Frontier Science Enabled by a Giant Segmented Mirror Telescope: Frontier Science Enabled by a Giant Segmented Mirror Telescope Rolf-Peter Kudritzki 1 for the GSMT Science Working Group 1 Chair, GSMT Science Working Group Institute for Astronomy, University of Hawaii http://www.aura-nio.noao.edu/gsmt_swg/SWG_Report/SWG_Report_7.2.03.pdf


GSMT SWG Members: GSMT SWG Members Chair: Rolf-Peter Kudritzki, UH IfA Vice-Chair: Steve Strom, NOAO SWG Members: Jill Bechtold -- UA Mike Bolte -- UCSC Ray Carlberg -- U Toronto Matthew Colless -- ANU Irena Cruz-Gonzales -- UNAM Alan Dressler -- OCIW Betsy Barton– UC Irvine Terry Herter -- Cornell Masanori Iye – NOAJ Jay Frogel – AURA HQ Paul Ho -- CfA Jonathan Lunine -- UA LPL Claire Max -- UCSC Chris McKee -- UCB Francois Rigaut -- Gemini Doug Simons -- Gemini Chuck Steidel -- Caltech Kim Venn -- Macalester http://www.aura-nio.noao.edu/gsmt_swg/


Slide3: Connecting the First Nanoseconds to the Origin of Life


The first stars in the universe - clues from hydrodynamic simulations: The first stars in the universe - clues from hydrodynamic simulations Hydrodynamic simulations by Davé, Katz, andamp; Weinberg Ly-α cooling radiation (green) Light in Ly-α from forming stars (red, yellow) z=10 z=8 z=6


Stars forming at z=10!: Stars forming at z=10! Simulation As observed through 30-meter telescope R=3000, 105 seconds, Barton et al., 2004, ApJ 604, L1 1 Mpc (comoving)


A possible IMF diagnostic at z=10: A possible IMF diagnostic at z=10 HeII (l1640 Å) Standard IMF HeII (l1640 Å) Top-Heavy IMF, zero metallicity (IMF + stellar model fluxes from Bromm, Kudritzki, andamp; Loeb 2001, ApJ 552,464)


Star formation at z ≥ 7: Star formation at z ≥ 7 area of 2’ × 2’ ~ (5 Mpc)3 at z = 10  simulations predict several tens of objects detectable with GSMT 2’ × 5’ FoV  fair sampling of very early universe with up to 400 pointings imaging (MCAO, GLAO) and follow-up spectroscopy (R ~ 3000, multiplex 100-600) Morphological studies on scales andlt; 100 pc with AO


Slide8: Predicted cosmic web of intergalactic gas and galaxies at z = 3.5 IGM clumps concentrated by dark matter  galaxies GSMT will reveal cosmic web 3D-structure and physics of assembly process of galaxies!! z = 3 galaxy building blocks Hubble Deep Field


Slide9: Tomographic survey of universe @ z = 3.5 Survey 5º × 5º ~ 600Mpc × 600 Mpc × 900Mpc @ 2.5 andlt; z andlt; 4.5 106 galaxies mR ≤ 26.5 MOS (1000) spectra: R ~ 2000, S/N ~ 5  redshifts, 3D-distribution, dark matter distribution, SFRs 105 galaxies mR ≤ 25.5 MOS (1000) spectra: R ~ 2000, S/N ~ 20  chemical composition, IMF 103 galaxies mR ≤ 25.0 MOS (20) spectra: R ~ 20000, S/N ~ 5  internal kinematics with resolution ≤ 1kpc some 250 galaxies with ≤ 100pc (MCAO) 104 galaxies mR ≤ 24.0 MOS (20) spectra: R ~ 20000, S/N ~ 30 background sources for IGM  3D-distribution and chemistry of IGM/galaxies Only GSMT can take spectra of these faint objects !!!


Slide10: Input 30m 8m The power of GSMT Intrinsic spectrum of faint quasar with 'forest' of intergalactic gas absorption lines All night exposure with 8m-telescope All night exposure with GSMT (J. Bechthold)


Formation of giant galaxies: Formation of giant galaxies Hydro-simulation 'Antennae' galaxy – two galaxies merging (C. Mihos, L. Hernquist) (HST, B. Whitmore)


GSMT narrow-band imaging of starbursts: GSMT narrow-band imaging of starbursts Simulated monochromatic images of the ‘Antennae’ (local starburst galaxy: 105 seconds integration time) Courtesy: E. Barton 2'


Galaxy Kinematics with GSMT: z=0.01 z=1.5 8m z=1.5 30m Galaxy Kinematics with GSMT Ha in typical spiral galaxy: 105 sec exposure 80' 3'


Connecting the Distant & Local Universe: Connecting the Distant andamp; Local Universe


Formation of giant galaxies: Formation of giant galaxies Hydro-simulation 'Antennae' galaxy – two galaxies merging


Slide16: The halos of Milky Way-like galaxies Simulation depicting streams of dynamically and chemically distinct stars (color coded) Remnants of multiple past merger events Spectroscopy with GSMT will provide complete genealogical record and nucleosynthesis history together with dynamics (P. Harding)


The different stellar populations in galaxies: The different stellar populations in galaxies Goals: Quantify ages; [Fe/H], [a/H], [s,r/H], ; for stars in nearby galaxies spanning all types Use ‘archaelogical record’ to understand the assembly process Quantify IMF in different environments Measurements: CMDs for selected areas in local group galaxies Spectroscopy (R ~ 1500  kinematics, ~ 40000  nucleosynthesis) Key requirements: MCAO delivering 2’ FOV; MCAO-fed NIR spectrograph


M32: M32 Gemini North Hokupa’a AO (IfA) same region JWST simulation same region GSMT simulation K. Olson, F. Rigaut, B. Ellerblok


