Transcript Workshop Summary & Discussion

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 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
Survey properties
Wider Surveys
LMT50m
ASTE-II 50m
NRO45m
LMT32m
IRAM30m
50
South
North
Evolution to
~50m class
mm & (long) submm telescopes
30
CCAT 25m
G.L.
12m
Evolution to
~30m class
Submm telescopes
JCMT 15m
APEX 12m
CSO 10.2m
SMTO 10m
ASTE 10m
10
NANTEN2 4m
100
500
1000 [GHz]
Observing Frequency [GHz]
Dish diameter [m]
Shaper beams
(observatory type)
Synergy between CCAT & TAO/ASTE
CCAT
existing, running telescopes
- Science preparation for CCAT
with AzTEC/TESCAM surveys
- ASTE as a test bench
of new instruments for CCAT
ASTE
IoA/UT is
one of the major
driving institutions
of ASTE project
- On-site collaboration
such as infrastructure
(road to the summit, etc)
- Science: NIR/MIR and submm
miniTAO/TAO
driven by IoA/UT
PI. Y. Yoshii
Synergies with SPICA, ALMA, and beyond
SPICA
・unbiased
wide field
photometric
surveys
CCAT
ASTE-II
ALMA
・unbiased survey
Identification of important
objects for detailed studies
・ionized / PDR gas
・very high angular +
spectral resolutions
detailed investigation
・cool ISM
（atomic hyperfine lines・ro-vibrational lines）、 （rotational transitions of
power source diagnostics
molecules）
Future large mm/submm missions
LMT 50m
(North)
CCAT 25m
(South)
ASTE-II
30-50m
(South)
Key words:
- Wide area imaging
- Wide band spectroscopy
Synergies with
big surveys at optical/IR
SPICA (Matsuhara); TAO (Doi); Subaru (Takada)
Frequency
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.