Introduction to Fitting PHA Spectra
Sherpa Threads (CIAO 4.15 Sherpa)
Overview
Synopsis:
The basic steps used in fitting spectral data are illustrated in this thread. The data used herein were created by running the Creating ACIS Spectra for Pointlike Sources thread.
There are many options and variables that may affect how this process is applied to your data; for a more detailed explanation of the steps, see the following threads:
 Fitting Spectral Data: Fitting PHA Data with MultiComponent Source Models
 Fitting Spectral Data: Simultaneously Fitting Source and Background Spectra
For a detailed explanation of the fitting concepts behind Xray spectral analysis in Sherpa, see the document Spectral Fitting on the Sherpa References page.
Before fitting ACIS data sets with restricted pulseheight ranges, please read the CIAO caveat page "Spectral analyses of ACIS data with a limited pulseheight range."
Last Update: 28 Nov 2022  updated screen output for CIAO 4.15.
Contents
 Load the Spectrum & Instrument Responses
 Filter the Data & Subtract the Background
 Defining the Source Model
 Fitting
 Examining Fit Results
 Scripting It
 History

Images
 Figure 1: Plot of source spectrum
 Figure 2: Source spectrum, filtered and backgroundsubtracted
 Figure 3: Fit and sigma residuals
 Figure 4: How does the statistic vary with the gamma parameter?
 Figure 5: How does the statistic vary with the gamma and amplitude parameters?
 Figure 6: Tweaking the range
Load the Spectrum & Instrument Responses
First, load the spectrum file:
sherpa> load_pha("3c273.pi") WARNING: systematic errors were not found in file '3c273.pi' statistical errors were found in file '3c273.pi' but not used; to use them, reread with use_errors=True read ARF file 3c273.arf read RMF file 3c273.rmf WARNING: systematic errors were not found in file '3c273_bg.pi' statistical errors were found in file '3c273_bg.pi' but not used; to use them, reread with use_errors=True read background file 3c273_bg.pi
Since the RESPFILE, ANCRFILE, and BACKFILE header keywords were updated in the spectrum file, the response files (RMF and ARF) and background file are automatically read in as well. If the default dataset ID of "1" is to be used, it does not need to be explicitly included in the load function; only the data filenames are required in this case.
Sherpa issued a warning about systematic and statistical errors, which were not loaded. The statistical errors are calculated using the appropriate fit statistics set with set_stat in the Sherpa session. The standard treatment of systematic errors supplied with load_syserror is to add the array of systematic errors in quadrature to the statistical errors. Advanced methods to account for nonlinear calibration uncertainties described in Lee et al. (2011) are available within pyblocxs Bayesian functions. However, they require calibration products that are not available at this moment.
If Sherpa does not automatically read in the background and response files, read them manually:
sherpa> load_arf("3c273.arf") sherpa> load_rmf("3c273.rmf") sherpa> load_bkg("3c273_bg.pi")
Use show_all, show_data, and show_bkg to get the status of the Sherpa session. Some additional commands are used to get the total number of counts and counts rates calculated from the data.
