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Fast radio bursts (FRBs) are extragalactic radio flashes of unknown physical origin. Their high luminosities and short durations require extreme energy densities, such as those found in the vicinity of neutron stars and black holes. Studying the burst intensities and polarimetric properties on a wide range of timescales, from milliseconds down to nanoseconds, is key to understanding the emission mechanism. However, high-time-resolution studies of FRBs are limited by their unpredictable activity levels, available instrumentation and temporal broadening in the intervening ionized medium. Here we show that the repeating FRB 20200120E can produce isolated shots of emission as short as about 60 nanoseconds in duration, with brightness temperatures as high as 3 × 10 41  K (excluding relativistic effects), comparable with ‘nano-shots’ from the Crab pulsar. Comparing both the range of timescales and luminosities, we find that FRB 20200120E observationally bridges the gap between known Galactic young pulsars and magnetars and the much more distant extragalactic FRBs. This suggests a common magnetically powered emission mechanism spanning many orders of magnitude in timescale and luminosity. In this Article, we probe a relatively unexplored region of the short-duration transient phase space; we highlight that there probably exists a population of ultrafast radio transients at nanosecond to microsecond timescales, which current FRB searches are insensitive to. The range of timescales and luminosities measured from the nearby fast radio burst FRB 20200120E observationally connects these extreme extragalactic transients with studies of Galactic neutron stars.

IntroductionAcute clinical deterioration in hospital inpatients can be caused by a range of factors including dementia, delirium, substance withdrawal and psychiatric disturbance, creating challenges in diagnosis, often requiring a management plan with input from multiple disciplines. Staff forums and broader literature have confirmed that healthcare staff working in non-mental health settings, may not be as skilled in recognising and managing early signs of emerging and/or escalating clinical agitation. The BoC RRT is a consultation service within the Division of Medicine and CL Psychiatry. Staffed by Medical Registrars and Mental Health Nurses, the collaboration provides a unique healthcare response to acute general wards. The BoC RRT has been implemented to address the rising number of incidences whereby staff and patient safety are compromised. Using evidence-based skills the team aimed to: respond to episodes of clinical agitation that require an internal security response, assist ward referrals by exploring biopsychosocial contributants to behaviour, develop individual patient support plans and review and reduce restrictive intervention practices.ObjectivesTo determine if the rapid response model has influenced:- The impact on staff/patient safety- Frequency of emergency responses for aggression- Frequency of restrictive intervention useMethodsThis project was approved as a quality assurance project (QA2022018). The patients within scope of the BoC RRT include inpatients in medical and surgical wards. It excludes patients in Emergency Departments, mental health units, outpatient clinics, and visitors. The evaluation of the pilot has used a PDSA (Plan, Do, Study, Act) cycle when implementing new improvements. A mixed methods approach explored the impact of the BoC RRT. Staff consultation will identify challenges in responding to scenarios whereby there is risk of harm to staff and patients. Staff feedback and the emergency response data was monitored.ResultsIn 2021, there was approx. 720 code greys per month, requiring a security response. Since the implementation of BoC RRT, these numbers have reduced to 527. Reviewing restrictive intrvention practices has identified areas for policy review and need for education. Staff consultation found that nurses were confident caring for those patients exhibiting clinical agitation associated with delirium and dementia. However, caring for people with mental health or substance use disorders were more challenging.ConclusionsThese interim results indicate that BoC RRT has been generally well received by clinical staff. The decline in code grey responses indicates that it is likely having a positive impact in early identification and management of clinical agitation for hospital inpatients. There is support for this response model to continue beyond the pilot phase and further area for research.Disclosure of InterestNone Declared

Purpose The aim of this study was to investigate (a) the behavioral cues that are displayed by, and trait judgments formed about, anxious interviewees, and (b) why anxious interviewees receive lower interview performance ratings. The Behavioral Expression of Interview Anxiety Model was created as a conceptual framework to explore these relations. Design/Methodology/Approach We videotaped and transcribed mock job interviews, obtained ratings of interview anxiety and interview performance, and trained raters to assess several verbal and nonverbal cues and trait judgments. Findings The results indicated that few behavioral cues, but several traits were related to interviewee and interviewer ratings of interview anxiety. Two factors emerged from our factor analysis on the trait judgments—Assertiveness and Interpersonal Warmth. Mediation analyses were performed and indicated that Assertiveness and Interpersonal Warmth mediated the relation between interview anxiety and interview performance. Speech rate (words spoken per minute) and Assertiveness were found to mediate the relation between interviewee and interviewer ratings of interview anxiety. Implications Overall, the results indicated that interviewees should focus less on their nervous tics and more on the broader impressions that they convey. Our findings indicate that anxious interviewees may want to focus on how assertive and interpersonally warm they appear to interviewers. Originality/Value To our knowledge, this is the first study to use a validated interview anxiety measure to examine behavioral cues and traits exhibited by anxious interviewees. We offer new insight into why anxious interviewees receive lower interview performance ratings.

