# Sherpa Table Models

Sherpa Threads (CIAO 4.10 Sherpa v1)

## Overview

#### Synopsis:

It may be necessary to fit data to a function that is not
pre-packaged as a *Sherpa* model; to do so, we may write
that function as a *Sherpa* "table model". Table models are
those that contain data read from a file, and have only one
parameter, normalization. When the table model is
"calculated", the model returns the data—or more
generally, some calculated values based on those data
values. "User models" may also be defined in *Sherpa*;
these are models for which the user specifies the parameters
and model calculation function. In this thread,
examples of table models are shown; for user models, see the
thread "*Sherpa* User
Models."

**Last Update:** 29 May 2018 -
reviewed for CIAO 4.10, no content change.

## Contents

## Sherpa Table Models

In addition to the user
model class, a table model class has been added
to *Sherpa*; it stores the y-values from an input data file or
Crate, and returns them as an array when the table model is
asked to "calculate" y-values. The model has one parameter,
"ampl", the amplitude; the y-values are multiplied by the
amplitude.

The *Sherpa* astronomy UI package, "sherpa.astro.ui", contains a
simple function, load_table_model, to
read data from a file or Crate and assign it to an instance of the table
model class; it uses functions already defined by the astronomy
UI to read from file. First, it attempts to read the file as an
image; if that does not work, it tries to read it as a so-called
TABLE Crate (if the table model is to be defined by a set of arrays in
*Sherpa*—as opposed to being read from a file—the arrays must
first be read into a Crate and then assigned as the table model
with load_table_model.) To create a Crate,
the crates_contrib.utils
contributed package must be loaded; refer to the
make_table_crate ahelp file for details
and examples. If used
with CRATES, load_table_model
can pass along Data
Model syntax just as done by the
load_image and load_table functions.

In this simple example, we load data from an image, and the
resulting *Sherpa* data set is assigned to a table model:

sherpa> load_image(1, "image.fits") sherpa> load_table_model("mytable", "image.fits") sherpa> print(mytable) mytable Param Type Value Min Max Units ----- ---- ----- --- --- ----- mytable.ampl thawed 1 -1e+120 1e+120 sherpa> print(mytable.filename) image.fits sherpa> print(mytable._TableModel__y) [ 0., 1., 0., ..., 0., 0., 0.,] sherpa> set_model(mytable) sherpa> image_fit()

Here, an instance of the table model is created, and named "mytable". In this simplest example, it is assigned exactly the same data that is read in as the data to be fit. The print function shows that "mytable" has exactly one model parameter, "ampl", which by default is 1.

The model "mytable" also has two attributes, which are not
model parameters. The attribute "filename" is the name of the
file from which the table data are read, and the attribute
"_TableModel__y" simply stores the unfiltered
y-values read from that data file. As these are not
parameters to be varied during a fit, they are not printed by
the call "print(mytable)", which is meant to show a
model's parameters; model *attributes* may be printed
with "dir(mytable)".

The y-values which are read from the data file (and stored by the table model class) may be returned as an array when the table model is asked to "calculate" y-values. (Again, since this is not a parameter to be varied during a fit, the array of y-values is not printed by the call print(mytable)).

Then the table model is assigned as a model. The call to image_fit shows that data and model have identical values, and that the residuals are all zero, as expected.

### Figure 1: ds9 image of table model fit to the data contained in 'image.fits'

The *Sherpa* table model supports linear, nearest-neighbor,
and polynomial interpolation of data points on the data set
grid from the model grid supplied from file (interpolation is
used by the table model to match the data grid to the model
grid, which must match before the fit statistics can be
calculated for fitting). The grids need not be of constant
or comparable bin size, and it is not necessary to match the
length of the table model column to that of the data. If the
table model grid is not sorted, *Sherpa* will sort it in
ascending order.

### XSpec-style Tables

The load_xstable_model function accepts both additive and multiplicative XSpec-style table models, as demonstrated in the example below.

sherpa> load_pha("source.pi") sherpa> load_xstable_model("tab1", "bhmodel.fits") sherpa> print(tab1) xstablemodel.tab1 Param Type Value Min Max Units ----- ---- ----- --- --- ----- xstbl.log mass thawed 0.977121 0.477121 1.47712 xstbl.log lumin thawed -1 -2 0 xstbl.inc thawed 0.5 0 1 xstbl.spin thawed 0.4 0 0.8 xstbl.log alpha thawed -2 -2 -1 xstbl.norm thawed

In this example, we load PHA data set 'source.pi' and assign to it the multiplicative table model loaded from the file 'bhmodel.fits', which is written in the format required by the XSpec table model (i.e., an N-dimensional grid of model spectra).

