bluuebunny/crossref_metadata_2025_split huggingface dataset:
Clinical Trial Endpoints in Metastatic Cancer: Using Individual Participant Data to Inform Future Trials Methodology
Authors: Goldberg Richard M , Adams Richard , Buyse Marc , Eng Cathy , Grothey Axel , André Thierry , Sobrero Alberto F , Lichtman Stuart M , Benson Al B , Punt Cornelis J A , Maughan Tim , Burzykowski Tomasz , Sommeijer Dirkje , Saad Everardo D , Shi Qian , Coart Elisabeth , Chibaudel Benoist , Koopman Miriam , Schmoll Hans-Joachim , Yoshino Takayuki , Taieb Julien , Tebbutt Niall C , Zalcberg John , Tabernero Josep , Van Cutsem Eric , Matheson Alastair , de Gramont Aimery 
Published: November 2021

Abstract
Meta-analysis based on individual participant data (IPD) is a powerful methodology for synthesizing evidence by combining information drawn from multiple trials. Hitherto, its principal application has been in questions of clinical management, but an increasingly important use is in clarifying trials methodology, for instance in the selection of endpoints, as discussed in this review. In oncology, the Aide et Recherche en Cancérologie Digestive (ARCAD) Metastatic Colorectal Cancer Database is a leader in the use of IPD-based meta-analysis in methodological research. The ARCAD database contains IPD from more than 38 000 patients enrolled in 46 studies and continues to collect phase III trial data. Here, we review the principal findings of the ARCAD project in respect of endpoint selection and examine their implications for cancer trials. Analysis of the database has confirmed that progression-free survival (PFS) is no longer a valid surrogate endpoint predictive of overall survival in the first-line treatment of colorectal cancer. Nonetheless, PFS remains an endpoint of choice for most first-line trials in metastatic colorectal cancer and other solid tumors. Only substantial PFS effects are likely to translate into clinically meaningful benefits, and accordingly, we advocate an oncology research model designed to identify highly effective treatments in carefully defined patient groups. We also review the use of the ARCAD database in assessing clinical response including novel response metrics and prognostic markers. These studies demonstrate the value of IPD as a tool for methodological studies and provide a reference point for the expansion of this approach within clinical cancer research.
Meningioma-associated abscess: an unusual case report and review of the literature
Authors: Rashed Sami , Vassiliou Anna , Ogborne Rosalie , McKenna Gráinne 
Published: November 2021

Abstract
Central nervous system (CNS) infection and neoplasm occur most often independently. Their concomitant presentation has been noted across different CNS tumours but is considered a rare entity. The phenomenon is mostly seen in relation to direct seeding of infection via frontal air sinuses. Here, we present an unusual case of an occipital meningioma associated with intraparenchymal paratumoural abscess formation. It is also the second documented to culture methicillin-susceptible Staphylococcus aureus. We then review and surmise the relevant literature of meningioma-associated abscess. We discuss the clinical presentations, aetiology, suspected pathogenesis, management and outcomes reported.
Involvement of α-galactosidase OmAGAL2 in planteose hydrolysis during seed germination of Orobanche minor
Authors: Okazawa Atsushi , Baba Atsuya , Okano Hikaru , Tokunaga Tomoya , Nakaue Tsubasa , Ogawa Takumi , Shimma Shuichi , Sugimoto Yukihiro , Ohta Daisaku 
Published: November 2021

Abstract
Root parasitic weeds of the Orobanchaceae, such as witchweeds (Striga spp.) and broomrapes (Orobanche and Phelipanche spp.), cause serious losses in agriculture worldwide, and efforts have been made to control these parasitic weeds. Understanding the characteristic physiological processes in the life cycle of root parasitic weeds is particularly important to identify specific targets for growth modulators. In our previous study, planteose metabolism was revealed to be activated soon after the perception of strigolactones in germinating seeds of O. minor. Nojirimycin inhibited planteose metabolism and impeded seed germination of O. minor, indicating a possible target for root parasitic weed control. In the present study, we investigated the distribution of planteose in dry seeds of O. minor by matrix-assisted laser desorption/ionization–mass spectrometry imaging. Planteose was detected in tissues surrounding—but not within—the embryo, supporting its suggested role as a storage carbohydrate. Biochemical assays and molecular characterization of an α-galactosidase family member, OmAGAL2, indicated that the enzyme is involved in planteose hydrolysis in the apoplast around the embryo after the perception of strigolactones, to provide the embryo with essential hexoses for germination. These results indicate that OmAGAL2 is a potential molecular target for root parasitic weed control.
Chandra revisits WR 48a: testing colliding wind models in massive binaries
Authors: Zhekov Svetozar A , Gagné Marc , Skinner Stephen L 
Published: November 2021

