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Background Experience of stroke is associated with an increased risk for diabetes and metabolic syndrome, yet few interventions exist that have been tailored to the population's unique needs. Purpose To examine adherence and efficacy of the Diabetes Prevention Program Group Lifestyle Balance program (DPP-GLB) modified for individuals post stroke (GLB-CVA) using a randomized controlled trial. Methods Adults (18–85 years of age), >12 months post stroke, and body mass index ≥25 kg/m2 were included in this study. Sixty-five individuals were assigned to either the GLB-CVA intervention or a 6-month wait-list control. Participants completed the 12-month GLB-CVA intervention, with attendance and assessment of weight, anthropometric, biomarker, functional, and patient reported outcome data collected at baseline, 3, 6, and 12 months. Results High attendance (90%) and dietary and activity tracking (71%) suggest high adherence to the 12-month GLB-CVA. Six-month randomized controlled trial data indicate significant weight loss (p =.005) in the GLB-CVA group (7.4 ± 13.6 lbs, 3.65%) compared with the wait-list control (0.1 ± 10.1 lbs, 0%), and improvements in arm circumference (p =.04), high-density lipoprotein (HDL) cholesterol (p =.028), 8-year diabetes risk (p =.011), and pain interference (p <.001). Combined 12-month data showed participants lost 10.1 ± 16.8 lbs (4.88%) and improved waist circumference (p =.001), HbA1c (3.6%), diastolic blood pressure (p <.001), pain (p =.001), social participation (p =.025), and eating practices (p =.01) and habits (p <.001). Conclusions Engagement in the GLB-CVA can result in weight loss and improved health for individuals who are overweight or obese following stroke. Future efforts should examine effectiveness in real-world settings and focus on knowledge translation efforts. [ABSTRACT FROM AUTHOR]

We use the Galaxy and Mass Assembly (GAMA) and the Deep Extragalactic Visible Legacy Survey (DEVILS) observational data sets to calculate the cosmic star formation rate (SFR) and active galactic nuclei (AGN) bolometric luminosity history (CSFH/CAGNH) over the last 12.5 billion years. SFRs and AGN bolometric luminosities were derived using the spectral energy distribution fitting code ProSpect , which includes an AGN prescription to self-consistently model the contribution from both AGN and stellar emission to the observed rest-frame ultra-violet to far-infrared photometry. We find that both the CSFH and CAGNH evolve similarly, rising in the early Universe up to a peak at look-back time ≈10 Gyr (z ≈ 2), before declining towards the present day. The key result of this work is that we find the ratio of CAGNH to CSFH has been flat (⁠|$\approx 10^{42.5}\, \mathrm{erg \, s^{-1}\, {\rm M}_{\odot }^{-1}\, yr}$|⁠) for 11 Gyr up to the present day, indicating that star formation and AGN activity have been coeval over this time period. We find that the stellar masses of the galaxies that contribute most to the CSFH and CAGNH are similar, implying a common cause, which is likely gas inflow. The depletion of the gas supply suppresses cosmic star formation and AGN activity equivalently to ensure that they have experienced similar declines over the last 10 Gyr. These results are an important milestone for reconciling the role of star formation and AGN activity in the life cycle of galaxies. [ABSTRACT FROM AUTHOR]

We determine the atomic hydrogen (H  i) to halo mass relation (HIHM) using Arecibo Legacy Fast ALFA survey H  i data at the location of optically selected groups from the Galaxy And Mass Assembly (GAMA) survey. We make direct H  i detections for 37 GAMA groups. Using H  i group spectral stacking of 345 groups, we study the group H  i content as a function of halo mass across a halo mass range of 1011–1014.7 M⊙. We also correct our results for Eddington bias. We find that the group H  i mass generally rises as a function of halo mass from 1.3% of the halo mass at |$10^{11.6} \, \text{M}_\odot$| to 0.4% at |$10^{13.7} \, \text{M}_\odot$| with some indication of flattening towards the high-mass end. Despite the differences in optical survey limits, group catalogues, and halo mass estimation methods, our results are consistent with previous group H  i -stacking studies. Our results are also consistent with mock observations from shark and IllustrisTNG. [ABSTRACT FROM AUTHOR]

We present a revised measurement of the extragalactic background light (EBL) at radio frequencies based on a near complete compendium of radio source counts. We present the radio-EBL at 150 MHz, 325 MHz, 610 MHz, 1.4 GHz, 3 GHz, 5 GHz, and 8.4 GHz. In all cases the contribution to the radio-EBL, per decade of flux, exhibits a two-humped distribution well matched to the active galactic nucleus (AGN) and star-forming galaxy (SFG) populations, and with each population contributing roughly equal energy. Only at 3 GHz are the source count contributions to the EBL fully convergent, and hence we report empirical lower limits to the radio-EBL in the remaining bands. Adopting predictions from the SHARK semi-analytic model for the form of the SFG population, we can fit the fainter source counts providing measurements of the total contribution to the radio-EBL for the SFG and the AGN populations separately. This constitutes an empirically constrained model-dependent measurement for the SFG contribution, but a fully empirical measurement of the AGN contribution. Using the ProSpect spectral energy distribution code we can model the ultraviolet-optical-infrared-mm-radio SFG EBL at all frequencies from the cosmic star-formation history and the adoption of a Chabrier initial mass function. However, significant discrepancy remains (5 ×) between our source-count estimates of the radio-EBL and the direct measurements reported from the Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission-2 (ARCADE-2) experiment. We can rule out a significant missing discrete source radio population and suggest that the cause of the high ARCADE-2 radio-EBL values may need to be sought either in the foreground subtraction or as a yet unknown diffuse component in the radio sky. [ABSTRACT FROM AUTHOR]

Background Obesity after traumatic brain injury (TBI) is a public health issue and no evidence-based weight loss interventions exist to meet the unique needs of individuals after TBI. Purpose To (a) examine the efficacy of the Diabetes Prevention Program Group Lifestyle Balance for TBI (GLB-TBI) weight-loss intervention compared to an attention control for primary (weight-loss) and secondary health outcomes; (b) determine participant compliance with the GLB-TBI; and (c) determine if compliance is associated with improved outcomes. Methods Individuals with moderate to severe TBI, age 18–64 years, ≥6 months postinjury, and body mass index of ≥25 kg/m2 were randomized to a 12-month, 22-session GLB-TBI intervention or attention control condition. Weight-loss (lbs.), anthropometric, biomarkers, and patient-reported outcomes were collected at baseline, 3, 6, and 12 months. Results The GLB-TBI group (n = 27) lost 17.8 ± 41.4lbs (7.9%) over the 12-month program and the attention control group (n = 27) lost 0 ± 55.4lbs (0%). The GLB-TBI group had significant improvements in diastolic blood pressure, triglycerides, and HDL cholesterol. GLB-TBI attendance was 89.6% and weekly self-monitoring of diet and activity was 68.8%. Relative to baseline, the GLB-TBI compliant group (≥80% attendance; ≥85% self-monitoring; n = 10) had a statistically significant decrease in weight at each assessment, the noncompliant group had a significant decrease between 6 and 12 months (n = 17), with no change in weight in the attention control group (n = 27). Conclusions Findings suggest for adults with TBI who are overweight or obese, participation in the GLB-TBI can significantly reduce weight and metabolic risk factors and increase self-reported habits for diet and exercise. [ABSTRACT FROM AUTHOR]

