2013-01-19T11:34:06.000Z 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 Bando Cruz 0 Weak AR Observation at E Limb Quiet Sun DC DC 13 -929 200 111 111 2009-12-04T19:03:31.000Z 2009-12-05T00:39:42.000Z -929 200 HOP 135 Test Near DC AR mode Case 3 (AR at the Limb) G-Band 90min, CaH 30sec -- T. Cruz The primary instrument for the observations is the SOT/NFI. Duration: The observations should last for a minimum of 30 minutes, up to a maximum of two hours. Cadence: The goal for the cadence would be 10-15 seconds for images in both wings, with a maximum acceptable cadence of around 30 seconds. The cadence of the images is the highest priority observable. Field-of-View: The field of view would be primarily the solar disk near to the solar limb. It would be desirable to include the solar limb in the edge of the field of view. An overall coverage as small as 100" x 100" would be fine, with larger fields acceptable. Wavelengths: The wavelengths of the two wing positions should be approximately 0.6 A on either side of the nominal line core position. In order to ensure the proper positioning of these wing positions, a scan of the full line profile should be performed in order to determine the tuning of the filter relative to the true line center. This scan can be quickly analyszed to provide the optimal wavelength position of the two wing wavelengths. Some feedback concerning the wavelength drift of the NFI due to the day-night temperature fluctuations during eclipse season might be needed Auxillary observations from SOT/BFI and XRT would be useful, but only if they do not impact the cadence achieved with the NFI or reduce the duration of the observations below the 30 minute limit. SOT/BFI: Ca II H images, 30 second cadence XRT: Ti-Poly images, 60 second cadence ivo://sot.lmsal.com/VOEvent#2009-12-04T19:03:00Z