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13,038 results on '"Rudiger A"'

1. Overnight stay in Spanish emergency departments and mortality in older patients

Author

Miró, Òscar, Aguiló, Sira, Alquézar-Arbé, Aitor, Fernández, Cesáreo, Burillo, Guillermo, Martínez, Sergio Guzmán, Larrull, María Esther Martínez, Periago, Andrea B. Bravo, Molinas, Claudia Lorena Amarilla, Falcón, Carolina Rangel, Dacosta, Paz Balado, Flores, Rudiger Carlos Chávez, Calzada, Jorge Navarro, Blesa, Eva María Fragero, Martín, Manuel Ángel Palomero, Requena, Ángela Cobos, Fuentes, Lidia, Cortizo, Isabel Lobo, Garcinuño, Pablo González, García, María Bóveda, Del Valle, Pedro Rivas, Campos, Raquel Benavent, Jiménez, Verónica Castro, Cuñado, Vanesa Abad, Gutiérrez, Olga Trejo, del Mar Sousa Reviriego, María, Roussel, Melanie, and del Castillo, Juan González

Published
2024
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2. The boundary of cosmic filaments

Author

Wang, Wei, Wang, Peng, Guo, Hong, Kang, Xi, Libeskind, Noam I., Galarraga-Espinosa, Daniela, Springel, Volker, Kannan, Rahul, Hernquist, Lars, Pakmor, Rudiger, Yu, Haoran, Bose, Sownak, Guo, Quan, Yu, Luo, and Hernandez-Aguayo, Cesar

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

For decades, the boundary of cosmic filaments have been a subject of debate. In this work, we determine the physically-motivated radii of filaments by constructing stacked galaxy number density profiles around the filament spines. We find that the slope of the profile changes with distance to the filament spine, reaching its minimum at approximately 1 Mpc at z = 0 in both state-of-the-art hydrodynamical simulations and observational data. This can be taken as the average value of the filament radius. Furthermore, we note that the average filament radius rapidly decreases from z = 4 to z = 1, and then slightly increases. Moreover, we find that the filament radius depends on the filament length, the distance from connected clusters, and the masses of the clusters. These results suggest a two-phase formation scenario of cosmic filaments. The filaments experience rapid contraction before z = 1, but their density distribution has remained roughly stable since then. The subsequent mass transport along the filaments to the connected clusters is likely to have contributed to the formation of the clusters themselves., Comment: 12 pages, 11 figures, accepted by mnras

Published
2024
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4. Close encounters of black hole - star binaries with stellar-mass black holes

Author

Ryu, Taeho, Valli, Ruggero, Pakmor, Rudiger, Perna, Rosalba, de Mink, Selma E., and Springel, Volker

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

Dynamical interactions involving binaries play a crucial role in the evolution of star clusters and galaxies. We continue our investigation of the hydrodynamics of three-body encounters, focusing on binary black hole (BBH) formation, stellar disruption, and electromagnetic (EM) emission in dynamical interactions between a BH-star binary and a stellar-mass BH, using the moving-mesh hydrodynamics code {\small AREPO}. This type of encounters can be divided into two classes depending on whether the final outcome includes BBHs. This outcome is primarily determined by which two objects meet at the first closest approach. BBHs are more likely to form when the star and the incoming BH encounter first with an impact parameter smaller than the binary's semimajor axis. In this case, the star is frequently disrupted. On the other hand, when the two BHs encounter first, frequent consequences are an orbit perturbation of the original binary or a binary member exchange. For the parameters chosen in this study, BBH formation, accompanied by stellar disruption, happens in roughly 1 out of 4 encounters. The close correlation between BBH formation and stellar disruption has possible implications for EM counterparts at the binary's merger. The BH that disrupts the star is promptly surrounded by an optically and geometrically thick disk with accretion rates exceeding the Eddington limit. If the debris disk cools fast enough to become long-lived, EM counterparts can be produced at the time of the BBH merger., Comment: 16 pages, 11 figures, 2 table. Accepted for publication in MNRAS, movie here: https://studio.youtube.com/playlist/PLxLK3qI02cQfXhvhRZp9gkvts_E46t0kH/videos

Published
2023
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5. A biological sequence comparison algorithm using quantum computers

Author

Kösoglu-Kind, Büsra, Loredo, Robert, Grossi, Michele, Bernecker, Christian, Burks, Jody M, and Buchkremer, Rudiger

Subjects
Quantum Physics, Quantitative Biology - Genomics
Abstract

Genetic information is encoded in a linear sequence of nucleotides, represented by letters ranging from thousands to billions. Mutations refer to changes in the DNA or RNA nucleotide sequence. Thus, mutation detection is vital in all areas of biology and medicine. Careful monitoring of virulence-enhancing mutations is essential. However, an enormous amount of classical computing power is required to analyze genetic sequences of this size. Inspired by human perception of vision and pixel representation of images on quantum computers, we leverage these techniques to implement a pairwise sequence analysis. The methodology has a potential advantage over classical approaches and can be further applied to identify mutations and other modifications in genetic sequences. We present a method to display and analyze the similarity between two genome sequences on a quantum computer where a similarity score is calculated to determine the similarity between nucleotides., Comment: typos in some points and additional information was added

Published
2023
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6. Bayes Complexity of Learners vs Overfitting

Author

Głuch, Grzegorz and Urbanke, Rudiger

Subjects
Computer Science - Machine Learning, Statistics - Machine Learning
Abstract

We introduce a new notion of complexity of functions and we show that it has the following properties: (i) it governs a PAC Bayes-like generalization bound, (ii) for neural networks it relates to natural notions of complexity of functions (such as the variation), and (iii) it explains the generalization gap between neural networks and linear schemes. While there is a large set of papers which describes bounds that have each such property in isolation, and even some that have two, as far as we know, this is a first notion that satisfies all three of them. Moreover, in contrast to previous works, our notion naturally generalizes to neural networks with several layers. Even though the computation of our complexity is nontrivial in general, an upper-bound is often easy to derive, even for higher number of layers and functions with structure, such as period functions. An upper-bound we derive allows to show a separation in the number of samples needed for good generalization between 2 and 4-layer neural networks for periodic functions.

