POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.
Sensitive exposures should have an ETC run number provided.
Sensitive exposures should have an ETC run number provided.
POS TARG & PATTERN should be used carefully with ACS ramp or WFC3 quad filters as central wavelengths & transmission efficiencies vary within the apertures.This version includes the timing lnks for the overall sequence desired across all four programs in the Mars-CSS campaign (22 orbits total). We also converted two of our comet orbits to Mars SBC imaging to complement Clarke's program. A change request has been submitted for this. -- Max Mutchler
This is the final update from Jian-Yang Li on 9/29/2014. Thank you.
Updated comet ephemeris to JPL reference 85. 10/1/2014, Jian-Yang Li.-209842036----- Attempting Submission 1 (Mon Sep 08 02:39:48 GMT 2014) -----
----- Attempting Submission 2 (Sun Sep 21 20:05:46 GMT 2014) -----
----- Attempting Submission 3 (Mon Sep 29 21:31:45 GMT 2014) -----
----- Attempting Submission 4 (Wed Oct 01 13:27:33 GMT 2014) -----MOSSChandra and Hubble observations of Comet Siding Spring's Encounter with MarsComet Siding Spring's extremely close approach to Mars (within 138,000 km, or 1/3 the Earth-Moon distance) on 19 Oct 2014 offers us the first opportunity in the Chandra era to study the interaction between the solar wind, a comets extended atmosphere, and a planets exosphere. Chandra and Hubble will also be able to support the observations of the comet by the NASA and ESA Mars spacecraft as they study the comet during its close flyby. X-ray imagery, photometric lightcurves, and x-ray emission spectra obtained during the encounter will be compared to the Chandra comet database of 12 comets to determine the solar wind flux at Mars, the draping of the solar wind around the planet, and the input of comet gases into the Martian exosphere.On Oct 19 2014, circa 18:30 UT, dynamically new Oort Cloud comet C/2013 A1 (Siding Spring) will fly within 138,000 km of the planet Mars. This distance is so small (1/3 the mean Earth-Moon distance, and 10 times closer than any comet has approached the Earth in the modern spaceflight era) that Mars will be moving through the comet's outer atmosphere, or coma, carrying Mars, and its orbiting and ground based roving spacecraft fleet with it. In this way the Mars fleet will be participating in a close comet flyby. Both Mars and comets are known soft X-ray emitters, and the encounter will provide an opportunity for Chandra to observe a comet immersed in a planet's exosphere + draped magnetic field, and how a comet can affect a planet's exosphere. Coincident with our 19 Oct 2014 14:30 to 20 Oct 2014 05:30 UT Chandra measurements, we also request 10 orbits of HST time in order to accurately map out the comets neutral gas coma as it interacts with the solar wind to create the X-rays observed by Chandra. On our team is Dr Jian-Yang Li, PI of the HST program 13610 that has characterized the coma and tail of comet Siding Spring in Oct 2013 and Jan and Mar 2014. Observations of the Mars and Comet system will be feasible if we place Mars just outside the camera FOV. We require simultaneous HST observations because of the need for deep, continuous monitoring of the neutral gas around the comet and Mars, as we expect large changes in the comets coma structure as it flies through near-Mars space. The goal for these coordinated HST observations is to provide simultaneous measurement of the distribution of neutral gas species in the coma during the close encounter of C/Siding Spring with Mars. We plan to use the large FOV provided by the WFC3 camera. The V-band magnitude of Mars will be 0.9, while the total magnitude for C/Siding Spring will be 10.7. Despite the large brightness contrast between Mars and the comet, analysis of the scattered light from Mars shows that, as long as Mars is outside of the FOV by several hundred pixels (a few tens of arcsecond), the scattered light from Mars is sufficiently low and will not interfere with the observations of the cometary coma. This condition is easily satisfied with the 89 arcsec closest apparent angular separation between Mars and the comet as viewed from Earth. Lacking appropriate narrowband filters that are specifically designed to capture gas emission from comets, we will use the wideband Johnson B filter F438W to capture many strong gas emissions from several possible gas species in cometary coma (Feldman et al., 2004), and use a broadband R filter F775W to characterize the brightness distribution from dust coma for subtraction from B-band images. The subtraction also facilitates the removal of any possible low-level scattered light from Mars.
Working in concert with John Clarke's HST program 13795 we have converted two of our comet visits into copies of his ACS/SBC Mars imaging visits. In strategizing with all the HST teams involved in this observing campaign, we felt this would optimize the overall 22-orbit campaign. This change was made in cooperation with John Clarke, and a change request has been submitted.DefaultfalsefalsefalsefalsefalseAVAILABLESOLAR SYSTEMJPL orbit solution #85. Updated Oct-01, 2014.COMETComet C/2013 A1 (Siding Spring)TYPE=COMET,Q=1.398647410389588,E=1.000688626405008,I=129.0273584753412,O=300.9763462911545,W=2.442757978652319,T=25-OCT-2014:08:09:09,TTimeScale=TDB,EQUINOX=J2000,EPOCH=09-DEC-2013:00:00:00,EpochTimeScale=TDBEARTHSOLAR SYSTEMOffset Mars disc to corner of ACS/SBC field of view to image extended H Lyman alpha coronal emissionPLANETPlanet MarsSTD=MARSTYPE=POS_ANGLE,RAD=13,ANG=320,REF=NORTHUV emission line fluxes are given in the text.EARTH52.5/solaris/user1/aroman/work/OP-cache/13934-v11.xml(Tic-Visit
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