KEYWORDS: Comets, Receivers, Signal to noise ratio, Telescopes, Sensors, Heterodyning, Cryogenics, Solar system, Temperature metrology, Superconductors
Remote submm-wave spectrometers have the capability of providing statistically significant numbers of isotopic composition measurements within the budget constraints of available planetary missions. This talk will present a mission and instrument concept that would enable an accurate measurement of the D/H ratio on not one but several dozens of comets in a four-year mission lifetime. The instrument would utilize advanced cryogenic detectors that would allow us to measure the abundance of the para and ortho spin states of water and its isotopologues. State of the art superconducting heterodyne receivers have been developed that provide detection sensitivities approaching the quantum limit in the 500 GHz frequency range enabling the measurement of D/H ratio on around 50 comets from an observatory stationed for example at the thermally benign Lagrange point L2
We present the results from the magnetic field generation within the Kilopixel Array Pathfinder Project (KAPPa)
instrument. The KAPPa instrument is a terahertz heterodyne receiver using a Superconducting-Insulating-
Superconducting (SIS) mixers. To improve performance, SIS mixers require a magnetic field to suppress Josephson
noise. The KAPPa test receiver can house a tunable electromagnet used to optimize the applied magnetic field. The
receiver is also capable of accommodating a permanent magnet that applies a fixed field. Our permanent magnet design
uses off-the-shelf neodymium permanent magnets and then reshapes the magnetic field using machined steel
concentrators. These concentrators allow the use of an unmachined permanent magnet in the back of the detector block
while two small posts provide the required magnetic field across the SIS junction in the detector cavity. The KAPPa test
receiver is uniquely suited to compare the permanent magnet and electromagnet receiver performance. The current work
includes our design of a ‘U’ shaped permanent magnet, the testing and calibration procedure for the permanent magnet,
and the overall results of the performance comparison between the electromagnet and the permanent magnet counterpart.
Wideband receivers for the 3-mm band were developed for CARMA, the Combined Array for Research in Millimeterwave
Astronomy. Three cryogenic MMIC (monolithic microwave integrated circuit) amplifiers manufactured in InP 35-
nm technology are combined in a block with waveguide probes and gain equalizers to cover the 80–116 GHz band.
These are followed by a sideband-separating mixer that has two 17 GHZ wide outputs, for upper and lower sidebands.
Each receiver has a feed horn followed by a circular-to-linear polarizer and orthomode transducer. The two polarizations
are amplified by the cryogenic MMICs, and the outputs downconverted in sideband separating mixers, resulting in four
1–18 GHz channels that can be simultaneously correlated. The first receiver was tested in the lab, and on-sky tests
conducted at CARMA. Measured noise temperatures were in the range 40–70 K, with a sideband rejection of about
15 dB.
We report on the laboratory testing of KAPPa, a 16-pixel proof-of-concept array to enable the creation THz imaging spectrometer with ~1000 pixels. Creating an array an order of magnitude larger than the existing state of the art of 64 pixels requires a simple and robust design as well as improvements to mixer selection, testing, and assembly. Our testing employs a single pixel test bench where a novel 2D array architecture is tested. The minimum size of the footprint is dictated by the diameter of the drilled feedhorn aperture. In the adjoining detector block, a 6mm × 6mm footprint houses the SIS mixer, LNA, matching and bias networks, and permanent magnet. We present an initial characterization of the single pixel prototype using a computer controlled test bench to determine Y-factors for a parameter space of LO power, LO frequency, IF bandwidth, magnet field strength, and SIS bias voltage. To reduce the need to replace poorly preforming pixels that are already mounted in a large format array, we show techniques to improve SIS mixer selection prior to mounting in the detector block. The 2D integrated 16-pixel array design has been evolved as we investigate the properties of the single pixel prototype. Carful design of the prototype has allowed for rapid translation of single pixel design improvements to be easily incorporated into the 16-pixel model.