Published
2023

8. Thermal Remote Sensing

Author

Cristóbal, Jordi, Gens, Rudiger, Prakash, Anupma, Chaussard, Estelle, editor, Jones, Cathleen, editor, Chen, Jingyi Ann, editor, and Donnellan, Andrea, editor

Published
2024
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9. Magnetic fields do not suppress global star formation in low metallicity dwarf galaxies

Author

Whitworth, David J., Smith, Rowan J., Klessen, Ralf S., Mac Low, Mordecai-Mark, Glover, Simon C. O., Tress, Robin, Pakmor, Rudiger, and Soler, Juan D.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Many studies concluded that magnetic fields suppress star formation in molecular clouds and Milky Way like galaxies. However, most of these studies are based on fully developed fields that have reached the saturation level, with little work on investigating how an initial weak primordial field affects star formation in low metallicity environments. In this paper, we investigate the impact of a weak initial field on low metallicity dwarf galaxies. We perform high-resolution AREPO simulations of five isolated dwarf galaxies. Two models are hydrodynamical, two start with a primordial magnetic field of 10$^{-6} \mu$G and different sub-solar metallicities, and one starts with a saturated field of 10$^{-2} \mu$G. All models include a non-equilibrium, time-dependent chemical network that includes the effects of gas shielding from the ambient ultraviolet field. Sink particles form directly from the gravitational collapse of gas and are treated as star-forming clumps that can accrete gas. We vary the ambient uniform far ultraviolet field, and cosmic ray ionization rate between 1\% and 10\% of solar values. We find that the magnetic field has little impact on the global star formation rate, which is in tension with some previously published results. We further find that the initial field strength has little impact on the global star formation rate. We show that an increase in the mass fractions of both molecular hydrogen and cold gas, along with changes in the perpendicular gas velocity dispersion and the magnetic field acting in the weak-field model, overcome the expected suppression in star formation., Comment: 19 pages, 19 figures, accepted for publication in MNRAS

Published
2022
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10. Student Perceptions and Use of Mobile Devices for LIS Coursework: Implications for Educators

Author

Stephens, Michael, Rudiger, Nikki, and Faires, Debbie

Abstract

This study offers insights regarding the use of mobile devices by students to help educators in Library and Information Science (LIS) and across disciplines better understand their current and potential use. Using a web survey and descriptive content analysis methods, this article reports student perceptions of the role mobile devices play in LIS coursework, identifying areas where the technology is effective, providing recommendations regarding creative enhancements to course delivery, and offering insights for instructors into mobile-friendly course design and pedagogy. The data in this study indicate that current LIS students take their courses "on the go," moving easily between a formal learning setting to an informal one, and provide instructors with considerations for the multiple ways in which students may access course content and engage with others in their classes using mobile devices.

Published
2021

11. Accreting on the edge: a luminosity-dependent cyclotron line in the Be/X-ray Binary 2S 1553-542 accompanied by accretion regimes transition

Author

Malacaria, Christian, Bhargava, Yash, Coley, Joel B., Ducci, Lorenzo, Pradhan, Pragati, Ballhausen, Ralf, Fuerst, Felix, Islam, Nazma, Jaisawal, Gaurava K., Jenke, Peter, Kretschmar, Peter, Kreykenbohm, Ingo, Pottschmidt, Katja, Sokolova-Lapa, Ekaterina, Staubert, Rudiger, Wilms, Joern, Wilson-Hodge, Colleen A., and Wolff, Michael T.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Accreting X-ray pulsars (XRPs) undergo luminous X-ray outbursts during which the luminosity-dependent spectral and timing features of the neutron star's emission can be analyzed in detail, thus shedding light on the accretion regime at work. We took advantage of a monitoring campaign performed with NuSTAR, Swift/XRT, AstroSat and NICER, to follow the Be/X-ray Binary 2S 1553-542 along one of its rare outbursts and trace its spectral and timing evolution. We report the discovery of a luminosity-dependent cyclotron line energy for the first time in this source. The pulse profiles and pulsed fraction also show variability along the outburst, consistently with the interpretation that the source transitions from the sub-critical to the super-critical accretion regime, separated by a critical luminosity of L$_{crit}\approx4\times10^{37}$ erg/s., Comment: Accepted on ApJ. 11 pages, 7 figures, 3 tables

Published
2022
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16. Large-scale analysis of sheep rumen metagenome profiles captured by reduced representation sequencing reveals individual profiles are influenced by the environment and genetics of the host

Author

Hess, Melanie K., Hodgkinson, Hannah E., Hess, Andrew S., Zetouni, Larissa, Budel, Juliana C. C., Henry, Hannah, Donaldson, Alistair, Bilton, Timothy P., van Stijn, Tracey C., Kirk, Michelle R., Dodds, Ken G., Brauning, Rudiger, McCulloch, Alan F., Hickey, Sharon M., Johnson, Patricia L., Jonker, Arjan, Morton, Nickolas, Hendy, Shaun, Oddy, V. Hutton, Janssen, Peter H., McEwan, John C., and Rowe, Suzanne J.

Published
2023
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17. Combining host and rumen metagenome profiling for selection in sheep: prediction of methane, feed efficiency, production, and health traits

Author

Hess, Melanie K., Zetouni, Larissa, Hess, Andrew S., Budel, Juliana, Dodds, Ken G., Henry, Hannah M., Brauning, Rudiger, McCulloch, Alan F., Hickey, Sharon M., Johnson, Patricia L., Elmes, Sara, Wing, Janine, Bryson, Brooke, Knowler, Kevin, Hyndman, Dianne, Baird, Hayley, McRae, Kathryn M., Jonker, Arjan, Janssen, Peter H., McEwan, John C., and Rowe, Suzanne J.

Published
2023
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18. Y Tylwyth Teg : an analysis of a literary motif

Author

Rudiger, Angelika and Jones, Aled

Subjects
Tylwyth Teg, Welsh fairy traditions, Welsh literature, Welsh folklore, motifs of Welsh fairy traditions, history of Welsh fairy traditions
Abstract

This thesis has two main parts. Part 1 explores the names used as synonyms for 'Tylwyth Teg', giving an initial insight through semantics into the nature of these supernatural beings, and revealing the relevance of the cultural context of the relevant texts: motifs and tale types from both nineteenth-century folklore and medieval and early modern literature are explored. I ask anew whether the otherworld is identical to hell or a realm of the dead. The importance of folk beliefs related to the denizens of the otherworld for devising an imagery for the process of poetic creativity and for transformational processes will be shown. Part 2 focusses on the historical development of traditions connected with the Tylwyth Teg, a valuable tool for the historian, providing deepened social insight. The study is one of longue durée, covering a period from the Middle Ages onwards, and is a combination of overview and focus. I explore various tensions arising between the use of folklore in creative processes of appropriation, and mechanisms that 'other' the socially disadvantaged. The euhemerization of the fairies during the rivalry of druidic and Celtic traditions at the turn of the eighteenth to the nineteenth century provokes an extended study of John Rhŷs' influential model of British prehistory: I explore how he used social Darwinism to read fairy folklore for political and cultural reasons verging on the nationalist and suggest how the broad traditions of interpretation and recreation manifest themselves in nineteenth-century literature. I take here as specific comparative case studies the prose of Daniel Owen and the poetry of Glasynys, highlighting the contrast between more romantic readings, and the novel ideas originating in Rhŷs. Finally, and more briefly, the theories are pushed in the direction of the present day, with an analysis of the role of fairy traditions in alternative religion, once again performed with special attention to how Rhŷs was appropriated (this time by the feminist goddess movement and neo-pagan syncretism). Appendices gives examples from twentieth century literature which suggest future directions of research.

