Merge branch '1646-add-cstssplit-to-docs' into integration

Jürgen Knödlseder
2 parents 3064f16a 3d4fd4b7
Showing 1 changed file with 360 additions and 294 deletions
doc/source/users/user_manual/iact_analysis/tips.rst
@@ -2,245 +2,269 @@
  
 Tips, Tricks and FAQs
 =====================
-This section shows some of the wrinkles that could fascilitate the users' life when running IACT analyses.
+This section shows some of the wrinkles that could ease your life when
+running IACT analyses.
+
  
 Visualise observations
 ----------------------
-A very common task is to inspect the observation container and visualise several quantities.
+A very common task is to inspect the observation container and visualise several
+quantities.
  
 Create a skymap of counts
 ^^^^^^^^^^^^^^^^^^^^^^^^^
-The tool :ref:`ctskymap` allows to create a single map of counts contained inside an observation container.
-In contrast to :ref:`ctbin`, ctskymap takes into account all events that fall into the skymap energy range and spatial range.
-Since :ref:`ctbin` is intended for binned/stacked analysis, it respects energy thresholds, RoI selections etc.
-Accordingly, :ref:`ctskymap` could be used for a simple visualisation of the counts.
-
+The tool :ref:`ctskymap` allows to create a single map of counts contained
+inside an observation container. In contrast to :ref:`ctbin`, ctskymap takes
+into account all events that fall into the skymap energy range and spatial
+range. Since :ref:`ctbin` is intended for stacked analysis, it respects energy
+thresholds, RoI selections, etc. In contrast, :ref:`ctskymap` may be used for
+a simple visualisation of the counts.
  
 .. code-block:: bash
  
-	$ ctskymap debug=yes
-	Input event list or observation definition XML file [events.fits] obs.xml 
-	Lower energy limit (TeV) [0.1] 
-	Upper energy limit (TeV) [100.0] 
-	First coordinate of image center in degrees (RA or galactic l) (0-360) [83.63] 
-	Second coordinate of image center in degrees (DEC or galactic b) (-90-90) [22.01] 
-	Projection method (AIT|AZP|CAR|MER|MOL|STG|TAN) [CAR] 
-	Coordinate system (CEL - celestial, GAL - galactic) (CEL|GAL) [CEL] 
-	Image scale (in degrees/pixel) [0.02] 
-	Size of the X axis in pixels [200] 
-	Size of the Y axis in pixels [200] 
-	Output skymap file [skymap.fits] 
-	
-Alternatively, one could use count cube and collapse the maps into one single image via Python:
+   $ ctskymap debug=yes
+   Input event list or observation definition XML file [events.fits] obs.xml
+   Lower energy limit (TeV) [0.1]
+   Upper energy limit (TeV) [100.0]
+   First coordinate of image center in degrees (RA or galactic l) (0-360) [83.63]
+   Second coordinate of image center in degrees (DEC or galactic b) (-90-90) [22.01]
+   Projection method (AIT|AZP|CAR|MER|MOL|STG|TAN) [CAR]
+   Coordinate system (CEL - celestial, GAL - galactic) (CEL|GAL) [CEL]
+   Image scale (in degrees/pixel) [0.02]
+   Size of the X axis in pixels [200]
+   Size of the Y axis in pixels [200]
+   Output skymap file [skymap.fits]
+	
+Alternatively, you may start from a counts cube and collapse the maps into one
+single map via Python:
  
 .. code-block:: python
  
-   import gammalib
-   map = gammalib.GSkyMap("myCountCube.fits") # Loads the count cube
-   map.stack_maps() # Stack energy slices
-   map.save("myCountMap.fits") # Save to file
+   >>> import gammalib
+   >>> map = gammalib.GSkyMap("myCountCube.fits") # Load counts cube
+   >>> map.stack_maps()                           # Stack all cube maps into a single map
+   >>> map.save("myCountMap.fits")                # Save map to file
  
