cassini mission correction

Elena.Budnik
1 parent ff4c5a95
Showing 7 changed files with 85 additions and 328 deletions Show diff stats
Instrument/AMDA/Cassini/Ephemeris.xml
Instrument/AMDA/Cassini/RPWS.xml
NumericalData/AMDA/Cassini/Ephemeris/cass-ephem-eqt.xml
NumericalData/AMDA/Cassini/Ephemeris/cass-ephem-polar.xml
Observatory/AMDA/Cassini.xml
Person/Joseph.Groene.xml
Person/Linda.Spilker.xml
@@ -5,36 +5,29 @@
     <ResourceID>spase://CDPP/Instrument/AMDA/Cassini/Ephemeris</ResourceID>
     <ResourceHeader>
       <ResourceName>Ephemeris: Cassini</ResourceName>
-      <AlternateName></AlternateName>
-      <ReleaseDate>2009-05-20T21:10:13Z</ReleaseDate>
-      <Description>    Cassini Ephemeris are calculated by Joseph Groene of University of Iowa based on CASSINI SPICE kernels. All data are taken from Joseph Groene site
-       Ephemeris are presented in geographic Saturn barycentric coordinates and include
-        Western Longitude_IAU,
-        based on the Voyager determination of the period of Saturn kilometric radiation (SKR).
-        Seidelmann et al.:2002, "Report on the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites: 2000", CELESTIAL MECHANICS AND DYNAMICAL ASTRONOMY 82: 83-110, 2002.
-        Western Longitude_SLS3,
-        based on Cassini SKR measurements.
-        The SLS3 longitude system is only valid for time period: 01.01.2004 - 10.08.2007.
-        Kurth et al. (2008), An update to a Saturnian longitude system based on kilometric radio emissions, Journal of Geophysical Research, Volume 113, Issue A5, CiteID A05222
-        Latitude
-        Local Time
-        L-shell (dipole) value
-        Radius 
- 
+      <AlternateName>Cassini Orbit</AlternateName>
+      <ReleaseDate>2017-05-20T21:10:13Z</ReleaseDate>
+      <Description>   
+        'Regular' Cassini Ephemeris are calculated in IRAP by using Cassini SPICE kernels.
+         Special Cassini Ephemeris are calculated by Joseph Groene of University of Iowa.      
         </Description>
       <Acknowledgement/>
-      <Contact>
-        <PersonID></PersonID>
+      <Contact>       
+        <PersonID>spase://CDPP/Person/NAIF</PersonID> 
+        <Role>PrincipalInvestigator</Role>
+      </Contact>
+      <Contact>       
+        <PersonID>spase://CDPP/Person/Joseph.Groene</PersonID> 
         <Role>PrincipalInvestigator</Role>
       </Contact>
       <InformationURL>
-        <Name></Name>
-        <URL></URL>
+        <Name>Joseph Groene Page</Name>
+        <URL>http://www-pw.physics.uiowa.edu/~jbg/cas.html</URL>
       </InformationURL>
-      <PriorID></PriorID>
+      <PriorID/>
     </ResourceHeader>
     <InstrumentType>Platform</InstrumentType>
-    <InvestigationName></InvestigationName>
+    <InvestigationName/>
     <ObservatoryID>spase://CDPP/Observatory/AMDA/Cassini</ObservatoryID>
     <Caveats/>
   </Instrument>
@@ -6,290 +6,22 @@
     <ResourceHeader>
       <ResourceName>RPWS</ResourceName>    
       <AlternateName>Radio and Plasma Wave Science</AlternateName>
-      <ReleaseDate>2012-11-27T21:10:13Z</ReleaseDate>
+      <ReleaseDate>2017-11-27T21:10:13Z</ReleaseDate>
       <Description>The Cassini Radio and Plasma Wave Science instrument consists of
     three electric field sensors, three search coil magnetometers, and a
     Langmuir probe as well as an array of receivers covering the
     frequency range from 1 Hz to 16 MHz with varying degrees of spectral
     and temporal resolution.
-    
-    
-    The text of this instrument description has been abstracted from the
-    instrument paper:
-    
-     Gurnett, D. A., W. S. Kurth, D. L. Kirchner, G. B. Hospodarsky, T.
