Slide 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 Slide 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 Slide 3 Date 31-08-2011, Ischia (NA) HST-view Effect of distance on the resolution of individual stars =28.54=18.47 =31.3 Slide 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 Slide 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 Slide 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. Zoccalis and G. Bonos talk) Star formation throughout the Universe (see C. Gallart and L. Greggios talk) The Initial Mass function in a range of environments Cosmic distance scale in the GAIA era Slide 7 Date 31-08-2011, Ischia (NA) Cepheids with HST Measurement of H 0 ULP Cepheids with HST Freedman et al. 2002 Slide 8 Date 31-08-2011, Ischia (NA) Cepheids: 62.31.3(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): 70.41.4 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 Slide 9 Date 31-08-2011, Ischia (NA) simulations of the E-ELT with MAORY+MICADO Deep et al. 2011, published on A&A Slide 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, Cllia; 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; Petillia; 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. Bonos talk).Multi conjugate Adaptive optics Demonstrator (MAD) Multi-conjugate Adaptive Optics Relay for E-ELT, Diolaiti et al. 2009 for details see P. Ciliegis talk (Tomorrow) Slide 11 Date 31-08-2011, Ischia (NA) MAORY http://www.bo.astro.it/maory/Maory/PSF_03_2010.html for details see P. Ciliegis talk (Tomorrow) Slide 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.; Frster 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.; Frer, 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) Slide 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 Slide 14 Date 31-08-2011, Ischia (NA) Simulations 3) Limiting magnitude for S/N ~4 corresponds to ~ 0.25 using =-2.5 log(1+N/S) 4) An old Stellar Population. with IAC-star (C. Gallarts talk) using BASTI evolutionary tracks I~29.5 J~28.0 H~26.8 K s ~26.2 Deep et al. 2011, A&A Slide 15 Date 31-08-2011, Ischia (NA) Simulations 5) IRAF- noao.mkobject task texp = 1 hour filters: I J H Ks V = 21, 20, 19, 18, 17 mag/arcsec 2 FoV = 3 x 3 arcsec 2 or 250x250 pixels. d=18Mpc or 0 =31.3 Stars uniformly and randomly distributed. Random selection of stars from Isochrones. Deep et al. 2011, A&A Slide 16 Date 31-08-2011, Ischia (NA) some examples... Slide 17 Date 31-08-2011, Ischia (NA) some examples... Slide 18 Date 31-08-2011, Ischia (NA) some examples... Slide 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 Slide 20 Date 31-08-2011, Ischia (NA) CMDs in I, I-Ks Deep et al. 2011, A&A Slide 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 Slide 22 Date 31-08-2011, Ischia (NA) Completeness... Deep et al. 2011, A&A Slide 23 Date 31-08-2011, Ischia (NA)...errors 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. 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. 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 Slide 24 Date 31-08-2011, Ischia (NA)...summarizing ELT compared with JWST... Deep et al. 2011, A&A Slide 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 arcsec accuracy! Slide 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. Slide 27 Date 31-08-2011, Ischia (NA) looking for 2021... THANKS, everyone Metropolitan Museum of art, NY city