SuperCam, a 64-pixel heterodyne imaging array for the 870 micron atmospheric window

We report on the development of SuperCam, a 64 pixel, superheterodyne camera designed for operation in the astrophysically important 870 micron atmospheric window. SuperCam will be used to answer fundamental questions about the physics and chemistry of molecular clouds in the Galaxy and their direct relation to star and planet formation. The advent of such a system will provide an order of magnitude increase in mapping speed over what is now available and revolutionize how observational astronomy is performed in this important wavelength regime. Unlike the situation with bolometric detectors, heterodyne receiver systems are coherent, retaining information about both the amplitude and phase of the incident photon stream. From this information a high resolution spectrum of the incident light can be obtained without multiplexing. SuperCam will be constructed by stacking eight, 1x8 rows of fixed tuned, SIS mixers. The IF output of each mixer will be connected to a low-noise, broadband MMIC amplifier integrated into the mixer block. The instantaneous IF bandwidth of each pixel will be ~2 GHz, with a center frequency of 5 GHz. A spectrum of the central 500 MHz of each IF band will be provided by the array spectrometer. Local oscillator power is provided by a frequency multiplier whose output is divided between the pixels by using a matrix of waveguide power dividers. The mixer array will be cooled to 4K by a closed-cycle refrigeration system. SuperCam will reside at the Cassegrain focus of the 10m Heinrich Hertz telescope (HHT). A prototype single row of the array will be tested on the HHT in 2006, with the first engineering run of the full array in late 2007. The array is designed and constructed so that it may be readily scaled to higher frequencies.Comment: 12 pages, 14 figures, to be published in the Proceedings of SPIE Vol. 6275, "Astronomical Telescopes and Instrumentation, Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III

Seventy Years of Getting Transistorized

Vacuum tubes appeared at the break of the twentieth century giving birth to electronics. By the 1930s, they had become established as a mature technology, spreading into areas such as radio communications, long distance radiotelegraphy, radio broadcasting, telephone communication and switching, sound recording and playing, television, radar, and air navigation. During World War II, vacuum tubes were used in the first electronic computers, which were built in the United Kingdom and the United States. Although vacuum tubes had been a successful technology, they were also bulky, fragile and expensive, had a short life, and consumed a lot of power to heat the thermo-emitters. These drawbacks promoted the search for completely new devices. Alternative solutions had long been considered, but without significant developments

A 2 GHz Bandpass Analog to Digital Delta-sigma Modulator for CDMA Receivers with 79 DB Dynamic Range in 1.23 MHz Bandwidth

This paper presents the design of a second-order single-bit analog-to-digital continuous-time delta-sigma modulator that can be used in wireless CDMA receivers. The continuous-time delta-sigma modulator samples at 2 GHz, consumes 18 mW at 1.8 V and has a 79-dB signal-to-noise ratio (SNR) over a 1.23-MHz bandwidth. The continuous-time delta-sigma modulator was fabricated in a 0.18- m 1-poly 6-metal, CMOS technology and has an active area of approximately 0.892 mm2 . The delta-sigma modulator\u27s critical performance specifications are derived from the CDMA receiver specifications

Development Of Inductively-Degenerated LNA For W-CDMA Application Utilizing 0.18 Um RFCMOS Technology

Satu metodologi terperinci dan bersistematik untuk merekabentuk penguat hingar rendah (LNA) induktif ternyahjana kaskod, juga dikenali sebagai topologi Padanan Masukan dan Hingar Serentak (SNIM), A detailed and systematic methodology on the design of the inductivelydegenerated cascode LNA, also known as the Simultaneously Noise and Input Matching (SNIM) LNA

Design of Analog-to-Digital Converters with Embedded Mixing for Ultra-Low-Power Radio Receivers

In the field of radio receivers, down-conversion methods usually rely on one (or more) explicit mixing stage(s) before the analog-to-digital converter (ADC). These stages not only contribute to the overall power consumption but also have an impact on area and can compromise the receiver’s performance in terms of noise and linearity. On the other hand, most ADCs require some sort of reference signal in order to properly digitize an analog input signal. The implementation of this reference signal usually relies on bandgap circuits and reference buffers to generate a constant, stable, dc signal. Disregarding this conventional approach, the work developed in this thesis aims to explore the viability behind the usage of a variable reference signal. Moreover, it demonstrates that not only can an input signal be properly digitized, but also shifted up and down in frequency, effectively embedding the mixing operation in an ADC. As a result, ADCs in receiver chains can perform double-duty as both a quantizer and a mixing stage. The lesser known charge-sharing (CS) topology, within the successive approximation register (SAR) ADCs, is used for a practical implementation, due to its feature of “pre-charging” the reference signal prior to the conversion. Simulation results from an 8-bit CS-SAR ADC designed in a 0.13 μm CMOS technology validate the proposed technique

