Search

The Extreme Ultraviolet Imager (EUI) onboard Solar Orbiter ob-served an eruption through both of its channels (17.4/30.4 nm) of its Full Sun Imager, on 22 April 2021. At the time, the spacecraft was at 0.87 au from the Sun,and 98◦ east of the Sun-Earth line. The eruption was slightly back-sided, emerging close to the southwest limb, starting at 04:24 UT, with the source located at S20W103 from the Solar Orbiter perspective. The Solar Orbiter coronagraph, Metis, observed the CME at 06:05 UT. The Spectrometer/Telescope for Imaging X-rays (STIX) on Solar Orbiter sampled the associated X-ray flare, which was partially occulted. This allowed the characterization of both the thermal plasmaand any potential contribution of non-thermal electrons in the tenuous coronal source. The X-ray source location is compared to the extreme ultraviolet coronal structures seen by EUI, and it is established that STIX imager only sees the top part of the flaring loops, while most of the flare – in particular the non-thermal foot points – remain occulted. From the Earth’s perspective the eruption source region was observed at S20W05 (close to disk centre), the Atmospheric Imaging Assembly (AIA), onboard the Solar Dynamics Observatory (SDO) and the Sun Watcher using Active Pixel System detector and Image Processing (SWAP), onboard the PRoject for OnboardAutonomy (PROBA2) observed dimmings and an associated large-scale coronal wave starting around 04:07 UT. The Extreme Ultraviolet Imager (EUVI) on the Solar-TErrestial RElations Observatory (STEREO-A), located 53◦ east of the Sun-Earth line at the time, observed similar signatures of an eruption starting around 04:17 UT, on-disk at S20W50. The corresponding CME was observedas a partial halo CME shortly after (∼06:00 UT) by the C2 Large Angle and Spectrometric Coronagraph (LASCO), from the Earth perspective onboard the SOlar and Heliospheric Observatory (SOHO), and by the STEREO-A/COR2 coronagraph as a clear structured CME around 05:23 UT. The corresponding ICME arrived at Earth on 24 April 2021, it was driving ashock and created minor geomagnetic storm conditions. We simulate the CMEwith the 3D MHD heliospheric model EUHFORIA. We provide an analysis ofthe eruption as observed by these various instruments from different vantage points. The combination of data from Solar Orbiter as well as other space-based assets with numerical modeling clearly showcases the scientific potential for the science phase of Solar Orbiter, and the unique observations available.

Context. Accurate detections of frequent small-scale extreme ultraviolet (EUV) brightenings are essential to the investigation of the physical processes heating the corona. Aims. We detected small-scale brightenings, termed campfires, using their morphological and intensity structures as observed in coronal EUV imaging observations for statistical analysis. Methods. We applied a method based on Zernike moments and a support vector machine (SVM) classifier to automatically identify and track campfires observed by Solar Orbiter/Extreme Ultraviolet Imager (EUI) and Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA). Results. This method detected 8678 campfires (with length scales between 400 km and 4000 km) from a sequence of 50 High Resolution EUV telescope (HRIEUV) 174 Å images. From 21 near co-temporal AIA images covering the same field of view as EUI, we found 1131 campfires, 58% of which were also detected in HRIEUV images. In contrast, about 16% of campfires recognized in HRIEUV were detected by AIA. We obtain a campfire birthrate of 2 × 10−16 m−2 s−1. About 40% of campfires show a duration longer than 5 s, having been observed in at least two HRIEUV images. We find that 27% of campfires were found in coronal bright points and the remaining 73% have occurred out of coronal bright points. We detected 23 EUI campfires with a duration greater than 245 s. We found that about 80% of campfires are formed at supergranular boundaries, and the features with the highest total intensities are generated at network junctions and intense H I Lyman-α emission regions observed by EUI/HRILya. The probability distribution functions for the total intensity, peak intensity, and projected area of campfires follow a power law behavior with absolute indices between 2 and 3. This self-similar behavior is a possible signature of self-organization, or even self-organized criticality, in the campfire formation process.

INTRODUCTION Gastrointestinal stromal tumours (GISTs) are the most common connective tissue neoplasms of the gastrointestinal tract, the most common clinical presentation of which is with abdominal pain or gastrointestinal bleeding. METHODS We describe a case of a perforated gastric GIST as well as reviewing the relevant published literature. RESULTS A 51-year-old woman presented to the acute assessment unit with a 1-day history of severe epigastric pain on a background of longstanding reflux symptoms. Radiological investigation demonstrated a perforated mass in the gastric antrum and the patient subsequently underwent an emergency distal gastrectomy. She recovered well postoperatively and was discharged home. Her condition remains stable six months following surgery. Histological analysis revealed the perforated lesion to be a GIST. A PubMed search suggests that this is the first English report to describe a perforated gastric GIST. Six further published reports (written in English or with an English abstract) describing the presentation of small bowel GISTs with perforation are reviewed. CONCLUSIONS We present the first English report of a perforated gastric GIST. More common presentations include abdominal pain and gastrointestinal bleeding. Although rare, GISTs should be considered in the differential diagnoses of perforated gastrointestinal masses.

