bluuebunny/crossref_metadata_2025_split huggingface dataset:
Genomic Alterations and Outcomes with VEGF-Targeted Therapy in Patients with Clear Cell Renal Cell Carcinoma
Authors: Carlo M.I. , Manley B. , Patil S. , Woo K.M. , Coskey D.T. , Redzematovic A. , Arcila M. , Ladanyi M. , Lee W. , Chen Y.B. , Lee C.H. , Feldman D.R. , Hakimi A.A. , Motzer R.J. , Hsieh J.J. , Voss M.H. 
Published: April 2017

Background: Mutations in VHL, PBRM1, SETD2, BAP1, and KDM5C are common in clear cell renal cell carcinoma (ccRCC), and presence of certain mutations has been associated with outcomes in patients with non-metastatic disease. Limited information is available regarding the correlation between genomic alterations and outcomes in patients with metastatic disease, including response to VEGF-targeted therapy. Objective: To explore correlations between mutational profiles and cancer-specific outcomes, including response to standard VEGF-targeted agents, in patients with metastatic cc RCC. Methods: A retrospective review of 105 patients with metastatic ccRCC who had received systemic therapy and had targeted next-generation sequencing of tumors was conducted. Genomic alterations were correlated to outcomes, including overall survival and time to treatment failure to VEGF-targeted therapy. Results: The most frequent mutations were detected in VHL (83%), PBRM1 (51%), SETD2 (35%), BAP1 (24%), KDM5C (16%), and TERT (14%). Time to treatment failure with VEGF-targeted therapy differed significantly by PBRM1 mutation status ( p = 0.01, median 12.0 months for MT versus 6.9 months for WT) and BAP1 mutation status ( p = 0.01, median 6.4 months for MT versus 11.0 months for WT). Shorter overall survival was associated with TERT mutations ( p = 0.03, median 29.6 months for MT versus 52.6 months for WT) or BAP1 mutations ( p = 0.02, median 28.7 months for MT versus not reached for WT). Conclusions: Genomic alterations in ccRCC tumors have prognostic implications in patients with metastatic disease. BAP1 and TERT promoter mutations may be present in higher frequency than previously thought, and based on this data, deserve further study for their association with poor prognosis.
Synthesis and Characterization with Antimicrobial Activity Studies on some Transition Metal Complexes of N, O Donor Novel Schiff Base Ligand
Authors: Hossain M. S. , Zakaria C. M. , Zahan M. K. 
Published: April 2017

Metal complexes of Mn(II), Fe(II), Co(II) and Cd(II) ions with Schiff base ligand 4-{(pyridin-2-ylimino)methyl}phenol derived from condensation of 2-amino pyridine with 4-hydroxybenzaldehyde was prepared. The ligand and complexes were isolated from the reaction in the solid form and characterized by conductivity, magnetic moment, TLC, IR, UV-Visible, thermal analysis and some physical measurements. During complexation reaction with transition metal ions Schiff base act as a deprotonated tridentate ligand and IR spectra showed that N and O atoms are coordinated to the central metal atom. The observed values confirmed that the complexes have octahedral geometry. The Schiff base and its metal complexes have been found to have moderate to strong antibacterial activity.
Some Theorems For Generalized (U,M)-Derivations In Semiprime Gamma-Rings
Authors: Rahman M. M. , Paul A. C. 
Published: April 2017

The objective of this paper is to establish some results for generalized (U,M)-derivation in semiprime Gamma-ring, where U is a Lie ideal of a semiprime Gamma-ring. Let d be a-(U,M)-derivation and f be a generalized (U,M)-derivation of M then we prove that f(u?v)=f(u)?v+u?d(v) for all u,v belongs to U and a belongs to Gamma, when U is an admissible Lie ideal of M; f(u?m)=f(u)?m+u?d(m) for all u belongs to U, m belongs to M and a belongs to Gamma, when U is a square closed Lie ideal of M.
Correlation amongst Indoor Air Quality, Ventilation and Carbon Dioxide
Authors: Sireesha N. L. 
Published: April 2017

