Search

The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters is providing a major breakthrough in our knowledge of Globular Clusters (GCs) and their stellar populations. Among the main results, we discovered that all the studied GCs host two main discrete groups consisting of first generation (1G) and second generation (2G) stars. We exploit the multiwavelength photometry from this project to investigate, for the first time, the Red Giant Branch Bump (RGBB) of the two generations in a large sample of GCs. We identified, with high statistical significance, the RGBB of 1G and 2G stars in 26 GCs and found that their magnitude separation as a function of the filter wavelength follows comparable trends. The comparison of observations to synthetic spectra reveals that the RGBB luminosity depends on the stellar chemical composition and that the 2G RGBB is consistent with stars enhanced in He and N and depleted in C and O with respect to 1G stars. For metal-poor GCs the 1G and 2G RGBB relative luminosity in optical bands mostly depends on helium content, Y. We used the RGBB observations in F606W and F814W bands to infer the relative helium abundance of 1G and 2G stars in 18 GCs, finding an average helium enhancement $\Delta$Y=0.011$\pm$0.002 of 2G stars with respect to 1G stars. This is the first determination of the average difference in helium abundance of multiple populations in a large number of clusters and provides a lower limit to the maximum internal variation of helium in GCs., Comment: 16 pages, 11 figures, 2 tables. Accepted for publication in MNRAS

This paper presents a study of the production of a single W boson in association with one or more jets in proton-antiproton collisions at s=1.96 TeV, using the entire data set collected in 2001-2011 by the Collider Detector at Fermilab at the Tevatron, which corresponds to an integrated luminosity of 9.0 fb-1. The W boson is identified through its leptonic decays into electron and muon. The production cross sections are measured for each leptonic decay mode and combined after testing that the ratio of the W(→μν)+jets cross section to the W(→eν)+jets cross section agrees with the hypothesis of e-μ lepton universality. The combination of measured cross sections, differential in the inclusive jet multiplicity (W+≥N jets with N=1, 2, 3, or 4) and in the transverse energy of the leading jet, are compared with theoretical predictions. © 2018 authors.

The Collider Detector at Fermilab collected a unique sample of jets originating from bottom-quark fragmentation (b-jets) by selecting online proton-antiproton (p (p) over bar) collisions with a vertex displaced from p (p) over bar interaction point, consistent with the decay of a bottom-quark hadron. This data set, collected at a center-of-mass energy of 1.96 TeV, and corresponding to an integrated luminosity of 5.4 fb(-1), is used to measure the Z-boson production cross section times branching ratio into b (b) over bar. The number of Z -> b (b) over bar events is determined by fitting the dijet-mass distribution, while constraining the dominant b-jet background, originating from QCD multijet events, with data. The result, sigma(p(p)over bar> -> Z) x B(Z -> b (b) over bar) = 1.11 +/- 0.08(stat) +/- 0.14(syst) nb, is the most precise measurement of this process, and is consistent with the standard-model prediction. The data set is also used to search for Higgs-boson production. No significant signal is expected in our data and the first upper limit on the cross section for the inclusive p(p)over bar>-> H -> b (b) over bar process at root s = 1.96 TeV is set, corresponding to 33 times the expected standard-model cross section, or sigma = 40.6 pb, at the 95% confidence level.

The split main sequences (MSs) and extended MS turnoffs (eMSTOs) detected in a few young clusters have demonstrated that these stellar systems host multiple populations differing in a number of properties such as rotation and, possibly, age.We analyze Hubble Space Telescope photometry for thirteen clusters with ages between ~40 and ~1000 Myrs and of different masses. Our goal is to investigate for the first time the occurrence of multiple populations in a large sample of young clusters. We find that all the clusters exhibit the eMSTO phenomenon and that MS stars more massive than ~1.6 solar masses define a blue and red MS, with the latter hosting the majority of MS stars. The comparison between the observations and isochrones suggests that the blue MSs are made of slow-rotating stars, while the red MSs host stars with rotational velocities close to the breakup value. About half of the bright MS stars in the youngest clusters are H-alpha emitters. These Be stars populate the red MS and the reddest part of the eMSTO thus supporting the idea that the red MS is made of fast rotators. We conclude that the split MS and the eMSTO are a common feature of young clusters in both Magellanic Clouds. The phenomena of a split MS and an eMSTO occur for stars that are more massive than a specific threshold which is independent of the host-cluster mass. As a by-product, we report the serendipitous discovery of a young SMC cluster, GALFOR1., Comment: 22 pages, 20 figures, accepted for publication in MNRAS

We present a multi-year survey aimed at collecting (1) high-precision (~5 milli-mag), (2) fast-cadence (~3 min), and (3) relatively long duration (~10 days) multi-band photometric series. The goal of the survey is to discover and characterize efficiently variable objects and exoplanetary transits in four fields containing five nearby open clusters spanning a broad range of ages. More in detail, our project will (1) constitute a preparatory survey for HARPS-N@TNG, which will be used for spectroscopic follow-up of any target of interest that this survey discovers or characterizes, (2) measure rotational periods and estimate the activity level of targets we are already monitoring with HARPS and HARPS-N for exoplanet transit search, and (3) long term characterization of selected targets of interest in open clusters within the planned K2 fields. In this first paper we give an overview of the project, and report on the variability of objects within the first of our selected fields, which contains two open clusters: M 35 and NGC 2158. We detect 519 variable objects, 273 of which are new discoveries, while the periods of most of the previously known variables are considerably improved., 12 pages, 11 figures (4 at low resolution), 2 tables. Accepted for publication in MNRAS on December 17, 2014. Electronic materials available at the url http://groups.dfa.unipd.it/ESPG/aphn.html , and later on the Journal and at the CDS

