About Sherpa
Sherpa is the CIAO modeling and fitting application for Python made available by the Chandra Xray Center (CXC). Development takes place at the Sherpa GitHub repository and contibutions  whether new code, bug fixes, or documentation input  are welcome. Information on recent releases and citation information for Sherpa is available using the Digital Object Identifier (DOI) 10.5281/zenodo.593753.
Sherpa can be used for analysis of images, spectra and time series from many telescopes, including optical telescopes such as Hubble. It can also be easily used with nonAstronomical data. Sherpa is flexible, modular and extensible. It has an IPython user interface and it is also an importable Python module. Sherpa models, optimization and statistic functions are available via both C++ and Python for software developers wishing to link such functions directly to their own compiled code.
Sherpa supports fitting of 1D Xray spectra from Chandra and other Xray missions, as well as 1D nonXray data, including generic data arrays, radial profiles, and lightcurves. The options for grating data analysis include fitting the spectrum with multiple response files required for overlapping orders in LETG observations. Modeling of 2D spatial data is fully supported, including the PSF and exposure maps. User specified models can be added to Sherpa with advanced "user model" functionality.
A list of recent publications featuring the various uses of Sherpa may be found here.
The Sherpa website concentrates on using Sherpa within CIAO. There is also documentation for the "standalone" version of Sherpa which advanced users may find useful.
Features
 Python environment

Sherpa is an importable module for the Python scripting language, providing users with the ability to write their own Python scripts for use in Sherpa. This easily allows for creating complex analysis and modeling functions, building batchmode analysis, and extending the provided functionality to meet required needs.
 Multiple startup options

There are six commandline options which may be specified when Sherpa is started:
 h
Provide help on the options.
 x
launch sherpa shell in separate display terminal.
 b
Run in batch mode.
 n
Do not print banner on start up.
 rcfile <filename>
Specify a specific .sherpa.rc file to use; refer to "ahelp sherparc" for details.
 norcfile
Do not load any .sherpa.rc file; overrides rcfile if both are set.

The Sherpa application uses the $HOME/.ipythonciao/ directory to store configuration information. The first time Sherpa s started you may see a message about old IPython profile information being found.
unix% sherpa ATTENTION: The IPython profile found in $HOME/.ipythonciao//profile_sherpa is not compatible with this version of sherpa. Update to a compatible version? [Y/N]:
Unless you have manually changed the file it is safe to answer "Y" here. The outdated file is renamed with a timestamp to preserve it.
 Visualization

For plotting, Sherpa uses Matplotlib. Image visualization is provided by DS9.
 Parallelization

The following computationally intensive functions are parallelized to make use of multicore systems, providing users with such systems significant improvements in efficiency compared to previous releases of Sherpa. Each function has a "numcores" option to specify the number of cores to use in parallelization; the default is to use all cores available.
 Access to data structures

In addition to the normal mode of loading data from files, Sherpa allows you to manipulate the data arrays internally at the Python prompt and then "reload" them before fitting and modeling further. The resulting data may be manipulated without writing it to a file, making it easy to incorporate into scripts.

The analysis of data from modern instruments requires a flexible modeling and fitting system. The Sherpa infrastructure provides the user with an environment to develop complex and sophisticated analysis that goes beyond the default Sherpa functionality. Examples of usercontributed Python packages which extend Sherpa's functionality are Deproject and Cosmocalc (although the cosmology routines provided by AstroPy are to be preferred to Cosmocalc nowadays). The DataStack support was a userprovided extension but was integrated into Sherpa in CIAO 4.7.
The standalone Sherpa project allows users to install  and develop  Sherpa outside of CIAO. This allows users to combine Sherpa with external packages  such as SciPy and AstroML  which may not be easily installed into the CIAO directory structure.
Support for installing Python packages into CIAO has been greatly improved with the CIAO 4.11 release, and CIAO 4.12 was the first release of CIAO (and hence Sherpa including the XSPEC model library) using the conda package manager.
 User Interface

There are many functions available for accessing internal data, model data, fit and projection results, plotting objects, etc., in a Sherpa session. These provide the user with easy access and interaction with the system required by modern data analysis. Examples of such functions include:
 show_data()
 show_bkg()
 show_model()
 show_filter()
 show_fit()
 show_all()
 get_arf()
 get_rmf()
 get_response()
 get_bkg_scale()
 get_backscal()
 get_conf_results()
 get_data_plot_prefs()
 get_delchi_plot()
The much longer list of get*, set*, show*, etc., functions may be accessed by typing, e.g., "*get*?" at the Sherpa prompt.
 Optimization methods

There are four optimization methods available in Sherpa: "levmar", a modification of the LevenbergMarquardt algorithm which uses the LMDIF algorithm; "neldermead", A NelderMead Simplex direct search; "moncar", a Monte Carlo method  differential evolution  based on the paper by Hedar & Fukushima; and "gridsearch", a grid searching method available for fitting data with Sherpa template models. These algorithms are robust and show very good convergence required by modern data analysis.
The Sigmarejection iterative fitting method in Sherpa allow the chosen optimization method to be called multiple times during a fit, instead of just once, until the fit can no longer be improved. the Sigmarejection method excludes poorly fit data points at each successive fit. Primini method was removed in CIAO 4.15.
 Statistics

There are several choices of fit statistic in Sherpa, including MaximumLikelihood based ones (cash, cstat, and wstat) and many options of weighted χ^{2} statistics. The full list is:
 cash
 cstat
 wstat

χ^{2} statistics:
 leastsq
 chi2constvar (CHI PARENT  CVAR)
 chi2datavar (CHI DVAR)
 chi2gehrels (CHI GEHRELS)
 chi2modvar (CHI MVAR)
 chi2xspecvar
Descriptions of all available fit statistics are provided on the Sherpa Statistics page.

