/* file: /ansa4/gll_archive/gen_templates/goeuvedr.ds */ /* file: GLLUVS1:[GLL_RAW.PDS_ARCHIVE.GEN_TEMPLATES]GOeuvEDR.DS */ /* The Galileo Orbiter (GO) UVS/EUV EDR (EDR) DataSet.cat (DS) */ /* Nov 18, 1998 - kes */ /* Updated for GEM and GMM, Jan 24, 2001 - kes */ /* small changes by Huber, Feb 9,2001 */ /* corrected the GEM vs GMM objectives Feb 19,01 */ /* GMM data sets added Jan 31,06 - kes */ PDS_VERSION_ID = PDS3 LABEL_REVISION_NOTE = "KAREN SIMMONS, 1998-11-18, 2001-01-24, 2006-02-01" OBJECT = DATA_SET DATA_SET_ID = "GO-J-EUV-2-EDR-V1.0" OBJECT = DATA_SET_INFORMATION DATA_SET_NAME = "Galileo Orbiter UVS/EUV Jupiter operations EDR data" DATA_SET_COLLECTION_MEMBER_FLG = "N" DATA_OBJECT_TYPE = SPECTRUM START_TIME = 1995-342T00:00:00 STOP_TIME = 2002-252T23:35:33 DATA_SET_RELEASE_DATE = 1999-01-15 PRODUCER_FULL_NAME = "Karen E. Simmons" DETAILED_CATALOG_FLAG = "N" DATA_SET_DESC = " Data Set Overview ================= Observations by the group of Galileo science instruments are coordinated by the Project Science Group (PSG). Spacecraft resources are divided between the needs of the three main disciplines: Atmospheres, Satellites and Magnetospheres. These disciplines coordinate science operations with their three Galileo Science Working Groups (WGs). These are the Satellite Working Group (SWG), the Magnetospheres WG (MWG) and the Atmospheres WG (AWG). The UVS team constitutes the science group from the University of Colorado. The PI is Dr. Charles W. Hord. The instrument consists of two pieces of hardware, the UltraViolet Spectrometer (UVS) and the Extreme UltraViolet (EUV) Spectrometer. The data resource negotiations with the WGs were considered as one team within the WGs. Data for the separate hardware are kept in separate data files. In the descriptions below, UVS may indicate the team, and thus both instruments, or may refer to only the UVS hardware. Separate EUV observation classes do exist and they are described below. Other data, like calibrations, are included where appropriate. Each Science WG has its own set of observations. The observations described in this EDR data set label include all observations from the Nominal Mission period, from Jupiter-Orbit-Insertion until End-Of-Millennium Mission, I33. All Jupiter, Torus, satellite, etc target objects are described. Data from different orbits may contain observations from all or none of the described WG Observation classes. EUV data from just before Jupiter-Orbit-Insertion (J0CD) are included in this set. Pre-orbital data are a separate data set. Experiment Data Record (EDR) data for EUV may be in either of two file formats: one for Playback (PB) data and one for the Phase 2 Real-Time-Science (RTS) data. Some of the observations are done only with the on-board summing RTS mode. Playback (PB) observations are recorded on the tape and played back at full, 1000 bps data rate. EUV obtained only RTS data during the nominal mission. EUV playback was used only in the pre-Jupiter planet encounters. During the Nominal mission five EUV/UVS cross-calibration observations were made (in G02C, E06A, G08A, C10B and E19.) These were periods when both instruments observed the Hydrogen Lyman-alpha 'sky-background' simultaneously over the same piece of sky. A cross-calibration in C03C observed Spica with the EUV and UVS simultaneously. An observation of the same Earth 1 and Earth 2 EUV star (Sirius) was made during Galileo Europa Mission (GEM) orbit E19C, when the z-axis pointed to the earth in RA and Dec 180 degrees from where it was pre-Jupiter. Besides these two 'absolute stellar cross-calibrations' the EUV occasionally observes an EUV bright star within its field while making torus measurements. These data sets are also archived in the PDS. These EUV stallar observations allowed the team to verify EUV instrument detector stability. All EUV EDRs are raw, uncalibrated spectra. EDRs have been re-formatted by the team from spacecraft packets. The data set includes all EDR data from orbital operations for the Nominal/Prime Mission. File labels describe the file format of each data file. Each data file record has header information containing time tags, followed by the spectral/sector data (see description below, in MWG observations discussion section). There may be more than one record per file. Generally, each file contains all the data for that individual science Observation_ID, as classed below. EUV RDRs are generally heavily processed data sets and do not normally contain full spectra. EDR calibration is described in the calibration documents and files archived with PDS and discussed in the published papers. A list of recent publications appears at the end of this Description; a long publication list is available on the PDS archive CD. The PDS label file, for each data file, contains a PRODUCT_NAME which contains the Galileo Observation ID. These 12-character Observation IDs actually appear in the sequence (SEF) file. These are related to the WG Observation classes described below. An example of a PRODUCT_NAME is G07A_UPB_G7MANS01 ____ is the 4-character Orbit load number _EUV_ is EUV for EUV RTS data format __ is the Orbit number OR ------ is the observation name __ is the observation series number. As with all well made plans, these Observation_ID rules were not always followed. The observation names might also be proper names of features or other new names. The data files are named by the observation name given in the SEF. The .DAT file extension indicates the file is a binary Vax formatted data file; an .XDR file extension indicates the file is an IEEE standard (transfer format) file. UVS and EUV data files are distinguished by their file names. Real-time commands to both instruments, especially after spacecraft safing, can generate non-sequenced data files; generally these are POWER files where the configuration returned in the engineering verifies the correct power-on state. The file extensions .LBL and .XLBL are used for the EDR labels. A list of all commands (file: CMD_ARCHIVE.LIS) is in the CD's Document directory. The UVS Mission science objectives are given, in great detail, in several Galileo JPL mission documents. The Science Requirements Document (625-50) and the Orbit Planning Guides, OPG, (JPL 625-100, Vol. 2) are two. There is an OPG for the Nominal Mission and one for the Galileo Europa Mission. The OPG describes both the instrument objectives and the observation classes as well as specific observation ID names. On-line (web access) copies of the OAPEL (Orbit Activity Planning ELement) planning sheets and graphic designs provide additional information. JPL may have this information available in the public archive. They may also still be online at http://lasp.colorado.edu/galileo/ . The UVS Prime (Nominal) Mission Observation classes are discussed below. These descriptions come from the planning documents. They are grouped by Working Group (WG). The Galileo Europa Mission (GEM, orbits E12 to I25) and the Galileo Millenium Mission (GMM, orbits E26 to End-of-Mission, I33) continued this same observation planning and ID nomenclature although written documents became more scarce. The observation planning for GEM and GMM are listed beyond the AWG/MWG/SWG discussion sections. ++++++++++++++++++++++++++++++++++++++ AWG SCIENCE AND OBSERVATION OBJECTIVES ++++++++++++++++++++++++++++++++++++++ The EUV instrument does not make observations within the AWG class of science. Jupiter EUV Aurora observations are done from the MWG but in some cases these are in conjunction with UVS AWG aurora observations so the UVS aurora descriptions