 Create region file of pointings
 ^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^
-In particular, one might want to know how the pointings of the observation container distribute across the sky.
-For this purpose, :ref:`csobsinfo` provides the hidden parameter ``ds9file`` which signals to produce a region file that
-contains these information:
+You may want to know how the pointings of the observation container distribute
+across the sky. For this purpose, :ref:`csobsinfo` provides the hidden parameter
+``ds9file`` which instructs the script produce a region file that contains the
+pointing information:
  
 .. code-block:: bash
  
-	$ csobsinfo ds9file=pointings.reg debug=yes
-	Event list, counts cube, or observation definition file [obs.xml] 
+   $ csobsinfo ds9file=pointings.reg debug=yes
+   Event list, counts cube, or observation definition file [obs.xml]
  
-Together with the previously produced skymap, one can plot the pointings using e.g. ds9:
+Together with the previously produced skymap, you can plot the pointings using
+for example ds9:
  
 .. code-block:: bash
  
-  $ ds9 skymap.fits -regions pointings.reg
+   $ ds9 skymap.fits -regions pointings.reg
+
  
 Plot zenith angle distribution of observations
 ----------------------------------------------
-The tool :ref:`csobsinfo` dumps more information into the log file. Some of them might be of interest to catch in a script.
-Therefore, one could simply use this tool via python and plot some distributions:
+The script :ref:`csobsinfo` logs information about an observation container
+into a log file. You may access the information through dedicated class methods
+and plot the information using for example matplotlib:
  
 .. code-block:: python
  
-  # Run script
-  import cscripts
-  info = cscripts.csobsinfo()
-  info["inobs"] = "selected_obs.xml"
-  info.run()
-  
-  # Plot data
-  import matplotlib.pyplot as plt
-  plt.hist(info.zeniths(), bins=10, range=[0,90])
-  plt.show()
+   >>> # Run script
+   >>> import cscripts
+   >>> info = cscripts.csobsinfo()
+   >>> info["inobs"] = "selected_obs.xml"
+   >>> info.run()
+
+   >>> # Plot data
+   >>> import matplotlib.pyplot as plt
+   >>> plt.hist(info.zeniths(), bins=10, range=[0,90])
+   >>> plt.show()
  
-This will plot a histogram showing the zenith angle distribution of the observation container. In addition there are more methods
-to access information in python:
+This example will plot a histogram showing the zenith angle distribution of the
+observation container. In addition there are more methods to access information
+in Python:
  
 .. code-block:: python
  
-  # csobsinfo can also return:
-  info.azimuths() # list of azimuth values
-  info.offsets()  # list of offset values (only computed if hidden parameter offset=yes was specified)
-  info.ebounds()  # gammalib.GEbounds object of energy ranges
-  info.gti()      # gammalib.GGti object containing good time intervals 
+   >>> info.azimuths() # list of azimuth values
+   >>> info.offsets()  # list of offset values (only computed if hidden parameter offset=yes was specified)
+   >>> info.ebounds()  # gammalib.GEbounds object of energy ranges
+   >>> info.gti()      # gammalib.GGti object containing good time intervals
  
-There is also an example script to plot several information about an observation container which might be useful
-for a quick visualisation of the observations inside a container:
+There is also an example script to plot information about an observation
+container which might be useful for a quick visualisation:
  
 .. code-block:: bash
  
-  $ python $CTOOLS/examples/show_obs.py selected_obs.xml
+   $ python $CTOOLS/examples/show_obs.py selected_obs.xml
+
  
 Visualise models
 ----------------
-Similar to :ref:`csobsinfo`, there is :ref:`csmodelinfo` to find out more about the content of a model XML file. In order to show the
-position and sizes of the model on top of a skymap, this tool has the hidden parameter ``ds9file``, too.
+Similar to :ref:`csobsinfo`, there is the :ref:`csmodelinfo` script to find out
+more about the content of a model XML file. In order to show the position and
+sizes of the model on top of a skymap, this tool has the hidden parameter
+``ds9file``, too.
  
