paranal observatory. vlt(i) instrumentation an extensive - coverage 110 (µm) vlti

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

HARPS@3.6M: Cen B Oscillations (400 exposures, 6.5 hours)

Built by Geneva Observ. & Bern Univ. (CH), OHP & Service d’Aéronomie (F), ESO La Silla & Garching