0Assigned ID: 6005
----- Attempting Submission 1 (Fri Nov 08 00:58:07 GMT 2024) -----
HST Phase I Proposal 6005 successfully submitted.
Receipt: # 6005-1
----- Attempting Submission 2 (Fri Nov 08 00:58:46 GMT 2024) -----
HST Phase I Proposal 6005 successfully submitted.
Receipt: # 6005-2
----- Attempting Submission 3 (Fri Nov 08 01:00:02 GMT 2024) -----Adjusted the ORIENT constraints on visit 03 so that only those with guide stars available are given.1433200842----- Attempting Submission 1 (Sat Feb 01 04:57:16 GMT 2025) -----
HST Phase II Proposal 17919 successfully submitted.
Receipt: # 17919-1
----- Attempting Submission 2 (Tue Feb 18 20:39:45 GMT 2025) -----
HST Phase II Proposal 17919 successfully submitted.
Receipt: # 17919-2
----- Attempting Submission 3 (Thu Feb 20 15:17:14 GMT 2025) -----
----- Attempting Submission 4 (Sun Mar 09 20:53:49 GMT 2025) -----A legacy epoch for Hubble's optical jets: a reference for the futureWhile we have long known that jets from super-massive black holes exhibit highly relativistic speeds on parsec scales from radio interferometry, it is not generally known how the jet evolves 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. With the development of state-of-the-art astrometry techniques and new data from the Gaia mission, it is now possible register images of nearby jets first observed by HST in the 1990s to extremely high precision, reaching accuracies on proper motions of better than 0.3 mas/year. This enabled the dramatic finding of colliding superluminal knots in the jet of 3C264 and helical motions of plasma on kpc scales in M87. We propose a new epoch of joint HST/JWST observations on the 12 nearby optical jets which are essentially a legacy sample of monitored sources with observations spanning nearly 3 decades. This sample is an extremely unique one, and only HST and JWST can provide the precision astrometry and sensitivity needed to track the motion of plasma in jets on kpc scales.This is a proposal to re-observe the most well-known and well-observed of the optical synchrotron jets, many of which were first discovered/observed by Hubble in the 1990s. The very fast bulk motion of the plasma, near the speed of light, causes "superluminal" motion which can be traced in repeated HST observations over only a few years. The 12 targets in this study have most recently been observed with ACS/WFC in the F606W filter, and this bridge program will obtain a new observation in the coming HST cycle, roughly concurrent (within ~ 1 year) of matching JWST optical/R-band imaging of the same targets.
Here, we are essentially repeating an observation that has been carried out 1-3 times in the recent past with identical instrument setups to minimize systematic variability in the measurements. Most targets host bright cores embedded in a giant elliptical galaxy. Because these cores are variable and have been known to saturate the detector in a high state, we have specified orient constraints in most cases, to keep bright saturation spikes from overrunning the jet since this would severely impact the science. However there are no time constraints on the observations, and we have been careful to maximize the ORIENT windows to ease the effects on scheduling.The team includes several leading experts in the study of resolved optical jets with HST (E. Meyer, W. Sparks, M. Chiaberge, E. perlman) and the team has collectively lead dozens of previous HST programs on jets and other targets. The most directly relevant is the Cycle 21 program (GO-13327), |"Proper Motions at 500 Mpc: Measuring Superluminal Motions in Optical Jets with HST|", which provided the observations which lead to the discovery of the internal shocks in 3C 264 (published in Nature) that we are proposing to further monitor in this program, and the previous monitoring epochs in cycles 23 and 25, which were published in Archer et al., 2020. The team includes experts in polarimetry, including the use of HST polarizers (W. Sparks, E. Perlman, E. Meyer) who have published several dozen refereed papers on large-scale relativistic jets. The team includes experts on HST astrometry and proper motions (J. Anderson, R. van der Marel, E. Meyer) as well as experts in radio-wavelength studies of jets (E. Meyer, E. perlman, O. Shuvo, K. Reddy) and a leading theoretical expert on AGN jets (M. Georganopoulos).Supermassive Black Holes and Active Galaxies6falsefalsefalsefalsefalsefalsetruePRIMARY15trueSUPPORTEDGALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000GALAXYJETRADIO GALAXYJ2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF606WThe scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.3C 15 is an optical jet hosted by an elliptical galaxy. The core is sufficiently dim that saturation of the core is not a risk.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.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.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.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. We are using a subarray to enable shorter exposures to reduce saturation in the bright core.(Tic-Visit
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)false10The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.The target is an optical jet hosted by one of two merging elliptical galaxies. The core is sufficiently dim in the most recent epoch of imaging to allay concerns about saturation and diffraction spikes over-running the jet so no orient constraints are given.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.The target is an optical jet, of several arcseconds 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.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.Target is an optical jet approximately 45 degrees south of west. The host elliptical has a bright core - Vmag = 13. We have thus adopted relatively short exposures, and orient constraints to avoid diffraction spikes over the jet.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.Orient constraints are specified to avoid the bright core from producing diffraction spikes over the jet. POS TARGS and ORIENT constraints are used both for dithering and to place the target near to the WFC1 readouts to lessen CTE and to avoid having bright sources too near to the chip edge.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.4C 00.58 is an optical jet hosted by an elliptical galaxy. The core is sufficiently dim that saturation of the core is not a risk.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.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) and saturated in the previous imaging, so we have opted for relatively short exposures ~220 seconds, to lessen the diffraction spikes/core saturation. Orient constraints are specified to avoid the bright core from producing diffraction spikes over the jet.(Tic-Visit
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)true10The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode.(Tic-Visit
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