bluuebunny/crossref_metadata_2025_split huggingface dataset:
Fault Fracture Detection Using Borehole Constrained Gaussian Reflection Seismic Q Extraction (QRS) in LA Concepcion Field, Lake Maracaibo, Venezuela
Authors: pigott John , Alahdal Ahmed , Gebretsadik Eshetu Serawitu 
Published: May 2016

Abstract
Reflection Seismic Q (QRS) can be economically extracted from Gaussian approximations of windowed Fourier transform frequency spectra of 3-D post-stack time migrated seismic data. Though unable to distinguish intrinsic from extrinsic attenuation and with much lower resolution than laboratory measurements, QRS, extraction still can be a robust indicator of gross spatial absorption anisotropy on a reservoir scale. As an application example, the observed differences in QRS of fracture/fault zones of La Concepcion field, Maracaibo Basin, Venezuela are interpreted as differences in fluid-gas and/or lithologic content, in the later case suggesting differences in fault gouge permeability, with high QRS values representing higher permeabilities and low QRS values representing lower permeabilities. Comparison of the poorer vertical resolution extracted QRS values to higher resolution laboratory measurements of core data in the studied interval are supportive. Comparison of extracted QRS values to laboratory measurements of core data in the studied interval are supportive.
Feasibility Study of In-Situ Combustion Huff and Puff for EOR in Super-Deep Heavy Oil Reservoir
Authors: Jinzhong Liang , Wenlong Guan , Bojun Wang , Jihong Huang 
Published: May 2016

Abstract
LKQ oil field is a super-deep heavy oil reservoir with the dead oil viscosity of 9,680~12,000mPa.s at 50?, the depth at 2,100 m~3,200 m and the reservoir temperature at 60~95°C. High oil viscosity and low flowability result in low production and rapid decline of primary development. The steam injection, as its low thermal efficiency, is not suitable for the super-deep heavy oil reservoir. In situ combustion is a promising oil recovery process in which thermal energy is generated inside the reservoir. However, the LKQ oil field has a reservoir depth of more than 2000m, no heavy oil field with such a high reservoir depth has applied high pressure in situ combustion all over the world. For the reasons, it is decided to study the feasibility of producing the field by in-situ combustion huff and puff (ISCHF) to enhance oil recovery. In this paper, the mechanism of ISCHF was analyzed firstly, and then a 3-D numerical model was constructed using STARS reservoir simulator to study the operating parameter and the economical efficiency of the ISCHF. As oxygen and natural gas may be produced together which may result in explosion, the security measures were researched by using numerical simulation. According to the simulation results, the fire line can advance symmetrically toward radial direction after the ignition; the oil was displaced to production well by steam, water and flue gas in the back production process; the accumulative air-oil ratios is below 1,000; and the oxygen content in the production gas is blow 3% if a nitrogen slug was injected after air injection stopped. The results can be used to ISCHF design and has great instruction meaning for the super-deep heavy oil reservoir development.
Characterization of procoagulant extracellular vesicles and platelet membrane disintegration in DMSO‐cryopreserved platelets
Authors: Tegegn Tseday Z. , De Paoli Silvia H. , Orecna Martina , Elhelu Oumsalama K. , Woodle Samuel A. , Tarandovskiy Ivan D. , Ovanesov Mikhail V. , Simak Jan 
Published: May 2016

