bluuebunny/crossref_metadata_2025_split huggingface dataset:
Measuring Aging and Identifying Aging Phenotypes in Cancer Survivors
Authors: Guida Jennifer L , Ahles Tim A , Belsky Daniel , Campisi Judith , Cohen Harvey Jay , DeGregori James , Fuldner Rebecca , Ferrucci Luigi , Gallicchio Lisa , Gavrilov Leonid , Gavrilova Natalia , Green Paige A , Jhappan Chamelli , Kohanski Ronald , Krull Kevin , Mandelblatt Jeanne , Ness Kirsten K , O’Mara Ann , Price Nathan , Schrack Jennifer , Studenski Stephanie , Theou Olga , Tracy Russell P , Hurria Arti 
Published: July 2019

Abstract
Observational data have shown that some cancer survivors develop chronic conditions like frailty, sarcopenia, cardiac dysfunction, and mild cognitive impairment earlier and/or at a greater burden than similarly aged individuals never diagnosed with cancer or exposed to systemic or targeted cancer therapies. In aggregate, cancer- and treatment-related physical, cognitive, and psychosocial late- and long-term morbidities experienced by cancer survivors are hypothesized to represent accelerated or accentuated aging trajectories. However, conceptual, measurement, and methodological challenges have constrained efforts to identify, predict, and mitigate aging-related consequences of cancer and cancer treatment. In July 2018, the National Cancer Institute convened basic, clinical, and translational science experts for a think tank titled “Measuring Aging and Identifying Aging Phenotypes in Cancer Survivors.” Through the resulting deliberations, several research and resource needs were identified, including longitudinal studies to examine aging trajectories that include detailed data from before, during, and after cancer treatment; mechanistic studies to elucidate the pathways that lead to the emergence of aging phenotypes in cancer survivors; long-term clinical surveillance to monitor survivors for late-emerging effects; and tools to integrate multiple data sources to inform understanding of how cancer and its therapies contribute to the aging process. Addressing these needs will help expand the evidence base and inform strategies to optimize healthy aging of cancer survivors.
Review on global change status and its impacts on the Tibetan Plateau environment
Authors: Latif Aamir , Ilyas Sana , Zhang Yangjian , Xin Yuqin , Zhou Lin , Zhou Quan 
Published: July 2019

Abstract
The Tibetan Plateau (TP) holds fundamental ecological and environmental significances to China and Asia. The TP also lies in the core zone of the belt and road initiative. To protect the TP environment, a comprehensive screening on current ecological research status is entailed. The teased out research gap can also be utilized as guidelines for the recently launched major research programs, i.e. the second TP scientific expedition and silk and belt road research plan. The findings showed that the TP has experienced significant temperature increase at a rate of 0.2°C per decade since 1960s. The most robust warming trend was found in the northern plateau. Precipitation also exhibited an increasing trend but with high spatial heterogeneity. Changing climates have caused a series of environmental consequences, including lake area changes, glacier shrinkage, permafrost degradation and exacerbated desertification. The rising temperature is the main reason behind the glaciers shrinkage, snow melting, permafrost degradation and lake area changes on the TP and neighboring regions. The projected loss of glacial area on the plateau is estimated to be around 43% by 2070 and 75% by the end of the century. Vegetation was responsive to the changed environments, varied climates and intensified human activities by changing phenology and productivity. Future global change study should be more oriented toward integrating various research methods and tools, and synthesizing diverse subjects of water, vegetation, atmosphere and soil.
The global South as a solution to cope with the crisis: Following the transnational itineraries of the precarised Spaniards towards Algeria
Authors: Cabezón-Fernández María-Jesús , Sempere-Souvannavong Juan-David 
Published: July 2019

