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Transcript of 1 Comparative Performance of a 30m Groundbased GSMT and a 6.5m (and 4m) NGST NAS Committee of...
![Page 1: 1 Comparative Performance of a 30m Groundbased GSMT and a 6.5m (and 4m) NGST NAS Committee of Astronomy & Astrophysics 9 th April 2001 Matt Mountain Gemini.](https://reader034.fdocuments.net/reader034/viewer/2022052418/5a4d1aca7f8b9ab05996f42c/html5/thumbnails/1.jpg)
1
Comparative Performance of a 30m Groundbased GSMT and a 6.5m
(and 4m) NGST
NAS Committee of Astronomy & Astrophysics9th April 2001
Matt MountainGemini Observatory/AURA NIO
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Overview• Science Drivers for a GSMT• Performance Assumptions
– Backgrounds, Adaptive Optics and Detectors• Results
– Imaging and Spectroscopy• compared to a 6.5m & 4m NGST
– A special case, • high S/N, R=100,000 spectroscopy
• Conclusions
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GSMT Science Case“The Origin of Structure in the Universe”
From the Big Bang… to clusters, galaxies, stars and planets
Najita et al (2000,2001)
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Mass Tomography of the Universe
z~0.5
Existing Surveys + Sloan
z~3
Hints of Structure at z=3(small area)
100Mpc (5Ox5O), 27AB mag (L* z=9), dense samplingGSMT 1.5 yrGemini 50 yrNGST 140 yr
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Tomography of Individual Galaxies out to z ~3
• Determine the gas and mass dynamics within individual Galaxies• Local variations in starformation rate Multiple IFU spectroscopy R ~ 5,000 – 10,000
GSMT 3 hour, 3 limit at R=5,000
0.1”x0.1” IFU pixel(sub-kpc scale structures)
J H K 26.5 25.5 24.0
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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
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).
S/N=100, R=100,000, >4m
Gemini out to 0.2pc sample ~ 10sGSMT 1.5kpc ~100sNGST X
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30m Giant Segmented Mirror Telescope concept
Typical 'raft', 7 mirrors per raft
Special raft - 6 places, 4 mirrors per raft
1.152 m mirror across flats
Circle, 30m dia.30m F/1 primary, 2m adaptive secondary
GEMINI
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GSMT Control ConceptLGSs provide full sky coverage
Deformable M2 : First stage MCAO, wide field seeing improvement and M1 shape control
10-20’ field at 0.2-0.3” seeing
1-2’ field fed to the MCAO module
M2: rather slow, large stroke DM to compensate ground layer and telescope figure, or to use as single DM at >3 m. (~8000 actuators) Dedicated, small field (1-2’) MCAO system (~4-6DMs).
Focal plane
Active M1 (0.1 ~ 1Hz)619 segments on 91 rafts
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GSMT Implementation concept- wide field (1 of 2)
Barden et al (2001)
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GSMT Implementation concept- wide field (2 of 2)
20 arc minute MOSon a 30m GSMT
• 800 0.75” fibers• R=1,000 350nm – 650nm• R=5,000 470nm – 530nm• Detects 13% - 23% photons hitting 30m primary
1m
Barden et al (2001)
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Spot Diagrams for Spectrograph
R=1000 case with 540 l/mm grating.
R=5000 case with 2250 l/mm grating.
350 nm 440 nm 500 nm 560 nm 650 nm
470 nm 485 nm 500 nm 515 nm 530 nm
On-axis
On-axis
Circle is 85 microns equal tosize of imaged fiber.
Barden et al (2001)
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GSMT Implementation concept- MCAO/AO foci and instruments
MCAO opticsmoves with telescope
Narrow field AO ornarrow field seeing limited port
MCAO Imagerat vertical Nasmyth
elevation axis
4m
Oschmann et al (2001)
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Spot diagrams for MCAO + Imager
Diffraction limited performance for 1.2m – 2.2 m can be achieved
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MCAO Optimized Spectrometer
• Baseline design stems from current GIRMOS d-IFU tech study occurring at ATC and AAO– ~2 arcmin deployment field– 1 - 2.5 µm coverage using 6 detectors
• IFUs– 12 IFUs total ~0.3”x0.3” field– ~0.01” spatial sampling R ~ 6000 (spectroscopic OH suppression)
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Quantifying the gains of NGST compared to a groundbased telescope
• Assumptions (Gillett & Mountain 1998)• SNR = Is . t /N(t): t is restricted to 1,000s for NGST
• Assume moderate AO to calculate Is , Ibg
• N(t) = (Is . t + Ibg. t + n . Idc .t + n . Nr2)1/2
• For spectroscopy in J, H & K assume “spectroscopic OH suppression”
• When R < 5,000 SNR(R) = SNR(5000).(5000/R)1/2
and 10% of the pixels are lost
Source noise background dark-current read-noise
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Space verses the Ground
Takamiya (2001)
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Adaptive Optics enables groundbased telescopes to be competitive
For background or sky noise limited observations:
S Telescope Diameter .
N Delivered Image Diameter
Where: is the product of the system throughput and detector QE is the instantaneous background flux
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Adaptive Opticsworks well
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Modeling verses Data
20 arcsec
M15: PSF variations and stability measured as predicted
GEMINI AO Data
Mod
el R
esu l
ts
2.5 arc min.
