<?xml version="1.0" encoding="UTF-8" ?>
<VOEvent role="utility"
	ivorn="ivo://sot.lmsal.com/VOEvent#VOEvent_ObsS2007-07-27T06:44:43.000.xml"
	version="1.11"
	xmlns="http://www.ivoa.net/xml/VOEvent/v1.11"
	xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance"
	xmlns:lmsal="http://sot.lmsal.com/lmsal"
	xmlns:crd="urn:nvo-coords"
	xsi:schemaLocation="http://www.ivoa.net/xml/VOEvent/VOEvent-v1.1.xsd">


	<Who>
		<!-- Data pertaining to curation: observer, telescope, instrument, planner, tohbans, ... -->
		<Date>2007-07-31T22:35:55.000Z</Date>    <!-- Time VOEvent was generated. -->
		<PublisherID>http://sot.lmsal.com</PublisherID>

		<Contact>
			<Name>Mr. Sam Freeland</Name>
			<Institution>Lockheed Martin Solar and Astrophysics Laboratory (LMSAL)</Institution>
			<Communication>
				<Uri>http://www.lmsal.com</Uri>
				<AddressLine>Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304</AddressLine>
				<Telephone>null</Telephone>
				<Email>null</Email>
			</Communication>		</Contact>

		<lmsal:Telescope>HINODE</lmsal:Telescope>
		<lmsal:Instrument>SOT</lmsal:Instrument>
		<lmsal:Tohbans>Arikawa</lmsal:Tohbans>
		<lmsal:ChiefPlanner>Sterling</lmsal:ChiefPlanner>
		<lmsal:ChiefObserver>Isobe, Nakamura and Shine</lmsal:ChiefObserver>
	</Who>


	<What>
		<!-- Data about what was measured/observed.  Some tags come from predicted event. -->
		<Param name="URLParent" value="http://www.lmsal.com/solarsoft/hinode/movies/voevent_movies_sot/2007/07/27/20070727_0000_20070728_0000_prog_12/20070727_0000_20070728_0000_prog_12.html" />
		<Param name="catalogLink" value="http://www.lmsal.com/cgi-ssw/sot_time2form.sh?start_time=2007-07-27+06%3A44%3A43.000&amp;amp;stop_time=2007-07-27+17%3A35%3A07.000&amp;amp;obs_type=*" />
		<lmsal:JOP_ID>10</lmsal:JOP_ID>
		<lmsal:OBSTITLE>H lc, CaH, G-b 2Kx2K</lmsal:OBSTITLE>
		<lmsal:TARGET>Filament</lmsal:TARGET>
		<lmsal:SCI_OBJ>FIL</lmsal:SCI_OBJ>
		<lmsal:SCI_OBS>FIL</lmsal:SCI_OBS>
		<lmsal:slotNumber>12</lmsal:slotNumber>
	</What>


	<WhereWhen>
		<!-- Space and Time Coordinates. -->
		<ObservatoryLocation ID="HINODE" />

		<ObservationLocation>
			<lmsal:xCen>423</lmsal:xCen>		<!-- xcen and ycen from FITS -->
			<lmsal:yCen>-397</lmsal:yCen>
			<lmsal:xFov>111</lmsal:xFov>
			<lmsal:yFov>111</lmsal:yFov>
			<crd:AstroCoords coord_system_id="UTC-HGS-TOPO">
				<crd:Time>
					<crd:TimeInterval>2007-07-27T06:44:43.000Z 2007-07-27T17:35:07.000Z</crd:TimeInterval>
				</crd:Time>
				<crd:Position3D>423 -397</crd:Position3D>
			</crd:AstroCoords>
		</ObservationLocation>

	</WhereWhen>


	<Why>
		<!-- Why was observation performed.  Initial scientific assessment, hypothesized mechanisms, classifications, ... -->
		<Concept>
			<lmsal:Goal>filament</lmsal:Goal>
			<lmsal:Purpose>H lc, CaH, G-b 2Kx2K 2x2, 30s</lmsal:Purpose>
		</Concept>

		<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; andnbsp; andnbsp; andnbsp;; 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.
		</Description>
	</Why>

	<Citations>
	</Citations>
</VOEvent>