sherpa> show_all() Data Set: 1 Filter: 0.001514.9504 Energy (keV) Bkg Scale: 0.134921 Noticed Channels: 11024 name = 3c273.pi channel = Float64[1024] counts = Float64[1024] staterror = None syserror = None bin_lo = None bin_hi = None grouping = Int16[1024] quality = Int16[1024] exposure = 38564.608926889 backscal = 2.5264364698914e06 areascal = 1.0 grouped = True subtracted = False units = energy rate = True plot_fac = 0 response_ids = [1] background_ids = [1] RMF Data Set: 1:1 name = 3c273.rmf energ_lo = Float64[1090] energ_hi = Float64[1090] n_grp = UInt64[1090] f_chan = UInt32[2002] n_chan = UInt32[2002] matrix = Float64[61834] e_min = Float64[1024] e_max = Float64[1024] detchans = 1024 offset = 1 ethresh = 1e10 ARF Data Set: 1:1 name = 3c273.arf energ_lo = Float64[1090] energ_hi = Float64[1090] specresp = Float64[1090] bin_lo = None bin_hi = None exposure = 38564.141454905 ethresh = 1e10 Background Data Set: 1:1 Filter: 0.001514.9504 Energy (keV) Noticed Channels: 11024 name = 3c273_bg.pi channel = Float64[1024] counts = Float64[1024] staterror = None syserror = None bin_lo = None bin_hi = None grouping = Int16[1024] quality = Int16[1024] exposure = 38564.608926889 backscal = 1.872535141462e05 areascal = 1.0 grouped = True subtracted = False units = energy rate = True plot_fac = 0 response_ids = [1] background_ids = [] Background RMF Data Set: 1:1 name = 3c273.rmf energ_lo = Float64[1090] energ_hi = Float64[1090] n_grp = UInt64[1090] f_chan = UInt32[2002] n_chan = UInt32[2002] matrix = Float64[61834] e_min = Float64[1024] e_max = Float64[1024] detchans = 1024 offset = 1 ethresh = 1e10 Background ARF Data Set: 1:1 name = 3c273.arf energ_lo = Float64[1090] energ_hi = Float64[1090] specresp = Float64[1090] bin_lo = None bin_hi = None exposure = 38564.141454905 ethresh = 1e10 sherpa> data_sum = calc_data_sum(id=1) # total counts (or values) in the data sherpa> print(data_sum) 736.0 sherpa> data_cnt_rate = calc_data_sum()/get_exposure(id=1) # calculating count rate in cts/sec sherpa> print(data_cnt_rate) 0.019084855790844735 sherpa> bkg_sum = calc_data_sum(bkg_id=1) # total counts (or values) in the background data sherpa> print(bkg_sum) 216.0 sherpa> bkg_cnt_rate = calc_data_sum(bkg_id=1)/get_exposure(bkg_id=1) # calculating background count rate in cts/sec sherpa> print(bkg_cnt_rate) 0.005600990286443563
Plot the data:
sherpa> plot_data()
The data are plotted in energy space—as seen in Figure 1—since the instrument model provides the information necessary to compute the predicted counts for each bin. In general, the units of the xaxis are determined by the value in the units field of the data, which may be accessed with 'print(get_data().units)' or show_filter, and modified with set_analysis.
Figure 1: Plot of source spectrum
Filter the Data & Subtract the Background
The CIAO 'Why' topic on Choosing an Energy Filter contains information on selecting energy range for spectral modeling. We can use the Sherpa ignore or notice functions to select the energy range between 0.3 and 6.0 keV. These functions are applied to all data sets. The other two functions, notice_id()/ignore_id(), require explicit input of the source data set ID, as the first argument; the second argument defines the lower energy of the range, and the third the higher energy of the range. These are useful for multiple data sets requiring different filters. The data between 0.3 and 6.0 keV will be noticed with the command:
sherpa> notice(0.3, 6.0) dataset 1: 0.00146:14.9504 > 0.2482:6.57 Energy (keV)
The notice_id filter will automatically be applied to the associated background data when the background data set ID (bkg_id) parameter is not used, as in the example in this thread. A different filter for the background may be set by issuing the notice_id or ignore_id command with the bkg_id entered as the fourth argument to the function.
with the change in the filter also reported, as bounded by the appropriate bin edges from the response energy grid. At this point, we also opt to subtract the background data:
sherpa> subtract() sherpa> plot_data()
Figure 2 shows the resulting plot.
Figure 2: Source spectrum, filtered and backgroundsubtracted
The axis scaling for all plots created in the current Sherpa session may be changed to log by calling set_xlog and set_ylog with no arguments (and changed back to linear with set_xlinear/set_ylinear):
sherpa> set_xlog() sherpa> set_ylog()
To set the plot axis scaling for a specific type of plot, e.g., model, data, or fit plots, the set_xlog/set_ylog or set_xlinear/set_ylinear commands should be called with the appropriate argument, either "data", "model", "source", "fit", or "delchi"—similar to those accepted by the generic Sherpa plot function.