Published
2022

19. An integrated whispering-gallery-mode resonator for solid-state coherent quantum photonics

Author

Brooks, Arianne, Chu, Xiao-Liu, Liu, Zhe, Schott, Rudiger, Ludwig, Arne, Wieck, Andreas D., Midolo, Leonardo, Lodahl, Peter, and Rotenberg, Nir

Subjects
Quantum Physics
Abstract

Tailored photonic cavities allow enhancing light-matter interaction ultimately to create a fully coherent quantum interface. Here, we report on an integrated microdisk cavity containing self-assembled quantum dots to coherently route photons between different access waveguides. We measure a Purcell factor of $F_{exp}=6.9\pm0.9$ for a cavity quality factor of about 10,000, allowing us to observe clear signatures of coherent scattering of photons by the quantum dots. We show how this integrated system can coherently re-route photons between the drop and bus ports, and how this routing is controlled by detuning the quantum dot and resonator, or through the strength of the excitation beam, where a critical photon number less than one photon per lifetime is required. We discuss the strengths and limitations of this approach, focusing on how the coherent scattering and single-photon nonlinearity can be used to increase the efficiency of quantum devices such as routers or Bell-state analyzers.

Published
2021
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20. Spatially Resolved Star Formation and Inside-out Quenching in the TNG50 Simulation and 3D-HST Observations

Author

Nelson, Erica J., Tacchella, Sandro, Diemer, Benedikt, Leja, Joel, Hernquist, Lars, Whitaker, Katherine E., Weinberger, Rainer, Pillepich, Annalisa, Nelson, Dylan, Terrazas, Bryan A., Nevin, Rebecca, Brammer, Gabriel B., Burkhart, Blakesley, Cochrane, Rachel, van Dokkum, Pieter, Johnson, Benjamin D., Mowla, Lamiya, Pakmor, Rudiger, Skelton, Rosalind E., Speagle, Joshua, Springel, Volker, Torrey, Paul, Vogelsberger, Mark, and Wuyts, Stijn

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We compare the star forming main sequence (SFMS) -- both integrated and resolved on 1kpc scales -- between the high-resolution TNG50 simulation of IllustrisTNG and observations from the 3D-HST slitless spectroscopic survey at z~1. Contrasting integrated star formation rates (SFRs), we find that the slope and normalization of the star-forming main sequence in TNG50 are quantitatively consistent with values derived by fitting observations from 3D-HST with the Prospector Bayesian inference framework. The previous offsets of 0.2-1dex between observed and simulated main sequence normalizations are resolved when using the updated masses and SFRs from Prospector. The scatter is generically smaller in TNG50 than in 3D-HST for more massive galaxies with M_*>10^10Msun, even after accounting for observational uncertainties. When comparing resolved star formation, we also find good agreement between TNG50 and 3D-HST: average specific star formation rate (sSFR) radial profiles of galaxies at all masses and radii below, on, and above the SFMS are similar in both normalization and shape. Most noteworthy, massive galaxies with M_*>10^10.5Msun, which have fallen below the SFMS due to ongoing quenching, exhibit a clear central SFR suppression, in both TNG50 and 3D-HST. In TNG this inside-out quenching is due to the supermassive black hole (SMBH) feedback model operating at low accretion rates. In contrast, the original Illustris simulation, without this same physical SMBH mechanism, does not reproduce the central SFR profile suppression seen in data. The observed sSFR profiles provide support for the TNG quenching mechanism and how it affects gas on kiloparsec scales in the centers of galaxies., Comment: Main results in Figs 1 and 3. The TNG50 data is now fully publicly available at https://www.tng-project.org/

Published
2021
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21. Comparison of downscaling techniques for high resolution soil moisture mapping

Author

Sabaghy, Sabah, Walker, Jeffrey, Renzullo, Luigi, Akbar, Ruzbeh, Chan, Steven, Chaubell, Julian, Das, Narendra, Dunbar, R. Scott, Entekhabi, Dara, Gevaert, Anouk, Jackson, Thomas, Merlin, Olivier, Moghaddam, Mahta, Peng, Jinzheng, Piepmeier, Jeffrey, Piles, Maria, Portal, Gerard, Rudiger, Christoph, Stefan, Vivien, Wu, Xiaoling, Ye, Nan, and Yueh, Simon

Subjects
Physics - Applied Physics
Abstract

Soil moisture impacts exchanges of water, energy and carbon fluxes between the land surface and the atmosphere. Passive microwave remote sensing at L-band can capture spatial and temporal patterns of soil moisture in the landscape. Both ESA and NASA have launched L-band radiometers, in the form of the SMOS and SMAP satellites respectively, to monitor soil moisture globally, every 3-day at about 40 km resolution. However, their coarse scale restricts the range of applications. While SMAP included an L-band radar to downscale the radiometer soil moisture to 9 km, the radar failed after 3 months and this initial approach is not applicable to developing a consistent long term soil moisture product across the two missions anymore. Existing optical-, radiometer-, and oversampling-based downscaling methods could be an alternative to the radar-based approach for delivering such data. Nevertheless, retrieval of a consistent high resolution soil moisture product remains a challenge, and there has been no comprehensive inter-comparison of the alternate approaches. This research undertakes an assessment of the different downscaling approaches using the SMAPEx-4 field campaign data

Published
2020
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22. Deep remembering: A Proustian novelist caught up in the age of extremes

Author

Gorner, Rudiger

Subjects
Ausgewahlte Werke: All Das Vergangene, vol. 1 (Nonfiction work) -- Sperber, Manes -- Stancic, Mirjana, Ausgewahlte Werke: Wie Eine Trane Im Ozean, vol. 2 (Nonfiction work) -- Sperber, Manes -- Isler, Rudolf, Ausgewahlte Werke: Zur Analyse Der Tyrannis, vol. 3 (Nonfiction work) -- Sperber, Manes -- Muller-Funk, Wolfgang, Books -- Book reviews, Literature/writing
Abstract

AUSGEWAHLTE WERKE MANES SPERBER VOLUME 1: ALL DAS VERGANGENE Edited by Mirjana Stancic 692pp. Sonderzahl. 44 [euro]. VOLUME 2: WIE EINE TRANE IM OZEAN Edited by Rudolf Isler 872pp. Sonderzahl. [...]