The internal dynamics of multiple stellar populations in Globular Clusters (GCs) provides unique constraints on the physical processes responsible for their formation. Specifically, the present-day kinematics of cluster stars, such as rotation and velocity-dispersion, could be related to the initial configuration of the system. In recent work, we provided the first study of the kinematics of different stellar populations in NGC$\,$0104 over a large field of view in the plane of the sky, exploiting Gaia Data Release 2 (DR2) proper motions combined with multi-band ground-based photometry. In this paper, we combine Gaia DR2 proper motions with Very Large Telescope radial velocities to investigate the kinematics along the line of sight and in the plane of the sky of multiple populations in seven GCs, namely NGC$\,$0104, NGC$\,$0288, NGC$\,$5904, NGC$\,$6121, NGC$\,$6254, NGC$\,$6752 and NGC$\,$6838. Among the analyzed clusters only NGC$\,$0104 and NGC$\,$5904 show significant rotation. Separating our sample into two groups of first- and second-population stars (1P and 2P) we find that overall these two populations exhibit a similar rotation pattern in NGC$\,$0104. However, some hints of different rotation are observed in the external regions of this cluster. Interestingly, 1P and 2P stars in NGC$\,$5904 show different rotation curves, with distinct phases and such difference is significant at the $\sim$2.5-$\sigma$ level. The analysis of the velocity-dispersion profiles of multiple populations confirms that 2P stars of NGC$\,$0104 show stronger anisotropy than the 1P., Comment: Accepted for publication in ApJ, 22 pages, 15 figures, 3 tables

We present high-precision multi-band photometry for the globular cluster (GC) M2. We combine the analysis of the photometric data obtained from the Hubble Space Telescope UV Legacy Survey of Galactic GCs GO-13297, with chemical abundances by Yong et al.(2014), and compare the photometry with models in order to analyze the multiple stellar sequences we identified in the color-magnitude diagram (CMD). We find three main stellar components, composed of metal-poor, metal-intermediate, and metal-rich stars (hereafter referred to as population A, B, and C, respectively). The components A and B include stars with different $s$-process element abundances. They host six sub-populations with different light-element abundances, and exhibit an internal variation in helium up to Delta Y~0.07 dex. In contrast with M22, another cluster characterized by the presence of populations with different metallicities, M2 contains a third stellar component, C, which shows neither evidence for sub-populations nor an internal spread in light-elements. Population C does not exhibit the typical photometric signatures that are associated with abundance variations of light elements produced by hydrogen burning at hot temperatures. We compare M2 with other GCs with intrinsic heavy-element variations and conclude that M2 resembles M22, but it includes an additional stellar component that makes it more similar to the central region of the Sagittarius galaxy, which hosts a GC (M54) and the nucleus of the Sagittarius galaxy itself., 12 pages, 7 figures, accepted for publication in MNRAS

We present CN and CH indices and CaII triplet metallicities for 34 giant stars and chemical abundances for 33 elements in 14 giants in the globular cluster M2. Assuming the program stars are cluster members, our analysis reveals (i) an extreme variation in CN and CH line strengths, (ii) a metallicity dispersion with a dominant peak at [Fe/H] = -1.7 and smaller peaks at -1.5 and -1.0, (iii) star-to-star abundance variations and correlations for the light elements O, Na, Al and Si and (iv) a large (and possibly bimodal) distribution in the abundances of all elements produced mainly via the s-process in solar system material. Following Roederer et al. (2011), we define two groups of stars, "r+s" and "r-only", and subtract the average abundances of the latter from the former group to obtain a "s-process residual". This s-process residual is remarkably similar to that found in M22 and in M4 despite the range in metallicity covered by these three systems. With recent studies identifying a double subgiant branch in M2 and a dispersion in Sr and Ba abundances, our spectroscopic analysis confirms that this globular cluster has experienced a complex formation history with similarities to M22, NGC 1851 and omega Centauri., Comment: Accepted for publication in MNRAS

