bluuebunny/crossref_metadata_2025_split huggingface dataset:
PRIMUS: ONE- AND TWO-HALO GALACTIC CONFORMITY AT 0.2 < z < 1
Authors: Berti Angela M. , Coil Alison L. , Behroozi Peter S. , Eisenstein Daniel J. , Bray Aaron D. , Cool Richard J. , Moustakas John 
Published: January 2017

ABSTRACT
We test for galactic conformity at

to a projected distance of 5 Mpc using spectroscopic redshifts from the PRism MUlti-object Survey (PRIMUS). Our sample consists of ∼60,000 galaxies in five separate fields covering a total of ∼5.5 square degrees, which allows us to account for cosmic variance. We identify star-forming and quiescent “isolated primary” (i.e., central) galaxies using isolation criteria and cuts in specific star formation rate. We match the redshift and stellar mass distributions of these samples to control for correlations between quiescent fraction and redshift and stellar mass. We detect a significant (>3σ) one-halo conformity signal, or an excess of star-forming neighbors around star-forming central galaxies, of ∼5% on scales of 0–1 Mpc and a 2.5σ two-halo signal of ∼1% on scales of 1–3 Mpc. These signals are weaker than those detected in the Sloan Digital Sky Survey and are consistent with galactic conformity being the result of large-scale tidal fields and reflecting assembly bias. We also measure the star-forming fraction of central galaxies at fixed stellar mass as a function of large-scale environment and find that central galaxies are more likely to be quenched in overdense environments, independent of stellar mass. However, we find that environment does not affect the star formation efficiency of central galaxies, as long as they are forming stars. We test for redshift and stellar mass dependence of the conformity signal within our sample and show that large volumes and multiple fields are required at intermediate redshift to adequately account for cosmic variance.
NEW EVIDENCE FOR CHARGE-SIGN-DEPENDENT MODULATION DURING THE SOLAR MINIMUM OF 2006 TO 2009
Authors: Di Felice V. , Munini R. , Vos E. E. , Potgieter M. S. 
Published: January 2017

ABSTRACT
The PAMELA space experiment, in orbit since 2006, has measured cosmic rays (CRs) through the most recent period of minimum solar activity with the magnetic field polarity as A < 0. During this entire time, galactic electrons and protons have been detected down to 70 MV and 400 MV, respectively, and their differential variation in intensity with time has been monitored with unprecedented accuracy. These observations are used to show how differently electrons and protons responded to the quiet modulation conditions that prevailed from 2006 to 2009. It is well known that particle drifts, as one of four major mechanisms for the solar modulation of CRs, cause charge-sign-dependent solar modulation. Periods of minimum solar activity provide optimal conditions in which to study these drift effects. The observed behavior is compared to the solutions of a three-dimensional model for CRs in the heliosphere, including drifts. The numerical results confirm that the difference in the evolution of electron and proton spectra during the last prolonged solar minimum is attributed to a large extent to particle drifts. We therefore present new evidence of charge-sign-dependent solar modulation, with a perspective on its peculiarities for the observed period from 2006 to 2009.
LAMOST OBSERVATIONS OF FLARING M DWARFS IN THE KEPLER FIELD
Authors: Chang H.-Y. , Song Y.-H. , Luo A.-L. , Huang L.-C. , Ip W.-H. , Fu J.-N. , Zhang Y. , Hou Y.-H. , Cao Z.-H. , Wang Y.-F. 
Published: January 2017

ABSTRACT
A sample of the Large Sky Area Multi-Object Fibre Spectroscopic Telescope spectra of early-type M0–M3 dwarfs is compared with Kepler observations. It is found that M dwarfs with strong chromospheric emission in

have large flare activity in general. The rotational periods derived from the Kepler measurements have close correlations with the sizes of the flares, the power-law distribution index, and the equivalent widths of the

emission. A clear trend exists for higher magnetic activities being detected in faster-rotating M dwarfs (rotation periods < 20 days).
DIFFERENTIALLY ROTATING WHITE DWARFS. I. REGIMES OF INTERNAL ROTATION
Authors: Ghosh Pranab , Wheeler J. Craig 
Published: January 2017