Multi-compartment tissue modeling using diffusion magnetic resonance imaging has proven valuable in the brain, offering novel indices sensitive to the tissue microstructural environment in vivo on clinical MRI scanners. However, application, characterization, and validation of these models in the spinal cord remain relatively under-studied. In this study, we apply a diffusion “signal” model (diffusion tensor imaging, DTI) and two commonly implemented “microstructural” models (neurite orientation dispersion and density imaging, NODDI; spherical mean technique, SMT) in the human cervical spinal cord of twenty-one healthy controls. We first provide normative values of DTI, SMT, and NODDI indices in a number of white matter ascending and descending pathways, as well as various gray matter regions. We then aim to validate the sensitivity and specificity of these diffusion-derived contrasts by relating these measures to indices of the tissue microenvironment provided by a histological template. We find that DTI indices are sensitive to a number of microstructural features, but lack specificity. The microstructural models also show sensitivity to a number of microstructure features; however, they do not capture the specific microstructural features explicitly modelled. Although often regarded as a simple extension of the brain in the central nervous system, it may be necessary to re-envision, or specifically adapt, diffusion microstructural models for application to the human spinal cord with clinically feasible acquisitions – specifically, adjusting, adapting, and re-validating the modeling as it relates to both theory (i.e. relevant biology, assumptions, and signal regimes) and parameter estimation (for example challenges of acquisition, artifacts, and processing).

Fast radio bursts (FRBs) are flashes of unknown physical origin 1 . The majority of FRBs have been seen only once, although some are known to generate multiple flashes 2 , 3 . Many models invoke magnetically powered neutron stars (magnetars) as the source of the emission 4 , 5 . Recently, the discovery 6 of another repeater (FRB 20200120E) was announced, in the direction of the nearby galaxy M81, with four potential counterparts at other wavelengths 6 . Here we report observations that localized the FRB to a globular cluster associated with M81, where it is 2 parsecs away from the optical centre of the cluster. Globular clusters host old stellar populations, challenging FRB models that invoke young magnetars formed in a core-collapse supernova. We propose instead that FRB 20200120E originates from a highly magnetized neutron star formed either through the accretion-induced collapse of a white dwarf, or the merger of compact stars in a binary system 7 . Compact binaries are efficiently formed inside globular clusters, so a model invoking them could also be responsible for the observed bursts. The fast radio burst FRB 20200120E is shown to originate from a globular cluster in the galaxy M81, and may be a collapsed white dwarf or a merged compact binary star system.

Children in child‐centered preschools and kindergartens were compared to children in didactic, highly academic programs in terms of their basic skills achievement and a set of motivation variables. The study included 227 poor, minority, and middle‐class children between the ages of 4 and 6 years. Children in didactic programs that stressed basic skills had significantly higher scores on a letters/reading achievement test but not on a numbers achievement test. Being enrolled in a didactic early childhood education program was associated with relatively negative outcomes on most of the motivation measures. Compared to children in child‐centered programs, children in didactic programs rated their abilities significantly lower, had lower expectations for success on academic tasks, showed more dependency on adults for permission and approval, evidenced less pride in their accomplishments, and claimed to worry more about school. Program effects were the same for economically disadvantaged and middle‐class children, and for preschoolers and kindergartners.

The latencies of visually guided saccadic eye movements can form bimodal distributions. The ‘express saccades’ associated with the first mode of the distribution are thought to be generated via an anatomical pathway different from that for the second mode, which comprises regular saccades. The following previously published observations are the basis for a new alternative model of these effects: (i) visual stimuli can cause oscillations to appear in the electroencephalogram ; (ii) visual stimuli can cause a negative shift in the electroencephalogram that lasts for several hundreds of milliseconds; and (iii) negativity in the electroencephalogram can be associated with reduced thresholds of cortical neurons to stimuli. In the new model both express and regular saccades are generated by the same anatomical structures. The differences in saccadic latency are produced by an oscillatory reduction of a threshold in the saccade-generating pathway that is transiently produced under certain stimulus paradigms. The model has implications regarding the functional significance of spontaneous and stimulus-induced oscillations in the central nervous system.

