fairdataihub/poster-sentry-training-data huggingface dataset:
Co-Creative Decision-Makers for 5.0 Organizations Value Co-Creation Labs 6 national networks of socio-economic actors dedicated to 5.0 collaborative value creation will be established. The VCC Labs are physical installations based on the Digital Innovation Environment powered by OMiLAB, enhanced with 5.0 resources that facilitate multi-stakeholder collaboration. Innovation Boosters and Catalyzers A knowledge sharing platform dedicated to support both BOOSTERS (collaborative 5.0 networks and initiatives among socio-economic actors) and CATALYZERS (learning and educational activities for the certification and development of knowledge, skills and competences) will be developed. 30 cases studies of 5.0 collaborative innovation projects will be implemented, emphasized by an annual International Prize of Innovation. 5.0 Certification A unique European Open Badge Certification for Decision-Makers for 5.0 Organization will be created and experimented, with an objective of more than 450 badges at the end of the project. Materials and methodologies, covering knowledge, skills and competencies with a unique development frame, shared by all sectors of application (health, agritechnology, industry) are included. Educational and Vocational Training The learning content required for 5.0 organizational Decision-Makers is collaboratively designed by Higher Education Institutions (HEI) and Vocational Education and Training (VET) facilities, supported by the industry partners with case-study and praxis examples. 8 vocational training offers and 11 academic training curriculum will be implemented and experimented through 6 European countries. Project Lead: Prof. Xavier Boucher Mines Saint-Etienne, France info@codemo-project.eu Follow & Join Us on the 5.0 Journey! Duration: Oct. 23 - Sept. 26 Project Number: 101104819 Our Partners: resilient . human-centric . sustainable
New Immunofluorescence-Based Services CD BioSciences, a US-based biotechnology company focusing on the development of imaging technology, has recently launched its new services based on immunofluorescence technology to provide researchers with diverse analysis and accurate results on fixed or fresh samples. These new services can be applied to the detection of circulating autoantibodies/antigens in cells and cell membranes/ immune complexes in biopsy material/circulating immune cells. Immunofluorescence is one of many techniques used in biomedical research and diagnosis. It uses the sensitivity and selectivity of fluorescence to analyze biological tissues. The basic reaction in immunology is the antigen-antibody reaction. When an antigen-antibody reaction occurs, the high specificity of the reaction means that once one factor is known, another factor can be identified. In the immunofluorescence technique, an antibody (or antigen) is labeled with a fluorochrome that does not interfere with the activity of the antigen and antibody, binds to its counterpart, and shows a specific fluorescent reaction under a fluorescence microscope. Immunofluorescence techniques can be used to detect proteins and other biomolecules in cells and tissues. Scientists can utilize immunofluorescence technology for a variety of laboratory tests and observations, providing a new perspective on the samples being analyzed. Researchers can also apply this technique to fixed or fresh samples to obtain multiple analysis and accurate results. CD BioSciences now offers customers with customized services based on immunofluorescence technology for scientific studies, including detection techniques of Fluorescence Microscopy, Laser Scanning Confocal Microscopy, and Flow Cytometry. The basic function of a fluorescence microscope is to transfer excitation energy to a fluorescent dye in the specimen, separate the weakly emitted fluorescence from the excitation light, and deliver it to a detector to produce a contrast image. The specificity and high sensitivity of Fluorescence Microscopy allow it to study cellular and subcellular structures in biological tissues at high resolution. It provides three-dimensional spatial information and temporal variation of spatial information in living cells. Confocal Microscopy is a well-established biomedical research tool that provides enhanced light microscopic imaging of cells labeled with fluorescent dyes. Its main application is the high-resolution analysis of subcellular components in three dimensions. The main difference to conventional epifluorescence microscopy is the imaging method. The former provides an image of the entire specimen, while Confocal Microscopy focuses on a single spot of light and scans the specimen line by line.
