Clinical Features, Cardiovascular Risk Profile, and Therapeutic Trajectories of Patients with Type 2 Diabetes Candidate for Oral Semaglutide Therapy in the Italian Specialist Care

Introduction: This study aimed to address therapeutic inertia in the management of type 2 diabetes (T2D) by investigating the potential of early treatment with oral semaglutide. Methods: A cross-sectional survey was conducted between October 2021 and April 2022 among specialists treating individuals with T2D. A scientific committee designed a data collection form covering demographics, cardiovascular risk, glucose control metrics, ongoing therapies, and physician judgments on treatment appropriateness. Participants completed anonymous patient questionnaires reflecting routine clinical encounters. The preferred therapeutic regimen for each patient was also identified. Results: The analysis was conducted on 4449 patients initiating oral semaglutide. The population had a relatively short disease duration (42%  60% of patients, and more often than sitagliptin or empagliflozin. Conclusion: The study supports the potential of early implementation of oral semaglutide as a strategy to overcome therapeutic inertia and enhance T2D management

Supplement: "Localization and broadband follow-up of the gravitational-wave transient GW150914" (2016, ApJL, 826, L13)

This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands

Multi-messenger observations of a binary neutron star merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta

Localization and broadband follow-up of the gravitational-wave transient GW150914

A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline, and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams

Localization and Broadband Follow-up of the Gravitational-wave Transient GW150914

A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline, and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams. </p

Multi-messenger Observations of a Binary Neutron Star Merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ∼ 1.7 {{s}} with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of {40}-8+8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 {M}ȯ . An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ∼ 40 {{Mpc}}) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ∼ 9 and ∼ 16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.</p

Localization and broadband follow-up of the gravitational-wave transient GW150914

A gravitational-wave transient was identified in data recorded by the Advanced LIGO detectors on 2015 September 14. The event candidate, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the gravitational wave data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network Circulars, giving an overview of the participating facilities, the gravitational wave sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the electromagnetic data and results of the electromagnetic follow-up campaign will be disseminated in the papers of the individual teams

Retour d'expérience sur les dispositifs d'alerte appliqués aux instabilités de pente

International audienceWith climate change and the growing urbanization of areas at risk, the development of early warning systems has progressed considerably. Now, they are deployed at local and/or regional scale and integrate a set of complex tools and processes. Feedback underlines the need to develop practices to improve their efficiency and obtain better support from the population.Avec le changement climatique et l’urbanisation croissante de territoires à risque, le développement des dispositifs d’alerte a beaucoup progressé. Ils sont maintenant déployés à l’échelle locale et/ou territoriale et intègrent un ensemble d’outils et de processus complexes. Le retour d’expérience souligne la nécessité de faire évoluer les pratiques pour améliorer leur efficacité et obtenir une meilleure adhésion de la population

Feedback on four exemplary early warning systems for landslides

International audienceIn some contexts, the only solution to manage the risk of slope instability induced by precipitation is to set up an early warning system. Such systems are designed to issue warnings at the right time to enable action to be taken and to guarantee public safety, for landslides can be deployed at the scale of a single slope or at regional scale. Sometimes, local and regional systems coexist in the same area without a real synergy. In order to illustrate the conditions and frameworks in which these different systems operate, this article focuses on four exemplary systems: the Ruines de Séchilienne in France and the Ancona landslide in Italy at the local scale, Norway and Hong Kong systems at the regional scale. This article is based on scientific literature. Note that the scientific observation systems and the monitoring systems, that do not address the issue of response capability, are not included in it.Dans certains contextes, la seule solution pour gérer le risque d’instabilités de pente induites par les précipitations est l’installation de dispositifs d’alerte. Ces dispositifs sont déployés pour produire des alertes en temps opportun afin de garantir la sécurité des populations exposées, pour les instabilités de pente ils sont installés à l’échelle d’un seul versant ou à l’échelle régionale. Parfois, les deux échelles coexistent sur le même territoire sans une réelle synergie. Pour illustrer les conditions et les contextes de ces dispositifs, cet article présente quatre dispositifs emblématiques : les Ruines de Séchilienne en France et Ancône en Italie, à l’échelle locale, la Norvège et Hong Kong à l’échelle régionale. Cet article se base sur la littérature scientifique. A noter que ni les dispositifs d’observation ni les systèmes de surveillance, qui ne prennent pas en compte la capacité de réponse, n’y sont pas inclus

Accurate 3D location of mine induced seismicity in complex near-field underground conditions

International audienceThe monitoring of mine induced seismicity and rockburst hazard can be carried out at different scales of resolution. The strategy usually adopted aims to get a global coverage of the mine layout, based on a large-scale array of low-frequency seismic sensors which may extend up to tens of squared kilometers, in order to monitor the numerous disseminated mining works and enable a periodical rating of seismic hazard. However, some major drawbacks must be dealt with. First, the microseismic detection limits for each mining work considered as a stand-alone rockburst prone area induces the loss of all those small magnitude events occurring in the vicinity of the working faces. Moreover, quality of the seismic source location reveals insufficient to pinpoint unambiguously its very origin in the surrounding geology and mining voids. These two limits affect strongly the capabilities of ground engineers to detect for sure significant change in the seismic regime of any specific seismogenic zone. Refining the monitoring may be reached by the deployment of mobile local-scale arrays made of short period sensors around those mining works rated at higher risk. These permit to record a much more complete microseismic catalogue while enhancing drastically the accuracy and reliability of the expertise. However, the processing of small magnitude events recorded locally calls for some precautions due to some nearfield conditions adverse to accuracy. Besides the increasing complexity of the rock mass when dealing with higher frequency waves, the presence of important ancient backfilled works more or less interlaced with multilevel fast advancing mining works may be a very issue. This is often the case for highly productive methods based on retreat mining, cut-and-fill or sub-level mining. Because installing a socalled high resolution microseismic network rises new expectations in the understanding of the seismic activity versus the local geology and the mining process, the authors have undertaken the development of an evolving 3D velocity model taking into account not only the underground geological aspects encountered, but also and above all the dynamic mining process itself. Besides synthetic numerical tests that have been run to assess the relevance of this issue, we applied this new numerical procedure to a true microseismic dataset recorded during the controlled collapse of a large solution mined cavern lying 220 meters deep. Tens of thousands of microseismic events were recorded with the critical enlargement of the cavern towards the surface. 3D surveys of the cavern itself together with geophysical loggings of its geological overburden have been used to dimension the presence of this volume full brine and calibrate this innovative location procedure applied to selected microseismic swarms. Detailed comparisons with conventional 3D location studies have been established emphasizing the considerable gain brought by a more realistic three dimensional velocity model including the pre-existent and evolving voids before and during seismic crisis. This gain includes a much better separation of the fracturing processes in the cap rock and on the sidewalls of the cavern, discerning unambiguously the impact of the roof falls at the bottom of the cavity, delineating geological rock strata and discontinuities playing clearly a role in the physics of the collapse phenomena. Such a numerical procedure is currently being improved and automated for operational implementation in a deep mine