2020-05-29T04:51:16.000Z 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 SOTSP Arikawa Sakao Ichimoto 25 Hinode-ITP campaign (Disc Centre) Quiet Sun Hinode-ITP campaign QS NONE 5 23.8 6.949 2.936 40.576 2007-09-05T11:14:38.000Z 2007-09-05T11:27:35.000Z 23.8 6.949 Hinode-ITP campaign Dynamic Mode, 2.9x40 arcsec, repeat Daily Note and User Entry: XRT calibrations: 1) G-band exposures at the 5 pointing positions (10min each, 4 pointings near 4 extreme positions and disk center) to characterize the position of contaminants. 2) Dither-pattern pointings (3 points at the disk center, about 21min) to characterize the X-ray flat-field. SOT: HOP 25 andnbsp; andnbsp; andnbsp; 07:00UT - 11:30UT@(0,0) andnbsp; andnbsp; andnbsp; 11:30UT - 15:00UT@(-495,0) andnbsp; andnbsp; andnbsp; 15:00UT - 18:00UT@(-315,0) andnbsp; andnbsp; andnbsp; andnbsp; 07:00UT - 12:30UT@(-800, 0) andnbsp; andnbsp; HOP 02 North pole (6 hours); Request to SOT: We would propose to use the SP instrument in SOT to measure the photospheric magnetic field with the line pair at 630.2 nm. Additional Filtergram observations with SOT would be necessary for doing the alignment with the ground- based data. We propose to perform a time series of rather short scans with a high repetition cadence of about 2 minutes at disk center. With an exposure time of 4.8 seconds and a step size of 0.16'' the scan would amount to some 4''. That means that alignment is an issue. But since the slit of SP is 160'', there should be enough room for overlapping field of views. ; Scientific Objectives: The goal of our campaign is an understanding of the dynamic quiet sun magnetic and of its coupling from the photosphere to the chromosphere. We will acquire spectro-polarimetric ;data from the SST, the VTT, and THEMIS. At the VTT ;will use the spectropolarimeter TIP and POLIS to measure the deep photosphere (Fe I 1564.8 nm), the middle photosphere (Fe I 6302 nm), and the chromosphere (intensity profiles of Ca II H 397 nm). At THEMIS we will concentrate on the infrared Ca lines (849.8 nm, 854.2 nm) to study the chromospheric response on photospheric magnetic field. For alignment we will also record a photospheric line like Fe I 525.0 nm at THEMIS. At the SST we will take advantage of the tunable filter imaging system to obtain context information (images and magnetograms) at highest possible resolution. ; This multi-wavelength approach will be complemented with speckle- reconstructed Halpha images from DOT. For this campaign it would be of great advantage to complement the data set with spectro-polarimetric data at 0.3'' spatial resolution (at the VTT we may achieve a spatial resolution of only 0.5'' at best with the help of the adaptive optics system). ; Other Instruments: STT, VTT, THEMIS, DOT ivo://sot.lmsal.com/VOEvent#2007-09-05T10:12:00Z