## Fitting a Spectrum with a Table Model

In this section, we consider another example of defining
a *Sherpa* table model using model data read from file, but take it a step further and
also show the procedure for fitting a
1-D spectrum with the defined model. We consider the
Spectral Energy Distribution (SED) template model of
radio-loud quasar data
in Elvis
et al. 1994.

First, we read into *Sherpa* the data representing the source(s) to
be fit, a 3-column × 46-row array of quasar data
contained in the ASCII
file spectrum.dat. We
choose to read in this data array using the Python Crates
module, pycrates, and manipulate it within the *Sherpa* session using
Python. (ASCII data can also be read into *Sherpa* using the
*Sherpa*
commands load_ascii/load_table/load_data;
see the *Sherpa* FAQ entry "How do *Sherpa* 'load' commands handle ASCII files?" for details.)

We assign to variable "dat" the Numpy array which contains our three columns of data fom spectrum.dat: 'Freq', 'Flux' (flux density), and 'Error'. We use Numpy for the mathematical operation of calculating the logarithm of the frequency and flux density columns of the "dat" array, and the Python "array[::-1]" syntax for reversing the order of the arrays. We manipulate the data in this way in order to have it match the SED template model for fitting.

sherpa> import pycrates as pcr sherpa> dat = pcr.read_file("spectrum.dat") sherpa> pcr.get_col_names(dat) ['Freq', 'Flux', 'Error'] #convert to log frequency and reverse the order of the arraysherpa> freq = dat.get_column('Freq').values sherpa> lfreq = np.log10(freq) sherpa> lfreqr = lfreq[::-1] #convert to log and reversesherpa> flux = dat.get_column('Flux').values sherpa> lflux = np.log10(flux) sherpa> lfluxr = lflux[::-1] #Propagate errors read from the file and reversesherpa> err = dat.get_column('Error').values sherpa> lerr = err/flux sherpa> lerr2 = lerr[::-1]

Here, we have assigned the spectral coordinate array, in
frequency (Hz) units, to variable "freq"; the flux
density values (Jy-Hz) to "flux"; the errors on the
flux density to "err"; and the logarithm of the
(reversed) frequency and flux density arrays to variables
"lfreqr" and "lfluxr". The "lerr2"
array stores the logarithm of the flux density error-to-value
ratio. We use these variables as input to the *Sherpa*
load_arrays function in order to
assign the loaded data to *Sherpa* data set ID "1" (the
default data set ID).

sherpa> load_arrays(1,lfreqr,lfluxr,lerr2) sherpa> show_data() #equivalent to "show_data(1)"Data Set: 1 Filter: 7.1004-17.3838 x name = x = Float64[46] y = Float64[46] staterror = Float64[46] syserror = None sherpa> notice(13,18.)

We have also used the *Sherpa* notice function to restrict the data range to be
considered in the fit to the log_{10}(freq) = 13-18 [Hz] range.

Now that the quasar data set has been properly set up for fitting, the next step is to define the model to be used for fitting the data. We use the load_table_model function in the usual way to read in table model data from ASCII file radio_loud.txt, and assign it to model ID "temp". We customize the table model further by freezing its amplitude parameter so that it is not allowed to vary in the fit; this is in order to have the normalization defined as an additive parameter, not multiplicative.

sherpa> load_table_model("temp","radio_loud.txt") sherpa> print(temp) tablemodel.temp Param Type Value Min Max Units ----- ---- ----- --- --- ----- temp.ampl frozen 1 -3.40282e+38 3.40282e+38 sherpa> freeze(temp)

Finally, we use the *Sherpa* set_model function to define the final model
expression for fitting, the sum of the table model
"temp" and a constant, the *Sherpa*
const1d model. Since the normalization
of the template SED model is frozen, the constant is used to
shift this model up and down during the fitting process.

sherpa> set_model("temp+const1d.c1")

Suppose there is an interest in using the spectrum of one source (SourceB)
as the model fitted to that of another source (SourceA). This can
be approached by using a *Sherpa* table model.