Processus d’apprentissages et de développement de compétences en situation informelle à travers l’utilisation des TIC Valérie Payen Jean Baptiste, Haïti, valeriejbpayen@gmail.com Doctorante, Université de Genève-TECFA, Suisse Brève présentation de l’étude: cette thèse est centrée sur l’étude des apprentissages réalisés en dehors d’un milieu formel. L’objectif est de rendre compte des processus d’apprentissages et de développement de compétences en milieu informel via l’utilisation des TIC. Pour explorer l’objet d’étude les pratiques des vendeurs et réparateurs évoluant dans le secteur économique informel en Haïti furent observés et analysés. Ces pratiques regroupent les activités d’appropriation, d’exploitation, et de transformations exercées sur et avec l’outil téléphonique par les acteurs du milieu, leurs modes d’organisations, de production et leurs processus de transmission de savoirs. Cadre théorique: Trois axes théoriques son mobilisées pour étudier le concept de l’apprentissage informel 1- Les systèmes d’activité humaine médiatisée par un artefact pour l’apprentissage de nouvelles compétences (Théorie instrumentale de Rabardel , 1995. Les théories des systèmes d’action, Leontiev, 1978; Vygosky , 1978; Engerström, 1987 2- L’influence des pratiques sociales sur le processus d’apprentissage (Les trois dimensions d’influence des pratiques sociales, Wenger, 2005). 3- Parcours de développement des compétences: les trois approches de reconnaissance des compétences (Le Bortef,1998). L’influence des trajectoires sur le développement des compétences Dominice, 1999 Méthodologie: Recherche ethnographique en immersion sur plusieurs sites d’observations différentes selon l’approche ethnographique itinérante multi située (Marcus, 1995) sur deux années consécutives : 2017 – 2019. Collectes des données - Entretiens, Observation participante et non participante audios via WhatsApp - Entretiens semi diriges. - Observation participante in situ - Enregistrements audios et vidéos. Analyse des données Analyse thématique descriptive et interprétative des données Vander Maren, 1996; Braun & Clark, 2006; Miles, M. B., Huberman, A. M., & Saldana, 2013 Question principale de recherche: quelles sont les actions, les interactions, les modes d’organisation, les trajectoires qui influencent l’apprentissage et le développement de compétences des vendeurs, des réparateurs et fabricants de téléphones mobiles sur le marché informel en Haïti ? FACULTÉ DE PSYCHOLOGIE ET DES SCIENCES DE L’ÉDUCATION
Humanities for Change Un network sul futuro delle discipline umanistiche CHI SIAMO Humanities for Change è un network di giovani studiosi e studenti universitari che intende presentare un ideale alternativo per il presente e il futuro della cultura umanistica. L’assunto di base è che le discipline umanistiche debbano fuoriuscire dalle cerchie ristrette del dibattito accademico per divenire strumento dell’agire pratico e prerequisito essenziale per una società democratica. In questo modo possono offrire una maggiore consapevolezza della complessità propria delle problematiche di ordine politico, sociale ed economico. IL PUBBLICO Con la sua attività di divulgazione, il network si propone di raggiungere una vasta platea, non di soli esperti del settore. L’approccio contaminatorio e multidisciplinare di cui si avvale è perseguito con il costante utilizzo di più canali di comunicazione (social network, video, blog, rivista) in grado di intercettare diverse fasce di pubblico ed è favorito dalla distribuzione di tutti i contenuti con una licenza Creative Commons che ne incentiva la condivisione. ✦ Il blog di Humanities for Change, con i suoi articoli in italiano e/o in inglese pubblicati sul sito principale