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mkkd95 - Kuijken-Dubinski-95 composite disk-bulge-halo model


mkkd95 [parameter=value]


mkkd95 creates a composite Disk-Bulge-Halo galaxy in near equilibrium following the procedure described in Kuijken & Dubinksi (1995). This program is merely a NEMO wrapper that assembles all the correct parameters, runs the a set of KD95 programs (commonly referred to as the GalactICS Software) in a temporary rundirectory and converts the ascii output to a NEMO snapshot(5NEMO) .

The bulge and halo are a King and lowered Evans distribution resp, whereas the disk a 3D generalization of Shu’s planar disk to include a 3rd integral of motion to account for the vertical structure. The construction occurs in 3 steps. First the potential is calculated, after which the disk distribution function is constructed which generates the given potential. Finally, each component is realized with a self-consistent distribution of particle orbits.

Although one has the option of including any combination of components, leaving out the halo probably won’t work.

Two new versions have been published since the current 1995 K&D version: Widrow & Dubinski (2005) and Widrow, Pym and Dubinski (2008). These are not (yet) supported in the current mkkd95 program.


The following parameters are recognized in any order if the keyword is also given:
output snapshot (a rundirectory $out.tmpdir is also created). No default.
Number of particles in disk. Set them to 0 to leave out this component. Notice these are the first set (of three) of particles in the snapshot. [8000]
Number of particles in bulge, the second set of particles in the output snapshot. [4000]
Number of particles in halo. Notice these are the thirds and last set of particles in the snapshot. [6000]
in.dbh: Psi0 (HALO) central potential - the smaller (the more negative) this parameter the deeper the potential and the more extended the halo [-4.6]
in.dbh: v0 = sqrt(2.0)*sigma0 where sigma0 is the central velocity dispersion. roughly the velocity where the halo rotation curve peaks [1.42]
in.dbh: q an optional flattening parameter for the potential - generally 0.7 < q < 1.05 - q=1.0 will give a nearly spherical halo [1]
in.dbh: (rc/rk)^2 a core smoothing parameter - ratio of the core radius to the derived King radius for halo only models set this to 1.0. For multicomponent models, this can be a smaller number 0.0 to 0.1. I’ve found that with this parameter=0.0 the program can crash. [0.1]
in.dbh: Ra - a scaling radius for the halo - The halo Ra radius is the radius at which the halo rotation curve, at its initial slope ignoring cutoffs and the other components, reaches v0. [0.8]
in.dbh: M_d - mass of the exponential disk ignoring cutoffs [0.867]
in.dbh: R_d - exponential scale length [1]
in.dbh: R_outer - outer radius where we begin to truncate the disk density [5]
in.dbh: z_d - disk scale height assuming a sech^2(z/zd) vertical density law [0.1]
in.dbh: dR_trunc - truncation width - the disk density smoothly drops to zero in the range R_outer < R < ~R_outer + 2*dR_trunc. [0.5]
in.dbh: rho_b - bulge central density [14.45]
in.dbh: psi_cut - bulge cut-off potential psi0 < psi_cut < 0.0 - energy cut-off for the bulge
in.dbh: sig_b - bulge central potential [0.714]
in.dbh: delta_r the width of the radial bins used to calculate the potential [0.01]
in.dbh: nr - number of radial bins - initially a guess since we don’t know the radial extent of the system [2400]
in.dbh: the largest value in the potential harmonic expansion - use lmax=2 to get a quick look at the mass profile and lmax=10 for the final calculation of the model number of harmonics [10]
in.diskdf: central radial velocity dispersion [0.47]
in.diskdf: scalelength of sig_r^2 [1.0]
in.diskdf: number of intervals for correction function [50]
in.diskdf: number of iterations [10]
in.bulge: the streaming fraction of stars with L_z > 0. This controls the rotation of the bulge and the halo, with f=0.5 the non-rotating case. [0.75]
in.halo: see above, for the halo. [0.5]
in.- Random Seed - KD95 convention. Notice this seed is shared by all 3 components. [-1]
in.- Center the snapshot? Notice again this is shared by all three components. [t]
directory in which KD95 binaries live. Unless your binaries have been added to your search PATH, you need to specify the directory where these live. [.]
Base K&D95 model. The default model parameters above are already for model-A, but with this keyword another one of the 4 published models can be quickly loaded. After that specific parameters can still be overriden by setting their value explicitly. By default model is not set via this method.
Number of models computed. Useful if you want to stack a large number of models to increase signal to noise. Default: 1.
Cleanup the temporary run directory after usage. The contents of this directory is probably only useful for debugging, it contains the output of all the individual programs and temporary files before final conversion to the out file. Default: t


Creating a galaxy model from these parameters is sort of a black art since the halo and bulge models are not parameterized in terms of their mass profiles but rather properties of their distribution functions. Changes in psi0, v0 etc. have weird but predictable effects on the mass profile.

The halo is a flattened analogue of the King model so the concentration (R_tidal/R_core) is determined by the dimensionless central potential psi_0/sigma_0^2. The more negative the value the greater the concentration. The parameters R_a and v_0, affect the scaling of the halo mass profile.

The effect of different bulge parameters is more predictable. Decreasing the central velocity dispersion will create a more centrally concentrated bulge and decreasing the psi cut off will truncate the bulge and decrease its total mass.

The disk is parameterized directly by its mass profile so its effect on the rotation curve is predictable ahead of time.

