The University of Tokyo Atacama Observatory (TAO) Project ...
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The University of Tokyo Atacama Observatory (TAO) Project
Sep.12,13,2011Osaka Pref. Univ.
Observatory (TAO) Project
Mamoru Doi, University of Tokyo, On behalf of TAO projectLarge Aperture Millimeter/Submillimeter Telescopes in the ALMA Era
Mamoru Doi, University of Tokyo, On behalf of TAO project
1‐m MiniTAO telescope
Chajnantor Summit (5640m) in the Parque Astronómico Atacama
6.5‐m Infrared telescope
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PeopleInstitute of Astronomy Graduate School of Science University of TokyoInstitute of Astronomy, Graduate School of Science, University of Tokyo
Headquarters at Mitaka, Tokyo(Next to NAOJ)
Kiso Observatoryat Nagano 1 05m Schmidt Telescope
Prof. Yuzuru Yoshii Director & Project Leader TAO members at IoA
(Next to NAOJ) 1.05m Schmidt Telescopesince 1974
3 Professors, 4 Associate Professors, 5 Assistant Professors, 4 EngineersUniv of Chile: Profs Bronfman Hamuy Ruiz Maza Lopez RubioUniv. of Chile: Profs. Bronfman, Hamuy, Ruiz, Maza, Lopez, Rubio…, Univ. of Catolica: Profs. Infante, Vanzi, …,Univ. of Concepcion, Univ. of Andres Bello, ..Chilean Government CONICYT DoE/Ministry of Foreign AffairsChilean Government: CONICYT , DoE/Ministry of Foreign Affairs,.. Dept of Astronomy UT, NOAJ, JAXA, other Japanese universitiesCCAT project
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Site Studies since 1999Satellite data analysis (with other institutes)Northern ChileNorthern ChileWest (Ocean) side: larger clear fractionbut no high (>4000m) mountainCompromise for IR astronomyCompromise for IR astronomy ⇒ Cerro Chajnantor (5640m)
View from San Pedro de Atacama
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TAO site
TAO siteCo. Chajnantor (5640m)Co. Chajnantor (5640m)
ASTE, NANTEN2ACT
APEX, QUIET
ALMA site
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Frontier of the infrared astronomyNew atmospheric window
4200m
New atmospheric window
4200m
10μm 20μm 30μm 40μm
New window at26-40um!
Best 10%Median
μ μ μ μ
5600m
10μm 20μm 30μm 40μm
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Almost continuous wavelength coverage at NIR
5600m
2600m2600m
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NIR: almost continuous coverage
Little transmittance at TAO site Little transmittance at ~2600m
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Access Road to the Chajnantor summit
• ~5.6kmU i f T k t t d• Univ. of Tokyo constructed
in 2006
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Summit area of Cerro Chajnantor
TAO Site CCAT Site
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Site Studies Summary
Good weather
bl 82%usable 82%
photometric 63%( )(Miyata et al. 2008)
Low water vapor
PWV 0.38mm(10%)0.85mm(median)
(Miyata et al. 2008)
Good Seeing
Median 0.69”
(Motohara et al. 2008)( )
Papers in SPIE proceedings
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The miniTAO telescopeP i iPrimary mirror
Φ1.0m
Cassegrain focus
focal ratio F/12
field of view Φ10’
plate scale 16.6”/mm
Vendor
Nishimura Co.
First Light March 2009Pointing accuracy σ=1.8 arcsecH t t t 0 19Hartmann constant σ=0.19 arcsecSeeing FWHM=0.5‐1.0 arcsec
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explores 30 micron astronomical windows
TAO 5,640m
2,600m
✓ First scientific observations were successfully carried out in 2010/09✓N‐ and Q‐band imaging mode is opened for Chilean time✓ Imaging mode at 31/38 micron is now commissioning
“30μm” Image Gallery obtained by MAX38Planetary Nebula : NGC6302 Jupiter LBV : η Car
10″10″10″ 101010
blue : Pa-beta (ANIR) , red : 31un blue: 8.9um, green: 18.7um red : 31un
31un
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31 micron sky background v.s. Object count for each frame (5sec)y g j ( )
Extremely clear sky appears on (rare?) occasions
tbject cou
nO
data (2010/10/03) +
Sky background count
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ANIR: Atacama Near Infrared Camera• NIR/Optical (0.4‐2.5μm) imager
with FoV of 5 2’with FoV of 5.2
Paα (1.8751μm) imaging from the ground
Galactic HII Region Survey in PaαTowards the Galactic Plane, esp. GC.1deg x 120 deg1deg x 120 deg
Galactic Center (SgrA)
1.48degree
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new lines – e.g. Paα 1.8751μm
5600mPWV=0.5mm
2600mPWV=6mm
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Nearby LIRG/Merger SurveyNearby LIRG/Merger Survey• Redshifted Pa‐alpha ~ 1 91um (N191 filter)Redshifted Pa‐alpha 1.91um (N191 filter)
• Probe for Dust Enshrouded Star Formation
• Calibration Method almost established
VV254 : J/H/N191 Paα Emission Line/ /
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Cerro Chajnantor ~5640mHighest IR observatory in the worldg est obse ato y t e o d
One of the Best IR Sites in the World!
