1. STScI - May 8, 20081 Destiny, The Dark Energy Space Telescope

2. STScI - May 8, 20082 Science Goals & Overview Determine the expansion history of the Universe to 1% accuracy in  z = 0.1 bins over the last 10 10 yr. Constrain Dark Energy equation of state parameters w 0 to 0.05 and w a to 0.20. Destiny is a Stage IV dark energy program.

3. STScI - May 8, 20083 DESTINY Fact Sheet 1.65m telescope at L2 H2RG FPA SN1a survey over > 3° 2 WL survey 1000° 2 NIR imaging 0.85  m <  1.7  m Imaging Spectrograph with  ~ 75

4. STScI - May 8, 20084 A Brief History of Destiny Astronomical community recognizes the potential of dark energy space probes. NASA & DOE propose a generic Joint Dark Energy Mission Initial Destiny concept for JDEM proposed in 2003. Wins initial concept study. LMCO & LANL partners. NASA creates general “Beyond Einstein” program for astrophysical missions: Con-X, LISA, CMB probes, etc. Includes JDEM. Destiny wins 1 of 3 JDEM concept studies in 2006. NRC BEPAC recommends JDEM for first BE start in 2007. Probable JDEM call in September 2008 for 2009 start.

5. STScI - May 8, 20085 DESTINY Philosophy Complete heritage - Well understood technology in a unique configuration. Use the minimal instrument required Do only in space what must be done in space - leverage ground based observations. All spectra all the time. Complete spectro- photometric time series on all SN events. Highly automated survey - no time critical operations.

6. STScI - May 8, 20086 Destiny Science Team PI: Tod R. Lauer (NOAO) Matthew Beasley (Colorado) Chris Burns (OCIW) Kenneth Carpenter (GSFC) Doug Clowe (Ohio U) Ian Dellantonio (Brown) Megan Donahue (MSU) Olivier Dore (Toronto) Chris Fassnacht (UC Davis) Wendy Freedman (OCIW) Chris Fryer (LANL) Peter Garnavich (notre Dame) Jay Holberg (Arizona) Aimee Hungerford (LANL) Robert Kirshner (Harvard) Lori Lubin (UC Davis) Deputy PI: Dominic Benford (GSFC) Sangeeta Malhotra (ASU) Tom Matheson (NOAO) Phillip Pinto (Arizona) Nor pirzkal (STScI) Marc Postman (STScI) James Rhoads (ASU) Yong-Seon Song (Chicago) George Sonneborn (GSFC) Sumner Starrfield (ASU) Nicholas Suntzeff (TAMU) Frank Timmes (ASU) Thomas Vestrand (LANL) Mike Warren (LANL) Rogier Windhorst (ASU) Robert Woodruff (LMCO) Ann Zabludoff (Arizona)

7. STScI - May 8, 20087 Supernovae

8. STScI - May 8, 20088 Why go to high redshifts? Dark energy can be detected at low redshift, but precise constraints on the DE Eos requires measurements over both the acceleration and deceleration epochs. SpaceGround

9. STScI - May 8, 20089 NIR available only in space Crucial near-infrared observations are impossible from the ground for the required photometric accuracy Sky is very bright in NIR: >100x brighter than in visible Sky is not transparent in NIR: absorption due to water is very strong and extremely variable Data from Gemini Observatory & ATRAN: Lord (1992)

10. STScI - May 8, 200810 Riess et al. (2004) obtain ACS grism spectra of z ~ 1.3 SN Ia

11. STScI - May 8, 200811 ACS Grism Images of SN2002FW (z = 1.30) Riess et al. (2004)

12. STScI - May 8, 200812 Supernova Observations 1. Filter: locate SN & host galaxy 2. Dispersed mode: spectral time series 3. Difference & extract SN spectrophotometry

13. STScI - May 8, 200813 Supernovae Survey Schema Survey area is a contiguous Mosaic of Destiny FOVs. Orientation rolls by 90º every 3 months. Dithering will fill in chip gaps and ensure Nyquist sampling.

14. STScI - May 8, 200814 Observing Timeline for SN Survey Times and slews are not shown to scale

15. STScI - May 8, 200815 Preliminary Operations Times for SN Survey Times and slews are not shown to scale

16. STScI - May 8, 200816 Supernova Types

17. STScI - May 8, 200817 Supernova Spectra Simultaneous spectrum & photometry = redshift & brightness Redshift from 615nm SiII line Equal precision & more accuracy than broadband filters alone

18. STScI - May 8, 200818 Light Curve Calibration

19. STScI - May 8, 200819 Supernova Light Curves Always get photometry around maximum light Sample every 5 days

20. STScI - May 8, 200820 Sn Photometric Calibration Obtain high fidelity external and internal flats in ground tests. Monitor with internal flats on orbit, plus field stars. Absolute photometric calibration with DA white Dwarfs. Sn spectra isolated with differencing. Ad hoc spectral flat extracted from data cube of monochromatic flats.

21. STScI - May 8, 200821 Supernova Survey Present day & ongoing surveys find hundreds

22. STScI - May 8, 200822 Supernova Survey Present day & ongoing surveys find hundreds Destiny will find >3000 SN in 2 yrs. Most at z~1; requires 3.2 deg 2 survey area

24. STScI - May 8, 200824 Weak Lensing

25. STScI - May 8, 200825 Dark Energy equation of state: w=p/  (w=-1 for  ) modifies: angular-diameter distance growth rate of structure power spectrum on large scales  w can be measured from the lensing power spectrum Dark Energy and Weak Lensing a(t)

26. STScI - May 8, 200826 Predicted Survey Results Assuming a Flat Universe

27. STScI - May 8, 200827 Predicted Survey Results Not Assuming a Flat Universe See Knox, Song & Zhan 2006

28. STScI - May 8, 200828 Observatory Lockheed Spacecraft bus Goodrich Optical Telescope Assembly GSFC Science Instrument, Teledyne FPA GSFC Instrument Outer Baffle Destiny Observatory Destiny OTA + Science Instrument Destiny Optics Spacecraft Bus Fixed Solar Array Instrument Radiators Outer Baffle Assembly Goodrich OTA GSFC Science Instrument 1.65m primary mirror Telescope Optical Bench

29. STScI - May 8, 200829 Launch Around 2015 ~1,500,000 km ~340,000 km ~ 1,500,000 km L2

30. STScI - May 8, 200830 Mission Operations / Data Flow

31. STScI - May 8, 200831 Destiny, The Dark Energy Space Telescope