We report on a search for faint (R total magnitude fainter than 21) and low surface brightness galaxies (R central surface brightness fainter than ~24) (fLSBs) in a 0.72x0.82 deg2 area centered on the Coma cluster. We analyzed deep B and R band CCD imaging obtained using the CFH12K camera at CFHT and found 735 fLSBs. The total B magnitudes, at the Coma cluster redshift, range from -13 to -9 with B central surface brightness as faint as 27 mag/arcsec2. Using empty field comparisons, we show that most of these fLSBs are probably inside the Coma cluster. We present the results of comparing the projected fLSB distributions with the distributions of normal galaxies and with known X-ray over densities. We also investigate their projected distribution relative to their location in the color magnitude relation. Colors of fLSBs vary between B-R~0.8 and ~1.4 for 2/3 of the sample and this part is consistent with the known CMR red-sequence for bright (R, To be published in A&A, 3 jpeg figures, data and full resolution article can be retrieved from http://cencosw.oamp.fr/. Updated CFHT ackowledgements

Previous studies have demonstrated variable effects on systemic inflammatory and immune responses following improved periodontal health. This study examined changes in serum levels of the inflammatory mediators IL-1β, IL-6, TNF-α and sICAM-1, and antibodies to Porphyromonas gingivalis, human heat shock protein (hHSP) 60 and P. gingivalis GroEL following improvement in periodontal health in high cardiovascular (CV) risk and low CV-risk patients.Patients retrospectively selected from a longitudinal study, had undergone yearly periodontal examinations and peripheral blood collections. They had demonstrated a quantifiable improvement in periodontal health (60% reduction in number of sites with probing depth ≥ 4 mm from the baseline visit) and could be classified as either high CV-risk (≥ 6 classical risk factors, n = 13) or low CV-risk (≤ 1 classical risk factor, n = 14). Serum levels of the cytokines and antibodies were measured using ELISA.For sICAM-1 and anti-P. gingivalis GroEL and anti-hHSP60 antibodies, most patients recorded decreased levels. Reductions in serum sICAM-1 levels were more notable in low CV-risk patients (p = 0.006); and reductions in levels of anti-P. gingivalis GroEL and anti-hHSP60 antibodies (p = 0.001 and 0.009 respectively) were more notable in high CV-risk patients.This study found that subsequent to improved periodontal health, the anti-HSP (HSP60 and GroEL) antibody response was reduced, particularly for high CV-risk patients. sICAM-1 levels were also lowered, more so for low CV-risk patients.

This study follows a recent analysis of the galaxy luminosity functions and colour-magnitude red sequences in the Coma cluster (Adami et al. 2007). We analyze here the distribution of very faint galaxies and globular clusters in an east-west strip of $\sim 42 \times 7$ arcmin$^2$ crossing the Coma cluster center (hereafter the CS strip) down to the unprecedented faint absolute magnitude of M$_R \sim -9.5$. This work is based on deep images obtained at the CFHT with the CFH12K camera in the B, R, and I bands. The analysis shows that the observed properties strongly depend on the environment, and thus on the cluster history. When the CS is divided into four regions, the westernmost region appears poorly populated, while the regions around the brightest galaxies NGC 4874 and NGC 4889 (NGC 4874 and NGC 4889 being masked) are dominated by faint blue galaxies. They show a faint luminosity function slope of -2, very significantly different from the field estimates. Results are discussed in the framework of galaxy destruction (which can explain part of the very faint galaxy population) and of structures infalling on to Coma., To be published in A&A

