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LSST followup

LSST followup. Jeremy Mould NOAO. Followup challenge. Every night LSST is expected to survey over 3000 sq deg and compare objects < 24th magnitude with a template image. Spectroscopic followup of supernovae, GRBs, novae, and AGN will tax the resources of the U.S. system:

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LSST followup

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  1. LSST followup Jeremy Mould NOAO

  2. Followup challenge • Every night LSST is expected to survey over 3000 sq deg and compare objects < 24th magnitude with a template image. • Spectroscopic followup of supernovae, GRBs, novae, and AGN will tax the resources of the U.S. system: • IMACS, GWFMOS, Hectospec, MODS, HET's spectrographs • and their successors. • To plan to make the most of this opportunity, we should develop the capability to followup LSST's precursors: • PanStarrs • Dark Energy Camera. • + need imaging followup to supplement LSST's limited cadence

  3. Areas of available spectrographs This 3.5 degree field is accessed twice a minute by LSST

  4. LSST followup science

  5. GSMT SWG The GSMT SWG is a community-based group convened to: • Formulate a powerful science case for federal investment in GSMT • Identify key science drivers • Develop clear and compelling arguments for GSMT in the era of JWST/ALMA • Discuss realization of key science as a function of design parameters: aperture, FOV, PSF…… • Generate unified, coherent community support

  6. GSMT SWG Members Chair: Rolf-Peter Kudritzki, UH IfA SWG Members: • Jill Bechtold -- UA • Mike Bolte -- UCSC • Ray Carlberg -- U of T • Matthew Colless -- ANU • Irena Cruz-Gonzales -- UNAM • Alan Dressler -- OCIW • Betsy Gillespie -- UA • Terry Herter -- Cornell • Jonathan Lunine -- UA LPL • Claire Max -- UCSC • Chris McKee -- UCB • Francois Rigaut -- Gemini • Chuck Steidel -- CIT • Steve Strom -- NOAO

  7. GSMT CELT VLOT The GSMT, CELT and VLOT point design telescope concepts. TMT is a fusion of 3 concepts

  8. Highest Priority Capabilities for First Light • diffraction-limited (10 mas @ 1.6m) imaging & spectroscopy • 0.8- to 2.5-micron wavelength • 1-2 arcminutes multi-conjugate adaptive optics (MCAO) field • Strehl ratio at K-band of 0.7, constant across the field to 10%; • highly-multiplexed (~1,000 slits) • seeing-limited 100 < R < 7,000 spectroscopy • 0.32- to 1-micron wavelength range • wide (10-20 arc-minute) field • high-spectral-resolution (20,000 < R < 100,000) spectroscopy • 1- to 5-micron • 7- to 28-micron

  9. Giant Magellan Telescope (GMT) GMT alternate 7 x 8.4 meter mirrors

  10. LSST followup science

  11. TMT AO modes

  12. LSST followup science

  13. TMT phased implementation • optical spectroscopy with 20,000 < R < 100,000 • 0.3 microns to 1 micron • very high-contrast imaging near diffraction limit 1 to 2.5m • contrast ratio > 108 at q > 4l/D from bright stars • R ~3,000-5,000 spectroscopy • fields ≥5 arcminutes • 0.7- to 2.5-micron • sampling 0.15 arcseconds • image quality 80% enclosed energy in 0.3 arc-sec. • unit (IFU) heads or microslits • ground-layer adaptive optics system (GLAO); • mid-IR diffraction-limited imaging (Strehl > 0.5, 7m <  < 28m) over a field >30 arcseconds;

  14. LSST followup science

  15. LSST observing Simulator • Initially Created By Abi Saha • New Simulation Tool in Development • K. Cook et. al. • Foundation and Testbed for Scheduler A. Saha, NOAO

  16. Mt John observatory, Wise observatory in Israel, the Boyden and SAAO observatories, MDM and MONET, the CIDA, CTIO, EROS and ESO. Networks of moderate aperture telescopes are needed to follow up planetary transits A possible future role for the 4 meter telescopes MOA/PLANET network

  17. LSST followup science

  18. Galactic Archaeology • Star-by-star reconstruction of the formation of the Milky Way • Substructure retains signatures in chemical elements, kinematics and age distributions • Chemical and kinematic `tagging’ of significant samples of thin disk/thick disk/halo stars -- a million stars (factor 104 beyond present) • Elemental abundances, r,s, , accurate kinematics

  19. Galactic Substructure Sgr dSph; Smecker-Hane & McWilliam 03 dSph plus Galactic stars; Tolstoy et al 03 Sgr dSph extent known in 97 Wyse, Gilmore & Franx 97 Sgr dSph tidal streams from 2MASS Majewski et al 03

  20. K.A.O.S.!Kilo-Aperture Optical Spectrograph • Gemini WFMOS • 1.5 degree field of view • ~4800 fibers • 12 spectrographs (4k x 4k CCDs) • Nod-and-shuffle sky subtraction • Currently a Gemini feasibility study led by the AAO 10-100 times better than any extant or planned facility

  21. LSST followup science

  22. Baryon oscillations as a standard ruler 1º peak Harmonics of sound horizon

  23. How it should work Blake & Glazebrook (2003) • 0.5<z<1.3 • 2×106 galaxies (unbiassed) • 6 Vsloan(~1 Gpc3) • 600 deg2 http://www.noao.edu/kaos/

  24. KAOS survey for baryon acoustic fluctuations • 0.5 < z < 1.3 1000 deg2 • ∼2–3 106 galaxies • 1 hour exposures • 2.5 < z < 3.5 400 deg2 • ∼0.5-1 × 106 galaxies • 3 hour exposures • 150 nights Subaru implementation is also being studied

  25. KAOS w(z) constraints

  26. Note that AW = 5 x 105 is 4p sr covered continuously by 4 m telescopes Survey capability is growing all the time AW deg2m2 Cost $M PS1 DESPS4 LSST JDEM

  27. PS1 PS4 DES LSST IMACS Hectospec AAOmega GWFMOS GSMT-MOS Important to keep spectroscopic capability growing alongside

  28. NOAO Planning • Note that the earliest first light on these facilities (subject to funding) is ~ • GWFMOS 2008 • LSST 2012 • GSMT 2016 • NOAO will need to enable access to the followup facilities that matches the LSST driven needs • Long Range Planning Committee (Chair: C. Pilachowski) is currently working on a roadmap for large scale facilities http://www.noao.edu/dir/lrplan/lrp-committee.html

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