The calculation of carbon dioxide (CO2) intensities can be employed to see the quality of indoor air and ventilation. The studies undertaken till date have been distorted. The current study summaries the association amongst carbon dioxide and building air quality and ventilation, with carbon dioxide being the marker to evaluate air quality and ventilation performance. High carbon dioxide intensities may show insufficient ventilation per occupant and high indoor contaminants intensities, resulting in the Sick Building Syndrome (SBI) Symptoms. The researcher assessed the literature related to indoor air quality (IAQ), ventilation, and building-linked health issues in schools linked to CO2 discharges and recognised general indicated building-linked well-being signs found in schools. A high rise in the ventilation rate or enhancement in ventilation efficacy and/or indoor contaminant source regulation would be anticipated to reduce the occurrence of chosen signs to its optimum.
The evolution of aluminum accumulation in ferns and lycophytes
Authors: Schmitt Marco , Mehltreter Klaus , Sundue Michael , Testo Weston , Watanabe Toshihiro , Jansen Steven 
Published: April 2017

PREMISE OF THE STUDY:This paper investigates the occurrence and evolution of aluminum (Al) accumulation within ferns and lycophytes, which is characterized by Al concentrations above 1000 mg·kg−1 in aboveground plant tissues. We hypothesize that this feature is more common in ferns than in angiosperms, and potentially correlated with growth form and other chemical elements.METHODS:Aluminum concentrations were obtained from novel analyses and literature for a total of 354 specimens and 307 species. Moreover, a semiquantitative aluminon test was applied for a subset of 105 species and validated against exact Al measurements.KEY RESULTS:Molecular phylogenetic analyses showed that the major Al‐accumulating groups were primarily found in the Gleicheniales and Cyatheales, and largely absent in the Polypodiales. At the species and generic level, Al accumulation was typically either absent or present, and mixed results within a single species and genus were limited to less than 30% of the species and genera tested. Epiphytic ferns had significantly lower Al levels than terrestrial ferns, although this finding was not significant after phylogenetic correction. In addition, a significant, positive correlation was found between Al and iron, while Al was negatively correlated with phosphorus and potassium concentrations.CONCLUSIONS:Aluminum accumulation is most common outside of the Polypodiales and occurs in 38% of the species studied, indicating that this trait is indeed common within subtropical and tropical ferns, a finding that could be in line with their role as pioneer species on landslides and soils with high levels of soluble Al.
The Kepler-19 System: A Thick-envelope Super-Earth with Two Neptune-mass Companions Characterized Using Radial Velocities and Transit Timing Variations
Authors: Malavolta Luca , Borsato Luca , Granata Valentina , Piotto Giampaolo , Lopez Eric , Vanderburg Andrew , Figueira Pedro , Mortier Annelies , Nascimbeni Valerio , Affer Laura , Bonomo Aldo S. , Bouchy Francois , Buchhave Lars A. , Charbonneau David , Cameron Andrew Collier , Cosentino Rosario , Dressing Courtney D. , Dumusque Xavier , Fiorenzano Aldo F. M. , Harutyunyan Avet , Haywood Raphaëlle D. , Johnson John Asher , Latham David W. , Lopez-Morales Mercedes , Lovis Christophe , Mayor Michel , Micela Giusi , Molinari Emilio , Motalebi Fatemeh , Pepe Francesco , Phillips David F. , Pollacco Don , Queloz Didier , Rice Ken , Sasselov Dimitar , Ségransan Damien , Sozzetti Alessandro , Udry Stéphane , Watson Chris 
Published: April 2017

Abstract
We report a detailed characterization of the Kepler-19 system. This star was previously known to host a transiting planet with a period of 9.29 days, a radius of 2.2 R
⊕, and an upper limit on the mass of 20 M
⊕. The presence of a second, non-transiting planet was inferred from the transit time variations (TTVs) of Kepler-19b over eight quarters of Kepler photometry, although neither the mass nor period could be determined. By combining new TTVs measurements from all the Kepler quarters and 91 high-precision radial velocities obtained with the HARPS-N spectrograph, using dynamical simulations we obtained a mass of 8.4 ± 1.6 M
⊕ for Kepler-19b. From the same data, assuming system coplanarity, we determined an orbital period of 28.7 days and a mass of 13.1 ± 2.7 M
⊕ for Kepler-19c and discovered a Neptune-like planet with a mass of 20.3 ± 3.4 M
⊕ on a 63-day orbit. By comparing dynamical simulations with non-interacting Keplerian orbits, we concluded that neglecting interactions between planets may lead to systematic errors that can hamper the precision in the orbital parameters when the data set spans several years. With a density of 4.32 ± 0.87 g cm−3 (0.78 ± 0.16 ρ
⊕) Kepler-19b belongs to the group of planets with a rocky core and a significant fraction of volatiles, in opposition to low-density planets characterized only by transit time variations and an increasing number of rocky planets with Earth-like density. Kepler-19 joins the small number of systems that reconcile transit timing variation and radial velocity measurements.
Saving Super-Earths: Interplay between Pebble Accretion and Type I Migration
Authors: Brasser R. , Bitsch B. , Matsumura S. 
Published: April 2017

