bluuebunny/crossref_metadata_2025_split huggingface dataset:
Daily sodium consumption and CVD mortality in the general population: systematic review and meta-analysis of prospective studies
Authors: Poggio Rosana , Gutierrez Laura , Matta María G , Elorriaga Natalia , Irazola Vilma , Rubinstein Adolfo 
Published: May 2014

AbstractObjectiveThe purpose of the present study was to determine whether elevated dietary Na intake could be associated with CVD mortality.DesignWe performed a systematic review and meta-analysis of prospective studies representing the general population. The adjusted relative risks and their 95 % confidence intervals were pooled by the inverse variance method using random-effects models. Heterogeneity, publication bias, subgroup and meta-regression analyses were performed.SettingsMEDLINE (since 1973), Embase (since 1975), the Cochrane Library (since 1976), ISI Web of Science, Google Scholar (until September 2013) and secondary referencing were searched for inclusion in the study.SubjectEleven prospective studies with 229 785 participants and average follow-up period of 13·37 years (range 5·5–19 years).ResultsHigher Na intake was significantly associated with higher CVD mortality (relative risk=1·12; 95 % CI 1·06, 1·19). In the sensitivity analysis, the exclusion of studies with important relative weights did not significantly affect the results (relative risk=1·08; 95 % CI 1·01, 1·15). The meta-regression analysis showed that for every increase of 10 mmol/d in Na intake, CVD mortality increased significantly by 1 % (P=0·016). Age, hypertensive status and length of follow-up were also associated with increased CVD mortality.ConclusionsHigher Na intake was associated with higher CVD mortality in the general population; this result suggests a reduction in Na intake to prevent CVD mortality from any cause.
Analytical Formulae for Calculation of X-Ray Detector Solid Angles in the Scanning and Scanning/Transmission Analytical Electron Microscope
Authors: Zaluzec Nestor J. 
Published: May 2014

AbstractClosed form analytical equations used to calculate the collection solid angle of six common geometries of solid-state X-ray detectors in scanning and scanning/transmission analytical electron microscopy are presented. Using these formulae one can make realistic comparisons of the merits of the different detector geometries in modern electron column instruments. This work updates earlier formulations and adds new detector configurations.
Self-rating makes the difference: Identifying palliative care needs of patients feeling severely affected by multiple sclerosis
Authors: Strupp Julia , Golla Heidrun , Galushko Maren , Buecken Raphael , Ernstmann Nicole , Hahn Moritz , Pfaff Holger , Voltz Raymond 
Published: May 2014

AbstractObjective:People feeling severely affected by multiple sclerosis (MS) comprise a heterogeneous group, and this heterogeneity leads to very distinct needs and makes planning for needs difficult. To provide optimal care, it is important to identify specific needs in specific subgroups. Our objective was to identify the specific palliative care (PC) needs of patients who felt severely affected by the disease by analyzing their feeling (1) more or (2) less severely affected and their possible differences in expressed care needs.Method:A self-report questionnaire with 25 needs categories including 7 categories pertaining to care was applied to patients who felt severely affected by MS. An additional single question identified patients feeling more (≥7, median-split) and less (<7) severely affected. Differences were analyzed by chi-squared and Mann–Whitney U tests. The sample (N = 573) was composed of respondents who replied to an invitation by the German Multiple Sclerosis Society to participate in a survey on unmet needs of severely affected patients.Results:Of 573 patients (median age 51), 358 (62.48%) felt more severely affected. Compared to patients feeling less severely affected, they found the stress on their next of kin to be higher (p < 0.001), were in greater need of home visitation (p < 0.001), did not have permanent neurologists (p = 0.016), and felt that they visited them too rarely (p < 0.0001). They also needed more emotional support from their nursing care service (p = 0.006).Significance of results:A self-rating scale can identify two groups of patients with different care needs. These data may help shaping patient-centered support structures. Palliative care, with its multidisciplinary approach, might be one further option to meet the specific needs of patients and their relatives.
Physical conditions and chemistry of molecular gas in galactic centers
Authors: Aalto Susanne 
Published: May 2014

