SOTSP: Emerging flux and jet, SP
2007-07-27T19:49:37 to 2007-07-27T20:52:27
Science Goal: Emerging flux and jet
Program: Scanstep 2 bni2 15arcsec
Target: East Limb
xcen=-876 ycen=-193
Instrument: SOTSP
HOP/JOP: 10
Description:
Daily Note and User Entry: Weekly Meeting SOT: Support HOP10 Norikura and HOP24, which observes prominences and filaments at limb. XRT: Stop X-ray observation (and will likely perform CCD bakeout soon). EIS: Memory table upload (to EEPROM) in preparation for next week's likely s/w upload. NHK video taping of Hinode operations today(!).
Request to SOT: Observation of Ca H spicules. The sequence that was run previously is used. Widest FOV in the NS direction is desired.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines
Other Instruments: Norikura: High dispersion spectra of Fe X6374 and Fe XIV5303 are obtained. High-acuracy Doppler velocity and line width are given. Independent Fe XIV 5303 imaging observations provide high-cadence imaging and Doppler informaiton. Bi-products: <
This is the most important for EIS team.>
: By the simultaneous observations with Norikura Solar Observatory, EIS line width of instrumental origin is absolutely calibrated. In EIS bandpass there are Fe X lines in the short wavelength band and Fe XIV lines in the long wavelength band. These are calibrated with Fe X 6374 and Fe XIV 5303 emission lines. Norikura Solar Observatory is going to support this campaign observation with a high priority.
Daily Note and User Entry: Weekly Meeting SOT: Support HOP10 Norikura and HOP24, which observes prominences and filaments at limb. XRT: Stop X-ray observation (and will likely perform CCD bakeout soon). EIS: Memory table upload (to EEPROM) in preparation for next week's likely s/w upload. NHK video taping of Hinode operations today(!).
Request to SOT: Observation of Ca H spicules. The sequence that was run previously is used. Widest FOV in the NS direction is desired.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines
Other Instruments: Norikura: High dispersion spectra of Fe X6374 and Fe XIV5303 are obtained. High-acuracy Doppler velocity and line width are given. Independent Fe XIV 5303 imaging observations provide high-cadence imaging and Doppler informaiton. Bi-products: <
This is the most important for EIS team.>
: By the simultaneous observations with Norikura Solar Observatory, EIS line width of instrumental origin is absolutely calibrated. In EIS bandpass there are Fe X lines in the short wavelength band and Fe XIV lines in the long wavelength band. These are calibrated with Fe X 6374 and Fe XIV 5303 emission lines. Norikura Solar Observatory is going to support this campaign observation with a high priority.
wavelength: 6302A Continuum Intensity cadence: 0.01 min fov: 8,162 images: 856 JavaScript Landing Page