Published
2024

23. Synthetically Encapsulated \& Self-Organized Transition Metal Oxide Nano Structures inside Carbon Nanotubes as Robust Li-ion Battery Anode Materials

Author

Kapoor, Aakanksha, Patrike, Apurva L., Singh, Nitesh, Thauer, Elisa, Ottmann, Alexander, Klingeler, Rudiger, Ogale, Satishchandra, and Bajpai, A.

Subjects
Condensed Matter - Materials Science, Condensed Matter - Mesoscale and Nanoscale Physics
Abstract

We report a comprehensive study on the electrochemical performance of four different Transition Metal Oxides encapsulated inside carbon nanotubes (CNT). Irrespective of the type of oxide-encapsulate, all these samples exhibit superior cyclic stability as compared to the bare-oxide. Innovative use of camphor during sample synthesis enables precise control over the morphology of these self-organized carbon nanotube structures, which in turn appears to play a crucial role in the magnitude of the specific capacity. A comparative evaluation of the electrochemical data on different samples bring forward interesting inferences pertaining to the morphology, filling fraction of the oxide-encapsulate, and the presence of oxide nano-particles adhering outside the filled CNT. Our results provides useful pointers towards the optimization of critical parameters, thus paving the way for using these synthetically encapsulated and self-organized carbon nanotube structures as anode materials for Li-ion batteries, and possibly other electrochemical applications.

Published
2020

24. Observing the stellar halo of Andromeda in cosmological simulations: the Auriga2PAndAS pipeline

Author

Thomas, Guillaume F., Martin, Nicolas F., Fattahi, Azadeh, Ibata, Rodrigo A., Helly, John, McConnachie, Alan W., Frenk, Carlos, Gomez, Facundo A., Grand, Robert J. J., Gwyn, Stephen, Mackey, Dougal, Marinacci, Federico, and Pakmor, Rudiger

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present a direct comparison of the Pan-Andromeda Archaeological Survey (PAndAS) observations of the stellar halo of M31 with the stellar halos of 6 galaxies from the Auriga simulations. We process the simulated halos through the Auriga2PAndAS pipeline and create PAndAS-like mocks that fold in all observational limitations of the survey data (foreground contamination from the Milky Way stars, incompleteness of the stellar catalogues, photometric uncertainties, etc). This allows us to study the survey data and the mocks in the same way and generate directly comparable density maps and radial density profiles. We show that the simulations are overall compatible with the observations. Nevertheless, some systematic differences exist, such as a preponderance for metal-rich stars in the mocks. While these differences could suggest that M31 had a different accretion history or has a different mass compared to the simulated systems, it is more likely a consequence of an under-quenching of the star formation history of galaxies, related to the resolution of the Auriga simulations. The direct comparison enabled by our approach offers avenues to improve our understanding of galaxy formation as they can help pinpoint the observable differences between observations and simulations. Ideally, this approach will be further developed through an application to other stellar halo simulations. To facilitate this step, we release the pipeline to generate the mocks, along with the six mocks presented and used in this contribution., Comment: Accepted to ApJ; 23 pages, 12 figures. Pipeline available here: https://github.com/GFThomas/Auriga2PAndAS, and mocks here: https://wwwmpa.mpa-garching.mpg.de/auriga/gaiamock.html

Published
2020
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25. Embodied Synaptic Plasticity with Online Reinforcement learning

Author

Kaiser, Jacques, Hoff, Michael, Konle, Andreas, Tieck, J. Camilo Vasquez, Kappel, David, Reichard, Daniel, Subramoney, Anand, Legenstein, Robert, Roennau, Arne, Maass, Wolfgang, and Dillmann, Rudiger

Subjects
Computer Science - Neural and Evolutionary Computing, Computer Science - Artificial Intelligence, Computer Science - Machine Learning, Computer Science - Robotics
Abstract

The endeavor to understand the brain involves multiple collaborating research fields. Classically, synaptic plasticity rules derived by theoretical neuroscientists are evaluated in isolation on pattern classification tasks. This contrasts with the biological brain which purpose is to control a body in closed-loop. This paper contributes to bringing the fields of computational neuroscience and robotics closer together by integrating open-source software components from these two fields. The resulting framework allows to evaluate the validity of biologically-plausibe plasticity models in closed-loop robotics environments. We demonstrate this framework to evaluate Synaptic Plasticity with Online REinforcement learning (SPORE), a reward-learning rule based on synaptic sampling, on two visuomotor tasks: reaching and lane following. We show that SPORE is capable of learning to perform policies within the course of simulated hours for both tasks. Provisional parameter explorations indicate that the learning rate and the temperature driving the stochastic processes that govern synaptic learning dynamics need to be regulated for performance improvements to be retained. We conclude by discussing the recent deep reinforcement learning techniques which would be beneficial to increase the functionality of SPORE on visuomotor tasks., Comment: 18 pages, 5 figures, published in frontiers in neurorobotics

Published
2020
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26. Castration delays epigenetic aging and feminizes DNA methylation at androgen-regulated loci.

Author

Sugrue, Victoria J, Zoller, Joseph Alan, Narayan, Pritika, Lu, Ake T, Ortega-Recalde, Oscar J, Grant, Matthew J, Bawden, C Simon, Rudiger, Skye R, Haghani, Amin, Bond, Donna M, Hore, Reuben R, Garratt, Michael, Sears, Karen E, Wang, Nan, Yang, Xiangdong William, Snell, Russell G, Hore, Timothy A, and Horvath, Steve

Subjects
DNA methylation, aging, androgens, castration, developmental biology, epigenetic clock, genetics, genomics, human, mouse, sheep, Biochemistry and Cell Biology
Abstract

In mammals, females generally live longer than males. Nevertheless, the mechanisms underpinning sex-dependent longevity are currently unclear. Epigenetic clocks are powerful biological biomarkers capable of precisely estimating chronological age and identifying novel factors influencing the aging rate using only DNA methylation data. In this study, we developed the first epigenetic clock for domesticated sheep (Ovis aries), which can predict chronological age with a median absolute error of 5.1 months. We have discovered that castrated male sheep have a decelerated aging rate compared to intact males, mediated at least in part by the removal of androgens. Furthermore, we identified several androgen-sensitive CpG dinucleotides that become progressively hypomethylated with age in intact males, but remain stable in castrated males and females. Comparable sex-specific methylation differences in MKLN1 also exist in bat skin and a range of mouse tissues that have high androgen receptor expression, indicating that it may drive androgen-dependent hypomethylation in divergent mammalian species. In characterizing these sites, we identify biologically plausible mechanisms explaining how androgens drive male-accelerated aging.

