LAMA - astro.ubc.ca
Transcript of LAMA - astro.ubc.ca
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LAMA
LAMA
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LAMA
Large Astronomical Mercury-Mirror Array
Paul Hickson University of British ColumbiaKen Lanzetta SUNY Stony BrookRick Puetter UC San DiegoGene Sprouse SUNY Stony BrookAmos Yahil SUNY Stony Brook
Photo Credit: S. Radford.
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LAMA
Very Large Optical Telescope Concepts
“Continued progress in optical astronomy requires a telescope of aperture and resolution significantly larger than that of present instruments” – Next Generation CFHT CommitteeAperture in the range 30-100 meters is needed
Major Optical Telescope Projects/Proposals
2012?~ 1000 M$~ 50 mMAXAT
2007~ 800 M$8 m (space)NGST
2015+> 1000 M$~ 100 mOWL
2010?~ 600 M$~ 30 mCELT
First LightCostApertureProject
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LAMA
Primary Science Goals
Detect and study the first luminous systemsStudy the process of galaxy formation and evolution from redshift z ~ 20 to the presentDetermine the star formation history of the UniverseDetermine the cosmological parametersResolve the innermost regions of AGN and QSOsDetect and study the oldest and faintest stars
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LAMA
Observing Galaxy Formation
Photo Credit:NASA.
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LAMA
Finding The First Galaxies
Wavelength range 0.4 < ? < 2.5 umLyman-a visible to z = 19.6
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LAMA
Early Protogalaxies
Credit: NGST
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LAMA
Importance of ResolutionHST 2.4m NGST 8m LAMA 60m
Photo Credit:NASA
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Early Globular Clusters
Credit: NGST
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LAMA
Star-Formation History of the Universe?
Credit: NASA
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LAMA
Supernova Detection
-2
-1
0
1
2
3
0 2 4 6 8 10 12 14
z
log
Fv (
nJy)
LAMA 2um 300s flux limitType II, k = 0, lambda = 0Type II, k = 0, lambda = 1
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Object Counts (per square arcmin)
0.4z > 10173Strong Gravitational lenses
45 < z < 1074z < 578Active Galactic Nuclei
10.5Supernovae II per year0.3z > 1055 < z < 1051z < 557Lyman-a emitters (R = 100)
202z > 10778675 < z < 101757708z < 52628781Galaxies1 (KAB = 31.4)10 (KAB = 28.9)Flux (nJy)
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LAMA
Performance Goals
0.4 – 2.5 um wavelength range< 0.1 nJy detection limit for point sources< 1 nJy detection limit for galaxiesMilliarcsec resolution~ 100 square arcmin survey area:
> 105 galaxies~ 100 supernovae per year
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LAMA
Emerging Technologies
Adaptive OpticsOptical interferometry Large mercury mirrorsNear-zenith tracking opticsOH absorption cellLarge VIS/NIR arrays
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Adaptive Optics FWHM = 0.08 arcsec
FWHM = 0.8 arcsec
Credit: Gemini Project
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Adaptive Optics Performance
Distance from Guide Star (arcsec)Credit: Matt Mountain
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Image Intensity
00.10.20.30.40.50.60.70.80.9
1
0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4
wavelength (um)
Rel
ativ
e V
alue
FWHMStrehlIntensity
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LAMA
Optical Interferometry NPOI
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LAMA
Optical Interferometry
Frontier technologyPhase closure with independent telescopes has been demonstratedPrototype arrays: I2T, MkIII, IRMAOperational arrays: PTI, IOTA, NPOI, ISI, GI2T, SUSIUpcoming arrays: COAST, VLTI, KeckPhase errors within individual apertures are corrected with adaptive opticsMoving mirrors remove zero-point (piston) phase differencesPhase tracking on light from natural guide starLBT design gives interferometric imaging over 40 arcsec
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LAMA
LBT Imaging Interferometer
2 x 8.4 m interferometer22.8 m baselinef/15 phase-combined beamLaser guide-star AO on individual telescopesPhase tracking on natural guide star40 arcsec FOV5 mas resolution in optical80-96% Strehl ratio in interferometric image
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LAMA
Liquid-Mirror Telescopes
Three 3m telescopes in operationA 6m nearing completionA 4m project in Chile
Photo Credit: Chip Simons Photography
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LAMA
Liquid-Mirror Technology
Strehl RatioS = central intensity/ideal central intensity