ABSTRACT
Most viable models of Type Ia supernovae (SNe Ia) require the thermonuclear explosion of a carbon/oxygen white dwarf that has evolved in a binary system. Rotation could be an important aspect of any model for SNe Ia, whether single or double degenerate, with the white dwarf mass at, below, or above the Chandrasekhar limit. Differential rotation is specifically invoked in attempts to account for the apparent excess mass in the super-Chandrasekhar events. Some earlier work has suggested that only uniform rotation is consistent with the expected mechanisms of angular momentum transport in white dwarfs, while others have found pronounced differential rotation. We show that if the baroclinic instability is active in degenerate matter and the effects of magnetic fields are neglected, both nearly uniform rotation and strongly differential rotation are possible. We classify rotation regimes in terms of the Richardson number, Ri. At small values of Ri

0.1, we find both the low-viscosity Zahn regime with a nonmonotonic angular velocity profile and a new differential rotation regime for which the viscosity is high and scales linearly with the shear, σ. Employment of Kelvin–Helmholtz viscosity alone yields differential rotation. Large values of Ri ≫ 1 produce a regime of nearly uniform rotation for which the baroclinic viscosity is of intermediate value and scales as

. We discuss the gap in understanding of the behavior at intermediate values of Ri and how observations may constrain the rotation regimes attained by nature.
ERRATUM: “UNDERSTANDING THE EFFECTS OF STELLAR MULTIPLICITY ON THE DERIVED PLANET RADII FROM TRANSIT SURVEYS: IMPLICATIONS FOR KEPLER, K2, AND TESS” (2015, ApJ, 805, 16)
Authors: Ciardi David R. , Beichman Charles A. , Horch Elliott P. , Howell Steve B. 
Published: January 2017

ABSTRACT
There was an error in the published version of Equation (6); the equation should read as

The calculations and results presented in the paper utilized the correct form of the equation and are unaffected by the error in the equation. The authors sincerely regret the error.
BRIGHT TIMES FOR AN ANCIENT STAR
Authors: Fuhrmann K. , Chini R. 
Published: January 2017

ABSTRACT
Field stars of Population II are among the oldest sources in the Galaxy. Most of their solar-type dwarfs are non-single and, given their extreme age, a significant fraction is accompanied by stellar remnants. Here we report the discovery of the bright F7V star 49 Lib as a massive and very metal-rich Population II field blue straggler, along with evidence for a white dwarf as its dark and unseen companion. 49 Lib is known as a relatively fast-rotating, single-lined spectroscopic binary in a 3 year orbit and with an apparent age of about τ ≃ 2.3 Gyr. Its chemistry and kinematics, however, both consistently imply that 49 Lib must be an ancient Population II star at τ ≃ 12 Gyr. With reference to the inclination from the astrometric orbit, leading to a

M
⊙ low-mass white dwarf, and in view of the

M
⊙ massive, evolved F-type blue straggler star, we demonstrate that 49 Lib must have been the subject of a mostly conservative mass transfer with a near-equal-mass M ≃ 1.06 + 1.00 M
⊙ G-type binary at birth. For its future evolution, we point to the possibility as a progenitor system toward a type Ia supernova. Most importantly, however, we note that the remarkable metal enrichment of 49 Lib at [Mg/H] = +0.23 and [Fe/H] = −0.11 has principally very relevant implications for the early epoch when the Milky Way came into being.
PLANETARY ENGULFMENT AS A TRIGGER FOR WHITE DWARF POLLUTION
Authors: Petrovich Cristobal , Muñoz Diego J. 
Published: January 2017

ABSTRACT
The presence of a planetary system can shield a planetesimal disk from the secular gravitational perturbations due to distant outer massive objects (planets or stellar companions). As the host star evolves off the main sequence to become a white dwarf, these planets can be engulfed during the giant phase, triggering secular instabilities and leading to the tidal disruptions of small rocky bodies. These disrupted bodies can feed the white dwarfs with rocky material and possibly explain the high-metallicity material in their atmospheres. We illustrate how this mechanism can operate when the gravitational perturbations are due to the KL mechanism from a stellar binary companion, a process that is activated only after the planet has been removed/engulfed. We show that this mechanism can explain the observed accretion rates if: (1) the planetary engulfment happens rapidly compared to the secular timescale, which is generally the case for wide binaries (

au) and planetary engulfment during the asymptotic giant branch; (2) the planetesimal disk has a total mass of

. We show that this new mechanism can provide a steady supply of material throughout the entire life of the white dwarfs for all cooling ages and can account for a large fraction (up to nearly half) of the observed polluted white dwarfs.
MASSIVE STAR FORMATION IN THE LMC. I. N159 AND N160 COMPLEXES
Authors: Gordon Michael S. , Jones Terry J. , Gehrz Robert D. , Helton L. Andrew 
Published: January 2017