Supercam is a 345 GHz, 64-pixel heterodyne imaging array for the Heinrich Hertz Submillimeter Telescope
(HHSMT). By integrating SIS mixer devices with Low Noise Ampliers (LNAs) in 8 - 1x8 pixel modules, the
size needed for the cryostat and the complexity of internal wiring is signicantly reduced. All subsystems
including the optics, cryostat, bias system, IF boxes, and spectrometer have been integrated for all 64 pixels. In
the spring of 2012, SuperCam was installed on the HHSMT for an engineering run where it underwent system
level tests and performed rst light observations. In the fall of 2012 SuperCam will begin a 500 square degree
survey of the Galactic Plane in 12CO J=3-2. This large-scale survey will help answer fundamental questions
about the formation, physical conditions, and energetics of molecular clouds within the Milky Way. The data
set will be available via the web to all interested researchers.
We report on the application of a new technique for actively stabilizing the power of a far infrared gas laser as the local
oscillator (LO) in a superconducting hot electron bolometer (HEB) heterodyne receiver system at 2.5 THz. The
technique utilizes PID feedback control of the local oscillator intensity by means of a voice-coil based swing arm
actuator placed in the beam path. The HEB itself is used as a direct detector to measure incident LO power whilst
simultaneously continuing to function as heterodyne mixer. Results presented here demonstrate a factor of 50
improvement in the measured total power and spectroscopic Allan variance time. Allan times of 30 seconds and 25
seconds respectively are shown for large and small area HEB's with a measured effective noise fluctuation bandwidth of
12 MHz. The technique is versatile and can be applied to any LO source and at any LO frequency.
KAPPa (the Kilopixel Array Pathfinder Project) is developing key technologies to enable the construction of heterodyne
focal plane arrays in the terahertz frequency regime with ~1000 pixels. The leap to ~1000 pixels requires solutions to
several key technological problems before the construction of such a focal plane is possible. The KAPPa project will
develop a small (16-pixel) 2D integrated heterodyne focal plane array for the 660 GHz atmospheric window as a
technological pathfinder towards future kilopixel heterodyne focal plane arrays.
KEYWORDS: Double sideband modulation, Temperature metrology, Receivers, Waveguides, Fourier transforms, Amplifiers, Single sideband modulation, Astronomy, Signal to noise ratio, Prototyping
The ALMA Band 9 receiver cartridge (600-720 GHz) based on Dual Sideband (DSB) superconductor-insulatorsuperconductor
(SIS) mixer is currently in full production. In the case of spectral line observations, the integration time
to reach a certain signal-to-noise level can be reduced by about a factor of two by rejecting an unused sideband. The goal
is to upgrade the current ALMA band 9 cartridge to a full dual-polarization sideband separating (2SB) capability, with
minimal-cost upgrade path. A new compact and modular sideband separating mixer was designed, and a prototype
manufactured. The individual SIS mixer devices in the 2SB block are implemented as conventional Band 9 DSB mixers,
so that existing devices can be reused and tested individually. Any ALMA DSB developments contribute to the 2SB
upgrade. The first experimental results demonstrate noise temperature from 300K to 500K over 80% of the band, which
will be improved to fit the ALMA requirements. Nevertheless, the frequency response for 2SB is the same as for DSB,
showing that the RF design is still valid, even with different SIS mixer devices. The quality of the RF and IF design is
confirmed by a sideband rejection ratio of about 15 dB, which is within the ALMA spec (>10dB ).
Kinetic Inductance Detectors (KIDs) with frequency domain read-out are intrinsically very suitable to use as
building blocks for very large arrays. KIDs therefore are an attractive detector option for the SAFARI instrument on
SPICA, Millimetron and also for large scale ground based imaging arrays. To study the properties of large KID
arrays we have fabricated 400 pixels array made from 40 nm thick Al films on high resistivity Si substrates. The
array is tested in a dry dilution refrigerator at 100 mK. We present the device design and experimental results. We
also present a new design of the array with lithographic air bridges over the coplanar waveguide feedline. The air
bridges are designed to suppress the slot line mode in the feedline and that will improve the pixel to pixel
reproducibility of large arrays.