Abstract
Overcoming type I migration and preventing low-mass planets from spiralling into the central star is a long-studied topic. It is well known that outward migration is possible in viscously heated disks relatively close to the central star because the entropy gradient can be sufficiently steep for the positive corotation torque to overcome the negative Lindblad torque. Yet efficiently trapping planets in this region remains elusive. Here we study disk conditions that yield outward migration for low-mass planets under specific planet migration prescriptions. In a steady-state disk model with a constant α-viscosity, outward migration is only possible when the negative temperature gradient exceeds ∼0.87. We derive an implicit relation for the highest mass at which outward migration is possible as a function of viscosity and disk scale height. We apply these criteria, using a simple power-law disk model, to planets that have reached their pebble isolation mass after an episode of rapid accretion. It is possible to trap planets with the pebble isolation mass farther than the inner edge of the disk provided that α
crit ≳ 0.004 for disks older than 1 Myr. In very young disks, the high temperature causes the planets to grow to masses exceeding the maximum for outward migration. As the disk evolves, these more massive planets often reach the central star, generally only toward the end of the disk lifetime. Saving super-Earths is therefore a delicate interplay between disk viscosity, the opacity profile, and the temperature gradient in the viscously heated inner disk.
A Hubble Space Telescope Survey for Novae in M87. II. Snuffing out the Maximum Magnitude–Rate of Decline Relation for Novae as a Non-standard Candle, and a Prediction of the Existence of Ultrafast Novae*
Authors: Shara Michael M. , Doyle Trisha , Lauer Tod R. , Zurek David , Baltz Edward A. , Kovetz Attay , Madrid Juan P. , Mikołajewska Joanna , Neill J. D. , Prialnik Dina , Welch D. L. , Yaron Ofer 
Published: April 2017

Abstract
The extensive grid of numerical simulations of nova eruptions from the work of Yaron et al. first predicted that some classical novae might significantly deviate from the Maximum Magnitude–Rate of Decline (MMRD) relation, which purports to characterize novae as standard candles. Kasliwal et al. have announced the observational detection of a new class of faint, fast classical novae in the Andromeda galaxy. These objects deviate strongly from the MMRD relationship, as predicted by Yaron et al. Recently, Shara et al. reported the first detections of faint, fast novae in M87. These previously overlooked objects are as common in the giant elliptical galaxy M87 as they are in the giant spiral M31; they comprise about 40% of all classical nova eruptions and greatly increase the observational scatter in the MMRD relation. We use the extensive grid of the nova simulations of Yaron et al. to identify the underlying causes of the existence of faint, fast novae. These are systems that have accreted, and can thus eject, only very low-mass envelopes, of the order of 10−7–10−8
M
⊙, on massive white dwarfs. Such binaries include, but are not limited to, the recurrent novae. These same models predict the existence of ultrafast novae that display decline times, t
2, to be as short as five hours. We outline a strategy for their future detection.
Living on a Flare: Relativistic Reflection in V404 Cyg Observed by NuSTAR during Its Summer 2015 Outburst
Authors: Walton D. J. , Mooley K. , King A. L. , Tomsick J. A. , Miller J. M. , Dauser T. , García J. A. , Bachetti M. , Brightman M. , Fabian A. C. , Forster K. , Fürst F. , Gandhi P. , Grefenstette B. W. , Harrison F. A. , Madsen K. K. , Meier D. L. , Middleton M. J. , Natalucci L. , Rahoui F. , Rana V. , Stern D. 
Published: April 2017

