0 Assigned ID: 809 ----- Attempting Submission 1 (Fri Apr 10 20:52:52 GMT 2015) ----- HST Phase I Proposal 809 (phase1-Bodewits.apt) successfully submitted. Receipt: # 809-1 ----- Attempting Submission 2 (Fri Apr 10 22:26:57 GMT 2015) ----- HST Phase I Proposal 809 (phase1-Bodewits.apt) successfully submitted. Receipt: # 809-2 ----- Attempting Submission 3 (Fri Apr 10 22:32:09 GMT 2015) ----- HST Phase I Proposal 809 (phase1-Bodewits.apt) successfully submitted. Receipt: # 809-3 ----- Attempting Submission 4 (Fri Apr 10 23:39:24 GMT 2015) ----- HST Phase I Proposal 809 (phase1-Bodewits.apt) successfully submitted. Receipt: # 809-4 ----- Attempting Submission 5 (Fri Apr 10 23:49:04 GMT 2015) ----- HST Phase I Proposal 809 (phase1-Bodewits.apt) successfully submitted. Receipt: # 809-5 ----- Attempting Submission 6 (Fri Apr 10 23:52:57 GMT 2015) ----- HST Phase I Proposal 809 (phase1-Bodewits.apt) successfully submitted. Receipt: # 809-6 A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. change to correct single guide star scenario -1600762771 ----- Attempting Submission 1 (Thu Jul 23 15:23:25 GMT 2015) ----- HST Phase II Proposal 14257 (Bodewits v3.apt) successfully submitted. Receipt: # 14257-1 ----- Attempting Submission 3 (Fri Nov 27 13:06:25 GMT 2015) ----- HST Phase II Proposal 14257 (Bodewits APT v5.apt) successfully submitted. Receipt: # 14257-3 ----- Attempting Submission 4 (Mon Nov 30 18:31:42 GMT 2015) ----- ----- Attempting Submission 5 (Mon Nov 30 19:07:10 GMT 2015) ----- ----- Attempting Submission 8 (Wed Apr 06 16:14:41 GMT 2016) ----- ----- Attempting Submission 10 (Wed May 18 15:34:11 GMT 2016) ----- HST Phase II Proposal 14257 (Bodewits APT v8 prep X1.apt) successfully submitted. Receipt: # 14257-10 ----- Attempting Submission 11 (Wed May 18 18:38:35 GMT 2016) ----- HST Phase II Proposal 14257 (Bodewits APT v8 prep X1.apt) successfully submitted. Receipt: # 14257-11 ----- Attempting Submission 12 (Wed May 18 19:20:38 GMT 2016) ----- ----- Attempting Submission 13 (Thu May 19 13:13:26 GMT 2016) ----- HST Phase II Proposal 14257 (14257.apt) successfully submitted. Receipt: # 14257-13 ----- Attempting Submission 14 (Thu May 19 13:30:00 GMT 2016) ----- HST Phase II Proposal 14257 (14257.apt) successfully submitted. Receipt: # 14257-14 ----- Attempting Submission 15 (Thu May 19 13:43:08 GMT 2016) ----- HST Phase II Proposal 14257 (14257.apt) successfully submitted. Receipt: # 14257-15 ----- Attempting Submission 16 (Thu May 19 13:49:25 GMT 2016) ----- HST Phase II Proposal 14257 (14257.apt) successfully submitted. Receipt: # 14257-16 ----- Attempting Submission 17 (Thu May 19 14:47:58 GMT 2016) ----- HST Phase II Proposal 14257 (14257.apt) successfully submitted. Receipt: # 14257-17 ----- Attempting Submission 18 (Thu May 19 15:05:21 GMT 2016) ----- HST Phase II Proposal 14257 (14257.apt) successfully submitted. Receipt: # 14257-18 ----- Attempting Submission 19 (Thu May 19 15:51:08 GMT 2016) ----- The APT cannot process the off-set pointing of comet 1. Far UV spectroscopic measurements of the deuterium abundance of comets We propose to use STIS Echelle spectroscopy to measure the deuterium to hydrogen ratio in two ToO comets to investigate the origin of their water ice. The deuterium abundance of water in comets preserves information about the formation conditions of our solar system, while also constraining the possible contribution of cometary water to Earth's oceans. The D/H values in JF comets and the ice ratios (CO/CO2/H2O) in both Jupiter Family and Oort Cloud comets call into question the details of the dynamical processes for populating the modern reservoirs for these two dynamical classes. However, currently too few D/H ratios have been measured in comets to allow for a meaningful interpretation. With a dedicated observing campaign we will measure the ratio between Ly-alpha emission from deuterium and hydrogen atoms from two different comets. We have defined strict conditions that ensure the quality of our measurement which we will use to trigger our ToO request. HST is essential for these observations as it is the only telescope that has the spectroscopic capabilities in the Far ultraviolet that is needed for these measurements. We plan to observe two Target of Opportunity comets, each for 5 orbits (totaling 10 orbits). These visits both consist of the following observations: - 4 orbits with STIS/FUV MAMA using the E140M grating, centered on the nucleus to measure the D/H ratio - 1 orbit with the same set up, but pointing off the nucleus where the comet's Ly-a emission is optically thin. We have identified two potential targets (C/2013 US10 Catalina and C/2013 X1 Panstarrs), but these comets are currently still far from the Sun and the extrapolation of their brightness are not yet reliable. Additionally, at least one or two bright new comets are discovered every year, and a better