bluuebunny/crossref_metadata_2025_split huggingface dataset:
Treatment of chronic subdural hematomas with subdural evacuating port system placement in the intensive care unit: evolution of practice and comparison with bur hole evacuation in the operating room
Authors: Flint Alexander C. , Chan Sheila L. , Rao Vivek A. , Efron Allen D. , Kalani Maziyar A. , Sheridan William F. 
Published: January 2017

OBJECTIVEThe aims of this study were to evaluate a multiyear experience with subdural evacuating port system (SEPS) placement for chronic subdural hematoma (cSDH) in the intensive care unit at a tertiary neurosurgical center and to compare SEPS placement with bur hole evacuation in the operating room.METHODSAll cases of cSDH evacuation were captured over a 7-year period at a tertiary neurosurgical center within an integrated health care delivery system. The authors compared the performance characteristics of SEPS and bur hole placement with respect to recurrence rates, change in recurrence rates over time, complications, length of stay, discharge disposition, and mortality rates.RESULTSA total of 371 SEPS cases and 659 bur hole cases were performed (n = 1030). The use of bedside SEPS placement for cSDH treatment increased over the 7-year period, from 14% to 80% of cases. Reoperation within 6 months was higher for the SEPS (15.6%) than for bur hole drainage (9.1%) across the full 7-year period (p = 0.002). This observed overall difference was due to a higher rate of reoperation during the same hospitalization (7.0% for SEPS vs 3.2% for bur hole; p = 0.008). Over time, as the SEPS procedure became more common and modifications of the SEPS technique were introduced, the rate of in-hospital reoperation after SEPS decreased to 3.3% (p = 0.02 for trend), and the difference between SEPS and bur hole recurrence was no longer significant (p = 0.70). Complications were uncommon and were similar between the groups.CONCLUSIONSOverall performance characteristics of bedside SEPS and bur hole drainage in the operating room were similar. Modifications to the SEPS technique over time were associated with a reduced reoperation rate.
Anchored phylogenomics improves the resolution of evolutionary relationships in the rapid radiation ofProteaL.
Authors: Mitchell Nora , Lewis Paul O. , Lemmon Emily Moriarty , Lemmon Alan R. , Holsinger Kent E. 
Published: January 2017

PREMISE OF THE STUDY:Estimating phylogenetic relationships in relatively recent evolutionary radiations is challenging, especially if short branches associated with recent divergence result in multiple gene tree histories. We combine anchored enrichment next‐generation sequencing with species tree analyses to produce a robust estimate of phylogenetic relationships in the genusProtea(Proteaceae), an iconic radiation in South Africa.METHODS:We sampled multiple individuals within 59 out of 112 species ofProteaand 6 outgroup species for a total of 163 individuals, and obtained sequences for 498 low‐copy, orthologous nuclear loci using anchored phylogenomics. We compare several approaches for building species trees, and explore gene tree–species tree discrepancies to determine whether poor phylogenetic resolution reflects a lack of informative sites, incomplete lineage sorting, or hybridization.KEY RESULTS:Phylogenetic estimates from species tree approaches are similar to one another and recover previously well‐supported clades withinProtea, in addition to providing well‐supported phylogenetic hypotheses for previously poorly resolved intrageneric relationships. Individual gene trees are markedly different from one another and from species trees. Nonetheless, analyses indicate that differences among gene trees occur primarily concerning clades supported by short branches.CONCLUSIONS:Species tree methods using hundreds of nuclear loci provided strong support for many previously unresolved relationships in the radiation of the genusProtea. In cases where support for particular relationships remains low, these appear to arise from few informative sites and lack of information rather than strongly supported disagreement among gene trees.
Floral function: effects of traits on pollinators, male and female pollination success, and female fitness across three species of milkweeds (Asclepias)
Authors: La Rosa Raffica J. , Conner Jeffrey K. 
Published: January 2017