are listed, for collaborative completeness, where appropriate. An EUV whole-body spin-scan image of Callisto was done from the SWG. ++++++++++++++++++++++++++++++++++++++ MWG SCIENCE AND OBSERVATION OBJECTIVES ++++++++++++++++++++++++++++++++++++++ GLL EUV/UVS OBSERVATIONS OF THE IO TORUS INTRODUCTION The Voyager UVS investigation discovered bright EUV emissions from what was soon identified as a plasma torus in Io's orbit, and the almost simultaneous prediction and discovery of active volcanism on Io answered the immediate question of where the material and energy of the torus came from. Since then, Io's torus has been the focus of intense interest and of considerable observational and theoretical efforts. The ions S II, S III, S IV, O II, and O III have been observed; neutral Na was known to be present for some time before Voyager; and a vast nebula of Na I surrounding Jupiter has been discovered since. Similar distributions of S I and O I are expected at greater densities than Na I, but have never been detected. The EUV channel was added to the GLL UVS investigation specifically to add to our understanding of the torus. Because of great observational difficulties, little work has been done in the EUV since Voyager. This wavelength region includes most of the energy emitted by the torus, and EUV radiation is the major cooling process for its ions and electrons. We can therefore expect that the EUV offers great diagnostic capabilities, particularly of the secular and periodic behavior of the processes that produce, control, and dissipate the torus. SCIENTIFIC RATIONALE The Jovian magnetosphere rotates past Io at about 55 km/sec. Material sputtered off Io or its atmosphere, or thrown off directly by volcanic activity, is accelerated after ionization to near co-rotation speed as it is picked up by the magnetic field. Radiative energy loss from the torus is severe and without sustained injection of energy, the torus would lose most of its energy content in less than two rotations. Part of the energy supply is provided by ion pickup with subsequent transfer to the electrons. However, a heterogeneous energy source is needed to explain the relatively high temperature of the main part of the torus. There is currently no satisfactory explanation for the additional energy source, and the torus energy budget remains one of the major issues to be resolved. The energy budget can be directly addressed with judicious observations by the Galileo UVS. The torus is trifurcated, with a cold inner region, a very narrow ribbon region near 5.7 Rj, connected to a warm outer plasma region. The inner region has no measurable EUV emission. The ribbon is assumed to be at a temperature high enough to produce EUV emission, but currently is observed only in infrared lines of S II and S III. The outer region presumably in combination with the ribbon region is responsible for the observed EUV emission spectrum obtained by the Voyager UVS. There is a general agreement that the ribbon region may be an important and possibly a key factor in the dynamics of the system, but current information on the energetics and temporal and spatial morphology is limited to the ground based observations. The Galileo UVS can directly address the partitioning, plasma temperature, and energy budget questions. There is a dependence of ion partitioning on electron kinetic distribution. The more highly stripped ions, S IV and O III, are sensitive to the high energy component of the electron population and their mixing ratios can be utilized as measures of how energy is inserted, and limits to the mean input rate can be calculated from limits on the emission lines of these species. The torus is strongly affected by the rotation of Jupiter. Ions are trapped in a potential well formed by the rotation of the magnetic field and the curvature of the field lines; they spread in this potential well to about 1 Rj from the centrifugal equator. The torus wobbles in Jupiter's rotational frame because of the tilt and offset of the magnetic field. It is brighter in the local evening sector than in the morning, implying that the electrons are heated periodically in a region fixed in local time. All these effects require observations that have time resolution substantially greater than Jupiter's rotation period of 10 hrs. The source of material for the torus - Io - rotates around Jupiter with a period of 43 hrs, and the response of the torus to episodic events on Io, such as large volcanic eruptions, may be expected to exhibit this periodicity. Ions are lost from the torus by diffusion, whose timescale is thought to be 60-100 days. Secular changes in torus density and/or temperature were observed between the Voyager 1 and Voyager 2 flybys, and major changes also occurred between the Pioneer and Voyager missions, five years apart. The chief thrust of the GLL EUV/UVS torus observations is to measure and characterize the hot and cold torus densities, composition, and temperatures on time scales varying from the shortest achievable in the light of signal-to- noise considerations (nominally 30 mins) to the length of the orbital mission (about 2 years). EUV/UVS MEASUREMENTS Emission lines suitable for observations are those that are diagnostic of composition and/or temperature and that produce adequately strong signals. Table 1 shows, for selected lines, the expected brightness and signal-to- noise for 1-hour observations. The EUV S/N values take account of the spin-scan nature of these observations, and the UVS values assume a fixed inertial 'stare' at an ansa. The noise levels are estimated from Voyager UVS data. See the OPG document for additional figures and tables. TABLE 1 - TORUS EMISSION LINES AND S/N VALUES Line Wavelength Brightness Signal S/N for 60 min. obs (A) (Rayleigh) cts/s @ 65 Rj @ 40 Rj S III 685 360 13.6 8.7 5.7 O II 834 250 7.8 5.6 3.4 S III 1194 53 7.1 20. 11. S II 1259 34 7.0 20. 11. S IV 1406 8 1.2 3.6 1.9 O III 1666 6* O II 2471 48 2.0 5.9 3.1 O II 3728 270 189 310 230 S II 4070 76 46 110 67 * No confirmed detection; estimated intensity at Voyager 1 encounter according to model partitioning calculations. Estimated intensity at Voyager 2 encounter is ~1 R. The relevance of the above emissions to the scientific goals can be summarized as follows: a) To monitor the energy radiated by the torus, the EUV spectrum, which carries about 80% of the total, must be measured. b) The most abundant ion in the torus is O II, followed by S III and S II. Measurements of the 3728A and 4070A emissions will establish the S II/O II ratio. Measurements of the 1259A and 1194A emissions will establish the S III/S II ratio. c) Measurements of the ratio of the S II features at 4070A and 1259A will establish the effective electron temperature. d) The densities of the minor ions S IV and O III are diagnostic of the presence of hot electrons. Its emission at 1406A will be monitored to establish S IV population. The species most sensitive to the hot component of the electron population is O III. It is therefore expected to be the most unstable component, and a very sensitive measure of energy input by the hot electron population. Measurements of the upper limit to the 1666A line therefore constitute an important limitation on energy source mechanisms. e) In addition to the above, the excellent S/N in the O II emission at 3728A makes it possible to 'map' the extent of the torus beyond 7 Rj in Io's orbital plane and beyond 1 Rj above and below it. A typical estimate of the ion composition has O II, O III, S II, S III, and S IV present with partition fractions .62, .01, .175, .180, and .02 respectively. The S/N values at 65 Rj allow variations in these partition fractions, and therefore in the total ion density also, to be detected at or below the 1% level. The ratio of the S II line at 1259A to that at 4070A varies almost linearly with electron temperature, and at 65 Rj the S/N in the two lines allows the temperature to be measured to +- 5%, or +- 3000 deg. OBSERVING PLAN Opportunities to make the above measurements are subject to several constraints. The EUV instrument looks at a S/C cone angle of 90 deg; its observing times are determined by orbital parameters and by the pointing of the S/C spin axis. The UVS is on the scan platform, so the above measurements require the dual-spin S/C mode. UVS measurements must be made at S/C cone angles not less than 90 deg, and for the N channel the 'sun cone' angle must also be not less than 90 deg. In addition, both instruments are subject to radiation noise, and measurements will not be made within specific distances from Jupiter, currently set at 25 Rj for the EUV and 15 Rj for the UVS. Five 'events' on each orbit are defined for each cone constraint, to wit: the midnight and noon ansae of Io's orbit, Jupiter itself, and the midnight and noon 'ansae' of Europa's orbit at which the EUV measurements are begun and ended. The noise constraints are also shown; these override any other constraint. The PROFILE measurements will characterize the torus ansae as a function of longitude, time and radius. The observing strategy is as follows: During the EUV observing window, the UVS will observe at a S/C cone of 90 deg to provide simultaneous coverage with the EUV. UVS measurements will be of O II at 3728A, S II at 4070A and 1259A, and S III at 1194A, to satisfy the scientific goals (a), (b), and (c) above. After the end of the EUV measurements, and before the UVS reaches its noise limit, the UVS can observe the dawn-side ansa of the torus. On some orbits, the dusk-side ansa can also be observed after Jupiter closest approach (C/A). During these opportunities, the UVS will measure O II at 3728A, S II at 4070A and at 1259A, and S III at 1194A, to further goals (a), (b), and (c). It will also look for S IV at 1406A, to fulfill goal (d). Finally, it will look for O II at 3728A and S II at 4070A above and below Io's orbit plane to satisfy goal (e). The EUV utilizes an instrument memory buffer configured in a wavelength by sky-sector matrix to accumulate Phase 2 RTS data. This buffer configuration is controlled by the Fixed Pattern Noise Table (FPNT); the FPNT is uplinked via the sequence whenever the instrument is powered on. There are three standard FPNTs: the Torus table, the Aurora table, and a General table. If EUV is to make Aurora observations, for example as the spacecraft causes the EUV FOV to pass over Jupiter, then the Torus table is replaced by the Aurora table for the duration of that observation. The Torus table would then reconfigure the buffer matrix for the remaining Torus observations. Generally, these tables determine the wavelength resolution by summing over the specified detector pixels; line features and background criteria determine the construction of these tables so that the optimum resolution may be obtained for the science in consideration. Which table is in effect is given in the data file label. The three FPNT tables are described in the EUV instrument label file. Table 2 gives a skeleton timeline for EUV/UVS torus measurements. A full list of the commanded Torus, Auroral and Sky-background observations, through the GMM period, is in the file EUV_CMD_ARCHIVE in the CD's Documents folder #### TABLE 2 - INSTRUMENT ON/OFF AND TARGET TIMELINE orb inst begin end pointing G1 EUV 176/21:40-182/11:47 @ 90 deg S/C cone UVS 176/21:20-182/11:47 @ 90 deg S/C cone UVS 182/11:47-186/10:04 torus a.m. ansa G2 EUV 238/15:19-244/23:22 @ 90 deg S/C cone UVS 238/15:19-244/23:22 @ 90 deg S/C cone UVS 244/23:22-250/19:00 torus a.m. ansa C3 EUV 301/22:37-307/04:15 @ 90 deg S/C cone UVS 301/22:37-307/04:15 @ 90 deg S/C cone UVS 307/04:15-310/17:17 torus a.m. ansa E4 EUV 346/20:07-351/08:40 @ 90 deg S/C cone UVS 346/20:07-351/08:40 @ 90 deg S/C cone UVS 351/08:40-353/07:17 torus a.m. ansa E6 EUV 048/04:07-049/23:29 @ 90 deg S/C cone UVS 048/04:07-050/23:28 @ 90 deg S/C cone UVS 050/23:28-051/00:49 torus a.m. ansa G7 EUV 091/12:30-092/14:30 @ 90 deg S/C cone UVS 091/12:30-093/14:52 @ 90 deg S/C cone (post-perijove) UVS 095/04:50-096/16:00 torus p.m. ansa G8 EUV 125/05:23-126/15:11 @ 90 deg S/C cone UVS 125/05:23-127/15:56 @ 90 deg S/C cone (post-perijove) UVS 129/05:10-129/16:00 torus p.m. ansa C9 EUV 176/11:38-176/16:51 @ 90 deg S/C cone UVS 176/11:38-177/17:46 @ 90 deg S/C cone (post-perijove) UVS 179/03:20-180/16:00 torus p.m. ansa C10 EUV 259/11:17-260/03:23 @ 90 deg S/C cone UVS 259/11:17-261/03:20 @ 90 deg S/C cone (post-perijove) UVS 262/16:50-263/16:00 torus p.m. ansa E11 EUV 308/11:42-309/04:57 @ 90 deg S/C cone UVS 308/11:42-310/04:52 @ 90 deg S/C cone (post-perijove) UVS 311/18:43-313/16:00 torus p.m. ansa MWG MEASUREMENT SETS The UVS and EUV measurement sets are listed by acronym and fully described above. There are no recorded observations. The realtime observations include high priority EUV and UVS activities and will use realtime bits-to-ground (BTG). EUV file names are coordinated with UVS OAPEL observation names so that time periods of simultaneous observations have like file names. Orbits JA/J0-E11: UVS observation names MANSxx - Midnight Ansa, cone = 90 deg NANSxx - Noon Ansa, cone = 90 deg MPROxx - Midnight Profile, cone > 90 deg NPROxx - Noon Profile, cone > 90 deg CROSSCAL, XCALxx - UVS/EUV cross-calibration EUV observation names MANSxx - Midnight Ansa NANSxx - Noon Ansa MPROxx - Midnight Profile NPROxx - Noon Profile AURAxx - Jupiter Aurora (UVS aurora observations are listed under AWG) CROSSCAL, XCALxx - UVS/EUV cross-calibration ++++++++++++++++++++++++++++++++++++++ SWG SCIENCE AND OBSERVATION OBJECTIVES ++++++++++++++++++++++++++++++++++++++ KEY QUESTIONS The UVS and EUV satellite observations during the Jupiter tour will answer several key questions related to the state of evolution and the surface composition of the Jovian satellites. The observational goals and strategies detailed below, combined with the Galileo's capabilities based upon the Phase II flight software, will permit observations which can answer these questions. The UVS and EUV satellite observations will determine the composition, or upper limits to the number density, of the neutral atmosphere of the Galilean satellites and the Io neutral cloud. The UVS observations will also determine the excitation mechanisms and escape rates of the satellite atmospheres. In addition, the UV albedo, when combined with the visible and infrared spectra, will determine surface composition and particle size. A unique EUV satellite observation (CVSPNSCN) before Callisto closest approach, in orbit C10, will search for extreme UV (60-130 nm) absorptions and emissions. OBSERVATION GOALS The UVS and EUV satellite observations will be conducted during each Jovian orbit with the exception of the non-targeted fifth orbit (J5). The principal goal of these observations will be to answer these key scientific questions as well as to support the Satellite Working Group observations where possible. OBSERVATION STRATEGY Observations which will address the science questions are based upon the detailed observation descriptions below. UVS and EUV observations can be grouped into two general science area categories. These are 1) Volatile Escape; and 2) Surface Albedo and Composition observations. The categories are described below where the capitalized acronyms are the six-character observation names. 