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Observing Possibilities in Europe
 Medium-sized telescopes (2 - 4m class)
• optical & NIR instrumentation
• observing techniques
VLT, GTC, LBT
radio & mm (IRAM, APEX, ALMA)
solar telescopes
• why still needed
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OPTICON
– COMET transnational access programme
– Pays your travel costs
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OPTICON
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OPTICON
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OPTICON
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OPTICON
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Co-ordination network of European optical and infrared
astronomy
Astronomy institutes and infrastructure operators
Access, Networks, JRAs, 19.2 M€
COMET transnational access programme
International access to national observatories
EC Framework Programmes (FP6)
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Support international collaborations
Lissabon Strategy: build the
European Research Area (ERA)
Integrated Infrastructure Initiatives (I3)
European Research Council in FP7
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COMET
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COMET
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Transnational access programme
European medium-sized (2-4m class) telescopes
La Silla, Hawaii, AAT, WHT, TNG, CAHA
5 – 10% pool of observing time
Short term benefits
• International users:
– telescope access
– travel & subsistence
• Training (NEON summer schools)
• Telescope directors forum
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Medium term
• Full co-operation, complementary instrumentation
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INSTRUMENTS
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Instruments & observing techniques
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General instrumentation (brief)
• NIR and TIR instruments
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MOS and IFUs
• integral field spectroscopy
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Survey Instruments
• optical & NIR wide-field imagers, surveys, s Ori
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High-resolution spectrographs
• high precision radial velocity determination
– extrasolar planets, ways of detection
 Adaptive
Optics
• wavefront sensing
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Work horse instrumentation, optical
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imaging/low resolution spectroscopy
• TNG/DOLORES
• NTT/EMMI
• 3.6m/EFOSC2
• CAHA/MOSCA
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long slit, medium resolution spectroscopy, blue/red arm
• WHT/ISIS
• NTT/EMMI
• CAHA/TWIN
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check OPTICON web pages
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NIR and TIR
Spectrographs
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NIR spectrographs
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UKIRT
• CGS4, UIST
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NTT
• SOFI
 WHT
• LIRIS
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CAHA
• OmegaCass
– imaging
– low/medium resolution spectroscopy, R = 100 – 3000
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– polarimetry
UKIRT
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CGS4
• 1 – 5 mu, R= 400 – 40.000
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UIST
• 1 – 5 mu, 1k InSb array, 0.06‘‘ and 0.12‘‘/px
• Imaging, long-slit, IFU
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Michelle (now Gemini)
• SBRC 320 x 240 Si:As
• 10 – 20 mu imaging, 90‘‘ long-slit
• R up to 30.000
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Thermal infrared
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La Silla 3.6m
• TIMMI2
– 3.5 – 28 mm, 320 x 240 Si:As, R=160
– imaging, spectroscopy, polarimetry
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La Silla
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MOS & IFUs
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MOS and IFUs
 AAT Two
Degree Field: 2dF
• wide field multi-object spectroscopy
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Integral/WYFFOS
• MOS in WHT prime focus with robotic fibre positioner
• 150 fibres, 2 CCD mosaic
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PMAS
• optical IFU, wide field
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SAURON (private)
• IFU with lenslet array
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OASIS/NAOMI
• 0.6 – 1 mm
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AAT
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3.9m AAO
• 2dF 2 degree field
• 2 spectrographs with 200 fibres each
• automatic fibre positioner
• 5/03 relaease of 2dF Galaxy & Quasar Survey
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Calar Alto/PMAS
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PMAS
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IFU with nod & shuffle
16x16 pixel lenslet array with 8´´x8´´ or 16‘‘ x 16‘‘
PPAK hexagonal fibre bundle 75‘‘ plus sky
0.35, 0.8, 1.7 A/px gratings
PYTHEAS, scanning FP with R = 100.000
Euro3D
MUSE (VLT 2012)
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SURVEY
INSTRUMENTS
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Survey Instruments
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UKIRT
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CFHT
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MEGACAM, CFHTLS
CAHA
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WFCAM, UKIDSS
Omega2000
LAICA
Paranal
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4m VISTA, 1 square degree
2.5m VST, 16k x 16k OmegaCam, 1 sqd.
