64 research outputs found
The cognitive and motivational effects of imagery on sport performance
No full textSIGLEAvailable from British Library Document Supply Centre-DSC:DXN032936 / BLDSC - British Library Document Supply CentreGBUnited Kingdo
The rate of extreme coronal line emitters in the Baryon Oscillation Spectroscopic Survey LOWZ sample
No full textJ. Callow et al.Extreme coronal line emitters (ECLEs) are a rare class of galaxy that exhibit strong, high-ionization iron coronal emission lines in their spectra. In some cases, these lines are transient and may be the result of tidal disruption event (TDEs). To test this connection, we calculate the rate of variable ECLEs (vECLEs) at redshift. We search for ECLEs in the Baryon Oscillation Spectroscopic Survey (BOSS) LOWZ sample and discover two candidate ECLEs. Using follow-up spectra from the Dark Energy Spectroscopic Instrument and Gemini Multi-Object Spectrograph, and mid-infrared observations from the Wide-field Infrared Survey Explorer, we determine that one of these galaxies is a vECLE. Using this galaxy, we calculate the galaxy-normalized vECLE rate at redshift to be and the mass-normalized rate to be. This is then converted to a volumetric rate of. Formally, the LOWZ vECLE rates are times lower than the rates calculated from the Sloan Digital Sky Survey Legacy sample at redshift. However, given the large uncertainties on both measurements, they are consistent with each other at. Both the galaxy-normalized and volumetric rates are one to two orders of magnitude lower than TDE rates from the literature, consistent with vECLEs being caused by per cent of all TDEs.This work was supported by the Science and Technology Facilities Council [grants ST/S000550/1 and ST/W001225/1]. Funding for the Sloan Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, and the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Website is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, The University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. This material is based upon work supported by the U.S. Department of Energy (DOE), Office of Science, Office of High-Energy Physics, under Contract no. DE-AC02-05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising–Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Humanities, Science and Technology of Mexico (CONAHCYT); the Ministry of Science, Innovation and Universities of Spain (MICIU/AEI/10.13039/501100011033), and by the DESI Member Institutions: https://www.desi.lbl.gov/collaborating-institutions. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U. S. National Science Foundation, the U. S. Department of Energy, or any of the listed funding agencies. This research has made use of NASA’s Astrophysics Data System Bibliographic Services and the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration (NASA) and operated by the California Institute of Technology. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of NASA. The CRTS survey is supported by the U.S. National Science Foundation (NSF) under grants AST-0909182 and AST-1313422.Peer reviewe
The neural substrates for the different modalities of movement imagery.
No full textResearch highlights that internal visual, external visual and kinesthetic imagery differentially effect motor performance (White & Hardy, 1995; Hardy & Callow, 1999). However, patterns of brain activation subserving these different imagery perspectives and modalities have not yet been established. In the current study, we applied the Vividness of Movement Imagery Questionnaire-2 (VMIQ-2) to study the brain activation underpinning these types of imagery. Participants with high imagery ability (using the VMIQ-2) were selected to participate in the study. The experimental conditions involved imagining an action (one item from the VMIQ-2) using internal visual imagery, external visual imagery, kinesthetic imagery and a perceptual control condition involved looking at a fixation cross. The imagery conditions were presented using a block design and the participants' brain activation was recorded using 3T fMRI. A post-experimental questionnaire was administered to test if participants were able to maintain the imagery during the task and if they switched between the imagery perspective/modalities. Four participants failed to adhere to the imagery conditions, and their data was excluded from analysis. As hypothesized, the different perspectives and modalities of imagery elicited both common areas of activation (in the right supplementary motor area, BA6) and dissociated areas of activation. Specifically, internal visual imagery activated occipital, parietal and frontal brain areas (i.e., the dorsal stream) while external visual imagery activated occipital ventral stream areas and kinesthetic imagery activated caudate and cerebellum areas. These results provide the first central evidence for the visual perspectives and modalities delineated in the VMIQ-2, and, initial biological validity for the VMIQ-2. However, given that only one item from the VMIQ-2 was employed, future fMRI research needs to explore all items to further examine these contentions
The relationship between the use of kinaesthetic imagery and different visual imagery perspectives
No full textThe rate of extreme coronal line emitting galaxies in the Sloan Digital Sky Survey and their relation to tidal disruption events
No full textThe data underlying this article are available in the article and in its online supplementary material through Zenodo at Callow et al. (2024). The reduced data and derived measurements in this article will be shared on reasonable request to the corresponding author.J. Callow et al.High-ionization iron coronal lines (CLs) are a rare phenomenon observed in galaxy and quasi-stellar object spectra that are thought to be created by high-energy emission from active galactic nuclei and certain types of transients. In cases known as extreme coronal line emitting galaxies (ECLEs), these CLs are strong and fade away on a time-scale of years. The most likely progenitors of these variable CLs are tidal disruption events (TDEs), which produce sufficient high-energy emission to create and sustain the CLs over these time-scales. To test the possible connection between ECLEs and TDEs, we present the most complete variable ECLE rate calculation to date and compare the results to TDE rates from the literature. To achieve this, we search for ECLEs in the Sloan Digital Sky Survey (SDSS). We detect sufficiently strong CLs in 16 galaxies, more than doubling the number previously found in SDSS. Using follow-up spectra from the Dark Energy Spectroscopic Instrument and Gemini Multi-Object Spectrograph, Wide-field Infrared Survey Explorer mid-infrared observations, and Liverpool Telescope optical photometry, we find that none of the nine new ECLEs evolve in a manner consistent with that of the five previously discovered variable ECLEs. Using this sample of five variable ECLEs, we calculate the galaxy-normalized rate of variable ECLEs in SDSS to be RG = 3.6 +2.6 −1.8 (statistical) +5.1 −0.0 (systematic) × 10−6 galaxy−1 yr−1. The mass-normalized rate is RM = 3.1 +2.3 −1.5 (statistical) +4.4 −0.0 (systematic) × 10−17 M−1 yr−1 and the volumetric rate is RV = 7 +20 −5 (statistical) +10 −0.0 (systematic) × 10−9 Mpc−3 yr−1. Our rates are one to two orders of magnitude lower than TDE rates from the literature, which suggests that only 10–40 per cent of all TDEs produce variable ECLEs. Additional uncertainties in the rates arising from the structure of the interstellar medium have yet to be included.This work was supported by the Science & Technology Facilities Council (grants ST/S000550/1 and ST/W001225/1).