ABSTRACT
We present results of new Chandra High-Energy Transmission Grating (HETG) observations (2019 November–December) of the massive Wolf–Rayet binary WR 48a. Analysis of these high-quality data showed that the spectral lines in this massive binary are broadened (full width at half-maximum, FWHM = 1400 km s−1) and marginally blueshifted (∼−100 km s−1). A direct modelling of these high-resolution spectra in the framework of the standard colliding stellar wind (CSW) picture provided a very good correspondence between the shape of the theoretical and observed spectra. Also, the theoretical line profiles are in most cases an acceptable representation of the observed ones. We applied the CSW model to the X-ray spectra of WR 48a from previous observations: Chandra-HETG (2012 October) and XMM–Newton (2008 January). From this expanded analysis, we find that the observed X-ray emission from WR 48a is variable on the long time-scale (years) and the same is valid for its intrinsic X-ray emission. This requires variable mass-loss rates over the binary orbital period. The X-ray absorption (in excess of that from the stellar winds in the binary) is variable as well. We note that lower intrinsic X-ray emission is accompanied by higher X-ray absorption. A qualitative explanation could be that the presence of clumpy and non-spherically symmetric stellar winds may play a role.
Low-frequency quasi-periodic oscillations and shocks in accretion on to black hole
Authors: Singh Chandra B , Mondal Santanu , Garofalo David 
Published: November 2021

ABSTRACT
Low-frequency quasi-periodic oscillations (LFQPOs) have been routinely observed in black hole X-ray binaries (BHXRBs). These LFQPOs can be explained by axisymmetric shock oscillation in accretion flow around a rotating black hole. We address the physical origin of Type-C LFQPOs in BHXRBs observed by the Rossi X-ray Timing Explorer satellite considering a minimum number of free parameters, namely, specific energy and specific angular momentum of the infalling matter for a given set of BH mass and spin parameter. We apply the solution for a large number of BH candidates to further strengthen the scenario of an anticorrelation between the QPO frequency and the location of the shock. Our study also confirms that Compton cooling can be sufficient to explain the observed QPOs.
Satellite quenching was not important for z ∼ 1 clusters: most quenching occurred during infall
Authors: Werner S V , Hatch N A , Muzzin A , van der Burg R F J , Balogh M L , Rudnick G , Wilson G 
Published: November 2021

ABSTRACT
We quantify the relative importance of environmental quenching versus pre-processing in z ∼ 1 clusters by analysing the infalling galaxy population in the outskirts of 15 galaxy clusters at 0.8 &lt; z &lt; 1.4 drawn from the GOGREEN and GCLASS surveys. We find significant differences between the infalling galaxies and a control sample; in particular, an excess of massive quiescent galaxies in the infalling region. These massive infalling galaxies likely reside in larger dark matter haloes than similar-mass control galaxies because they have twice as many satellite galaxies. Furthermore, these satellite galaxies are distributed in an NFW profile with a larger scale radius compared to the satellites of the control galaxies. Based on these findings, we conclude that it may not be appropriate to use ‘field’ galaxies as a substitute for infalling pre-cluster galaxies when calculating the efficiency and mass dependence of environmental quenching in high-redshift clusters. By comparing the quiescent fraction of infalling galaxies at 1 &lt; R/R200&lt;3 to the cluster sample (R/R200&lt;1) we find that almost all quiescent galaxies with masses &gt;1011 M⊙ were quenched prior to infall, while up to half of lower mass galaxies were environmentally quenched after passing the virial radius. This means most of the massive quiescent galaxies in z ∼ 1 clusters were self-quenched or pre-processed prior to infall.
Revised event rates for extreme and extremely large mass-ratio inspirals
Authors: Vázquez-Aceves Verónica , Zwick Lorenz , Bortolas Elisa , Capelo Pedro R , Amaro Seoane Pau , Mayer Lucio , Chen Xian 
Published: November 2021