e sulla piattaforma di blog accademici Hypotheses, è uno spazio di dialogo dove i giovani specializzandi possono pubblicare i loro contributi. Accoglie anche le recensioni delle principali novità editoriali del settore. ✦ Grazie alla collaborazione con altre associazioni culturali, a partire dagli articoli di digital and public history proposti nel blog vengono realizzate alcune interviste a docenti ed esperti. In aggiunta a ciò, il network pubblica in autonomia podcast e brevi video su alcune tematiche di rilievo. ✦ Con il ﬁnanziamento degli enti universitari, il network realizza alcuni eventi nei quali un relatore esterno dialoga con un docente dell’università ospitante e con un collaboratore del network. Per raggiungere un pubblico più ampio, gli incontri sono trasmessi in streaming. ✦ L’ultima sﬁda (ancora in corso) è quella di realizzare una rivista scientiﬁca internazionale, quadrimestrale, con un sistema di double-peer review. Accoglierà contributi in lingua inglese più corposi di quelli del blog e sarà distribuita in formato open- access su un nuovo sito e sui portali tematici di riferimento. INIZIATIVE E PROGETTI www.humanitiesforchange.org ✦ www.hfc.hypotheses.org ✦ info@humanitiesforchange.org CREDITS: SARTOR 2020
Space Weather Monitoring at the Rosse Solar-Terrestrial Observatory Peter Gallagher, Eoin Carley, Pietro Zucca, Joseph McCauley, Diana Morosan, Sean Blake School of Physics, Trinity College Dublin, Ireland Alan Jones, Colin Hogg School of Cosmic Physics, Dublin Institute for Advanced Studies, Ireland ! The Rosse Solar-Terrestrial Observatory (RSTO) was established at Birr Castle in the midlands of Ireland to study solar activity and space weather effects on the Earth's ionosphere and geomagnetic field. A set of solar radio spectrometers based on CALLISTO receivers monitor the Sun at 10-400 MHz, while a magnetometer is used to measure the local geomagnetic field and associated K-index. In addition, the ionosphere is monitored using a sudden ionospheric disturbance instrument. All data are provided in near-realtime at www.rosseobservatory.ie. X-rays associated with solar flares can disturb the Earth’s ionosphere and interrupt radio-based communications systems across the day side of the Earth. The RSTO sudden ionospheric disturbance instrument is used to m o n i t o r v e r y l o w frequency (VLF) signals. The ionosphere reacts rapidly to radiation from solar flares and can take hours to recover. Solar radio bursts can cause interruptions in communications systems on Earth. At RSTO, solar radio bursts are monitored using CALLISTO spectrometers at 10-400 MHz (Zucca et al, Solar Physics, 2012). ! A bicone and a LOFAR Low Band Antenna array observe the Sun at 10-100 MHz while a log-periodic operates at 100-400 MHz. The frequency band is covered by 1,800 channels, sampling at 250 ms per sweep. ! The system is optimised to measure dynamic spectra of Type II radio bursts produced by coronal shocks, and Type III radio bursts produced by near-relativistic electrons streaming along open magnetic field lines. ! Solar Radio Bursts Ionospheric Distrubances The Future of RSTO RSTO is part of an international effort to study the physics of space weather, and monitor the effects of the Sun on the Earth. We are now exploring joining a number of networks, such as LOFAR and SuperDARN, which w o u l d e n a b l e u s t o m o r e accurately monitor the causes and consequences of space weather. I-LOFAR www.lofar.ie Geomagnetic Storms Geomagnetic storms can be produced by the coronal mass ejections and changes in the interplanetary magnetic field. ! A magnetometer at RSTO measures the geomagnetic field which is used to derive a local K-index in near-realtime.
