Broad-line radio galaxies ( BLRGs ) are active galactic nuclei that produce powerful , large-scale radio jets , but appear as Seyfert 1 galaxies in their optical spectra .
In the X-ray band , BLRGs also appear like Seyfert galaxies , but with flatter spectra and weaker reflection features .
One explanation for these properties is that the X-ray continuum is diluted by emission from the jet .
Here , we present two NuSTAR observations of the BLRG 3C 382 that show clear evidence that the continuum of this source is dominated by thermal Comptonization , as in Seyfert 1 galaxies .
The two observations were separated by over a year and found 3C 382 in different states separated by a factor of 1.7 in flux .
The lower flux spectrum has a photon-index of \Gamma = 1.68 ^ { +0.03 } _ { -0.02 } , while the photon-index of the higher flux spectrum is \Gamma = 1.78 ^ { +0.02 } _ { -0.03 } .
Thermal and anisotropic Comptonization models provide an excellent fit to both spectra and show that the coronal plasma cooled from kT _ { e } = 330 \pm 30 keV in the low flux data to 231 ^ { +50 } _ { -88 } keV in the high flux observation .
This cooling behavior is typical of Comptonizing corona in Seyfert galaxies and is distinct from the variations observed in jet-dominated sources .
In the high flux observation , simultaneous Swift data are leveraged to obtain a broadband spectral energy distribution and indicates that the corona intercepts \sim 10 % of the optical and ultraviolet emitting accretion disk .
3C 382 exhibits very weak reflection features , with no detectable relativistic Fe K \alpha line , that may be best explained by an outflowing corona combined with an ionized inner accretion disk .