Changes between Version 9 and Version 10 of IPP_Progress_Report_20101025

Timestamp:

Nov 2, 2010, 10:10:07 AM (16 years ago)

Author:

eugene

Comment:

--

IPP_Progress_Report_20101025

@@ -11 +11 @@
 The regular processing is now being performed with the IPP tag
 ipp-20101029 (the Black Friday tag...).  This can be found in our svn
-tree at:
-
-https://svn.pan-starrs.ifa.hawaii.edu/repo/ipp/tags/ipp-20101029
+tree at: [source:tags/ipp-20101029]
 
 This update incorporates a number of changes that have been in the
@@ -19 +17 @@
 of the most important changes and improvements:
 
- * new output formats : PS1_V3 and PS1_DV2, with a number of new fields.  see: http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/CMF_PS1_V3 http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/CMF_PS1_DV2
+ * new output formats : PS1_V3 and PS1_DV2, with a number of new fields.  see: [wiki:CMF_PS1_V3] and [wiki:CMF_PS1_DV2]
 
- * the Star likelihood measurement and the Cosmic Ray detection are improved, see the discussion at: http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/StarGalaxySeparation
+ * the Star likelihood measurement and the Cosmic Ray detection are improved, see the discussion at: [wiki:StarGalaxySeparation]
 
  * Cosmic Rays are now masked in the chip-stage output images
 
- * Some improvements to both the DUAL and SINGLE convolution analysis, discussed at the following link (more discussion to be added soon):  http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/ppSubModifications_201009
+ * Some improvements to both the DUAL and SINGLE convolution analysis, discussed at the following link (more discussion to be added soon):  [wiki:ppSubModifications_201009]
 
- * Stack masking now includes information about the cause of masked pixels, as well as information about suspicious pixels.  see: http://svn.pan-starrs.ifa.hawaii.edu/trac/ipp/wiki/Stack
+ * Stack masking now includes information about the cause of masked pixels, as well as information about suspicious pixels: [wiki:Stack]
 
  * Fixes to the bright star masking:  The size of the bright star circles was OK for very bright stars (-23 inst mags), but too small for stars at or just beyond the saturation limit.  This is now fixed. Also, the w-band images used too small of a zero point for the over all scaling.