The Science Cases for CSTAR, AST3, and...
Transcript of The Science Cases for CSTAR, AST3, and...
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The Science Cases for CSTAR, AST3, and KDUST
Lifan Wang
CCAA & TAMU
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CSTAR
• A pathfinder telescope
• Sky background and transmission
- See Zhou Xu’s talk
• Time domain astronomy
- Variable stars
• A wide area polarization map
of nearby bright stars
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Variable Stars from CSTAR
Credit: Lingzhi Wang, TAMU/BNU
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Credit: Lingzhi Wang, TAMU/BNU
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An RR Lyrae Star
Uninterrupted 4.5-d light curve (representing 3.5% of the entire data).
Folded light curve of the data on the left using P = 0.6466d; the photometric uncertainty is 3 mmag/bin.
RR Lyrae star Y Oct
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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.
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A Long-period (P~116.7d) Variable
Using the ASAS period as a starting point, the dominant periodicity was fit using a a five-term Fourier expansion fit. Left: the original data; Right, residual light curve, showing a small-amplitude (< 0.01 mag) periodicity with P = 17.3 d.
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An Exoplanet Candidate
Black dots: Raw data Red dots: Data binned to 10 min interval
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One of previous design
1) Adjustable tower height (preliminary designed to be about 1.5m);
2) Foldable dome;
3) Active snow removing;
4) Auto-focusing.
AST3
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Transportation and assembly at Dome A
Standard size container (about 2991×2591×2438mm)
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AST3
• Supernovae - Very early discovery - Uniform multicolor light curve coverage • Planet transients - Transients - Microlensing • LMC - Novae - Microlensing • Variable stars
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AST3 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 region
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KDUST 2.5
Observational Mode: Wide Area Survey Scientific Objectives: Dark Universe, Exoplanets Scientific Methods: Gravitational Lensing, Supernovae, and Precision Photometry Construction Period: 2011-2015 Cost: RMB 230 million
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Survey Area
5000 deg2 Cosmological Survey
Overlaps with South Pole Telescope
1% photometric precision
SPT overlap area
SDSS Southern Equatorial Stripe
Tie region
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KDUST2.5 Data Products
• 5000 sq degree high resolution image survey • 0.1-0.15 arcsec/pixel • 0.3 arcsec FWHM
• 10,000 sq deg K-Dark (2.4 micron) survey to KAB = 27mag
• ~ 5,000 SNIa to z ~ 3; PPSN search to z ~ 7
• LMC/SMC high cadence survey
• Galactic center K-Dark survey
• Cepheids in nearby galaxies – Hubble constant
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Synergistic Considerations
• CSTAR – Kepler/Corot/Other small telescopes
• AST3 – VLT Xshooter/Other telescope arrays/Other small telescopes
• KDUST2.5 – TMT/ELT/JWST
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The Construction of the Antarctica Observatory at Dome A may become one of the most remarkable achievements of the human race
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Study of the Early Universe with KDUST
Xuelei Chen (NOAC)
Wei Zheng (JHU)
August 17, 2010, XiAn
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August 17, 2010, XiAn
Epoch at Redshift z>7
• Reionization of the IGM
• First generation of black holes
• Rapid star formation
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August 17, 2010, XiAn
Kunlun Station at Dome A
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August 17, 2010, XiAn
Spectra of Quasar at z~6
White et al. 2003
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August 17, 2010, XiAn
Number of Quasars
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August 17, 2010, XiAn
Reionization of the IGM
Fan et al. 2006
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August 17, 2010, XiAn
Requirements
At least 5000 square degrees
YJHK bands
Limiting magnitude AB=24
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August 17, 2010, XiAn
Supernovae of Population III
• Massive: 100-250 solar mass
• Pair-instability outburst
• Bright: M~-24
• Metal free
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August 17, 2010, XiAn
SCP 06F6
Quimby et al. 2009
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Peak brightness of 250 M PISNe as a function of redshift in the spectral region around Ly-alpha assuming both no significant extinction and the "worst case" extinction for the Ly region
An Example KDUST K-Dark Science
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August 17, 2010, XiAn
Surface Density of PISN
Weinmann & Lilly 2005
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August 17, 2010, XiAn
Requirements
Repeated observations over 10 square degrees
Cadence of ~1-3 months
Magnitude AB>26
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August 17, 2010, XiAn
Gamma Ray Bursts
Detectable at very high redshift
Peak magnitude AB~20
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August 17, 2010, XiAn
GRB at z=8.3
Tanvir et al. 2009
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August 17, 2010, XiAn
Requirements
Fast communication link
Fast slew capability (within minutes)
Low- or medium-resolution spectrograph
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August 17, 2010, XiAn
Summary
KDUST is a powerful in high-z studies
Complimentary to JWST, TMT
Need both wide and deep surveys