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CMDs in the E-ELT Era

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. Date 31-08-2011, Ischia (NA). Science cases on resolved stellar populations with E-ELT The E-ELT future: maory + MICADO

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CMDs in the E-ELT Era

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  1. 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 Date 31-08-2011, Ischia (NA)

  2. 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 OUTLINE Date 31-08-2011, Ischia (NA)

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

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

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

  6. 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 Open Questions for the E-ELTfrom http://www.eso.org/sci/facilities/eelt/docs/E-ELTScienceCase_Lowres.pdf Cosmic distance scale in the GAIA era Date 31-08-2011, Ischia (NA)

  7. Measurement of H0 Cepheids with HST ULP Cepheids with HST Freedman et al. 2002 Date 31-08-2011, Ischia (NA)

  8. Summarizing the H0 measurement • Cepheids:62.3±1.3(ran)±5 (sys)Km s-1Mpc-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) Date 31-08-2011, Ischia (NA)

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

  10. for details see P. Ciliegi’s talk (Tomorrow) Multi-conjugate Adaptive Optics Relay for E-ELT, Diolaiti et al. 2009 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). MAORY Maory consortium: INAF-OABo; ONERA; UNIBO; OAPD; IASFBO; OAA; ESO. People: Diolaiti, 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; Date 31-08-2011, Ischia (NA)

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

  12. Multi-AO Camera for Deep Observations (Davies et al 2009) MICADO srequiring an image correction of high quality and uniformity across a field of view of 53"x53" on the covered wavelength range. MICADO MICADO consortium: MPE, MPIA, USM, NOVA, OAPD, LESIA People: Davies, 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. Date 31-08-2011, Ischia (NA)

  13. I-band 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 Simulations Deep et al. 2011, A&A Date 31-08-2011, Ischia (NA)

  14. I~29.5 J~28.0 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 H~26.8 Ks~26.2 Simulations Deep et al. 2011, A&A Date 31-08-2011, Ischia (NA)

  15. 5) IRAF- noao.mkobject task texp = 1 hour filters: I J H Ks µV= 21, 20, 19, 18, 17 mag/arcsec2 FoV = 3 x 3 arcsec2 or 250x250 pixels. d=18Mpc or µ0=31.3 Stars uniformly and randomly distributed. Random selection of stars from Isochrones. Simulations Deep et al. 2011, A&A Date 31-08-2011, Ischia (NA)

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

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

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

  19. Photometry 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. starfinder extracted PSF maory PSF Deep et al. 2011, A&A Date 31-08-2011, Ischia (NA)

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

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

  22. μV= 21 mag/arcsec2 (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. μV= 19 mag/arcsec2 (distance of ~25”) we get I∼28.2, J∼27.2, H∼25.7 and Ks ∼25.4 with the same photometric accuracy. μV= 17 mag/arcsec2 (distance of ~5”) we get I∼27.2, J∼26.2, H∼25.0 and Ks ∼24.6or brighter, with the same photometric errors (BUT careful to the Blending Effect!!). ...errors Deep et al. 2011, A&A Date 31-08-2011, Ischia (NA)

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

  24. finally coming back to H0 GAIA: direct calibration of LMC ULPs with parallaxes at µarcsec accuracy! Cepheids with HST E-ELT Date 31-08-2011, Ischia (NA)

  25. 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 H0 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. Date 31-08-2011, Ischia (NA)

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

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