Abstract
The rising economies in the global South have been a destination of expatriates, businessmen, and high-skilled migrants during the bonanza times. A move to these places was seen as cosmopolitan way to improve professional careers by acquiring international experience or higher quality of education. However, in the post-crisis context after the crash of 2008, the needs of the Southern European populace have changed due to the precarisation of their social contexts in terms of economic insecurity which instead have been pushed them to seek job opportunities across borders to avoid unemployment. In this article, we shed light on the transnational strategies performed by the precarised Spaniards moving to Algeria to cope with the constraints that the crisis initiated in their day-to-day needs. In doing so, under the lens of the transnational theory and the mobility turn, we performed multi-sited fieldwork between 2012 and 2016, based on in-depth interviews with participant observation of Spaniards who have developed a transnational strategy between both countries since 2005 to 2016. The goal of this longitudinal methodology was to identify how the effects of the crisis have encouraged the evolution of these transnational itineraries attending to the particular tensions when moving to this country culturally different in the other side of the Mediterranean. Through three specific cases, we show how these Spaniards reshaped their trajectories from short-term mobilities, punctual and voluntarily planned and scheduled, to circular mobilities, perceived as an imposition by the social context without the possibility to decide when to come back home.
Biofluorescent Worlds – II. Biological fluorescence induced by stellar UV flares, a new temporal biosignature
Authors: O'Malley-James Jack T , Kaltenegger Lisa 
Published: July 2019

ABSTRACT
Our first targets in the search for signs of life are orbiting nearby M stars, such as the planets in the Proxima Centauri, Ross-128, LHS-1140, and TRAPPIST-1 systems. Future ground-based discoveries, and those from the TESS mission, will provide additional close-by targets. However, young M stars tend to be very active, flaring frequently and causing UV fluxes on the surfaces of HZ planets to become biologically harmful. Common UV-protection methods used by life (e.g. living underground, or underwater) would make a biosphere harder to detect. However, photoprotective biofluorescence, ‘up-shifting’ UV to longer, safer wavelengths, could increase a biosphere's detectability. Here we model intermittent emission at specific wavelengths in the visible spectrum caused by biofluorescence as a new temporal biosignature for planets around active M stars. We use the absorption and emission characteristics of common coral fluorescent pigments and proteins to create model spectra and colours for an Earth-like planet in such a system, accounting for different surface features, atmospheric absorption, and cloud cover. We find that for a cloud-free planet biofluorescence could induce a temporary change in brightness that is significantly higher than the reflected flux alone, causing up to two orders-of-magnitude change in planet–star contrast, compared to a non-fluorescent state, if the surface is fully covered by a highly efficient fluorescent biosphere. Hence, UV-flare induced biofluorescence presents previously unexplored possibilities for a new temporal biosignature that could be detectable by instruments like those planned for the extremely large telescope and could reveal hidden biospheres.
Mass transport in galaxy discs limits black hole growth to sub-Eddington rates
Authors: Eastwood Daniel S , Khochfar Sadegh , Trew Arthur 
Published: July 2019

ABSTRACT
Supermassive black holes (SMBHs) observed to have masses of $M_\bullet \sim 10^9 \, \mathrm{M_\odot }$ at z ≳ 6, <1 Gyr after the big bang, are thought to have been seeded by massive black holes that formed before growing concurrently with the formation of their host galaxies. We model analytically the idealized growth of seed black holes, fed through gas inflow from growing proto-galaxy discs. The inflow depends on the disc gravitational stability and thus varies with black hole and disc mass. We find that for a typical host halo, the efficiency of angular momentum transport, as parametrized by the disc viscosity, is the limiting factor in determining the inflow rate and the black hole accretion rate. For our fiducial case, we find an upper black hole mass estimate of $M_\bullet \sim 1.8 \times 10^7 \, \mathrm{M_{\odot }}$ at z = 6. Only in the extreme case of ∼1016 M⊙ haloes at z = 6 produces SMBH masses of ∼109 M⊙. However, the number density of such haloes is many orders of magnitude below the estimated 1 Gpc−3 of SMBHs at z = 6, indicating that viscosity driven accretion is too inefficient to feed the growth of seeds into $M_\bullet \sim 10^9 \, \mathrm{M_\odot }$ SMBHs by z ∼ 6. We demonstrate that major mergers are capable of resolving the apparent discrepancy in black hole mass at z = 6, with some dependence on the exact choice of orbital parameters of the merger.
Massive neutrinos leave fingerprints on cosmic voids
Authors: Kreisch Christina D , Pisani Alice , Carbone Carmelita , Liu Jia , Hawken Adam J , Massara Elena , Spergel David N , Wandelt Benjamin D 
Published: July 2019

