workshop summary & discussion
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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.
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