We construct the halo mass function (HMF) from the GAMA (Galaxy And Mass Assembly) galaxy group catalogue over the mass range of 1012.7–1015.5 M⊙, and find good agreement with the expectation from Lambda cold dark matter. In comparison to previous studies, this result extends the mass range over which the HMF has now been measured over by an order of magnitude. We combine the GAMA data release (DR) 4 HMF with similar data from the Sloan Digital Sky Survey (SDSS) DR12 and REFLEX II (ROSAT -ESO Flux Limited X-ray Galaxy Cluster Survey) surveys, and fit a four-parameter Murray–Robotham–Power function, valid at |$\tilde{z} \approx 0.1$|⁠ , yielding a density normalization of log10 (ϕ* Mpc |$^{3})= -3.96^{+0.55}_{-0.82}$|⁠ , a high mass turnover of log10 (M * M |$_{\odot }^{-1})=14.13^{+0.43}_{-0.40}$|⁠ , a low-mass power-law slope of |$\alpha =-1.68^{+0.21}_{-0.24}$|⁠ , and a high-mass softening parameter of |$\beta =0.63^{+0.25}_{-0.11}$|⁠. If we fold in the constraint on ΩM from the Planck 2018 cosmology, we are able to reduce these uncertainties further, but this relies on the assumption that the power-law trend can be extrapolated from 1012.7 M⊙ to zero mass. Throughout, we highlight the effort needed to improve on our HMF measurement: improved halo mass estimates that do not rely on calibration to simulations; reduced halo mass uncertainties needed to mitigate the strong Eddington bias that arises from the steepness of the HMF low-mass slope; and deeper wider area spectroscopic surveys. To our halo mass limit of 1012.7 M⊙, we are directly resolving ('seeing') 41 ± 5 per cent of the total mass density, i.e. ΩM,>12.7 = 0.128 ± 0.016, opening the door for the direct construction of three-dimensional dark matter mass maps at Mpc resolution. [ABSTRACT FROM AUTHOR]

We present a complete structural analysis of the ellipticals (E), diffuse bulges (dB), compact bulges (cB), and discs (D) within a redshift range 0 < z < 1, and stellar mass log10(M*/M⊙) ≥ 9.5 volume-limited sample drawn from the combined DEVILS and HST -COSMOS region. We use the profit code to profile over ∼35 000 galaxies for which visual classification into single or double component was pre-defined in Paper-I. Over this redshift range, we see a growth in the total stellar mass density (SMD) of a factor of 1.5. At all epochs we find that the dominant structure, contributing to the total SMD, is the disc, and holds a fairly constant share of |$\sim 60{{\ \rm per\ cent}}$| of the total SMD from z  = 0.8 to z  = 0.2, dropping to |$\sim 30{{\ \rm per\ cent}}$| at z  = 0.0 (representing |$\sim 33{{\ \rm per\ cent}}$| decline in the total disc SMD). Other classes (E, dB, and cB) show steady growth in their numbers and integrated stellar mass densities. By number, the most dramatic change across the full mass range is in the growth of diffuse bulges. In terms of total SMD, the biggest gain is an increase in massive elliptical systems, rising from 20 per cent at z  = 0.8 to equal that of discs at z  = 0.0 (30 per cent) representing an absolute mass growth of a factor of 2.5. Overall, we see a clear picture of the emergence and growth of all three classes of spheroids over the past 8 Gyr, and infer that in the later half of the Universe's timeline spheroid-forming processes and pathways (secular evolution, mass-accretion, and mergers) appear to dominate mass transformation over quiescent disc growth. [ABSTRACT FROM AUTHOR]

In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift sample. This includes 248 682 galaxy spectra, and, in combination with earlier surveys, results in 330 542 redshifts across five sky regions covering ∼250 deg2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to r KiDS = 19.65 mag), and is well-suited for the study of galaxy mergers, galaxy groups, and the low redshift (z  < 0.25) galaxy population. DR4 includes 32 value-added tables or Data Management Units (DMUs) that provide a number of measured and derived data products including GALEX , ESO KiDS, ESO VIKING, WISE , and Herschel Space Observatory imaging. Within this release, we provide visual morphologies for 15 330 galaxies to z  < 0.08, photometric redshift estimates for all 18 million objects to r KiDS ∼ 25 mag, and stellar velocity dispersions for 111 830 galaxies. We conclude by deriving the total galaxy stellar mass function (GSMF) and its sub-division by morphological class (elliptical, compact-bulge and disc, diffuse-bulge and disc, and disc only). This extends our previous measurement of the total GSMF down to 106.75 M |$_{\odot } \, h_{70}^{-2}$| and we find a total stellar mass density of ρ * = (2.97 ± 0.04) × 108 M |$_{\odot } \, h_{70}$|  Mpc−3 or |$\Omega _*=(2.17 \pm 0.03) \times 10^{-3} \, h_{70}^{-1}$|⁠. We conclude that at z  < 0.1, the Universe has converted 4.9 ± 0.1 per cent of the baryonic mass implied by big bang Nucleosynthesis into stars that are gravitationally bound within the galaxy population. [ABSTRACT FROM AUTHOR]

Using high-resolution Hubble Space Telescope imaging data, we perform a visual morphological classification of ∼36 000 galaxies at z < 1 in the deep extragalactic visible legacy survey/cosmological evolution survey region. As the main goal of this study, we derive the stellar mass function (SMF) and stellar mass density (SMD) sub-divided by morphological types. We find that visual morphological classification using optical imaging is increasingly difficult at z > 1 as the fraction of irregular galaxies and merger systems (when observed at rest-frame UV/blue wavelengths) dramatically increases. We determine that roughly two-thirds of the total stellar mass of the Universe today was in place by z ∼ 1. Double-component galaxies dominate the SMD at all epochs and increase in their contribution to the stellar mass budget to the present day. Elliptical galaxies are the second most dominant morphological type and increase their SMD by ∼2.5 times, while by contrast, the pure-disc population significantly decreases by |$\sim 85{{\ \rm per\ cent}}$|⁠. According to the evolution of both high- and low-mass ends of the SMF, we find that mergers and in situ evolution in discs are both present at z < 1, and conclude that double-component galaxies are predominantly being built by the in situ evolution in discs (apparent as the growth of the low-mass end with time), while mergers are likely responsible for the growth of ellipticals (apparent as the increase of intermediate/high-mass end). [ABSTRACT FROM AUTHOR]