AbstractStudying the molecular phase of the interstellar medium in galaxy nuclei is fundamental for the understanding of the onset and evolution of star formation and the growth of supermassive black holes. We can use molecules as observational tools exploiting them as tracers of chemical, physical and dynamical conditions. The molecular physical conditions in galaxy centers show large variety among galaxies, but in general the average gas densities (traced by e.g. HCN) and temperatures (probed by e.g. H2CO, NH3) are greater than in their disks. Molecular gas and dust is being funneled to the centers of galaxies by spiral arms, bars, and interactions - and one example of this is the minor merger NGC1614. Gas surface densities are also greater in galaxy nuclei and in extreme cases they become orders of magnitudes larger than what we find in the center of our own Milky Way. We can use IR excited molecular emission to probe the very inner regions of galaxies with deeply obscured nuclei where N(H2)>1024 cm−2 - for example the luminous infrared galaxy (LIRG) NGC4418. Abundances of key molecules such as HCN, HCO+, HNC, HC3N, CN, H3O+ are important tools in identifying the nature of buried activity and its evolution. Standard astrochemical scenarios (including X-ray Dominated regions (XDRs) and Photon Dominated Regions (PDRs)) are briefly discussed in this review and how we can use molecules to distinguish between them. High resolution studies are often necessary to separate effects of excitation and radiative transfer from those of chemistry - one example is absorption and effects of stimulated emission in the ULIRG Arp220. The nuclear activity in luminous galaxies often drives outflows and winds and in some cases molecular gas is being entrained in the outflows. Sometimes the molecular gas is carrying the bulk of the momentum. We can study the structure and physical conditions of the molecular gas to constrain the mass outflow rates and the evolution and nature of the driving source and two examples are discussed here: NGC1377 and Mrk231.
The Galactic center: not an active galactic nucleus
Authors: An Deokkeun , Ramírez Solange V. , Sellgren Kris 
Published: May 2014

AbstractWe present 10 μm – 35μm Spitzer spectra of the interstellar medium in the central molecular zone (CMZ), the central 210 pc × 60 pc of the Galactic center (GC). We present maps of the CMZ in ionic and H2 emission, covering a more extensive area than earlier spectroscopic surveys in this region. We compare diagnostic line ratios measured in the Spitzer Infrared Nearby Galaxies Survey to our data. Previous work shows that forbidden line ratios can distinguish star-forming galaxies from low-ionization nuclear emission-line regions (LINERs) and active galactic nuclei (AGNs). Our GC line ratios agree with star-forming galaxies and not with LINERs or AGNs.
The thermal state of molecular clouds in the Galactic center: evidence for non-photon-driven heating
Authors: Ao Y. , Henkel C. , Menten K. M. , Requena-Torres M. A. , Stanke T. , Mauersberger R. , Aalto S. , Mühle S. , Mangum J. 
Published: May 2014

AbstractWe have used the Atacama Pathfinder Experiment (APEX) 12 m telescope at 218 GHz to observe molecular clouds simultaneously in the JKaKc = 303→202, 322→221, and 321→220 transitions of para-H2CO to determine kinetic temperatures of the dense gas in the central molecular zone of the Galaxy. Gas kinetic temperatures for individual molecular clouds range from 55 to 125 K or even higher. The molecular clouds at high temperatures may be heated by turbulent dissipation and/or cosmic-rays.
An X-ray survey of the central molecular zone: variability of the FeKα emission line
Authors: Soldi Simona , Clavel Maïca , Goldwurm Andrea , Morris Mark R. , Ponti Gabriele , Terrier Régis , Trap Guillaume 
Published: May 2014

AbstractThe bulk of the FeKα emission detected in the central molecular zone (CMZ) is thought to be associated with reflection by the central molecular clouds of enhanced past emission from an external X-ray source, most likely Sgr A*. In order to follow the propagation of the reflected emission through the Galactic center (GC), we analyzed all XMM-Newton observations carried out from 2000 to 2012. Preliminary results indicate that while most of the regions that were bright at 6.4 keV in 2000–2001 have a significantly lower flux in 2012, a few other experienced a flux increase. We report for the first time a significant decrease of the FeKα emission in the Sgr C complex, supporting the reflection origin of the 6.4 keV emission detected in this region.
Opening again the debate: the transient nature of the circumnuclear disk
Authors: Requena-Torres M. A. , Mills E. A. C. , Güsten R. , Morris M. R. , Weiss A. , Martín-Pintado J. , Harris A. 
Published: May 2014

