Modeling the Milky Way disk dynamics

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Bar effects: Hercules accross the discΩp=49 km/s/kpc20 o•Kinematic response to the bar depends ondisc position•The Hercules gap moves to lowerazimuthal velocities for largerGalactocentric radius•More changes in radius than azimuthT. Antoja Sydney, 24/07/2012
Bar effects: Hercules accross the discΩp=49 km/s/kpc-60 km/s20 o-40 km/s-20 km/s0 km/s•Kinematic response to the bar depends ondisc position•The Hercules gap moves to lowerazimuthal velocities for largerGalactocentric radius•More changes in radius than azimuthT. 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 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 30 and 31: 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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