1 / 29

KDUST Supernova Cosmology

KDUST Supernova Cosmology. Lifan Wang CCAA. Key Problems. Absolute photometric precision to 1%? Relative photometric precision to ??? K-correction Extinction Intrinsic evolution Nearby Cepheid calibration. Survey Field. SDSS calibration – is it good enough? SPT field

olinda
Télécharger la présentation

KDUST Supernova Cosmology

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. KDUST Supernova Cosmology Lifan Wang CCAA

  2. Key Problems • Absolute photometric precision to 1%? • Relative photometric precision to ??? • K-correction • Extinction • Intrinsic evolution • Nearby Cepheid calibration

  3. Survey Field • SDSS calibration – is it good enough? • SPT field • DES calibration – need to communicate with DES on their calibration precision and wavelength • LSST overlap • IR photometry to 1%? How?

  4. Survey Cadence • LSST simulation pipeline • Deep field? • Shallow field?

  5. New Sciences with SNIa • Strong lensing, Hubble constant • Weak lensing of SNIa • Mass sheet degeneracy • Dark matter halo around clusters • Dark matter halo around galaxies • Metallicity evolution • Star formation

  6. Pre-KDUST • AST3+KPT • About 1000 Nearby SN with nightly spectroscopy • KDUST • Narrow field - Over a 10 sq degrees of complete SN mapping • Wide field – Over 100 square degrees of less dense coverage

  7. For Mission Updates • http://aag.bao.ac.cn/ - updates at NAOC • http://kdust.org - latest on KDUST • http://dome-a.physics.tamu.edu/~lifanwang • http://ccaa.pmo.ac.cn/

  8. The Collaborating Institutes • The project will be coordinated by CCAA, whose member institutes include: PMO, NAOC, NIAOT, IHEP, PRIC, and more … • International partners interested in the project: LBNL, Texas A&M University, Johns Hopkins University, and JPL.

  9. Project Goals • Engineering pathfinder to cope with technical challenges • Site verification telescope to derive important data on seeing, sky background, and the overall stability of the site • Forefront astronomical study in dark energy, dark matter, black holes, stellar structures, and extrasolar planets

  10. Basic Characteristics • 1 meter aperture • Fully steerable, with pointing accuracy to within one arc second • Routine high quality imaging at seeing of ~0.3 arc seconds • Optical spectroscopy • Near infrared imaging from 1000-3500 nm.

  11. Project Schedule • Conceptional Design 2009-2011 • Telescope construction 2010-2012 • Integration and testing 2012-2013 • First light at Dome A 2013-2014

  12. Technical and Scientific Projects • Telescope: built by NIAOT • First generation instruments: IFU and NIR Camera • Second generation instruments: PI instruments • PI sciences

  13. PI Instruments and PI Sciences • Supernova Cosmology • Asteroseismology • Extrasolar Planets • Black holes • Time domain astronomy – GRBs, supernovae, novae, etc. • Strong lensing The PIs will be in charge of successful execution of relevant science projects. CCAA will form review panels to evaluate the feasibility of PI instruments and related science projects.

  14. Supernova Cosmology Observations of 800 Type Ia supernovae at red shift between 0.03-0.08 There are less than 100 well observed SNIa today, most of them with poor spectral coverage KPT will improve the situation by at least a factor of 10. This paves the road for future dark energy programs such as JDEM, LSST, and KDUST KPT is the necessary first step in building up the distance ladder for cosmological probes

  15. AST3 Kim et al. 2010

  16. AST3 Kim et al. 2010

  17. AST3 Kim et al. 2010

  18. KPT-IFU Kim et al. 2010

  19. KPT-IFU Kim et al. 2010

  20. KPT-SLITLESS Kim et al. 2010

  21. KPT-SLITLESS Kim et al. 2010

  22. KPT-NIRCAM Kim et al. 2010

  23. KDUST • Dense field • Rates of various events • Observational simulation – cadence etc • Porous field • What’s for? • Dark energy constraints • Dark matter constraints

  24. KDUST • Over 10,000 SNIa a day • Many many more SNII, SNIbc, … • Orphan GRBs • Exposure time calculator: http://dome-a.physics.tamu.edu/~lifanwang • More updates in the future: http://kdust.org

  25. KDUST(8m) Multiply the exposure time by a factor of 4 to get the exposure time for a 4 meter KDUST Kim et al. 2010

  26. KDUST(8m) Kim et al. 2010

  27. Summary 1. A self-contained search and survey over five years can yield a spectrophotometrictime series of 1000 z < 0.08 supernovae. 2. These can serve to anchor the Hubble diagram and quantify the relationship between luminosities and heterogeneities within the Type Ia supernova class,reducingsystematics. 3. Larger aperture (&4-m) telescopes are capable of discovering supernovae shortly after explosion out to z~3. 4. These can be fed to space telescopes, and can isolate systematics and extend the redshiftrange over which we measure the expansion history of the universe. Kim et al. 2010

More Related