0 The polar aurora, an important energy source for the Earth's upper atmosphere, is about two orders of magnitude more intense at Jupiter where it releases approximately 10 GW in Jupiter's thermosphere. So far, HST observations of Jupiter's aurora have concentrated on the morphology and the relationship between the solar wind and the brightness distribution. While STIS-MAMA is still operational, time is now critical to move into a new era where FUV long-slit spectroscopy and the spatial scanning capabilities of HST are combined. We propose to use this powerful tool to remotely sense the characteristics of the precipitated electrons by slewing the spectral slit over the different auroral components. It will then be possible to associate electron energies with spatial auroral components and constrain acceleration mechanisms (field-aligned acceleration, magnetic field reconnection, pitch angle electron scattering) associated with specific emission regions. For this, a combination of FUV imaging with STIS long slit spectroscopy will map the spatial variations of the auroral depth and thus the energy of the precipitated electrons. These results will be compared with current models of the Jovian magnetosphere-ionosphere interactions and will provide key inputs to a 3-D model of the Jupiter's atmosphere global heat budget and dynamics currently under development. This compact timely program is designed to provide a major step forward for a better understanding of the physical interactions taking place in Jupiter's magnetosphere and their effects on giant planets' atmospheres, a likely paradigm for many giant fast spinning planets with massive magnetic field in the universe. Spectral observations will be made with the 52x0.5 arcsec long slit aperture and the G140L grating to cover the full FUV spectral range necessary for electron energy studies. The spectra will be collected in the time-tag mode. The slit will scan the auroral oval from equatorward of the auroral boundary to above the planetary limb. This spatial scan will be continuous across the aurora. It will be oriented with the minimum possible inclination on the equatorial plane compatible with the spacecraft orientations constraints. Once the HST orbit is accurately known, the slew rate during the time-tag observations will be determined in order to best cover the entire auroral oval. Experience gained during execution program 12883 (where telescope slews were performed to scan the Jovian aurora) will be used to program the detailed observations. Indeed, the amplitude of the slews depends on the angular size of Jupiter which varies with the exact date of the observations. Ideally, the observations should be performed within one month from opposition (Jan. 5, 2014). STIS spectra of Jupiter previously obtained by the PI and team members have demonstrated that the STIS count rate limit is far from being reached during to the spectral observations with the STIS long slit. The strategy for the observations will be as follows: VISIT 1 (1 orbit): One spatial scan with the 52x0.5 arc sec long slit and G140L grating from above the north limb to equatorward (southward) of the auroral emission. The exposure will be timetagged. Jupiter's System III central meridian longitude (CML) will be in the range 150-190 deg offering optimal view of the north polar region. Io will be visible within a specified range from the central meridian. VISITS 2 (1 orbit): Repeat of the same sequence with Jupiter's CML in the range 200-240 deg, providing a view complementary to visit 1. VISITS 3 (1 orbit): Repeat of the same sequence in the South polar region, starting from above the south limb till equatorward (northward) of the auroral emission. Jupiter's CML will be in the range 20-60 deg, offering optimal view of the south polar region. Io will be visible within a specified range from the central meridian. The three visits are independent and should be distant in time by at least one week. None None SOLAR SYSTEM Default false false false false false SUPPORTED SOLAR SYSTEM -Constraints on CML and OLG may be relaxed by +/-10deg. -POS_ANGLE RAD and ANG are date and ROLL dependent. Current values are suitable for 5-JAN-2014. -Ideally, the spectral slit should be as parallel as possible to Jupiter's equatorial plane. -POS_ANGLE R_RAD depends on actual exposure time. -The slew rate R_RAD is negative, meaning that the motion is from above Jupiter's pole towards Jupiter's center. -It will be necessary to iterate with our Program Coordinator to adjust these values once final execution date and ROLL are known. PLANET Spectrum North 1 STD=JUPITER TYPE=POS_ANGLE,RAD=24.6,ANG=7,REF=NORTH,R_RAD=-417.6,R_ANG=0,EPOCH=08-JAN-2014:23:04:47,EpochTimeScale=UTC OLG OF IO BETWEEN 90 240, CML OF JUPITER FROM EARTH BETWEEN 150 190 EARTH SOLAR SYSTEM -Constraints on CML and OLG may be relaxed by +/-10deg. -POS_ANGLE RAD and ANG are date and ROLL dependent. Current values are suitable for 5-JAN-2014. -Ideally, the spectral slit should be as parallel as possible to Jupiter's equatorial plane. -POS_ANGLE R_RAD depends on actual exposure time. -The slew rate R_RAD is negative, meaning