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

• 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

30 arcsec

ELT-MOS/MOSAIC

High Multiplex Mode à la OPTIMOS-EVE : 100-250 Fibers with GLAO/seeing resolution

30 arcsec

ELT-MOS/MOSAIC

High Def. Mode à la EAGLE : ≥10 MOAO-fed IFUs with ~ 40-80 mas/pix

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

Issue 1.0 : ArXiv:1303.0029Issue 2.0 : This Fall

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

Simulated Science Case : Galaxy mass assembly

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 Science Case : First light galaxies & Reionisation

First light galaxies & Reionisation

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)