The ELT-MOS (MOSAIC) White Paper

Mathieu Puech

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

ELT-MOS White Paper

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)

ELT-MOS White Paper

SC1: First galaxies & Reionisation

First galaxies & Reionisation

See JG Cuby’s

talk

10s (in absorption) to

100s (in emission) of sources expected

in the E-ELT FoV

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

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)

SC2 & SC3: mass assembly of galaxies

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

Conclusions

●MOS essential for a number of prominent E-ELT SCs

●TLR summarized in a ELT-MOS white paper

●Two complementary modes: HDM + HMM

●ELT-MOS should be optimized for survey speed: simulations suggest ~ 80 mas/pixel (TBC)

●Second issue of the White Paper by the end of 2013