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Novel kinematic methods to trace Spiral Arms nature using Gaia data

  • S. Roca-Fàbrega (a1), F. Figueras (a1), O. Valenzuela (a2), M. Romero-Gómez (a1), T. Antoja (a3), P. Colín (a4), B. Pichardo (a2) and H. Velázquez (a5)...

Abstract

In this work we shed new light in the nature of spiral arm structures in galaxies. We present a disk kinematic and dynamic study of MW like galaxies using complementary approaches: analytical models, test-particle simulations, pure N-body and cosmological N-body plus hydrodynamic simulations. Using collisionless N-body data we have found that models with strong bar present a flat rotation frequency, i.e. rigid body rotation, whereas in the opposite extreme case, i.e. in unbarred systems, spiral arms are disk corotant (Roca-Fàbrega et al. 2013). Complementary to this work, we discuss how the vertex deviation parameter is a good tracer of corotation (CR) and outer Lindblad resonance radius (OLR) (Roca-Fàbrega et al. 2014). We have succeeded to produce MW like models in fully cosmological N-body plus hydrodynamic simulations with a high resolution (Roca-Fàbrega et al., in preparation). First results concerning disk phase space properties in terms of spiral arm nature using these simulations are presented (http://www.am.ub.edu/ sroca/shared/PosterRocaFabrega.pdf).

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[1]1Roca-Fàbrega, S., Valenzuela, O., Figueras, F., et al., 2013, MNRAS, 432, 2878
[2]2Roca-Fàbrega, S., Antoja, T., Figueras, F., et al., 2014, MNRAS, 440, 1950

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