documentation change

docs/index.rst

@@ -44,6 +44,7 @@ We are using Astropy's excellent workflow - more details can be found at `<http:
     installation
     running
     gui
+    uses
     atomic
     plasma
     montecarlo

docs/running.rst

@@ -47,37 +47,3 @@ Graphical User Interface
 
 A graphical user interface is being developed for this code using QT. We envision to have this available in the next few minor releases.
 
-
-**************************
-What can I do with TARDIS?
-**************************
-
-TARDIS is designed to carry out calculations of synthetic supernova spectra (see Kerzendorf & Sim 2014). A TARDIS calculation requires
-
-1) a model for the supernova eject (density and composition distribution) to be specified;
-2) parameters determining the physical and numerical properties of the code are give.
-
-These inputs are specified via the input file (yaml file). As a starting point, examine the input file in the example download (above). The example file sets up a very simple model in which the density distribution is based on the well-known W7 model () and in which uniform abundances are specified. To get you started, here is a short list of settings that can be experimented with to get a feel for using TARDIS. Please contact us if you have questions or woudl like information on more advanced possibilities!
-
-Change the abundances
----------------------
-
-In the example file you can alter the elemental abundances (mass fractions; specified in the "abundances" section). Use this to explore the sensitivity of features to composition.
-
-Change the luminosity
----------------------
-
-You can alter the (emergent) luminosity and see how this affects the synthetic spectrum. Do this by varying the "luminosity requested" in the "supernova" section.
-
-Change the epoch
-----------------
-
-In the example file, you can change the epoch for which the synthetic spectrum is calculated (change the value of "time explosion"; specified in the "supernova" section). When doing this you might also change the inner boundary velocity ("start" value in the "velocity" section), and probably the luminosity (see above)!
-
-Experiment with the treatment of line opacity
----------------------------------------------
-
-In the "plasma" section you can change the "line interaction type" between "scatter", "downbranch" and "macroatom" - investigate how important fluorescence is in your synthetic spectrum. (See Kerzendorf & Sim and references therein for the meaning of these settings.)
-
-
-

docs/uses.rst

@@ -0,0 +1,33 @@
+**************************
+What can I do with TARDIS?
+**************************
+
+TARDIS is designed to carry out calculations of synthetic supernova spectra (see Kerzendorf & Sim 2014). A TARDIS calculation requires
+
+1) a model for the supernova eject (density and composition distribution) to be specified;
+2) parameters determining the physical and numerical properties of the code are give.
+
+These inputs are specified via the input file (yaml file). As a starting point, examine the input file in the example download (above). The example file sets up a very simple model in which the density distribution is based on the well-known W7 model () and in which uniform abundances are specified. To get you started, here is a short list of settings that can be experimented with to get a feel for using TARDIS. Please contact us if you have questions or woudl like information on more advanced possibilities!
+
+Change the abundances
+===============
+
+In the example file you can alter the elemental abundances (mass fractions; specified in the "abundances" section). Use this to explore the sensitivity of features to composition.
+
+Change the luminosity
+==============
+
+You can alter the (emergent) luminosity and see how this affects the synthetic spectrum. Do this by varying the "luminosity requested" in the "supernova" section.
+
+Change the epoch
+===========
+
+In the example file, you can change the epoch for which the synthetic spectrum is calculated (change the value of "time explosion"; specified in the "supernova" section). When doing this you might also change the inner boundary velocity ("start" value in the "velocity" section), and probably the luminosity (see above)!
+
+Experiment with the treatment of line opacity
+=============================
+
+In the "plasma" section you can change the "line interaction type" between "scatter", "downbranch" and "macroatom" - investigate how important fluorescence is in your synthetic spectrum. (See Kerzendorf & Sim and references therein for the meaning of these settings.)
+
+
+