22 GHz Observations with the Resurfaced Central 17 m of the Parkes Radio Telescope

1976 ◽  
Vol 3 (1) ◽  
pp. 61-63 ◽  
Author(s):  
J. L. Caswell ◽  
R. A. Batchelor ◽  
W. M. Goss ◽  
R. F. Haynes ◽  
S. H. Knowles ◽  
...  
Keyword(s):  
Liquid Nitrogen ◽  
Radio Telescope ◽  
Noise Temperature ◽  
Parametric Amplifier ◽  
Total System ◽  
High Frequencies ◽  
Second Stage ◽  
System Noise ◽  
Front End ◽  
5 Ghz

At the centre of the Parkes 64—m radio telescope a region of diameter 17 m has recently been resurfaced to improve its efficiency at high frequencies. The first measurements using this section have been made at 22 GHz, in observations of both continuum sources and water tfapour masers. For these observations the receiver front-end used a mixer cooled in liquid nitrogen, followed by a 5 GHz cryogenic parametric amplifier as a second stage. The option of switching against an offset horn was available and the total system noise temperature was ∽ 750 K.

scholarly journals A 10-GHZ Radio Continuum Survey of the Galactic Plane

1987 ◽  
Vol 115 ◽  
pp. 538-539
Author(s):  
T. Handa ◽  
Y. Sofue ◽  
N. Nakai ◽  
H. Hirabayashi ◽  
K. Akabane ◽  
...  
Keyword(s):  
Galactic Plane ◽  
Noise Temperature ◽  
Radio Continuum ◽  
Beam Size ◽  
Calibration Source ◽  
Polarization Component ◽  
Radio Observatory ◽  
System Noise ◽  
Ngc 7027 ◽  
5 Ghz

A radio continuum survey of the galactic plane has been made with the 45-m telescope of the Nobeyama Radio Observatory at 10.55 GHz, which is the highest frequency among such surveys. The sensitivity of the telescope was Tb/S = 0.47 K/Jy and the HPBW was 2!6, which was a great advantage because of the same beam size of the Bonn 5-GHz survey (Altenhoff et al. 1978). The receiver was a cooled parametric amplifier. The instantaneous bandwidth was 500 MHz, and the system noise temperature was about 100 K. The calibration source was NGC 7027, which was assumed to be 6.6 Jy. One circular polarization component was observed. The observational parameters are summarized in Table I.

scholarly journals The Sgr B2 Region Seen at 43 GHZ

1987 ◽  
Vol 115 ◽  
pp. 158-160
Author(s):  
Hisashi Hirabayashi ◽  
Kenji Akabane ◽  
Masaki Morimoto ◽  
Yosiaki Sofue ◽  
Makato Inoue ◽  
...  
Keyword(s):  
Flux Density ◽  
Noise Temperature ◽  
Central Frequency ◽  
Radio Observatory ◽  
System Noise ◽  
Ngc 7027 ◽  
Pointing Accuracy ◽  
Half Power ◽  
5 Ghz ◽  
Better Than

The Sgr B2 region was mapped at 43 GHz (λ = 6.9 mm) with the 45m radio telescope of Nobeyama Radio Observatory. The observing parameters were: a) half power beamwidth 38″, b) pointing accuracy better than 10″, c) central frequency 43.0 GHz, d) bandwidth 500 MHz, and e) system noise temperature 400 K; and the observational aspects were: a) mapping with one polarization, b) liquid-nitrogen cooled load switching and c) reduction by NOD-2 programme. The obtained map is shown in Figure 1. Sgr B2 is resolved into several components which correspond to those by Martin and Downes (1972) and Downes et al. (1978). But the component at RA = 17h44m11.8s Dec. = −28°23′55″ at 1950 is not seen in Martin and Downes (1972) nor in the 5 GHz map of Downes et al. (1978), although the feature is seen in the 10.7 GHz map of Downes et al. (1978). The components derived from the map in Figure 1 by a morphological estimate are listed in Table 1. The total flux density of the region is 146J±30 Jy. The intensity calibration was made by observing NGC 7027.