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UKIRT
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WFCAM
• four 2k x 2k Hawaii II
• 0.8 - 2.5 mm 0.‘‘4 pixel scale
– UKIRT Deep Sky Survey (UKIDSS)
– Sep 2004, 7500 sqd to K=18.5 mag
– 3 mag deeper than 2MASS
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NIR counterpart of SLOAN
Coolest and nearest BDs
High redshift starburst galaxies
Galaxy clusters at 1 < z < 2
High redshift quasars at z > 7
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CFHT
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MegaPrime/MegaCam
• 40 2k x 4k CCDs, 0.‘‘187 pixel
– Legacy Survey
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CFHTLS
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CFHT Legacy Survey
• 50% of dark/grey time
• 450 nights over 5 years
– Very wide, shallow
• 1300 square degrees
• TNOs, stellar populations, Galactic structure
– Wide
• i‘ = 24.5 mag, 50-70 sqd, cosmology, large scale distribution
– Deep
• 4 sqd, r‘ = 28 mag, 2000 type Ia SN monitoring
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CAHA
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OMEGA2000
• Prime focus, 2k x 2k Hawaii II, 16´ x 16´ FOV
LAICA
• 4 4k x 4k CCDs, 1 sqare degree FOV
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30% of time used for LBT and GTC preps
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ALHAMBRA, HIROCS, MANOS
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Scientific results: s Ori
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Brown Dwarfs and Free Floating Planets in Orion
 Rebolo: s Ori
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Extrasolar Planets
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Free Floating Planets??
 What about real planets?
 1995: 51 Peg
 May 04: 122 planets around solar type stars
• 107 planet systems
• 13 systems with > 1 planets
• Jovian planets, 0.1 – 5 MJupiter
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How detected?
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ESP Detection: radial velocities
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OHP/ELODIE
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51 Peg B: first extrasolar planet
• ELODIE: spectral resolution about 6 km s-1
• RV modulation: amplitude 50 m s-1
• How possible?
• Iodine Cell or ThAr superposition
• MM & DQ
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HIGH – R
SPECTROGRAPHS
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High resolution spectrographs
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UHRF
• 1 Million
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HARPS
• cross dispersed
• 3.6m, fibre fed, ThAr Superposition
• ELODIE
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SARG
• TNG, up to R = 164.000, Iodine Cell
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CES/VLC
• long slit
• 3.6m, fibre fed, R = 235.000, Iodine Cell
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OHP/ELODIE
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1.93m telescope
– Elodie
• Echelle Spectrograph
• 1k TK detector
• R=45.000
• 2850 - 6800 coverage
• first extrasolar planet discovered
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Iodine Cell
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Iodine: forest of narrow lines
 Place Iodine cell in spectrograph
 Obtain composite Iodine/Stellar spectrum
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Very accurate radial velocities
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Iodine Cell
• full modelling of composite spectrum required
• simultaneous model of instrumental profile
• developed by M. Endl, AUSTRAL sw
• accuracies down to 1 m s-1
 ThAr
superposition
• HARPS
• Correlation technique
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La Silla: HARPS
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HARPS
• high accuracy radial velocity planet finder
• fibre fed, cross dispersed echelle spectrometer
• 0.005o C temperature stabilisation
• R = 120.000 or about 3 km s-1
• ThAr superposition: precision to 1m s-1
• 1/1000 pixel
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TNG
SARG: HD 219542
• Period: 111.8 days
• velocity semi – amplitude: 13 m/s
• Eccentricity: ~ 0.3
• Planet mass: 0.30 Mjupiter (~ 1 Msaturn)
• Orbital semiaxis: 0.46 AU
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AAT UHRF
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UHRF
• 31.6 lines/mm 200 x 400 mm echelle
• R = 300.000 – 1.000.000
• 1 – 0.3 km s-1
• wavelength coverage 4A (300nm) – 13A (1100nm)
• interstellar line studies
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Detection of extrasolar planets
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Radial velocities
 Transits
– June 8th Venus Transit
– HD 209458
– CAHA: 0.5m robotic telescope
– OGLE experiment Las Campanas
– giant planets, Jupiter
– COROT, Kepler
– terrestrial planets
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Direct detection
– adaptive optics
– differential methods, CHEOPS, nulling interferometry
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ESP: Direct Detection
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High angular resolution
• 60 light years, 5AU (Jupiter): 0.“25
• 3.5m, K-band: diffraction limit 0.‘‘13
– Adaptive Optics
– AO principles, wavefront sensing