Primary Objective: To discuss the biopsychosocial factors that affect being overweight or obese after acquired brain injury (ABI) Research Design: Narrative review Methods and Procedures: Based on the biopsychosocial model, we discuss the unique injury-specific factors that can affect bring overweight or obese among individuals with ABI including: (1) biological, (2) psychological and (3) social/ecological factors. Main Outcomes and Results: Injury-specific factors that impact being overweight or obese following ABI include endocrine dysfunction, pain, bowel and bladder incontinence, balance problems and motor impairment, medications, sleep quality and fatigue, alcohol and tobacco use, psychological disorders and symptoms, cognitive changes, social support, isolation, participation, transportation, independence, and knowledge. These factors may also compound general factors impacting weight management, making it difficult for individuals with ABI to maintain a healthy lifestyle. Conclusions: It is important to recognize the biopsychosocial factors that impact weight-loss and lifestyle change after ABI so that interventions can be tailored to meet individuals' unique needs. Empirical research is needed to better understand how biopsychosocial factors interact and impact overweight/ obesity after ABI. [ABSTRACT FROM AUTHOR]

Using high-resolution Hubble Space Telescope imaging data, we perform a visual morphological classification of ∼36 000 galaxies at z < 1 in the deep extragalactic visible legacy survey/cosmological evolution survey region. As the main goal of this study, we derive the stellar mass function (SMF) and stellar mass density (SMD) sub-divided by morphological types. We find that visual morphological classification using optical imaging is increasingly difficult at z > 1 as the fraction of irregular galaxies and merger systems (when observed at rest-frame UV/blue wavelengths) dramatically increases. We determine that roughly two-thirds of the total stellar mass of the Universe today was in place by z ∼ 1. Double-component galaxies dominate the SMD at all epochs and increase in their contribution to the stellar mass budget to the present day. Elliptical galaxies are the second most dominant morphological type and increase their SMD by ∼2.5 times, while by contrast, the pure-disc population significantly decreases by |$\sim 85{{\ \rm per\ cent}}$|⁠. According to the evolution of both high- and low-mass ends of the SMF, we find that mergers and in situ evolution in discs are both present at z < 1, and conclude that double-component galaxies are predominantly being built by the in situ evolution in discs (apparent as the growth of the low-mass end with time), while mergers are likely responsible for the growth of ellipticals (apparent as the increase of intermediate/high-mass end). [ABSTRACT FROM AUTHOR]

We present the first look at star formation histories of galaxy components using ProFuse , a new technique to model the 2D distribution of light across multiple wavelengths using simultaneous spectral and spatial fitting of purely imaging data. We present a number of methods to classify galaxies structurally/morphologically, showing the similarities and discrepancies between these schemes. We show the variation in componentwise mass functions that can occur simply due to the use of a different classification method, which is most dramatic in separating bulges and spheroids. Rather than identifying the best-performing scheme, we use the spread of classifications to quantify uncertainty in our results. We study the cosmic star formation history (CSFH), forensically derived using ProFuse with a sample of ∼7000 galaxies from the Galaxy And Mass Assembly survey. Remarkably, the forensic CSFH recovered via both our method (ProFuse) and traditional Spectral Energy Distribution (SED) fitting (ProSpect) are not only exactly consistent with each other over the past 8 Gyr, but also with the in situ CSFH measured using ProSpect. Furthermore, we separate the CSFH by contributions from spheroids, bulges, and discs. While the vast majority (70 per cent) of present-day star formation takes place in the disc population, we show that 50 per cent of the stars that formed at cosmic noon (8–12 Gyr ago) now reside in spheroids, and present-day bulges are composed of stars that were primarily formed in the very early Universe, with half their stars already formed ∼12 Gyr ago. [ABSTRACT FROM AUTHOR]

BACKGROUND: Problem-Solving Training (PST) during inpatient rehabilitation could provide care partners the skills needed to manage their life roles after discharge. OBJECTIVE: Determine the feasibility of PST+ Education versus Education for care partners of adults with traumatic brain injury (TBI) during inpatient rehabilitation. METHODS: We conducted a multisite randomized feasibility trial across three sites. We present recruitment rates, reasons for refusal to participate, and reasons for non-completion of interventions. We measured client satisfaction, participant engagement, and fidelity for both interventions. We compared change in depressive symptoms and caregiver burden between PST and Education groups. RESULTS: Though the interventions were generally feasible, recruitment and retention rates were lower than anticipated largely due to the COVID-19 pandemic. Participants who completed >3 sessions were less likely to be employed full-time and more often spouses and co-residing. Length of inpatient rehabilitation stay was correlated with number of sessions completed. We observed potential benefits of PST over Education, specifically for reducing depression symptoms and caregiver burden. CONCLUSION: High satisfaction, engagement, and fidelity, overall recruitment and retention, and positive change in outcomes suggest that PST is generally feasible and beneficial for care partners of persons with TBI. Adaptations, such as developing a 3-session version of PST, could improve feasibility. [ABSTRACT FROM AUTHOR]

The tight relationship between infrared luminosity (L TIR) and 1.4 GHz radio continuum luminosity (⁠|$L_\mathrm{1.4\, GHz}$|⁠) has proven useful for understanding star formation free from dust obscuration. Infrared emission in star-forming galaxies typically arises from recently formed, dust-enshrouded stars, whereas radio synchrotron emission is expected from subsequent supernovae. By leveraging the wealth of ancillary far-ultraviolet – far-infrared photometry from the Deep Extragalactic VIsible Legacy Survey and Galaxy and Mass Assembly surveys, combined with 1.4 GHz observations from the Meer Karoo Array Telescope International GHz Tiered Extragalactic Exploration survey and Deep Investigation of Neutral Gas Origin projects, we investigate the impact of time-scale differences between far-ultraviolet – far-infrared and radio-derived star formation rate (SFR) tracers. We examine how the spectral energy distribution (SED)-derived star formation histories (SFHs) of galaxies can be used to explain discrepancies in these SFR tracers, which are sensitive to different time-scales. Galaxies exhibiting an increasing SFH have systematically higher L TIR and SED-derived SFRs than predicted from their 1.4 GHz radio luminosity. This indicates that insufficient time has passed for subsequent supernovae-driven radio emission to accumulate. We show that backtracking the SFR(t) of galaxies along their SED-derived SFHs to a time several hundred megayears prior to their observed epoch will both linearize the SFR– |$L_\mathrm{1.4\, GHz}$| relation and reduce the overall scatter. The minimum scatter in the SFR(t)– |$L_\mathrm{1.4\, GHz}$| is reached at 200 – 300 Myr prior, consistent with theoretical predictions for the time-scales required to disperse the cosmic ray electrons responsible for the synchrotron emission. [ABSTRACT FROM AUTHOR]

