Dear Adam and Andy, We have been successful with visit 01 which was testing the global count rate with Jupiter in ACS/SBC FOV. It turns out that we are way below the bright object limit so that we may go ahead with the rest of the program (visits 02 to 04). For safety reasons (our estimations could be inaccurate to a factor of 2) we have decided to switch the filter from F115LP to F125LP for all exposures. In this new phase 2 (the original was downloaded from STScI), I changed all occurrences of F115LP to F125LP, and removed the 'ON-HOLD for VISIT 1' requirements. Regards, Denis Grodent (PI) ----- Submission 1 (Fri Dec 10 17:10:30 GMT 2004) ----- ----- Submission 2 (Thu Feb 10 10:34:22 GMT 2005) ----- Identification of a magnetic anomaly at Jupiter from satellite footprints Repeated imaging of Jupiter's aurora has shown that the northern main oval has a distorted 'kidney bean' shape in the general range of 90-140? System III longitude, which appears unchanged since 1994. While it is more difficult to observe the conjugate regions in the southern aurora, no corresponding distortion appears in the south. Recent improved accuracy in locating the satellite footprint auroral emissions has provided new information about the geometry of Jupiter's magnetic field in this and other areas. The study of the magnetic field provides us with insight into the state of matter and the dynamics deep down Jupiter. There is currently no other way to do this from orbit. The persistent pattern of the main oval implies a disturbance of the local magnetic field, and the increased latitudinal separation of the locus of satellite footprints from each other and from the main oval implies a locally weaker field strength. It is possible that these phenomena result from a magnetic anomaly in Jupiter's intrinsic magnetic field, as was proposed by A. Dessler in the 1970's. There is presently only limited evidence from the scarcity of auroral footprints observed in this longitude range. We propose to obtain HST UV images with specific observing geometries of Jupiter to determine the locations of the auroral footprints of Io, Europa, and Ganymede in cycle 13 to accurately determine the magnetic field geometry in the suggested anomaly region, and to either confirm or refute the suggestion of a local magnetic anomaly.
We propose to obtain FUV--MAMA STIS images of the Io, Ganymede, and Europa auroral footprints in the northern hemisphere of Jupiter. We will concentrate on the anomaly region in the S3 longitude range $90^{\circ}-140^{\circ}$. To best probe this region with the satellite footprints, the CML must be close to $110^{\circ}$ and the footprints should appear at a longitude close to the CML (Fig.~4). The bulk of the auroral emission rotates with the magnetic field at an angular velocity of $1^{\circ}/100 sec$. On the other hand, the footprints are bound to their satellite through magnetic field lines and rotate at a velocity mainly constrained by the satellite orbital motion (Io: $\sim0.24^{\circ}/100~sec$, Europa: $\sim0.12^{\circ}/100~sec$, and Ganymede: $\sim0.06^{\circ}/100~sec$). This differential motion of the footprints and the bulk of the auroral emision provides us with a mean to scan a longitude range of the anomaly region of $\sim30^{\circ}$, during a regular visibility period of HST (52~min). After one complete HST orbit (96~min) the CML increases by $58^{\circ}$ while the footprints move by $14^{\circ}$ for Io, $7^{\circ}$ for Europa, and $3.5^{\circ}$ for Ganymede. Accordingly, it is possible to cover most of the anomaly region with one visit consisting of two consecutive orbits. Previous FUV--MAMA STIS images of 300~sec using the F25SRF2 (Ly-$\alpha$ blocker) have proven to show the different footprints and the Io trailing tail with sufficient signal to planetary background noise ratio. Moreover at the requested CML and footprints longitudes these emissions will be substantially limb--brightened. The F25SRF2 filter will prevent Ly-$\alpha$ contamination due to geocoronal dayglow emission and will reduce the amount of reflected sunlight by the jovian planetary disk. We will use the TIMETAG mode