bluuebunny/crossref_metadata_2025 huggingface dataset:
RELIGION IN THE EARLY REPUBLIC: A SECOND TOM PAINE EFFECT
Authors: NOLL MARK A.
Published: October 2016

Tom Paine, it turns out, may have done almost as much to shape public discourse in the early national period of the United States as he did in moving aggrieved colonists to take up arms against King George III in the Revolutionary period. As historians have documented time and again, the arguments in Paine'sCommon Sense(1776), especially “On Monarchy and Hereditary Succession,” worked as an elixir to transform mixed opinions about dealing with Parliamentary overreach into an unalloyed determination to throw off the king. The four books reviewed here point to the same sort of conclusion about the importance of Paine'sThe Age of Reason, published in two parts in 1794 and 1795 and then reprinted almost as often over the next few years asCommon Sensehad been at the outset of the War of Independence. With the latter work, however, Paine accomplished more through the opposition he generated than by the readers he convinced. Although a few doughty Loyalists had ventured to take onCommon Sense, that opposition was as nothing compared to the groundswell of denunciation that arose in the 1790s to defuse what Americans of many stripes considered Paine's incendiary provocations. Thoroughly researched and persuasively argued monographs from Eric Schlereth, Jonathan Den Hartog, and Sam Haselby provide, in effect, an account of whyThe Age of Reasoncaused such a stir, how those who regarded its arguments as threatening damnation for individuals and poison for the republic mobilized for their own counterpurposes, and then what resulted from the ambiguous success that this mobilization achieved.
THE CHIEF END OF MAN AT PRINCETON: THE RISE OF GENDERED MORAL FORMATION IN AMERICAN HIGHER EDUCATION
Authors: Turpin Andrea L.
Published: October 2016

During the decades around 1900, changing intellectual currents and the creation of the research university led American colleges and universities to alter the role of religion in students' education. Simultaneously, women matriculated in large numbers for the first time, forcing individual institutions to ask whether and how to incorporate them. Using the lens of all-male Princeton University, this article explores how these two trends combined to help instill gender ideals in the Progressive Era male elite. Princeton sought to attract an elite constituency by no longer seeking to inculcate in students simply moral excellence in general, but rather traits associated with prominent men specifically. Princeton's leaders reinforced this gendered moral formation as they shifted from evangelical spirituality focused on relating rightly to God to modernist spirituality focused on relating rightly to the human community. That students embraced these changes suggests that a new approach to moral formation at prominent men's colleges—and coeducational universities that copied their approach—may help explain why, in an era when women could first access an education equal to men's, educated men nevertheless continued to see themselves as uniquely suited for certain public leadership roles by virtue of their sex.
An Overview of Inside-Out Planet Formation
Authors: Tan Jonathan C. , Chatterjee Sourav , Hu Xiao , Zhu Zhaohuan , Mohanty Subhanjoy
Published: October 2016

TheKepler-discovered Systems with Tightly-packed Inner Planets (STIPs), typically with several planets of Earth to super-Earth masses on well-aligned, sub-AU orbits may host the most common type of planets, including habitable planets, in the Galaxy. They pose a great challenge for planet formation theories, which fall into two broad classes: (1) formation further out followed by inward migration; (2) formationin situ, in the very inner regions of the protoplanetary disk. We review the pros and cons of these classes, before focusing on a new theory of sequentialin situformation from the inside-out via creation of successive gravitationally unstable rings fed from a continuous stream of small (~cm-m size) “pebbles,” drifting inward via gas drag. Pebbles first collect at the pressure trap associated with the transition from a magnetorotational instability (MRI)-inactive (“dead zone”) region to an inner, MRI-active zone. A pebble ring builds up that begins to dominate the local mass surface density of the disk and spawns a planet. The planet continues to grow, most likely by pebble accretion, until it becomes massive enough to isolate itself from the accretion flow via gap opening. This reduces the local gas density near the planet, leading to enhanced ionization and a retreat of the dead zone inner boundary. The process repeats with a new pebble ring gathering at the new pressure maximum associated with this boundary. We discuss the theory's predictions for planetary masses, relative mass scalings with orbital radius, and minimum orbital separations, and their comparison with observed systems. Finally, we discuss open questions, including potential causes of diversity of planetary system architectures, i.e., STIPs versus Solar System analogs.
Planet migration and magnetic torques
Authors: Strugarek A. , Brun A. S. , Matt S. P. , Reville V.
Published: October 2016

