Weak lensing, which is the deflection of light by matter along the line of sight, has proven to be an efficient method for constraining models of structure formation and reveal the nature of dark ...energy. So far, most weak-lensing studies have focused on the shear field that can be measured directly from the ellipticity of background galaxies. However, within the context of forthcoming full-sky weak-lensing surveys such as
Euclid
, convergence maps (mass maps) offer an important advantage over shear fields in terms of cosmological exploitation. While it carry the same information, the lensing signal is more compressed in the convergence maps than in the shear field. This simplifies otherwise computationally expensive analyses, for instance, non-Gaussianity studies. However, the inversion of the non-local shear field requires accurate control of systematic effects caused by holes in the data field, field borders, shape noise, and the fact that the shear is not a direct observable (reduced shear). We present the two mass-inversion methods that are included in the official
Euclid
data-processing pipeline: the standard Kaiser & Squires method (KS), and a new mass-inversion method (KS+) that aims to reduce the information loss during the mass inversion. This new method is based on the KS method and includes corrections for mass-mapping systematic effects. The results of the KS+ method are compared to the original implementation of the KS method in its simplest form, using the
Euclid
Flagship mock galaxy catalogue. In particular, we estimate the quality of the reconstruction by comparing the two-point correlation functions and third- and fourth-order moments obtained from shear and convergence maps, and we analyse each systematic effect independently and simultaneously. We show that the KS+ method substantially reduces the errors on the two-point correlation function and moments compared to the KS method. In particular, we show that the errors introduced by the mass inversion on the two-point correlation of the convergence maps are reduced by a factor of about 5, while the errors on the third- and fourth-order moments are reduced by factors of about 2 and 10, respectively.
On average, aromatase inhibitors are better than tamoxifen when used as initial or sequential therapy for postmenopausal women with endocrine-responsive early breast cancer. Because there may be ...contraindications to their use based on side-effects or cost, we investigated subgroups in which aromatase inhibitors may be more or less important.
Breast International Group 1-98 trial randomized 6182 women among four groups comparing letrozole and tamoxifen with sequences of each agent; 5177 (84%) had centrally confirmed estrogen receptor (ER) positivity. We assessed whether centrally determined ER, progesterone receptor (PgR), human epidermal growth factor receptor 2, and Ki-67 labeling index, alone or in combination with other prognostic features, predicted the magnitude of letrozole effectiveness compared with either sequence or tamoxifen monotherapy.
Individually, none of the markers significantly predicted differential treatment effects. Subpopulation treatment effect pattern plot analysis of a composite measure of prognostic risk revealed three patterns. Estimated 5-year disease-free survival for letrozole monotherapy, letrozole→tamoxifen, tamoxifen→letrozole, and tamoxifen monotherapy were 96%, 94%, 93%, and 94%, respectively, for patients at lowest risk; 90%, 91%, 93%, and 86%, respectively, for patients at intermediate risk; and 80%, 76%, 74%, and 69%, respectively, for patients at highest risk.
A composite measure of risk informs treatment selection better than individual biomarkers and supports the choice of 5 years of letrozole for patients at highest risk for recurrence.
Aims. With an observed and rest-frame duration of <2 s and <0.5 s, respectively, GRB 090426 could be classified as a short GRB. The prompt detection, both from space and ground-based telescopes, of a ...bright optical counterpart to this GRB offered a unique opportunity to complete a detailed study. Methods. Based on an extensive ground-based observational campaign, we obtained the spectrum of the optical afterglow of GRB 090426, measuring its redshift and obtaining information about the medium in which the event took place. We completed follow-up observations of the afterglow optical light curve down to the brightness level of the host galaxy that we firmly identified and studied. We also retrieved and analyzed all the available high-energy data of this event, and compared the results with our findings in the optical. This represents one of the most detailed studies of a short-duration event presented so far. Results. The time properties qualify GRB 090426 as a short burst. In this case, its redshift of $z = 2.61$ would be the highest yet found for a GRB of this class. On the other hand, the spectral and energy properties are more similar to those of long bursts. LBT late-time deep imaging identifies a star-forming galaxy at a redshift consistent with that of the GRB. The afterglow lies within the light of its host and shows evidence of local absorption.
Hereditary haemorrhagic telangiectasia (HHT) is a rare disease characterized by a multisystemic vascular dysplasia and epistaxis, that is the most common cause of disability and social impairment. ...Patient management strictly depends on the severity of this symptom; therefore, it is of paramount importance for the clinicians to effectively grade epistaxis severity. The aim of this report was to validate the Frequency, Intensity and Duration score (FID) for grading epistaxis severity in patients with HHT; we studied repeatability and external validity comparing FID score with Epistaxis Severity Score (ESS).
This is a descriptive, observational study that included 264 adult HHT patients with epistaxis. Diagnosis of HHT was established with Curacao criteria or positivity at genetic testing. Nosebleed severity was evaluated according to the FID score and the ESS. The first 30 patients were included in the validation of the FID score, which was graded on days 0, 1, 3 and 7. In the remaining 234 patients, a comparison between the ESS and FID score was performed.
The statistical analysis performed in order to validate the FID score showed very good agreement between scores calculated on different days; analysis comparing the FID score with the ESS revealed a high correlation between the two grading systems.
The FID score is a quick, easy and precise tool for evaluating HHT-related epistaxis and could be a possible alternative to the ESS. The FID score meets the need for an intuitive and smart grading system that is easy to manage in clinicians’ hands.
