Synergies between and E-ELT

Transcription

1 Synergies between and E-ELT Aprajita Verma & Isobel Hook 1) E- ELT Summary 2) E- ELT Project Status 3) Parameter space 4) Examples of scientific synergies

2 The World s Biggest Eye on the Sky 39.3m diameter, adaptive telescope First light early 2020s Total Cost: 1082 million (2012) Top priority for European ground- based astronomy (ASTRONET) E-ELT VLT

3 E-ELT Project Status ª Dec 2011: Construction proposal submitted to ESO Council ª Dec 2012: ESO Council approved ELT Programme ª Awaiting Brazil to complete ratification procedure ª Preparatory work going ahead ª Detailed design of M4 ª Infrastructure & access road ª Main dome and structure ª New ESO E- ELT Project Science Team formed (Jun 2012) ª Definition of instrument requirements ª ELT- IFU & ELT- CAM done ª ELT- MIR, ELT- MOS, ELT- HIRES

4 Phase A Instrument Studies EAGLE EPICS Multi- IFU, AO- fed near- IR spectrometer XAO imager/spectro- polarimeter for exo- planets HARMONI Diffraction- limited, near- IR IFU with optical extension METIS Mid- IR (3-14μm) imager & spectrometer OPTIMOS Seeing- limited/glao high- multiplex spectrograph CODEX Ultra- high- resolution optical spectrograph MICADO Near- IR, high- resolution imaging camera SIMPLE Near- IR, high- resolution spectrograph AO- relays MAORY (MCAO relay) & ATLAS (LTAO relay)

5 E-ELT Instrumentation Roadmap ª Two first light instruments ª ELT- CAM ª ELT- IFU ª with associated AO system(s) ª MID- IR instrument shortly after ª Subject to readiness review ª ELT- MIR, ELT- MOS, ELT- HIRES equal scientific priority ª Future decision points specified ª New instruments every ~2 years ª MOS and HIRES will be included ª Planetary camera will be included ª High priority, subject to technical readiness ª Open slot for new ideas ª Choices will continue to be made The roadmap (above) is part of the construction proposal

6 E-ELT and LSST Complementarity Parameter E-ELT LSST FOV Single object to 10 diameter patrol field 3.5 deg diameter λ range Optical to mid-ir Optical (ugrizy) Spatial resolution Spectral resolution ~Few mas (with AO) to seeing limited Broadband imaging to R~130,000 (TBD) Seeing limited Broadband imaging Location Cerro Armazones Cerro Pachon E- ELT fully steerable & capable of non- sidereal tracking Switching between instruments < 10 mins (same FS) 20 mins (different FS) Classification and detailed follow- up of rare and transient objects found by LSST

7 E-ELT sensitivity (39m) Band λ/d (mas) E- ELT LTAO imaging (AB) R=4000 Spectroscopy (AB) V (3.0) 27.3* 25.1 R (3.4) 28.5* 25.3 I J H K s point source limiting magnitudes (AB) in 1hr LSST 5σ depth for point sources: r ~ 24.5 (AB) per visit, 27.5 (AB) coadded E- ELT can do deep imaging E- ELT can do mid- high R spectroscopy at LSST single image depth E- ELT can do low- mid R spectroscopy at LSST stacked depth

8 E-ELT Spectroscopic Complementarity LSST Gold Sample E-ELT 1h E-ELT 10h E-ELT 20h Figure adapted from the LSST Science Book

9 Scientific synergies LSST Dark Matter Dark Energy Solar System Transients Milky Way E-ELT Fundamental Physics Black Holes Galaxy Formation Resolved Stellar Populations Exo-planets

10 Scientific synergies: Solar System LSST E-ELT Dark Matter Dark Energy Solar System Discovery and Orbits: Asteroids Search for NEOs Spectra and high-resolution imaging: Cometary volatiles, Fundamental Physics Black Holes Galaxy Formation Transients Milky Way TNOs Comets Sedna-like objects beyond the Kuiper belt Atmospheres, weather Surface structure, volcanic activity Resolved Stellar Populations Exo-planets

