lifan wang texas a and m, usa/ chinese center for antarctic astronomy, (director), nanjing, china
DESCRIPTION
News on Developing Dome A as an International Astronomical Observatory and Progress on the Successful Traverse (driving in!) by the Polar Research Institute of China and the Chinese Center for Antarctic Astronomy HOU Teacher Conference, June, 2008 Carl Pennypacker, LBNL, UCB. - PowerPoint PPT PresentationTRANSCRIPT
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News on Developing Dome A as an International Astronomical Observatory and Progress on the Successful
Traverse (driving in!) by the
Polar Research Institute of China
and the
Chinese Center for Antarctic Astronomy
HOU Teacher Conference, June, 2008
Carl Pennypacker, LBNL, UCB
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Lifan WangLifan Wang Texas A and M, USA/ Chinese Center for Antarctic Astronomy, (Director), Nanjing, Texas A and M, USA/ Chinese Center for Antarctic Astronomy, (Director), Nanjing, ChinaChina
Huigen Yang , Huigen Yang , Y. LiPolar Research Institute of ChinaPolar Research Institute of China
Xiangqun Cui, Xiangqun Cui, Xiangyan Yuan Xiangyan Yuan Nanjing Institute of Astronomical Optics and Technology, ChinaNanjing Institute of Astronomical Optics and Technology, China
Jingyao Hu, Zhaoji Jiang, Xu Zhou Jingyao Hu, Zhaoji Jiang, Xu Zhou National Astronomical Observatories of ChinaNational Astronomical Observatories of China
Feng Longlong, Jun Yan, Zhu Zhenxi Feng Longlong, Jun Yan, Zhu Zhenxi Purple Mountain Observatory, China Purple Mountain Observatory, China
Zhaohui Shang Zhaohui Shang Tianjin Normal University, ChinaTianjin Normal University, China
Michael Ashley, Colin Bonner, Jon Everett, Jon Lawrence, Daniel Luong-Van, Suzanne Kenyon, Michael Ashley, Colin Bonner, Jon Everett, Jon Lawrence, Daniel Luong-Van, Suzanne Kenyon, Shane Hengst, John StoreyShane Hengst, John Storey University of New South Wales, AustraliaUniversity of New South Wales, Australia
Anna Moore, Reed Riddle, Tony TravouillonAnna Moore, Reed Riddle, Tony Travouillon California Institute of Technology, USACalifornia Institute of Technology, USA
Craig Kulesa, Chris Walker Craig Kulesa, Chris Walker University of Arizona, USAUniversity of Arizona, USA
Don YorkDon York University of Chicago, USA University of Chicago, USA
Nick Tothill Nick Tothill University of Exeter, UKUniversity of Exeter, UK
Bob Tripp Bob Tripp LBNL, USALBNL, USA
Carl PennypackerCarl Pennypacker LBNL, LBNL, Space Sciences Laboratory, USASpace Sciences Laboratory, USA
Collaboration
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Outline
1) More rationale on goals of this traverse
2) The Traverse itself
3) Closer inspection of some of the instruments on this traverse.
4) Antarctic Schmidt Telescope Progress
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From Lifan’s Talk:
Chinese Center for Antarctic Astronomy
• Dome A Site Survey-Pilot system
- 2007 and 2008 Traverse
- Survey site, determine height of boundary layer, measure seeing
- Do Science with C-STAR -- limiting magnitudes of about 17 (five sigma) in ten
seconds, stack images,
• Antarctic Schmidt Telescopes x 3 (AST3) -- being built now for 2009 traverse!
- 3x 0.5 meter telescopes, 10K x 10K CCD’s,
1”per pixel- ~ 100 good SNe per year, ~1 earth mass
planet a year due to micro lensing, hello-seismology, etc.
• Dome A Survey Telescope (4 - 6 meters ~> 12 - 18 meter in Chile or Mauna Kea) 10,000’s SNe per year, etc.
• Infrared Telescopes -- e.g., very high redshift studies.
