fix the target name and the link in APT 19.4 ----- Attempting Submission 4 (Sat Jan 14 17:56:57 GMT 2012) ----- ----- Attempting Submission 5 (Sat Jan 14 20:17:35 GMT 2012) ----- This is a rush because replanning is needed this week. We propose a 10-orbit program to observe any newly discovered bright comet as a non-disruptive Target of Opportunity during cycle 19. For a comet whose water production rate meets our basic ToO selection criterion, Hubble observations can be used to measure abundances of three highly volatile species (CO, CO2, and S2), providing critical information on the origin and evolution of the comet's nucleus. If the comet additionally has geocentric and heliocentric radial velocities in a favorable range, our Hubble observations will measure atomic deuterium emission, from which we can derive the D/H ratio for comparison to the values measured in other comets and Earth's water. The D/H ratio in cometary water is a key indicator of the role played by comets in the delivery of volatiles to the terrestrial planets. It has been 7 years since a bright comet has been available for Hubble observations, and the statistics suggest we are overdue for another opportunity.

We use our considerable experience observing comets with HST over two decades to define the optimal spectroscopic configurations for our program. We request 2 orbits using STIS/G140L and the 0.2" slit to measure CO 4PG emissions with a spectral resolution of ~5 A. This will allow us to probe the CO abundance to ~0.3% (SNR=3) for the minimal comet. If the abundance is higher, or the comet has a larger production rate, the long slit allows a determination of the source of the CO (nucleus vs extended) from the spatial profile. We request 1 additional orbit using COS/G160M, reaching down to an abundance of ~0.1% for the minimal ToO but with no spatial information on the emission, to measure the CO 4PG emissions with a spectral resolution of ≤0.5 A to determine the rotational excitation of the CO. If the comet is more active than the minimal ToO, or if the CO abundance is relatively high, the 3 orbits will provide information on any temporal variation in Q(CO), which provides a test of chemical heterogeneity within the nucleus. We request 3 orbits using STIS/G230L with the 0.2" slit to measure CO Cameron, CS, S2, and OH emissions at ~13 A resolution. Although the CO Cameron bands should be detectable with SNR≈6 in 1 orbit for our minimal comet and a nominal CO2 abundance (~5%), 3 orbits would permit a more robust detection (SNR≈10; Fig 3 shows an example of a 3-orbit sum for 153P/I-Z, which exceeded the ToO criterion by ~3.2×). Furthermore, if the comet is bright enough, measurements of CO Cameron emission in multiple orbits will determine whether the CO2 abundance varies with time, as it did rather dramatically (by a factor of ~2) during the EPOXI flyby of 103P/Hartley. For the observations of D (assuming the comet satisfies the requirements discussed in the next section), we will use STIS/E140H with the 0.2" × 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" × 0.2" slit. We request 3 orbits to obtain a secure D/H detection, even for our minimal comet (see Fig 4; C/NEAT exceeded our ToO selection criterion by 1.9×). Finally, we request a 1 orbit observation using E140H offset by a large distance from the nucleus, so that we can measure the H Ly-α 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. We can also compare Q(H2O) derived from this offset measurement to the values derived from the other orbits using OH emission. In summary, we request a total of 10 orbits to accomplish all the objectives of our program. The *desired* cadence is to have 10 consecutive orbits, if possible, in the following order: V01 (G230L), V02 (E140H), V03 (G140L), V04 (COS/G160M), V05 (G230L), V06 (E140H), V07 (G140L), V08 (E140H), V09 (G230L), V10 (E140H-OFFSET). If 10 consecutive orbits aren't available, we'll make do with what we can get. SOLAR SYSTEM 12 false 0.0 0.0 false false false false SUPPORTED SOLAR SYSTEM COMET Bright-Comet TYPE=COMET,Q=1.550538823121793,E=1.001060180395493,I=106.1774779466713,O=325.9980001854605,W=90.74781959207823,T=23-DEC-2011:04:15:39,TTimeScale=TDB,EQUINOX=J2000,EPOCH=15-JAN-2012,EpochTimeScale=TDB EARTH SOLAR SYSTEM COMET Comet-Garradd-Offset TYPE=COMET,Q=1.550538823121793,E=1.001060180395493,I=106.1774779466713,O=325.9980001854605,W=90.74781959207823,T=23-DEC-2011:04:15:39,TTimeScale=TDB,EQUINOX=J2000,EPOCH=15-JAN-2012,EpochTimeScale=TDB TYPE=POS_ANGLE,RAD=1500,ANG=0,REF=SUN EARTH SOLAR SYSTEM COMET COMET TYPE=COMET,Q=1.5505372,E=1.0010494,I=106.17749,O=325.99769,W=90.74772,T=23-DEC-2011:16:15:53,TTimeScale=TDB,EQUINOX=J2000,EPOCH=25-DEC-2011,EpochTimeScale=TDB EARTH SOLAR SYSTEM COMET COMET TYPE=COMET,Q=1.5505372,E=1.0010494,I=106.17749,O=325.99769,W=90.74772,T=23-DEC-2011:16:15:53,TTimeScale=TDB,EQUINOX=J2000,EPOCH=25-DEC-2011,EpochTimeScale=TDB TYPE=POS_ANGLE,RAD=1500,ANG=0,REF=SUN EARTH COS/FUV Spectroscopic No No G160M 1589 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No E140H 1234 STIS/FUV-MAMA Spectroscopic No No E140H 1234 Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06 07 08 09 10) within 2.0 days]) The scheduling data was generated by CASM 19.3. 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