Select Cluster To Download
CMC CLUSTER CATALOGWelcome to the CMC Cluster Catalog web server. This server is the home for the database of CMC (for Cluster Monte Carlo) simulations described in Kremer et al. 2019, arXiv:1911.00018.
For a detailed description of the computational methods of CMC, choices of initial model parameters, and discussion of results, see Kremer et al. 2019. Here, we describe the various output files for the downloadable CMC simulations. The CMC source code, with accompanying tutorials and documentation, will be presented in a forthcoming paper.
If you have specific questions, feel free to reach out to Kyle Kremer: email@example.com
OrganizationFour initial cluster parameters are varied in this set of simulations: N (initial number of particles), virial radius, Galactocentric distance (assuming a Milky Way like potential), and metallicity. This gives us 4x4x3x3=144 total simulations. We also include four additional simulations with N=3.2e6, giving us 148 independent simulations in total. The user can select a particular cluster simulation of interest by choosing each of these four initial parameters from the relevant drop down menus.
Once a particular simulation is selected, the user is prompted to download a compressed folder containing several files of interest for this simulation. We describe each of these files below:
initial.conv.shThe file initial.conv.sh contains all conversion factors used to convert from code to physical units. For example, to convert from code units of time to Myr, multiply by the factor timeunitsmyr, and so on.
Snapshot FilesThe files initial.snap…dat.gz are time snapshots at distinct points in the clusters evolution. We output here up to 11 snapshots per simulation at t=0, 0.1, 1, 6, 10, 10.5, 11, 11.5, 12, 12.5, and 13 Gyr. If a particular simulation disrupts before 13 Gyr, then fewer snapshots are outputted. The specific time of each snapshot is indicated in the first line of each snapshot file (in code units).
Each snapshot contains stellar radial positions, stellar types, and stellar properties for all N objects in the cluster at the given evolutionary time. These snapshots can be used to create, for example, surface brightness or velocity dispersion profiles, for a given cluster model. Below we summarize our stellar type and stellar ID label schemes.
Stellar Type Labels: We adopt the stellar type labeling scheme of SSE/BSE (Hurley et al. 2000, 2002), as summarized below.
- 0 - deeply or fully convective low mass MS star
- 1 - Main Sequence star
- 2 - Hertzsprung Gap
- 3 - First Giant Branch
- 4 - Core Helium Burning
- 5 - First Asymptotic Giant Branch
- 6 - Second Asymptotic Giant Branch
- 7 - Main Sequence Naked Helium star
- 8 - Hertzsprung Gap Naked Helium star
- 9 - Giant Branch Naked Helium star
- 10 - Helium White Dwarf
- 11 - Carbon/Oxygen White Dwarf
- 12 - Oxygen/Neon White Dwarf
- 13 - Neutron Star
- 14 - Black Hole
- 15 - Massless Supernova