bluuebunny/crossref_metadata_2025_split huggingface dataset:
Associations of Common -Thalassemia Mutations With -Globin Gene Frameworks in Northern Thailand
Authors: Sanguansermsri P , Shimbu D , Wongvilairat R , Sanguansermsri T 
Published: November 2017

This study aimed to characterize polymorphism of the b-globin gene (framework) among common b-thalassemia mutations found in northern Thailand. Thirty-one homozygous b-thalassemia major patients admitted to Chiang Mai University Hospital were identified using direct DNA sequencing method. Among 15 patients with homozygous of codon 41/42 (-TCTT), eight were homozygous of framework 1 (FW1), one was homozygous of FW3A, and the remainders were heterozygousof FW1 and FW3A. The gene frequencies of FW1 and FW3A in the patients were 0.733 (22/ 30) and 0.267 (8/30), respectively. All 11 patients with homozygous of codon 17 (A-T) were homozygous of FW3A, while three patients with homozygous of intron 1 nt 1 (G-T) were homozygous of FW1. Both patients with homozygous of codon 71/72 (+A) were FW3A. In this report, the numbers of b-globin gene frameworks were restricted in each b-thalassemia mutation. This investigation may provide further information for the study of the evolution of common mutations causing b-thalassemia major in northern Thailand.
Characterization of Lignin Precipitated From The Soda Black Liquor of Oil Palm Empty Fruit Bunch Fibers by Various Mineral Acids
Authors: Mohamad Ibrahim M.N , Chuah S.B , Wan Rosli W.D. 
Published: November 2017

Soda lignin from oil palm empty fruit bunch was directly isolated by various mineral acids i.e. sulfuric acid, hydrochloric acid, phosphoric acid and nitric acid at three levels of concentration (20% v/v, 60%v/v and concentrated). A comparison study was performed through physicochemical properties and structural features using FT-IR, UV, 13C-NMR and nitrobenzene oxidation. The FT-IR results showed that there is no significant difference between the main structures of the lignin isolated by various acids. However, low concentration of phosphoric acid is preferable because of its highest yield. The S: V: H ratio of 7-15:6-11:1 as evaluated by the nitrobenzene oxidation procedure suggests that soda lignin can be classified as belonging to either the cereal straw on grass type. The UV results indicate that phosphoric acid consistently gave the highest absorbance value among the four acids tested in this study regardless of its concentration level. The C13-FTNMR spectra, suggest that the lignin structure is independent of the type of acid used for precipitation.
Development of competences of personnel of service and sales network of the Russian automobile companies in the context of requirements of the standard GOST P ISO 9001-2015
Authors: Федоськина Людмила , Fedoskina Lyudmila 
Published: November 2017

The personnel of the entities of corporate dealer network of automobile company have direct interaction with final consumers of products of the company, quality of the provided service and sales services and quality of process of customer service depends on the level of his competence. The new version of the standard GOST R ISO 9001-2015 contains a number of requirements for continuous competence development of personnel. Satisfaction of this requirement is possible on the basis of competence approach, within which came the development of a competency concept that reflects the most progressive scientific views on the development of staff competencies.
Analysis of scientific literature allowed to reveal the feasibility of using the definition of the competence of employees of the dealer centers of the automotive company techniques based on the qualimetric assessment of personnel. Its application in combination with ranging of workers on the reached competence-based levels in relation to various categories of personnel will allow to increase justification of functional distribution of job responsibilities.
It is revealed that forming and development of system of corporate training acts as the main form of personnel development of the modern entity of automotive industry. On the example of the Russian automobile companies it is shown that all of them have the operating training systems of personnel of service and sales network in the form of the organization of multi-profile training centers. However, only in recent years, these centres began to turn attention to the development of competences not only technical, but also the service personnel of the dealer centers.
It is offered to expand an arsenal of the applied methods of personnel development of the entities of service and sales network of automobile company by means of more active application of the approaches used in foreign practice – Secondment and Shadowing. In article the short characteristic of these technologies is provided and the directions of their applied application in case of development of specific competences of personnel of the automobile dealer centers are proved.
Period Variations for the Cepheid VZ Cyg
Authors: Sirorattanakul Krittanon , Engle Scott , Pepper Joshua , Wells Mark , Laney Clifton D. , Rodriguez Joseph E. , Stassun Keivan G. 
Published: November 2017

