text: 15,94,1063100286686781441,14975979,Abhimat Gautam,"Here’s a really brief summary thread of my work and results. Check out the paper for full details behind these results and graphs: <LINK> We developed some new techniques to get precise stellar photometry from adaptive optics images of the Galactic center! (1/4) <LINK> With the precise photometry, we found that roughly half of all stars in our sample are variable over the 11.5 years of our experiment! (2/4) <LINK> We recovered the two known young eclipsing binary star systems at the Galactic center, and put a tight lower limit on the eclipsing binary fraction at the Galactic center. (3/4) <LINK> We discovered a new periodic variable at the Galactic center, with a roughly 39 day period! Figuring out what is causing this variability still requires a little more work! (4/4) <LINK>",https://arxiv.org/abs/1811.04898,"We present a $\approx 11.5$ year adaptive optics (AO) study of stellar variability and search for eclipsing binaries in the central $\sim 0.4$ pc ($\sim 10''$) of the Milky Way nuclear star cluster. We measure the photometry of 563 stars using the Keck II NIRC2 imager ($K'$-band, $\lambda_0 = 2.124 \text{ } \mu \text{m}$). We achieve a photometric uncertainty floor of $\Delta m_{K'} \sim 0.03$ ($\approx 3\%$), comparable to the highest precision achieved in other AO studies. Approximately half of our sample ($50 \pm 2 \%$) shows variability. $52 \pm 5\%$ of known early-type young stars and $43 \pm 4 \%$ of known late-type giants are variable. These variability fractions are higher than those of other young, massive star populations or late-type giants in globular clusters, and can be largely explained by two factors. First, our experiment time baseline is sensitive to long-term intrinsic stellar variability. Second, the proper motion of stars behind spatial inhomogeneities in the foreground extinction screen can lead to variability. We recover the two known Galactic center eclipsing binary systems: IRS 16SW and S4-258 (E60). We constrain the Galactic center eclipsing binary fraction of known early-type stars to be at least $2.4 \pm 1.7\%$. We find no evidence of an eclipsing binary among the young S-stars nor among the young stellar disk members. These results are consistent with the local OB eclipsing binary fraction. We identify a new periodic variable, S2-36, with a 39.43 day period. Further observations are necessary to determine the nature of this source. ",An Adaptive Optics Survey of Stellar Variability at the Galactic Center,4,"['Here’s a really brief summary thread of my work and results. Check out the paper for full details behind these results and graphs: <LINK>\n\nWe developed some new techniques to get precise stellar photometry from adaptive optics images of the Galactic center!\n(1/4) <LINK>', 'With the precise photometry, we found that roughly half of all stars in our sample are variable over the 11.5 years of our experiment!\n(2/4) https://t.co/ZVCU7S4NnI', 'We recovered the two known young eclipsing binary star systems at the Galactic center, and put a tight lower limit on the eclipsing binary fraction at the Galactic center.\n(3/4) https://t.co/kzHKOuO81e', 'We discovered a new periodic variable at the Galactic center, with a roughly 39 day period! Figuring out what is causing this variability still requires a little more work!\n(4/4) https://t.co/DaoCW3yV3G']",18,11,788