bluuebunny/crossref_metadata_2025_split huggingface dataset:
Characterization of Aeromonashydrophila Type Strains Isolates from Industrial Wastewater Hilla - Iraq
Authors: Alahmed Suad Ghali Kadhim , AL-Saffar Anwar Kadhim , Al-Chaabawi Thekraabdulaali Abed 
Published: October 2017

Twenty one strains of motile Aeromonas species were isolated fromIndustrial wastewaterAl- Furat Company Hilla- Iraq. The Study aimed to evaluate the possible ecological effect of the industrial waste water released from Company . Samples were monthly taken started from may 2013 to October 2013 . The results showed that the natural properties of waste water were variable due to the nature of the materials dumping in the derange stream . It was found the pH ranged from (1.5 - 5.2 ) , conductivity reached to 3100 Ms / cm while the higher concentration of COD, TDS , Cl , SO4 , Ca and Mg were 140, 1953, 335, 738, 200 and 104 mg/l respectively. A. hydrophila suspected isolale was screening by traditionally tests and then confirmed by Vitek 2 system and PCR technique (16S r RNA gene). Inthis study A. hydrophilstrains are highly resistance to several antibiotics that was considered as pathogen for human being causing several disease.
Modelling of Risk Factors of Diabetes in United Arab Emirates (UAE)
Authors: Haroun Suheer 
Published: October 2017

Objectives: The aim of this study was to model and determine factors influencing the risk of diabetes mellitus (DM) in the United Arab Emirates and to analyze data related to the topic.
Methods: The study was carried out in UAE, using a questionnaire to out-patients in a medical clinic that contained socio-demographic characteristics and risk factors were used for data collection. Sample survey data analyzed using descriptive techniques, correlations, and binary logistic regression models. Binary logistic regression were performed to find the crude and adjusted odds ratio (OR) and 95% confidence interval (CI) was calculated to find the significance of the observed OR. A p-value ≤ 0.05 was considered statistically significant All Analysis was performed using SPSS and Microsoft excels.
Results: study results showed that six main factors influence the risk of diabetes in UAE, which are, blood glucose, blood pressure, physical activity, waist size, gender and family history of diabetes. Marital status, smoking, and intake of fresh vegetables and fruits did not show any statistically significant association with risk of diabetes in UAE. Blood glucose is observed as the most statistically significant factor (for every one unit increase in blood glucose, the study expect a 5.422 increase in the risk of developing diabetes), at the meantime gender observed as the lowest statistically significant factor (if the respondent is male the probability of being diabetic is 0.809 percent) holding all other independent variables constant.
Conclusion: Results of the present study will be one of use in planning primordial, primary and secondary measures of prevention at the community. Encouraging physical activity, controlling blood pressure and blood glucose may significantly decrease the risk of diabetes mortality; effective health education programs promoting regular exercise and effective advices may needed to reduce the burden of diabetes in UAE.
The Relationship Between Personality Traits and Managers` Leadership Styles
Authors: Simic Jelena , Ristic Marija Runic , Milosevic Tamara Kezic , Ristic Dusan 
Published: October 2017

Abstract
This research study starts with the hypothesis that the personality traits of managers influence their leadership styles. Personality traits are taken from the model Big Five (McCrae and Costa) since it is one of the most dominant models of personality in modern psychology. Management styles (leadership) were investigated within the theories of transformational and transactional leadership, including laissez-faire style (Bruce Avolio & Bernard Bass). The research was conducted with 160 lower-level, middle-level and high-level managers in Serbia, employed in private and public sectors. From the questionnaire the NEO Personality Inventory (Serbian version, Kostić, P. 2002), and with the analysis of the main components, five dimensions of personality have been extracted: extraversion, neuroticism, conscientiousness, agreeableness and openness to experience. From the shorter version of Multifactor Leadership Questionnaire, three factors of leadership have been extracted: transformational, transactional and laissez-faire. The relationship between the received factors was checked by Pearson`s correlation coefficient and by multiple regression analysis. The received information showed that there is a statistically significant relationship between personality traits and leadership styles, and the most dominant relationship is between the transformational leadership style and extraversion (in a positive sense) and neuroticism (in a negative sense).
Karyotypic variation and pollen stainability in resynthesized allopolyploids Tragopogon miscellus and T. mirus
Authors: Spoelhof Jonathan P. , Chester Michael , Rodriguez Roseana , Geraci Blake , Heo Kweon , Mavrodiev Evgeny , Soltis Pamela S. , Soltis Douglas E. 
Published: October 2017

