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Internal photos of Laser Synthesizer instrument: left - top view of optical circuitry including Erbium Doped Fiber Amplifier and custom Fiber Bragg Grating filter assembly; right - bottom view of RF power amplifier, Mach-Zehnder modulator, DC power supplies (x3), and monitor & control. Developed at the SMA project office by Derek Kubo and Ranjani Srinivasan in collaboration with NAOJ, this instrument was designed to provide a pure optical local oscillator reference for distribution over long distances of optical fiber (Kubo et al. Aug 2013, IEEE T Microw Theory: 61(8), 3005-3014).
MZM Laser Synthesizer LO Source
The cryostat chamber mounted on an alumina holding structure (The dewar frame) shown in the center of the picture. Except for few instruments fixed on the dewar frame, most frontend hardware is installed into 36U height rack that locates on dewar left and right side. The vacuum pump sits under the dewar with long bellow pipe connect to the dewar chamber.
GLT Frontend System
The SMA antenna built in Taiwan.
The SMA antenna built in Taiwan.
Cleaned SZE images of clusters observed by seven-element AMiBA. The white circles indicate the half-maximum contour of the primary beam (the field of view; 23'), and the blue patches at the bottom-right corners show the half-maximum regions of the dirty beams (~6').
The first SZE signal with the 7-element AMiBA
The AMiBA receiver with the vacuum chamber removed (Chen et al., 2009, ApJ, 694, 1664).
The AMiBA receiver with the vacuum chamber removed
The evolution of the SMA receiver configuration: the low-noise amplifier (LNA) upgrade. In 2007, the LNA bandwidth remained in 4-6GHz for first generation receiver. By 2011, the amplifier was upgraded to TTI-CLNA-4080 with 4-8GHz bandwidth, manufacture by a Spanish company. Now, we are using the new amplifier, CITCRYO1-12A, made by California Institute of Technology. This new upgrade increases the receiver bandwidth to 4-12GHz.
The SMA Receivers Upgrade
SMA 7-pixel array receiver co-polarization radiation pattern at 345 GHz. The peak value of each pixel is indicated. Each contour is 3dB apart.
Co-polarization radiation pattern of the 7-pixel array receiver optics design for SMA
A wideband digital correlator utilizing high-speed Analog-to-Digital Converters (ADCs) and Field Programmable Gate Arrays (FPGAs) was developed for the Array for Microwave Background Anisotropy (AMiBA). The objective is to detect spectral lines for intensity mapping for cosmology study. A prototype one-baseline correlator using 5 Gsps ADC modules has been deployed for testing.
Prototype digital correlator for AMiBA
From observations of Orion-KL, the HCO+ and HCN lines were detected using the prototype digital correlator for AMiBA.
Orion-KL observations using AMiBA prototype digital correlator
To increase the mapping speed of the Submillimeter Array (SMA), a focal plane array receiver is considered. The optics for a 7-pixel receiver at around 350 GHz were designed using quasi optics techniques. Physical optics calculation is performed with a reflector optics simulation software GRASP to simulate the beam efficiency.
Array receiver optics design for SMA
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 225 GHz ASIAA radiometer has been surveying the atmospheric clarity on the Greenland ice sheet since the summer of 2011. It has provided us the precious data regarding the submillimeter transmission for the GLT project.
ASIAA Radiometer in Greenland
Another night on Mauna Loa
AMiBA Operation
Disassembly of the ALMA NA Prototype in Nov. 2012. The antenna will be retrofitted for the extreme cold environment operations on the Greenland ice sheet.
Greenlan Telescope Project -- Disassembly in Socorro, NM
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
Two SMA antennas built in Taiwan. ASIAA has delivered receiver systems with three bands of 230 GHz, 345 GHz, and 690 GHz.
Two SMA antennas built in Taiwan
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, built at the top of Mauna Kea (el~4000 m), Hawaii
The Submillimeter Array
In the dedication ceremony of AMiBA held in Oct 2006, the NTU President S.C. Lee officially announced that the AMiBA is named as the “Yuan Tseh Lee Array for Microwave Background Anisotropy” and presented the name plaque of the Array to AS President Yuan
Dedication ceremony of AMiBA
AMiBA on Mauna Loa, Hawaii in September 2006. Seven 60-cm antennas, covered with GoreTex sun protection shields, form the most compact configuration on the carbon fiber platform. An optical telescope, the correlator, associated mechanical and electronic p
AMiBA on Mauna Loa, Hawaii
Chen, Ming-Tang
Deputy Director for Hawaii Operations; Research Fellow
Download PDF version of CV
photo of Chen, Ming-Tang
Office: ASMAB 1018
TEL: +886-2-2366-5348
FAX: +886-2-2367-7849
Email: mtchen_replace2@_asiaa.sinica.edu.tw

Education and Positions

  • JCMT Future Instrumentation Board (2016~present)
  • JCMT Board (2015~present)
  • Assistant Director, ASIAA (2008~present)
  • Research Fellow, ASIAA (2004~present)
  • Deputy Director, ASIAA Hawaii Operations (2003~present)
  • Acting Deputy Director, JCMT (2015~2016)
  • Associate Research Fellow, ASIAA (1999~2004)
  • Assistant Research Fellow, ASIAA (1996~1999)
  • Research Assistant, ASIAA (1995~1996)
  • Postdoctoral Fellow, Case Western Reserve University (1993~1995)
  • Teaching Assistant, Cheng-Kung University (1989)
  • Ph.D., Physics, University of Illinois Urbana-Champaign (1993)
  • B.S., Physics, Nat’l Cheng-Kung University (1986)

Research Interests

Detector science and instrumentation; simulation and modeling of scientific processes; image processing, recognition, and generation.

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