This is a fixed-text formatted version of a Jupyter notebook

Fitting 2D images with Sherpa¶

Introduction¶

Sherpa is the X-ray satellite Chandra modeling and fitting application. It enables the user to construct complex models from simple definitions and fit those models to data, using a variety of statistics and optimization methods. The issues of constraining the source position and morphology are common in X- and Gamma-ray astronomy. This notebook will show you how to apply Sherpa to CTA data.

Here we will set up Sherpa to fit the counts map and loading the ancillary images for subsequent use. A relevant test statistic for data with Poisson fluctuations is the one proposed by Cash (1979). The simplex (or Nelder-Mead) fitting algorithm is a good compromise between efficiency and robustness. The source fit is best performed in pixel coordinates.

This tutorial has 2 important parts 1. Generating the Maps 2. The actual fitting with sherpa.

Since sherpa deals only with 2-dim images, the first part of this tutorial shows how to prepare gammapy maps to make classical images.

Necessary imports¶

[1]:

%matplotlib inline
import matplotlib.pyplot as plt
from pathlib import Path
import numpy as np
from astropy.io import fits
import astropy.units as u
from astropy.coordinates import SkyCoord
from gammapy.data import DataStore
from gammapy.irf import make_mean_psf
from gammapy.maps import WcsGeom, MapAxis, Map
from gammapy.cube import MapMaker, PSFKernel


Generate the required Maps¶

We first generate the required maps using 3 simulated runs on the Galactic center, exactly as in the analysis_3d tutorial.

It is always advisable to make the maps on fine energy bins, and then sum them over to get an image.

[2]:

# Define which data to use
data_store = DataStore.from_dir("\$GAMMAPY_DATA/cta-1dc/index/gps/")
obs_ids = [110380, 111140, 111159]
observations = data_store.get_observations(obs_ids)

[3]:

energy_axis = MapAxis.from_edges(
np.logspace(-1, 1.0, 10), unit="TeV", name="energy", interp="log"
)
geom = WcsGeom.create(
skydir=(0, 0),
binsz=0.02,
width=(10, 8),
coordsys="GAL",
proj="CAR",
axes=[energy_axis],
)

[4]:

%%time
maker = MapMaker(geom, offset_max=4.0 * u.deg)
maps = maker.run(observations)

WARNING: Tried to get polar motions for times after IERS data is valid. Defaulting to polar motion from the 50-yr mean for those. This may affect precision at the 10s of arcsec level [astropy.coordinates.builtin_frames.utils]

CPU times: user 16.9 s, sys: 1.84 s, total: 18.7 s
Wall time: 9.84 s


Making a PSF Map¶

Make a PSF map and weigh it with the exposure at the source position to get a 2D PSF

[5]:

# mean PSF
src_pos = SkyCoord(0, 0, unit="deg", frame="galactic")
table_psf = make_mean_psf(observations, src_pos)

# PSF kernel used for the model convolution
psf_kernel = PSFKernel.from_table_psf(table_psf, geom, max_radius="0.3 deg")

# get the exposure at the source position
exposure_at_pos = maps["exposure"].get_by_coord(
{
"lon": src_pos.l.value,
"lat": src_pos.b.value,
"energy": energy_axis.center,
}
)

# now compute the 2D PSF
psf2D = psf_kernel.make_image(exposures=exposure_at_pos)


Make 2D images from 3D ones¶

Since sherpa image fitting works only with 2-dim images, we convert the generated maps to 2D images using run_images() and save them as fits files. The exposure is weighed with the spectrum before averaging (assumed to be a power law by default).

[6]:

maps = maker.run_images()

[7]:

Path("analysis_3d").mkdir(exist_ok=True)

maps["counts"].write("analysis_3d/counts_2D.fits", overwrite=True)
maps["background"].write("analysis_3d/background_2D.fits", overwrite=True)
maps["exposure"].write("analysis_3d/exposure_2D.fits", overwrite=True)
fits.writeto("analysis_3d/psf_2D.fits", psf2D.data, overwrite=True)


Read the maps and store them in a sherpa model¶

We now have the prepared files which sherpa can read. This part of the notebook shows how to do image analysis using sherpa