AbstractDespite many investigations, the physical characteristics of the molecular gas in the Galactic center circumnuclear disk (CND) remain a topic of debate. Its mass is highly uncertain, between 104 (from dust) and 105–6 M⊙ (derived from gas tracers), and depending on the probe, density estimates for the dense clumps are 105–8 cm−3 and gas temperatures run from 50 to a few hundred K. The range of physical parameters leaves open many questions about the nature and fate of the CND. Using several ground-based observatories, together with Herschel and SOFIA, we have studied the physical conditions of the dense clumps using CO, HCN and HCO+, finding that most of them are transient. Their densities are not large enough for them to be gravitationally bound in the tidal field in the center of our Galaxy.
A radio survey of Galactic center clouds
Authors: Mills E. A. C. , Lang C. C. , Morris M. R. , Ott J. , Butterfield N. , Ludovici D. , Schmitz S. , Schmiedeke A. 
Published: May 2014

AbstractWe present a radio survey of molecules in a sample of Galactic center molecular clouds, including M0.25 + 0.01, the clouds near Sgr A, and Sgr B2. The molecules detected are primarily NH3 and HC3N; in Sgr B2-N we also detect non-metastable NH3, vibrationally-excited HC3N, torsionally-excited CH3OH, and numerous isotopologues of these species. 36 GHz Class I CH3OH masers are ubiquitous in these fields, and in several cases are associated with new NH3 (3,3) maser candidates. We also find that NH3 and HC3N are depleted or absent toward several of the highest dust column density peaks identified in submillimeter observations, which are associated with water masers and are thus likely in the early stages of star formation.
The Galactic center: a model for cosmic ray interactions in starburst galaxies?
Authors: Yoast-Hull T. , Gallagher J. S. , Zweibel E. 
Published: May 2014

AbstractThe Galactic center contains strong magnetic fields, high radiation fields, and dense molecular gas, as is also the case in starburst galaxies. The close proximity of the Galactic center allows for more and better observations of the interstellar medium than for extragalactic sources making it an ideal place for testing models for cosmic ray interactions. We compare our semi-analytic model for cosmic ray interactions to published data for both the Galactic center and the starburst galaxy NGC 253. We present the predicted radio and γ-ray spectra and compare the results with published measurements. In this way we provide a quantitative basis for assessing the degree to which the Galactic center resembles a starburst system.
Gas inflow and nuclear star formation in galaxies with non-axisymmetric bulges
Authors: Kim E. , Kim S. S. , Lee G.-H. , Lee M. G. , de Grijs R. 
Published: May 2014

AbstractWe present the dependence of the amount of nuclear star formation on the non-axisymmetry of a bulge of disk galaxies. For this, we use a volume-limited sample of spiral galaxies at 0.02 < = z < 0.055 from the SDSS DR7. Among 3173 final sample galaxies with an axis ratio b/a > 0.6 and a bulge fraction ranged in B/T <= 0.41, nuclear starburst galaxies are 10%. We find that a fraction of the nuclear starburst galaxies become higher when ellipticity of a bulge increases in early type galaxies. Also, the fraction increases clearly when early type galaxies are isolated and in low density region. Our results indicate that the non-axisymmetry of bulges assists gas to fall inside and affects the nuclear starburst process in disk galaxies.
A 3-D mid-infrared view of the central parsec
Authors: Moultaka J. , Eckart A. , Mužić K. , Sabha N. 
Published: May 2014

AbstractWe present a mid-infrared 3D view of the central parsec using ISAAC spectrograph (ESO/VLT) with its spectroscopic mode. We mapped the central parsec in L- and M-bands by using 27 and 21 slit positions, respectively, that allowed us to build two data cubes of the region in these spectral domains. We also use an original method to distinguish the contribution of the foreground extinction to the absorbed spectra from that of the local extinction in both wavelength ranges. We find that there are residual water and CO ices in the central parsec as well as hydrocarbons and gaseous CO implying very low temperatures of the order of tens of Kelvin in the local environment of Sgr A*.
Chemical differentiation in Sagittarius B2(N): first high resolution results
Authors: Corby J. F. , Jones P. A. , Cunningham M. R. , Remijan A. J. 
Published: May 2014

