bluuebunny/crossref_metadata_2025_split huggingface dataset:
Horizontal Well Accuracy and its Effect on Infill Drilling in the Winter Area
Authors: Cameron Bill , Baldwin Chris , Miller Karl , Becker Lane 
Published: February 2016

ABSTRACT
The Winter pool in Saskatchewan has been developed using horizontal wells 800 to 1400 meters long at 75 meter nominal spacing. The horizontal sections are located near the top of the reservoir to maximize the area swept by the coning behavior of the bottom water. Section 31-42-25 W3M is now being infill drilled to 37.5 meter spacing in an attempt to increase reservoir drainage. The heels of the infill wells are being placed between the toes of the original wells to avoid expected greater oil depletion and water coning at the heels of the original wells.
Several initial infill wells encountered lost circulation and/or magnetic interference from offsetting original wells, indicating the locations of the original wells obtained from MWD data were not accurate. For subsequent infill wells gyros were run in the original offsetting wells to verify trajectories. The gyro-based well locations disagreed with the MWD-based well locations. This prompted an examination of existing drilling, Gyro, MWD, and magnetic North positioning data and technology.
This paper will discuss the theoretical and practical aspects of (1) establishing the locations of existing horizontal wells, and (2) placing infill horizontal wells in optimum locations between the existing wells in the Winter pool.
Dependence of Some Sagd Operations Characteristics on Steam Zone Pressure
Authors: Thimm H. F. 
Published: February 2016

Abstract
A number of operations characteristics of Steam Assisted Gravity Drainage (SAGD) projects, such as production rates of hydrogen sulphide and carbon dioxide, silica dissolution, and scale production are strong functions of steam zone pressure.
The present paper explores the pressure dependence of acid gas (CO2 and H2S) production, acid gas quality, and the associated potential for the need to recover sulphur in commercial SAGD projects. Further aspects explored are silica production, carbonate scaling, and the formation of unusual scales in SAGD facilities, as a function of steam zone pressure.
Statistical Review of the Performance of Some Horizontal wells Drilled in IOR/EOR Projects and Gas Pools in the WCSB
Authors: Springer Selwyn , Sadal D (SID) , Turta Alex 
Published: February 2016

Abstract
More than 10 000 horizontal wells have been drilled in the Westem Canadian Sedimentary Basin (WCSB) between 1987 and the present. About 5 000 of these wells have been drilled in conventional oil pools on primary production, and about 1000 wells have been drilled in heavy oil bitumen reservoirs. In addition about 3000 wells have been drilled in enhanced oil recovery (EOR} projects (mainly waterfloods, and miscible/immiscible gas/hydrocarbon injection solvent floods), and about 1000 horizontal wells have been drilled in natural gas reservoirs. As expected in each group the initial production rate and cumulative production (5 years) show some variation from the mean/average rates..
In this review we will focus our attention on the performance of horizontal wells drilled in EOR projects and natural gas pools. We have grouped these wells into conventional heavy oil sandstone waterflood projects; Light-medium oil sandstone waterflood projects; carbonate waterflood projects; carbonate "horizontal miscible" solvent floods projects; carbonate "vertical miscible" solvent floods projects; sandstone gas horizontal wells projects; and carbonate gas horizontal wells project. Horizontal wells drilled in conventional oil pools on primary production and heavy oil/bitumen in-situ projects are not included in this review. We have identified representative samples for each group. The median, mean/average, 75th percentile and 25th percentile have been determined for the initial rates, and 5-year cumulative (5-year cum.) production. Production Performance Rate-Time Plots for each group are shown.
We have also provided a short discussion of the performance of each group. In our discussion we have tried to identify wells/pools and formations which are chiefly responsible for the 75th and 25th percentile performance, and have discussed some of the reservoir rock and fluid characteristics which may be responsible for the variation in performance. Brief comments are also made on some drilling or operational techniques employed which may have affected the performance.
Effective Translation of an Intensive Lifestyle Intervention for Hispanic Women With Prediabetes in a Community Health Center Setting
Authors: Van Name Michelle A. , Camp Anne W. , Magenheimer Elizabeth A. , Li Fangyong , Dziura James D. , Montosa Abmaridel , Patel Anisha , Tamborlane William V. 
Published: February 2016

OBJECTIVE
The Diabetes Prevention Program (DPP) demonstrated that weight loss from intensive lifestyle intervention (ILI) in adults with prediabetes could decrease progression to type 2 diabetes. Inner-city, low-income Hispanic women are at high risk for developing type 2 diabetes; however, this type of intervention is not well established in this group. We hypothesized that a DPP intervention modified for a community health center (CHC) setting would decrease weight and improve metabolic measures in Hispanic women with prediabetes.

