Target CALLISTO-LEADING: There is no need or capability to test the scheduling of observations of moving targets in Phase I. This warning will go away the next time the proposal is loaded. Target CALLISTO-TRAILING: There is no need or capability to test the scheduling of observations of moving targets in Phase I. This warning will go away the next time the proposal is loaded. 0 Assigned ID: 976 ----- Attempting Submission 1 (Fri Apr 08 23:10:06 GMT 2016) ----- HST Phase I Proposal 976 (callisto24_v2.apt) successfully submitted. Receipt: # 976-1 ----- Attempting Submission 2 (Fri Apr 08 23:34:32 GMT 2016) ----- I get an error that the Visit Planner needs to be run, but when I run it I get messages like: Observation 1: 1 CALLISTO-LEADING won't be processed using the visit planner because it targets a Moving target. POS TARG OUTSIDE OF APERTURE NO ORIENT POS TARG OUTSIDE OF APERTURE INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. INEFFICIENT ORDERING OF FP-POS POSITIONS POS TARG OUTSIDE OF APERTURE NO ORIENT INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS POS TARG OUTSIDE OF APERTURE Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Sensitive exposures should have an ETC run number provided. We do not include ETC number references because the exposures are very similar to ones obtained in proposal 11535, which had adequate SNR for our purposes (Cunningham et al. 2015) 1001832819 ----- Attempting Submission 1 (Thu Jul 21 13:56:20 GMT 2016) ----- - We deliberately use POS_TARG to put Callisto fully or partially out of the aperture in some exposures- , for background measurements - We do not include ETC number references because the exposures are very similar to ones obtained in proposal 11535, which had adequate SNR for our purposes (Cunningham et al. 2015) - We repeat FP-POS positions between target and background measurements, which inevitably leads to sometimes going to smaller FP-POS numbers, triggering the "inefficient ordering" warning - We are aware of the calibration issues with extended targets, having performed similar observations before We plan to address first-order questions about the nature and origin of the mysterious atmosphere of Callisto, including its composition, longitudinal distribution, formation, and support mechanisms. This investigation is made possible by the remarkable sensitivity of the COS instrument, which has recently detected faint 1304 A and 1356 A O I emission from Callisto's leading / Jupiter-facing quadrant. The emission is probably due to dissociation of O2 molecules in Callisto's atmosphere by photo-electrons, and resonant scattering from an extended atomic O corona. We suspect, from Galileo ionospheric data, that the atmosphere may be much denser, and brighter in emission, on the trailing hemisphere, as expected for a sputter-generated atmosphere, and propose to test the sputter generation hypothesis with 4-orbit COS integrations on the leading and trailing hemispheres. If the trailing side emissions are indeed brighter, the improved SNR there will also allow much improved determination of atmospheric and coronal composition and optical depth. The observations will set the stage for, and aid in planning of, the extensive observations of Callisto's environment planned for the JUICE mission. Because Callisto's atmospheric oxygen emissions are indirectly illuminated by sunlight, which is uniform and quantifiable, it is much easier to understand atmospheric spatial distribution, and thus origin, than on Europa and Ganymede were emissions depend on magnetospheric excitation which is spatially variable and poorly understood. Callisto's atmosphere thus provides a unique chance to better understand the oxygen atmospheres of all the icy Galilean moons. Four orbits with the G130M grating at 1300?, to achieve >= 8000s. Solar System 12 false true false false false 0.0 0.0 false SUPPORTED SOLAR SYSTEM YES As the oxygen lines to be observed are also present in terrestrial airglow, we choose to observe near opposition to maximize time in Earth's shadow. We specify this by requiring that the solar elongation of Callisto be greater than 160 degrees SATELLITE CALLISTO STD=JUPITER STD=CALLISTO F(1356 A) = 3 Rayleigh SEP OF CALLISTO-LEADING JUPITER FROM EARTH GT 30", SEP OF CALLISTO-LEADING IO FROM EARTH GT 10", SEP OF CALLISTO-LEADING EUROPA FROM EARTH GT 10", SEP OF CALLISTO-LEADING GANYMEDE FROM EARTH GT 10", OLG OF CALLISTO-LEADING FROM EARTH BETWEEN 60 120, SEP OF CALLISTO-LEADING SUN FROM EARTH GT 160D EARTH SOLAR SYSTEM YES As the oxygen lines to be observed are also present in terrestrial airglow, we choose to observe near opposition to maximize time in Earth's shadow. We specify this by requiring that the solar elongation of Callisto be greater than 160 degrees SATELLITE CALLISTO STD=JUPITER STD=CALLISTO F(1356 A) = 3 Rayleigh SEP OF CALLISTO-TRAILING JUPITER FROM EARTH GT 30", SEP OF CALLISTO-TRAILING IO FROM EARTH GT 10", SEP OF CALLISTO-TRAILING EUROPA FROM EARTH GT 10", SEP OF CALLISTO-TRAILING GANYMEDE FROM EARTH GT 10", OLG OF CALLISTO-TRAILING FROM EARTH BETWEEN 240 300, SEP OF CALLISTO-TRAILING SUN FROM EARTH GT 160D EARTH COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 Using ephemeris for target 14755-01-CALLISTO-TRAILING The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 1469108218242 /Users/spencer/1_work/cos/14755_callistoatmos/phase2/OP-cache/14755_final-v01.xml * We use four consecutive orbits to minimize exposure time loss due to acquisition * For the first