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(Breath-taking) Timeline of Astronomy Ideas:
June, 2006: Beijing Dome C - Dome A meeting
January 2007: Go decision from Purple Mtn. Observatory, PRIC, NAOC, and Chinese National Academy of Sciences -- Astronomy becomes part of China’s PANDA IPY proposal
November, 2007: Xue Long leaves Shanghai, loaded for traverse (mostly --> on to Freemantle
November 30, 2007: Departs Freemantle, Australia to load PLATO
December 10, 2007: Arrive at Zhongshan Station
December 17: PLATO airlifted to Progress Airfield, tank filled
December 22: Begin Traverse
January 12 : Arrive at Dome A
February 21 , Depart Dome A
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Why is the excitement? Example 1
Above A boundary Layer(at Dome C ~ 30 meters) seeing is amazing :
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From Poisson Statistics:
Easy arithmetic, for point sources against a sky background, ignoring detector noise:
“Effective” Aperture diameter 1/(seeing disk diamter)
Hence, a 5 meter at Dome A should behave like a 15 meter in Chile.
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How to Rise Above the Boundary Layer (if needed) with a translation-only tower ~ 1 micron rotational movement/tilt due to wind -- two studies by Robert Hammerschlag, Netherlands -- based on Dutch Open Telescope Tower on La Palma
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With Good Seeing and 4-meter optics, you can do pretty well:
Exposure time -- seconds
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Seeing Review:
Ground-based Astronomical Seeing, due to high frequency temperature fluctuations in the path of the beam is often sub-divided into three components, with different physical heights along path:
1) Dome Seeing
2) Boundary Layer seeing
3) “Free atmosphere seeing in Jet Stream
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Dome A:
1) No Dome Seeing
2) Boundary layer is low
3) No Jet Stream (polar vortex protects us!)
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Characteristics of the Collaboration:
• Support a wide and useful set of astronomy projects, in the price range of $0.001M to $100M
• Do amazing science at lower cost than other sites or orbits (planet finding, deep imaging, infrared imaging, sub-millimeter astronomy, etc.)
• Be a nimble collaboration, that can change goals, science, detectors, many times in response to science and technology opportunities -- aim for Evolution ---> Revolution!
• Do projects with 2 to five year horizons
• Build on the profound commitment of China to Dome A (both for Polar Work and astronomy -- “Dome A is the Best Mountain in China”)
• Good governance, collaboration rules, clear path to joining collaboration
• Very respectful, smart collaboration with good resources, moving incrementally and carefully.
• China’s National Funding agencies, Academy of Science, broader government. In addition, many people of China are supportive of this effort, along with their support for science and technology in general. (hint, hint US Congress)
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More Details and Familiar Landmarks
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Google Earth View (rotated)
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Google Earth View (close-up and rotated)
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Progress
Nov 30: Xuelong departs Fremantle
Dec 10: Xuelong arrives Zhongshan
Dec 17: PLATO airlifted to Progress airfield
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Dome A Office
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Goodbye ‘til Next January
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Height of Boundary Layer and Ground Seeing vs. Wind Speeds from Swain/Gallee simulation
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Dome A
Courtesy A. Monaghan, Byrd Polar Research Centre
