cmds in the e-elt era
DESCRIPTION
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 - PowerPoint PPT PresentationTRANSCRIPT
Date 31-08-2011, Ischia (NA)
CMDs in the E-ELT EraGiuliana 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)
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
Date 31-08-2011, Ischia (NA)
HST-viewEffect of distance on the resolution of individual stars
µ=28.54µ=18.47
µ=31.3
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
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
Date 31-08-2011, Ischia (NA)
Open Questions for the E-ELTfrom
http://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
Date 31-08-2011, Ischia (NA)
Cepheids with HST
Measurement of H0
ULP Cepheids with HST
Freedman et al. 2002
Date 31-08-2011, Ischia (NA)
★ 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)
Summarizing the H0 measurement
Date 31-08-2011, Ischia (NA)
simulations of the E-ELT with MAORY+MICADO
Deep et al. 2011, published on A&A
Date 31-08-2011, Ischia (NA)
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;
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 Relay for E-ELT, Diolaiti et al. 2009
for details see P. Ciliegi’s talk (Tomorrow)
Date 31-08-2011, Ischia (NA)
MAORY
http://www.bo.astro.it/maory/Maory/PSF_03_2010.htmlfor details see P. Ciliegi’s talk
(Tomorrow)
Date 31-08-2011, Ischia (NA)
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.
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)
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 andEncircled Energy
I-band
Deep et al. 2011, A&A
Date 31-08-2011, Ischia (NA)
Simulations
3) Limiting magnitude for S/N ~4 corresponds to σ ~ 0.25using σ=-2.5 log(1+N/S)
4) An old Stellar Population. with IAC-star (C. Gallart’s talk) using BASTI evolutionary tracks
I~29.5J~28.0
H~26.8
Ks~26.2
Deep et al. 2011, A&A
Date 31-08-2011, Ischia (NA)
Simulations
5) IRAF- noao.mkobject task
texp = 1 hourfilters: I J H KsµV= 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.
Deep et al. 2011, A&A
Date 31-08-2011, Ischia (NA)
some examples...
Date 31-08-2011, Ischia (NA)
some examples...
Date 31-08-2011, Ischia (NA)
some examples...
Date 31-08-2011, Ischia (NA)
Photometry
starfinder extracted PSF maory 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
Date 31-08-2011, Ischia (NA)
CMDs in I, I-Ks
Deep et al. 2011, A&A
Date 31-08-2011, Ischia (NA)
CMDs in I, I-H
H band looks more promising than Ks
Deep et al. 2011, A&A
Date 31-08-2011, Ischia (NA)
...errors
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 ∼24.6 or brighter, with the same photometric errors (BUT careful to the Blending Effect!!).
Deep et al. 2011, A&A
Date 31-08-2011, Ischia (NA)
...summarizing ELT compared with JWST...
Deep et al. 2011, A&A
Date 31-08-2011, Ischia (NA)
Cepheids with HST
finally coming back to H0
E-ELT
GAIA: direct calibration of LMC ULPs with parallaxes at µarcsec accuracy!
Date 31-08-2011, Ischia (NA)
ConclusionsThe 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)
looking for 2021...THANKS, everyone
Metropolitan Museum of art, NY city