ASTE III
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1 ASTE II +III ALMA/SPICA SYNERGY TELESCOPE
2 ASTE III
3 ASTE III! A new large mm/submm single-dish telescope in Chile! natural extension from 45 m / ASTE.! complementary to ALMA, SPICA, SKA,...! will open new discovery space in the ALMA/SPICA/SKA era. Natural Evolution!"!#!$%&!'()!*&!'!!+,-./!0!1&!234!5!6&&!234!$78!9:!;!<34)!=:'8>-?:@!#!A&;B(A&!CC DEFGH-!+G->HE! =IJK=LLM!<:':N,O8PQ D!=-@R7R!G@!9P-!S@GT-,R- D!W-,-@HG8G9Q D!L@U7VO9-!!!!I,GNG@O>!LH-OR
4 ! Summary of the ASTE III project! m class wide-field (~ 1 ) single dish telescope! 70 GHz (4 mm) 400 GHz / 1 THz (0.7/0.3 mm)! Multi-band wide-field camera + multi-pixel ultra-wideband spectrograph (mm/submm version of MOS)! Will start its operation from ! Will cost 8.5 billion JPY (~ 10 billion JPY)! Plan for open use and international collaboration! legacy-type surveys (public data), common use observations.! Planing international collaboration with Korea, China, Taiwan, as well as the CCAT 25m project.! Project promotion, operation plan! On the basis of cooperation between universities plus NAOJ.! (Potential collaborators) K. Kohno, S. Yamamoto, Y. Tamura (Tokyo), H. Matsuhara (JAXA), E. Komatsu (Texas/MPI), T. Onishi (Osaka Pref.), M. Momose (Ibaraki), H. Nakanishi, Y. Imai (Kagoshima), R. Kawabe, M. Saito, T. Oshima, M. Honma, Y. Sekimoto, Y. Uzawa, T. Noguchi, N. Kuno, D. Iono, S. Iguchi, M. Hayashi (NAOJ), T. Minamidani (Hokkaido), N. Sugiyama (Nagoya), M. Hazumi (KEK) et al.
5 ! ASTE III will depict 3-dimensional distribution of dark matter and its evolution across the Hubble time by an intensive survey of a sizable number of submm galaxies as a signpost of the cosmic large-scale structures, and will provide breakthrough on the study of formation processes of galaxies and clusters of galaxies.! Needs tight operational combination with SPICA + long-term continuous combination with ALMA Herschel Epoch of Reionization Ground-based Large SDs 5x more sensitive than ALMA 2x more sensitive than ALMA comparable to ALMA Blain et al. (2002)
![z = 5 z = 6 z = 7 z = 3 z = 4 z = 2 z = 1 ASTE III CO and [CII] emitters](/docs-images/69/61862637/images/6-1.jpg "Feasibility study for ASTE III (YT+11) based on S-cubed SAX")
6 z = 5 z = 6 z = 7 z = 3 z = 4 z = 2 z = 1 ASTE III CO and [CII] emitters Feasibility study for ASTE III (YT+11) based on S-cubed SAX (Obreschkow+09)
7 CO and [CII] emitters Feasibility study for ASTE III (YT+11) based on S-cubed SAX (Obreschkow+09) Required density for BAO measurements galaxies are expected to be found in the Epoch of Reionization 7
8 CO and [CII] emitters Feasibility study for ASTE III (YT+11) based on S-cubed SAX (Obreschkow+09) 10
9 artist concept of GRB! Key Science (promoted by closer cooperation with universities) 1. Constructing a big catalog of galaxies ( submm version of SDSS ) to comprehensively understand distribution of dark matter and formation of galaxies and clusters. 2. Shooting submm flash in afterglows of gamma-ray burst (GRBs) as a probe of the cosmic star-formation history. 3. Improving the precision of CMB measurements and supporting to seek the evidence for inflation. 4. Making the best of the Sunyaev-Zel dovich effect to understand the physical processes of distant clusters of galaxies. 5. Systematic search for the earliest phase of star and planet formation and understanding of physical/chemical processes of them; understanding the evolutionary history of cosmic matter. 6. Utilizing it as a station of submm VLBI to image the BH shadow.! Commissioning of P.I. instruments led by universities will be encouraged.
10 ! Several options! Built our own by Japan? Participating to CCAT? LMT?! Preliminary discussion in the astronomy & astrophysics section committee, under the Science Council of Japan, has been started, as well as bottom-up discussion in the community Z[<!*&' $\:,9P) ==X<!A*' $W:79P) XW<Y(LLL!%&(*&' $W:79P)! Key words: Wide area imaging Wide band spectroscopy!synergies with big surveys in opt./ir SPICA (Matsuhara); TAO (Doi); Subaru (Takada) Frequency
11 ASTE II OSF, Chile, 29-Jun-2012
12 ! Submm galaxy survey! AzTEC deep extragalactic surveys (leading to discoveries of a lot of dusty extreme starburst galaxies at high redshift)! 45m redshift search machine!! ( H24 ) S ( H25 )! A
13 ! ASTE III ( 30 50m ) 45 / ASTE! 100! ALMA TMT NAOJ!! 11 12/21 22!
