  Hard X-ray emission in radio-quiet active galactic nuclei (AGNs) is believed
to be produced via inverse Compton scattering by hot and compact coronae near
the super massive black hole. However the origin and physical properties of the
coronae, including geometry, kinematics and dynamics, yet remain poorly known.
In this work, taking [OIV] 25.89um emission line as an isotropic indicator of
AGN's intrinsic luminosity, we compare the intrinsic corona X-ray emission
between Seyfert 1 and Compton-thin Seyfert 2 galaxies, which are viewed at
different inclinations according to the unification scheme. We compile a sample
of 130 Compton-thin Seyfert galaxies with both [OIV] 25.89um line luminosities
measured with Spitzer-IRS and X-ray spectra observed by XMM-Newton, Chandra,
Suzaku or Swift. Known radio-loud sources are excluded. We fit the X-ray
spectra to obtain the absorption-corrected 2-10 keV continuum luminosities. We
find that Seyfert 1 galaxies are intrinsically brighter in intrinsic 2-10 keV
emission by a factor of 2.8+0.5-0.4 (2.2+0.9-0.3 in Swift-BAT 14-195 keV
emission), comparing with Compton-thin Seyfert 2 galaxies. The Seyfert 1 and
Compton-thin Seyfert 2 galaxies follow a statistically identical correlation
between the absorption-corrected 2-10 keV luminosity and the 14-195 keV
luminosity, indicating that our absorption correction to the 2-10 keV flux is
sufficient. The difference in X-ray emission between the two populations is
thus unlikely due to X-ray absorption, and instead implies an intrinsic
anisotropy in the corona X-ray emission. This striking anisotropy of X-ray
emission can be explained by a bipolar outflowing corona with a bulk velocity
of ~0.3-0.5c. This would provide a natural link between the so-called coronae
and weak jets in these systems. Other consequences of outflowing coronae are
also discussed.
