CORRELATION BETWEEN IMPAIRMENT AND MOTOR PERFORMANCE DURING REACHING TASKS IN SUBJECTS WITH SPASTIC HEMIPARESIS

Objective: The main purposes of this study were to examine, in subjects with chronic hemiparesis following a stroke: (i) the correlations between tests of muscle tone, stiffness, spasticity, paresis and co-contraction, and (ii) the correlations of these tests and measurements of impairment to upper extremity motor performance. Design: Prospective, cross-sectional, correlation matrix using sample of convenience. Subjects: Thirteen subjects with chronic hemiparesis secondary to a cerebrovascular accident (stroke) were tested. Methods: Subjects were assessed using the Fugl-Meyer Upper Extremity Motor Assessment, modified Ashworth scale, deep tendon reflexes, and muscle characteristics that included quantification of muscle stiffness, paresis and co-contraction during a voluntary reaching task and during passive movements. Surface electromyographic and myotonometric muscle stiffness data were obtained during movement trials. Results: Biceps and triceps brachii muscle paresis and excess biceps brachii co-contraction during voluntary reaching had the highest correlations to decreased motor performance. Muscle tone measurements did not have significant correlations to upper extremity performance. Conclusion: Paresis of elbow flexors and extensors and excess co-contraction of the biceps brachii during voluntary reaching appear to be most predictive of upper extremity motor performance. Results are discussed in relation to the specific challenges these findings pose for spastic paresis clinical management

Galaxy formation in the Planck cosmology - III. The high-redshift universe

We present high-redshift predictions of the star formation rate distribution function (SFRDF), UV luminosity function (UVLF), galactic stellar mass function (GSMF), and specific star formation rates (sSFRs) of galaxies from the latest version of the Munich semi-analytic model L-GALAXIES. We find a good fit to both the shape and normalization of the SFRDF at z = 4–7, apart from a slight underprediction at the low-SFR end at z = 4. Likewise, we find a good fit to the faint number counts for the observed UVLF at brighter magnitudes our predictions lie below the observations, increasingly so at higher redshifts. At all redshifts and magnitudes, the raw (unattenuated) number counts for the UVLF lie above the observations. Because of the good agreement with the SFR we interpret our underprediction as an overestimate of the amount of dust in the model for the brightest galaxies, especially at high redshift. While the shape of our GSMF matches that of the observations, we lie between (conflicting) observations at z = 4–5, and underpredict at z = 6–7. The sSFRs of our model galaxies show the observed trend of increasing normalization with redshift, but do not reproduce the observed mass dependence. Overall, we conclude that the latest version of L-GALAXIES, which is tuned to match observations at z ≤ 3, does a fair job of reproducing the observed properties of galaxies at z ≥ 4. More work needs to be done on understanding observational bias at high redshift, and upon the dust model, before strong conclusions can be drawn on how to interpret remaining discrepancies between the model and observations

Effects of Footwear on Performance in a Barbell Backsquat

Varying philosophies exist on the type of footwear that is most beneficial to wear when strength training. Olympic/power lifters prefer to train in a stiff shoe with a raised heel (0.6-0.75 inches) to provide more stability through the movement. Bodybuilders prefer lifting barefoot or with a minimalist shoe. The purpose of this experiment was to determine the effects that a weightlifting shoe has on peak vertical force, peak vertical power, total center of pressure migration (COP), anterior-posterior (AP) COP migration, and mediolateral (ML) COP migration. Eleven participants, (178.7±7.2 cm and 84.6±15.3 kg) performed barbell back squats while wearing a weightlifting shoe and a running shoe with a minimal drop height. All trials were performed atop a force plate with force and moment data collected at 200 Hz. Participants reported on three separate days for testing. Day one was used to determine 1-RM using a multi-rep test (Brzycki, 1993). Participants then were given 48 hours rest before reporting for the next day. Days two and three were used to collect data kinetic data from a submaximal (70% 1-RM) squat trial while wearing either a weightlifting shoe or running shoe. The same 48 hours rest was given between the two days. Peak vertical force while wearing weightlifting shoes (2096±449 N) was not different than when wearing running shoes (2086±486 N) (t32 =.154, p=.87, d=.015). Similarly, peak vertical power while wearing weightlifting shoes (30.7±19.6 W) was not different than when wearing running shoes (31.1±23.4 W) (t32 =-.12, p=.9, d=.01). Wearing running shoes decreased total migration of the COP (0.61±0.18 m) by 34% from the weightlifting shoe (0.93±0.67 m) (t32 = 2.82, p=.008, d=.45). Likewise, AP COP migration wearing the running shoes (0.35±0.13 m) was reduced by 51% compared to using the weightlifting shoe (0.71±0.73 m) (t32 = 2.96, p=.005, d=.47). As indicated by Cohen’s d, approximately 45% of the reduction in COP migrations was accounted for by shoe type. These data suggest that use of a flatter, less stable shoe resulted in more stable body position throughout the squat exercise. Less body sway during the movement may produce a more effective lifting technique that minimizes the risk of injury

