Workshop Summary & Discussion Kotaro Kohno Univ. of Tokyo

The goals of this workshop 1.Exploring the astrophysical potential of next generation large single-dish telescopes in the ALMA era with ultra-wide field of view and bandwidth at millimeter and submillimeter wavelengths. 2.Exchanging current status of future and existing mm/submm telescopes, including NRO 45m, ASTE, CCAT, LMT, NANTEN, APEX, IRAM 30m, ALMA, etc. 3.Sharing updated information on astrophysical activities and technology developments. 4.Discussion on the future (mid-term and long-term) collaboration among projects.

1) Exploring the astrophysical potential of next generation large single-dish telescopes in the ALMA era with ultra-wide FoV and bandwidth at mm/submm We confirmed that the next generation large single-dish telescopes with wide FoV and bandwidth will be extremely rich in discoveries, which is very complementary to ALMA.

Need for large dishes: Star and planet formation Wide area GMC surveys in the Galaxy and LMC/SMCs filling the gap between ALMA and existing CO surveys (Ohnishi) Wide area high resolution unbiased surveys of dust continuum for studies of short time scale objects such as first cores and transitional disks (Momose) Unbiased survey in both spatial and frequency domains to probe the origin of stars and planets (Yamamoto) CCAT will have a similar point source sensitivity with ALMA at 350 um and more sensitive to extended sources. Explore transition from diffuse to dense clouds, clump mass function to stellar mass function, mass evolution of primordial disks, (Carpenter)

Need for large dishes: the Galaxy and galaxies Lessons from NANTEN/NANTEN2; large scale spectroscopic CO survey with fine velocity resolution is essential for the discovery of cloud-cloud collision induced massive star formation process (Fukui) High velocity compact clouds (HVCCs) in the Galactic Centers; relation to intermediate mass black hole? Unbiased surveys in high-J high density tracers (Tanaka) Sgr A* BH shadow imaging; need large collecting area to improve sensitivity and uv coverage in submm VLBI (Honma; Asada) Multi-J CO and atomic line imaging surveys of nearby mergers and galaxies (Iono; Kuno; also Stacey)

Need for large dishes: galaxies, clusters, and cosmology CO+[CII] tomography with the proposed 50m (with an extremely ambitious specification RX) for galaxy formation and cosmology; proving EoR (Tamura) Ground-based observations of redshifted atomic lines [CII], [OIII], [NII], etc. are now feasible with ZEUS  ZEUS2; new, unique capabilities for mm/submm to probe physical properties of high-z galaxies (Stacey) High resolution thermal SZE will explore the dynamic evolution of the most massive object in the universe, i.e., cluster of galaxies; Kinematic SZE is very challenging but worth trying also (Kitayama); need wide field

Very rapid growth of technologies Multi-color TES array for ASTE (Oshima), Multichroic TES array (Myers) KIDs array for IRAM (NIKA, Mauskopf) & for APEX (Endo)  imaging spectrometers, DESHIMA (Endo), ZEUS2 (Stacey) Heterodyne receivers: ALMA band 10 (Uzawa) Wide band spectroscopy: SAM45+NRO45m (Iono), Redshift Search Receiver on LMT (Schloerb), Z-Spec/CSO, APEX (Stacey) – also EMIR on IRAM 30m, etc.

Progress of future telescopes planning Congratulations for the 1 st light of LMT ! Effort to the completion of 50m is ongoing. First phase instruments, such as AzTEC and RSR, are already well prepared, demonstrated, and got 1 st lights! (Schloerb) Very high priority of CCAT in decadal survey Astro2010; design studies are on-going with successful budget requests as well as proto-typing of 1 st light instruments of CCAT (Zivick, Stacey) Large mm/submm telescope project in Japan (ASTE-II; Kawabe): discussions from the bottom (mm/submm community) and the top (Science Council of Japan) are on-going; after the completion of ALMA, activities will be rapidly accelerated.

Possible collaborations: mid-term (& on-going) Continue and encourage existing partnership between the projects – AzTEC-ASTE collaboration (UMASS/INAOE/NAOJ/U. Tokyo etc.) continuously producing papers; possible further exchanges of opportunities were discussed, such as follow up of AzTEC/ASTE sources in LMT and extension of AzTEC/ASTE deep surveys at shorter wavelengths with TESCAM on ASTE – TESCAM collaboration (UC Berkeley/Cardiff/McGill/ NAOJ/Hokkaido Univ./U. Tokyo etc.) : extension to multichroic TES arrays (Myers’ talk); to shorter wavelengths (<350 μm ? with Cardiff; Mauskopf)

Possible collaborations: mid-term Participating commissioning and science verification (CSV) activities is very beneficial for next telescope design (Iguchi’s talk) – LMT provides us with the best opportunity ! Test of instrument at existing telescopes, such as LMT and ASTE; “Guest instrument” – Installation of 1 st light instruments for CCAT in ASTE (for instance) as a test – e.g., SuperCAM (U. of Arizona), 64 pix 350GHz heterodyne RX array, SMTO first, then ASTE to cover whole sky – DESHIMA for ASTE ? Discussion is started. (Dutch-JP !)

Current & future mm/submm telescopes [GHz] Dish diameter [m] Survey properties Wider Surveys Shaper beams NANTEN2 4m 50 NRO45m ASTE-II 50m LMT50m LMT32m IRAM30m CCAT 25m APEX 12m ASTE 10m Observing Frequency [GHz] JCMT 15m CSO 10.2m SMTO 10m SouthNorth G.L. 12m Evolution to ~30m class Submm telescopes Evolution to ~50m class mm & (long) submm telescopes (observatory type)

Synergy between CCAT & TAO/ASTE - Science preparation for CCAT with AzTEC/TESCAM surveys - ASTE as a test bench of new instruments for CCAT miniTAO/TAO ASTE - On-site collaboration such as infrastructure (road to the summit, etc) - Science: NIR/MIR and submm driven by IoA/UT IoA/UT is one of the major driving institutions of ASTE project existing, running telescopes CCAT PI. Y. Yoshii

Synergies with SPICA, ALMA, and beyond ・ unbiased survey  Identification of important objects for detailed studies ・ ionized / PDR gas （ atomic hyperfine lines ・ ro-vibrational lines ）、 power source diagnostics ・ very high angular + spectral resolutions  detailed investigation ・ cool ISM （ rotational transitions of molecules ） SPICA ALMA CCAT ASTE-II ・ unbiased wide field photometric surveys

Future large mm/submm missions ASTE-II 30-50m (South) CCAT 25m (South) Frequency LMT 50m (North) Key words: - Wide area imaging - Wide band spectroscopy  Synergies with big surveys at optical/IR SPICA (Matsuhara); TAO (Doi); Subaru (Takada)

Thank you for extensive support ! Osaka Pref. Univ: Profs. Hideo Ogawa, Toshikazu Onishi, Drs. Hiroyuki Maezawa, Kazuyuki Muraoka, Kimihiko Kimura, Ms. Yoko Hasegawa; Ms. Ikuko Fujii And all post-docs & students ! Also thanks to Ms. Satomi Kato (NAOJ) & Ms. Toshiko Tachibana (Univ. of Tokyo)

Final announcement We will have “after-workshop dinner” tonight in Nanba ( 難波 ) area. See you at 6:30 PM at the lobby of Comfort Hotel Sakai, if you want to join the dinner.