-    F. Averkamp, P. Zarka, A. Lecacheux, R. Manning, A. Roux, P. Canu,
-    N. Cornilleau-Wehrlin, P. Galopeau, A. Meyer, R. Bostrom, G.
-    Gustafsson, J.-E. Wahlund, L. Aahlen, H. O. Rucker, H. P. Ladreiter,
-    W. Macher, L. J. C. Woolliscroft, H. Alleyne, M. L. Kaiser, M. D.
-    Desch, W. M.  Farrell, C. C. Harvey, P. Louarn, P. J. Kellogg, K.
-    Goetz, and A.  Pedersen, The Cassini Radio and Plasma Wave Science
-    Investigation, Space Sci. Rev., 114, 395-463, 2004.
-
- Scientific Objectives
-  =====================
-    The primary objectives of the Cassini Radio and Plasma Wave
-    investigation are to study radio emissions, plasma waves, thermal
-    plasma, and dust in the vicinity of Saturn.
-
-    Objectives concerning radio emissions include:
-
-      Improve our knowledge of the rotational modulation of Saturn's
-      radio sources, and hence of Saturn's rotation rate.
-
-      Determine the location of the SKR source as a function of
-      frequency, and investigate the mechanisms involved in generating
-      the radiation.
-
-      Obtain a quantitative evaluation of the anomalies in Saturn's
-      magnetic field by performing direction-finding measurements of the
-      SKR source.
-
-      Establish if gaseous ejections from the moons Rhea, Dione, and
-      Tethys are responsible for the low frequency narrow-band radio
-      emissions.
-
-      Determine if SKR is controlled by Dione's orbital position.
-
-      Establish the nature of the solar wind-magnetosphere interaction
-      by using SKR as a remote indicator of magnetospheric processes.
-
-      Investigate the relationship between SKR and the occurrence of
-      spokes and other time dependent phenomena in the rings.
-
-      Study the fine structure in the SKR spectrum, and compare with the
-      fine structure of terrestrial and Jovian radio emissions in order
-      to understand the origin of this fine structure.
-
-    Objectives concerning plasma waves include:
-
-      Establish the spectrum and types of plasma waves associated with
-      gaseous emissions from Titan, the rings, and the icy satellites.
-
-      Determine the role of plasma waves in the interaction of Saturn's
-      magnetospheric plasma (and the solar wind) with the ionosphere of
-      Titan.
-
-      Establish the spectrum and types of plasma waves that exist in the
-      radiation belt of Saturn.
-
-      Determine the wave-particle interactions responsible for the loss
-      of radiation belt particles.
-
-      Establish the spectrum and types of waves that exist in the
-      magnetotail and polar regions of Saturn's magnetosphere.
-
-      Determine if waves driven by field-aligned currents along the
-      auroral field lines play a significant role in the auroral charged
-      particle acceleration.
-
-      Determine the electron density in the magnetosphere of Saturn,
-      near the icy moons, and in the ionosphere of Titan.
-
-    Objectives concerning lightning include:
-
-      Establish the long-term morphology and temporal variability of
-      lightning in the atmosphere of Saturn.
-
-      Determine the spatial and temporal variation of the electron
-      density in Saturn's ionosphere from the low frequency cutoff and
-      absorption of lightning signals.
-
-      Carry out a definitive search for lightning in Titan's atmosphere
-      during the numerous close flybys of Titan.
-
-      Perform high-resolution studies of the waveform and spectrum of
-      lightning in the atmosphere of Saturn, and compare with
-      terrestrial lightning.
-
-    Objectives concerning thermal plasma include:
-
-      Determine the spatial and temporal distribution of the electron
-      density and temperature in Titan's ionosphere.
-
-      Characterize the escape of thermal plasma from Titan's ionosphere
-      in the downstream wake region.
-
-      Constrain and, when possible, measure the electron density and
-      temperature in other regions of Saturn's magnetosphere.
-
-    Objectives concerning dust include:
-
-      Determine the spatial distribution of micron-sized dust particles
-      through out the Saturnian system.
-
-      Measure the mass distribution of the impacting particles from
-      pulse height analyses of the impact waveforms.
-
-      Determine the possible role of charged dust particles as a source
-      of field-aligned currents.
