SOTSP: Effects of Quiet Sun Weak Fields on the Chromosphere and Transition Region
2016-03-26T22:30:00 to 2016-03-27T00:20:00
Science Goal:
Program: HOP 243 Plage, Lower-TLM DynMode, 9x82, centered
Target: Plage
xcen=701 ycen=304
Instrument: SOTSP
HOP/JOP: 0
Description:
request to SOT SOT should use a FOV slightly larger than that of IRIS in both dimensions, to allow for pointing inaccuracy, and cadence of 30-75 seconds, to follow the evolution of the weak fields. For the BFI and NFI, the FOV should be at least 25 x 80 arcsec. NFI: magnetograms with high SNR, using ROI # 2 to shift by 25 arcsec towards the lower part of the CCD to have best image quality. Two programs being tested are: FG 0x04eb IHOP243 low-TLM, Shless Na IV 31x82", ROI 1, 32 s, Ca, CN SP: very fast maps, to obtain the required time resolution with enough slit positions to maximize the chance of overlap with the IRIS slit. Both sides of the CCD are used to increase SNR. Two programs have been tested so far: SP 0x15b Very Fast Map, 9"x82", 2-side CCD, Q65, repeats: cadence = 73 sec, telemetry usage = 500 Mbits/hour SP 0x190 HOP 243 low-TLM, Very Fast map 9x82, lower half For a plage target observed with IRIS, use either SP 0x0194 HOP 243 Plage, DynamicsMode 9x82, bottom half, uses ~1000 Mbits/hr SP 0x0195 HOP 243 Plage, Lower-TLM DynMode, 9x82, bottom half, uses ~500 Mbits/hr Note: margin factor FG 0x4eb --- 1.3 SP 0x15b --- 0.6 SP 0x190 --- 0.6 SP 0x194 and 195 --- 0.5 (edited on 2016 Feb. 10)
