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Research > Instrumentation Research

Instrumentation Research

Some of the key people associated with the Greenland Telescope (GLT) project posting in front of the ALMA NA prototype antenna.The GLT project will retrofit and redeploy this antenna to Greenland. Several of the major antenna components require new design, revision, or retrofitting to survive the extreme cold environment, on the ice sheet of Greenland. This project, with the antenna located in US now and moved to Greenland later, posts some great challenge in management and technology that we have never faced before.
Some of the key people associated with the Greenland Telescope (GLT) project posting in front of the ALMA NA prototype antenna
The filter exchanger of Subaru Hyper SuprimeCam inside the Subaru telescope dome.
Filter exchanger for Subaru HSC
Hyper SuprimeCam installed on Subaru telescope
Hyper SuprimeCam (HSC) of Subaru
The performances of developed SIS mixers for KVN, SMA, and ALMA band-10 mixers. The noise of receiver, tested in lab, includes the noise contribution of IF chain of 10K.
The performances of developed SIS mixers for two SMA telescopes
A Cryogenically coolde 31-50GHz Metamorphic High-Electron-Mobility Transistor (MHEMT) monolithic microwave integrated circuit (MMIC) low-noise amplifier (LNA) Modules has been developed for ALMA Band-1 receiver key component development.
Cryogenically coolde 31-50GHz MHEMT MMIC LNA Modules
The 31 - 50 GHz Cryogenic HEMT Cascode mixer was developed in ASIAA Microwave Device Laboratory for the ALMA Band-1 Receiver Key component development. The mixer is with very low conversion loss and even some positive conversion gain over very broadband frequency range.
31 - 50 GHz Cryogenic HEMT Cascode Mixer
The one baseline digital correlator is under testing on AMIBA now. Employed the ROACH2 by CASPER community as the platform and used two of our own 5 Gsps ADCs to digitize the signals from 2 antennae.
One baseline digital correlator
10 Giga samples per second Analog to Digital Printed Circuit Board is developing by digital group of the Institute.
10 Gsps Analog to Digital Converter
The mixer is fabricated using ASIAA junction process. The performance is verified by NAOJ band-10 team. The receiver noise temperature is quite close to the specifications of ALMA band-10 reciever.
ALMA band-10 mixer made in ASIAA
The AMiBA project, observing at 3 mm wavelength, is an important initiative to develop our observational cosmology program in a very competitive field of science. This project has challenged several novel technological difficulties, such as the 16-GHz, wide-band analog correlator, an unprecedented size of Steward mount, and a 6-meter, detachable, composite-material platform.
The 7-element vs. 13-element AMiBA on the Mauna Loa Observatory, Hawaii
The AMiBA project, observing at 3 mm wavelength, is an important initiative to develop our observational cosmology program in a very competitive field of science. This project has challenged several novel technological difficulties, such as the 16-GHz, wide-band analog correlator, an unprecedented size of Steward mount, and a 6-meter, detachable, composite-material platform.
The 7-element vs. 13-element AMiBA on the Mauna Loa Observatory, Hawaii
The AMiBA project, observing at 3 mm wavelength, is an important initiative to develop our observational cosmology program in a very competitive field of science. This project has challenged several novel technological difficulties, such as the 16-GHz, wide-band analog correlator, an unprecedented size of Steward mount, and a 6-meter, detachable, composite-material platform.
The 7-element vs. 13-element AMiBA on the Mauna Loa Observatory, Hawaii
A niobium SIS mixer developed in ASIAA to operate at 850 GHz. The establishment of the SIS fabrication facility in ASIAA is one of the most important milestones in the SMA project. Not only does it securely supply key components in the SMA, it also leads
A niobium SIS mixer developed in ASIAA to operate at 850 GHz
The Submillimeter Array, an eight-element radio telescope ensemble in the foreground of the figure, is currently one of the most powerful telescopes directly accessible by the astronomers in Taiwan. With its observing frequency of 180 - 690 GHz, the SMA i
The Submillimeter Array
The Submillimeter Array, an eight-element radio telescope ensemble in the foreground of the figure, is currently one of the most powerful telescopes directly accessible by the astronomers in Taiwan. With its observing frequency of 180 - 690 GHz, the SMA i
The Submillimeter Array
The Submillimeter Array, an eight-element radio telescope ensemble in the foreground of the figure, is currently one of the most powerful telescopes directly accessible by the astronomers in Taiwan. With its observing frequency of 180 - 690 GHz, the SMA i
The Submillimeter Array
A MMIC Layout of a voltage-control-oscillator ready for fabrication in a local semiconductor foundry. This is a development project to facilitate our MMIC design and fabrication capability, which may benefit the construction of the Atacama Large Millimete
A MMIC Layout of a voltage-control-oscillator

ASIAA has always focused on developing forefront technology programs which will drive the next generation of instruments. In our first decade, ASIAA concentrated on establishing a strong research program in radio astronomy. The assembly of a strong team which can develope its expertise in millimeter and submillimeter wavelength technologies has been the driver for the Submillimeter Array (SMA), the Anisotropy Microwave Background Array (AMiBA), and the Atacama Large Millimeter/submillimeter Array (ALMA) programs. The technical group now has a broad range of capabilities, including superconductor-insulator-superconductor mixers and Superconducting Quantum Interference Device (SQUID) chips, Monolithic Microwave Integrated Circuit (MMIC) devices, IF electronics, cryogenics, correlator, submillimeter wavelength antennas, carbon fiber reflectors, and control software.

In our second decade, ASIAA began to develop a technical group in optical/infrared (OIR) wavelengths. This assembled team has been the driver for the TAOS and CFHT/WIRCam programs. The success of WIRCam collaboration brought the experience of array testing and control electronics to the core expertise of the OIR laboratory. With such expertise, we continue to work on advanced instrumentation project in large telescopes, such as Spectropolarimètre Infra-Rouge (SPIROU) of CFHT and Hyper SuprimeCam (HSC) and Prime Focus Spectrograph (PFS) of Subaru telescope. Negotiation with Japanese space agency JAXA to join the next generation infrared satellite project Space Infrared telescope for Cosmology and Astrophysics (SPICA) is ongoing. In addition, working on the future thirty-meter class telescope instruments is also planned.

The research of instrumentation in ASIAA includes receiver technology development, microwave device design and assembly, superconducting device development, and OIR detector array development. ASIAA will continue to expand on its technical development groups, with the goal of increasing capabilities in detection sensitivity in various domains.

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