  We study the 0.5-10keV emission of a sample of five of the broadest
double-peaked Balmer-line emitters with Chandra. The Balmer lines of these
objects originate close (within a few hundred gravitational radii) to the
central black holes of the Active Galactic Nuclei (AGNs), and their
double-peaked profiles suggest an origin in the AGN accretion disk. We find
that four of the five targets can be modeled by simple power-law continua with
photon indices (1.6-1.8) typical of similar luminosity AGNs. One object, SDSS
J0132-0952, shows evidence of ionized intrinsic absorption. The most-luminous
SDSS double-peaked emitter, SDSS J2125-0813, has either an unusual flat
spectrum (~1) or is also highly absorbed. It is the only double-peaked emitter
for which no external illumination is necessary to account for the Balmer line
emission. The strength of the Balmer-line emission in the remaining four
objects suggests that the total line flux likely exceeds the viscous energy
that can be extracted locally from the accretion disk and external illumination
is necessary. All five double-peaked emitters have unusually strong X-ray
emission relative to their UV/optical emission, which is the likely source of
the external illumination necessary for the production of the observed strong
broad lines. On average about 30% of their bolometric luminosities are emitted
between 0.5-10keV. The spectral energy distributions of the five double-peaked
emitters show the big blue bumps characteristic of radiatively efficient
accretion flows. The Balmer line profiles, as well as the optical and X-ray
fluxes of the double-peaked emitters, are highly variable on timescales of
months to years in the AGN rest frame.
