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Merge pull request #349 from LSSTDESC/internal_tracer_functions
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added functionality to return internal tracer functions (e.g. dndz)
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damonge committed Mar 21, 2018
2 parents b778440 + b3dda70 commit f6f2d48
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2 changes: 1 addition & 1 deletion doc/0000-ccl_note/main.tex
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Expand Up @@ -968,7 +968,7 @@ \section{Tests and validation}
\section{Examples for C implementation}
\label{sec:example}

Examples of how to run \ccl are provided in the {\tt tests} sub-directory of the library. The first resource for a new user should be the {\tt ccl$\_$sample$\_$run.c} file. This starts by setting up the \ccl default configuration. Then, it creates the ``cosmo'' structure, which contains distances and power spectra splines, for example. There are example calls for routines that output comoving radial distances, the scale factor, the growth factor and $\sigma_8$. Toy models are created for the redshift distributions of galaxies in the clustering and lensing samples, and for the bias of the clustering sample ($b(z)=1+z$). These are used for constructing the ``tracer'' structures via {\tt CCL$\_$Cltracer}, which can then be called to obtain the angular power spectra for clustering, cosmic shear and galaxy lensing.
Examples of how to run \ccl are provided in the {\tt tests} sub-directory of the library. The first resource for a new user should be the {\tt ccl$\_$sample$\_$run.c} file. This starts by setting up the \ccl default configuration. Then, it creates the ``cosmo'' structure, which contains distances and power spectra splines, for example. There are example calls for routines that output comoving radial distances, the scale factor, the growth factor and $\sigma_8$. Toy models are created for the redshift distributions of galaxies in the clustering and lensing samples, and for the bias of the clustering sample ($b(z)=1+z$). These are used for constructing the ``tracer'' structures via {\tt CCL$\_$Cltracer}, which can then be called to obtain the angular power spectra for clustering, cosmic shear and CMB lensing. All functions of redshift associated to each tracer can be retrieved at any arbitrary point using the same interpolation scheme used by \ccl internally.


\section{Python wrapper}
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Expand Up @@ -150,7 +150,7 @@ INLINE_INHERITED_MEMB = NO
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Expand Down Expand Up @@ -252,7 +252,7 @@ <h2 class="groupheader">Function Documentation</h2>
<tr><td class="paramname">na</td><td>Number of scale factors in a </td></tr>
<tr><td class="paramname">a</td><td>array of scale factors </td></tr>
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Expand Down Expand Up @@ -348,7 +348,7 @@ <h2 class="groupheader">Function Documentation</h2>
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<tr><td class="paramname">na</td><td>Number of scale factors in a </td></tr>
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<tr><td class="paramname">cosmo</td><td>Cosmological parameters </td></tr>
<tr><td class="paramname">a</td><td>scale factor, normalized to 1 for today </td></tr>
<tr><td class="paramname">label</td><td>species type. Available: 'matter' (0), 'dark_energy'(1), 'radiation'(2), and 'curvature'(3) </td></tr>
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<table class="params">
<tr><td class="paramname">cosmo</td><td>Cosmological parameters </td></tr>
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<tr><td class="paramname">nchi</td><td>Number of chis in chi </td></tr>
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<tr><td class="paramname">status</td><td>Status flag. 0 if there are no errors, nonzero otherwise. For specific cases see documentation for <a class="el" href="ccl__error_8c.html">ccl_error.c</a> </td></tr>
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</dd>
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<table class="params">
<tr><td class="paramname">cosmo</td><td>Cosmological parameters </td></tr>
<tr><td class="paramname">chi</td><td>Comoving radial distance of two objects </td></tr>
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