Einstein-Face (CASA 3.2)
Simulations using non-science images: the face of Einstein
Simdata can be used to simulate any digitized image. In this example, we use the face of Albert Einstein.
Step 1: obtain your image. Typically from the internet.
In this case, it is a jpg file.
Step 2: Convert your image to FITS
For the GIMP, start up the software
and in the main window select "Open" from the "File" menu.
The image will open up in a new window, you can use the GIMP to modify the image (adjust contrast, colormap etc).
Then, select "Save as" from the "File" menu in the window containing the image, and hit "Select File Type" in the dialog box to bring up the file type options, and select "Flexible Image Transport System". Pick a name for your file ending in .fits
Step 3: check your file
Read your file into e.g. ds9to check that a valid FITS file has been produced. You can also examine the pixel values to examine the scaling of the image. In this case, Einstein's forehead has pixel values around 230 and the background around 40, so there is plenty of contrast. You can also examine the image header in ds9. Under the "File" menu, select "Display FITS Header" and examine the output. Make sure that SIMPLE = T, NAXIS=2 and check BITPIX. In this case, BITPIX=8, which is not valid for reading into CASA, so we need to change that at the next step.
FITS header produced by GIMP:
SIMPLE = T
BITPIX = 8
NAXIS = 2
NAXIS1 = 300
NAXIS2 = 327
BZERO = 0.000000
BSCALE = 1.000000
DATAMIN = 0.000000
DATAMAX = 255.000000
HISTORY THIS FITS FILE WAS GENERATED BY GIMP USING FITSRW
COMMENT FitsRW is (C) Peter Kirchgessner (email@example.com), but available COMMENT under the GNU general public licence. COMMENT For sources see http://www.kirchgessner.net
COMMENT Image type within GIMP: GIMP_GRAY_IMAGE
Step 4 Add FITS header keywords and change the format
At this stage, we need to perform some manipulations on the FITS file to get it readable by CASA. For convenience, we are also adding a WCS at this point (though this can also be done in simdata). This routine is written in IDL, using the IDL astronomy library, but similar manipulations can be carried out in IRAF, or using the python PyWCS and PyFITS libraries, available from the astropython project.
The IDL code performs the following manipulations:
1) Reads in the FITS file as a 2D array, trims it to 300x300 pixels and converts it to real, 300x300x1 array (the third dimension is added for generality to allow the construction of an image cube, it is not actually necessary in this particular case). The image is also divided by 200000 to give it an approximately realistic scaling in Jy/pixel (again, not actually necessary).
2) Creates header keywords corresponding to the axis types (CTYPE1,2,3) values at the reference pixels (CRVAL1,2,3), the reference pixel positions (CRPIX1,2,3) and the axis increments (CDELT1,2,3), and the epoch (EPOCH).
3) Writes out the modified FITS file as "twodmodel.fits"