This is a resubmission due to a failed visit (01, now to be replaced with visit 51). See HOPR 91044.
These comments still apply 12/11/18405390608----- Attempting Submission 1 (Mon Jul 10 08:45:40 GMT 2017) -----
----- Attempting Submission 2 (Tue Aug 21 13:53:01 GMT 2018) -----
----- Attempting Submission 3 (Wed Dec 12 01:18:36 GMT 2018) -----Visit Planner Was Run.Monitoring an Internal Shock Collision in Action in 3C 2643C264 is a nearby radio galaxy with a prominent optical jet. Recent HST observations (May 2014) have revealed not only the fastest-ever superluminal speed (on kpc scales) of 7c for knot B, but also that knot B is in the very early stages of a collision with slow-moving downstream knot C (Meyer et al. 2015, Nature). This remarkable discovery represents the first strong evidence for the "internal shock" model for particle acceleration, a mechanism proposed to explain sources as diverse as gamma-ray bursts, microquasars, and jetted AGN. While a popular theoretical framework, such a collision has never actually been observed directly in any astrophysical object. Our recent HST imaging has captured the collision in its incipient stages, thus we have a unique opportunity to monitor a major shock collision as it unfolds. We propose 2 epochs of WFC3/UVIS (near-UV, B, and I band) imaging to monitor the optical-UV spectral energy distribution for the colliding knots and continue spatial proper motion measurements of the jet over the next 2-3 years. We also request 1 orbit of polarimetry in F606W with ACS/WFC in each epoch to monitor the polarization structure in the jet for changes as a result of the collision. The collision is expected to manifest in brightening and hardening of the optical spectrum and increasing polarization over the next several years, and our observations will allow us to evaluate the applicability, efficiency and physical characterization of the internal shock mechanism.Observations are of an optical jet approximately 2" long in the northeast direction, as part of a monitoring proposal for flaring behavior (this is the follow-up of an identical set of observations in Cycle 23). The field of view is dominated by the host galaxy, a nearby elliptical. The observations consist of two visits: the first is WFC3/UVIS imaging in three filters (F475W, F814W splitting the first orbit, F225W in the second orbit). The second visit is ACS/WFC polarimetry in F606W filter. Orient constraints are specified to avoid any risk of the central nucleus from producing diffraction spikes that run over the jet. Secondly, we request that the observations occur after Feb 2018 in order to evaluate the flux level of the jet with an even cadence (previous observations were in May 2014 and April 2016, so ideally these would occur in Spring/Summer of 2018).AGN/QUASARS6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYELLIPTICALJETNUCLEUSRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoYesF555WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoYesF555WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT1falsePOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX2falsePOS-TARGDITHER3.011LINEfalsefalse285.28ACS-WFC-DITHER-LINE3falseThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.We used a 3-point dithering pattern for the sets of F475W (3 exp) and F814W (3 exp) observations in the first epoch. We used a 4-point dithering pattern for the 4 F225W exposures in the second orbit. Orient constraints are specified to avoid any risk of the central nucleus from producing diffraction spikes that run over the jet. We request observations in late 2015 in order to evaluate if the flux from the jet is rapidly increasing (i.e. flaring). POS TARGS are also used to put the target somewhat closer to the readout corner to minimize CTE.1528452320000114.80736614397551(Tic-Visit
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)true20The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode./home/meyer/OP-cache/3c264_151091-v51.xmlThis is a resubmission of failed visit 01 (see HOPR 91044).
We used a 3-point dithering pattern for the sets of F475W (3 exp) and F814W (3 exp) observations in the first epoch. We used a 4-point dithering pattern for the 4 F225W exposures in the second orbit. Orient constraints are specified to avoid any risk of the central nucleus from producing diffraction spikes that run over the jet. We request observations in late 2015 in order to evaluate if the flux from the jet is rapidly increasing (i.e. flaring). POS TARGS are also used to put the target somewhat closer to the readout corner to minimize CTE.(Tic-Visit
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)true20The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.1 orbit of ACS polarization in F606W filter. The observations cover the three polarization angle filters, with two exposures each, using a 2-point dither pattern to improve image quality and mitigate cosmic ray artifacts. Orient constraints are specified to avoid any risk of the central nucleus from producing diffraction spikes that run over the jet. We request observations in late 2015 in order to evaluate if the flux from the jet is rapidly increasing (i.e. flaring).1521866806000161.5390750860505(Tic-Visit
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