.. only:: html
.. note::
:class: sphx-glr-download-link-note
Click :ref:`here ` to download the full example code
.. rst-class:: sphx-glr-example-title
.. _sphx_glr_auto_examples_correlated_examples_plot_2_astronomy.py:
Astronomy, 2D{1,1,1} dataset (Creating image composition)
^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^^
.. code-block:: default
More often, the images in astronomy are a composition of datasets measured
at different wavelengths over an area of the sky. In this example, we
illustrate the use of the CSDM file-format, and `csdmpy` module, beyond just
reading a CSDM-compliant file. We'll use these datasets, and compose an image,
using Numpy arrays.
The following example is the data from the `Eagle Nebula` acquired at three
different wavelengths and serialized as a CSDM compliant file.
Import the `csdmpy` model and load the dataset.
.. code-block:: default
import csdmpy as cp
filename = "https://osu.box.com/shared/static/of3wmoxcqungkp6ndbplnbxtgu6jaahh.csdf"
eagle_nebula = cp.load(filename)
Let's get the tuple of dimension and dependent variable objects from
the ``eagle_nebula`` instance.
.. code-block:: default
x = eagle_nebula.dimensions
y = eagle_nebula.dependent_variables
Before we compose an image, let's take a look at the individual
dependent variables from the dataset. The three dependent variables correspond
to signal acquisition at 502 nm, 656 nm, and 673 nm, respectively. This
information is also listed in the
:attr:`~csdmpy.DependentVariable.name` attribute of the
respective dependent variable instances,
.. code-block:: default
y[0].name
.. rst-class:: sphx-glr-script-out
Out:
.. code-block:: none
'Eagle Nebula acquired @ 502 nm'
.. code-block:: default
y[1].name
.. rst-class:: sphx-glr-script-out
Out:
.. code-block:: none
'Eagle Nebula acquired @ 656 nm'
.. code-block:: default
y[2].name
.. rst-class:: sphx-glr-script-out
Out:
.. code-block:: none
'Eagle Nebula acquired @ 673 nm'
Data Visualization
------------------
For convince, let’s view this CSDM object with three dependent-variables as three
CSDM objects, each with a single dependent variable. We use the split() method.
.. code-block:: default
data0, data1, data2 = eagle_nebula.split()
Here, ``data0``, ``data1``, and ``data2`` contain the dependent-variable at index
0, 1, 2 of the ``eagle_nebula`` object. Let's plot the data from these dependent
variables.
.. code-block:: default
import matplotlib.pyplot as plt
_, ax = plt.subplots(3, 1, figsize=(6, 14), subplot_kw={"projection": "csdm"})
ax[0].imshow(data0 / data0.max(), cmap="bone", vmax=0.1, aspect="auto")
ax[1].imshow(data1 / data1.max(), cmap="bone", vmax=0.1, aspect="auto")
ax[2].imshow(data2 / data1.max(), cmap="bone", vmax=0.1, aspect="auto")
plt.tight_layout()
plt.show()
.. image:: /auto_examples/correlated_examples/images/sphx_glr_plot_2_astronomy_001.png
:alt: Eagle Nebula acquired @ 502 nm, Eagle Nebula acquired @ 656 nm, Eagle Nebula acquired @ 673 nm
:class: sphx-glr-single-img
Image composition
-----------------
.. code-block:: default
import numpy as np
For the image composition, we assign the dependent variable at index zero as
the blue channel, index one as the green channel, and index two as the red
channel of an RGB image. Start with creating an empty array to hold the RGB
dataset.
.. code-block:: default
shape = y[0].components[0].shape + (3,)
image = np.empty(shape, dtype=np.float64)
Here, ``image`` is the variable we use for storing the composition. Add
the respective dependent variables to the designated color channel in the
``image`` array,
.. code-block:: default
image[..., 0] = y[2].components[0] / y[2].components[0].max() # red channel
image[..., 1] = y[1].components[0] / y[1].components[0].max() # green channel
image[..., 2] = y[0].components[0] / y[0].components[0].max() # blue channel
Following the intensity plot of the individual dependent variables, see the
above figures, it is evident that the component intensity from ``y[1]`` and,
therefore, the green channel dominates the other two. If we
plot the ``image`` data, the image will be saturated with green intensity. To
attain a color-balanced image, we arbitrarily scale the intensities from the
three channels. You may choose any scaling factor. Each scaling factor will
produce a different composition. In this example, we use the following,
.. code-block:: default
image[..., 0] = np.clip(image[..., 0] * 65.0, 0, 1) # red channel
image[..., 1] = np.clip(image[..., 1] * 7.50, 0, 1) # green channel
image[..., 2] = np.clip(image[..., 2] * 75.0, 0, 1) # blue channel
Now to plot this composition.
.. code-block:: default
# Set the extents of the image plot.
extent = [
x[0].coordinates[0].value,
x[0].coordinates[-1].value,
x[1].coordinates[0].value,
x[1].coordinates[-1].value,
]
# add figure
plt.imshow(image, origin="lower", extent=extent)
plt.xlabel(x[0].axis_label)
plt.ylabel(x[1].axis_label)
plt.title("composition")
plt.tight_layout()
plt.show()
.. image:: /auto_examples/correlated_examples/images/sphx_glr_plot_2_astronomy_002.png
:alt: composition
:class: sphx-glr-single-img
.. rst-class:: sphx-glr-timing
**Total running time of the script:** ( 0 minutes 5.519 seconds)
.. _sphx_glr_download_auto_examples_correlated_examples_plot_2_astronomy.py:
.. only :: html
.. container:: sphx-glr-footer
:class: sphx-glr-footer-example
.. container:: sphx-glr-download sphx-glr-download-python
:download:`Download Python source code: plot_2_astronomy.py `
.. container:: sphx-glr-download sphx-glr-download-jupyter
:download:`Download Jupyter notebook: plot_2_astronomy.ipynb `
.. only:: html
.. rst-class:: sphx-glr-signature
`Gallery generated by Sphinx-Gallery `_