ESO Extremely Large Telescope • MICADO Near Infrared Diffraction Limited Camera λ= 800nm – 2.5µm T≤100K R≤5000 • METIS (PI Institute) Mid Infrared Camera & Spectrograph λ= 2.8µm – 14µm T≤30K R≤100000 • MOSAIC Multi Object Spectrograph λ= 500nm – 1.7µm T=300K R≤10000 • EPICS Extreme AO Planet IFS & Spectro-Polarimeter λ= 500nm – 930nm T=300K R≤300 ESO Very Large Telescope 2003 MIDI 2 Telescope Interferometer Spectrometer 2003 λ=7µm – 14µm T≤40K R≤700 2004 VISIR Mid InfraRed Imager and Spectrograph 2004 λ= 7µm – 27µm T≤30K R≤25000 2004 SPIFFI 2k Spectroscopic Camera for SINFONI 2005 λ= 1µm – 2.5µm T≤100K R≤4000 2009 X-Shooter UV-VIS-IR Spectrograph 2009 λ= 300nm – 2.5µm T≤100K R≤10000 2014 Sphere-ZIMPOL Extreme Adaptive Optics Imaging Polarimeter 2014 λ= 570nm – 900nm T=300K >25 Filters 2017 MATISSE 4 telescope Interferometer Spectrometer 2015 λ= 2.8µm – 14µm T≤35K R≤6000 James Webb Space Telescope MIRI Mid InfraRed Instrument Spectrometer Main Optics λ=5µm-28µm T=6.8K VLT in 2030 Heritage ELT in 2030 GAIA Future VLT more surveys - less individual small projects. MAVIS (optical AO high resolution imaging – excellent complement to MICADO) Moderate resolution Cass UV spectrograph (CUBES / UVES upgrade) ERIS & MOONS BLUEMUSE MUSE-like AO-assisted IFU spectrograph operating up to K band micron FLAMES upgrade / replacement (complementary to 4MOST / MOONS). Wide field IFU - spectroscopic wide field survey (SDSS V but deeper, better and everything). - repeat observations for transients - slave spectroscopic-imager IFU to Athena's WFI (FoV 40’x40’). VLT prime focus camera for larger field of view / VLTI capabilities? new wide field multi-fibre spectroscopy faculity - high spectral resolution: R>40-60k - Complementary to 4MOST & WEAVE & GAIA - 130fibres over 30arcmin diameter (or more?) wide field MOS on a 10m telescope dedicated to surveys. - R=20k - galactic archaeology (GAIA), cosmology (Euclid). Transients (LSST). Wide field with massive MOS (4most on an 8m) careful tradeoff with VLTI Wide-field NIR imager (VISTA/VIRCAM detectors) complementary to Euclid in K band and better image quality than Euclid. - large-scale structure and galaxies at redshift ~1. - wide area survey, 100s of nights. Very wide-field VIS+IR imaging capabilities - >1 square degree area - find targets in the EoR redshift range via photo-z's. - Complementary to SKA deep fields, targets selection for follow-up and HI absorption measurements with SKA. All sky survey with MOS doing polarimetry Dedicated UT for Transiting Exoplanet Atmospheres - similar to having the HARPS instrument on a dedicated La Silla Telescope. - high resolution spectroscopy from Optical to IR, something like ESPRESSO+CRIRES+. - 50-to-100 nights/year Improved FORS – better calibrate instrumental systematics 2 UT’s working in parallel - both low and high resolution spectroscopy simultaneously IFU high-dispersion spectroscopy with high-contrast imaging at the VLT for exoplanet characterization (RISTRETTO) SPHERE upgrade: AO, coronagraphs, polarimetry, IFU Synoptic, time-domain astronomy, Follow-up BlackGEM & LSST - longer time-series spectroscopy/photometry - lower-resolution spectroscopic identification. - spectroscopic surveys - ToO overrides - Long term monitoring Support / enhance / capitalise on ESA's Large missions Athena & LISA JWST and Euclid follow-up HIPERCAM X-Shooter with VIS/NIR AO fast-and-dirty low res R=1000 spectroscopy Robotised VLT as a transient follow-up machine VLT in 2030 VLT in 2030 Synergy Exoplanet wishes and ideas Wide Field Trade off Ramon Navarro NOVA instrumentation Manager with input from NOVA community