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
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
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
TAO site
TAO siteCo. Chajnantor (5640m)Co. Chajnantor (5640m)
ASTE, NANTEN2ACT
APEX, QUIET
ALMA site
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
Almost continuous wavelength coverage at NIR
5600m
2600m2600m
NIR: almost continuous coverage
Little transmittance at TAO site Little transmittance at ~2600m
Access Road to the Chajnantor summit
• ～５.６kmU i f T k t t d• Univ. of Tokyo constructed
in 2006
Summit area of Cerro Chajnantor
TAO Site CCAT Site
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
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
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
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
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
new lines – e.g. Paα 1.8751μm
5600mPWV=0.5mm
2600mPWV=6mm
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/ /
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!
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
■ 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
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
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
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
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.
Two Instruments being assembled
SWIMS (NIR) MIMIZUKU(MIR)
Two instruments werefunded by Japanese government In 2009.g
New building is completedin April 2011.
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