The annual vector mean winds from Polar MM5Dome A
4100 altitude
highest driestcoldest calmest
Wind speed (m/s)
How much better is Dome A than South Pole, Dome C??? PLATO
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South Pole Temperature Profile
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Temperature
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Dome A Temperature Profile
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Atmospheric parameters for astronomy Turbulence (SNODAR)
Boundary layer height, distribution and variability Upper atmospheric distribution
Sky emission (Gattini) Auroral spectral intensity and distribution, (visible and infrared) sky
background versus sun/moon elevation
Sky transmission (Pre-HEAT) Transparency and noise in long wave (sub-millimetre) windows
Cloud (Gattini ASC) Cloud cover statistics and distribution
Science (C-STAR) Optical transients: variable stars, transits, micro-lensing, GRB, etc
Site testing
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PLATO
PLATO (PLATeau Observatory)PLATO (PLATeau Observatory)
Deployment Jan 2008 via PRIC traverse Completely autonomous and self powered High reliability control system Low bandwidth communications Set up 2 weeks 2 people Dual module design
Instrument moduleInstrument moduleengine moduleengine module
solar panel arraysolar panel array
30 m tilt tower30 m tilt tower
2 m2 m50 m50 m
Concept design Feb 07Concept design Feb 07
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PLATO
PLATO (PLATeau Observatory)PLATO (PLATeau Observatory)
Deployment Jan 2008 via PRIC traverse Completely autonomous and self powered High reliability control system Low bandwidth communications Set up 2 weeks 2 people Dual module design
Instrument moduleInstrument moduleengine moduleengine module
solar panel arraysolar panel array
30 m tilt tower30 m tilt tower
2 m2 m
Delivery Nov 07Delivery Nov 07
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Provides Power, Shelter, and Control for Antarctic instrumentation Two modules:
Power module Instrument module Separated by 50 meters Modified shipping containers
Shipping containers? Logistics Manufacture Durability
Two modules? Manufacture and testing Diesel contamination Acoustic Water vapour Expansion
PLATO design
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MASSMASSportport
Pre-HEATPre-HEAT
Gattini SBCGattini SBC
Nigel portNigel portGattini all-skyGattini all-sky
Iridium antennasIridium antennas
webcamswebcams
Instrument module
sparespareportsports
CSTAR, SNODAR, CSTAR, SNODAR, Sonics located Sonics located externally on snow externally on snow surfacesurface
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IM layout
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Supervisor nodes (x2)
PC104 computer:
400 MHz Celeron
256MB SDRAM
2 x 4 GB USB flashdisc with read only filesystem on master
Lithium back-up battery
CAN microcontroller:
ATMEL development board
Software wakey-wakey and handshaking
Custom power-switching interface PCB
Iridium L band transceiver
SDB and direct-ssh
Externally located low-temperature antenna
Thermally regulated enclosure
IM Control
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SNODAR Surface layer Non-Doppler Acoustic Radar
Designed and built by UNSW / Univ Aukland
high frequency piezo-electric transducer with 1.2 m dish
Measures: high resolution (1 m) Cn2 in boundary layer (5-100/800 m)
Mounting: externally on snow surface
Power: 30 W (internal) + 100 W (external)
Weight: 300 kg (total)
Installation: 1 day
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SNODAR
outputSouth Pole 2001…
… Dome C 2003
…and Dome A 2008 ???
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Collaborators…Collaborators…
