English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We study the 0.5-10keV emission of a sample of five of the broadestdouble-peaked Balmer-line emitters with Chandra. The Balmer lines of theseobjects originate close (within a few hundred gravitational radii) to thecentral black holes of the Active Galactic Nuclei (AGNs), and theirdouble-peaked profiles suggest an origin in the AGN accretion disk. We findthat four of the five targets can be modeled by simple power-law continua withphoton indices (1.6-1.8) typical of similar luminosity AGNs. One object, SDSSJ0132-0952, shows evidence of ionized intrinsic absorption. The most-luminousSDSS double-peaked emitter, SDSS J2125-0813, has either an unusual flatspectrum (~1) or is also highly absorbed. It is the only double-peaked emitterfor which no external illumination is necessary to account for the Balmer lineemission. The strength of the Balmer-line emission in the remaining fourobjects suggests that the total line flux likely exceeds the viscous energythat can be extracted locally from the accretion disk and external illuminationis necessary. All five double-peaked emitters have unusually strong X-rayemission relative to their UV/optical emission, which is the likely source ofthe external illumination necessary for the production of the observed strongbroad lines. On average about 30% of their bolometric luminosities are emittedbetween 0.5-10keV. The spectral energy distributions of the five double-peakedemitters show the big blue bumps characteristic of radiatively efficientaccretion flows. The Balmer line profiles, as well as the optical and X-rayfluxes of the double-peaked emitters, are highly variable on timescales ofmonths to years in the AGN rest frame.

A Chandra Look at Five of the Broadest Double-Peaked Balmer-Line Emitters