ABSTRACT
One of the main targets of the Laser Interferometer Space Antenna (LISA) is the detection of extreme mass-ratio inspirals (EMRIs) and extremely large mass-ratio inspirals (X-MRIs). Their orbits are expected to be highly eccentric and relativistic when entering the LISA band. Under these circumstances, the inspiral time-scale given by Peters’ formula loses precision and the shift of the last-stable orbit (LSO) caused by the massive black hole spin could influence the event rates estimate. We re-derive EMRIs and X-MRIs event rates by implementing two different versions of a Kerr loss-cone angle that includes the shift in the LSO, and a corrected version of Peters’ time-scale that accounts for eccentricity evolution, 1.5 post-Newtonian hereditary fluxes, and spin-orbit coupling. The main findings of our study are summarized as follows: (1) implementing a Kerr loss-cone changes the event rates by a factor ranging between 0.9 and 1.1; (2) the high-eccentricity limit of Peters’ formula offers a reliable inspiral time-scale for EMRIs and X-MRIs, resulting in an event-rate estimate that deviates by a factor of about 0.9–3 when compared to event rates computed with the corrected version of Peters’ time-scale and the usual loss-cone definition. (3) Event-rate estimates for systems with a wide range of eccentricities should be revised. Peters’ formula overestimates the inspiral rates of highly eccentric systems by a factor of about 8–30 compared to the corrected values. Besides, for e0 ≲ 0.8, implementing the corrected version of Peters’ formula is necessary to obtain accurate estimates.
The viewing angle in AGN SED models: a data-driven analysis
Authors: Ramos Padilla Andrés F , Wang Lingyu , Małek Katarzyna , Efstathiou Andreas , Yang (杨光) Guang 
Published: November 2021

ABSTRACT
The validity of the unified active galactic nuclei (AGNs) model has been challenged in the last decade, especially when different types of AGNs are considered to only differ in the viewing angle to the torus. We aim to assess the importance of the viewing angle in classifying different types of Seyfert galaxies in spectral energy distribution (SED) modelling. We retrieve photometric data from publicly available astronomical data bases: CDS and NED, to model SEDs with x-cigale in a sample of 13 173 Seyfert galaxies located at redshift range from z = 0 to 3.5, with a median redshift of z ≈ 0.2. We assess whether the estimated viewing angle from the SED models reflects different Seyfert classifications. Two AGN models with either a smooth or clumpy torus structure are adopted in this paper. We find that the viewing angle in Type-1 AGNs is better constrained than in Type-2 AGNs. Limiting the viewing angles representing these two types of AGNs does not affect the physical parameter estimates such as star formation rate (SFR) or AGN fractional contribution (fAGN). In addition, the viewing angle is not the most discriminating physical parameter to differentiate Seyfert types. We suggest that the observed and intrinsic AGN disc luminosity can (i) be used in z &lt; 0.5 studies to distinguish between Type-1 and Type-2 AGNs, and (ii) explain the probable evolutionary path between these AGN types. Finally, we propose the use of x-cigale for AGN galaxy classification tasks. All data from the 13 173 SED fits are available at Zenodo1.
Uncovering the chemical structure of the pulsating low-mass white dwarf SDSS J115219.99+024814.4
Authors: Romero A D , Lauffer G R , Istrate A G , Parsons S G 
Published: November 2021

ABSTRACT
Pulsating low-mass white dwarf (WD) stars are WDs with stellar masses between 0.30 and 0.45 M⊙ that show photometric variability due to gravity-mode pulsations. Within this mass range, they can harbour both a helium core and hybrid core, depending if the progenitor experienced helium-core burning during the pre-WD evolution. SDSS J115219.99+024814.4 is an eclipsing binary system where both components are low-mass WDs, with stellar masses of 0.362 ± 0.014 M⊙ and 0.325 ± 0.013 M⊙. In particular, the less-massive component is a pulsating star, showing at least three pulsation periods of ∼1314, ∼1069, and ∼582.9 s. This opens the way to use asteroseismology as a tool to uncover its inner chemical structure, in combination with the information obtained using the light-curve modelling of the eclipses. To this end, using binary evolutionary models leading to helium- and hybrid-core WDs, we compute adiabatic pulsations for ℓ = 1 and ℓ = 2 gravity modes with Gyre. We found that the pulsating component of the SDSS J115219.99+024814.4 system must have a hydrogen envelope thinner than the value obtained from binary evolution computations, independently of the inner composition. Finally, from our asteroseismological study, we find a best-fitting model characterized by T$_{\rm eff}=10\,917$ K, M = 0.338 M⊙, and MH = 10−6 M⊙ with the inner composition of a hybrid WD.
No need for dark matter: resolved kinematics of the ultra-diffuse galaxy AGC 114905
Authors: Mancera Piña Pavel E , Fraternali Filippo , Oosterloo Tom , Adams Elizabeth A K , Oman Kyle A , Leisman Lukas 
Published: November 2021