11 Scientific synergies: Transients LSST E-ELT Dark Matter Fundamental Physics Dark Energy GRB detection and photometry, GRB Photometry & spectroscopy Black Holes Solar System SNe SN spectra Galaxy Formation Transients Milky Way AGN variability Lensing events Classification and redshifts for new transients Resolved Stellar Populations Exo-planets LSST will generate a huge number of transient events. E-ELT follow-up likely to be focussed on well understood (i.e. easily identified from the transient pool) objects or rare, exotic events.

12 ª GRBs to z~8 and above ª Type Ia SNe to z~4 ª Ultralumuninous SNe to z~6 E-ELT Spectroscopy of transients Above: VLT and simulated GRB spectrum at z=8 [HIRES white paper] Right: Simulated ELT spectrum of a SNIa at z=4 [by Tim Goodsall & I. Hook]

13 Scientific synergies: Cosmology LSST E-ELT Dark Matter Fundamental Physics Dark Energy WL LSS SNe (spectra) CODEX Black Holes Solar System Transients BAO SNe Fundamental constants Galaxy Formation Resolved Stellar Populations Milky Way Exo-planets Calibration of photo-z s: ELT WF MOS spectroscopy will improve accuracy (+ perfect sample for galaxy evolution studies)

14 Scientific synergies: Nearby Galaxies LSST E-ELT Dark Matter Fundamental Physics Dark Energy Solar System Transients Milky Way Map galactic structure and streams (photometry and astrometry) Galactic centre Resolved stellar abundances and kinematics from spectra Structure of galaxies beyond the LG Black Holes Galaxy Formation Resolved Stellar Populations Exo-planets

15 Scientific synergies: Galaxies LSST E-ELT Dark Matter Dark Energy LF evolution with z, morphology, colour Internal structure and dynamics of galaxies to z~4 Fundamental Physics Black Holes Solar System Transients Milky Way Bulge-disk devonvolution AGN survey (colour & variability) The highest redshift galaxies Census of BHs via dynamical effects Galaxy Formation Resolved Stellar Populations Exo-planets Simulated major merger at z ~ 4 (1.4bn yrs) (Puech et al 2008): v σ

16 Weighing Dark Sub-halos ª Steep halo mass function at sub- galactic mass scales is a strong prediction of CDM see far fewer MW satellites than predicted ª Strong lenses: Extragalactic complement to MW satellite studies ª LSST will find >10 4 strong lenses ª ELTs follow- up 100s of M DM sub- halos identify dark substructure through ª High resolution imaging ª IFU spectroscopy Strigari et al Vegetti et al Vegetti et al. 2010

17 LSST imaging surveys will contain many lenses Expect 8000 lensed AGN, galaxy- scale lenses, 1000s of clusters, 100s of lensed SNe... Strong gravitational lens research is traditionally very labor- intensive (even automated searches): Inspection of lens candidates Detailed modelling of individual systems Will we have enough people?

18 LSST imaging surveys will contain many lenses Expect 8000 lensed AGN, galaxy- scale lenses, 1000s of clusters, 100s of lensed SNe... spacewarps.org

19 LSST imaging surveys will contain many lenses Expect 8000 lensed AGN, galaxy- scale lenses, 1000s of clusters, 100s of lensed SNe... CFHTLS images + Space Warps sims & new lenses (More, Marshall, Verma, et al)

20 Summary ª E- ELT and LSST very complementary ª E- ELT will follow LSST transients and other new sources ª Classification spectroscopy & deep photometry ª Optical to mid- IR ª E- ELT will do detailed follow- up of LSST sources, e.g. ª High spatial resolution (few mas) near- IR imaging and integral field spectroscopy ª High spectral resolution spectroscopy ª Multi- object spectroscopy ª Complementary approach to many key science questions