Objective: The purposes were to (1) describe the prevalence of clinical profiles and modifiers, (2) examine the association between clinical profiles and prolonged recovery, and (3) examine the interaction between clinical profiles and modifiers and prolonged recovery in adolescents with sport-related concussion (SRC). Design: Retrospective, cross-sectional. Setting: Interdisciplinary specialty sports concussion clinic. Patients: Patients (n = 299) aged 12 to 19 years who were diagnosed with SRC within 30 days of injury. Independent Variables: Clinical profiles and modifiers were decided by the clinical judgment of the clinical neuropsychologist and sports medicine physician, using data from the Clinical Profile Screen and information gathered from the clinical interview, neurocognitive, and vestibular and ocular motor testing. Main Outcome Measures: Prolonged recovery was defined as ≥28 days from the date of injury to the date of clearance. Results: The most common clinical profiles were migraine (34.8%) and cognitive–fatigue (23.4%). There were no significant relationships between clinical profiles and prolonged recovery (Wald = 5.89, df = 4, P = 0.21). The presence of a modifier did not significantly affect the relationship between clinical profiles and prolonged recovery (x²= 6.5, df = 5, P = 0.26). The presence of any modifier yielded a 10-day increase in median recovery time within the cognitive/fatigue clinical profile (Wilcoxon rank-sum = 268.5, P = 0.01). Conclusions: Although patients with a clinical profile and modifier may not experience prolonged recovery, they may experience longer recovery time than patients with a clinical profile and no modifier. [ABSTRACT FROM AUTHOR]

To describe the safety, feasibility, and tolerability of overground exoskeleton gait training (OEGT) integrated into clinical practice for patients after severe acquired brain injury (ABI). Inpatient rehabilitation hospital. Eligible patients with severe ABI met the following criteria: age > 18, medically stable, met exoskeleton frame limitations, and a score of ≤ 3 on the motor function portion of the Coma Recovery Scale – Revised (CRS-R). Presence of consciousness disorder was not exclusionary. Prospective observational study. Outcomes examined safety (adverse events), feasibility (session count and barriers to session completion), and tolerability of OEGT (session metrics and heart rate). Ten patients with ABI completed 10.4 ± 4.8 OEGT sessions with no adverse events. Barriers to session completion included clinical focus on prioritized interventions. Sessions [median up time = 17 minutes, (IQR: 7); walk time = 13 minutes, (IQR: 9); step count = 243, (IQR: 161); device assist = 74, (IQR: 28.0)] were primarily spent in Very Light to Light heart rate intensities [89%, (IQR: 42%) and 9%, (IQR: 33%), respectively]. OEGT incorporated into the rehabilitation plan of care during inpatient rehabilitation after severe ABI was observed to be safe, feasible, and tolerable. However, intentional steps must be taken to facilitate patient safety. [ABSTRACT FROM AUTHOR]

BACKGROUND: Individuals with moderate to severe traumatic brain injury (msTBI) have reported a lack of motivation, lack of time, and fatigue as perceived barriers to exercise. OBJECTIVE: To evaluate the effects of an exercise program on self-reported health-related symptoms and quality of life in persons 45-years and older with msTBI. METHODS: Post-hoc analysis of a prospective community-based 12-week exercise program of 20 adults, age 45–80 years, with msTBI. Ten were in aerobic exercise training (AET) program and 10 in a stretching and toning (SAT) program. The AET group was instructed to exercise based on their estimated maximal heart rate (HR) for 150 minutes weekly. The SAT group was to stretch for the same target time without significantly increasing HR or level of exertion. Outcome measures were Traumatic Brain Injury Quality of Life (TBI-QOL) for global, cognitive, emotional, and social health, Patient Health Questionnaire-9 (PHQ-9) for depressive symptoms, and Pittsburgh Sleep Quality Index (PSQI) for sleep quality. RESULTS: AET was associated with improved self-reported cognitive health and sleep compared to SAT. Moderate to large, positive effect sizes were also observed in the AET group in the QOL categories of global, emotional, and social health, and depressive symptoms. CONCLUSIONS: This study offers preliminary evidence that AET may improve health-related QOL, especially for cognition and sleep, in middle-aged and older adults with msTBI. [ABSTRACT FROM AUTHOR]

AbstractPurposeMaterials and MethodsResultsConclusions\nIMPLICATIONS FOR REHABILITATIONPeople with spinal cord injury (PwSCI) can experience life changes, including impacts on their physical and mental health. PwSCI often report less life satisfaction and lower subjective well-being than peers without SCI. These challenges and adversities increase the demand on them to be more resilient. Healthcare providers need quick and valid instruments to assess adult patients’ resilience in clinical settings. We aimed to validate the factor validity and discrimination ability of a resilience scale, CD-RISC-10, for clinical usage in adults with SCI during hospitalization.93 adults with SCI responded to the self-reported survey, including CD-RISC-10, the Patient Health Questionnaire-9 Scale (PHQ-9), the Satisfaction with Life Scale (SWLS), and the Intrinsic Spirituality Scale. We conducted descriptive statistics, exploratory factor analysis (EFA), and item response theory (IRT).Two items were deleted from CD-RISC-10 after EFA, forming CD-RISC-8. The item discriminations of the remaining eight items from the unconstrained IRT model ranged from a high of 3.071 to a relatively low 1.433. CD-RISC-8 is significantly related to PHQ-9 and SWLS.The factor validity of the CD-RISC-8 was improved. Significantly, the CD-RISC-8 has excellent potential for clinical usage due to its discriminant ability between low and intermediate resilience.Spinal Cord InjuryPeople with spinal cord injury (PwSCI) experience unique challenges and adversities that can negatively affect physical, mental, social, and financial health and life satisfaction.PwSCI with higher resilience adapt to challenges quicker, and have better mental health outcomes and improved quality of life.The CD-RISC-8 is useful for screening PwSCI who need resilience intervention and it is sensitive enough to evaluate resilience improvement within two minutes.People with spinal cord injury (PwSCI) experience unique challenges and adversities that can negatively affect physical, mental, social, and financial health and life satisfaction.PwSCI with higher resilience adapt to challenges quicker, and have better mental health outcomes and improved quality of life.The CD-RISC-8 is useful for screening PwSCI who need resilience intervention and it is sensitive enough to evaluate resilience improvement within two minutes. [ABSTRACT FROM AUTHOR]