The repeating fast radio burst (FRB) source FRB 20200120E is exceptional because of its proximity and association with a globular cluster. Here we report \\(60\\) bursts detected with the Effelsberg telescope at 1.4 GHz. We observe large variations in the burst rate, and report the first FRB 20200120E `burst storm', where the source suddenly became active and 53 bursts (fluence \\(\\geq 0.04\\) Jy ms) occurred within only 40 minutes. We find no strict periodicity in the burst arrival times, nor any evidence for periodicity in the source's activity between observations. The burst storm shows a steep energy distribution (power-law index \\(\\alpha = 2.39\\pm0.12\\)) and a bi-modal wait-time distribution, with log-normal means of 0.94\\(^{+0.07}_{-0.06}\\) s and 23.61\\(^{+3.06}_{-2.71}\\) s. We attribute these wait-time distribution peaks to a characteristic event timescale and pseudo-Poisson burst rate, respectively. The secondary wait-time peak at \\(\\sim1\\) s is \\(\\sim50\\times\\) longer than the \\(\\sim24\\) ms timescale seen for both FRB 20121102A and FRB 20201124A -- potentially indicating a larger emission region, or slower burst propagation. FRB 20200120E shows order-of-magnitude lower burst durations and luminosities compared with FRB 20121102A and FRB 20201124A. Lastly, in contrast to FRB 20121102A, which has observed dispersion measure (DM) variations of \\(\\Delta{\\rm DM} >1\\) pc cm\\(^{-3}\\) on month-to-year timescales, we determine that FRB 20200120E's DM has remained stable (\\(\\Delta{\\rm DM} <0.15\\) pc cm\\(^{-3}\\)) over \\(>10\\) months. Overall, the observational characteristics of FRB 20200120E deviate quantitatively from other active repeaters, but it is unclear whether it is qualitatively a different type of source.

Very long baseline interferometric (VLBI) localisations of repeating fast radio bursts (FRBs) have demonstrated a diversity of local environments: from nearby star-forming regions to globular clusters. Here we report the VLBI localisation of FRB 20201124A using an ad-hoc array of dishes that also participate in the European VLBI Network (EVN). In our campaign, we detected 18 total bursts from FRB 20201124A at two separate epochs. By combining the visibilities from both observing epochs, we were able to localise FRB 20201124A with a 1-\\(\\sigma\\) error of 4.5 milliarcseconds (mas). We use the relatively large burst sample to investigate astrometric accuracy, and find that for \\(\\gtrsim20\\) baselines (\\(\\gtrsim7\\) dishes) that we can robustly reach milliarcsecond precision even using single-burst data sets. Sub-arcsecond precision is still possible for single bursts, even when only \\(\\sim\\) six baselines (four dishes) are available. We explore two methods for determining the individual burst positions: the peaks of the dirty maps and a Gaussian fit to the cross fringe pattern on the dirty maps. We found the latter to be more reliable due to the lower mean and standard deviation in the offsets from the FRB position. Our VLBI work places FRB 20201124A 705\\(\\pm\\)26 mas (1-\\(\\sigma\\) errors) from the optical centre of the host galaxy, and consistent with originating from within the recently-discovered extended radio structure associated with star-formation in the host galaxy. Future high-resolution optical observations, e.g. with Hubble Space Telescope, can determine the proximity of our FRB 20201124A VLBI position to nearby knots of star formation.

Fast radio bursts (FRBs) are exceptionally luminous flashes of unknown physical origin, reaching us from other galaxies (Petroff et al. 2019). Most FRBs have only ever been seen once, while others flash repeatedly, though sporadically (Spitler et al. 2016, CHIME/FRB Collaboration et al. 2021). Many models invoke magnetically powered neutron stars (magnetars) as the engines producing FRB emission (Margalit & Metzger 2018, CHIME/FRB Collaboration et al. 2020). Recently, CHIME/FRB announced the discovery (Bhardwaj et al. 2021) of the repeating FRB 20200120E, coming from the direction of the nearby grand design spiral galaxy M81. Four potential counterparts at other observing wavelengths were identified (Bhardwaj et al. 2021) but no definitive association with these sources, or M81, could be made. Here we report an extremely precise localisation of FRB 20200120E, which allows us to associate it with a globular cluster (GC) in the M81 galactic system and to place it ~2pc offset from the optical center of light of the GC. This confirms (Bhardwaj et al. 2021) that FRB 20200120E is 40 times closer than any other known extragalactic FRB. Because such GCs host old stellar populations, this association strongly challenges FRB models that invoke young magnetars formed in a core-collapse supernova as powering FRB emission. We propose, instead, that FRB 20200120E is a highly magnetised neutron star formed via either accretion-induced collapse of a white dwarf or via merger of compact stars in a binary system (Margalit et al. 2019). Alternative scenarios involving compact binary systems, efficiently formed inside globular clusters, could also be responsible for the observed bursts.