Post on 18-Dec-2015
ELT-MOS Requirements
Workshop in AmsterdamWorkshop in Amsterdam
Assembled a science team
Assembled a science team
New science simulationsNew science simulations
ELT-MOS White PaperELT-MOS White Paper
Meetings in UK, Italy, Brazil, NL
Meetings in UK, Italy, Brazil, NL
SPIE 2012 in AmsterdamSPIE 2012 in Amsterdam
Proc. SPIE ArXiv:1207.0768
Issue 1.0 : ArXiv:1303.0029Issue 2.0 : This Fall
ELT-MOS White Paper
Next stage:
Prioritise TLR via trade-offsIterate with technical & operational
feasibility
TLR for MOSAIC (see F. Hammer’s talk)
Next stage:
Prioritise TLR via trade-offsIterate with technical & operational
feasibility
TLR for MOSAIC (see F. Hammer’s talk)
First galaxies & reionisation
OH
OH
OH
OH
Sky continuum is ~ 19.5-20 arcsec-2 in J/HAB (Sullivan+12)Sky continuum is ~ 19.5-20 arcsec-2 in J/HAB (Sullivan+12)
Spectroscopy down to J/HAB~27-28 in absorption (see K. Disseau’s talk)
Spectroscopy down to J/HAB~27-28 in absorption (see K. Disseau’s talk)
TLR on the sky subtraction :
Systematics ≲ 0.1 %
TLR on the sky subtraction :
Systematics ≲ 0.1 %
Yang et al. 2013
Cross beam switching observations
FLAMES-GIRAFFE tech. time
Demonstrated on sky
with FLAMES
Demonstrated on sky
with FLAMES
Accurate sky subtraction
Yang et al. 2013
Foreseen achievable accuracy: ~ 0.1%-Optimize design & operations
-Specific algorithm (PCA, Sharp+10)
Better performances expected for IFUs
Foreseen achievable accuracy: ~ 0.1%-Optimize design & operations
-Specific algorithm (PCA, Sharp+10)
Better performances expected for IFUs
Accuracy to be limited by
scattered light (like with slits)
Accuracy to be limited by
scattered light (like with slits)
Physical limit of the sky subtraction =
spatial variations of the sky continuum
Physical limit of the sky subtraction =
spatial variations of the sky continuum
Cross beam switching observation to be implemented on MOONS (VLT 3rd generation)
Cross beam switching observation to be implemented on MOONS (VLT 3rd generation)
Probing the mass assembly of galaxies
80
kpc
J≤26
J≤27
HDM: spatially-resolved properties of massive
galaxies
HDM: spatially-resolved properties of massive
galaxies
HMM: integrated properties of smaller-
mass galaxies
HMM: integrated properties of smaller-
mass galaxies
Dynamics of the inner halos & evolution of the faint-end slope of the LF
Dynamics of the inner halos & evolution of the faint-end slope of the LF
Accepted proposal @ VLT/VIMOS
Accepted proposal @ VLT/VIMOS
Newman et al. (2012)
A survey workhorse
VLT+AO(F) & ELT-IFU /
HARMONI as 1st light
instrument
will focus on the small-
scale galaxy physics
VLT+AO(F) & ELT-IFU /
HARMONI as 1st light
instrument
will focus on the small-
scale galaxy physics
ELT-MOS to be optimized for survey speed
Best trade-off between resolution & SB sensitivity
ELT-MOS to be optimized for survey speed
Best trade-off between resolution & SB sensitivity
Newman+13
Optimizing the pixel scale
Rotating disk
Major m
erger
TLR:≥10 MOAO-fed IFUs with ~75mas/pixel (~ 10 D.L.)TLR:≥10 MOAO-fed IFUs with ~75mas/pixel (~ 10 D.L.)
Puech+08
~2x10-20 erg/s/cm²
Puech et al. (2010)
z=4