1) Volatile Escape observations will search for atomic spectral lines (H,O,C,N), molecular bands (OH,CO,CO2+), and neutral clouds (SO2,SO,O,S,K,Na) to determine the altitude near the Jovian satellites. These measurements will enable an understanding of the excitation mechanisms and the escape rates to determine the state of evolution of the Jovian satellites. The measurement set used to obtain this information consists of the BRTLMB, DRKLMB, ECLIPS, NRLCLD and SPNSCN observations. 2) Surface Albedo and composition observations will extend the surface scattering property measurements into the ultraviolet (1600A-3200A) and extreme ultraviolet (500A-1300A) wavelengths. The data retrieved will provide information about particle size and absorption properties of the surface materials at resolutions and phase angles which cannot be obtained from Earth. The data will also be used to supplement and complement the NIMS surface property measurements. The measurement set used to obtain this information consists of the GLOBAL, MAPPNG, PHASE and SPNSCN observations. 3) Additional data are required through AACS-provided pointing information for all realtime and recorded observations. These data are provided through the realtime science formats and the recorded low-rate science ancillary data packets. SWG MEASUREMENT SET PRIORITIES The EUV measurement sets are listed by acronym and described below. The only EUV observations are realtime observations. Orbit JA/J0: No EUV satellite observations. Orbits G1-E11: SPNSCN - EUV Callisto Spin Scan Image Observations Realtime SPNSCN Objective: Map Callisto in the 600A to 1300A wavelength regions. Strategy: Using the All Purpose EUV FPNT, build up a spin-scan map of Callisto in wavelength versus longitude-latitude bins. The sky-sector bins will be selected to optimize the latitudinal resolution and the wavelength bins will optimize key wavelengths. The map will be downloaded using the EUV 10 bps realtime capability. Orbits: C10 only. +++++++++++++++++++++++++++++++++++++ GEM SCIENCE OBJECTIVES +++++++++++++++++++++++++++++++++++++ EUV GEM science objectives continued to be identical to those in the Primary Mission. These GEM observations will complete the correlated set of observa- tions needed to answer the science questions given above. Also see the GEM and GMM discussions in the AWG OBJECTIVES section. See the discussion in the UVS hardware data set catalog file GOUVSEDR.DS regarding the failure of the UVS grating drive optics in orbit C20. Orbit E12: *Magnetosphere None in this orbit Orbit E14: *Magnetosphere Io plasma torus energetics *Jovian Atmosphere North polar aurora energetics Orbit E15: *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Upper atmosphere energy budget Orbit E16: *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Stratosphere composition and upper atmosphere energy budget Orbit E17: Io: Real-time EUV map of Io torus midnight ansa. 24 EUV sectors (part of an annulus at 90 deg cone) centered on wobbling torus. EUV on, by agreement with HIC, between the time 90 deg cone crosses Jupiter (0 Rj) and the ansa of Europa's orbit (9 Rj), catching the UV-bright ansa ribbon at 5.76 Rj. Spacecraft distance from Jupiter is at least 17 Rj. EUV spectrum is 540 to 1280, including torus emission lines at 685 (S++), 765 (S+), and 834 (O+). In conjuction with UVS observation centered on torus ansa ribbon. (17TV17MANS01-). Orbit E18: (no data obtained) *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Upper atmosphere energy budget Orbit E19: * 19TV19MANS01 (not obtained) EUV/UVS map of Io torus midnight ansa to determine morphological changes in torus over the timescale of several years. * 19HV_STARCAL: Star cross calibration using Lyman-alpha for EUV on Sirius and the sky background. Orbit C20: * 20TV20NANS01, 20TU20NANS01 EUV/UVS map of Io torus noon ansa during the C20 outbound to determine morphological changes in torus over the timescale of several years. EUV emission lines: S++ 685, S+ 765, O+ 834; UVS emission lines:H 1215, S+ 1259, S+ 4070. * 20HU_STARCAL (not obtained, see E19C cal) Star cross calibration between UVS and EUV on Lyman-alpha sky background and star calibration on Sirius at RA/Dec ~ 100.73/-16.659, type A061, mag -1.6. This is a realtime observation using F/N and F/G full scans at a distance from Jupiter ~ 25.4 Rj. The Sirius Ly-a flux (UARS data from Tom Woods) is 20 ph cm-2 s-1 A-1. Orbit C21: *Magnetosphere None *Jovian Atmosphere None Orbit C22: * 22TV22NANS01, 22TU22NANS01-02 (02 not obtained) EUV/UVS map of Io torus noon ansa during the C22 outbound to determine morphological changes in torus over the timescale of several years and to look at dusk torus sectors. EUV emission lines: S++ 685, S+ 765, O+ 834; UVS emission lines:H 1215, S+ 1259, S+ 4070. Orbit C23: * 23TV23NANS01, 23TU23NANS01 EUV/UVS map of Io torus noon ansa during the C23 outbound to determine morphological changes in torus over the timescale of several years and to look at dusk torus sectors. EUV emission lines: S++ 685, S+ 765, O+ 834; UVS emission lines:H 1215, S+ 1259, S+ 4070. Orbit I24: Orbit I24 enables the UVS and EUV to concentrate upon Io science related to studies of: - Io torus morphology (24TV24NANS01, 24TU24NANS01, 24TU24NANS02): Io torus observations with the EUV and UVS continue the morphological study of the Io torus and provide the basis for a long term comparison between prime mission and GMM datasets over 4 years as well as asymmetries between dawn (prime mission) and dusk (GMM) torus ansae. Orbit I25: In orbit I25, the EUV will concentrate upon Io science related to studies of: - Io torus morphology (25TV24NANS01, 25TU25NANS01, and 25TU25NANS02). The three (3) Io torus observations with the EUV and UVS continue the morphological study of the Io torus and provide the basis for a long term comparison between prime mission and GMM datasets over 4 years as well as asymmetries between dawn (prime mission) and dusk (GMM) torus ansae. - Jupiter aurora (I25JVAURORA) +++++++++++++++++++++++++++++++++++++ GMM SCIENCE OBJECTIVES +++++++++++++++++++++++++++++++++++++ See the discussion in the UVS hardware data set catalog file GOUVSEDR.DS regarding the failure of the UVS grating drive optics in orbit C20. Io Phase: * Orbits I27, along with I24 and I25 above, enable the EUV to concentrate upon Io science related to studies of: - satellite aurora (24IUECLIPS01, 25IUECLIPS01, 27IUECLIPS01); and - Io torus morphology (24TV24NANS01, 24TU24NANS01, 24TU24NANS02, 25TV24NANS01, 25TU25NANS01, 25TU25NANS02, 27TVNANSA_01, 27TUNANSA_01). Orbit E26 is limited solely to EUV observations of the Io torus (26TVMANSA_01). The three (3) satellite aurora observations (I25)are all made when Io is in eclipse and, where possible, will be compared to SSI images of Io in eclipse. In particular, the removal of scattered sunlight for these FUV-MUV-NUV observations will potentially reveal new information about Jupiter's magneto- spheric and energetic interactions with the Io atmosphere and surface. The nine (9) Io torus observations with the EUV and UVS continue the morphological study of the Io torus and provide the basis for a long term comparison between prime mission and GMM datasets over 4 years as well as asymmetries between dawn (prime mission) and dusk (GMM) torus ansae. * Cassini Phase: Orbits G28 and G29 provide a duet of unique opportunities to study the Jovian system close-in while Cassini