Study 000501:

ACRONYM: kappa

HOP266 study

Scanning raster type, parameters:

2" slit -  to reduce errors due to photon statistics for very weak lines
600 s exposure raster scanning the region 20"X512" - the selected 
lines are very different in the number of counts. Both scans should observe 
the same region and without any interruptions, if possible.

Because our exposures are very long, some additional calibration data will be 
required to monitor cosmic rays and hot/warm pixels.  

Line list for diagnostics of kappa for both scanning raster exposures
Ion Species  and Wavelength (Angstrom) / Approximate Total Counts for
Exposure (10 s) (per pixel) - AR

Ca XVII 192.82 / 572.40
Fe XII 195.12 / 4240.80
He II 256.32 / 246.90
O IV 207.24 / 0.5
O IV 279.93 / 0.9
O V 271.04 /0.2
S X 180.73 / 3.6
S X 264.23 / 106.2
S XI 246.90 / 12.7
S XI 281.40 / 9.9
S XI 285.82 / 9.2
Ca XIV 193.87 / 163.1
Ca XV 176.92 / 0.7
Ca XV 200.98 / 71.2
Ar XIV 191.36 / 21.6
Ar XIV 194.39 / 67.4
Fe XI 182.17 / 61.2
Fe XI 188.23 / 747.9
Fe XI 257.77 / 7.9
Fe XII 186.85 / 222.0
Fe XIII 196.53 / 335.8
Fe XIII 202.04 / 729.6
Fe XIII 203.82 / 458.0

Pointing:
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For the main science observations, use studies KAPPA and KAPPA_SHORT. The slit 
should be located through the center of an active region near the center of 
the solar disk, encompassing the AR core, moss, and outlying coronal loops.

Instruction to planner:
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The observation should be run in following (CHAINED) sequence:

1) 1 x PRY_slot_context_v3,
2) 1 x KAPPA_SHORT,
3) 1 x KAPPA,
4) 1 x KAPPA_SHORT,
5) 1 x PRY_slot_context_v3

Repeating the whole sequence above in three consecutive days are desired
(three days in total). If necessary, this can be split across two OP periods.

WARNING:
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None