessary coordination.

scholarly journals Monitoring the brightness temperature of the Moon throughout the lunar cycle from radio observations in the Ku band

2021 ◽  
Vol 2090 (1) ◽  
pp. 012159
Author(s):  
David Galeano ◽  
A. Quintero Edwin
Keyword(s):  
Brightness Temperature ◽  
Lunar Cycle ◽  
Climatic Conditions ◽  
Maximum Temperature ◽  
Radio Telescopes ◽  
The Moon ◽  
Great Opportunity ◽  
Receiver System ◽  
Wide Range ◽  
Ku Band

Abstract Within the spectrum of radio waves, the Ku band (12 - 18 GHz ) stands out for the wide range of instruments available and for its relative ease of acquisition, given that satellite television operates in this band. This situation offers a great opportunity for the development of radio astronomy in countries with unfavorable climatic conditions for optical astronomy, since this band is only affected by dense masses of water vapor. In this article we present a methodology for the calibration of the receiver system of compact Ku-band radio telescopes, and its application in the determination of the brightness temperature of the Moon. Our methodology involves modeling the influence of the atmosphere of the Earth on the response of the radioreceptor, which minimizes the error in the calculation of the brightness temperature of the observed object. We applied the proposed methodology in the monitoring of the Lunar cycle using the Ku-band radio telescope of the Observatorio Astronomico of Universidad Tecnológica de Pereira, Colombia (OAUTP). After observing during May, June, and July of 2021, we obtained an average temperature of 213.15 K, with maximum and minimum values of 275.55 K and 150.75 K, respectively. In addition, we evidenced a delay of 5.75 days between the phase in which the maximum temperature is presented and the phase of the full Moon, which is consistent with the frequency of observation. The results show that our methodology is useful to optimize the calibration of compact Ku-band radio telescopes, and expand the potential of this type of instrument for the scientific study of radio sources other than the Sun, in this case the Moon.

scholarly journals Proposed Very Long Baseline Interferometry at 103 MHz in India

1984 ◽  
Vol 110 ◽  
pp. 391-395
Author(s):  
R. V. Bhonsle ◽  
S. K. Alurkar ◽  
S. S. Degaonkar ◽  
A. D. Bobra ◽  
R. Sharma
Keyword(s):  
Solar Wind Plasma ◽  
General Purpose ◽  
Radio Sources ◽  
Radio Telescopes ◽  
Relative Time ◽  
Plasma Dynamics ◽  
Long Baseline ◽  
General Purpose Computer ◽  
Time Accuracy ◽  
Phase Distortions

Three radio telescopes operating at 103 MHz are being installed at Ahmedabad, Rajkot and Surat separated by about 200 km from each other for observing interplanetary scintillations (IPS) of compact radio sources for study of solar wind plasma dynamics as well as radio source size measurements for cosmological studies. Of these, two radio telescopes at Ahmedabad and Rajkot have been commissioned and started synchronous daily observations of IPS of a few compact radio sources with relative time accuracy of about ± 1 millisec. The third telescope at Surat is expected to go in operation by the end of 1983. As soon as all the three telescopes go in for simultaneous operation, it is proposed to (1) augment the telescope sensitivity so as to detect sources with flux density ~ 1 Jansky (2) incorporate better time and frequency standards at each station which can be synchronised to better than μs relative time accuracy (3) develop suitable receivers and data acquisition system for generating interference fringes using a general purpose computer and (4) take advantage of the availability of three telescopes to incorporate ‘closure phase and amplitude’ techniques which eliminate undesirable atmospheric and ionospheric phase distortions.

scholarly journals Pulsar Studies at High Radio Frequencies

2000 ◽  
Vol 177 ◽  
pp. 205-210 ◽  
Author(s):  
Richard Wielebinski
Keyword(s):  
Radio Sources ◽  
Radio Telescopes ◽  
Frequency Range ◽  
High Luminosity ◽  
Max Planck ◽  
Pulsar Emission ◽  
Millisecond Pulsars ◽  
Pulsar Radio ◽  
Radio Frequencies ◽  
Pulsar Radio Emission

AbstractPulsars were discovered at 81.5 MHz and a lot of the studies of these exciting objects have been made up to the present time at radio frequencies below 1.6 GHz. The reasons for this concentration on the low radio frequency characteristics of pulsars is the fact that the spectra are very steep and that very few radio telescopes exist that are capable of efficient operations at high radio frequencies. The Effelsberg 100-m radio telescope of the Max-Planck-Institut fur Radioastronomie operates regularly up to the frequency of 50 GHz and was used to study pulsars at cm/mm-wavelengths. In the southern skies the Parkes 64-m telescope has been used to study pulsars up to 8.4 GHz. One pulsar has been detected at 87 GHz with the 30-m Pico Veleta telescope of IRAM.The studies of pulsars over the whole frequency range are of great importance because this is necessary for the elucidation of the mechanism that is responsible for the pulsar emission. The high polarization of pulsar radio emission at lower radio frequencies has supported the hypothesis of a coherent emission mechanism, which is required to generate the high luminosity. It has been known for some time that pulsars, unlike other radio sources, have a lower polarization at high radio frequencies. Recently a change of pulsar spectrum, a flattening or possibly an inversion has been observed at the highest radio frequencies. The inversion of the pulsar spectrum seems to coincide with a complete depolarization of some pulsars.Millisecond pulsars are less luminous than normal pulsars. This makes them even more difficult to detect at higher radio frequencies. Recent observations have extended the spectra of ten millisecond pulsars up to 4.85 GHz. The results imply that millisecond pulsars have properties very similar to normal (slow) pulsars, which suggests similar emission mechanisms.

scholarly journals Observations of extragalactic radio emission

1959 ◽  
Vol 9 ◽  
pp. 328-336 ◽  
Author(s):  
C. A. Shain
Keyword(s):  
Radio Emission ◽  
Brightness Distribution ◽  
Radio Sources ◽  
Pencil Beam ◽  
Radio Telescopes ◽  
General Picture ◽  
Extragalactic Radio Sources

Several extragalactic radio sources within reach of Sydney radio telescopes have been found to have angular sizes so great that they can be resolved with the pencil-beam aerials, which are available at three frequencies. It is possible to study in some cases the brightness distribution in some detail; in others to study the qualitative general picture. The observations with which the present paper is concerned are set out in Table I.

scholarly journals Methods for detection and analysis of weak radio sources with single-dish radio telescopes

2020 ◽  
Vol 49 (3) ◽  
pp. 159-182
Author(s):  
M. Marongiu ◽  
A. Pellizzoni ◽  
E. Egron ◽  
T. Laskar ◽  
M. Giroletti ◽  
...  
Keyword(s):  
Radio Sources ◽  
Radio Telescopes
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