The possibility that magnetic torques may participate in close-in planet migration has recently been postulated. We develop three dimensional global models of magnetic star-planet interaction under the ideal magnetohydrodynamic (MHD) approximation to explore the impact of magnetic topology on the development of magnetic torques. We conduct twin numerical experiments in which only the magnetic topology of the interaction is altered. We find that magnetic torques can vary by roughly an order of magnitude when varying the magnetic topology from an aligned case to an anti-aligned case. Provided that the stellar magnetic field is strong enough, we find that magnetic migration time scales can be as fast as ~100 Myr. Hence, our model supports the idea that magnetic torques may participate in planet migration for some close-in star-planet systems.
The AURA Observatory in Chile—part of the IAU/UNESCO Extended Case Study
Authors: Smith Malcolm G. , Smith R. Chris , Sanhueza Pedro
Published: October 2016

Brief report. The Extended Case Study for AURA-O as a “Window to the Universe” (http://www2.astronomicalheritage.net/index.php/show-entity?identity=000059&idsub-entity=005) was prepared in the context of supporting the desire to preserve humanity's scientific/cultural heritage of outstanding, high-mountain, ground-based, observatory sites developed over the period 1870–2000.
Advances in the Kepler Transit Search Engine
Authors: Jenkins Jon M.
Published: October 2016

Twenty years ago, no planets were known outside our own solar system. Since then, the discoveries of ~1500 exoplanets have radically altered our views of planets and planetary systems. This revolution is due in no small part to the Kepler Mission, which has discovered >1000 of these planets and >4000 planet candidates. While Kepler has shown that small rocky planets and planetary systems are quite common, the quest to find Earth's closest cousins and characterize their atmospheres presses forward with missions such as NASA Explorer Program's Transiting Exoplanet Survey Satellite (TESS) slated for launch in 2017 and ESA's PLATO mission scheduled for launch in 2024.

These future missions pose daunting data processing challenges in terms of the number of stars, the amount of data, and the difficulties in detecting weak signatures of transiting small planets against a roaring background. These complications include instrument noise and systematic effects as well as the intrinsic stellar variability of the subjects under scrutiny. In this paper we review recent developments in the Kepler transit search pipeline improving both the yield and reliability of detected transit signatures.

Many of the phenomena in light curves that represent noise can also trigger transit detection algorithms. The Kepler Mission has expended great effort in suppressing false positives from its planetary candidate catalogs. Over 18,000 transit-like signatures can be identified for a search across 4 years of data. Most of these signatures are artifacts, not planets. Vetting all such signatures historically takes several months' effort by many individuals. We describe the application of machine learning approaches for the automated vetting and production of planet candidate catalogs. These algorithms can improve the efficiency of the human vetting effort as well as quantifying the likelihood that each candidate is truly a planet. This information is crucial for obtaining valid planet occurrence rates. Machine learning approaches may prove to be critical to the success of future missions such as TESS and PLATO.
Combining Transit and Radial Velocity Data
Authors: Rogers Leslie A.
Published: October 2016

The Kepler Mission, combined with ground based radial velocity (RV) follow-up, has revolutionized the observational constraints on sub-Neptune-size planet compositions. Kepler's unprecedentedly large and homogeneous samples of planets with both mass and radius constraints open the possibility of statistical studies of the underlying planet composition distribution. This presentation describes the application of hierarchical Bayesian models to constrain the underlying planet composition distribution from a sample of noisy mass-radius measurements. This approach represents a promising avenue toward a quantitative measurement of the amount of physical scatter in small planet compositions, the identification of planet sub-populations that may be tied to distinct formation pathways, and empirical constraints on the dominant compositional trends in the planet sample. Both the transit and radial velocity techniques are subject to selection effects, and approaches to mitigate the resulting biases will be addressed. In addition to distilling composition-distribution insights from the current sample of Kepler planets with RV masses, this framework may be used to optimize the target selection for future transiting planet RV follow-up surveys.
Comet composition and Lab
Authors: Bockelée-Morvan Dominique
Published: October 2016