The Stratospheric TeraHertz Observatory (STO) is a NASA funded, Long Duration Balloon (LDB) experiment designed to
address a key problem in modern astrophysics: understanding the Life Cycle of the Interstellar Medium (ISM). STO will
survey a section of the Galactic plane in the dominant interstellar cooling line [C II] (1.9 THz) and the important star
formation tracer [N II] (1.46 THz) at ~1 arc minute angular resolution, sufficient to spatially resolve atomic, ionic and
molecular clouds at 10 kpc. STO itself has three main components; 1) an 80 cm optical telescope, 2) a THz instrument
package, and 3) a gondola [1]. Both the telescope and gondola have flown on previous experiments [2,3]. They have been reoptimized
for the current mission. The science flight receiver package will contain four [CII] and four [NII] HEB mixers,
coupled to a digital spectrometer. The first engineering test flight of STO was from Ft. Sumner, NM on October 15, 2009.
The ~30 day science flight is scheduled for December 2011.
We report on both laboratory and telescope integration results from SuperCam, a 64 pixel imaging spectrometer
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 SuperCam key project is a fully sampled Galactic plane survey covering over
500 square degrees of the Galaxy in 12CO(3-2) and 13CO(3-2) with 0.3 km/s velocity resolution
In the past, all heterodyne focal plane arrays have been constructed using discrete mixers, arrayed in the focal plane.
SuperCam reduces cryogenic and mechanical complexity by integrating multiple mixers and amplifiers into a single
array module with a single set of DC and IF connectors. These modules are housed in a closed-cycle cryostat with a
1.5W capacity 4K cooler. The SuperCam instrument is currently undergoing laboratory testing with four of the eight
mixer array modules installed in the cryostat (32 pixels). Work is now underway to perform the necessary modifications
at the 10m Heinrich Hertz Telescope to accept the SuperCam system. SuperCam will be installed in the cassegrain cabin
of the HHT, including the optical system, IF processing, spectrometers and control electronics. SuperCam will be
integrated with the HHT during the 2009-2010 observing season with 32 pixels installed. The system will be upgraded to
64 pixels during the summer of 2010 after assembly of the four additional mixer modules is completed.
The Heterodyne Instrument for the Far-Infrared (HIFI) is one of three instruments to be launched aboard the
Herschel Space Observatory (HSO) in 2009. HIFI will provide unprecedented spectral sensitivity and resolution
between 490-1250 GHz and 1410-1910 GHz. In this paper, we report on the analysis of electrical standing waves
that are present between the hot electron bolometer (HEB) heterodyne mixing element and the first low noise
amplifier in the HIFI instrument. We show that the standing wave shape is not a standard sinusoid and difficult
to remove from the resulting spectrum using standard fitting methods. We present a method to remove the
standing waves based on data taken during the HIFI instrument level test, and anticipate the use of a similar
calibration procedure in actual flight. Using the standing wave profile we obtain direct evidence of the complex
IF output impedance of the HEB mixer.
We report on the development of SuperCam, a 64 pixel imaging spectrometer 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 Supercam key project is a fully sampled Galactic plane survey covering over 500 square degrees of the Galaxy in
12CO(3-2) and 13CO(3-2) with 0.3 km/s velocity resolution.
7010-5Thijs de Graauw, Nick Whyborn, Frank Helmich, Pieter Dieleman, Peter Roelfsema, Emmanuel Caux, Tom Phillips, Jürgen Stutzki, Douwe Beintema, Arnold Benz, Nicolas Biver, Adwin Boogert, Francois Boulanger, Sergey Cherednichenko, Odile Coeur-Joly, Claudia Comito, Emmanuel Dartois, Albrecht de Jonge, Gert de Lange, Ian Delorme, Anna DiGiorgio, Luc Dubbeldam, Kevin Edwards, Michael Fich, Rolf Güsten, Fabrice Herpin, Netty Honingh, Robert Huisman, Herman Jacobs, Willem Jellema, Jon Kawamura, Do Kester, Teun Klapwijk, Thomas Klein, Jacob Kooi, Jean-Michel Krieg, Carsten Kramer, Bob Kruizenga, Wouter Laauwen, Bengt Larsson, Christian Leinz, Rene Liseau, Steve Lord, Willem Luinge, Anthony Marston, Harald Merkel, Rafael Moreno, Patrick Morris, Anthony Murphy, Albert Naber, Pere Planesas, Jesus Martin-Pintado, Micheal Olberg, Piotr Orleanski, Volker Ossenkopf, John Pearson, Michel Perault, Sabine Phillip, Mirek Rataj, Laurent Ravera, Paolo Saraceno, Rudolf Schieder, Frank Schmuelling, Ryszard Szczerba, Russell Shipman, David Teyssier, Charlotte Vastel, Huib Visser, Klaas Wildeman, Kees Wafelbakker, John Ward, Roonan Higgins, Henri Aarts, Xander Tielens, Peer Zaal
This paper describes the Heterodyne Instrument for the Far-Infrared (HIFI), to be launched onboard of ESA's Herschel Space Observatory, by 2008. It includes the first results from the instrument level tests. The instrument is designed to be electronically tuneable over a wide and continuous frequency range in the Far Infrared, with velocity resolutions better than 0.1 km/s with a high sensitivity. This will enable detailed investigations of a wide variety of astronomical sources, ranging from solar system objects, star formation regions to nuclei of galaxies.