[8]:

import sherpa.astro.ui as sh

sh.set_stat("cash")
sh.set_method("simplex")

sh.set_coord("logical")


WARNING: imaging routines will not be available,
failed to import sherpa.image.ds9_backend due to
'RuntimeErr: DS9Win unusable: Could not find ds9 on your PATH'
WARNING: failed to import sherpa.astro.xspec; XSPEC models will not be available

/Users/adonath/software/anaconda3/envs/gammapy-dev/lib/python3.7/importlib/_bootstrap.py:219: RuntimeWarning: Unable to load the ciao_version module to determine version number- defaulting 'group' version to 0.0.0
return f(*args, **kwds)


In principle one might first want to fit the background amplitude. However the background estimation method already yields the correct normalization, so we freeze the background amplitude to unity instead of adjusting it. The (smoothed) residuals from this background model are then computed and shown.

[9]:

sh.set_full_model(bkg)
bkg.ampl = 1
sh.freeze(bkg)

[10]:

resid = Map.read("analysis_3d/counts_2D.fits")
resid.data = sh.get_data_image().y - sh.get_model_image().y
resid_smooth = resid.smooth(width=4)


Find and fit the brightest source¶

We then find the position of the maximum in the (smoothed) residuals map, and fit a (symmetrical) Gaussian source with that initial position:

[11]:

yp, xp = np.unravel_index(
np.nanargmax(resid_smooth.data), resid_smooth.data.shape
)
ampl = resid_smooth.get_by_pix((xp, yp))[0]

# creates g0 as a gauss2d instance
sh.set_full_model(bkg + psf(sh.gauss2d.g0) * expo)
g0.xpos, g0.ypos = xp, yp
sh.freeze(g0.xpos, g0.ypos)  # fix the position in the initial fitting step

# fix exposure amplitude so that typical exposure is of order unity
expo.ampl = 1e-9
sh.freeze(expo)
sh.thaw(g0.fwhm, g0.ampl)  # in case frozen in a previous iteration

g0.fwhm = 10  # give some reasonable initial values
g0.ampl = ampl

[12]:

%%time
sh.fit()

/Users/adonath/software/anaconda3/envs/gammapy-dev/lib/python3.7/site-packages/sherpa/instrument.py:723: UserWarning: No PSF pixel size info available. Skipping check against data pixel size.
warnings.warn("No PSF pixel size info available. Skipping check against data pixel size.")

Dataset               = 1
Statistic             = cash
Initial fit statistic = 291433
Final fit statistic   = 289598 at function evaluation 230
Data points           = 200000
Degrees of freedom    = 199998
Change in statistic   = 1834.36
g0.fwhm        113.287
g0.ampl        0.439958
CPU times: user 11.1 s, sys: 83.2 ms, total: 11.2 s
Wall time: 11.1 s


Fit all parameters of this Gaussian component, fix them and re-compute the residuals map.

[13]:

sh.thaw(g0.xpos, g0.ypos)
sh.fit()
sh.freeze(g0)

Dataset               = 1
Statistic             = cash
Initial fit statistic = 289598
Final fit statistic   = 289503 at function evaluation 383
Data points           = 200000
Degrees of freedom    = 199996
Change in statistic   = 95.2248
g0.fwhm        106.247
g0.xpos        234.649
g0.ypos        195.635
g0.ampl        0.478146

[14]:

resid.data = sh.get_data_image().y - sh.get_model_image().y
resid_smooth = resid.smooth(width=3)
resid_smooth.plot();


Iteratively find and fit additional sources¶

Instantiate additional Gaussian components, and use them to iteratively fit sources, repeating the steps performed above for component g0. (The residuals map is shown after each additional source included in the model.) This takes some time…

[15]:

# initialize components with fixed, zero amplitude
for i in range(1, 10):
model = sh.create_model_component("gauss2d", "g" + str(i))
model.ampl = 0
sh.freeze(model)

gs = [g0, g1, g2]
sh.set_full_model(bkg + psf(g0 + g1 + g2) * expo)

[16]:

