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Background: Although research on children's motor competence is a growing field of interest, especially among young children (4-6 years), several questions remain to be answered. Differences in children’s motor competence and their determinants, must be made transparent since early childhood is a critical period for the development of fundamental movement skills, and thereby a lifelong active lifestyle and health. Objective: The purpose of this cross-sectional study was to determine differences in actual motor competence (AMC), perceived motor competence (PMC) and enjoyment of physical activity among young children with different weight status. Methods: AMC, PMC and enjoyment were measured among 1708 children (50.4% male, mean age: 5.34 ± 0.73 years) from 36 primary schools in The Netherlands. AMC was measured by using the Athletic Skills Track (AST-1). The Pictorial Scale of Perceived Movement Skill Competence for Young Children was used for determining PMC and enjoyment of physical activity was measured using a Visual Analogue Scale. The data were analyzed using a three-way ANOVA to examine the differences between AMC, PMC and enjoyment by sex (boys/girls), age (4, 5, 6 years) and weight status (normal, overweight, obesity). Results: Overall, AMC was ranked as ‘average motor gifted’. Average PMC and enjoyment scores were 3.31 (SE 0.01) (1-4 scale) and 4.41 (SE 0.02) (1-5 scale) respectively. No interaction effects were found between sex, age and weight status on AMC or PMC. However, there was a statistically significant two-way interaction effect for enjoyment between age and weight status (F (4,1454) =2.464, p =.043). Relative enjoyment scores for normal weight and overweight groups between high and low enjoyment were distributed 99% to 1%. However, in the obese group there was a distribution of 92% to 8% between high and low enjoyment. Conclusions: The results of this study suggest that there are no significant differences in AMC and PMC between children of different sex, ages (4, 5 and 6 years), and weight status in this age group. However, children with obesity more often experience less enjoyment during physical activity than children with another weight status. Targeted intervention for increasing enjoyment during physical activity in combination with reducing obesity seems advisable even at young age.

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., Gamma-ray bursts (GRBs) are fascinating events due to their panchromatic nature. We study optical plateaus in GRB afterglows via an extended search into archival data. We comprehensively analyze all published GRBs with known redshifts and optical plateaus observed by many ground-based telescopes (e.g., Subaru Telescope, RATIR) around the world and several space-based observatories such as the Neil Gehrels Swift Observatory. We fit 500 optical light curves, showing the existence of the plateau in 179 cases. This sample is 75% larger than the previous one, and it is the largest compilation so far of optical plateaus. We discover the 3D fundamental plane relation at optical wavelengths using this sample. This correlation is between the rest-frame time at the end of the plateau emission, ${T}_{\mathrm{opt}}^{* }$, its optical luminosity, Lopt, and the peak in the optical prompt emission, Lpeak,opt, thus resembling the three-dimensional (3D) X-ray fundamental plane (the so-called 3D Dainotti relation). We correct our sample for redshift evolution and selection effects, discovering that this correlation is indeed intrinsic to GRB physics. We investigate the rest-frame end-time distributions in X-rays and optical (${T}_{\mathrm{opt}}^{* }$, ${T}_{{\rm{X}}}^{* }$), and conclude that the plateau is achromatic only when selection biases are not considered. We also investigate if the 3D optical correlation may be a new discriminant between optical GRB classes and find that there is no significant separation between the classes compared to the Gold sample plane after correcting for evolution. © 2022. The Author(s). Published by the American Astronomical Society., D.A.K. acknowledges support from Spanish National Research Project RTI2018-098104-J-I00 (GRBPhot). S.Y. and D.L. acknowledge the support by the United States Department of Energy in funding the Science Undergraduate Laboratory Internship (SULI) program. S.Y. gratefully acknowledges the support of the Vagelos Challenge Award at the University of Pennsylvania. R.L.B. acknowledges support from the DGAPA/UNAM IG100820 and the DGAPA/UNAM postdoctoral fellowship. N.F. acknowledges support from the DGAPA/UNAM IN106521. Some of the data used in this paper were acquired with the RATIR instrument, funded by the University of California and NASA Goddard Space Flight Center, and the 1.5-meter Harold L. Johnson telescope at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir, operated and maintained by the Observatorio Astronómico Nacional and the Instituto de Astronomía of the Universidad Nacional Autónoma de México. Operations are partially funded by the Universidad Nacional Autónoma de México (DGAPA/PAPIIT IG100414, IT102715, AG100317, IN109418, IG100820, IN106521, and IN105921). We acknowledge the contribution of Leonid Georgiev and Neil Gehrels to the development of RATIR. M.F., L.Z., and A.Z. are grateful for the support from the Scientific Caribbean Foundation. E.S. thanks the Latino Education Advancement Foundation for their support., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

