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

## TL;DR

This study confirms NGC 5347 as a Compton-thick AGN using multi-mission X-ray data, revealing its obscured nature and emphasizing the importance of future X-ray observatories in identifying such sources.

## Contribution

The paper provides the first definitive classification of NGC 5347 as a Compton-thick AGN through combined archival and new X-ray observations, employing multiple models for robust analysis.

## Key findings

- NGC 5347 is confirmed as a Compton-thick AGN with N_H > 2.23×10^24 cm^-2.
- The spectrum shows a strong Fe Kα line and a Compton hump, typical of CTAGN.
- Future missions like XRISM and Athena can effectively identify CTAGN in soft X-rays.

## 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 \rm ~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 ($N_{\rm H} > 2.23\times 10^{24}~\rm cm^{-2}$). Its 2-30~keV spectrum is dominated by reprocessed emission from distant material, characterized by a strong Fe K$\alpha$ line and a Compton hump. We found a large equivalent width of the Fe K$\alpha$ line ($\rm EW = 2.3 \pm 0.3$ 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 $L_{\rm bol} \simeq 0.014 \pm 0.005~L_{\rm Edd.}$. The $Chandra$ image of NGC 5347 reveals the presence of extended emission dominating the soft X-ray spectrum ($E < 2\,\rm keV$), which coincides with the [O III] emission detected in the $Hubble ~Space~ Telescope$ 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.