1. The ELT-MOS (MOSAIC) White Paper Mathieu Puech

2. ELT-MOS Requirements Workshop in Amsterdam Assembled a science team New science simulations ELT-MOS White Paper Meetings in UK, Italy, Brazil, NL SPIE 2012 in Amsterdam Proc. SPIE ArXiv:1207.0768 Issue 1.0 : ArXiv:1303.0029 Issue 2.0 : This Fall

3. ELT-MOS White Paper

5. Next stage: Prioritise TLR via trade-offs Iterate with technical & operational feasibility  TLR for MOSAIC (see F. Hammer’s talk) Next stage: Prioritise TLR via trade-offs Iterate with technical & operational feasibility  TLR for MOSAIC (see F. Hammer’s talk)

6. ELT-MOS White Paper

7. SC1: First galaxies & Reionisation

8. First galaxies & Reionisation See JG Cuby’s talk

9. 10s (in absorption) to 100s (in emission) of sources expected in the E-ELT FoV

10. First galaxies & reionisation OH Sky continuum is ~ 19.5-20 arcsec -2 in J/H AB (Sullivan+12) Spectroscopy down to J/H AB ~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 %

11. Yang et al. 2013 Cross beam switching observations FLAMES-GIRAFFE tech. time

12. Yang et al. 2013 Cross beam switching observations FLAMES-GIRAFFE tech. time Demonstrated on sky with FLAMES Demonstrated on sky with FLAMES

13. 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) Physical limit of the sky subtraction = spatial variations of the sky continuum Cross beam switching observation to be implemented on MOONS (VLT 3rd generation)

14. SC2 & SC3: mass assembly of galaxies

16. Probing the mass assembly of galaxies 80 kpc J≤26 J≤27 HDM: spatially-resolved properties of massive galaxies HMM: integrated properties of smaller-mass galaxies Dynamics of the inner halos & evolution of the faint-end slope of the LF Accepted proposal @ VLT/VIMOS

17. 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

18. Optimizing the pixel scale Rotating disk Major merger TLR:≥10 MOAO-fed IFUs with ~75mas/pixel (~ 10 D.L.) Puech+08 ~2x10 -20 erg/s/cm² Puech et al. (2010) z=4

19. 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