8 2018 16:25
 ! () -  ()1.8m PLANETS *' , ), %, , '!$# (&"PLANETS 1.8-m off-axis
telescope https://www.planets.life/ü ("-.PSFü #'$&
ü %,+ !)&→  &→ TOO&→ AO, *"*, ,535AO42
3 522,#$+42352 2!4
5*0$3%$(4")$'3-.
/2%$(4")$'3 4",.1&3AO42

1.

VI]D"%)#-/B4>

$T8]^=?H
(!,*'(L<AFmicro-roughness6  $%*&-→<O9W
++#L<ZK7C : !)(AOAdoptive Secondary
@_3SG\EX($+$8L

U.6"+"/E

KVF1RJ:Q53C@

0>BG

*&!,/0?WR'#$.5Q
-TM;A2MIDNPIDTOOF1U.6,ISE

47XOISTER9MJ=H2PU/ :1 ;[  NY O PLANETS 1.8-m off-axis
telescope https://www.planets.life/• (. (50-100kg)- '/&- -$-!)• '0: 6/   1/ *%•   (.
- #)-!)/&"+,
M1: parabola, 1.86m
4.333m fl
M2: ellipse, 12cm
0.26m fl4

Jupiter Io torus

AELby Spencer

Satarn Enceladus torus

by Johnson

Mars HDO/H2O map

Exoplanet'ü  ü "$%ü #%!ü AO
ü  ü '( &)• Brightness of planetary disk isroughly 10-5*10-7 times
greater than that of targets.
→ coronagraphy→ high-resolution spectroscopy
5PSF • %$e.g.,  → !#• "&e.g.,  → &  

OI630nm 1kROI630nm 1kRarcsec

arcsec4FRMS(nm)   

CaseA
CaseB
CaseC
CaseD
   cyc/m)

•<21 , 4, 411)0)021••4 4 6- 2
2121

RMS(nm)CaseA
CaseB
CaseC
CaseD

cyc/m)S/N
S/N


 

1.85-m

Ohara Clearceram Z-HS (same as TMT)
Φ1850mm, t=100mm

Melting(Dec. 2010)

Blank reached to L.A.
(May 2011)

Grinding at Harris/EXELIS(July 2012)
Arrived in Maui (June 2017)! #/  "Hydra""→  

10.5µm PV
0.7µm RMS
9• '!!   $"•  &• 3# %
By the only robot-arm, polishing and measuring are
executed on large and free form optics(including flat and convex shapes).
mirrorDragging 3 probe method
Data stitching algorithm
Flow of data processing
Sample result

2 m%&

Prototype for Kyoto 3.8mü)3.8m $#%ü)ü .- 
, &+*ü2" & 
ü!('"!$üR/
#' &→  11••••••

./-,('#$+  &2Geregorian")
* (%!12Three views
Truss structure 820 kg
Primary+cell
600kg
Elevation support 1 ton
Azimuthal stage 1 ton
Total
3 - 4 ton

→ R 180
Elevation=013 Eigenfrequency
Alt=90oMode-1: 28.0 Hz
Mode-2: 31.7 Hz

Alt=30oMode-1: 31.3 Hz
Mode-2: 32.0 Hz 30kg
90kg 

ü 6000 N load for primary mirror
ü 300 N load for secondary mirror

→




14

 Displacement at secondary mirror
Displacement at secondary is
0.05 mm when altitude = 90o

Displacement at secondary is
0.31 mm when altitude = 30o
Alt=30oMax displacement = 0.31mm

Alt=90oMax displacement = 0.085mm→2





15




We could not find any place in our university campus.
Fortunately, our Iitate observatory (37.6oN, 2-hour
drive from Sendai) can enclose the structure withminor renovation.

Roll-off roof building in Iitate observatory

Sendai↑ Iitate observatory
Tokyo16, TOO•
(3050m)• UH  • 17T60





InstrumentSpec.

Fiber : Vispec(Visible Imager and Spectrograph withCoronagrpahy)

0.4-0.9µm, FOV~1’ / R~70,000

Fiber : MILAHI (Mid-infrared laser heterodynespectrometer)

7-11µm, R ~ 106-7

Gregorian: DiPOL-2 (Polarization imager) (KIS)

B, V, R

Nas: NIREchelle spectrograph (ESPRIT)

1-4µm, R ~ 20,000

Nas: MID-IRGIGMICS (Nagoya U.)

7-12µm, R ~ 40,000

polarimetry (DoLP ~ 10-5~6)

• 1.8m口径PLANETS望遠鏡は、低散乱光学系である特長をもつ。
• せいめい望遠鏡プロトタイプ架台を再利用する。グレゴリアン焦点でのFOVは6arcminで、回折限界達成領域は1arcmin程度予定。
• 大型装置（ゲスト装置含む）はナスミス焦点。
• 主鏡研磨、検査は国内メーカーで実施する計画を進行中。
• 主鏡保持はウィッフルツリーをベースに検討中。
• 福島・飯舘観測所を改造し、国内でファーストライトを達成する。
• 今後、海外観測好適地（ハレアカラ）の建物建築の予算化を目指す。


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Akatsuki, Juno, Haya-2, ExoMars, MMX, JUICE…
( 1Subaru, VLT, LSST, TMT, GMT, E-ELT…
(,/1
ALMA, SKA…

(12(.2(.(3("(($#-(…

4&'%+' +0 4&( 

ü [1f+:;p= "#'a@3V ebBM0hS7( ?_Z3Vi pW3V
cdIM % $ Y, ToO^&!3V
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