observes the system from afar. The EUV instrument will study: - satellite and Jupiter aurora (28IUAURORA01, 28JUAUR_SW01, 29EUECLIPS01, 29EUECLIPS02, 29IUAURORA01, 29GUAURORA01, 29GUAURORA02, 29JUAUR_SW01, 29JUAURZON01); - Io torus morphology (28TVNANSA_01, 28TUNANSA_01, 29TUMIDPRO01); - conduct calibration activities (EUV ALLSKY and SKYBKG observations). The nine (9) satellite and Jupiter aurora observations are made under a variety of conditions such as when Io and Ganymede are in eclipse and, where possible, will be compared to SSI eclipse images. In particular, the removal of scattered sunlight for these FUV-MUV-NUV observations will potentially reveal new information about Jupiter's magnetospheric and energetic interact- ions with the satellites' atmosphere and surface. In addition, the JUAUR_SW01 observations will study the solar wind perturbation to the Jovian magneto- sphere (aurora) over a full solar rotation in coincidence with Cassini solar wind observations while the JUAURZON recorded observation will characterize newly hypothesized flares in the Jovian auroral region at high time resolution. The three (3) Io torus observations with the EUV and UVS continue the morphological study of the Io torus and provide the basis for a long term comparison between prime mission and GMM datasets over 4 years as well as asymmetries between dawn (prime mission) and dusk (GMM) torus ansae. Finally, the instrument team will perform an end-of-mission star and cross calibration between the two instruments. Orbit I26: I26 is limited solely to EUV observations of the Io torus (26TVMANSA_01). This was lost due to spacecraft safing. Orbit I27: In orbit I27, the EUV concentrates upon Io torus science (27TVNANSA_01). This observation will be the most complete (ansa to ansa) spatial and feature (two ansae, torus profiles, and Jupiter aurora) data set since early in the prime mission. The EUV Io torus observation continues the morphological study of the Io torus and provide the basis for a long term comparison between prime mission and GMM datasets over 4 years as well as asymmetries between dawn (prime mission) and dusk (GMM) torus ansae. Orbit G28: In orbit G28, the EUV concentrates upon Io torus science. This observation will be the most complete (ansa to ansa) spatial and feature (two ansae, torus profiles, and Jupiter aurora) data set since early in the prime mission. The EUV Io torus observation continues the morphological study of the Io torus and provide the basis for a long term comparison between prime mission and GMM datasets over 4 years as well as asymmetries between dawn (prime mission) and dusk (GMM) torus ansae. Jupiter aurora and sky background data will also be obtained by the EUV to recapture two of the UVS science objectives in G28, i.e., the characterization of the derived solar wind during the period of the Cassini encounter with Jupiter. Orbits G29, C30, I32 and I33: All these orbits studied the 'All-Sky' Hydrogen Lyan-Alpha background. Parameters ========== The Real-Time-Science (RTS) data format integrates wavelength bins over sky-sector into an instrument buffer every spacecraft revolution. After the commanded integration duration (in integral numbers of RIMs) the buffer is sent to the ground in real time packets. Files of the RTS EUV image matrix are formatted to contain one summation buffer with its associated (time tags and engineering) header. The duration of the summation period varies, as does the instrument configuration (via the FPNT and 24EUV command), within and across Observation classes. The file label and command sequence must be used to verify the observation criteria. Data ==== The following EDR data files are available as of 1 September 1998. The files are grouped with the descriptions of SWG, MWG and AWG observation objectives for the orbit. The descriptions originate with the planning package. Some described observations may have been lost during downlink. They are included for completeness of the science concepts and designs. All available data files are shown. Files showing the data file names versus begin and end times are available in The CD's Document/Orbit_planning folder. Orbit J0CD/G1 * G1 AWG The G1 UVS Jovian atmosphere observations focus on 4 types of activities that are obtained in collaboration with the EUV instrument: Auroral studies: 3 observations investigate Jovian auroral processes. a) G1JUEWMAPS01 is a recorded, 1/2 hour observation of the southern auroral region, including the footprint of the Io fluxtube. Precipitating electron energies, as they impact the upper atmosphere hydrogen, will be derived. This observation is planned in collaboration with near-simultaneous HST Jovian auroral observations by John Clarke of Univ. of Michigan. b) G1JUAURMAP01, also in a campaign with HST observations, will observe the southern auroral region asymmetries between dayside and nightside aurorae. (RTS only) c) G1JUFIXTMD01 will observe northern auroral activity in a unique look at precipitating electron energies as they vary with longitude during 1 full Jupiter day (10 hours). (RTS only) * MWG - The standard Torus ansa (MANSxx, NANSxx) and Profile measurements (MPROxx, NPROxx) were obtained. * IFL2 is data from the Phase 2 In-Flight-Load software load and checkout. J0CD_EUV_G1AURA02.DAT;1 J0CD_EUV_G1AURA03.DAT;1 J0CD_EUV_G1AURA11.DAT;2 J0CD_EUV_G1AURA12.DAT;1 J0CD_EUV_G1AURA12_XP.DAT;1 J0CD_EUV_G1EUVANS01.DAT;1 J0CD_EUV_G1MANS02.DAT;2 J0CD_EUV_G1MANS03.DAT;2 J0CD_EUV_G1MANS11.DAT;2 J0CD_EUV_G1MANS12.DAT;2 J0CD_EUV_G1MANS12_XP.DAT;1 J0CD_EUV_G1MPRO01.DAT;1 J0CD_EUV_G1MPRO02.DAT;1 J0CD_EUV_G1MPRO03.DAT;1 J0CD_EUV_G1MPRO04.DAT;1 J0CD_EUV_G1MPRO05.DAT;1 J0CD_EUV_G1MPRO06.DAT;1 J0CD_EUV_G1NANS01.DAT;2 J0CD_EUV_G1NANS02.DAT;1 J0CD_EUV_G1NANS02_XP.DAT;1 J0CD_EUV_G1NANS31.DAT;2 J0CD_EUV_G1NANS32.DAT;2 J0CD_EUV_G1NANS32_XP.DAT;1 J0CD_EUV_G1NANS33.DAT;2 J0CD_EUV_G1NANS33_XP.DAT;1 J0CD_EUV_G1NANS34.DAT;1 J0CD_EUV_G1NANS34_XP.DAT;1 J0CD_IFL2_EUV_EUVON.DAT;1 Orbit G2 * G2 MWG The highest priority UVS magnetospheric observations during this orbit will be those in conjunction with the EUV instrument for the observations of the Io torus. There are two general segments of these observations, one set for the G2 inbound torus measurements at the beginning of the G2A encounter period and the second set for the C3 inbound measurements at the end of the G2C cruise period. Both sets of realtime measurements (G2NANS/G2MPRO, C3NANS/C3MPRO/C3NPRO) will map the torus ansae simultaneously with the EUV in S and O emission lines using the FUV/MUV wavelengths. Ratios of the emission lines will determine electron temperatures. The profile measurements, in particular, will characterize the torus ansae as a function of longitude, time and radius. Additionally, in conjunction with the MWG's magnetospheric survey, the UVS will conduct magnetonebula measurements (MAGNEB) during the G2B,C outbound cruise period. These long duration realtime measurements of FUV S I and O I emission lines looking down the magnetonebula axis (antisun direction) will integrate the flux in 24-hour segments. A cross-calibration with UVS was performed; the star was delta-Scorpii. Note: files with _XP as part of their filename are files containing additional EUV data which do not overlap in time with the simultaneous, collaborative UVS data file. Note: The Galileo spacecraft 'safed' during the G1C load and was not brought up until G2A was about to start. A very small set of EUV data was obtained. The star cal, NPROs and MPROs were never taken. One NANSA was obtained and the data from the instrument turn on (TURNON). G02A_EUV_TURNON__.DAT;1 G02A_EUV_G2NANS04.DAT;1 Orbit C3 * C3 AWG UVS collaborative observations include realtime southern auroral full spectral FUV observations (AURMAP) to provide dayside/nightside asymmetries for an analysis of color ratios. These ratios will provide the energies of the electrons precipitating into the auroral zone. These AWG UVS aurora observations augment the EUV/UVS MWG aurora observations. * C3 MWG The highest priority UVS magnetospheric observations during this orbit will be those in conjunction with the EUV instrument for the observations of the Io torus and Jupiter aurora. There are two general segments of the torus observations, one set for the C3 inbound torus measurements at the beginning of the C3A encounter period and the second set for the E4 inbound measurements at the end of the C3C cruise period. Both sets of realtime torus measurements (C3NPRO and E4MANS/E4MPRO/E4NANS) will map the torus ansae simultaneously with the EUV in S and O ion emission lines using the FUV/MUV wavelengths. Ratios of the emission lines will determine electron temperatures. The profile measurements, in particular, will characterize the torus ansae as a function of longitude, time, and radius. The realtime auroral measurements (E4AURA) will map the aurora and electroglow simultaneously with the EUV in the H2 bands. The integrated intensities will characterize the global energy output and the latitudinal and time variation of energetic particles input into the atmosphere. G02C_EUV_C3AURA01.DAT;1 G02C_EUV_C3AURA02.DAT;1 G02C_EUV_C3AURA03.DAT;1 G02C_EUV_C3MANS01.DAT;1 G02C_EUV_C3MANS02.DAT;1 G02C_EUV_C3MANS03.DAT;1 G02C_EUV_C3MPRO02.DAT;2 G02C_EUV_C3MPRO02_XP.DAT;1 G02C_EUV_C3MPRO03.DAT;1 G02C_EUV_C3MPRO03_XP.DAT;1 G02C_EUV_C3MPRO04.DAT;1 G02C_EUV_C3MPRO04_XP.DAT;1 G02C_EUV_C3MPRO05.DAT;2 G02C_EUV_C3MPRO06.DAT;1 G02C_EUV_C3NANS01.DAT;1 G02C_EUV_C3NANS02.DAT;1 G02C_EUV_C3NANS31.DAT;1 G02C_EUV_C3NANS31_XP.DAT;1 G02C_EUV_C3NANS32.DAT;1 G02C_EUV_CROSSCAL.DAT;1 Orbit E4 * E4 AWG Realtime data rate southern auroral observations with UVS using full spectral FUV observations will provide longitudinal coverage during part of a Jupiter rotation on both the dayside and nightside (AURMAP). Analysis of the ratios between different spectral lines (color ratios) will yield energies of the electrons that are precipitating into the auroral zones. A star cross-calibration on Spica will be performed. (UVS observation:C03C_URT_CROSSCAL.DAT;1 and EUV observation C03C_EUV_CROSSCAL.DAT;1). * E4 MWG The highest priority UVS magnetospheric observations during this orbit will be those of the Io torus in conjunction with the EUV instrument (both pointed perpendicular to the spacecraft). This 10-hour set of E4-inbound torus measurements at the beginning of the E4A encounter period (E4NANS) completes the Io torus observations begun during C3C, and will map the torus noon ansa in S and O emission lines using UVS FUV and MUV wavelengths simultaneously with the EUV. Ratios of emission lines will determine electron temperatures. The profile measurements (MPRO) will characterize the torus ansae as a function of longitude, time, and radius. * There are no UVS or EUV science observations during E4-E6 cruise. C03C_EUV_CROSSCAL.DAT;1 C03C_EUV_E4AURA01.DAT;1 C03C_EUV_E4AURA02.DAT;1 C03C_EUV_E4AURA02_XP.DAT;1 C03C_EUV_E4AURA03.DAT;1 C03C_EUV_E4MANS02.DAT;1 C03C_EUV_E4MANS02_XP.DAT;1 C03C_EUV_E4MANS03.DAT;1 C03C_EUV_E4MANS11.DAT;1 C03C_EUV_E4MANS11_XP.DAT;1 C03C_EUV_E4MANS12.DAT;3 C03C_EUV_E4MPRO01.DAT;2 C03C_EUV_E4MPRO02.DAT;1 C03C_EUV_E4MPRO02_XP.DAT;1 C03C_EUV_E4MPRO03.DAT;1 C03C_EUV_E4MPRO04.DAT;1 C03C_EUV_E4MPRO05.DAT;1 C03C_EUV_E4MPRO05_XP.DAT;1 C03C_EUV_E4MPRO06.DAT;1 C03C_EUV_E4MPRO06_XP.DAT;1 C03C_EUV_E4NANS01.DAT;1 C03C_EUV_E4NANS02.DAT;2 C03C_EUV_E4NANS31.DAT;1 C03C_EUV_E4NANS31_XP.DAT;1 C03C_EUV_E4NANS32.DAT;1 C03C_EUV_E4NANS32_XP.DAT;1 E04A_EUV_E4NANS04.DAT;1 Orbit E5 Orbit E5 was the navigation 'transfer orbit' and there were no science data. The transfer orbit causes the EUV observations to be made DURING the A load instead of in the cruise (C) load just before the encounter load (A). Orbit E6 * E6 AWG Realtime southern auroral full spectral FUV observations will provide new longitudinal coverage on both the dayside and nightside (AURMAP). Analysis of the ratios between different spectral lines (color ratios) in these data will yield energies of the electrons precipitating into the auroral zones. These are done in collaboration with EUV. * E6 MWG The highest priority UVS magnetospheric observations during E6 will be realtime encounter measurements of the Io torus and Jupiter aurora at approximately 90 degree cone angle in conjunction with the EUV instrument. Io torus midnight ansa maps (E6MANS01-03) will consist of spectra centered on ionized S and O emission lines using the UVS FUV and MUV wavelengths simultaneously with the EUV. Ratios of emission line strengths will determine electron temperatures. E6MANS04 will map the inner, colder part of the Io torus at FUV wavelengths that also cover hydrogen Lyman alpha emission lines; the last 4 hours of this observation are designed to cross-calibrate the EUV with the UVS since Lyman alpha is observed by both instruments (CROSSCAL). Jupiter dark-side aurora measurements in this orbit (E6AURA01-03) focus on northern hemisphere hydrogen emissions at FUV and MUV wavelengths. Brief dark-side equatorial electroglow and southern aurora observations are also made. Integrated intensities will help to characterize the global energy output and the latitudinal and time variation of energetic particle input into the atmosphere. Inside the EUV 25 Rj radiation limit, the UVS will map the Io torus noon ansa at FUV and MUV wavelengths corresponding to ionized S and O emissions. During E6 cruise, the UVS instrument will make its first measurements of neutral O and S emissions in the anti-solar direction of the Jovian magnetosphere. These magnetonebula observations (MAGNEB01-05) will be 2 to 5 days in duration, with UVS readouts occurring every 24 hours. Finally, at the end of E6C, UVS is performing a first-time search for neutral H and O emissions in the orbits of Ganymede and Callisto. 18-hour observations centered on the ansa of each orbit (GTORUS and CTORUS) allow for the possible detection of a neutral torus of material associated with the surfaces and atmospheres of the two Galilean satellites. In GTORUS, the UVS will look at 70 degree cone angle through the spacecraft booms, demonstrating whether such measurements are feasible. E06A_EUV_CROSSCAL.DAT;1 E06A_EUV_E6AURA01.DAT;1 E06A_EUV_E6AURA02.DAT;1 E06A_EUV_E6AURA03.DAT;1 E06A_EUV_E6MANS01.DAT;1 E06A_EUV_E6MANS02.DAT;1 E06A_EUV_E6MANS03.DAT;1 E06A_EUV_E6MANS04.DAT;2 Orbit G7 * G7 AWG UVS observations will provide a realtime fixed local time map for northern and southern auroral FUV spectral coverage and precipitating electron energy (color ratio) measurements (FIXTMD01). This observation is slightly different from previous FIXTMD observations in that the UVS will drift at cone 90 deg from the darkside onto the dayside. This observation will benefit from a NIMS ridealong for looking at H3+ and from EUV realtime observations occurring during this time. Additional realtime coverage of the southern and northern auroral darkside and brightside asymmetries (AURMAP01) will occur immediately following FIXTMD01 and will benefit from SSI, NIMS, and EUV ridealongs. Analysis of the ratios between different spectral lines (color ratios) will yield energies of the electrons precipitating into the auroral zones. * G7 MWG At