PREMISE OF THE STUDY:Polyploidy has extensively shaped the evolution of plants, but the early stages of polyploidy are still poorly understood. The neoallopolyploid species Tragopogon mirus and T. miscellus are both characterized by widespread karyotypic variation, including frequent aneuploidy and intergenomic translocations. Our study illuminates the origins and early impacts of this variation by addressing two questions: How quickly does karyotypic variation accumulate in Tragopogon allopolyploids following whole‐genome duplication (WGD), and how does the fertility of resynthesized Tragopogon allopolyploids evolve shortly after WGD?METHODS:We used genomic in situ hybridization and lactophenol‐cotton blue staining to estimate the karyotypic variation and pollen stainability, respectively, of resynthesized T. mirus and T. miscellus during the first five generations after WGD.KEY RESULTS:Widespread karyotypic variation developed quickly in synthetics and resembled that of naturally occurring T. mirus and T. miscellus by generation S4. Pollen stainability in resynthesized allopolyploids was consistently lower than that of natural T. mirus and T. miscellus, as well as their respective diploid progenitor species. Logistic regression showed that mean pollen stainability increased slightly over four generations in resynthesized T. mirus but remained at equivalent levels in T. miscellus.CONCLUSIONS:Our results clarify some of the changes that occur in T. mirus and T. miscellus immediately following their origin, most notably the rapid onset of karyotypic variation within these species immediately following WGD.
Complete chloroplast genome sequences contribute to plant species delimitation: A case study of the Anemopaegma species complex
Authors: Firetti Fabiana , Zuntini Alexandre Rizzo , Gaiarsa Jonas Weismann , Oliveira Renata Souza , Lohmann Lúcia G. , Van Sluys Marie‐Anne 
Published: October 2017

PREMISE OF THE STUDY:Bignoniaceae is an important component of neotropical forests and a model for evolutionary and biogeographical studies. A previous combination of molecular markers and morphological traits improved the phylogeny of the group. Here we demonstrate the value of next‐generation sequencing (NGS) to assemble the chloroplast genome of eight Anemopaegma species and solve taxonomic problems.METHODS:Three NGS platforms were used to sequence total DNA of Anemopaegma species. After genome assembly and annotation, we compared chloroplast genomes within Anemopaegma, with other Lamiales species, and the evolutionary rates of protein‐coding genes using Tanaecium tetragonolobum as the outgroup. Phylogenetic analyses of Anemopaegma with different data sets were performed.KEY RESULTS:Chloroplast genomes of Anemopaegma species ranged from 167,413 bp in A. foetidum to 168,987 bp in A. acutifolium (“typical” form). They exhibited a characteristic quadripartite structure with a large single‐copy region (75,070−75,761 bp), a small single‐copy region (12,766−12,817 bp) and a pair of inverted repeat regions (IRs) (39,480−40,481) encoding an identical set of 112 genes. An inversion of a fragment with ca. 8 kb, located in the IRs and containing the genes trnI‐AAU, ycf2, and trnL‐CAA, was observed in these chloroplast genomes when compared with those of other Lamiales.CONCLUSIONS:Anemopaegma species have the largest genomes within the Lamiales possibly due to the large amount of repetitive sequences and IR expansion. Variation was higher in coding regions than in noncoding regions, and some genes were identified as markers for differentiation between species. The use of the entire chloroplast genome gave better phylogenetic resolution of the taxonomic groups. We found that two forms of A. acutifolium result from different maternal lineages.
Insights from Synthetic Star-forming Regions. II. Verifying Dust Surface Density, Dust Temperature, and Gas Mass Measurements With Modified Blackbody Fitting
Authors: Koepferl Christine M. , Robitaille Thomas P. , Dale James E. 
Published: October 2017

