text: 191,197,1301869927410794496,882307001451069440,Francisco J. Mercado,"SO SO excited bc it's my first paper day!! We use a suite of isolated dwarf galaxy (FIRE) simulations to study stellar metallicity gradients and their origins: <LINK> <LINK> We predict that dwarf galaxies follow a gradient-strength-galaxy-age relationship such that galaxies with older stellar populations tend to have stronger (more negative) stellar metallicity gradients. <LINK> We also use published results for 10 existing Local Group dwarf galaxies to show that they, too, follow a VERY similar gradient-strength-galaxy-age relationship. <LINK> Interestingly, most of these observed galaxies are satellites of the MW while our simulated galaxies are ISOLATED systems... Yet they follow this very similar relationship! This suggests that the environment of a dwarf galaxy likely plays a secondary role in shaping stellar metallicity gradients. Check the paper out to learn about what drives these gradients! <LINK> I dedicate this paper to José A. Flores Velázquez and Perla Maritza Mercado. I wish they were both still here to celebrate with me but I know they're both proud ❤️❤️ It's important to remember that none of this would be possible w/o support from the community around me. My thanks go out to my co-authors especially @jbprime and @jorgito__moreno. And thanks to @DarthLazar for always being willing to answer my endless onslaught of questions! @j_tharindu thanks Tharindu! @astrochicana Muchísimas gracias!! 😊 @astroarianna 💜💜💜 @8minutesold Thank you!! 😃 @ynxmonica Thanks Monica!! 😃 @Naj_Astro Thanks Najmeh!!",https://arxiv.org/abs/2009.01241,"We explore the origin of stellar metallicity gradients in simulated and observed dwarf galaxies. We use FIRE-2 cosmological baryonic zoom-in simulations of 26 isolated galaxies as well as existing observational data for 10 Local Group dwarf galaxies. Our simulated galaxies have stellar masses between $10^{5.5}$ and $10^{8.6} \msun$. Whilst gas-phase metallicty gradients are generally weak in our simulated galaxies, we find that stellar metallicity gradients are common, with central regions tending to be more metal-rich than the outer parts. The strength of the gradient is correlated with galaxy-wide median stellar age, such that galaxies with younger stellar populations have flatter gradients. Stellar metallicty gradients are set by two competing processes: (1) the steady ""puffing"" of old, metal-poor stars by feedback-driven potential fluctuations, and (2) the accretion of extended, metal-rich gas at late times, which fuels late-time metal-rich star formation. If recent star formation dominates, then extended, metal-rich star formation washes out pre-existing gradients from the ""puffing"" process. We use published results from ten Local Group dwarf galaxies to show that a similar relationship between age and stellar metallicity-gradient strength exists among real dwarfs. This suggests that observed stellar metallicity gradients may be driven largely by the baryon/feedback cycle rather than by external environmental effects. ","A Relationship Between Stellar Metallicity Gradients and Galaxy Age in