Quantifying the UV-continuum slopes of galaxies to z ˜ 10 using deep Hubble+Spitzer/IRAC observations

Measurements of the UV-continuum slopes β provide valuable information on the physical properties of galaxies forming in the early universe, probing the dust reddening, age, metal content, and even the escape fraction. While constraints on these slopes generally become more challenging at higher redshifts as the UV-continuum shifts out of the Hubble Space Telescope bands (particularly at z > 7), such a characterization actually becomes abruptly easier for galaxies in the redshift window z = 9.5-10.5 due to the Spitzer/Infrared Array Camera 3.6 μm-band probing the rest-UV continuum and the long wavelength baseline between this Spitzer band and the Hubble Hf160w band. Higher S/N constraints on β are possible at z ˜ 10 than at z = 8. Here, we take advantage of this opportunity and five recently discovered bright z = 9.5-10.5 galaxies to present the first measurements of the mean β for a multi-object sample of galaxy candidates at z ˜ 10. We find the measured βobs's of these candidates are -2.1 ± 0.3 ± 0.2 (random and systematic), only slightly bluer than the measured β's (βobs ≈ -1.7) at 3.5 < z < 7.5 for galaxies of similar luminosities. Small increases in the stellar ages, metallicities, and dust content of the galaxy population from z ˜ 10 to z ˜ 7 could easily explain the apparent evolution in β

Landscape Values and Aesthetic Preferences Across the Front Range

Boulder’s Open Space and Mountain Parks (OSMP) lands are managed to provide a diverse set of benefits valued by Boulder’s residents as well as tourists. Not all OSMP lands provide the same set of benefits however. Understanding how the values associated with OSMP lands vary across the region can provide managers with insights into how best to allocate resources so that they yield the maximum public benefit. In addition to an understanding of the values visitors associate with OSMP lands, management can benefit from knowledge of how different features of the landscape impact user experiences, both positively and negatively

Aesthetic Characteristics of the Front Range: An Analysis of Viewsheds Provided by Boulder OSMP Lands

The city of Boulder’s Open Space and Mountain Parks (OSMP) lands offer residents and visitors a variety of unique recreational, scenic, and cultural experiences that are often captured and shared publicly via social media. Given the diversity of OSMP lands, visitor experiences likely differ based on the aesthetic and biophysical features that can be viewed from these landscapes. For instance, the peaks of the iconic Flatirons provide visitors with different scenic views than the low-lying grasslands in the southeastern area of the city. Furthermore, visitor use and enjoyment of OSMP lands could be directly related to the landscape features that are visible from these different locations. Understanding how visible landscape features vary across OSMP lands can help managers target their planning efforts to improve the quality of outdoor recreation experiences, and potentially identify new locations for outdoor recreation infrastructure (e.g., trails, pavilions, etc.) that offer the ability to see the regions most desirable landscape features. This study: (1) identifies points in the landscape where users are often inspired to take photographs; (2) maps the landscapes most often viewed by visitors; (3) summarizes the types of landscape features viewed from OSMP lands; and (4) determines how these landscape features vary across LCAs

Detailed dust modelling in the L-Galaxies semi-analytic model of galaxy formation

We implement a detailed dust model into the L-Galaxies semi-analytical model which includes: injection of dust by type II and type Ia supernovae (SNe) and AGB stars; grain growth in molecular clouds; and destruction due to supernova-induced shocks, star formation, and reheating. Our grain growth model follows the dust content in molecular clouds and the inter-cloud medium separately, and allows growth only on pre-existing dust grains. At early times, this can make a significant difference to the dust growth rate. Above z ∼ 8, type II SNe are the primary source of dust, whereas below z ∼ 8, grain growth in molecular clouds dominates, with the total dust content being dominated by the latter below z ∼ 6. However, the detailed history of galaxy formation is important for determining the dust content of any individual galaxy. We introduce a fit to the dust-to-metal (DTM) ratio as a function of metallicity and age, which can be used to deduce the DTM ratio of galaxies at any redshift. At z ≲ 3, we find a fairly flat mean relation between metallicity and the DTM, and a positive correlation between metallicity and the dust-to-gas (DTG) ratio, in good agreement with the shape and normalisation of the observed relations. We also match the normalisation of the observed stellar mass – dust mass relation over the redshift range of 0 − 4, and to the dust mass function at z = 0. Our results are important in interpreting observations on the dust content of galaxies across cosmic time, particularly so at high redshift

