KEYWORDS: Receivers, Optical amplifiers, Radio astronomy, Antennas, Astronomy, Observatories, Cryogenics, Simulation of CCA and DLA aggregates, Roads, Galactic astronomy
The Atacama large millimeter/submillimeter array (ALMA) band-1 receiver covers the frequency band between 35-50 GHz. An extension of up to 52 GHz is on a best-effort basis. Covering the longest wavelengths visible with ALMA, this receiver is enabling studies of dust grain evolution in proto-planetary systems probing dust grain sizes close to 1 cm, and with multiple red-shifted molecular lines it will open up a new window in the high-redshift universe. The band-1 project has recently achieved first light and with this passed a major project milestone. We present the challenges, from initial development to prototype, to establishing the infrastructure, integration, and evaluation of 73 production receiver units, and to the final tasks to complete the project. We conclude with the initial performance and characterization of the first band-1 receivers installed on ALMA.
We present the results of a digital calibration technique applied to an Atacama Large Millimeter/submillimeter Array sideband separating wideband astronomical receiver of 275 to 500 GHz radio frequency (RF) and 3 to 22 GHz intermediate frequency bandwidth. The calibration technique consists of computing the magnitude ratio and the phase difference of the receiver output, and then applying correction constants to the digitized signals. Two analog-digital converters are used to digitize the signals and an field-programmable gate array for the processing. No modification in the analog receiver is required to apply the calibration, as it works directly on upper sideband/lower sideband signals. The technique improved the receiver temperature compared with the double sideband case by increasing the sideband rejection ratio by around 30 dB on average. It is shown that even more rejection can be obtained with more careful control of the RF calibration input power.
The Atacama Large Millimeter/submillimeter Array (ALMA) Band 1 receiver covers the frequency range of 35-50 GHz. An extension of up to 52 GHz is on a best-effort basis. A total of 73 units have to be built in two phases: 8 preproduction and then 65 production units. This paper reports on the assembly, testing, and performance of the preproduction Band 1 receiver. The infrastructure, integration, and evaluation of the fully-assembled Band 1 receiver system will be covered. Finally, a discussion of the technical and managerial challenges encountered for this large number of receivers will be presented.
The Atacama Large Millimeter/submillimeter Array(ALMA) Band 1 receiver covers the 35-50 GHz frequency band. Development of prototype receivers, including the key components and subsystems has been completed and two sets of prototype receivers were fully tested. We will provide an overview of the ALMA Band 1 science goals, and its requirements and design for use on the ALMA. The receiver development status will also be discussed and the infrastructure, integration, evaluation of fully-assembled band 1 receiver system will be covered. Finally, a discussion of the technical and management challenges encountered will be presented.
KEYWORDS: Telescopes, Receivers, Amplifiers, Extremely high frequency, Calibration, Spectroscopy, Control systems, Microcontrollers, Servomechanisms, Analog electronics
Here we describe the status of the upgrade program that is being performed to modernize the Southern 1.2m
Wave Telescope. The Telescope was built during early ´80 to complete the first Galactic survey of Molecular
Clouds in the CO(1-0) line. After a fruitful operation in CTIO the telescope was relocated to the Universidad
de Chile, Cerro Calán Observatory. The new site has an altitude of 850m and allows observations in the
millimeter range throughout the year. The telescope was upgraded, including a new building to house
operations, new control system, and new receiver and back-end technologies. The new front end is a
sideband-separating receiver based on a HEMT amplifier and sub-harmonic mixers. It is cooled with Liquid
Nitrogen to diminish its noise temperature. The back-end is a digital spectrometer, based on the
Reconfigurable Open Architecture Computing Hardware (ROACH). The new spectrometer includes IF
hybridization capabilities to avoid analog hybrids and, therefore, improve the sideband rejection ratio of the
receiver.
KEYWORDS: Polarization, Field programmable gate arrays, Receivers, Calibration, Analog electronics, Signal processing, Spectroscopy, Digital signal processing, Radio astronomy, Telescopes
Field Programmable Gate Arrays (FPGAs) capacity and Analog to Digital Converters (ADCs) speed have largely increased in the last decade. Nowadays we can find one million or more logic blocks (slices) as well as several thousand arithmetic units (ALUs/DSP) available on a single FPGA chip. We can also commercially procure ADC chips reaching 10 GSPS, with 8 bits resolution or more. This unprecedented power of computing hardware has allowed the digitalization of signal processes traditionally performed by analog components. In radio astronomy, the clearest example has been the development of digital sideband separating receivers which, by replacing the IF hybrid and calibrating the system imbalances, have exhibited a sideband rejection above 40dB; this is 20 to 30dB higher than traditional analog sideband separating (2SB) receivers. In Rodriguez et al.,1 and Finger et al.,2 we have demonstrated very high digital sideband separation at 3mm and 1mm wavelengths, using laboratory setups. We here show the first implementation of such technique with a 3mm receiver integrated into a telescope, where the calibration was performed by quasi-optical injection of the test tone in front of the Cassegrain antenna. We also reported progress in digital polarization synthesis, particularly in the implementation of a calibrated Digital Ortho-Mode Transducer (DOMT) based on the Morgan et al. proof of concept.3 They showed off- line synthesis of polarization with isolation higher than 40dB. We plan to implement a digital polarimeter in a real-time FPGA-based (ROACH-2) platform, to show ultra-pure polarization isolation in a non-stop integrating spectrometer.
