<?xml version="1.0" encoding="UTF-8" ?>
<VOEvent role="prediction"
	ivorn="ivo://sot.lmsal.com/VOEvent#2014-03-01T23:55:00Z"
	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>2014-03-03T21:30:50.000Z</Date>    <!-- Time VOEvent was generated. -->
		<PublisherID>http://sot.lmsal.com</PublisherID>

		<Contact>
			<Name>Ted Tarbell</Name>
			<Institution>LMSAL</Institution>
			<Communication>
				<Uri>http://lmsal.com</Uri>
				<AddressLine>3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA, 94304</AddressLine>
				<Telephone>+1-650-424-2400</Telephone>
				<Email>tarbell@lmsal.com</Email>
			</Communication>		</Contact>

		<lmsal:Telescope>Hinode</lmsal:Telescope>
		<lmsal:Instrument>SOTSP</lmsal:Instrument>
		<lmsal:Tohbans>Miyoshi</lmsal:Tohbans>
		<lmsal:ChiefPlanner>Minoshima</lmsal:ChiefPlanner>
		<lmsal:ChiefObserver>Cruz(RCO)</lmsal:ChiefObserver>
	</Who>


	<What>
		<!-- Data pertaining to what was observed, measured, ...   Some of these tags might move into Who section. -->
		<lmsal:obsId></lmsal:obsId>
		<lmsal:OBS_NUM>0</lmsal:OBS_NUM>
		<lmsal:JOP_ID>0</lmsal:JOP_ID>
		<lmsal:JOP></lmsal:JOP>
		<lmsal:JOIN_SB>null</lmsal:JOIN_SB>    <!-- S=SOT, X=XRT, E=EIS, SX=SOT+XRT, EX=EIS+XRT -->
		<lmsal:OBSTITLE>HOP 246 (hot plasma)</lmsal:OBSTITLE>
		<lmsal:SCI_OBJ>AR</lmsal:SCI_OBJ>     <!--  Scientific objectives -->
		<lmsal:SCI_OBS>AR</lmsal:SCI_OBS>     <!-- Objects being observed -->
		<lmsal:NOAA_NUM>11991</lmsal:NOAA_NUM>
		<lmsal:TARGET>disk center</lmsal:TARGET>
		<lmsal:slotNumber>1</lmsal:slotNumber>
	</What>


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

		<ObservationLocation>
			<lmsal:xCen>-212</lmsal:xCen>		<!-- xcen and ycen from FITS -->
			<lmsal:yCen>-130</lmsal:yCen>
			<lmsal:xFov>0</lmsal:xFov>
			<lmsal:yFov>0</lmsal:yFov>
			<crd:AstroCoords coord_system_id="UTC-HGS-TOPO">
				<crd:Time>
					<crd:TimeInterval>2014-03-01T23:55:00.000Z 2014-03-02T03:03:00.000Z</crd:TimeInterval>
				</crd:Time>
				<crd:Position3D>-212 -130</crd:Position3D>
			</crd:AstroCoords>
		</ObservationLocation>

		<Group name="saaIntervals">
			<Param name="saaInterval" value="2014-03-02T02:42:30Z 2014-03-02T03:03:00Z" />
		</Group>
	</WhereWhen>


	<Why>
		<!-- Why was observation performed.  Initial scientific assessment, hypothesized mechanisms, classifications, ... -->
		<Concept>
			<lmsal:Goal>Hot plasma properties in Active Regions</lmsal:Goal>
			<lmsal:Purpose>Fast map, BFI Full FOV, Q65, 1-side CCD</lmsal:Purpose>
		</Concept>

		<Description>
			abstract of observational proposal Objective: Determination of coronal plasma properties of core of AR: in particular, temperature distribution (high temperature peak, slope, and low T end of distribution at TR temperatures), and Doppler shifts at different temperatures exploiting the large temperature coverage of spectral observations of EIS and IRIS.  Scientific Background: Determining the properties of coronal plasma (temperature, density, velocity distributions) can provide stringent constraints on the characteristics of the mechanisms of coronal heating (e.g., Klimchuk 2006, Reale 2010, Testa et al. 2012, Tripathi et al. 2012).  of coronal plasma properties of core of AR: in particular, temperature distribution (high temperature peak, slope, and low T end of distribution at TR temperatures), and Doppler shifts.  Coordinated imaging and spectral observations of active regions with Hinode and IRIS will determine the plasma temperature, density and velocity with unprecedented temperature coverage (low TR to corona). IRIS also provides plasma spectral diagnostics at high spatial resolution at transition region temperatures (O IV, Si IV) and coronal temperatures (the FeXII line in the IRIS spectral range is intrinsically weak so we request 30s exposures to be able to get good S/N), and high spatial resolution (0.166???/pix) imaging at transition region and chromospheric temperatures.
		</Description>
	</Why>

</VOEvent>
