spimodfit_analysis script

A set of standard parameters based on the ones used for the SPI quick look analysis available at the MPE

http://www.mpe.mpg.de/gamma/instruments/integral/www/integral-data.html

is implemented in the script spimodfit_analaysis that is delivered for a more user friendly utilization of spimodfit .

The first steps before the background calculation are the same of spi_science_analysis. The energy channels of the input data and the set of detectors which are used must be coherently set between the binning and spectral extraction steps.

Regarding the background the default option is the calculation internal to spimodfit . The time variability is set by default to account for variability on science window time scale and at each annealing or detector failure. A feature which regards the ``background multipliers'' is introduced to account for different efficiency of the pixels. The relative default time variability accounts for the annealings and detector failures, and a monthly timescale variation to be fitted.

In case the user would like to use the external background, the parameter background_input_file should be set to back_model_idx.fits[1]. Either the flatfield, template or model options can be used. For the flatfield option, the option spi_flatfield_single should be set to yes, as done in the default settings. Furthermore, a combination of several background models can be used by setting the appropriate parameters. For this option and the introduction of images for the diffuse emission models, we refer to the spimodfit handbook. However, we warn the reader that the full exploitation of these and more advanced features should be carried out in touch with the experts at MPE. In Fig. , we show the GUI with the standard settings for a flat-field background and logarithmically increasing energy binning.

Figure: GUI with the standard settings for a flat-field background and logarithmically increasing energy binning.

Finally, the spimodfit final products are not attached to the observation group, decoupling the spectral extraction step from the previous ones. The program can then be used separately once the data are binned and the optional background is created, without the need of running any DAL tool to clean the observation group. However, the side effect is that the user should delete the output files by hand if he/she wants to run spimodfit another time since the program does not replace existing files. In Fig. , we show the GUI with the standard settings for internal background computation, no image fitting and standard background multipliers.

Figure: GUI with the standard settings for internal background computation, no image fitting and standard background multipliers.