RESEARCH DESIGN AND METHODS
Women diagnosed with prediabetes on a screening oral glucose tolerance test were recruited from a CHC. Participants (90% of whom were Hispanic) were randomized to either usual care (age 43 ± 9.7 years, BMI 35.2 ± 7.3 kg/m2) or ILI (age 43.8 ± 10.8 years, BMI 35.4 ± 8.5 kg/m2), structured as 14 weeks of group sessions focused on food choices, behavior change, physical activity, and weight loss. One year after enrollment, 122 women repeated baseline measures.

RESULTS
Groups had similar baseline weight, BMI, and fasting and 2-h glucose. One year later, the ILI group had lost 3.8 kg (4.4%), while the usual care group had gained 1.4 kg (1.6%, P &lt; 0.0001). Two-hour glucose excursion decreased 15 mg/dL (0.85 mmol/L) in the ILI and 1 mg/dL (0.07 mmol/L) in the usual care group (P = 0.03). Significant decreases favoring the ILI group were noted in BMI, percent body fat, waist circumference, and fasting insulin.

CONCLUSIONS
A 14-week ILI program based on the DPP can effectively be translated into a predominantly Hispanic CHC setting, resulting in decreased weight, improved fasting insulin, and smaller glucose excursions 1 year after enrolling in the program.
Standard Information Models for Representing Adverse Sensitivity Information in Clinical Documents
Authors: Seger D. L. , Goss F. , Lai K. , Slight S. P. , Lau J. J. , Nandigam H. , Zhou L. , Topaz M. 
Published: February 2016

SummaryBackground: Adverse sensitivity (e.g., allergy and intolerance) information is a critical component of any electronic health record system. While several standards exist for structured entry of adverse sensitivity information, many clinicians record this data as free text.Objectives: This study aimed to 1) identify and compare the existing common adverse sensitivity information models, and 2) to evaluate the coverage of the adverse sensitivity information models for representing allergy information on a subset of inpatient and outpatient adverse sensitivity clinical notes.Methods: We compared four common adverse sensitivity information models: Health Level 7 Allergy and Intolerance Domain Analysis Model, HL7-DAM; the Fast Health-care Interoperability Resources, FHIR; the Consolidated Continuity of Care Document, C-CDA; and OpenEHR, and evaluated their coverage on a corpus of inpatient and out-patient notes (n = 120).Results: We found that allergy specialists’ notes had the highest frequency of adverse sensitivity attributes per note, whereas emergency department notes had the fewest attributes. Overall, the models had many similarities in the central attributes which covered between 75% and 95% of adverse sensitivity information contained within the notes. However, representations of some attributes (especially the value-sets) were not well aligned between the models, which is likely to present an obstacle for achieving data interoperability. Also, adverse sensitivity exceptions were not well represented among the information models.Conclusions: Although we found that common adverse sensitivity models cover a significant portion of relevant information in the clinical notes, our results highlight areas needed to be reconciled between the stand -ards for data interoperability.
ELECTROMAGNETIC EMISSION FROM LONG-LIVED BINARY NEUTRON STAR MERGER REMNANTS. I. FORMULATION OF THE PROBLEM
Authors: Siegel Daniel M. , Ciolfi Riccardo 
Published: February 2016

ABSTRACT
Binary neutron star (BNS) mergers are the leading model to explain the phenomenology of short gamma-ray bursts (SGRBs). Recent observations of long-lasting X-ray afterglows of SGRBs challenge standard paradigms and indicate that in a large fraction of events a long-lived neutron star (NS) may be formed rather than a black hole. Understanding the mechanisms underlying these afterglows is necessary in order to address the open questions concerning the nature of SGRB central engines. However, recent theoretical progress has been hampered by the fact that the timescales of interest for the afterglow emission are inaccessible to numerical relativity simulations. Here we present a detailed model to bridge the gap between numerical simulations of the merger process and the relevant timescales for the afterglows, assuming that the merger results in a long-lived NS. This model is formulated in terms of a set of coupled differential equations that follow the evolution of the post-merger system and predict its electromagnetic (EM) emission in a self-consistent way, starting from initial data that can be extracted from BNS merger simulations. The model presented here also allows us to search for suitable EM counterparts for multimessenger astronomy, which is expected to become reality within the next few years thanks to ground-based GW detectors such as advanced LIGO and Virgo. This paper discusses the formulation and implementation of the model. In a companion paper, we employ this model to predict the EM emission from

to

after a BNS merger and discuss the implications in the context of SGRBs and multimessenger astronomy.
ON THE TIDAL RADIUS OF SATELLITES ON PROGRADE AND RETROGRADE ORBITS
Authors: Gajda Grzegorz , Łokas Ewa L. 
Published: February 2016

