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Scientific cases of the Italian community for LGS @ LBT

Scientific cases of the Italian community for LGS @ LBT. Filippo Mannucci. Projects and requirements. *: see also Firenze Oct 2006: http://lbtwww.arcetri.astro.it/adoptws/agenda.html. Comparison AO+LSG vs. HST. Seeing limited 0.8” FWHM. LBT GLAO 4’x4’ H,K=24. 1x1. WFPC3 2.2’x2.2’

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Scientific cases of the Italian community for LGS @ LBT

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  1. Scientific cases of the Italian community for LGS @ LBT Filippo Mannucci

  2. Projects and requirements *: see also Firenze Oct 2006: http://lbtwww.arcetri.astro.it/adoptws/agenda.html

  3. Comparison AO+LSG vs. HST Seeing limited 0.8” FWHM LBT GLAO 4’x4’ H,K=24 1x1 WFPC3 2.2’x2.2’ H=26.5 NACO LBT DL 0.9’x0.9’ H,K=24 NIC3 0.9’x0.9’ H=25.8

  4. Herbig Ae/Be stars SII 6717 Å3.5m Calar Alto XZ Tau HL Tau HH 30 jet Ray et al. 1996 Mundt et al. 1990. Stellar disks and Jets • Disks and Jets: • extraction of excess angular moment, efficiency of formation • exact nature of acceleration of the jet is unclear • jet rotation and precession? • peculiar velocity fields, bow shocks

  5. Stellar disks and Jets Dougados et al 2000 Magnetic flow surfaces 1” Alfve'n Surface 0.5” High spatial (<0.1”) and spectral (R>5/10000) resol. near-IR (FeII 1.2, 1.6, H2 2.1 mic) or optical R (OI λ 6300, Hα, SIIλ6716) Habart, Natta & Testi (2006) ESO/NACO

  6. Stellar disks and Jets best with IFU, possible with multislit Ha SII 1” 1” N II OI 1” Increasing radial velocity HST/STIS Bacciotti et al. 2000 0.5” LGS: imaging and spec.– DL - sky coveragemost jets have no bright star

  7. SNe at z~1 • High redshift (z>0.5) • Ia: cosmology • CC: tracer of SFH SNe: • metal production • feedback for galaxy formation • thermal history of ICM and IGM Mannucci et al. 2007

  8. SNe associated to GRB Della Valle et al. (2006a) Della Valle et al. (2006b) • Long GRB: death of a massive star • diversity of SNe • z>1 • Imaging and Spectroscopy • LGS: DL, sky coverage

  9. Black Hole in Galactic Nuclei • correlation BH mass – bulge mass • Coformation and coevolution galaxy-central BH • Feedback Measuring the BH mass: • Star dynamics • Gas dynamics • (size of BLR, line width, reverbaration mapping) Only ~40 measures Sphere of influence: BH gravitational field = Galactic Radius = 0.1” for M = 108M⊙ σ = 200 Km/sec D = 20 Mpc Marconi & Hunt (2003)

  10. Black Hole in Galactic Nuclei NGC3227 D=17 Mpc log(MBH/M⊙) = 6.8-7.3 Davies et al. 2006

  11. Black Hole in Galactic Nuclei NGC4593 (D=38 Mpc) log(MBH/M⊙)=7.5 Pastorini et al (2007) SINFONI, H2 (2.12 mic) Best with IFU, slits work fine Spectral R>3000 LGS:DL, sky coverage

  12. z~7HST/ACS VLT/ISAAC SPITZER/IRAC Optically faint galaxies Mannucci et al (2007) UV bright (LBG) UV faint (EROS, DRG…) Rodighiero et al (2007)

  13. Optically faint galaxies GLAO K’ band 1 hour 0.3” FWHM

  14. intermediate- and high-z galaxies • Tests of ΛCDM: • number of large (M>1011M⊙) halos at z=3 • number of centrifugally supported large disks at z>2 • increase in galaxy size from z=3 • Galaxies at z≥2 • fundamental plane of E • metallicity and stellar gradients • disk dynamical mass • Morphology: GLAO/images • large field • stable PSF • “known” PSF • sky coverage Redshifts, metallicity, dynamics? GLAO/MOS

  15. Dynamics of high-z galaxies • Dark halo, dynamical to stellar mass, metallicity z=3.23 1 arcsec Mannucci et al. (2007)

  16. Mass-Metallicity relation at high z downsizing: large galaxies form first? star formation and mass assebly AMAZE, ESO large project, SINFONI (PI: Maiolino)

  17. Mass-Metallicity relation at high z AMAZE, ESO large project, SINFONI (PI: Maiolino) IFU, DL, sky coverage

  18. Merging history evolution of the merging rate among galaxies simpler non-baryonic physics Strong predictions of CDM Near-IR to avoid star-forming blobs High spatial resolution , large fields GLAO, imaging z=3.1

  19. Projects and requirements

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