the beginning of G7A, UVS will observe the Callisto and Ganymede orbit ansae (CTORUS02 and GTORUS02), continuing measurements begun in E6C and designed to search for neutral H and O emissions. The highest priority UVS magnetospheric observations during the G7 orbit will be those in conjunction with the EUV instrument for observations of the Io torus midnight ansa and Jupiter aurora. This set of realtime torus measurements (G7MANS01-03) will map the torus ansa simultaneously with the EUV in S and O ion emission lines using FUV and near-ultraviolet (NUV: ~400 nm) wavelengths. Ratios of emission line intensities will determine electron temperatures. A UVS-only midnight ansa profile will also be taken (G7MPRO01), using the scan platform to target at greater than 90 deg cone angle, while EUV continues to observe the colder portion of the inner torus. Realtime auroral measurements (G7AURA01-03) will map the aurora and electroglow simultaneously with the EUV in the FUV hydrogen bands. AURA03 is EUV-only, and occurs at the same time as UVS-AWG, NIMS, SSI, and HST observations of the aurora. Integrated intensities will characterize the global energy output and the latitudinal and time variation of energetic particle input into the atmosphere. Inside 23 Rj, the UVS alone will map the Io torus noon ansa (G7NANS02-03) in S and O ion emission lines. Again, a UVS-only noon ansa profile will also be taken (G7NPRO01). The noon and midnight ansa observations will help characterize the torus ansae as a function of longitude, time, and radial distance. During cruise, several UVS magnetonebula observations are planned. These observations are long-duration measurements of FUV neutral H and O emissions along the axis of the magnetonebula in the antisun direction. G07A_EUV_G7AURA01.DAT;1 G07A_EUV_G7AURA02.DAT;1 G07A_EUV_G7AURA03.DAT;1 G07A_EUV_G7MANS01.DAT;2 G07A_EUV_G7MANS02.DAT;1 G07A_EUV_G7MANS03.DAT;1 G07A_EUV_G7MPRO01.DAT;1 G07A_EUV_G7MPRO01_XP.DAT;1 Orbit G8 * G8 MWG The highest priority EUV magnetospheric observations in G8, are a set of four real-time Io torus midnight ansa measurements performed inbound to Jupiter C/A, in conjunction with UVS, when both are pointed at 90 deg cone angle. These G8MANS observations are designed to obtain S and O ion emission line strengths at EUV as well as FUV and NUV (UVS N channel, 280-430 nm) wavelengths. Ratios of intensities will determine electron temperatures, while the integrated intensity characterizes the torus energy output for energy budget considerations. These EUV/UVS G8MANS begin with a cross-calibration with both instruments observing the sky background for two hours (the EUV observation is G08A_EUV_CROSSCAL.DAT;1 and the UVS observation is G08A_URT_CROSSCAL.DAT;1). G08A_EUV_CROSSCAL.DAT;1 G08A_EUV_G8MANS02.DAT;1 G08A_EUV_G8MANS03.DAT;1 G08A_EUV_G8MANS11.DAT;1 G08A_EUV_G8MANS12.DAT;1 G08A_EUV_G8MPRO01_XP.DAT;1 Orbit C9 * C9 AWG The Southern aurora will be mapped from 260 to 360 deg longitude by the UVS; H2 band color ratios will be observed to determine precipitating particle energies (AURMAP01-02). Northern aurora will be mapped on the dayside at 170 deg longitude with a similar objective (FIXLON). Of unique importance are two outbound auroral observations. AURMAP04 observes southern dusk aurora with objectives similar to AURMAP01-02. AURVAR is coincident with the Fields and Particles Campaign A observation and will record southern aurora short time-scale variability as well as spatial characteristics of the Io fluxtube footprint at H Lyman-alpha wavelengths. * C9 MWG The highest priority UVS magnetospheric observation during C9 is a set of realtime Io torus midnight ansa measurements performed outbound from Jupiter C/A, in conjunction with EUV, when both are pointed at 90 deg cone angle. This C9MANS04 observation is designed to obtain S and O ion emission line strengths at EUV as well as FUV and NUV (UVS N channel, 280-430 nm) wavelengths. Ratios of intensities will determine electron temperatures, and the integrated intensity characterizes the torus energy output for energy budget considerations. One independent real-time EUV observation occurs after the instrument is turned on 19 Rj outbound from Jupiter C/A: an aurora map (C9AURA). C09A_EUV_C9AURA02.DAT;1 C09A_EUV_C9MANS04.DAT;1 C09B_EUV_C9MANS04.DAT;1 Orbit C10 * C10 MWG The highest priority UVS magnetospheric observations in C10 are realtime Io torus noon and midnight ansa measurements. A far-midnight ansa observation (10FANS01), is performed inbound to Jupiter C/A, observing the torus outside of the orbit of Europa in conjunction with EUV, when both are pointed at 90 deg cone angle. It is designed to obtain S and O ion emission line strengths at EUV as well as FUV and NUV wavelengths. Intensity ratios will determine electron temperatures, and integrated intensity characterizes the torus energy output for energy budget considerations. * C10 SWG A unique EUV satellite observation (CVSPNSCN) before Callisto closest approach will search for extreme UV (60-130 nm) absorptions and emissions. UVS will observe Callisto three times at high resolution. C10A_EUV_10FANS01.DAT;1 C10A_EUV_SPNSCN01.DAT;1 C10B_EUV_11XCAL01.DAT;1 Orbit E11 * E11 MWG The highest priority UVS magnetospheric observations in E11 are realtime Io torus midnight ansa measurements (11MANS01-03) performed inbound to Jupiter in conjunction with EUV, when both are pointed at 90 deg cone angle. They are designed to obtain S and O ion emission line strengths at EUV as well as FUV (115-320 nm) and NUV (280-430 nm) wavelengths. Intensity ratios will determine electron temperatures, and integrated intensity characterizes the torus energy output for energy budget considerations. Other simultaneous UVS/EUV goals include two midnight ansa profiles (11MPRO01-02: UVS observes ansa at >90 deg cone angle, while EUV views the cold inner torus) and two Jupiter northern aurora observations (11AURA01-02: UVS at ~90 deg). A final observation of the cold torus occurs with EUV (11MPRO04) before it is shut off at 17.0 Rj (closest operation in the prime mission, although it is intended to be operated to 17 Rj in GEM). A UVS-EUV cross-calibration at Lyman-alpha wavelengths (sky background) will also occur inbound to E11 (11XCAL01). E11A_EUV_11AURA01.DAT;1 E11A_EUV_11AURA02.DAT;2 E11A_EUV_11MANS01.DAT;1 E11A_EUV_11MANS02.DAT;1 E11A_EUV_11MANS03.DAT;1 E11A_EUV_11MPRO01.DAT;1 E11A_EUV_11MPRO02.DAT;1 E11A_EUV_11MPRO04.DAT;1 Orbit E12, E13: There were no observations planned in Orbits E12 and E13. Orbit E14: E14A_EUV_MANS01.DAT Orbit E15: E15A_EUV_15AURA02.DAT E15A_EUV_15MANS01.DAT Orbit E16: All EUV data was lost from this orbit due to spacecraft safing. Orbit E17: E17A_EUV_TV17MANS01.DAT;1 Orbit E18: All EUV data was lost from this orbit due to spacecraft safing. Orbit E19: e19c_euv_starcal.dat;3 Orbit C20: c20a_euv_tv20mans01.dat;2 Orbit C21: There were no observations planned in Orbit C21. Orbit C22: C22A_EUV_TVNANS01.DAT;1 Orbit C23: C23A_EUV_TVNANS01.DAT;1 Orbit I24: I24A_EUV_TV24NANS01.DAT;6 Orbit I25: I25A_EUV_JVAURORA.DAT;2 I25A_EUV_TV25NANS01.DAT;2 Orbit I26: There were no observations planned in Orbit I26. Orbit I27: I27A_EUV_TV27NANS01.DAT;2 Orbit G28: G28A_EUV_TVNANS01.DAT;1 G28B_EUV_TVNANS01.DAT;1 G28B_EUV_ALLSKY.DAT;2 G28B_EUV_SKYBKG.DAT;3 Orbit G29: G29A_EUV_ALLSKY.DAT;1 Orbit C30: C30B_EUV_TVALLSKY.DAT;1 Orbit I32: I32B_EUV_TVALLSKY.DAT;1 Orbit I33: I33X_EUV_ALLSKY.DAT;1 Ancillary Data ============== These are raw EUV data sets. For analysis, geometry parameters are obtained from the SPICE kernels for the time period of analysis. Geometry