BACKGROUND CONTEXT Various forms of computer assisted surgical navigation (CAS navigation) are primarily used to improve pedicle screw placement in both open and minimally invasive spine surgical procedures. These technologies generally employ computer modeling of the osseous anatomy, based upon preoperative CT scan or intraoperative 2D to 3D conical CT fluoroscopic scanning. The virtual representation of the spine is positioned in space with some form of registration and monitored for movement with a skeletally fixed array. Two dimensional representations of both instrumentation and anatomy are superimposed in various planes and the surgeon is tasked with manually (ie, free-hand) aligning pedicle screw instruments with virtual reality anatomic targets. As little as a 3° departure from ideal axial alignment is known to result in pedicle wall violation in the thoracic spine. It is also reported by experienced CAS practitioners, that CAS navigation should be used to “confirm,” not determine, instrument positioning, as virtual reality errors can produce substantial deviations from the intended and represented intervention axes. The use of robotics provides another level of surgical guidance that is superimposed upon CAS navigation, providing for constraint of surgeon intervention along defined axes. Both CAS navigation and robotic navigation are capital intensive in acquisition, maintenance, and utilization costs. Many facilities will be unable to afford these technologies. Portable fluoroscopy or C-arms are relatively ubiquitous in both inpatient and outpatient surgical facilities. A means of utilizing these C-arms for accurate and precise surgical navigation with reduced patient radiation exposure and minimal or negligible surgeon radiation would be desirable. This presentation demonstrates that this is achievable with a proprietary, relatively intuitive, and simple adaptation to existing C-arms. The resulting navigation can provide 3D guidance at anticipated reduced costs with accuracy and precision that rivals if not equals CAS and robotic techniques and eliminates virtual reality error. Immediate concurrent fluoroscopic confirmation of surgical intervention ("what you see is what you get" technology) provides a level of navigational assurance that is not readily available with CAS or robotic navigation. The "cobotic" feature of constraining the surgeon's intervention along a specific axis reduces error associated with "free-hand" technique. PURPOSE To demonstrate the accuracy and precision of a novel adaptation of existing portable fluoroscopic imaging for the purpose of "cobotic navigation" in a pedicle screw simulation model. STUDY DESIGN/SETTING This was an experimental study, utilizing a standard portable fluoroscopic machine (GE/OEC 9800), proprietary prototype C-arm accessories (HaloNav by Trinity Orthopedics, San Diego, CA, USA), with a pedicle surrogate model, a partially radiolucent operative table, in an outpatient surgical facility. PATIENT SAMPLE Not applicable as this was a surrogate model study. OUTCOME MEASURES The entry and exit holes of the guide pins within each of 20 surrogate pedicles was noted and measured (visually, using a digital caliper) and recorded to the nearest hundredth of a millimeter, relative to the central axis of each balsa wood cylinder. Translational error (ie, entry hole relative to the central axis) and angulatory error (calculated from entry and exit holes relative to central axis) were determined for each pedicle surrogate. The cumulative fluoroscopic time (additive time of single shot fluoroscopic images) required to place the guide pin on either side of a midline, starting from an initial localization AP acquisition image, was recorded in seconds. METHODS A portable fluoroscopic machine or C-arm (GE/OEC 9800) was reversibly modified with simple accessories (wheel cover replacement and "snap" on friction motor drives for a floor wheel and the boom) in an ambulatory surgical center setting. An attachment is cam locked to the C-arm receiver unit housing. Two millimeter diameter pedicle screw guide pins were advanced into 8 mm diameter by 30 mm long balsa wood cylinders, spray painted with zinc (for radiodensity/visualization purposes), housed in a balsa wood and plywood block at various known angles of sagittal and transverse plane inclination (convergence and lordotic angles), utilizing a standard partially radiolucent table in an ambulatory surgical facility setting. Sharp trocar tipped nitinol guide pins were advanced, utilizing a cordless pin driver (Stryker, Kalamazoo, MI, United States), within a radiolucent bushing, that is coaxially superimposed within the central beam axis of the image intensifier. The C-arm was manually rotated into various angles of sagittal convergence and lordosis using known convergence angles and the radiographic lateral projection respectively. The rotational plane of the C-arm is aligned with "common" pedicle plane for each surrogate level utilizing a radiodense wire marker and the guide pin support sleeve bushing is radiographically aligned with radiodense markers (constituting a reticle for the navigation device) with an enface view of the pedicle. Variable incremental movement of the C-arm in the X-Y coordinates of the floor plane (in submillimeter, multimillmeter, to continuous movement) electronically controlled using a dual axes gimbal (ie, joy-stick) and step motors operating friction drives. An experienced spine surgeon (presenter) with the aid of a biomechanical engineer, utilized single shot ALARA technique (no continuous fluoro and low exposure setting) to place the 2 mm guide pins and record deviations in entry position and angulation from the intended central axes of balsa wood cylinders. Fluoroscopic times required to place each pin from an initial AP acquisition images were noted as well. Simple statistical analysis was performed, based upon the measured variables. RESULTS In all 20 pedicle 8 mm × 30 mm cylindrical balsa wood surrogates, the guide pin entered and exited within the cross-sectional area of the cylinders and the entry and exit sites were readily identifiable. Translational error (ie, deviation of the entry hole from the intended central axis) varied from 0.12 mm to 1.67 mm, with an average of 0.68 mm, and a standard deviation of 0.47 mm. Angulational error (ie, calculated from entry and exit hole departures from the central axis) varied from 0.42° to 2.4°, with an average of 1.19°, and a standard deviation of 0.53°. Fluoroscopic time required to place the guide pins ranged from 10.3 to 15.5 seconds with an average time of 12.2 seconds and a standard deviation of 1.4 seconds. CONCLUSIONS This experimental study utilizing relatively simple and fully reversible modifications to a standard C-arm demonstrates the accuracy and precision obtainable in placing 2 mm guide pins into a surrogate pedicle model. The tested technology provides the equivalent of a "gun-sight" for the C-arm and the virtues of cobotic constraint in guide pin placement. Virtual reality error is not entertained with this methodology, as "what you see is what you get." Although the technology is not as yet commercially available, it provides evidence that a relatively low-cost alternative to CAS and robotic technologies for accurate cannulated pedicle screw placement is possible with the use of existing C-arm machines, commonly found in virtually all surgical facilities. FDA DEVICE/DRUG STATUS This abstract does not discuss or include any applicable devices or drugs.

We present an overview of the ongoing Hubble Space Telescope large program GO-12911. The program is focused on the core of M4, the nearest Galactic globular cluster, and the observations are designed to constrain the number of binaries with massive companions (black holes, neutron stars, or white dwarfs) by measuring the ``wobble'' of the luminous (main-sequence) companion around the center of mass of the pair, with an astrometric precision of ~50 micro-arcseconds. The high spatial resolution and stable medium-band PSFs of WFC3/UVIS will make these measurements possible. In this work we describe: (i) the motivation behind this study, (ii) our observing strategy, (iii) the many other investigations enabled by this unique data set, and which of those our team is conducting, and (iv) a preliminary reduction of the first-epoch data-set collected on October 10, 2012.

We present a general overview and the first results of the SUMO project (a SUrvey of Multiple pOpulations in Globular Clusters). The objective of this survey is the study of multiple stellar populations in the largest sample of globular clusters homogeneously analysed to date. To this aim we obtained high signal-to-noise (S/N>50) photometry for main sequence stars with mass down to ~0.5 M_SUN in a large sample of clusters using both archival and proprietary U, B, V, and I data from ground-based telescopes. In this paper, we focus on the occurrence of multiple stellar populations in twenty three clusters. We have defined a new photometric index cubi= (U-B)-(B-I), that turns out to be very effective for identifying multiple sequences along the red giant branch (RGB). We found that in the V-cubi diagram all clusters presented in this paper show broadened or multimodal RGBs, with the presence of two or more components. We found a direct connection with the chemical properties of different sequences, that display different abundances of light elements (O, Na, C, N, and Al). The cubi index is also a powerful tool to identify distinct sequences of stars along the horizontal branch and, for the first time in the case of NGC104 (47 Tuc), along the asymptotic giant branch. Our results demonstrate that i) the presence of more than two stellar populations is a common feature among globular clusters, as already highlighted in previous work; ii) multiple sequences with different chemical contents can be easily identified by using standard Johnson photometry obtained with ground-based facilities; iii) in the study of GC multiple stellar populations the cubi index is alternative to spectroscopy, and has the advantage of larger statistics., 23 pages, 20 figures, accepted for publication in MNRAS