Hit and miss seems to be a good strategy for finding a suitable profile. Generate a model to lmax=2 and then view the resulting rotation curve by using the vcirc program, in which the contributions to the total rotation curve are tabulated. Another useful file is mr.dat which tells you the mass and radial extent of the disk bulge and halo.

The program plotforce will also generate the rotation curves for you directly from the dbh.dat, b.dat and h.dat files.

The potential is determined iteratively: starting from an initial guess at the potential, the density implied by the halo and bulge DFs is calculated, the disk density added, and the potential of that mass distribution is used as starting point for the next iteration. Initially only the monopole (l=0) components are calculated until the model converges, then one more harmonic is added per iteration up to the maximum requested, and once all harmonics are included the iterations are continued until the outer (tidal) radius of the halo is unchanged between iterations. At each iterations plots of the harmonic expansion coefficients are produced. If the tidal radius reported is "outside grid" for a large number of iterations, increase the number of radial bins or increase their size. Sometimes infinite tidal radii are also reported: this happens when the total mass of the model using the current guess for the potential is insufficient to generate a potential well as deep as requested. If this persists over many iterations, again increase the number or size of the radial bins.


Although mkkd95 calls a number of KD95 programs, here is a brief explanation of some of them:

dbh calculates the potential. From in.dbh is computes dbh.dat, h.dat, b.dat and mr.dat.

getfreqs tabulates various characteristic frequencies (omega, kappa etc.) in the equatorial plane for use by diskdf. Input files are dbh.dat h.dat b.dat, and it generates freqdbh.dat

diskdf iteratively calculates the correction functions for the disk distribution function. These functions are multiplicative corrections to the surface density and vertical velocity dispersion which appear to leading order in the Shu (1969) distribution functions. See KD95 for details. The keywords sigrv0, sigr0, ncorr, niter are used for this. It also outputs the Toomre Q as a function of radius in the file toomre.dat.

gendisk, genbulge, genhalo assembled the respective components using an input file.

mergerv is a small shell script that merges the 3 ascii files.


The bulk of the CPU is in creating the disk particles, the bulge and halo are a much smaller fraction of the cpu. On a 1.6 GHz Pentium-4 laptop the cpu cost is about (Ndisk/1000)+32 secs for the gnu compiler (the 32 secs is to account for building tables, which is independantly of the number of particles.


The default keywords are for Kuijken-Dubinski’s model-A.

% mkkd95 A0.dat
% snapmstat A0.dat sort=f
0 0:7999  = 8000 Mass= 0.000108822 TotMas= 0.87058 CumMas= 0.87058
1 8000:11999  = 4000 Mass= 0.00010631 TotMas= 0.425242 CumMas= 1.29582
2 12000:17999 = 6000 Mass= 0.000819365 TotMas= 4.91619 CumMas= 6.21201
% snapplot A0.dat color=’i<8000?2.0/16.0:(i<12000?3.0/16.0:4.0/16.0)’ yvar=z
% snapxyz A0.dat - color=’i<8000?1:(i<12000?2:4)’ | xyzview - maxpoint=18000 nfast=18000
scale=8 fullscreen=t
% mkkd95 B0.dat model=B
% snapplot B0.dat color=’i<1000?2.0/16.0:(i<2000?3.0/16.0:4.0/16.0)’ yvar=z
% mkkd95 C0.dat model=C
% snapplot C0.dat color=’i<4000?2.0/16.0:(i<6000?3.0/16.0:4.0/16.0)’ yvar=z
% mkkd95 D0.dat model=D
% snapplot D0.dat color=’i<1000?2.0/16.0:(i<2000?3.0/16.0:4.0/16.0)’ yvar=z

See Also

gendisk, genbulge, genhalo, dbh, getfreqs, diskdf, snapmstat(1NEMO) , tabtos(1NEMO) , magalie(1NEMO)     original GalactICS distribution

1995MNRAS.277.1341K - Kuijken, K.; Dubinski, J.  
Nearly Self-Consistent Disc / Bulge / Halo Models for Galaxies

Widrow & Dubinski 2005 (version 2)

Deg, N., Widrow, L. M., & Randriamampandry, T. 2019, MNRAS, 486, 5391 (updated
release to include gas)

Widrow, Pym and Dubinski 2008 (version 3)


GalIC    [ascl:1408.008] GALIC: Galaxy initial conditions construction 

makediskgalaxy  Springel et. al 2005 - 2005MNRAS.361..776S 


@ads 1995MNRAS.277.1341K


$out.tmdir/dbh.dat            contains tabulated values of the harmonic coefficients
                  for the Legendre expansion of the density, potential
                  radial force at the specified radii for the entire model
$out.tmdir/h.dat              same as above, but only for halo
$out.tmdir/b.dat              same as above, but only for bulge
$out.tmdir/mr.dat             mass and radial extent (or edge) of disk, bulge
and halo


Konrad Kuijken & John Dubinski (fortran programs - 1995) Peter Teuben (NEMO interface) -

Update History

06-Mar-04    V1.0 Created, using kd95’s  README file     PJT
11-mar-04    V1.2 added nmodel= and warns about using model=     PJT
23-mar-04    V1.4 use logfile in tmpdir, added cleanup=, some key reorder    PJT
19-jul-06    V1.5 fix POSIX problems and document order of particles better
27-jul-06    fixed documentation on vcirc usage, disabled pgplot for ia64    PJT
5-aug-06    merged two previous (CVS) docs    PJT

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