ABSTRACT
Do void statistics contain information beyond the tracer 2-point correlation function? Yes! As we vary the sum of the neutrino masses, we find void statistics contain information absent when using just tracer 2-point statistics. Massive neutrinos uniquely affect cosmic voids. We explore their impact on void clustering using both the DEMNUni and MassiveNuS simulations. For voids, neutrino effects depend on the observed void tracers. As the neutrino mass increases, the number of small voids traced by cold dark matter particles increases and the number of large voids decreases. Surprisingly, when massive, highly biased, haloes are used as tracers, we find the opposite effect. The scale at which voids cluster, as well as the void correlation, is similarly sensitive to the sum of neutrino masses and the tracers. This scale-dependent trend is not due to simulation volume or halo density. The interplay of these signatures in the void abundance and clustering leaves a distinct fingerprint that could be detected with observations and potentially help break degeneracies between different cosmological parameters. This paper paves the way to exploit cosmic voids in future surveys to constrain the mass of neutrinos.
Fast likelihood-free cosmology with neural density estimators and active learning
Authors: Alsing Justin , Charnock Tom , Feeney Stephen , Wandelt Benjamin 
Published: July 2019

Abstract
Likelihood-free inference provides a framework for performing rigorous Bayesian inference using only forward simulations, properly accounting for all physical and observational effects that can be successfully included in the simulations. The key challenge for likelihood-free applications in cosmology, where simulation is typically expensive, is developing methods that can achieve high-fidelity posterior inference with as few simulations as possible. Density-estimation likelihood-free inference (DELFI) methods turn inference into a density estimation task on a set of simulated data-parameter pairs, and give orders of magnitude improvements over traditional Approximate Bayesian Computation approaches to likelihood-free inference. In this paper we use neural density estimators (NDEs) to learn the likelihood function from a set of simulated datasets, with active learning to adaptively acquire simulations in the most relevant regions of parameter space on-the-fly. We demonstrate the approach on a number of cosmological case studies, showing that for typical problems high-fidelity posterior inference can be achieved with just $\mathcal {O}(10^3)$ simulations or fewer. In addition to enabling efficient simulation-based inference, for simple problems where the form of the likelihood is known, DELFI offers a fast alternative to MCMC sampling, giving orders of magnitude speed-up in some cases. Finally, we introduce pydelfi – a flexible public implementation of DELFI with NDEs and active learning – available at https://github.com/justinalsing/pydelfi.
Maximally rotating supermassive stars at the onset of collapse: effects of gas pressure
Authors: Dennison Kenneth A , Baumgarte Thomas W , Shapiro Stuart L 
Published: July 2019

ABSTRACT
The ‘direct collapse’ scenario has emerged as a promising evolutionary track for the formation of supermassive black holes early in the Universe. In an idealized version of such a scenario, a uniformly rotating supermassive star spinning at the mass-shedding (Keplerian) limit collapses gravitationally after it reaches a critical configuration. Under the assumption that the gas is dominated by radiation pressure, this critical configuration is characterized by unique values of the dimensionless parameters J/M2 and Rp/M, where J is the angular momentum, Rp the polar radius, and M the mass. Motivated by a previous perturbative treatment, we adopt a fully non-linear approach to evaluate the effects of gas pressure on these dimensionless parameters for a large range of masses. We find that gas pressure has a significant effect on the critical configuration even for stellar masses as large as $M \simeq 10^6 \, \mathrm{M}_{\odot }$. We also calibrate two approximate treatments of the gas pressure perturbation in a comparison with the exact treatment, and find that one commonly used approximation in particular results in increasing deviations from the exact treatment as the mass decreases, and the effects of gas pressure increase. The other approximation, however, proves to be quite robust for all masses $M \gtrsim 10^4 \, \mathrm{M}_{\odot }$.
Crust cooling of the neutron star in Aql X-1: different depth and magnitude of shallow heating during similar accretion outbursts
Authors: Degenaar N , Ootes L S , Page D , Wijnands R , Parikh A S , Homan J , Cackett E M , Miller J M , Altamirano D , Linares M 
Published: July 2019