Studies in Software-Defined Radio System Implementation

Over the past decade, software-defined radios (SDRs) have an increasingly prevalent aspect of wireless communication systems. Different than traditional hardware radios which implement radio protocols using static electrical circuit, SDRs implement significant aspects of physical radio protocol using software programs running on a host processor. Because they use software to implement most of the radio functionality, SDRs are much more easily modified, edited, and upgraded than their hardware-defined counterparts. Consequently, researchers and developers have been developing previously hardware-defined radio systems within software. Thus, communication standards can be tested under different conditions or swapped out entirely by simply changing some code. Additionally, developers hope to implement more advanced functionality with SDRs such as cognitive radios that can sense the conditions of the environment and change parameters or protocol accordingly. This paper will outline the major aspects of SDRs including their explanation, advantages, and architecture. As SDRs have become more commonplace, many companies and organizations have developed hardware front-ends and software packages to help develop software radios. The most prominent hardware front-ends to date have been the USRP hardware boards. Additionally, many software packages exist for SDR development, including the open source GNU Radio and OSSIE and the closed source Simulink and Labview SDR packages. Using these development tools, researchers have developed many of the most relevant radio standards. This paper will explain the major hardware and software development tools for creating SDRs, and it will explain some of the most important SDR projects that have been implemented to date

Contribution to the design of continuous -time Sigma - Delta Modulators based on time delay elements

The research carried out in this thesis is focused in the development of a new class of data converters for digital radio. There are two main architectures for communication receivers which perform a digital demodulation. One of them is based on analog demodulation to the base band and digitization of the I/Q components. Another option is to digitize the band pass signal at the output of the IF stage using a bandpass Sigma-Delta modulator. Bandpass Sigma- Delta modulators can be implemented with discrete-time circuits, using switched capacitors or continuous-time circuits. The main innovation introduced in this work is the use of passive transmission lines in the loop filter of a bandpass continuous-time Sigma-Delta modulator instead of the conventional solution with gm-C or LC resonators. As long as transmission lines are used as replacement of a LC resonator in RF technology, it seems compelling that transmission lines could improve bandpass continuous-time Sigma-Delta modulators. The analysis of a Sigma- Delta modulator using distributed resonators has led to a completely new family of Sigma- Delta modulators which possess properties inherited both from continuous-time and discretetime Sigma-Delta modulators. In this thesis we present the basic theory and the practical design trade-offs of this new family of Sigma-Delta modulators. Three demonstration chips have been implemented to validate the theoretical developments. The first two are a proof of concept of the application of transmission lines to build lowpass and bandpass modulators. The third chip summarizes all the contributions of the thesis. It consists of a transmission line Sigma-Delta modulator which combines subsampling techniques, a mismatch insensitive circuitry and a quadrature architecture to implement the IF to digital stage of a receiver

The design of a two-element radio interferometer using satellite TV equipment

This research presents the design of a two-element radio interferometer capable of performing complex correlation. With the development of sophisticated radio astronomy instruments, particularly in South Africa, there is a need to develop an affordable educational instrument which can be used to demonstrate the fundamental concepts of radio interferometry to university students. The mass production of satellite TV equipment has resulted in relatively sensitive radio frequency (RF) equipment such as parabolic reflector dishes and low-noise block down-converters (LNBs) being available at significantly reduced costs. This served as the front-end of the interferometer which was used to observe the sun between 10.70 GHz - 12.75 GHz (RF). The LNB then down-converted these to an intermediate frequency (IF) between 0.95 GHz - 2.15 GHz. The LNBs were modified to make use of a common 25 MHz reference, which ensured that the observed fringes were only as a result of the source's geometric time delay. A power detector was also designed since the adding interferometer architecture was chosen. This power detector included the Analog Devices LT 5534 power detector integrated circuit (IC) and a Teensy 3.6 microcontroller. The calibrated power detector could detect signals as weak as - 60 dBm and showed less than 21 mV error in output for input signals in the range [- 50 dBm, -30 dBm]. The modified LNBs experienced issues, in particular the presence of a spurious LO signal, which distorted initial observations of the sun. This was resolved by the design and manufacture of narrowband hairpin filters and quarterwavelength stub filters which were used to isolate the IF band between 1.05 GHz - 1.15 GHz (corresponding RF between 10.80 GHz - 10.90 GHz). This also improved the interferometer's resolution. A series of filter-integrated Wilkinson power dividers and branchline couplers were designed to filter and further separate signals into in-phase and quadrature-phase (I-Q) components - these were required for complex correlation. The integrated quarter-wavelength stub filter and Wilkinson power divider achieved a maximum amplitude imbalance of 0.13 dB and phase imbalance of 0.9◦ between output ports. The integrated quarter-wavelength stub filter and branchline coupler achieved a maximum amplitude imbalance of 0.13 dB and phase imbalance of 91.1◦ between output ports. These results closely agreed with the simulated performance. First light was observed on the 5th December 2020 when the sun was successfully detected using the coherent two-element interferometer along a 1.1 m baseline. Other tests included using the observed fringe phase to verify the physical baseline. A theoretical baseline of 1.11 m was calculated for a physical baseline of 1.3 m indicating an error of less than 0.2 m. The sun's fringe frequency and amplitude was also observed for varying baselines - the sun was resolved along a 3 m baseline. Finally, full-system observations of the sun were conducted. These included observing the sun's cosine and sine fringes, which indicated that the analogue complex correlator was operating correctly. Thus, the primary goal of this project had been fulfilled. Specifically, developing a low-cost, educational two-element radio interferometer capable of detecting the sun