Abstract
We use a large data set of realistic synthetic observations (produced in Paper I of this series) to assess how observational techniques affect the measurement physical properties of star-forming regions. In this part of the series (Paper II), we explore the reliability of the measured total gas mass, dust surface density and dust temperature maps derived from modified blackbody fitting of synthetic Herschel observations. We find from our pixel-by-pixel analysis of the measured dust surface density and dust temperature a worrisome error spread especially close to star formation sites and low-density regions, where for those “contaminated” pixels the surface densities can be under/overestimated by up to three orders of magnitude. In light of this, we recommend to treat the pixel-based results from this technique with caution in regions with active star formation. In regions of high background typical in the inner Galactic plane, we are not able to recover reliable surface density maps of individual synthetic regions, since low-mass regions are lost in the far-infrared background. When measuring the total gas mass of regions in moderate background, we find that modified blackbody fitting works well (absolute error: + 9%; −13%) up to 10 kpc distance (errors increase with distance). Commonly, the initial images are convolved to the largest common beam-size, which smears contaminated pixels over large areas. The resulting information loss makes this commonly used technique less verifiable as now χ
2 values cannot be used as a quality indicator of a fitted pixel. Our control measurements of the total gas mass (without the step of convolution to the largest common beam size) produce similar results (absolute error: +20%; −7%) while having much lower median errors especially for the high-mass stellar feedback phase. In upcoming papers (Paper III; Paper IV) of this series we test the reliability of measured star formation rate with direct and indirect techniques.
Chemical Mapping of the Milky Way with The Canada–France Imaging Survey: A Non-parametric Metallicity–Distance Decomposition of the Galaxy
Authors: Ibata Rodrigo A. , McConnachie Alan , Cuillandre Jean-Charles , Fantin Nicholas , Haywood Misha , Martin Nicolas F. , Bergeron Pierre , Beckmann Volker , Bernard Edouard , Bonifacio Piercarlo , Caffau Elisabetta , Carlberg Raymond , Côté Patrick , Cabanac Rémi , Chapman Scott , Duc Pierre-Alain , Durret Florence , Famaey Benoît , Fabbro Sébastien , Gwyn Stephen , Hammer Francois , Hill Vanessa , Hudson Michael J. , Lançon Ariane , Lewis Geraint , Malhan Khyati , Matteo Paola di , McCracken Henry , Mei Simona , Mellier Yannick , Navarro Julio , Pires Sandrine , Pritchet Chris , Reylé Celine , Richer Harvey , Robin Annie C. , Jannsen Rubén Sánchez , Sawicki Marcin , Scott Douglas , Scottez Vivien , Spekkens Kristine , Starkenburg Else , Thomas Guillaume , Venn Kim 
Published: October 2017

Abstract
We present the chemical distribution of the Milky Way, based on 2900

of u-band photometry taken as part of the Canada–France Imaging Survey. When complete, this survey will cover 10,000

of the northern sky. By combing the CFHT u-band photometry together with Sloan Digital Sky Survey and Pan-STARRS

and i, we demonstrate that we are able to reliably measure the metallicities of individual stars to ∼0.2 dex, and hence additionally obtain good photometric distance estimates. This survey thus permits the measurement of metallicities and distances of the dominant main-sequence (MS) population out to approximately

, and provides a much higher number of stars at large extraplanar distances than have been available from previous surveys. We develop a non-parametric distance–metallicity decomposition algorithm and apply it to the sky at

and to the North Galactic Cap. We find that the metallicity–distance distribution is well-represented by three populations whose metallicity distributions do not vary significantly with vertical height above the disk. As traced in MS stars, the stellar halo component shows a vertical density profile that is close to exponential, with a scale height of around

. This may indicate that the inner halo was formed partly from disk stars ejected in an ancient minor merger.
A New Stellar Outburst Associated with the Magnetic Activities of the K-type Dwarf in a White Dwarf Binary
Authors: Qian S.-B. , Han Z.-T. , Zhang B. , Zejda M. , Michel R. , Zhu L.-Y. , Zhao E.-G. , Liao W.-P. , Tian X.-M. , Wang Z.-H. 
Published: October 2017

