Dark Matter Direct Detection with Non-Maxwellian Velocity Structure
Michael Kuhlen (
), Neil Weiner (
), Jürg Diemand, Piero Madau, Ben Moore, Doug Potter, Marcel Zemp
submitted to JCAP, arXiv/0912.2358
), Neil Weiner (), Jürg Diemand, Piero Madau, Ben Moore, Doug Potter, Marcel Zemp
Below you can download ascii tables
of 
, where
f(v) is the velocity modulus distribution in the Earth rest frame
(normalized to unity), and N(vmin), the cumulative number
of particles with velocity modulus exceeding
vmin. g(vmin) and N(vmin) are
provided at 12 equally spaced times (g00 - g11), tracing out the
annual modulation arising from Earth's orbit around the Sun. The
format is as follows:
# Via Lactea II - spherical shell sample - g(v_min) # # v_min g00 g01 ... g11 # [km/s] [(km/s)^-1] # 0.0 4.095e-03 4.073e-03 ... 4.072e-03 1.0 4.095e-03 4.072e-03 ... 4.072e-03 . . . . . . . . . . . . 650.0 9.325e-06 8.777e-06 ... 8.951e-06 651.0 9.009e-06 8.544e-06 ... 8.579e-06 . . . . . . . . . . . . 998.0 0.000e+00 0.000e+00 ... 0.000e+00 999.0 0.000e+00 0.000e+00 ... 0.000e+00 |
# Via Lactea II - spherical shell sample - N(v_min) # # v_min N00 N01 ... N11 # [km/s] # 0.0 2117320 2117320 ... 2117320 1.0 2117320 2117319 ... 2117320 . . . . . . . . . . . . 650.0 13290 12503 ... 12751 651.0 12856 12187 ... 12234 . . . . . . . . . . . . 998.0 0 0 ... 0 999.0 0 0 ... 0 |
[g00/N00 corresponds to the peak of the modulation, i.e. June 2nd for a Maxwell-Boltzmann distribution.]
We provide tables for the VL2, GHALO, and GHALOs simulations. (See the paper and references therein for details on the simulations.) Additionally we provide tables for a case where we scaled the velocities of the particles to give v0=220 km/s, where v0 is the peak of halo rest frame f(v) (i.e. the most probable speed). The velocity scaling factor is fv = 1.1875 for VL2 and GHALOs and 1.5556 for GHALO. An escape velocity cutoff of vesc=550 km/s was applied. Note that we did not use these scaled distributions in our analysis, because we found that a lot of the interesting structure was pushed to beyond the escape velocity.
For each simulation, we provide one table for the spherical shell
average (all particles with 8 kpc < r < 9 kpc), a tarball containing
tables for all 100 sample spheres, and a smaller tarball containing 10
DAMA-favorable sample spheres (i.e. spheres lying in the lower left
corner of Fig.8).
VL2