 .. code-block:: bash
  
-	csmodelinfo ds9file=models.reg debug=yes
-	Input model XML file [$CTOOLS/share/models/crab.xml]
+   $ csmodelinfo ds9file=models.reg debug=yes
+   Input model XML file [$CTOOLS/share/models/crab.xml]
  
-There are several options regarding the color, text and other attributes of the region file. To see a full list, 
-:ref:`visit the reference page <csmodelinfo>`.
-Analogous to the pointings of the observation container, the models can be visualised using e.g. ds9:
+There are several options regarding the color, text and other attributes of the
+region file. To see a full list, :ref:`visit the reference page <csmodelinfo>`.
+Analogous to the pointings of the observation container, the models can be
+visualised using for example ds9:
  
 .. code-block:: bash
  
-  $ ds9 skymap.fits -regions models.reg
+   $ ds9 skymap.fits -regions models.reg
+
  
 Manipulating models in python
 -----------------------------
-This step will give some guidance how to work with model XML files in python and how to manipulate their content
+This example will give you some guidance on how to work with model XML files in
+Python and how to manipulate their content:
  
 .. code-block:: python
  
-	import gammalib
-	
-	# Open model file
-	models = gammalib.GModels("$CTOOLS/share/models/crab.xml")
-	
-	# Access a model component
-	src = models["Crab"]
-	print(src)
-	
-	# Retrieve the spectral or spatial component
-	print(src.spectral())
-	print(src.spatial())
-	
-	# Print the spectral parameter "Prefactor"
-	prefactor = src.spectral()["Prefactor"]
-	print("Prefactor: "+str(prefactor.value())+" +- "+str(prefactor.error()))
-	
-	# Set the prefactor value
-	prefactor.value(3.5e-17)
-	
-	# Loop over models and fix all parameters
-	for model in models:
-		
-		# Loop over model parameters
-		for par in model:
-			
-			# Fix parameter
-			par.fix()
-	
-	# Release one specific parameter
-	models["Crab"]["Prefactor"].free()
-	
-	# Set the parameter range
-	models["Crab"]["Prefactor"].min(1e-18)
-	models["Crab"]["Prefactor"].max(1e-16)
-	
-	# ... or in one step:
-	models["Crab"]["Prefactor"].range(1e-18, 1e-16)
-	
-	# Remove model from container
-	models.remove("Crab")
-	
-	# Save model to another XML file
-	models.save("mymodels.xml")
+   >>> import gammalib
+
+   >>> # Open model file
+   >>> models = gammalib.GModels("$CTOOLS/share/models/crab.xml")
+
+   >>> # Access a model component
+   >>> src = models["Crab"]
+   >>> print(src)
+
+   >>> # Retrieve the spectral or spatial component
+   >>> print(src.spectral())
+   >>> print(src.spatial())
+
+   >>> # Print the spectral parameter "Prefactor"
+   >>> prefactor = src.spectral()["Prefactor"]
+   >>> print("Prefactor: "+str(prefactor.value())+" +- "+str(prefactor.error()))
+
+   >>> # Set the prefactor value
+   >>> prefactor.value(3.5e-17)
+
+   >>> # Loop over models and fix all parameters
+   >>> for model in models:
+   >>>     for par in model:   # Loop over model parameters
+   >>>         par.fix()       # Fix parameter
+
+   >>> # Release one specific parameter
+   >>> models["Crab"]["Prefactor"].free()
+
+   >>> # Set the parameter range
+   >>> models["Crab"]["Prefactor"].min(1e-18)
+   >>> models["Crab"]["Prefactor"].max(1e-16)
+
+   >>> # ... or in one step:
+   >>> models["Crab"]["Prefactor"].range(1e-18, 1e-16)
+
+   >>> # Remove model from container
+   >>> models.remove("Crab")
+
+   >>> # Save model to another XML file
+   >>> models.save("mymodels.xml")
  
  
-Retrieve likelihood values from :ref:`ctlike`
----------------------------------------------
-For some purposes, it might be useful to retrieve the fitted likelihood value and other results of the fit with :ref:`ctlike`.
+Retrieve likelihood values from ctlike
+--------------------------------------
+For some purposes, it might be useful to retrieve the fitted likelihood value
+and other results of the fit with :ref:`ctlike`.
  