that the motion is from above Jupiter's pole towards Jupiter's center. -It will be necessary to iterate with our Program Coordinator to adjust these values once final execution date and ROLL are known. PLANET Spectrum North 2 STD=JUPITER TYPE=POS_ANGLE,RAD=24.6,ANG=7,REF=NORTH,R_RAD=-417.6,R_ANG=0,EPOCH=14-JAN-2014:00:12:23,EpochTimeScale=UTC CML OF JUPITER FROM EARTH BETWEEN 200 258 EARTH SOLAR SYSTEM -Constraints on CML and OLG may be relaxed by +/-10deg. -POS_ANGLE RAD and ANG are date and ROLL dependent. Current values are suitable for 5-JAN-2014. -Ideally, the spectral slit should be as parallel as possible to Jupiter's equatorial plane. -POS_ANGLE R_RAD depends on actual exposure time. -The slew rate R_RAD is negative, meaning that the motion is from above Jupiter's pole towards Jupiter's center. -It will be necessary to iterate with our Program Coordinator to adjust these values once final execution date and ROLL are known. PLANET Spectrum South STD=JUPITER TYPE=POS_ANGLE,RAD=25,ANG=187,REF=NORTH,R_RAD=-340,R_ANG=0,EPOCH=12-JAN-2014:22:42:21,EpochTimeScale=UTC CML OF JUPITER FROM EARTH BETWEEN 20 100 EARTH SOLAR SYSTEM -Constraints on CML and OLG may be relaxed by +/-10deg. -POS_ANGLE RAD and ANG are date and ROLL dependent. Current values are suitable for 5-JAN-2014. -Ideally, the spectral slit should be as parallel as possible to Jupiter's equatorial plane. -POS_ANGLE R_RAD depends on actual exposure time. -The slew rate R_RAD is negative, meaning that the motion is from above Jupiter's pole towards Jupiter's center. -It will be necessary to iterate with our Program Coordinator to adjust these values once final execution date and ROLL are known. PLANET Spectrum North 2 STD=JUPITER TYPE=POS_ANGLE,RAD=21.1,ANG=-7,REF=NORTH,R_RAD=-291.35,R_ANG=0,EPOCH=15-MAR-2014:18:30:44,EpochTimeScale=UTC CML OF JUPITER FROM EARTH BETWEEN 200 240 EARTH STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/FUV-MAMA Imaging No No F25SRF2 Using ephemeris for target 13402-01-SPECTRUM-NORTH-1 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. BETWEENs for are for coordinated ground based observing. Each visit may be considered independently. Ideally, orbits should be executed at least 1 week apart. 1389221523000 129.0 (Tic-Visit :proposal-id 13402 :visit-id "01" :proposal-version -1 :trans-version "20130502" :date "05-Jul-2013 11:05:36.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1843984 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13402 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13402 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2607 :al-overhead-at-end 0 :internal-dur-at-end 625 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3229 :pcs-gap 0 ) false 1 0 Using ephemeris for target 13402-02-SPECTRUM-NORTH-2 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. BETWEENs for are for coordinated ground based observing. Each visit may be considered independently. Ideally, orbits should be executed at least 1 week apart. 1389657589000 125.89269013823679 (Tic-Visit :proposal-id 13402 :visit-id "02" :proposal-version -1 :trans-version "20130502" :date "05-Jul-2013 11:05:40.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1843984 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13402 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13402 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2607 :al-overhead-at-end 0 :internal-dur-at-end 625 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3229 :pcs-gap 0 ) false 1 0 Using ephemeris for target 13402-03-SPECTRUM-SOUTH The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. BETWEENs for are for coordinated ground based observing. Each visit may be considered independently. Ideally, orbits should be executed at least 1 week apart. 1389565791000 124.0 (Tic-Visit :proposal-id 13402 :visit-id "03" :proposal-version -1 :trans-version "20130502" :date "05-Jul-2013 11:05:42.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1843984 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13402 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13402 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2607 :al-overhead-at-end 0 :internal-dur-at-end 625 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3229 :pcs-gap 0 ) false 1 0 Using ephemeris for target 13402-12-SPECTRUM-NORTH-3 ephemeris data for target 13402-12-SPECTRUM-NORTH-3 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 13.342 to 15.092. ephemeris interval: 14.031 to 16.032 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 1392041812006 Each visit may be considered independently. Ideally, orbits should be executed at least 1 week apart. (Tic-Visit :proposal-id 13402 :visit-id "12" :proposal-version -1 :trans-version "20130502" :date "10-Feb-2014 15:16:51.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1843984 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13402 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13402 :visit-id "12" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2607 :al-overhead-at-end 0 :internal-dur-at-end 625 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3229 :pcs-gap 0 ) false 1 0