The emission line spectrum of the UV deficient quasar Ton 34: evidence of shock excitation?

TL;DR

This study analyzes the emission line spectrum of the UV-deficient quasar Ton 34, finding that shock excitation, rather than photoionization, explains the unusually strong far-UV emission lines.

Contribution

It provides evidence that shock excitation is a significant mechanism for certain emission lines in Ton 34, challenging the traditional photoionization model.

Findings

Shock models with Vs ~ 100 km/s explain the line strengths.

Photoionization models fail to reproduce the observed lines.

Ton 34 exhibits unusually strong low to intermediate excitation lines.

Abstract

Emission lines in quasars are believed to originate from a photoionized plasma. There are, however, some emission features which appear to be collisionally excited, such as the FeII multiplet bands. Shortward of Ly_alpha, there also are a few permitted lines of species from low to intermediate ionization. Ton 34 (z=1.928) exhibits the steepest far-UV continuum decline known (Fnu propto nu^{-5.3}) shortward of 1050A. This object also emits unusually strong low to intermediate excitation permitted lines shortward of the Lyman limit. Using archive spectra of Ton 34 from HST, IUE and Palomar, we measure the fluxes of all the lines present in the spectra and compare their relative intensities with those observed in composite quasar spectra. Our analysis reveals unusual strengths with respect to Ly_alpha of the following low to intermediate excitation permitted lines: OII+OIII (835A), NIII+OIII (686-703A) and NIII+NIV (765A). We compare the observed line spectrum with both photoionization and shock models. Photoionization cannot reproduce the strengths of these far-UV lines. Shocks with Vs ~ 100 km/s turn out to be extremely efficient emitters of these lines and are favored as excitation mechanism.