The presence of evolved stars in high-redshift galaxies can place valuable indirect constraints on the onset of star formation in the Universe. Thus, we use PEARLS GTO (Prime Extragalactic Areas for Reionization and Lensing Science Guaranteed Time Observations) and public NIRCam (Near Infrared Camera) photometric data to search for Balmer-break candidate galaxies at 7 < z < 12. We find that our Balmer-break candidates at z ∼ 10.5 tend to be older (115 Myr), have lower inferred [O  iii ] + Hβ equivalent widths (120 Å), have lower specific star formation rates (6 Gyr−1) and redder UV slopes (β = −1.8) than our control sample of galaxies. However, these trends all become less strong at z ∼ 8, where the F 444 W filter now probes the strong rest-frame optical emission lines, thus providing additional constraints on the current star formation activity of these galaxies. Indeed, the bursty nature of epoch of reionization galaxies can lead to a disconnect between their current spectral energy distribution (SED) profiles and their more extended star formation histories. We discuss how strong emission lines, the cumulative effect of weak emission lines, dusty continua, and active galactic nuclei can all contribute to the photometric excess seen in the rest-frame optical, thus mimicking the signature of a Balmer break. Additional medium-band imaging will thus be essential to more robustly identify Balmer-break galaxies. However, the Balmer break alone cannot serve as a definitive proxy for the stellar age of galaxies, being complexly dependent on the star formation history. Ultimately, deep Near Infrared Spectrograph (NIRSpec) continuum spectroscopy and Mid-Infrared Instrument (MIRI) imaging will provide the strongest indirect constraints on the formation era of the first galaxies in the Universe, thereby revealing when cosmic dawn breaks. [ABSTRACT FROM AUTHOR]

The Prime Extragalactic Areas for Reionization and Lensing Science, a James Webb Space Telescope (JWST) GTO program, obtained a set of unique NIRCam observations that have enabled us to significantly improve the default photometric calibration across both NIRCam modules. The observations consisted of three epochs of 4-band (F150W, F200W, F356W, and F444W) NIRCam imaging in the Spitzer IRAC Dark Field (IDF). The three epochs were six months apart and spanned the full duration of Cycle 1. As the IDF is in the JWST continuous viewing zone, we were able to design the observations such that the two modules of NIRCam, modules A and B, were flipped by 180° and completely overlapped each other's footprints in alternate epochs. We were therefore able to directly compare the photometry of the same objects observed with different modules and detectors, and we found significant photometric residuals up to ∼0.05 mag in some detectors and filters, for the default version of the calibration files that we used (jwst_1039.pmap). Moreover, there are multiplicative gradients present in the data obtained in the two long-wavelength bands. The problem is less severe in the data reduced using the latest pmap (jwst_1130.pmap as of 2023 September), but it is still present, and is non-negligible. We provide a recipe to correct for this systematic effect to bring the two modules onto a more consistent calibration, to a photometric precision better than ∼0.02 mag. [ABSTRACT FROM AUTHOR]

With mobile health technologies serving as an alternative means of providing healthcare, evaluating patients' abilities to navigate digital infrastructures is becoming increasingly relevant. The goal of this study is to investigate smartphone use patterns among individuals with history of moderate-to-severe traumatic brain injury (TBI). An anonymous survey was delivered via e-mail or text message to eligible participants who had a history of moderate-to-severe TBI and were prospectively followed at one of the eight participating Traumatic Brain Injury Model Systems centers for at least 1-year post-injury. The survey captured demographic data and included a questionnaire to evaluate smartphone use (calling, texting, web browsing, etc.). A total of 2665 eligible individuals were contacted to complete the survey, 472 of which responded. 441 of them reported smartphone use. Individuals ages 45 and older were significantly less likely to use their phones for functions other than calling and texting when compared to individuals ages 18–44 (p < 0.05). Most individuals with moderate-to-severe TBI in this cohort demonstrated intentional smartphone use, suggesting that mobile health technologies may be feasible as a cost-effective healthcare alternative. However, doing so will require additional interventions to provide further technological education especially in older individuals with TBI. [ABSTRACT FROM AUTHOR]

We identify 71 distant stars in James Webb Space Telescope/NIRCam early release observations (ERO) images of the field of galaxy cluster SMACS J0723.3-7327 (SMACS 0723). Given the relatively small (∼10°) angular separation between SMACS 0723 and the Large Magellanic Cloud (LMC), it is likely that these stars are associated with the LMC outskirts or the Leading Arm. This is further bolstered by a spectral energy distribution (SED) analysis, which suggests an excess of stars at a physical distance of 40–100 kpc, consistent with being associated with or located behind the Magellanic system. In particular, we find that the overall surface density of stars brighter than 27.0 mag in the field of SMACS 0723 is ∼2.3 times that of stars in a blank field with similar Galactic latitude (the North Ecliptic Pole Time Domain Field), and that the density of stars in the SMACS 0723 field with SED-derived distances consistent with the Magellanic system is ∼6.1 times larger than that of the blank field. The candidate stars at these distances are consistent with a stellar population at the same distance modulus with [Fe/H] = −1.0 and an age of ∼5.0 Gyr. On the assumption that all of the 71 stars are associated with the LMC, then the stellar density of the LMC at the location of the SMACS 0723 field is ∼740 stars kpc−3, which helps trace the density of stars in the LMC outskirts. [ABSTRACT FROM AUTHOR]

We present an analysis of a sample of robust high-redshift galaxies selected from the 'blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey and Early Release Observations (ERO) data from JWST with the aim of selecting candidate high-redshift active galactic nuclei (AGN). Sources were identified from this parent sample using a threefold selection procedure, which includes spectral energy distribution (SED) fitting to identify sources that are best fitted by AGN SED templates, a further selection based on the relative performance of AGN and non-AGN models, and finally morphological fitting to identify compact sources of emission, resulting in a purity-oriented procedure. Using this procedure, we identify a sample of nine AGN candidates at 6.5 < z < 12, from which we constrain their physical properties as well as measure a lower bound on the AGN fraction in this redshift range of 5 ± 1 per cent. As this is an extreme lower limit due to our focus on purity and our SEDs being calibrated for unobscured Type 1 AGN, this demonstrates that AGN are perhaps quite common at this early epoch. The rest-frame UV colours of our candidate objects suggest that these systems are potentially candidate obese black hole galaxies (OBGs). We also investigate Chandra and VLA maps of these areas from which we calculate detection limits. Of note is a z  = 11.9 candidate source exhibiting an abrupt morphological shift in the reddest band as compared to bluer bands, indicating a potential merger or an unusually strong outflow. [ABSTRACT FROM AUTHOR]

