CLUMPY executable (profiles, 1D or 2D- $J$ skymaps, stat. analysis, ...) More...

#include "../include/janalysis.h"
#include "../include/misc.h"
#include "../include/params.h"
#include <iostream>
#include <math.h>
#include <stdlib.h>

Include dependency graph for clumpy.cc:

Go to the source code of this file.

Functions
int	main (int argc, char *argv[])

Detailed Description

CLUMPY executable (profiles, 1D or 2D- $J$ skymaps, stat. analysis, ...)

     I. Command line and input ASCII files: ./bin/clumpy
     II. Examples and CLUMPY output
     III. Other useful plots

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I. Command line and input ASCII files: ./bin/clumpy

The executable clumpy is dedicated to the calculation of the astrophysical $J$ -factor for annihilating and decaying Dark Matter. Dark matter halos are present at many scales (sub-galactic, Galactic, galaxy cluster scale...). The Galactic centre is the obvious location for indirect detection of dark matter annihilation. However, it is plagued by a large background of astrophysical sources. Other potentially promising targets are dSphs, dark clumps of the Gal. halo, radients of the smooth halo (towards but slightly offset the Gal. centre), galaxy clusters...

For this reason, several modes are available in CLUMPY, to deal with all the above situations. Each mode is reached by using the appropriate flag in the command line. Specific formats for user-defined ASCII files are also required, depending on the option used. Help for the various options (and allowed parameters) should be self-explaining, so we only briefly describe the main characteristics of ASCII files required and modes availables in CLUMPY.

1. ASCII files

CLUMPY parameter file: clumpy_params.txt
List of halos file: data/list_generic.txt
Statistical analysis file: data/stat_dummy.txt

Warning: it is up to the user to check that his/her parameters are not unreasonable (there is no built-in check for that in CLUMPY).

2. Clumpy modes

./bin/clumpy -g for Galactic profiles and J-factor
This provides prints/plots for calculations involving the Galactic dark matter halo. The global configuration is set from a parameter file (e.g., clumpy_params.txt). Contributions from Galactic sub-halos and/or from a list of halos on top of the Galactic signal are optional. A complete skymap includes all these possible contributions (awaiting the addition of the extragalactic signal in CLUMPY), i.e. $J_{\rm sm}^{\rm Gal.}+J_{<{\rm sub}>}^{\rm Gal.}+J_{\rm drawn}^{\rm Gal.}+J_{\rm list}$ . The J-factor for each component is stored in an output file and ROOT plots should pop-up.
./bin/clumpy -h for list of halos analyses
A DM halo is fully described by its distance, position on the sky, and DM profile ( $\rho_s,\,r_s,\,\dots$ , see profiles.h). This is passed/read from a list-formatted file (e.g., data/list_generic.txt) the path of which is given in the parameter file (e.g., clumpy_params.txt, see the variable gLIST_HALOES). All the profiles/signal can be plotted on the same graph for comparison purpose. For the 2D option, you have to pick a halo in the list, and sub-clumps can be drawn.
./bin/clumpy -s for statistical analysis (PDF and CLs) on a single halo
This calculates the PDF and CLS on $\rho(r)$ , , $J(\alpha_{\rm int})$ , $J(\theta)$ , we have to run CLUMPY on a list of allowed profiles, the format of which is data/stat_dummy.txt. The list of profile given for a single halo can be the output from an MCMC analysis (see, e.g., Charbonnier et al. (2011)) or from a grid $\chi^2$ analysis (or any other fancy statistical method).

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II. Examples and CLUMPY output

Clumpy commands require an option and a series of arguments. We provide below several examples to illustrate CLUMPY capabilities, but also so that you can check that your CLUMPY installation is successful.

The commands are (if you don't use a bash shell, drop the 'dot'):

./bin/clumpy -gN (see examples below)
./bin/clumpy -hN (see examples below)
./bin/clumpy -sN (see examples below)

where $N$ is a number (1, 2, 3...). Note that for any $N$ , it is always possible to get a full default argument list, by typing, e.g.

./bin/clumpy -g1D

Remarks:

The default (be it for -g, or -h, or -s options) is to enable displays (d) and print (p) on screen, but

./bin/clumpy -gd $\Rightarrow$ display only;
./bin/clumpy -gp $\Rightarrow$ print on screen only.

All displays are based on the ROOT (CERN) interface. (ROOT canvas and objects can be straightforwardly saved in many formats - eps, jpeg, etc.).

1. Examples for ./bin/clumpy -gN

./bin/clumpy -g1 clumpy_params.txt 1.e-2 1.e2 50 1
$\rightarrow$ $\rho_{\rm Gal.}(r)$ (smooth, sub-continuum and total).

