MOSAIC@E-ELT: a MOS for Astrophysics, IGM & Cosmology

1. MOSAIC@E-ELT: a MOS for Astrophysics, IGM & Cosmology by François Hammer

2. TODAY: physics of z < 1 galaxies WISH meeting, 2013

3. TOMORROW: physics of z >> 1 galaxies with E-ELT + JWST Multiplex is a key issue for studies of galaxy evolution & formation See ELT-MOS white paper by Evans, Puech et al. WISH meeting, 2013

4. France-UK-Netherlands-Brazil: an international team to build the MOS of the E-ELT http://mosaic.obspm.fr/ MOSAIC team have developed then implemented: GIRAFFE/FLAMES - NACO - X-SHOOTER - KMOS WISH meeting, 2013

5. : with 2 main different observing modes • High definition (HDM, 40-80 mas/pix), 10-20 MOAO IFUs EAGLE science cases e.g., first sources, detailed kinematics of galaxies up to z=5, R=5000 • High multiplex (HMM, 100-250), GLAO/seeing resolution OPTIMOS-EVE science cases e.g., 1600 z > 1.5 galaxies in 1 FoV, galactic archeology, R=5000-20000 WISH meeting, 2013

6. A CENSUS for z >> 1 galaxies 30 arcseconds • spatially resolved kinematics of z>>1 massive galaxies • spectroscopy of dwarfs and their link to massive galaxies WISH meeting, 2013

7. ELT-MOS White Paper Issue 1.0 : ArXiv:1303.0029 Issue 2.0 : 2014 WISH meeting, 2013

8. ELT-MOS Science Cases WISH meeting, 2013

9. Science Team Jose Afonso, David Alexander, Omar Almaini, Beatriz Barbuy, Nate Bastian, Xavier Bonfils, Piercarlo Bonifacio, Nicolas Bouche, Enzo Brocato, Andy Bunker, Elisabetta Caffau, Karina Caputi, Andrea Cimatti, Michele Cirasuolo, Christopher Conselice, Thierry Contini, Jean-Gabriel Cuby, Katia Cunha, Massimo Dall'Ora, Gavin Dalton, Ben Davies, Reinaldo de Carvalho, Alex de Koter, Karen Disseau, James Dunlop, Benoit Epinat, Chris Evans, Michele Fabrizio, Annette Ferguson, Fabrizio Fiore, Hector Flores, Adriano Fontana, Emanuele Giallongo, Eike Guenther, Francois Hammer, Vanessa Hill, Marc Huertas-Company, Lex Kaper, Thierry Lanz, Soeren Larsen, Bertrand Lemasle, Claudia Maraston, Ross McLure, Simona Mei, Simon Morris, Goran Ostlin, Roser Pello, Laura Pentericci, Celine Peroux, Rolf-Peter Kudritzki, Patrick Petitjean, Henri Plana, Mathieu Puech, Myriam Rodrigues, Emmanuel Rollinde de Beaumont, Hugues Sana, Daniel Schaerer, Mark Swinbank, William Taylor, Eduardo Telles, Goncalves Thiago, Scott Trager, Niraj Welikala, Yanbin Yang, Stefano Zibetti, Bodo Ziegler Numerous science cases have been simulated

10. Need for imagery & photometry • Imagery for comparing with kinematics • 3D-spectroscopy, with small multiplex (10-20/ELT fov), • requires high spatial resolution images: JWST / ELT-CAM • (Multi-band) photometry to catch very high-z sources • spectroscopy with higher multiplex (100-200/ELT fov), • low spatial resolution images are OK: WISH / Ground based telescopes • 1 E-ELT fov ~ 40-50 arcmin2

11. Need for imagery & photometry 1 mag

12. Deepest existing images CANDLES Area: 0.25 deg2 Groging+11 Keokemoer+11 • HAB= 27: • 8000 galaxies in an E-ELT FoV (~40 arcmin2) • 1600 z > 1.5 galaxies MOS can already detect highest z galaxies from HST photometry WISH meeting, 2013

13. SC1: First galaxies & Reionisation 10s (in absorption) to 100s (in emission) of sources expected in the E-ELT FoV WISH meeting, 2013

14. SC2: galaxy mass assemblyDiscriminating mergers/disks TLR:≥10 MOAO-fed IFUs with ~75mas/pixel, z=2-4 Puech+08 Rotatingdisk Major merger WISH meeting, 2013

15. Future existing galaxy imagery (excerpt from Hervé Aussel) MOS will be able to detect/study highest z galaxies from JWST/ELT-CAM imagery & photometry WISH meeting, 2013