Abstract
The Cepheid Period–Luminosity law is a key rung on the extragalactic distance ladder. However, numerous Cepheids are known to undergo period variations. Monitoring, refining, and understanding these period variations allows us to better determine the parameters of the Cepheids themselves and of the instability strip in which they reside, and to test models of stellar evolution. VZ Cyg, a classical Cepheid pulsating at ∼4.864 days, has been observed for over 100 years. Combining data from literature observations, the Kilodegree Extremely Little Telescope (KELT) transit survey, and new targeted observations with the Robotically Controlled Telescope (RCT) at Kitt Peak, we find a period change rate of dP/dt = −0.0642 ± 0.0018 s yr−1. However, when only the recent observations are examined, we find a much higher period change rate of dP/dt = −0.0923 ± 0.0110 s yr−1. This higher rate could be due to an apparent long-term (P ≈ 26.5 years) cyclic period variation. The possible interpretations of this single Cepheid’s complex period variations underscore both the need to regularly monitor pulsating variables and the important benefits that photometric surveys such as KELT can have on the field. Further monitoring of this interesting example of Cepheid variability is recommended to confirm and better understand the possible cyclic period variations. Further, Cepheid timing analyses are necessary to fully understand their current behaviors and parameters, as well as their evolutionary histories.
Radial Velocities of 41 Kepler Eclipsing Binaries
Authors: Matson Rachel A. , Gies Douglas R. , Guo Zhao , Williams Stephen J. 
Published: November 2017

Abstract
Eclipsing binaries are vital for directly determining stellar parameters without reliance on models or scaling relations. Spectroscopically derived parameters of detached and semi-detached binaries allow us to determine component masses that can inform theories of stellar and binary evolution. Here we present moderate resolution ground-based spectra of stars in close binary systems with and without (detected) tertiary companions observed by NASA’s Kepler mission and analyzed for eclipse timing variations. We obtain radial velocities and spectroscopic orbits for five single-lined and 35 double-lined systems, and confirm one false positive eclipsing binary. For the double-lined spectroscopic binaries, we also determine individual component masses and examine the mass ratio

distribution, which is dominated by binaries with like-mass pairs and semi-detached classical Algol systems that have undergone mass transfer. Finally, we constrain the mass of the tertiary component for five double-lined binaries with previously detected companions.
The Structure of the Young Star Cluster NGC 6231. II. Structure, Formation, and Fate
Authors: Kuhn Michael A. , Getman Konstantin V. , Feigelson Eric D. , Sills Alison , Gromadzki Mariusz , Medina Nicolás , Borissova Jordanka , Kurtev Radostin 
Published: November 2017

Abstract
The young cluster NGC 6231 (stellar ages ∼2–7 Myr) is observed shortly after star formation activity has ceased. Using the catalog of 2148 probable cluster members obtained from Chandra, VVV, and optical surveys (Paper I), we examine the cluster’s spatial structure and dynamical state. The spatial distribution of stars is remarkably well fit by an isothermal sphere with moderate elongation, while other commonly used models like Plummer spheres, multivariate normal distributions, or power-law models are poor fits. The cluster has a core radius of 1.2 ± 0.1 pc and a central density of ∼200 stars pc−3. The distribution of stars is mildly mass segregated. However, there is no radial stratification of the stars by age. Although most of the stars belong to a single cluster, a small subcluster of stars is found superimposed on the main cluster, and there are clumpy non-isotropic distributions of stars outside ∼4 core radii. When the size, mass, and age of NGC 6231 are compared to other young star clusters and subclusters in nearby active star-forming regions, it lies at the high-mass end of the distribution but along the same trend line. This could result from similar formation processes, possibly hierarchical cluster assembly. We argue that NGC 6231 has expanded from its initial size but that it remains gravitationally bound.
A 2500 deg2 CMB Lensing Map from Combined South Pole Telescope and Planck Data
Authors: Omori Y. , Chown R. , Simard G. , Story K. T. , Aylor K. , Baxter E. J. , Benson B. A. , Bleem L. E. , Carlstrom J. E. , Chang C. L. , Cho H-M. , Crawford T. M. , Crites A. T. , Haan T. de , Dobbs M. A. , Everett W. B. , George E. M. , Halverson N. W. , Harrington N. L. , Holder G. P. , Hou Z. , Holzapfel W. L. , Hrubes J. D. , Knox L. , Lee A. T. , Leitch E. M. , Luong-Van D. , Manzotti A. , Marrone D. P. , McMahon J. J. , Meyer S. S. , Mocanu L. M. , Mohr J. J. , Natoli T. , Padin S. , Pryke C. , Reichardt C. L. , Ruhl J. E. , Sayre J. T. , Schaffer K. K. , Shirokoff E. , Staniszewski Z. , Stark A. A. , Vanderlinde K. , Vieira J. D. , Williamson R. , Zahn O. 
Published: November 2017

