KDUST Supernova Cosmology

Lifan WangCCAA

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• DES calibration – need to communicate with

DES on their calibration precision and wavelength

• LSST overlap

• IR photometry to 1%? How?

Survey Cadence

• LSST simulation pipeline• Deep field?• Shallow field?

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

Pre-KDUST

• AST3+KPT1. About 1000 Nearby SN with nightly spectroscopy

• KDUST1. Narrow field - Over a 10 sq degrees of complete

SN mapping2. Wide field – Over 100 square degrees of less

dense coverage

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/

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.

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

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.

Project Schedule

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

Technical and Scientific Projects

• Telescope: built by NIAOT• First generation instruments: IFU and NIR

Camera• Second generation instruments: PI

instruments• PI sciences

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.

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

AST3

Kim et al. 2010

AST3

Kim et al. 2010

AST3

Kim et al. 2010

KPT-IFU

Kim et al. 2010

KPT-IFU

Kim et al. 2010

KPT-SLITLESS

Kim et al. 2010

KPT-SLITLESS

Kim et al. 2010

KPT-NIRCAM

Kim et al. 2010

KDUST

• Dense field 1. Rates of various events2. Observational simulation – cadence etc

• Porous field1. What’s for?

• Dark energy constraints • Dark matter constraints

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

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

KDUST(8m)

Kim et al. 2010

Summary1. A self-contained search and survey over five years can yield

a spectrophotometric time 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,reducing systematics.

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 redshift range over which we measure the expansion history of the universe.

Kim et al. 2010