-
-
-  Calibration
-  ===========
-  
-    An extensive series of amplitude calibrations, frequency responses,
-    phase calibrations, and instrument performance checks were carried
-    out on the RPWS prior to launch, both before and after integration
-    on the spacecraft. These tests and calibrations were performed at
-    room temperature (25 deg C), -20 deg C, and 40 deg C. While there are
-    calibration signals available in the instrument for in-flight
-    calibration purposes, these are mainly used to check for drifts due
-    to aging or radiation exposure. The primary calibration information
-    to derive physical units (spectral density, etc.) is derived from
-    the prelaunch tests.
-
-
-  Operational Considerations
-  ==========================
-  
-    The different types of receivers used to cover the spectral and
-    temporal range covered by the RPWS does not lend itself to a
-    monolithic, synchronous mode of operation. Nevertheless, to reduce
-    the magnitude of the in-flight operations to an acceptable level
-    requires that many of the measurements be scheduled in a systematic
-    way. The approach is to attempt to acquire survey information in the
-    form of uniform spectral and temporal observations at a low enough
-    data rate, ~1 kbps, to ensure that such coverage is available for
-    the entire Saturnian tour and for a large portion of the cruise and
-    approach to Saturn. The survey data set will support spatial
-    mapping, statistical studies, and studies of dynamical effects in
-    the magnetosphere and their possible correlation with solar wind
-    variations. In addition to the survey information, special
-    observations will be added (sometimes at greatly increased data
-    rates) at specific locations or times to provide enhanced
-    information required by several of the science objectives. The
-    special observations may include full polarization and
-    direction-finding capability or high spectral or temporal resolution
-    observations by the high frequency receiver, wideband measurements
-    at one of the possible bandwidths, acquisition of delta-ne/ne
-    measurements, or intensive wave-normal analysis afforded by
-    acquiring five-channel waveforms on an accelerated schedule. While
-    minimizing the number of different modes in which the instrument is
-    operated both simplifies operations and yields a more manageable
-    data set, flexibility (for example in the duty cycle of wideband
-    measurements) increases the likelihood that enhanced measurements
-    can be integrated successfully with the resource requirements of the
-    other instruments. One of the resources which will be most limited
-    on Cassini is the overall data volume; RPWS requires large data
-    volumes for some of its measurements.
-
-
-  Detectors
-  =========
-  
-    The RPWS utilizes three 10-m electric antennas, three magnetic
-    antennas, and a Langmuir probe for detectors.  Three monopole
-    electric field antennas, labeled Eu, Ev, and Ew, are used to provide
-    electric field signals to the various receivers. The physical
-    orientations of these three antennas relative to the x, y, and z
-    axes of the spacecraft are given below. However, the electrical
-    orientations of these are strongly affected by the asymmetric nature
-    of the ground plane of the spacecraft chassis.  These electrical
-    orientations are incorporated into the calibrations, primarily of
-    the High Frequency Receiver.  By electronically taking the
-    difference between the voltages on the Eu and Ev monopoles, these
-    two antennas can be used as a dipole, Ex, aligned along the x axis
-    of the spacecraft.
-
-+-------------------------------------------------------------+
-|    Physical orientations of the electric monopole antennas: |
-|-------------------------------------------------------------|
-|    Antenna  |  theta (degrees) | phi (degrees)              |
-|        Eu   |     107.5        |   24.8                     |
-|        Ev   |     107.5        |  155.2                     |
-|        Ew   |      37.0        |   90.0                     |
-+-------------------------------------------------------------+
-
-    The angle theta is the polar angle measured from the spacecraft +z
-    axis.  The angle phi is the azimuthal angle, measured from the
-    spacecraft +x axis.
-
-    The tri-axial search coil magnetic antennas, labeled Bx, By, and Bz,
-    are used to detect three orthogonal magnetic components of
-    electromagnetic waves. The search coil axes are aligned along the x,
-    y, and z axes of the spacecraft.
-
-    The spherical Langmuir probe is used for electron density and
-    temperature measurements.  This is extended from the spacecraft in
-    approximately the -x direction, in spacecraft coordinates.
-
-
-  Electronics
-  ===========
-  
-    The electronics consists of five receivers. These receivers are
-    connected to the antennas described above by a network of switches.
