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Frontier Science Enabled by a Giant Segmented Mirror Telescope
Rolf-Peter Kudritzki 1 forthe 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
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GSMT SWG Members
Chair: Rolf-Peter Kudritzki, UH IfAVice-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/
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Connecting the First Nanoseconds to the Origin of Life
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The first stars in the universe - clues from hydrodynamic simulations
• Hydrodynamic simulations by Davé, Katz, & Weinberg
– Ly-α cooling radiation (green)
– Light in Ly-α from forming stars (red, yellow)
z=10 z=8 z=6
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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)
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A possible IMF diagnostic at z=10HeII (1640 Å)Standard IMF
HeII (1640 Å)Top-Heavy IMF, zero metallicity
(IMF + stellar model fluxes from Bromm, Kudritzki,& Loeb 2001, ApJ 552,464)
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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 < 100 pc with AO
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Predicted cosmic web of intergalactic gas and galaxies at z = 3.5
IGM
clumpsconcentrated by darkmatter galaxies
GSMT will reveal cosmic web 3D-structure and physics of assembly process of galaxies!!
z = 3 galaxy building blocksHubble Deep Field
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Tomographic survey of universe @ z = 3.5
Survey 5º × 5º ~ 600Mpc × 600 Mpc × 900Mpc @ 2.5 < z < 4.5
106 galaxies mR ≤ 26.5 MOS (1000) spectra: R ~ 2000, S/N ~ 5 redshifts, 3D-distribution, dark matter distribution, SFRs105 galaxies mR ≤ 25.5 MOS (1000) spectra: R ~ 2000, S/N ~ 20 chemical composition, IMF103 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 !!!
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Input
30m
8m
The power of GSMT
Intrinsic spectrum of faint quasar with “forest”of intergalactic gas absorption lines
All night exposure with8m-telescope
All night exposure withGSMT
(J. Bechthold)
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Formation of giant galaxies
Hydro-simulation “Antennae” galaxy – two galaxies merging(C. Mihos, L. Hernquist) (HST, B. Whitmore)
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GSMT narrow-band imaging of starbursts
Simulated monochromatic images of the ‘Antennae’ (local starburst galaxy: 105 seconds integration time)Courtesy: E. Barton
GSMT
2”
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z=0.01 z=1.5 8m
z=1.530m
Galaxy Kinematics with GSMT
Hin typical spiral galaxy: 105 sec exposure
80” 3”
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Connecting the Distant & Local Universe
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Formation of giant galaxies
Hydro-simulation “Antennae” galaxy – two galaxies merging
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The halos of Milky Way-like galaxies
Simulation depictingstreams of dynamicallyand chemically distinctstars (color coded)
Remnants of multiple past merger events
Spectroscopy with GSMTwill provide completegenealogical recordand nucleosynthesishistory together with dynamics
(P. Harding)
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The different stellar populations in galaxies
• Goals:– Quantify ages; [Fe/H], 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
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M32
Gemini NorthHokupa’a AO (IfA)
same region JWSTsimulation
same region GSMTsimulation
K. Olson, F. Rigaut, B. Ellerblok
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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
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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
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NGC 3621
7Mpc
Bresolin, Kudritzki,
Mendez, Przybilla,
2001, ApJ Letters,
548, L159
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NGC 3621
NGC 3621
7Mpc
Bresolin, Kudritzki,
Mendez, Przybilla,
2001, ApJ Letters,
548, L159
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NGC 3621
7Mpc
Bresolin, Kudritzki,
Mendez, Przybilla,
2001, ApJ Letters,
548, L159
NGC 3621
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Formation and Evolution of Planetary Systems
Direct observation of hundreds of extra-solar giant planets and thousands of the disks from which they form
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Proto-planetary disks around stars
Keck Telescope, AOMichael Liu, IfA, 2004
AU Microscopii
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Proto-planetary disks around stars
planetary gap
Keck Telescope, AOMichael Liu, IfA, 2004 FWHM = 0.04 arcsecH-Band
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Probing Planet Formationwith High Resolution Infrared Spectroscopy
Simulated 8 hr exposure of mid-IRCO fundamental spectral line profileemitted by gas in gap produced by giant planet
width of line location in disk Width of line peaks width of gap mass of planets
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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; in SF regions
Key requirements
● on axis, high Strehl AO; low emissivity
● exploit near-diffraction-limited mid-IR performance
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Exploring other solar systems
Artist conception of planetary system orbiting around 55 Cancri using results of radial velocity Keck observations
More than 100 planetsaround other starsdetected so far (“indirect” technique-very small periodicspectral line shifts indicate orbital motion)
Most planetary systemsvastly different fromSolar System
No direct images ofother planetary systemsso far
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Planets around other stars “Brown Dwarf”orbiting a star at samedistance as Saturn from sun
Gemini/Keck AO detectionby Michael Liu (IfA), 2002
Problem: Planets much fainter than Brown Dwarfs
30m telescope needed !!
GSMT !!
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The power of GSMTGSMT 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
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GSMT Detection of 55 CnC b/cChemical composition ofAtmosphere of 55 CnC b
Sudarsky, Burrows& Hubeny, 2003
55 Cancri – physical characterization by spectroscopy
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GSMT discovery space
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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 & R ~ 200 spectra– Near-infrared (reflected light)– Mid-infrared (thermal emission)
Role of GSMT: Enable measurements via– High sensitivity– High angular resolution
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GSMT & 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
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• 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 λ>2 µm PSF constant across field
PSF stable with time
High dynamic range
Each has unique capabilites:
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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
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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