SOTSP: Norikura CMPN, E limb
2007-07-27T11:35:12 to 2007-07-27T12:14:41
Science Goal: Coroal loop line width
Program: Fast map 200 arcsec, ROI 2
Target: East Limb
xcen=342 ycen=-392
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: -1 min fov: 198,162 images: 625 JavaScript Landing Page
