* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Download Extremely Large Telescopes
Fermi paradox wikipedia , lookup
Aquarius (constellation) wikipedia , lookup
History of astronomy wikipedia , lookup
Modified Newtonian dynamics wikipedia , lookup
Dialogue Concerning the Two Chief World Systems wikipedia , lookup
Corvus (constellation) wikipedia , lookup
History of Solar System formation and evolution hypotheses wikipedia , lookup
Formation and evolution of the Solar System wikipedia , lookup
Non-standard cosmology wikipedia , lookup
Hubble Space Telescope wikipedia , lookup
Rare Earth hypothesis wikipedia , lookup
Astrobiology wikipedia , lookup
History of the telescope wikipedia , lookup
Physical cosmology wikipedia , lookup
Satellite system (astronomy) wikipedia , lookup
Jodrell Bank Observatory wikipedia , lookup
History of gamma-ray burst research wikipedia , lookup
Space Interferometry Mission wikipedia , lookup
Chronology of the universe wikipedia , lookup
Leibniz Institute for Astrophysics Potsdam wikipedia , lookup
Gamma-ray burst wikipedia , lookup
Lambda-CDM model wikipedia , lookup
Star formation wikipedia , lookup
Observable universe wikipedia , lookup
Extraterrestrial life wikipedia , lookup
Spitzer Space Telescope wikipedia , lookup
H II region wikipedia , lookup
Astrophotography wikipedia , lookup
Structure formation wikipedia , lookup
International Ultraviolet Explorer wikipedia , lookup
Timeline of astronomy wikipedia , lookup
James Webb Space Telescope wikipedia , lookup
Extremely Large Telescopes Isobel Hook University of Oxford JENAM 2005 OPTICON ELT Science Working Group • • • • • OPTICON activity under EU FP5 & FP6 Over 100 volunteers Open to all Parallel to Design Study Recent meeting: Florence, Nov 2004 JENAM 2005 ELT Projects - Europe Euro-50 VLT –UT1 OverWhelmingly Large (OWL) Science with a 50-100m telescope Planets orbiting other stars Star formation history across the Universe Planetary environments of other stars Dark Matter Solar system: planetary weather Dark Energy Solar system: complete census of small bodies First objects and the reionisation of the Universe Resolved stellar populations High redshift intergalactic medium Massive Black Holes demography THE UNEXPECTED Our Solar System Object Surface Resln* (km) ~106 Illustrative + Repeat observations Pixels across typical disc Moon 4m Mars ~2 Asteroids Notes Equivalent to flotilla of spacecraft 3-7 3400 ~200 Ceres, Vesta Jupiter 8 ~500 moons Saturn 15 ~300 Titan Uranus 30 ~25 Ariel Neptune 45 ~90 Triton Pluto 60 ~90 Varuna 63 ~15 Large TNO *Assuming 100m telescope diffraction limit at 1mm Jovian Satellite Io JENAM 2005 ELT terrestrial planet studies – are we alone? • 30m telescope can observe mature gas-giant exoplanets to 10-20pc Candidate Hot Giant Exo-planet observed with VLT/NACO (Sep 04) • To study exo-earths, need: – – – – – large sample (~1000 stars) to reach ~30pc resolution (~33mas) contrast ~1010 >50m • Want to obtain: – – – Spectroscopy > O2, H2O Orbits Whole systems GQ Lupi b – Neuhauser et al (Apr 05) JENAM 2005 Planet detection models for OWL O. Hainaut and R. Gilmozzi • Simulated eX-AO-corrected psf • Spectra of Sun, Jupiter, Earth • Sky • OWL efficiency simulator • Photon noise • cophasing errors Filter R, t= 10ks strehl=0.5 d = 10pc, D=100m Jupiter: S/N=80 Earth: S/N=10 100m may detect Earth to 25pc Spectroscopy to about 15pc 0.5” JENAM 2005 Factors affecting contrast • Now have quantitative estimates/ simulations - or requirements on control for: – – – – – – JENAM 2005 Seeing speckles (differential imaging) Scintillation Piston errors (static & non-static) Coronography Wavelength difference between WFS and science Non common-path WF errors Planets and Stars • Giant planets – – Moons Rings • Planetary disks • gaps • Low-mass (planetary?) objects • Jets, outflows Simulation of planetary disk formation – Lucio Mayer Gemini observations of the Orion nebula - Lucas, Roche & Riddick (2003) HST image of Eta Carinae -Morse & Davidson, NASA Resolved Stellar populations and Galaxy Formation • Measuring age & chemical composition of individual stars > merger history • Colour-mag diagram reveals multiple stellar