Jets at Intermediate Redshifts: Shedding Light on Emission Mechanisms and Physics

Ran into trouble trying to set a dither. I did not expect the template patterns to default to CR-SPLIT=2 (not obvious we had to set CR-SPLIT=NO explicitly). Also, APT did something funny with putting the individual dithered exposures into separate orbits...should have been smart enough to try to put everything into as few orbits as possible. ----- Attempting Submission 1 (Mon Oct 20 19:05:36 GMT 2008) ----- Phase II Proposal 11830 (11830_final.apt) successfully submitted. ----- Attempting Submission 2 (Wed Feb 25 20:25:34 GMT 2009) ----- Phase II Proposal 11830 (11830_resubdither.apt) successfully submitted. ----- Attempting Submission 3 (Fri Mar 13 10:44:50 GMT 2009) ----- Jets at Intermediate Redshifts: Shedding Light on Emission Mechanisms and Physics We propose observations of a small sample of intermediate-redshift radio jets (2<z<3) matched in radio properties with the one we previously observed at z<=1. The goal is to investigate the physics of jets in a significantly different cosmological environment. While observations of jets at high z (>=3-4) tend to confirm the IC/CMB origin of the X-ray emission, the limited morphological information available due to the faintness of the radio emission prevents more detailed studies. Observations at intermediate z will bridge the gap, allowing us to study the role of both the increase of the CMB energy and intergalactic matter densities on the X-ray emission properties and physics of jets.

Each of the 3 targets require 1 orbit of F606W imaging. Assuming a radio-to-optical spectral index, $\alpha_{\rm ro}=0.9$ and normalizing to the radio fluxes, we expect a range of detections of 0.07 $\mu$Jy (18$\sigma$) for the faintest radio knots, to 0.64 $\mu$Jy (89$\sigma$) for the brightest. Conversely, we can probe $\alpha_{\rm ro}$ values down to $>$0.95 and $>$1.14 (5$\sigma$). Thus, a single filter observation is sufficiently sensitive to determine if the radio and X-ray points are from a single power-law component or if two spectral components are necessary (e.g., Sambruna et al. 2006). According to the WFC3 ETC, the 2 V~18 targets will take ~200 sec to saturate. We have put in a short (92-93 sec) exposure to obtain an unsaturated image. The third target, the faintest one, is not expected to saturate. 12 false 0.0 0.0 false false false false false SUPPORTED GALAXY QUASAR J2000 00 00 0.0000 +00 00 0.00 J2000 GALAXY QUASAR J2000 00 00 0.0000 +00 00 0.00 J2000 GALAXY QUASAR J2000 00 00 0.0000 +00 00 0.00 J2000 POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1

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