A Comparison of Materials in Knee Sleeves for Osteoarthritis: Affects and Function

Limited research has been done on specific materials in knee sleeves and the impact on the knee sleeve effectiveness. PURPOSE: The purpose of this study is to investigate the different types of materials in knee sleeves used for managing knee osteoarthritis symptoms. Neoprene, nylon-spandex, and copper infused knee sleeves used to determine which material is the most effective in managing osteoarthritis symptoms. METHODS: Four males and four females (age= 37.6±11.6 yrs, ht=167.9±10.9 cm, wt=69.1±33.4 kg, %BF= 33.7±12.1kg) participated in four randomly assigned trials: Trial 1 was completed without wearing any knee sleeves and trials 2-4 were completed wearing a knee sleeve. Repeated measures ANOVAs were used to examine the effect of knee swelling, pain, range of motion (ROM), balance, walk time, step counts, and average torque power. Alpha was set at .05 for all tests. RESULTS: No significant differences were found in knee swelling, pain, range of motion (ROM), balance, walk time, step counts, and average torque power between the four conditions (no sleeve, neoprene, spandex, and copper compression © sleeves), p\u3e.05. CONCLUSIONS: These findings suggest that knee sleeves do not influence knee swelling, pain, range of motion (ROM), balance, walk time, step counts, and average torque power in knee osteoarthritis. This research was funded by the A&M-SA College of Education and Human Development’s Student Research Grant

Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev–Zel’dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at - + -h2.4 Mpc0.4 0.3 1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr

Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

International audienceWe measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at ${2.4}_{-0.4}^{+0.3}\,\mathrm{Mpc}\,{h}^{-1}$ . We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr