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19 th International Symposium on Space Terahertz Technology P6-3 Upgrade of the SMART Focal Plane Array Receiver for NANTEN2 U.U. Graf, C.E. Honingh, K. Jacobs, M. Justen, P. Pütz, M. Schultz, S. Wulff, J. Stutzki KOSMA, 1. Physikalisches Institut der Universität zu Köln, Germany We present the recent upgrade to the KOSMA SMART 2x 8-pixel dual-color focal plane array receiver. The 460–490 GHz channel has been upgraded from 4 to 8 pixels. We use standard tunerless waveguide mixers with corrugated horns and all-Niobium single junction SIS devices. The measured noise temperatures are around 70 K over the RF band for an IF of 3.5–4.5 GHz for all pixels. At the IF the receiver is enhanced with new bias-tees and low noise MMIC amplifiers developed at Caltech. In the 800–880 GHz channel, devices with NbTiN-SiO 2 -Al tuning structures replace older SIS devices with Al-SiO 2 -Al tuning microstrip circuits. Their fabrication at KOSMA’s nanofabrication facilities utilizes electron beam lithography and chemical-mechanical planarization processing steps developed for the HIFI Band 2 devices. These devices need less local oscillator power, which facilitates the upgrade from 4 to 8 pixels. Measured noise temperatures per pixel are between 250 K and 300 K over the RF band for an IF of 4–8 GHz. In SMART the IF band is 1–2 GHz in order to simultaneously cover the CO 7-6 and the 3 P 2 - 3 P 1 Carbon lines at 807 GHz and 809 GHz in the lower and upper sidebands. All noise temperatures are measured with a 13 µm thick Mylar beam splitter, are uncorrected and calculated according to the Callen-Welton formalism. The receiver is currently being installed at the KOSMA Gornergrat observatory. After a twomonth test run, it will be shipped to the NANTEN2 telescope in Chile to be installed as a facility instrument in time for the southern hemisphere winter. 132
19 th International Symposium on Space Terahertz Technology P6-4 New Challenge for 0.1 - 0.3 THz Technology: Development of Apparatus for Radio Telescope RT-70 V. Vdovin 1 , I. Zinchenko 1 Yu. Artemenko 2 , V. Dubrovich 3 A. Baryshev 4 1 Institute of Applied Physics of Russian Academy of Sciences, Nizhniy Novgorod, Russia (IAP RAS) 2 Astro Space Center of Lebedev Physical Institute of Russian Academy of Sciences, Moscow, Russia (LPI RAS) 3 Special Astrophysical Observatory of Russian Academy of Sciences, St. Petersburg, Russia (SAO RAS). 4 Institute of Radio-engineering and Electronics of Russian Academy of Sciences, Moscow, Russia (IRE RAS) The 70-m radio telescope is now under construction on plateau Suffa in Uzbekistan at an altitude of 2500 m. It will have an actively controlled main mirror with the goal to achieve the shortest operational wavelength 1 mm. The project started many years ago but was frozen after USSR disintegration. The telescope support and the basic parts of the antenna were manufactured (Fig. 1). During the last few years the project has restarted and plans are being made to complete it in collaboration with Russia and Uzbekistan. The organization which is responsible for the project as a whole in Russia is the Astro Space Center of the Lebedev Physical Institute. The telescope should operate both in single-dish mode and as a part of VLBI networks, in particular in combination with planned radio telescopes in space such as Millimetron. The collecting area of the antenna greatly exceeds that of existing mm-wave facilities and is comparable to the total area of the ALMA antennas. This provides unprecedented capabilities for studies of compact faint objects which will be the primary targets for this instrument. The scientific program includes a wide range of astrophysical problems from studies of Solar system objects to the most distant radio galaxies and quasars. One of the most important tasks will be investigations of small scale primordial and secondary fluctuations of the CMB. For this task RT-70 will be significantly more efficient than a system of smaller telescopes like ALMA. In this report we mainly discuss the project status and development of the scientific instruments for this antenna which is still at a preliminary stage. They should incorporate the latest technological achievements and provide a superior performance over the operational frequency range. Both singlepixel and large format array (direct detection and heterodyne) receivers are considered. The receiver design is performed in the framework of a wide cooperation of Russian and Ukrainian organizations but is also open for the international community. The work is supported by the Program of Fundamental Researches of the Russian Academy of Sciences #5.2. “Electromagnetic THz- waves” and a special program Suffa project of ASC LPI RAS. Fig 1. The Suffa observatory with the radio telescope RT-70 now and after 2012. 133
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