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Quantitative AO Corrected Data
• AO performance can be well modeled• Quantitative predictions confirmed by observations
• AO is now a valuable scientific tool:
• predicted S/N gains now being realized
• measured photometric errors in crowded fields ~ 2%
Rigaut et al 2001
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•Tomographic calculations correctly estimated the measured atmospheric phase errors to an accuracy of 92%
–better than classical AO–MCAO can be made to work
Multi-Conjugate Adaptive Optics
MCAO
2.5 arc min.
Mod
el r
esul
ts
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AO Technology constraints (50m telescope)
r0(550 nm) = 10cm No. of Computer CCD pixel Actuator pitch S(550nm) S(1.65m) actuators power rate/sensor
(Gflops) (M pixel/s) 10cm 74% 97% 200,000 9 x 105 800
25cm 25% 86% 30,000 2 x 104 125 50cm 2% 61% 8,000 1,500 31 SOR (achieved) 789 ~ 2 4 x 4.5
Early 21st Century technology will keep AO confined to > 1.0mfor telescopes with D ~ 30m – 50m
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MCAO on a 30m: summary• MCAO on 30m telescopes should be used m• Field of View should be < 3.0 arcminutes,
• Assumes the telescope residual errors ~ 100 nm rms• Assumes instrument residual errors ~ 70 nm rms
– Equivalent Strehl from focal plane to detector/slit/IFU > 0.8 @ 1 micron– Instruments must have:
• very high optical quality• very low internal flexure
(m) Delivered Strehl
1.25 0.2 ~ 0.4 1.65 0.4 ~ 0.6 2.20 0.6 ~ 0.8
9 Sodium laser constellation4 tip/tilt stars (1 x 17, 3 x 20 Rmag)
PSF variations < 1% across FOV
Rigaut & Ellerbroek (2000)
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Modeled characteristics of a 30m GSMT with MCAO (AO only, m) and a 6.5m NGST
Assumed detector characteristics
m <m 5.5m <m
Id Nr qe Id Nr qe
0.01 e/s 4e 80% 10 e/s 30e 40%
Assumed encircled-energy diameter (mas) containing energy fraction
30M 1.2m 1.6m 2.2m 3.8m 5.0m 10m 17m 20m(mas) 23 29 41 34 45 90 154 181Strehl 0.40 0.56 0.73 0.85 0.91]
NGST 1.2m 1.6m 2.2m 3.8m 5.0m 10m 17m 20m (mas) 100 100 82 138 182 363 617 726
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Comparative performance of a 30m GSMT with a 6.5m NGST
1 101E-3
0.01
0.1
1
10
Comparative performance of a 30m GSTM with a 6.5m NGST
S/N
Gai
n (G
SMT
/ NG
ST)
Wavelength (microns)
R=5 R=1,000 R=10,000
Assuming a detected S/N of 10 for NGST on a point source, with 4x1000s integration
GSM
T ad
vant
age
NG
ST a
dvan
tage
R = 10,000 R = 1,000 R = 5
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Comparative performance of a 30m GSMT with a 4m NGST
1 10
0.01
0.1
1
10
Comparative performance of a 30m GSTM with a 4.0m NGST
S/N
Gai
n (G
SMT
/ NG
ST)
Wavelength (microns)
R=5 R=1,000 R=10,000 R = 10,000 R = 1,000 R = 5
Assuming a detected S/N of 10 for NGST on a point source, with 4x1000s integration
GSM
T ad
vant
age
NG
ST a
dvan
tage
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Observations with high Signal/Noise, R>30,000 is a new regime
- source flux shot noise becomes significant
10 1000.1
1
10
100
1000
10 1000.1
1
10
100
1000
GSMT 30m
Com
para
tive
nois
e co
ntrib
utio
ns a
fter f
irst 1
,000
s(e
lect
rons
)1/2
Target S/N after 4,000s
Detector Backgr ound Source
4.6m Spectroscopy at R=100,000
NGST 6.5m
Target S/N after 4,000s
Detector Backgr ound Source
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High resolution, high Signal/Noise observations
1 10
0.01
0.1
1
10
17.0
12.3
4.6
Molecular line spectroscopy S/N = 100
S/N
Gai
n (G
SMT
/ NG
ST)
Wavelength (microns)
R=10,000 R=30,000 R=100,000
Detecting the molecular gas from gaps sweptout by a Jupiter mass protoplanet, 1 AU from a 1 MO young star in Orion (500pc) (Carr & Najita 1998)
GSMT observation ~ 40 mins (30 mas beam)
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Conclusions
6.5m 4.0m Comments
1. Camera 0.6 – 5 mDeep imaging from space; consistent image quality, IR background, even for < 2.5m if D>4.0m
2.MOSR=1,000
1.2 – 2.5m2.5 – 5.0 m
NGST MOS still competitive for < 2.5m only if D~6.0m (consistent image quality, coverage)
3.CameraSpec. R=1500
5 – 28 m5 – 28 m
Clear IR background advantage observing from space, even for D~4mand R< 30,000
4. IFU R=5,000
1.2 – 2.5m2.5 – 5.0 m
Detector noise limited for < 2.5m D2 advantage for groundbased GSMTFor >2.5m, NGST wins even D~4m
D2 advantage for groundbased GSMTFor <12m
A advantage of GSMT,technology challenges from space (fibers)
NGST advantage GSMT advantage X
X
X
X
NGST
NG
S T I n
s tru
me n
t
High S/N, R~100,000 spectroscopy
WF MOS Spectroscopy m
XXX X