The instrument comprises 5 frequency bands covering 480-1150 GHz with SIS mixers and a sixth dual frequency band, for the 1410-1910 GHz range, with Hot Electron Bolometer Mixers (HEB). The Local Oscillator (LO) subsystem consists of a dedicated Ka-band synthesizer followed by 7 times 2 chains of frequency multipliers, 2 chains for each frequency band. A pair of Auto-Correlators and a pair of Acousto-Optic spectrometers process the two IF signals from the dual-polarization front-ends to provide instantaneous frequency coverage of 4 GHz, with a set of resolutions (140 kHz to 1 MHz), better than < 0.1 km/s. After a successful qualification program, the flight instrument was delivered and entered the testing phase at satellite level. We will also report on the pre-flight test and calibration results together with the expected in-flight performance.
We report on the development of SuperCam, a 64 pixel, superheterodyne camera designed for operation in the astrophysically important 870 μm 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, 1×8 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.
Balanced receivers are under development at the Caltech Submillimeter Observatory (CSO) for the 230/460 GHz and 345/660 GHz atmospheric windows. The mixers are tunerless, implemented in a balanced configuration, have a 4-8 GHz IF, and can be used in dual frequency observation mode. As shall be seen, the balanced arrangement provides a high level of amplitude noise immunity and allows all of the available LO power to be used. In turn, this permits complete automation of the receivers by means of synthesized LO source(s).
A disadvantage of balanced mixers is, perhaps, that the sidebands at the IF remain convolved (DSB), unlike sideband separating (2SB) receivers. The latter, however are unbalanced and do not have the noise and LO injection advantages of balanced mixers. For the CSO, balanced mixers covering the range 180-720 GHz were judged most promising to facilitate many of the astrophysical science goals in the years to come.
In parallel, a dual polarization 280-420~GHz continuous comparison (correlation) receiver is in an advanced state of development. The instrument has two beams on the sky; a reference and a signal beam. Using only cooled reflecting optics, two polarizing grids, and a quadrature hybrid coupler, the sky beams are coupled to four tunerless SIS mixers (both polarizations). The 4-12 GHz mixer IF outputs are, after amplification, correlated against each other. In principle, this technique results in flat baselines with very low RMS noise, and is especially well suited for high redshift Galaxy work.
Not only do these changes greatly enhance the spectroscopic capabilities of the CSO, they will also enable the observatory to be integrated into the Harvard-Smithsonian Submillimeter Array (SMA), as an additional telescope.
We present the first astronomical results from DesertSTAR, a 7 pixel heterodyne array receiver designed for operation in the astrophysically rich 345 GHz atmospheric window. DesertSTAR was constructed for the 10m Heinrich Hertz Telescope located at 3150m elevation on Mt. Graham, Arizona. This receiver promises to increase mapping speed at the HHT by a factor of ~15 over the facility's existing single beam, dual polarization receiver. DesertSTAR uses tunerless, single-ended waveguide SIS mixers to achieve uncorrected receiver noise temperatures of ~60K. The instantaneous bandwidth is 2 GHz, with a 5 GHz Intermediate Frequency, offering 1600 km/s of velocity coverage. Cryogenic isolators are employed between the mixers and low noise amplifiers to assure a flat IF passband. The system uses a Joule-Thompson closed-cycle refrigerator with 180W capacity at 70K and 1.8W capacity at 4K. A novel reflective phase grating is used for Local Oscillator multiplexing, while a simple Mylar beamsplitter is used as an LO diplexer. Optics include only polyethelene mixer lenses and a single, cold, flat mirror, maximizing simplicity for high efficiency and easy optical alignment. The computer controlled bias system provides low noise bias for the SIS junctions, magnets and LNAs through a modular and hardware independent GUI interface, and allows remote operation and monitoring. We present measurements of receiver noise, beam quality, efficiency and stability in addition to astronomical observations obtained during engineering runs at the HHT.