ABSTRACT
A tidal radius is the distance from a satellite orbiting in a host potential beyond which its material is stripped by the tidal force. We derive a revised expression for the tidal radius of a rotating satellite that properly takes into account the possibility of prograde and retrograde orbits of stars. Besides the eccentricity of the satellite orbit, the tidal radius also depends on the ratio of the satellite internal angular velocity to the orbital angular velocity. We compare our formula to the results of two N-body simulations of dwarf galaxies orbiting a Milky-Way-like host on a prograde and retrograde orbit. The tidal radius for the retrograde case is larger than for the prograde. We introduce a kinematic radius that separates stars still orbiting the dwarf galaxy from those already stripped and following the potential of the host galaxy. We find that the tidal radius matches the kinematic radius very well. Our results provide a connection between the formalism of the tidal radius derivation and the theory of resonant stripping.
EVOLUTION OF OH AND CO-DARK MOLECULAR GAS FRACTION ACROSS A MOLECULAR CLOUD BOUNDARY IN TAURUS
Authors: Xu Duo , Li Di , Yue Nannan , Goldsmith Paul F. 
Published: February 2016

ABSTRACT
We present observations of 12CO J = 1-0, 13CO J = 1-0, H i, and all four ground-state transitions of the hydroxyl (OH) radical toward a sharp boundary region of the Taurus molecular cloud. Based on a photodissociation region (PDR) model that reproduces CO and [C i] emission from the same region, we modeled the three OH transitions, 1612, 1665, and 1667 MHz successfully through escape probability non-local thermal equilibrium radiative transfer model calculations. We could not reproduce the 1720 MHz observations, due to unmodeled pumping mechanisms, of which the most likely candidate is a C-shock. The abundance of OH and CO-dark molecular gas is well-constrained. The OH abundance [OH]/[H2] decreases from

to

as A

v
increases from 0.4 to 2.7 mag following an empirical law:

which is higher than PDR model predictions for low-extinction regions by a factor of 80. The overabundance of OH at extinctions at or below 1 mag is likely the result of a C-shock. The dark gas fraction (DGF, defined as the fraction of molecular gas without detectable CO emission) decreases from 80% to 20% following a Gaussian profile:

This trend of the DGF is consistent with our understanding that the DGF drops at low visual extinction due to photodissociation of H2 and drops at high visual extinction due to CO formation. The DGF peaks in the extinction range where H2 has already formed and achieved self-shielding but 12CO has not. Two narrow velocity components with a peak-to-peak spacing of ∼1 km s−1 were clearly identified. Their relative intensity and variation in space and frequency suggest colliding streams or gas flows at the boundary region.
A SURVEY OF LUMINOUS HIGH-REDSHIFT QUASARS WITH SDSS AND WISE. I. TARGET SELECTION AND OPTICAL SPECTROSCOPY
Authors: Wang Feige , Wu Xue-Bing , Fan Xiaohui , Yang Jinyi , Yi Weimin , Bian Fuyan , McGreer Ian D. , Yang Qian , Ai Yanli , Dong Xiaoyi , Zuo Wenwen , Jiang Linhua , Green Richard , Wang Shu , Cai Zheng , Wang Ran , Yue Minghao 
Published: February 2016

ABSTRACT
High-redshift quasars are important tracers of structure and evolution in the early universe. However, they are very rare and difficult to find when using color selection because of contamination from late-type dwarfs. High-redshift quasar surveys based on only optical colors suffer from incompleteness and low identification efficiency, especially at

. We have developed a new method to select

quasars with both high efficiency and completeness by combining optical and mid-IR Wide-field Infrared Survey Explorer (WISE) photometric data, and are conducting a luminous

quasar survey in the whole Sloan Digital Sky Survey (SDSS) footprint. We have spectroscopically observed 99 out of 110 candidates with z-band magnitudes brighter than 19.5, and 64 (64.6%) of them are quasars with redshifts of

and absolute magnitudes of

. In addition, we also observed 14 fainter candidates selected with the same criteria and identified 8 (57.1%) of them as quasars with