The XXIX IAU General Assembly took place during the golden year of the exploration of small solar system bodies. With the Rosetta ESA mission around comet 67P, NASA Dawn and New Horizons missions nearby dwarf planets Ceres and Pluto, respectively, and the NASA/Cassini mission in Saturn neighborhood, year 2015 marked an important step towards further understanding of small solar system bodies. On August 11-13, Focus meeting 9 "Highlights in the exploration of small worlds" gathered scientists of all over the world to present and discuss the spectacular results obtained from these missions, as well as recent achievements obtained from past missions, comprehensive spectroscopic surveys from space (e.g., Herschel, NEOWISE, Gaia), ground-based observations, and geochemical analyses. This meeting was also the opportunity to discuss the state of our understanding of the nature of the various populations of small bodies in the Solar System, including icy satellites, in a cosmo-chemistry perspective.
Measuring the Distribution and Excitation of Cometary CH3OH Using ALMA
Authors: Cordiner M. A. , Charnley S. B. , Mumma M. J. , Bockelée-Morvan D. , Biver N. , Villanueva G. , Paganini L. , Milam S. N. , Remijan A. J. , Lis D. C. , Crovisier J. , Boissier J. , Kuan Y.-J. , Coulson I. M.
Published: October 2016

The Atacama Large Millimeter/submillimeter Array (ALMA) was used to obtain measurements of spatially and spectrally resolved CH3OH emission from comet C/2012 K1 (PanSTARRS) on 28-29 June 2014. Detection of 12-14 emission lines of CH3OH on each day permitted the derivation of spatially-resolved rotational temperature profiles (averaged along the line of sight), for the innermost 5000 km of the coma. On each day, the CH3OH distribution was centrally peaked and approximately consistent with spherically symmetric, uniform outflow. The azimuthally-averaged CH3OH rotational temperature (Trot) as a function of sky-projected nucleocentric distance (ρ), fell by about 40 K between ρ= 0 and 2500 km on 28 June, whereas on 29 June,Trotfell by about 50 K between ρ =0 km and 1500 km. A remarkable (~50 K) rise inTrotat ρ = 1500-2500 km on 29 June was not present on 28 June. The observed variations in CH3OH rotational temperature are interpreted primarily as a result of variations in the coma kinetic temperature due to adiabatic cooling, and heating through Solar irradiation, but collisional and radiative non-LTE excitation processes also play a role.
The THS experiment: Simulating Titan's atmospheric chemistry at low temperature (200 K)
Authors: Sciamma-O'Brien Ella , Upton Kathleen T. , Beauchamp Jack L. , Salama Farid
Published: October 2016

In the Titan Haze Simulation (THS) experiment, Titan's atmospheric chemistry is simulated by plasma discharge in the stream of a supersonic expansion, i.e. at low Titan-like temperature (150 K). Here, we present complementary gas and solid phase analyses of four N2-CH4-based gas mixtures that demonstrate the unique capability of the THS to monitor the chemical growth evolution in order to better understand Titan's chemistry and the origin of aerosol formation.
Underground Nuclear Astrophysics in China
Authors: WeiPing Liu ,   for JUNA collaboration
Published: October 2016

Underground Nuclear Astrophysics in China (JUNA) will take the advantage of the ultra-low background in Jinping underground lab. High current accelerator with an ECR source and detectors will be set up. We plan to study directly a number of nuclear reactions important to hydrostatic stellar evolution at their relevant stellar energies, such as 25Mg(p,γ)26Al, 19F(p,α)16O, 13C(α,n)16O and 12C(α,γ)16O.
MACHETE: A transit Imaging Atmospheric Cherenkov Telescope to survey half of the Very High Energy γ-ray sky
Authors: López-Coto Rubén , Cortina Juan , Moralejo Abelardo
Published: October 2016

Current Cherenkov Telescopes for VHE gamma ray astrophysics are pointing instruments with a field of view up to a few tens of deg2. We propose to build an array of two non-steerable telescopes with a FoV of 5×60 deg2 oriented along the meridian. Roughly half of the sky drifts through this FoV in a year. We have performed a MC simulation to estimate the performance of this instrument, which we dub MACHETE. The sensitivity that MACHETE would achieve after 5 years of operation for every source in this half of the sky is comparable to the sensitivity that a current IACT achieves for a specific source after a 50 h devoted observation. The analysis energy threshold would be 150 GeV and the angular resolution 0.1 deg. For astronomical objects that transit over MACHETE for a specific night, it would achieve an integral sensitivity of 12% of Crab in a night. This makes MACHETE a powerful tool to trigger observations of variable sources at VHE or any other wavelengths.
An Evidence-Based Framework to Optimise Social Impact in Astronomy for Development
Authors: Grant Eli
Published: October 2016

