2007-07-28T00:04:26.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE XRT Sterling, A. Matsumoto, Takuma 0 Synoptic FS AR, FS, QS, SYN 18 -870.12 -200.16 522.68 522.68 2007-07-25T00:18:36.000Z 2007-07-25T23:59:58.000Z -870.12 -200.16 Joint Observation of the Solar Corona between Hinode EIS and NAOJ Norikura Observatory for nonthermal line broadening in the coronal emission Synoptic_with_bright_AR_3 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 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 ivo://sot.lmsal.com/VOEvent#2007-07-25T00:20:54Z