bluuebunny/crossref_metadata_2025_split huggingface dataset:
KEPLER-108: A MUTUALLY INCLINED GIANT PLANET SYSTEM
Authors: Mills Sean M. , Fabrycky Daniel C. 
Published: January 2017

ABSTRACTThe vast majority of well studied giant-planet systems, including the solar system, are nearly coplanar, which implies dissipation within a primordial gas disk. However, intrinsic instability may lead to planet–planet scattering, which often produces non-coplanar, eccentric orbits. Planet scattering theories have been developed to explain observed high-eccentricity systems and also hot Jupiters; thus far their predictions for mutual inclination (I) have barely been tested. Here we characterize a highly mutually inclined (°), moderately eccentric () giant planet system: Kepler-108. This system consists of two approximately Saturn-mass planets with periods of approximately 49 and 190 days around a star with a wide (∼300 au) binary companion in an orbital configuration inconsistent with a purely disk migration origin.
THE NEXT GENERATION VIRGO CLUSTER SURVEY. XXII. SHELL FEATURE EARLY-TYPE DWARF GALAXIES IN THE VIRGO CLUSTER*
Authors: Paudel Sanjaya , Smith Rory , Duc Pierre-Alain , Côté Patrick , Cuillandre Jean-Charles , Ferrarese Laura , Blakeslee John P. , Boselli Alessandro , Cantiello Michele , Gwyn S. D. J. , Guhathakurta Puragra , Mei Simona , Mihos J. Christopher , Peng Eric W. , Powalka Mathieu , Sánchez-Janssen Rúben , Toloba Elisa , Zhang Hongxin 
Published: January 2017

ABSTRACT
The Next Generation Virgo Cluster Survey is a deep (with a 2σ detection limit μ

g
= 29 mag arcsec−2 in the g-band) optical panchromatic survey targeting the Virgo cluster from its core to virial radius, for a total areal coverage of 104 square degrees. As such, the survey is well suited for the study of galaxies’ outskirts, haloes, and low surface brightness features that arise from dynamical interactions within the cluster environment. We report the discovery of extremely faint (μ

g
> 25 mag arcsec−2) shells in three Virgo cluster early-type dwarf galaxies: VCC 1361, VCC 1447, and VCC 1668. Among them, VCC 1447 has an absolute magnitude M

g
= −11.71 mag and is the least massive galaxy with a shell system discovered to date. We present a detailed study of these low surface brightness features. We detect between three and four shells in each of our galaxies. Within the uncertainties, we find no evidence of a color difference between the galaxy main body and shell features. The observed arcs of the shells are located up to several effective radii of the galaxies. We further explore the origin of these low surface brightness features with the help of idealized numerical simulations. We find that a near equal mass merger is best able to reproduce the main properties of the shells, including their quite symmetric appearance and their alignment along the major axis of the galaxy. The simulations provide support for a formation scenario in which a recent merger, between two near-equal mass, gas-free dwarf galaxies, forms the observed shell systems.
BINARY BLACK HOLES IN DENSE STAR CLUSTERS: EXPLORING THE THEORETICAL UNCERTAINTIES
Authors: Chatterjee Sourav , Rodriguez Carl L. , Rasio Frederic A. 
Published: January 2017