16. 1600 galaxies at z> 1.5 in an E-ELT FoV (mostly dwarfs) • Origin of dwarves: primordial galaxies or tidal dwarfs? • Low surface brightness galaxies in the gaseous-rich Universe • Test of curvature (L using HII galaxies) SC3: Study the numerous distant galaxy population mJ(AB)<26 Based on CANDEL counts & Dahlen photo’z

17. Optical imagery/photometry for searching very high z sources • WISH will probe deep imagery in additional FoVs (at large depths, cosmic variance has to be tested); • with its Extreme Survey (AB ~ 29-30, 0.25 sq deg.) it will bring a very important addition to the “single cosmological field” problem (e.g., the 3hr field -GOODS- with the VLT); • For z ~ 7-8, it is necessary to have imagery IAB ~ 28+2=30 to warrant Lyman break detection • Other needs are mostly for (larger) survey modes (galaxy statistics, ids of large scale structures) WISH meeting, 2013

18. Fibre Only Option: High Definition Mode (HDM) HDM focal plate Courtesy: David Pearson Assumptions 12 science channels Light transfer optics: - Pick off mirror - Intermediate fold mirror - Receiving mirror In-plane rotation >180deg Known issues Further degrees of freedom required in each optical item. Pick-and-place system required to cope with optical items of different shapes and sizes. Synchronisation of plate rotation with LGS system. Spectrographs WISH meeting, 2013

19. Fibre Only Option: High Multiplex Mode (HMM) Courtesy: David Pearson HMM focal plate Assumptions 120 science channels Buttons with fibre retraction scheme Stepped focal plate In-plane rotation >180deg Known issues Change in field curvature causes difficulty in fibre alignment and focus. Synchronisation of plate rotation with LGS system. Spectrographs WISH meeting, 2013

20. Mixed Architecture Design: implementation Focal plate close up 1x LGS light path 1x NGS light path 1xHDM light path 6x HMM or IGM light paths WISH meeting, 2013

21. Conclusions • An E-ELT FoV contains 8000 HAB<27 sources, 1600 z > 1.5 galaxies • High multiplex & high definition modes needed: this is MOSAIC • MOSAIC@E-ELT with multi-IFUs can detect the first light, solve the reionisation problem & probe the galaxy mass assembly • Best solution for stellar and galaxy SCs is to couple high multiplex with R=3000-20000 & moderate multiplex with MOAO IFUs! 100 billions stars per galaxy & 100 billions galaxies: they require a MOS WISH meeting, 2013

22. PRESENT STATUS OF MOSAIC • Science: • a white paper written for most science cases (see Evans, Puech et al., 2013, arXiv1303.002E) • all MOS science cases shown at ‘Shaping E-ELT Science and Instrumentation’ (Feb. 2013, ~ 200 attendees) require both high multiplex and high definition modes • Up-dated version expected this end of this year: European & Brazilian astronomers very present: increasing involvement from French community • compromise between pixel size and need for K-band (high definition mode, MOAO-IFUs) and the high multiplex mode (100 to 300) • final compromise in course, this mid-2013 • Technics: • 2 solutions already investigated (FOO & MAD) • Teleconferences each 15 days (organised by P. Jagourel, PM) • Cost/risk/operability firstly evaluated • AO meeting this October to revisit the existing solutions/conditions • Mid of 2014: one choice and one back-up, ready for ESO Call WISH meeting, 2013

23. Sky subtraction with fibers demonstrated with FLAMES (I-band) on sky Expected in J-band: 0.6% of the sky-continuum & at the theoretical limit (~ 0.2-0.3%) with IFUs (Yang et al., Messenger, March 2013 issue) WISH meeting, 2013

24. OH OH OH OH TLR on the sky subtraction : Systematics ≲ 0.1 % First light galaxies & reionisation Spectroscopy down to J/HAB~27-28 in absorption (see K. Disseau’s talk) Sky continuum is ~ 19.5-20 arcsec-2 in J/HAB (Sullivan+12) WISH meeting, 2013

25. Cross beam switching observations Yang et al. 2013 FLAMES-GIRAFFE tech. time WISH meeting, 2013

26. Cross beam switching observations Yang et al. 2013 FLAMES-GIRAFFE tech. time WISH meeting, 2013

27. Accurate sky subtraction Yang et al. 2013 Physical limit reached & demonstrated on sky Residual signal limited by scattered light (like with slits) Foreseen achievable accuracy: ~ 0.1% -Optimize design & operations -Specific algorithm (PCA, Sharp+10) WISH meeting, 2013