CIAO 4.12 added support for sending in options to the plot calls, so you can also select a logarithmic scale on the yaxis for just a single pot with:
sherpa> plot_fit(ylog=True)
To change the default settings for plot_data so that both the x and yaxes will be drawn using a logscale each time the function is called in the session, use the get_data_plot_prefs function:
sherpa> p = get_data_plot_prefs() sherpa> p["xlog"] = True sherpa> p["ylog"] = True
To learn how to change the default axis scale from linear to logarithmic so that these commands do not have to be run in each Sherpa session, see this Sherpa FAQ.
Defining the Source Model
Before fitting the data, it is necessary to define a model that characterizes the source. All models available in Sherpa, or only models belonging to a specific category, may be returned at the Sherpa prompt by calling the list_models function accordingly:
sherpa> list_models() # all models, same as 'list_models("all")' sherpa> list_models("xspec") # all xspec models sherpa> list_models("2d") # Sherpa 2D analytic models
Here, we use a source model composed of two model components:
 powlaw1d — a onedimensional powerlaw.
 xsphabs — an XSpec photoelectric absorption model.
We define an expression that is the product of these two components. The hydrogen column density (nH) is set to the known Galactic value for the source, in units of 10^{22} atoms/cm^{2}, and the parameter is frozen so that it will not be allowed to vary in the fit.
sherpa> set_source(xsphabs.abs1 * powlaw1d.p1) sherpa> abs1.nH = 0.07 sherpa> freeze(abs1.nH)
The current source definition may be displayed:
sherpa> show_source() Model: 1 (xsphabs.abs1 * powlaw1d.p1) Param Type Value Min Max Units       abs1.nH frozen 0.07 0 100000 10^22 atoms / cm^2 p1.gamma thawed 1 10 10 p1.ref frozen 1 3.40282e+38 3.40282e+38 p1.ampl thawed 1 0 3.40282e+38
and the full model definition—which includes the instrument reponse—with:
sherpa> show_model() Model: 1 apply_rmf(apply_arf((38564.608926889 * (xsphabs.abs1 * powlaw1d.p1)))) Param Type Value Min Max Units       abs1.nh frozen 0.07 0 100000 10^22 atoms / cm^2 p1.gamma thawed 1 10 10 p1.ref frozen 1 3.40282e+38 3.40282e+38 p1.ampl thawed 1 0 3.40282e+38
Note that Sherpa and XSpec absorption models have to be multiplied by a model which has normalization and amplitude parameters, such as powlaw1d; they should not be used as single models in the source expression. It may be necessary to modify the parameter values, since the Sherpa guess functionality does not apply to absorption models. However, we can use this command to guess the initial parameter values and ranges for the powerlaw model component (parameter values are not automatically guessed in Sherpa. To have Sherpa automatically query for the initial parameter values when a model is established, set 'paramprompt(True)' (it is 'False' by default).
sherpa> guess(p1) sherpa> show_model() Model: 1 apply_rmf(apply_arf((38564.608926889 * (xsphabs.abs1 * powlaw1d.p1)))) Param Type Value Min Max Units       abs1.nh frozen 0.07 0 100000 10^22 atoms / cm^2 p1.gamma thawed 1 10 10 p1.ref frozen 1 3.40282e+38 3.40282e+38 p1.ampl thawed 0.000148802 1.48802e06 0.0148802
The guess command makes an initial guess at parameter values to ensure convergence, but it is always a good idea to check that the initial range of values (soft limits) is sensible for the data being fit. Note that the initial parameter values can also be entered with set_par which is more appropriate for complex models, as guess is just a simple function and can make the parameter space too narrow for the search. set_par should be used in scripts.