S = 0.81 measured in lab tests of 2.5m LM
S ~ 0.5-0.7 estimated for NODO 3m telescope
S ~ exp(-k2σ2)k = 2π/λσ = RMS OPD error
Images courtesy of Dr. E. Borra, Universite Laval
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LAMA
Liquid-Mirror Interferometric Testing
Image courtesy of Dr. E. Borra, UniversiteLaval
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Liquid-Mirror Surface Quality
85 nm RMS error ð S = 0.93 at λ = 2 um
Image courtesy of Dr. E. Borra, Universite Laval
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LAMA
Scattered Light
Credit: Dr. E. Borra, Universite Laval
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LAMA
Mercury Telescopes NODO
Photo credit: Mark K. Mulrooney
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LAMA
LMT Imaging Arp 270
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LMT Imaging Field Galaxies
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LMT Imaging Distant Cluster
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LMT Imaging Cluster Core
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LAMA
Large Zenith Telescope
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6m Primary Mirror Truss
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LZT Mirror Truss
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Making the mirror-segment mold
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LZT Air Bearing
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LMT Tracking Optics
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LAMA
Preliminary Design (Single element)
M1: 10 m f/1.5 parabolicM2: 0.75 m hyperbolicM3: 0.2 m flat2 compensation lenses5 min trackingRMS spot dia < 150 masStrehl ratio > 0.1 @ 2 um
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LAMA
Background Light
Credit: Space Telescope Science Institute
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LAMA
OH Absorption Cell
NIR sensitivity is directly proportional to backgroundGain of ~ 100 is possibleOH Production: Radiative excitation by Meinel photonsCollisional dexcitation in ~100 usColumn density > 1018 cm-2
Path length ~ 10 mPressure ~ 0.1 TorrLifetime ~ 10 msGas consumption ~ 2 kg/hr O3, 40 g/hr H
23 OOHHO +→+
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LAMA
OH Absorption vs Column Density
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LAMA
Sample Model Calculation (N = 1018 cm-3)
Before
After
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LAMA
Cerro Chanjnantor
5000 m high desert in Northern ChileSite of ALMA millimeter arrayProposed site of Cornell IR telescope and several others
Photo credit: S. Radford
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LAMA
Chajnantor Seeing vs Paranal (ESO VLT)
Credit: Cornell University
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LAMA
LAMA Concept
Optical-NIR interferometerNear-zenith pointing and trackingSurvey fields around natural guide starsWavefront control on each element (AO)Phase tracking on all beamsDiffraction limit of 60m telescopeEquivalent area of 42m telescopeFully sample isoplanatic areaBackground reduction by gas-phase OH absorption cells0.1 nJ point source sensitivity (AB = 33.9)Mercury primary mirrorsHigh dry site (eg. Alto-Plano)Low project cost (~ $50M)
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LAMA
Array Geometry
|___
____
____
____
____
____
____
____
____
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60m
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Array Transfer Function
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Single-Element PSF
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LAMA
LAMA PSF
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PSF Profile
0
0.2
0.4
0.6
0.8
1
0 10 20 30 40 50
radius (mas)
Intensity
Encircled Energy
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LAMA
Conceptual Design
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10m Array Element
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LAMA
Survey Mode
~ 360 survey fields, each 30 x 30 arcsec~ 150 observations per year for each field
ò100 pJy detection limit for galaxies (0.1”)
10 pJy detection limit for point sources
ò90 square arcmin in one year~ 40,000 sec integration time
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LAMA
Summary
A Very-Large Optical Telescope is feasible nowA 60 m optical interferometer would provide unprecedented sensitivity and resolutionGains of an order of magnitude or more over NGST are possiblefor survey-type observationsLiquid-Mirrors provide a way to beat the cost curve by a factor of 10-50Such a telescope could be built on a relatively short timescale (~ 6 yrs)