Published
2021

28. Aortic valve versus root surgery after failed transcatheter aortic valve replacement

Author

Saha, Shekhar, Hagl, Christian, Kiefer, Philipp, Holzhey, David, Noack, Thilo, Borger, Michael A., Desai, Nimesh D., Bavaria, Joseph E., Voisine, MDPierre, Mohammadi, Siamak, Rodés-Cabau, Josep, Harrington, Katherine B., Squiers, John J., Szerlip, Molly I., DiMaio, J. Michael, Mack, Michael J., Rovin, Joshua, Gennari, Marco, Fukuhara, Shinichi, Deeb, G. Michael, Sengupta, Aditya, Demers, Philippe, Ibrahim, Reda, Wyler von Ballmoos, Moritz, Atkins, Marvin D., Kleiman, Neal S., Reardon, Michael J., Maisano, Francesco, Bhadra, Oliver D., Conradi, Lenard, Shults, Christian, Satler, Lowell F., Waksman, Ron, Pirelli, Luigi, Brinster, Derek R., Algadheeb, Muhanad, Chu, Michael W.A., Bagur, Rodrigo, Ramlawi, Basel, Grubb, Kendra J., Robinson, Newell B., Wang, Lin, Petrossian, George A., Leroux, Lionel, Doty, John R., Whisenant, Brian K., Kempfert, Joerg, Unbehaun, Axel, Rahim, Hussein, Nazif, Tamim M., George, Isaac, Geirsson, Arnar, Forrest, John K., Vincent, Flavien, Van Belle, Eric, Koussa, Mohamad, Goldberg, Joshua B., Ahmad, Hasan A., Ben Ali, Walid, Andreas, Martin, Werner, Paul, Goel, Kashish, Shah, Ashish S., Gelpi, Guido, Ruel, Marc, Al-Atassi, Talal, Van Mieghem, Nicholas M., Hokken, Thijmen W., D'Onofrio, Augusto, Tessari, Chiara, Hirji, Sameer, Shah, Pinak B., Belluschi, Igor, Garatti, Andrea, Bruschi, Giuseppe, Ouzounian, Maral, Pizano, Alejandro, Di Eusanio, Marco, Capestro, Filippo, Taramasso, Maurizio, Colli, Andrea, Estevez-Loureiro, Rodrigo, Pinon, Miguel A., Salinger, Michael H., Di Virgilio, Antonio, Nguyen, Tom C., Lange, Rudiger, Vitanova, Keti, Zaid, Syed, Tang, Gilbert H.L., Kaneko, Tsuyoshi, Bapat, Vinayak N., Modine, Thomas, and Denti, Paolo

Published
2023
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30. On-chip nanomechanical filtering of quantum-dot single-photon sources

Author

Zhou, Xiaoyan, Uppu, Ravitej, Liu, Zhe, Papon, Camille, Schott, Rudiger, Wieck, Andreas D., Ludwig, Arne, Lodahl, Peter, and Midolo, Leonardo

Subjects
Physics - Applied Physics, Physics - Optics, Quantum Physics
Abstract

Semiconductor quantum dots in photonic integrated circuits enable scaling quantum-information processing to many single photons and quantum-optical gates. On-chip spectral filters are essential to achieve high-purity and coherent photon emission from quantum dots embedded in waveguides, without resorting to free-space optics. Such spectral filters should be tunable, to compensate for the inhomogeneous spectral distribution of the quantum dots transitions. Here, we report an on-chip filter monolithically integrated with quantum dots, that uses nanomechanical motion for tuning its resonant wavelength over 10 nm, enabling operation at cryogenic temperatures and avoiding cross-talk with the emitter. We demonstrate single-photon emission from a quantum dot under non-resonant excitation by employing only the on-chip filter. These results are key for the development of fully-integrated de-multiplexing, multi-path photon encoding schemes, and multi-emitter circuits.

Published
2019

32. Satellites of Satellites: The Case for Carina and Fornax

Author

Pardy, Stephen A., D'Onghia, Elena, Navarro, Julio, Grand, Robert, Gomez, Facundo A., Marinacci, Federico, Pakmor, Rudiger, Simpson, Christine, and Springel, Volker

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We use the Auriga cosmological simulations of Milky Way (MW)-mass galaxies and their surroundings to study the satellite populations of dwarf galaxies in $\Lambda$CDM. As expected from prior work, the number of satellites above a fixed stellar mass is a strong function of the mass of the primary dwarf. For galaxies as luminous as the Large Magellanic Cloud (LMC), and for halos as massive as expected for the LMC (determined by its rotation speed), the simulations predict about 3 satellites with stellar masses exceeding $M_*>10^5\, M_\odot$. If the LMC is on its first pericentric passage, then these satellites should be near the LMC and should have orbital angular momenta roughly coincident with that of the LMC. We use 3D positions and velocities from the 2nd data release of the Gaia mission to revisit which of the "classical" MW dwarf spheroidals could plausibly be LMC satellites. The new proper motions of the Fornax and Carina dwarf spheroidals place them on orbits closely aligned with the orbital plane of the Magellanic Clouds, hinting at a potential Magellanic association. Together with the Small Magellanic Cloud (SMC), this result raises to $3$ the number of LMC satellites with $M_*>10^5\, M_\odot$, as expected from simulations. This also fills the 12-mag luminosity gap between the SMC and the ultra-faints Hyi1, Car2, Hor1, and Car3, the few ultra-faint satellites confirmed to have orbits consistent with a Magellanic origin., Comment: 7 pages, 3 figures. Accepted for publication in the Monthly Notices of the Royal Astronomical Society

Published
2019
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33. The local high velocity tail and the Galactic escape speed

Author

Deason, Alis J., Fattahi, Azadeh, Belokurov, Vasily, Evans, Wyn, Grand, Robert J., Marinacci, Federico, and Pakmor, Rudiger

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We model the fastest moving (v_tot > 300 km/s) local (D < 3 kpc) halo stars using cosmological simulations and 6-dimensional Gaia data. Our approach is to use our knowledge of the assembly history and phase-space distribution of halo stars to constrain the form of the high velocity tail of the stellar halo. Using simple analytical models and cosmological simulations, we find that the shape of the high velocity tail is strongly dependent on the velocity anisotropy and number density profile of the halo stars --- highly eccentric orbits and/or shallow density profiles have more extended high velocity tails. The halo stars in the solar vicinity are known to have a strongly radial velocity anisotropy, and it has recently been shown the origin of these highly eccentric orbits is the early accretion of a massive (M_star ~ 10^9 M_Sun) dwarf satellite. We use this knowledge to construct a prior on the shape of the high velocity tail. Moreover, we use the simulations to define an appropriate outer boundary of 2r_200, beyond which stars can escape. After applying our methodology to the Gaia data, we find a local (r_0=8.3 kpc) escape speed of v_esc(r_0) = 528(+24,-25) km/s. We use our measurement of the escape velocity to estimate the total Milky Way mass, and dark halo concentration: M_200,tot = 1.00(+0.31,-0.24) x 10^12 M_Sun, c_200 = 10.9(+4.4,-3.3). Our estimated mass agrees with recent results in the literature that seem to be converging on a Milky Way mass of M_200,tot ~ 10^12 M_Sun., Comment: 13 pages, 10 Figures. MNRAS accepted