Abstract
We present a cosmic microwave background (CMB) lensing map produced from a linear combination of South Pole Telescope (SPT) and Planck temperature data. The 150 GHz temperature data from the 2500 deg2 SPT-SZ survey is combined with the Planck 143 GHz data in harmonic space to obtain a temperature map that has a broader ℓ coverage and less noise than either individual map. Using a quadratic estimator technique on this combined temperature map, we produce a map of the gravitational lensing potential projected along the line of sight. We measure the auto-spectrum of the lensing potential

, and compare it to the theoretical prediction for a ΛCDM cosmology consistent with the Planck 2015 data set, finding a best-fit amplitude of

. The null hypothesis of no lensing is rejected at a significance of 24σ. One important use of such a lensing potential map is in cross-correlations with other dark matter tracers. We demonstrate this cross-correlation in practice by calculating the cross-spectrum,

, between the SPT+Planck lensing map and Wide-field Infrared Survey Explorer (WISE) galaxies. We fit

to a power law of the form

with a, L
0, and b fixed, and find

, which is marginally lower, but in good agreement with

, the best-fit amplitude for the cross-correlation of Planck-2015 CMB lensing and WISE galaxies over ∼67% of the sky. The lensing potential map presented here will be used for cross-correlation studies with the Dark Energy Survey, whose footprint nearly completely covers the SPT 2500 deg2 field.
Signature of a Newborn Black Hole from the Collapse of a Supra-massive Millisecond Magnetar
Authors: Chen Wei , Xie Wei , Lei Wei-Hua , Zou Yuan-Chuan , Lü Hou-Jun , Liang En-Wei , Gao He , Wang Ding-Xiong 
Published: November 2017

Abstract
An X-ray plateau followed by a steep decay (“internal plateau”) has been observed in both long and short gamma-ray burst (GRBs), implying that a millisecond magnetar operates in some GRBs. The sharp decay at the end of the plateau, marking the abrupt cessation of the magnetar’s central engine, has been considered the collapse of a supra-massive magnetar into a black hole (BH) when it spins down. If this “internal plateau” is indeed evidence of a magnetar central engine, the natural expectation in some candidates would be a signature from the newborn BH. In this work, we find that GRB 070110 is a particular case which shows a small X-ray bump following its “internal plateau.” We interpret the plateau as a spin-down supra-massive magnetar and the X-ray bump as fallback BH accretion. This indicates that a newborn BH is likely active in some GRBs. Therefore, GRB 070110-like events may provide further support to the magnetar central engine model and enable us to investigate the properties of the magnetar as well as the newborn BH.
Diffuse Ionized Gas in the Milky Way Disk
Authors: Luisi Matteo , Anderson L. D. , Balser Dana S. , Wenger Trey V. , Bania T. M. 
Published: November 2017

Abstract
We analyze the diffuse ionized gas (DIG) in the first Galactic quadrant from

ℓ
=
18
°

to 40° using radio recombination line (RRL) data from the Green Bank Telescope. These data allow us to distinguish DIG emission from H ii region emission and thus study the diffuse gas essentially unaffected by confusion from discrete sources. We find that the DIG has two dominant velocity components, one centered around 100

km

s

−
1

associated with the luminous H ii region W43, and the other centered around 45

km

s

−
1

not associated with any large H ii region. Our analysis suggests that the two velocity components near W43 may be caused by noncircular streaming motions originating near the end of the Galactic bar. At lower Galactic longitudes, the two velocities may instead arise from gas at two distinct distances from the Sun, with the most likely distances being ∼6 kpc for the 100

km

s

−
1

component and ∼12 kpc for the 45

km

s

−
1

component. We show that the intensity of diffuse Spitzer GLIMPSE 8.0 μm emission caused by excitation of polyaromatic hydrocarbons (PAHs) is correlated with both the locations of discrete H ii regions and the intensity of the RRL emission from the DIG. This implies that the soft ultraviolet photons responsible for creating the infrared emission have a similar origin as the harder ultraviolet photons required for the RRL emission. The 8.0 μm emission increases with RRL intensity but flattens out for directions with the most intense RRL emission, suggesting that PAHs are partially destroyed by the energetic radiation field at these locations.
Equation of State Dependence of Nonlinear Mode-tide Coupling in Coalescing Binary Neutron Stars
Authors: Zhou Yixiao , Zhang Fan 
Published: November 2017

