The Science Cases for CSTAR, AST3, and KDUST

Transcription

1 The Science Cases for CSTAR, AST3, and KDUST Lifan Wang CCAA & TAMU

2 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

3 Variable Stars from CSTAR Credit: Lingzhi Wang, TAMU/BNU

4 Credit: Lingzhi Wang, TAMU/BNU

5 An RR Lyrae Star RR Lyrae star Y Oct Uninterrupted 4.5-d light curve (representing 3.5% of the entire data). Folded light curve of the data on the left using P = d; the photometric uncertainty is 3 mmag/bin.

6 d Scuti star Uninterrupted 4.5-d light curve (representing 3.5% of the entire data). Folded light curve using P = d; the photometric uncertainty is 1.5 mmag/bin.

7 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.

8 An Exoplanet Candidate Black dots: Raw data Red dots: Data binned to 10 min interval

9 AST3 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.

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11 Transportation and assembly at Dome A Standard size container (about mm)

12 AST3 Supernovae - Very early discovery - Uniform multicolor light curve coverage Planet transients - Transients - Microlensing LMC - Novae - Microlensing Variable stars

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15 AST3 Schedule: Installation in Survey Operation: Data Products: SPT overlap area Tie region SDSS Southern Equatorial Stripe >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

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18 KDUST 2.5 Observational Mode: Wide Area Survey Scientific Objectives: Dark Universe, Exoplanets Scientific Methods: Gravitational Lensing, Supernovae, and Precision Photometry Construction Period: Cost: RMB 230 million

19 Survey Area 5000 deg 2 Cosmological Survey Overlaps with South Pole Telescope 1% photometric precision SPT overlap area Tie region SDSS Southern Equatorial Stripe

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22 KDUST2.5 Data Products 5000 sq degree high resolution image survey 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

23 Synergistic Considerations CSTAR Kepler/Corot/Other small telescopes AST3 VLT Xshooter/Other telescope arrays/other small telescopes KDUST2.5 TMT/ELT/JWST

24 The Construction of the Antarctica Observatory at Dome A may become one of the most remarkable achievements of the human race

25 Study of the Early Universe with KDUST Xuelei Chen (NOAC) Wei Zheng (JHU) August 17, 2010, XiAn

26 Epoch at Redshift z>7 Reionization of the IGM First generation of black holes Rapid star formation August 17, 2010, XiAn

27 August 17, 2010, XiAn Kunlun Station at Dome A

28 Spectra of Quasar at z~6 August 17, 2010, XiAn White et al. 2003

29 August 17, 2010, XiAn Number of Quasars

30 Reionization of the IGM August 17, 2010, XiAn Fan et al. 2006

31 Requirements At least 5000 square degrees YJHK bands Limiting magnitude AB=24 August 17, 2010, XiAn

32 Supernovae of Population III Massive: solar mass Pair-instability outburst Bright: M~-24 Metal free August 17, 2010, XiAn

33 SCP 06F6 August 17, 2010, XiAn Quimby et al. 2009

34 An Example KDUST K-Dark Science 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

35 Surface Density of PISN August 17, 2010, XiAn Weinmann & Lilly 2005

36 Requirements Repeated observations over 10 square degrees Cadence of ~1-3 months Magnitude AB>26 August 17, 2010, XiAn

37 Gamma Ray Bursts Detectable at very high redshift Peak magnitude AB~20 August 17, 2010, XiAn

38 GRB at z=8.3 August 17, 2010, XiAn Tanvir et al. 2009

39 Requirements Fast communication link Fast slew capability (within minutes) Low- or medium-resolution spectrograph August 17, 2010, XiAn

40 Summary KDUST is a powerful in high-z studies Complimentary to JWST, TMT Need both wide and deep surveys August 17, 2010, XiAn