A broad-band low-noise SIS receiver for submillimeter astronomy

1988 ◽  
Vol 36 (12) ◽  
pp. 1720-1726 ◽  
Author(s):  
T.H. Buttgenbach ◽  
R.E. Miller ◽  
M.J. Wengler ◽  
D.M. Watson ◽  
T.G. Phillips
Keyword(s):  
Broad Band ◽  
Low Noise ◽  
Sis Receiver ◽  
Submillimeter Astronomy

A broadband low noise SIS receiver for submillimeter astronomy

2003 ◽  
Author(s):  
T.H. Buttgenbach ◽  
R.E. Miller ◽  
M.J. Wengler ◽  
D.M. Watson ◽  
T.G. Phillips
Keyword(s):  
Low Noise ◽  
Sis Receiver ◽  
Submillimeter Astronomy

scholarly journals A Low Noise Receiver for Submillimeter Astronomy

1986 ◽  
Author(s):  
M. J. Wengler ◽  
D. P. Woody ◽  
R. E. Miller ◽  
T. G. Phillips
Keyword(s):  
Low Noise ◽  
Submillimeter Astronomy ◽  
Noise Receiver

Femtosecond pulses from the ultraviolet to the infrared: Optical parametric processes in a new light

1993 ◽  
Vol 71 (1-2) ◽  
pp. 47-58 ◽  
Author(s):  
H. M. van Driel ◽  
G. Mak
Keyword(s):  
Broad Band ◽  
Average Power ◽  
Low Noise ◽  
High Threshold ◽  
Femtosecond Pulses ◽  
Solid State Lasers ◽  
Ti:Sapphire Laser ◽  
Optical Parametric ◽  
Parametric Processes ◽  
Pump Lasers

Although the optical parametric oscillator (OPO) is more than 25 years old, it has not seen widespread use unlike other tunable sources such as the dye laser. Part of the reason for this is the low-gain – high-threshold associated with the weak conversion mechanism in the nonlinear optical crystals. Pump lasers with high peak intensities are usually required, which, unfortunately, run the risk of damaging the crystals, especially if their pulse duration is nanoseconds or picoseconds. Recently, however, the emergence of new, more efficient, nonlinear crystals and the development of continuously mode-locked, solid-state lasers, such as the Kerr-lens mode-locked Ti:sapphire laser, has led to a renaissance for OPOs. For example, the Ti:sapphire laser with an average power of over 1 W, with pulses [Formula: see text] long at a 100 MHz repetition rate, has allowed us to construct a stable, low-noise, synchronously pumped OPO. The output pulses are as short as 60 fs and can be produced in the wavelength range from 1 to 4 μm with average power as high as 200 mW. Harmonic generation of the OPO or the Ti:sapphire laser beams provides wavelength coverage from 200 nm to 4 μm. Through difference-frequency-mixing of the two output beams of the OPO in chalcopyrite or proustite crystals we anticipate being able to generate femtosecond pulses at wavelengths from 200 nm to beyond 20 μm. This broad-band, stable light source will open up new areas of investigation in physics, chemistry, and engineering.

Geodetic VLBI ultra low noise broad-band receiver for 13 meter VGOS radiotelescopes

2016 ◽  
Author(s):  
Pablo Garcia-Carreno ◽  
Sonia Garcia-Alvaro ◽  
Jose A. Lopez-Perez ◽  
Maria Patino-Esteban ◽  
Jose M. Serna ◽  
...  
Keyword(s):  
Broad Band ◽  
Low Noise ◽  
Geodetic Vlbi ◽  
Ultra Low Noise

Methods for the robust computation of the long-period seismic spectrum of broad-band arrays

2020 ◽  
Vol 222 (3) ◽  
pp. 1480-1501
Author(s):  
Ross C Caton ◽  
Gary L Pavlis ◽  
David J Thomson ◽  
Frank L Vernon
Keyword(s):  
Signal To Noise Ratio ◽  
Spectral Band ◽  
Broad Band ◽  
Low Noise ◽  
Small Aperture ◽  
Transient Signals ◽  
Seismic Arrays ◽  
Low Snr ◽  
Long Period ◽  
Student’S T

SUMMARY We describe array methods to search for low signal-to-noise ratio (SNR) signals in long-period seismic data using Fourier analysis. This is motivated by published results that find evidence of solar free oscillations in the Earth's seismic hum. Previous work used data from only one station. In this paper, we describe methods for computing spectra from array data. Arrays reduce noise level through averaging and provide redundancy that we use to distinguish coherent signal from a random background. We describe two algorithms for calculating a robust spectrum from seismic arrays, an algorithm that automatically removes impulsive transient signals from data, a jackknife method for estimating the variance of the spectrum, and a method for assessing the significance of an entire spectral band. We show examples of their application to data recorded by the Homestake Mine 3-D array in Lead, SD and the Piñon Flats PY array. These are two of the quietest small aperture arrays ever deployed in North America. The underground Homestake data has exceptionally low noise, and the borehole sensors of the PY array also have very low noise, making these arrays well suited to finding very weak signals. We find that our methods remove transient signals effectively from the data so that even low-SNR signals in the seismic background can be found and tested. Additionally, we find that the jackknife variance estimate is comparable to the noise floor, and we present initial evidence for solar g-modes in our data through the T2 test, a multivariate generalization of Student's t-test.

