Commit dab7c5832e6c2ae882eba17d80cd383105075b13

Authored by Luigi Tibaldo
1 parent 47dab4bf

started tutorial

doc/source/users/tutorials/1dc/classical_analysis.rst 0 → 100644
  1 +.. _classical_analysis:
  2 +
  3 +Performing a classical analysis
  4 +--------------------------------
  5 +
  6 + .. admonition:: What you will learn
  7 +
  8 + You will learn how to perform a *classical* atmospheric Cherenkov analysis
  9 + of a source. In thys type of analysis you do not need to have a 3D (spatial
  10 + and spectral) model of the residual hadronic background. First you create a
  11 + skymap to identify a source region. Then, you extract the measured counts
  12 + from the source region and from one or more background regions, and perform
  13 + a 1D maximum likelihood analysis to derive the source's spectrum.
  14 +
  15 +We will assume that you have selected the observations available around your
  16 +source of interest. You can do this using the :ref:`csobsselect` script.
  17 +
  18 +We will derive the spectrum of a source with known position, i.e., the supernova
  19 +remnants Cassiopeia A. First, you want to create a skymap to identify the source
  20 +region. You can do this using the :ref:`ctskymap` tool.
  21 +
  22 +.. code-block:: bash
  23 +
  24 +In the spirit of the classical analysis we have chosen to derive the background
  25 +using the RING method. You need to choose inner/outer radii such that you avoid
  26 +emission from a source when deriving the background. This means that the inner
  27 +radius must be larger than the source's size, or the instrument PSF for a
  28 +pointlike source. This has produced a FITS file ``skymap.fits`` that contains
  29 +three images of the region around the source. The primary image shows the excess
  30 +counts, i.e., the total number of counts minus the estimated background counts.
  31 +The BACKGROUND image shows the number of estimated background counts. Finally,
  32 +the SIGNIFICANCE image shows the significance of the excess, calculated
  33 +according to Li&Ma
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