PREMISE OF THE STUDY:Central questions in plant reproductive ecology are whether the functions of floral traits in hermaphrodites create conflict between sexes that could slow evolution, and whether individual floral traits function in pollinator attraction, efficiency, or both. We studied how floral traits affect pollinator visitation and efficiency, and how they affect male and female function and female fitness within and across three Asclepias species that differ in floral morphology.METHODS:Using separate multiple regressions, we regressed pollen removal, deposition, and fruit number onto six floral traits. We also used path analyses integrating these variables with pollinator visitation data for two of the species to further explore floral function and its effects on fruit production.KEY RESULTS:Most traits affected male pollination success only, and these effects often differed between species. The exception was increased slit length, which increased pollinia insertion in two of the species. There were no interspecific differences in the effects of the traits on female pollination success. All traits except horn reach affected pollination efficiency in at least one species, and horn reach and two hood dimensions were the only traits to affect pollinator attraction, but in just one species.CONCLUSIONS:Traits tended to function in only one sex, and more traits affected function through pollinator efficiency than through attraction. There was no significant link between female pollination success and female fitness in any of the three species; this pattern is consistent with fruit production not being limited by pollen deposition.
DIFFERENT ORIGINS OR DIFFERENT EVOLUTIONS? DECODING THE SPECTRAL DIVERSITY AMONG C-TYPE ASTEROIDS
Authors: Vernazza P. , Castillo-Rogez J. , Beck P. , Emery J. , Brunetto R. , Delbo M. , Marsset M. , Marchis F. , Groussin O. , Zanda B. , Lamy P. , Jorda L. , Mousis O. , Delsanti A. , Djouadi Z. , Dionnet Z. , Borondics F. , Carry B. 
Published: January 2017

ABSTRACT
Anhydrous pyroxene-rich interplanetary dust particles (IDPs) have been proposed as surface analogs for about two-thirds of all C-complex asteroids. However, this suggestion appears to be inconsistent with the presence of hydrated silicates on the surfaces of some of these asteroids, including Ceres. Here, we report the presence of enstatite (pyroxene) on the surface of two C-type asteroids (Ceres and Eugenia) based on their spectral properties in the mid-infrared range. The presence of this component is particularly unexpected in the case of Ceres, because most thermal evolution models predict a surface consisting of hydrated compounds only. The most plausible scenario is that Ceres’ surface has been partially contaminated by exogenous enstatite-rich material, possibly coming from the Beagle asteroid family. This scenario questions a similar origin for Ceres and the remaining C-types, and it possibly supports recent results obtained by the Dawn mission (NASA) that Ceres may have formed in the very outer solar system. Concerning the smaller D ∼ 200 km C-types such as Eugenia, both their derived surface composition (enstatite and amorphous silicates) and low density (<1.5 g cm−3) suggest that these bodies accreted from the same building blocks, namely chondritic porous, pyroxene-rich IDPs and volatiles (mostly water ice), and that a significant volume fraction of these bodies has remained unaffected by hydrothermal activity likely implying a late accretion. In addition, their current heliocentric distance may best explain the presence or absence of water ice at their surfaces. Finally, we raise the possibility that CI chondrites, Tagish-Lake-like material, or hydrated IDPs may be representative samples of the cores of these bodies.
PREPARING FOR ADVANCED LIGO: A STAR–GALAXY SEPARATION CATALOG FOR THE PALOMAR TRANSIENT FACTORY
Authors: Miller A. A. , Kulkarni M. K. , Cao Y. , Laher R. R. , Masci F. J. , Surace J. A. 
Published: January 2017

Abstract
The search for fast optical transients, such as the expected electromagnetic counterparts to binary neutron star mergers, is riddled with false positives (FPs) ranging from asteroids to stellar flares. While moving objects are readily rejected via image pairs separated by ∼1 hr, stellar flares represent a challenging foreground, significantly outnumbering rapidly evolving explosions. Identifying stellar sources close to and fainter than the transient detection limit can eliminate these FPs. Here, we present a method to reliably identify stars in deep co-adds of Palomar Transient Factory (PTF) imaging. Our machine-learning methodology utilizes the random forest (RF) algorithm, which is trained using

sources with Sloan Digital Sky Survey (SDSS) spectra. When evaluated on an independent test set, the PTF RF model outperforms the SExtractor star classifier by ∼4%. For faint sources (

mag), which dominate the field population, the PTF RF model produces a ∼19% improvement over SExtractor. To avoid false negatives in the PTF transient-candidate stream, we adopt a conservative stellar classification threshold, corresponding to a galaxy misclassification rate of 0.005. Ultimately, ∼