 .. code-block:: python
  
-	import gammalib
-	import ctools
-	
-	# Create ctlike
-	like = ctools.ctlike()
-	like["inobs"]   = "selected_obs.xml"
-	like["inmodel"] = "mymodels.xml"
-	like.run()
-	
-	# Get optimizer from ctlike
-	opt = like.opt()
-	print(opt)
-	
-	# Get likelihood value from optimizer
-	print(opt.value())
-	
-	# Get fit status:
-	print(opt.status())
-	# 0: converged
-	# 1: stalled
-	# 2: singular curvature matrix encountered
-	# 3: curvature matrix not positive definite
-	# 4: errors are inaccurate
+   >>> import gammalib
+   >>> import ctools
+
+   >>> # Create and run ctlike
+   >>> like = ctools.ctlike()
+   >>> like["inobs"]   = "selected_obs.xml"
+   >>> like["inmodel"] = "mymodels.xml"
+   >>> like.run()
+
+   >>> # Get optimizer from ctlike
+   >>> opt = like.opt()
+   >>> print(opt)
+
+   >>> # Get likelihood value from optimizer
+   >>> print(opt.value())
+
+   >>> # Get fit status:
+   >>> print(opt.status())
+   >>> # 0: converged
+   >>> # 1: stalled
+   >>> # 2: singular curvature matrix encountered
+   >>> # 3: curvature matrix not positive definite
+   >>> # 4: errors are inaccurate
+
  
 Speed up analysis
 -----------------
-In some cases it may occur that the analysis takes very long. There are several reasons that can slow down the analysis quite severly.
-Not all issues can be tackled. Nevertheless, here is a list of actions that have proven to speed up the fit.
+In some cases it may occur that the analysis takes very long. There are several
+reasons that can slow down the analysis quite severly. Not all issues can be
+tackled. Nevertheless, here is a list of actions that have proven to speed up
+the fit.
+
+* Consider switching to stacked analysis if the observation time exceeds 50-100
+  hours.
+* Diffuse and extended sources in the RoI are computational expensive. However,
+  in unbinned analysis they impact the speed much more.
+* Usage of energy dispersion could also cause a long fit. Try switching it off
+  if speed is important. Keep in mind this will have an effect on the results.
+* Switch to a machine that supports OpenMP. This allows to parallelise the fit
+  onto several cores.
  
-* Consider switching to binned analysis if the observation time exceeds 50-100 hours.
-* Diffuse and extended sources in the RoI are computational expensive. However, in unbinned analysis they impact the speed much more.
-* Usage of energy dispersion could also cause a long fit. Try switching it off if speed is important. Keep in mind this will have an effect on the results.
-* Switch to a machine that supports OpenMP. This allows to parallelise the fit onto several cores.
  
 Compute excess maps
 -------------------
-A very important means to visualise images of sources are excess maps. The tool :ref:`csresmap` can also be used to create such a map.
-The user, however, has to manually remove the source(s) of interest from the input model XML file.
+A very important means to visualise images of sources are excess maps. The script
+:ref:`csresmap` can also be used to create such a map. The user, however, has to
+manually remove the source(s) of interest from the input model XML file.
  
 .. code-block:: python
  
-  import gammalib
-  models = gammalib.GModels("crab_models.xml")
-  models.remove("Crab")
-  models.save("models_without_crab.xml")
+   >>> import gammalib
+   >>> models = gammalib.GModels("crab_models.xml")
+   >>> models.remove("Crab")
+   >>> models.save("models_without_crab.xml")
  
 Of course, this can also be done by editing the XML file with an editor.
  