Fitting
Now we are ready to run the fit, using the Sherpa default fit statistic (chi2gehrels) and optimization method (levmar). The available fit statistics and optimization methods may be returned with the list_stats and list_methods commands, and they may be changed with set_method and set_stat.
sherpa> fit() Dataset = 1 Method = levmar Statistic = chi2gehrels Initial fit statistic = 710.713 Final fit statistic = 29.3673 at function evaluation 19 Data points = 43 Degrees of freedom = 41 Probability [Qvalue] = 0.9124 Reduced statistic = 0.716276 Change in statistic = 681.345 p1.gamma 2.13925 +/ 0.078812 p1.ampl 0.000220978 +/ 1.44103e05
The fit information returned by the fit command includes the statistic value for chi2gehrels, goodnessoffit and reduced χ^{2}, along with the bestfit parameter values of the photon index and amplitude. The "+/" values in the fit are byproducts of using the LevenbergMarquardt optimizer where the uncertanty estimates are overly simplified, derived from the fitted covariance matrix and should not be relied upon. More robust error estimates can be determined using the separate functions discussed below. The function calc_stat_info and its associated get_stat_info command, may be used to return the goodnessoffit statistics without having to rerun the fit:
sherpa> calc_stat_info() Dataset = 1 Statistic = chi2gehrels Fit statistic value = 29.3673 Data points = 43 Degrees of freedom = 41 Probability [Qvalue] = 0.9124 Reduced statistic = 0.716276 sherpa> goodness = get_stat_info() sherpa> print(goodness[0]) name = Dataset [1] ids = [1] bkg_ids = None statname = chi2gehrels statval = 29.36731057199169 numpoints = 43 dof = 41 qval = 0.9123996703894587 rstat = 0.7162758676095534
The calc_stat_info command is appropriate for accessing the fit statistics at the Sherpa prompt, where the information is printed to the screen, whereas get_stat_info is more useful for parsing this information within a script. Note that get_fit_results is available to access the full information returned by the fit, which is also useful when working on a script.
The bestfit model with the data and residuals may be plotted in the same window:
sherpa> plot_fit_delchi(xlog=True, ylog=True)
which creates Figure 3. The errors are plotted as "sigma" or "delchi", the sigma residuals of the fit \(\sigma = \delta\chi = \mathrm{\frac{data  model}{error}}\).
Figure 3: Fit and sigma residuals
The plot can be modified using matplotlib pyplot functions directly.
Examining Fit Results
Goodness of fit
The show_fit and get_fit_results commands allow access to the bestfit values and detailed information after the fit has been performed:
sherpa> show_fit() Optimization Method: LevMar name = levmar ftol = 1.1920928955078125e07 xtol = 1.1920928955078125e07 gtol = 1.1920928955078125e07 maxfev = None epsfcn = 1.1920928955078125e07 factor = 100.0 numcores = 1 verbose = 0 Statistic: Chi2Gehrels Chi Squared with Gehrels variance. The variance is estimated from the number of counts in each bin, but unlike `Chi2DataVar`, the Gaussian approximation is not used. This makes it moresuitable for use with lowcount data. The standard deviation for each bin is calculated using the approximation from [1]_: sigma(i,S) = 1 + sqrt(N(i,s) + 0.75) where the higherorder terms have been dropped. This is accurate to approximately one percent. For data where the background has not been subtracted then the error term is: sigma(i) = sigma(i,S) whereas with background subtraction, sigma(i)^2 = sigma(i,S)^2 + [A(S)/A(B)]^2 sigma(i,B)^2 A(B) is the offsource "area", which could be the size of the region from which the background is extracted, or the length of a background time segment, or a product of the two, etc.; and A(S) is the onsource "area". These terms may be defined for a particular type of data: for example, PHA data sets A(B) to `BACKSCAL * EXPOSURE` from the background data set and A(S) to `BACKSCAL * EXPOSURE` from the source data set. See Also  Chi2DataVar, Chi2ModVar, Chi2XspecVar Notes  The accuracy of the error term when the background has been subtracted has not been determined. A preferable approach to background subtraction is to model the background as well as the source signal. References  .. [1] "Confidence limits for small numbers of events in astrophysical data", Gehrels, N. 1986, ApJ, vol 303, p. 336346. http://adsabs.harvard.edu/abs/1986ApJ...303..336G Fit:Dataset = 1 Method = levmar Statistic = chi2gehrels Initial fit statistic = 710.713 Final fit statistic = 29.3673 at function evaluation 19 Data points = 43 Degrees of freedom = 41 Probability [Qvalue] = 0.9124 Reduced statistic = 0.716276 Change in statistic = 681.345 p1.gamma 2.13925 +/ 0.078812 p1.ampl 0.000220978 +/ 1.44103e05 # retrieve a single value with get_fit_results: sherpa> fitres = get_fit_results() sherpa> print(fitres.qval) 0.9123996703894587 sherpa> print(fitres.rstat) 0.7162758676095534
The number of bins in the fit (Data points), the number of degrees of freedom, i.e. the number of bins minus the number of free parameters, and the final fit statistic value are reported. If the chosen statistic is one of the χ^{2} statistics, as in this example, the reduced statistic (i.e. the statistic value divided by the number of degrees of freedom) and the probability (Qvalue) are included as well.
The calc_chisqr command calculates the statistic contribution per bin:
sherpa> calc_chisqr() array([5.92219689e+00, 1.15095438e+00, 2.67144137e01, 1.51313185e01, 5.57811410e03, 7.39920674e01, 3.84220524e01, 7.93894437e01, 8.92233791e02, 6.43705828e01, 2.20535462e+00, 2.31863201e01, 2.37124647e02, 9.02061151e01, 4.35570832e01, 6.67330704e03, 1.17580452e+00, 1.61370022e+00, 2.31836814e01, 6.96734907e02, 1.55987296e01, 5.55911748e01, 4.24866413e02, 1.99746379e+00, 9.33450840e02, 1.06955971e+00, 4.45717186e01, 3.32144464e01, 6.90133232e02, 1.52576625e01, 1.24063898e+00, 5.91068198e01, 1.31817201e04, 8.78320376e01, 1.11984115e+00, 1.59891448e01, 5.79323503e02, 2.60885837e01, 2.20699877e+00, 2.04946799e01, 1.82494758e01, 1.20470103e01, 3.85081946e01])
Confidence intervals
The covariance() command—which may be shortened to covar()—computes covariance matrices and provides an estimate of confidence intervals for the thawed parameters; also see the related command conf():
sherpa> covar() Dataset = 1 Confidence Method = covariance Iterative Fit Method = None Fitting Method = levmar Statistic = chi2gehrels covariance 1sigma (68.2689%) bounds: Param BestFit Lower Bound Upper Bound     p1.gamma 2.13925 0.0815616 0.0815616 p1.ampl 0.000220978 1.46038e05 1.46038e05 sherpa> conf() p1.gamma lower bound: 0.0815616 p1.ampl lower bound: 1.46038e05 p1.ampl upper bound: 1.46038e05 p1.gamma upper bound: 0.0821867 Dataset = 1 Confidence Method = confidence Iterative Fit Method = None Fitting Method = levmar Statistic = chi2gehrels confidence 1sigma (68.2689%) bounds: Param BestFit Lower Bound Upper Bound     p1.gamma 2.13925 0.0815616 0.0821867 p1.ampl 0.000220978 1.46038e05 1.46038e05
The output is the bestfit parameter value with positive and negative error estimates.
Sensitivity to a single parameter
The int_proj function can be used to how the search statistic varies with a parameter, which lets us see how much we can trust the error analysis (a nice smooth curve centered at the bestfit location is good, and one with a lot of structure is not).
sherpa> int_proj(p1.gamma)
Figure 4: How does the statistic vary with the gamma parameter?
Sensitivity to two parameters
The reg_proj function lets us see how two parameters are related:
sherpa> reg_proj(p1.gamma, p1.ampl)
Figure 5: How does the statistic vary with the gamma and amplitude parameters?
