2009-12-04T13:49:29.000Z http://sot.lmsal.com Ted Tarbell LMSAL http://lmsal.com 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA, 94304 +1-650-424-2400 tarbell@lmsal.com Hinode SOT Arikawa Bando Cruz 0 0 null HOP 135 Test Near DC DC DC Quiet Sun 10 -632 200 0 0 2009-12-07T07:01:00.000Z 2009-12-07T08:16:00.000Z -632 200 HOP 135 Test Near DC HOP 135d, H alpha wings+cont, 56x108" -- 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