| GANYMEDE_FLYBY_RPWI_IONO_AJS | | Working Group 3 |
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| JM_PE | assuming:
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 |
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| C_IS_OBS | C_IS_OBS | Working Group 3 |
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| CALLISTO_IONO | CALLISTO_IONO
In situ Callisto ionosphere observation | Working Group 3 |
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| E_IS_OBS | E_IS_OBS | Working Group 3 |
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| EUROPA_IONO_IS | EUROPA_IONO_IS
In situ Europa ionosphere observation | Working Group 3 |
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| CALLISTO_ENA | Far approach energetic neutral atom imaging of Callisto | Working Group 3 |
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| EUROPA_ENA | Far approach energetic neutral atom imaging of Europa | Working Group 3 |
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| GANYMEDE_ENA | Far approach energetic neutral atom imaging of Ganymede | Working Group 3 |
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| G_IS_OBS | G_IS_OBS | Working Group 3 |
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| G_IS_3G3 | Ganymede in-situ observations around closest approach | Working Group 3 |
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| GANYMEDE_IONO | GANYMEDE_IONO
In situ Ganymede ionosphere observation | Working Group 3 |
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| JUPITER_ENA | Imaging 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 torus | Working Group 3 |
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| CALLISTO_WAKE | In situ Callisto wake observation | Working Group 3 |
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| EUROPA_TOR_IS | In situ Europa torus observation | Working Group 3 |
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| EUROPA_WAKE | In situ Europa wake observation | Working Group 3 |
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| GANYMEDE_WAKE | In situ Ganymede wake observation | Working Group 3 |
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| JUPITER_CP | In 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.
CP stands for corotation profile | Working Group 3 |
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| JUPITER_CB | In 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 |
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| JUPITER_CPS | In situ Jupiter current/plasma sheet observation | Working Group 3 |
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| JUPITER_NULL | In situ Jupiter magnetic null search | Working Group 3 |
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| JUPITER_PDT | In situ Jupiter particle distribution transition region observation.
Maximize pitch angle coverage for PEP/JEI, JDC,JoEE, JENI (ion mode) | Working Group 3 |
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| GANYMEDE_GM | In situ mapping of global configuration and monitoring dynamics of Ganymede's magnetospheric environment | Working Group 3 |
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| JUPITER_GM | In 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 |
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| JUPITER_TAIL | In situ search for signatures of local magnetic reconnection in the Jovian magnetotail | Working Group 3 |
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| JM_PE_OBS | Jupiter Magnetosphere perijove segments containing link to observations database | Working Group 3 |
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| JM_PE_P4 | Perijoves 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 |
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| JM_PE33 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE31 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE29 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE27 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE25 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE23 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE21 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE19 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE17 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE15 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JM_PE13 | share prime high lat PJ between WG3 and WG4 | Working Group 3 |
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| JA_PE59 | | Working Group 4 |
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| JA_PE58 | | Working Group 4 |
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| JA_PE57 | | Working Group 4 |
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| JA_PE56 | | Working Group 4 |
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| JA_PE55 | | Working Group 4 |
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| JA_PE54 | | Working Group 4 |
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| JA_PE53 | | Working Group 4 |
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| JA_PE52 | | Working Group 4 |
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| STAR_OCC | | Working Group 4 |
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| JA_PE51 | | Working Group 4 |
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| JA_PE50 | | Working Group 4 |
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| JA_PE49 | | Working Group 4 |
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| JA_PE48 | | Working Group 4 |
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| JA_PE47 | | Working Group 4 |
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| JA_PE46 | | Working Group 4 |
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| JA_PE45 | | Working Group 4 |
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| JA_PE44 | | Working Group 4 |
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| JA_PE43 | | Working Group 4 |
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| JA_PE42 | | Working Group 4 |
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| JA_PE41 | | Working Group 4 |
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| JA_PE40 | | Working Group 4 |
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| JA_PE39 | | Working Group 4 |
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| JA_PE38 | | Working Group 4 |
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| JA_PE37 | | Working Group 4 |
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| JA_PE36 | | Working Group 4 |
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| JA_PE34 | | Working Group 4 |
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| JA_PE32 | | Working Group 4 |
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| JA_PE30 | | Working Group 4 |
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| JA_PE28 | | Working Group 4 |
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| JA_PE26 | | Working Group 4 |
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| JA_PE24 | | Working Group 4 |
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| JA_PE22 | | Working Group 4 |
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| JA_PE20 | | Working Group 4 |
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| JA_PE18 | | Working Group 4 |
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| JA_PE16 | | Working Group 4 |
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| JA_PE14 | | Working Group 4 |
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| JA_PE12 | | Working Group 4 |
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| JA_PE11 | | Working Group 4 |
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| JA_PE10 | | Working Group 4 |
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| JA_PE9 | | Working Group 4 |
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| JA_PE8 | | Working Group 4 |
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| JA_PE7 | | Working Group 4 |
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| JA_PE6 | | Working Group 4 |
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| JA_PE5 | | Working Group 4 |
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| JA_PE4 | | Working Group 4 |
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| JA_PE3 | | Working Group 4 |
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| JA_PE2 | | Working Group 4 |
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| J_AURORA | | Working Group 4 |
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| JA_PE_MAJIS | | Working Group 4 |
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| JA_PE | | Working Group 4 |
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| JA_PH | | Working Group 4 |
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| JA_PE_noDL | | Working Group 4 |
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| JA_M | | Working Group 4 |
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| JA_INCL | | Working Group 4 |
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| INCLINED_NORTH | | Working Group 4 |
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| INCLINED_SOUTH | | Working Group 4 |
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| JUPITER_INCLINED_AURORA | | Working Group 4 |
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| JUPITER_PHASE_090 | | Working Group 4 |
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| JUPITER_PHASE_120_DEC | | Working Group 4 |
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| JUPITER_PHASE_120_INC | | Working Group 4 |
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| JUPITER_PHASE_135_DEC | | Working Group 4 |
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| JUPITER_PHASE_135_INC | | Working Group 4 |
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