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Simulations of high-z galaxy observations with an E-ELT/MOS Mathieu Puech

Simulations of high-z galaxy observations with an E-ELT/MOS Mathieu Puech. COMPASS. ELT-MOS. MOS are workhorse instruments for the VLT (3 in ops, 1 in commissioning, 1 proceeding to phase B). ELT-MOS.

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Simulations of high-z galaxy observations with an E-ELT/MOS Mathieu Puech

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  1. Simulations of high-z galaxy observations with an E-ELT/MOS Mathieu Puech COMPASS

  2. ELT-MOS • MOS are workhorse instruments for the VLT (3 in ops, 1 in commissioning, 1 proceeding to phase B)

  3. ELT-MOS • Exploiting high-density SCs (1-10 arcmin-2) efficiently within the E-ELT patrol field (~40 arcmin²) requires a MOS

  4. ELT-MOS • ESO E-ELT Instrument Phase A studies : PI : F. Hammer PI : JG Cuby / S. Morris Seeing/GLAO limited mono-apertures (240) + 30 IFUs 20 MOAO-fed IFUs

  5. ELT-MOS • ESO E-ELT Instrument Phase A studies : + PI : F. Hammer PI : JG Cuby / S. Morris Seeing/GLAO limited mono-apertures (240) (+ 30 IFUs) 20 MOAO-fed IFUs =

  6. ELT-MOS/MOSAIC 30 arcsec

  7. ELT-MOS/MOSAIC 30 arcsec High Multiplex Mode à la OPTIMOS-EVE : 100-250 Fibers with GLAO/seeing resolution

  8. ELT-MOS/MOSAIC 30 arcsec High Def. Mode à la EAGLE : ≥10 MOAO-fed IFUs with ~ 40-80 mas/pix

  9. BOARD: Beatriz Barbuy Jean-Gabriel Cuby Lex Kaper Simon Morris Coordination: François Hammer Project Scientist: Chris Evans Dep. : Mathieu Puech Project Manager: Pascal Jagourel Dep. : Phil Parr Burman Science Team Instrument Scientist: Gavin Dalton Dep. : Hector Flores Engineering Team System Engineer: Phil Rees Other contacts: LNA & AIP (fibers), Univ. Nice, Vienna, Stockholm

  10. ELT-MOS/MOSAIC Mixed-Architecture Design (MAD) Fiber-Only Option (FOO) HMM focal plate HDM focal plate Courtesy: David Pearson

  11. ELT-MOS White Paper Issue 1.0 : ArXiv:1303.0029 Issue 2.0 : This Fall

  12. ELT-MOS White Paper Next step is to prioritise TLR and iterate with technical & operational feasibility SIMULATIONS

  13. ELT-MOS White Paper Next step is to prioritise TLR and iterate with technical & operational feasibility SIMULATIONS

  14. WEBSIM COMPASS PI : D. Gratadour ANR founding Major update of Websim over 2013-15 : -include sky background variations -include telluric features -implementation of batch mode -complete AO PSF library -extensive astrophysical templates as inputs -to be freely accessible http://websim.obspm.fr

  15. Simulated Science Case : Galaxy mass assembly

  16. Spatially-resolved spectroscopy of z~2-6 galaxies is required for distinguishing merger from rotation (Puech+10) MOAO GLAO is unable to recover the dynamical nature of z>2 distant galaxies (with ≲ 50 % of the Cn2 in the GL) GLAO Shaping E-ELT Science and Instrumentation

  17. Newman et al. (2012) VLT/AO + ELT-IFU/HARMONI as 1st light : Detailed kinematics of distant galaxies will be largely covered by the time ELT-MOS arrives  ELT-MOS to focus on large surveys with optimized pixel scale (resolution vs. SB)

  18. Simulated SC : galaxy mass assembly MOAO / 75mas/pix / R=5000 : no need for very high resolution ! Rotating disk Major merger Puech+08