KEYWORDS: Receivers, Terahertz radiation, Far infrared lasers, Bolometers, Signal detection, Oscillators, Superconductors, Solid state lasers, Solid state physics, Heterodyning
Stability of a hot-electron bolometer (HEB) heterodyne receiver was investigated at frequencies from 0.6THz to 1.9THz. The Allan variance was measured as a function of the integration time and the Allan time was obtained for HEB mixers of different size, as well as with different types of the local oscillator: FIR laser, multiplier chain, and BWO. We have found that due to stronger dependence of the mixer gain and noise vs mixer bias voltage and current the Allan time is shorter for smaller mixers. At 1.6THz the Allan time is 3 sec for 4x0.4μm2 bolometer, and 0.15-0.2 sec for 1x0.15μm2 bolometer. Obtained stability apears to be the same for the FIR laser and the mulitplier chain. The Allan time for smaller bolometers increases to 0.4-0.5sec at 0.6-0.7THz LO frequencies. The influence of the IF chain on the obtained results is also analyzed.
We have proposed to develop a prototype 0.5-meter far-infrared telescope and heterodyne receiver/spectrometer system for fully-automated remote operation at the summit of Dome A, the highest point on the Antarctic plateau. The unparalleled stability, exceptional dryness, low wind and extreme cold make Dome A a ground-based site without equal for astronomy at infrared and submillimeter wavelengths. HEAT, the High Elevation Antarctic Terahertz Telescope, will operate in the atmospheric windows between 150 and 400 microns, in which the most crucial astrophysical spectral diagnostics of the formation of galaxies, stars, planets, and life are found. At these wavelengths, HEAT will have high aperture efficiency and excellent atmospheric transmission most of the year. The proposed superheterodyne receiver system will be comprised of 0.8, 1.4 and 1.9 THz channels which will observe the pivotal J=7-6 line of CO, the J=2-1 line of atomic carbon, and the far-infrared fine structure lines of N+ and C+, the brightest emission lines in the entire Milky Way Galaxy. When combined with the HEAT telescope, the receiver system represents a uniquely powerful instrument for reconstructing the history of star formation in our Galaxy, with application to the distant Universe. The receiver system itself serves as a valuable testbed for heterodyne Terahertz components, using leading-edge mixer, local oscillator, low-noise amplifier, cryogenic, and digital signal processing technologies that will play essential roles in future Terahertz observatories. The proposed study will pave the way for future astronomical investigations from Dome A.
Under development at the Caltech Submillimeter Observatory is a dual polarization, continuous comparison (correlation) receiver. The instrument has two beams on the sky; a reference and a signal beam. Using only cooled reflecting optics, two polarizing grids, and a quadrature hybrid coupler, the sky beams are coupled to four tunerless SIS mixers (both polarizations). The 4-8 GHz mixer IF outputs are, after amplification, correlated against each other. In principle, this technique results in flat baselines with very low RMS noise and is especially well suited for high redshift Galaxy work. At the same time an upgrade is planned to the existing facility heterodyne instrumentation. Dual frequency mode receivers are under development for the 230/460 GHz and 345/660 GHz atmospheric windows. The higher frequency receivers are implemented in a balanced configuration, which reduces both the LO power requirement and noise. Each mixer has 4 GHz of IF bandwidth and can be controled remotely.
Not only do these changes greatly enhance the spectroscopic capabilities of the CSO, they also enable the observatory to be integrated into the Harvard-Smithsonian Submillimeter Array (SMA) as an additional baseline.
The advent of large format (~100 pixel) spectroscopic imaging cameras at submillimeter wavelengths would fundamentally change the way in which astronomy is performed in this important wavelength regime. While the possibility of such instruments has been discussed for more than two decades, only recently have advances in mixer technology, device fabrication, micromachining, digital signal processing, and telescope design made the construction of such an instrument possible and economical. In our paper, we will present the design concept for a
10×10 heterodyne camera.
