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Mnemonic
Description
Group
G_IS_OBSG_IS_OBSWorking Group 3
G_IS_3G3Ganymede in-situ observations around closest approachWorking Group 3
JM_PE_OBSJupiter Magnetosphere perijove segments containing link to observations databaseWorking Group 3
CALLISTO_IONOCALLISTO_IONO In situ Callisto ionosphere observationWorking Group 3
EUROPA_IONO_ISEUROPA_IONO_IS In situ Europa ionosphere observationWorking Group 3
GANYMEDE_IONOGANYMEDE_IONO In situ Ganymede ionosphere observationWorking Group 3
G_IS_4G4 Working Group 3
JM_PE35 Working Group 3
JM_PE33share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE31share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE29share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE27share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE25share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE23share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE21share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE19share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE17share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE15share prime high lat PJ between WG3 and WG4Working Group 3
JM_PE13share prime high lat PJ between WG3 and WG4Working Group 3
TOR_RS Working Group 3
JM_INCL Working Group 3
JM_PE_P4_noDL Working Group 3
JM_PE_P4Perijoves with WG3 prime (--> 20/09/18: modified (discussion with OW). assuming ~2 times what is produced in G4-G5 scenario (~6.5-7 Gb). Corresponds roughly to 19kbps, copied from JA_INCL) RS rate assumes no D/L suspension (case 2)Working Group 3
JM_CB Working Group 3
JM_ENA Working Group 3
JM_GM Working Group 3
JM_PEassuming: JMAG: 2.31 kbps RPWI: 1.7*2.167 kbps PEP: 2 kpbs (ball park number; discussion with Gabriella at WG3 F2F meeting in Sept 2018)Working Group 3
G_IS Working Group 3
E_IS Working Group 3
C_IS Working Group 3
CALLISTO_ENAFar approach energetic neutral atom imaging of CallistoWorking Group 3
CALLISTO_FLYBY_RPWI_IONO_AJS Working Group 3
CALLISTO_WAKEIn situ Callisto wake observationWorking Group 3
EUROPA_ENAFar approach energetic neutral atom imaging of EuropaWorking Group 3
EUROPA_FLYBY_RPWI_IONO_AJS Working Group 3
EUROPA_TOR_ISIn situ Europa torus observationWorking Group 3
EUROPA_WAKEIn situ Europa wake observationWorking Group 3
GANYMEDE_ENAFar approach energetic neutral atom imaging of GanymedeWorking Group 3
GANYMEDE_GMIn situ mapping of global configuration and monitoring dynamics of Ganymede's magnetospheric environmentWorking Group 3
GANYMEDE_FLYBY_RPWI_IONO_AJS Working Group 3
GANYMEDE_WAKEIn situ Ganymede wake observationWorking Group 3
JUPITER_CBIn situ Jupiter corotation breakdown region and plasma transport observation. Maximize the intervals for which co-rotation is measured to build spatial and temporal coverage of corotation profiles across the magnetosphere and also in the local moon environments.Working Group 3
JUPITER_CPSIn situ Jupiter current/plasma sheet observationWorking Group 3
JUPITER_ENAImaging of Jupiter's magnetosphere in energetic neutral atoms (ENAs).Maximize pitch angle coverage with PEP JEI,JDC,JoEE, JENI (ion mode) a) JENI has a broad FoV and captures Jupiter and the Io/Europa torus and magnetosphere at most times. No special pointing design required for JENI besides requiring an approximate nadir pointing (considerable offsets can still be acceptable) b) JNA disk-shaped/slit FoV has a slight offset from the XZ spacecraft plane, meaning that during nadir pointing, it images preferentially the northern or southern extension of the Europa/Io torus, whereas Jupiter may be in the edge or outside of the FoV, especially at large distances. Scans (small rotations around Sc-X) or periods with stable, small offset of the SC-xz plane from Nadir can help to better image stronger emissions from the equatorial torusWorking Group 3