objects are included in our PTF point-source catalog, of which only ∼106 are expected to be galaxies. We demonstrate that the PTF RF catalog reveals transients that otherwise would have been missed. To leverage its superior image quality, we additionally create an SDSS point-source catalog, which is also tuned to have a galaxy misclassification rate of 0.005. These catalogs have been incorporated into the PTF real-time pipelines to automatically reject stellar sources as non-extragalactic transients.
THE RADIAL VELOCITY EXPERIMENT (RAVE): FIFTH DATA RELEASE
Authors: Kunder Andrea , Kordopatis Georges , Steinmetz Matthias , Zwitter Tomaž , McMillan Paul J. , Casagrande Luca , Enke Harry , Wojno Jennifer , Valentini Marica , Chiappini Cristina , Matijevič Gal , Siviero Alessandro , de Laverny Patrick , Recio-Blanco Alejandra , Bijaoui Albert , Wyse Rosemary F. G. , Binney James , Grebel E. K. , Helmi Amina , Jofre Paula , Antoja Teresa , Gilmore Gerard , Siebert Arnaud , Famaey Benoit , Bienaymé Olivier , Gibson Brad K. , Freeman Kenneth C. , Navarro Julio F. , Munari Ulisse , Seabroke George , Anguiano Borja , Žerjal Maruša , Minchev Ivan , Reid Warren , Bland-Hawthorn Joss , Kos Janez , Sharma Sanjib , Watson Fred , Parker Quentin A. , Scholz Ralf-Dieter , Burton Donna , Cass Paul , Hartley Malcolm , Fiegert Kristin , Stupar Milorad , Ritter Andreas , Hawkins Keith , Gerhard Ortwin , Chaplin W. J. , Davies G. R. , Elsworth Y. P. , Lund M. N. , Miglio A. , Mosser B. 
Published: January 2017

ABSTRACT
Data Release 5 (DR5) of the Radial Velocity Experiment (RAVE) is the fifth data release from a magnitude-limited (

) survey of stars randomly selected in the Southern Hemisphere. The RAVE medium-resolution spectra (

) covering the Ca-triplet region (8410–8795 Å) span the complete time frame from the start of RAVE observations in 2003 to their completion in 2013. Radial velocities from 520,781 spectra of 457,588 unique stars are presented, of which 255,922 stellar observations have parallaxes and proper motions from the Tycho-Gaia astrometric solution in Gaia DR1. For our main DR5 catalog, stellar parameters (effective temperature, surface gravity, and overall metallicity) are computed using the RAVE DR4 stellar pipeline, but calibrated using recent K2 Campaign 1 seismic gravities and Gaia benchmark stars, as well as results obtained from high-resolution studies. Also included are temperatures from the Infrared Flux Method, and we provide a catalog of red giant stars in the dereddened color

interval (0.50, 0.85) for which the gravities were calibrated based only on seismology. Further data products for subsamples of the RAVE stars include individual abundances for Mg, Al, Si, Ca, Ti, Fe, and Ni, and distances found using isochrones. Each RAVE spectrum is complemented by an error spectrum, which has been used to determine uncertainties on the parameters. The data can be accessed via the RAVE Web site or the VizieR database.
Multiepoch Spectropolarimetry of SN 2011fe
Authors: Milne Peter A. , Williams G. Grant , Porter Amber , Smith Paul S. , Smith Nathan , Leising Mark D. , Jannuzi Buell T. , Green E. M. 
Published: January 2017

Abstract
We present multiple spectropolarimetric observations of the nearby Type Ia supernova (SN) 2011fe in M101, obtained before, during, and after the time of maximum apparent visual brightness. The excellent time coverage of our spectropolarimetry has allowed better monitoring of the evolution of polarization features than is typical, which has allowed us new insight into the nature of normal SNe Ia. SN 2011fe exhibits time-dependent polarization in both the continuum and strong absorption lines. At early epochs, red wavelengths exhibit a degree of continuum polarization of up to 0.4%, likely indicative of a mild asymmetry in the electron-scattering photosphere. This behavior is more common in subluminous SNe Ia than in normal events, such as SN 2011fe. The degree of polarization across a collection of absorption lines varies dramatically from epoch to epoch. During the earliest epoch, a λ4600–5000 Å complex of absorption lines shows enhanced polarization at a different position angle than the continuum. We explore the origin of these features, presenting a few possible interpretations, without arriving at a single favored ion. During two epochs near maximum, the dominant polarization feature is associated with the Si ii
λ6355 Å absorption line. This is common for SNe Ia, but for SN 2011fe the polarization of this feature increases after maximum light, whereas for other SNe Ia, that polarization feature was strongest before maximum light.
ARRIVAL TIME DIFFERENCES BETWEEN GRAVITATIONAL WAVES AND ELECTROMAGNETIC SIGNALS DUE TO GRAVITATIONAL LENSING
Authors: Takahashi Ryuichi 
Published: January 2017