which will permit us to follow the short timescale variations of the auroral emissions in the anomaly region. The need to use HST-STIS rather than a ground-based infrared observatory is that the latter does not provide sufficient signal to noise ratio, temporal resolution, and spatial resolution to reach the scientific goals of the present program. After the loss of STIS, the original 10140 program was switched to ACS-SBC (TTRB). This is the first time that Jupiter is observed with SBC in the FUV. Consequently, the first orbit of this 6-orbit program will be used to test the global count rate of different filters to make sure that Jupiter does not exceed the bright object limit. This means that orbits 2 to 6 might have to be modified according to the results of the first orbit. SOLAR SYSTEM 12 false 0.0 false false false false false SUPPORTED SOLAR SYSTEM = This phase 2 replaces the previously accepted one. STIS is now replaced by ACS/SBC (TTRB) = FOV center is about 5 arcsec above north pole along Jupiter's spin axis. In this configuration, less than 20% of Jupiter's disk appears in the FOV. = One must take the bending of the magnetic field lines into account (use VIP4 magnetic model) to map the OLG of Io and other satellites onto the Jovian ionosphere. = CML of Jupiter at the begining of the orbit should be close to 80deg (S3) = All Jupiter longitudes are System 3. PLANET JUPITER_NORTH_POLE_AURORA_CML_80_IO_FAR STD=JUPITER TYPE=POS_ANGLE,RAD=25.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 80.0 160.0, OLG OF IO BETWEEN 190.0 250.0 SOLAR SYSTEM = CML of Jupiter at the begining of this orbit should be close to 140deg (S3). It is automatically the case if this orbit immediately follows the previous one (JUPITERA) when the CML is close to 80deg. = Similarly, the OLG of Io increases by ~14deg every HST orbit and the new Io OLG range constraint is automatically met. = If necessary, we may relax or remove the constraint on Ganymede's OLG PLANET JUPITER_NORTH_POLE_AURORA_CML_140_IO_FAR STD=JUPITER TYPE=POS_ANGLE,RAD=25.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 120.0 170.0, OLG OF IO BETWEEN 224.0 254.0 SOLAR SYSTEM Copy of JUPITERA, with smaller OLG of Io (the relative motion of the Io footprint is used to scan the region of interest) PLANET JUPITER_NORTH_POLE_AURORA_CML_80_IO_MED STD=JUPITER TYPE=POS_ANGLE,RAD=25.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 80.0 160.0, OLG OF IO BETWEEN 190.0 250.0 SOLAR SYSTEM Copy of JUPITERB, with smaller OLG of Io (the relative motion of the Io footprint is used to scan the region of interest) PLANET JUPITER_NORTH_POLE_AURORA_CML_140_IO_MED STD=JUPITER TYPE=POS_ANGLE,RAD=25.0,ANG=25.0,REF=NORTH SOLAR SYSTEM Copy of JUPITERC, with smaller OLG of Io (the relative motion of the Io footprint is used to scan the region of interest) PLANET JUPITER_NORTH_POLE_AURORA_CML_80_IO_CLOSE STD=JUPITER TYPE=POS_ANGLE,RAD=25.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 80.0 160.0, OLG OF IO BETWEEN 190.0 250.0 SOLAR SYSTEM Copy of JUPITERD, with smaller OLG of Io (the relative motion of the Io footprint is used to scan the region of interest) PLANET JUPITER_NORTH_POLE_AURORA_CML_140_IO_CLOSE STD=JUPITER TYPE=POS_ANGLE,RAD=25.0,ANG=25.0,REF=NORTH SOLAR SYSTEM Copy of JUPITERB. Offset from Jupiter is 10" above the north pole (instead of 5") so that only ~10% of the jovian disk is intercepted by SBC FOV. This reduces the risk of bright object limit excess with SBC+F140LP. PLANET JUPITER_NORTH_POLE_AURORA_CML_140_IO_FAR STD=JUPITER TYPE=POS_ANGLE,RAD=30.