We have obtained deep and wide field imaging of the Coma cluster of galaxies with the CFH12K camera at CFHT in the B, V, R and I filters. In this paper, we present the observations, data reduction, catalogs and first scientific results. We investigated the quality of our data by internal and external literature comparisons. We also checked the realisation of the observational requirements we set. Our observations cover two partially overlapping areas of $42 \times 28$ arcmin$^2$, leading to a total area of 0.72 $\times$ 0.82 deg$^2$. We have produced catalogs of objects that cover a range of more than 10 magnitudes and are complete at the 90% level at B$\sim$25, V$\sim$24, R$\sim$24 and I$\sim$23.5 for stellar-like objects, and at B$\sim$22, V$\sim$21, R$\sim$20.75 and I$\sim$20.5 for faint low-surface-brightness galaxy-like objects. Magnitudes are in good agreement with published values from R$\sim$16 to R$\sim$25. The photometric uncertainties are of the order of 0.1 magnitude at R$\sim$20 and of 0.3 magnitude at R$\sim$25. Astrometry is accurate to 0.5~arcsec and also in good agreement with published data. Our catalog provides a rich dataset that can be mined for years to come to gain new insights into the formation and evolution of the Coma cluster and its galaxy population. As an illustration of the data quality, we examine the bright part of the Colour Magnitude Relation (B-R versus R) derived from the catalog and find that it is in excellent agreement with that derived for galaxies with redshifts in the Coma cluster, and with previous CMRs estimated in the literature., A&A, 2006, 451, 1159. Catalog available at http://cencosw.oamp.fr/ with no restriction. High resolution figures can be found at A&A, 2006, 451, 1159

Clusters of galaxies are believed to be at the intersections of cosmological filaments and to grow by accreting matter from these filaments. Such continuous infall has major consequences not only on clusters but also on the physics of cluster galaxies. Faint galaxies are particularly interesting as they are very sensitive to environmental effects, and may have a different behaviour from that of bright galaxies. The aim of this paper is to sample the Coma cluster building history, based on the analysis of galaxy luminosity functions and red sequences in the Color Magnitude Relation down to faint magnitudes, which are privileged tools for this purpose. The present analysis is based on deep (R~24), wide (~0.5 deg2) multiband (BVRI Vega system) images of the Coma cluster obtained with the CFH12K camera at the CFHT. We have derived LFs and CMRs in twenty 10x10 arcmin2 regions and in larger regions. In all photometric bands, we found steeply rising LFs in the north-northeast half of the cluster (due to early type galaxies at bright magnitudes and due to late type galaxies at the faint end), and much flatter LFs in the south-southwest region. Although the fine behaviour of the CMR RS is different in these two regions, a good agreement is found in general between the RS computed for faint and for bright galaxies. All these results can be interpreted consistently in the framework of the building up process previously proposed. The Northern Coma area is a relatively quiescent region while the southern area experiences several infalls., Comment: To be published in A&A, several figures in jpg format, full resolution figures and paper available at http://cencosw.oamp.fr/ under the Coma page. The lacking figures are available at the same adress. Updated CFHT acknowledgements and aa format

Relative ages for the globular cluster (GC) subpopulations in the Virgo giant elliptical galaxy M87 (NGC 4486) have been determined from Stroemgren photometry obtained with WFPC2 on board HST. Using a variety of population synthesis models, and assuming the GC mass at the turnover of the luminosity function is the same for both subpopulations, differential ages have been determined from the observed magnitudes at the turnover of the globular cluster luminosity function and from the mean color of each subpopulation. We measure an age difference between the two subpopulations of 0.2 +/- 1.5 (systematic) +/- 2 (random) Gyr, in the sense that the blue GCs are formally older. Thus, to within our measurement errors, the two subpopulations are found to be coeval. Combined with previous spectroscopic age determinations for M87 GCs, our results favor a picture in which the GCs associated with this galaxy are formed at high redshift, and within a period of a few Gyr., Comment: 5 pages, 2 postscript figures. Accepted for publication in ApJ Letters

The principle that formed the basis of the most popular "assumption based" stereological methods for counting cells that were available prior to the advent of the more recently developed "design based" methods will be described in general terms. The major weaknesses inherent in the older methods will be described, along with how they have been eliminated by the design based methods.

We have studied the antiemetic effects of propofol when mixed with morphine in a patient-controlled analgesia (PCA) pump after major gynaecological surgery. In a double-blind, randomized, controlled study, 50 women, ASA I or II, received a standardized anaesthetic comprising thiopental, morphine, atracurium, nitrous oxide and oxygen with enflurane, and received postoperative PCA with morphine mixed with either 1% propofol or lvelip. The PCA bolus was morphine 1 mg with propofol 5 mg or lvelip 0.5 ml, with a lockout time of 5 min. Postoperative nausea and vomiting (PONV) were assessed by the nursing staff using a four-point ordinal scale and by the patient using a visual analogue scale for 48 h after surgery. The two groups were similar in the potential factors influencing the incidence of PONV. There were no significant differences between the two groups in any of the study measurements of PONV. There were, no side effects after propofol. Propofol, when mixed with morphine in this dose combination for PCA, did not decrease the incidence of nausea and vomiting in women undergoing major gynaecological surgery.

