ING logoDifferences between UltraDAS and ancestral systems

This page is part of document INS-DAS-29, Operations manual for UltraDAS

Differences between s9.1 for IDS and s7.1 for IDS

S7.1 was released on the INT for IDS in February 1999. It was the culmination of the Unix-based observing systems including the "Data-Cell DAS" (i.e. the DAS based around the image-capture interface supplied by Data-Cell limited) and was the last system to be commissioned before the advent of UltraDAS.

S9.1 replaced s7.1 for IDS in July 2000. The intermediate systems, s8.1..s8.4 were tried out with IDS but were never released for routine observing.

These are differences between s9 and and s7 for IDS that are apparent to observers.

These are changes that are only visible to operations staff:

Differences between s8.2 for INT WFC and s7.1 for

S7.1 was released on the INT for WFC in February 1999, at hte same time as the
release for IDS. S8.2 for WFC was released in August 1999 and replaced s7.1 for INT
WFC only (s7.1 remained in use for IDS). S8.2 was the first system to include UltraDAS.
During 1999 and 2000, various upgrades were added to S8.2 as patches, including
some extra features from s8.3 at the WHT.

These are differences between s7 and s8 that are apparent to observers:

These are changes that are only visible to operations staff:


Differences between s8.3 for UES and PFIP and the VAX-ADAM DAS

The VAX-ADAM DAS, which employs the DMS, was first released on the WHT in the telescope's first year of operation. That system has been gradually adapted and improved over the years; the part visible to the observer dates from around 1993.

S8.3, including UltraDAS, was introduced in September 1999 to drive the new WHT WFC, a two-chip mosaic camera which produces too much data to handle in the ADAM DAS. The new system replaces the ADAM DAS (but not yet the ADAM ICS) when the mosaic camera is in use at UES or PFIP.

These are some differences of s8.3 from the ADAM DAS.