AbstractSgr B2 is an active high mass star forming region in the Galactic center and the pre-eminent interstellar source of organic chemistry. Newly available broad bandwidth radio interferometry data enables a spatially resolved study of the chemical environments within the Sgr B2(N) core. We present selections from a 30 - 50 GHz spectral line survey conducted with the ATCA.
On the origin of young stars at the Galactic center
Authors: Madigan Ann-Marie , Pfuhl Oliver , Levin Yuri , Gillessen Stefan , Genzel Reinhard , Perets Hagai B. 
Published: May 2014

AbstractThe center of our Galaxy is home to a massive black hole, Sgr A*, and a nuclear star cluster containing stellar populations of various ages. While the late type stars may be too old to have retained memory of their initial orbital configuration, and hence formation mechanism, the kinematics of the early type stars should reflect their original distribution. In this contribution we present a new statistic which uses directly-observable kinematic stellar data to infer orbital parameters for stellar populations, and is capable of distinguishing between different origin scenarios. We use it on a population of B-stars in the Galactic center that extends out to large radii (∼0.5 pc) from the massive black hole. We find that the high K-magnitude population (≲15 M⊙) form an eccentric distribution, suggestive of a Hills binary-disruption origin.
Forming misaligned stellar disks around a massive black hole: cloud infall in the Galactic center
Authors: Lucas William , Bonnell Ian , Davies Melvyn , Rice Ken 
Published: May 2014

AbstractThe innermost parsec around Sgr A* has been found to play host to two disks or streamers of O and W-R stars. They are misaligned by an angle approaching 90°. That the stars are approximately coeval indicates that they formed in the same event rather than independently. We have performed smoothed particle hydrodynamic simulations of the infall of a single prolate cloud towards a massive black hole. As the cloud is disrupted, the large spread in angular momentum can, if conditions allow, lead to the creation of misaligned gas disks. In turn, stars may form within those disks. We are now investigating the origins of these clouds in the Galactic center (GC) region.
Hydrodynamical simulations of a compact source scenario for G2
Authors: Ballone A. , Schartmann M. , Burkert A. , Gillessen S. , Genzel R. , Fritz T. K. , Eisenhauer F. , Pfuhl O. , Ott T. 
Published: May 2014

AbstractThe origin of the dense gas cloud “G2” discovered in the Galactic center (Gillessen et al. 2012) is still a debated puzzle. G2 might be a diffuse cloud or the result of an outflow from an invisible star embedded in it. We present here detailed simulations of the evolution of winds on G2's orbit. We find that the hydrodynamic interaction with the hot atmosphere present in the Galactic center and the extreme gravitational field of the supermassive black hole must be taken into account when modeling such a source scenario. We also find that in this scenario most of the Brγ luminosity is expected to come from the highly filamentary densest shocked wind material. G2's observational properties can be used to constrain the properties of the outflow and our best model has a mass outflow rate of Ṁw=8.8 × 10−8 M⊙ yr−1 and a wind velocity of vw = 50 km s−1. These values are compatible with those of a young TTauri star wind, as already suggested by Scoville & Burkert (2013).
The reflection of two past outbursts of Sagittarius A* observed by Chandra during the last decade
Authors: Clavel M. , Terrier R. , Goldwurm A. , Morris M. R. , Ponti G. , Soldi S. , Trap G. 
Published: May 2014

