DARKexp
Statistical Mechanics Approach to Collisionless Relaxation
Papers:
Statistical Mechanics of Collisionless Orbits. I. Origin of Central Cusps in Dark-matter Halos
Hjorth, J., Williams, L.L.R. 2010, ApJ, 722, 851
Statistical Mechanics of Collisionless Orbits. II. Structure of Halos
Williams, L.L.R., Hjorth, J. 2010, ApJ, 722, 856
Statistical Mechanics of Collisionless Orbits. III. Comparison with N-body Simulations
Williams, L.L.R., Hjorth, J., Wojtak, R. 2010, ApJ, 725, 282
Statistical Mechanics of Collisionless Orbits. IV. Distribution of Angular Momentum
Williams, L.L.R., Hjorth, J., Wojtak, R. 2013, ApJ, in press
DARKexp vs other models:
Testing phenomenological and theoretical models of dark matter density profiles with galaxy clusters
L. J. Beraldo e Silva, M. Lima, L. Sodré. 2013, MNRAS, 436, 2616
Kinematics of a globular cluster with an extended profile: NGC 5694
Bellazzini, M., Mucciarelli, A., Sollima, A., Catelan, M., Dalessandro, E., Correnti, M., D'Orazi, V., Cortés, C., Amigo, P. 2015, MNRAS, 446, 3130
CLASH: Joint Analysis of Strong-Lensing, Weak-Lensing Shear and Magnification Data for 20 Galaxy Clusters
Umetsu, K., Zitrin, A., Gruen, D., Merten, J., Donahue, M., Postman, M. arXiv:1507.04385
Download density profiles:
DARKexp model has 1 shape parameter, phi0, which is the dimensionless depth of the halo potential.
The distribution of scaled particle energy, e, of DARKexp models has a simple form, N(e)~exp(phi0-e)-1,
which was derived in Paper I, but the corresponding density profiles for isotropic systems do not have
an analytical form, so below we provide computed density profiles; see Paper II for how these were
obtained from N(e).
Files are labeled by the DARKexp phi0, the scaled potential depth, the model's only shape parameter.
Note that the potential at the center, phi[r-->0], is phi0.
The radius r is scaled such that in 3D the "isothermal" slope, gamma=2, corresponds to log[r]=0.
The normalization of 3D and 2D density profiles are such that rho_3D,2D[r]=1 at r=1.
The columns in the files are:
1. line number
2. log10[r], same for 3D and projected 2D
3. log10(rho_3D[r])
4. 3D density slope, gamma
5. log10(rho_2D[r])
6. 2D density slope
7. ignore
...And more finely spaced phi0 values:
