Architecture de transformée de cosinus discrète sur deux dimensions sans multiplication et mémoire de transposition

Au cours des dix dernières années, les capacités technologiques de transmission vidéo rendent possible une panoplie d'applications de télésanté. Ce média permet en effet la participation de médecins spécialisés à des interventions médicales ayant lieu à des endroits distants. Cependant, lorsque ces dernières se déroulent loin des grands centres, les infrastructures de télécommunication n'offrnt pas un débit assez important pour permettre à la fois une transmission d'images fluides et de bonne qualité. Un des moyens entrepris pour pallier ce problème est l'utilisation d'encodeur et décodeur vidéo (CODEC) permettant de compresser les images avant leur transmission et de les décompresser à la réception. Il existe un bon nombre de CODEC vidéo offrant différent compromis entre la qualité d'image, la rapidité de compression, la latence initiale de traitement et la robustesse du protocole de transmission. Malheureusement, aucun n'est en mesure de rencontrer simultanément toutes les exigences définies en télésanté. Un des problèmes majeurs réside dans le délai de traitement initial causé par la compression avec perte du CODEC. L'objet de la recherche s'intéresse donc à deux CODEC qui répondent aux exigences de délais de traitement et de qualité d'image en télésanté, et plus particulièrement pour une application de téléassistance en salle d'urgence. L'emphase est mise sur les modules de quantification des CODEC qui utilisent la transformée en cosinus discrète. Cette transformée limite la transmission des images vidéo fluide et quasi sans délais en raison des délais de traitement initiaux issus des nombreuses manipulations arithmétiques qu'elle requiert. À l'issu de la recherche, une structure efficace de la transformée en cosinus est proposée afin de présenter une solution au temps de latence des CODEC et ainsi de répondre aux exigences de télécommunication en télésanté. Cette solution est implémentée dans un CODEC JPEG développé en VHDL afin de simuler un contexte d'application réelle

A Coupled 2 × 2D Babcock–Leighton Solar Dynamo Model. I. Surface Magnetic Flux Evolution

The need for reliable predictions of the solar activity cycle motivates the development of dynamo models incorporating a representation of surface processes sufficiently detailed to allow assimilation of magnetographic data. In this series of papers we present one such dynamo model, and document its behavior and properties. This first paper focuses on one of the model's key components, namely surface magnetic flux evolution. Using a genetic algorithm, we obtain best-fit parameters of the transport model by least-squares minimization of the differences between the associated synthetic synoptic magnetogram and real magnetographic data for activity cycle 21. Our fitting procedure also returns Monte Carlo-like error estimates. We show that the range of acceptable surface meridional flow profiles is in good agreement with Doppler measurements, even though the latter are not used in the fitting process. Using a synthetic database of bipolar magnetic region (BMR) emergences reproducing the statistical properties of observed emergences, we also ascertain the sensitivity of global cycle properties, such as the strength of the dipole moment and timing of polarity reversal, to distinct realizations of BMR emergence, and on this basis argue that this stochasticity represents a primary source of uncertainty for predicting solar cycle characteristics

Clinical validation of a software for quantitative follow-up of abdominal aortic aneurysm maximal diameter and growth by CT angiography

Purpose To compare the reproducibility and accuracy of abdominal aortic aneurysm (AAA) maximal diameter (D-max) measurements using segmentation software, with manual measurement on double-oblique MPR as a reference standard. Materials and methods The local Ethics Committee approved this study and waived informed consent. Forty patients (33 men, 7 women; mean age, 72 years, range, 49–86 years) had previously undergone two CT angiography (CTA) studies within 16 ± 8 months for follow-up of AAA ≥35 mm without previous treatment. The 80 studies were segmented twice using the software to calculate reproducibility of automatic D-max calculation on 3D models. Three radiologists reviewed the 80 studies and manually measured D-max on double-oblique MPR projections. Intra-observer and inter-observer reproducibility were calculated by intraclass correlation coefficient (ICC). Systematic errors were evaluated by linear regression and Bland–Altman analyses. Differences in D-max growth were analyzed with a paired Student's t-test. Results The ICC for intra-observer reproducibility of D-max measurement was 0.992 (≥0.987) for the software and 0.985 (≥0.974) and 0.969 (≥0.948) for two radiologists. Inter-observer reproducibility was 0.979 (0.954–0.984) for the three radiologists. Mean absolute difference between semi-automated and manual D-max measurements was estimated at 1.1 ± 0.9 mm and never exceeded 5 mm. Conclusion Semi-automated software measurement of AAA D-max is reproducible, accurate, and requires minimal operator intervention

Reproducibility of abdominal aortic aneurysm diameter measurement and growth evaluation on axial and multiplanar computed tomography reformations

Purpose: Compare different methods measuring abdominal aortic aneurysm (AAA) maximal diameter (Dmax) and its progression on multi-detector computed tomography scan (MDCT). Materials and Methods: Forty AAA patients with 2 MDCT acquired at different time (baseline and follow-up) were included. Three observers measured AAA diameters by 7 different methods: on axial images (antero-posterior, transverse, maximal and short axis) and on multi-planar reformation (MPR) images (coronal, sagittal and orthogonal). Diameter measurement and progression were compared over time for the 7 methods. Reproducibility of measurement methods was assessed by intraclass correlation coefficient (ICC) and Bland-Altman analysis. Results: Dmax measured on axial slices at baseline and follow-up (FU) MDCTs was larger than that measured with use of orthogonal method (p=0.00001), whereas Dmax with the orthogonal method was larger than for all other measurement methods (p≤0.0001). The highest inter-observer ICCs were obtained for the orthogonal and transverse method (0.972) at baseline and for orthogonal and sagittal MPR at FU (0.973 and 0.977). Interobserver ICC of the orthogonal method to document AAA progression was higher (ICC=0.833) than measurements taken on axial images (ICC=0.662-0.780) and single plane MPRs (0.772-0.817). Conclusion: AAA Dmax measured on MDCT axial slices overestimates aneurysm size. Diameter measured by the orthogonal method is more reproducible, especially to document AAA progression

The Zwicky Transient Facility Census of the Local Universe. I. Systematic Search for Calcium-rich Gap Transients Reveals Three Related Spectroscopic Subclasses

Using the Zwicky Transient Facility alert stream, we are conducting a large spectroscopic campaign to construct a complete, volume-limited sample of transients brighter than 20 mag, and coincident within 100" of galaxies in the Census of the Local Universe catalog. We describe the experiment design and spectroscopic completeness from the first 16 months of operations, which have classified 754 supernovae. We present results from a systematic search for calcium-rich gap transients in the sample of 22 low-luminosity (peak absolute magnitude M > −17), hydrogen-poor events found in the experiment. We report the detection of eight new events, and constrain their volumetric rate to ≳ 15% ± 5% of the SN Ia rate. Combining this sample with 10 previously known events, we find a likely continuum of spectroscopic properties ranging from events with SN Ia–like features (Ca-Ia objects) to those with SN Ib/c–like features (Ca-Ib/c objects) at peak light. Within the Ca-Ib/c events, we find two populations distinguished by their red (g − r ≈ 1.5 mag) or green (g - r ≈ 0.5 mag) colors at the r-band peak, wherein redder events show strong line blanketing features and slower light curves (similar to Ca-Ia objects), weaker He lines, and lower [Ca ii]/[O i] in the nebular phase. We find that all together the spectroscopic continuum, volumetric rates, and striking old environments are consistent with the explosive burning of He shells on low-mass white dwarfs. We suggest that Ca-Ia and red Ca-Ib/c objects arise from the double detonation of He shells, while green Ca-Ib/c objects are consistent with low-efficiency burning scenarios like detonations in low-density shells or deflagrations

Real-time Monitoring for the Next Core-Collapse Supernova in JUNO

Core-collapse supernova (CCSN) is one of the most energetic astrophysical events in the Universe. The early and prompt detection of neutrinos before (pre-SN) and during the SN burst is a unique opportunity to realize the multi-messenger observation of the CCSN events. In this work, we describe the monitoring concept and present the sensitivity of the system to the pre-SN and SN neutrinos at the Jiangmen Underground Neutrino Observatory (JUNO), which is a 20 kton liquid scintillator detector under construction in South China. The real-time monitoring system is designed with both the prompt monitors on the electronic board and online monitors at the data acquisition stage, in order to ensure both the alert speed and alert coverage of progenitor stars. By assuming a false alert rate of 1 per year, this monitoring system can be sensitive to the pre-SN neutrinos up to the distance of about 1.6 (0.9) kpc and SN neutrinos up to about 370 (360) kpc for a progenitor mass of 30$M_{\odot}$ for the case of normal (inverted) mass ordering. The pointing ability of the CCSN is evaluated by using the accumulated event anisotropy of the inverse beta decay interactions from pre-SN or SN neutrinos, which, along with the early alert, can play important roles for the followup multi-messenger observations of the next Galactic or nearby extragalactic CCSN.Comment: 24 pages, 9 figure

GROWTH on GW190425: Searching thousands of square degrees to identify an optical or infrared counterpart to a binary neutron star merger with the Zwicky Transient Facility and Palomar Gattini IR

