paranal observatory. vlt(i) instrumentation an extensive - coverage 110 (µm) vlti
TRANSCRIPT
Paranal Observatory
VLT(I) Instrumentation
An extensive An extensive - - Coverage Coverage
1 10 (µm)
VLTI
VLT Instrumentation
An extensive An extensive - - / / Coverage Coverage
FORS-1 & FORS-2FORS-1 & FORS-2
FORS Image Quality & Stability
Image Quality Telescope drivenBest image obtained (HR mode)
• 0.18” (integration time: a few seconds)
• 0.25” (integration time: several minutes)
VLT + FORS-1VLT + FORS-1Seeing ~ 0.6”
Keck + LRISKeck + LRISSeeing ~ 0.55”
Image Stability exceptional
Ellipticity distributionEllipticity distribution
Red: uncorrectedBlue: corrected
young brown dwarfI band - TW5 system
ISAACISAAC
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
Built by LAM, OHP & OMP (F), IRA,, IFCTR & OAC (I) and ESO
Visible Imaging Multi-Object Spectrograph (VIMOS)
1st light on 26 February ‘02(2 over 4 channels only due to overweight)
Antennae NebulaVRI - 0.6 arcsec. fwhm
VIMOS IFU mode: first galaxy spectra, 3 March 2002
3120 spectra ; 2 x 27” x 27” field (zoomed); Antennae Nebula
First VIMOS Light
FLAMES Facility
FLAMES ARGUS
VISIR
Built by CEA-Saclay (F) and Astron (NL)
SINFONI
VLT UT4 (YEPUN)First Light Jan ‘04
SPIFFI3D spectrometer (0.95-2.5µm) FOV = 0”.8 to 8”, ~ 4000(32 x 32) pixels, 1024 channels
MPE
AO Module
60 elements curvatureNatural & Laser Guide Star
ESO internal development
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.
ESO or ESO Community or Consortium
IDEAINSand Consortium
ANALYSISESOExecutive
EVALUATIONSTC
Statement of InterestINS andConsortium
DESIGN / PLAN
ESO D.G.INTERNAL APPROVAL
STCRECOMMENDATION
FC /CouncilFINAL APPROVAL
FABRICATION / AITConsortium P.I.INS Project ResponsibleINS Scientist
Consortium P.I.INS Project ResponsibleINS ScientistDETAILED STUDY INSTALLATION /COMMISSIONING
Consortium P.I.INS Project ResponsibleINS ScientistFULL OPERATION
Paranal Astronomer ResponsibleINS ScientistSTART of OPERATIONSINS ScientistParanal Astronomer Responsible
C.D.R.Plan
BudgetContract
PDR / FDR PAE
Study
Decision
Development
Operation
VLT INSTRUMENTS DEVELOPMENT TRACKINSTRUMENTATION DIVISION
FAC 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
Huge stellar spectroscopic surveys of Local Group
Peering deeper into nearby galactic nuclei
A Closer view to stars (Doppler imaging, oscillations)
KMOS: Multi-IFU J-H-K spectrograph- Competition, Selection Fall ‘03.
- Prototype of multi-IFU concept
MUSE: Wide Field Surveyor -Image slicers & 24 low-cost spectrometers, AO assisted
choice in Spring ‘04
X-Shooter- 300-1800nm fast response spectrograph, R=10000
Planet Finder- Two concepts: reflected light versus intrinsic emission
choice in Spring ‘04
2ND Generation VLT Instruments
HAWK-1: IR large field imager
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
MPE/USM (R. Bender, PI)
Durham, ATC, Oxford, Bristol
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
Lyman-a spectra at 8200 A (R=3200) FORS2
Lyman-a Galaxies at Z>5 (Lehnert and Bremer 2003, ApJ 593,L630)
High-Z Galaxies and Ionization
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
B. Fosbury et al. 2003
Abundnces in ionized gas
In the Lynx galaxy at
z=3.4
[O II]
[O III]
ESI NIRSPEC
Ly
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
MUSEMUSE
1’ x 1’ field IFU; 0.48-0.95 µm
24 Spectrometers (4k x 4k)
No moving part, Nasmyth (fixed)~ 3,000
MCAO
CRAL-Lyon (R. Bacon, PI)
Durham, ESO, OP, Leiden, Cambridge, IAP, LAM, ETH, AIP-Postdam
MCAOfocal plane
Enlarger/Anamorphoser Field-splitter
Split focal plane
Image slicer
Spectrometerpseudo-
entrance slit
CollimatorCamera
CCDplane
Dispersing element
Spectrometer
Sub-FoV
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>4Development 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
0.2
3.2
z
1 arcmin
1 a
rcm
in
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
6.7
z
4.7
Deep Field 399 gal. arcmin-2
1 arcmin
0.2
3.2
Continuum
z
2.8
6.7
z
4.7
Ly
Deep Field
F(Ly> 3.10-19 erg.s-1.cm-2IAB<26.5
redshift
Gal.arcmin-2
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
Seeing limited observations in poor seeing conditions
0.2
3.2
Continuum
z
Intensity in log scale
260 gal.arcmin-2 in total, 75 gal.arcmin-2 in z=[4-6.7]
z
Ly
2.8
6.7
4.7
Source confusion
0.2
3.2
Continuum
z
Intensity in log scale
AO observations in poor seeing conditions
317 gal.arcmin-2 in total, 101 gal.arcmin-2 in z=[4-6.7]
z
Ly
2.8
6.7
4.7
Source confusion
0.2
3.2
Continuum
z
Intensity in log scale
Seeing limited observations in good seeing conditions
346 gal.arcmin-2 in total, 112 gal.arcmin-2 in z=[4-6.7]
z
Ly
2.8
6.7
4.7
Source confusion
0.2
3.2
Continuum
z
Intensity in log scale
AO observations in good seeing conditions
399 gal.arcmin-2 in total, 132 gal.arcmin-2 in z=[4-6.7]
z
Ly
2.8
6.7
4.7
Field to Field variation
Field Variations
2.8
6.7
4.7
z
Ly
0.2
3.2
Continuum
z
2nd Generation Instruments: IV- Planet Imager
Nasmyth (fixed)
H+J integral field; I polarimetric imaging
2 conjugate high-order AO mirrors
MPIA-Heidelberg (M. Feldt, PI)
Padova, Lisboa, Amsterdam, MPE, Tautenburg, ETH, Postdam, OAC, Leiden, Jena, Arcetri, Brera
2nd Generation Instruments: IV- Planet Imager
Advanced coronography
differential multi- & polarimetric imaging
High-order AO mirror
LAOG-Grenoble (A.M. Lagrange, PI)
LAM, ONERA, OP, Nice, OCA, Montreal, Durham, UCL, ATC, Geneve
Phase Stop
• 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
High-Accuracy Radial velocity Planetary Searcher (HARPS)
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]: Cen B Oscillations (400 exposures, 6.5 hours)
Built by Geneva Observ. & Bern Univ. (CH), OHP & Service d’Aéronomie (F), ESO La Silla & Garching