BackgroundFreezing is promising for extended platelet (PLT) storage for transfusion. 6% DMSO cryopreserved PLTs (CPPs) are currently in clinical development. CPPs contain significant amount of platelet membrane vesicles (PMVs). PLT‐membrane changes and PMV release in CPP are poorly understood, and haemostatic effects of CPP PMVs are not fully elucidated. This study aims to investigate PLT‐membrane alterations in CPPs and provide comprehensive characterization of CPP PMVs, and their contribution to procoagulant activity (PCA) of CPPs.MethodsCPPs and corresponding liquid‐stored PLTs (LSPs) were characterized by flow cytometry (FC), fluorescence polarization (FP), nanoparticle tracking analysis (NTA), electron microscopy (SEM, TEM), atomic force microscopy (AFM) and thrombin‐generation (TG) test.ResultsSEM and TEM revealed disintegration and vesiculation of the PLT‐plasma membrane and loss of intracellular organization in 60% PLTs in CPPs. FP demonstrated that 6% DMSO alone and with freezing–thawing caused marked increase in PLT‐membrane fluidity. The FC counts of annexin V‐binding PMVs and CD41a+ PMVs were 68‐ and 56‐folds higher, respectively, in CPPs than in LSPs. The AFM and NTA size distribution of PMVs in CPPs indicated a peak diameter of 100 nm, corresponding to exosome‐size vesicles. TG‐based PCA of CPPs was 2‐ and 9‐folds higher per PLT and per volume, respectively, compared to LSPs. Differential centrifugation showed that CPP supernatant contributed 26% to CPP TG‐PCA, mostly by the exosome‐size PMVs and their TG‐PCA was phosphatidylserine dependent.ConclusionsMajor portion of CPPs does not show activation phenotype but exhibits grape‐like membrane disintegration with significant increase of membrane fluidity induced by 6% DMSO alone and further aggravated by freezing–thawing process. DMSO cryopreservation of PLTs is associated with the release of PMVs and marked increase of TG‐PCA, as compared to LSPs. Exosome‐size PMVs have significant contribution to PCA of CPPs.
THE HUBBLE SPACE TELESCOPE UV LEGACY SURVEY OF GALACTIC GLOBULAR CLUSTERS. VII. IMPLICATIONS FROM THE NEARLY UNIVERSAL NATURE OF HORIZONTAL BRANCH DISCONTINUITIES*
Authors: Brown T. M. , Cassisi S. , D’Antona F. , Salaris M. , Milone A. P. , Dalessandro E. , Piotto G. , Renzini A. , Sweigart A. V. , Bellini A. , Ortolani S. , Sarajedini A. , Aparicio A. , Bedin L. R. , Anderson J. , Pietrinferni A. , Nardiello D. 
Published: May 2016

ABSTRACT
The UV-initiative Hubble Space Telescope Treasury survey of Galactic globular clusters provides a new window into the phenomena that shape the morphological features of the horizontal branch (HB). Using this large and homogeneous catalog of UV and blue photometry, we demonstrate that the HB exhibits discontinuities that are remarkably consistent in color (effective temperature). This consistency is apparent even among some of the most massive clusters hosting multiple distinct sub-populations (such as NGC 2808, ω Cen, and NGC 6715), demonstrating that these phenomena are primarily driven by atmospheric physics that is independent of the underlying population properties. However, inconsistencies arise in the metal-rich clusters NGC 6388 and NGC 6441, where the discontinuity within the blue HB (BHB) distribution shifts ∼1000–2000 K hotter. We demonstrate that this shift is likely due to a large helium enhancement in the BHB stars of these clusters, which in turn affects the surface convection and evolution of such stars. Our survey also increases the number of Galactic globular clusters known to host blue-hook stars (also known as late hot flashers) from 6 to 23 clusters. These clusters are biased toward the bright end of the globular cluster luminosity function, confirming that blue-hook stars tend to form in the most massive clusters with significant self-enrichment.
Hα IMAGING OF NEARBY SEYFERT HOST GALAXIES
Authors: Theios Rachel L. , Malkan Matthew A. , Ross Nathaniel R. 
Published: May 2016

