tokens: of dust extinction. Generally, the single-band SFRs are in agreement or are slightly lower than those derived from SED modeling with MAGPHYS. If we are unable to use either of the first two methods and we have at least one detection in another filter, we scale the SEDs from the DLA counterparts that were fit with the first method to match the detected host galaxy flux. We then use the scaled SEDs to estimate the rest-frame UV flux and use the median and standard deviation of the scaled SEDs to calculate the rest-frame UV SFR. Finally, if there are no detections in any band but there are upper limits in the rest-frame UV band, we calculate SFR upper limits using the second method. Photometric measurement were made using the aperture photometry technique, using the HST point-spread function (PSF) for GRB-DLA counterparts with HST data and the DCT 12 PSF for the ground-based data (corresponding to ∼2 and ∼17 kpc diameter apertures respectively). The large difference in apertures comes from the fact that HST is able to resolve the host galaxy. We assume that the light from unresolved sources is solely from the host galaxy and background sky. All SFRs are calculated from dust-corrected observations unless otherwise stated. The host extinction, A V , is taken either from SED models or from GRB afterglow measurements using a Small Magellanic Cloud (SMC)-like extinction law which has been shown to best depict the GRB explosion environment (e.g., Schady et al. 2012 ). We assume the host extinction is the same as the GRB line-of-sight extinction, which Perley et al. ( 2013 ) has shown is fairly consistent within a factor of two to three. If the host extinction is an upper limit, we use that value in all dust-corrected calculations and report SFR upper limits. In Table 1 , we report these GRB-DLAs with SFR error estimates but treat these as SFRs upper limits in all plots using dust-corrected SFRs. Our host extinction is, in general, higher than the reported for DLAs in the SDSS survey for our sample’s column densities (Murphy Bernet 2016 ). This may likely be because GRB-DLAs are found at a smaller impact parameter of (Blanchard et al. 2016 ) than the general DLA population of (Fumagalli et al. 2015 ) or more simply because our DLA sample traces, in general, metal-rich, and likely dust rich, systems (for example, see the correlation between and metal line equivalent widths in Murphy Bernet 2016 ). 3.1.1. SED Fitting Star Formation Rate We use MAGPHYS with the HIGHZ extension (da Cunha et al. 2008 , 2015 ), to model the host galaxy SEDs from photometry. MAGPHYS models templates to the data and returns an SED with fitted parameters which include SFR, stellar mass ( M ), dust mass ( M ), and A V . This particular package is well suited for galaxies and takes into account bursty star formation which is appropriate for GRB host galaxies as suggested by Hunt et al. ( 2014 ). MAGPHYS uses a continuous model of star formation with superimposed random bursts that
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