target might present itself. We therefore request these observations in the Target of Opportunity category. We have combined archival observations by HST with ETC estimates to provide realistic estimates for D/H measurements and to optimize our observing strategy. Comet C/2001 Q4 (NEAT) was observed with HST/STIS between April 23rd to 27th, 2004. To get an estimate of the brightness of the DI line, we scale the measured flux of comet NEAT by the heliocentric distance r, geocentric distance D, and its water production Q (ignoring the Swings effect on the fluorescent efficiency of the Ly-a line as we will only observe at dD > 20 km/s), and the same D/H ratio as to comet NEAT. For each comet, we request a total of 5 consecutive orbits, in all of which we use STIS' E140M grating with the 0.2" x 6" slit. This slit was used successfully to detect D in C/NEAT and provides a five-fold improvement in sensitivity compared to the standard 0.2" x 0.2" slit. Four of these orbits should be centered at the comet's nucleus. We request that one orbit is offset by a large distance from the nucleus, so that we can measure the H Ly- emission in a region of the coma where it is optically thin. From these data we can derive a highly reliable H production rate, which is needed for the D/H ratio. This offset should be toward the Sun along the comet-Sun axis to have the minimum column from the Sun to the comet. After each spectroscopic observation, we will acquire a short STIS/CCD exposure to allow us to determine the exact position in the coma with respect to the nucleus. We will use the F28x50LP filter or the F28x50OII if predicted count rates of the comet are too high. Observing conditions are constrained by the combination of optimum brightness and a relative geocentric velocity large enough to Doppler shift the comet's line away from the telluric Ly-a, dD > 20 km/s. We have identified two potential targets and have worked out the observing details for those observations, but will monitor their development to trigger our TOOS. Both comets' geocentric velocity is large enough so that the lower resolution E140M grating (R = 45,800) can be used to separate the telluric and cometary line. Should one of the targets be observable only during a smaller geocentric velocity, we will consider using the E140H grating instead. A. C/2013 US10 (Catalina) The current prediction is C/2013 US10 is best oberved between Dec 15-31, 2015. Using mv 5, Q_gas~3x10^29/s, r= 1.0 AU, D=1.25 AU, the STIS ETC predicts an excellent SNR of 12 for the DI Ly-a line using the E140M grating. At this distance and production rate, the 5th orbit should have an offset of 100 arcsec from the nucleus towards the Sun. B. C/2013 X1 (Panstarrs) Observing conditions for C/2013 X1 would be best between May 11 - June 11, 2016. Using mv 6.7, Q_gas~8x10^28/s, r= 1.5 AU, D=0.74 AU, we calculate a FoM of 0.14 and a flux of 2.1 x 10-15 erg/s/cm2. For this scenario, the ETC yields a SNR of 5. At this distance and production rate, the 5th orbit should have an offset of 45 arcsec from the nucleus towards the Sun. Solar System 12 false true false false false false SUPPORTED SOLAR SYSTEM YES Orbital elements reference: JPL #54 Predicted optimal observing time Dec 15-31, 2015 COMET Comet C/2013 US10 TYPE=COMET,Q=.8229686842714407,E=1.000384580127557,I=148.8754312250078 ,O=186.1395352627515 ,W=340.3513189554529 ,T=15-NOV-2015:17:00:00,TTimeScale=TDB,EQUINOX=J2000,EPOCH=02-NOV-2014,EpochTimeScale=TDB EARTH SOLAR SYSTEM YES Orbital elements reference: JPL #54 Predicted optimal observing time Dec 15-31, 2015 COMET Comet C/2013 US10 TYPE=COMET,Q=.8229686842714407,E=1.000384580127557,I=148.8754312250078,O=186.1395352627515,W=340.3513189554529 ,T=15-NOV-2015:17:00:00,TTimeScale=TDB,EQUINOX=J2000,EPOCH=02-NOV-2014,EpochTimeScale=TDB TYPE=POS_ANGLE,RAD=350,ANG=0,REF=SUN EARTH SOLAR SYSTEM YES Orbital elements reference: JPL #104 Observations June 10-15 2016 COMET Comet C/2013 X1 TYPE=COMET,Q=1.314353796433672,E=1.00101952188355,I=163.2298012978591,O=130.9600582567145,W=164.4482176452008,T=20-APR-2016:17:06:48,TTimeScale=UTC,EQUINOX=J2000,EPOCH=12-MAY-2016:00:00:00,EpochTimeScale=TDB,A1=5.910011291504E-8,A2=1.104533314705E-8,A3=1.639675974846E-8 EARTH SOLAR SYSTEM YES Orbital elements reference: JPL #104 Observations June 10-15 2016 COMET Comet C/2013 X1 TYPE=COMET,Q=1.314353796433672,E=1.00101952188355,I=163.2298012978591,O=130.9600582567145,W=164.4482176452008,T=20-APR-2016:17:06:48,TTimeScale=UTC,EQUINOX=J2000,EPOCH=12-MAY-2016:00:00:00,EpochTimeScale=TDB,A1=5.910011291504E-8,A2=1.104533314705E-8,A3=1.639675974846E-8 TYPE=POS_ANGLE,RAD=45,ANG=0,REF=SUN EARTH STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 Timing link suitability includes constraints ([35 After 34 by at most 0.1 days]) The scheduling data was generated by CASM 23.2. 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