Commissioning of ASTECAM New Trends in Radio Astronomy in the ALMA Era (Hakone, Japan 3−8 Dec 2012 ASTE-II ALMA / SPICA SYNERGY TELESCOPE Here we report on the new medium-scale plan in Japan to construct a 30 – 50 m class millimeter (mm) and sub-mm single dish telescope. The main observing frequency of the telescope is 70 to 400 GHz, which just covers main atmospheric windows in good observing sites at mm and sub-mm wavelengths such as the ALMA site. We are also aiming at observations at higher frequency up to 1 THz with the limited use of the antenna surface, e.g., under-illumination of the telescope. One of important science goals in this new telescope project is unveiling the large scale structure of the high-z universe and cosmic star formation history by spectroscopic surveys of high-z galaxies in CO and [CII] lines. With exploiting synergy with ALMA this telescope can contribute to the breadth of astronomy and astrophysics, e.g, astrochemistry, star formation in the galaxy and external galaxies, cosmology, and sub-mm VLBI. R. Kawabe (JAO/NAOJ), K. Kohno , S. Yamamoto. Y. Tamura, T. Totani (U. Tokyo), T. Kitayama (Toho), E. Komatsu (MPI), Onishi (Osaka P. U.),T. Oshima, M. Honma, D. Iono, N. Kuno (NAOJ), H. Matsuhara (ISAS/JAXA), M. Momose (Ibaraki), H. Nakanishi (Kagoshima) & Working Group (As of Dec. 3-8, 2012) Nominal Specification Dish diameter: 35 m (up to 50m) Main observing frequency: 70−400 GHz Highest obs. frequency: up to THz (with limited use of surface) Beam size: 6” @ 350GHz Remote operation is available from Japan. Timeline (Tentative) 2013− Survey design & conceptual design 2014−2017 R&D 2018− Start Construction 2023− Start Operations Partners CO Tomography; Blind CO Search Survey Example of CO Tomography; D = 35 m, 1000 hours, 2 deg2 Survey with Imaging Spectrometer, Npix =100 & 70-350 GHz (6 deg2 with Super-DESHIMA, Npix= 300) LSS (Large Scale Structure) up to z ~ 5 CO luminosity Functions at various redshifts and CO SEDs for high-z galaxies can be obtained Num Count dN/dz ~ 104 at z~2 for Npix = 300, RSD (Redshift Space Distortion) can be investigated to estimate growth rate of large-scale structure and dark energy Merit of large single dishes Confusion Noise ∝ D−1.4 Spatial Resolution ∝ D−1 Survey Speed ∝ D2 Speed of pointed Obs. ∝ D4 Proposed Instruments Multi-chroic wide-field camera(s) covering 90 to 350 GHz (+ 650 GHz) Multi-pix imaging spectrometers, e.g., at 70–400 GHz (e.g., “Super-DESHIMA”) Heterodyne receivers, 70 GHz to 1 THz, + Ultra-wideband spectrometer Heterodyne receiver array, e.g., at 100, 230, 350, 492 GHz Other Proposed Surveys ASTECAM (T. Oshima, NRO) Multi-wavelength SMG survey for z = 1−5 & Establishing large sample of forming dusty galaxies (down to SMGs with SFR ~ 100 Msun/yr) Blind [C II] survey to prove more distant universe, e.g., epoch of reionization (EoR) up to z ~ 7 or 8 High Spatial Resolution Mapping survey of distant SZ cluster to probe structure and mass of clusters, and blind SZ Cluster survey up to z ~ 2 to probe high-mass end of LSS Spectral line survey to investigate chemical and physical evolution in core to protoplanetary disk Galactic-plane survey & survey of nearby star-forming regions Multi-color bolometer camera for ASTE based on the transition-edge sensor (TES) technology 270, 350, 670 GHz Scientific interest: SMG search and photo-z Cosmic history of star/galaxy formation Evolution of the cosmic LSS at z ≧ 3 Phase I commissioning on ASTE was successful. Phase I II III Test Science operation Date 2012/4-6 2013/3-4 TBD Target frequency 270, 350 GHz 350, 650 GHz No. of pixels 169, 271 pix 271, 881 pix Field of View 7.5’ Φ NEFD (mJy/√sec) 10, 35 35, 80 First light image of the Moon at 270 GHz Detector array TESCAM dewar Commissioning of ASTECAM on ASTE 10-m (Apr, 2012)