Background: Overground exoskeleton gait training (OEGT) after neurological injury is safe, feasible, and may yield positive outcomes. However, no recommendations exist for initiation, progression, or termination of OEGT. This retrospective study highlights the clinical use and decision-making of OEGT within the physical therapy plan of care for patients after neurological injury during inpatient rehabilitation. Methods: The records of patients admitted to inpatient rehabilitation after stroke, spinal cord injury, or traumatic brain injury who participated in at least one OEGT session were retrospectively reviewed. Session details were analyzed to illustrate progress and included: "up" time, "walk" time, step count, device assistance required for limb swing, and therapist-determined settings. Surveys were completed by therapists responsible for OEGT sessions to illuminate clinical decision-making. Results: On average, patients demonstrated progressive tolerance for OEGT over successive sessions as shown by increasing time upright and walking, step count, and decreased assistance required by the exoskeleton. Therapists place preference on using OEGT with patients with more functional dependency and assess feedback from the patient and device to determine when to change settings. OEGT is terminated when other gait methods yield higher step repetitions or intensities, or to prepare for discharge. Conclusion: Our descriptive retrospective data suggests that patients after neurological injury may benefit from OEGT during inpatient rehabilitation. As no guidelines exist, therapists' clinical decisions are currently based on a combination of knowledge of motor recovery and experience. Future efforts should aim to develop evidence-based recommendations to facilitate functional recovery after neurological injury by leveraging OEGT. [ABSTRACT FROM AUTHOR]

Our team developed an attention control condition, called the Brain Health Group (BHG), for a randomized controlled trial (RCT; NCT03594734). The focus of the BHG was on brain health education and self-management. The objectives of this supplementary analysis are to (1) Describe compliance with the 12-month BHG; (2) Examine efficacy for improving general self-efficacy (GSE, primary) and secondary outcomes; and (3) Describe findings from the program evaluation. English-speaking adults (18–64 years old) who were ≥6 months post a moderate-to-severe TBI were randomized to the BHG (n = 29) or active intervention (n = 28). Data were collected at baseline and 12 months, including GSE, depression, satisfaction with life (SWL), self-rated abilities for health practices (SRAHP), and alcohol use. Program evaluation was conducted at 12 months. Attendance was 89%, and goal tracking was 63%. Within group analysis showed a significant increase in SRAHP scores (p = 0.018). Non-significant increases in GSE and SWL were observed, and participants perceived the BHG as helpful. No significant changes in depression or alcohol use were reported. People with TBI can engage in and benefit from the BHG and perceive the program as helpful for improving knowledge about brain health and awareness of self-management skills. [ABSTRACT FROM AUTHOR]

We present the first JWST observations of the z  = 4.11 luminous radio galaxy TN J1338–1942, obtained as part of the 'Prime Extragalactic Areas for Reionization and Lensing Science' ('PEARLS') project. Our NIRCam observations, designed to probe the key rest-frame optical continuum and emission line features at this redshift, enable resolved spectral energy distribution modelling that incorporates both a range of stellar population assumptions and radiative shock models. With an estimated stellar mass of log10(M /M⊙) ∼ 10.9, TN J1338–1942 is confirmed to be one of the most massive galaxies known at this epoch. Our observations also reveal extremely high equivalent-width nebular emission coincident with the luminous AGN jets that is best fit by radiative shocks surrounded by extensive recent star formation. We estimate the total star-formation rate (SFR) could be as high as |$\sim 1600\, \text{M}_{\odot }\, \text{yr}^{-1}$| , with the SFR that we attribute to the jet induced burst conservatively |$\gtrsim 500\, \text{M}_{\odot }\, \text{yr}^{-1}$|. The mass-weighted age of the star-formation, t mass < 4 Myr, is consistent with the likely age of the jets responsible for the triggered activity and significantly younger than that measured in the core of the host galaxy. The extreme scale of the potential jet-triggered star-formation activity indicates the potential importance of positive AGN feedback in the earliest stages of massive galaxy formation, with our observations also illustrating the extraordinary prospects for detailed studies of high-redshift galaxies with JWST. [ABSTRACT FROM AUTHOR]

We present early science results from Deep Investigation of Neutral Gas Origins (DINGO), an |$\rm H$| i survey using the Australian Square Kilometre Array Pathfinder (ASKAP). Using ASKAP subarrays available during its commissioning phase, DINGO early science data were taken over ∼60 deg2 of the Galaxy And Mass Assembly (GAMA) 23 h region with 35.5 h integration time. We make direct detections of six known and one new sources at z < 0.01. Using |$\rm H$|   i spectral stacking, we investigate the |$\rm H$|   i gas content of galaxies at 0.04 < z < 0.09 for different galaxy colours. The results show that galaxy morphology based on optical colour is strongly linked to |$\rm H$|   i gas properties. To examine environmental impacts on the |$\rm H$| i gas content of galaxies, three subsamples are made based on the GAMA group catalogue. The average |$\rm H$| i mass of group central galaxies is larger than those of satellite and isolated galaxies, but with a lower |$\rm H$| i gas fraction. We derive a variety of |$\rm H$| i scaling relations for physical properties of our sample, including stellar mass, stellar mass surface density, NUV − r colour, specific star formation rate, and halo mass. We find that the derived |$\rm H$| i scaling relations are comparable to other published results, with consistent trends also observed to ∼0.5 dex lower limits in stellar mass and stellar surface density. The cosmic |$\rm H$| i densities derived from our data are consistent with other published values at similar redshifts. DINGO early science highlights the power of |$\rm H$| i spectral stacking techniques with ASKAP. [ABSTRACT FROM AUTHOR]

We present a pilot study to assess the potential of Hyper Suprime-Cam Public Data Release 2 (HSC-PDR2) images for the analysis of extended faint structures within groups of galaxies. We examine the intragroup light (IGL) of the group 400138 (M dyn = 1.3 ± 0.5 × 1013 M⊙, z ∼ 0.2) from the Galaxy And Mass Assembly (GAMA) survey using Hyper Suprime-Cam Subaru Strategic Program Public Data Release 2 (HSC-SSP PDR2) images in g, r , and i bands. We present the most extended IGL measurement to date, reaching down to |$\mu _{g}^{\rm {lim}}=30.76$|  mag arcsec−2 (3σ; 10 × 10 arcsec2) at a semimajor axis of 275 kpc. The IGL shows mean colour values of g − i  = 0.92, g − r  = 0.60, and r − i  = 0.32 (±0.01). The IGL stellar populations are younger (2–2.5 Gyr) and less metal rich ([Fe/H] ∼ −0.4) than those of the host group galaxies. We find a range of IGL fractions as a function of total group luminosity of |${\sim} 2\!-\!36 {{\ \rm per\ cent}}$| depending on the definition of IGL, with larger fractions the bluer the observation wavelength. The early-type to late-type galaxy ratio suggests that 400138 is a more evolved group, dominated by early-type galaxies, and the IGL fraction agrees with that of other similarly evolved groups. These results are consistent with tidal stripping of the outer parts of Milky Way-like galaxies as the main driver of the IGL build-up. This is supported by the detection of substructure in the IGL towards the galaxy member 1660615 suggesting a recent interaction (<1 Gyr ago) of that galaxy with the core of the group. [ABSTRACT FROM AUTHOR]

