We present theoretical expectations for infall toward superclusterscale cosmological filaments, motivated by the Arecibo Pisces–Perseus Supercluster Survey (APPSS) to map the velocity field around the Pisces–Perseus Supercluster (PPS) filament. We use a minimum spanning tree applied to dark matter halos the size of galaxy clusters to identify 236 large filaments within the Millennium simulation. Stacking the filaments along their principal axes, we determine a welldefined, sharppeaked velocity profile function that can be expressed in terms of the maximum infall rate
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Abstract V _{max}and the distanceρ _{max}between the location of maximum infall and the principal axis of the filament. This simple, twoparameter functional form is surprisingly universal across a wide range of linear mass densities.V _{max}is positively correlated with the halo mass per length along the filament, andρ _{max}is negatively correlated with the degree to which the halos are concentrated along the principal axis. We also assess an alternative, singleparameter method usingV _{25}, the infall rate at a distance of 25 Mpc from the axis of the filament. Filaments similar to the PPS have 116 km s^{−1}, ${V}_{\mathrm{max}}=612\phantom{\rule{0.33em}{0ex}}\pm $ Mpc, and ${\rho}_{\mathrm{max}}=8.9\pm 2.1$V _{25}= 329 ± 68 km s^{−1}. We create mock observations to model uncertainties associated with viewing angle, lack of threedimensional velocity information, limited sample size, and distance uncertainties. Our results suggest that it would be especially useful to measure infall for a larger sample of filaments to test our predictions for the shape of the infall profile and the relationships among infall rates and filament properties. 
Tao, Liu ; KelleyDerzon, Jessica ; Green, Anna_C ; Fulda, Paul ( , Optics Letters)
This paper analytically and numerically investigates misalignment and modemismatchinduced power coupling coefficients and losses as a function of Hermite–Gauss (HG) mode order. We show that higherorder HG modes are more susceptible to beam perturbations when, for example, coupling into optical cavities: the misalignment and modemismatchinduced power coupling losses scale linearly and quadratically with respect to the mode indices, respectively. As a result, the modemismatch tolerance for the
${\mathrm{H}\mathrm{G}}_{3,3}$ mode is reduced to a factor of 0.28 relative to the currently used${\mathrm{H}\mathrm{G}}_{0,0}$ mode. This is a potential hurdle to using higherorder modes to reduce thermal noise in future gravitationalwave detectors.