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Wireless connection betweenthe summit and the base
The base facilityt S P d d At
the summit and the basesince June 2011
at SanPedro de Atacama
The miniTAO telescopeat Co. Chajnantor
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■ Base Facility at San Pedro de Atacama• Land at San Pedro de Atacama
14 000m^2 at walking distance from the14,000m 2 at walking distance from the town center
• Long-term Base facility being designedremote observations laboratory for maintenancerooms for observers
C Ch jCo.Chajnantor
Co.Chajnantor
48km
SPdA
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TAO 6.5m telescope
• Design Ritchey‐Chretien Field of View φ25 arcmin
IR optimized, simple
F ratio 12.2 ← Subaru TelescopepConceptual Design under way
Basic parameters (size, weight,…)p ( , g , )
drive designs, FEM, …
~6 years for construction6 years for construction
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Scientific Topics for the 6.5‐m telescope– Formation & Evolution of Galaxies
– Formation of planet systems
VISTA
– cosmology, AGN, ISM, stars, …
VISTAUKIRTCFHT TAO Cassegrain
utio
n
TAO-NIR1
KeckVLT
atia
l res
olu
csec
)
TMT
KeckSubaru sp
a(a
rc
TMTJWSTHST
(PSF different)
wavelength
NIR: Wide FieldMIR: High spatial resolution
g
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TAOMIR instrument ‐ MIMIZUKU Mid Infrared Multi field Imager for gaZing at the UnKnown UniverseMid‐Infrared Multi‐field Imager for gaZing at the UnKnown Universe
✓ Highest spatial resolution in 30um~ 1” @ 30um @ TAO 6.5m
✓ Wide wavelength coverage with three channels* InSb channel for 1‐5um (AlladinnII 1k)* Si:As channel for 6 25um (Aquarious 1k)
2m x 2m x 2m Si:As channel for 6‐25um (Aquarious 1k)* Si:Sb channel for 25‐38um (DRS HF 128x128)
✓Fi ld St k U it
Fore Optic
InSb Channel
✓Field Stacker Unit‐‐ picks up two discrete fields from the telescope FOV‐‐ achieves simultaneous observations of two objects
dramatically improves accuracy of the photometry
cs
Si:As Channel
S
enables us monitoring observations in MIR
from telescopefrom telescope
Si:Sb Channel
pick-up mirrors
trun-table
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TAO-NIR Instrument - SWIMSSi lt l Wid fi ld I f d M lti bj t S t hSimultaneous-color Wide-field Infrared Multi-object Spectrograph
Key Feature C l d M lti litKey FeatureNear-IR “Two-band Simultaneous” Obs.
•Wide F.o.V. (φ 9’.6)
Cooled Multi‐slitMask Stocker
W de F.o.V. (φ 9 .6)•High Spatial Resolution (0”.12 /pix)•R~1000 Grism MOS
with Filter Wheels
Blue Channel
Main Dewar
Science CaseCont. atmos. Window at NIR @ 5,640m
Wid t l b t b d MOSDichroic2Kx4K Arrays
Blue Channel(0.9‐1.4μm)
Wide spectral coverage by two-band MOSComprehensive Redshift Surveys
(z~1-3)
MirrorFilter Wheels
Red Channel
PlanPerformance Verification on Subaru@Hawaii
f Ob ll T O@Ch
( )
2Kx4K Arrays
(1.4‐2.5μm)
Scientific Obs. will start on TAO@Chajnantor.
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Two Instruments being assembled
SWIMS (NIR) MIMIZUKU(MIR)
Two instruments werefunded by Japanese government In 2009.g
New building is completedin April 2011.
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summaryy• Chajnantor SummitOne of the best sites on the earthOne of the best sites on the earthbeing shared with CCATTh i iTAO hfi d l• The miniTAO pathfinder telescopeTelescope: First Light March, 2009NIR and MIR Instruments: successful start upRemote operation being commissionedBase Facility being designed
• The TAO (6.5m) telescopeThe TAO (6.5m) telescopeconceptual design under waytwo instruments being builttwo instruments being built