their catalogued magnitudes from PanSTARRS data release 1 [@Flewelling2016].

AT2019qiz resides in a bright galaxy, 2MASXJ04463790-1013349, with $m_r=14.2$mag (Section \[sec:host\]). A three-colour ($gri$) image of the host, comprised of deep stacks from PanSTARRS, is shown in Figure \[fig:ps1\]. To isolate the transient flux, we aligned each LCO image with the PanSTARRS image in the corresponding filter using the <span style="font-variant:small-caps;">geomap</span> and <span style="font-variant:small-caps;">geotran</span> tasks in <span style="font-variant:small-caps;">pyraf</span>, computing the transformation from typically $> 50$ stars, before convolving the PanSTARRS reference image to match the PSF of the science image and subtracting with <span style="font-variant:small-caps;">hotpants</span> [@Becker2015].

![Optical and UV light curves of AT2019qiz. The host contribution has been removed using image differencing (ZTF, ATLAS, LCO) or subtraction of fluxes estimated from the galaxy SED (UVOT).[]{data-label="fig:phot"}](lc.pdf){width="\columnwidth"}

Astrometry
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Measuring the TDE position in an LCO $r$ band image obtained on 2019-10-10 (at the peak of the optical light curve), and the centroid of the galaxy in the aligned PanSTARRS $r$ band image, we measure an offset of $0.12\pm0.37$ pixels (or $0.047''\pm0.144$) between the transient and the host nucleus, where the uncertainty is dominated by the root-mean-square error in aligning the images. This corresponds to a physical offset of $15\pm46$pc at this distance; 