ABSTRACT
We present images and spectral energy distributions (SEDs) of massive young stellar objects (YSOs) in three star-forming H ii regions of the Large Magellanic Cloud: N159A, N159 Papillon, and N160. We use photometry from SOFIA/FORCAST at 25.3–37.1 μm to constrain model fits to the SEDs and determine luminosities, ages, and dust content of the embedded YSOs and their local environments. By placing these sources on mid-infrared color–magnitude and color–color diagrams, we analyze their dust properties and consider their evolutionary status. Since each object in the FORCAST images has an obvious bright near-infrared counterpart in Spitzer Space Telescope images, we do not find any evidence for new, very cool, previously undiscovered Class 0 YSOs. Additionally, based on its mid-infrared colors and model parameters, N159A is younger than N160 and the Papillon. The nature of the first extragalactic protostars in N159, P1, and P2, is also discussed.
THE EFFECT OF VARIABILITY ON X-RAY BINARY LUMINOSITY FUNCTIONS: MULTIPLE-EPOCH OBSERVATIONS OF NGC 300 WITH CHANDRA
Authors: Binder B. , Gross J. , Williams B. F. , Eracleous M. , Gaetz T. J. , Plucinsky P. P. , Skillman E. D. 
Published: January 2017

ABSTRACT
We have obtained three epochs of Chandra ACIS-I observations (totaling ∼184 ks) of the nearby spiral galaxy NGC 300 to study the logN–logS distributions of its X-ray point-source population down to ∼2 × 10−15 erg s−1 cm−2 in the 0.35–8 keV band (equivalent to ∼1036 erg s−1). The individual epoch logN–logS distributions are best described as the sum of a background active galactic nucleus (AGN) component, a simple power law, and a broken power law, with the shape of the logN–logS distributions sometimes varying between observations. The simple power law and AGN components produce a good fit for “persistent” sources (i.e., with fluxes that remain constant within a factor of ∼2). The differential power-law index of ∼1.2 and high fluxes suggest that the persistent sources intrinsic to NGC 300 are dominated by Roche-lobe-overflowing low-mass X-ray binaries. The variable X-ray sources are described by a broken power law, with a faint-end power-law index of ∼1.7, a bright-end index of ∼2.8–4.9, and a break flux of

erg s−1 cm−2 (∼4 × 1036 erg s−1), suggesting that they are mostly outbursting, wind-fed high-mass X-ray binaries, although the logN–logS distribution of variable sources likely also contains low-mass X-ray binaries. We generate model logN–logS distributions for synthetic X-ray binaries and constrain the distribution of maximum X-ray fluxes attained during outburst. Our observations suggest that the majority of outbursting X-ray binaries occur at sub-Eddington luminosities, where mass transfer likely occurs through direct wind accretion at ∼1%–3% of the Eddington rate.
The Repeating Fast Radio Burst FRB 121102 as Seen on Milliarcsecond Angular Scales
Authors: Marcote B. , Paragi Z. , Hessels J. W. T. , Keimpema A. , Langevelde H. J. van , Huang Y. , Bassa C. G. , Bogdanov S. , Bower G. C. , Burke-Spolaor S. , Butler B. J. , Campbell R. M. , Chatterjee S. , Cordes J. M. , Demorest P. , Garrett M. A. , Ghosh T. , Kaspi V. M. , Law C. J. , Lazio T. J. W. , McLaughlin M. A. , Ransom S. M. , Salter C. J. , Scholz P. , Seymour A. , Siemion A. , Spitler L. G. , Tendulkar S. P. , Wharton R. S. 
Published: January 2017

Abstract
The millisecond-duration radio flashes known as fast radio bursts (FRBs) represent an enigmatic astrophysical phenomenon. Recently, the sub-arcsecond localization (∼100 mas precision) of FRB 121102 using the Very Large Array has led to its unambiguous association with persistent radio and optical counterparts, and to the identification of its host galaxy. However, an even more precise localization is needed in order to probe the direct physical relationship between the millisecond bursts themselves and the associated persistent emission. Here, we report very-long-baseline radio interferometric observations using the European VLBI Network and the 305 m Arecibo telescope, which simultaneously detect both the bursts and the persistent radio emission at milliarcsecond angular scales and show that they are co-located to within a projected linear separation of ≲40 pc (≲12 mas angular separation, at 95% confidence). We detect consistent angular broadening of the bursts and persistent radio source (∼2–4 mas at 1.7 GHz), which are both similar to the expected Milky Way scattering contribution. The persistent radio source has a projected size constrained to be ≲ 0.7 pc (≲0.2 mas angular extent at 5.0 GHz) and a lower limit for the brightness temperature of

