analysis tools provided by the UK *Swift* Science Data Centre [@Evans2007; @Evans2009]. We first combined all of the data into a single deep stack (total exposure time 30ks), which we then downloaded for local analysis. The stacked image, shown in Figure \[fig:x\], clearly exhibits an X-ray source at the position of AT2019qiz. Using a $50''$ aperture ($\sim2.5$ times the instrumental half-energy width) centered at the coordinates of the transient, we measure an excess $46.9 \pm 8.4$ counts above the background, giving a mean count rate of $(1.6\pm0.3)\times10^{-3}$ cts$^{-1}$.

We then used the same tools to extract the mean X-ray spectrum, shown in Figure \[fig:xspec\], and light curve. Given the low number of counts we fit the spectrum using Cash statistics, and fixed the Galactic column density to $6.5\times 10^{20}$ cm$^{-2}$. The fit with a power law does not need an intrinsic column ($<2.8\times 10^{21}$ cm$^{-2}$, $90\%$ confidence level). The photon index of the fit is $\Gamma=1.1^{+0.6}_{-0.4}$. A blackbody model can give a comparable fit, but the inferred temperature and radius ($kT=0.9$keV, $R=6.0\times10^7$cm) are not consistent with other TDEs. The 0.3-10 keV unabsorbed flux from the power-law fit is $9.9^{+3.7}_{-3.4}\times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$. At the distance of AT2019qiz, this corresponds 