We derive single Sérsic fits and bulge-disc decompositions for 13 096 galaxies at redshifts z < 0.08 in the GAMA II equatorial survey regions in the Kilo-Degree Survey (KiDS) g, r , and i bands. The surface brightness fitting is performed using the Bayesian two-dimensional profile fitting code ProFit. We fit three models to each galaxy in each band independently with a fully automated Markov chain Monte Carlo analysis: a single Sérsic model, a Sérsic plus exponential and a point source plus exponential. After fitting the galaxies, we perform model selection and flag galaxies for which none of our models are appropriate (mainly mergers/Irregular galaxies). The fit quality is assessed by visual inspections, comparison to previous works, comparison of independent fits of galaxies in the overlap regions between KiDS tiles and bespoke simulations. The latter two are also used for a detailed investigation of systematic error sources. We find that our fit results are robust across various galaxy types and image qualities with minimal biases. Errors given by the MCMC underestimate the true errors typically by factors 2–3. Automated model selection criteria are accurate to |$\gt 90{{\ \rm per\ cent}}$| as calibrated by visual inspection of a subsample of galaxies. We also present g − r component colours and the corresponding colour–magnitude diagram, consistent with previous works despite our increased fit flexibility. Such reliable structural parameters for the components of a diverse sample of galaxies across multiple bands will be integral to various studies of galaxy properties and evolution. All results are integrated into the GAMA database. [ABSTRACT FROM AUTHOR]

We investigate changes in stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift (0.60 ≤   |$z$| ≤ 0.76) using the LEGA-C Survey to low redshift (0.014 ≤   |$z$| ≤ 0.10) using the SAMI Galaxy Survey. Specifically, we study how the spatially integrated global age and metallicity of individual quiescent galaxies vary in the mass–size plane, using the stellar mass M * and a dynamical mass proxy derived from the virial theorem M D  ∝ σ2  R e. We find that, similarly to at low redshift, the metallicity of quiescent galaxies at 0.60 ≤   |$z$| ≤ 0.76 closely correlates with M / R e (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals by determining the escape velocity for metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. Conversely, we find no correlation between age and surface density (⁠|$M/R_\mathrm{e}^2$|⁠) at 0.60 ≤   |$z$| ≤ 0.76, despite this relation being strong at low redshift. We consider this change in the age– |$M/R_\mathrm{e}^2$| relation in the context of the redshift evolution of the star-forming and quiescent mass–size relations, and find our results are consistent with galaxies forming more compactly at higher redshifts and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The |$z$| ∼  0 age– |$M/R_\mathrm{e}^2$| relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and therefore a range of surface densities. [ABSTRACT FROM AUTHOR]

Introduction: As technological advances allow the use of robotic exoskeleton devices with gait training, there is a critical need to establish a robotic gait training (RGT) program to meet the needs of people with spinal cord injury (SCI) during inpatient rehabilitation. The purposes of this study are to prospectively examine the efficacy of a stakeholder informed RGT program compared to usual care gait training (UC) during inpatient rehabilitation in people with incomplete SCI and compare the intensity of RGT and UC gait training during inpatient rehabilitation. Study design: 128 patients with incomplete SCI admitted to our inpatient rehabilitation facility will be screened for eligibility and randomized to either the RGT or UC group. RGT sessions will use the Ekso robotic exoskeleton [class II medical device (United States FDA)]. UC sessions will use traditional gait training approaches such as manually assisted overground gait training with walkers and orthotics and body weight–supported treadmill training (BWSTT). Our primary outcome is gait function as characterized by the Walking Index for Spinal Cord Injury–II (WISCI-II). Secondary outcomes are gait speed, Spinal Cord Independence Measure (SCIM), Numeric Pain Rating Scale (NPRS), Fatigue Severity Scale (FSS), Penn Spasm Frequency Scale (PSFS), Patient Health Questionnaire-9 (PHQ-9), General Anxiety Disorder– 7 (GAD-7), International Spinal Cord Injury Quality of Life Basic Data Set, and a Qualitative Questionnaire. Assessments of primary and secondary outcomes will occur at admission and discharge from inpatient rehabilitation. General or generalized linear models will be used to analyze differences between groups for all measures. Clinical impact: Successful completion of this study will provide a usable, replicable, stakeholder informed RGT intervention for use with individuals with incomplete SCI during inpatient rehabilitation. [ABSTRACT FROM AUTHOR]

Resilience is central to living well with a spinal cord injury (SCI). To provide a timely, targeted, and individualized intervention supporting resilience, it is necessary to assess an individual's resilience level and characteristics of resilience on an ongoing basis. We aimed to validate the different types of resilient coping among people with SCI (PwSCI), using the Connor–Davidson resilience scale, and to identify the relationships between resilience and other psychosocial factors among the types of resilient coping. We recruited 93 PwSCI, who took the self-report measures of resilience, depression, life satisfaction, and spirituality. Using latent class analysis, we found three types: (a) goal-pursuing, bouncing-back, and persevering, named GP; (b) uncertainty about coping with setbacks, named UC; and (c) loss of resilient coping, named LOSS. The multivariate tests indicated that the three types differed on a linear combination of resilience, depression, and life satisfaction, with a large effect size. We discuss the three types of resilient coping and the implications for psychosocial interventions. We also recommend that rehabilitation clinicians examine PwSCI's resilience levels and types of resilience during initial and follow-up visits. In doing so, PwSCI will have timely, targeted supports for developing and/or re-building their resilience. [ABSTRACT FROM AUTHOR]