Published
2019
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34. First measurement of the Hubble constant from a dark standard siren using the Dark Energy Survey galaxies and the LIGO/Virgo binary-black-hole merger GW170814

Author

The DES Collaboration, the LIGO Scientific Collaboration, the Virgo Collaboration, Soares-Santos, M., Palmese, A., Hartley, W., Annis, J., Garcia-Bellido, J., Lahav, O., Doctor, Z., Fishbach, M., Holz, D. E., Lin, H., Pereira, M. E. S., Garcia, A., Herner, K., Kessler, R., Peiris, H. V., Sako, M., Allam, S., Brout, D., Rosell, A. Carnero, Chen, H. Y., Conselice, C., deRose, J., deVicente, J., Diehl, H. T., Gill, M. S. S., Gschwend, J., Sevilla-Noarbe, I., Tucker, D. L., Wechsler, R., Berger, E., Cowperthwaite, P. S., Metzger, B. D., Williams, P. K. G., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, R. C., Walker, A. R., Wester, W., Zuntz, J., Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Bell, A. S., Beniwal, D., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderon, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglia, M., Cavalieri, R., Cella, G., Cerda-Duran, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chatziioannou, K., Cheeseboro, B. D., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dalya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davis, D., Daw, E. J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Del Pozzo, W., DeMarchi, L. M., Demos, N., Dent, T., De Pietri, R., Derby, J., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., Diaz, M. C., Dietrich, T., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Dmitriev, A., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Giordano, G., Glover, L., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., Gonzalez, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, M. K., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannuksela, O. A., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Vivanco, Francisco Hernandez, Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Hreibi, A., Huerta, E. A., Hughey, B., Hulko, M., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kefelian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnendu, N., Krolak, A., Kuehn, G., Kumar, A., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A., Letendre, N., Levin, Y., Li, J., Li, K. J. L., Li, T. G. F., Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Luck, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., MacInnis, M., Macleod, D. M., Macquet, A., Hernandez, I. Magana, Magana-Sandoval, F., Zertuche, L. Magana, Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCann, J. J., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIver, J., McManus, D. J., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muniz, E. A., Muratore, M., Murray, P. G., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O'Brien, B. D., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., Ormiston, R. G., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Purrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, K., Rosinska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rudiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Santiago, K. A., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schonbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Shao, L., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., ShyamSundar, S., Siellez, K., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepanczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tapai, M., Taracchini, A., Tasson, J. D., Taylor, R., Thies, F., Thomas, M., Thomas, P., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forne, A., Torrie, C. I., Toyra, D., Travasso, F., Traylor, G., Tringali, M. C., Trovato, A., Trozzo, L., Trudeau, R., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van Heijningen, J. V., van der Schaaf, L., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Vicere, A., Viets, A. D., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Wessels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Yvert, M., Zadrozny, A. K., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A., Zucker, M. E., and Zweizig, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a multi-messenger measurement of the Hubble constant H_0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the LIGO/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black-hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black-hole merger. Our analysis results in $H_0 = 75.2^{+39.5}_{-32.4}~{\rm km~s^{-1}~Mpc^{-1}}$, which is consistent with both SN Ia and CMB measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20,140] ${\rm km~s^{-1}~Mpc^{-1}}$, and it depends on the assumed prior range. If we take a broader prior of [10,220] ${\rm km~s^{-1}~Mpc^{-1}}$, we find $H_0 = 78^{+ 96}_{-24}~{\rm km~s^{-1}~Mpc^{-1}}$ ($57\%$ of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on $H_0$., Comment: 18 pages, 2 Figures, submitted to ApJL

Published
2019
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35. DNA methylation study of Huntington's disease and motor progression in patients and in animal models.

Author

Lu, Ake T, Narayan, Pritika, Grant, Matthew J, Langfelder, Peter, Wang, Nan, Kwak, Seung, Wilkinson, Hilary, Chen, Richard Z, Chen, Jian, Simon Bawden, C, Rudiger, Skye R, Ciosi, Marc, Chatzi, Afroditi, Maxwell, Alastair, Hore, Timothy A, Aaronson, Jeff, Rosinski, Jim, Preiss, Alicia, Vogt, Thomas F, Coppola, Giovanni, Monckton, Darren, Snell, Russell G, William Yang, X, and Horvath, Steve

Subjects
Animals, Animals, Genetically Modified, Sheep, Humans, Mice, Huntington Disease, Disease Models, Animal, Disease Progression, Recombinant Proteins, Severity of Illness Index, Registries, Longitudinal Studies, Follow-Up Studies, Prospective Studies, Cross-Sectional Studies, Behavior, Animal, DNA Methylation, Epigenesis, Genetic, CpG Islands, Mutation, Adolescent, Adult, Aged, Aged, 80 and over, Middle Aged, Female, Male, Genome-Wide Association Study, Young Adult, Gene Knock-In Techniques, Genetic Loci, Huntingtin Protein, Global Burden of Disease, Genetically Modified, Disease Models, Animal, Behavior, Epigenesis, Genetic, and over
Abstract

Although Huntington's disease (HD) is a well studied Mendelian genetic disorder, less is known about its associated epigenetic changes. Here, we characterize DNA methylation levels in six different tissues from 3 species: a mouse huntingtin (Htt) gene knock-in model, a transgenic HTT sheep model, and humans. Our epigenome-wide association study (EWAS) of human blood reveals that HD mutation status is significantly (p

Published
2020

43. Better Crop-Livestock Integration for Enhanced Agricultural System Resilience and Food Security in the Changing Climate: Case Study from Low-Rainfall Areas of North Africa

Author

Devkota, Mina, Frija, Aymen, Dhehibi, Boubaker, Rudiger, Udo, Alary, Veronique, M’hamed, Hatem Cheikh, Louahdi, Nasreddine, Idoudi, Zied, Rekik, Mourad, Behnassi, Mohamed, editor, Baig, Mirza Barjees, editor, Sraïri, Mohamed Taher, editor, Alsheikh, Abdlmalek A., editor, and Abu Risheh, Ali Wafa A., editor

