The X-Ray Emission Mechanism from Optical Jets: 3c 78

Details The X-Ray Emission Mechanism from Optical Jets: 3c 78 The X-Ray Emission Mechanism from Optical Jets: 3c 78

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002cxo..prop.1298b&link_type=abstract

Chandra Proposal ID #04700407

Computer Science

Chandra Proposal Id #04700407

Scientific paper

Radio to X-ray spectral coverage and sub-arcsec imaging provide powerful diagnostics of the electron energy distribution and electron acceleration in jets. 3C 78 is the longest optical jet not to have been adequately observed with Chandra, although it is one of only three jets with HST polarimetry. Our 5-ks exploratory ACIS-S3 observation of 3C 78 in AO-3 demonstrated that the jet is detectable in the X-ray, lying outside the PRF of the core and above any diffuse emission from the host galaxy. Here we request a 55 ks ACIS-S observation to complete X-ray work on this jet, and two HST NICMOS near-IR exposures. These data will investigate electron acceleration mechanisms both in the diffuse regions of the jet and in the anomalous X-ray/optical knot 1.5 arcsec from the core.

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