Abstract
Recently, an instability due to the nonlinear coupling of p-modes to g-modes in tidally deformed neutron stars in coalescing binaries has been studied in some detail. The result is significant because it could influence the inspiral and leave an imprint on the gravitational wave signal that depends on the neutron star equation of state (EOS). Because of its potential importance, the details of the instability should be further elucidated and its sensitivity to the EOS should be investigated. To this end, we carry out a numerical analysis with six representative EOSs for both static and non-static tides. We confirm that the absence of the p-g instability under static tides, as well as its return under non-static tides, is generic across EOSs, and further reveal a new contribution to it that becomes important for moderately high-order p-g pairs (previous studies concentrated on very high order modes), whose associated coupling strength can vary by factors of ∼10–100 depending on the EOS. We find that, for stars with stiffer EOSs and smaller buoyancy frequencies, the instability onsets earlier in the inspiral and the unstable modes grow faster. These results suggest that the instability’s impact on the gravitational wave signal might be sensitive to the neutron star EOS. To fully assess this prospect, future studies will need to investigate its saturation as a function of the EOS and the binary parameters.
Propagation and Interaction Properties of Successive Coronal Mass Ejections in Relation to a Complex Type II Radio Burst
Authors: Liu Ying D. , Zhao Xiaowei , Zhu Bei 
Published: November 2017

Abstract
We examine the propagation and interaction properties of three successive coronal mass ejections (CMEs) from 2001 November 21–22, with a focus on their connection with the behaviors of the associated long-duration complex type II radio burst. In combination with coronagraph and multi-point in situ observations, the long-duration type II burst provides key features for resolving the propagation and interaction complexities of the three CMEs. The two CMEs from November 22 interacted first and then overtook the November 21 CME at a distance of about 0.85 au from the Sun. The timescale for the shock originally driven by the last CME to propagate through the preceding two CMEs is estimated to be about 14 and 6 hr, respectively. We present a simple analytical model without any free parameters to characterize the whole Sun-to-Earth propagation of the shock, which shows a remarkable consistency with all the available data and MHD simulations even out to the distance of Ulysses (2.34 au). The coordination of in situ measurements at the Earth and Ulysses, which were separated by about 71.°4 in latitude, gives important clues for the understanding of shock structure and the interpretation of in situ signatures. The results also indicate a means by which to increase geo-effectiveness with multiple CMEs, which can be considered as another manifestation of the “perfect storm” scenario proposed by Liu et al., although the current case is not “super” in the same sense as the 2012 July 23 event.
An Ultraviolet Survey of Low-redshift Partial Lyman-limit Systems with the HST Cosmic Origins Spectrograph
Authors: Shull J. Michael , Danforth Charles W. , Tilton Evan M. , Moloney Joshua , Stevans Matthew L. 
Published: November 2017

Abstract
We present an ultraviolet spectroscopic survey of strong H i absorbers in the intergalactic medium, probing their evolution over the last 6–7 Gyr at redshifts 0.24 ≤ z ≤ 0.84. We measure column densities N
H i
(cm−2) from the pattern of Lyman-series absorption lines and flux decrement at the Lyman limit (LL) when available. We analyzed 220 H i absorbers in ultraviolet spectra of 102 active galactic nuclei (AGNs) taken by the Cosmic Origins Spectrograph on board the Hubble Space Telescope with G130M/G160M gratings (1134–1795 Å). For 158 absorbers with log N
H i
≥ 15, the mean frequency is

d


/

dz
=
4.95
±
0.39

over path length Δz = 31.94 (0.24 ≤ z ≤ 0.84). We identify eight Lyman limit systems (LLS, log N
H i
≥ 17.2) and 54 partial systems (pLLS) with 16.0 ≤ log N
H i
< 17.2. Toward 159 AGNs in the range 0.01 < z
abs < 0.84 with Δz ≈ 48, we find four damped Lyα absorbers (DLA) with