ABSTRACT
The structure and composition of the crust of neutron stars plays an important role in their thermal and magnetic evolution, hence in setting their observational properties. One way to study the properties of the crust of a neutron star, is to measure how it cools after it has been heated during an accretion outburst in a low-mass X-ray binary (LMXB). Such studies have shown that there is a tantalizing source of heat, of currently unknown origin, that is located in the outer layers of the crust and has a strength that varies between different sources and different outbursts. With the aim of understanding the mechanism behind this ‘shallow heating’, we present Chandra and Swift observations of the neutron star LMXB Aql X-1, obtained after its bright 2016 outburst. We find that the neutron star temperature was initially much lower, and started to decrease at much later time, than observed after the 2013 outburst of the source, despite the fact that the properties of the two outbursts were very similar. Comparing our data to thermal evolution simulations, we infer that the depth and magnitude of shallow heating must have been much larger during the 2016 outburst than during the 2013 one. This implies that basic neutron star parameters that remain unchanged between outbursts do not play a strong role in shallow heating. Furthermore, it suggests that outbursts with a similar accretion morphology can give rise to very different shallow heating. We also discuss alternative explanations for the observed difference in quiescent evolution after the 2016 outburst.
Kelvin–Helmholtz instability in self-gravitating streams
Authors: Aung Han , Mandelker Nir , Nagai Daisuke , Dekel Avishai , Birnboim Yuval 
Published: July 2019

ABSTRACT
Self-gravitating gaseous filaments exist on many astrophysical scales, from sub-pc filaments in the interstellar medium to Mpc scale streams feeding galaxies from the cosmic web. These filaments are often subject to Kelvin–Helmholtz Instability (KHI) due to shearing against a confining background medium. We study the non-linear evolution of KHI in pressure-confined self-gravitating gas streams initially in hydrostatic equilibrium, using analytic models and hydrodynamic simulations, not including radiative cooling. We derive a critical line mass, or mass per unit length, as a function of the stream Mach number and density contrast with respect to the background, μcr(Mb, δc) ≤ 1, where μ = 1 is normalized to the maximal line mass for which initial hydrostatic equilibrium is possible. For μ < μcr, KHI dominates the stream evolution. A turbulent shear layer expands into the background and leads to stream deceleration at a similar rate to the non-gravitating case. However, with gravity, penetration of the shear layer into the stream is halted at roughly half the initial stream radius by stabilizing buoyancy forces, significantly delaying total stream disruption. Streams with μcr < μ ≤ 1 fragment and form round, long-lived clumps by gravitational instability (GI), with typical separations roughly eight times the stream radius, similar to the case without KHI. When KHI is still somewhat effective, these clumps are below the spherical Jeans mass and are partially confined by external pressure, but they approach the Jeans mass as μ → 1 and GI dominates. We discuss potential applications of our results to streams feeding galaxies at high redshift, filaments in the ISM, and streams resulting from tidal disruption of stars near the centres of massive galaxies.
Low-frequency radio study of MACS clusters at 610 and 235 MHz using the GMRT
Authors: Paul Surajit , Salunkhe Sameer , Datta Abhirup , Intema Huib T 
Published: July 2019

Abstract
Studies have shown that mergers of massive galaxy clusters produce shocks and turbulence in the intracluster medium, these events possibly creating radio relics, as well as radio haloes. Here we present Giant Metrewave Radio Telescope (GMRT) dual-band (235- and 610-MHz) radio observations of four such clusters from the MAssive Cluster Survey (MACS) catalogue. We report the discovery of a very faint, diffuse, elongated radio source with a projected size of about 0.5 Mpc in cluster MACSJ0152.5−2852. We also confirm the presence of a radio-relic-like source (about 0.4 Mpc, previously reported at 325 MHz) in cluster MACSJ0025.4−1222. Proposed relics in both these clusters are found apparently inside the virial radius, instead of at their usual peripheral location, while no radio haloes are detected. These high-redshift clusters (z = 0.584 and 0.413) are among the earliest merging systems detected from cluster radio emission. In cluster MACSJ1931.8-2635, we found a radio mini-halo and an interesting highly bent pair of radio jets. Also, we present here a maiden study of low-frequency (GMRT 235- and 610-MHz) spectral and morphological signatures of the previously known radio cluster MACSJ0014.3−3022 (Abell 2744). This cluster hosts a relatively flat spectrum ($\alpha ^{610}_{235}\sim -1.15$), giant (∼1.6 Mpc each) halo–relic structure and a nearby high-speed ($1769\pm ^{148}_{359}$ km s−1) merger shock ($\mathcal {M}=2.02\pm ^{0.17}_{0.41}$) originating from a possible second merger in the cluster.
A multiwavelength study of the debris disc around 49 Cet
Authors: Pawellek Nicole , Moór Attila , Milli Julien , Kóspál Ágnes , Olofsson Johan , Ábrahám Péter , Keppler Miriam , Kral Quentin , Pohl Adriana , Augereau Jean-Charles , Boccaletti Anthony , Chauvin Gaël , Choquet Élodie , Engler Natalia , Henning Thomas , Langlois Maud , Lee Eve J , Ménard François , Thébault Philippe , Zurlo Alice 
Published: July 2019