Abstract M. Tsantaki1, D. Andreasen2 1Osservatorio Astrofisico di Arcetri – INAF, 2Instituto de Astrofísica e Ciências do Espaço Methodology We knowledge the funding from MIUR Premiale 2016: MITIC The synthetic spectra are created on-the-fly and are convolved with: 1) macroturbulence, 2) projected rotational velocity, 3) instrumental broadening to match the observations. Models atmospheres: Kurucz (Kurucz 1993) & MARCS models (Gustafsson et al 2008). Line lists: Tsantaki et al. (2018) for stellar parameters and Adibekyan et al. (2015) and Delgado Mena et al. (2015) for the chemical abundances. Spectral manipulation: local normalization and filters for cosmic rays The line list Li abundances The atomic data of the line list is calibrated based on the Solar & Arcturus Atlases. Comparison of synthetic spectrum with VALD3 data (green line), synthetic spectrum after the calibration of the atomic data (red line) and the Atlases (black line) (see Tsantaki et al. 2018). An example of the fit of the lithium line for a giant star from our recent work on Li abundances in open clusters. The synthetic fit is in green and the observations in black. Acknowledgements References Resutls FASMA has been used in the following works: - characterization of planet hosts for the Ariel mission Brucalassi et al. 2021 - characterization of high and medium resolution samples Tsantaki et al. 2018 - derivation of Li abundances for giant stars in open clusters (Tsantaki et al. 2021 in prep.) FASMA: a package for stellar parameters and chemical abundances Code description: Tsantaki et al. 2020 https://github.com/MariaTsantaki/FASMA-synthesis Science validation: Tsantaki et al. 2018 FASMA delivers the atmospheric stellar parameters: effective temperature, surface gravity, metallicity, microturbulence, macroturbulence, and rotational velocity based on the spectral synthesis technique. The principle of the technique relies on the comparison of synthetic spectra with observations to yield the best- fit parameters under a χ2 minimization. FASMA also delivers chemical abundances of 13 elements (Li, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, and Ni). The python code is wrapped around the spectral synthesis package: MOOG version 2019 (Sneden et al. 1973) in a very user-friendly way.
Variable Star Science with Community Brokers: Overview and goals Nina Hernitschek (CITEVA, Universidad de Antofagasta; Rubin LSST Transients and Variable Stars Science Collaboration) Community Alert Brokers How LSST can help Variable Stars software systems to provide, characterize and classify big data to enable science change in luminosity few parts per million factor 1000 temporal baseline seconds centuries signal shape periodic aperiodic/ random Periodic Variable Stars: RR Lyrae, Cepheids ►measure apparent mean brightness m ►measure period P ►using period-luminosity relation, get absolute brightness M ►solve distance modulus equation: log d [parsec]= (m−M+5) /5 period (days) absolute magnitude -7 -6 -5 -4 -3 -2 -1 0 1 0.3 1 3 10 30 100 RR Lyrae Type II Cepheids Type I (classical) Cepheids Rubin Observatory's real-time difference image analysis will produce a world-public stream of alerts which will be distributed to community brokers. The Importance of Long-Time Monitoring accurate, up-to-date information (and not from data taken years ago) necessary to dynamically characterize substructure in the outer Galactic halo periodic variable stars allow for distance calculation: Their period is directly related to their true brightness. variability important for velocity calculation: vobs = vsystemic + vphotospheric from pulsation models: observe at φ = 0.37 where vphotospheric ∼0 crucial: accurate light curve information What are variable stars? A star is a variable star if we can measure its brightness changing over time. Variable stars differ regarding how those brightness changes are caused by events inside, on the surface of, or around that star. Why are variable stars important? variations provide unique information about the nature and evolution of stars and the galaxies that host them and our universe in general period-amplitude modulations (Blazhko effect) must be taken into account to correctly determine distances and velocities allow us for creating 3D maps of structures in our Milky Way typical use cases from complex data: ►immediate follow-up (e.g.: supernova, multi-messenger astronomy) ►“unknown unknowns” ►known rare “1-in-a-million” events possible with LSST: large footprint high cadence depth 10 years + ´+ + ´ LSST: ~400 kpc PS1 3π: ~120 kpc 10 kpc limit of SDSS studies for kinematics and [Fe/H] Point of Interest Broker (POI) The idea: An alert broker to enable users to get updates on variable star observations within interesting regions. predefined stellar streams, dwarf galaxies and globular clusters (frequently updated) user-defined The Implementation POI is a downstream broker of ANTARES. ►store feature history ►more specific classification ►amplitude-period-phase modulation (Blazhko effect) ►watch for modulation ►specific “Points of Interest” ►specific calculations for follow-up: phase/time from model