pops • Currently limited to MW and its satellites • 30-m telescope could extend this to other galaxies in LG e.g. M32 • What about a representative slice of the Universe? • Need ~100m to reach Virgo – Overcome crowding – Collecting area Aparicio and Gallert (2004) JENAM 2005 Resolved stellar populations -II • Spectroscopic observations give dynamics (eg CaT) • Intemediate-res measures metallicity indicators • High-res spectroscopy gives abundances • Simulations needed to set requirements on – PSF shape – Stability (temporal and spatial across field) – Optimal wavelength Figure credit: Paul Harding JENAM 2005 Black Holes • ELT can resolve sphere of influence of Black holes at large distances from us • E.g. a 100m telescope at diffraction limit can resolve – 104 Mo BH out to 10 Mpc from us – Supermassive 109 Mo BH at all redshifts (where they exist!) Artist’s conception of an AGN (GLAST/NASA) JENAM 2005 M. Hughes et al Evolution of galaxies: Physics of galaxies 1<z<5 • Goal: to understand formation of galaxies & feedback processes (SNe, AGN) • Want to spatially resolve on kpc scales: – – – – – – – Star formation history Stellar mass Extinction Metallicity Ionisation state Line shapes (> winds) Internal dynamics • Relate this to galaxy haloes JENAM 2005 Velocity fields of distant galaxies from GIRAFFE Integral-field Unit observations (Flores et al 2004) Evolution of Galaxies: Assembly of galaxy haloes • Map evolution dark matter from 1<z<5 • Understand effects of merging and feedback processes • Want to measure: – kinematics within large galaxies – kinematics of satellites – lensing of background objects (halo masses) Evolution of dark matter in a galaxy halo- Abadi et al 2003 JENAM 2005 Evolution of galaxies: Requirements • Similar for galaxies & haloes • Multiple IFUs: 2 types – 10 with 2”x2” – 100 with 0.5”x0.5” • R~ 5000-10000 • 0.5-2.5mm – (goal 0.3-2.5mm) • AO system for resolved studies (0.01-0.05”) • FOV >2’ (10’ goal) • ~ 1 night per field with a 100m JENAM 2005 FALCON concept (Hammer et al) The First Galaxies • z~ 6-7 galaxies have been found • Higher-z must exist – – – Old populations seen at z~6 Z~6 QSOs imply massive galaxies at earlier epochs Universe is ionised by something! • Find by imaging – – Use JWST to find candidates? Probably too faint for JWST continuum spectroscopy • 60m could reach mH~29 in 100hrs (depending on source size) • Spectroscopy at z>10 hard even for 100m The Universe at z=6.1 (Gnedin 2000) Neutral H, ionising intensity (z), gas density, gas temperature Re-ionisation history of the Universe • Probe IGM and its reionisation structure to very high redshift • Possible point sources at z>10 QSOs GRBs SNe (Pop III?) • Requirements: – – – – JENAM 2005 High R: 1000 –10,000 Single sources Near-IR (JHK) > 30m needed for R=104 in NIR for all except brightest GRBs Cosmology and Fundamental parameters • What drives the expansion of the Universe? • What is the Dark Energy? – – – – – JENAM 2005 Primary distance indicators – e.g. Cepheids to z~0.1 Type Ia Supernovae to z~4 Type II SNe to z~10 (and get SF history for free!) Gamma-Ray Bursts as distance indicators QSO absorption lines • Direct measurement of expansion [e.g. CODEX, R~400,000] • Variation of fundamental parameters? Keck observations of Q1422+231 (Sargent & Rauch) European ELT Design Study • Started March 2005 • Collaboration of 30 participants • Awarded Funding under EC Framework Programme 6 • + Funding from ESO & other participants • Programme managed by ESO • Runs for 4 yrs (2005-2008) • Focus: Enabling technology JENAM 2005 • • • • • • • • • • • 01000 Project coordination 02000 Science requirements 04000 Wave-front Control 05000 Optical Fabrication 06000 Mechanics 08000 Enclosure & infrastructure 09000 Adaptive Optics 10000 Observatory & science ops 11000 Instrumentation 12000 Site Characterization 13000 System layout, analysis & integrated modelling ELT Design Study • Adaptive Optics – Simulations of AO, MCAO – APE – large deformable mirrors • Effects of wind – Wind tunnel tests – Sensors on Jodrell Bank – Is an enclosure necessary? • Instrumentation – Flexure – gravity stable platforms? – ADC JENAM 2005 ELT Projects