ABSTRACT
In this study we demonstrate that general relativity predicts arrival time differences between gravitational wave (GW) and electromagnetic (EM) signals caused by the wave effects in gravitational lensing. The GW signals can arrive earlier than the EM signals in some cases if the GW/EM signals have passed through a lens, even if both signals were emitted simultaneously by a source. GW wavelengths are much larger than EM wavelengths; therefore, the propagation of the GWs does not follow the laws of geometrical optics, including the Shapiro time delay, if the lens mass is less than approximately 105
M
⊙(f/Hz)−1, where f is the GW frequency. The arrival time difference can reach ∼0.1 s (f/Hz)−1 if the signals have passed by a lens of mass ∼8000 M
⊙(f/Hz)−1 with the impact parameter smaller than the Einstein radius; therefore, it is more prominent for lower GW frequencies. For example, when a distant supermassive black hole binary (SMBHB) in a galactic center is lensed by an intervening galaxy, the time lag becomes of the order of 10 days. Future pulsar timing arrays including the Square Kilometre Array and X-ray detectors may detect several time lags by measuring the orbital phase differences between the GW/EM signals in the SMBHBs. Gravitational lensing imprints a characteristic modulation on a chirp waveform; therefore, we can deduce whether a measured arrival time lag arises from intrinsic source properties or gravitational lensing. Determination of arrival time differences would be extremely useful in multimessenger observations and tests of general relativity.
KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE WITH ALMA
Authors: Saigo Kazuya , Onishi Toshikazu , Nayak Omnarayani , Meixner Margaret , Tokuda Kazuki , Harada Ryohei , Morioka Yuuki , Sewiło Marta , Indebetouw Remy , Torii Kazufumi , Kawamura Akiko , Ohama Akio , Hattori Yusuke , Yamamoto Hiroaki , Tachihara Kengo , Minamidani Tetsuhiro , Inoue Tsuyoshi , Madden Suzanne , Galametz Maud , Lebouteiller Vianney , Chen C.-H. Rosie , Mizuno Norikazu , Fukui Yasuo 
Published: January 2017

ABSTRACT
We present the ALMA Band 3 and Band 6 results of 12CO(2-1), 13CO(2-1), H30α recombination line, free–free emission around 98 GHz, and the dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active high-mass star-forming face-on galaxy at a distance of 50 kpc and is the best target for studing high-mass star formation. ALMA observations show that N159E is the complex of filamentary clouds with the width and length of ∼1 pc and several parsecs. The total molecular mass is 0.92 × 105
M
⊙ from the 13CO(2-1) intensity. N159E harbors the well-known Papillon Nebula, a compact high-excitation H ii region. We found that a YSO associated with the Papillon Nebula has the mass of 35 M
⊙ and is located at the intersection of three filamentary clouds. It indicates that the formation of the high-mass YSO was induced by the collision of filamentary clouds. Fukui et al. reported a similar kinematic structure toward two YSOs in the N159 West region, which are the other YSOs that have the mass of ≳35 M
⊙. This suggests that the collision of filamentary clouds is a primary mechanism of high-mass star formation. We found a small molecular hole around the YSO in Papillon Nebula with a sub-parsec scale. It is filled by free–free and H30α emission. The temperature of the molecular gas around the hole reaches ∼80 K. It indicates that this YSO has just started the distruction of parental molecular cloud.
THE ROLE OF PEBBLE FRAGMENTATION IN PLANETESIMAL FORMATION. II. NUMERICAL SIMULATIONS
Authors: Jansson Karl Wahlberg , Johansen Anders , Syed Mohtashim Bukhari , Blum Jürgen 
Published: January 2017

ABSTRACT
Some scenarios for planetesimal formation go through a phase of collapse of gravitationally bound clouds of millimeter- to centimeter-size pebbles. Such clouds can form, for example, through the streaming instability in protoplanetary disks. We model the collapse process with a statistical model to obtain the internal structure of planetesimals with solid radii between 10 and 1000 km. During the collapse, pebbles collide, and depending on their relative speeds, collisions have different outcomes. A mixture of particle sizes inside a planetesimal leads to better packing capabilities and higher densities. In this paper we apply results from new laboratory experiments of dust aggregate collisions (presented in a companion paper) to model collision outcomes. We find that the internal structure of a planetesimal is strongly dependent on both its mass and the applied fragmentation model. Low-mass planetesimals have no/few fragmenting pebble collisions in the collapse phase and end up as porous pebble piles. The number of fragmenting collisions increases with increasing cloud mass, resulting in wider particle size distributions and higher density. The collapse is nevertheless “cold” in the sense that collision speeds are damped by the high collision frequency. This ensures that a significant fraction of large pebbles survive the collapse in all but the most massive clouds. Our results are in broad agreement with the observed increase in density of Kuiper Belt objects with increasing size, as exemplified by the recent characterization of the highly porous comet 67P/Churyumov–Gerasimenko.
DUST IN CLUSTERS: SEPARATING THE CONTRIBUTION OF GALAXIES AND INTRACLUSTER MEDIA
Authors: Gutiérrez C. M. , López-Corredoira M. 
Published: January 2017