-Subsequently, :ref:`csresmap` can be executed using the ``algorithm=SUB`` parameter:
+Subsequently, :ref:`csresmap` can be executed using the ``algorithm=SUB``
+parameter:
  
 .. code-block:: bash
  
-	$ csresmap
-	Input event list, counts cube, or observation definition XML file [selected_obs.xml]
-	Input model XML file [models_without_crab.xml]
-	First coordinate of image center in degrees (RA or galactic l) (0-360) [83.63] 
-	Second coordinate of image center in degrees (DEC or galactic b) (-90-90) [22.01] 
-	Coordinate System (CEL|GAL) [CEL] 
-	Projection method (AIT|AZP|CAR|MER|MOL|STG|TAN) [CAR] 
-	Size of the X axis in pixels [100]
-	Size of the Y axis in pixels [100]
-	Pixel size (deg/pixel) [0.02]
-	Residual map computation algorithm (SUB|SUBDIV|SUBDIVSQRT) [SUB]
-	Output residual map file [excessmap.fits] 
+   $ csresmap
+   Input event list, counts cube, or observation definition XML file [selected_obs.xml]
+   Input model XML file [models_without_crab.xml]
+   First coordinate of image center in degrees (RA or galactic l) (0-360) [83.63]
+   Second coordinate of image center in degrees (DEC or galactic b) (-90-90) [22.01]
+   Coordinate System (CEL|GAL) [CEL]
+   Projection method (AIT|AZP|CAR|MER|MOL|STG|TAN) [CAR]
+   Size of the X axis in pixels [100]
+   Size of the Y axis in pixels [100]
+   Pixel size (deg/pixel) [0.02]
+   Residual map computation algorithm (SUB|SUBDIV|SUBDIVSQRT) [SUB]
+   Output residual map file [excessmap.fits]
  
  
 Compute flux maps
 -----------------
-The creation of a flux map is much more expensive in terms of computing than an excess map. In the section about
-:ref:`high level analysis tools <sec_high_level>`, the usage of :ref:`cttsmap` was demonstrated. This tool can also
-be used to generate flux maps. For this, the user has to incoorporate a test source in the XML model file. This source
-should consist of a spectral component using a PowerLaw2 model:
+The creation of a flux map is much more expensive in terms of computing than an
+excess map. In the section about :ref:`high level analysis tools <sec_high_level>`,
+the usage of :ref:`cttsmap` was demonstrated. This tool can also be used to
+generate flux maps. For this, the user has to incorporate a test source in the
+XML model file. This source should consist of a spectral component using a
+PowerLaw2 model:
  
 .. code-block:: xml
  
@@ -257,24 +281,30 @@ should consist of a spectral component using a PowerLaw2 model:
 	 </spatialModel>
 	</source>
  
-The further content of the rest of the XML model file depends on the user requirements:
+The further content of the rest of the XML model file depends on the user
+requirements:
  
 * For an absolute flux map, all other sky models should be removed
 * For a residual flux map, all other sky models should be kept
  
-The tool :ref:`cttsmap` will create one skymap per free spectral parameter in the model. In the result FITS file,
-there will be an extension called "Integral" that contains the flux map. For the above XML example, the source name
-"TestSource" should be specified to :ref:`cttsmap`.
+The tool :ref:`cttsmap` will create one skymap per free spectral parameter in
+the model. In the result FITS file, there will be an extension called ``Integral``
+that contains the flux map. For the above XML example, the source name
+``TestSource`` should be specified to :ref:`cttsmap`.
+
  
 Speed up TS map computation
 ---------------------------
-Since the computation of a TS map can be extremely time consuming, the option of splitting the computation into several jobs
-is supported. This might be of particular interest if the user has access to a batch farm.
+Since the computation of a TS map can be extremely time consuming, the option of
+splitting the computation into several jobs is supported. This might be of
+particular interest if the user has access to a batch farm.
  
 Split TS map computation
 ^^^^^^^^^^^^^^^^^^^^^^^^
-For the purpose of job splitting, the hidden parameter ``binmin`` and ``binmax`` were included in the tool. These are integer parameter
-that specify which bins should be computed. For instance, if the map should consist of 30x30(=900) pixels, the user could e.g. execute
+For the purpose of job splitting, the hidden parameter ``binmin`` and ``binmax``
+were included in the tool. These are integer parameter that specify which bins
+should be computed. For instance, if the map should consist of 30x30(=900) pixels,
+the user could for example execute
  
 .. code-block:: bash
  
@@ -289,13 +319,46 @@ Each command could run on a different machine.
  
