0 Assigned ID: 605 ----- Attempting Submission 1 (Fri Apr 11 17:27:33 GMT 2014) ----- HST Phase I Proposal 605 (hst_m87_phase1.apg.apt) successfully submitted. ----- Attempting Submission 2 (Fri Apr 11 19:42:37 GMT 2014) ----- 0 The Real Impact of Extragalactic Jets on Their Environments: Measuring the Advance Speed of Hotspots with HST We propose moderately deep imaging of two nearby radio galaxies, M87 and Pictor A, in which the terminal shock of the jet as it impacts the IGM (aka 'hotspot') has previously been imaged in the optical with HST. The primary goal of this program is to leverage the 20 year imaging baselines afforded by Hubble archival data and state-of-the-art precision astrometry in order to measure, for the first time, the proper motions of a terminal shock/hotspot. This is the most direct method of constraining the velocity of the working surface, and when combined with existing multi-wavelength data, yields an estimate of the momentum carried by the jet, an important, but difficult-to-measure physical characteristic necessary for understanding the impact of extragalactic jets on their hosts and environments. In addition, the proposed imaging will allow us to study the inner kpc-scale jets of M87 and Pictor A, as well as the counter-jet and counter-hotspot of Pictor A. This proposal is for two known radio/optical jets. For Pictor A, the size of the source (7.6 arcminutes between terminal hotspots) will require two pointings to cover the entire extent, focused on covering either the eastern or western hotspot, with the jet falling on the diagonal of the ACS/WFC detector so that the jet and core (host galaxy) are also capture in all images. Each orbit is partitioned into 4 exposures of ~ 600 seconds each. We utilized an 8-point dithering strategy with a shift to cover the chip gap. Please note that in order to maximize the time when HST could observe this source given our ORIENT constraints, we used a WFCCENTER pointing which is midway between the core and the hotspot, the latter being the main science target. The finding charts do not thus show the hotspot because of the size of the source. The primary scientific target of the M87 observations is the counter-jet hotspot, 25" from the core which is centered in a giant elliptical host galaxy, though the main optical jet will also be captured in the planned exposures. The four orbits for M87 have been partitioned into 20 exposures of 408-446 seconds, with the exposure time chosen to minimize saturation of the core/HST-1 regions of the jet (a secondary scientific target). A repeated 5-point dithering pattern has been utilized, with a shift to cover the chip gap. Note: We are aware that another GO program, 13759 (PI J. Madrid) will also observe M87 during Cycle 22. The two programs have different science goals (13759 is specifically focused on jet variability), and most critically, the planned STIS observations of that proposal (GO-13759) will not cover the M87 southeast hotspot, which is the primary scientific target in this proposal. In addition, the goal of this project is to measure proper motions, so these observations are not duplicates of previous existing exposures, since the goal is to measure changes over time. AGN/QUASARS Default false false false false false SUPPORTED GALAXY JET KNOT QUASAR RADIO GALAXY The host galaxy is at 05h19m49.7s -45d46m44s, with an optical magnitude of 16.45. The Western hotspot is 4.1 arcminutes to the west-northwest with a magnitude of 18.3. J2000 J2000 GALAXY JET KNOT QUASAR RADIO GALAXY The host galaxy is at 05h19m49.7s -45d46m44s, with an optical magnitude of 16.45. The eastern (radio) hotspot is 3.5 arcminutes to the east-southeast, and not visible in the SDSS image. J2000 J2000 GALAXY JET RADIO GALAXY This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W /private/var/folders/8k/sxlgy5ts2xdbykzf_vw6jrfw0001c5/T/OPVisit4450121861031560705.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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