(
d


/

dz
)

DLA

=

0.083

−
0.040

+
0.066

at

〈
z
〉
=
0.18

. The mean LLS frequency in z = 0.24–0.48 is

(
d


/

dz
)

LLS

=

0.36

−
0.13

+
0.20

fitted to

N

(
z
)
=
(

0.25

−
0.09

+
0.13

)
(
1
+
z
)

1.14

. For 54 pLLSs, we find

(
d


/

dz
)

pLLS

=
1.69
±
0.23

at

〈
z
〉
=
0.39

, a frequency consistent with gaseous halo sizes R ≈ 100 h
−1 kpc for (0.3–3L*) galaxies. A maximum-likelihood analysis yields a distribution

f

(
N
,
z
)
=

C

0

N

−
β

(
1
+
z
)

γ

with β = 1.48 ± 0.05 and

γ
=

1.14

−
0.89

+
0.88

for 15 ≤ log N
H i
≤ 17.5. The far-UV opacity gradient is d τ
eff/dz ≈ (0.444)(1 + z)1.14 over the range 15 ≤ log N
H i
≤ 17, implying mean LyC optical depth τ
eff ≈ 0.3–0.5 toward sources at z = 1–2.
The Properties of the Galactic Hot Gaseous Halo from X-Ray Emission
Authors: Li Yunyang , Bregman Joel 
Published: November 2017

Abstract
The extended hot X-ray emitting gaseous halo of the Milky Way has an optical depth ∼1 for the dominant emission lines of O vii and O viii, which are used to infer the halo properties. To improve on halo gas properties, we treat optical depth effects with a Monte Carlo radiative transfer model, which leads to slightly steeper density profiles (

β
≈
0.5

) than if optical depths effects were ignored. For the preferred model where the halo is rotating on cylinders at 180 km s−1, independent fits to both lines lead to identical results, where the core radius is 2.5 kpc and the turbulent component of the Doppler-b parameter is 100–120 km s−1; the turbulent pressure is 20% of the thermal pressure. The fit is improved when emission from a disk is included, with a radial scale length of 3 kpc (assumed) and a fitted vertical scale height of approximately 1.3 kpc. The disk component is a minor mass constituent and has low optical depth, except at low latitudes. The gaseous mass is

3
–
4
×

10

10

M

⊙

within

250

kpc

, similar to our previous determinations and significantly lower than the mass of the missing baryons, which is

1.7
×

10

11

M

⊙

.
Les modes de paiements à la coordination : État des lieux et pistes pour une application en France
Authors: Girault Anne , Gervès-Pinquié Chloé , Minvielle Étienne 
Published: November 2017

L’émergence de nouveaux modes de paiement occupe une place majeure dans la transformation du système de soins. Parmi eux, les « paiements à la coordination » retiennent l’attention des pouvoirs publics, désireux d’améliorer la coordination des soins. L’objectif de ce travail est de dresser un état des lieux de ces paiements et de proposer des pistes pour leur mise en œuvre dans le contexte français. Pour cela, nous avons conduit une revue intégrative de la littérature à partir des bases de données Medline, Econlit et Cochrane. Nous avons identifié 569 papiers puis, après application de nos critères, notre recherche a finalement inclus 39 papiers. Peu de preuves robustes peuvent, pour le moment, être portées au crédit de ces paiements, malgré quelques signes prometteurs. Les papiers sélectionnés concernaient en grande majorité des expériences aux Etats-Unis. Différents écueils à éviter ont été identifiés concernant notamment le niveau d’intégration des offreurs de soins, la question du transfert de risque du payeur vers les offreurs de soins ainsi que la variabilité des prises en charge. Cette analyse critique a également permis de dessiner les différents jalons pour la construction d’un tel paiement. Une fois le type de paiement choisi et la pathologie ciblée, différentes étapes sont à suivre : définir un parcours standard en collaboration avec les offreurs de soins ; calculer le montant du paiement ; définir des critères qualité qui serviront de variables d’ajustement éventuelles ; et enfin, s’entendre sur la clé de répartition du paiement entre les organisations concernées. De même, des évaluations externes de ces nouveaux modes de paiement sont nécessaires pour tester la valeur-ajoutée du dispositif. L’ensemble constitue des pistes pour une éventuelle application dans le contexte français.