0Assigned ID: 7
----- Attempting Submission 1 (Wed Jun 20 15:10:10 GMT 2018) -----A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.16th November 2018
ACS imaging of Mars revisit added with 3 orbits scheduled for 7-9 December 2018
Orbits 1 and 2 are Mars and orbit 3 is sky background 5 arcminutes away from Mars-643313098----- Attempting Submission 1 (Fri Jun 29 20:02:47 GMT 2018) -----
----- Attempting Submission 2 (Tue Jul 03 20:52:09 GMT 2018) -----
HST Phase II Proposal 15595 (15595_phase2.apt) successfully submitted.
Receipt: # 15595-2
----- Attempting Submission 3 (Wed Jul 04 19:53:28 GMT 2018) -----
----- Attempting Submission 4 (Thu Jul 05 13:28:53 GMT 2018) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 5 (Thu Jul 05 18:15:09 GMT 2018) -----
HST Phase II Proposal 15595 (Untitled.apt) successfully submitted.
Receipt: # 15595-5
----- Attempting Submission 6 (Thu Jul 05 18:28:09 GMT 2018) -----
----- Attempting Submission 7 (Thu Jul 05 22:41:04 GMT 2018) -----
----- Attempting Submission 8 (Fri Nov 16 22:32:17 GMT 2018) -----no ETC runs needed, count rates known from earlier observationsGlobal Dust Storm Effects on Martian Atmospheric EscapeHST observations revealed an order of magnitude seasonal changes in martian H escape flux which peaked at southern summer solstice. This large seasonal change is due to transport of H2O into the upper atmosphere which is either driven by seasonal winds from solar heating, or dust storms, or both. The currently ongoing global dust storm at Mars (~3 months before perihelion), provide an opportunity to separate the effects of solar flux from dust activity. In this DD proposal, ACS-SBC imaging of the extended H corona along with STIS spectra of D emission at Mars is proposed to characterize the effects of the global dust storm on martian atmospheric escape. While currently orbiting spacecraft at Mars effectively trace the dynamical changes occurring at lower altitudes, HST is uniquely positioned to image the highest exospheric altitudes which harbor the hot hydrogen population. The presence of this population increases previous estimates of martian hydrogen escape rate and thereby water escape by a factor of ~2. Observing the D emission at the same time will allow estimation of the D/H ratio and help determine any changes to it during a global dust storm. Instruments onboard the MAVEN spacecraft are capable of detecting the D emission. But the noise levels on the detector support detection only above 100 Rayleighs (Ls = 220 - 330). By contrast, HST is capable of detecting emissions as low as 20 Rayleighs. Since, global dust storm events are a rare (recurrence rate ~7-10 Earth-years) at Mars, the current event (Ls= 190) presents a good opportunity towards accessing their contribution in aiding atmospheric/water escape from Mars. This proposal supports the HST UV initiative.This program will obtain ACS SBC images of the martian hydrogen exosphere in the ultraviolet to characterize the effects of a global dust storm on the hot hydrogen population present in the exosphere of Mars. It will use the STIS spectrograph's echelle grating (E140H) capable of resolving the D and H Lyman alpha emissions to obtain the D/H ratio in the upper atmosphere of Mars during the occurrence of a global dust storm. The ACS SBC imager onboard HST will be used to obtain a series of images of Mars with the F115 LP filter, which transmits Lyman alpha, and the F140 LP filter which blocks Lyman alpha for one HST orbit. The scaled difference between the clear and filtered images will reveal the Lyman alpha emission coming from the hydrogen exosphere of Mars. This method produces highly effective results as the martian atmosphere is dominated by hydrogen above an altitude of ~250 km, which scatters solar Lyman alpha photons and is very bright at that wavelength.
For the deuterium Lyman alpha observations we will use the STIS spectrograph with the E140 H echelle grating, which is capable of resolving the H and D Lyman alpha line separated by 0.33 Angstroms. The STIS echelle spectrograph has a high resolution of 0.057 Angstroms using the 0.5 arcsec aperture, which is more than enough to separate the two lines at Mars. We will utilize the TIMETAG configuration and the 52x0.5 aperture for the STIS observation. The long aperture provides a higher count rate for the extended emission region, and has been well demonstrated in observations of Mars, Jupiter and the interplanetary hydrogen.
