.. note::
    :class: sphx-glr-download-link-note

    Click :ref:`here <sphx_glr_download_generated_gallery_skip_psf_deconvolution.py>` to download the full example code
.. rst-class:: sphx-glr-example-title

.. _sphx_glr_generated_gallery_skip_psf_deconvolution.py:


=============================================================
Deconvolving Images with the Instrument Point Spread Function
=============================================================

This example demonstrates how to deconvolve an AIA image with
the instrument point spread function (PSF).


.. code-block:: default

    import astropy.units as u
    from astropy.coordinates import SkyCoord
    from astropy.visualization import ImageNormalize, LogStretch, AsinhStretch
    from sunpy.net import Fido, attrs
    import sunpy.map
    import matplotlib.pyplot as plt

    import aiapy.psf



AIA images are subject to convolution with the instrument point-spread
function (PSF) due to effects introduced by the filter mesh of the telescope
and the CCD, among others. This has the effect of "blurring" the image.
The PSF diffraction pattern may also be particularly noticable during the
impulsive phase of a flare where the intensity enhancement is very localized.
To remove these artifacts, the PSF must be deconvolved from the image.

First, we'll download a single level 1 image from the 171 Å channel from
7 June 2011. Note that deconvolution should be performend on level 1 images
only. This is because, as with the level 1 data, the PSF model is defined
on the CCD grid. Once deconvolved, the image can be passed to
`~aiapy.calibrate.register`
(see the :ref:`sphx_glr_generated_gallery_prepping_level_1_data.py` example).


.. code-block:: default

    q = Fido.search(
        attrs.Time('2011-06-07T06:52:00', '2011-06-07T06:52:10'),
        attrs.Instrument('AIA'),
        attrs.Wavelength(wavemin=171*u.angstrom, wavemax=171*u.angstrom),
    )
    m = sunpy.map.Map(Fido.fetch(q))
    fig = plt.figure()
    ax = fig.add_subplot(111, projection=m)
    m.plot(axes=ax,)


Next, we'll calculate the PSF using `~aiapy.psf.psf` for the 171 Å channel.
The PSF model accounts for several different effects, including diffraction
from the mesh grating of the filters, charge spreading, and jitter. See
`Grigis et al (2012) <https://hesperia.gsfc.nasa.gov/ssw/sdo/aia/idl/psf/DOC/psfreport.pdf>`_
for more details. Currently, this only works for
:math:`4096\times4096` full frame images.

Note that this will be significantly faster if you have a GPU and the `cupy`
package installed.


.. code-block:: default

    psf = aiapy.psf.psf(m.wavelength)


We'll plot just a 500-by-500 pixel section centered on the center pixel. The
diffraction "arms" extending from the center pixel can often be seen in
flare observations due to the intense, small-scale brightening.


.. code-block:: default

    fov = 500
    lc_x, lc_y = psf.shape[0]//2 - fov//2, psf.shape[1]//2 - fov//2
    plt.imshow(psf[lc_x:lc_x+fov, lc_y:lc_y+fov],
               norm=ImageNormalize(vmin=1e-8, vmax=1e-3, stretch=LogStretch()))
    plt.colorbar()


Now that we've downloaded our image and computed the PSF, we can deconvolve
the image with the PSF using the
`Richardson-Lucy deconvolution algorithm <https://en.wikipedia.org/wiki/Richardson%E2%80%93Lucy_deconvolution>`_.
Note that passing in the PSF is optional. If you exclude it, it will be
calculated automatically. However, when deconvolving many images of the same
wavelength, it is most efficient to only calculate the PSF once.

As with `~aiapy.psf.psf`, this will be much faster if you have
a GPU and `cupy` installed.


.. code-block:: default

    m_deconvolved = aiapy.psf.deconvolve(m, psf=psf)


Let's compare the convolved and deconvolved images.


.. code-block:: default

    norm = ImageNormalize(vmin=0, vmax=1.5e4, stretch=AsinhStretch(0.01))
    fig = plt.figure()
    ax = fig.add_subplot(121, projection=m)
    m.plot(axes=ax, norm=norm)
    ax = fig.add_subplot(122, projection=m_deconvolved)
    m_deconvolved.plot(axes=ax, annotate=False, norm=norm)
    ax.coords[0].set_axislabel(' ')
    ax.coords[1].set_axislabel(' ')
    ax.coords[1].set_ticklabel_visible(False)


The differences become a bit more obvious when we zoom in. Note that the
deconvolution has the effect of "deblurring" the image.


.. code-block:: default

    left_corner = 500*u.arcsec, -600*u.arcsec
    right_corner = 1000*u.arcsec, -100*u.arcsec
    fig = plt.figure()
    m_sub = m.submap(
        SkyCoord(*left_corner, frame=m.coordinate_frame),
        SkyCoord(*right_corner, frame=m.coordinate_frame)
    )
    ax = fig.add_subplot(121, projection=m_sub)
    m_sub.plot(axes=ax, norm=norm)
    m_deconvolved_sub = m_deconvolved.submap(
        SkyCoord(*left_corner, frame=m_deconvolved.coordinate_frame),
        SkyCoord(*right_corner, frame=m_deconvolved.coordinate_frame)
    )
    ax = fig.add_subplot(122, projection=m_deconvolved_sub)
    m_deconvolved_sub.plot(axes=ax, annotate=False, norm=norm)
    ax.coords[0].set_axislabel(' ')
    ax.coords[1].set_axislabel(' ')
    ax.coords[1].set_ticklabel_visible(False)


.. rst-class:: sphx-glr-timing

   **Total running time of the script:** ( 0 minutes  0.000 seconds)


.. _sphx_glr_download_generated_gallery_skip_psf_deconvolution.py:


.. only :: html

 .. container:: sphx-glr-footer
    :class: sphx-glr-footer-example



  .. container:: sphx-glr-download

     :download:`Download Python source code: skip_psf_deconvolution.py <skip_psf_deconvolution.py>`



  .. container:: sphx-glr-download

     :download:`Download Jupyter notebook: skip_psf_deconvolution.ipynb <skip_psf_deconvolution.ipynb>`


.. only:: html

 .. rst-class:: sphx-glr-signature

    `Gallery generated by Sphinx-Gallery <https://sphinx-gallery.github.io>`_