%%time
for i in range(1, len(gs)):
yp, xp = np.unravel_index(
np.nanargmax(resid_smooth.data), resid_smooth.data.shape
)
ampl = resid_smooth.get_by_pix((xp, yp))[0]
gs[i].xpos, gs[i].ypos = xp, yp
gs[i].fwhm = 10
gs[i].ampl = ampl

sh.thaw(gs[i].fwhm)
sh.thaw(gs[i].ampl)
sh.fit()

sh.thaw(gs[i].xpos)
sh.thaw(gs[i].ypos)
sh.fit()
sh.freeze(gs[i])

resid.data = sh.get_data_image().y - sh.get_model_image().y
resid_smooth = resid.smooth(width=6)

/Users/adonath/software/anaconda3/envs/gammapy-dev/lib/python3.7/site-packages/sherpa/instrument.py:723: UserWarning: No PSF pixel size info available. Skipping check against data pixel size.
warnings.warn("No PSF pixel size info available. Skipping check against data pixel size.")

Dataset               = 1
Statistic             = cash
Initial fit statistic = 289067
Final fit statistic   = 288814 at function evaluation 214
Data points           = 200000
Degrees of freedom    = 199998
Change in statistic   = 253.351
g1.fwhm        3.76114
g1.ampl        16.7742
Dataset               = 1
Statistic             = cash
Initial fit statistic = 288814
Final fit statistic   = 288735 at function evaluation 428
Data points           = 200000
Degrees of freedom    = 199996
Change in statistic   = 79.3409
g1.fwhm        2.13994
g1.xpos        253.123
g1.ypos        197.983
g1.ampl        50.184
Dataset               = 1
Statistic             = cash
Initial fit statistic = 288525
Final fit statistic   = 288460 at function evaluation 223
Data points           = 200000
Degrees of freedom    = 199998
Change in statistic   = 64.6649
g2.fwhm        20.0902
g2.ampl        0.919413
Dataset               = 1
Statistic             = cash
Initial fit statistic = 288460
Final fit statistic   = 288348 at function evaluation 333
Data points           = 200000
Degrees of freedom    = 199996
Change in statistic   = 112.159
g2.fwhm        35.2131
g2.xpos        185.688
g2.ypos        197.289
g2.ampl        0.587145
CPU times: user 1min 1s, sys: 322 ms, total: 1min 1s
Wall time: 1min 1s

[17]:

resid_smooth.plot(add_cbar=True);


Generating output table and Test Statistics estimation¶

When adding a new source, one needs to check the significance of this new source. A frequently used method is the Test Statistics (TS). This is done by comparing the change of statistics when the source is included compared to the null hypothesis (no source ; in practice here we fix the amplitude to zero).

$$TS = Cstat(source) - Cstat(no source)$$

The criterion for a significant source detection is typically that it should improve the test statistic by at least 25 or 30. We have added only 3 sources to save time, but you should keep doing this till del(stat) is less than the required number.

[18]:

from astropy.stats import gaussian_fwhm_to_sigma
from astropy.table import Table

rows = []
for g in gs:
ampl = g.ampl.val
g.ampl = 0
stati = sh.get_stat_info()[0].statval
g.ampl = ampl
statf = sh.get_stat_info()[0].statval
delstat = stati - statf

geom = resid.geom
# sherpa uses 1 based indexing
coord = geom.pix_to_coord((g.xpos.val - 1, g.ypos.val - 1))
pix_scale = geom.pixel_scales.mean().deg
sigma = g.fwhm.val * pix_scale * gaussian_fwhm_to_sigma
rows.append(
dict(delstat=delstat, glon=coord[0], glat=coord[1], sigma=sigma)
)

table = Table(rows=rows, names=rows[0])
for name in table.colnames:
table[name].format = ".5g"
table

/Users/adonath/software/anaconda3/envs/gammapy-dev/lib/python3.7/site-packages/sherpa/instrument.py:723: UserWarning: No PSF pixel size info available. Skipping check against data pixel size.
warnings.warn("No PSF pixel size info available. Skipping check against data pixel size.")

[18]:

Table length=3
delstatglonglatsigma
float64float64float64float64
1825.10.31702-0.0973090.90238
768.39359.95-0.0503390.018175
386.671.2962-0.064230.29907

Exercises¶

1. Keep adding sources till there are no more significat ones in the field. How many Gaussians do you need?
2. Use other morphologies for the sources (eg: disk, shell) rather than only Gaussian.
3. Compare the TS between different models

[19]: