Galaxies falling into a cluster
Joachim Köppen Kiel Sep 2017


Some brief explanations

This Monte Carlo simulation shows the properties of galaxies which are falling radially but from all directions to the centre of a spherically symmetric cluster of galaxies. While they follow this path, the ram pressure by the hot intracluster medium (ICM) removes some of the interstellar gas of the galaxy. Since this pressure increases with diminishing distance from the centre, the gas loss also increases. This can be studied for galaxies of a single type, but also for a population of galaxies with different properties. The simulation does not follow the actual flight of a galaxy, the spatial distribution of galaxies does represent the snapshot computed for a certain instant; instead, one chooses a radial profile for this distribution. The user may show the various quantities of the cluster and the galaxies as plots, histograms or false colour maps.
Since the simulation is fairly complex, has many options, and needs various parameters, here are some examples of its use.


Cluster properties: Galaxy properties: Simulation display:
Cluster properties
Dark matter
beta
core radius [kpc]
virial radius [kpc]
central density [Msun/pc³]
central density [g/cm³]

Intracluster gas (ICM)
beta
core radius [kpc]
virial radius [kpc]
central density [1/cm³]
central density [g/cm³]
central density [Msun/pc³]

within radius [Mpc]
DM mass [Msun]
ICM mass [Msun]

Galaxy properties
single type:
gas radius [kpc]
rotation speed [km/s]
surface density [Msun/pc²]


distribution of types:
gas radii [kpc]:
v²/r scatter factor
surface density [Msun/pc²]



Galaxy population
density profile
inner Radius [Mpc]
outer Radius [Mpc]
sigma Radius [Mpc]
beta
Core Radius [Mpc]
Simulation display
objects/step
objects now
no. of bins


X =
Zoom: ...
Y =
Zoom: ...




Mouse position:

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