Astronomy for development projects conceive of development in very broad terms and seek to affect a wide range of social outcomes. The histories of education, development economics and science communication research indicate that positive social impacts are often difficult to achieve. Without a scientific approach, astronomy's potential as a tool for development may never be realised nor recognised. Evidence-informed project design increases the chances of a project's success and likely impact while reducing the risk of unintended negative outcomes. The IAU Office of Astronomy for Development (OAD) Impact Cycle is presented here as a possible framework for integrating evaluation and evidence-based practice in global Astronomy outreach and education delivery. The suggested framework offers a way to gradually accumulate knowledge about which approaches are effective and which are not, enabling the astronomy community to gradually increase its social impact by building on its successes.
GalileoMobile, sharing astronomy with students and teachers around the world
Authors: Benitez-Herrera Sandra , Spinelli Patricia F.
Published: October 2016

GalileoMobile is a non-profit, itinerant, science outreach initiative that brings Astronomy closer to young people in areas with little or no access to outreach programs. We perform astronomy-related activities in schools and communities we visit and encourage follow-up activities through teacher training workshops and the donation of telescopes and other educational resources. GalileoMobile also extends its impact to a worldwide audience through deliverable products. Our work is shared worldwide through the production of documentaries, books and a wide range of Internet resources (OfficialWebsite - www.galileo-mobile.org - and Blog, Facebook page, Google+,Twitter, Youtube and Vimeo). GalileoMobile is an unprecedented initiative promoting science knowledge and the interaction beyond borders through Astronomy while raising awareness for the diversity of human cultures, conveying the message of “unity under the same sky”. We take advantage of the local astronomical culture of the visited communities to establish a dialogue between different ways of understanding the world and to share different types of knowledge (historic, scientific, anthropological . . .), encouraging a process of mutual learning.
Star Parties in Mexico extended to Colombia and China
Authors: Torres-Peimbert Silvia , Franco José
Published: October 2016

The preparation for The International Year of Astronomy 2009 stirred our interest in preparing star parties in Mexico. The lunar eclipse of February 20th 2008 was the perfect event for the first massive observation in Mexico City that attracted over 25,000 people. To accompany this event there were additional attractions: a massive astronomical lecture, more than 100 telescopes were set up for people to watch the sky, exhibits of astronomical images, children hands-on projects, rock concert, dance performance, and chats with astronomers. Already in 2009 a collective program was organized to involve more than 30 sites in Mexico to hold star parties at the same time once a year. These star parties were more in the spirit of science fairs, that include lectures, astronomy exhibits, children projects, as well as concerts and other cultural displays. The scope of each one of them depended on the local support from volunteers and from the local authorities. After the International Year of Astronomy the group that organized these star parties decided to continue its activities. The main attraction in these fairs has been the opportunity to see the Moon, Jupiter and Saturn (if observable) through a telescope. For this program the presence of the amateur astronomers has been crucial. They have brought their instruments to the sites and have generously taught the public how to look through the telescopes and pointed out to the interesting features on the sky.
Southern African Office of Astronomy for Development: A New Hub for Astronomy for Development
Authors: Mutondo Moola S. , Simpemba Prospery
Published: October 2016

A new Astronomy for Development hub needs innovative tools and programs. SAROAD is developing exciting tools integrating Raspberry Pi technology to bring cost-effective astronomy content to learning centres. SAROAD would also like to report achievements in realizing the IAU's strategic plan. In order to manage, evaluate and coordinate regional IAU (International Astronomical Union) capacity building programmes, including the recruitment and mobilization of volunteers, SAROAD has built an intranet that is accessible to regional members upon request. Using this resource, regional members can see and participate in regional activities. SAROAD has commenced with projects in the three Task Force areas of Universities and Research, Children and Schools and Public Outreach. Under the three Task Force areas, a total of seven projects have commenced in Zambia (some supported by funds from IAU Annual Call for proposals).
IAU South West Asian ROAD
Authors: Mickaelian Areg , Azatyan Naira , Farmanyan Sona , Mikayelyan Gor
Published: October 2016

