Fitting FITS Image Data
Sherpa Threads (CIAO 4.9 Sherpa v1)
Overview
Synopsis:
This thread models image data of the supernova remnant G21.50.9 using a source model expression that involves multiple model components. The Create and Read Fits Image Data section shows how the input file was created.
Last Update: 31 Oct 2016  reviewed for CIAO 4.9: updated fit results
Contents
 Create and Read Fits Image Data
 Filtering Image Data
 Defining a Source Model
 Fitting the model
 Adding an extra component
 Checking the Sherpa session
 Scripting It
 Summary
 History

Images
 Figure 1: Image of the data
 Figure 2: Filter region defined on the image
 Figure 3: Filtered data
 Figure 4: FITS image file containing filter information
 Figure 5: Residuals of the bestfit model using: g1+bgnd
 Figure 6: Residuals of the bestfit model using: g1+g2+bgnd
 Figure 7: The g2 model contribution to the bestfit model g1+g2+bgnd
Create and Read Fits Image Data
Download the sample data: 1838 (ACISS, G21.50.9)
unix% download_chandra_obsid 1838
In this example, the data has been reprocessed with chandra_repro. First, an image of the region of interest is created:
unix% punlearn dmcopy unix% dmcopy \ "acisf01838_repro_evt2.fits[sky=box(4059.25,4235.75,521.5,431.5)][bin x=::2,y=::2]" \ image2.fits
Because we plan to model the extended structure, not detailed features in the image, we can use coarser binning to reduce the time taken for the fit—a binning factor of 2 is used. The choice of binning should be determined by the quality of the data and the models to be fit with the data. Increasing the binning factor when creating the image is likely to lose smallscale spatial information.
After starting a Sherpa session, the dataset is input using the load_image command. The image is then displayed by the image_data command:
sherpa> load_image("image2.fits") sherpa> image_data()
which creates Figure 1. The DS9 imager is used by default; see the Using SAOImage DS9 CIAO thread for more information.
Setting the coordinate system
The default coordinate system for fitting images is that of logical (also called image), which uses the FITS convention for numbering pixels: the first pixel is centered at (1,1) with the bottomleft corner being at (0.5,0.5) and the topright corner being at (1.5,1.5).
Although a simple system, it can be difficult when converting the bestfit parameters, such as source location, back to moremeaningful coordinate systems. For this reason, the physical coordinate system is chosen for fitting. This is done with the set_coord function:
sherpa> set_coord("physical")
Choosing the appropriate statistics
When fitting Chandra or XMMNewton imaging data, it is almost certain that many pixels will only contain a small number of counts, making the source model fit with Cash statistic, the Poisson loglikelihood, to the Poisson image suitable. Subsequently, subtracting a background data set is not permitted and must either be accounted for with a background model—as shown in this example—or the background signal is ignored.
sherpa> set_stat("cash")
The CSTAT statistic—equivalent to the XSPEC C statistic—may also be used in fitting image data. The advantage of CSTAT over CASH is that an approximate goodnessoffit measure may be assigned to a given value of the CSTAT statistic for Xray spectral fitting.
Setting the fit method
The default fitting method (LevenbergMarquardt) is not well suited for use with the Cash statistic, so we choose to use the Simplex optimizer instead (the NelderMead method is the same as simplex).
sherpa> set_method("simplex")
The fit should also be tried with the Monte Carlo (moncar) optimization method to ensure that the global bestfit has been found, rather than a local one.
The current Sherpa status may be reviewed by using the show_all command:
sherpa> show_all() Data Set: 1 Filter: name = image2.fits x0 = Float64[56376] x1 = Float64[56376] y = Float64[56376] shape = (216, 261) staterror = None syserror = None sky = physical crval = [ 3798.5 4019.5] crpix = [ 0.5 0.5] cdelt = [ 2. 2.] eqpos = world crval = [ 278.3866, 10.5893] crpix = [ 4096.5, 4096.5] cdelt = [0.0001, 0.0001] crota = 0 epoch = 2000 equinox = 2000 coord = physical
Filtering Image Data
Here we illustrate several ways of filtering image data within Sherpa.