two orbits, after acquisition, Callisto is offset 0.9" in the aperture- an identical strategy to visit 4 of our previous program 11535 * For the second two orbits, we use the second half of orbit 3 and the first half of orbit 4 to characterize the background 5" away from Callisto, at the same HST orbital position as integrations centered on Callisto in the first half of orbit 3 and the second half of orbit 4. For each of these integrations we use just 2 FP-POS positions to minimize overhead (Tic-Visit :proposal-id 14755 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "21-Jul-2016 07:36:57.0" :trans-errors '(:WARNINGS 6 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 496048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14755 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14755 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2682 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14755 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14755 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2799 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14755 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2799 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) true 4 0 Callisto is 6.2 +/- 0.5 mags over 2009 (based on JPL ephem generator), and is effectively 1.1 mag dimmer in this grating bandpass than in the visible (based on albedo = 0.06 here vs. 0.17 in visible). So I use mV_effective = 7.3 and get 0.44/0.96 seconds for ACQ-Search/ACQ-PeakXD modes to reach S/N = 40 (ETC IDs COS78131 / COS78132). 5 seconds gives plenty of margin Callisto is 6.2 +/- 0.5 mags over 2009 (based on JPL ephem generator), and is effectively 1.1 mag dimmer in this grating bandpass than in the visible (based on albedo = 0.06 here vs. 0.17 in visible). So I use mV_effective = 7.3 and get 0.44/0.96 seconds for ACQ-Search/ACQ-PeakXD modes to reach S/N = 40 (ETC IDs COS78131 / COS78132) estimates are same as for exposure 1, ACQ/SEARCH COS76584 for calculation of buffer time. Assumes effective mV = 6.8 and 15 Rayleigh (8.2e-16 ergs/cm^2/s) 1356? line. Gives buffer time = 2/3 * 5939s. POS TARG is designed to place Callisto 0.9" in the cross-dispersion (+Y) direction. This is intended to allow a portion of the the aperture, and therefore a portion of the spectrum, to contain purely airglow, while the upper part of the aperture contains Callisto's spectrum in addition to oxygen airglow. The cross-dispersion variation in oxygen emission line intensity will help indicate whether Callisto has a significant additional oxygen signal. Using ephemeris for target 14755-02-CALLISTO-LEADING The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 1469108220898 /Users/spencer/1_work/cos/14755_callistoatmos/phase2/OP-cache/14755_final-v02.xml * We use four consecutive orbits to minimize exposure time loss due to acquisition * For the first two orbits, after acquisition, Callisto is offset 0.9" in the aperture- an identical strategy to visit 4 of our previous program 11535 * For the second two orbits, we use the second half of orbit 3 and the first half of orbit 4 to characterize the background 5" away from Callisto, at the same HST orbital position as integrations centered on Callisto in the first half of orbit 3 and the second half of orbit 4. For each of these integrations we use just 2 FP-POS positions to minimize overhead (Tic-Visit :proposal-id 14755 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "21-Jul-2016 07:37:00.0" :trans-errors '(:WARNINGS 6 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 496048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14755 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14755 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2682 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14755 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2766 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14755 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2799 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14755 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2799 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3035 :pcs-gap 0 ) true 4 0 Callisto is 6.2 +/- 0.5 mags over 2009 (based on JPL ephem generator), and is effectively 1.1 mag dimmer in this grating bandpass than in the visible (based on albedo = 0.06 here vs. 0.17 in visible). So I use mV_effective = 7.3 and get 0.44/0.96 seconds for ACQ-Search/ACQ-PeakXD modes to reach S/N = 40 (ETC IDs COS78131 / COS78132). 5 seconds gives plenty of margin Callisto is 6.2 +/- 0.5 mags over 2009 (based on JPL ephem generator), and is effectively 1.1 mag dimmer in this grating bandpass than in the visible (based on albedo = 0.06 here vs. 0.17 in visible). So I use mV_effective = 7.3 and get 0.44/0.96 seconds for ACQ-Search/ACQ-PeakXD modes to reach S/N = 40 (ETC IDs COS78131 / COS78132) estimates are same as for exposure 1, ACQ/SEARCH COS76584 for calculation of buffer time. Assumes effective mV = 6.8 and 15 Rayleigh (8.2e-16 ergs/cm^2/s) 1356? line. Gives buffer time = 2/3 * 5939s. POS TARG is designed to place Callisto 0.9" in the cross-dispersion (+Y) direction. This is intended to allow a portion of the the aperture, and therefore a portion of the spectrum, to contain purely airglow, while the upper part of the aperture contains Callisto's spectrum in addition to oxygen airglow. The cross-dispersion variation in oxygen emission line intensity will help indicate whether Callisto has a significant additional oxygen signal.