E. Aristidi E. Aristidi Uni. NiceUni. Nice M. AshleyM. Ashley Uni. NSWUni. NSW R. BriguglioR. Briguglio Roma/La SapienzaRoma/La Sapienza M. BussoM. Busso Uni. PerugiaUni. Perugia M. CandidiM. Candidi PNRAPNRA G. CutispotoG. Cutispoto CataniaCatania E. DistefanoE. Distefano CataniaCatania J. EverettJ. Everett Uni. NSWUni. NSW S. KenyonS. Kenyon Uni. NSWUni. NSW J. LawrenceJ. Lawrence Uni. NSW (co-PI)Uni. NSW (co-PI) D, Luong-VanD, Luong-Van Uni. NSWUni. NSW A. PhillipsA. Phillips Uni. NSWUni. NSW B. Le RouxB. Le Roux INAF:ArcetriINAF:Arcetri R. RagazzoniR. Ragazzoni INAF:PerugiaINAF:Perugia L. SabbatiniL. Sabbatini Roma/La SapienzaRoma/La Sapienza P. SalinariP. Salinari INAF:ArcetriINAF:Arcetri J. StoreyJ. Storey Uni. NSWUni. NSW M TaylorM Taylor Uni. NSWUni. NSW G. TostiG. Tosti Uni. PerugiaUni. Perugia T. TravouillonT. Travouillon CaltechCaltech
Gattini-DomeC are part of the IRAIT site testing campaign (Tosti et al)
Dome C
Dome A G. AllenG. Allen Solar MobilitySolar Mobility M. AshleyM. Ashley Uni. NSWUni. NSW T. BeddingT. Bedding Uni SydneyUni Sydney C. BeichmanC. Beichman JPL/MSCJPL/MSC D. CiardiD. Ciardi MSCMSC X. CuiX. Cui Nanjing/NAONanjing/NAO P. EspyP. Espy BASBAS J. EverettJ. Everett Uni. NSWUni. NSW L. FengL. Feng Purple Mountain ObsPurple Mountain Obs J. HuJ. Hu NAO/BeijingNAO/Beijing Z. JiangZ. Jiang NAO/BeijingNAO/Beijing C. KulesaC. Kulesa Steward ObsSteward Obs J. LawrenceJ. Lawrence Uni. NSWUni. NSW Y. LiY. Li PRICPRIC D. Luong-VanD. Luong-Van Uni. NSWUni. NSW W. QinW. Qin PRICPRIC C. PennypackerC. Pennypacker Livermore/BerkeleyLivermore/Berkeley R. RiddleR. Riddle TMT (co-PI)TMT (co-PI) W. SaundersW. Saunders AAOAAO Z. ShangZ. Shang TianjinTianjin D. StelloD. Stello Uni SydneyUni Sydney J. StoreyJ. Storey Uni. NSWUni. NSW B. SunB. Sun PRICPRIC N. SuntzeffN. Suntzeff Texas A&MTexas A&M N. TothillN. Tothill Uni Exeter (co-PI)Uni Exeter (co-PI) T. TravouillonT. Travouillon Caltech (co-PI)Caltech (co-PI) G. van BelleG. van Belle ESOESO K von BraunK von Braun MSCMSC L. WangL. Wang Texas A&MTexas A&M J. YanJ. Yan Purple Mountain ObsPurple Mountain Obs H. YangH. Yang Purple Mountain ObsPurple Mountain Obs X. YuanX. Yuan Nanjing/NAONanjing/NAO Z. ZhenxiZ. Zhenxi Purple Mountain ObsPurple Mountain Obs X. ZhouX. Zhou NAO/BeijingNAO/Beijing
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Why Gattini?Why Gattini?
0.27” mean seeing (=550nm) above boundary layer at Dome C (Lawrence et al, Agabi et al) and likely Dome A
Groups want to take the next step2m+ aperture OIR at Dome C
BUT optical sky brightness (including twilight and aurora) largely unquantified GATTINI cameras are giving first estimate of these
parameters essential for ““BIG OPTICAL ASTRONOMY”BIG OPTICAL ASTRONOMY”
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Gattini DomeA SBC camera(SBC=Sky Brightness Camera)
Transit camera pointed to South Pole
General features• 2.8 deg x 2.8 deg FoV• 5.1 arsec/pix• Sloan g’, r’, I’ filters
Technical features• Apogee Alta USB CCD camera • 2000x2000 pixels• Thermally controlled to ~ -40C• Objective aperture : 75 mm • Objective focal length: 300 mmSelf-calibrating on stars
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Gattini-DomeA Allsky
Transit camera pointed to Zenith
General features• ~90deg x ~90 deg FoV• Bessell B, V, R and long pass red for
OH emission
Technical features• Apogee Alta USB CCD camera • 2000x2000 pixels• Thermally controlled to ~ -40 0C• Objective aperture : ~3.5 mm Self-calibrating on stars
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SBC camera works!
Raw image of April 8th 2006 at 23:4840sec exposure
Raw image of July 2nd 2006 at 00:03
40sec exposure
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Allsky works !
Raw image of March 29th 200640sec exposure
Satellite trail
SMC
LMC
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Field coverage of SBCField coverage of SBC
SBC images 6deg by 4deg centered on SP
~40 sec exp time – no star trails (though not mandatory)
Identify bright stars and use for flux calibration of sky pixel intensity
Produce 2D sky brightness map every 20 mins
Side project- variable star monitoring?