Define the region to filter
After the data has been displayed, the filter region may be determined from the imager. Alternatively, an existing region file may be used.
Use the Region → Shape menu in DS9 to choose a region shape, then leftclick on the display to draw the desired shape. For further instructions on how to create regions in DS9, see the Using CIAO Region Files thread.
After the desired region size is set, as shown in Figure 2, use the Region → List Regions menu to get the region definition, first setting the format to CIAO and the coordinate system to Physical in the menu that pops up:
# Region file format: CIAO version 1.0 circle(4072.46,4249.34,108)
The region may also be saved to a file; see the DS9 thread for instructions.
Define the filter on the command line
Sherpa and the DS9 session opened with image_data can interact with each other, so that the defined region may be displayed on on the Sherpa commandline with the image_getregion function.
sherpa> image_getregion(coord="physical") 'circle(4072.46,4249.34,108);'
The image_getregion command be default returns region strings in logical/image coordinates, so the coordinates must be explicitly set to "physical".
The filter is now set on the commandline with the region definition:
or by formatting the string returned by image_getregion with the Python replace string method:
One may also specify a FITS or ASCII file which contains the region definition:
sherpa> notice2d("filter.reg")
Using the image_data() command again displays the filtered data, as shown in Figure 3.
Load filter information from file
As of the release of Sherpa version 2 in CIAO 4.2, it is possible to filter 2D data sets with filter information read from FITS image files using the load_filter function. The filter image input to load_filter should contain 1s and 0s to indicate which pixels should be noticed/ignored, and should match the source image in shape and number of pixels. When the new ignore argument of load_filter is set to False (default), the pixels in the data image which correspond to those marked by 1s in the filter image will be noticed, and the reverse when ignore is True.
The filter information contained in a FITS image filter file would be applied to the source image data set using the load_filter function as follows:
sherpa> load_filter("load_filter_image.fits", ignore=False)
An example of a FITS image file which can be used to filter the source image might look like that shown in Figure 4, where the pixels to be noticed are those which have a value of 1 (because ignore=False), and those which should be excluded from the analysis are the pixels with a value of 0.
Defining a Source Model
We wish to fit the image using a source model expression that involves multiple model components. By the end of the thread, we will use two twodimensional Gaussian functions together with a constant background component, but for now we begin with only one Gaussian.
Since this is an example, these choices are not physically motivated but just an empirical choice to describe the emission.
sherpa> set_source(gauss2d.g1)
It may be necessary to modify the initial parameter values and boundaries before performing the fit. For complex models, physical knowledge of the problem can guide the initial settings of parameters and their ranges, and improve the final convergence of the fit. For simple, singlecomponent models, the Sherpa guess function may be used to automatically set sensible starting values and ranges for the model parameters. To have Sherpa automatically query for the initial parameter values when a model is established, set 'paramprompt(True)' (the default value is False).
Note that the ellipticity and its angle (theta) are already frozen, so they do not vary during the fit.
sherpa> g1.ampl = 20 sherpa> g1.fwhm = 20 sherpa> g1.xpos = 4065.5 sherpa> g1.ypos = 4250.5
The upperlimits of the fwhm, xpos, and ypos parameters are constrained to roughly the size of the image in physical coordinates (300). ampl is restricted to the range 1:1000.
sherpa> g1.fwhm.max = 4300 sherpa> g1.xpos.max = 4300 sherpa> g1.ypos.max = 4300 sherpa> g1.ampl.min = 1 sherpa> g1.ampl.max = 1000
The current source model definition may be displayed:
sherpa> show_model() Model: 1 gauss2d.g1 Param Type Value Min Max Units       g1.fwhm thawed 20 1.17549e38 4300 g1.xpos thawed 4065.5 3.40282e+38 4300 g1.ypos thawed 4250.5 3.40282e+38 4300 g1.ellip frozen 0 0 0.999 g1.theta frozen 0 6.28319 6.28319 radians g1.ampl thawed 20 1 1000
The image_fit command displays a montage of the data, current model, and residuals that can be used to see how well the model describes the data.
