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Paranal Observatory

Paranal Observatory. VLTI.  ( µm). 1. 10. VLT(I) Instrumentation. An extensive  - Coverage. VLT Instrumentation. An extensive  -  / Coverage. FORS-1 & FORS-2. young brown dwarf I band - TW5 system. Keck + LRIS Seeing ~ 0.55”. VLT + FORS-1 Seeing ~ 0.6”.

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Paranal Observatory

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  1. Paranal Observatory

  2. VLTI  (µm) 1 10 VLT(I) Instrumentation An extensive  - Coverage

  3. VLT Instrumentation An extensive  -  / Coverage

  4. FORS-1 & FORS-2

  5. young brown dwarf I band - TW5 system Keck + LRIS Seeing ~ 0.55” VLT + FORS-1 Seeing ~ 0.6” 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) Ellipticity distribution Red: uncorrected Blue: corrected • Image Stability exceptional

  6. ISAAC

  7. ISAAC Spectroscopic Sensitivity z =3.2 galaxy “rotation” (V ~ 700 km/s) OIII lines; 6 hr exposure; 0”.4 seeing

  8. UVES @ UT2 Nasmyth

  9. UVES: highly sensitive R~105 Spectrometer Be (0.313 µm) abundance in stars of a Globular Cluster (V=16(!))

  10. NAOS-CONICA Nov. ‘01

  11. NAOS-CONICA Galactic Center

  12. Visible Imaging Multi-Object Spectrograph (VIMOS) Built by LAM, OHP & OMP (F), IRA,, IFCTR & OAC (I) and ESO

  13. 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

  14. FLAMES Facility

  15. FLAMES ARGUS

  16. VISIR Built by CEA-Saclay (F) and Astron (NL)

  17. AO Module 60 elements curvature Natural & Laser Guide Star ESO internal development SPIFFI 3D spectrometer (0.95-2.5µm) FOV = 0”.8 to 8”, l/Dl ~ 4000 (32 x 32) pixels, 1024 channels MPE VLT UT4 (YEPUN) First Light Jan ‘04 SINFONI AO-corrected 3D IR spectro-imager  any small structured target

  18. 1-5 m range • ~ 105 • single order(echelle + pre-disperser)

  19. 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.

  20. 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)

  21. 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

  22. 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

  23. 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

  24. 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

  25. 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

  26. 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.

  27. 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

  28. 2nd Generation Instruments: X-SHOOTER FAST, EFFICIENT, FAINT, LARGE COVERAGE

  29. 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

  30. 2nd Generation Instruments: MUSE MUSE CRAL-Lyon (R. Bacon, PI) Durham, ESO, OP, Leiden, Cambridge, IAP, LAM, ETH, AIP-Postdam • 1’ x 1’ field IFU; 0.48-0.95 µm • 24 Spectrometers (4k x 4k) • No moving part, Nasmyth (fixed) • ~ 3,000 MCAO

  31. 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

  32. Deep Field • MUSE deep field • 80x1 hours integration • Galics simulation • Escape fraction of Lya 15% • Convolved with MUSE PSF • AO or non AO • MUSE Image Quality

  33. Continuum detection IAB < 26.7 Reduced R (300) 154 gal. arcmin-2 95% at z<3 z 0.2 3.2 Deep field 1 arcmin 1 arcmin

  34. Lya detection Flux Lya> 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] Deep Field - Lya z 2.8 4.7 6.7

  35. Lya 2.8 z z 0.2 z 2.8 4.7 3.2 6.7 Lya Continuum Deep Field • 399 gal. arcmin-2 1 arcmin 4.7 6.7

  36. F(Lya)> 3.10-19 erg.s-1.cm-2 IAB<26.5 Deep Field Gal.arcmin-2 redshift

  37. Deep Field - Lya • Continuum of high z Lya 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 ?

  38. z 4.7 z z 2.8 0.2 4.7 6.7 3.2 Lya Continuum Spatial resolution Intensity in log scale Seeing limited observations in poor seeing conditions 260 gal.arcmin-2 in total, 75 gal.arcmin-2 in z=[4-6.7] Lya 2.8 6.7

  39. z Lya 6.7 2.8 4.7 z z 2.8 0.2 4.7 6.7 3.2 Lya Continuum Source confusion 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]

  40. Lya 6.7 4.7 z z 2.8 0.2 4.7 6.7 3.2 Lya Continuum Source confusion 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] 2.8 z

  41. Lya 4.7 z z 2.8 0.2 4.7 6.7 3.2 Lya Continuum Source confusion 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] 6.7 2.8 z

  42. z z 0.2 3.2 Lya Continuum Field to Field variation 2.8 4.7 6.7 Field Variations

  43. 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

  44. Phase Stop 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 High-order AO mirror

  45. 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

  46. 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

  47. HARPS@3.6M: ACen B Oscillations (400 exposures, 6.5 hours) Built by Geneva Observ. & Bern Univ. (CH), OHP & Service d’Aéronomie (F), ESO La Silla & Garching

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