Epistaxis is the main complaint in patients with Hereditary haemorrhagic telangiectasia (HHT). Even though the role of epistaxis in affecting the quality of life (QoL) is well-known, little is known ...about epidemiological and clinical factors contributing to epistaxis severity and QoL.
This is a cross-sectional study, including adult patients with HHT with epistaxis. All patients underwent an otolaryngological evaluation with nasal endoscopy. Epistaxis severity was graded using the FID score, and QoL was evaluated with the Short-Form Health Survey (SF-36). Descriptive statistics were produced for demographic characteristics; the Shapiro-Wilk test was used to test the normal distribution of quantitative variables. Correlation between the quantitative variables was evaluated with Pearson's correlation coefficient. Both univariate and multivariate linear regression models were fitted to find associations between demographic or clinical factors and the FID score or SF-36.
A total of 234 patients with HHT were included in the study. The univariate analysis highlighted the association between high blood pressure, septal perforation, nocturnal epistaxis, surgery, blood transfusion, hormonal therapy and both FID score and QoL. Sex, allergic rhinitis and nasal polyposis were neither related to epistaxis severity nor perceived health.
Epistaxis severity and QoL in patients with HHT are influenced by several clinical factors both dependent and independent from HHT. Some of the results are consistent with those already published, but for the first time, we extended the analysis to different clinical parameters, such as endoscopic findings, never assessed before.
Context.
The ESA
Euclid
space telescope could observe up to 150 000 asteroids as a side product of its primary cosmological mission. Asteroids appear as trailed sources, that is streaks, in the ...images. Owing to the survey area of 15 000 square degrees and the number of sources, automated methods have to be used to find them.
Euclid
is equipped with a visible camera, VIS (VISual imager), and a near-infrared camera, NISP (Near-Infrared Spectrometer and Photometer), with three filters.
Aims.
We aim to develop a pipeline to detect fast-moving objects in
Euclid
images, with both high completeness and high purity.
Methods.
We tested the
StreakDet
software to find asteroids from simulated
Euclid
images. We optimized the parameters of
StreakDet
to maximize completeness, and developed a post-processing algorithm to improve the purity of the sample of detected sources by removing false-positive detections.
Results.
StreakDet
finds 96.9% of the synthetic asteroid streaks with apparent magnitudes brighter than 23rd magnitude and streak lengths longer than 15 pixels (10 arcsec h
−1
), but this comes at the cost of finding a high number of false positives. The number of false positives can be radically reduced with multi-streak analysis, which utilizes all four dithers obtained by
Euclid
.
Conclusions.
StreakDet
is a good tool for identifying asteroids in
Euclid
images, but there is still room for improvement, in particular, for finding short (less than 13 pixels, corresponding to 8 arcsec h
−1
) and/or faint streaks (fainter than the apparent magnitude of 23).
Aims. The aim of this paper is to study the stellar population of galaxies hosting an active galactic nucleus (AGN). We studied a subsample of hard X-ray emitting AGNs from the INTEGRAL and Swift ...catalogs, which were previously identified and characterized through optical spectroscopy. Our analysis provides complementary information, namely age and metallicity, which is necessary to complete the panoramic view of these interesting objects. Methods. We selected hard X-ray emitting objects, identified as AGNs, by checking their optical spectra in search of absorption lines suitable for the stellar population analysis. We obtained a final sample consisting of 20 objects with a redshift lower than 0.3. We used the full-spectrum fitting method; particularly, we use penalized pixel method and apply the PPXF code. After masking all the regions affected by emission lines, we fitted the spectra with the MILES single stellar population templates, and we derived mass-weighted ages and metallicities. Results. Most of the objects in our sample show an old stellar population; however, three of them are characterized by a bimodal distribution with a non-negligible contribution from young stars. The values of the mass-weighted metallicity span a wide range with most of them slightly above the solar value. No relations between the stellar population properties and the morphological ones have been found.
The aim of this retrospective study was to perform an epidemiological analysis of all odontogenic tumors treated in the University Hospitals "Ospedali Riuniti" in Ancona and "Policlinico" in Bari, ...from 1990 to 2015.
A retrospective survey of 277 patients treated for odontogenic tumors from 1990 to 2015 was performed. Data were retrieved from the archives of the above quoted Sections of Pathology. The lesions were classified according to 2005 WHO histological classification, and the following variables were analyzed: age, sex, histopathological diagnosis, site distribution, tumor size, and relapses. Peripheral odontogenic tumors were analyzed considering these lesions separately from their central counterparts.
In a total of 344 surgical specimens, there were 277 primary tumors and 67 recurrences. As regards primary lesions, there were 185 odontogenic keratocysts (keratocystic odontogenic tumors) (66.8%), 49 ameloblastomas (17.7%), and 40 other benign odontogenic tumors (14.4%). As to malignant tumors, only 3 ameloblastic carcinomas were found (1.1%). The mean age was 46.7 years, with a M:F ratio of 1.8:1. The mandible was the most common site of localization, with 211 cases (76.2%). Also, 21 cases of peripheral odontogenic tumors were found, ameloblastomas being the most common (8 cases, 38.1%).
There is a wide variety of cysts, some of which are subject to variations according to sex, localization, and age. Odontogenic tumors are rare neoplasms and appear to show variations according to sex, localization, and age, and may be useful to the clinicians who need to make clinical judgments before biopsy about the most probable diagnosis.
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