tokens: NGC 4449 must have been ongoing for a significant fraction of the burst lifetime. Depending on the 3D distribution of the extended H i , this material may not have been expelled into the IGM, but may instead reside at extended radii around the galaxy and/or recycled back into the galaxy. For NGC 5253, the detected outflow surrounds much of the central star-forming region and is strongest in the south. Marlowe et al. ( 1995 ) measure velocities of the Hα detected shells of 35 km s −1 with physical extents of ∼1 kpc. Summers et al. ( 2004 ) find the extent of the X-ray emission to be somewhat smaller (∼0.5 kpc). However, using combined Chandra observations, we find a more extended region in the south of the galaxy that reaches ∼2.4 kpc in projection that cannot be explained by dynamical arguments and short star formation time-scales. These inconsistencies are alleviated when the longer star formation time-scales from the SFHs are considered. Furthermore, the SFR in NGC 5253 has declined by nearly a factor of 6 over the duration of the burst. The declining SFRs and small-scale outflow in NGC 5253 indicate that we are seeing the end of a wind phase (see also Fig. 7 ), rather than just the beginning of an outflow as has been previously suggested (Summers et al. 2004 ). For NGC 1569, the dynamical age of the outflow was previously estimated to be 10 Myr (Heckman et al. 1995 ; Martin 1998 ). Using this time-scale, Martin et al. ( 2002 ) estimate the amount of oxygen that could be in the wind of NGC 1569 and compare this to the amount of metals produced by star formation over a 10–20 Myr time-scale assuming a nucleosynthesis yield. Based on their best-fitting model of a solar metallicity in the wind, and to maintain consistency with the current gas-phase oxygen abundance in the galaxy, these authors report nearly all metals formed in the recent star formation activity have been expelled in the wind. However, as stated in Martin et al. ( 2002 ), this requires that the present-day gas-phase oxygen content in the galaxy was created in previous episodes of star formation that must have been quiescent (i.e. not energetic enough to drive an outflow). Based on the CMDs and the derived SFHs, there has been significant star formation in the last few 100 Myr in NGC 1569, with the peak star formation occurring 65 Myr. This suggests that the wind has been ongoing. Furthermore, the best-fitting model of a solar oxygen abundance in the hot wind does not take into account the uncertainties; a nearly equal χ 2 is found for 0.25 Z ⊙ , as well as for supersolar abundances for NGC 1569 (Martin et al. 2002 , see their table 5). The amount of metals ejected by the wind in NGC 1569 remains an open question. 6 CONCLUSIONS We have examined the diffuse soft X-ray emission from Chandra observations in six nearby starburst dwarf galaxies from the STARBIRDS sample (McQuinn et al. 2015a ) and compared the X-ray properties with the neutral gas distributions, SFHs quantified from
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