. Among 72 newly identified quasars, 12 of them are at

, which leads to an increase of ∼36% of the number of known quasars at this redshift range. More importantly, our identifications doubled the number of quasars with

at

, which will set strong constraints on the bright end of the quasar luminosity function. We also expand our method to select quasars at z ≳ 5.7. In this paper we report the discovery of four new luminous z ≳ 5.7 quasars based on SDSS–WISE selection.
MORPHOLOGICAL PROPERTIES OF Lyα EMITTERS AT REDSHIFT 4.86 IN THE COSMOS FIELD: CLUMPY STAR FORMATION OR MERGER?*
Authors: Kobayashi Masakazu A. R. , Murata Katsuhiro L. , Koekemoer Anton M. , Murayama Takashi , Taniguchi Yoshiaki , Kajisawa Masaru , Shioya Yasuhiro , Scoville Nick Z. , Nagao Tohru , Capak Peter L. 
Published: February 2016

ABSTRACT
We investigate morphological properties of 61 Lyα emitters (LAEs) at z = 4.86 identified in the COSMOS field, based on Hubble Space Telescope Advanced Camera for Surveys (ACS) imaging data in the F814W band. Out of the 61 LAEs, we find the ACS counterparts for 54 LAEs. Eight LAEs show double-component structures with a mean projected separation of 0.″63 (∼4.0 kpc at z = 4.86). Considering the faintness of these ACS sources, we carefully evaluate their morphological properties, that is, size and ellipticity. While some of them are compact and indistinguishable from the point-spread function (PSF) half-light radius of 0.″07 (∼0.45 kpc), the others are clearly larger than the PSF size and spatially extended up to 0.″3 (∼1.9 kpc). We find that the ACS sources show a positive correlation between ellipticity and size and that the ACS sources with large size and round shape are absent. Our Monte Carlo simulation suggests that the correlation can be explained by (1) the deformation effects via PSF broadening and shot noise or (2) the source blending in which two or more sources with small separation are blended in our ACS image and detected as a single elongated source. Therefore, the 46 single-component LAEs could contain the sources that consist of double (or multiple) components with small spatial separation (i.e., ≲0.″3 or 1.9 kpc). Further observation with high angular resolution at longer wavelengths (e.g., rest-frame wavelengths of ≳4000 Å) is inevitable to decipher which interpretation is adequate for our LAE sample.
THE X-RAY ZURICH ENVIRONMENTAL STUDY (X-ZENS). II. X-RAY OBSERVATIONS OF THE DIFFUSE INTRAGROUP MEDIUM IN GALAXY GROUPS
Authors: Miniati Francesco , Finoguenov Alexis , Silverman John D. , Carollo Marcella , Cibinel Anna , Lilly Simon J. , Schawinski Kevin 
Published: February 2016

ABSTRACT
We present the results of a pilot XMM-Newton and Chandra program aimed at studying the diffuse intragroup medium (IGM) of optically selected nearby groups from the Zurich ENvironmental Study (ZENS) catalog. The groups are in a narrow mass range about

, a mass scale at which the interplay between the IGM and the group member galaxies is still largely unprobed. X-ray emission from the IGM is detected in the energy band 0.5–2 keV with flux

erg s−1 cm−2, which is one order of magnitude fainter than for typical ROSAT groups (RASS). For many groups, we set upper limits on the X-ray luminosity, indicating that the detections are likely probing the upper envelope of the X-ray emitting groups. We find that weighting the group halo mass by the fraction of the total stellar mass locked in the bulge galaxy components might reduce the bias of mass estimates based on the total optical luminosity with respect to the X-ray mass estimates, (consistent with Andreon, at larger mass scales). We measure a stellar mass fraction with a median value of about 1%, with a contribution from the most massive galaxies between 30% and 50%. Optical and X-ray data often give complementary answers concerning the dynamical state of the groups, and are essential for a complete picture of the group system. Extending this pilot program to a larger sample of groups is necessary to unveil any imprint of interaction between member galaxies and IGM in halo potentials of key importance for environmentally driven galactic evolution.
DEMONSTRATING HIGH-PRECISION, MULTIBAND TRANSIT PHOTOMETRY WITH MUSCAT: A CASE FOR HAT-P-14B
Authors: Fukui Akihiko , Narita Norio , Kawashima Yui , Kusakabe Nobuhiko , Onitsuka Masahiro , Ryu Tsuguru , Ikoma Masahiro , Yanagisawa Kenshi , Izumiura Hideyuki 
Published: February 2016