-    The high frequency receiver (HFR) provides simultaneous auto- and
-    cross-correlation measurements from two selected antennas over a
-    frequency range from 3.5 kHz and 16 MHz. By switching the two inputs
-    of this receiver between the three monopole electric antennas, this
-    receiver can provide direction-of-arrival measurements, plus a full
-    determination of the four Stokes parameters. The high frequency
-    receiver includes a processor that performs all of its digital
-    signal processing, including data compression. The high frequency
-    receiver also includes a sounder transmitter that can be used to
-    transmit short square wave pulses from 3.6 to 115.2 kHz. When used
-    in conjunction with the high frequency receiver, the sounder can
-    stimulate resonances in the plasma, most notably at the electron
-    plasma frequency, thereby providing a direct measurement of the
-    electron number density.  The medium frequency receiver (MFR)
-    provides intensity measurements from a single selected antenna over
-    a frequency range from 24 Hz to 12 kHz. This receiver is usually
-    operated in a mode that toggles every 32 seconds between the Ex
-    electric dipole antenna and the Bx magnetic search coil, thereby
-    providing spectral information for both the electric and magnetic
-    components of plasma waves. The low frequency receiver (LFR)
-    provides intensity measurements from 1 Hz to 26 Hz, typically from
-    the Ex electric dipole antenna and the Bx magnetic antenna. The
-    five-channel waveform receiver (WFR) collects simultaneous waveforms
-    from up to five sensors for short intervals in one of two frequency
-    bands, either 1 to 26 Hz, or 3 Hz to 2.5 kHz. When connected to two
-    electric and three magnetic antennas, this receiver provides wave
-    normal measurements of electromagnetic plasma waves. The wideband
-    receiver is designed to provide nearly continuous wideband waveform
-    measurements over a bandwidth of either 60 Hz to 10.5 kHz, or 800 Hz
-    to 75 kHz. These waveforms can be analyzed on the ground in either
-    the temporal domain, or in the frequency domain (Fourier
-    transformed) to provide high-resolution frequency-time spectrograms.
-    In a special frequency-conversion mode of operation, the high
-    frequency receiver can provide waveforms to the wideband receiver in
-    a 25-kHz bandwidth that is tunable to any frequency between 125 kHz
-    and 16 MHz.
-
-    The Langmuir probe controller is used to sweep the bias voltage of
-    the probe over a range from -32 to +32 V in order to obtain the
-    current-voltage characteristics of the probe, and thereby the
-    electron density and temperature. The controller can also set the
-    bias voltage on the Eu and Ev monopoles over a range from -10 to +10
-    V in order to operate them in a current collection mode for
-    delta-ne/ne measurements.
-
-    The RPWS data processing unit consists of three processors. The
-    first processor, called the low-rate processor, controls all
-    instrument functions, collects data from the high frequency
-    receiver, the medium frequency receiver, the low frequency receiver,
-    and the Langmuir probe, and carries out all communications with the
-    spacecraft Command and Data System (CDS). The second processor,
-    called the highrate processor, handles data from the wideband and
-    five-channel waveform receivers and passes the data along to the
-    low-rate processor for transmission to the CDS. The third processor,
-    called the data compression processor, is primarily used for data
-    compression, but can also perform specialized operations such as
-    on-board dust detection by using waveforms from the wideband
-    receiver."
-
-
     </Description>
       <Acknowledgement/>
-            <Contact>
-                <PersonID>spase://SMWG/Person/Donald.A.Gurnett</PersonID>
-                <Role>PrincipalInvestigator</Role>
-            </Contact>
-            <Contact>
-                <PersonID>spase://SMWG/Person/William.S.Kurth</PersonID>
-                <Role>CoInvestigator</Role>
-            </Contact>
+      <Contact>
+        <PersonID>spase://SMWG/Person/William.S.Kurth</PersonID>
+        <Role>PrincipalInvestigator</Role>
+      </Contact>
+      <Contact>
+        <PersonID>spase://SMWG/Person/Donald.A.Gurnett</PersonID>
+        <Role>CoInvestigator</Role>
+      </Contact>
       <InformationURL>
         <Name>Instrument home page at The University of Iowa</Name>
         <URL>http://www-pw.physics.uiowa.edu/cassini/</URL>
@@ -5,7 +5,8 @@
         <ResourceID>spase://CDPP/NumericalData/AMDA/Cassini/Ephemeris/cass-ephem-eqt</ResourceID>
         <ResourceHeader>
             <ResourceName>flyby jupiter</ResourceName>
-            <ReleaseDate>2015-10-06T10:30:00</ReleaseDate>
+            <AlternateName>Cassini : Jupiter Flyby</AlternateName>
+            <ReleaseDate>2017-10-06T10:30:00</ReleaseDate>
             <Description>Ephemeris of the Cassini spacecraft around Jupiter (during the Jupiter flyby in 2000-2001). Obtained from University of Iowa server.
