simulations of high-z galaxy observations with an e-elt/mos mathieu puech compass
TRANSCRIPT
ELT-MOS
• MOS are workhorse instruments for the VLT (3 in ops, 1 in commissioning, 1 proceeding to phase B)
ELT-MOS
• Exploiting high-density SCs (1-10 arcmin-2) efficiently within the E-ELT patrol field (~40 arcmin²) requires a MOS
ELT-MOS
• ESO E-ELT Instrument Phase A studies :
PI : F. Hammer
Seeing/GLAO limited mono-apertures (240)+ 30 IFUs
PI : JG Cuby / S. Morris
20 MOAO-fed IFUs
ELT-MOS
• ESO E-ELT Instrument Phase A studies :
PI : F. Hammer
Seeing/GLAO limited mono-apertures (240)(+ 30 IFUs)
PI : JG Cuby / S. Morris
20 MOAO-fed IFUs
+
=
30 arcsec
ELT-MOS/MOSAIC
High Multiplex Mode à la OPTIMOS-EVE : 100-250 Fibers with GLAO/seeing resolution
Coordination: François Hammer
BOARD:Beatriz BarbuyJean-Gabriel CubyLex KaperSimon Morris
Project Scientist:Chris EvansDep. : Mathieu Puech
Instrument Scientist:Gavin DaltonDep. : Hector Flores
Science Team
Project Manager:Pascal JagourelDep. : Phil Parr Burman
System Engineer:Phil Rees
Engineering Team
Other contacts: LNA & AIP (fibers), Univ. Nice, Vienna, Stockholm
HDM focal plate
Courtesy: David Pearson
HMM focal plate
Fiber-Only Option (FOO)Mixed-Architecture Design (MAD)
ELT-MOS/MOSAIC
ELT-MOS White Paper
Next step is to prioritise TLRand iterate with technical &operational feasibility
SIMULATIONS
ELT-MOS White Paper
Next step is to prioritise TLRand iterate with technical &operational feasibility
SIMULATIONS
WEBSIM
COMPASSPI : 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
Shaping E-ELT Science and Instrumentation
MO
AO
GLA
O
Spatially-resolved spectroscopy of z~2-6 galaxies is required for
distinguishing merger from rotation (Puech+10)
GLAO is unable to recover the dynamical nature
of z>2 distant galaxies (with ≲ 50 % of the Cn2
in the GL)
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)
Simulated SC : galaxy mass assembly
Rotating disk
Major m
erger
MOAO / 75mas/pix / R=5000 : no need for very high resolution !
Puech+08
Simulated SC : first light galaxies & reionisation
Simulated IFU observations of Ly- emission lines at z~9 (LAEs) :
Spatial template
Simulation of z~0 clumpy disks (Bournaud+07) rescaled in flux
and size to z~9using current HST
observations(eg, Grazian+12)
Spectral template
Half-Gaussian sized to currentobservations at z~3-7 (Steidel+03 ; Hu+10 ;
Jiang+13;Swinbank+07)EW(Ly) ↗ with J
AB
MOAO PSF : EE=30 % within 80x80 mas² (from EAGLE Phase A)
Kinematics
VLy= 200 km/s
(constant outflow ; Swinbank+07)
scaled at 270 km/s to observedIntegrated spectroscopy (Hu+10)
0.1-0.2’’
Optimal integratedSpectra (Rosales-Ortega et al. 2012)
JAB
=30R
half=100mas
« Faint & compact » atz~9
Very deep obs. :Exp. Time=40 hr
Simulated SC : first light galaxies & reionisation
Simulated LAEs at z~9 :
Grazian+12 obs.
Simulation grid
S∕N=5 in Ly- for pix=40/60/80/100/120 mas
JAB
=27
JAB
=28
JAB
=29
S/N-Optimal sampling : 40-120 mas
JAB
=30
40 hr4 hrPRELIMINARY
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~7using 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)
Optimal integratedSpectra (Rosales-Ortega et al. 2012)
JAB
=26R
half=150mas
Averaged size & flux at z~7
Exp. Time=40 hr
Optimal integratedSpectra (Rosales-Ortega et al. 2012)
JAB
=27R
half=100mas
« Faint & compact » atz~7
Exp. Time=40 hr
Simulated SC : first light galaxies & reionisation
Simulated UV interstellar lines at z~7 :
JAB
=25
JAB
=26
JAB
=27
S/N-Optimal sampling : 80-100 masS∕N=5 in SII(1527A) for pix=40/60/80/100/120 mas
40 hr40 hr
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?
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)
ELT-MOS
• ESO E-ELT Instrument Phase A studies : 2008-10
PI : JG Cuby / S. Morris
20 MOAO-fed IFUs
PI : F. Hammer
Seeing/GLAO limited observations
x 30
Mono-Object mode : x 240
Multi-IFU mode (0.3''/pix):
0.9''
(main OPTIMOS-EVE modes)
Simulated SC : galaxy mass assembly
MOAO z=4 GLAO z=450mas/pixR=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)