The Jet Driven Motions in the Narrow Line Region of NGC 1068 |
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| Authors: | David J Axon A Marconi FD Macchetto A Capetti Andrew Robinson |
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| Institution: | (1) Affiliated to the Astrophysics Division of ESA, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21218;(2) Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21218;(3) Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze, Largo E. Fermi 5, I-50125, Italy;(4) Scuola Internazionale Superiore di Studi Avanzati, Via Beirut 2-4, 34014 Trieste, Italy;(5) Department of Physical Sciences, University of Hertfordshire, College Lane, Hatfield, Herts, AL10 9AB, UK |
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| Abstract: | We have obtained HST FOC f/48 long-slit spectroscopy of the central 2 arcseconds of the Narrow Line Region of NGC 1068 between
3500-5400\OA with a spectral resolution of 1.78\OA/pixel. At a spatial scale of 0″.0287 per pixel these data provide an order
of magnitude improvement in resolution over previous ground based spectra and allow us to trace the interaction between the
radio jet and the gas in the NLR. Our results show that, within ±0″.5 of the radio-jet the emission lines are split into two
components whose velocity separation is 1500 km s-1. The emission line structure is reminiscent of that seen previously around
the jet of 3C120. Furthermore, this material enveloping the radio-jet is in a much higher ionization state than that of the
surrounding NLR gas. The highest excitation is coincident with the jet axis where emission in the coronal line of FeVII]
λ3769\OA is detected but where OII] λ3727 \OA is depressed. These results imply that we are witnessing a cocoon of hot gas
in expansion around the radio-jet created by its interaction with the gas, and that these shocks are sufficiently fast, at
least ± km s-1, that they are creating localized ionization effects.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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