./bin/clumpy -g2 clumpy_params.txt 1.e-2 5. 10 1 0 0
$\rightarrow$ $J(\alpha_{\rm int})$ towards the Galactic centre.

./bin/clumpy -g4 clumpy_params.txt 0. 180. 50 0
$\rightarrow$ gives the $J(\theta)$ , the angle away from the Galactic centre + $J_{\rm list}$ (from halos in gLIST_HALOES in CLUMPY parameter file).

./bin/clumpy -g7 clumpy_params.txt 180. 0. 2. 2. 5
$\rightarrow$ should give, among the babbling, the following (for a quick check):

and the skymaps

Otherwise, larger skymaps using option -7, depending on the number of clumps to draw, can be quite lengthy (a few hours for on a desktop for $\alpha_{\rm int}\sim 0.01^\circ$ and a 5x5 FOV) depending on your parameters.

5x5 skymap towards the GC (top) and anti-centre (bottom)

2. Examples for ./bin/clumpy -hN

./bin/clumpy -h1 clumpy_params.txt 0. 5. 20 1
$\rightarrow$ DM density profile (smooth, sub continuum, and total).

./bin/clumpy -h2 clumpy_params.txt 1.e-2 2. 10 1 0
$\rightarrow$ boost $B(\alpha_{\rm int})$ from the substructures.

./bin/clumpy -h3 clumpy_params.txt 0. 1. 10 0
$\rightarrow$ boost $B(\theta)$ with $\theta$ the angle away from the dwarf centre.

./bin/clumpy -h5 clumpy_params.txt rs01_gamma00 2. 10.
$\rightarrow$ 2D J-factor including smooth, sub-continuum, cross-product, and drawn sub-clumps.

./bin/clumpy -h5 clumpy_params.txt rs01_gamma00 2. 10.
[gSIMU_ALPHAINT_DEG=0.01 and gSIMU_IS_ANNIHIL_OR_DECAY=0] in clumpy_parameters
$\rightarrow$ 2D J-factor for decay (including smooth, sub-continuum, and drawn sub-clumps).

3. Examples for ./bin/clumpy -sN

./bin/clumpy -s5 data/stat_dummy.txt 1.e-2 1.e1 50 0.68,0.95 2 1.e19
For illustration purpose, the next plots are based on the MCMC analysis of the classical dwarf spheroidals as detailed in Charbonnier et al. 2011 (CLs for can also be downloaded here). These MCMC files are not publicly available, so that we provided in CLUMPY a dummy file stat_dummy.txt from which the 2 above plots were obtained.
- ./bin/clumpy -s2 stat_files n_par r_for_mr rho_sat[Msol/kpc3]
- ./bin/clumpy -s5 stat_files rmin[kpc] rmax[kpc] n CL1,CL2,...CLi[%] switch_stat rho_sat[Msol/kpc3]
- ./bin/clumpy -s6 stat_files amin[deg] amax[deg] n CL1,CL2,...CLi[%] switch_stat rho_sat[Msol/kpc3] eps is_annihil
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III. Other useful plots

The following plots display a comparison of the various profiles as a function of $(l,\psi,\theta)$ , as well as the corresponding $J(\psi,\theta, \Delta\Omega)$ profiles or skymaps. This relies on trivial calls to some of the functions in CLUMPY and is provided for information only, but not documented further.

Line of sight density squared $\rho^2(l,\psi,\theta)$ . From top to bottom: anticentre=(-180,0) to GC=(0,0). Note the peak around (when $\psi\rightarrow 0$ ), corresponding to the GC DM peak.
Latitudinal dependence of $J(\psi,\theta, \Delta\Omega)$ for the various profiles. The left-hand plot is for an angular resolution $\alpha_{\rm int}=0.1^{o}$ , and the right-hand plot for $\alpha_{\rm int}=0.01^{o}$ . Toward the GC, the integral is completely dominated by the central density, so that it makes no difference for the two cases if the profiles are spiky enough (all but the ISO profile). On the other hand, for any other position, the integrand appearing in the -factor does not vary much with $\alpha_{\rm int}$ , so that
$J\propto \alpha_{\rm int}^2 \,.$
We recover a factor of between the two curves, as expected.
Cumulative along the l.o.s. We see that most of the "flux" is already accounted for at . Note that these cumulative plots are not very sensitive to the angular resolution of the instrument.
Skymaps of , for $\alpha_{\rm int}=0.1^{o}$ . A slice along $\theta=0$ would give the above plotted latitudinal dependence.

Definition in file clumpy.cc.

Functions

Detailed Description