ABSTRACTWe present new H i interferometric observations of the gas-rich ultra-diffuse galaxy AGC 114905, which previous work, based on low-resolution data, identified as an outlier of the baryonic Tully–Fisher relation. The new observations, at a spatial resolution ∼2.5 times higher than before, reveal a regular H i disc rotating at about 23 km s−1. Our kinematic parameters, recovered with a robust 3D kinematic modelling fitting technique, show that the flat part of the rotation curve is reached. Intriguingly, the rotation curve can be explained almost entirely by the baryonic mass distribution alone. We show that a standard cold dark matter halo that follows the concentration–halo mass relation fails to reproduce the amplitude of the rotation curve by a large margin. Only a halo with an extremely (and arguably unfeasible) low concentration reaches agreement with the data. We also find that the rotation curve of AGC 114905 deviates strongly from the predictions of modified Newtonian dynamics. The inclination of the galaxy, which is measured independently from our modelling, remains the largest uncertainty in our analysis, but the associated errors are not large enough to reconcile the galaxy with the expectations of cold dark matter or modified Newtonian dynamics.
Current-driven kink instabilities in relativistic jets: dissipation properties
Authors: Bodo G , Mamatsashvili G , Rossi P , Mignone A 
Published: November 2021

ABSTRACT
We analyse the evolution of current-driven kink instabilities of a highly magnetized relativistic plasma column, focusing in particular on its dissipation properties. The instability evolution leads to the formation of thin current sheets where the magnetic energy is dissipated. We find that the total amount of dissipated magnetic energy is independent of the dissipation properties. Dissipation occurs in two stages: a peak when the instability saturates that is characterized by the formation of a helicoidal current sheet at the boundary of the deformed plasma column, followed by a weaker almost flat phase, in which turbulence develops. The detailed properties of these two phases depend on the equilibrium configuration and other parameters, in particular on the steepness of the pitch radial profile, on the presence of an external axial magnetic field and on the amount of magnetization. These results are relevant for high energy astrophysical sources, since current sheets can be the sites of magnetic reconnection where particles can be accelerated to relativistic energies and give rise to the observed radiation.
K2-99 revisited: a non-inflated warm Jupiter, and a temperate giant planet on a 522-d orbit around a subgiant
Authors: Smith A M S , Breton S N , Csizmadia Sz , Dai F , Gandolfi D , García R A , Howard A W , Isaacson H , Korth J , Lam K W F , Mathur S , Nowak G , Pérez Hernández F , Persson C M , Albrecht S H , Barragán O , Cabrera J , Cochran W D , Deeg H J , Fridlund M , Georgieva I Y , Goffo E , Guenther E W , Hatzes A P , Kabath P , Livingston J H , Luque R , Palle E , Redfield S , Rodler F , Serrano L M , Van Eylen V 
Published: November 2021

