1. Date 31-08-2011, Ischia (NA) CMDs in the E-ELT Era Giuliana Fiorentino, INAF-OABo A. Deep, E. Tolstoy, E. Diolaiti, M. Bellazzini, P. Ciliegi, R.I. Davies & J.-M. Conan

2. Date 31-08-2011, Ischia (NA) OUTLINE Science cases on resolved stellar populations with E-ELT The E-ELT future: maory + MICADO Our systematic approach: simulations Results and conclusions Clues on the cosmic distance scale

3. Date 31-08-2011, Ischia (NA) HST-view Effect of distance on the resolution of individual stars µ=28.54µ=18.47 µ=31.3

4. Date 31-08-2011, Ischia (NA) HST-view CMDs from HST/WFPC2. Distances: 50Kpc (LMC), 5.1 Mpc (NGC1705) and 18Mpc (IZw18), from Cignoni & Tosi 2010. Effect of distance on the resolution of individual stars

5. Date 31-08-2011, Ischia (NA) HST-view CMDs from HST/ACS. Distance: ~800 Kpc. M31 from Brown et al 2006, M32 from Fiorentino et al. 2011 (submitted) Effect of crowding on the resolution of individual stars M32 fieldM31 field RR Lyrae

6. Date 31-08-2011, Ischia (NA) Open Questions for the E-ELT from http://www.eso.org/sci/facilities/eelt/docs/E-ELTScienceCase_Lowres.pdfhttp://www.eso.org/sci/facilities/eelt/docs/E-ELTScienceCase_Lowres.pdf Galaxy formation and evolution (M. Zoccali’s and G. Bono’s talk) Star formation throughout the Universe (see C. Gallart and L. Greggio’s talk) The Initial Mass function in a range of environments Cosmic distance scale in the GAIA era

7. Date 31-08-2011, Ischia (NA) Cepheids with HST Measurement of H 0 ULP Cepheids with HST Freedman et al. 2002

8. Date 31-08-2011, Ischia (NA) ★ Cepheids: 62.3±1.3(ran)±5 (sys)Km s -1 Mpc -1, Sandage et al. 2006, (G. Tammann, conference in Naples) ★ TRGB: 73 ± 5 Km s -1 Mpc -1, Mould & Sakai (2008) ★ WMAP+SDSS+SNIa(5 years): 65.6± 2.5 Km s -1 Mpc -1 (Reid et al.2010) ★ WMAP(5/7years): 70.4±1.4 Km s -1 Mpc -1, Komatsu et al. (2010) ★ Cepheids: 73.8 ± 2.4 Km s -1 Mpc -1, Riess et al. (2011) (W. Freedmann, conference in Naples) Summarizing the H 0 measurement

9. Date 31-08-2011, Ischia (NA) simulations of the E-ELT with MAORY+MICADO Deep et al. 2011, published on A&A

10. Date 31-08-2011, Ischia (NA) MAORY Maory consortium: INAF-OABo; ONERA; UNIBO; OAPD; IASFBO; OAA; ESO. People: Diolaiti, EmilianoDiolaiti, Emiliano; Conan, Jean-Marc; Foppiani, Italo; Marchetti, Enrico; Baruffolo, Andrea; Bellazzini, Michele; Bregoli, Giovanni; Butler, Christopher R.; Ciliegi, Paolo; Cosentino, Giuseppe; Delabre, Bernard; Lombini, Matteo; Petit, Cyril; Robert, Clélia; Rossettini, Pierfrancesco; Schreiber, Laura; Tomelleri, Raffaele; Biliotti, Valdemaro; D'Odorico, Sandro; Fusco, Thierry; Hubin, Norbert; Meimon, Serge;Foppiani, Italo; Baruffolo, An Michele; Bregoli Christopher R.; entino, Giuseppe; Dini, Matteo; Petilélia; Rossettini, Pieaura; Tomelleriotti, Valdemaro; Dco, Thierry; Hubn, Serge; MAORY uses several deformable mirrors and several (Laser + Natural) guide stars UNIFORM performance on an extended field of views. This technique was successfully demonstrated on-sky by the Multi conjugate Adaptive optics Demonstrator (MAD) on the Very Large Telescope (G. Bono’s talk).Multi conjugate Adaptive optics Demonstrator (MAD) Multi-conjugate Adaptive Optics Relay for E-ELT, Diolaiti et al. 2009 for details see P. Ciliegi’s talk (Tomorrow)

11. Date 31-08-2011, Ischia (NA) MAORY http://www.bo.astro.it/maory/Maory/PSF_03_2010.html for details see P. Ciliegi’s talk (Tomorrow)