We study the globular cluster (GC) systems in three representative fossil group galaxies: the nearest (NGC6482), the prototype (NGC1132) and the most massive known to date (ESO306-017). This is the first systematic study of GC systems in fossil groups. Using data obtained with the Hubble Space Telescope Advanced Camera for Surveys in the F475W and F850LP filters, we determine the GC color and magnitude distributions, surface number density profiles, and specific frequencies. In all three systems, the GC color distribution is bimodal, the GCs are spatially more extended than the starlight, and the red population is more concentrated than the blue. The specific frequencies seem to scale with the optical luminosities of the central galaxy and span a range similar to that of the normal bright elliptical galaxies in rich environments. We also analyze the galaxy surface brightness distributions to look for deviations from the best-fit S\'ersic profiles; we find evidence of recent dynamical interaction in all three fossil group galaxies. Using X-ray data from the literature, we find that luminosity and metallicity appear to correlate with the number of GCs and their mean color, respectively. Interestingly, although NGC6482 has the lowest mass and luminosity in our sample, its GC system has the reddest mean color, and the surrounding X-ray gas has the highest metallicity., Comment: 16 pages, 13 figures. Accepted for publication in A&A

Cation transport across the red-cell membrane was studied in subjects with essential hypertension and their relatives using rubidium-86 as an analogue of potassium. The activity of the ouabain-sensitive sodium-potassium pump was significantly greater in patients with untreated essential hypertension than in controls (p less than 0.001). No clear separation was seen between normotensive and hypertensive subjects. Activity of the sodium-potassium pump was also increased in a proportion of normotensive relatives of subjects with essential hypertension. Rubidium uptake was significantly lower in normotensive black subjects than in normotensive whites, the difference being in a ouabain-resistant pathway of cation transport. These results provide further evidence that a defect in membrane cation transport contributes to the pathogenesis of essential hypertension.

In a cross sectional study of 137 women of childbearing age (16-40) the effects of normal pregnancy, hypertensive pregnancy, and oral contraceptives on red cell electrolyte content and sodium efflux rates were examined and the results compared with values in a control group of normotensive, non-pregnant women. Efflux rate constants were significantly increased in normotensive pregnancy and in women taking oral contraceptives. This was associated with a significant increase in sodium permeability in the contraceptive group. A much larger increase in sodium permeability and efflux rate constant was seen in the hypertensive group. The results permit a hypothesis that the hormonal changes induced by pregnancy and oral contraceptives increase membrane permeability to sodium and stimulate sodium efflux. The rise in blood pressure associated with use of oral contraceptives may have a similar aetiology to that occurring in pregnancy induced hypertension.

An earlier observational study of mothers and toddlers in the supermarket revealed differential success of 2 styles of maternal behavior. A proactive style of preempting opportunities for misbehavior, in contrast to a reactive style of responding only after misbehavior occurred, was correlated with a lower incidence of undesirable child acts. Here, the 2 styles were studied in the laboratory to explore their function further. In an analog of the supermarket situation, mothers behaved proactively and reactively in trials in which the task was to prevent their 2- or 3-year-old children from playing with desirable toys. Children responded to proactive behavior by engaging in acceptable behaviors longer and by violating fewer rules. The 2-year-old children were less able to comply with the rules. The data illustrate the role parents play in promoting and supporting the development of compliance and self-regulation in children.

We use N-body simulations of competing cosmological scenarios to study the relative orientations of the principal axes of clusters of galaxies and the lines connecting them to neighboring clusters and find that they provide a sensitive test for the formation of the large-scale structure in the universe. The observed tendency of clusters to point toward each other reflects the existence of 20-50 Mpc h/sup -1/ elongated superclusters that construct a large-scale cell structure. Tidal interactions between clusters are found not to produce similar alignments, presumably because the clusters are surrounded by underdense regions. Hence the scenario in which superclusters have collapsed from excessive fluctuations on large scales in favored over hierarchical clustering from fluctuations on smaller scales. Rich clusters (but not necessarily galaxies) had to be formed after, or during, the aspherical collapse of superclusters, i.e., not long before zapprox.1.

Difficulties in the use of percolation as a complementary statistic for the galaxy clustering pattern are pointed out by studying simple toy models and dynamical N-body models that represent the competing clustering scenarios. The percolation properties are found not to be very sensitive to the presence of pancakes and strings once they are clumpy, and hence they do not distinguish properly between models that are very different. In the case of very smooth pancakes, the ability to percolate depends on sampling parameters, such as the mean number density and the volume, in a way which is unknown a priori because it depends on the same properties that the test ought to measure. This problem could, in principle, be eased by using volume-limited samples of high mean number density (an order of magnitude denser than the CfA redshift survey volume limited at 4000 km/s) and by comparing to models of identical number density and volume. An alternative approach, based on the sampling effects themselves, may provide a qualitative test for pancakes in samples of lower densities.