– LGS
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Problems
– 109 difference in brightness in visual, Zodiacal light
• differential polarimetry: CHEOPS
• Nulling interferometry: LBT, DARWIN
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ACTIVE & ADAPTIVE
OPTICS
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Adaptive Optics
 ADONIS
(decommissioned): first steps
 PUEO: most productive
 ALFA
• LGS development
• PARSEC for VLT
• Pyramid wavefront sensors
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NAOMI
• GLAS Rayleigh laser
• INGRID
• OASIS, from CFHT
• 0.6 – 1mm
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Active optics
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Archimedes destruction of the Roman fleet, Syracruse
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Active optics: control shape of primary mirror
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Second punic war, 219BC – 210 BC
Large, thin mirrors (VLT)
Static aberrations from M1
M2 de-centering coma: correct M2 position
One step further: tip-tilt secondary mirrors: UKIRT
3.5m New Technology Telescope on La Silla
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Active control of shape of M1
75 actuators, 3 fixed points, 24 lateral actuators
0.05 Hz correction frequency: slow
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Adaptive Optics
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Correct wavefront
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Deformable mirror, fast
Small mirrors, after telescope optics
Phase conjugation
AO secondaries (MMT, LBT)
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Requirements: 1/50 mm, 103 Hz
Determine shape of wavefront
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Use science object, NGS, LGS
Wavefront sensor: Shack-Hartmann, curvature,
pyramids
Analytic representation of WF: Zernike polynomials
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AO, routine performance
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K-band seeing of 0.´´8
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Seeing disk, no tip-tilt, no AO
Tip-tilt corrections: resolution 0.´´4
Tip-tilt and AO: resolution 0.´´13
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AO: possibilities from the ground
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Wavefront sensing
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Shack-Hartmann sensor
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Lenslet array, sub-pupils
Measure slope of wavefront at different positions
Reconstruction of wavefront from array of slopes
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Wavefront sensing
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Wavefront sensing
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Curvature sensing
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Intra- and extrafocal images
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I1 (r ) - I 2 (r ) lF ( F - l )    Fr 
F
r
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c -  
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I1 ( r )  I 2 ( r )
2l  n  l 
x y
 l 
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Wavefront sensing
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Pyramid wavefront sensor
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4 sub-pupils
Sub-apertures defined by detector pixels
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Wavefront sensing
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Shearing interferometer
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Neural networks
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Interfering beams represent wave-fronts
with small lateral shift r
Obtain wavefront tilt in shear direction
Experienced opticians can recognise dominant types of aberrations
from pupil images
Phase diversity
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Retrieval of phase error from focused and
de-focused image of a star
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ALFA
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Laser guide stars
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WHT/GLAS
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ESP future projects
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VLT
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Kepler
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CHEOPS
1m Telescope
42 2x1k Detectors
about 900 planets with 1 – 2 REarth
> 10% of planetary systems with > 1 planets
LBT and DARWIN/TPF
• direct detection: nulling interferometry
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Terra Nova: Space
 55 Cancri
 G8V
 M55 Cancri = 0.85 MSonne
 T = 5250 K
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Summary
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European 2 – 4m class opt/NIR telescopes
• wide range of competitive instrumentation
• transnational access programme
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Science
• very interesting science per se
– extrasolar planets
• support/preparation of 10m class
– surveys, PMAS  MUSE
• development of new instrumentation
– ALFA/LGS  PARSEC
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medium sized telescopes are still needed
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