A hard look at NGC 5347: revealing a nearby Compton-thick AGN

Abstract

Current measurements show that the observed fraction of Compton-thick (CT) AGN is smaller than the expected values needed to explain the cosmic X-ray background. Prior fits to the X-ray spectrum of the nearby Seyfert-2 galaxy NGC 5347 ($z=0.00792,D=35.5\mathrm{Mpc}$) have alternately suggested a CT and Compton-thin source. Combining archival data from $Suzaku$, $Chandra$, and - most importantly - new data from $NuSTAR$, and using three distinct families of models, we show that NGC 5347 is an obscured CTAGN ($N_{\mathrm{H}}>2.23\times 10^{24}\mathrm{c}{\mathrm{m}}^{-2}$). Its 2-30~keV spectrum is dominated by reprocessed emission from distant material, characterized by a strong Fe K$\hat{I}\pm$ line and a Compton hump. We found a large equivalent width of the Fe K$\hat{I}\pm$ line ($\mathrm{EW}=2.3\pm 0.3$ keV) and a high intrinsic-to-observed flux ratio ($\sim 100$). All of these observations are typical for bona fide CTAGN. We estimate a bolometric luminosity of $L_{\mathrm{bol}}\simeq 0.014\pm 0.005L_{Edd.}$. The $Chandra$ image of NGC 5347 reveals the presence of extended emission dominating the soft X-ray spectrum ($E<2\mathrm{keV}$), which coincides with the [O III] emission detected in the $HubbleSpaceTelescope$ images. Comparison to other CTAGN suggests that NGC 5347 is broadly consistent with the average properties of this source class. We simulated $XRISM$ and $Athena$/X-IFU spectra of the source, showing the potential of these future missions in identifying CTAGN in the soft X-rays.

Accepted for publication in ApJ