12. Date 31-08-2011, Ischia (NA) MICADO MICADO consortium: MPE, MPIA, USM, NOVA, OAPD, LESIA People: Davies, RichardDavies, Richard; Ageorges, N.; Barl, L.; Bedin, L. R.; Bender, R.; Bernardi, P.; Chapron, F.; Clenet, Y.; Deep, A.; Deul, E.; Drost, M.; Eisenhauer, F.; Falomo, R.; Fiorentino, G.; Förster Schreiber, N. M.; Gendron, E.; Genzel, R.; Gratadour, D.; Greggio, L.; Grupp, F.; Held, E.; Herbst, T.; Hess, H.-J.; Hubert, Z.; Jahnke, K.; Kuijken, K.; Lutz, D.; Magrin, D.; Muschielok, B.; Navarro, R.; Noyola, E.; Paumard, T.; Piotto, G.; Ragazzoni, R.; Renzini, A.; Rousset, G.; Rix, H.-W.; Saglia, R.; Tacconi, L.; Thiel, M.; Tolstoy, E.; Trippe, S.; Tromp, N.; Valentijn, E. A.; Verdoes Kleijn, G.; Wegner, M.arl, L.; Bedder, R.; P.; ChapronY.; Deep, ; Drost, M.;.; Falomo, o, G.; Förer, N. M, E.; GeGratadourio, L.; Grupp,erbst, T.; Hubert, Z.; ken, K.; Lutz, D.; Magriarro, R.; Numard, T.; Ragazzoni, R Rousset, G; Saglia,i, L.; TTolstoy, E.; Tromp, N E. A.; Ve, G.; Wegn MICADO srequiring an image correction of high quality and uniformity across a field of view of 53"x53" on the covered wavelength range. Multi-AO Camera for Deep Observations (Davies et al 2009)

13. Date 31-08-2011, Ischia (NA) Simulations 1) Resampling the UPDATED PSFs for each filter to the MICADO pixel scale (released on march 2010) 2) Seeing conditions = 0.6” and corresponding Strehl Ratio and Encircled Energy I-band Deep et al. 2011, A&A

14. Date 31-08-2011, Ischia (NA) Simulations 3) Limiting magnitude for S/N ~4 corresponds to σ ~ 0.25 using σ=-2.5 log(1+N/S) 4) An old Stellar Population. with IAC-star (C. Gallart’s talk) using BASTI evolutionary tracks I~29.5 J~28.0 H~26.8 K s ~26.2 Deep et al. 2011, A&A

15. Date 31-08-2011, Ischia (NA) Simulations 5) IRAF- noao.mkobject task texp = 1 hour filters: I J H Ks µ V = 21, 20, 19, 18, 17 mag/arcsec 2 FoV = 3 x 3 arcsec 2 or 250x250 pixels. d=18Mpc or µ 0 =31.3 Stars uniformly and randomly distributed. Random selection of stars from Isochrones. Deep et al. 2011, A&A

16. Date 31-08-2011, Ischia (NA) some examples...

17. Date 31-08-2011, Ischia (NA) some examples...

18. Date 31-08-2011, Ischia (NA) some examples...

19. Date 31-08-2011, Ischia (NA) Photometry starfinder extracted PSFmaory PSF The analysis was made with Starfinder and Daophot. Main difference= how the PSF is treated Starfinder= purely numerical PSF Daophot= model the PSF with an analytical model + a look-up table that account for possible deviation from the model. Deep et al. 2011, A&A

20. Date 31-08-2011, Ischia (NA) CMDs in I, I-Ks Deep et al. 2011, A&A

21. Date 31-08-2011, Ischia (NA) CMDs in I, I-H H band looks more promising than K s Deep et al. 2011, A&A

22. Date 31-08-2011, Ischia (NA) Completeness... Deep et al. 2011, A&A

23. Date 31-08-2011, Ischia (NA)...errors μ V = 21 mag / arcsec 2 (distance of ~80” from the center of a typical giant elliptical galaxy) we get I ∼ 29.3, J ∼ 28.2, H ∼ 26.5 and Ks ∼ 26.2 with a photometric accuracy of ± 0.25 mag. μ V = 19 mag / arcsec 2 (distance of ~25”) we get I ∼ 28.2, J ∼ 27.2, H ∼ 25.7 and Ks ∼ 25.4 with the same photometric accuracy. μ V = 17 mag / arcsec 2 (distance of ~5”) we get I ∼ 27.2, J ∼ 26.2, H ∼ 25.0 and Ks ∼ 24.6 or brighter, with the same photometric errors (BUT careful to the Blending Effect!!). Deep et al. 2011, A&A

24. Date 31-08-2011, Ischia (NA)...summarizing ELT compared with JWST... Deep et al. 2011, A&A

25. Date 31-08-2011, Ischia (NA) Cepheids with HST finally coming back to H 0 E-ELT GAIA: direct calibration of LMC ULPs with parallaxes at µarcsec accuracy!

26. Date 31-08-2011, Ischia (NA) Conclusions The photometry of MAORY+MICADO-like images is feasible with the actual photometric packages The filter combination I, I-H seems to be the more promising in the field of the stellar population studies E-ELT will allow us to resolve galaxy in stars at Surface Brightness value not accessible to any other facilities E-ELT will allow to use a single distance indicators to measure the H 0 In Future we will simulate more realistic images (adding several images) to increase the S/N ratio and we will simulate the specific scientific case of a Blue Compact Dwarf galaxy, to see if we will be able to see the oldest population of these galaxies.

27. Date 31-08-2011, Ischia (NA) looking for 2021... THANKS, everyone Metropolitan Museum of art, NY city