The work involves the use of optical resonating cavity used for light analyte interaction which is based on a coupled ring resonator geometery. The procedure is to sense the presence of a chemical and to covert the presence of chemical/biochemical analyte into a measurable optical signal. Introduction • Optical sensors fundamentally require interaction between light and target molecules. • Increased interaction result in increased sensitivity. • In a waveguide or optical sensor light interacts with target molecule only once. In a resonator, light circulates in resonator multiple times. • Ring resonators finds application as a chemical sensor for variety of applications like biochemical assays, sample preparation, genomics ,drug development and investigation, food safety and environmental monitoring. • Various chemical sensors based on ring resonating cavity had different operational geometries solely dependent on the fabrication method. Simulation • Parameters considered in simulation : Waveguide width, height, thickness, radius and coupling length to be constant. • Coupling Gap is variable. • Top clad changed from a solution to water (optimization analysis). • Method : Wavelength Scanning. • 50000 test points. • Results discussed : resonance spectrum, mainly drop port. • Optimized Geometry. Results Experimental Setup Remarks • Light Source : Collimation, Beam width and Spot Size • Test Setup : Detection, Microscope, 3 dimensional motion controllers, Spectrometer, power meter, microscope. • The detection methodology is to detect the resonance wavelength which can be identified by intensity measurement at resonant wavelength picked up at drop port. Optical Characterization Of A Polymer Ring- Resonator Used For Environmental Monitoring Of Chemical Pollutants Zain Hayat, Farida Meziane, Simon Joly, Vincent Raimbault, Laurent Bechou Laboratory Material Integration System (IMS) University of Bordeaux France
The Stellar and Observational Properties of the TESS Prime Mission 2-min Targets Joshua Pepper1, Thomas Barclay2,3, Luke G. Bouma4, Christopher J. Burke5, Michael Fausnaugh5, B. Scott Gaudi6, Ryan J. Oelkers7,8, Keivan G. Stassun8,9, Joshua N. Winn4 1 Lehigh University, 2 NASA Goddard Space Flight Center, 3 University of Maryland, Baltimore County, 4 Princeton University, 5 Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 6 The Ohio State University, 7 Texas A&M University, 8 Vanderbilt University, 9 Fisk University See upcoming paper from Fausnaugh, et al. The K-dwarf valley Photometric precision across the main sequence TESS Observing Duration Properties for all Targets 153,000 stars observed for one sector 9,000 stars observed for >260d, but only 3,900 observed continuously References: • Stassun, et al. 2018 “The TESS Input Catalog and Candidate Target List“ AJ, 156, 102 • Stassun, et al. 2019 “The Revised TESS Input Catalog and Candidate Target List“ AJ, 158, 138 Figure 3: Since photometric precision is generally a monotonic function of apparent brightness, early-type stars being more luminous have more precise light curves. Although the TESS target selection process prioritized smaller stars at a given apparent brightness, late-type dwarfs are substantially fainter, yielding light curves with lower precision. Figure 2: Stars are prioritized for transit observations according to their sensitivity to the smallest detectable transits. That depends on their brightness and size. F and G dwarfs dominate that set due to their brightness, while M dwarfs are also included due to their small size. Once the closest F and G dwarfs are included, M dwarfs (being more common) occupy the next batch of targets. K dwarfs suffer in this metric due to being too faint for good photometric precision compared to F and G dwarfs, but too big to yield deep transits compared to M dwarfs. Figure 1: TESS observed 232,705 stars with 2-min cadence in the prime mission. The stars were selected for a number of science purposes, with the largest batch coming from the exoCTL, which prioritized stars based on their suitability for small planet transit detection and the length of time TESS observes them. Stars closer to the continuous viewing zones thus have higher priority. But the mission requires a certain number of target stars in each camera and CCD. Therefore the stars observed at mid-latitudes have different population characteristics than those at high latitudes, as shown in Fig 2 above. Figure 4: Most stars (abut 153,000 out of 233,000) were observed for just a single sector in the prime mission. But just because a star is in or near the continuous viewing zone, they are not necessarily observed during every sector, due to gaps between cameras or detectors. Only 3,900 stars were observed in 13 consecutive sectors. All data described in this poster will be distributed as machine- readable tables in an upcoming paper.