Serological diagnosis of North American paragonimiasis by western blot using Paragonimus kellicotti adult worm antigen

We studied the value of an IgG Western blot (WB) with Paragonimus kellicotti (Pk) antigen for diagnosis of North American paragonimiasis. The test was evaluated with sera from patients with Pk and Paragonimus westermani infections, with control sera from patients with other helminth infections, and sera from healthy Americans. All 11 proven Pk infection sera and two samples from suspected cases that were negative by P. westermani WB at the Centers for Disease Control and Prevention (CDC) contained antibodies to antigens at 34 kDa and at 21/23 kDa. Seven of 7 P. westermani sera contained antibodies to the 34 kDa antigen, but only 2 recognized the 21/23 kDa doublet. No control samples were reactive with these antigens. Antibody reactivity declined after praziquantel treatment. Thus, the P. kellicotti WB appears to be superior to P. westermani WB for diagnosing Pk infections, and it may be useful for assessing responses to treatment

Rotating black hole orbit functionals in the frequency domain

In many astrophysical problems, it is important to understand the behavior of functions that come from rotating (Kerr) black hole orbits. It can be particularly useful to work with the frequency domain representation of those functions, in order to bring out their harmonic dependence upon the fundamental orbital frequencies of Kerr black holes. Although, as has recently been shown by W. Schmidt, such a frequency domain representation must exist, the coupled nature of a black hole orbit's $r$ and $\theta$ motions makes it difficult to construct such a representation in practice. Combining Schmidt's description with a clever choice of timelike coordinate suggested by Y. Mino, we have developed a simple procedure that sidesteps this difficulty. One first Fourier expands all quantities using Mino's time coordinate $\lambda$. In particular, the observer's time $t$ is decomposed with $\lambda$. The frequency domain description is then built from the $\lambda$-Fourier expansion and the expansion of $t$. We have found this procedure to be quite simple to implement, and to be applicable to a wide class of functionals. We test the procedure using a simple test function, and then apply it in a particularly interesting case, the Weyl curvature scalar $\psi_4$ used in black hole perturbation theory.Comment: 16 pages, 2 figures. Submitted to Phys Rev D. New version gives a vastly improved algorithm due to Drasco for computing the Fourier transforms. Drasco has been added as an author. Also fixed some references and exterminated a small herd of typos; final published versio

Twelve-month prevalence of haemarthrosis and joint disease using the Haemophilia Joint Health score: evaluation of the UK National Haemophilia Database and Haemtrack patient reported data: an observational study

Objectives: To report the 12-month prevalence of joint bleeds from the National Haemophilia Database (NHD) and Haemtrack, a patient-reported online treatment diary and concurrent joint disease status using the haemophilia joint health score (HJHS) at individual joint level, in children and adults with severe haemophilia A and B (HA/HB) without a current inhibitor. Design: A 2018 retrospective database study of NHD from which 2238 cases were identified, 463 patients had fully itemised HJHS of whom 273 were compliant in recording treatment using Haemtrack. Setting: England, Wales and Scotland, UK. Participants: Children (<18 years) and adults (≥18 years) with severe HA and HB (factor VIII/factor IX, <0.01 iu/mL) without a current inhibitor. Primary and secondary outcomes: Prevalence of joint haemarthrosis and concurrent joint health measured using the HJHS. Results: The median (IQR) age of children was 10 (6-13) and adults 40 (29-50) years. Haemarthrosis prevalence in HA/HB children was 33% and 47%, respectively, and 60% and 42%, respectively, in adults. The most common site of haemarthrosis in children was the knee in HA and ankle in HB. In adults, the incidence of haemarthrosis at the ankles and elbows was equal. The median total HJHS in HA/HB children was 0 and in adults with HA/HB, were 18 and 11, respectively. In adults with HA/HB, the median ankle HJHS of 4.0 was higher than the median HJHS of 1.0 for both the knee and elbow. Conclusion: Despite therapeutic advances, only two-thirds of children and one-third of adults were bleed-free, even in a UK cohort selected for high compliance with prophylaxis. The median HJHS of zero in children suggests joint health is relatively unaffected during childhood. In adults, bleed rates were highest in ankles and elbows, but the ankles led to substantially worse joint health scores