Welcome to the EIT CALROC World Wide Web server.
Welcome to the home page for the NRL Extreme-ultraviolet Imaging Telescope Calibration Rocket (EIT CalRoc). The EIT CalRoc program is a cooperative effort invloving contributions from all the groups of the EIT Consortium.
The flight successfully occured 16 October 1997, from White Sands Missile Range, New Mexico (WSMR). The payload landed very gently (less than 5 km beyond the lava beds!!!) and the filters appear to be intact, so a post-flight calibration will be meaningful. We have started the post-flight field calibrations (171 and 304 Angstrom) here at WSMR with the NRL/LMPARL EUV collimator. Initial indications are that there is no change between the pre-flight and post-flight field calibrations.
The last image taken during the EIT CalRoc flight can be viewed by clicking on the thumbnail image below. This is a 1024x1024 image in the 171 Angstrom bandpass. The image has been scaled for presentation in a GIF format. You are invited to return frequently to this WWW site to view the CalRoc data as they are reduced and applied to the SOHO EIT analysis.
primary calibration images
are now available. These are a series of 512x512 images taken in each
waveband around the apogee of the fight. The reduced spatial resolution images require shorter exposure and readout times than full resolution images. Thus, 512x512 images can be obtained in all wavelengths during the time of minimum absorption of the residual atmosphere.
Preliminary images of the
ratio of the EIT CalRoc data to the EIT SOHO data are now available. Although this analysis requires much more work, the preliminary results are very interesting. In this first approach, the images have been normalized at their edges. The most obvious difference is that the detector response in the region covered by the solar disk has degraded to about 50% of the response at the edge of the field of view. There is increased degradation at the limb, corresponding to the increased EUV dose in this region. There is also increased degradation in the active region bands for the same reason. Although it is difficult to scale the GIF images to also show the pattern in the degradation caused by the shadow of the filter support grid for the focal plane
filter, this pattern can be seen in the Fe IX,X and Fe XII ratio images. Sharp, small scale structures in these ratio images are artifacts of the time difference between the SOHO and CalRoc images. This problem is the worst for the He II ratio image (in which a SOHO data dropout causes further problems).
From the above ratios, a general flatfield correction can be derived for the SOHO EIT images. Such a correction can then be applied to data from the time immediately before and after the CalRoc flight. The validity of this correction will slowly decline with increasing time from the CalRoc flight because of the changing level of degradation with time. Proceedures for tracking the relative degradation are under development. A very preliminary example of the general CalRoc correction can be seen in the CalRoc corrected 18 October 1997 Fe IX,X SOHO EIT image. This should be compared with the uncorrected Fe IX,X SOHO EIT image from the SOHO Summary Database. The most obvious improvements are the removal of spurious darkening at the limb and the removal of the residual burned-in grid pattern from the focal plane filter support grid. These improvements represent a major advance for observational programs invloving features extending from the disk to beyond the limb (e.g. EUV plumes and jets).
This welcome page is still under development.