Target MARS3: 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.0Assigned ID: 251
----- Attempting Submission 1 (Thu Apr 04 19:51:48 GMT 2019) -----Not sure why I am getting this warning, but I hope it will be clarified if and when there is a PhaseII.
The warning message states it will go away when the proposal is reloaded.A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
A target acquisition should probably be performed before doing
spectroscopy or coronography with STIS or COS.
Sensitive exposures should have an ETC run number provided.Visit planning has been modified (finalized, hopefully). Need to figure out wavecal options and tackle ETC warning, if necessary.
Thank you - Majd
Added links to keep visit pairs within 24hrs
broke the different targets into seperate visits, and adjusted the exposure time as necessary
fixed links to include new visits
added wavecals to the end of the orbits
after gs acqs were lengthened, I set the visibility interval to 50min and auto-adjusted the exposures. About a cut of 2 minutes per orbit.-342377696----- Attempting Submission 1 (Sun Jul 21 15:06:44 GMT 2019) -----
HST Phase II Proposal 15976 (15976_PhaseII.apt) successfully submitted.
Receipt: # 15976-1
----- Attempting Submission 2 (Mon Jul 22 17:11:35 GMT 2019) -----
----- Attempting Submission 3 (Mon Jul 22 17:31:32 GMT 2019) -----
HST Phase II Proposal 15976 (15976.apt) successfully submitted.
Receipt: # 15976-3
----- Attempting Submission 4 (Mon Jul 22 18:03:03 GMT 2019) -----
HST Phase II Proposal 15976 (15976.apt) successfully submitted.
Receipt: # 15976-4
----- Attempting Submission 5 (Mon Jul 22 18:08:14 GMT 2019) -----
----- Attempting Submission 6 (Tue Jul 23 17:04:52 GMT 2019) -----
----- Attempting Submission 7 (Tue Jul 23 17:46:01 GMT 2019) -----
----- Attempting Submission 8 (Wed Oct 30 18:48:46 GMT 2019) -----please see updates to submission commentsConstraining Water Loss from MarsHow does water loss at Mars vary with time? Early theory predicted a slow and steady loss, where surface water molecules are dissociated by sunlight into atoms that take dozens of years to diffuse to the upper atmosphere and escape to space. Recent observations showed water escape rates to vary by a factor of 10 with martian seasons, consistent with variations near the surface and lower atmosphere of Mars - the regions that provide water to the upper atmosphere by global turbulent mixing during perihelion. However, key water constituents in the upper atmosphere, hydrogen (H) and its heavier isotope deuterium (D), vary on timescales that differ from the lower atmosphere indicating a surface-to-space water cycle that does not reconcile with theory. Upper atmospheric H and D comprise the escaping components of planetary water. The ratio and variability of their abundance, D/H, is a key metric for determining water loss. Understanding water loss requires establishing a full seasonal timeline of D and H densities. A Mars orbiter can presently make such measurements near perihelion but does not have the sensitivity to measure D near aphelion, thereby leaving a glaring gap in our ability to establish seasonal variations of water escape. Here we propose to observe D at Mars with HST STIS at times when no other instrument can. The results will address a two-part science investigation: to determine the variability of D/H (1) seasonally, and (2) with solar activity using new and archived HST data. The observations will be conducted in parallel with lower (H2O, HDO) and upper (D, H) atmospheric water measurements from orbiting spacecraft. This proposal supports the HST UV initiative.This program requires high-resolution observations of Mars to resolve the solar Lyman-alpha photons for D and H that are separated by 0.33 Angstrom. The HST STIS E140H echelle spectrograph has a resolution of 0.057 Angstrom using the 0.5 Angstrom aperture and is sufficient to separate the D and H lines. We propose to utilize the TIMETAG configuration with the 52x0.5 arcsec aperture for the STIS observations. The long-aperture mode that provides a higher count rate for the extended emission region, has been well demonstrated in observations of Mars, Jupiter and the interplanetary hydrogen, and can obtain spectra across the entire martian disc and limb. The HST STIS observations requested can be conducted at any roll angle since we can account for the observing geometry when modeling the lines of sight to Mars.
Both Mars as well Earth's corona emit resonantly scattered solar Lyman-alpha. Past observations have shown the background geocorona emission to be highly variable and would necessitate consistent measurement. Therefore, a sky observation near Mars, during the same visit is needed to accurately subtract the Lyman-alpha emissions of the background geocorona and interplanetary hydrogen. This measurement will require pointing the line of sight at a portion of the sky a few arcmin away from Mars.