We decide to include a background component before fitting, and so add in a constant model to the source expression. The value of the background model (0.2) was estimated from a radial profile. The upper limit is set to 100 as a reasonable constraint.
sherpa> set_source(g1+const2d.bgnd) sherpa> bgnd.c0 = 0.2 sherpa> bgnd.c0.max = 100
The model is now:
sherpa> show_model(); Model: 1 (gauss2d.g1 + const2d.bgnd) Param Type Value Min Max Units       g1.fwhm thawed 20 1.17549e38 4300 g1.xpos thawed 4065.5 3.40282e+38 4300 g1.ypos thawed 4250.5 3.40282e+38 4300 g1.ellip frozen 0 0 0.999 g1.theta frozen 0 6.28319 6.28319 radians g1.ampl thawed 20 1 1000 bgnd.c0 thawed 0.2 3.40282e+38 100
Fitting the model
We are now ready to fit the data:
sherpa> fit() Dataset = 1 Method = neldermead Statistic = cash Initial fit statistic = 20661.5 Final fit statistic = 48907.8 at function evaluation 529 Data points = 9171 Degrees of freedom = 9166 Change in statistic = 69569.3 g1.fwhm 57.9477 g1.xpos 4070.4 g1.ypos 4251.11 g1.ampl 23.3562 bgnd.c0 0.266365
The bestfit values for the Gaussian's FWHM and amplitude, and the background level are close to the values we guessed previously. Since we are using the PHYSICAL coordinate system the xpos, ypos, and fwhm parameters are given in the physical system. For this ACIS image this is the SKY coordinate system, which means the FWHM corresponds to 57.8 * 0.492 = 28.5 arcseconds. This can be calculated at the Sherpa prompt since we can easily access parameter values:
sherpa> g1.fwhm.val * 0.492
If g1.fwhm * 0.492 is just used, then the desired answer is not returned; the .val suffix for the parameter name is required to return the value at the Sherpa prompt.
The fit can be visualised using image_fit, which displays the data, model, and residual image. Here we are interested in just the residuals:
sherpa> image_resid()
The resulting image is shown in Figure 5. Although the Gaussian does a reasonable job at describing the radial profile of the largescale emission, the residuals do appear to be spatially correlated. This suggests that the model used here is insufficient to describe all the structure in the source; however, it will suffice for this example.
The save_model and save_resid functions may be used to save the 2D fit results to FITS image files:
sherpa> save_model("model.fits") sherpa> save_resid("resid.fits")
Here, save_model saves the model array associated with 2D data set id=1 to the FITS image file model.fits, and the save_resid function saves the simple dataminusmodel counts residuals array to the FITS image file resid.fits.
Calculating errors on the fit parameters
Note that the statistic value is negative because we are using the Cash statistic—which is a maximumlikelihood statistic—rather than a χ^{2} statistic. This means that we cannot get an "absolute" measure of the fit—i.e. how well the model actually fits the data. However, we can still use the conf command to estimate errors on these parameters, since this relies on the change in the statistic value rather than the absolute value:
sherpa> conf() g1.ypos lower bound: 0.178832 g1.fwhm lower bound: 0.28347 g1.ypos upper bound: 0.178832 g1.fwhm upper bound: 0.28347 g1.xpos lower bound: 0.1807 g1.xpos upper bound: 0.1807 g1.ampl lower bound: 0.243301 g1.ampl upper bound: 0.245803 bgnd.c0 lower bound: 0.00931359 bgnd.c0 upper bound: 0.00946505 Dataset = 1 Confidence Method = confidence Iterative Fit Method = None Fitting Method = neldermead Statistic = cash confidence 1sigma (68.2689%) bounds: Param BestFit Lower Bound Upper Bound     g1.fwhm 57.9477 0.28347 0.28347 g1.xpos 4070.4 0.1807 0.1807 g1.ypos 4251.11 0.178832 0.178832 g1.ampl 23.3562 0.243301 0.245803 bgnd.c0 0.266365 0.00931359 0.00946505
Adding an extra component
The residual image and profile of the fit show excess emission at the center of the source. We will add another Gaussian component to try and account for this emission. The upper parameter limits used for g1 are also used for g2.
