XRT: Synoptic
2007-07-19T20:05:16 to 2007-07-19T20:06:59
Science Goal: Joint Observation of the Solar Corona between Hinode EIS and NAOJ Norikura Observatory for nonthermal line broadening in the coronal emission
Program: Synoptic_with_bright_AR_4
Target: FS
xcen=70 ycen=-589
Instrument: XRT
HOP/JOP: 0
Description:
Tim File-OBS_DEC: Synoptics Open+Al/Mesh (181/4096) - Backup Period
Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines Daily Note: none
Request to XRT HOP Number 0010: The sequence that was run previously is used. No strong request.
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: andlt
This is the most important for EIS team.andgt
: 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.
Scientific Objectives: To understand the origin of non-thermal line broadening in coronal emission lines
wavelength: Open cadence: 0.1 min fov: 392,392 images: 13 JavaScript Landing Page