                 http://www-pw.physics.uiowa.edu/~jbg/cas.html</Description>
             <Contact>
@@ -7,7 +7,21 @@
             <ResourceName>orbit saturn : SLS3 longitude</ResourceName>
             <ReleaseDate>2015-10-12T11:24:00</ReleaseDate>
             <Description>Ephemeris of the Cassini spacecraft around Saturn. Obtained from University of Iowa server.
-                http://www-pw.physics.uiowa.edu/~jbg/cas.html</Description>
+                http://www-pw.physics.uiowa.edu/~jbg/cas.html
+                 Cassini Ephemeris (special) are calculated  by Joseph Groene of University of Iowa based on CASSINI SPICE kernels. All data are taken from Joseph Groene site
+       Ephemeris are presented in geographic Saturn barycentric coordinates and include
+        Western Longitude_IAU,
+        based on the Voyager determination of the period of Saturn kilometric radiation (SKR).
+        Seidelmann et al.:2002, "Report on the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites: 2000", CELESTIAL MECHANICS AND DYNAMICAL ASTRONOMY 82: 83-110, 2002.
+        Western Longitude_SLS3,
+        based on Cassini SKR measurements.
+        The SLS3 longitude system is only valid for time period: 01.01.2004 - 10.08.2007.
+        Kurth et al. (2008), An update to a Saturnian longitude system based on kilometric radio emissions, Journal of Geophysical Research, Volume 113, Issue A5, CiteID A05222
+        Latitude
+        Local Time
+        L-shell (dipole) value
+        Radius 
+            </Description>
             <Contact>
                 <PersonID>spase://SMWG/Person/Elena.budnik</PersonID>
                 <Role>TechnicalContact</Role>
@@ -7,36 +7,30 @@
       <ResourceName>Cassini</ResourceName>
       <AlternateName>Cassini-Huygens, NASA/ESA mission to Saturn</AlternateName>
       <ReleaseDate>2017-08-05T18:19:17Z</ReleaseDate>
-      <Description>
-        The Cassini spacecraft, launched in October 1997, entered 
-        a Saturn-centered orbit in July 2004.  It is instrumented for a wide range of 
-        remote sensing and in situ observations. It delivered the ESA-built Huygens Probe
-        to investigate Titan.
-        
-        The Cassini mission to Saturn is one of the most ambitious efforts in planetary 
-        space exploration ever mounted. A joint endeavor of NASA, the European Space Agency (ESA) 
-        and the Italian space agency, Agenzia Spaziale Italiana (ASI), Cassini is a 
-        sophisticated robotic spacecraft orbiting the ringed planet and studying the 
-        Saturnian system in detail. Cassini also carried a probe called Huygens, which 
-        parachuted to the surface of Saturn’s largest moon, Titan, in January 2005 and 
-        returned spectacular results.
+      <Description>The Cassini spacecraft, launched in October 1997, entered a Saturn-centered orbit in July 2004. It is instrumented for a wide range of remote sensing and in situ observations. It delivered the ESA-built Huygens Probe to investigate Titan. 
+      
  
-Cassini completed its initial four-year mission to explore the Saturn System in June 2008, 
-and the first extension, called the Cassini Equinox Mission, in September 2010. Now, the healthy 
-spacecraft is making exciting new discoveries in a second extension called the Cassini Solstice 
-Mission.
+The Cassini mission to Saturn is one of the most ambitious efforts in planetary space exploration ever mounted.
