0Assigned ID: 3456
----- Attempting Submission 1 (Fri Mar 25 19:38:57 GMT 2022) -----The number of orbits used exceeds the number allocatedThis is a resubmission due to a failed guide star acquisition in visit 07 which affected 1 orbit. HOPR request 92658 was approved on 13 October. I have slightly relaxed the orient constraints to make the visit more scheduleable since the one orbit we did obtain shows the core is not currently producing large PSF spikes.-878997047----- Attempting Submission 1 (Thu Jul 14 12:14:26 GMT 2022) -----
HST Phase II Proposal 17201 successfully submitted.
Receipt: # 17201-1
----- Attempting Submission 2 (Thu Jul 14 20:18:20 GMT 2022) -----
----- Attempting Submission 3 (Sun Sep 25 23:43:02 GMT 2022) -----
----- Attempting Submission 4 (Tue Oct 24 10:58:27 GMT 2023) -----The excess orbit is expected and due to the HOPR-approved repeat orbit.Determining the High-Energy Emission Mechanism in Extragalactic Jets with HSTBipolar jets of relativistic plasma are a well-known phenomenon associated with active galaxies, which are seen to emit high-energy radiation (optical through X-ray) on very large (kpc-Mpc) scales, requiring in-situ particle acceleration by an unknown mechanism. While the radio emission in these large-scale jets is understood to be synchrotron in origin, recent observations with HST, ALMA, and Chandra have revealed a second mysterious component at higher energies. While some optical jets have a very soft spectrum associated with the tail of the radio synchrotron component, a handful of sources have a favorable alignment such that the optical emission is very hard, indicating that it arises from the second component associated with the anomalous X-ray emission. We propose IR, optical, and UV observations of the 3 extragalactic jets known to have a very hard optical spectral index, in order to precisely measure the full IR-UV spectral shape of this rising component. The two main alternatives for the origin of the high-energy component, synchrotron and inverse Compton emission, predict different spectral slopes in the optical/UV, and these observations will allow us to conclusively determine which of these mechanisms is consistent with the data. Distinguishing the emission mechanism is critical -- the two alternatives are vastly different in terms of physical properties and implied jet powers, by orders of magnitude.Here are requested near-IR, optical, and UV observations of 3 AGN jets previously detected in the optical. In all cases the science target is the faint jet extending out on tens of arcsecond scales from a central bright 'core' which appears star-like (V-mag ~16-18). The central core is variable, so there is some concern that diffraction spikes could interfere with imaging the jet. Some roll constraints are specified to avoid this. Minor saturation of the core is not an issue since it is not the science target.E. Meyer is an expert on multi-wavelength imaging of jets and has extensive experience with using HST (as well as many other observatories from radio to gamma-rays) to observe jets both for continuum and polarization emission and with precision astrometry for tracking proper motions. W. Sparks, E. Perlman, and M. Chiaberge are also experts in observing with HST and in jet observations in particular. K. Reddy Solipuram is an expert in radio and X-ray observations of jets, with a particular expertise in observations of jets with Chandra. M. Georganopoulos is an expert in both numerical and analytical work on jet theory.Supermassive Black Holes and Active Galaxies6falsefalsetruefalsefalsefalsefalsetruePRIMARY160trueSUPPORTEDGALAXYJETKNOTNUCLEUSQUASARRADIO GALAXYYESJ2000J2000GALAXYJETKNOTNUCLEUSQUASARRADIO GALAXYYESJ2000J2000GALAXYJETKNOTNUCLEUSQUASARRADIO GALAXYYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/IRImagingNoNoF110WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF336WPOS-TARGDITHER0.605LINEfalsefalse341.788WFC3-IR-DITHER-LINE-3PT1falsePOS-TARGDITHER0.145LINEfalsefalse246.84WFC3-UVIS-DITHER-LINE2falseThe scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.PKS 1136-135 is a bright quasar hosting a faint arcseconds-scale optical jet previously imaged at optical wavelengths with HST. The flux ratio between the bright core and the faint jet knots is approximately 2000:1, which complicates the observing strategy. We have opted to place the target near one of the readouts to lessen CTE and therefore do not use the full recommended FLASH level. This is because the poisson noise from the FLASH significantly degrades the sensitivity of the observations to the faint extended jet knots. NOTE: this visit contains 2/4 total orbits allocated to this target in the F22W filter to increase schedulability.1689653973000125.0(Tic-Visit
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)true20PKS 1136-135 is a bright quasar hosting a faint arcseconds-scale optical jet previously imaged at optical wavelengths with HST. The flux ratio between the bright core and the faint jet knots is approximately 2000:1, which complicates the observing strategy. We have opted to place the target near one of the readouts to lessen CTE and therefore do not use the full recommended FLASH level. This is because the poisson noise from the FLASH significantly degrades the sensitivity of the observations to the faint extended jet knots. NOTE: this visit contains 2/4 total orbits allocated to this target in the F22W filter to increase schedulability.1702823385000295.0(Tic-Visit
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)true20PKS 1136-135 is a bright quasar hosting a faint arcseconds-scale optical jet previously imaged at optical wavelengths with HST. The flux ratio between the bright core and the faint jet knots is approximately 2000:1, which complicates the observing strategy. We have opted to place the target near one of the readouts to lessen CTE and therefore do not use the full recommended FLASH level. This is because the poisson noise from the FLASH significantly degrades the sensitivity of the observations to the faint extended jet knots. NOTE: this visit contains 2/4 total orbits allocated to this target in the F22W filter to increase schedulability.1690247277000122.77761224163743(Tic-Visit
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)true20The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.PKS 1136-135 is a bright quasar hosting a faint arcseconds-scale optical jet previously imaged at optical wavelengths with HST. In the IR, the AGN core is expected to be very bright, ~ 8e-4 Jy at 1.2 microns. For this reason relatively short exposures are needed. Some low-level self-persistence may be present but should be manageable.1702834781000295.0(Tic-Visit
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)true20PKS 2209+080 is a moderately bright quasar hosting a prominant optical/IR jet discovered by HST. ORIENT constraints have been specified in the case the (variable) core brightens and produces significant diffraction spikes, to avoid these running over the fainter jet knots which extend from the bright central AGN on a ~ 10" scale.1683323425000255.73316200111714(Tic-Visit
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)true10PKS 2209+080 is a moderately bright quasar hosting a prominant optical/IR jet discovered by HST. ORIENT constraints have been specified in the case the (variable) core brightens and produces significant diffraction spikes, to avoid these running over the fainter jet knots which extend from the bright central AGN on a ~ 10" scale. Further constraints were introduced to avoid the same from a bright source to the SW.1683066655000252.0(Tic-Visit
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