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Looking ahead to MOONS

Looking ahead to MOONS. William Taylor on behalf of the MOONS consortium. 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

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Looking ahead to MOONS

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  1. Looking ahead to MOONS William Taylor on behalf of the MOONS consortium

  2. 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. Instrument specifics

  4. MOONS current spectrograph baseline 0.65 – 0.95 μm R ~ 3500

  5. Fibre positioners

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

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

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

  11. 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. 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. VVV ‘new’ clusters Borissova et al., 2011, A&A Considerations: • Small spatial scales • Cluster membership • Target numbers • Target density

  14. 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. And finally… possible surveys And finally… 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!

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