0Assigned ID: 827
----- Attempting Submission 1 (Fri Apr 11 21:08:03 GMT 2014) -----This replaces the earlier submission of the phase 2. Either set of observations would have been acceptable, but the current version updates the IR observations to be more efficient & easier to analyze.-1792621253----- Attempting Submission 1 (Sat Jul 19 07:15:48 GMT 2014) -----
----- Attempting Submission 2 (Mon Aug 11 13:00:59 GMT 2014) -----Solving the X-ray Origin Problem in Kiloparsec-Scale Relativistic Jets: Hubble Provides the Missing KeyWe propose infrared and optical imaging of four active galaxies with powerful kpc-scale jets, chosen based on existing radio, X-ray, and gamma-ray observations. The proposed observations present a significant opportunity to advance our understanding of both the kinetic energy carried by jets, and the particle accleration mechanisms that produce high-energy emission seen hundreds of kiloparsecs from the black hole. All four of the kpc-scale jets have been shown with Chandra observations to have very hard X-ray spectra which has lead to the prevailing interpretation that the X-rays are due to inverse-Compton upscattering of CMB photons (IC/CMB) by a jet which is still relativistic on kpc scales. However, very recent work by our group has shown that the gamma-ray flux implied by this mechanism is not apparent in over 5 years of gamma-ray monitoring with the Fermi telescope for several sources, leading us to rule out the IC/CMB mechanism for the nearby source 3C 273 (Meyer et al., 2014). In order to positively rule out the IC/CMB model in the four proposed targets, we require an accurate measurement of the synchrotron spectrum of the jet, in order to exactly predict the gamma-ray spectrum expected and interpret the existing upper limits. As we have shown, the presence of relativistic, synchrotron-emitting electrons necessitates that high-energy IC/CMB emission should be present at a level which depends solely on the speed of the jet, assuming equipartition magnetic fields. Thus, with the HST imaging we propose, we will be able to settle over a decade of ambiguity about the emission mechanism of the X-rays, and place strong limits on the bulk speed of these large-scale jets.We propose straightforward imaging observations of 4 jet targets in two instruments/bands: All four will be imaged with 1 orbit of WFC3/IR (F160W), as well as 2 orbits of ACS/WFC (F606W), except for the target 1745+624 which will be imaged with 4 orbits of ACS/WFC (F606W), due to a need for higher sensitivity. In the optical observations, roll constraints have been specified to avoid any risk of bleeding from the bright quasar cores or nearby bright stars from "over-running" the 3-8" jet extension from the core which is the actual science target. The proposed exposure times are optimized for detecting the faint jet emission and some mild saturation of the cores is anticipated. For the WFC3/IR observations, we have used a line-type dithering strategy (with roll constraints) to ensure that possible persistence in some pixels from exposure to the bright quasar cores does not land on the jet in subsequent exposures, and to minimize saturating individual pixels repeatedly. Note that we have used POS TARGs in addition to the pre-set pattern containers, both to fill out the remainder of the orbits and for sequential PATTERN containers, to ensure that the pointings continue along the same line without going 'backwards' for the above reasons.AGN/QUASARSDefaultfalsefalsefalsefalsefalseSUPPORTEDGALAXYJETQUASARRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.1745+624J2000J2000GALAXYJETQUASARRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.2209+080J2000J2000GALAXYJETQUASARRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.1323+655J2000J2000GALAXYJETQUASARRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.1603+001J2000J2000WFC3/IRImagingNoNoF160WACS/WFCImagingNoNoF606WWFC3/IRImagingNoNoF160WACS/WFCImagingNoNoF606WWFC3/IRImagingNoNoF160WACS/WFCImagingNoNoF606WWFC3/IRImagingNoNoF160WACS/WFCImagingNoNoF606WPOS-TARGDITHER0.605LINEfalsefalse341.788WFC3-IR-DITHER-LINE-3PT1falsePOS-TARGDITHER0.605LINEfalsefalse3221.788WFC3-IR-DITHER-LINE-3PT2falseThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./private/var/folders/b0/drp6b6xd035ffsllvk6c2zvr00050f/T/OPVisit7138105623615428826.xmlThe jet is at ~ 215 deg orientation to the optical point source at the nominal target location. ORIENT constraints for this source are necessary to avoid nearby saturated point sources from producing bleeding/trailing effects which might over-run the jet. In particular, the quasar 'core' associated with the jet we are trying to image is potentially variable, and relatively bright (Vmag ~19). Because it is exactly adjacent to the 3"-long jet, relatively wide avoidance zones were used (+/- 15 degrees). A bright star (17th mag) 20" away is avoided already by these constraints. Another 17th mag star at 12" distance (PA towards the jet is 326 - 342 deg) is also avoided by the given constraints.(Tic-Visit
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)true40The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./private/var/folders/b0/drp6b6xd035ffsllvk6c2zvr00050f/T/OPVisit8777355055323714487.xmlThe jet is located at PA ~ 180 deg relative to the bright point source at the nominal target location, with an extent of 8". ORIENT constraints are given to avoid any saturation bleeding/trailing from the core and from a bright (16th mag) star 15" from the target from over-running the jet region. The only other bright star (Vmag 14.5) in the vicinity is also avoided by these constraints.(Tic-Visit
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)true20The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./private/var/folders/b0/drp6b6xd035ffsllvk6c2zvr00050f/T/OPVisit8487216550252426779.xmlThe jet of this source is two-sided, with the dominant side (science target) directed to the southwest of the optical point source core that is the nominal target location. This jet goes through a 90 degree bend, so the ORIENT constraints are set to avoid any bleeding/saturation streaks from the core (17th mag) from over-running the jet region. There are no other bright stars in the vicinity.(Tic-Visit
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Of the jet components, we used the radio-to-X-ray spectral index of -1.1 (in F_lambda) to extrapolate an upper limit of the IR flux (most likely lower) expected from the brightest knot, which occurs at the end (terminal hotspot). The time-to-saturation was 17,000 seconds, so our 360 second observations should have no risk of saturation from any of the scientific targets. A dithering strategy has been used which avoids any persistence from bright sources from over-running the jet.(Tic-Visit
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