 .. note::
  
-  The output file name of individual jobs should be different. Otherwise files could overwrite each other. The naming of the individual slices
-  is up to the user.
+  The output file name of individual jobs should be different. Otherwise files
+  could overwrite each other. The naming of the individual slices is up to the
+  user.
  
-Merge sliced TS maps
-^^^^^^^^^^^^^^^^^^^^
-The tool :ref:`cstsmapmerge` is intended to take care of merging the files that were produced while splitting the TS map computation.
-There are several options to pass the files to be merged as arguments:
+The script :ref:`cstsmapsplit` will take care of this bookkeeping. It creates an
+ASCII file containing all the commands according to the user input. The following
+example will create split the computation of a TS map into 2000 separate task.
+Each task will only compute 5 bins on its own. This is very useful if the
+observation container is large or the fit simply takes a long time.
+
+.. code-block:: bash
+
+  $ cstsmapsplit
+  Input event list, counts cube or observation definition XML file [selected_obs.xml]
+  Input model definition XML file [$CTOOLS/share/models/crab.xml]
+  First coordinate of image center in degrees (RA or galactic l) (0-360) [83.63] 
+  Second coordinate of image center in degrees (DEC or galactic b) (-90-90) [22.01] 
+  Projection method (AIT|AZP|CAR|MER|MOL|STG|TAN) [CAR] 
+  Coordinate system (CEL - celestial, GAL - galactic) (CEL|GAL) [CEL] 
+  Image scale (in degrees/pixel) [0.02]
+  Size of the X axis in pixels [100]
+  Size of the Y axis in pixels [100]
+  Test source name [Crab] 
+  Output Test Statistic map file [tsmap.fits] 
+  Number of TS map bins per task [5] 
+  Compute null hypothesis first? [yes] 
+  ASCII file containing all commands [commands.dat] 
+  
+.. note::
+  
+  One can decide if we want to compute the null hypothesis first. This way, a
+  parameter optimisation will be performed without the test source. The obtained
+  likelihood value will then be passed to each individual task of :ref:`cttsmap`.
+  If ``compute_null=no``, each task has to compute the null hypothesis itself.
+  
+Merge splitted TS maps
+^^^^^^^^^^^^^^^^^^^^^^
+The script :ref:`cstsmapmerge` is intended to take care of merging the files
+that were produced while splitting the TS map computation. There are several
+options to pass the files to be merged as arguments:
  
 * a space-separated list of file names (e.g. tsmap1.fits tsmap2.fits)
 * a comma-separated list of file names (e.g. tsmap1.fits,tsmap2.fits)
@@ -306,132 +369,135 @@ In this example the ASCII file method is presented:
  
 .. code-block:: bash 
  
-	# Put slice files into an ascii file
-	$ ls tsmap_*.fits > tsmapfiles.txt
-	
-	# Run cstsmapmerge
-	$ cstsmapmerge
-	Input TS map FITS files [@tsmapfiles.txt]
-	Output TS map FITS file [mytsmap.fits]
+   # Put slice files into an ascii file
+   $ ls tsmap_*.fits > tsmapfiles.txt
+
+   # Run cstsmapmerge
+   $ cstsmapmerge
+   Input TS map FITS files [@tsmapfiles.txt]
+   Output TS map FITS file [mytsmap.fits]
  
  
 Creating a python analysis pipeline
 -----------------------------------
-It is easily possible to build an own analysis workflow with a simple python script. The following source code example shows a python script
-running from gathering observations until fitting spectral points without storing intermediate data products on disk. It assumes that the
-environment variable ``$VHEFITS`` is set to the path where IACT FITS data is located.
+It is easily possible to build an own analysis workflow with a simple python
+script. The following source code example shows a python script running from
+gathering observations until fitting spectral points without storing intermediate
+data products on disk. It assumes that the environment variable ``$VHEFITS`` is
+set to the path where IACT FITS data is located.
  