ABSTRACT
Recent N-body simulations predict that large numbers of stellar black holes (BHs) could at present remain bound to globular clusters (GCs), and merging BH–BH binaries are produced dynamically in significant numbers. We systematically vary “standard” assumptions made by numerical simulations related to, e.g., BH formation, stellar winds, binary properties of high-mass stars, and IMF within existing uncertainties, and study the effects on the evolution of the structural properties of GCs, and the BHs in GCs. We find that variations in initial assumptions can set otherwise identical initial clusters on completely different evolutionary paths, significantly affecting their present observable properties, or even affecting the cluster’s very survival to the present. However, these changes usually do not affect the numbers or properties of local BH–BH mergers. The only exception is that variations in the assumed winds and IMF can change the masses and numbers of local BH–BH mergers, respectively. All other variations (e.g., in initial binary properties and binary fraction) leave the masses and numbers of locally merging BH–BH binaries largely unchanged. This is in contrast to binary population synthesis models for the field, where results are very sensitive to many uncertain parameters in the initial binary properties and binary stellar-evolution physics. Weak winds are required for producing GW150914-like mergers from GCs at low redshifts. LVT151012 can be produced in GCs modeled both with strong and weak winds. GW151226 is lower-mass than typical mergers from GCs modeled with weak winds, but is similar to mergers from GCs modeled with strong winds.
THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. XVII. EXAMINING OBSCURED STAR FORMATION WITH SYNTHETIC ULTRAVIOLET FLUX MAPS IN M31*
Authors: Lewis Alexia R. , Simones Jacob E. , Johnson Benjamin D. , Dalcanton Julianne J. , Skillman Evan D. , Weisz Daniel R. , Dolphin Andrew E. , Williams Benjamin F. , Bell Eric F. , Fouesneau Morgan , Kapala Maria , Rosenfield Philip , Schruba Andreas 
Published: January 2017

ABSTRACT
We present synthetic far- and near-ultraviolet (

FUV

and

NUV

) maps of M31, both with and without dust reddening. These maps were constructed from spatially resolved star formation histories (SFHs) derived from optical Hubble Space Telescope imaging of resolved stars, taken as part of the Panchromatic Hubble Andromeda Treasury program. We use stellar population synthesis modeling to generate synthetic UV maps with a spatial resolution of ∼100 pc (∼24 arcsec), projected. When reddening is included, these maps reproduce all of the main morphological features in the GALEX imaging, including rings and large star-forming complexes. The predicted UV flux also agrees well with the observed flux, with median ratios between the modeled and observed flux of

log

10

(

f

FUV

syn

/

f

FUV

obs

)
=
0.03
±
0.24

and

log

10

(

f

NUV

syn

/

f

NUV

obs

)
=
−
0.03
±
0.16

in the

FUV

and

NUV

, respectively. This agreement is particularly impressive given that we used only optical photometry to construct these UV maps. Having verified the synthetic reddened maps, we use the dust-free maps to examine properties of obscured flux and star formation. We compare our dust-free and reddened maps of

FUV

flux with the observed GALEX

FUV

flux and

FUV

+ 24 μm flux to examine the fraction of obscured flux. We find that the maps of synthetic flux require that ∼90% of the

FUV

flux in M31 is obscured by dust, while the GALEX -based methods suggest that ∼70% of the

FUV

flux is absorbed by dust. This 30% increase in the estimate of the obscured flux is driven by significant differences between the dust-free synthetic

FUV

flux and that derived when correcting the observed

FUV

flux for dust absorption with 24 μm emission observations. The difference is further illustrated when we compare the SFRs derived from the

FUV

+ 24 μm flux with the 100 Myr average SFR from the CMD-based SFHs. We find that the 24 μm corrected

FUV

flux underestimates the SFR by a factor of 2.3–2.5, depending on the chosen calibration. This discrepancy could be reduced by allowing for variability in the weight applied to the 24 μm data, as has been recently suggested in the literature.
ON THE ORIGIN OF THE NEAR-INFRARED EMISSION FROM THE NEUTRON-STAR LOW-MASS X-RAY BINARY GX 9+1*
Authors: van den Berg Maureen , Homan Jeroen 
Published: January 2017

ABSTRACT
We have determined an improved position for the luminous persistent neutron-star low-mass X-ray binary and atoll source GX 9+1 from archival Chandra X-ray Observatory data. The new position significantly differs from a previously published Chandra position for this source. Based on the revised X-ray position we have identified a new near-infrared (NIR) counterpart to GX 9+1 in K

s
-band images obtained with the PANIC and FourStar cameras on the Magellan Baade Telescope. NIR spectra of this

mag star, taken with the FIRE spectrograph on the Baade Telescope, show a strong Br γ emission line, which is a clear signature that we discovered the true NIR counterpart to GX 9+1. The mass donor in GX 9+1 cannot be a late-type giant, as such a star would be brighter than the estimated absolute K

s
magnitude of the NIR counterpart. The slope of the dereddened NIR spectrum is poorly constrained due to uncertainties in the column density N
H and NIR extinction. Considering the source’s distance and X-ray luminosity, we argue that N
H likely lies near the high end of the previously suggested range. If this is indeed the case, the NIR spectrum is consistent with thermal emission from a heated accretion disk, possibly with a contribution from the secondary. In this respect, GX 9+1 is similar to other bright atolls and the Z sources, whose NIR spectra do not show the slope that is expected for a dominant contribution from optically thin synchrotron emission from the inner regions of a jet.
Enhanced recovery after surgery: Neuroanaesthetic perspective
Authors: Mishra Rajeeb , Kapoor Indu , Mahajan Charu , Prabhakar Hemanshu 
Published: January 2017

