<|endoftext|> are thus fundamental for measuring the intrinsic X-ray luminosity of obscured AGN hosted in ULIRGs and its contribution to their high observed FIR emission.\
IRAS 19254-7245 (also known as the [*SuperAntennae*]{}) belongs to a flux limited sample at $60\mu$m composed of the 15 brightest nearby ULIRGs [@Genzel]. Located at $z=0.062$, [IRAS 19254-7245]{} has an infrared luminosity of $L_\mathrm{8-1000{\:\mu\mbox{\scriptsize m}}}=1.1\times 10^{12}L_\odot$ corresponding to a bolometric luminosity of $L_{bol}\sim 4\times 10^{45}$erg s$^{-1}$. Like most of the ULIRGs, IRAS 19254-7245 is a merger system of two gas-rich spiral galaxies.
The southern nucleus, optically classified as a Seyfert 2, is one of the brightest nearby ULIRGs which has proved to host both a powerful starburst and an obscured AGN, while there is no evidence of AGN activity in the northern nucleus.\
A previous X-ray observation of [IRAS 19254-7245]{} performed with [[*XMM-Newton*]{}]{} suggested that this ULIRG harbors a heavily obscured and high-luminosity AGN. Indeed the hard power-law continuum above 2 keV (photon index $\Gamma
=1.3$) and the detection of a strong Fe-K$\alpha$ emission line at $6.5\pm 0.1$ keV ($EW \sim 1.4$ keV) were highly indicative of a Compton-thick source [@Braito]. As the two nuclei are located $\sim$ 9 arcsec apart from each other, [[*XMM-Newton*]{}]{} could not resolve them; however the centroid of the hard X-ray emission was spatially coincident with the southern nucleus. Chandra observation which would settle or solve this issue has not been performed yet.\
The best fit model obtained for the 0.5-10 keV X-ray emission detected with [[*XMM-Newton*]{}]{} was composed by a strong soft thermal component, associated with the starburst emission and a hard X-ray component associated with the AGN activity. This AGN component was parametrized with a Compton thick AGN model and was composed of a pure Compton-reflected continuum (with $\Gamma\sim
1.8$), a scattered power law component and a strong Fe emission line. The observed 2–10 keV luminosity of the AGN was found to be $\sim 4\times 10^{42}$ [erg s$^{-1}$]{}. Due to the limited energy bandpass of XMM-Newton, this observation did not allow us to directly see the intrinsic continuum, thus to measure the absorbing column density and the intrinsic X-ray luminosity of IRAS 19254-7245.\
Here we present the analysis of a deep Suzaku observation ($\sim 150$ ksec) of this system, which allowed us for the first time to constrain the intrinsic power of the AGN hosted in [IRAS 19254-7245]{}, as well as to investigate in detail the properties of the Fe line complex. In Sec. 2 we present the Suzaku data analysis and results, while in Sec. 3 we discuss the overall scenario for X-ray emission of [IRAS 19254-7245]{}. Throughout this paper, the current popular cosmology is assumed with $H_0=73$ km s$^{-1}$ Mpc$^{-1}$, $\Omega_{\rm{M}}=0.27$ and $\Omega_\lambda=0.73$.
Observations and data reduction
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Suzaku ([@Mitsuda]) is the fifth Japanese X-ray satellite, which carries on board four sets of X-ray mirrors, with a X-ray CCD (XIS; three front illuminated, FI, and one back illuminated, BI [@XISref]) at their focal plane, and a non imaging hard X-ray detector (HXD, [@Takahashi]). The latter is composed by 2 main instruments: the Si PIN photodiodes and the GSO scintillator counter. Altogether the XIS and the HXD-PIN cover the 0.5–10 keV and 12–70 keV bands respectively.\
Suzaku observed IRAS19254-7245 for a total exposure time of about 150 ksec; the observation was performed at the beginning of November 2005, when all the 4 XIS were still working[^1].\
Cleaned event files from the version 2 of the Suzaku pipeline processing were used with the standard screening[^2]. The net exposure times are $97.9$ ksec for each of the XIS and $142.1$ ksec for the HXD-PIN. The XIS source spectra were extracted from a circular region of 2.9$