This program conforms to safe observing of Mars (where the instrument line of sight is more than 55 degrees from the Sun). Specifically, between March and June 2020. A minimum of three data points of HST-observed D Lyman-alpha emissions are needed during the off-perihelion range in order to disambiguate a linear vs polynomial trend in D variability and to assess sudden vs gradual variations. Visits are therefore requested at Ls of 160, 185, and 210 degrees in order to obtain an adequate slope of the enhancement of D emission brightness and water escape rate as the martian seasons change. A total of 4 orbits are requested when Mars is at Ls of 160, three of which are pointed at the disk of Mars, and one of which points at the sky near Mars to account for sky background during image reduction and analysis. A similar sequence is requested for when Mars is at Ls of 185. Finally, one sequence is requested when Mars is at Ls 210 with 3 orbits requested. Two for Mars and one for the sky near Mars. The orbits with exposures targeting the near-Mars sky background, a pointing offset of ~3 arcmin away from the Mars disk is requested, to gather a background telluric and interplanetary Lyman-alpha signal. The remaining orbits will point at Mars. The STIS E140H 0.5 arcsec aperture gives 5 counts/sec/kR integrating across the 52 arcsec detector. Assuming 2400 second integration per orbit, we would get 300 counts from a 25 Rayleigh emission (expected near aphelion). Three orbits are requested for the first epochs (correponding to Ls 160 and 185 degrees) in order to obtain an adequate signal to noise. Only two orbits would be required for the third visit (requested at 210 degrees Ls) since the D emission is expected to be brighter at that time. Observations from the three visits would be analyzed to calculate the D/H ratio and water escape rate over the present Mars year as the orbital position of Mars progresses toward perihelion. The observations from the three visits will uniquely convey how the properties of water change with season in the present epoch.PI, Majd Mayyasi is a member of the MAVEN Science Team and is involved with both the MAVEN UV echelle spectrograph as well as the Neutral Gas and Mass Spectrometer instruments. Dr. Mayyasi is also a recent member of the TGO ACS team and an active collaborator with the TGO NOMAD team. These TGO instruments are the two IR spectrometers used to measure lower atmospheric HDO/H2O. Dr. Mayyasi is keeper of a Mars atmospheric model that will be used to produce D and H density profiles and water escape rates. As co-investigator of past funded HST programs, Dr. Mayyasi is experienced with HST STIS data reduction. Her expertise with the MAVEN data and TGO collaborations provide the capabilities of completing the comparisons required after the HST data analysis is completed. Dr. Mayyasi will oversee the completion of all the tasks required for the science investigation and will be responsible for reporting requirements.
Co-Investigators Jean-Yves Chaufray and Dolon Bhattacharyya are keepers of radiative transfer models. These models have been validated with observations from HST as well as other spacecraft and will be used with the proposed HST observations to determine the H and D densities at the exobase (~200 km). Dr. Mayyasi would use the results from the models to produce upper atmospheric profiles of D, H, D/H as well as produce water escape rates.
Co-Investigator John Clarke is an expert with multiple instruments on HST and is a lead investigator on the MAVEN echelle channel. His contribution will be to provide advice on the HST data analysis and to provide feedback as needed.
Co-Investigators Geronimo Villanueva and Frack Montmessin are senior scientists involved with the TGO mission two IR instruments, NOMAD and ACS, respectively. Their involvement would be to provide feedback to TGO observations synergies and comparisons at altitudes where the upper and lower atmospheric boundaries overlap. This is to maximize utilization of the results of this investigation to the broader community.
None of the investigators are funded by MAVEN to work on the HST tasks described here. Should this proposal be selected, the budget would include efforts that are explicit to HST data analysis and tasks related to this proposal investigations.Solar SystemSolar System6falsefalsetruefalsefalsefalsefalseAVAILABLESOLAR SYSTEMYESPLANETPlanet MARSSTD=MARSEARTHSOLAR SYSTEMYESPLANETPlanet MARSSTD=MARSTYPE=POS_ANGLE,RAD=300,ANG=0,REF=NORTHNOT OCC OF MARS1-LS160-BCKSKY BY MARS FROM EARTH,
SEP OF MARS1-LS160-BCKSKY MARS FROM EARTH GT 10"EARTHSOLAR SYSTEMYESPLANETPlanet MARSSTD=MARSEARTHSOLAR SYSTEMYESPLANETPlanet MARSSTD=MARSTYPE=POS_ANGLE,RAD=300,ANG=0,REF=NORTHNOT OCC OF MARS2-LS185-BCKSKY BY MARS FROM EARTH,
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SEP OF MARS3-LS210-BCKSKY MARS FROM EARTH GT 10"EARTHSTIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1234Timing link suitability includes constraints ([Group (01 02 03) Within 1.0 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode./private/var/folders/q9/0jb3sqc10kx2dw3wnl21b_dw000702/T/OPVisit16487649820636032898.xml50(Tic-Visit
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