AbstractEnhanced recovery after surgery (ERAS) is a systematic multimodal perioperative care aimed at reducing the immense surgical stress of the patient and thereby facilitating early recovery. This is basically a multidiscipline, multimodal integrated approach in patient care and it integrates the basic knowledge in a more streamlined fashion, which ultimately improves the outcome of surgery. This article reviews the various aspects of ERAS, and its implementation in neurosurgical practice as some concepts of ERAS may not be applicable in the setting of neurosurgery.
Awareness during anaesthesia for surgery requiring evoked potential monitoring: A pilot study
Authors: Korula Pritish , Mariappan Ramamani , James Justin , Kumar Prashant , Korula Grace 
Published: January 2017

Abstract
Background: Evoked potential monitoring such as somatosensory-evoked potential (SSEP) or motor-evoked potential (MEP) monitoring during surgical procedures in proximity to the spinal cord requires minimising the minimum alveolar concentrations (MACs) below the anaesthetic concentrations normally required (1 MAC) to prevent interference in amplitude and latency of evoked potentials. This could result in awareness. Our primary objective was to determine the incidence of awareness while administering low MAC inhalational anaesthetics for these unique procedures. The secondary objective was to assess the adequacy of our anaesthetic technique from neurophysiologist’s perspective. Methods: In this prospective observational pilot study, 61 American Society of Anesthesiologists 1 and 2 patients undergoing spinal surgery for whom intraoperative evoked potential monitoring was performed were included; during the maintenance phase, 0.7–0.8 MAC of isoflurane was targeted. We evaluated the intraoperative depth of anaesthesia using a bispectral (BIS) index monitor as well as the patients response to surgical stimulus (PRST) scoring system. Post-operatively, a modified Bruce questionnaire was used to verify awareness. The adequacy of evoked potential readings was also assessed. Results: Of the 61 patients, no patient had explicit awareness. Intraoperatively, 19 of 61 patients had a BIS value of above sixty at least once, during surgery. There was no correlation with PRST scoring and BIS during surgery. Fifty-four out of 61 patient’s evoked potential readings were deemed ‘good’ or ‘fair’ for the conduct of electrophysiological monitoring. Conclusions: This pilot study demonstrates that administering low MAC inhalational anaesthetics to facilitate evoked potential monitoring does not result in explicit awareness. However, larger studies are needed to verify this. The conduct of SSEP electrophysiological monitoring was satisfactory with the use of this anaesthetic technique. However, the conduct of MEP monitoring was satisfactory, only in patients with Nurick Grade 1 and 2. The MEP response was poor in patients with Nurick Grade 4 and 5.
Wolff–Parkinson–White syndrome: Implications for an anaesthesiologist
Authors: Udaybhaskar Vinaya , Sreemayee C. , Ingley Prasad 
Published: January 2017

AbstractWolff–Parkinson–White (WPW) syndrome is an electrical conduction abnormality of the heart that can induce potentially fatal arrhythmias at intermittent intervals. The induction and maintenance of general anaesthesia for a patient with WPW syndrome are risky due to the triggering capability of arrhythmias by various drugs and instrumentation. We hereby present the case of a 28-year-old male with previous cardiac illness, admitted for neurosurgical procedure, with drug-controlled WPW syndrome. The pre-operative optimisation, intraoperative scrutiny and vigil, along with readiness of standby medications and defibrillator made the ingress and egress from general anaesthesia uneventful. Thus, the potential dangers of WPW syndrome can be circumvented with watchful preparedness and meticulous monitoring.
Study of the footprints of short-term variation in XCO2 observed by TCCON sites using NIES and FLEXPART atmospheric transport models
Authors: Belikov Dmitry A. , Maksyutov Shamil , Ganshin Alexander , Zhuravlev Ruslan , Deutscher Nicholas M. , Wunch Debra , Feist Dietrich G. , Morino Isamu , Parker Robert J. , Strong Kimberly , Yoshida Yukio , Bril Andrey , Oshchepkov Sergey , Boesch Hartmut , Dubey Manvendra K. , Griffith David , Hewson Will , Kivi Rigel , Mendonca Joseph , Notholt Justus , Schneider Matthias , Sussmann Ralf , Velazco Voltaire A. , Aoki Shuji 
Published: January 2017

