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Paranal Observatory
VLT(I) Instrumentation
An extensive  - Coverage
1
10
 (µm)
VLT Instrumentation
An extensive  -  / Coverage
FORS-1 & FORS-2
FORS Image Quality & Stability
 Image Quality Telescope driven
Best image obtained (HR mode)
• 0.18” (integration time: a few seconds)
• 0.25” (integration time: several minutes)
young brown dwarf
I band - TW5 system
Ellipticity distribution
Red: uncorrected
Blue: corrected
 Image Stability exceptional
Keck + LRIS
Seeing ~ 0.55”
VLT + FORS-1
Seeing ~ 0.6”
ISAAC
ISAAC Spectroscopic Sensitivity

z =3.2 galaxy “rotation” (V ~ 700 km/s)
OIII lines; 6 hr exposure; 0”.4 seeing
UVES @ UT2 Nasmyth
UVES: highly sensitive R~105 Spectrometer
Be (0.313 µm) abundance in stars of a Globular Cluster (V=16(!))
NAOS-CONICA Nov. ‘01
NAOS-CONICA Galactic Center
Visible Imaging Multi-Object Spectrograph (VIMOS)
Built by LAM, OHP & OMP (F), IRA,, IFCTR & OAC (I) and ESO
First VIMOS Light
Antennae Nebula
VRI - 0.6 arcsec. fwhm
VIMOS IFU mode: first galaxy spectra, 3 March 2002
1st light on 26 February ‘02
(2 over 4 channels only due to overweight)
3120 spectra ; 2 x 27” x 27” field (zoomed); Antennae Nebula
FLAMES Facility
FLAMES ARGUS
VISIR
Built by CEA-Saclay (F) and Astron (NL)
VLT UT4 (YEPUN)
First Light Jan ‘04
SINFONI
AO Module
60 elements curvature
Natural & Laser Guide Star
ESO internal development
SPIFFI
3D spectrometer (0.95-2.5µm)
FOV = 0”.8 to 8”, / ~ 4000
(32 x 32) pixels, 1024 channels
MPE
AO-corrected 3D IR spectro-imager  any small structured target
• 1-5 m range
• ~ 105
• single order
(echelle + pre-disperser)
1st Generation Lesson Learned
Management and Contracts
-Upfront R&D, Phase A added.
- Agreement on use of Management Tools
- More ESO-Consortium Partnership
-Global approach (including operations), close involvement prior to PAE
-Commissioning painful. Early science added. Early involvement Paranal
Technical Aspects
- Instruments have too many modes.
- Positive overall evaluation of VLT (HW and SW) standards
-Move towards pipelines which produce science products.
INSTRUMENTATION DIVISION
Operation
Development
Decision
Study
VLT INSTRUMENTS DEVELOPMENT TRACK
IDEA
ES O
or
ES O C om m u n i ty
or
C on sortiu m
ANALYSIS
EVALUATION
Statement of Interest
DESIGN / PLA N
INS
and
Consortium
ESO
Executive
STC
INS
and
Consortium
FINAL APPROVAL
Contract
RECOMMENDATION
INTERNAL APPROVAL
Budget
FC /
Council
STC
DETAILED STUDY
FABRICATION / AIT
Consortium P.I.
INS Project Responsible
INS Scientist
PDR / FDR
Paranal Astronomer Responsible
INS Scientist
Plan
INSTALLATION /COMMISSIONING
Consortium P.I.
INS Project Responsible
INS Scientist
FULL OPERATION
C.D.R.
ESO D.G.
PAE
Consortium P.I.
INS Project Responsible
INS Scientist
START of OPERATIONS
FAC
INS Scientist
Paranal Astronomer Responsible
PAC
2nd Generation Instruments
Detecting First Fireworks: Gamma-ray bursts and SNae
High Z evolution of galaxies and ISM
First galaxy building blocks and galaxy mass assembly
Star formation environments and detection of exo-planets
Peering deeper into nearby galactic nuclei
Huge stellar spectroscopic surveys of Local Group
A Closer view to stars (Doppler imaging, oscillations)
2ND Generation VLT Instruments
KMOS: Multi-IFU J-H-K spectrograph
- Competition, Selection Fall ‘03.
- Prototype of multi-IFU concept
X-Shooter
- 300-1800nm fast response spectrograph, R=10000
HAWK-1: IR large field imager
MUSE: Wide Field Surveyor