T

b

≳
5
×

10

7

K

. Together, these observations provide strong evidence for a direct physical link between FRB 121102 and the compact persistent radio source. We argue that a burst source associated with a low-luminosity active galactic nucleus or a young neutron star energizing a supernova remnant are the two scenarios for FRB 121102 that best match the observed data.
Les citations des dirigeants dans les communiqués de presse diffusés lors d’OPA/OPE : Une analyse lexicale
Authors: Nègre Emmanuelle 
Published: January 2017

La présente recherche s’intéresse aux citations de dirigeants présentes dans les communiqués de presse diffusés dans le contexte particulier des OPA/OPE. Plus précisément, 35 offres publiques d’acquisitions visées par l’AMF entre décembre 2006 et juin 2011 ont été étudiées et une analyse lexicale de 95 citations a été effectuée. Les résultats révèlent l’utilisation, par les dirigeants, d’un discours non standardisé axé sur les conséquences des opérations. Ces discours semblent varier selon le type d’offre (amical ou hostile ; volontaire ou obligatoire) ainsi que selon le type de porte-parole (dirigeant de la cible et/ou de l’acquéreuse). Une discussion est aussi opérée autour du public visé par ces discours.
3D LASER SCANNING FOR PRESERVATION AND STRUCTURAL MONITORING OF HISTORIC CALIFORNIA ADOBE MISSIONS
Authors: Böttger H. M. , Arce Bazán C. J. , Saarman N. P. 
Published: January 2017

INTRODUCTION At the University of San Francisco Architecture & Community Design Program, the Architectural Engineering curriculum utilizes a Leica ScanStation C10 3D Laser Scanner to document historic structures and monitor their structural behavior. Some of the oldest structures in the State of California are the historic adobe missions built by Native Americans and Spanish Catholic missionaries between 1769 and 1833. California is a region of very high seismic activity, and the adobe structures have withstood significant earthquakes and other erosive or destructive forces over their lifetime. However, they are sensitive structures in need of active preservation and very few original adobe buildings remain. Working together with local structural engineers who specialize in seismic restoration of historic adobe structures, USF students have conducted laser scanning at Mission Santa Cruz and Mission San Miguel Arcángel, creating extensive 3D point cloud records, and developing architectural drawings which establish the current state of these structures for the purposes of historic preservation and structural study. Because of the delicate and irregular nature of these structures, the 3D laser scanner is the most appropriate tool for detailed yet non-invasive documentation. Completed in 1821, Mission San Miguel Arcángel suffered significant damage in the nearby 2003 San Simeon earthquake. The original adobe structure has undergone partial repairs such as banding at the top of the walls of the Sacristy. Using the 3D laser scanner, thorough scans are stitched together to create full interior and exterior 3D point cloud files, which are processed in Leica Cyclone and Autodesk Recap, and then imported into AutoCAD to create detailed line drawings of plans, elevations and sections of significant areas. Wall lean and other indicators of crack progress and deterioration are areas of special focus. With these records, a structural monitoring program has begun to document the condition of the buildings in wet seasons and dry seasons, and to determine the long-term effect of seismic restorations which have been implemented. This paper presents a detailed account of the process, pedagogical value and structural and architectural lessons learned over the course of the 3D scanning of these valuable heritage landmarks.
PERFORMANCE OF SUSTAINABLE BUILDINGS IN COLDER CLIMATES
Authors: Gorgolewski Mark , Brown Craig , Chu Anne-Mareike , Turcato Adrian , Bartlett Karen , Ebrahimi Ghazal , Hodgson Murray , Mallory-Hill Shauna , Ouf Mohamed , Scannell Leila 
Published: January 2017

