Lifan Wang TAMUCCAA The Site Dome A Elevation 4091 m 13422 ft Coordinates 80d22m E77d 21m The highest peak on the Plateau Marching toward Antarctica A team of Pioneers led by Yuanshen ID: 475373
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Slide1
Optical/Infrared Astronomy of AST3
Lifan Wang
TAMU/CCAASlide2
The Site
Dome A
Elevation 4,091 m (13,422 ft)
Coordinates: -80d22m, E77d 21m Slide3
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.Slide4
Dome A
An example of a very successful
collaboration
China/Australia/USASlide5
CSTAR
2008－2011Slide6
Kunlun Station
Jan 27, 2009Slide7
Continuous observing time for more than 3 months
Low
t
emperature
, low
sky background in thermo IRLow turbulence boundary layers, good seeingDry air,
high transmission in IRLarge Isoplanatic
AngleAurora
High relative humidityDifficult to accessMajor Relevant FeaturesSlide8
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 PWVSlide9
Zou
et al. 2010Slide10
Zou
et al. 2010Slide11
Zou
et al. 2010Slide12
Dome C
Dome A
Height of Turbulence Layer at Dome A & C
Boner et al. 2010Slide13
Precipitable
Water VaporSlide14
Nigel
at Dome A
Nigel
Black
spectrum: Hill & Jones JGR
105,
9421 (2000)Slide15
IR Background
It is also noteworthy that there are summer time IR background measurement at
Dome 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.Slide16
Example Science
CSTAR Data
An
Exoplanet
Candidate
Black dots: Raw data
Red dots:
Data binned to 10 min intervalSlide17Slide18
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. 2011Slide19
Survey
E
fficiency
Define 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:
D-Diameter of the telescope
W
-Field of view of the cameraq
-fwhm of the image (seeing or diffraction limit)B-Sky surface brightness
If the background is lower by a factor of 50-100,
a
s is the case for 2.4 micron at Dome A, a 0.5
m
eter telescope can survey as fast as a 3.5-5.0
m
eter telescope at a temperate site
A single KDUST field is 2 sq degree.Slide20
Antarctica Survey TelescopesSlide21
AST3
68/50cm Diameter
FoV
4.2 Sq Deg
1”/pixSlide22
Studies of Universe’s
Expansion
Physics Nobel in 2011
Johns Hopkins University; University Of California At Berkeley; Australian National University
From 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Slide23
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.Slide24
Standard CandlesSlide25
SensitivitySlide26
SensitivitySlide27Slide28
AST3
SN Survey/
DES Overlap
Schedule: Installation in 2011-2012
Survey Operation: 2012 – 2017
Data Products:>2000
SNIa to z ~ 0.15
Core-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 Southern
Equatorial Stripe
Tie regionSlide29
Supernova Cosmology
More precise Hubble diagram
Peculiar motion of nearby galaxies
Measurement of
s
8
Dark matter and neutrino properties
29
超新星
标准烛光
红移
星等
Wang, 2007Slide30Slide31
Halo StructureSlide32
Pop III SNeSlide33
Pop III SNe
AST3!!!
KDUST4.0
KDUST2.5Slide34
Survey
E
fficiency
Define 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:
D-Diameter of the telescope
W
-Field of view of the cameraq
-fwhm of the image (seeing or diffraction limit)B-Sky surface brightness
If the background is lower by a factor of 50-100,
a
s is the case for 2.4 micron at Dome A, a 0.5
m
eter telescope can survey as fast as a 3.5-5.0
m
eter telescope at a temperate site
A single KDUST field is 2 sq degree.Slide35
z=7 Quasar and VISTA Filters
May, 2010
VISTA bands
SDSS bandsSlide36
IR Background
It is also noteworthy that there are summer time IR background measurement at
Dome 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.Slide37
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 source
3 times faster than VISTA for diffuse sourceSlide38
Kunlun Dark Universe Telescope
Intermediate Scale Project Supernovae
Weak
Lensing
Strong
Lensing
BAO?
Slide39
Hubble Ultra Deep Field
南极冰穹
A
天文观测优势Slide40
PILOT/KDUST SensitivitySlide41
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 sourceSlide42
Thanks!
周伯星
，
黄色，煌煌然，所见之国大昌。