1. 1 Palermo 20-22 nd May Looking ahead to MOONS William Taylor on behalf of the MOONS consortium

2. 2 Palermo 20-22 nd May MOONS: Multi Object Optical and Near infra-red Spectrograph Selected by ESO as third generation instrument for the VLT Operational by 2019 PI: Michele Cirasuolo Consortium UK France Italy Switzerland Portugal Chile Primary science cases: Galactic Archeology Galaxy Evolution

3. 3 Palermo 20-22 nd May Instrument specifics ParameterSpecification Field of view25’ diameter (same as FLAMES) Number of fibres~1000 Wavelength range0.8 – 1.8 μm Throughput> 30% Fibre diameter1.05 arcsec Resolution modesJust “Low” and “High” Field reconfiguration time< 5 mins

4. 4 Palermo 20-22 nd May MOONS current spectrograph baseline 4 0.65 – 0.95 μm R ~ 3500

5. 5 Palermo 20-22 nd May Fibre positioners

6. 6 Palermo 20-22 nd May Sky troubles Require R > 4000 to get continuum between the sky lines Rodrigues et al., 2012, SPIE Sky subtraction tests with FLAMES Proposed A-B-B-A observing strategy Molecfit – Telluric absorption models Smette et al., 2014

7. 7 Palermo 20-22 nd May Galactic science case Coordinators (past and present): Livia Origlia, Carine Babusiaux, Chris Evans, Lex Kaper Loosely split into: The bulge The inner disc Stellar clusters Halo of globular clusters The Magellanic systems Dwarf galaxies in the local group? Tidal streams in the MW? and more…

8. 8 Palermo 20-22 nd May Wavelength selection IR to give: penetrating power for cool stars fewer absorption bands, easier to determine continuum (arguably) potential to build-on (and learn from) APOGEE survey Low-res mode: Calcium Triplet commonly used for metallicity estimates R>a-few-thousand, RSG abundance determination High-res mode: To determine different evolutionary processes need to sample certain species Include a few DIBs Windows also chosen to avoid strong telluric absorption

9. 9 Palermo 20-22 nd May Galactic centre H < 15.5 at R~20,000 with a S/N ~ 30 in 1hr Absorption (Av=0.7mag/kpc; Besancon model)

10. 10 Palermo 20-22 nd May V< 20 ( as selected by Gaia) V<16 (4m opt. telesc. R~20,000) H<15.5 (MOONS R~20,000) GAIA follow up MOONS can access all the GAIA targets in the CaT window

11. 11 Palermo 20-22 nd May Data sets GAIA, VISTA, UKIDSS, VPHAS, in the future LSST (?) etc. From VISTA: VISTA Variables in the Vía Láctea (VVV ) VISTA Magellanic Clouds (VMC)

12. 12 Palermo 20-22 nd May Clusters To observe parameters such as: everything discussed in the last 48 hours! Can do this in both: Embedded clusters Obscured clusters Basically: a larger, possibly broader data set

13. 13 Palermo 20-22 nd May VVV ‘new’ clusters Borissova et al., 2011, A&A Considerations: Small spatial scales Cluster membership Target numbers Target density

14. 14 Palermo 20-22 nd May S/LMC… Study kinematics and chemical abundances of both Clouds to learn about their interaction and the impact on their evolution Low metallicity clusters …and beyond Use RSG as abundance tracers in nearby local group galaxies

15. 15 Palermo 20-22 nd May And finally… And finally… possible surveys And finally… Inner Galaxy survey to obtain complete kinematic and chemical screening of the old stellar populations of the inner disc and bulge regions. 1-2 hrs per pointing at R=20,000 in the J- and H-bands (i.e. down to H<15.5 mag) + CaT at R=8,000 for free: - 50 nights, spectra for ~250,000 stars Wide-area Gaia survey to follow-up stars observed with Gaia in Thin and Thick disc, tidal streams, the field populations around halo and clusters. 0.5-1hr integration obtain CaT at R=8,000 and simultaneously near-IR low-resolution spectra in J & H-band (i.e. I<21) : - 50 nights, spectra for ~500,000 stars Thanks!