Published
2022
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45. Surgical Explantation of Failed Transcatheter Aortic Valve Replacement

Author

Saha, Shekhar, Kiefer, Philipp, Holzhey, David, Noack, Thilo, Voisine, Pierre, Mohammadi, Siamak, Harrington, Katherine B., Squiers, John J., Fukuhara, Shinichi, von Ballmoos, Moritz Wyler, Goel, Sachin S., Atkins, Marvin D., Bhadra, Oliver D., Conradi, Lenard, Shults, Christian, Satler, Lowell F., Pirelli, Luigi, Brinster, Derek R., Algadheeb, Muhanad, Chu, Michael W.A., Bagur, Rodrigo, Ramlawi, Basel, Grubb, Kendra J., Desai, Nimesh D., Robinson, Newell B., Wang, Lin, Petrossian, George A., Leroux, Lionel, Doty, John R., Kempfert, Joerg, Unbehaun, Axel, Rahim, Hussein, Geirsson, Arnar, Forrest, John K., Vincent, Flavien, Van Belle, Eric, Koussa, Mohamad, Goldberg, Joshua B., Ahmad, Hasan A., Ben Ali, Walid, Demers, Philippe, Ibrahim, Reda, Andreas, Martin, Werner, Paul, Goel, Kashish, Shah, Ashish S., Gelpi, Guido, Ruel, Marc, Al-Atassi, Talal, Van Mieghem, Nicholas M., Hokken, Thijmen W., D'Onofrio, Augusto, Tessari, Chiara, Shah, Pinak B., Belluschi, Igor, Garatti, Andrea, Bruschi, Giuseppe, Ouzounian, Maral, Pizano, Alejandro, Di Eusanio, Marco, Capestro, Filippo, Rovin, Joshua, Taramasso, Maurizio, Gennari, Marco, Colli, Andrea, Estevez-Loureiro, Rodrigo, Pinon, Miguel A., Salinger, Michael H., Di Virgilio, Antonio, Whisenant, Brian K., Nazif, Tamim M., Kleiman, Neal S., Szerlip, Molly I., Waksman, Ron, Rodés-Cabau, Josep, George, Isaac, DiMaio, J. Michael, Maisano, Francesco, Deeb, G. Michael, Vitanova, Keti, Lange, Rudiger, Borger, Michael A., Hagl, Christian, Bavaria, Joseph E., Zaid, Syed, Hirji, Sameer A., Bapat, Vinayak N., Denti, Paolo, Modine, Thomas, Nguyen, Tom C., Mack, Michael J., Reardon, Michael J., Kaneko, Tsuyoshi, and Tang, Gilbert H.L.

Published
2023
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46. Subhalo destruction in the Apostle and Auriga simulations

Author

Richings, Jack, Frenk, Carlos, Jenkins, Adrian, Robertson, Andrew, Fattahi, Azadeh, Grand, Robert J. J., Navarro, Julio, Pakmor, Rudiger, Gomez, Facundo A., and Marinacci, Federico

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

N-body simulations make unambiguous predictions for the abundance of substructures within dark matter halos. However, the inclusion of baryons in the simulations changes the picture because processes associated with the presence of a large galaxy in the halo can destroy subhalos and substantially alter the mass function and velocity distribution of subhalos. We compare the effect of galaxy formation on subhalo populations in two state-of-the-art sets of hydrodynamical CDM simulations of Milky Way mass halos, APOSTLE and AURIGA. We introduce a new method for tracking the orbits of subhalos between simulation snapshots that gives accurate results down to a few kiloparsecs from the centre of the halo. Relative to a dark matter-only simulation, the abundance of subhalos in APOSTLE is reduced by 50% near the centre and by 10% within r200. In AURIGA the corresponding numbers are 80% and 40%. The velocity distributions of subhalos are also affected by the presence of the galaxy, much more so in AURIGA than in APOSTLE . The differences on subhalo properties in the two simulations can be traced back to the mass of the central galaxies, which in AURIGA are typically twice as massive as those in APOSTLE . We show that some of the results from previous studies are inaccurate due to systematic errors in the modelling of subhalo orbits near the centre of halos., Comment: Submitted to MNRAS

Published
2018
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47. Search for Multi-messenger Sources of Gravitational Waves and High-energy Neutrinos with Advanced LIGO during its first Observing Run, ANTARES and IceCube

Author

ANTARES, IceCube, LIGO, Collaborations, Virgo, Albert, A., Andre, M., Anghinolfi, M., Ardid, M., Aubert, J. -J., Aublin, J., Avgitas, T., Baret, B., Barrios-Marti, J., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bormuth, R., Boumaaza, J., Bourret, S., Bouwhuis, M. C., Brânzas, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chabab, M., Moursli, R. Cherkaoui El, Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Colomer, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Diaz, A. F., Deschamps, A., Distefano, C., Di Palma, I., Domi, A., Dona, R., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., Bojaddaini, I. El, Khayati, N. El, Elsasser, D., Enzenhofer, A., Ettahiri, A., Fassi, F., Felis, I., Fermani, P., Ferrara, G., Fusco, L., Gay, P., Glotin, H., Gregoire, T., Ruiz, R. Gracia, Graf, K., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Hol, J., Hofestadt, J., Illuminati, G., de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefevre, D., Leonora, E., Levi, G., Lotze, M., Loucatos, S., Maggi, G., Marcelin, M., Margiotta, A., Marinelli, A., Martinez-Mora, J. A., Mele, R., Melis, K., Migliozzi, P., Moussa, A., Navas, S., Nezri, E., Nunez, A., Organokov, M., Pavalas, G. E., Pellegrino, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Randazzo, N., Riccobene, G., Sanchez-Losa, A., Saldana, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schussler, F., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Vallage, B., Van Elewyck, V., Versari, F., Vivolo, D., Wilms, J., Zaborov, D., Zornoza, J. D., Zuniga, J., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Arguelles, C., Auffenberg, J., Axani, S., Backes, P., Bagherpour, H., Bai, X., Barbano, A., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Becker, K. -H., BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Borner, M., Bos, F., Boser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brenzke, M., Bretz, H. -P., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Clark, K., Classen, L., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., de Andre, J. P. A. M., De Clercq, C., DeLaunay, J. J., Dembinski, H., Deoskar, K., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Diaz-Velez, J. C., di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Ganster, E., Garrappa, S., Gerhardt, L., Ghorbani, K., Giang, W., Glauch, T., Glusenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Hallgren, A., Halve, L., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hunnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Kopke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Kruckl, G., Kunwar, S., Kurahashi, N., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Leuermann, M., Liu, Q. R., Lohfink, E., Mariscal, C. J. Lozano, Lu, L., Lunemann, J., Luszczak, W., Madsen, J., Mahn, K. B. M., Makino, Y., Mancina, S., Maris, I. C., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momente, G., Montaruli, T., Moore, R. W., Moulai, M., Nagai, R., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Pepper, J. A., Heros, C. Perez de los, Pieloth, D., Pinat, E., Pizzuto, A., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Renzi, G., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schaufel, M., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schoneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stol, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Tonnis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Ty, B., Unger, E., Elorrieta, M. A. Unland, Usner, M., Vandenbroucke, J., Van Driessche, W., van Eijk, D., van Eijndhoven, N., Vanheule, S., van Santen, J., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandler, F. D., Wandkowsky, N., Watson, T. B., Waza, A., Weaver, C., Weiss, M. J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woolsey, E., Woschnagg, K., Wrede, G., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, z P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderon, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cerda-Duran, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dalya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Del Pozzo, W., DeMarchi, L. M., Demos, N., Dent, T., Denys, M., De Pietri, R., Derby, J., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., Diaz, M. C., Dietrich, T., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Renzo, F., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia, A., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. 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Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Astrophysical sources of gravitational waves, such as binary neutron star and black hole mergers or core-collapse supernovae, can drive relativistic outflows, giving rise to non-thermal high-energy emission. High-energy neutrinos are signatures of such outflows. The detection of gravitational waves and high-energy neutrinos from common sources could help establish the connection between the dynamics of the progenitor and the properties of the outflow. We searched for associated emission of gravitational waves and high-energy neutrinos from astrophysical transients with minimal assumptions using data from Advanced LIGO from its first observing run O1, and data from the ANTARES and IceCube neutrino observatories from the same time period. We focused on candidate events whose astrophysical origin could not be determined from a single messenger. We found no significant coincident candidate, which we used to constrain the rate density of astrophysical sources dependent on their gravitational wave and neutrino emission processes., Comment: 20 pages, 2 figures

