CSE6SSM Spectrum and Dark Matter

Analysis code for studying the mass spectrum and dark matter in the CSE6SSM, used for the numerical analysis reported in arXiv:1610.03374.

Requirements

To obtain analytic results using SARAH requires

• Mathematica (version 7.0 or higher)
• SARAH (version 4.5.6 or higher)

The C++ spectrum generators were generated using FlexibleSUSY. To compile them requires

• C++ compiler (g++ >= 4.7.2 or clang++ >= 3.1 or icpc >= 12.1)
• Fortran compiler (gfortran, ifort)
• Boost (version 1.37.0 or higher)
• Eigen 3 (version 3.1 or higher)
• GNU scientific library (GSL)
• Lapack / Blas

Calculation of the lightest CP-even Higgs mass using the EFT framework requires

• SUSYHD version 1.0.2

To calculate dark matter predictions in the models requires

• micrOMEGAs version 4.1.8

The results reported in arXiv:1610.03374 were obtained using

• SARAH-4.5.6 running on Mathematica 10.0
• FlexibleSUSY-1.1.0
• g++ and gfortran, version 4.8.2
• Boost version 1.60.0
• Eigen version 3.2.8
• GSL version 1.15
• SUSYHD-1.0.2
• micrOMEGAs-4.1.8

Analytic Expressions

Analytic expressions for the mass matrices, loop corrections and renormalization group equations can be generated using the SARAH model files found under ./sarah. To run the SARAH model, a new model must first be created in your SARAH installation, for example,

    $ mkdir /path/to/SARAH/Models/SE6SSM
    $ cp ./sarah/* /path/to/SARAH/Models/SE6SSM/

The model can then be run within a SARAH session using Start["SE6SSM"];.

Mass Spectrum Calculation

Spectrum generators for the CSE6SSM and MSSM are located in the ./models directory. The compilation procedure is the same as documented for an ordinary FlexibleSUSY model. The Makefile is generated and the code built by running

    $ ./configure --with-models=CSE6SSM,MSSM
    $ make

The generated executables are located in the directory for the corresponding model. See ./configure --help for more options.

By default, only the two-scale spectrum generators are compiled. To also compile the semi-analytic solvers, the package should be configured using

    $ ./configure --with-models=CSE6SSM,MSSM --with-algorithms=semianalytic

Optionally, the lightest CP-even Higgs mass can be calculated using SUSYHD. To do so, install the FlexibleSUSY addon susyhd_call to the addons directory (see the documentation provided with the addon for how to do this). Executables calling SUSYHD can then be built using

    $ ./configure --with-addons=susyhd_call

After compiling with make, the executable ./models/CSE6SSM/run_susyhd_CSE6SSM.x can be used to compute the CP-even Higgs mass. Note that the approximation of using the MSSM EFT calculation is expected to be reasonable only when the additional exotic contributions to the mass are small. In general it is advisable to use a model specific EFT calculation, see for example the calculation provided by FlexibleEFTHiggs.

Dark Matter Calculations

micrOMEGAs models for the CSE6SSM and CMSSM are contained in the directories ./micro-models/CSE6SSM and ./micro-models/CMSSM, respectively. To run the dark matter calculation, the desired model should be added to your micrOMEGAs installation and compiled. The Makefiles for the models should first be generated by configuring with microMEGAs enabled, using

   $ ./configure --enable-micromegas --with-micromegas-dir=/path/to/micromegas

The models can then be added to your micrOMEGAs installation and used. For example, assuming the main micrOMEGAs package has already been compiled, the CSE6SSM model can be installed using

    $ make install-micro-CSE6SSM
    $ cd /path/to/micromegas/CSE6SSM
    $ make

Similar steps should be followed to install the CMSSM model.

After building the model, the executable run_slha_file.x is produced in the ./src sub-directory. It reads an SLHA file and, by default, computes the relic density for the point. For example,

    $ ./src/run_slha_file.x LesHouches.out

See ./src/run_slha_file.x --help for more options.

References

If you use this code in your work please cite

• P. Athron, D. Harries, R. Nevzorov, and A. G. Williams, Phys. Lett. B760, 19 (2016), arXiv:1512.07040 [hep-ph]
• P. Athron, D. Harries, R. Nevzorov, and A. G. Williams, (2016), arXiv:1610.03374 [hep-ph]

The analytic results and micrOMEGAs model files were produced using SARAH. Please also cite the appropriate references for SARAH,

• F. Staub, Comput. Phys. Commun. 181, 1077 (2010), arXiv:0909.2863 [hep-ph]
• F. Staub, Comput. Phys. Commun. 182, 808 (2011), arXiv:1002.0840 [hep-ph]
• F. Staub, Comput. Phys. Commun. 184, 1792 (2013), arXiv:1207.0906 [hep-ph]
• F. Staub, Comput. Phys. Commun. 185, 1773 (2014), arXiv:1309.7223 [hep-ph]

The C++ spectrum generators were produced using FlexibleSUSY, which itself also depends on SARAH and components of SOFTSUSY. If you use this aspect of the code, please cite the above as well as

• P. Athron, J.-h. Park, D. Stöckinger, and A. Voigt, Comput. Phys. Commun. 190, 139 (2015), arXiv:1406.2319 [hep-ph]
• B. C. Allanach, Comput. Phys. Commun. 143, 305 (2002), hep-ph/0104145
• B. C. Allanach, P. Athron, L. C. Tunstall, and A. G. Williams, Comput. Phys. Commun. 185, 2322 (2014), arXiv:1311.7659 [hep-ph]

If you use SUSYHD to compute the Higgs mass in the model, please cite

• J. P. Vega and G. Villadoro, JHEP 07, 159 (2015), arXiv:1504.05200 [hep-ph]

If you use this code to calculate dark matter predictions for the models, please cite the above as well as

• G. Bélanger, F. Boudjema, A. Pukhov, and A. Semenov, Comput. Phys. Commun. 149, 103 (2002), hep-ph/0112278
• G. Bélanger, F. Boudjema, A. Pukhov, and A. Semenov, Comput. Phys. Commun. 174, 577 (2006), hep-ph/0405253
• G. Bélanger, F. Boudjema, A. Pukhov, and A. Semenov, Comput. Phys. Commun. 176, 367 (2006), hep-ph/0607059
• G. Bélanger, F. Boudjema, A. Pukhov, and A. Semenov, Comput. Phys. Commun. 180, 747 (2009), arXiv:0803.2360 [hep-ph]
• G. Bélanger, F. Boudjema, P. Brun, A. Pukhov, S. Rosier-Lees, P. Salati, and A. Semenov, Comput. Phys. Commun. 182, 842 (2011), arXiv:1004.1094 [hep-ph]
• G. Bélanger, F. Boudjema, A. Pukhov, and A. Semenov, Comput. Phys. Commun. 185, 960 (2014), arXiv:1305.0237 [hep-ph]
• G. Bélanger, F. Boudjema, A. Pukhov, and A. Semenov, Comput. Phys. Commun. 192, 322 (2015), arXiv:1407.6129 [hep-ph]

License

This program is free software: you can redistribute it and/or modify it under the terms of the GNU General Public License as published by the Free Software Foundation, either version 3 of the License, or (at your option) any later version.

This program is distributed in the hope that it will be useful, but WITHOUT ANY WARRANTY; without even the implied warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the GNU General Public License for more details.

You should have received a copy of the GNU General Public License along with this program. If not, see http://www.gnu.org/licenses/.