Workshop Summary & Discussion

Kotaro KohnoUniv. of Tokyo

The goals of this workshop1. 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 1st 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 1st 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 1st 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 1st 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

100 500 1000 [GHz]

Dish

diam

eter [m]S

urv

ey p

rop

erti

es

Wid

er

Sur

veys

Sh

ape

r be

ams

30

10

NANTEN2 4m

50

NRO45mASTE-II 50m

LMT50m

LMT32m

IRAM30m

CCAT 25m

APEX 12m

ASTE 10m

Observing Frequency [GHz]

JCMT 15m

CSO 10.2mSMTO 10m

South North

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/TAOASTE

- On-site collaboration such as infrastructure (road to the summit, etc)- Science: NIR/MIR and submm

driven by IoA/UTIoA/UT is one of the majordriving institutions of ASTE project

existing, running telescopes

CCAT

PI. Y. Yoshii

Synergies with SPICA, ALMA, and beyond

・ unbiased surveyIdentification 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

CCATASTE-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 spectroscopySynergies 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.