ABSTRACT
We used narrowband (Δλ = 70 Å) interference filters with the CCD imaging camera on the Nickel 1.0 m telescope at Lick Observatory to observe 31 nearby (z < 0.03) Seyfert galaxies in the 12 μm active galaxy sample. We obtained pure emission-line images of each galaxy, which reach down to a flux limit of 7.3 × 10−15 erg cm−2 s−1 arcsec−2, and corrected these images for [N ii] emission and extinction. We separated the Hα emission line of the “nucleus” (central 100–1000 pc) from that of the host galaxy. The extended Hα emission is expected to be powered by newly formed hot stars, and indeed correlates well with other indicators of current star formation rates (SFRs) in these galaxies: extended 7.7 μm polycyclic aromatic hydrocarbon, total far-infrared, and radio luminosity. Relative to what would be expected from recent star formation, there is a 0.8 dex excess of radio emission in our Seyfert galaxies. The Hα luminosity we measured in the centers of our galaxies is dominated by the active galactic nucleus (AGN), and is linearly correlated with the hard X-ray luminosity. There is, however, an upward offset of 1 dex in this correlation for the Seyfert 1s, because their nuclear Hα emission includes a strong additional contribution from the broad-line region. We found a correlation between SFR and AGN luminosity. In spite of selection effects, we concluded that the absence of bright Seyfert nuclei in galaxies with low SFRs is real, albeit only weakly significant. Finally, we used our measured spatial distributions of Hα emission to determine what these Seyfert galaxies would look like when observed through fixed apertures (e.g., a spectroscopic fiber) at high redshifts. We found that although all of these Seyfert galaxies would be detectable emission-line galaxies at any redshift, most of them would appear to be dominated by (>67%) their H ii region emission. Only the most luminous AGNs (log(L
Hα
/erg s−1) > 41.5) would still be identified as such at z ∼ 0.3.
A NEW CONSTRAINT ON THE Lyα FRACTION OF UV VERY BRIGHT GALAXIES AT REDSHIFT 7
Authors: Furusawa Hisanori , Kashikawa Nobunari , Kobayashi Masakazu A. R. , Dunlop James S. , Shimasaku Kazuhiro , Takata Tadafumi , Sekiguchi Kazuhiro , Naito Yoshiaki , Furusawa Junko , Ouchi Masami , Nakata Fumiaki , Yasuda Naoki , Okura Yuki , Taniguchi Yoshiaki , Yamada Toru , Kajisawa Masaru , Fynbo Johan P. U. , Fèvre Olivier Le 
Published: May 2016

ABSTRACT
We study the extent to which very bright (

) Lyman-break-selected galaxies at redshifts

display detectable Lyα emission. To explore this issue, we obtained follow-up optical spectroscopy of 9

galaxies from a parent sample of 24

galaxy candidates selected from the 1.65 deg2 COSMOS-UltraVISTA and SXDS-UDS survey fields using the latest near-infrared public survey data, and new ultra-deep Subaru z′-band imaging (which we also present and describe in this paper). Our spectroscopy yielded only one possible detection of Lyα at z = 7.168 with a rest-frame equivalent width

. The relative weakness of this line, combined with our failure to detect Lyα emission from the other spectroscopic targets, allows us to place a new upper limit on the prevalence of strong Lyα emission at these redshifts. For conservative calculation and to facilitate comparison with previous studies at lower redshifts, we derive a 1σ upper limit on the fraction of UV-bright galaxies at

that display

, which we estimate to be

. This result may indicate a weak trend where the fraction of strong Lyα emitters ceases to rise, and possibly falls between z ≃ 6 and

. Our results also leave open the possibility that strong Lyα may still be more prevalent in the brightest galaxies in the reionization era than their fainter counterparts. A larger spectroscopic sample of galaxies is required to derive a more reliable constraint on the neutral hydrogen fraction at

based on the Lyα fraction in the bright galaxies.
K2 ROTATION PERIODS FOR LOW-MASS HYADS AND THE IMPLICATIONS FOR GYROCHRONOLOGY
Authors: Douglas S. T. , Agüeros M. A. , Covey K. R. , Cargile P. A. , Barclay T. , Cody A. , Howell S. B. , Kopytova T. 
Published: May 2016