Rolf Guesten, Geoffrey Ediss, Frederic Gueth, K. Gundlach, H. Hauschildt, Christoph Kasemann, Thomas Klein, Jacob Kooi, A. Korn, I. Kramer, Henry LeDuc, H. Mattes, K. Meyer, E. Perchtold, M. Pilz, R. Sachert, M. Scherschel, P. Schilke, G. Schneider, J. Schraml, Detlef Skaley, Ronald Stark, W. Wetzker, H. Wiedenhover, W. Wiedenhover, S. Wongsowijoto, F. Wyrowski
A 16-element SIS heterodyne array for operation in the 625 micrometer atmospheric window is under development at the MPIfR. The array consists of 2 X 8 elements with closest feasible spacing of the pixels on the sky ((root)2 (DOT) (Theta) mb). The L.O. tuning range covers the astronomically important CI and the CO(4-3) transitions, and an IF bandwidth of 2 GHz (1200 kms-1) will permit mapping of extragalactic systems. For best system sensitivity the design allows for cold optics ( 15K) and single-sideband operation. The frontend will be linked to a flexible autocorrelator, with a maximum bandwidth of 2 GHz (2048 channels) for each of the 16 modules. In the high-resolution mode, 500 MHz of bandwidth can be operated with 8192 channels of 61 kHz spectral resolution. System components are currently undergoing final integration and critical evaluation in our laboratories. First astronomical commissioning is scheduled for later this year. The sensitivity expected with CHAMP, for e.g. carbon studies, will be unparalleled. With the full array in SSB operation the mapping speed will be enhanced by a factor of 50 - 100 compared to current single-pixel detectors.
SIS heterodyne mixer technology based on niobium tunnel junctions has now been pushed to frequencies over 1 THz, clearly demonstrating that the SIS junctions are capable of mixing at frequencies up to twice the energy gap frequency (4(Delta) /h). However, the performance degrades rapidly above the gap frequency of niobium (2(Delta) /h approximately equals 700 GHz) due to substantial ohmic losses in the on-chip tuning circuit. To solve this problem, the tuning circuit should be fabricated using a superconducting film with a larger energy gap, such as NbN; unfortunately, NbN films often have a substantial excess surface resistance in the submillimeter band. In contrast, the SIS mixer measurements we present in this paper indicate that the losses for NbTiN thin films can be quite low.
The Caltech Submillimeter observatory (CSO) is one of the World's premier submillimeter telescopes. It consists of a 10.4 meter diameter Leighton radio dish situated in compact dome near the summit of Mauna Kea, Hawaii. The telescope has been operating under a contract from the National Science Foundation on a regular basis since 1988. For the first time heterodyne Superconducting-Insulating-Superconducting (SIS) receivers with a 1 GHz intermediate frequency (IF) are available for the entire 180 - 950 GHz Submillimeter band. To enhance the extra-galactic capabilities of the observatory and to allow interferometry with the upcoming Submillimeter Array (SMA) project, we are actively working towards upgrading all heterodyne instruments with a 3 GHz IF bandwidth. Concurrent to the planned IF upgrade, we are constructing a dual polarization beam switching 345 GHz extra-galactic receiver, also with a 3 GHz IF bandwidth. Ideally, this instrument will give the CSO a factor of 8 improvement in integration time over the current 345 GHz receiver, and will be ideally suited for the study of highly red-shifted extra-galactic sources.
We report on the performance of power amplifiers as local oscillator drivers for millimeter and submillimeter-wave receivers. A MMIC power amplifier based on 0.1 micron GaAs HEMT technology on 50 micron thick substrate has been packaged in a waveguide block and characterized. Output power in excess of 100 mW is demonstrated over 88 - 94 GHz with more power easily achievable. The noise properties of the MMIC amplifier in multiplied local oscillator chains are characterized in a low noise superconductor-insulator-superconductor mixer based heterodyne receiver. A 386 GHz SIS mixer was used to characterize noise temperature in a laboratory environment. A more sensitive measurement of noise contribution from the amplifier was performed on a 278 GHz mixer/receiver at the Caltech Submillimeter-Wave Observatory, during astronomical observations. It is concluded that the MMIC amplifier does not add additional significant noise to the radiometer system.
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