is archived in the EUV 'LOOK' files. Two EUV files can be used to verify instrument configuration(s) within any data set. The orbit Status files (form: orbit-number_EUV_PB/RT_ORBIT_STATUS.LIS) and the instrument history command file (CMD_ARCHIVE.LIS) indicate instrument configuration. The Galileo SEF (Sequence of Events) file may also be used to verify the EUV configuration during the observation. There are also OAPEL descriptions and plots in the CD's Document/Orbit_lanning folders. Calibration files are available from the PDS EUV Instrument sets. Analysis techniques for various data classes are described in the published papers. A publication list is also available from PDS. Torus geometry parameters are supplied with the RDR data sets; otherwise use the SPICE kernel files to determine needed geometry. Software tools are supplied for interpreting the EUV RTS data matrix. The Galileo Project archives the SEF and ASRUN sequence products as well as some observation design materials. These may be used to help understand each observation. The UVS/EUV team retains some design materials as well. The team visualization tool, called GGGS, can be used to review the observation geometry, based on SEF and SPICE products. See the LASP web site for availability. The following is a list of the available orbit Status files. Use these to verify the commanded and obtained instrument configuration. The label describes the contents. Status and Orbit Status files: The archive has renamed these and incorporated the label in the file header as well as shortened the file name to a format as follows: (Orbit)(instrument, U or E))(PB or RT)(STAT or ST).TXT For example, the file uvs_pb_c03_status.lis;1 is called C9UPBST.TXT . Orbit Status files: euv_rts_c03_status.lis;2 euv_rts_e06_status.lis;2 euv_rts_g07_status.lis;1 euv_rts_c09_status.lis;1 euv_rts_e11_status.lis;1 euv_rts_g08_status.lis;1 euv_rts_c10_status.lis;1 euv_rts_e14_status.lis;1 euv_rts_g28_status.lis;1 euv_rts_c20_status.lis;1 euv_rts_e15_status.lis;1 euv_rts_i24_status.lis;3 euv_rts_c22_status.lis;2 euv_rts_e17_status.lis;1 euv_rts_i25_status.lis;1 euv_rts_c23_status.lis;2 euv_rts_e19_status.lis;1 euv_rts_i27_status.lis;1 euv_rts_e04_status.lis;1 euv_rts_g02_status.lis;1 euv_rts_j0cd_status.lis;4 euv_rts_g29_status.lis;1 euv_rts_i32_status.lis;1 euv_rts_i33x_status.lis;1 euv_rts_c30b_status.lis;1 Coordinate System ================= Time tags are given in spacecraft clock (SCET), UTC as well as ground receipt time (ERT), UTC. Specific timing details are given in the file labels. A description of the Galileo spacecraft clock is given in the Documents folder file called TIME_CLOCKS.DOC The EUV hardware is mounted on the spinning (Rotor) section of the Galileo spacecraft. Care should be taken to note the coordinate systems defined in the instrument paper, especially that of the viewed field - referred to as the sky sector. Software is provided to help interpret the sky sector view geometry. See the file #### in the Software folder. Any value not recovered by the ground system is assigned a value of -1. Zero is a legitimate EUV EDR value. The Jupiter atmospheric radius used is 71492.km. Software ======== EUV EDR data files are written with IDL (Interactive Data Language, a product of Research Systems, Inc. of Boulder, Colorado.) The files are created on a Digital Equipment Vax computer. No special software is necessary to read the simple array structures. IEEE standard transfer-file formatted data are also available in support of Unix platforms. Vax files may be read on the unix platform with the IDL OPEN function option referred to as '/vax_float'. Media/Format ============ The standard distribution format for the data is electronic transfer. Confidence Level Overview ========================= All EDR data are exactly as recovered from the ground system. Ground system data recovery flags are included in the EDR headers. Resultant reliability and accuracy of the raw data are 100% described. Completeness can be derived from the data file header information. Pointing accuracy in the supplemental (SPICE) data kernels may be the largest uncertainty in analyzing the data. Reduced downlink capacity caused less raw pointing information to be downlinked. The position and rotation angles of the z-axis (spin axis) are crucial to the field viewed by the EUV on the rotating spacecraft section. This knowledge is available to the instrument on a Real-Time Interrupt (RTI) time frame so the instrument can obtain its data consistently. The user has less accuracy in the after-the-fact z-axis position files due to the RTS rate. Subsequently, there can be difficulty in coordinating the data with pointing knowledge. Gyros are only used during Encounter sequence load periods; raw pointing knowledge is on 5 RIM centers in Cruise loads and 10 minor frame centers during Encounter loads. SPICE kernel granularity is much greater in the final orbits however the SPICE Toolkit interpolation routines are superior. Recent Publications =================== For a list of publications updated to 2010, see the GOUVPUBS.CAT file. Simultaneous Extreme Ultraviolet and Far Ultraviolet Observations of Jupiter Aurora From The Galileo Orbiter, Ajello, J., D. Shemansky, W. Pryor, K. Tobiska, C. Hord, S. Stephens, I. Stewart, J. Clarke, K. Simmons, W. McClintock, C. Barth, J. Gebben, D. Miller and B. Sandel, submitted to GRL, June 1, 1997. Galileo Ultraviolet Spectrometer Observations of Jupiter's Auroral Spectrum from 1600-3200A, Pryor, Wayne R., Joseph M. Ajello, W. Kent Tobiska, Donald E. Shemansky, Geoffrey K. James, Charles W. Hord, Stuart K. Stephens, Robert A. West, A. Ian F. Stewart, William E. McClintock, Karen E. Simmons, Amanda R. Hendrix, Deborah A. Miller, JGR, Vol. 103, No. E9, pp 20,149- 20,158, August 30, 1998. Galileo Ultraviolet Spectrometer Observations of Atomic Hydrogen in the Atmosphere of Ganymede, C.A.Barth, C.W.Hord, A.I.F.Stewart, W.R.Pryor, K.E.Simmons, W.E.McClintock, J.M.Ajello, K.L.Naviaux, J.J.Aiello, GRL, Vol.24, No.17, pp 2147-2150, September 1, 1997. The following paper is particularly helpful in that it describes the EUV calibration process: Ajello, J.M., D.E. Shemansky, W.R. Pryor, A.I. Stewart, K.E. Simmons, T. Majeed, J.H. Waite, G.R. Gladstone, D. Grodent, Spectroscopic Evidence for High-Altitude Aurora at Jupiter from Galileo Extreme Ultraviolet Spectrometer and Hopkins Ultraviolet Telescope Observations, Icarus, v.152, I.1, pp.151-171, July, 2001. Data Coverage and Quality ========================= Any value not recovered by the ground system is assigned a value of -1. Zero is a legitimate EUV EDR value. The EUV instrument puts out 8-bit values of range 0-277 (octal). The PB data are in this range. The RTS data are accumulated in an on-board 16-bit, roll-over buffer. Zero is a legitimate RTS value; values greater that 2^15 roll-over to zero and continue accumulating. See the CALINFO.CAT and Software files for descriptions on dealing with the roll-over buffer values. Limitations =========== Sequenced science observations may not necessarily have been recovered to the ground. All available EDR EUV data sets have been archived in PDS. There are no known EUV instrument operation questions. An EUV 'status' file is archived for each orbit which compiles the EUV instrument reported configuration (from the telemetered data). Spacecraft safing just prior to the closest approach of several GEM orbits caused the loss of EUV data. ............................................................................." 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