Abstract
1SWASP J162117.36+441254.2 was originally classified as an EW-type binary with a period of 0.20785 days. However, it was detected to have undergone a stellar outburst on 2016 June 3. Although the system was later classified as a cataclysmic variable (CV) and the event was attributed as a dwarf nova outburst, the physical reason is still unknown. This binary has been monitored photometrically since 2016 April 19, and many light curves were obtained before, during, and after the outburst. Those light and color curves observed before the outburst indicate that the system is a special CV. The white dwarf is not accreting material from the secondary and there are no accretion disks surrounding the white dwarf. By comparing the light curves obtained from 2016 April 19 to those from September 14, it was found that magnetic activity of the secondary is associated with the outburst. We show strong evidence that the L
1 region on the secondary was heavily spotted before and after the outburst and thus quench the mass transfer, while the outburst is produced by a sudden mass accretion of the white dwarf. These results suggest that J162117 is a good astrophysical laboratory to study stellar magnetic activity and its influences on CV mass transfer and mass accretion.
An X-Ray Periodicity of ∼1.8 hr in Narrow-line Seyfert 1 Galaxy Mrk 766
Authors: Zhang Peng , Zhang Peng-fei , Yan Jing-zhi , Fan Yi-zhong , Liu Qing-zhong 
Published: October 2017

Abstract
In the narrow-line Seyfert 1 galaxy Mrk 766, a quasi-periodic oscillation (QPO) signal with a period of ∼6450 s is detected in the XMM-Newton data collected on 2005 May 31. This QPO signal is highly statistically significant at the ∼5σ confidence level, with a quality factor of

Q
=
f

/

Δ
f
>
13.6

. The X-ray intensity changed by a factor of 3, with a root mean square fractional variability of 14.3%. Furthermore, this QPO signal is present in the data of all three EPIC detectors and two RGS cameras and its frequency follows the

f

QPO

–

M

BH

relation spanning from stellar-mass to supermassive black holes. Interestingly, a possible QPO signal with a period of ∼4200 s had been reported in the literature. The frequency ratio of these two QPO signals is ∼3:2. Our result is also in support of the hypothesis that the QPO signals can just be transient. The spectral analysis reveals that the contribution of the soft excess component below ∼1 keV is different between epochs with and without QPO. This property, as well as the former frequency ratio, are well-detected in X-ray BH binaries, which may shed some light on the physical origins of our event.
Post-main-sequence Evolution of Icy Minor Planets. III. Water Retention in Dwarf Planets and Exomoons and Implications for White Dwarf Pollution
Authors: Malamud Uri , Perets Hagai B. 
Published: October 2017

Abstract
Studies suggest that the pollution of white dwarf (WD) atmospheres arises from the accretion of minor planets, but the exact properties of polluting material, and in particular the evidence for water in some cases are not yet understood. Several previous works studied the possibility of water surviving inside minor planets around evolving stars. However, they all focused on small, comet-sized to moonlet-sized minor planets, when the inferred mass inside the convection zones of He-dominated WDs could actually be compatible with much more massive minor planets. Here we explore for the first time, the water retention inside exoplanetary dwarf planets, or moderate-sized moons, with radii of the order of hundreds of kilometers. This paper concludes a series of papers that has now covered nearly the entire potential mass range of minor planets, in addition to the full mass range of their host stars. We find that water retention is (a) affected by the mass of the WD progenitor, and (b) it is on average at least 5%, irrespective of the assumed initial water composition, if it came from a single accretion event of an icy dwarf planet or moon. The latter prediction strengthens the possibility of habitability in WD planetary systems, and it may also be used in order to distinguish between pollution originating from multiple small accretion events and singular large accretion events. To conclude our work, we provide a code that calculates ice and water retention by interpolation and may be freely used as a service to the community.
GASP. III. JO36: A Case of Multiple Environmental Effects at Play?
Authors: Fritz Jacopo , Moretti Alessia , Gullieuszik Marco , Poggianti Bianca , Bruzual Gustavo , Vulcani Benedetta , Nicastro Fabrizio , Jaffé Yara , Cervantes Sodi Bernardo , Bettoni Daniela , Biviano Andrea , Fasano Giovanni , Charlot Stéphane , Bellhouse Callum , Hau George 
Published: October 2017