 .. code-block:: python
  
-	import gammalib
-	import ctools
-	import cscripts
-	
-	# Set debug flag
-	debug = True
-	
-	# Set flag to use energy dispersion
-	edisp = False
-	
-	# Set inmodel file name
-	inmodel = "$GAMMALIB/test/data/model_point_plaw.xml"
-	
-	# Expand environment variable
-	inmodel = gammalib.expand_env(inmodel)
-	
-	# Extract coordinates and model properties
-	models  = gammalib.GModels(inmodel)
-	srcname = models[0].name()
-	ra      = models[0]["RA"].value()
-	dec     = models[0]["DEC"].value()
-	
-	# Find FITS production name
-	iactdata          = cscripts.csiactdata()
-	iactdata["debug"] = debug
-	iactdata.run()
-	
-	# Use first available production
-	prodname = iactdata.names()[0]
-	
-	# Run csfindobs
-	findobs             = cscripts.csfindobs()
-	findobs["ra"]       = ra
-	findobs["dec"]      = dec
-	findobs["rad"]      = 2.5
-	findobs["prodname"] = prodname
-	findobs["debug"]    = debug
-	findobs["outfile"]  = "NONE"
-	findobs.run()
-	
-	# Retrieve obervation IDs (runlist)
-	obs_ids = findobs.obs_ids()
-	
-	# Build observation container
-	iactobs             = cscripts.csiactobs()
-	iactobs["prodname"] = prodname
-	iactobs["inmodel"]  = inmodel
-	iactobs["bkgpars"]  = 1
-	iactobs["outobs"]   = "NONE"
-	iactobs["outmodel"] = "NONE"	
-	iactobs["debug"]    = debug
-	iactobs.runlist(obs_ids)
-	iactobs.run()
-	
-	# Retrieve observation container and energy boundaries
-	obs     = iactobs.obs()
-	ebounds = iactobs.ebounds()
-	
-	# Run ctselect
-	select             = ctools.ctselect(obs)
-	select["usepnt"]   = True
-	select["rad"]      = 2.5
-	select["usethres"] = "DEFAULT"
-	select["tmin"]     = 0.0
-	select["tmax"]     = 0.0
-	select["emin"]     = 0.1
-	select["emax"]     = 100.0
-	select["debug"]    = debug
-	select.run()
-	
-	# Pass selected observations to ctlike
-	like          = ctools.ctlike(select.obs())
-	like["debug"] = debug
-	like["edisp"] = edisp
-	like.run()
-	
-	# Compute a spectrum and save
-	spec             = cscripts.csspec(like.obs())
-	spec["srcname"]  = srcname
-	spec["emin"]     = ebounds.emin().TeV()
-	spec["emax"]     = ebounds.emax().TeV()
-	spec["enumbins"] = 10
-	spec["edisp"]    = edisp
-	spec["ebinalg"]  = "LOG"
-	spec["debug"]    = debug
-	spec["outfile"]  = "spectrum.fits"
-	spec.execute()
-	
-	# Remove model for excess map computation
-	like.obs().models().remove(srcname)
-	
-	# Compute an excess map
-	resmap             = cscripts.csresmap(like.obs())
-	resmap["xref"]     = ra
-	resmap["yref"]     = dec
-	resmap["proj"]     = "CAR"
-	resmap["coordsys"] = "CEL"
-	resmap["emin"]     = ebounds.emin().TeV()
-	resmap["emax"]     = ebounds.emax().TeV()
-	resmap["nxpix"]    = 100
-	resmap["nypix"]    = 100
-	resmap["binsz"]    = 0.02
-	resmap["outmap"]   = "excessmap.fits"
-	resmap.execute()
-
-The results of this analysis workflow can be inspected using an example python script and e.g. ds9:
+   >>> import gammalib
+   >>> import ctools
+   >>> import cscripts
+
+   >>> # Set debug flag
+   >>> debug = True
+
+   >>> # Set flag to use energy dispersion
+   >>> edisp = False
+
+   >>> # Set inmodel file name
+   >>> inmodel = "$GAMMALIB/test/data/model_point_plaw.xml"
+
+   >>> # Expand environment variable
+   >>> inmodel = gammalib.expand_env(inmodel)
+
