For these models, we set up a spherical two component (stars/dark matter) “dwarf-like” galaxy. This has a Dehnen profile for both the stars and the dark matter:

<latex> \rho = \frac{M(3-\alpha)}{4\pi a^3}\frac{1}{(r/a)^\alpha(1+r/a)^{4-\alpha}} </latex>

With parameters:

This was then put on a range of orbits of increasing ellipticity in a Miyamoto-Nagai-Log potential:

<latex> \Phi = \Phi_M + \Phi_L </latex> <latex> \Phi_M(R,z) = -\frac{GM_{\rm disk}}{\sqrt{R^2 + (a+\sqrt{b^2+z^2})^2}} </latex> <latex> \Phi_L(R,z) = \frac{v_0^2}{2}\ln\left(R_c^2 + R^2 + \frac{z^2}{q_0^2}\right) + {\rm const.} </latex>

with:

<latex> M_{\rm disk} = 5 \times 10^{10}\,{\rm M}_\odot v_0 = 220\,{\rm km/s} r_t = 8\,{\rm kpc} a = 4\,{\rm kpc} b = 0.5\,{\rm kpc} q_0 = 1.0 </latex>

Four orbits were chosen as follows; each aligned at 40 degrees to the x-z plane; each evolved for 5 Gyrs.

Density projections of the final stellar distribution are as follows (left to right :: Orbit1 → Orbit4):

The following give data files for each. These include .txt files of all stars for the final disrupted satellite centred on the origin. This amounts to three data sets if using only projected data (i.e. one along each of the x,y,z projections). In addition, the raw Gadget data files are included. These have not been centred. PyNbody python tools for loading and manipulating these Gadget data can be found here. Units for each file are as follows:

• .txt files :: x(kpc),y(kpc),z(kpc),vx(km/s),vy(km/s),vz(km/s)
• .dat files (Gadget) :: <latex>L = {\rm kpc}</latex>, <latex>M = 2.33\times 10^5\,{\rm M}_\odot</latex>, <latex>V = {\rm km/s}</latex>