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 120.0 170.0, OLG OF IO BETWEEN 224.0 254.0 SOLAR SYSTEM = This phase 2 replaces the previously accepted one. STIS is now replaced by ACS/SBC (TTRB) = FOV center is about 5 arcsec above north pole along Jupiter's spin axis. In this configuration, less than 20% of Jupiter's disk appears in the FOV. = One must take the bending of the magnetic field lines into account (use VIP4 magnetic model) to map the OLG of Io and other satellites onto the Jovian ionosphere. = CML of Jupiter at the begining of the orbit should be close to 80deg (S3) = All Jupiter longitudes are System 3. PLANET JUPITER_NORTH_POLE_AURORA_CML_80_IO_FAR STD=JUPITER TYPE=POS_ANGLE,RAD=25.0,ANG=25.0,REF=NORTH CML OF JUPITER FROM EARTH BETWEEN 80.0 160.0, OLG OF IO BETWEEN 190.0 280.0 STIS/FUV-MAMA Imaging No No F25SRF2 STIS/FUV-MAMA Imaging No No 25MAMA This orbit is used to test the global count rates obtained with SBC + F165LP, F122M, and F140LP. The results of this test will condition the next 5 orbits. For F165LP and F122M the center of SBC FOV is placed at 5 arcsec above the north pole of Jupiter, along the spin axis. This way approximately 20% of the jovian disk appears in the FOV and limits the estimated global count rate to less than 10,000 cps. For F140LP, which is more sensitive than the two others, the FOV centert is placed at 10 arcsec above the north pole of Jupiter and the visible portion of the disk decreases to ~10%, leading to a global count rate which should be close to 20,000 cps. This test orbits must be completed as soon as possible, so that we have a chance to adjust the other orbits as required. (Tic-Visit :proposal-id 10140 :visit-id "01" :proposal-version -1 :trans-version "20041107" :date "10-Feb-2005 10:47:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 148112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10140 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 10140 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10140 :visit-id "01" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2654 :al-overhead-at-end 0 :internal-dur-at-end 200 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) false 1 0 BEGIN ORBIT 1 END ORBIT 1 Celestial North Up (Jupiter North Up) in ACS FOV (Tic-Visit :proposal-id 10140 :visit-id "02" :proposal-version -1 :trans-version "20041107" :date "10-Feb-2005 10:47:45.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 277696 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10140 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10140 :visit-id "02" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 342 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) false 1 0 BEGIN ORBIT 2 END ORBIT 2 Celestial North Up (Jupiter North Up) in STIS FOV (Tic-Visit :proposal-id 10140 :visit-id "03" :proposal-version -1 :trans-version "20041107" :date "10-Feb-2005 10:47:50.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 573952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10140 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 10140 :visit-id "03" :obset-id "A3" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10140 :visit-id "03" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10140 :visit-id "03" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2650 :al-overhead-at-end 0 :internal-dur-at-end 342 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) false 2 0 BEGIN ORBIT 3 END ORBIT 3 BEGIN ORBIT 4 END ORBIT 4 Celestial North Up (Jupiter North Up) in STIS FOV (Tic-Visit :proposal-id 10140 :visit-id "04" :proposal-version -1 :trans-version "20041107" :date "10-Feb-2005 10:47:56.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 573952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10140 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 10140 :visit-id "04" :obset-id "A4" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10140 :visit-id "04" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10140 :visit-id "04" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2650 :al-overhead-at-end 0 :internal-dur-at-end 342 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) false 2 0 BEGIN ORBIT 5 END ORBIT 5 BEGIN ORBIT 6 END ORBIT 6 Celestial North Up (Jupiter North Up) in ACS FOV (Tic-Visit :proposal-id 10140 :visit-id "02" :proposal-version -1 :trans-version "20041107" :date "10-Feb-2005 10:47:45.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 277696 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10140 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10140 :visit-id "02" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 342 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) false 1 0 BEGIN ORBIT 2 END ORBIT 2