Palomar 5 N-Body Simulation

<p>Please cite&nbsp;<a href="https://ui.adsabs.harvard.edu/abs/2020MNRAS.493.4978S/abstract">https://ui.adsabs.harvard.edu/abs/2020MNRAS.493.4978S</a></p> <p>Contained is an&nbsp;ECSV file of an N-body simulation,&nbsp;using&nbsp;the the direct N-body code NBODY6 (Aarseth 2006)&nbsp;to simulate the evolution of a Palomar 5-like globular cluster. The initial cluster is taken to be a Plummer model consisting of 100,000 stars and has a half-mast radius of 10 pc. Stellar masses follow a Kroupa initial mass function with the minimum and maximum stellar mass set to 0.1 and 50 solar masses respectively. Single stars evolve using the stellar evolution prescription of Hurley 2000 assuming a metallicity of Z=0.001 while binary stars, in the event that binaries form, follow Hurley&nbsp;2002.</p> <p>The properties of the external tidal field were set to reflect MWPotential2014, from Bovy&nbsp;2015, and is a good approximation of the Galactic potential (Bovy&nbsp;2016). The specific linear combination of potentials is a spherical potential from a power-law density with an exponential cut-off Galactic bulge, an NFW dark matter halo, and a Miyamoto-Nagai&nbsp;disc. The model cluster was evolved for 12 Gyr with an initial position and velocity that resulted in it being located at the present day location of Palomar 5&nbsp;at the end of the simulation. The final mass and mass function of the model cluster are comparable to the observed properties of Palomar 5, but the model cluster is too compact relative to Palomar 5, which is in the process of dissolving.</p>