We take advantage of the exquisite quality of the Hubble Space Telescope 26-filter astro-photometric catalog of the core of Omega Cen presented in the first paper of this series and the empirical differential-reddening correction presented in the second paper in order to distill the main sequence into its constituent populations. To this end, we restrict ourselves to the five most useful filters: the magic "trio" of F275W, F336W, and F438W, along with F606W and F814W. We develop a strategy for identifying color systems where different populations stand out most distinctly, then we isolate those populations and examine them in other filters where their sub-populations also come to light. In this way, we have identified at least 15 sub-populations, each of which has a distinctive fiducial curve through our 5-dimensional photometric space. We confirm the MSa to be split into two subcomponents, and find that both the bMS and the rMS are split into three subcomponents. Moreover, we have discovered two additional MS groups: the MSd (which has three subcomponents) shares similar properties with the bMS, and the MSe (which has four subcomponents), has properties more similar to those of the rMS. We examine the fiducial curves together and use synthetic spectra to infer relative heavy-element, light-element, and Helium abundances for the populations. Our findings show that the stellar populations and star formation history of Omega Cen are even more complex than inferred previously. Finally, we provide as a supplement to the original catalog a list that identifies for each star which population it most likely is associated with., Comment: 22 pages, 17 figures (most in lower res), 2 tables, accepted for publication in ApJ

We use high-precision photometry of red-giant-branch (RGB) stars in 57 Galactic globular clusters (GCs), mostly from the `Hubble Space Telescope (HST) UV Legacy Survey of Galactic globular clusters', to identify and characterize their multiple stellar populations. For each cluster the pseudo two-color diagram (or `chromosome map') is presented, built with a suitable combination of stellar magnitudes in the F275W, F336W, F438W and F814W filters that maximizes the separation between multiple populations. In the chromosome map of most GCs (Type I clusters), stars separate in two distinct groups that we identify with the first (1G) and the second generation (2G). This identification is further supported by noticing that 1G stars have primordial (oxygen-rich, sodium-poor) chemical composition, whereas 2G stars are enhanced in sodium and depleted in oxygen. This 1G-2G separation is not possible for a few GCs where the two sequences have apparently merged into an extended, continuous sequence. In some GCs (Type II clusters) the 1G and/or the 2G sequences appear to be split, hence displaying more complex chromosome maps. These clusters exhibit multiple SGBs also in purely optical color-magnitude diagrams, with the fainter SGB joining into a red RGB which is populated by stars with enhanced heavy-element abundance. We measure the RGB width by using appropriate colors and pseudo-colors. When the metallicity dependence is removed, the RGB width correlates with the cluster mass. The fraction of 1G stars ranges from ~8% to ~67% and anticorrelates with the cluster mass, indicating that incidence and complexity of the multiple population phenomenon both increase with cluster mass., Comment: 21 pages, 24 figures, accepted for publication in MNRAS

A measurement of the inclusive production cross section of isolated prompt photons in proton-antiproton collisions at center-of-mass energy s=1.96 TeV is presented. The results are obtained using the full Run II data sample collected with the Collider Detector at the Fermilab Tevatron, which corresponds to an integrated luminosity of 9.5 fb-1. The cross section is measured as a function of photon transverse energy, ETγ, in the range 30

This paper focuses on NGC 454, a nearby interacting pair of galaxies (AM0112-554, RR23), composed of an early-type (NGC 454 E) and a star forming late-type companion (NGC 454 W). We aim at characterizing this wet merger candidate via a multi-lambda analysis, from near-UV to optical using SWIFT-UVOT, and mapping the Halpha intensity (I) distribution, velocity (Vr), and velocity dispersion (sigma) fields with SAM+Perot-Fabry at SOAR observations. Luminosity profiles suggest that NGC 454 E is an S0. Distortions in its outskirts caused by the on-going interaction are visible in both optical and near-UV frames. In NGC 454 W, the NUV-UVOT images and the Halpha show a set of star forming complexes connected by a faint tail. Halpha emission is detected along the line connecting NGC 454 E to the NGC 454 main HII complex. We investigate the (I-sigma), (I-Vr ) (Vr-sigma) diagnostic diagrams of the HII complexes, most of which can be interpreted in a framework of expanding bubbles. In the main HII complex, enclosed in the UV brightest region, the gas velocity dispersion is highly supersonic reaching 60 km/s. However, Halpha emission profiles are mostly asymmetric indicating the presence of multiple components with an irregular kinematics. Observations point towards an advanced stage of the encounter. Our SPH simulations with chemophotometric implementation suggest that this mixed pair can be understood in terms of a 1:1 gas/halos encounter giving rise to a merger in about 0.2 Gyr from the present stage., Accepted for publication in MNRAS (21pages, 20 figures)

We report on a measurement of the D+ -meson production cross section as a function of transverse momentum (p(T)) in proton-antiproton (p (p) over bar) collisions at 1.96 TeV center-of-mass energy, using the full data set collected by the Collider Detector at Fermilab in Tevatron Run II and corresponding to 10 fb(-1) of integrated luminosity. We use D-broken vertical bar -> K- pi(broken vertical bar) pi(broken vertical bar) decays fully reconstructed in the central rapidity region broken vertical bar y broken vertical bar < 1 with transverse momentum down to 1.5 GeV/c, a range previously unexplored in p collisions. Inelastic p (p) over bar -scattering events are selected online using minimally biasing requirements followed by an optimized offline selection. The K- pi(+) pi(+) mass distribution is used to identify the D+ signal, and the D+ transverse impact-parameter distribution is used to separate prompt production, occurring directly in the hard-scattering process, from secondary production from b-hadron decays. We obtain a prompt D+ signal of 2950 candidates corresponding to a total cross section sigma(D+), 1.5 < P-T < 14.5 GeV/c, vertical bar y vertical bar < 1) = 71.9 +/- 6.8 (stat) +/- 9.3 (syst) mu b.While the measured cross sections are consistent with theoretical estimates in each p(T) bin, the shape of the observed p(T) spectrum is softer than the expectation from quantum chromodynamics. The results are unique in p collisions and can improve the shape and uncertainties of future predictions.

