The Resolved Outflow From 3c 48

Abstract

We investigate the properties of the high-velocity outflow driven by the young radio jet of 3C 48, a compact-steepspectrum source. We use the Space Telescope Imaging Spectrograph on board the Hubble Space Telecope to obtain (1) low-resolution UV and optical spectra and (2) multi-slit medium-resolution spectra of the ionized outflow. With supporting data from ground-based spectrographs, we are able to accurately measure the ratios of diagnostic emission lines such as, and [Ne iii] λ3869. We fit the observed emission-line ratios using a range of ionization models, powered by active galactic nucleus (AGN) radiation and shocks, produced by the MAPPINGS code. We have determined that AGN radiation is likely the dominant ionization source. The outflow's density is estimated to be in the range n = 10 3 -10 4 cm −3 , the mass is ∼6 × 10 6 M , and the metallicity is likely equal to or higher than solar. Compared with the typical outflows associated with more evolved radio jets, this young outflow is denser, less massive, and more metal rich. Multi-slit observations allow us to construct a two-dimensional velocity map of the outflow that shows a wide range of velocities with distinct velocity components, suggesting a wide-angle clumpy outflow.

Compact steep-spectrum and peaked-spectrum radio sources

“…100 pc from the nucleus appears to be pushing an HI cloud with a blue-shifted velocity of 1000 km s −1 providing the direct link between the radio jet and the outflow (Morganti et al, 2013). In addition, the high velocity [Oiii] λ5007 gas in 3C48 is associated with the base of the radio jet (Stockton et al, 2007;Shih and Stockton, 2014). Mullaney et al (2013) studied [Oiii] λ5007 line profiles using SDSS spectra of a sample of 24,264 optically selected AGN.…”

Radio Jet Feedback and Star Formation in Heavily Obscured, Hyperluminous Quasars at Redshifts ∼ 0.5–3. I. Alma Observations

“…High resolution observations of nearby low luminosity AGN show that the MIR emission can lie in the polar direction and may be associated with NLR clouds or with thermal winds from the AGN (Zhang et al 2013 and references therein). It is also known that a significant fraction of FRII radio AGN have extended emission line regions (EELRs) up to tens of kpc in size (Fu & Stockton 2007), which are outflowing (Shih & Stockton 2014). The Compact-Steep-Spectrum (CSS) sources, which are younger versions of the FR IIs, have smaller EELRs which are better aligned with the radio structures than in FR IIs (Axon et al 2000).…”

Observable Emission Features of Black Hole GRMHD Jets on Event Horizon Scales

“…It is a pressing question as to how the radiation that is observed in relativistic jets in active galactic nuclei (AGN) is generated (e.g., Blandford & Königl 1979;Marscher 1980;Zensus 1997;Laing & Bridle 2002;Honda 2010;Levinson & Rieger 2011;Mościbrodzka et al 2011;Ito et al 2013;Mason et al 2013;Potter & Cotter 2013;Wang et al 2014;Scott & Stewart 2014;Shih & Stockton 2014;Hovatta et al 2014;Turner & Shabala 2015; ⋆ hpu@perimeterinstitute.ca; kinwah.wu@ucl.ac.uk; younsi@th.physik.uni-frankfurt.de;asada@asiaa.sinica.edu.tw; mizuno@th.physik.uni-frankfurt.de; nakamura@asiaa.sinica.edu.tw Asada et al 2016;Hirotani et al 2016;Koay et al 2016;Khabibullin et al 2016;Prieto et al 2016). Although there is a common consensus that the emitters are energetic particles, how these particles are accelerated to such high energies, how they dissipate their energy, and how they are transported with the jets themselves are still the subject of feverish investigation (e.g., Blandford & Eichler 1987).…”