+   >>> # Extract coordinates and model properties
+   >>> models  = gammalib.GModels(inmodel)
+   >>> srcname = models[0].name()
+   >>> ra      = models[0]["RA"].value()
+   >>> dec     = models[0]["DEC"].value()
+
+   >>> # Find FITS production name
+   >>> iactdata          = cscripts.csiactdata()
+   >>> iactdata["debug"] = debug
+   >>> iactdata.run()
+
+   >>> # Use first available production
+   >>> prodname = iactdata.names()[0]
+
+   >>> # Run csfindobs
+   >>> findobs             = cscripts.csfindobs()
+   >>> findobs["ra"]       = ra
+   >>> findobs["dec"]      = dec
+   >>> findobs["rad"]      = 2.5
+   >>> findobs["prodname"] = prodname
+   >>> findobs["debug"]    = debug
+   >>> findobs["outfile"]  = "NONE"
+   >>> findobs.run()
+
+   >>> # Retrieve obervation IDs (runlist)
+   >>> obs_ids = findobs.obs_ids()
+
+   >>> # Build observation container
+   >>> iactobs             = cscripts.csiactobs()
+   >>> iactobs["prodname"] = prodname
+   >>> iactobs["inmodel"]  = inmodel
+   >>> iactobs["bkgpars"]  = 1
+   >>> iactobs["outobs"]   = "NONE"
+   >>> iactobs["outmodel"] = "NONE"
+   >>> iactobs["debug"]    = debug
+   >>> iactobs.runlist(obs_ids)
+   >>> iactobs.run()
+
+   >>> # Retrieve observation container and energy boundaries
+   >>> obs     = iactobs.obs()
+   >>> ebounds = iactobs.ebounds()
+
+   >>> # Run ctselect
+   >>> select             = ctools.ctselect(obs)
+   >>> select["usepnt"]   = True
+   >>> select["rad"]      = 2.5
+   >>> select["usethres"] = "DEFAULT"
+   >>> select["tmin"]     = 0.0
+   >>> select["tmax"]     = 0.0
+   >>> select["emin"]     = 0.1
+   >>> select["emax"]     = 100.0
+   >>> select["debug"]    = debug
+   >>> select.run()
+
+   >>> # Pass selected observations to ctlike
+   >>> like          = ctools.ctlike(select.obs())
+   >>> like["debug"] = debug
+   >>> like["edisp"] = edisp
+   >>> like.run()
+
+   >>> # Compute a spectrum and save
+   >>> spec             = cscripts.csspec(like.obs())
+   >>> spec["srcname"]  = srcname
+   >>> spec["emin"]     = ebounds.emin().TeV()
+   >>> spec["emax"]     = ebounds.emax().TeV()
+   >>> spec["enumbins"] = 10
+   >>> spec["edisp"]    = edisp
+   >>> spec["ebinalg"]  = "LOG"
+   >>> spec["debug"]    = debug
+   >>> spec["outfile"]  = "spectrum.fits"
+   >>> spec.execute()
+
+   >>> # Remove model for excess map computation
+   >>> like.obs().models().remove(srcname)
+
+   >>> # Compute an excess map
+   >>> resmap             = cscripts.csresmap(like.obs())
+   >>> resmap["xref"]     = ra
+   >>> resmap["yref"]     = dec
+   >>> resmap["proj"]     = "CAR"
+   >>> resmap["coordsys"] = "CEL"
+   >>> resmap["emin"]     = ebounds.emin().TeV()
+   >>> resmap["emax"]     = ebounds.emax().TeV()
+   >>> resmap["nxpix"]    = 100
+   >>> resmap["nypix"]    = 100
+   >>> resmap["binsz"]    = 0.02
+   >>> resmap["outmap"]   = "excessmap.fits"
+   >>> resmap.execute()
+
+The results of this analysis workflow can be inspected using an example Python
+script and for example ds9:
  
 .. code-block:: bash
  
-  $ python $CTOOLS/examples/show_spectrum.py spectrum.fits
-  $ ds9 excessmap.fits
+   $ python $CTOOLS/examples/show_spectrum.py spectrum.fits
+   $ ds9 excessmap.fits
  
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