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Gruppo Stellare: Sommario

Gruppo Stellare: Sommario. Persone direttamente interessate: LT, Antonella Natta, Francesca Bacciotti, Emilie Habart Collegamento con progetti AMBER-GTO Interesse Scientifico in AdOpt: Detezione e caratterizzazione di pianeti extrasolari Struttura ed Evoluzione dei Dischi Circumstellari

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Gruppo Stellare: Sommario

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  1. Gruppo Stellare: Sommario • Persone direttamente interessate: • LT, Antonella Natta, Francesca Bacciotti, Emilie Habart • Collegamento con progetti AMBER-GTO • Interesse Scientifico in AdOpt: • Detezione e caratterizzazione di pianeti extrasolari • Struttura ed Evoluzione dei Dischi Circumstellari • Struttura dei Getti Collimati da Stelle Giovani • Lavoro Preparatorio per Progetti AMBER • [Stelle multiple; Ammassi stellari giovani] • Progetti in Corso • Osservazioni NACO (spec) di Dischi Circumstellari • Osservazioni NACO (spec) di Getti Collimati

  2. Detezione di Pianeti Extraolari • Grosso contrasto di luminosità [Coronografo?] • Detezione di Candidati in Imaging [Bande Strette “mirate”?] • Verifica del moto proprio [Osservazioni ripetute] • Caratterizzazione multibanda e spettroscopica [Amici Spec]

  3. The flow is resolved transversely Optical 'channel maps' in different velocity bins From line ratios, 2D excitation maps of Ne, Xe, Te ... From line profiles, rotation ? DG Tau, RW Aur jets with HST/STIS (0.”1) Bacciotti et al. 2000, Woitas et al. 2002 SLITS

  4. l Position 0.”3 Position Velocity IV. Jet rotation : various jets “Perpendicular Slit” Cycle 11,12 microjets with 1 SlitPERPENDICULAR to each flow lobe at 0.”3 from source HST/STIS ...switching axes...

  5. The measured visibilities will be compared with U,V map predictions from existing wind models and jet opening angles VLTI/AMBER : Geometry of the first AUs of a microjet ATs, large U,V coverage with short – medium baselines Spectral Resolution = 1000 Fe 1.25m, Pa , HeI 1.083m

  6. Jet P.A.: -225º • Fe 1.25m, Pa  • High Spectral Resolution: R=10000 • Dv=30 km/s • (rotation at A. Surface = 50 –100 km/s) • J=12 in each vel. bin --> UT sensitivity • UT1, UT2, UT4 are // and l to jet dir. • good UV coverage Model of the jet visibility from a toy hollow jet model with P.A.: -225º and opening angle 45º , with superposed UV tracks for the UTs VLTI/AMBER : Kinematics of the RU Lupi jet N

  7. Sommario • Desiderata: • Alto Strehl e stabilità PSF • Bassa risoluzione spettrale -> Amici like • Alta risoluzione spettrale (if possible >= 10000) • Infrared WFS • Proposte: • Planet Searches • Disk Structure • Jet Structure • AMBER Targets • …Not all of these may be feasible...

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