Published
2018
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48. The origin of galactic metal-rich stellar halo components with highly eccentric orbits

Author

Fattahi, Azadeh, Belokurov, Vasily, Deason, Alis J., Frenk, Carlos S., Gomez, Facundo A., Grand, Robert J. J., Marinacci, Federico, Pakmor, Rudiger, and Springel, Volker

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Using the astrometry from the ESA's Gaia mission, previous works have shown that the Milky Way stellar halo is dominated by metal-rich stars on highly eccentric orbits. To shed light on the nature of this prominent halo component, we have analysed 28 Galaxy analogues in the Auriga suite of cosmological hydrodynamics zoom-in simulations. Some three quarters of the Auriga galaxies contain significant components with high radial velocity anisotropy, beta > 0.6. However, only in one third of the hosts do the high-beta stars contribute significantly to the accreted stellar halo overall, similar to what is observed in the Milky Way. For this particular subset we reveal the origin of the dominant stellar halo component with high metallicity, [Fe/H]~-1, and high orbital anisotropy, beta>0.8, by tracing their stars back to the epoch of accretion. It appears that, typically, these stars come from a single dwarf galaxy with a stellar mass of order of 10^9-10^10 Msol that merged around 6-10 Gyr ago, causing a sharp increase in the halo mass. Our study therefore establishes a firm link between the excess of radially anisotropic stellar debris in the Milky Way halo and an ancient head-on collision between the young Milky Way and a massive dwarf galaxy, Comment: replaced with the accepted version (very minor changes)

Published
2018
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49. Ingredients for 21cm intensity mapping

Author

Villaescusa-Navarro, Francisco, Genel, Shy, Castorina, Emanuele, Obuljen, Andrej, Spergel, David N., Hernquist, Lars, Nelson, Dylan, Carucci, Isabella P., Pillepich, Annalisa, Marinacci, Federico, Diemer, Benedikt, Vogelsberger, Mark, Weinberger, Rainer, and Pakmor, Rudiger

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

[Abridged] We study the abundance and clustering properties of HI at redshifts $z\leqslant5$ using TNG100, a large state-of-the-art magneto-hydrodynamic simulation of a 75 Mpc/h box size. We show that most of the HI lies within dark matter halos and quantify the average HI mass hosted by halos of mass M at redshift z. We find that only halos with circular velocities larger than $\simeq$ 30 km/s contain HI. While the density profiles of HI exhibit a large halo-to-halo scatter, the mean profiles are universal across mass and redshift. The HI in low-mass halos is mostly located in the central galaxy, while in massive halos is concentrated in the satellites. We show that the HI and matter density probability distribution functions differ significantly. Our results point out that for small halos the HI bulk velocity goes in the same direction and has the same magnitude as the halo peculiar velocity, while in large halos differences show up. We find that halo HI velocity dispersion follows a power-law with halo mass. We find a complicated HI bias, with HI becoming non-linear already at $k=0.3$ h/Mpc at $z\gtrsim3$. Our simulation reproduces the DLAs bias value from observations. We find that the clustering of HI can be accurately reproduced by perturbative methods. We identify a new secondary bias, by showing that the clustering of halos depends not only on mass but also on HI content. We compute the amplitude of the HI shot-noise and find that it is small at all redshifts. We study the clustering of HI in redshift-space, and show that linear theory can explain the ratio between the monopoles in redshift- and real-space down to small scales at high redshift. We find that the amplitude of the Fingers-of-God effect is larger for HI than for matter. We point out that accurate 21 cm maps can be created from N-body or approximate simulations rather than full hydrodynamic simulations., Comment: 41 pages. 30 figures. Analysis tools publicly available at https://github.com/franciscovillaescusa/Pylians/tree/master/HI_Illustris

Published
2018
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50. Query Shortest Paths Amidst Growing Discs

Author

Nouri, Arash and Sack, Jorg-Rudiger

Subjects
Computer Science - Data Structures and Algorithms
Abstract

The determination of collision-free shortest paths among growing discs has previously been studied for discs with fixed growing rates. Here, we study a more general case of this problem, where: (1) the speeds at which the discs are growing are polynomial functions of degree $\dd$, and (2) the source and destination points are given as query points. We show how to preprocess the $n$ growing discs so that, for two given query points $s$ and $d$, a shortest path from $s$ to $d$ can be found in $O(n^2 \log (\dd n))$ time. The preprocessing time of our algorithm is $O(n^2 \log n + k \log k)$ where $k$ is the number of intersections between the growing discs and the tangent paths (straight line paths which touch the boundaries of two growing discs). We also prove that $k \in O(n^3\dd)$.

Published
2018

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