-Image slicers & 24 low-cost spectrometers, AO assisted
choice in Spring ‘04
Planet Finder
- Two concepts: reflected light versus intrinsic emission
 choice in Spring ‘04
2nd Generation Instruments: I- KMOS
MPE/USM (R. Bender, PI)
Durham, ATC, Oxford, Bristol
Fully Cryogenic multi-IFUs
7’.2 dia. Field; 24 IFUs
3 (2k x 2k) Detectors
~ 3500
Wavelength Coverage: 1-2.45 micron
Sampling: 0.2 arcseconds
2nd Generation Instruments: I- KMOS
•Investigate the physical processes which drive galaxy
formation and evolution over red shift range 1<z<10.
•Map the variations in star formation histories, spatially
resolved star-formation properties, and merger rates
•Dynamical masses of galaxies across a wide range of
environments at a series of progressively earlier epochs
•Extremely High-Redshift Galaxies and Re-ionisation
•The Connection Between Galaxy Formation and
Active Galactic Nuclei
•Age-Dating of Ellipticals at z = 2 to 3
2nd Generation Instruments: I- KMOS
High-Z Galaxies and Ionization
Lyman-a spectra at 8200 A (R=3200) FORS2
Lyman-a Galaxies at Z>5
(Lehnert and Bremer 2003, ApJ 593,L630)
Challenge: IFU High Sensitivity
2nd Generation Instruments: X-SHOOTER
Amsterdam, Njimegen, ASTRON(Co-Pi l. Kaper)/ Copenhagen(Co-PI
P.Kjaergaard Rasmussen)/ ESO(Co-PI S. D’Odorico)/ INAF
Merate, Palermo, Trieste,Catania(Co-PI, R. Pallavicini)
 High throughput, matching or surpassing existing spectrographs
 Intermediate Resolution ( ~5000-10000)
 Simultaneous wavelength coverage from the UV to the H band
 Possibly including spectro-polarimetry
 Possibly including a mini-IFU (small area spectroscopy and image slicer)
 Fast centering and setting-up
2nd Generation Instruments: X-SHOOTER
More than burst: Star Formation at high Z (Fosbury et al.)
Emission line galaxies magnified by
an intervening cluster provide unique
information on star formation history
at early epochs. The Lynx galaxy was
studied at Keck with ESI and
NIRSPEC. Intermediate resolution
spectroscopy has provided line
intensities and kinematics. Used to
infer the properties of the ionizing
sources and abundances.Low spatial
density. Intermediate resolution,
spectral coverage from UV to IR required
2nd Generation Instruments: X-SHOOTER
[O III]
Ly 
[O II]
B. Fosbury et al. 2003
Abundnces in ionized gas
In the Lynx galaxy at
z=3.4
ESI
NIRSPEC
2nd Generation Instruments: X-SHOOTER
FAST, EFFICIENT, FAINT, LARGE COVERAGE
2nd Generation Instruments: X-SHOOTER
RESOLUTION: An intermediate Resolution spectrograph reaches
sky limits in the OH-free regions (80% of spectrum) in 35-40 min
2nd Generation Instruments: MUSE
MUSE
CRAL-Lyon (R. Bacon, PI)
Durham, ESO, OP, Leiden,
Cambridge, IAP, LAM, ETH, AIPPostdam
MCAO
focal plane
Enlarger/
Anamorphoser
Field-splitter
1’ x 1’ field IFU; 0.48-0.95 µm
CCD
plane
Dispersing element
Camera
Collimator
Spectrometer
Split focal
plane
Spectrometer
pseudoentrance slit
Sub-FoV
Image slicer
24 Spectrometers (4k x 4k)
No moving part, Nasmyth (fixed)
~ 3,000
MCAO
MUSE
3D Ultra Deep Field: 10-19 erg s-1 cm-2
Faint Ly a emitters; Progenitors of Milky Way ?
Star Formation History at Z>4
Development of dark matter halos
Link between Lya emitters and High Res. QSO absorption
Physiscs of high Z galaxies from resolved spectroscopy
Kinematics, population, cluster, outflows, merger...
In (nearby) galaxies
Stars: massive spectroscopy of crowded regions,
Origin of bipolar stellar outflows and shock waves
SERENDIPITY
Deep Field
 MUSE deep field
 80x1 hours integration
 Galics simulation

