Observation

Observation Details

SOT: H lc, CaH, G-b 2Kx2K

2007-07-27T06:44:39 to 2007-07-27T17:35:07

Science Goal: filament

Program: H lc, CaH, G-b 2Kx2K 2x2, 30s

Target: Filament

xcen=423 ycen=-397

Instrument: SOT

HOP/JOP: 10

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 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 HOP 24, which observes prominences and filaments at limb. andnbsp
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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: 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.

Annotations:

Chief Observer

Isobe, Nakamura and Shine

Related Links
Cites: H lc, CaH, G-b 2Kx2K

Timeline: gif use