ABSTRACT
As the closest open cluster to the Sun, the Hyades is an important benchmark for many stellar properties, but its members are also scattered widely over the sky. Previous studies of stellar rotation in the Hyades relied on targeted observations of single stars or data from shallower all-sky variability surveys. The re-purposed Kepler mission, K2, is the first opportunity to measure rotation periods (P
rot) for many Hyads simultaneously while also being sensitive to fully convective M dwarf members. We analyze K2 data for 65 Hyads and present P
rot values for 48. Thirty-seven of these are new measurements, including the first P
rot measurements for fully convective Hyads. For 9 of the 11 stars with P
rot in the literature and this work, the measurements are consistent; we attribute the two discrepant cases to spot evolution. Nearly all stars with masses ≲0.3 M
⊙ are rapidly rotating, indicating a change in rotation properties at the boundary to full convection. When confirmed and candidate binaries are removed from the mass–period plane, only three rapid rotators with masses ≳0.3 M
⊙ remain. This is in contrast to previous results showing that the single-valued mass–period sequence for ≈600 Myr old stars ends at ≈0.65 M
⊙ when binaries are included. We also find that models of rotational evolution predict faster rotation than is actually observed at ≈600 Myr for stars ≲0.9 M
⊙. The dearth of single rapid rotators more massive than ≈0.3 M
⊙ indicates that magnetic braking is more efficient than previously thought, and that age–rotation studies must account for multiplicity.
UNBOUND DEBRIS STREAMS AND REMNANTS RESULTING FROM THE TIDAL DISRUPTIONS OF STARS BY SUPERMASSIVE BLACK HOLES
Authors: Guillochon James , McCourt Michael , Chen Xian , Johnson Michael D. , Berger Edo 
Published: May 2016

ABSTRACT
The kinetic energy of a star in orbit about a supermassive black hole is a significant fraction of its rest mass energy when its periapse is comparable to its tidal radius. Upon its destruction, a fraction of this energy is extracted and injected into the stellar debris, half of which becomes unbound from the black hole, with the fastest material moving at

. In this paper, we present a formalism for determining the fate of these unbound debris streams (UDSs) as they depart from the black hole and interact with the surrounding gas. As the density and velocity varies along the length of a UDS, we find that hydrodynamical drag quickly shapes UDSs into loop-like structures, with the densest portions of the streams leading portions of lower density. As UDSs travel outwards, their drag against the ISM increases quadratically with distance, which causes UDSs to deposit their momentum and energy into the ambient medium before the surrounding shocked ISM has a chance to cool. This sudden injection of

erg into the ambient medium generates a Sedov-like unbound debris remnant (UDR) that mimics supernova remnants (SNRs) in energetics and appearance, accelerates particles which will produce cosmic rays and synchrotron emission, and provides momentum feedback into the molecular clouds surrounding a black hole. We estimate that a few of these UDRs might be present within a couple degrees of the Galactic Center masquerading as SNRs, and that the UDR scenario is a plausible explanation for Sgr A east.
STAR FORMATION IN W3—AFGL 333: YOUNG STELLAR CONTENT, PROPERTIES, AND ROLES OF EXTERNAL FEEDBACK
Authors: Jose Jessy , Kim Jinyoung S. , Herczeg Gregory J. , Samal Manash R. , Bieging John H. , Meyer Michael R. , Sherry William H. 
Published: May 2016

ABSTRACT
One of the key questions in the field of star formation is the role of stellar feedback on the subsequent star formation process. The W3 giant molecular cloud complex at the western border of the W4 super bubble is thought to be influenced by the massive stars in W4. This paper presents a study of the star formation activity within AFGL 333, a ∼104
M
⊙ cloud within W3, using deep JHK

s
photometry obtained from the NOAO Extremely Wide Field Infrared Imager combined with Spitzer IRAC and MIPS photometry. Based on the infrared excess, we identify 812 candidate young stellar objects (YSOs) in the complex, of which 99 are Class I and 713 are Class II sources. The stellar density analysis of YSOs reveals three major stellar aggregates within AFGL 333, namely AFGL 333 Main, AFGL 333 NW1 and AFGL 333 NW2. The disk fraction within AFGL 333 is estimated to be ∼50%–60%. We use the extinction map made from the