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Gattini-Allsky
Transit camera pointed to Zenith
General features• 110deg x 80 deg FoV• Limiting magnitude: mV16/arcsec2
• Full CCD spectral response, no filter
Technical features• Apogee Alta USB CCD camera • 1600x1200 pixels• Thermally controlled to ~ -30 0C• Objective aperture : ~3.5 mm
Self-calibrating on stars
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Sky Brightness
• 6.5 months continuous data from the all sky camera gave initial brightness estimates (2006 winter season)
• Brightness values are uncalibrated values across the visual spectrum (this is changed for 2007 data)
• Icing issues with the SBC meant the all sky camera was more appropriate for preliminary analysis (solved for 2007 data)
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• Sky brightness with no moon contribution
•M(θ) = Ms - 10(20.32 - 11.66θ)
The sun!
Astronomical darknesssun elevation < -18˚
Astronomical twilightsun elevation > -18˚
UNFILETERED Magnitude
(mag/arcsec2)
sun zenith distance (rad)
moon zenith distance (rad)
-18deg-13deg
(-13deg)
(-39deg)
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• Sky brightness with no sun contribution
•M(θ, Φ) = Mm - Φ10(-0.97 - 0.58θ)
The Moon!
Moon phase:Φ = 0%Φ = 50%Φ = 100%
below horizonabove horizon
Magnitude (mag/arcsec2)
moon zenith distance (rad)
moon phase (%)
(+46deg ZD) (-39deg ZD)
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MechanicalInterface to PLATO
Gattini DomeA allsky Gattini DomeA SBC
Camera enclosures
OUR HERO!
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So, are there clouds or what?
•Photometric images: 83%
•Low extinction images: 85%
•Photometric, low extinction images: 79%
These numbers provide a lower bound on the number of cloud free images for the period April 1 - Oct 12, 2006
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CSTAR
Yuanxiang YanTelescopes
Design/Manufacture
Xu ZhouCCD/Computers
All hardware/software modifications
Shang Zhaohui/Zhu ZhenxiProject ManagersIntegration of CSTAR with PLATO
NIAOT/Zhenxi ZhuWinterization
Low temperature experiments
PLATO PRIC
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C-STAR: Rapid Response Camera for Wide-Field Imaging
• 10 second exposures• ~ 16th magnitude limit in 10 seconds• ~ 5 degs x 5 Degs fov• 15.77” pixel
Optical Layout: 14.5 cm telescopes x 3
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C-STAR Science
• Variables with high temporal resolution photometry in four colours,
• SNe, Novae, Orphan afterglows of bursts.
• Search for extrasolar planets using micro-lensing
• Best light curves of variable objects (stars, AGNs, etc.)
• Statistics of the bright variables
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Enabling Technology for the Dome A Survey Telescopes: the STA 10K x 10K CCD
Carl Pennypacker, Berkeley
Don York, Univ. of Chicago
Lifan Wang, Texas A&M
Dick Bredthauer, STA
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• 0.5 meter aperture
• 1” pixels (on surface for now)
• 5 deg x 5 deg field of view
Telescope Design: 3x Schmidt Telescopes,
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10K x 10K STA on USNO Telescope
Similar CCD’s are on Telescopes Now!
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Experienced and Successful CCD Team:
STA (San Juan Capistrano, California) is presently :
• developing CCD's for the LSST
• the Wynn ODI instrument.
• STA President Dick Bredthauer has developed CCD’s for Space Telescope and many planetary missions.
• Uses 1000 Ohm-cm silicon (medium resistivity -- Dalsa is Foundry.
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New Read-out Architecture for Drift Scan and Shutter-less Equatorial Tracking (to be built for Dome A AST’s)
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Existing Readout Architecture and CCD Quantum Efficiency
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Features, etc.:
Dark Current: negligible
Read Noise: ~ electrons at 1 MHz readout
Camera to be developed can work at Ambient of Antarctica (low or no power
on Peltier coolers) or testing in mid-latitudes
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What it Looks Like:
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Camera Detail:
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Camera Detail:
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• 100 Supernovae a year, with exquisite light curves
• One ~ Earth mass planet per year, through micro-lensing (in Baade’s window)
• Astro-seismology
• Lots of other variables of interest.
AST3 Science
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AST3 Micro-lensing