Abstract
We present first results from a series of NuSTAR observations of the black hole X-ray binary V404 Cyg obtained during its summer 2015 outburst, primarily focusing on observations during the height of this outburst activity. The NuSTAR data show extreme variability in both the flux and spectral properties of the source. This is partly driven by strong and variable line-of-sight absorption, similar to previous outbursts. The latter stages of this observation are dominated by strong flares, reaching luminosities close to Eddington. During these flares, the central source appears to be relatively unobscured and the data show clear evidence for a strong contribution from relativistic reflection, providing a means to probe the geometry of the innermost accretion flow. Based on the flare properties, analogies with other Galactic black hole binaries, and also the simultaneous onset of radio activity, we argue that this intense X-ray flaring is related to transient jet activity during which the ejected plasma is the primary source of illumination for the accretion disk. If this is the case, then our reflection modeling implies that these jets are launched in close proximity to the black hole (as close as a few gravitational radii), consistent with expectations for jet launching models that tap either the spin of the central black hole, or the very innermost accretion disk. Our analysis also allows us to place the first constraints on the black hole spin for this source, which we find to be

(99% statistical uncertainty, based on an idealized lamp-post geometry).
Characterizing the Transition from Diffuse Atomic to Dense Molecular Clouds in the Magellanic Clouds with [C ii], [C i], and CO
Authors: Pineda Jorge L. , Langer William D. , Goldsmith Paul F. , Horiuchi Shinji , Kuiper Thomas B. H. , Muller Erik , Hughes Annie , Ott Jürgen , Requena-Torres Miguel A. , Velusamy Thangasamy , Wong Tony 
Published: April 2017

Abstract
We present and analyze deep Herschel/HIFI observations of the [C ii] 158 μm, [C i] 609 μm, and [C i] 370 μm lines toward 54 lines of sight in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC). These observations are used to determine the physical conditions of the line-emitting gas, which we use to study the transition from atomic to molecular gas and from C+ to C0 to CO in their low-metallicity environments. We trace gas with molecular fractions in the range

, between those in the diffuse H2 gas detected by UV absorption (

) and well-shielded regions in which hydrogen is essentially completely molecular. The C0 and CO column densities are only measurable in regions with molecular fractions

in both the LMC and the SMC. Ionized carbon is the dominant gas-phase form of this element that is associated with molecular gas, with C0 and CO representing a small fraction, implying that most (89% in the LMC and 77% in the SMC) of the molecular gas in our sample is CO-dark H2. The mean

conversion factors in our LMC and SMC sample are larger than the value typically found in the Milky Way. When applying a correction based on the filling factor of the CO emission, we find that the values of

in the LMC and SMC are closer to that in the Milky Way. The observed [C ii] intensity in our sample represents about 1% of the total far-infrared intensity from the lines of sight observed in both Magellanic clouds.
Extreme Variability in a Broad Absorption Line Quasar
Authors: Stern Daniel , Graham Matthew J. , Arav Nahum , Djorgovski S. G. , Chamberlain Carter , Barth Aaron J. , Donalek Ciro , Drake Andrew J. , Glikman Eilat , Jun Hyunsung D. , Mahabal Ashish A. , Steidel Charles. C. 
Published: April 2017

Abstract
CRTS J084133.15+200525.8 is an optically bright quasar at z = 2.345 that has shown extreme spectral variability over the past decade. Photometrically, the source had a visual magnitude of V ∼ 17.3 between 2002 and 2008. Then, over the following five years, the source slowly brightened by approximately one magnitude, to V ∼ 16.2. Only ∼1 in 10,000 quasars show such extreme variability, as quantified by the extreme parameters derived for this quasar assuming a damped random walk model. A combination of archival and newly acquired spectra reveal the source to be an iron low-ionization broad absorption line quasar with extreme changes in its absorption spectrum. Some absorption features completely disappear over the 9 years of optical spectra, while other features remain essentially unchanged. We report the first definitive redshift for this source, based on the detection of broad Hα in a Keck/MOSFIRE spectrum. Absorption systems separated by several 1000 km s−1 in velocity show coordinated weakening in the depths of their troughs as the continuum flux increases. We interpret the broad absorption line variability to be due to changes in photoionization, rather than due to motion of material along our line of sight. This source highlights one sort of rare transition object that astronomy will now be finding through dedicated time-domain surveys.
Vertical Structure of Radiation-pressure-dominated Thin Disks: Link between Vertical Advection and Convective Stability
Authors: Gong Hong-Yu , Gu Wei-Min 
Published: April 2017