High-resolution spectroscopic observations were taken of 29 extended main sequence turn-off (eMSTO) stars in the young ($\sim$200 Myr) LMC cluster, NGC 1866 using the Michigan/Magellan Fiber System and MSpec spectrograph on the Magellan-Clay 6.5-m telescope. These spectra reveal the first direct detection of rapidly rotating stars whose presence has only been inferred from photometric studies. The eMSTO stars exhibit H-alpha emission (indicative of Be-star decretion disks), others have shallow broad H-alpha absorption (consistent with rotation $\gtrsim $150 km s$^{-1}$), or deep H-alpha core absorption signaling lower rotation velocities ($ \lesssim $150 km s$^{-1}$ ). The spectra appear consistent with two populations of stars - one rapidly rotating, and the other, younger and slowly rotating., Comment: 9 pages, 4 figures, Accepted for publication in ApJ Letters

Stars in open clusters are expected to share an identical abundance pattern. Establishing the level of chemical homogeneity in a given open cluster deserves further study as it is the basis of the concept of chemical tagging to unravel the history of the Milky Way. M67 is particularly interesting given its solar metallicity and age as well as being a dense cluster environment. We conducted a strictly line-by-line differential chemical abundance analysis of two solar twins in M67: M67-1194 and M67-1315. Stellar atmospheric parameters and elemental abundances were obtained with high precision using Keck/HIRES spectra. M67-1194 is essentially identical to the Sun in terms of its stellar parameters. M67-1315 is warmer than M67-1194 by ~ 150 K as well as slightly more metal-poor than M67-1194 by ~ 0.05 dex. M67-1194 is also found to have identical chemical composition to the Sun, confirming its solar twin nature. The abundance ratios [X/Fe] of M67-1315 are similar to the solar abundances for elements with atomic number Z, 10 pages, 6 figures, accepted for publication in MNRAS

Cosmological models predict the oldest stars in the Galaxy should be found closest to the centre of the potential well, in the bulge. The EMBLA Survey successfully searched for these old, metal-poor stars by making use of the distinctive SkyMapper photometric filters to discover candidate metal-poor stars in the bulge. Their metal-poor nature was then confirmed using the AAOmega spectrograph on the AAT. Here we present an abundance analysis of 10 bulge stars with -2.8, Comment: 20 pages, 16 figures. Accepted to Monthly Notices of the Royal Astronomical Society. Online tables can be found at http://www.astro.lu.se/~louise/data

nbsp nbsp nbsp Objectives Postoperative pain after hemorrhoidectomy is the most feared complication that may result in severe patient discomfort and in a delayed return to daily activities nbsp nbsp nbsp Methods In a prospective randomized controlled clinical trial consecutive patients pts with grades III and IV hemorrhoids were enrolled All pts who underwent conventional Milligan Morgan hemorrhoidectomy were randomly assigned to receive either mg intravenous iv paracetamol infusion times daily group I pts or iv constant infusion pump of tramadol plus ketorolac group II patients Pain was evaluated using a visual analogue scale VAS at and h postoperatively Length of hospital stay and severe complications were recorded nbsp nbsp nbsp Results The two groups were homogeneous with respect to sex age and degree of hemorrhoidal disease No pain was recorded after h in both groups due to persistence of the analgesic effect of the spinal anesthesia Group II had a significant reduction in VAS scores at h compared to group I p lt At h pts in group II vs pts in group I were discharged p There were two cases of bleeding requiring surgery in group I nbsp nbsp nbsp Conclusion Pain after hemorrhoidectomy is more likely to be controlled by constant infusion pump of tramadol plus ketorolac than by interspersed infusion of paracetamol A better pain control is associated with a shorter hospital stay nbsp

P2X receptors (P2XRs) are ligand-gated ion channels activated by extracellular ATP. Although the crystal structure of the zebrafish P2X4R has been solved, the exact mode of ATP binding and the conformational changes governing channel opening and desensitization remain unknown. Here, we used voltage clamp fluorometry to investigate movements in the cysteine-rich head domain of the rat P2X1R (A118-I125) that projects over the proposed ATP binding site. On substitution with cysteine residues, six of these residues (N120–I125) were specifically labeled by tetramethyl-rhodamine-maleimide and showed significant changes in the emission of the fluorescence probe on application of the agonists ATP and benzoyl-benzoyl-ATP. Mutants N120C and G123C showed fast fluorescence decreases with similar kinetics as the current increases. In contrast, mutants P121C and I125C showed slow fluorescence increases that seemed to correlate with the current decline during desensitization. Mutant E122C showed a slow fluorescence increase and fast decrease with ATP and benzoyl-benzoyl-ATP, respectively. Application of the competitive antagonist 2′,3′- O -(2,4,6-trinitrophenyl)-ATP (TNP-ATP) resulted in large fluorescence changes with the N120C, E122C, and G123C mutants and minor or no changes with the other mutants. Likewise, TNP-ATP–induced changes in control mutants distant from the proposed ATP binding site were comparably small or absent. Combined with molecular modeling studies, our data confirm the proposed ATP binding site and provide evidence that ATP orients in its binding site with the ribose moiety facing the solution. We also conclude that P2XR activation and desensitization involve movements of the cysteine-rich head domain.