colors of the background stars and CO data to understand the cloud structure and to estimate the cloud mass. From the stellar and cloud mass associated with AFGL 333, we infer that the region is currently forming stars with an efficiency of ∼4.5% and at a rate of ∼2–3 M
⊙ Myr−1 pc−2. In general, the star formation activity within AFGL 333 is comparable to that of nearby low mass star-forming regions. We do not find any strong evidence to suggest that the stellar feedback from the massive stars of nearby W4 super bubble has affected the global star formation properties of the AFGL 333 region.
THE NEXT GENERATION VIRGO CLUSTER SURVEY XVI: THE ANGULAR MOMENTUM OF DWARF EARLY-TYPE GALAXIES FROM GLOBULAR CLUSTER SATELLITES
Authors: Toloba Elisa , Li Biao , Guhathakurta Puragra , Peng Eric W. , Ferrarese Laura , Côté Patrick , Emsellem Eric , Gwyn Stephen , Zhang Hongxin , Boselli Alessandro , Cuillandre Jean-Charles , Jordan Andres , Liu Chengze 
Published: May 2016

ABSTRACT
We analyze the kinematics of six Virgo cluster dwarf early-type galaxies (dEs) from their globular cluster (GC) systems. We present new Keck/DEIMOS spectroscopy for three of them and re-analyze the data found in the literature for the remaining three. We use two independent methods to estimate the rotation amplitude (V
rot) and velocity dispersion (σ
GC) of the GC systems and evaluate their statistical significance by simulating non-rotating GC systems with the same number of GC satellites and velocity uncertainties. Our measured kinematics agree with the published values for the three galaxies from the literature and, in all cases, some rotation is measured. However, our simulations show that the null hypothesis of being non-rotating GC systems cannot be ruled out. In the case of VCC 1861, the measured V
rot and the simulations indicate that it is not rotating. In the case of VCC 1528, the null hypothesis can be marginally ruled out, and thus it might be rotating although further confirmation is needed. In our analysis, we find that, in general, the measured V
rot tends to be overestimated and the measured σ
GC tends to be underestimated by amounts that depend on the intrinsic V
rot/σ
GC, the number of observed GCs (N
GC), and the velocity uncertainties. The bias is negligible when N
GC ≳ 20. In those cases where a large N
GC is not available, it is imperative to obtain data with small velocity uncertainties. For instance, errors of ≤2 km s−1 lead to V
rot < 10 km s−1 for a system that is intrinsically not rotating.
A UNIFORM CATALOG OF MOLECULAR CLOUDS IN THE MILKY WAY
Authors: Rice Thomas S. , Goodman Alyssa A. , Bergin Edwin A. , Beaumont Christopher , Dame T. M. 
Published: May 2016

ABSTRACT
The all-Galaxy CO survey of Dame et al. is by far the most uniform, large-scale Galactic CO survey. Using a dendrogram-based decomposition of this survey, we present a catalog of 1064 massive molecular clouds throughout the Galactic plane. This catalog contains 2.5 × 108 solar masses, or