Total System Noise Temperature: 15°K (Correspondence)

1964 ◽  
Vol 12 (6) ◽  
pp. 619-620 ◽  
Author(s):  
R.C. Clauss ◽  
W. Higa ◽  
C. Stelzried ◽  
E. Wiebe
Keyword(s):  
Noise Temperature ◽  
Total System ◽  
System Noise

Measurements of radio telescope receiving system noise temperatures of two-elements radio interferometer with very long baseline

2018 ◽  
pp. 51-54
Author(s):  
I. E. Arsaev ◽  
Yu. V. Vekshin ◽  
A. I. Lapshin ◽  
V. V. Mardyshkin ◽  
M. V. Sargsyan ◽  
...  
Keyword(s):  
Radio Telescope ◽  
Radio Interferometer ◽  
System Noise ◽  
Long Baseline

scholarly journals Passive Switched Capacitor RF Front Ends for Spectrum Sensing in Cognitive Radios

2014 ◽  
Vol 2014 ◽  
pp. 1-20
Author(s):  
Bodhisatwa Sadhu ◽  
Martin Sturm ◽  
Brian M. Sadler ◽  
Ramesh Harjani
Keyword(s):  
Spectrum Sensing ◽  
Circuit Design ◽  
Software Defined Radio ◽  
High Speed ◽  
Cognitive Radios ◽  
Optimization Techniques ◽  
Switched Capacitor ◽  
Rf Receiver ◽  
Front End ◽  
5 Ghz

This paper explores passive switched capacitor based RF receiver front ends for spectrum sensing. Wideband spectrum sensors remain the most challenging block in the software defined radio hardware design. The use of passive switched capacitors provides a very low power signal conditioning front end that enables parallel digitization and software control and cognitive capabilities in the digital domain. In this paper, existing architectures are reviewed followed by a discussion of high speed passive switched capacitor designs. A passive analog FFT front end design is presented as an example analog conditioning circuit. Design methodology, modeling, and optimization techniques are outlined. Measurements are presented demonstrating a 5 GHz broadband front end that consumes only 4 mW power.

Unified Definitions of Efficiencies and System Noise Temperature for Receiving Antenna Arrays

2010 ◽  
Vol 58 (6) ◽  
pp. 2121-2125 ◽  
Author(s):  
Karl F Warnick ◽  
Marianna V Ivashina ◽  
Rob Maaskant ◽  
Bert Woestenburg
Keyword(s):  
Antenna Arrays ◽  
Noise Temperature ◽  
System Noise ◽  
Receiving Antenna

Frequency Bandwidth Adjustment by Precision Post-Processing for a 0.78–0.95 THz Band SIS Mixer

2015 ◽  
Vol 643 ◽  
pp. 157-163
Author(s):  
Akihira Miyachi ◽  
Takafumi Kojima ◽  
Yasunori Fujii ◽  
Masanori Takeda ◽  
Yoshinori Uzawa ◽  
...  
Keyword(s):  
Mass Production ◽  
Noise Temperature ◽  
Back Side ◽  
Frequency Bandwidth ◽  
Post Processing ◽  
Sis Mixer ◽  
Optimal Method ◽  
High Frequencies ◽  
Em Simulation ◽  
The Relationship

In this study, we demonstrate a method for adjusting the frequency bandwidth of a Superconductor-insulator-superconductor (SIS) mixer device by controlling its thickness after microfabrication. We estimate the relationship between SIS mixer device thickness and frequency bandwidth using electromagnetic (EM) simulation. We propose an optimal method for the precision polishing of the back side of the device. We evaluate the noise temperature and measure the frequency bandwidth of SIS mixer devices with different thicknesses. This study presents the adjustment of the frequency bandwidth of a device through controlling its thickness after microfabrication. This technique may improve the yield of SIS mixer device mass production and support the construction of receivers for ultra-high frequencies such as Atacama Large Millimeter/Submillimeter Array (ALMA) Band 10.

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