ABSTRACT
We report new photometric and spectroscopic observations of the K2-99 planetary system. Asteroseismic analysis of the short-cadence light curve from K2’s Campaign 17 allows us to refine the stellar properties. We find K2-99 to be significantly smaller than previously thought, with R⋆ = 2.55 ± 0.02 R⊙. The new light curve also contains four transits of K2-99 b, which we use to improve our knowledge of the planetary properties. We find the planet to be a non-inflated warm Jupiter, with Rb = 1.06 ± 0.01 $\mathrm{R_{\rm Jup}}$. 60 new radial velocity measurements from HARPS, HARPS-N, and HIRES enable the determination of the orbital parameters of K2-99 c, which were previously poorly constrained. We find that this outer planet has a minimum mass Mcsin ic = 8.4 ± 0.2 $\mathrm{M_{\rm Jup}}$, and an eccentric orbit (ec = 0.210 ± 0.009) with a period of 522.2 ± 1.4 d. Upcoming TESS observations in 2022 have a good chance of detecting the transit of this planet, if the mutual inclination between the two planetary orbits is small.
The GALAH Survey: improving our understanding of confirmed and candidate planetary systems with large stellar surveys
Authors: Clark Jake T , Wright Duncan J , Wittenmyer Robert A , Horner Jonathan , Hinkel Natalie R , Clerté Mathieu , Carter Brad D , Buder Sven , Hayden Michael R , Bland-Hawthorn Joss , Casey Andrew R , De Silva Gayandhi M , D’Orazi Valentina , Freeman Ken C , Kos Janez , Lewis Geraint F , Lin Jane , Lind Karin , Martell Sarah L , Schlesinger Katharine J , Sharma Sanjib , Simpson Jeffrey D , Stello Dennis , Zucker Daniel B , Zwitter Tomaž , Munari Ulisse , Nordlander Thomas 
Published: November 2021

ABSTRACT
Pioneering photometric, astrometric, and spectroscopic surveys is helping exoplanetary scientists better constrain the fundamental properties of stars within our galaxy and the planets these stars host. In this study, we use the third data release from the stellar spectroscopic GALAH Survey, coupled with astrometric data of eDR3 from the Gaia satellite, and other data from NASA’s Exoplanet Archive, to refine our understanding of 279 confirmed and candidate exoplanet host stars and their exoplanets. This homogenously analysed data set comprises 105 confirmed exoplanets, along with 146 K2 candidates, 95 TESS Objects of Interest (TOIs), and 52 Community TOIs (CTOIs). Our analysis significantly shifts several previously (unknown) planet parameters while decreasing the uncertainties for others. Our radius estimates suggest that 35 planet candidates are more likely brown dwarfs or stellar companions due to their new radius values. We are able to refine the radii and masses of WASP-47 e, K2-106 b, and CoRoT-7 b to their most precise values yet to less than 2.3 per cent and 8.5 per cent, respectively. We also use stellar rotational values from GALAH to show that most planet candidates will have mass measurements that will be tough to obtain with current ground-based spectrographs. With GALAH’s chemical abundances, we show through chemo-kinematics that there are five planet hosts that are associated with the galaxy’s thick disc, including NGTS-4, K2-183, and K2-337. Finally, we show that there is no statistical difference between the chemical properties of hot Neptune and hot rocky exoplanet hosts, with the possibility that short-period rocky worlds might be the remnant cores of hotter, gaseous worlds.
Planetary core formation via multispecies pebble accretion
Authors: Andama G , Ndugu N , Anguma S K , Jurua E 
Published: November 2021

ABSTRACT
In the general classical picture of pebble-based core growth, planetary cores grow by accretion of single pebble species. The growing planet may reach the so-called pebble isolation mass, at which it induces a pressure bump that blocks inward drifting pebbles exterior to its orbit, thereby stalling core growth by pebble accretion. In recent hydrodynamic simulations, pebble filtration by the pressure bump depends on several parameters including core mass, disc structure, turbulent viscosity and pebble size. We have investigated how accretion of multiple, instead of single, pebble species affects core growth rates, and how the dependence of pebble isolation mass on turbulent viscosity and pebble size sets the final core masses. We performed numerical simulations in a viscous one-dimensional disc, where maximal grain sizes were regulated by grain growth, fragmentation and drift limits. We confirm that core growth rates and final core masses are sensitive to three key parameters: the threshold velocity at which pebbles fragment on collision, the turbulent viscosity and the distribution of pebble species, which yield a diversity of planetary cores. With accretion of multiple pebble species, planetary cores can grow very fast, reaching over 30–40 ME in mass. Potential cores of cold gas giants were able to form from embryos initially implanted as far as 50 au. Our results suggest that accretion of multispecies pebbles could explain: the estimated 25–45 ME heavy element abundance inside Jupiter’s core; the massive cores of extrasolar planets; the disc rings and gaps at wider orbits; and the early and rapid formation of planetary bodies.