25

−
5.8

+
10.7

%

of the Milky Way's estimated H2 mass. We track clouds in some spiral arms through multiple quadrants. The power index of Larson's first law, the size-linewidth relation, is consistent with 0.5 in all regions—possibly due to an observational bias—but clouds in the inner Galaxy systematically have significantly (∼30%) higher linewidths at a given size, indicating that their linewidths are set in part by the Galactic environment. The mass functions of clouds in the inner Galaxy versus the outer Galaxy are both qualitatively and quantitatively distinct. The inner Galaxy mass spectrum is best described by a truncated power law with a power index of γ = −1.6 ± 0.1 and an upper truncation mass of M
0 = (1.0 ± 0.2) × 107
M
⊙, while the outer Galaxy mass spectrum is better described by a non-truncating power law with γ = −2.2 ± 0.1 and an upper mass of M
0 = (1.5 ± 0.5) × 106
M
⊙, indicating that the inner Galaxy is able to form and host substantially more massive GMCs than the outer Galaxy. Additionally, we have simulated how the Milky Way would appear in CO from extragalactic perspectives, for comparison with CO maps of other galaxies.
A key to the East Palaearctic and Oriental species of the genus Rhysipolis Foerster, and the first host records of Rhysipolis longicaudatus Belokobylskij (Hymenoptera: Braconidae: Rhysipolinae)
Authors: Zhang Ying , Xiong Zi-Cheng , van Achterberg Kees , Li Tao 
Published: May 2016

A key to the East Palaearctic and northern Oriental species of Rhysipolis Foerster, 1862 (Hymenoptera: Braconidae: Rhysipolinae) is presented. Rhysipolis longicaudatus Belokobylskij, 1994 (stat. nov.) is redescribed, the first host records are given and it is reported new for China.
Rhysipolis longicaudatus was reared from Taleporia sp. (Lepidoptera: Psychidae) in Inner Mongolia Autonomous Region and from Bazaria turensis Ragonot (Lepidoptera: Pyralidae) in Qinghai Province.
Field growth traits and insect-host plant interactions of two transgenic canola (Brassicaceae) lines with elevated trichome numbers
Authors: Alahakoon U. , Adamson J. , Grenkow L. , Soroka J. , Bonham-Smith P. , Gruber M. 
Published: May 2016

AbstractPlant growth and insect resistance characteristics were determined for two Brassica napus Linnaeus (Brassicaceae) lines, AtGL3+ and K-5-8, developed for enhanced trichome densities relative to their parental cultivar Westar. In the field, both transgenic lines had glabrous cotyledons that curled upwards at emergence but flattened with time, and young leaves with elevated trichome density. Flea beetle (Phyllotreta cruciferae (Goeze) and Phyllotreta striolata (Fabricius); Coleoptera: Chrysomelidae) feeding was reduced on true leaves of both lines by 30–50% compared with insecticide-free Westar. Flea beetle feeding levels on cotyledons of the two hairy-leaved lines were lower than on unprotected Westar and similar to those seen on insecticide-treated Westar. Antixenosis and antibiosis resistance was observed when diamondback moths (Plutella xylostella (Linnaeus); Lepidoptera: Plutellidae) interacted with the hairy AtGL3+ and K-5-8 lines in the laboratory. Although the numbers of eggs laid by female diamondback moths on the transformed lines were similar to or higher than on Westar, in feeding bioassays larvae moved off AtGL3+ plants and larval feeding injury decreased on the transformed lines compared with Westar leaves. No agronomic or seed yield penalties were found for plants of K-5-8. These data highlight the utility of manipulating trichome regulatory genes to increase plant resistance against brassicaceous insect pests.
Integrating Heterogeneous Biomedical Data for Cancer Research: the CARPEM infrastructure
Authors: Canuel Vincent , Countouris Hector , Laurent-Puig Pierre , Burgun Anita , Rance Bastien 
Published: May 2016

SummaryCancer research involves numerous disciplines. The multiplicity of data sources and their heterogeneous nature render the integration and the exploration of the data more and more complex. Translational research platforms are a promising way to assist scientists in these tasks. In this article, we identify a set of scientific and technical principles needed to build a translational research platform compatible with ethical requirements, data protection and data-integration problems. We describe the solution adopted by the CARPEM cancer research program to design and deploy a platform able to integrate retrospective, prospective, and day-to-day care data. We designed a three-layer architecture composed of a data collection layer, a data integration layer and a data access layer. We leverage a set of open-source resources including i2b2 and tranSMART.Citation: Rance B, Canuel V, Countouris H, Laurent-Puig P, Burgun A. Integrating heterogeneous biomedical data for cancer research: the CARPEM infrastructure.