Design Analysis of Inductorless Active Loaded Low Power UWB LNA Using Noise Cancellation Technique

Frequenz ◽  
2020 ◽  
Vol 74 (3-4) ◽  
pp. 137-144 ◽  
Author(s):  
Dheeraj Kalra ◽  
Manish Kumar ◽  
Aasheesh Shukla ◽  
Laxman Singh ◽  
Zainul Abdin Jaffery
Keyword(s):  
Low Power ◽  
Noise Figure ◽  
Broad Band ◽  
Wide Band ◽  
Cmos Technology ◽  
Noise Cancellation ◽  
Low Noise ◽  
Design Analysis ◽  
Common Source ◽  
Power Gain

AbstractThis paper includes a design analysis of an inductorless low-power (LP) low-noise amplifier (LNA) with active load for Ultra Wide Band (UWB) applications. The proposed LNA consists of two parallel paths, one is the common source (CS) path and second is the CG path. The CG path has the edge advantage of improving overall Noise figure (NF) due to wide band impedance matching in UWB, while the CS path provides high power gain. A method for noise cancellation is adopted, to reduce the noise of CS path with the help of CG path. The proposed LNA successfully simulated in 90 nm CMOS technology. The results of proposed work indicate optimization at frequency 5.70 GHz with 3 dB bandwidth of 4.3 GHz–8.9 GHz. All simulations have been done for a range of frequency 03 GHz–13 GHz in Cadence virtuoso software. The results quoted 1.15 dB NF, −18.12 dB S11, 13.7 dB S21, maximum operating power gain (GP) 11.756 dB at frequency 5.7 GHz and available power gain (GA) is 10.17 dB at frequency 8.61 GHz, with 0.6 V, 0.92 mW broad band LNA.

ON-CHIP INDUCTORS OPTIMIZATION FOR ULTRA WIDE BAND LOW NOISE AMPLIFIERS

2011 ◽  
Vol 20 (07) ◽  
pp. 1231-1242 ◽  
Author(s):  
J. DEL PINO ◽  
SUNIL L. KHEMCHANDANI ◽  
ROBERTO DÍAZ-ORTEGA ◽  
R. PULIDO ◽  
H. GARCÍA-VÁZQUEZ
Keyword(s):  
Quality Factor ◽  
Noise Figure ◽  
Impedance Matching ◽  
Broad Band ◽  
Wide Band ◽  
Design Guidelines ◽  
Low Noise ◽  
Low Noise Amplifiers ◽  
Integrated Inductor ◽  
On Chip

In this work, the influence of the inductor quality factor in wide band low noise amplifiers has been studied. Electromagnetic simulations have been used to model the integrated inductor broad band response. The influence of the quality factor on LNA performance of the inductors that compound the impedance matching networks, inductive degeneration and broadband load has been studied, obtaining design guidelines for optimizing the amplifier gain flatness. Using this guidelines, an LNA with wideband input matching, shunt-peaking load, and an output buffer was designed. Using Austria Mikro Systems BiCMOS 0.35 m process, a prototype has been fabricated achieving the following measured specifications: maximum gain of 12.5 dB at 3.4 GHz with a -3 dB bandwidth of 1.7–5.3 GHz, noise figure from 4.3 to 5.2 dB, and unity gain at 9.4 GHz.

scholarly journals Wide-Band Tunerless Mixer Mounts for 100 GHz and 150 GHz SIS receivers

1994 ◽  
Vol 140 ◽  
pp. 78-81
Author(s):  
K. Sunada ◽  
R. Kawabe ◽  
J. Inatani
Keyword(s):  
Noise Temperature ◽  
Wide Band ◽  
Wide Frequency Range ◽  
Low Noise ◽  
Frequency Range ◽  
Sis Receiver ◽  
Embedding Impedance

AbstractThe performance of the new SIS receiver systems at the Nobeyama Millimeter Array are described. These receivers operate at 100 GHz and 150 GHz bands and tunerless mixer mounts have been adopted. These receivers show very low noise temperature (< 50 K) over a very wide frequency range because of the large embedding impedance range.

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