Modeling the Milky Way disk dynamics

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Finding substructure: Wavelet TransformMR Software (CEA, Saclay)Starck & Murtagh 2002Slezak et al. 19931) Point distribution2) Wavelet transform3) Significant peaks 2σ and 3σT. Antoja Sydney, 24/07/2012
Revisiting <strong>the</strong> solar neighbourhoodRAVE Local sample•Similar significant groups in GC and RAVE local sample•Main groups: Coma Berenices, Hyades, Sirius, Pleiades,Hercules57178 starseU,V~4 km/s•New group at (U, V)∼ (90, -20) km/sRAVEGCT. Antoja Sydney, 24/07/2012
Page 1 and 2: Dynamics of the spiral armsand the
Page 3 and 4: IntroductionVelocities of stars in
Page 5 and 6: Y (kpc)Outline:X (kpc)• Models: o
Page 7 and 8: Groups and resonances (Monari et al
Page 14 and 15: VOLR for different bar propertiesfr
Page 16 and 17: Bar effects: Hercules accross the d
Page 18 and 19: VOLR as a function of RT. Antoja Sy
Page 24 and 25: Y (kpc)Outline:X (kpc)• Models: o
Page 26 and 27: RAVE sample• multi-fiber spectros
Page 28 and 29: Finding substructure: Wavelet Trans
Page 32 and 33: Revisiting the solar neighbourhoodR
Page 34 and 35: Revisiting the solar neighbourhoodR
Page 36 and 37: Beyond the solar neighbourhoodAntoj
Page 38 and 39: Hercules changes with R in RAVET. A
Page 40 and 41: Hercules changes with R in RAVE8 kp
Page 46 and 47: Constrains on bar properties β=0Ω
Page 48 and 49: Constrains on bar properties β=0Ω
Page 50 and 51: Integrating for all βΩp =56.8+1.9
Page 52 and 53: Hot population•Some groupspersist

Modeling the Milky Way disk dynamics

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