Small correction to text, and figure 1!1929774310Assigned ID: 129
----- Attempting Submission 1 (Wed Apr 09 21:27:36 GMT 2014) -----
HST Phase I Proposal 129 (Hines_67P.apt) successfully submitted.
----- Attempting Submission 2 (Wed Apr 09 22:03:04 GMT 2014) -----
HST Phase I Proposal 129 (Hines_67P.apt) successfully submitted.
----- Attempting Submission 3 (Thu Apr 10 21:29:03 GMT 2014) -----
HST Phase I Proposal 129 (Hines_67P.apt) successfully submitted.
----- Attempting Submission 4 (Thu Apr 10 21:34:28 GMT 2014) -----
HST Phase I Proposal 129 (Hines_67P.apt) successfully submitted.
----- Attempting Submission 5 (Fri Apr 11 19:01:21 GMT 2014) -----
HST Phase I Proposal 129 (Hines_67P.apt) successfully submitted.added links the same as the first set, and use of FGS3
hours not days! on link on v. 6509021415----- Attempting Submission 1 (Mon Jun 30 11:58:07 GMT 2014) -----
HST Phase II Proposal 13863 (Hines_67P.apt) successfully submitted.
----- Attempting Submission 2 (Fri Jul 04 10:30:04 GMT 2014) -----
HST Phase II Proposal 13863 (Hines_67P.apt) successfully submitted.
----- Attempting Submission 4 (Fri Jul 18 20:36:14 GMT 2014) -----
----- Attempting Submission 5 (Fri Jul 25 20:00:48 GMT 2014) -----
HST Phase II Proposal 13863 (13863.apt) successfully submitted.
----- Attempting Submission 6 (Fri Jul 25 20:11:35 GMT 2014) -----
HST Phase II Proposal 13863 (13863.apt) successfully submitted.
----- Attempting Submission 7 (Fri Jul 25 20:15:25 GMT 2014) -----
----- Attempting Submission 8 (Mon Jul 28 12:55:15 GMT 2014) -----
----- Attempting Submission 9 (Mon Jul 28 13:17:29 GMT 2014) -----
----- Attempting Submission 10 (Mon Aug 04 20:03:19 GMT 2014) -----
----- Attempting Submission 11 (Wed Aug 13 12:44:48 GMT 2014) -----
----- Attempting Submission 12 (Wed Sep 17 18:39:21 GMT 2014) -----
HST Phase II Proposal 13863 (13863.apt) successfully submitted.
----- Attempting Submission 13 (Wed Sep 17 19:13:33 GMT 2014) -----The errors come from the 8 internal orbits of subarray bias frames that have been inserted for
calibration purposes. These errors can be ignored.Imaging Polarimetry of the 67P/Churyumov-Gerasimenko with ACS: Supporting the Rosetta MissionWe propose ACS/WFC imaging polarimetry of Comet 67P/Churyumov-Gerasimenko (hereafter 67P), in support of the Rosetta mission, to place stringent constraints on dust particles in the coma. Our observations bracket the period when Rosetta operates closest to 67P, and will deploy the Philae lander. Fortunately, this occurs when the comet phase angle is well centered in the negative-polarization branch (12-15 degrees), enabling the different materials within the coma to be mapped using their polarization response, providing information on comet heterogeneity, and on the size, shape/structure, composition, or orientation of the particles. Our results will compare directly with in-situ measurements from Rosetta, placing strong constraints on material on small scales near and at the nucleus, and on larger scales within the coma. During the encounter, 67P will subtend only about 4-5", so ground-based observations would only provide one or two "polarimetric resolution elements" across the coma, at most. Laser AO systems can provide higher spatial resolution, but do not have visible wavelength polarimetry modes. In addition to our high spatial resolution requirement, this exciting period in the Rosetta mission coincides with the end of the visibility window from Earth, with 67P only visible for around 45 minutes between the end of astronomical twilight and reaching 2 airmasses in mid-November for ground-based telescopes. The necessary S/N could not be achieved by polarimeters on even the largest ground-based telescopes during this window. HST/ACS is the only asset capable of achieving our objectives during this once-in-a-lifetime opportunity.We use POLV polarizers. This will enable us to construct a broadband polarization image of the coma with a high S/N ~ 300. For ACS, all wavelengths < 0.6 um are potentially contaminated by molecular line emission, and strong CN bands exist at 0.92 um. Molecular emission will be essentially unpolarized, which artificially reduces the measured degree of polarization. While narrowband filters are ideal, their use is prohibitively expensive to obtain sufficient S/N for the comet at its distance and size on in August 2014. We therefore choose the F606W filter. We acknowledge that our results may suffer contamination from the molecular species CN, C2, and C3 that will dilute the polarization signal. However, at 3.5AU from the Sun, the contamination should not be a problem (it was not an issue for Comet ISON at similar distances: Hines et al. 2014), and near-contemporaneous ground-based spectroscopic monitoring (e.g., as coordinated by Co-I, Snodgrass) will provide accurate equivalent-width measurements of the contaminating emission that will then be used to correct the polarimetry . In addition, while the F775W would be less contaminated, the calibration of the filter is less accurate, and the exposure times would need to be about 40% longer to achieve similar S/N in the polarimetry.
