There has been evidence that due to poor hygienic practices dust has
accumulated in the CIRSI dewar and when the filter wheel is rotated this
dust gets displaced or moved. It is therefore important that
filter wheel changes are minimized during the night and that
dome flats are taken frequently to track this dust.
CIRSI has two J band filter and we will need to determine which one
to use: more on this later. Basically the wider higher throughput
filter has a red leak and the background in a dark dome needs to
be measured for these two filters: Jc and Jx(or Jg).
Perl script to generate grid of 4 positions for a complete tile
cirsi_grid3.pl download this, make it
executable i.e. chmod +x cirsi_grid3.pl; type cirsi_grid3.pl; if it
does not work check the path to perl as explain in the source code.
The script works well except at the exact pole which is pretty good.
Filters that were loaded when CIRSI was shipped to LCO:
0 Dk Dark position; metal plate
1 Jc New Carnegie J replacing Z
2 Jg J(Gemini consortium specification)
3 Hs H short side
4 Hx H(Geminini consortium spec)
5 Hl H long side
6 Jn JOH narrow band in OH gap in J
7 Hn HOH " " " "
Some notes on Dithering and Macros
Some useful scripts: These also reside in rigel.lco.cl:/home/cirsi/bin
tonight script to create and make a link to the nightly data directory
H-band only: g133 g133_dupont.tcs The file
contains the position that the telescope should be pointed
at to make a CIRSI tile. There are 4 tiles. Try to
get 1 pass around all 2 tiles each night. Say a 7 point
dither pattern with 3 times 40secs at each position. Using
a dither step of around 10arcsecs.
The 4 separare tiles are called:
G133_NE; G133_NW; G133_SE, G133_SW
For each tile 5 positions are given, e.g.
G133_NE_A; B, C, D, X
X is the centre of the tile and should not be used as a pointing
centre. A, B, C and D are the pointings required to make a contiguous tile.