AbstractThe supermassive black hole at the Galactic center, Sagittarius A* has experienced periods of higher activity in the past. The reflection of these past outbursts is observed in the molecular material surrounding the black hole but reconstructing its precise lightcurve is difficult since the distribution of the clouds along the line of sight is poorly constrained.Using Chandra high-resolution data collected from 1999 to 2011 we studied both the 6.4 keV and the 4–8 keV emission of the region located between Sgr A* and the Radio arc, characterizing its variations down to 15″ angular scale and 1-year time scale. The emission from the molecular clouds in the region varies significantly, showing either a 2-year peaked emission or 10-year linear variations. This is the first time that such fast variations are measured. Based on the cloud parameters, we conclude that these two behaviors are likely due to two distinct past outbursts of Sgr A* during which its luminosity rose to at least 1039 erg s−1.
Nonthermal filamentary radio features within 20 pc of the Galactic center
Authors: Morris M. R. , Zhao J.-H. , Goss W. M. 
Published: May 2014

AbstractDeep imaging of the Sgr A complex at 6 cm wavelength with the B and C configurations of the Karl G. Jansky VLA† has revealed a new population of faint radio filaments. Like their brighter counterparts that have been observed throughout the Galactic center on larger scales, these filaments can extend up to ∼10 parsecs, and in most cases are strikingly uniform in brightness and curvature. Comparison with a survey of Paschen-α emission reveals that some of the filaments are emitting thermally, but most of these structures are nonthermal: local magnetic flux tubes illuminated by synchrotron emission. The new image reveals considerable filamentary substructure in previously known nonthermal filaments (NTFs). Unlike NTFs previously observed on larger scales, which tend to show a predominant orientation roughly perpendicular to the Galactic plane, the NTFs in the vicinity of the Sgr A complex are relatively randomly oriented. Two well-known radio sources to the south of Sgr A – sources E and F – consist of numerous quasi-parallel filaments that now appear to be particularly bright portions of a much larger, strongly curved, continuous, nonthermal radio structure that we refer to as the “Southern Curl”. It is therefore unlikely that sources E and F are Hii regions or pulsar wind nebulae. The Southern Curl has a smaller counterpart on the opposite side of the Galactic center – the Northern Curl – that, except for its smaller scale and smaller distance from the center, is roughly point-reflection symmetric with respect to the Southern Curl. The curl features indicate that some field lines are strongly distorted, presumably by mass flows. The point symmetry about the center then suggests that the flows originate near the center and are somewhat collimated.
Characteristics of millimeter variability of Sgr A*
Authors: Tsutsumi T. , Miyazaki A. , Tsuboi M. 
Published: May 2014

AbstractWe present the analysis of flux variations of Sgr A* at millimeter wavelengths based on the long-term monitoring project spanning over a decade using the Nobeyama Millimeter Array. We investigate basic characteristics of the flux variability using some standard parameterizations of the data. Such basic properties of the flux variations in the mm-regime can provide valuable information not only for its underlying mechanisms in general but also for understanding observed radio/mm flux measurements during an accretion event.
Effects of magnetic field on the runaway instability of relativistic accretion tori near a rotating black hole
Authors: Karas V. , Hamerský J. 
Published: May 2014

AbstractRunaway instability operates in accretion tori around black holes, where it affects systems close to the critical (cusp overflowing) configuration. The runaway effect depends on the radial profile l(R) of the angular momentum distribution of the fluid, on the dimension-less spin a of the central black hole (|a| ≤ 1), and other factors, such as self-gravity. Here we discuss the role of runaway instability within a framework of an axially symmetric model of perfect fluid endowed with a purely toroidal magnetic field.
High-energy particles from SN-explosions near the Galactic center
Authors: Dorfi Ernst A. , Steiner Daniel 
Published: May 2014

AbstractSeveral supernovae exploding in a compact cluster of massive stars generate a galactic outflow with embedded shock waves. Based on numerical simulations for an expanding superbubble above the Galactic center we find that these individual waves generated by the repeated SN-explosions, interact with each other and finally coalesce into a single strong shock at a distance of 5 kpc above the Galactic plane at about 5 ċ 106 years after outbreak. The resulting shock with a Mach number M ≃ 10 propagates up to 100 kpc in less than 108 years. The time-dependent mass an energy loss out of the superbubble affects the further evolution of the outflow. In such long lasting shock waves energetic particles can be accelerated above the knee of 1015 eV already near the galactic plane by a first-order Fermi-mechanism. The additional pressure gradients from such cosmic rays lead to further accelerations of the galactic outflow since these ultra-relativistic particles suffer less from adiabatic losses than the thermal gas.