Building performance evaluations (BPEs) were carried out for nine Canadian green buildings using a standardised assessment framework. The aim was to explore and measure the discrepancies between the operational performance of the buildings and their predicted performance, as well as to identify lessons for their owners, design teams and the construction industry. The objective of this paper is not to report individual buildings in detail (we refer the reader to the individual building reports) but to report on some general lessons that came from doing this study. Overall these buildings performed well compared to benchmarks. However, the findings suggest that occupancy is not well understood and often incorrectly predicted during design, and that this affects various aspects of performance, including energy and water use. Also energy and water use modelling is often undertaken principally for building code/green rating compliance purposes and does not necessarily represent an accurate prediction of likely operational use. Combined with variations in occupancy this can lead to considerable discrepancies in performance from the modelled values. This may be understood by experts but is often misleading to building owners and others. Water use is often not well predicted and also not carefully managed in buildings and there is a lack of understanding of what constitutes good water performance. Overall, it is important to recognise that each building has its own individual “story” that provides necessary context for effective management and improvement of the building during its ongoing life. It is proposed that a BPE process allows that context to be better understood, and enables more effective decision making about building management, improvements, occupant satisfaction, energy use, etc.
OFF-GRID TINY HOUSE SMART RESIDENTIAL ENERGY MANAGEMENT SYSTEM
Authors: Alexander David G. 
Published: January 2017

INTRODUCTION Students at California State University (CSU), Chico designed, built, and tested an off-grid solar powered tiny house and competed in the 2016 Sacramento Municipal Utility District's (SMUD) Tiny House Competition. Top tier research institutions, predominantly undergraduate universities, and community colleges from all over California competed against one another in a variety of performance and aesthetic events in SMUD's first ever competition. One of the main goals of the CSU, Chico's Tiny House was to design and implement an autonomous energy management system to maximize energy capture, use, and efficiency and provide a seamless, comfortable, and uninterrupted indoor living environment. This system, smart residential energy management system (SREMS), was designed to monitor and sense solar energy collected and stored, indoor heating and cooling loads, occupant cooking and personal water heating needs, and electrical outlets and to determine and allow energy related activities given the amount of stored energy. Thermodynamic and heat transfer models were developed to predict heating, cooling, and appliance requirements. These models were used to size the solar array, battery storage, and appliances. SREMS was installed in the tiny house and its performance was tested and validated during the week long SMUD Tiny House competition. Results showed close correlation with the predicted energy requirements of the models, and the tiny house maintained net-zero energy use even during overcast and rainy skies throughout the three-day event. The CSU, Chico team won best control system and best technology at the statewide event. This paper describes the design, installation and testing results of CSU, Chico's Tiny House SREMS.
Impact of hospital and sociodemographic factors on utilization of drug-eluting stents in 2011-2012 Medicare cohort
Authors: Tuliani Tushar A , Shenoy Maithili , Parikh Milind , Cohen Mauricio G , Grines Cindy , Jutzy Kenneth , Hilliard Anthony 
Published: January 2017

Abstract
Objective: Insurance status is a predictor of drug-eluting stent (DES) usage. Our study sought to determine the effect of hospital and sociodemographic characteristics on utilization of DES in nationwide inpatient discharges with uniform insurance (Medicare). Methods: We linked data from the 2011 to 2012 Medicare discharges, 2011 Medicare hospital referral region (HRR) report (racial composition of each HRR), American Hospital Association (number of beds, rural/urban location, public/private status, and academic affiliation of hospitals), and American Community Survey 2011 (median income using zip code). We analyzed diagnosis-related group (DRG) codes 249 (bare metal stent without complications), 246, and 247 (DES with and without complications, respectively). Univariate and multivariable logistic regression was conducted to determine odds ratios (OR) for utilization of DES. Results: There were 322,002 discharges with DRG codes 246 (54,279), 247 (209,365), and 249 (58,358) in our database. Higher odds of DES usage was observed in Hispanic dominant HRR(s) (OR: 1.37, 95% confidence interval [CI]: 1.33-1.42, P < 0.001) compared to Caucasian dominant HRR(s). DES utilization was similar in African-American and Caucasian dominant HRR (s). Higher odds of DES use was observed in median household income groups ≥$20,001 (OR: 1.07, 95% CI: 1.01-1.13, P - 0.03). Lower DES usage was observed in hospitals with higher total stent volume (quartile 4 vs. quartile 1: OR: 0.66, 95% CI: 0.63-0.69, P < 0.001) and for-profit hospitals (OR: 0.88, 95% CI: 0.85-0.92, P < 0.001). Conclusions: Our study findings suggest that there are significant differences in DES utilization in a national cohort of individuals with uniform insurance.