We measure how the atomic gas (H i) fraction f H I = M H I M * of groups and pairs taken as single units vary with average stellar mass (〈 M *〉) and average star formation rate (〈SFR〉), compared to isolated galaxies. The H i 21 cm emission observation are from (i) archival ALFALFA survey data covering three fields from the GAMA survey (provides environmental and galaxy properties), and (ii) DINGO pilot survey data of one of those fields. The mean f H i for different units (groups/pairs/isolated galaxies) are measured in regions of the log(〈 M *〉)â€"log(〈SFR〉) plane, relative to the z ∼ 0 star-forming main sequence (SFMS) of individual galaxies, by stacking f H i spectra of individual units. For ALFALFA, f H i spectra of units are measured by extracting H i spectra over the full groups/pair areas and dividing by the total stellar mass of member galaxies. For DINGO, f H i spectra of units are measured by co-adding H i spectra of individual member galaxies, followed by division by their total stellar mass. For all units, the mean f H i decreases as we move to higher 〈 M *〉 along the SFMS and as we move from above the SFMS to below it at any 〈 M *〉. From the DINGO-based study, mean f H i in groups appears to be lower compared to isolated galaxies for all 〈 M *〉 along the SFMS. From the ALFALFA-based study, we find substantially higher mean f H i in groups compared to isolated galaxies (values for pairs being intermediate) for 〈 M *〉 ≲ 109.5 M ⊙, indicating the presence of substantial amounts of H i not associated with cataloged member galaxies in low mass groups. [ABSTRACT FROM AUTHOR]

To examine the usability of an Apple Watch-based, two-way Personalized Mobile Trainer (PMT) in community-based exercise programs for individuals with chronic traumatic brain injury (cTBI). This is a prospective pilot study. Twenty participants with cTBI aged 46–73 were enrolled in a 3-month individualized exercise program. After one in-person training session on PMT and exercise program, participants were prescribed either aerobic exercise training (AET) or stretching and toning (SAT) performed at home. The PMT was used to remotely deliver updated exercise prescription, track exercise progress, and communicate with the participants. The primary outcome was compliance with the exercise programs. All the participants completed the assigned exercise program with an average compliance of 76%. Nineteen (95%) participants were able to use the PMT properly during exercise sessions. After 3 months of training, the AET trended toward maintaining exercise endurance when compared with the SAT group (0.3% vs −4%, p = 0.14) with a medium effect size of 0.43. Using the PMT system to support and track exercise in community-based exercise programs is feasible. The PMT may promote compliance with the training program but testing its effectiveness with larger trials is warranted. [ABSTRACT FROM AUTHOR]

We use the 21-cm emission-line data from the Deep Investigation of Neutral Gas Origin-Very Large Array (DINGO-VLA) project to study the atomic hydrogen gas H  i of the Universe at redshifts z < 0.1. Results are obtained using a stacking analysis, combining the H  i signals from 3622 galaxies extracted from 267 VLA pointings in the G09 field of the Galaxy and Mass Assembly Survey (GAMA). Rather than using a traditional one-dimensional spectral stacking method, a three-dimensional cubelet stacking method is used to enable deconvolution and the accurate recovery of average galaxy fluxes from this high-resolution interferometric data set. By probing down to galactic scales, this experiment also overcomes confusion corrections that have been necessary to include in previous single-dish studies. After stacking and deconvolution, we obtain a 30σ H  i mass measurement from the stacked spectrum, indicating an average H  i mass of |${\rm{M_{\rm{{H}\,\small{I}}}}}=(1.67\pm 0.18)\times 10^{9}~{\rm{{\rm M}_{\odot }}}$|⁠. The corresponding cosmic density of neutral atomic hydrogen is |${\rm{\Omega _{\rm{{H}\,\small{I}}}}}=(0.38\pm 0.04)\times 10^{-3}$| at redshift of z = 0.051. These values are in good agreement with earlier results, implying there is no significant evolution of |$\Omega _{\rm{{H}\,\small{I}}}$| at lower redshifts. [ABSTRACT FROM AUTHOR]

We present catalogues of stellar masses, star formation rates (SFRs), and ancillary stellar population parameters for galaxies spanning 0 < z < 9 from the Deep Extragalactic VIsible Legacy Survey (DEVILS). DEVILS is a deep spectroscopic redshift survey with very high completeness, covering several premier deep fields including COSMOS (D10). Our stellar mass and SFR estimates are self-consistently derived using the spectral energy distribution (SED) modelling code ProSpect , using well-motivated parametrizations for dust attenuation, star formation histories, and metallicity evolution. We show how these improvements, and especially our physically motivated assumptions about metallicity evolution, have an appreciable systematic effect on the inferred stellar masses, at the level of ∼0.2 dex. To illustrate the scientific value of these data, we map the evolving galaxy stellar mass function (SMF) and the SFR– M ⋆ relation for 0 < z < 4.25. In agreement with past studies, we find that most of the evolution in the SMF is driven by the characteristic density parameter, with little evolution in the characteristic mass and low-mass slopes. Where the SFR– M ⋆ relation is indistinguishable from a power law at z > 2.6, we see evidence of a bend in the relation at low redshifts (z < 0.45). This suggests evolution in both the normalization and shape of the SFR– M ⋆ relation since cosmic noon. It is significant that we only clearly see this bend when combining our new DEVILS measurements with consistently derived values for lower redshift galaxies from the Galaxy And Mass Assembly (GAMA) survey: this shows the power of having consistent treatment for galaxies at all redshifts. [ABSTRACT FROM AUTHOR]

Objective Athletes with ADHD may experience longer and/or more complicated recoveries following SRC; however, previous research has focused on neurocognitive outcomes. The objective of this study was to investigate the relationship between a history of ADHD among adolescent athletes and vestibular impairments following SRC. Method Participants included 166 athletes aged 15.9 +/− 1.5 who sustained an SRC, including 25 with a documented history of ADHD. Appropriate summary statistics were used to describe the data. ADHD and non-ADHD groups were compared using t-tests and Mann–Whitney U tests for continuous variables and Chi-square tests for categorical variables. A linear regression model analyzed the relationship between a history of ADHD and vestibular outcomes including horizontal and vertical vestibulo-ocular reflex (hVOR; vVOR), visual motion sensitivity (VMS), and Dizziness Handicap Index (DHI), while referral to vestibular therapy (VT) was analyzed using logistic regression. Results Athletes with ADHD experienced significantly higher rates of on-field dizziness, (p = 0.039) and dizziness following vVOR testing on the Vestibular/Ocular Motor Screening (VOMS; p = 0.041). Athletes with ADHD were more likely to be referred to vestibular therapy (VT) (p = 0.033) and displayed abnormal vVOR test during the initial VT visit (p = 0.040). Conclusions Adolescent athletes with a history of ADHD are more likely to report on-field dizziness following SRC and increased dizziness with vVOR testing on VOMS, thus resulting in more frequent referrals to VT, where they also display abnormal vVOR results. Additional research is needed to improve treatment strategies and recovery outcomes in athletes after SRC. [ABSTRACT FROM AUTHOR]