The Sherpa interface also provides an easy way to define new statistics required for analysis by the user. The load_user_stat function accommodates userdefined functions for a statistic and statistical errors, in addition to defining a list of model parameters and hyperparameters for prior distributions (if prior desired).
 Parameter Uncertainty and Confidence

Confidence and covariance calculate the confidence range for the bestfit model parameters; intervalprojection and regionprojection provide a way to visualize the model constraints on the bestfit parameter values. The results are easily accessible with the user functions get_conf_results and get_covar_results.
The PPP statistic function plot_pvalue (with associated get_pvalue_results and get_pvalue_plot functions) performs a likelihood ratio test to compare a fit to data done with a simple, null model versus a more complex, alternative model. This function helps users determine if the fitted model is statistically significant compared to the null model.
The sample_flux function calculates the flux and flux uncertainty due to a subcomponent of a Sherpa model, returning the model parameter values and associated fluxes from each of the userspecified number of simulations, along with the median flux value and the lower and upper quantiles defined by the confidence level supplied to the function.
 Models

Sherpa allows the user to define customized models and provides several flexible options for defining complex model expressions for fitting data.

Multicomponent, multiresponse expressions
Complex model expressions which apply response matrices, or PSFs, to some model components, while not applying the response or the PSF to the rest of the model expression, may be defined with the set_full_model and set_bkg_full_model functions. This allows for including both convolved and unconvolved model components in a single model expression for fitting source and/or background data.
There are plotting functions available for visualizing the contribution of individual model components to a fit of a multicomponent model to data. These functions can accept one or multiple Sherpa model components. Similarly, users can view 2D model components in DS9.
 plot_model_component()
 plot_source_component()
 get_model_component_plot()
 get_source_component_plot()
 image_model_component()
 image_source_component()
 get_model_component_image()
 get_source_component_image()
 get_model_component()
It is possible to simultaneously fit multiple data sets with each independent source model convolved by a different PSF model.

User models
The add_model function may be used to register a userdefined Sherpa model class as a Sherpa model type, to create instances of models that are recognized automatically in Sherpa model expressions.
The Sherpa table model reads data from a file or crate and assigns it to an instance of the table model class that can be combined arithmetically with the source model. It supports additive and multiplicative XSpecstyle table models, as well as linear interpolation of data points on the data set grid from the model grid supplied from file.
The Sherpa template model can read in a collection of templates from a directory full of template files, and can compare a data set to all the templates in that collection. Sherpa finds the template that best matches the data, and reports back the parameter values associated with that template.
Both the table and template models support linear, nearestneighbor, and polynomial interpolation.
 Fitting

The fit_bkg function is available for fitting only background data sets when fitting with PHA spectral data. The function's list of arguments is the same as the fit function.
Iterative fitting can be done with the Primini and Sigmarejection methods using the following functions:
calc_stat_info and get_stat_info give the full statistical information based on the current models.
 Filtering and Grouping Data

The following grouping functions are avaible for grouping PHA channel data. These functions use the CIAO group module to group data in various ways:
 group_bins  Group into a specified number of bins
 group_width  Group so there are N channels in each group
 group_counts  Group by a number of counts
 group_snr  Group by a signaltonoise value
 group_adapt  Adaptively bin based on the number of counts
 group_adapt_snr  Adaptively bin based on a signaltonoise value
 Saving the Sherpa Session

save_all command saves all the settings which define the current Sherpa session to an ASCII file. The resulting file can be read into a future Sherpa session to recreate the data, models, filter, grouping and quality flags, statistic and method used at that time.

The save command creates a binary file that can be restored in Sherpa with the restore.
 Advanced options

Bayesian analysis with pyBLoCXS
pyBLoCXS, a sophisticated Markov chain Monte Carlo based algorithm designed to carry out Bayesian LowCount Xray Spectral (BLoCXS) analysis in the Sherpa environment, is available via the functions listed below. (For more information on BLoCXS, see van Dyk, D.A., Connors, A., Kashyap, V.L., & Siemiginowska, A. 2001, Ap.J., 548, 224, "Analysis of Energy Spectra with Low Photon Counts via Bayesian Posterior Simulation")
 get_draws()
 list_priors()
 set_prior()
 get_prior()
 list_samplers()
 set_sampler()
 set_sampler_opt()
 get_sampler()
 get_sampler_opt()
 get_sampler_name()
The code is a Python extension to Sherpa that explores parameter space at a suspected minimum using a predefined Sherpa model to highenergy Xray spectral data. The get_draws function runs a pyBLoCXS chain using fit information associated with the specified data set(s), and the currently set sampler and parameter priors, for a specified number of iterations. It returns an array of statistic values, an array of acceptance Booleans, and a 2D array of associated parameter values.