SECCHI/HI-1 Ahead Level-2 files from SwRI

C. E. DeForest, March 2015

(More information can be found here.)

The HI-1 images have been post-processed using two separate pipelines. The first, "L2S", uses a slight variant of the steps in DeForest et al. 2011, only through the starfield subtraction step. This results in the best photometry in the bright portions of each image, but leaves a noticeable remnant of the starfield. The second, "L2M", uses also the motion-filtering step mentioned in DeForest et al. 2011. This results in the best photometry in the faint portions of each image, but results in slight ringing artifacts near the bright edge of the field (amplitude is about 1%-3% of the Thomson signal) and also rejects some quasi-stationary features that are retained by the L2S series.

For general-purpose viewing, L2M is preferred, but for some applications (e.g. comet tracking) L2S is preferred.

The HI-1 L2M and L2S images are both batch-processed. The batches are 7 days long and are staggered by 0.5 day. They include steps that take place in the celestial plane rather than the instrument plane, so a small number of pixels on the left and right side of each image are set to NaN by each processing step. The images are resampled back to the original focal plane after processing, leaving a small and variable margin at the right and left side of each image.

 Name                                      Last modified      Size  
 Parent Directory                                               -   
 L2M-QL-frames/                            2015-02-24 10:16    -   
 L2M-QL-movies/                            2015-02-24 10:52    -   
 L2M/                                      2015-02-24 03:10    -   
 L2S-QL-frames/                            2015-02-24 11:30    -   
 L2S-QL-movies/                            2015-02-24 09:02    -   
 L2S/                                      2015-02-23 23:57    -