Spatial and Time Clustering of the High-Energy Photons collected by the Fermi LAT

The past decade has seen a dramatic improvement in the quality of data available at both high (HE, > 10 GeV ) and very high (VHE, > 100 GeV ) gamma-ray energies. Thanks to the latest Pass8 data release by Fermi LAT which increases the overlap in energy coverage with Cherenkov Telescopes, we can extend the observation in gamma rays until few TeV. We developed, applied and tested a new time and spatial clustering algorithm, which is able to analyse the whole Fermi LAT data set (about 7 years) as well as sets of shorter time intervals. Using time and spatial clusters of HE photons collected by the Fermi LAT data we both provide new candidates for VHE experiments and study the variability of gamma-ray properties of known HE sources.ope

Test Ordering Practices in Cancer Genetic Counseling

The widespread use of Next Generation Sequencing (NGS) has allowed multi-gene panel testing to become common practice in clinical cancer genetic testing over the past six years. Over this time, guidelines have been established and modified, but there is no consensus on how panel testing should be utilized in cancer genetic counseling. There is also limited research into how cancer genetic testing is ordered among different providers. In our study, 1,402 cancer genetic tests were ordered by a variety of provider types from a large academic institution consisting of 16 private and public hospitals as well as a laboratory serving the Long Island and New York City metropolitan area. Data was collected between 01/01/2018 and 09/30/2019 and analyzed to identify discrepancies in the ordering practices among different provider types. Out of the 1,402 cancer genetic tests ordered, 505 were general multi-gene panels, 330 of which were ordered by genetic counselors and geneticists, and the other 175 were ordered by a variety of non-genetics providers. Based on our analysis, there is a statistically significant difference (P-value \u3c 0.0001) in test ordering practices among genetics and non-genetics providers. Our study serves as a foundation for future research into these discrepancies, as well as for research into how to rectify these differences in test ordering practice

Deconstructing double-barred galaxies in 2D and 3D. II. Two distinct groups of inner bars

The intrinsic photometric properties of inner and outer stellar bars within 17 double-barred galaxies are thoroughly studied through a photometric analysis consisting of: i) two-dimensional multi-component photometric decompositions, and ii) three-dimensional statistical deprojections for measuring the thickening of bars, thus retrieving their 3D shape. The results are compared with previous measurements obtained with the widely used analysis of integrated light. Large-scale bars in single- and double-barred systems show similar sizes, and inner bars may be longer than outer bars in different galaxies. We find two distinct groups of inner bars attending to their in-plane length and ellipticity, resulting in a bimodal behaviour for the inner/outer bar length ratio. Such bimodality is related neither to the properties of the host galaxy nor the dominant bulge, and it does not show a counterpart in the dimension off the disc plane. The group of long inner bars lays at the lower end of the outer bar length vs. ellipticity correlation, whereas the short inner bars are out of that relation. We suggest that this behaviour could be due to either a different nature of the inner discs from which the inner bars are dynamically formed, or a different assembly stage for the inner bars. This last possibility would imply that the dynamical assembly of inner bars is a slow process taking several Gyr to happen. We have also explored whether all large-scale bars are prone to develop an inner bar at some stage of their lives, possibility we cannot fully confirm or discard.Comment: 14 pages, 8 figures, 1 table. Accepted for publication in MNRA

Current Research on Flexibilizing the Labor Market – first part –

Increasing the competitiveness of companies is closely linked to its development of a strategic human resources management. Such a trend has emerged in response to dynamic environment, most of organizations including human resources functionin the global strategy, based on the fact that human resources can have a decisive influence upon the success of an organisation. In these conditions, the main concern of the entities is to locate and identify the human resources to ensure their competitive advantage in an international environment Under conditions of globalization process amplification, human resources should be managed as investments, the organizations will consider human capital as a cost of work required and will have very small chances of success

The intrinsic three-dimensional shape of galactic bars

We present the first statistical study on the intrinsic three-dimensional (3D) shape of a sample of 83 galactic bars extracted from the CALIFA survey. We use the galaXYZ code to derive the bar intrinsic shape with a statistical approach. The method uses only the geometric information (ellipticities and position angles) of bars and discs obtained from a multi-component photometric decomposition of the galaxy surface-brightness distributions. We find that bars are predominantly prolate-triaxial ellipsoids (68%), with a small fraction of oblate-triaxial ellipsoids (32%). The typical flattening (intrinsic C/A semiaxis ratio) of the bars in our sample is 0.34, which matches well the typical intrinsic flattening of stellar discs at these galaxy masses. We demonstrate that, for prolate-triaxial bars, the intrinsic shape of bars depends on the galaxy Hubble type and stellar mass (bars in massive S0 galaxies are thicker and more circular than those in less massive spirals). The bar intrinsic shape correlates with bulge, disc, and bar parameters. In particular with the bulge-to-total (B/T) luminosity ratio, disc g-r color, and central surface brightness of the bar, confirming the tight link between bars and their host galaxies. Combining the probability distributions of the intrinsic shape of bulges and bars in our sample we show that 52% (16%) of bulges are thicker (flatter) than the surrounding bar at 1$\sigma$ level. We suggest that these percentages might be representative of the fraction of classical and disc-like bulges in our sample, respectively.Comment: 18 pages, 11 figures, accepted for publication in MNRA

Stellar populations in the bulges of isolated galaxies

open7siWe present photometry and long-slit spectroscopy for 12 S0 and spiral galaxies selected from the Catalogue of Isolated Galaxies. The structural parameters of the sample galaxies are derived from the Sloan Digital Sky Survey i-band images by performing a two-dimensional photometric decomposition of the surface brightness distribution. This is assumed to be the sum of the contribution of a Sersic bulge, an exponential disc, and a Ferrers bar characterized by elliptical and concentric isophotes with constant ellipticity and position angles. The rotation curves and velocity dispersion profiles of the stellar component are measured from the spectra obtained along the major axis of galaxies. The radial profiles of the Hβ, Mg and Fe line- strength indices are derived too. Correlations between the central values of the Mg2 and Fe line-strength indices and the velocity dispersion are found. The mean age, total metallicity and total α/Fe enhancement of the stellar population in the centre and at the radius, where the bulge gives the same contribution to the total surface brightness as the remaining components, are obtained using stellar population models with variable element abundance ratios. We identify intermediate-age bulges with solar metallicity and old bulges with a large spread in metallicity. Most of the sample bulges display supersolar α/Fe enhancement, no gradient in age and negative gradients of metallicity and α/Fe enhancement. These findings support a formation scenario via dissipative collapse where environmental effects are remarkably less important than in the assembly of bulges of galaxies in groups and clusters.openMorelli, Lorenzo; Parmiggiani, Marco; Corsini, ENRICO MARIA; Costantin, Luca; DALLA BONTA', Elena; Méndez Abreu, J.; Pizzella, AlessandroMorelli, Lorenzo; Parmiggiani, Marco; Corsini, ENRICO MARIA; Costantin, Luca; DALLA BONTA', Elena; Méndez Abreu, J.; Pizzella, Alessandr