1. Atmospheres: Empirical or Theoretical ? (some selected) Observed Spectral Libraries GUNN, J.E.; STRYKER, L.L. 1983 (3130 to 10800 Å) JACOBY, G.H., HUNTER, D.A., CHRISTIAN, C.A., 1984 (3130 to 7000Å at 4Å ) PICKLES, A. J., 1998 (1150-25000 Å at 5 Å ) PRUGNIEL, P., SOUBIRA, C., 2002 (ELODIE 4100-6800 Å) VALDES ET AL., 2004 (INDO-US 3460-9464 at 4Å) LE BORGNE ET AL. 2003 (STELIB 3200 to 9500Å at 3Å) SANCHEZ-BLAZQUEZ ET AL. 2006 (MILES 3525-7500Å at 2.3 Å )

2. SANCHEZ-BLAZQUEZ ET AL. 2006 M10 M4

3. Theoretical: ATLAS code http://kurucz.harvard.edu/ Robert L. Kurucz Castelli, F. INAF OATS Bonifacio, P. INAF OATS Bertone, E. INAOE, Pue, Mex Chavez, M. INAOE, Pue, Mex Rodriguez, L. INAOE, Pue, Mex Buser, R.AIU, Basel, Switz. Cuisinier, F. Dpt. Astr. Rio de Janeiro, Brasil Lejeune, T.OA Univ. Coimbra, Portugal

4. Theoretical: NextGen Hauschildt, Allard & Baron http://www.hs.uni-hamburg.de/EN/For/ThA/phoenix/index.html 1D plane parallel or spherical symmetric radiative transfer multilevel NLTE calculations for atoms with a total of more than 10000 levels and 100000 primary lines line blanketing and background opacities are included by design over 650 species in the EOS including atoms, ions, molecules and grains depth dependent Voigt profiles for Stark and van der Waals broadening dynamical opacity sampling (dOS) of about 42 Million atomic lines and over 550 Million (and growing) molecular lines (more than 10GB worth of data) spectra can be calculated for any desired resolution (standard are 20000 to 500000 wavelength points spread from the UV to the radio)

5. Solar Model From Hauschildt et al

6. Teff vs. gravity model distribution Log T(eff) vs. log g model distribution Luminosity class: MK V = small solid dots MK IV = big solid dots MK III = small open dots MK II--I = big open dots Evolutionary tracks M = 1, 2, 5, 10 Mo (from Girardi et al. 00) Bertone et al 05

7. HD 154760, G2V (Gunn & Stryker 83) best fit ATLAS model ( Bertone, E et al. 04)

8. Accuracy of Teffs, g ATLAS vs. NextGen Star BD+38 2457: standard deviation of flux residuals for fitting models; dotted line for log g = 0, dash-dotted log g(NG) = 5.5 log g(ATLAS) = 5.0 T(eff) = 4850 ± 70 K, log g = 5.5 ± 0.5 dex s(min) = 0.12 NextGen T(eff) = 4520 ± 30 K, log g = 4.0 ± 0.5 dex s(min) = 0.06 ATLAS Bertone et al 05

9. s min distribution vs. spectral type Gunn & Stryker (1983) Jacoby et al. (1984) o ATLAS NextGen Bertone et al 05

10. Teff scale Gunn & Stryker (1983) Jacoby et al. (1984) Bertone et al 05

11. Bolometric corrections Empirical calibrations: Flower (1977) dotted line for MS stars dashed for giants Johnson (1966) solid) Bessell (1991) dashed-dotted) Code et al. (1976) crosses

12. M Giant Stars Database of M giants (97 MIII stars spectra from 3800-9000 A) Pletz et al. Atmospheric models –match with optical spectra used to determine Teff In general poor U-B-V fluxes –e.g. strange B-V or V-K colours Combine observed (3800-9000) with synthetic best match models to obtain a wide wavelength coverage Apply scale corrections to reproduce observed average colour- colour relations Models by Fluks et al (1994)

13. Theoretical: MARCS stellar model-atmosphere and flux library This is a grid of one-dimensional, plane-parallel and spherical LTE model atmospheres and sampled fluxes. The library supplies model-atmosphere tables and sampled energy fluxes for about 9000 stellar models with Teff between 4000 and 8000K (step 250K) Log g between -1.0 to 5.0 (step 0.5) Metallicities between -5.0 and 1.0 Plane-parallel models are calculated for log g from +3.0 to +5.0 Models with spherical geometry are supplied for log g < +4.0, masses of 0.5, 1.0, 2.0 and 5.0 M Sun, http://marcs.astro.uu.se/ Gustafsson B., Edvardsson B., Eriksson K., Jørgensen U.G., Nordlund Å, Plez B., 06 B. Gustafsson, R. A. Bell, K. Eriksson, and A. Nordlund, 75 Photospheric surface fluxes from 1300Å to 20μm sampled with λ/Δλ = 20,000

14. M-Giant Scales

15. Bessel Castelli Plez, 98

16. Observed vs Theretical Colours

17. My own method: from Fluks et al. 1994

19. M Giant Spectra

20. http://www.iaa.csic.es/~rosa/research/synthesis/HRES/ESPS-HRES.html A High-Resolution Stellar Library for Evolutionary Population Synthesis. Other Theoretical Libraries 2500-10500 Ang Library of Synthetic Spectra Munari, Sordo, Castelli, Zwitter, 2006 Martins, González Delgado, Leitherer, Cerviño, Hauschildt 2005 http://web.pd.astro.it/adsd/index.html