Transcript Simulations of high-z galaxy observations with an E

COMPASS
Simulations of high-z galaxy
observations
with an E-ELT/MOS
Mathieu Puech
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
PI : JG Cuby / S. Morris
Seeing/GLAO limited mono-apertures (240)
(+ 30 IFUs)
=
20 MOAO-fed IFUs
ELT-MOS/MOSAIC
30 arcsec
ELT-MOS/MOSAIC
30 arcsec
High Multiplex Mode à la OPTIMOS-EVE :
100-250 Fibers with GLAO/seeing resolution
ELT-MOS/MOSAIC
30 arcsec
High Def. Mode à la EAGLE :
≥10 MOAO-fed IFUs with ~ 40-80 mas/pix
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
Engineering
Team
System Engineer:
Phil Rees
Science Team
Instrument Scientist:
Gavin Dalton
Dep. : Hector Flores
Other contacts: LNA & AIP (fibers), Univ. Nice, Vienna, Stockholm
ELT-MOS/MOSAIC
Mixed-Architecture Design (MAD)
Fiber-Only Option (FOO)
HMM focal plate
HDM focal plate
Courtesy: David Pearson
ELT-MOS White Paper
Issue 1.0 : ArXiv:1303.0029
Issue 2.0 : This Fall
ELT-MOS White Paper
Next step is to prioritise TLR
and iterate with technical &
operational feasibility
SIMULATIONS
ELT-MOS White Paper
Next step is to prioritise TLR
and iterate with technical &
operational feasibility
SIMULATIONS
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
Simulated Science Case :
Galaxy mass assembly
MOAO
Spatially-resolved
spectroscopy of z~2-6
galaxies is required for
distinguishing merger from
rotation (Puech+10)
GLAO
GLAO is unable to recover the
dynamical nature
of z>2 distant galaxies
(with ≲ 50 % of the Cn2
in the GL)
Shaping E-ELT Science and Instrumentation
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
MOAO / 75mas/pix / R=5000 : no need for very high resolution !
Rotating disk
Major merger
Puech+08
Simulated Science Case :
First light galaxies & Reionisation
First light galaxies & Reionisation
Simulated SC : first light galaxies &
reionisation
Simulated IFU observations of Ly-a emission lines at z~9 (LAEs) :
Spatial template
Kinematics
Simulation of z~0 clumpy disks
(Bournaud+07) rescaled in flux
and size to z~9
using current HST
observations
(eg, Grazian+12)
VLya= 200 km/s
(constant outflow ; Swinbank+07)
0.1-0.2’’
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)
Optimal
integrated
Spectra
(RosalesOrtega et al.
2012)
JAB=30
Rhalf=100mas
« Faint &
compact » at
z~9
Very deep obs. :
Exp. Time=40 hr
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=30
JAB=29
S/N-Optimal sampling : 40-120 mas
S∕N=5 in Ly-a for Dpix=40/60/80/100/120 mas
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)
Optimal
integrated
Spectra
(RosalesOrtega et al.
2012)
JAB=26
Rhalf=150mas
Averaged size &
flux at z~7
Exp. Time=40 hr
Optimal
integrated
Spectra
(RosalesOrtega et al.
2012)
JAB=27
Rhalf=100mas
« Faint &
compact » at
z~7
Exp. Time=40 hr
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
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
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
Simulated SC : galaxy mass
assembly
MOAO z=4
50mas/pix
R=5000
GLAO z=4
(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)