We begin with loading the data and responses for SourceA and SourceB to dataset IDs 1 and 2, respectively, and use the background-subtracted spectrum of SourceB as the model.

sherpa> load_data(1,"SourceA.fits") sherpa> load_arf(1,"SourceA.fits") sherpa> load_rmf(1,"SourceA.fits") sherpa> load_data(2,"SourceB.fits") sherpa> load_arf(2,"SourceB.fits") sherpa> load_rmf(2,"SourceB.fits") sherpa> load_bkg(2,"SourceB_bkg.fits") sherpa> subtract(2)

In order to define a model compatible with the response files of
SourceA, it necessitates deconvolving the corresponding responses
from the observed spectrum of SourceB. Numerically, this can be
done by dividing the observed spectrum by the detector responses.
In *Sherpa*, the plot_ratio command—which divides
the observed spectrum with a model spectrum, the model spectrum
being a source spectrum convolved with the ARF and RMF—using
a constant source model set to unity, so that the model spectrum
is a discrete representation of just the detector responses, may
be used for this purpose.

sherpa> set_source(2,polynom1d.truespec) sherpa> truespec.c0 = 1 sherpa> photonflux = get_ratio_plot(2).y # ph/s/cm**2/keV sherpa> energy = get_ratio_plot(2).x # keV sherpa> photonflux[photonflux < 0] = 0 # replace negative fluxes, if background subtraction is done, with zeroes

To cast the energy and photonflux vectors as usable by load_table_model, a table Crate, cr, is defined as the first and second columns, respectively, in the table.

sherpa> cr = TABLECrate() sherpa> col1 = CrateData() sherpa> col1.name = "energy" sherpa> col1.values = energy sherpa> col2 = CrateData() sherpa> col2.name = "photon flux" sherpa> col2.values = photonflux sherpa> add_col(cr,col1) sherpa> add_col(cr,col2)

The unconvolved spectrum of SourceB is now read in as a table model, tt, and then set as the source model for SourceA, convolved with the response files of SourceA.

sherpa> load_table_model("tt",cr,dstype=Data1D) sherpa> delete_data(2) sherpa> set_source(tt)

Rather than defining a Crate in memory, writing the table to disk could have also been done easily with save_arrays.

Before fitting the defined model to the quasar data with the
*Sherpa* fit function, we change the
minimum value of the constant model to allow for negative "shifts".

sherpa> c1.c0.min=-100 sherpa> show_model() Model: 1 (tablemodel.temp + const1d.c1) Param Type Value Min Max Units ----- ---- ----- --- --- ----- temp.ampl frozen 1 -3.40282e+38 3.40282e+38 c1.c0 thawed 1 -100 3.40282e+38 sherpa> set_stat("leastsq") sherpa> fit() Dataset = 1 Method = levmar Statistic = leastsq Initial fit statistic = 9960.05 Final fit statistic = 0.434571 at function evaluation 4 Data points = 8 Degrees of freedom = 7 Change in statistic = 9959.61 c1.c0 -34.2839

Finally, we display the full, unfiltered range of the quasar spectrum with the fitted model overplotted, and the errors read in from the data file and defined in variable "lerr2".

sherpa> notice() sherpa> plot_fit() sherpa> set_plot_ylabel("log(freq * Flux_freq)") sherpa> set_plot_xlabel("log(freq)")

### Figure 2: Quasar spectrum fit with binned SED template model

Noting that the plot_fit function shows the model which is binned on the data grid, we decide to overplot the original model using the following set of commands, in order to show the shape better.

sherpa> templ=pcr.read_file("radio_load.txt[opt skip=2]") sherpa> templ.get_colnames() ['col1', 'col2'] sherpa> factor0=templ.get_column('col2').values[250]-lfluxr[30] sherpa> add_curve(templ.get_column('col1').values,templ.get_column('col2').values-(factor0-1.7)) sherpa> set_curve(["symbol.style","none"]) sherpa> set_curve(["line.color","blue"]) sherpa> set_plot_ylabel("log(freq * Flux_freq)") sherpa> set_plot_xlabel("log(freq)")

### Figure 3: Quasar spectrum with binned and original SED template model

## History

09 Sep 2009 | originally "Table Models" section of "Sherpa User Models" thread |

17 Dec 2009 | updated for CIAO 4.2 |

02 Jul 2010 | updated for CIAO 4.2 Sherpa v2: the load_table_model function accepts XSpec-style table models; the Sherpa table model supports linear interpolation. S-Lang version of thread removed. |

06 Jul 2011 | added new section "Fitting a Spectrum with a Table Model" |

15 Dec 2011 | The Sherpa table model now supports nearest-neighbor and polynomial interpolation in CIAO 4.4 |

04 Dec 2013 | reviewed for CIAO 4.6: fixed broken links to example data ASCII datasets. |

17 Mar 2015 | reviewed and updated for CIAO 4.7. |

08 Apr 2015 | added tip on using one spectrum as a model for another spectrum. |

08 Dec 2015 | reviewed for CIAO 4.8, no content change. |

10 Nov 2016 | reviewed for CIAO 4.9, use pycrates instead of asciitable. Use new load_xstable_model to load in XSpec table models instead of load_table_model. |

29 May 2018 | reviewed for CIAO 4.10, no content change. |