At the 3-MV Tandetron accelerator of LABEC (INFN) an external beam facility is fully dedicated to particle-induced X-ray emission (PIXE) and particle-induced γ-ray emission (PIGE) measurements of atmospheric aerosol elemental composition. All the elements with Z > 10 are simultaneously detected by PIXE in a few minutes and an automatic system for positioning, changing and scanning of the samples allows the analysis of the aerosol collected by different kinds of devices: long series of daily PMX samples can be measured in short times, as well as size-segregated and high time-resolution aerosol samples. Thanks to the capability of detecting all the crustal elements, PIXE-PIGE analyses are unrivalled in the study of mineral dust: as a consequence, they are very effective in the study of natural aerosols, like, for example, mineral dust archived in polar ice cores (for environmental and paleoclimatic studies) and Saharan-dust intrusions. Among the detectable elements, there are also important markers of anthropogenic sources, which allow effective source apportionment studies in polluted urban environments. Examples regarding recent monitoring campaigns, performed in urban and remote areas, both on a daily basis and with high-time resolution (hourly samples), are presented to evidence how PIXE can still provide unique information in aerosol studies or can play a complementary role to X-ray fluorescence or induced coupled plasma mass spectroscopy analysis. Copyright © 2011 John Wiley & Sons, Ltd.

In the globular cluster NGC2808, a quasi-standard initial lithium abundance is derived for a red giant belonging to the `extreme' population, characterized by a large helium overabundance, and by abundances of proton capture elements typical of nuclear processing in gas at very high temperatures, where the initial lithium has been fully destroyed. The observations of lithium in such extreme cluster stars are important to test different models for the formation of multiple populations in old Globular Clusters. In the asymptotic giant branch (AGB) scenario, fresh lithium is synthetized during the initial phases of hot bottom burning which, afterwards, synthetize the other p-capture elements. We model the abundance of lithium in the ejecta of superAGB models, finding values consistent or larger than observed in the `extreme' giant; these same models describe correctly the magnesium depletion and silicon enrichment of the extreme population of NGC 2808, so the overall agreement provides further support to the AGB scenario. In the models involving massive or supermassive stars, the Lithium observed requires a mixture of the lithium-free ejecta of the polluting population with more than 40% of standard-lithium pristine gas. The extended chemical anomalies of NGC 2808 stars are then to be all explained within at most 60% of the possible dilution range, the initial helium mass fraction in the ejecta should be Y >= 0.5, to account for the Ye 0.38-0.40 of the extreme population, and further observations of p-process elements are needed to check the model., accepted for publication in The Astrophysical Journal Letters

Aim Sacral nerve stimulation (SNS) is an effective but expensive treatment for faecal incontinence. About 50% of the patients are unresponsive for unknown reasons, hence knowledge of any factors predictive of success would be highly desirable. The aim of this study was to analyse the potential factors associated with a successful outcome of the temporary test of electrostimulation. Method Eighty-five patients with faecal incontinence were tested for SNS. The cause was idiopathic in 45, iatrogenic or obstetric in 28, spinal lesion or neurological diseases in nine and anal malformation in three patients; 43 were tested with a unipolar electrode and 42 with a quadripolar electrode. The severity of faecal incontinence was evaluated using the American Medical System (AMS) score and Wexner’s score. Results A positive response was obtained in 45 patients (53%); 40 (47%) were implanted with a permanent pulse generator. Responders and nonresponders were comparable in age, duration of incontinence, anal manometry, pudendal nerve terminal motor latency and diabetes. Unipolar electrode test (PNE test) was able to elicit positive responses in 18 of 43 (42%) and the quadripolar in 27 of 42 patients (P

The stellar system ω Centauri (ω Cen) is well known for the large range in elemental abundances among its member stars. Recent work has indicated that the globular cluster M22 (NGC 6656) also possesses an internal abundance range, albeit substantially smallerthan that in ω Cen. Here we compare, as a function of [Fe/H], element-to-iron ratios in the two systems for a number of different elements using data from abundance analyses of red giant branch stars. It appears that the nucleosynthetic enrichment processes were very similar in these two systems despite the substantial difference in total mass.

Choice reaction time generally increases linearly with the logarithm of the number of potential stimulus–response alternatives, a regularity known as Hick’s law. Two apparent violations of this generalization, which have been reported for aimed eye movements (Kveraga, Boucher, & Hughes, Experimental Brain Research, 146, 307–314, 2002), and arm movements (Wright, Marino, Belovsky, & Chubb, Experimental Brain Research, 179, 475–496, 2007), occurred when the indicator stimulus was an abrupt change at the location that was the target of the to-be-made movement. We report two experiments that examined and rejected the hypothesis that these abrupt-onset indicator stimuli triggered a shift in exogenous attention and that this led to unusually small uncertainty effects. Each experiment compared this indicator stimulus with a single alternative: Experiment 1 tested an indicator stimulus at all locations other than the target; Experiment 2 tested a central pointer to the target. Neither alternative led to an uncertainty effect for pointing responses that was of the size typically observed for other responses using the same stimuli.

