Exploring the time domain

1. Exploring the time domain • Gamma ray bursters • Supernovae • accretion disk instabilities • galactic to stellar scales • planetary transits • moving objects LSST

2. View of the LSST telescope structure in the Steward Observatory straw man design. The primary mirror is at the center, and the secondary and tertiary are almost equidistant from the primary. The detectors are just ahead of the central hole in the primary (see: http://dmtelescope.org/ design.html) LSST, a digital survey of the sky each week • Weak lensing mass map of the Universe • 100,000 supernovae per year z < 1 • Earth crossing asteroids • 10,000 primordial trans-Neptunian objects

3. LSST Weak Lensing survey Low z WL

4. Deep Mode 1000’s/yr Need IR too Scan mode 1000’s/yr LSST Supernovae

5. LSST SN LSST Lensing MULTIPLE PROBES: TEST FOUNDATIONS w

6. Solar System Objects • Increase inventory of solar system x100 • 10,000 NEAs, 90% complete >250m • Over 10 million MBAs • Cometary nuclei >15km @ Saturn • Extend size-n of comets to <100m • TNOs beyond 100AU • rare new objects

7. NEO Hazard

8. LSST science working group • Dave Monet • David Morrison • Nick Kaiser • Peter Garnavich • Dennis Zaritsky • Mike Shara • Steve Larson • Alan Stern • Dan Eisenstein • Zeljko Ivesic • Andy Connolly • Fiona Harrison • Tony Tyson • Michael Strauss chair • Kem Cook • Gary Bernstein • Dave Jewitt • Chris Stubbs • Alan Harris

9. LSST SWG Charge • Develop science case and priorities for LSST • Flowdown to engineering goals & requirements • Identify key instrumentation capabilities • Prepare 10 year Design Reference Mission • Establish the relationship with other facilities • SNAP, Gemini, VISTA, PanStarrs, Lowell 4 m, VST • Prioritize key technology developments • Assess design concepts science performance • Assemble community wide partnerships for proposals to NSF and NASA

10. Technology Development • Large field of view telescope • 8 meter primary • Detector development • Large filters • Gigapixel camera • Data acquisition system • 10-20 petabyte database • National Virtual Observatory • Data mining • Systems engineering • Simulations and theory

11. Apparatus & Eff. Science goals site & optics Figure of Merit Area surveyed (number of objects found) to some SNR at some magnitude limit, per unit time: A – aperture W – camera FOV QE – det. Eff. e – observing eff. Fsky – sky flux dW – seeing footprint

12. 8.4 meter Primary Mirror 3.5 meter Secondary Trapped Focus 4.2 meter Tertiary Primary Mirror Cell is integral part of Structure C Ring

13. The Large Synoptic Survey Telescope DATA PUBLIC. Simultaneously address: • Solar System Probes: Earth-crossing asteroids, Comets, TNOs • Space assets & space junk to 1 cm • Dark matter/dark energy via weak lensing • Dark matter/dark energy via supernovae • Galactic Structure encompassing local group • Dense astrometry over 10000 sq.deg -> deep proper motion science • Gamma Ray Bursts and transients to high z • Gravitational mlensing • Variable stars/galaxies • QSO time delays vs z • Transients to 27 mag: the unknown • 5-band 28 mag photometric survey • Unprecedented many Pbyte time-tagged photometric database

14. http://lssto.org

15. GSMT Top optical infrared priority ground based of the McKee Taylor decadal survey

16. “21st century astronomy is uniquely positioned to study the evolution of the universe in order to relate causally the physical conditions during the Big Bang to the development of RNA & DNA” – Riccardo Giacconi Connecting recombination to the formation of planets

17. Kinematics of Individual Galaxies out to z ~3 • Determine the gas and mass dynamics within • individual Galaxies • Multiple IFU spectroscopy • R ~ 5,000 – 10,000 GSMT 3 hour, 3s limit at R=5,000 0.1”x0.1” IFU pixel (sub-kpc scale structures) J H K 26.5 25.5 24.0

18. Probing Planet Formation with High Resolution Infrared Spectroscopy • Planet formation studies in the infrared (5-30µm): • Planets forming at small distances (< few AU) in warm region of the disk • Spectroscopic studies: • Residual gas in cleared region emissions • Rotation separates disk radii in velocity • High spectral resolution high spatial resolution S/N=100, R=100,000, >4m Gemini out to 0.2kpc sample ~ 10s GSMT 1.5kpc ~100s JWST X • 8-10m telescopes with high resolution (R~100,000) spectrographs can detect the formation of Jupiter-mass planets in disks around nearby stars (d~100pc).

19. R = 10,000 R = 1,000 R = 5 Comparative performance of a 30m GSMT with a 6.5m JWST Assuming a detected S/N of 10 for NGST on a point source, with 4x1000s integration GSMT advantage NGST advantage

20. NOAO’s role in GSMT • partnering with ACURA, UC & Caltech on TMT Design and Development Phase • site testing • community input on: • science drivers for a 30m • complementarities to otherfacilities (e.g. JWST, ALMA) • technology development • e.g. AODP • instrumentation • operations role

21. GSMT Site Evaluation NIO collaborating with Carnegie, CELT, Cornell, ESO, UNAM; to test: • Chajnantor • One or two additional Chilean Sites • Mauna Kea ELT site • Las Campanas • San Pedro de Martir

22. 500 m Wind Las Campanas Peak 2 Turbulent Kinetic Energy CFD Tools available for any proposed ELT site

23. Giant Segmented Mirror Telescope Science Working Group • NSF AST Division authorized NOAO to maintain the Science Working Group for GSMT • community based body to develop the science case and justification for any federal investment by NSF or other agencies in GSMT. • represent US community in assembling relevant partnerships for describing and advocating the appropriate federal role in this project. • this guidance is intended to be a product of all public, private and international groups that expect to play a role in the GSMT.

24. Claire Max Doug Simons Terry Herter Irene Cruz Gonzales Betsy Barton Francois Rigaut Michael Bolte Observer: Tetsuo Nishimura Paul Ho Matthew Colless Jill Bechtold Rolf Kudritzki chair Chris McKee Alan Dressler Ray Carlberg GSMT SWG first report June 2003 Emailjrm@noao.edu if you’d like a copy

25. Two Studies, One Result Results from 2 x 2 years of studies: • It is feasible to build a 30m Telescope that will fulfill the science objectives of theAASC, on a time scale comparable to JWST • The optics for a ~700m2 mirror can be manufactured, polished and assembled • Wind buffeting effects can be managed • The technologies exist or can be developed to enable diffraction limited imaging and spectroscopy in at least the IR • The instrumentation, though challenging, is within the capabilities of major institutions and industry • The cost for telescope construction, adaptive optics, initial instrumentation and including 30% contingency is between $600M - $700M

26. GMT Consortium • Giant Magellan Telescope • Magellan partners • Carnegie, CfA, • U of A • Michigan, MIT

27. GSMT will complement ALMA & JWST Explore the cosmic era of reionization and galaxy assembly Understand star formation, now and in the early Universe 10 mas at 1.6m