and Timescales GMT - Giant Magellan Telescope • First mirror being made TMT - Thirty Meter Telescope • Design study part funded • Project office set up • Design decision 2007 • Aiming for First light 2014/2015 • Japan, China, Australia also interested in ELT projects JENAM 2005 European ELT • ESO council : “pursuing an ELT is an urgent priority” • European Design Study started • Design decision around 2008 – OWL (60-100m), Euro-50… • First light date depends on funding – 2016/17 (part-filled) to 2020/2021 • AURA MOU with ESO to collaborate in some areas http:www.saao.ac.za/IAUS232/ JENAM 2005 Conclusions A lot of activity Worldwide Full science case recently completed European Technical Design Study has started Developing Science Requirements JENAM 2005 OWL simulation ESO THE END JENAM 2005 Comparison with JWST resolved unresolved • JWST above atmosphere but many times smaller • ELTs outperform JWST in many regimes: – High-res spectroscopy to 4mm (25mm for a 100m ELT) – Imaging mode to 2.5mm (3.5mm) – High spatial resolution – Low-res spectroscopy: 100m is more sensitive up to J band for resolved objects JENAM 2005 From GMT science case Detectable star formation rates from Ly a emission-line spectroscopy with an AO-fed near-IR spectrometer on the 20m GMT and NIRSPEC on JWST (10 hour integrations). For this case, a 20m telescope is able to reach about a factor 4 fainter than JWST Exo-earth Detection Comparison (Angel, 2003) Telescope wave (mm) mode S/N* (earth@10pc, t=24h) space interf space filled 4x2m 7m 11 0.8 nulling 8.4 coron 5.5-34 Darwin, TPF JWST Antarctic 21m 30m ground 100m Antarctic 100m nulling coron nulling coron coron coron coron coron GMT ground 11 0.8 11 0.8 11 0.8 11 0.8 0.52 5.9 0.34 4.1 4.0 46 17 90 Celt, GSMT OWL BOWL=better OWL S/N is for detection of an Earth twin at 10pc 100m has ~twice the REACH of TPF t=24hrs, QE=0.2, bandwidth Dl/l=0.2 Surveys ~1000 stars cf 100 Context for 2010-2020 • Maturity of current generation telescopes – AO l/D performance, 2nd gen instruments • Interferometry – IR: “Faint object” regime (K~20), astrometry (mas) – ALMA mm, sub-mm “equivalent” of optical facilities • New space telescopes – JWST, XEUS, TPF/Darwin precursors… To obtain spectra of the faintest sources from HST need 30m To obtain spectra of the faintest sources from JWST need 100m JENAM 2005VLT Gemini Subaru Keck JWST Planet Detection from the Ground Lardiere et al 2003 Assumes •System at 10pc •S/N =3 in 10hrs in the J-band. •Mauna Kea site JENAM 2005 Point Sources at z>10 Detection limits estimated by J. Bergeron & M. Bremer • GRBs at R=104 – 30m could do very bright GRBs and/or within ~1 day – Bulk of GRB population at +10d need 100m (KAB=27.4) GRB NASA / SkyWorks Digital • Population-III SNe at R=104 – Massive stars (140-260 M) should explode as very bright supernovae: e.g. K=25.2 at z=12 (extrapolated from Heger et al 2001) – Detectable from the ground out to z~16 for ~one month – For z>10 this needs ELTs of 70-100m size • High-z QSOs – Bright QSOs are rare. More typical QSOs cannot be observed at R=104 even with 100m – R=2x103 could be done: e.g. to explore the metal-enrichment of the IGM at early times from CIV forest. Need R=104 NIR spectrograph JENAM 2005 Detectability of z=8-20 galaxies Imaging Spectroscopy • Expect rest-frame UV at • Ly-a in near IR from z = 8 to 8 <z<14 = 28-29 mag (vega) 19 • Redshifted to J-K • EW 100-200A expected • Feasible with 100m and AO – Detectable with 100m • Feasible at lower z (e.g. in J – Asymmetry a challenge band) with 30m • Require 5-10 arcmin field for multiplex • Are they resolved? – half-light radii 0.2” at z~6 • Could be used as – Are they “knotty”/more background to study IGM on compact at higher z? 1 arcmin scales (but – Instrumentation should resolved) match the scale of objects JENAM 2005 Hubble UDF image ELT Projects – N. America Giant Magellan Telescope GMT (21m) CELT GSMT TMT: Thirty Meter Telescope VLOT JENAM 2005 ELT performance - Spatial Resolution 0.5 arcsec Starburst region 0.6 arcsec Giant HII region Compact HII region AO-8m 100m VLT ELT Globular cluster + dramatic improvement in point-source sensitivity JENAM 2005 WM WL 0.3 0.7 0.0 0.0