Novel kinematic methods to trace Spiral Arms nature using Gaia data

¹ Institut de Ciencies del Cosmos, Universitat de Barcelona (DAM-ICCUB-IEEC), Spain
² Instituto de Astronomía, Universidad Nacional Autónoma de México (IA-CU), México
³ Research and Scientific Support Office, European Space Agency (ESA-ESTEC)
⁴ Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, México
⁵ Instituto de Astronomía, Universidad Nacional Autónoma de México (IA-Ensenada), México

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).