2007-07-25T21:36:02.000Z 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 SOT Arikawa Sterling Sekii, Watanabe and Shine 0 spicules and jets Spicule and Jets JET, LMB, SPI JET, LMB, SPI 5 935 100 55 55 2007-07-24T11:28:10.000Z 2007-07-24T14:03:28.000Z 935 100 spicules and jets G, Ca H, 4504, 1Kx1K, 1x1 Daily Note and User Entry: EIS: Limb observations, for 7 hours, once at east limb, once at west limb, for absolute wavelength calibration. These should be performed on the same day or on consecutive days. EIS will perform MHC software upload this week. We suggest that this takes after the first synoptic of the day, during the longest inter-synoptic gap. SOT: Support HOP10 Norikura and HOP 24, 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. XRT: CCD Bakeout probably from MOnday evening till Tuesday evening. andnbsp;Dark calibration routines before and after. andnbsp; Coalignment program run (N-limb, E-limb, 2hour for each) to run in Tuesday plan.; 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. ivo://sot.lmsal.com/VOEvent#2007-07-24T11:27:30Z