Abstract
The so-called jellyfish galaxies are objects exhibiting disturbed morphology, mostly in the form of tails of gas stripped from the main body of the galaxy. Several works have strongly suggested ram pressure stripping to be the mechanism driving this phenomenon. Here, we focus on one of these objects, drawn from a sample of optically selected jellyfish galaxies, and use it to validate sinopsis, the spectral fitting code that will be used for the analysis of the GASP (GAs Stripping Phenomena in galaxies with MUSE) survey, and study the spatial distribution and physical properties of the gas and stellar populations in this galaxy. We compare the model spectra to those obtained with gandalf, a code with similar features widely used to interpret the kinematics of stars and gas in galaxies from IFU data. We find that sinopsis can reproduce the pixel-by-pixel spectra of this galaxy at least as well as gandalf does, providing reliable estimates of the underlying stellar absorption to properly correct the nebular gas emission. Using these results, we find strong evidences of a double effect of ram pressure exerted by the intracluster medium onto the gas of the galaxy. A moderate burst of star formation, dating between 20 and 500 Myr ago and involving the outer parts of the galaxy more strongly than the inner regions, was likely induced by a first interaction of the galaxy with the intracluster medium. Stripping by ram pressure, plus probable gas depletion due to star formation, contributed to create a truncated ionized gas disk. The presence of an extended stellar tail on only one side of the disk points instead to another kind of process, likely gravitational interaction by a fly-by or a close encounter with another galaxy in the cluster.
Near L-edge Single and Multiple Photoionization of Singly Charged Iron Ions
Authors: Schippers Stefan , Martins Michael , Beerwerth Randolf , Bari Sadia , Holste Kristof , Schubert Kaja , Viefhaus Jens , Savin Daniel Wolf , Fritzsche Stephan , Müller Alfred 
Published: October 2017

Abstract
Absolute cross-sections for m-fold photoionization (

m
=
1
,

…
,

6

) of Fe+ by a single photon were measured employing the photon–ion merged-beams setup PIPE at the PETRA III synchrotron light source, operated by DESY in Hamburg, Germany. Photon energies were in the range 680–920 eV, which covers the photoionization resonances associated with

2
p

and

2
s

excitation to higher atomic shells as well as the thresholds for

2
p

and

2
s

ionization. The corresponding resonance positions were measured with an uncertainty of ±0.2 eV. The cross-section for Fe+ photoabsorption is derived as the sum of the individually measured cross-sections for m-fold ionization. Calculations of the Fe+ absorption cross-sections were carried out using two different theoretical approaches, Hartree–Fock including relativistic extensions and fully relativistic multiconfiguration Dirac–Fock. Apart from overall energy shifts of up to about 3 eV, the theoretical cross-sections are in good agreement with each other and with the experimental results. In addition, the complex de-excitation cascades after the creation of inner-shell holes in the Fe+ ion were tracked on the atomic fine-structure level. The corresponding theoretical results for the product charge-state distributions are in much better agreement with the experimental data than previously published configuration-average results. The present experimental and theoretical results are valuable for opacity calculations and are expected to pave the way to a more accurate determination of the iron abundance in the interstellar medium.
Evidence for Higher Black Hole Spin in Radio-loud Quasars
Authors: Schulze Andreas , Done Chris , Lu Youjun , Zhang Fupeng , Inoue Yoshiyuki 
Published: October 2017

Abstract
One of the major unsolved questions concerning the understanding of the active galactic nucleus population is the origin of the dichotomy between radio-quiet and radio-loud quasars. The most promising explanation is provided by the spin paradigm, which suggests that radio-loud quasars have a higher black hole spin. However, the measurement of black hole spin remains extremely challenging. We here aim at comparing the mean radiative efficiencies of carefully matched samples of radio-loud and radio-quiet Sloan Digital Sky Survey (SDSS) quasars at

0.3
<
z
<
0.8

. We use the [O iii] luminosity as an indirect average tracer of the ionizing continuum in the extreme-UV regime where the differences in the spectral energy distribution (SED) due to black hole spin are most pronounced. We find that the radio-loud sample shows an enhancement in [O iii] line strength by a factor of at least 1.5 compared to a radio-quiet sample matched in redshift, black hole mass, and optical continuum luminosity or accretion rate. We argue that this enhancement is caused by differences in the SED, suggesting higher average bolometric luminosities at fixed accretion rate in the radio-loud population. This suggests that the radio-loud quasar population has on average systematically higher radiative efficiencies and therefore higher black hole spin than the radio-quiet population, providing observational support for the black hole spin paradigm.