Abstract. The Total Carbon Column Observing Network (TCCON) is a network of ground-based Fourier transform spectrometers (FTSs) that record near-infrared (NIR) spectra of the sun. From these spectra, accurate and precise observations of CO2 column-averaged dry-air mole fractions (denoted XCO2) are retrieved. TCCON FTS observations have previously been used to validate satellite estimations of XCO2; however, our knowledge of the short-term spatial and temporal variations in XCO2 surrounding the TCCON sites is limited. In this work, we use the National Institute for Environmental Studies (NIES) Eulerian three-dimensional transport model and the FLEXPART (FLEXible PARTicle dispersion model) Lagrangian particle dispersion model (LPDM) to determine the footprints of short-term variations in XCO2 observed by operational, past, future and possible TCCON sites. We propose a footprint-based method for the collocation of satellite and TCCON XCO2 observations and estimate the performance of the method using the NIES model and five GOSAT (Greenhouse Gases Observing Satellite) XCO2 product data sets. Comparison of the proposed approach with a standard geographic method shows a higher number of collocation points and an average bias reduction up to 0.15 ppm for a subset of 16 stations for the period from January 2010 to January 2014. Case studies of the Darwin and Reunion Island sites reveal that when the footprint area is rather curved, non-uniform and significantly different from a geographical rectangular area, the differences between these approaches are more noticeable. This emphasises that the collocation is sensitive to local meteorological conditions and flux distributions.
WRF-Chem model simulations of a dust outbreak over the central Mediterranean and comparison with multi-sensor desert dust observations
Authors: Rizza Umberto , Barnaba Francesca , Miglietta Mario Marcello , Mangia Cristina , Di Liberto Luca , Dionisi Davide , Costabile Francesca , Grasso Fabio , Gobbi Gian Paolo 
Published: January 2017

Abstract. In this study, the Weather Research and Forecasting model with online coupled chemistry (WRF-Chem) is applied to simulate an intense Saharan dust outbreak event that took place over the Mediterranean in May 2014. Comparison of a simulation using a physics-based desert dust emission scheme with a numerical experiment using a simplified (minimal) emission scheme is included to highlight the advantages of the former. The model was found to reproduce well the synoptic meteorological conditions driving the dust outbreak: an omega-like pressure configuration associated with a cyclogenesis in the Atlantic coasts of Spain. The model performances in reproducing the atmospheric desert dust load were evaluated using a multi-platform observational dataset of aerosol and desert dust properties, including optical properties from satellite and ground-based sun photometers and lidars, plus in situ particulate matter mass concentration (PM) data. This comparison allowed us to investigate the model ability in reproducing both the horizontal and the vertical displacement of the dust plume, as well as its evolution in time. The comparison with satellite (MODIS-Terra) and sun photometers (AERONET) showed that the model is able to reproduce well the horizontal field of the aerosol optical depth (AOD) and its evolution in time (temporal correlation coefficient with AERONET of 0.85). On the vertical scale, the comparison with lidar data at a single site (Rome, Italy) confirms that the desert dust advection occurs in several, superimposed "pulses" as simulated by the model. Cross-analysis of the modeled AOD and desert dust emission fluxes further allowed for the source regions of the observed plumes to be inferred. The vertical displacement of the modeled dust plume was in rather good agreement with the lidar soundings, with correlation coefficients among aerosol extinction profiles up to 1 and mean discrepancy of about 50 %. The model–measurement comparison for PM10 and PM2.5 showed a good temporal matching, although it revealed a marked overestimation of PM10 and PM2.5 (of the order of 70 % during the dust peak). For PM10, it was also possible to investigate the accordance between the model- and the measurement-based dust PM10, this confirming the model PM10 overestimation to be related to over-predicted dust mass up to a factor of 140 %. In all the model–measurement comparisons performed, the enhanced capabilities of the physics-based emission scheme with respect to its simplified, minimal version were evident and are documented.
Open-loop GPS signal tracking at low elevation angles from a ground-based observation site
Authors: Beyerle Georg , Zus Florian 
Published: January 2017