+A joint endeavor of NASA, the European Space Agency (ESA) and the Italian space agency, Agenzia Spaziale Italiana (ASI), 
+Cassini is a sophisticated robotic spacecraft orbiting the ringed planet and studying the Saturnian system in detail. 
+Cassini also carried a probe called Huygens, which parachuted to the surface of Saturn’s largest moon, Titan, in January 2005 and 
+returned spectacular results.
  
-In late 2016, the Cassini spacecraft will begin a daring set of orbits called the Grand Finale, 
-which will be in some ways like a whole new mission. The spacecraft will repeatedly climb high 
-above Saturn’s poles, flying just outside its narrow F ring 20 times. After a 
-last targeted Titan flyby, the spacecraft will then dive between Saturn’s 
-uppermost atmosphere and its innermost ring 22 times. As Cassini plunges past Saturn, 
-the spacecraft will collect rich and valuable information far beyond the mission’s original plan,
-including measuring Saturn’s gravitational and magnetic fields, determining ring mass, 
-sampling the atmosphere and ionosphere, and making the last views of Enceladus.
+        
+Cassini completed its initial four-year mission to explore the Saturn System in June 2008, 
+a first extension (the Cassini Equinox Mission) in September 2010, and a second extension 
+(the Cassini Solstice Mission) in late 2016. 
+          
+          
+From that date until September 2017, the Cassini spacecraft has begun a daring set of orbits (the Cassini Grand Finale) where the spacecraft 
+repeatedly has climbed high above Saturn’s poles, flying just outside its narrow F ring 20 times. 
+After a last targeted Titan flyby, the spacecraft has then dived between Saturn’s uppermost atmosphere and its innermost ring 22 times. 
+As Cassini has plunged past Saturn, the spacecraft has collected rich and valuable information far beyond the mission’s original plan, 
+including measuring Saturn’s gravitational and magnetic fields, determining ring mass, sampling the atmosphere and ionosphere, 
+and making the last views of Enceladus.        
 </Description>
       <Contact>
-        <PersonID>spase://SMWG/Person/Dennis.L.Matson</PersonID>
+        <PersonID>spase://CDPP/Person/Linda.Spilker</PersonID>
         <Role>ProjectScientist</Role>
       </Contact>
       <InformationURL>
@@ -51,7 +45,8 @@ sampling the atmosphere and ionosphere, and making the last views of Enceladus.
     </Location>
     <OperatingSpan>
       <StartDate>1997-10-15T00:00:00</StartDate>
-      <Note>Saturn arrival : 2004-07</Note>
+      <StopDate>2017-09-15T00:00:00</StopDate>
+      <Note>Saturn arrival : 2004-07-01</Note>
     </OperatingSpan>    
   </Observatory>
 </Spase>
@@ -0,0 +1,11 @@
+<?xml version="1.0" encoding="UTF-8"?>
+<Spase xmlns="http://www.spase-group.org/data/schema" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.spase-group.org/data/schema http://www.spase-group.org/data/schema/spase-2_2_3.xsd">
+<Version>2.2.3</Version>
+<Person>
+        <ResourceID>spase://CDPP/Person/Joseph.Groene</ResourceID>
+        <ReleaseDate>2017-07-11T00:00:00Z</ReleaseDate>
+        <PersonName>Dr. Joseph Groene</PersonName>
+        <OrganizationName>University of Iowa</OrganizationName>
+        <Email>joseph-groene@uiowa.edu</Email>
+    </Person>
+</Spase>
@@ -0,0 +1,11 @@
+<?xml version="1.0" encoding="UTF-8"?>
+<Spase xmlns="http://www.spase-group.org/data/schema" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.spase-group.org/data/schema http://www.spase-group.org/data/schema/spase-2_2_3.xsd">
+<Version>2.2.3</Version>
+<Person>
+        <ResourceID>spase://CDPP/Person/Linda.Spilker</ResourceID>
+        <ReleaseDate>2017-07-11T00:00:00Z</ReleaseDate>
+        <PersonName>Dr. Linda J. Spilker</PersonName>
+        <OrganizationName>Jet Propulsion Laboratory, CA</OrganizationName>
+         <Email>Linda.J.Spilker@jpl.nasa.gov</Email>
+    </Person>
+</Spase>