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ASTE

ASTE. A tacama S ubmillimter T elescope E xperiment. Hajime Ezawa National Astronomical Observatory of Japan. ASTE Team National Astronomical Observatory of Japan The University of Tokyo (IoA & Dept. of Physics) Nagoya University Osaka-pref. University

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ASTE

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  1. ASTE Atacama Submillimter Telescope Experiment Hajime Ezawa National Astronomical Observatory of Japan ASTE Team National Astronomical Observatory of Japan The University of Tokyo (IoA & Dept. of Physics) Nagoya University Osaka-pref. University Universidad de Chile

  2. The ASTE Project • Install and Operate a 10-m submillimeter telescope at the one of the best observing site in nothern Chile. • Explore the southern sky with submillimeter waves • On-site evaluation of methods & techniques for submm. obs. • High precision antenna, high sensitivity submm. RX • Remote operation system • Provide opportunity for young students to study observation and instrumentation for submillimeter astronomy

  3. The ASTE Site • Located at alt. 4,800 m in the Atacama desert in northern Chile • CBI, APEX, NANTEN2, ALMA, RLT, …. in vicinity

  4. ASTE Bands The ASTE site FTS measurement Matsushita et al. 1999

  5. March, 2002 To 4,800 m telescope site Jan.-Mar., 2002 To Chile 2000 - 2001 Final Position Fabrication in San P. de Atacama↑ Initial installation in Nobeyama → Fabrication and installation

  6. Climbing the most difficult hill • Almost there, but still hard to go…

  7. Satellite Comunication ObservingRoom Generators & Fuel tanks Telescope • Satellite telephone • Oxygen cylinders & compressors • Safety rules (ex. time limit) Alt. 4,800 m = 570 hPa Safety equipments including

  8. The Antenna (1) • The Antenna: • 10 m diameter • Surface Accuracy < 20 mm • Adjustable 205 Al panels • BUS of CFRP and Invar • High accuracy encoder ~0.03” rms • Sub-reflector • Mounted on Steward platform • Wobbling capability • Optical telescope • Mounted on telescope structure

  9. Current surface accuracy = 18.9 mm r.m.s. Relative Pointing Accuracy 1.2” for AZ, EL The Antenna (2) Telescope Transmitter For Holography

  10. Receivers & Spectrometer SIS heterodyne Receivers Cartridge type RX (4 K) 345 GHz, 500 GHz, 800 GHz Tsys = 200 K ! @ 345 GHz Spectrometer Four XF type auto-corelators 1024 ch for 512 or 128 MHz BW Spectrometer 345 GHz RX Continuum Receivers • 3-band bolometer mainly for antenna evaluation (350, 650, 850 GHz) • Submillimter Camera array of SIS direct photon detectors at 650 GHz (Matsuo et al. 2004) CO(J=7-6) Ori-KL Sugimoto et al. 2004

  11. Operation & Control • Remote control through narrow band-width connection • Operation possible from multiple sites (incl. overseas) Santiago (U. de Chile) Telescope Site (Alt. 4800 m) Satellite Link 56~64 kbps Holography TX Power Generators Internet San Pedro de Atacama (Base Facility, 2400 m) Japan (NAOJ and Univ’s)

  12. Latest Results 5 arcmin CS(7-6) towards NGC 3576 Yamaguchi et al.  4.81 CO(3-2) towards M83 IRS 4 Muraoka et al.  4.51 IRS 6 Outflows from IRS 4 Cha MMS1 Hiramatsu et al.  4.30

  13. Summary • 10 m submillimeter telescope ASTE is now in operation at Pampa la Bola • Antenna shows good specification including surface accuracy of 18.9 mm r.m.s. • Cartdridge type 345 RX realizing Tsys=200 K @ 345 GHz • Telescope is remote-controllable from multiple sites through satellite connection and internet. • Following the evaluation phase, astronomical observation has been performed since 2003. - Posters - Hiramatsu et al. (4.30) YSO-close-packed region Cederbald 110 Mizuno et al. (4.48) Magellanic clouds Moriguchi et al.(4.50) TeV Gamma-ray SNR G347.3-0.5 Muraoka et al.(4.51) Disk region of the barred spiral galaxy M 83 Yamaguchi et al. (4.81) Southern massive star-forming regions

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