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1. 27 Open Problems in Kolmogorov Complexity

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   Romashchenko, Andrei; Shen, Alexander; Zimand, Marius (December 2021, ACM SIGACT News)

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2. The Global Higgs Picture at 27 TeV

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   Biekoetter, Anke; Gonçalves, Dorival; Plehn, Tilman; Takeuchi, Michihisa; Zerwas, Dirk (January 2019, SciPost Physics)

   We estimate the reach of global Higgs analyses at a 27 TeV hadroncollider in terms of Higgs couplings and in terms of a gauge-invarianteffective Lagrangian, including invisible Higgs decays and the Higgsself-coupling. The new collider will indirectly probe new physics in theTeV range and allow for a meaningful test of the Higgs self-couplingalso embedded in a global analysis. 

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3. 27 pT Silicon Nitride MEMS Magnetometer for Brain Imaging

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4. Small Cage Uranofullerenes: 27 Years after Their First Observation

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   Gómez‐Torres, Alejandra; Esper, Ronda; Dunk, Paul W.; Morales‐Martínez, Roser; Rodríguez‐Fortea, Antonio; Echegoyen, Luis; Poblet, Josep M. (May 2019, Helvetica Chimica Acta)
5. The Arecibo Pisces Perseus Supercluster Survey: Declination Strip 27

   Ricci, Mariah; Miller, Brendan; Team, APPSS; Team, Undergraduate ALFALFA; Team, ALFALFA (January 2018, American Astronomical Society, AAS Meeting)

   The Arecibo Pisces Perseus Supercluster Survey (APPSS) is an HI survey measuring galaxy infall into the filament and clusters. Galaxies were selected for HI observations based on their location within the Pisces Perseus supercluster and SDSS and GALEX colors predictive of cold gas content. Most of the HI observations were conducted at Arecibo using the L Band Wide receiver, with some high-declination coverage provided by Green Bank. The observations provide increased sensitivity compared to ALFALFA blind survey data. For this project, we investigated a subset of 132 APPSS galaxies with declinations near 27 degrees. Using custom data reduction and analysis tools developed for the Undergraduate ALFALFA Team, we determined the following information for galaxies in our subset: systemic velocity, line width, integrated flux density, HI mass, and gas fraction (or corresponding limits for non-detections). We calculate our HI detection fraction and mean gas fraction as a function of stellar mass and compare to previous results. We investigate the distribution of systemic velocities for our galaxies with their location on the sky. Finally, we discuss several interesting sources from our subset of APPSS galaxies. This work has been supported by NSF grants AST-1211005, AST-1637299, and AST-1637339 

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