optical/infrared astronomy of ast3
DESCRIPTION
Optical/Infrared Astronomy of AST3. Lifan Wang TAMU/CCAA. The Site Dome A Elevation4,091 m (13,422 ft) Coordinates: -80d22m, E77d 21m. The highest peak on the Plateau. Marching toward Antarctica. A team of Pioneers led by Yuanshen Li of Polar Research Institute - PowerPoint PPT PresentationTRANSCRIPT
Optical/Infrared Astronomy of AST3
Lifan Wang
TAMU/CCAA
The Site
Dome AElevation 4,091 m (13,422 ft)Coordinates: -80d22m, E77d 21m
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.
Dome AAn example of a very successfulcollaboration
China/Australia/USA
CSTAR
2008- 2011
Kunlun StationJan 27, 2009
• 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
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
Zou et al. 2010
Zou et al. 2010
Zou et al. 2010
Dome C
Dome A
Height of Turbulence Layer at Dome A & C
Boner et al. 2010
Precipitable Water Vapor
Nigel at Dome A
Nigel
Black spectrum: Hill & Jones JGR 105, 9421 (2000)
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.
Example ScienceCSTAR Data
An Exoplanet Candidate
Black dots: Raw data
Red dots:Data binned to 10 min interval
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
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.
Antarctica Survey Telescopes
AST3
• 68/50cm Diameter• FoV 4.2 Sq Deg• 1”/pix
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
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.
Standard Candles
Sensitivity
Sensitivity
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
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
Halo Structure
Pop III SNe
Pop III SNe
AST3!!!
KDUST4.0KDUST2.5
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.
z=7 Quasar and VISTA Filters
May, 2010
VISTA bandsSDSS bands
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.
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
Kunlun Dark Universe Telescope
Intermediate Scale Project Supernovae Weak Lensing Strong Lensing BAO?
Hubble Ultra Deep Field
南极冰穹 A天文观测优势
PILOT/KDUST Sensitivity
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
Thanks!
周伯星,黄色,煌煌然,所见之国大昌。