14 ASTE II! ALMA-J 12m! ATF/Scorro OSF! ALMA-J 12m ALMA spec THz! 12m 12m 10!?! ASTE
15 ! Summary! ALMA-J prototype 12-m dish (old PM04) + Nasmyth mount! installed close/next to the ASTE facility / completion by 2015/16! 12-m prototype dish = 1.5! ASTE 10-m in collecting area! Nighttime: 10 (best) to < 25 micron (rms)! accurate enough to conduct THz observations.! Daytime: < 50"60 micron (rms)! Deformation due to changes in ambient temp. + grav. deform.! Much better than ASTE (daytime), allowing daytime observations.! New Casegrain + Nasmyth receiver rooms and mount! will provide a large FoV up to Φ 26.4 arcmin submm version of Suprime-Cam! (c.f. Φ 7.5 arcmin for ASTE)! will simultaneously equip many facility receivers, allowing to quickly switch many instruments.
16 ! APEX!! ASTE (+45m) & ASTE II Synergy ( x2?)! ALMA Sci. / ASTE III ( Timeline)!!! ASTE III Road Map!! (
17 !! ASTE II+III Science WS (2012/3, 7, 9)! MELCO (2012/4, 7, 9)!!! 15 (max.) 10! 1. z > 5 6 SMG 2. z > 6 3. z > 6 4. THz ( )
18 ! (H23 )! WS ( ) 12 Y! (H24 )!! (9 11 )! (12 21, 22 )! WS Science Case Science Req. (9 29, )! CCAT WS ( ) CCAT (9 E)! NRO30 CCAT/LMT (12 )
19
20 LRR7-R!:]!XW<Y(LL!$^XW<Y) X_Y`!!(!!!!!!(!!(!XW<Y$^6*')!!a!XW<Y(LL ba!c)!!! XZ[X!WUG/JXW<Y(LLL L'8OU9!$ c:oh
23 ! CCAT!! ASTE III ( 30 50m) CCAT! Green Land Telescope (GLT)! ALMA-NA 12m Green Land submm VLBI THz NSF! ASTE! Caltech Submillimeter Observatory 10.4 m (CSO)! 1.5 M$/yr M$?
24 !! ASTE 12m! 30 50m 12m! (e.g. U. Arizona (supercam), Delft (DESHIMA), Caltech, Cardiff, UCB)!! 12m 10! MELCO (2012/4, 7, 9)
25 "#"! "#!!!"!" YiZX 2e< 6*' XZ[X XW<Y(LL ==X< W_L=X XW<Y [I_cX \X\<Y\(LL!""!"""!""""
26 XW<Y!LL!!!!*&'!*&!7'!,'R (!(!(!%f'!%&!7'!,'r ==X< XW<Y(LLL 2e<! XW<Y #;&&!5!1&&!234!!"!""!"""
27
28 1. ASTE 30-50m A~S 2. ASTE (e.g. RX cabin )... S/ 3. 12m 30 50m 30 50m
29 Wider Surveys Shaper beams Survey properties LMT50m NRO45m ASTE III 50m LMT32m IRAM30m Evolution to 30m-class Submm telescopes GLT 12m CCAT 25m JCMT 15m APEX 12m CSO 10.2m SMTO 10m ASTE 10m NANTEN2 4m!"#$% &"'$% Evolution to 50m-class mm and (long) submm telescopes Dish diameter [m] [GHz] Observing Frequency [GHz]
30
31 Vertex hole 50cm 85cm M3 Optics studies by Minamidani-san and Takekoshi-san
32 FoV Vertex hole 750mm 26.4 arcmin dia. Vertex 1360mm 2.5m 1344mm dia. Optics studies by Minamidani-san and Takekoshi-san
33 ! Vertex hole 750mm! El! φ mm! 600 mm 21 arcmin dia.! vertex! ray!! F/#! APEX Optics studies by Minamidani-san and Takekoshi-san
34 ! vertex hole focus El F/#! F/# Cassegrain F/# Limit point Max FoV Vertex hole to focus Focal plane size ~El axis dia. 8 Vertex hole mm 764mm 8 VH +El axis mm 600mm 10 Vertex hole mm 795mm 10 VH+El axis mm 600mm 12 Vertex hole mm 783mm 12 VH+El axis mm 600mm Optics studies by Minamidani-san and Takekoshi-san
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ASTE II +III ALMA/SPICA SYNERGY TELESCOPE 1 ASTE III 2 ASTE III! A new large mm/submm single-dish telescope in Chile! natural extension from 45 m / ASTE.! complementary to ALMA, SPICA, SKA,...! will open
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