Viewing and manipulating FITS images


Lia Corrales, Kris Stern, Stephanie T. Douglas, Kelle Cruz

Learning Goals

  • Open FITS files and load image data
  1. Make a 2D histogram with image data
  2. Stack several images into a single image
  3. Write image data to a FITS file


FITS, file input/output, image manipulation, numpy, matplotlib, histogram, colorbar


This tutorial demonstrates the use of to download a data file, then uses to open the file, and lastly uses matplotlib to view the image with different color scales and stretches and to make histograms. In this tutorial we've also included a demonstration of simple image stacking.

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import numpy as np

# Set up matplotlib
import matplotlib.pyplot as plt
%matplotlib inline

from import fits

Download the example FITS files for this tutorial.

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from import download_file
image_file = download_file('', cache=True )

Opening FITS files and loading the image data

Let's open the FITS file to find out what it contains.

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hdu_list =

Generally, the image information is located in the PRIMARY block. The blocks are numbered and can be accessed by indexing hdu_list.

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image_data = hdu_list[0].data

Our data is now stored as a 2D numpy array. But how do we know the dimensions of the image? We can look at the shape of the array.

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Great! At this point, we can close the FITS file because we've stored everything we wanted to a variable.

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If you don't need to examine the FITS header, you can call fits.getdata to bypass the previous steps.

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image_data = fits.getdata(image_file)

Viewing the image data and getting basic statistics

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plt.imshow(image_data, cmap='gray')

# To see more color maps

Let's get some basic statistics about our image:

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print('Min:', np.min(image_data))
print('Max:', np.max(image_data))
print('Mean:', np.mean(image_data))
print('Stdev:', np.std(image_data))

Plotting a histogram

To make a histogram with matplotlib.pyplot.hist(), we'll need to cast the data from a 2D array to something one dimensional.

In this case, let's use the ndarray.flatten() to return a 1D numpy array.

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histogram = plt.hist(image_data.flatten(), bins='auto')

Displaying the image with a logarithmic scale

What if we want to use a logarithmic color scale? To do so, we'll need to load the LogNorm object from matplotlib.

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from matplotlib.colors import LogNorm

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plt.imshow(image_data, cmap='gray', norm=LogNorm())

# I chose the tick marks based on the histogram above
cbar = plt.colorbar(ticks=[5.e3,1.e4,2.e4])['5,000','10,000','20,000'])

Basic image math: image stacking

You can also perform math with the image data like any other numpy array. In this particular example, we'll stack several images of M13 taken with a ~10'' telescope.

Let's start by opening a series of FITS files and store the data in a list, which we've named image_concat.

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base_url = '{0:04d}.fits'

image_list = [download_file(base_url.format(n), cache=True) 
              for n in range(1, 5+1)]
image_concat = [fits.getdata(image) for image in image_list]

Now we'll stack the images by summing the concatenated list.

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# The long way
final_image = np.zeros(shape=image_concat[0].shape)

for image in image_concat:
    final_image += image

# The short way
# final_image = np.sum(image_concat, axis=0)

We're going to show the image, but need to decide on the best stretch. To do so let's plot a histogram of the data.

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image_hist = plt.hist(final_image.flatten(), bins='auto')

We'll use the keywords vmin and vmax to set limits on the color scaling for imshow.

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plt.imshow(final_image, cmap='gray', vmin=2E3, vmax=3E3)

Writing image data to a FITS file

We can do this with the writeto() method.

Warning: you'll receive an error if the file you are trying to write already exists. That's why we've set overwrite=True.

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outfile = 'stacked_M13_blue.fits'

hdu = fits.PrimaryHDU(final_image)
hdu.writeto(outfile, overwrite=True)


Determine the mean, median, and standard deviation of a part of the stacked M13 image where there is not light from M13. Use those statistics with a sum over the part of the image that includes M13 to estimate the total light in this image from M13.

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Show the image of the Horsehead Nebula, but in units of surface brightness (magnitudes per square arcsecond). (Hint: the physical size of the image is 15x15 arcminutes.)

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Now write out the image you just created, preserving the header the original image had, but add a keyword 'UNITS' with the value 'mag per sq arcsec'. (Hint: it may be helpful to read the documentation if you're not sure how to include both the header and the data.)

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