Abstract
In the classic picture of standard thin accretion disks, viscous heating is balanced by radiative cooling through the diffusion process, and the radiation-pressure-dominated inner disk suffers convective instability. However, recent simulations have shown that, owing to the magnetic buoyancy, the vertical advection process can significantly contribute to energy transport. In addition, in comparing the simulation results with the local convective stability criterion, no convective instability has been found. In this work, following on from simulations, we revisit the vertical structure of radiation-pressure-dominated thin disks and include the vertical advection process. Our study indicates a link between the additional energy transport and the convectively stable property. Thus, the vertical advection not only significantly contributes to the energy transport, but it also plays an important role in making the disk convectively stable. Our analyses may help to explain the discrepancy between classic theory and simulations on standard thin disks.
AGN Outflow Shocks on Bonnor–Ebert Spheres
Authors: Dugan Zachary , Gaibler Volker , Bieri Rebekka , Silk Joseph , Rahman Mubdi 
Published: April 2017

Abstract
Feedback from active galactic nuclei (AGNs) and subsequent jet cocoons and outflow bubbles can have a significant impact on star formation in the host galaxy. To investigate feedback physics on small scales, we perform hydrodynamic simulations of realistically fast AGN winds striking Bonnor–Ebert spheres and examine gravitational collapse and ablation. We test AGN wind velocities ranging from 300 to 3000 km s−1 and wind densities ranging from 0.5 to 10 m
p cm−3. We include heating and cooling of low- and high-temperature gas, self-gravity, and spatially correlated perturbations in the shock, with a maximum resolution of 0.01 pc. We find that the ram pressure is the most important factor that determines the fate of the cloud. High ram pressure winds increase fragmentation and decrease the star formation rate, but they also cause star formation to occur on a much shorter timescale and with increased velocities of the newly formed stars. We find a threshold ram pressure of ∼2 × 10−8 dyn cm−2 above which stars are not formed because the resulting clumps have internal velocities large enough to prevent collapse. Our results indicate that simultaneous positive and negative feedback will be possible in a single galaxy, as AGN wind parameters will vary with location within a galaxy.
Three-dimensional Boltzmann-Hydro Code for Core-collapse in Massive Stars. II. The Implementation of Moving-mesh for Neutron Star Kicks
Authors: Nagakura Hiroki , Iwakami Wakana , Furusawa Shun , Sumiyoshi Kohsuke , Yamada Shoichi , Matsufuru Hideo , Imakura Akira 
Published: April 2017

Abstract
We present a newly developed moving-mesh technique for the multi-dimensional Boltzmann-Hydro code for the simulation of core-collapse supernovae (CCSNe). What makes this technique different from others is the fact that it treats not only hydrodynamics but also neutrino transfer in the language of the 3 + 1 formalism of general relativity (GR), making use of the shift vector to specify the time evolution of the coordinate system. This means that the transport part of our code is essentially general relativistic, although in this paper it is applied only to the moving curvilinear coordinates in the flat Minknowski spacetime, since the gravity part is still Newtonian. The numerical aspect of the implementation is also described in detail. Employing the axisymmetric two-dimensional version of the code, we conduct two test computations: oscillations and runaways of proto-neutron star (PNS). We show that our new method works fine, tracking the motions of PNS correctly. We believe that this is a major advancement toward the realistic simulation of CCSNe.
De la spoliation à l’accumulation : violence, pacification et conflits fonciers en Colombie
Authors: Grajales Jacobo 
Published: April 2017

Le conflit armé colombien de ces dernières décennies a été marqué par l’importance des affrontements d’ordre foncier. Déterminants dans l’apparition des acteurs armés, ces affrontements ont été exacerbés par des stratégies de spoliation et d’accaparement des terres, qui ont provoqué des déplacements forcés de populations ainsi que la reconfiguration des territoires. La démobilisation des milices paramilitaires, principaux auteurs de cette spoliation, et la relative stabilisation de la situation sécuritaire depuis le milieu des années 2000 n’ont pas conduit à une remise en cause profonde des formes d’accumulation issues de la guerre. Au contraire, les transformations en cours aujourd’hui se caractérisent soit par un usage plus discret de la violence, soit par l’émergence de nouveaux acteurs économiques, en phase avec le discours et les exigences normatives d’une situation qualifiée de « sortie de guerre ». Sur la base de ce constat, cette contribution propose une discussion critique non seulement de l’économie politique du foncier rural en situation de post-conflit mais aussi, plus généralement, de la caractérisation de ces contextes en termes de rupture et de transformation.