1. Towards the science case for E-ELT HIRES – Cambridge, Sept 13-14, 2012 E-ELT HIRES SCIENCE CASES: STELLAR SPECTROSCOPY and YOUNG STARS PMS 8-10m class telescopes massive stars, luminous giants/SGs in the Galaxy & LG E-ELT low luminosity stars in the Galaxy luminous stars in the LG and beyond optical+near IR high res stellar spectroscopy Livia Origlia – INAF Bologna, Italy

2. Towards the science case for E-ELT HIRES – Cambridge, Sept 13-14, 2012 E-ELT HIRES SCIENCE CASES: STELLAR SPECTROSCOPY and YOUNG STARS stellar populations (Tolstoy & de Laverny talks) chemical evolution & stellar archaeology stellar physics, evolution & nucleosynthesis young stars (Testi/Nisini) proto-star & star-disk interaction  planet formation distant star clusters (Larsen talk) chemical composition & dynamical mass constraints on the IMF & the host galaxy optical + near IR high res stellar spectroscopy @ E-ELT Livia Origlia – INAF Bologna, Italy

3. Towards the science case for E-ELT HIRES – Cambridge, Sept 13-14, 2012 E-ELT HIRES SCIENCE CASES: STELLAR SPECTROSCOPY and YOUNG STARS optical + near IR high res stellar spectroscopy @ E-ELT very precise chemical abundances (Gustafsson & Korn talk) very precise stellar parameters (Ammler-von Eiff, Tautenburg) isotopic abundances (Israelian talk + granulation in stars with transiting planets (Dravins – Lund) asteroseismology in M dwarfs (Gonzalez & Rodriguez-Lopez - Granada) - = 12 C 18 O, 12 C 17 O 2.349-2.352  m R>=100k) pulsations will help determining the frontier between partially- and fully-convective structure in M dwarfs (SpT M3.5 ?) pulsations will help determining the frontier between partially- and fully-convective structure in M dwarfs (SpT M3.5 ?) high resolution line profiles across spatially resolved stellar disks ! high resolution line profiles across spatially resolved stellar disks ! Livia Origlia – INAF Bologna, Italy very high s/n …

4. Towards the science case for E-ELT HIRES – Cambridge, Sept 13-14, 2012 E-ELT HIRES SCIENCE CASES: STELLAR SPECTROSCOPY and YOUNG STARS top level requirements spectral sampling: > 2 pix RV accuracy: m/s (stellar oscillations) spectral resolution: R~20k  R~100K  1medium, 1high observing modes/feeding: mostly point sources  fibers desirable for highly accurate measures (e.g. RV, line profiles etc.)  some MOS capability desirable for stellar pop studies  desirable spatially resolved slit/IFU for CS disks/jets spectral range: 0.31  0.38 - 2.4 micron Be 3130 AA R>50,000 OH UV lines NH 3360 AA Balmer jump ~3600 AA U II 3859 AA CN 3883 AA HF 2.336  m R>50,000 12 C 18 O, 12 C 17 O 2.349-2.352  m R>=100,000 Livia Origlia – INAF Bologna, Italy

5. Calibration: blaze effects very high resolution: 300k