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Developing sustainable software for the scientific community requires expertise in software engineering and domain science. This can be challenging due to the unique needs of scientific software, the insufficient resources for software engineering practices in the scientific community, and the complexity of developing for evolving scientific contexts. While open-source software can partially address these concerns, it can introduce complicating dependencies and delay development. These issues can be reduced if scientists and software developers collaborate. We present a case study wherein scientists from the SuperNova Early Warning System collaborated with software developers from the Scalable Cyberinfrastructure for Multi-Messenger Astrophysics project. The collaboration addressed the difficulties of open-source software development, but presented additional risks to each team. For the scientists, there was a concern of relying on external systems and lacking control in the development process. For the developers, there was a risk in supporting a user-group while maintaining core development. These issues were mitigated by creating a second Agile Scrum framework in parallel with the developers' ongoing Agile Scrum process. This Agile collaboration promoted communication, ensured that the scientists had an active role in development, and allowed the developers to evaluate and implement the scientists' software requirements. The collaboration provided benefits for each group: the scientists actuated their development by using an existing platform, and the developers utilized the scientists' use-case to improve their systems. This case study suggests that scientists and software developers can avoid scientific computing issues by collaborating and that Agile Scrum methods can address emergent concerns., Revisions: in response to peer-review recommendations, most sections have been substantially expanded and reworked, five new figures have been added, and the title has been changed. Results unchanged

According to the World Health Organization, about 15% of those who are infected by COVID-19 become seriously ill and 5% become so critically ill that they need intensive care, requiring mechanical ...

A large number of measurements with polarized beams and/or spin analysis of final state particles has been performed at the e^+e^- colliders LEP and SLC, providing important information on the dynamics of high energy interactions. In this paper three subjects, for which the role of spin studies was particularly relevant, will be covered: the measurements of the electroweak couplings, the study of fragmentation dynamics and the search for physics beyond the Standard Model., Comment: 11 pages, Invited talk given at the International Workshop on Symmetry and Spin - Prague, Czech Republic, August 30 - September 5, 1998

This report, based on the Dark Sectors workshop at SLAC in April 2016, summarizes the scientific importance of searches for dark sector dark matter and forces at masses beneath the weak-scale, the status of this broad international field, the important milestones motivating future exploration, and promising experimental opportunities to reach these milestones over the next 5-10 years., 66 pages, 15 figures, 3 tables. Workshop website and agenda: http://www-conf.slac.stanford.edu/darksectors2016/ https://indico.cern.ch/event/507783/ Editors: J. Alexander, M. Battaglieri, B. Echenard, R. Essig, M. Graham, E. Izaguirre, J. Jaros, G. Krnjaic, J. Mardon, D. Morrissey, T. Nelson, M. Perelstein, M. Pyle, A. Ritz, P. Schuster, B. Shuve, N. Toro, R. Van De Water

Several astrophysical observations, both on a galactic and cosmologicalscales, showing that there’s a “missing mass” in the observable Universe, can be explained assuming a non-luminous kind of matter, hence called “dark matter”. One of the most promising candidates is the Weakly Interacting Massive Particle (WIMP), a non-relativistic massive particle, gravitationally and weakly interacting with baryonic matter. The present work is specifically focused on the physics potential besides WIMP search of dark matter detectors filled with Liquid argon, like DarkSide and DEAP-3600. Liquid argon is an optimal target thanks to its high scintillation and ionization yields. DEAP-3600 is a single-phase detector, exploiting the scintillation channel only, while DarkSide-20k and Argo, future tonne scale experiments from the DarkSide program, are dual-phase Time Projection Chambers (TPCs), looking at both scintillation and ionization signals. The large mass (3.3 tons) of the DEAP-3600 target has allowed me to perform an analysis to search for Multi Interacting Massive Particles (MIMPs), a dark matter candidate alternative to WIMPs, at masses above 10 16 GeV and with argon-dark matter spin-independent cross-section of about 10 −22 cm 2 , fully setting up the upcoming unblinding of three years of data taking. Going from the present to the future dark matter detectors, DarkSide-20k and Argo will be characterized by an extraordinary sensitivity at low energy recoils. This is mainly consequence of the high energy resolution of the chosen photodetectors, Silicon Photomultipliers (SiPMs). Custom SiPMs have been designed for the dark matter search in DarkSide-20k; hence, SiPMs have been here characterized, with a focus on their correlated noises, namely afterpulses and optical crosstalks. The same sensitivity at low energy brings also to a strong potential in detecting supernova neutrinos via coherent elastic neutrino-nucleus scattering (CEvNS) in argon by exploiting the ionization signal. The related sensitivity study is here performed showing that the neutrino emission will be detected for any galactic supernova, with a good accuracy in reconstructing the main parameters of the burst, namely the total energy of neutrinos andtheir average energy.; Plusieurs observations astrophysiques, tant galactique que cosmologique, montrant qu’il y a une ”masse manquante” dans l’Univers observable, peuvent être expliquées en supposant une matière non lumineuse, donc appelée ”matière noire”. L’un des candidats les plus prometteurs est le Weak Interacting Massive Particle (WIMP), une particule massive non relativiste, capable d’une interaction gravitationnelle et d’une interaction faible avec la matière baryonique. Le présent travail est axé sur le potentiel physique en plus de la recherche des WIMPs des détecteurs de matière noire remplis d’argon liquide, comme DarkSide et DEAP-3600. L’argon liquide est une cible optimale grâce à ses rendements élevés de scintillation et d’ionisation.DEAP-3600 est un détecteur monophasique qui exploite uniquement le canal de scintillation, tandis que DarkSide-20k et Argo, les futures expériences à l’échelle des tonnes du programme DarkSide, sont des chambres de projection temporelle (TPCs) biphasiques qui examinent les signaux de scintillation et d’ionisation. La grande masse (3.3 tonnes) de la cible de DEAP-3600 a permis d’effectuer une analyse pour rechercher des Multi Interacting Massive Particles (MIMPs), une possible alternative aux WIMPs, à des masses supérieures à 10 16 GeV et avec une section efficace indépendante du spin matière noire-argon d’environ 10 −22 cm 2 . Ce travail est la phase préparatoire à l’ouverture de 3 années de collection de données. Du présent aux futurs détecteurs de matière noire, DarkSide-20k et Argo seront caractérisés par une sensibilité extraordinaire aux faibles reculs d’énergie. Ceci est principalement la conséquence de la haute résolution énergétique des photodétecteurs choisis, les photomultiplicateurs de silicium (SiPMs). Les SiPMs personnalisées ont été fabriques pour la recherche de la matière noire dans DarkSide-20k; par conséquence, les SiPMs ont été ici caractérisées, avec un accent sur leurs bruits corrélés : les afterpulses et les optical crosstalks. La même sensibilité à basse énergie apporte également un fort potentiel de détection des neutrinos de supernova par coherent elastic neutrino-nucleus scattering (CEvNS) dans l’argon en exploitant le signal d’ionisation. L’étude de sensibilité correspondante est ici réalisée et il montre que l’émission de neutrinos sera détectée pour toute supernova galactique, avec une bonne précision dans la reconstruction des principaux paramètres de l’éclatement, c’est-à-dire l’énergie totale des neutrinos et leur énergie moyenne.