Escape fraction of Ly 15%
 Convolved with MUSE PSF


AO or non AO
MUSE Image Quality
Deep field
 Continuum detection



IAB < 26.7
Reduced R (300)
154 gal. arcmin-2
95% at z<3
1 arcmin

0.2
3.2
z
1 arcmin
Deep Field - Ly
 Ly detection




Flux Ly > 2.5.10-19
erg.s-1.cm-2
245 gal. arcmin-2
113 gal. in z [2.8-4]
132 gal. in z [4-6.7]
2.8
4.7
6.7
z
Deep Field
 399 gal. arcmin-2
0.2
z
z
2.8
4.7
3.2
Continuum
6.7
Ly
1 arcmin
Deep Field
Gal.arcmin-2
IAB<26.5
F(Ly)> 3.10-19 erg.s-1.cm-2
redshift
Deep Field - Lya
 Continuum of high z Ly galaxies (z=5-6.7)






00% with IAB<26.5
03% with IAB<28 (HDF)
14% with IAB<29 (UDF)
37% with IAB<30
64% with IAB<31
83% with IAB<32
ground based limit
HST limit
JWST ?
Spatial resolution
0.2
z
z
2.8
4.7
Intensity in log scale
3.2
Continuum
Seeing limited observations in poor seeing conditions
260 gal.arcmin-2 in total, 75 gal.arcmin-2 in z=[4-6.7] Ly
6.7
Source confusion
0.2
z
z
2.8
4.7
Intensity in log scale
3.2
Continuum
AO observations in poor seeing conditions
317 gal.arcmin-2 in total, 101 gal.arcmin-2 in z=[4-6.7] Ly
6.7
Source confusion
0.2
z
z
2.8
4.7
Intensity in log scale
3.2
Continuum
6.7
Seeing limited observations in good seeing conditions
346 gal.arcmin-2 in total, 112 gal.arcmin-2 in z=[4-6.7] Ly
Source confusion
0.2
z
z
2.8
4.7
Intensity in log scale
3.2
Continuum
AO observations in good seeing conditions
399 gal.arcmin-2 in total, 132 gal.arcmin-2 in z=[4-6.7]Ly
6.7
Field to Field variation
0.2
z
z
2.8
4.7
3.2
Continuum
Field Variations
6.7
Ly
2nd Generation Instruments: IV- Planet Imager
MPIA-Heidelberg (M. Feldt, PI)
Padova, Lisboa, Amsterdam, MPE,
Tautenburg, ETH, Postdam, OAC,
Leiden, Jena, Arcetri, Brera
Nasmyth (fixed)
H+J integral field; I polarimetric imaging
2 conjugate high-order AO mirrors
2nd Generation Instruments: IV- Planet Imager
LAOG-Grenoble (A.M. Lagrange, PI)
LAM, ONERA, OP, Nice, OCA, Montreal,
Durham, UCL, ATC, Geneve
Advanced coronography
differential multi- & polarimetric imaging
Phase Stop
High-order AO mirror
High-Accuracy Radial velocity Planetary Searcher (HARPS)
• visible range; ~ 105 echelle
• fibre-coupled to Cassegrain Adapter
• 100 n./yr. x 5 yrs @ La Silla 3.6m
• ± 1m/s rms long-term accuracy
• 1st light 2Q ‘03 3.6M telescope
Built by Geneva Observ. & Bern Univ. (CH), OHP & Service d’Aéronomie (F), ESO La Silla & Garching
HARPS @3.6M : Tests on stellar jitter: Black G Subgiant,
Red: G Main Sequence
Built by Geneva Observ. & Bern Univ. (CH), OHP & Service d’Aéronomie (F), ESO La Silla & Garching
[email protected]: ACen B Oscillations (400 exposures, 6.5
hours)
Built by Geneva Observ. & Bern Univ. (CH), OHP & Service d’Aéronomie (F), ESO La Silla & Garching