As with the onedimensional analysis (int_proj) we can explicitly give the range and binning to use. Here we increase the number of bins (the default is 10 along each axis) to smooth out the contours:
sherpa> reg_proj(p1.gamma, p1.ampl, min=[1.8, 1.6e4], max=[2.5,2.8e4], nloop=[41, 41])
Figure 6: Tweaking the range
Flux and Counts
Please review the How can we calculate a flux in Sherpa? analysis guide on the CIAO site.
To calculate the flux of a PHA data set, use the calc_photon_flux and calc_energy_flux commands. The flux may be calculated over the entire data set or over a specific range:
sherpa> calc_photon_flux() 0.00047016461535720494 sherpa> calc_photon_flux(2., 10.) 7.317496311869523e05 sherpa> calc_energy_flux() 9.651851646748475e13 sherpa> calc_energy_flux(2., 10.) 4.599863613722727e13
To calculate the counts of a PHA data set, use the calc_data_sum, calc_model_sum, or calc_source_sum commands. As with the flux calculations, these commands may be given a range:
sherpa> calc_data_sum() 706.8571409201713 sherpa> calc_data_sum(2., 10.) 306.2301570173737 sherpa> calc_model_sum() 637.794750679389 sherpa> calc_model_sum(2., 10.) 272.49939336502973 sherpa> calc_source_sum() 0.047016461847183715 sherpa> calc_source_sum(2., 10.) 0.007317496309896684
These functions accept any range of values but they can only be relied on for values that lie wthin the instrument energy range (so roughly 0.1 to 12 keV for Chandra ACIS data using a default setup).
Scripting It
The file fit.py is a Python script which performs the primary commands used above; it can be executed by typing %run i fit.py on the Sherpa command line.
The Sherpa script command may be used to save everything typed on the command line in a Sherpa session:
sherpa> script(filename="sherpa.log", clobber=False)
(Note that restoring a Sherpa session from such a file could be problematic since it may include syntax errors, unwanted fitting trials, et cetera.)
History
14 Nov 2007  rewritten for CIAO 4.0 Beta 3 
29 Apr 2008  show_all command is available in CIAO 4.0 
09 Dec 2008  figures moved inline with text 
09 Dec 2008  updated for Sherpa 4.1 
16 Feb 2009  example of guess functionality added 
29 Apr 2009  new script command is available with CIAO 4.1.2 
15 Dec 2009  updated for CIAO 4.2 
09 Jul 2010  updated for CIAO 4.2 Sherpa v2: SLang version of thread removed 
15 Dec 2010  updated for Sherpa in CIAO 4.3: use of log_scale replaced with set_xlog/set_ylog; list_models is available with new argument options; new functions calc_stat_info and get_stat_info return goodnessoffit information 
15 Dec 2011  reviewed for CIAO 4.4 (no changes) 
13 Dec 2012  updated for CIAO 4.5: background data may now be filtered separately from associated source data using the new bkg_id argument of the notice_id/ignore_id commands 
04 Jun 2013  added a paragraph on statistical and systematic errors to the section "Load the Spectrum and Instrument Responses". Made small edits to the text. 
03 Dec 2013  reviewed for CIAO 4.6 
06 Apr 2015  updated for CIAO 4.7, no content change 
01 Dec 2015  updated for CIAO 4.8, outputs updated 
01 Dec 2015  updated for CIAO 4.9, updated for Python 3 compatibility. 
11 Apr 2018  updated for CIAO 4.10, outputs updated 
04 Dec 2018  updated for CIAO 4.11, outputs updated 
09 Dec 2019  updated for CIAO 4.12, ChIPS figures replaced with matplotlib 
15 Dec 2020  updated for CIAO 4.13: plot style has been updated, the default energy range changed to 0.36 keV, and two new sections have been added: Sensitivity to a single parameter and Sensitivity to two parameters. 
01 Mar 2022  updated for CIAO 4.14, added note about the "+/" uncertainties for fits using the LevenbergMarquardt optimizer. 
28 Nov 2022  updated screen output for CIAO 4.15. 