sherpa> freeze(g1) sherpa> set_source(gauss2d.g2+g1+bgnd) sherpa> g2.fwhm = 10 sherpa> g2.ampl = 100 sherpa> g2.xpos = 4065.5 sherpa> g2.ypos = 4250.5 sherpa> g2.fwhm.max=4300 sherpa> g2.xpos.max=4300 sherpa> g2.ypos.max=4300 sherpa> g2.ampl.min=1 sherpa> g2.ampl.max=1000 sherpa> fit() Dataset = 1 Method = neldermead Statistic = cash Initial fit statistic = 50788.3 Final fit statistic = 53918.2 at function evaluation 562 Data points = 9171 Degrees of freedom = 9166 Change in statistic = 3129.92 g2.fwhm 6.08634 g2.xpos 4070.78 g2.ypos 4249.34 g2.ampl 228.721 bgnd.c0 0.260454
Since the g1 model was frozen, those values did not change in the fit:
sherpa> show_model() Model: 1 ((gauss2d.g2 + gauss2d.g1) + const2d.bgnd) Param Type Value Min Max Units       g2.fwhm thawed 6.08634 1.17549e38 4300 g2.xpos thawed 4070.78 3.40282e+38 4300 g2.ypos thawed 4249.34 3.40282e+38 4300 g2.ellip frozen 0 0 0.999 g2.theta frozen 0 6.28319 6.28319 radians g2.ampl thawed 228.721 1 1000 g1.fwhm frozen 57.9477 1.17549e38 4300 g1.xpos frozen 4070.4 3.40282e+38 4300 g1.ypos frozen 4251.11 3.40282e+38 4300 g1.ellip frozen 0 0 0.999 g1.theta frozen 0 6.28319 6.28319 radians g1.ampl frozen 23.3562 1 1000 bgnd.c0 thawed 0.260454 3.40282e+38 100
To see if the central component is elliptical—as suggested by the earlier residual image (Figure 5)—we "thaw" the ellipticity and positionangle parameters of the second Gaussian. They are set to nonzero values to help the fit.
sherpa> thaw(g2.ellip) sherpa> thaw(g2.theta) sherpa> g2.ellip = 0.1 sherpa> g2.theta = 1 sherpa> fit() Dataset = 1 Method = neldermead Statistic = cash Initial fit statistic = 53955.8 Final fit statistic = 54058.2 at function evaluation 570 Data points = 9171 Degrees of freedom = 9164 Change in statistic = 102.481 g2.fwhm 7.42264 g2.xpos 4070.73 g2.ypos 4249.34 g2.ellip 0.315905 g2.theta 0.803424 g2.ampl 230.245 bgnd.c0 0.260308
The residuals of this fit are shown in Figure 6.