The beginning of the third observing run by the network of gravitational-wave detectors has brought the discovery of many compact binary coalescences. Prompted by the detection of the first binary neutron star merger in this run (GW190425 / LIGO/Virgo S190425z), we performed a dedicated follow-up campaign with the Zwicky Transient Facility (ZTF) and Palomar Gattini-IR telescopes. As it was a single gravitational-wave detector discovery, the initial skymap spanned most of the sky observable from Palomar Observatory, the site of both instruments. Covering 8000 deg$^2$ of the inner 99\% of the initial skymap over the next two nights, corresponding to an integrated probability of 46\%, the ZTF system achieved a depth of $\approx$\,21 $m_\textrm{AB}$ in $g$- and $r$-bands. Palomar Gattini-IR covered a total of 2200 square degrees in $J$-band to a depth of 15.5\,mag, including 32\% of the integrated probability based on the initial sky map. However, the revised skymap issued the following day reduced these numbers to 21\% for the Zwicky Transient Facility and 19\% for Palomar Gattini-IR. Out of the 338,646 ZTF transient "alerts" over the first two nights of observations, we narrowed this list to 15 candidate counterparts. Two candidates, ZTF19aarykkb and ZTF19aarzaod were particularly compelling given that their location, distance, and age were consistent with the gravitational-wave event, and their early optical lightcurves were photometrically consistent with that of kilonovae. These two candidates were spectroscopically classified as young core-collapse supernovae. The remaining candidates were photometrically or spectroscopically ruled-out as supernovae. Palomar Gattini-IR identified one fast evolving infrared transient after the merger, PGIR19bn, which was later spectroscopically classified as an M-dwarf flare. [abridged

GROWTH on S190425z: Searching Thousands of Square Degrees to Identify an Optical or Infrared Counterpart to a Binary Neutron Star Merger with the Zwicky Transient Facility and Palomar Gattini-IR

The third observing run by LVC has brought the discovery of many compact binary coalescences. Following the detection of the first binary neutron star merger in this run (LIGO/Virgo S190425z), we performed a dedicated follow-up campaign with the Zwicky Transient Facility (ZTF) and Palomar Gattini-IR telescopes. The initial skymap of this single-detector gravitational wave (GW) trigger spanned most of the sky observable from Palomar Observatory. Covering 8000 deg2 of the initial skymap over the next two nights, corresponding to 46% integrated probability, ZTF system achieved a depth of ≈21 m AB in g- and r-bands. Palomar Gattini-IR covered 2200 square degrees in J-band to a depth of 15.5 mag, including 32% integrated probability based on the initial skymap. The revised skymap issued the following day reduced these numbers to 21% for the ZTF and 19% for Palomar Gattini-IR. We narrowed 338,646 ZTF transient "alerts" over the first two nights of observations to 15 candidate counterparts. Two candidates, ZTF19aarykkb and ZTF19aarzaod, were particularly compelling given that their location, distance, and age were consistent with the GW event, and their early optical light curves were photometrically consistent with that of kilonovae. These two candidates were spectroscopically classified as young core-collapse supernovae. The remaining candidates were ruled out as supernovae. Palomar Gattini-IR did not identify any viable candidates with multiple detections only after merger time. We demonstrate that even with single-detector GW events localized to thousands of square degrees, systematic kilonova discovery is feasible

Architecture de transformée de cosinus discrète sur deux dimensions sans multiplication et mémoire de transposition

Au cours des dix dernières années, les capacités technologiques de transmission vidéo rendent possible une panoplie d'applications de télésanté. Ce média permet en effet la participation de médecins spécialisés à des interventions médicales ayant lieu à des endroits distants. Cependant, lorsque ces dernières se déroulent loin des grands centres, les infrastructures de télécommunication n'offrnt pas un débit assez important pour permettre à la fois une transmission d'images fluides et de bonne qualité. Un des moyens entrepris pour pallier ce problème est l'utilisation d'encodeur et décodeur vidéo (CODEC) permettant de compresser les images avant leur transmission et de les décompresser à la réception. Il existe un bon nombre de CODEC vidéo offrant différent compromis entre la qualité d'image, la rapidité de compression, la latence initiale de traitement et la robustesse du protocole de transmission. Malheureusement, aucun n'est en mesure de rencontrer simultanément toutes les exigences définies en télésanté. Un des problèmes majeurs réside dans le délai de traitement initial causé par la compression avec perte du CODEC. L'objet de la recherche s'intéresse donc à deux CODEC qui répondent aux exigences de délais de traitement et de qualité d'image en télésanté, et plus particulièrement pour une application de téléassistance en salle d'urgence. L'emphase est mise sur les modules de quantification des CODEC qui utilisent la transformée en cosinus discrète. Cette transformée limite la transmission des images vidéo fluide et quasi sans délais en raison des délais de traitement initiaux issus des nombreuses manipulations arithmétiques qu'elle requiert. À l'issu de la recherche, une structure efficace de la transformée en cosinus est proposée afin de présenter une solution au temps de latence des CODEC et ainsi de répondre aux exigences de télécommunication en télésanté. Cette solution est implémentée dans un CODEC JPEG développé en VHDL afin de simuler un contexte d'application réelle