The temporal and spectral evolution of gamma-ray burst (GRB) afterglows can be used to infer the density and density profile of the medium through which the shock is propagating. In long-duration (core-collapse) GRBs, the circumstellar medium (CSM) is expected to resemble a wind-blown bubble, with a termination shock, separating the stellar wind and the interstellar medium (ISM). A long standing problem is that flat density profiles, indicative of the ISM, are often found at lower radii than expected for a massive star progenitor. Furthermore, the presence of both wind-like environments at high radii and ISM-like environments at low radii remains a mystery. In this paper, we perform a ‘CSM population synthesis’ with long GRB progenitor stellar evolution models. Analytic results for the evolution of wind blown bubbles are adjusted through comparison with a grid of 2D hydrodynamical simulations. Predictions for the emission radii, ratio of ISM to wind-like environments, wind, and ISM densities are compared with the largest sample of afterglow derived parameters yet compiled, which we make available for the community. We find that high ISM densities of n ∼ 1000 cm−3 best reproduce observations. If long GRBs instead occur in typical ISM densities of n ∼ 1 cm−3, then the discrepancy between theory and observations is shown to persist at a population level. We discuss possible explanations for the origin of variety in long GRB afterglows, and for the overall trend of CSM modelling to over-predict the termination shock radius. © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society., BPG and MN are supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 948381). DAK acknowledges support from Spanish National Research Project RTI2018-098104-J-I00 (GRBPhot). AJvM is supported by the ANR-19-CE31-0014GAMALO project. AJL has received funding from the European Research Council (ERC) under the European Union’s Seventh Framework Programme (FP7-2007-2013) (Grant agreement No. 725246). ERS has been supported by STFC consolidated grant ST/P000495/1. PJG is supported by NRF SARChI Grant 111692. We gratefully acknowledge the use of GOTOHEAD, the computing cluster of the Gravitational-wave Optical Transient Observer (GOTO), as well as support from Joe Lyman and Krzysztof Ulaczyk., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Full list of authors: Rastinejad, Jillian C.; Gompertz, Benjamin P.; Levan, Andrew J.; Fong, Wen-Fai; Nicholl, Matt; Lamb, Gavin P.; Malesani, Daniele B.; Nugent, Anya E.; Oates, Samantha R.; Tanvir, Nial R.; Postigo, Antonio de Ugarte; Kilpatrick, Charles D.; Moore, Christopher J.; Metzger, Brian D.; Ravasio, Maria Edvige; Rossi, Andrea; Schroeder, Genevieve; Jencson, Jacob; Sand, David J.; Smith, Nathan; Fernandez, Jose Feliciano Agui; Berger, Edo; Blanchard, Peter K.; Chornock, Ryan; Cobb, Bethany E.; De Pasquale, Massimiliano; Fynbo, Johan P. U.; Izzo, Luca; Kann, D. Alexander; Laskar, Tanmoy; Marini, Ester; Paterson, Kerry; Escorial, Alicia Rouco; Sears, Huei M.; Thone, Christina C., Gamma-ray bursts (GRBs) are divided into two populations1,2; long GRBs that derive from the core collapse of massive stars (for example, ref. 3) and short GRBs that form in the merger of two compact objects4,5. Although it is common to divide the two populations at a gamma-ray duration of 2 s, classification based on duration does not always map to the progenitor. Notably, GRBs with short (≲2 s) spikes of prompt gamma-ray emission followed by prolonged, spectrally softer extended emission (EE-SGRBs) have been suggested to arise from compact object mergers6,7,8. Compact object mergers are of great astrophysical importance as the only confirmed site of rapid neutron capture (r-process) nucleosynthesis, observed in the form of so-called kilonovae9,10,11,12,13,14. Here we report the discovery of a possible kilonova associated with the nearby (350 Mpc), minute-duration GRB 211211A. The kilonova implies that the progenitor is a compact object merger, suggesting that GRBs with long, complex light curves can be spawned from merger events. The kilonova of GRB 211211A has a similar luminosity, duration and colour to that which accompanied the gravitational wave (GW)-detected binary neutron star (BNS) merger GW170817 (ref. 4). Further searches for GW signals coincident with long GRBs are a promising route for future multi-messenger astronomy. © 2022, The Author(s), under exclusive licence to Springer Nature Limited., The Fong group at Northwestern acknowledges support by the National Science Foundation under grant nos. AST-1814782 and AST-1909358 and CAREER grant no. AST-2047919. W.F. gratefully acknowledges support by the David and Lucile Packard Foundation. A.J.L. and D.B.M. are supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 725246). M.N. and B.P.G. are supported by the ERC under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 948381). M.N. acknowledges a Turing Fellowship. G.P.L. is supported by the UK Science and Technology Facilities Council grant ST/S000453/1. A.R. and E.M. acknowledge support from the INAF research project ‘LBT - Supporto Arizona Italia’. J.F.A.F. acknowledges support from the Spanish Ministerio de Ciencia, Innovación y Universidades through the grant PRE2018-086507. D.A.K. and J.F.A.F. acknowledge support from Spanish National Research Project RTI2018-098104-J-I00 (GRBPhot). W. M. Keck Observatory and MMT Observatory access was supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We wish to recognize and acknowledge the very important cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. On the basis of observations obtained at the international Gemini Observatory (programme ID GN2021B-Q-109), a programme of NOIRLab, 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). Processed using the Gemini IRAF package and DRAGONS (Data Reduction for Astronomy from Gemini Observatory North and South). This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the AURA, Inc., under NASA contract NAS 5-26555. These observations are associated with programme no. 16923. This work is partly based on observations made with the Gran Telescopio Canarias, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. Partly based on observations collected at the Calar Alto Astronomical Observatory, operated jointly by Instituto de Astrofísica de Andalucía (CSIC) and Junta de Andalucía. Partly based on observations made with the Nordic Optical Telescope, under programme 64-502, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, respectively, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofísica de Canarias. The LBT is an international collaboration among institutions in the United States, Italy and Germany. LBT Corporation partners are: The University of Arizona on behalf of the Arizona Board of Regents; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, The Leibniz Institute for Astrophysics Potsdam and Heidelberg University; The Ohio State University, representing OSU, University of Notre Dame, University of Minnesota and University of Virginia.