The ALMA Band-1 receiver front-end prototype cold and warm cartridge assemblies, including the system and key
components for ALMA Band-1 receivers have been developed and two sets of prototype cartridge were fully tested. The
measured aperture efficiency for the cold receiver is above the 80% specification except for a few frequency points.
Based on the cryogenically cooled broadband low-noise amplifiers provided by NRAO, the receiver noise temperature
can be as low as 15 – 32K for pol-0 and 17 – 30K for pol-1. Other key testing items are also measured. The receiver
beam pattern is measured, the results is well fit to the simulation and design. The pointing error extracted from the
measured beam pattern indicates the error is 0.1 degree along azimuth and 0.15 degree along elevation, which is well fit
to the specification (smaller than 0.4 degree). The equivalent hot load temperature for 5% gain compression is 492 -
4583K, which well fit to the specification of 5% with 373K input thermal load. The image band suppression is higher
than 30 dB typically and the worst case is higher than 20 dB for 34GHz RF signal and 38GHz LO signal, which is all
higher than 7 dB required specification. The cross talk between orthogonal polarization is smaller than -85 dB based on
present prototype LO. The amplitude stability is below 2.0 x 10-7 , which is fit to the specification of 4.0 x 10-7 for
timescales in the range of 0.05 s ≤ T ≤ 100 s. The signal path phase stability measured is smaller than 5 fs, which is
smaller than 22 fs for Long term (delay drift) 20 s ≤ T < 300 sec. The IF output phase variation is smaller than 3.5° rms
typically, and the specification is less than 4.5° rms. The measured IF output power level is -28 to -30.5 dBm with 300K
input load. The measured IF output power flatness is less than 5.6 dB for 2GHz window, and 1.3dB for 31MHz window.
The first batch of prototype cartridges will be installed on site for further commissioning on July of 2017.
KEYWORDS: Receivers, Oscillators, Waveguides, Prototyping, Amplifiers, Optical amplifiers, Antennas, Optical isolators, Field effect transistors, Simulation of CCA and DLA aggregates
The prototype cartridges for ALMA Band-1 receivers have been developed, based on the key components developed in ALMA Band-1 consortium laboratories. The prototype cartridges for each receiver consist of two parts, cold cartridge assembly and warm cartridge assembly. The cold cartridge assembly (CCA) consists of horn antenna, orthomode transducer and a pair of 35-52 GHz cold low-noise amplifiers, the amplified signals of both polarizations are transmitted to warm cartridge assembly by long waveguide sections. In warm cartridge assembly (WCA), two major modules incorporated, down-converter assembly including warm low-noise amplifier, high-pass filter, mixer and 4-12 GHz IF amplifier, and local oscillator based on a 31-40 GHz YIG-tunes oscillator. The frequency range is based on the upper sideband scheme. Based on the measured performance of the key components, the expected noise performance of the receiver will be 26-33K.
Sideband-separating receivers are usually preferred in the presence of high atmospheric noise. However, one of the most important figures of merit for this kind of receiver, the sideband ratio, is still low and typically around 10 dB. This is because keeping low amplitude and phase imbalances over large RF and IF frequencies is extremely difficult. However, by introducing a digital back-end that mimics the performance of an IF-hybrid, such imbalances can be calibrated out. We have recently presented a digital sideband-separating receiver, working at the W band, that can achieve sideband ratios well above 35 dB. Here we extend this work by demonstrating that it can also be applied to receivers that incorporate a second down-conversion stage with the same performance.
KEYWORDS: Receivers, Telescopes, Spectroscopy, Field effect transistors, Diodes, Digital signal processing, Astronomy, Signal processing, Computer architecture, Analog electronics
In this paper we describe the status of an upgrading program that it is being carried out to modernize the front
and back ends of the Southern 1.2-m mm-Wave Telescope to cover eciently the band from 86 to 115 GHz. On
the one hand, the new front end will have a sideband-separating conguration to suppress the image band noise.
This front end will use one low noise amplier and two Schottky diodes for down conversion. On the other hand,
we are developing a modern digital spectrometer, based on the Recongurable Open Architecture Computing
Hardware (ROACH), to ease the operation and improve the spectral resolution up to a factor of 4. Moreover,
the spectrometer will include IF hybridization capabilities to avoid analog hybrids and, therefore, improve the
sideband rejection ratio of the receiver.
The lowest spectroscopic band devised for the Atacama Large Millimeter Array (ALMA), the so-called Band 1,
covers the frequency range from 31 to 45 GHz. This band was not implemented during the rst construction
phase of the telescope, but will be included during a second ALMA development phase. During the past 4
years our group has been working on the development of technology to cover this band, complying with the
demanding ALMA specications. Among the most burdensome challenges are the stringent specications on
noise temperature, the large required bandwidth, and the limited space available for this receiver within the
ALMA cryostat. In this paper we present some of the technologies we have developed, including the design of
key components like horn, lens, ortho-mode transducer, and low noise ampliers. We also present an evaluation
of third-party components which can be used in the receiver. The work is used to present a preliminary layout
of the Band 1 receiver.
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