CLUMPY v3: γ-ray and ν signals from dark matter at all scales
CLUMPY v3: γ-ray and ν signals from dark matter at all scales
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DOI：
10.1016/j.cpc.2018.10.001
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发表时间：
2018-06
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影响因子：
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通讯作者：
M. Hütten;C. Combet;D. Maurin
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作者：
M. Hütten;C. Combet;D. Maurin
本文介绍了用于计算暗物质结构中湮灭或衰变的γ射线和ν信号的CLUMPY程序的第三版。这个版本包括河外信号的平均值，以及与宇宙学参数、暗物质结构的质量函数和高红移的γ射线吸收相关的几个预定义选项和关键词。为了更加灵活和一致，暗物质晕质量和浓度现在是根据用户定义的过密度Δ来定义的。我们还为用户的利益做了一些改变：通过git分发和版本化代码，减少依赖和简化安装，更好地处理运行命令行中的选项，一致的参数命名，以及http：//lpsc上的新Sphinx文档。在2 p3中。fr/clu/.程序摘要程序标题：笨重的程序文件doi：http：//dx. doi。org/10.17632/4n33mbh9bc。1许可条款：GPLv 2编程语言：C/C++外部例程/库：GSL（http：//www.gsl.com）gnu。org/software/gsl），cfitsio（http：//heasarc. gsfc。太空总署gov/fitsio/fitsio。html）、CERN ROOT（http：//root.欧洲核子研究中心。ch;可选，用于晕子结构的交互式图形和随机模拟），GreAT（http：//lpsc.在2 p3中。fr/great;问题的性质：计算在任何红移z处暗物质湮灭/衰变的γ射线和ν信号。解决方法：此版本中的新功能：质量函数、吸收和强度乘数（与沿着视线的DM密度相关）的矩（红移和质量）的数值积分。限制条件：来自暗物质轻子的次级辐射，取决于天体物理成分（宇宙中的辐射场），是最后一个缺失的部分，可以提供对预期信号的完整描述。
We present the third release of the CLUMPY code for calculating γ-ray and ν signals from annihilations or decays in dark matter structures. This version includes the mean extragalactic signal with several pre-defined options and keywords related to cosmological parameters, mass functions for the dark matter structures, and γ-ray absorption up to high redshift. For more flexibility and consistency, dark matter halo masses and concentrations are now defined with respect to a user-defined overdensity Δ. We have also made changes for the user’s benefit: distribution and versioning of the code via git, less dependencies and a simplified installation, better handling of options in run command lines, consistent naming of parameters, and a new Sphinx documentation at http://lpsc. in2p3. fr/clumpy/. Program summary Program Title: CLUMPY Program Files doi: http://dx. doi. org/10.17632/4n33mbh9bc. 1 Licensing provisions: GPLv2 Programming language: C/C++ External routines/libraries: GSL (http://www. gnu. org/software/gsl), cfitsio (http://heasarc. gsfc. nasa. gov/fitsio/fitsio. html), CERN ROOT (http://root. cern. ch; optional, for interactive figures and stochastic simulation of halo substructures), GreAT (http://lpsc. in2p3. fr/great; optional, for MCMC Jeans analyses) Nature of problem: Calculation of the γ-ray and ν signals from dark matter annihilation/decay at any redshift z. Solution method: New in this release: Numerical integration of moments (in redshift and mass) of the mass function, absorption, and intensity multiplier (related to the DM density along the line of sight). Restrictions: Secondary radiation from dark matter leptons, which depends on astrophysical ingredients (radiation fields in the Universe) is the last missing piece to provide a full description of the expected signal.