  19. Simulated Science Case : First light galaxies & Reionisation

  20. First light galaxies & Reionisation

  21. Simulated SC : first light galaxies & reionisation Simulated IFU observations of Ly-a emission lines at z~9 (LAEs) : Spatial template Simulation of z~0 clumpy disks (Bournaud+07) rescaled in flux and size to z~9 using current HST observations (eg, Grazian+12) Kinematics VLya= 200 km/s (constant outflow ; Swinbank+07) s scaled at 270 km/s to observed Integrated spectroscopy (Hu+10) 0.1-0.2’’ Spectral template Half-Gaussian sized to current observations at z~3-7 (Steidel+03 ; Hu+10 ; Jiang+13;Swinbank+07) EW(Lya) ↗ with JAB MOAO PSF : EE=30 % within 80x80 mas² (from EAGLE Phase A)

  22. Optimal integrated Spectra (Rosales- Ortega et al. 2012) JAB=30 Rhalf=100mas « Faint & compact » at z~9 Very deep obs. : Exp. Time=40 hr

  23. Simulated SC : first light galaxies & reionisation Simulated LAEs at z~9 : PRELIMINARY 4 hr 40 hr Grazian+12 obs. JAB=27 Simulation grid JAB=28 JAB=29 JAB=30 S∕N=5 in Ly-a for Dpix=40/60/80/100/120 mas S/N-Optimal sampling : 40-120 mas

  24. Simulated SC : first light galaxies & reionisation Simulated IFU observations of UV interstellar lines at z~7 : Spatial template Simulation of z~0 clumpy disks (Bournaud+07) rescaled in flux and size to z~7 using current HST observations (eg, Grazian+12) Spectral template Stacked z~3 LBG spectrum (Shapley+03) rescaled in flux & resampled at R=5000. Focus on the SII/CIV region. MOAO PSF : EE=30 % within 80x80 mas² (from EAGLE Phase A)

  25. Optimal integrated Spectra (Rosales- Ortega et al. 2012) JAB=26 Rhalf=150mas Averaged size & flux at z~7 Exp. Time=40 hr

  26. Optimal integrated Spectra (Rosales- Ortega et al. 2012) JAB=27 Rhalf=100mas « Faint & compact » at z~7 Exp. Time=40 hr

  27. Simulated SC : first light galaxies & reionisation Simulated UV interstellar lines at z~7 : 40 hr 40 hr JAB=25 JAB=26 JAB=27 S/N-Optimal sampling : 80-100 mas S∕N=5 in SII(1527A) for Dpix=40/60/80/100/120 mas

  28. Conclusions • A MOS will be essential on the E-ELT • New consortium inherited from/building on the phase A: MOSAIC = EAGLE + OPTIMOS-EVE • Updated Sc. Req. captured in a ELT-MOS white book • Simulations of MOAO-fed IFU observations: • Galaxy mass assembly: moderate spatial scales (~75 mas) favored with EE~25-30% • Integrated spectra of very high-z galaxies: spatial scales ~ 80-100 mas favored • Next steps for simulations: • Spatially-resolved kinematics of absorption lines (MOAO) • Simulation of mono-aperture (GLAO-fed) spectra: what is the optimal on-sky aperture? • Specifications on the MOAO system: EE vs. DM pitch?

  29. Sky subtraction with fibers demonstrated with FLAMES (I-band) on sky Expected in J-band: 0.6% of the sky-continuum & much better with IFUs (Yang et al., Messenger, in press; see also Yang et al’ Poster)

  30. ELT-MOS • ESO E-ELT Instrument Phase A studies : 2008-10 PI : JG Cuby / S. Morris PI : F. Hammer x 240 Mono-Object mode : 0.9'' Multi-IFU mode (0.3''/pix): x 30 (main OPTIMOS-EVE modes) Seeing/GLAO limited observations 20 MOAO-fed IFUs

  31. Simulated SC : galaxy mass assembly GLAO z=4 MOAO z=4 50mas/pix R=5000 (Bournaud+07) Puech+10 GLAO is unable to recover the small-scale kinematics and rotation curves of z>2 distant galaxies (with ≲ 50 % of the Cn2 in the GL)

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