sherpa.astro.ui.set_pileup_model(id, model=None)

Include a model of the Chandra ACIS pile up when fitting PHA data.

Chandra observations of bright sources can be affected by pileup, so that there is a non-linear correlation between the source model and the predicted counts. This process can be modelled by including the jdpileup model for a data set, using the set_pileup_model.


See also


Delete the pile up model for a data set.


Fit one or more data sets.


Return the pile up model for a data set.


The ACIS pile up model.


List of all the data sets with a pile up model.


Define the convolved model expression for a data set.


Set the source model expression for a data set.


The function does not follow the normal Python standards for parameter use, since it is designed for easy interactive use. When called with a single un-named argument, it is taken to be the model parameter. If given two un-named arguments, then they are interpreted as the id and model parameters, respectively.

This is a generic function, and can be used to model other non-linear detector effects, but at present the only available model is for the ACIS pile up provided by the jdpileup model.


Plot up the model (an xsphabs model multiplied by a powlaw1d component) and then overplot the same expression but including the effects of pile up in the Chandra ACIS instrument:

>>> load_pha('src.pi')
>>> set_source( *
>>> plot_model()
>>> set_pileup_model(jdpileup.jpd)
>>> plot_model(overplot=True)