Program and Abstract Book - SRON

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19 th International Symposium on Space Terahertz Technology Performance Characterization of GISMO, a 2 Millimeter TES Bolometer Camera used at the IRAM 30 m Telescope 10-3 Johannes Staguhn 1,2 , Christine Allen 1 , Dominic Benford 1 , Stephen Maher 1 , Elmer Sharp 1 , Troy Ames 1 , Rick Arendt 1 , David Chuss 1 , Eli Dwek 1 , Dale Fixsen 1,2 , Stephen Maher 1,5 , Catherine Marx 1 , Tim Miller 1 , S. Harvey Moseley 1 , Santiago Navarro 3 , Eva Schinnerer 4 , Albrecht Sievers 4 , George Voellmer 1 ,Fabian Walter 4 , Edward Wollack 1 1 NASA/ Goddard Space Flight Center, 2 University of Maryland, 3 IRAM Spain, 4 MPIA Heidelberg, 5 SSAI Lanham Abstract: We have developed key technologies to enable highly versatile, kilopixel, infrared through millimeter wavelength bolometer arrays. The Backshort-Under-Grid (BUG) array consists of three components: 1) a transition-edge-sensor (TES) based bolometer array with background-limited sensitivity and high filling factor, 2) a quarter-wave reflective backshort grid providing high optical efficiency, and 3) a superconducting bump-bonded large format Superconducting Quantum Interference Device (SQUID) multiplexer readout. In November of 2007 we demonstrated a monolithic 8x16 array with 2 mm-pitch detectors in the field using our 2 mm wavelength imager GISMO (Goddard IRAM Superconducting 2 Millimeter Observer) at the IRAM 30 m telescope in Spain for astronomical observations. The 2 mm spectral range provides a unique terrestrial window enabling ground-based observations of the earliest active dusty galaxies in the universe and thereby allowing a better constraint on the star formation rate in these objects. I will present early results from our observing run with the first fielded BUG bolometer array. 84
19 th International Symposium on Space Terahertz Technology 350GHz Sideband Separating Receiver for ASTE 10-4 Hirofumi INOUE 1 , Kazuyuki MURAOKA 1 , Takeshi SAKAI 2 , Akira ENDO 1, 2 , Kotaro KOHNO 1 , Shin’ichiro ASAYAMA 2 , Takashi NOGUCHI 2 , Hideo OGAWA 3 1. Institute of Astronomy, The University of Tokyo 2. National Astronomical Observatory of Japan 3. Department of Physical Science, Graduate School of Science, Osaka Prefecture University (Abstract) We have developed a 350GHz sideband separating (2SB) receiver “CATS345 (CArtridge Type Sideband separating receiver)” for the Atacama Sub-millimeter Telescope Experiment (ASTE), a project for observations of the southern sky at sub-millimeter wavelengths with a 10m telescope in Atacama, Chile. The LO frequency (fLO) of this receiver is from 330 to 360GHz and the IF band is from 4 to 8GHz. In laboratory, the receiver noise temperature (TRX) was typically 200K(SSB) for fLO=330-350GHz and image rejection ratio (IRR) was typically 10dB for fLO=330-360GHz. An automatic data acquisition system using LabVIEW and GPIB has been developed. This system allows one to sweep the entire (V1, V2, PLO) space semiautomatically, providing insight towards the general behavior of the receiver performance according to external tuning conditions. We installed this receiver on the ASTE telescope with a new 4GHz backend in October 2007. The system noise temperature on site was 200K(SSB) for fLO=335-350GHz, which is half of that of the previous DSB receiver. So the observation time is reduced to 1/4. The Allan time is about 10 sec in both sidebands. This is the first sideband separating receiver in the 350GHz band that can be used commonly. Figure 1. CATS345 Figure 2. System noise temperature (SSB) at ASTE site 85
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Program and Abstract Book - SRON

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