| Overview | Where | Groups: Mode, FOV, # spectra in map | Data Links |
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2007-07-26 02:36:05-03:34:39
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polar CH photospheric field polar CH photospheric field |
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| 6302A Continuum Intensity | 109"x162" | 690 spectra | | 6302A Longitudinal Flux Density | 109"x162" | 690 spectra | | 6302A Transverse Flux Density | 109"x162" | 690 spectra | | 6302A Velocity 6301.5A | 109"x162" | 690 spectra |
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Level 1 Summary
Level 2 Summary
Level 1 Monthly
Level 2 Monthly |
SOTSP: polar CH photospheric field
2007-07-26T02:36:05 to 2007-07-26T03:34:39
Science Goal: polar CH photospheric field
Program: Normal map 100 arcsec
Target: North pole
xcen=-2 ycen=937
Instrument: SOTSP
HOP/JOP: 0
Description:
Daily Note and User Entry: EIS: Would like polar coronal hole pointing for co-observing with XRT and SOT. Two programmes are being considered. 1) Slow context raster then fast sit'n'stare slit observations at several positions for short-timescale dynamics. 2) Jet dynamics with 40" slot sit'n'stare observations EIS will perform MHC software upload toward end of this week. For programme 2 we suggest SOT fast SP maps to observe changes in the photospheric field, and XRT single-filter, high-cadence observations to complement EIS temperature coverage. SOT: Support HOP10 Norikura and HOP24, which observes prominences and filaments at limb. andnbsp
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We may try tests for H-alpha dopplergrams, and H-alpha flat field imaging in the quiet sun. SOT: Memory upload operation to load new frame definition tables in FPP memory.
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: EIS: Would like polar coronal hole pointing for co-observing with XRT and SOT. Two programmes are being considered. 1) Slow context raster then fast sit'n'stare slit observations at several positions for short-timescale dynamics. 2) Jet dynamics with 40" slot sit'n'stare observations EIS will perform MHC software upload toward end of this week. For programme 2 we suggest SOT fast SP maps to observe changes in the photospheric field, and XRT single-filter, high-cadence observations to complement EIS temperature coverage. SOT: Support HOP10 Norikura and HOP24, which observes prominences and filaments at limb. andnbsp
andnbsp
andnbsp
andnbsp
We may try tests for H-alpha dopplergrams, and H-alpha flat field imaging in the quiet sun. SOT: Memory upload operation to load new frame definition tables in FPP memory.
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.
Annotations:
Hits: 45
Chief Observer
Sekii, Watanabe and Shine
See also
wavelength: 6302A Continuum Intensity cadence: -1 min fov: 109,162 images: 690 JavaScript Landing Page
