1.1 HOW-TO Calibrations: overview

The calibration part of the Astro-WISE Environment is divided into three major pipelines: a bias pipeline, a flat field pipeline, and a photometric pipeline. All of these are composed of several fine-grained, atomic processing steps known as tasks. In the following sections, these pipelines are discussed. A summary is given of the atomic tasks that make up the various pipelines, and their place therein is described. Also given are a few examples of how the different tasks can be steered through the DPU interface. For the interface and use of every individual task, please read the corresponding HOW-TO.

1.1.1 The atomic tasks and their context

The atomic tasks that make up the calibration pipelines are summarized in Table [*], together with their role in the system and the identifier under which these are known to the DPU interface.

The sequence of tasks that make up the bias and flat field pipelines is shown in Figure [*]. The sequence of tasks that should be run for the photometric calibration is shown in Figure [*]. In these figures, each one of the individual tasks is represented by one box. The arrows indicate the flow of the pipeline, and the shaded parts show particular (optional) branches therein. The bias and flatfield pipelines

The bias and flat field pipelines are pretty straightforward: no difficulties or surprises here. Note, however, that after having derived the masterflat, the processing continues in the photometric pipeline (hence the arrow at the end of the line in Fig. [*]). The photometric pipeline

The photometric pipeline is more tricky than the bias or flatfield pipeline for two reasons: (1) a piece of the image pipeline must be run to process the photometric standard fields (hence the Reduce and Astrometry boxes in Fig. [*]), (2) the optional branch of the illumination correction is an iterative loop that in Fig. [*] actually runs backwards (characterising the illumination variation is more of an interactive process).

Table: The atomic processing steps that make up the various calibration pipelines and the identifiers through which these can be selected by the user from the DPU interface. Note that not all processing steps are available through the DPU interface.
  Processing step Purpose DPU identifier
Bias pipeline ReadNoise Deriving the read noise ReadNoise
  Bias Creating a master bias Bias
  HotPixels Creating a hotpixel map HotPixels
  Gain Derive the gain Gain
Flat field pipeline DomeFlat Creating a domeflat DomeFlat
  ColdPixels Creating a coldpixel map ColdPixels
  TwilightFlat Creating a twilightflat TwilightFlat
  MasterFlat Creating a masterflat MasterFlat
  FringeFlat Creating a fringeflat FringeFlat
Photometric pipeline PhotCalExtractResulttable Measuring fluxes of standard stars Photcat
  PhotCalExtractZeropoint Deriving the zeropoint Photom
  PhotCalMonitoring1 Monitoring the atmosphere -
  IlluminationCorrectionVerify1 Characterizing illumination variations -
  IlluminationCorrection Creating an illumination correction frame -
1 This processing step is performed on a single node

Figure: The order and flow of the atomic processing steps in the bias and flat field pipelines. The lightly shaded parts show the (optional) branches.

Figure: The order and flow of the atomic processing steps needed to do the photometric calibration. The lightly shaded parts show the (optional) branches.

1.1.2 Examples of running the atomic tasks with the DPU

Make master biases for all CCDs of OmegaCAM for a certain bias template:

    awe> dpu.run('Bias', instrument='OMEGACAM', template='2014-07-04T10:39:28')

Make a twilightflat for the specified night and filter:

    awe> dpu.run('TwilightFlat', i='OMEGACAM', d='2014-06-29', f='OCAM_r_SDSS')
Make photometric catalogs from a particular standard field exposure:
    awe> dpu.run('Photcat', i='OMEGACAM', raw=['OMEGACAM.2014-04-26T23:55:32.384_32.fits'])

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