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, and the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Website is http://www.sdss.org/.
The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, The University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.
This material is based upon work supported by the U.S. Department of Energy (DOE), Office of Science, Office of High-Energy Physics, under Contract No. DE-AC02-05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: https://www.desi.lbl.gov/collaborating-institutions. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U.S. National Science Foundation, the U.S. Department of Energy, or any of the listed funding agencies.
The authors are honoured to be permitted to conduct scientific research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation.
This research has made use of NASA’s Astrophysics Data System Bibliographic Services and the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration (NASA) and operated by the California Institute of Technology. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of NASA. The CRTS survey is supported by the U.S. National Science Foundation (NSF) under grants AST-0909182 and AST-1313422.
Based on observations obtained at the international Gemini Observatory, a programme of NSF’s NOIRLab, processed using dragons (Data Reduction for Astronomy from Gemini Observatory North and South), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work was enabled by observations made from the Gemini North telescope, located within the Maunakea Science Reserve and adjacent to the summit of Maunakea. We are grateful for the privilege of observing the Universe from a place that is unique in both its astronomical quality and its cultural significance.Peer reviewe
Extending Relational Model Transformations to Better Support the Verification of Increasingly Autonomous Systems
No full textExtending relational model transformations to better support the verification of increasingly autonomous systems This item was submitted to Loughborough University’s Institutional Repository by the/an author. Additional Information: • A dissertation thesis submitted in partial fulfilment of the requirements fo
Better out than in: The influence of anger regulation on physical performance
No full textWe examined the influence of individual differences in anger regulation as potential moderators of the anger–performance relationship. Extending Lazarus, 1991 R.S. Lazarus, Cognition and motivation in emotion. American Psychologist, 46 (1991), pp. 352–367. [Lazarus, 1991] and [Lazarus, 2000a] cognitive–motivational–relational theory of emotion, we investigated the influence of trait anger and the anger regulation styles of anger-in and anger-out on the performance of a physical task. As hypothesized, trait anger and anger-out were positively associated with anger-derived performance enhancement on a peak force task; anger-in significantly inhibited the trait anger–performance relationship. Results are discussed in relation to Lazarus’s cognitive–motivational–relational theory and future research directions are offered
Review and Analysis of Successful PSA Interventions: An Applied Perspective
No full textPublic speaking can be a fear-inducing and anxiety-provoking experience for individuals, potentially resulting in poor performance and missed educational, social, and professional opportunities. In order to provide applied practitioners with effective methodologies for the reduction of public speaking anxiety (PSA), this paper aims to systematically review and meta-analyse theoretically driven interventions that successfully reduce PSA or maintain/increased public speaking performance. Following the preferred reporting items for systematic reviews and meta-analyses (PRISMA) guidelines, a systematic review and meta-analysis examined articles from 1st January 2000 to 1st June 2023. Of the 1,293 articles identified, 26 studies with 2,253 participants met the inclusion criteria. Research was of a moderate to high methodological standard, with interventions varying in type, duration, and focus (e.g., symptom vs. source). Intervention types included exposure, cognitive modification, combined, and other strategies. Although, the overall effect of psychological interventions for PSA across 42 interventions was g = 1.17 (95% CI = 0.88-1.45), with high heterogeneity, individual effect sizes varied greatly. While this review provides support for the efficacy of psychological interventions in reducing anxiety related to public speaking, rigorous research is warranted to examine long-term efficacy, real-world implications, self-efficacy development, and individual differences in treatment assignment. Finally, this review provides practitioners with a quick and easy guide to implementing successful interventions that reduce PSA or maintain/increase performance
The Effects of a motivational general mastery imagery intervention on the sport confidence of high level badminton players
No full text- …