ABSTRACT
We have analyzed a sample of 327 clusters of galaxies, spanning the range of 0.06–0.70 in redshift. Strong constraints on their mean intracluster emission of dust have been obtained using maps and catalogs from the Herschel MerMES project; within a radius of 5 arcmin centered in each cluster, the 95% C.L. limits obtained are 86.6, 48.2, and 30.9 mJy at the observed frequencies of 250, 350, and 500 μm. From these restrictions, and assuming physical parameters typical of interstellar media in the Milky Way, we have obtained tight upper limits on the visual extinction of background galaxies due to the intracluster media (ICM): A

V
(95% C.L.) ≲ 10−3 mag. Strong constraints are also obtained for the mass of such dust; for instance, using the data at 350 μm we establish a 95% upper limit of <109
M
⊙ within a circle with a radius of 5 arcmin centered in the clusters. This corresponds to a fraction of the total mass of the clusters of 9.5 × 10−6, and indicates a deficiency in the gas-to-dust ratio in the ICM by about three orders of magnitude in relation to the value found in the Milky Way. Computing the total infrared luminosity of the clusters in three ranges of redshift (0.05–0.24, 0.24–0.42, and 0.42–0.71) and two ranges of mass (<1014 and >1014
M
⊙), respectively, a strong evolution of luminosity in redshift (L ∼ z
1.5) for both ranges of masses is found. The results indicate a strong declining in star formation rate with time in the last ∼6 Gyr.
GEMINGA’S PUZZLING PULSAR WIND NEBULA
Authors: Posselt B. , Pavlov G. G. , Slane P. O. , Romani R. , Bucciantini N. , Bykov A. M. , Kargaltsev O. , Weisskopf M. C. , Ng C.-Y. 
Published: January 2017

ABSTRACT
We report on six new Chandra observations of the Geminga pulsar wind nebula (PWN). The PWN consists of three distinct elongated structures—two

≈
0.2

d

250

pc long lateral tails and a segmented axial tail of

≈
0.05

d

250

pc length, where

d

250

=
d

/

(
250

pc
)

. The photon indices of the power-law spectra of the lateral tails,

Γ
≈
1

, are significantly harder than those of the pulsar (

Γ
≈
1.5

) and the axial tail (

Γ
≈
1.6

). There is no significant diffuse X-ray emission between the lateral tails—the ratio of the X-ray surface brightness between the south tail and this sky area is at least 12. The lateral tails apparently connect directly to the pulsar and show indications of moving footpoints. The axial tail comprises time-variable emission blobs. However, there is no evidence for constant or decelerated outward motion of these blobs. Different physical models are consistent with the observed morphology and spectra of the Geminga PWN. In one scenario, the lateral tails could represent an azimuthally asymmetric shell whose hard emission is caused by the Fermi acceleration mechanism of colliding winds. In another scenario, the lateral tails could be luminous, bent polar outflows, while the blobs in the axial tail could represent a crushed torus. In a resemblance to planetary magnetotails, the blobs of the axial tail might also represent short-lived plasmoids, which are formed by magnetic field reconnection in the relativistic plasma of the pulsar wind tail.
BURST AND OUTBURST CHARACTERISTICS OF MAGNETAR 4U 0142+61
Authors: Göğüş Ersin , Lin Lin , Roberts Oliver J. , Chakraborty Manoneeta , Kaneko Yuki , Gill Ramandeep , Granot Jonathan , Horst Alexander J. van der , Watts Anna L. , Baring Matthew , Kouveliotou Chryssa , Huppenkothen Daniela , Younes George 
Published: January 2017

ABSTRACT
We have compiled the most comprehensive burst sample from magnetar 4U 0142+61, comprising 27 bursts from its three burst-active episodes in 2011, 2012 and the latest one in 2015 observed with Swift/Burst Alert Telescope and Fermi/Gamma-ray Burst Monitor. Bursts from 4U 0142+61 morphologically resemble typical short bursts from other magnetars. However, 4U 0142+61 bursts are less energetic compared to the bulk of magnetar bursts. We uncovered an extended tail emission following a burst on 2015 February 28, with a thermal nature, cooling over a timescale of several minutes. During this tail emission, we also uncovered pulse peak phase aligned X-ray bursts, which could originate from the same underlying mechanism as that of the extended burst tail, or an associated and spatially coincident but different mechanism.