The understanding of present atmospheric transport processes from Southern Hemisphere (SH) landmasses to Antarctica can improve the interpretation of stratigraphic data in Antarctic ice cores. In addition, long range transport can deliver key nutrients normally not available to marine ecosystems in the Southern Ocean and may trigger or enhance primary productivity. However, there is a dearth of observational based studies of dust transport in the SH. This work aims to improve current understanding of dust transport in the SH by showing a characterization of two dust events originating in the Patagonia desert (south end of South America). The approach is based on a combined and complementary use of satellite retrievals (detectors MISR, MODIS, GLAS, POLDER, OMI), transport model simulation (HYSPLIT) and surface observations near the sources and aerosol measurements in Antarctica (Neumayer and Concordia sites). Satellite imagery and visibility observations confirm dust emission in a stretch of dry lakes along the coast of the Tierra del Fuego (TdF) island (~54° S) and from the shores of the Colihue Huapi lake in Central Patagonia (~46° S) in February 2005. Model simulations initialized by these observations reproduce the timing of an observed increase in dust concentration at the Concordia Station and some of the observed increases in atmospheric aerosol absorption (here used as a dust proxy) in the Neumayer station. The TdF sources were the largest contributors of dust at both sites. The transit times from TdF to the Neumayer and Concordia sites are 6–7 and 9–10 days respectively. Lidar observations and model outputs coincide in placing most of the dust cloud in the boundary layer and suggest significant deposition over the ocean immediately downwind. Boundary layer dust was detected as far as 1800 km from the source and ~800 km north of the South Georgia Island over the central sub-Antarctic Atlantic Ocean. Although the analysis suggests the presence of dust at ~1500 km SW of South Africa five days after, the limited capabilities of existing satellite platforms to differentiate between aerosol types do not permit a definitive conclusion. In addition, the model simulations show dust lifting to the free troposphere as it travels south but it could not be confirmed by the satellite observations due to cloudiness. This work demonstrates that complementary information from existing transport models, satellite and surface data can yield a consistent picture of the dust transport from the Patagonia desert to Antarctica. It also illustrates the limitation of using any of these approaches individually to characterize the transport of dust in a heavily cloudy area.

The determination of the Ba abundance in globular cluster (GC) stars is a very powerful test to address several issues in the framework of multiple population scenarios. We measured the Ba content for a sample of more than 1200 stars in 15 Galactic GCs, using high-resolution FLAMES/Giraffe spectra. We found no variation in [Ba/Fe] ratios for different stellar populations within each cluster; this means that low-mass asymptotic giant branch stars do not significantly contribute to the intra-cluster pollution. Very interestingly, we obtained that the fraction of Ba-stars in first generation (FG) stars is close to the values derived for field stars ($\sim$2\%); on the other hand, second generation (SG) stars present a significant lower fraction. An independent and successful test, based on radial velocity variations among giant stars in NGC~6121, confirms our finding: the binary fraction among FG stars is about $\sim$12\% to be compared with $\sim$1\% of SG stars. This is an evidence that SG stars formed in a denser environment, where infant mortality of binary systems was particularly efficient., Comment: final version after proofs

IBM POWER9 is a family of processor chips designed to serve a diverse set of workloads. New features have been added to POWER9 to address emerging workloads such as cognitive and artificial intelligence applications. POWER9 also further enhances features introduced in IBM POWER8 for big data and cloud applications. Distinct chips using common intellectual property building blocks are provided to enable enterprise applications requiring large symmetric multiprocessor servers with large memory footprints, as well as one to two socket industry form-factor servers. In this paper, we describe new POWER9 features for both system types. Several highly differentiated new features are described in other papers in this issue of the IBM Journal, and they provide a more in-depth description of their unique design aspects.

The determination of Li and proton-capture element abundances in globular cluster (GC) giants allows us to constrain several key questions on the multiple population scenarios in GCs, from formation and early evolution, to pollution and dilution mechanisms. In this Letter, we present our results on Li abundances for a large sample of giants in the intermediate-metallicity GC NGC 6121 (M4), for which Na and O have been already determined by Marino et al. The stars analyzed are both below and above the red giant branch bump luminosity. We found that the first and second generation stars share the same Li content, suggesting that a Li production must have occurred. This is a strong observational evidence providing support for the scenario in which asymptotic giant branch stars are GC polluters., updated version after proof

A detailed ionic component record was performed on EPICA Dome C ice core (East Antarctica) to a depth of 3190 m using Ion Chromatography and Fast Ion Chromatography (FIC). At depths greater than 2800 m, the sulfate profile shows intense, sharp spikes which are not expected due to the smoothing of sulfate peaks by diffusion processes. Moreover, these spikes show an "anomalous" chemical composition (e.g., unusually low acidity, high Mg(2+) concentration and high Mg(2+)/Ca(2+) ratio). These peaks and the surrounding layers also exhibit good Mg(2+) vs SO(4)(2-) and Cl(-) vs Na(+) correlations through both glacial and interglacial periods. Furthermore, the high-resolution analysis of two horizontally contiguous ice sections showed that some fraction of the impurities are characterized by a heterogeneous distribution. Altogether, these results suggest the occurrence of long-term postdepositional processes involving a rearrangement of impurities via migration in the vein network, characterized by sulfuric acidity and leading to the formation of soluble particles of magnesium sulfate salts, along with ionic association of ions in the liquid films along boundaries. This evidence should be taken into consideration when inferring information on for rapid climatic and environmental changes from ice core chemical records at great depths. At Dome C, the depth threshold was found to be 2800 m.

We present an abundance analysis based on high-resolution spectra of red-giant-branch (RGB) stars in the Galactic globular clusters NGC 6121 (M4) and NGC 6656 (M22). Our aim was to study their stellar population in the context of the multipopulation phenomenon recently discovered to affect some globular clusters. Analysis was performed for the following elements: O, Na, Mg, Al, Ca, Fe, Y, and Ba. Spectroscopic data were completed by high-precision wide-field U BV IC ground-based photometry and HST/ACS observations. For M4, we find a well-defined Na–O anticorrelation composed of two distinct groups of stars with significantly different Na and O content. The two groups of Na-rich and Na-poor stars populate two different regions along the RGB. As regards M22, Na and O follow the well-known anticorrelation found in many other GCs. However, at odds with M4, it appears to be continuous without any hint of clumpiness. On the other hand, we identified two clearly separated groups of stars with significantly different abundances of the s-process elements Y, Zr and Ba. The relative numbers of the members of both groups are very similar to the ratio of the stars in the two subgiant branches of M22 recently found by Piotto (2009). The s-element-rich stars are also richer in iron and have higher Ca abundances. This makes M22 the second cluster after ω Centauri where an intrinsic spread in Fe was found. Both spectroscopic and photometric results imply the presence of two stellar populations in M4 and M22, even if both clusters have completely different characteristics.