ABSTRACT
The Multicolor Simultaneous Camera for studying Atmospheres of Transiting exoplanets (MuSCAT) is an optical three-band (

-,

- and

-band) imager that was recently developed for the 188 cm telescope at Okayama Astrophysical Observatory with the aim of validating and characterizing transiting planets. In a pilot observation with MuSCAT we observed a primary transit of HAT-P-14b, a high-surface gravity (g
p = 38 ms−2) hot Jupiter around a bright (V = 10) F-type star. From a 2.9 hr observation we achieved the five-minute binned photometric precisions of 0.028%, 0.022%, and 0.024% in the

,

, and

bands, respectively, which provided the highest-quality photometric data for this planet. Combining these results with those of previous observations, we search for variations of transit timing and duration over five years as well as variations of planet-star radius ratio (

) with wavelengths, but can find no considerable variation in any parameters. On the other hand, using the transit-subtracted light curves we simulate the achievable measurement error of

with MuSCAT for various planetary sizes, assuming three types of host stars: HAT-P-14, the nearby K-dwarf HAT-P-11, and the nearby M-dwarf GJ1214. Comparing our results with the expected atmospheric scale heights, we find that MuSCAT is capable of probing the atmospheres of planets as small as a sub-Jupiter (

) around HAT-P-14 in all bands, a Neptune (

) around HAT-P-11 in all bands, and a super-Earth (

) around GJ1214 in

and

bands. These results promise that MuSCAT will produce fruitful scientific outcomes in the K2 and TESS era.
THE ANGLO-AUSTRALIAN PLANET SEARCH XXIV: THE FREQUENCY OF JUPITER ANALOGS
Authors: Wittenmyer Robert A. , Butler R. P. , Tinney C. G. , Horner Jonathan , Carter B. D. , Wright D. J. , Jones H. R. A. , Bailey J. , O’Toole Simon J. 
Published: February 2016

ABSTRACT
We present updated simulations of the detectability of Jupiter analogs by the 17-year Anglo-Australian Planet Search. The occurrence rate of Jupiter-like planets that have remained near their formation locations beyond the ice line is a critical datum necessary to constrain the details of planet formation. It is also vital in our quest to fully understand how common (or rare) planetary systems like our own are in the Galaxy. From a sample of 202 solar-type stars, and correcting for imperfect detectability on a star-by-star basis, we derive a frequency of

% for giant planets in orbits from 3 to 7 au. When a consistent definition of “Jupiter analog” is used, our results are in agreement with those from other legacy radial-velocity surveys.
A VERSATILE FAMILY OF GALACTIC WIND MODELS
Authors: Bustard Chad , Zweibel Ellen G. , D’Onghia Elena 
Published: February 2016

ABSTRACT
We present a versatile family of model galactic outflows including non-uniform mass and energy source distributions, a gravitational potential from an extended mass source, and radiative losses. The model easily produces steady-state wind solutions for a range of mass-loading factors, energy-loading factors, galaxy mass, and galaxy radius. We find that, with radiative losses included, highly mass-loaded winds must be driven at high central temperatures, whereas low mass-loaded winds can be driven at low temperatures just above the peak of the cooling curve, meaning radiative losses can drastically affect the wind solution even for low mass-loading factors. By including radiative losses, we are able to show that subsonic flows can be ignored as a possible mechanism for expelling mass and energy from a galaxy compared to the more efficient transonic solutions. Specifically, the transonic solutions with low mass loading and high energy loading are the most efficient. Our model also produces low-temperature, high-velocity winds that could explain the prevalence of low-temperature material in observed outflows. Finally, we show that our model, unlike the well-known Chevalier & Clegg model, can reproduce the observed linear relationship between wind X-ray luminosity and star formation rate (SFR) over a large range of SFR from 1–1000 M
⊙ yr−1 assuming the wind mass-loading factor is higher for low-mass, and hence, low-SFR galaxies. We also constrain the allowed mass-loading factors that can fit the observed X-ray luminosity versus SFR trend, further suggesting an inverse relationship between mass loading and SFR as explored in advanced numerical simulations.