0Assigned ID: 958
----- Attempting Submission 1 (Fri Apr 10 22:32:42 GMT 2015) -----This is being resubmitted with slightly lower exposure times on visit 03, in order to ease scheduling.1990982652----- Attempting Submission 1 (Tue Jul 21 06:09:03 GMT 2015) -----
----- Attempting Submission 2 (Thu Mar 31 12:42:41 GMT 2016) -----No change in targets.Mapping the kpc-scale Velocity Structure of Jets with HSTHST has recently broken new ground in mapping the velocity profiles of resolved, kpc-scale relativistic jets in nearby active galaxies. While we have long known that the plasma in these jets exhibit highly relativistic speeds on parsec-scales near to the black hole from radio interferometry, it was not known how the jet evolved on kpc to Mpc scales, where the jet leaves the host galaxy and begins to interact with the intergalactic medium, with implications for our understanding of jet structure and quantifying the energy carried by the jet into the external environment. Our group has developed state-of-the-art astrometry techniques to register images of nearby jets taken with HST over the last 20 years to extremely high precision, reaching accuracies on proper motions of better than 0.3 mas/year. First results from a pilot program in Cycle 21 include the dramatic finding of colliding superluminal knots in the jet of 3C264 (Meyer et al. 2015, Nature). We propose moderately deep ACS/WFC imaging of the remaining seven jets which were first observed by HST in the 1990s and which are near enough to yield proper motion accuracies of 0.3-1c. These observations will give us a reference epoch against which to register images extending back over 20 years in the HST archive. The final sample of 11 jets with high-precision kpc-scale velocity measurements will be the only sample of its kind, and will allow us for the first time to begin understanding the evolution of velocity structure on kpc scales, and the connection to jet power and morphology.We will observe 7 targets which are active galaxies with optical jets coming from the bright central core. These optical jets have previously been detected with HST, and the current observations are looking for changes (i.e., proper motions) in the jet. For all targets the observation consists of 2 orbits with ACS/WFC in F606W filter. Roll angle specifications have been applied to avoid streaking from bright cores (or nearby bright objects) from over-running the fainter optical jets.AGN/QUASARS12falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHOTSPOTJETRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYELLIPTICALJETRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYELLIPTICALJETRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYELLIPTICALJETRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYELLIPTICALJETRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYELLIPTICALJETRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYELLIPTICALJETRADIO GALAXYThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WThe scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.Note: the brightest knot in the jet has been detected at 1e-4 Jy, which is extremely bright for an optical knot. To avoid any risk of saturation, we have kept the exposures to ~ 400 seconds or less.
The jet is very long, approximagely 1' just on the western side. There is also a hotspot about 1' to the east of the core position (the core position is the given location of the target). The target is positioned (and orient ranges specified) to ensure that both sides of the jet land on the WFC1 detector.
There is also a nearby companion galaxy at 19:52:16.66 +02:30:13.50 (Vmag=13.87). For both the bright core and this companion we avoid orient ranges where either could produce a diffraction spike which over-runs the jet.1441717833000115.0(Tic-Visit
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)true20The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.The appearance of the target in the optical is mainly dominated by the host elliptical galaxy which is moderately bright (Vmag=15). The jet itself runs to the northwest (PA approx 45 deg N->W) and is about 10" arcseconds long.
The main difficulties for the observation are two very bright, somewhat nearby sources -- one about 80" directly north (Vmag=9) and one about 80" south (Vmag=11.65). The orient ranges are specified to completley avoid having the brighter source on the WFC1 detector (where our target lies). In addition, we avoid roll angles where either the core of the host galaxy for our jet OR the Vmag=11.65 source to the south could possibly produce saturation spikes which would overrun the jet. We also avoid angles where bright sources would land at the edge of the detectors.
Overall the field is crowded with bright sources, so we have opted for relatively short exposures (~ 400 seconds).(Tic-Visit
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)true20/private/var/folders/rr/hp3f00092rx6cx3jys_kgn700000gp/T/OPVisit8650221574742319427.xmlThe scheduling data was generated by CASM 24.0.CASM was run in Phase II mode.The target is an optical jet hosted by a Vmag=13.8 elliptical galaxy. The field is relatively empty with no major nearby bright sources to require any special considerations. Orent constraints are specified to ensure that the bright core of the galaxy does not produce any saturation spikes which could over run the jet.
POS TARGS are used to place the target near the readout of the WFC1 detector to minimize CTE effects.(Tic-Visit
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:date "31-Mar-2016 08:41:05.0"
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)true20The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.3C 15 is an optical jet hosted by an elliptical galaxy. We have used orient constraints to ensure no diffraction spikes from the core and another nearby bright source overrun the jet.144664317500080.0(Tic-Visit
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)true20The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.The target is an optical jet pointed towards the southwest, approximately 6 arcseconds long. The host galaxy and central nucleus are very bright (V-mag 12), so we have opted for relatively short exposures ~400 seconds. Orient constraints are specified to avoid the bright core from producing diffraction spikes over the jet. POS TARGS are used both for dithering and to place the target near to the WFC1 readouts to lessen CTE.1441055530000110.0(Tic-Visit
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)true20The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.Another optical jet, approximately 45 degrees south of west. The host elliptical has a bright core - Vmag = 12. We have thus adopted relatively short exposures, and orient constraints to avoid diffraction spikes over the jet.1442178247000267.31545014559424(Tic-Visit
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)true20The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.The target is an optical jet, of 2-3" length pointed in the northwest direction. The host galaxy is an elliptical with a bright core. We have used orient constraints to avoid having the diffraction spikes run over the jet, also taking into account other nearby bright sources. POS TARGS are used for dithering and to put the target closer to the WFC1 readouts for improved CTE.144433509800067.18508691091671(Tic-Visit
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