JUPITER_GMIn situ mapping of global configuration and monitoring dynamics of the Jovian magnetospheric environment. corotation should be in the FoV of PEP/JDC or PEP/JEI. Conditions for coverage: ◦ Minimum angle less than about 11.25 deg (half-azimuthal sector size) of a JEI or JDC pixel from corotation ◦ Boresight angle of JDC or JEI less than ˜90 deg Conditions for ideal coverage: ◦ Minimum angle less than about 11.25 deg (half-azimuthal sector size) of a JEI or JDC pixel from corotation ◦ Boresight angle less than ˜75 deg (JEI) or 70 deg (JDC): corotation away from the FoV edge JDC is preferred for monitoring corotation, over JEI, when possible.Working Group 3
JUPITER_NULLIn situ Jupiter magnetic null searchWorking Group 3
JUPITER_PDTIn situ Jupiter particle distribution transition region observation. Maximize pitch angle coverage for PEP/JEI, JDC,JoEE, JENI (ion mode)Working Group 3
JUPITER_TAILIn situ search for signatures of local magnetic reconnection in the Jovian magnetotailWorking Group 3
RINGMOSAICRINGMOSAIC (Janus definition). impression of the extent of the whole ring systemWorking Group 2
RINGPHASE Working Group 2
G_RS_36G11G_RS_36G11Working Group 2
G_RS_35G10G_RS_35G10Working Group 2
G_RS_34G9G_RS_34G9Working Group 2
G_RS_32G8G_RS_32G8Working Group 2
G_RS_28G7G_RS_28G7Working Group 2
G_RS_27G6G_RS_27G6Working Group 2
C_RS_33C23C_RS_33C23Working Group 2
C_RS_31C22C_RS_31C22Working Group 2
C_RS_30C21 Working Group 2
C_RS_26C19 Working Group 2
RINGSPIRAL_MPRINGSPIRAL_MP (medium phase: JANUS Def)Working Group 2
RINGSPIRAL_HPRINGSPIRAL_HP (high phase, Janus def)Working Group 2
SHADOWEDGErings SHADOWEDGE. Imaging of the ring region intersected by the planetary shadow at moderate elevation and very high phase. Especially for the very faint gossamer rings and the Thebe extensionWorking Group 2
IO_MAJ_HOTSPOTSIO_MAJ_HOTSPOTSWorking Group 2
IO_MAJ_COMPOSITIONIO_MAJ_COMPOSITIONWorking Group 2
ASTRO_IRR1_MEGACLITEASTRO_IRR1_MEGACLITEWorking Group 2
RINGMATTERRINGMATTER. Observations of the main rings and the gossamer rings, imaging the ring ansae from moderately large elevation. The moderatly large elevation will reveal azimuthal structure in the rings and the presence of clumps at the resolution limit of the imaging.Working Group 2
J_SAT_OBSJ_SAT_OBSWorking Group 2
J_SAT_516_MetJ_SAT_516_MetWorking Group 2
J_SAT_515_AdrJ_SAT_515_AdrWorking Group 2
J_SAT_514_TheJ_SAT_514_TheWorking Group 2
J_SAT_505_AmaJ_SAT_505_AmaWorking Group 2
J_SAT_IRR_SEARCHJ_SAT_IRR_SEARCH discover new irregular moonsWorking Group 2
J_SAT_520_TayJ_SAT_520_TayWorking Group 2
J_SAT_559_17J1J_SAT_559_17J1Working Group 2
J_SAT_55503_3J9J_SAT_55503_3J9Working Group 2
J_SAT_548_CylJ_SAT_548_CylWorking Group 2
J_SAT_566_17J5J_SAT_566_17J5Working Group 2
J_SAT_556_11J2J_SAT_556_11J2Working Group 2
J_SAT_568_17J7J_SAT_568_17J7Working Group 2
J_SAT_569_17J8J_SAT_569_17J8Working Group 2
J_SAT_562_ValJ_SAT_562_ValWorking Group 2
J_SAT_567_17J6J_SAT_567_17J6Working Group 2
J_SAT_564_17J3J_SAT_564_17J3Working Group 2
J_SAT_543_ArcJ_SAT_543_ArcWorking Group 2
J_SAT_537_KleJ_SAT_537_KleWorking Group 2
J_SAT_538_PstJ_SAT_538_PstWorking Group 2
J_SAT_554_16J1J_SAT_554_16J1Working Group 2
J_SAT_542_TlxJ_SAT_542_TlxWorking Group 2
J_SAT_541_AoeJ_SAT_541_AoeWorking Group 2
J_SAT_522_HarJ_SAT_522_HarWorking Group 2
J_SAT_561_3J19J_SAT_561_3J19Working Group 2
J_SAT_540_MneJ_SAT_540_MneWorking Group 2
J_SAT_557_EirJ_SAT_557_EirWorking Group 2
J_SAT_547_EukJ_SAT_547_EukWorking Group 2
J_SAT_530_HerJ_SAT_530_HerWorking Group 2
J_SAT_532_EydJ_SAT_532_EydWorking Group 2
J_SAT_565_PdiJ_SAT_565_PdiWorking Group 2
J_SAT_523_KlkJ_SAT_523_KlkWorking Group 2
J_SAT_572_11J1J_SAT_572_11J1Working Group 2

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