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Clumpfinder (PHEW)
The block named &CLUMPFIND_PARAMS
contains the parameters related to the built-in RAMSES clump finder (PHEW). The parameters are described only briefly, for more backround information read the PHEW paper.
Variable name, syntax, default value | Fortran type | Description |
---|---|---|
ivar_clump=1 |
integer |
Control which density field is used for clump finding (1: gas density, 0: particle density) |
density_threshold=-1.d0 |
float |
Density threshold for the clump finder (code units) |
rho_clfind=-1.d0 |
float |
Density threshold for the clump finder (g/cc). Not recommended - use density_threshold instead. |
n_clfind=-1.d0 |
float |
Density threshold for the clump finder (H/cc). Not recommended -use density_threshold instead. |
relevance_threshold=2.d0 |
float |
Relevance (peak-to-saddle ratio) threshold for a clump to be considered real (instead of noise). |
saddle_threshold=-1.d0 |
float |
Saddle density threshold for sub-structure merging (code units). A negative value turns sub-structure merging off (PHEW will only merge noise). |
mass_threshold=0.d0 |
float |
When set to a value > 0, the properties of those clumps/haloes with mass > mass_threshold * particle_mass are written to disk. particle_mass is the smallest strictly positive particle mass in the simulation. Setting this parameter does NOT affect the merging of noise/clumps. |
age_cut_clfind=0.d0 |
float |
When set to a value > 0, only the stars with an age lower than age_cut_clfind are used by the clump finder. Stellar and DM particles are used otherwise. |
Updated