Comparison of X-ray Emission Properties of TDEs and Soft Flares from AGNs

Abstract

X-ray flaring activity from active galactic nuclei (AGNs) may mimic the expected emission from tidal disruption events (TDEs), thus contaminating TDE searches. To compare X-ray emission properties between TDEs and AGNs, we cross-match publicly available XMM-Newton and Swift-XRT point source catalogs with the Million Quasars Catalog and optically selected TDEs. We find that AGNs tend to become softer with a similar hardness ratio (HR) value as TDEs during their flaring events. The soft HRs during flaring events in these AGNs are driven by the emergence of a blackbody-like component below $\sim$2 keV, likely associated with the soft X-ray excess, as well as the continuum emission becoming steeper with the increase of accretion rate. We find 2.5% in XMM-Newton (23 out of 920) and 4.4% in Swift-XRT (179 out of 4089) AGNs display flares with peak count rate $>$$2\sigma$ from the median count rate and peak HR$<$$-0.75$. The rate of such flares in XMM-Newton and Swift-XRT is (1.1-2.5)$\times 10^{-3}\mathrm{galax}{\mathrm{y}}^{-1}\mathrm{y}{\mathrm{r}}^{-1}$ and (0.9-2.0)$\times 10^{-3}\mathrm{galax}{\mathrm{y}}^{-1}\mathrm{y}{\mathrm{r}}^{-1}$, respectively. We also estimate the rate of flares with a maximum flux change (peak/min) of $>20\times$ over on a rest-frame time scale of two years or more with a HR$<$$-0.75$ at peak to be (4.7-11.0)$\times 10^{-5}\mathrm{galax}{\mathrm{y}}^{-1}\mathrm{y}{\mathrm{r}}^{-1}$ and (3.1-7.1)$\times 10^{-5}\mathrm{galax}{\mathrm{y}}^{-1}\mathrm{y}{\mathrm{r}}^{-1}$ in XMM-Newton and Swift-XRT, respectively. Finding an optical or infrared counterpart may help to identify these flaring AGNs. We confirm 61% and 79% of flaring sources from XMM-Newton and Swift-XRT, respectively, as AGNs through variability in ZTF light curves or a WISE $W1$$-$$W2$$>$0.8 mag color cut.

19 pages, 15 figures, accepted for publication in ApJ