Observation

Observation Details

Overview

Where

Groups: Mode, FOV, # spectra in map

Data Links

2014-05-20 12:05:10-13:12:59

HOP 243

Effects of Quiet Sun Weak Fields on the Chromosphere and Transition Region

x,y:	347",805"
Max FOV:	9"x81"
Target:	Quiet Sun
Nearby Events

6302A Continuum Intensity	9"x81"	1680 spectra
6302A Longitudinal Flux Density	9"x81"	1680 spectra
6302A Transverse Flux Density	9"x81"	1680 spectra
6302A Velocity 6301.5A	9"x81"	1680 spectra

Level 1 Summary
Level 2 Summary
Level 1 Monthly
Level 2 Monthly

SOTSP: HOP 243

2014-05-20T12:05:10 to 2014-05-20T13:12:59

Science Goal: Effects of Quiet Sun Weak Fields on the Chromosphere and Transition Region

Program: HOP 243 Very Fast Map, 9"x82", 2-side CCD, Q75, repeats

Target: Quiet Sun

xcen=347 ycen=805

Instrument: SOTSP

HOP/JOP: 0

Description: Effects of Quiet Sun Weak Fields on the Chromosphere and Transition Region 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 0x4c9 IRIS Shless Na IV 31x82", ROI 2, 32 s, Ca, CN: Na FOV = 31x82 arcsec, cadence = 32 sec, telemetry usage = 280 Mbits/hour FG 0xTBD 5250 Shless IQUV + 5172 Shless IV + CaII ROI 2: 5250 FOV = 25x82 arcsec, cadence = 72 sec, telemetry usage = 180 Mbits/hour BFI: images in Ca H and CN or G-band, shifted to match the NFI FOV 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 0x15e Very Fast Map, 4.5"x82", 2-side CCD, Q75, repeats: cadence = 39 sec, telemetry usage = 640 Mbits/hour The program with wider FOV should be used if IRIS is not rolled
if IRIS rolls by at least 5 degrees, then the narrower, faster program may be used with equal probability of overlap. Note: margin factor FG 0x4c9 --- 1.3 SP 0x15b --- 0.6 SP 0x15f --- 0.5 (by HOP 250)

Effects of Quiet Sun Weak Fields on the Chromosphere and Transition Region 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 0x4c9 IRIS Shless Na IV 31x82", ROI 2, 32 s, Ca, CN: Na FOV = 31x82 arcsec, cadence = 32 sec, telemetry usage = 280 Mbits/hour FG 0xTBD 5250 Shless IQUV + 5172 Shless IV + CaII ROI 2: 5250 FOV = 25x82 arcsec, cadence = 72 sec, telemetry usage = 180 Mbits/hour BFI: images in Ca H and CN or G-band, shifted to match the NFI FOV 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 0x15e Very Fast Map, 4.5"x82", 2-side CCD, Q75, repeats: cadence = 39 sec, telemetry usage = 640 Mbits/hour The program with wider FOV should be used if IRIS is not rolled
if IRIS rolls by at least 5 degrees, then the narrower, faster program may be used with equal probability of overlap. Note: margin factor FG 0x4c9 --- 1.3 SP 0x15b --- 0.6 SP 0x15f --- 0.5 (by HOP 250)

Annotations:

Chief Observer

Shine (RCO)