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

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. Seeing/GLAO limited mono-apertures (240)
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. Seeing/GLAO limited mono-apertures (240)
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 High Multiplex Mode à la OPTIMOS-EVE : 30 arcsec
Fibers with GLAO/seeing resolution

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

9. Other contacts: LNA & AIP (fibers), Univ. Nice, Vienna, Stockholm
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
Engineering Team
System Engineer:
Phil Rees
Instrument Scientist:
Gavin Dalton
Dep. : Hector Flores
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:
Issue 2.0 : This Fall

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

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

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

15. Simulated Science Case : Galaxy mass assembly

17. 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

18. 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)

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

20. Simulated Science Case : First light galaxies & Reionisation

21. First light galaxies & Reionisation

23. 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) ’’
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)

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

25. 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-Optimal sampling : mas
S∕N=5 in Ly-a for Dpix=40/60/80/100/120 mas

26. 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)

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

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

29. 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 : mas
S∕N=5 in SII(1527A) for Dpix=40/60/80/100/120 mas

30. 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 ~ 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? 30

31. 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)

33. 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

34. Simulated SC : galaxy mass assembly
MOAO z=4
GLAO 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)