Abstract
In a multiwavelength study of thermal emission and scattered light images we analyse the dust properties and structure of the debris disc around the A1-type main-sequence star 49 Cet. As a basis for this study, we present new scattered light images of the debris disc known to possess a high amount of both dust and gas. The outer region of the disc is revealed in former coronagraphic H-band and our new Y-band images from the Very Large Telescope SPHERE instrument. We use the knowledge of the disc’s radial extent inferred from ALMA observations and the grain size distribution found by spectral energy distribution fitting to generate semidynamical dust models of the disc. We compare the models to scattered light and thermal emission data and find that a disc with a maximum surface density at 110 au and shallow edges can describe both the thermal emission and the scattered light observations. This suggests that grains close to the blow-out limit and large grains stem from the same planetesimal population and are mainly influenced by radiation pressure. The influence of inward transport processes could not be analysed in this study.
CTCF cooperates with CtIP to drive homologous recombination repair of double-strand breaks
Authors: Hwang Soon Young , Kang Mi Ae , Baik Chul Joon , Lee Yejin , Hang Ngo Thanh , Kim Byung-Gyu , Han Joo Seok , Jeong Jae-Hoon , Park Daechan , Myung Kyungjae , Lee Jong-Soo 
Published: July 2019

AbstractThe pleiotropic CCCTC-binding factor (CTCF) plays a role in homologous recombination (HR) repair of DNA double-strand breaks (DSBs). However, the precise mechanistic role of CTCF in HR remains largely unclear. Here, we show that CTCF engages in DNA end resection, which is the initial, crucial step in HR, through its interactions with MRE11 and CtIP. Depletion of CTCF profoundly impairs HR and attenuates CtIP recruitment at DSBs. CTCF physically interacts with MRE11 and CtIP and promotes CtIP recruitment to sites of DNA damage. Subsequently, CTCF facilitates DNA end resection to allow HR, in conjunction with MRE11–CtIP. Notably, the zinc finger domain of CTCF binds to both MRE11 and CtIP and enables proficient CtIP recruitment, DNA end resection and HR. The N-terminus of CTCF is able to bind to only MRE11 and its C-terminus is incapable of binding to MRE11 and CtIP, thereby resulting in compromised CtIP recruitment, DSB resection and HR. Overall, this suggests an important function of CTCF in DNA end resection through the recruitment of CtIP at DSBs. Collectively, our findings identify a critical role of CTCF at the first control point in selecting the HR repair pathway.
A hidden human proteome encoded by ‘non-coding’ genes
Authors: Lu Shaohua , Zhang Jing , Lian Xinlei , Sun Li , Meng Kun , Chen Yang , Sun Zhenghua , Yin Xingfeng , Li Yaxing , Zhao Jing , Wang Tong , Zhang Gong , He Qing-Yu 
Published: July 2019

Abstract
It has been a long debate whether the 98% ‘non-coding’ fraction of human genome can encode functional proteins besides short peptides. With full-length translating mRNA sequencing and ribosome profiling, we found that up to 3330 long non-coding RNAs (lncRNAs) were bound to ribosomes with active translation elongation. With shotgun proteomics, 308 lncRNA-encoded new proteins were detected. A total of 207 unique peptides of these new proteins were verified by multiple reaction monitoring (MRM) and/or parallel reaction monitoring (PRM); and 10 new proteins were verified by immunoblotting. We found that these new proteins deviated from the canonical proteins with various physical and chemical properties, and emerged mostly in primates during evolution. We further deduced the protein functions by the assays of translation efficiency, RNA folding and intracellular localizations. As the new protein UBAP1-AST6 is localized in the nucleoli and is preferentially expressed by lung cancer cell lines, we biologically verified that it has a function associated with cell proliferation. In sum, we experimentally evidenced a hidden human functional proteome encoded by purported lncRNAs, suggesting a resource for annotating new human proteins.