Currently the database contains models of globular clusters and their streams, simulated in three Galactic potentials, two of which contain an axisymmetric disk, with our without a central spheroid, while the third contains a slowly-rotating stellar bar. See Ferrone et al for additional details.
Axisymmetric potentials
The two axisymmetric potentials currently used are models I and II described in Pouliasis et al. 2017, A&A, 598, 66 . Model PI Model I by Pouliasis et al. (2017) (abbreviated name: PI) consists of four components: a thin, a thick disk (both represented by Miyamoto & Nagai potentials), a dark matter halo (with the same functional form adopted in the Allen & Santillan (1991) model) and a central bulge (modeled as a Pummer sphere). Model PII Model II by Pouliasis et al. (2017) (abbreviated name: PII) consists of a thin, a thick disk and a dark matter halo (with same functional forms as for model PI), and does not contain any central spheroid.
Asymmetric potential
The barred model (abbreviated name: PII-0.3-SLOW) is a version of model PII modified to include a rotating stellar bar, whose mass has been assigned to be 30% of the (thin+thick) disk mass of model PII. We assume that the bar rotates with a constant pattern speed of Ωbar = 38km/s/kpc, and that it is currently inclined of 25 degrees with respect to the Sun-Galactic center direction. We model it as a triaxial distribution, as given by Long &A Murali (1992).