0Assigned ID: 333
----- Attempting Submission 1 (Fri Apr 11 02:34:07 GMT 2014) -----
HST Phase I Proposal 333 (jetpol_cy21.pdf.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 03:20:42 GMT 2014) -----
HST Phase I Proposal 333 (jetpol_cy21.pdf.apt) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 15:22:43 GMT 2014) -----
HST Phase I Proposal 333 (jetpol_cy21.pdf.apt) successfully submitted.0----- Attempting Submission 1 (Mon Jul 21 14:00:33 GMT 2014) -----
HST Phase II Proposal 13764 (jetpol_cy21.pdf.apt) successfully submitted.
----- Attempting Submission 2 (Thu Jul 24 17:05:03 GMT 2014) -----
----- Attempting Submission 3 (Tue Nov 25 14:51:01 GMT 2014) -----The Physics of the Jets of Powerful Radio Galaxies and QuasarsWe propose HST polarimetry of the jet of 3C 273. Polarization is a critical parameter for understanding jet flows, and only HST has the resolution and capability to perform this measurement. The data will confirm which mechanisms are operating to create its optical and X-ray emission, and will show locations where the magnetic fields are being structured by shocks and shears. This will greatly advance modeling efforts for this jet and nail down its kinetic power, a key unknown parameter for understanding quasars and their cosmological effects. Comparison with in-hand radio and ground-based near-IR (AO) optical polarimetry at matched resolution will measure the flow speed in the plasma as a function of particle energy, in the same way as in our analysis of our earlier HST polarimetry data on low-power jets.
This proposal builds on our observations of two other quasar jets, where we measured high polarization in the X-ray brightest knots, and so showed that their optical and X-ray emission is most likely due to the synchrotron model, since the alternative, IC/CMB model fails to match those objects' steep radio spectra and modest variability, and requires exceptionally fast flows (Gamma>30) at hundreds of kpc and super-Eddington kinetic power. The proposed observations will provide much stronger constraints because this iconic jet, because of its brightness, exceptional angular separation from the core and low redshift (z=0.158). Our modelling techniques will also provide much information on the jet's internal structure, including shocks and the sites of particle acceleration.The goal of this proposal is to obtain HST polarimetry of the 3C 273 jet using the ACS/WFC + POLVIS + F606W filters. We are using F606W because it gives the optimal mix between rejection of cross-polarized light and high throughput of parallel polarized light with the POLVIS filters. In addition, the F606W band was shown by Jester et al. (2005, 2006, 2007) to lie on the same spectral component as the Chandra X-ray emission, so these observations will allow us to perform critical tests of the X-ray emission mechanism of the jet.
The observations have been constructed in a very simple way. All long integrations with the same POL filter are in a single visit. Thus POL0 observations are in Visit 01, POL60 observations are in Visit 02, and POL120 observations are in Visit 03. All of these orbits use standard dither patterns - orbit 1 is a 2-point ACS-WFC-DITHER-LINE and orbits 2 & 3 are a 4 point ACS-WFC-DITHER-BOX. This allows maximum efficiency by placing readouts during Earth-shadow times and maximizes exposure time.
We are also doing several short observations, for calibration purposes. All of these are in orbit 4 of Visit 01. The 60-s observations with the polarizers will allow us to calibrate the PSF so that the quasar, which will be saturated in the long-exposure images, can be modeled correctly and subtracted out of the long-exposure images along with the galaxy to reveal the inner jet components, which previous HST polarimetry was not deep enough to reveal. The 20-s observation without the polarizers will allow a check on the flux and polarization calibration, a strategy which we have used for our previous ACS polarization programs 9847 and 11138. Note that we cannot use previous observations of 3C 273 for this purpose because the quasar is variable. All of the calibration observations use a 2-position dither, also in a standard ACS-WFC-DITHER-LINE configuration.
We have specified four fairly wide, 40 degree orientation windows so that the jet can be placed near to or along a chip diagonal. We have required SAME-ORIENT so that the chip is then oriented identically and the jet is in the same chip quadrant in all three visits, thus minimizing calibration issues. This was recommended by Andre' Martel, a member of the team and also a previous member of the ACS instrument team.AGN/QUASARS12falsefalse0.00.0falsefalsefalseSUPPORTEDGALAXYACCRETION DISKJETNUCLEUSQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ACS/WFCImagingNoYesF606WACS/WFCImagingNoNoF606WPOS-TARGDITHER0.265LINE0.187falsefalse69.05420.67ACS-WFC-DITHER-BOX1falsePOS-TARGDITHER3.011LINEfalsefalse285.28ACS-WFC-DITHER-LINE2false/private/var/folders/_s/hnxrdqs13h18jclmhk9wv5ch0000gn/T/OPVisit3188005046859612003.xmlTiming link suitability includes constraints ([02 After 01 by at most 14.0 days] [03 After 01 by at most 14.0 days])Hst Same orient constraint links visits (01 02 03)The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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