To see how reliable the ellipticity and theta values are we calculate the 1σ errors using the conf() method. In this case we explicitly list the parameters we are interested in (g2.ellip and g2.theta) to avoid calculating the limits for the other parameters.
sherpa> conf(g2.ellip, g2.theta) g2.theta lower bound: 0.0399632 g2.ellip lower bound: 0.0222023 g2.ellip upper bound: 0.0215189 g2.theta upper bound: 0.0402757 Dataset = 1 Confidence Method = confidence Iterative Fit Method = None Fitting Method = neldermead Statistic = cash confidence 1sigma (68.2689%) bounds: Param BestFit Lower Bound Upper Bound     g2.ellip 0.315905 0.0222023 0.0215189 g2.theta 0.803424 0.0399632 0.0402757
We can use the image_source_component command to image one, or a combination of, individual unconvolved source model components in order to visualize the contribution to the full model being used to fit the image data.
The image_model_component command is available for visualizing PSFconvolved model components, and get_model_component_image/get_source_component_image for accessing the data arrays and preferences which define the corresponding image.
Here we image the extra g2 Gaussian component to quickly visualize its contribution to the fit of the emission.
sherpa> image_source_component(g2)
The g2 model component image is shown in Figure 7.
Checking the Sherpa session
The final overall status of this Sherpa session may be viewed as follows:
sherpa> show_all() Data Set: 1 Filter: Circle(4072.46,4249.34,108) name = image2.fits x0 = Float64[56376] x1 = Float64[56376] y = Float64[56376] shape = (216, 261) staterror = None syserror = None sky = physical crval = [ 3798.5, 4019.5] crpix = [ 0.5, 0.5] cdelt = [ 2., 2.] eqpos = world crval = [ 278.386 , 10.5899] crpix = [ 4096.5, 4096.5] cdelt = [0.0001, 0.0001] crota = 0 epoch = 2000 equinox = 2000 coord = physical Model: 1 ((gauss2d.g2 + gauss2d.g1) + const2d.bgnd) Param Type Value Min Max Units       g2.fwhm thawed 7.42264 1.17549e38 4300 g2.xpos thawed 4070.73 3.40282e+38 4300 g2.ypos thawed 4249.34 3.40282e+38 4300 g2.ellip thawed 0.315905 0 0.999 g2.theta thawed 0.803424 6.28319 6.28319 radians g2.ampl thawed 230.245 1 1000 g1.fwhm frozen 57.9477 1.17549e38 4300 g1.xpos frozen 4070.4 3.40282e+38 4300 g1.ypos frozen 4251.11 3.40282e+38 4300 g1.ellip frozen 0 0 0.999 g1.theta frozen 0 6.28319 6.28319 radians g1.ampl frozen 23.3562 1 1000 bgnd.c0 thawed 0.260308 3.40282e+38 100 Optimization Method: NelderMead name = simplex ftol = 1.19209289551e07 maxfev = None initsimplex = 0 finalsimplex = 9 step = None iquad = 1 verbose = 0 Statistic: Cash Maximum likelihood function. Counts are sampled from the Poisson distribution, and so the best way to assess the quality of model fits is to use the product of individual Poisson probabilities computed in each bin i, or the likelihood L: L = (product)_i [ M(i)^D(i)/D(i)! ] * exp[M(i)] where M(i) = S(i) + B(i) is the sum of source and background model amplitudes, and D(i) is the number of observed counts, in bin i. The Cash statistic [1]_ is derived by (1) taking the logarithm of the likelihood function, (2) changing its sign, (3) dropping the factorial term (which remains constant during fits to the same dataset), and (4) multiplying by two: C = 2 * (sum)_i [ M(i)  D(i) log M(i) ] The factor of two exists so that the change in cash statistic from one model fit to the next, (Delta)C, is distributed approximately as (Delta)chisquare when the number of counts in each bin is high. One can then in principle use (Delta)C instead of (Delta)chisquare in certain model comparison tests. However, unlike chisquare, the cash statistic may be used regardless of the number of counts in each bin. The magnitude of the Cash statistic depends upon the number of bins included in the fit and the values of the data themselves. Hence one cannot analytically assign a goodnessoffit measure to a given value of the Cash statistic. Such a measure can, in principle, be computed by performing Monte Carlo simulations. One would repeatedly