Abstract. A 1-year data set of ground-based GPS signal observations aiming at geometric elevation angles below +2° is analysed. Within the "GLESER" measurement campaign about 2600 validated setting events were recorded by the "OpenGPS" open-loop tracking receiver at an observation site located at 52.3808° N, 13.0642° E between January and December 2014. The measurements confirm the feasibility of open-loop signal tracking down to geometric elevation angles of −1 to −1.5° extending the corresponding closed-loop tracking range by up to 1°. The study is based on the premise that observations of low-elevation events by a ground-based receiver may serve as test cases for space-based radio occultation measurements, even if the latter proceed at a significantly faster temporal scale. The results support the conclusion that the open-loop Doppler model has negligible influence on the derived carrier frequency profile for strong signal-to-noise density ratios above about 30 dB Hz. At lower signal levels, however, the OpenGPS receiver's dual-channel design, which tracks the same signal using two Doppler models differing by 10 Hz, uncovers a notable bias. The repeat patterns of the GPS orbit traces in terms of azimuth angle reveal characteristic signatures in both signal amplitude and Doppler frequency with respect to the topography close to the observation site. Mean vertical refractivity gradients, extracted from ECMWF meteorological fields, correlate weakly to moderately with observed signal amplitude fluctuations at geometric elevation angles between +1 and +2°. Results from multiple phase screen simulations support the interpretation that these fluctuations are at least partly produced by atmospheric multipath; at negative elevation angles diffraction at the ground surface seems to contribute.
The Stedegenhet of Nordic STS
Authors: Karlstrøm Henrik , Finstad Terje 
Published: January 2017

The increasing formalization of STS research networks in the Nordic countries prompts a discussion of how research and academic work in the region is constituted – what makes something ‘Nordic’ STS as opposed to just ‘regular’ STS? Similarly, the degree to which international STS theories can be translated into a Nordic institutional context is a matter of importance for assessing the type of work that is being done by Nordic STS researchers. The article provides an overview of STS-related institutions and activities in the Nordic countries, and discusses the diffusion and diffraction of STS theory acrossnational and institutional barriers.
On Cultures and Artscience: Interdisciplinarity and Discourses of “Twos” and “Threes” after Snow’s Two Cultures
Authors: Vaage Nora Sørensen 
Published: January 2017

At least since C.P. Snow’s seminal Rede lecture The Two Cultures, the idea of a significant difference in kind between the natural sciences and the arts and humanities has been prevalent in Western culture. A gap has been perceived to exist not only in methodology and theory, but more fundamentally, in understandings and worldviews. This has resulted in a dichotomous debate both in academic and media discourses. As a reaction to this, and parallel in time, some actors have strived to achieve a ‘third culture’. This is a common attitude in the still emerging field of ‘artscience’, whose actors seek to combine the advantages and knowledges of the sciences with those of the arts and humanities. Researchers from every concerned field have contributed to the exploration of the interface between ‘art’ and ‘science’. However, I argue in this article that the very term artscience, in simply joining together the words ‘art’ and ’science’, is reenforcing an old notion of a binary opposition between these two fields. The idea of ‘two cultures’, still implied within the image of a ‘third culture’, disguises the plurality of perceptions and approaches within and across fields. While useful in pointing out lack of communication between fields, it tends to overemphasize divisions, ignore complexities, and, in some cases, leave out important parts of the picture. I suggest that the discourse of the ‘third culture’ and the term ‘artscience’ may jointly occlude the multiple possible constellations of practitioners, roles and approaches, and may be a potential limitation to interdisciplinary collaborations.