Optical/Infrared Astronomy of AST3
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Optical/Infrared Astronomy of AST3
Lifan Wang
TAMU/CCAA
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The Site
Dome AElevation 4,091 m (13,422 ft)Coordinates: -80d22m, E77d 21m
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The highest peak on the Plateau
Marching toward Antarctica
A team of Pioneers led by Yuanshen Li of Polar Research Institute Of China arrived at Dome Argus, Antarctica on Jan 18, 2005.
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Dome AAn example of a very successfulcollaboration
China/Australia/USA
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CSTAR
2008- 2011
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Kunlun StationJan 27, 2009
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• Continuous observing time for more than 3 months• Low temperature, low sky background in thermo IR• Low turbulence boundary layers, good seeing• Dry air, high transmission in IR• Large Isoplanatic Angle
• Aurora• High relative humidity• Difficult to access
Major Relevant Features
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Science Considerations• Time Domain Astronomy – Requires Clear Sky• High Spatial Resolution, Wide Field Astronomy – Requires Clear Sky,
Good Seeing• Wide Field Infrared Survey – Requires Clear Sky, Good Seeing, and Low
Sky Background
• Terahertz Telescope – Requires Low PWV
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Zou et al. 2010
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Zou et al. 2010
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Zou et al. 2010
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Dome C
Dome A
Height of Turbulence Layer at Dome A & C
Boner et al. 2010
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Precipitable Water Vapor
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Nigel at Dome A
Nigel
Black spectrum: Hill & Jones JGR 105, 9421 (2000)
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IR Background
It is also noteworthy that there are summer time IR background measurement atDome C (Walden et al. 2005). The summer time 3-20 m backgrounds were found to be very stable and at levels comparable to the measurements at South Pole during the winter.
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Example ScienceCSTAR Data
An Exoplanet Candidate
Black dots: Raw data
Red dots:Data binned to 10 min interval
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d Scuti star
Uninterrupted 4.5-d light curve (representing 3.5% of the entire data).
Folded light curve using P = 0.2193d; the photometric uncertainty is 1.5 mmag/bin.
Lingzhi Wang, Lucas Macri et al. 2011
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Survey EfficiencyDefine the survey efficiency k as the sky area a telescope can survey to a given S/N for a resolved source in a specific exposure time:
For an unresolved diffuse source:
€
κ ∝ΩDθ ⎛ ⎝ ⎜
⎞ ⎠ ⎟2 1B ⎛ ⎝ ⎜
⎞ ⎠ ⎟ 1S /N ⎛ ⎝ ⎜
⎞ ⎠ ⎟2
D-Diameter of the telescopeΩ-Field of view of the cameraq-fwhm of the image (seeing or diffraction limit)B-Sky surface brightness
€
κ ∝ΩD2 1B ⎛ ⎝ ⎜
⎞ ⎠ ⎟ 1S /N ⎛ ⎝ ⎜
⎞ ⎠ ⎟2 If the background is lower by a factor of 50-100,
as is the case for 2.4 micron at Dome A, a 0.5 meter telescope can survey as fast as a 3.5-5.0 meter telescope at a temperate site
A single KDUST field is 2 sq degree.
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Antarctica Survey Telescopes
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AST3
• 68/50cm Diameter• FoV 4.2 Sq Deg• 1”/pix
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Studies of Universe’s ExpansionPhysics Nobel in 2011
Johns Hopkins University; University Of California At Berkeley; Australian National UniversityFrom left, Adam Riess, Saul Perlmutter and Brian Schmidt shared the Nobel Prize in physics
52 44 41
2006年,邵逸夫天文奖曾颁发给同样的三位科学家及其发现
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SN1006——One Thousand Years After
Chandra Image
周伯星,黄色,煌煌然,所见之国大昌。The Zhoubo stars are yellowish and brilliant. Nations observing them will reach great prosperity.
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Standard Candles
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Sensitivity
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Sensitivity
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AST3 SN Survey/DES Overlap
Schedule: Installation in 2011-2012Survey Operation: 2012 – 2017
Data Products:
>2000 SNIa to z ~ 0.15Core-collapse SNe; GRB; Orphan GRB afterglow
LMC continuous monitoring –variable stars/microlensing/dark matter Galactic center continuous monitoring – variable stars/microlensing/transients
Galactic structure – RR Lyrae/Cepheids
SPT overlap area
SDSS SouthernEquatorial Stripe
Tie region
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Supernova Cosmology More precise Hubble diagram Peculiar motion of nearby galaxies Measurement of s8
Dark matter and neutrino properties
29
超新星标准烛光红移
星等
Wang, 2007
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Halo Structure
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Pop III SNe
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Pop III SNe
AST3!!!
KDUST4.0KDUST2.5
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Survey EfficiencyDefine the survey efficiency k as the sky area a telescope can survey to a given S/N for a resolved source in a specific exposure time:
For an unresolved diffuse source:
€
κ ∝ΩDθ ⎛ ⎝ ⎜
⎞ ⎠ ⎟2 1B ⎛ ⎝ ⎜
⎞ ⎠ ⎟ 1S /N ⎛ ⎝ ⎜
⎞ ⎠ ⎟2
D-Diameter of the telescopeΩ-Field of view of the cameraq-fwhm of the image (seeing or diffraction limit)B-Sky surface brightness
€
κ ∝ΩD2 1B ⎛ ⎝ ⎜
⎞ ⎠ ⎟ 1S /N ⎛ ⎝ ⎜
⎞ ⎠ ⎟2 If the background is lower by a factor of 50-100,
as is the case for 2.4 micron at Dome A, a 0.5 meter telescope can survey as fast as a 3.5-5.0 meter telescope at a temperate site
A single KDUST field is 2 sq degree.
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z=7 Quasar and VISTA Filters
May, 2010
VISTA bandsSDSS bands
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IR Background
It is also noteworthy that there are summer time IR background measurement atDome C (Walden et al. 2005). The summer time 3-20 m backgrounds were found to be very stable and at levels comparable to the measurements at South Pole during the winter.
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AST3 NIR
Synoptic Infrared Survey Telescope
In KDARK, compared to 2MASS, an increase of efficiency by (2048/256)2 * (0.5/1.3)2 * 50 = 473 times
GRBs at z ~15 !?
Comparable to VISTA for point source3 times faster than VISTA for diffuse source
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Kunlun Dark Universe Telescope
Intermediate Scale Project Supernovae Weak Lensing Strong Lensing BAO?
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Hubble Ultra Deep Field
南极冰穹 A天文观测优势
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PILOT/KDUST Sensitivity
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Hubble Ultra Deep Field
One Single KDUST Exposure
For Comparison: KDUST Reaches HUDF Depth at 750nm in 83 Hours for point sources and 251 hours for diffuse source
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Thanks!
周伯星,黄色,煌煌然,所见之国大昌。