Although the ISO data are now all public, allowing anyone to reduce any data they like, I've found it useful to place on the web some of my own data reduced with state-of-the-art package. This is not to imply that no-one can do better than me, but more to make sure that not to many versions of the same data go around in the litterature. So feel free to pick up anything you like here, though make sure you read the little texts I place in front of the images, and enjoy...

A general note on ISOCAM astrometry:

Although ISO's pointing is very accurate (1" or so for absolute pointing), jitter in ISOCAM lens wheel repositionning can lead to an offset of at most 2 pixel between the intended and actual positions. Please take this into account when using these images.

Currently available are:


M51 at 15 Ám

M 51 at 15 microns, click to download fits file Here is the data reduction history:
  • The image is the sum of two 10x10 rasters secured during revolutions 30 and 576.
  • Both observing setups were identical: integration time of 2.1 seconds, pixel field of view of 3 "/pix, raster steps of 2/3 of the array.
  • Dark correction was performed with the model dark as in CIA V3.0
  • Deglitching was done with the multiresolution median transform method, followed by manual flagging of glitches with positive tails.
  • Memory effects were corrected with the Fouks-Schubert algorithm
  • Flat-field and image reconstruction were done with Marc Antoine Miville-Deschênes SLICE package, that takes into account long-term variations, as well as short term flat-field variations and optical distortion.
  • The data have been converted to mJy/pix using the conversion factors available in CIA V3.0

Make sure you take a look at the gif image below that points to remaining artefacts in the image.

click on the image to download the gzipped fits file notes on remaining artefacts in the image

M51 at 6.75 Ám

M 51 at 6.75 microns, click to download fits file Here is the data reduction history:
  • The image is the sum of two 10x10 rasters secured during revolutions 30 and 576.
  • Both observing setups were identical: integration time of 2.1 seconds, pixel field of view of 3 "/pix, raster steps of 2/3 of the array.
  • Dark correction was performed with the model dark as in CIA V3.0
  • Deglitching was done with the multiresolution median transform method, followed by manual flagging of glitches with positive tails.
  • Memory effects were corrected with the Fouks-Schubert algorithm
  • Flat-field and image reconstruction were done with Marc Antoine Miville-Deschênes SLICE package. Contrary to the 15 Ám data, no correction for long-term transients were applied as this component of the transient could not be determined from the data.
  • The data have been converted to mJy/pix using the conversion factors available in CIA V3.0

Make sure you take a look at the gif image below that points to remaining artefacts in the image.

click on the image to download the gzipped fits file notes on remaining artefacts in the image


Last modified on January 17, 2000