The objective of this study is to update evidence-based best practice guidelines for pediatric/adolescent weight loss surgery (WLS). We performed a systematic search of English-language literature on WLS and pediatric, adolescent, gastric bypass, laparoscopic gastric banding, and extreme obesity published between April 2004 and May 2007 in PubMed, MEDLINE, and the Cochrane Library. Keywords were used to narrow the search for a selective review of abstracts, retrieval of full articles, and grading of evidence according to systems used in established evidence-based models. In light of evidence on the natural history of obesity and on outcomes of WLS in adolescents, guidelines for surgical treatment of obesity in this age group need to be updated. We recommend modification of selection criteria to include adolescents with BMIor= 35 and specific obesity-related comorbidities for which there is clear evidence of important short-term morbidity (i.e., type 2 diabetes, severe steatohepatitis, pseudotumor cerebri, and moderate-to-severe obstructive sleep apnea). In addition, WLS should be considered for adolescents with extreme obesity (BMIor= 40) and other comorbidities associated with long-term risks. We identified1,085 papers; 186 of the most relevant were reviewed in detail. Regular updates of evidence-based recommendations for best practices in pediatric/adolescent WLS are required to address advances in technology and the growing evidence base in pediatric WLS. Key considerations in patient safety include carefully designed criteria for patient selection, multidisciplinary evaluation, choice of appropriate procedure, thorough screening and management of comorbidities, optimization of long-term compliance, and age-appropriate fully informed consent.

The optimal treatment for large colorectal polyps (LCPs) is still a controversial issue. The aim of this study was to evaluate the safety and effectiveness of endoscopic polypectomy (EP) of colorectal polyps ≥2 cm in size. One hundred fifty-one EP LCPs were performed over a period of 7 years. Diathermal snare was used for pedunculated and pseudopedunculated polyps and endoscopic mucosal resection (EMR) or biopsy forceps polypectomy for sessile and flat polyps. The resected polyps were recovered and collected for histology. At scheduled follow-up visits 1, 3, 6, and 12 months after polypectomy, complications and recurrences were recorded in all patients. Fifteen polyps were located in the rectum, 84 in the sigmoid colon, 11 in the descending colon, four in the splenic flexure, 11 in the transverse colon, 11 in the hepatic flexure, seven in the ascending colon and eight in the cecum. Fifty-six polyps were sessile, 54 pedunculated, 25 pseudopedunculated, and 16 flat. At histology, most of polyps (131) were adenomas (nine with adenocarcinoma in situ). Five were invasive polypoid carcinomas and required colonic resection. Immediate bleeding occurred in ten patients (7.6%) and it was stopped by endoscopic hemoclips (7), epinephrine injection (1), or surgery (2). There were three perforations (2.3%; all polypoid carcinomas), managed endoscopically (1) or surgically (2). Delayed bleeding occurred in two patients (1.5%) and was treated by endoscopic diathermy and hemoclips (1) or surgery (1). During follow-up, six (4.6%) incompletely excised polyps and three (2.3%) relapses in the site of previous EP were detected and endoscopically removed. EP is relatively safe and effective for benign-appearing LCPs.

We present XMM-Newton X-ray observations of two shell galaxies, NGC 7070A and ESO 2400100, and far UV observations obtained with the Optical Monitor for these and for an additional shell galaxy, NGC 474, for which we also have near and far UV data from GALEX. We aim at gaining insight on the overall evolution traced by their star formation history and by their hot gas content. The X-ray and the far UV data are used to derive their X-ray spatial and spectral characteristics and their UV luminosity profiles. We use models developed ad hoc to investigate the age of the last episode of star formation from the (UV - optical) colors and line strength indices. The X-ray spatial and spectral analysis show significant differences in the two objects. A low luminosity nuclear source is the dominant component in NGC 7070A log L_X=41.7 erg s^{-1} in the 2-10 keV band. In ESO 2400100, the X-ray emission is due to a low temperature plasma with a contribution from the collective emission of individual sources. In the Optical Monitor image ESO 2400100 shows a double nucleus, one bluer than the other. This probably results from a very recent star formation event in the northern nuclear region. The extension of the UV emission is consistent with the optical extent for all galaxies, at different degrees of significance in different filters. The presence of the double nucleus, corroborated by the (UV - optical) colors and line strength indices analysis, suggests that ESO 2400100 is accreting a faint companion. We explore the evolution of the X-ray luminosity during accretion processes with time. We discuss the link between the presence of gas and age, since gas is detected either before coalescence or several Gyr (>3) after (Abridged)., 17 pages, 11 figures, accepted for publication in A&A

Background and Objectives In this EQA study a novel approach was used to assess the performance of blood centres and blood product manufacturers in detecting the possible contamination of plasma with HCV, HIV and HBV by NAT. Materials and Methods A panel of 12 samples, three negative and three positive for each virus, was distributed to the EQA participants. The positive samples were prepared, using the respective WHO standards, in order to obtain a viral concentration of about three times the 95% DL of the methods most commonly used by laboratories involved in blood screening by NAT. Participants were requested to test each sample of the panel on different days, possibly by different operators using their routine NAT assay. Results Overall, the participants’ performance was satisfactory. In particular, 49 of the 59 participants (83%) were able to correctly identify all samples. Regarding the remaining 10 laboratories, in three cases a deviation from the laboratory's procedure that could be attributed to an operator's mistake was observed, in two cases a possible cross-contamination occurred while in the remaining five cases the failure to detect the positive samples couldn't be ascribed to any relevant deviation in the laboratory's procedure. Conclusions The novel design of this EQA study allowed participants to verify their day by day activity as the study was carried out in the context of their routine testing. Under these conditions, it was demonstrated that, despite the high level of automation reached by NAT assays, human errors can still occur.