Stellar Populations in Galaxies: Stellar Populations in Galaxies M 32 (Gemini/Hokupaa) GSMT with MCAO 20' Population: 10% 1 Gyr, [Fe/H]=0; 45% 5 Gyr, [Fe/H]=0; 45% 10 Gyr, [Fe/H]=-0.3 Simulations from K. Olsen and F. Rigaut


Assumptions for MCAO simulations: Assumptions for MCAO simulations J K FWHM 0.009 0.015 arcsec Strehl 0.2 0.6 PSF includes effects of limited number of actuators in deformable mirrors optical effects of the primary mirror segments (tilt, de-phasing) limited temporal sampling of wave fronts limited spatial resolution of wave front sensors no PSF variations with time and position included


Slide21: NGC 3621 7Mpc Bresolin, Kudritzki, Mendez, Przybilla, 2001, ApJ Letters, 548, L159


NGC 3621: NGC 3621


Slide23: NGC 3621 7Mpc Bresolin, Kudritzki, Mendez, Przybilla, 2001, ApJ Letters, 548, L159 NGC 3621


Formation and Evolution of Planetary Systems: Formation and Evolution of Planetary Systems Direct observation of hundreds of extra-solar giant planets and thousands of the disks from which they form


Proto-planetary disks around stars: Proto-planetary disks around stars Keck Telescope, AO Michael Liu, IfA, 2004 AU Microscopii


Proto-planetary disks around stars: Proto-planetary disks around stars planetary gap Keck Telescope, AO Michael Liu, IfA, 2004 FWHM = 0.04 arcsec H-Band


Probing Planet Formationwith High Resolution Infrared Spectroscopy: Probing Planet Formation with High Resolution Infrared Spectroscopy Simulated 8 hr exposure of mid-IR CO fundamental spectral line profile emitted by gas in gap produced by giant planet width of line  location in disk Width of line peaks  width of gap  mass of planets


Formation of planets in proto-planetary disks : Formation of planets in proto-planetary disks Goals ● AO imaging and IR spectroscopy of thousands of disks around nearby young stars  diversity of disk systems ● characterize physics of disks T(r), ρ(r) ● detect giant planets directly ● detect giant planets indirectly from gravitational 'gaps' in disks ● characterize planets from properties of disks (location, widths) Measurements ● Spectra R~105; l ~ 5m in SF regions Key requirements ● on axis, high Strehl AO; low emissivity ● exploit near-diffraction-limited mid-IR performance


Exploring other solar systems: Exploring other solar systems Artist conception of planetary system orbiting around 55 Cancri using results of radial velocity Keck observations More than 100 planets around other stars detected so far ('indirect' technique- very small periodic spectral line shifts indicate orbital motion) Most planetary systems vastly different from Solar System No direct images of other planetary systems so far


Planets around other stars : Planets around other stars 'Brown Dwarf' orbiting a star at same distance as Saturn from sun Gemini/Keck AO detection by Michael Liu (IfA), 2002 Problem: Planets much fainter than Brown Dwarfs 30m telescope needed !!  GSMT !!


The power of GSMT: The power of GSMT GSMT will allow for the first time ● To image giant planets surrounding many hundred stars out to distances as great as 200 light years (coronography + AO) ● To determine masses and radii by imaging and spectroscopy ● To analyze their atmospheric structure and chemical composition by spectroscopy


Slide32: GSMT  Detection of 55 CnC b/c Chemical composition of Atmosphere of 55 CnC b Sudarsky, Burrows andamp; Hubeny, 2003 55 Cancri – physical characterization by spectroscopy


GSMT discovery space: GSMT discovery space


Slide34: The physics of giant exo-planets Goal: Image and characterize exo-planets Mass, radius, albedo Atmospheric structure Chemistry  physics of giant planet formation repercussion for formation of terrestrial planets, life on terrestrial planets Rotation 'Weather' Measurements: R~ 10 photometry andamp; R ~ 200 spectra Near-infrared (reflected light) Mid-infrared (thermal emission) Role of GSMT: Enable measurements via High sensitivity High angular resolution


GSMT & JWST – The Power of Two: GSMT andamp; JWST – The Power of Two The top two priority missions of the 2001 Decadal Survey in Astronomy and Astrophysics Each gives orders of magnitude gain in sensitivity over existing ground and space telescopes Each has its own set of unique capabilities The two sets of unique capabilities strongly complement each other. Complementary capabilities open a new, exciting epoch for cosmic discovery


Slide36: GSMT: Sensitivity 25 times JWST in accessible spectral regions Optical sensitivity 0.32 to 1.0 µm , FOV ≥ 10’ High spectral resolution up to 100,000 in O/IR Extreme spatial resolution in the infrared - 5x JWST with extreme AO Flexible and upgradeable advantage of new developments in instrumentation JWST: Full sky coverage with high observing efficiency continuous wavelength coverage 0.6 – 27 µm low thermal, no OH background  very high broadband sensitivity Imaging over wide FOV, diffraction limited for λandgt;2 µm PSF constant across field PSF stable with time High dynamic range Each has unique capabilites:


SWG recommendation : SWG recommendation Immediate NSF investment in support of a technology program to develop viable, cost-effective GSMT concepts within next four years (echoing decadal survey) Proposals in this program should show  evidence of value of proposed investment to multiple GSMT-type programs  proactive commitment to share results among programs Coherent supervision and coordination needed Investment should result in public access to telescope time


Slide38: http://www.aura-nio.noao.edu/gsmt_swg/ http://www.aura-nio.noao.edu/gsmt_swg/ SWG_Report/SWG_Report_7.2.03.pdf Complete information about SWG  This science report 