The efficacy of ACS/WFC imaging polarimetry for extended sources has been demonstrated in general (e.g., Sparks et al. 2008), and in particular for comets with low, but significant polarization (Hines et al. 2014). The calibration observations of the F606W + visible polarizer combinations were obtained during the Cycle 12 ACS polarimetric calibration campaign (CAL 10055), and Hines has used these to recalibrate the system, showing that precise (p~0.3%) polarization measurements with an absolute accuracy of p%~0.3%, can be achieved with the system.
We expect the measured polarization of 67P to range from ~2-6%. Since polarization follows a Rice, not a Gaussian, distribution, we require a P/sigp > 4 per resolution element. We therefore need p~0.3%. For three perfect polarizers oriented at 60 degrees relative position angles (as in the ACS), the uncertainty in the degree of polarization P (which ranges from 0 for unpolarized light to 1 for fully polarized light) is approximately the inverse of the signal-to-noise per image. Sparks & Axon (1999) find [see equation in their paper - DCH], where S/Ni is the signal-to-noise of the ith image. Therefore, in order to achieve P/sigp > 4 for P ~2%, we require S/Ni > 268.
Using our successful observations of Comet ISON (Hines et al. 2014) as a validation of our S/N calculations, we estimate the total integration time needed to achieve S/N. Using the above V-band surface brightness, we estimate the exposure time for 2.0e-/DN gain, and a G2V spectrum. To achieve the required S/N, we may have to bin the data by up to 19x19 pixels (we will bin only until we reach the desired precision, S/N). This still yields sub-acrsecond spatial resolution, and cannot be done from the ground.
The results of our exposure time estimates are shown in Table 3. The last column shows our expected allocation need including guide star acquisition (8 minutes), and reacquisition (6 minutes), plus instrument overheads. We use CRSPLIT=2, and a two-position dither. We request a total of 21 orbits for this program.
CALIBRATION ORBITS: As per STScI policy, 8 internal orbits have been added to this proposal for the purpose of obtaining subarray bias frames that are contemporaneous with the science observations. These internal orbits will be charged to STScI's Cycle 22 ACS Calibration Program, not to GO 13863. The ACS Instrument Team at STScI is responsible for producing superbias reference files from the bias frames obtained in this GO proposal.SOLAR SYSTEMDefaultfalsefalsefalsefalsefalseSUPPORTEDSOLAR SYSTEMEphemeris from HORIZONS JPL#K084/16COMETCOMET-67P-CHURYUMOV-GERASIMENKO which is the primary target for Rosetta SpacecraftTYPE=COMET,Q=1.243119605049142,E=0.6410532328350245,I=7.040848762748019,O=50.15180617652601,W=12.773219225972,T=13-AUG-2015:00:01:52,TTimeScale=TDT,EQUINOX=J2000,EPOCH=03-MAY-2014:00:00:00,EpochTimeScale=TDT,A1=1.074213162065E-9,A2=1.064203027636E-10,A3=1.297521963716E-10EARTHACS/WFCImagingNoYesF606WACS/WFCImagingNoYesF606WPOS-TARGDITHER3.265LINE3.187falsetrue69.05420.67ACS-WFC-DITHER-BOX1falsePOS-TARGDITHER0.149LINEfalsefalse234.25ACS-WFC-DITHER-LINE2falseUsing ephemeris for target 13863-01-COMET-67P-CHURYUMOV-GERASIMENKOTiming link suitability includes constraints ([Group (01 A4) Within 14.0 days] [02 After 01 by 1.0 to 1.0 days] [03 After 01 by 2.0 to 2.1 days])The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.140834239600077.38473072452229(Tic-Visit
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