The program consists of two visits to observe Mars, with each visit comprising of 4 orbits. The observations from the first visit will need to be executed before the end of July 2018. This timeframe will allow the effects of the massive dust storm to propagate to the upper atmosphere and the yearly seasonal effects on the D and H Lyman alpha intensity would not have quite manifested itself on the exosphere of Mars. Therefore, any significant changes in intensity of H and D in the martian exosphere will be due to the dust storm and will be captured during the first visit. Mars will reach an L_S value of 211 deg. on 14th July 2018. The second visit will be executed in late October 2018 when Mars is close to its southern summer solstice position (L_S = 270-280 deg.), where the peak in H and H intensity is. A previous observation of the martian hydrogen exosphere conducted on 19th November 2016 (GO 14752) exists under similar solar activity conditions and the same solar longitude.Solar SystemSolar System0falseAVAILABLESOLAR SYSTEMYESPLANETExosphere of MarsSTD=MARSTYPE=POS_ANGLE,RAD=20,ANG=100,REF=NORTHNOT OCC OF MARS-EXOSPHERE-1 BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETExosphere of MarsSTD=MARSTYPE=POS_ANGLE,RAD=52,ANG=100,REF=NORTHNOT OCC OF MARS-EXOSPHERE-1-OFFSET BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETExosphere of MarsSTD=MARSTYPE=POS_ANGLE,RAD=3,ANG=75,REF=NORTHNOT OCC OF MARS-EXOSPHERE-STIS-1 BY MARS FROM EARTHEARTHSOLAR SYSTEMYESOffset from MarsOFFSETOffset to sky near MarsSTD=MARSTYPE=POS_ANGLE,RAD=300,ANG=0,REF=NORTHNOT OCC OF SKY-NEAR-MARS-1 BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETExosphere of MarsSTD=MARSTYPE=POS_ANGLE,RAD=18,ANG=280,REF=NORTHNOT OCC OF MARS-EXOSPHERE-2 BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETExosphere of MarsSTD=MARSTYPE=POS_ANGLE,RAD=50,ANG=280,REF=NORTHNOT OCC OF MARS-EXOSPHERE-2-OFFSET BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETExosphere of MarsSTD=MARSEARTHSOLAR SYSTEMYESOffset from MarsOFFSETOffset to sky near MarsSTD=MARSTYPE=POS_ANGLE,RAD=300,ANG=0,REF=NORTHNOT OCC OF SKY-NEAR-MARS-2 BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETMars hydrogen exosphereSTD=MARSTYPE=POS_ANGLE,RAD=10,ANG=280,REF=NORTHNOT OCC OF MARS-EXOSPHERE-RERUN BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETMars hot hydrogen imagingSTD=MARSTYPE=POS_ANGLE,RAD=50,ANG=280,REF=NORTHNOT OCC OF MARS-EXOSPHERE-OFFSET-RERUN BY MARS FROM EARTHEARTHSOLAR SYSTEMYESPLANETgeocorona and IPH background near MarsSTD=MARSTYPE=POS_ANGLE,RAD=300,ANG=0,REF=NORTHNOT OCC OF SKY-BACKGROUND-RERUN BY MARS FROM EARTH,
SEP OF SKY-BACKGROUND-RERUN MARS FROM EARTH GT 10"EARTHSOLAR SYSTEMYESOffset from MarsOFFSETOffset to sky near MarsSTD=MARSTYPE=POS_ANGLE,RAD=350,ANG=0,REF=NORTHNOT OCC OF SKY-NEAR-MARS-4 BY MARS FROM EARTHEARTHACS/SBCImagingNoNoF115LPACS/SBCImagingNoNoF140LPSTIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1234ACS/SBCImagingNoNoF115LPACS/SBCImagingNoNoF140LPSTIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1234Using ephemeris for target 15595-01-MARS-EXOSPHERE-1ephemeris data for target 15595-01-MARS-EXOSPHERE-1 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 17.213 to 19.182. ephemeris interval: 18.181 to 20.183Using ephemeris for target 15595-01-MARS-EXOSPHERE-1-OFFSETephemeris data for target 15595-01-MARS-EXOSPHERE-1-OFFSET does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 17.213 to 19.182. ephemeris interval: 18.181 to 20.183Timing link suitability includes constraints ([02 After 01 by 0.2 to 3.1 days])The scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.52Observations of Mars during global dust storm in summer 20181532395852000295.5(Tic-Visit
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:visit-id "01"
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:trans-version "20180409"
