A 3mm band SIS receiver for the Sardinia Radio Telescope

2014 ◽  
Author(s):  
A. Ladu ◽  
T. Pisanu ◽  
A. Navarrini ◽  
P. Marongiu ◽  
G. Valente
Keyword(s):  
Radio Telescope ◽  
Sis Receiver

scholarly journals A New 100-GHz Band Two-Beam Sideband-Separating SIS Receiver for Z-Machine on the NRO 45-m Radio Telescope

2013 ◽  
Vol 125 (925) ◽  
pp. 252-262 ◽  
Author(s):  
T. Nakajima ◽  
K. Kimura ◽  
A. Nishimura ◽  
H. Iwashita ◽  
C. Miyazawa ◽  
...  
Keyword(s):  
Radio Telescope ◽  
Sis Receiver

scholarly journals A New 100-GHz Band Front-End System with a Waveguide-Type Dual-Polarization Sideband-Separating SIS Receiver for the NRO 45-m Radio Telescope

2008 ◽  
Vol 60 (3) ◽  
pp. 435-443 ◽  
Author(s):  
Taku Nakajima ◽  
Takeshi Sakai ◽  
Shin’ichiro Asayama ◽  
Kimihiro Kimura ◽  
Masayuki Kawamura ◽  
...  
Keyword(s):  
Radio Telescope ◽  
Dual Polarization ◽  
Sis Receiver ◽  
Front End ◽  
Waveguide Type ◽  
Band Front

The control system of the 3 mm band SIS receiver for the Sardinia Radio Telescope

2016 ◽  
Author(s):  
A. Ladu ◽  
P. Ortu ◽  
A. Saba ◽  
M. Pili ◽  
F. Guadiomonte ◽  
...  
Keyword(s):  
Control System ◽  
Radio Telescope ◽  
Sis Receiver

Interpretation of the Filament Depression at Millimetric and Centimetric Wavelengths

1979 ◽  
Vol 44 ◽  
pp. 131-134
Author(s):  
A. Raoult ◽  
P. Lantos ◽  
E. Fürst
Keyword(s):  
Radio Telescope ◽  
Active Regions ◽  
Simple Shape ◽  
Quiet Sun ◽  
Unstable Process

The depressions at centimetric and millimetric wavelengths associated with the filaments are studied using already published maps as well as unpublished observations from the Effelsberg 100 m radio telescope of the M.P.I., Bonn. The study has been restricted to large Ha quiescent prominences of relatively simple shape, situated far from the limb and from active regions. The data has been reduced employing one method whose main characteristics are choice of a local quiet sun definition and avoidance of the unstable process of deconvolution.

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

Radio recombination line observations towards Spitzer infrared bubbles with the TianMa radio telescope

2019 ◽  
Vol 489 (4) ◽  
pp. 4862-4874
Author(s):  
L G Hou ◽  
X Y Gao
Keyword(s):  
Radio Telescope ◽  
Detection Rate ◽  
Milky Way ◽  
Absorption Method ◽  
Recombination Line ◽  
Ionized Gas ◽  
Radio Recombination Line ◽  
Warm Ionized Medium

ABSTRACT Many of the Spitzer infrared bubbles identified by the Milky Way Project (MWP) are suggested to be $\rm{H \small {II}} $ regions in nature. More than 70 per cent of the ∼5000 known bubbles do not have radio recombination line (RRL) observations, hence have not been confirmed as $\rm{H \small {II}} $ regions. A systematic RRL survey should be helpful to identify the nature of the bubbles. With the Shanghai TianMa 65-m radio telescope, we searched for RRLs towards 216 selected Spitzer bubbles by simultaneously observing 19 RRLs in the C band (4–8 GHz). RRLs are detected in the directions of 75 of the 216 targets. 31 of the 75 RRL sources are classified as new detections, which are possibly from new $\rm{H \small {II}} $ regions or diffuse warm ionized medium; 36 of them are probably from the outskirts of nearby bright $\rm{H \small {II}} $ regions, rather than bubble-encircled ionized gas; and the detected RRLs towards 8 bubbles are identified from known $\rm{H \small {II}} $ regions. For 58 of the 75 RRL sources, we obtained their distances after resolving the kinematic distance ambiguity by combining the results of the H2CO absorption method, the $\rm{H \small {I}} $ emission/absorption method, and the $\rm{H \small {I}} $ self-absorption method. The low detection rate of new $\rm{H \small {II}} $ regions implies that a number of MWP bubbles in the DR1 catalogue are too faint if they are $\rm{H \small {II}} $ regions.

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