sample new datasets from the bestfit model, fit them, and note where the observed Cash statistic lies within the derived distribution of Cash statistics. Alternatively, the `cstat` statistic can be used. Notes  The background should not be subtracted from the data when this statistic is used. It should be modeled simultaneously with the source. The Cash statistic function evaluates the logarithm of each data point. If the number of counts is zero or negative, it's not possible to take the log of that number. The behavior in this case is controlled by the `truncate` and `trunc_value` settings in the .sherpa.rc file:  if `truncate` is `True` (the default value), then `log(trunc_value)` is used whenever the data value is <= 0. The default is `trunc_value=1.0e25`.  when `truncate` is `False` an error is raised. References  .. [1] "Parameter estimation in astronomy through application of the likelihood ratio", Cash, W. 1979, ApJ 228, 939 http://adsabs.harvard.edu/abs/1979ApJ...228..939C Fit:Dataset = 1 Method = neldermead Statistic = cash Initial fit statistic = 53955.8 Final fit statistic = 54058.2 at function evaluation 570 Data points = 9171 Degrees of freedom = 9164 Change in statistic = 102.481 g2.fwhm 7.42264 g2.xpos 4070.73 g2.ypos 4249.34 g2.ellip 0.315905 g2.theta 0.803424 g2.ampl 230.245 bgnd.c0 0.260308 Confidence:Dataset = 1 Confidence Method = confidence Iterative Fit Method = None Fitting Method = neldermead Statistic = cash confidence 1sigma (68.2689%) bounds: Param BestFit Lower Bound Upper Bound     g2.ellip 0.315905 0.0222023 0.0215189 g2.theta 0.803424 0.0399632 0.0402757
Scripting It
The commands used to run this thread may be saved in a text file such as fit.py, which can then be executed as a script with exec(open("fit.py").read()). Alternatively, the Sherpa session can be saved to a binary file with the save command (restored with the restore command), or to an editable ASCII file with save_all.
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.)
The CXC is committed to helping Sherpa users transition to new syntax as smoothly as possible. If you have existing Sherpa 3 scripts or save files, submit them to us via the CXC Helpdesk and we will provide the CIAO/Sherpa 4.9 syntax to you.
Summary
In this thread, we have shown you how you can fit a twodimensional model to your image data. As with fitting onedimensional data, care must be taken to avoid reaching a local, rather than global, minimum. It is suggested that you fit your data using different optimization methods—for instance the fit above could be redone with the Monte Carlo ("moncar") method—and to try different initial parameter values when fitting.
In the example above, the fit was not very complex: possible additions would have been to link the centers of the two Gaussians to be the same; simultaneously fit the same model to more than one dataset (e.g. for multiple observations of a source or when analysing the data from the three imaging cameras in XMMNewton); include an exposure map in the fit to account for instrumental features such as chip gaps and bad columns; or convolve the model by the PSF during fitting.
History
15 May 2008  rewritten for Sherpa Beta 
16 Jul 2008  minor update to use simplex rather than the neldermead optimisation method as they are the same 
11 Dec 2008  updated for CIAO 4.1 
05 Jan 2010  updated for CIAO 4.2 
07 Jun 2010  updated to include save_model and save_resid functions for saving 2D fit results 
12 Jun 2010  updated for CIAO 4.2 Sherpa v2: load_filter now accepts filter files in FITS image format for filtering 2D data sets. SLang version of thread removed 
15 Dec 2010  updated for CIAO 4.3: the new image_source_component function is available for visualizing the contribution of individual unconvolved model components to a fit 
30 Jan 2012  reviewed for CIAO 4.4 (no changes) 
05 Dec 2013  reviewed for CIAO 4.6: no changes 
09 Dec 2014  reviewed for CIAO 4.7: updated example file and fit results 
31 Oct 2016  reviewed for CIAO 4.9: updated fit results 