:date "04-Jul-2018 21:07:23.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 2
:saa-model "28"
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:data-volume 722128
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:orbit-number 2
:pcs-time 333
:si-vis-utilization 2777
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:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
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)false20Using ephemeris for target 15595-02-MARS-EXOSPHERE-STIS-1ephemeris data for target 15595-02-MARS-EXOSPHERE-STIS-1 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 17.213 to 19.182. ephemeris interval: 18.181 to 20.183Using ephemeris for target 15595-02-SKY-NEAR-MARS-1ephemeris data for target 15595-02-SKY-NEAR-MARS-1 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 17.213 to 19.182. ephemeris interval: 18.181 to 20.183Timing link suitability includes constraints ([02 After 01 by 0.2 to 3.1 days])The scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.52Observations of Mars during global dust storm in summer 20181532413023000297.0(Tic-Visit
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)false20Using ephemeris for target 15595-03-MARS-EXOSPHERE-2ephemeris data for target 15595-03-MARS-EXOSPHERE-2 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 17.213 to 19.182. ephemeris interval: 18.181 to 20.183Could not find ephemeris /Users/aroman/Desktop/visit-planner/15595_6.trh for target 15595-03-MARS-EXOSPHERE-2-OFFSET. Using default ephemeris /data/multi-mission/apt/Current/Mac/APT.app/Contents/MacOS/LispPrograms/casm/casmfiles/moss/mars.trh for MARS.Moss Window file /Users/aroman/Desktop/visit-planner/15595_6.wnd is missing. Assuming Schedulability everywhere. Please contact your PC if you need to obtain a target specific window file.The scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.Observations of Mars after global dust storm in summer 2018154169846700054.04601331751849(Tic-Visit
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)false20Using ephemeris for target 15595-04-MARS-EXOSPHERE-STIS-2ephemeris data for target 15595-04-MARS-EXOSPHERE-STIS-2 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 17.213 to 19.182. ephemeris interval: 18.181 to 20.183Could not find ephemeris /Users/dolonb/Desktop/visit-planner/15595_8.trh for target 15595-04-SKY-NEAR-MARS-2. Using default ephemeris /Applications/APT 26.0.3/APT.app/Contents/MacOS/LispPrograms/casm/casmfiles/moss/mars.trh for MARS.Moss Window file /Users/dolonb/Desktop/visit-planner/15595_8.wnd is missing. Assuming Schedulability everywhere. Please contact your PC if you need to obtain a target specific window file.The scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.Observations of Mars after global dust storm in summer 2018154171563900055.0(Tic-Visit
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)false20Using ephemeris for target 15595-53-MARS-EXOSPHERE-RERUNephemeris data for target 15595-53-MARS-EXOSPHERE-RERUN does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 18.175 to 19.305. ephemeris interval: 18.304 to 20.306Using ephemeris for target 15595-53-MARS-EXOSPHERE-OFFSET-RERUNephemeris data for target 15595-53-MARS-EXOSPHERE-OFFSET-RERUN does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 18.175 to 19.305. ephemeris interval: 18.304 to 20.306Using ephemeris for target 15595-53-SKY-BACKGROUND-RERUNephemeris data for target 15595-53-SKY-BACKGROUND-RERUN does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 18.175 to 19.305. ephemeris interval: 18.304 to 20.306The scheduling data was generated by CASM 26.2.CASM was run in Phase II mode./solaris/user1/aroman/work/hst/OP-cache/15595-v53.xml154423311100065.6559384815611(Tic-Visit
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