Armenia is hosting the IAU South West Asian (SWA) Regional Office of Astronomy for Development (ROAD). It is a county of ancient astronomy and is also rich in modern astronomical facilities and infrastructures, hence may successfully serve as a regional center for various activities. Byurakan Astrophysical Observatory (BAO) has 2.6m and 1m Schmidt, as well as a number of smaller telescopes that are an observational basis for joint projects and collaborations. Armenian Virtual Observatory (ArVO) is hosting astronomical databases, such as the Digitized First Byurakan Survey (DFBS) and may also serve as a basis for development of VO structures in this region. Recently we have conducted a number of new activities; a meeting on “Relation of Astronomy to other Sciences, Culture and Society" (RASCS) was organized by BAO and Armenian Astronomical Society (ArAS) in Oct 2014 in Byurakan. Activities related to Archaeoastronomy and Astronomy in Culture (AAC) were initiated as well. Discussions on future Armenian-Iranian collaboration in astronomy were carried out, including an Armenian-Iranian Astronomical Workshop held in Oct 2015 in Byurakan. Similar workshops have been carried out between BAO and Abastumani Astronomical Observatory (AbAO, Georgia) since 1974.
The Planetary Nebula Luminosity Function and its Issues
Authors: Ciardullo Robin
Published: October 2016

The bright-end cutoff of the [O III] λ5007 planetary nebula luminosity function (PNLF) is insensitive to population age and metallicity, making it an excellent extragalactic standard candle. We review our knowledge of the function and discuss the challenges related to modeling it. We show that, while there has been a great deal of progress in understanding the nuances of its shape, there is still no solid theory which explains the luminosity of the PNLF cutoff in old stellar populations. This is an extremely serious problem, as it affects a myriad of astrophysical issues, from the determination of the stellar masses of galaxies to our understanding of alternative channels of stellar evolution.
Using SOFIA for Stellar Physics Studies
Authors: Sankrit Ravi
Published: October 2016

The Stratospheric Observatory for Infrared Astronomy (SOFIA) operates in the 0.3–240 micron wavelength region, and offers imaging, polarimetric and high-resolution spectroscopic capabilities that can be used for a wide range of observations relevant for stellar physics studies. We summarize the advantages of using SOFIA, list some of the studies related to stellar physics that have been accomplished, and provide an example high-resolution spectrum of a red supergiant.
Modeling the early-time spectra of core-collapse supernovae
Authors: Groh Jose H.
Published: October 2016

Core-collapse supernovae (SNe) are the final act in the evolution of stars more massive than about 8–9 solar masses. Determining the progenitors of these explosive events and how massive stars are linked to the different SN types are topics of major significance for several fields of astrophysics. Recent progress in observational techniques now allow for rapid-response spectroscopic observations of SNe within a day of detection Gal-Yam et al. (2014). This allows the study of early phases when the SN shock front has not yet reached spatial scales of 1014 cm. Depending on the progenitor's wind density and SN shock front velocity, these early-time SN observations may probe epochs early enough that the dense parts of the progenitor wind and circumstellar medium (CSM) have not yet been overrun by the SN shock front.
Observations of Superluminous Supernovae and their Host Galaxies
Authors: Leloudas Giorgos
Published: October 2016

Superluminous supernovae (SLSNe) were discovered during the last decade by wide-field surveys. Despite their importance for stellar evolution and mass loss, especially at low metallicities, and their utility as high-redshift probes and possible distance indicators, their nature remains poorly understood. I present here new exciting observations of SLSNe and their host galaxies that offer new clues in the hunt for their progenitors and explosion mechanism. These include constraints on the ages and the metallicities at the SN environments, double peaks revealed by early observations, the presence of H in nebular spectra, and the first evidence on the explosion geometry, through polarimetry.
X-Shaped Radio Galaxies and the Nanohertz Gravitational Wave Background
Authors: Roberts David H. , Saripalli Lakshmi , Subrahmanyan Ravi
Published: October 2016

Coalescence of supermassive black holes (SMBHs) in galaxy mergers is potentially the dominant contributor to the low frequency gravitational wave background (GWB). It was proposed by Merritt & Ekers that X-shaped radio galaxies are signposts of such coalescences and that their abundance might be used to predict the magnitude of the GWB. Cheung identified a sample of 100 candidate X-shaped radio galaxies using the NRAO FIRST survey; these are small-axial-ratio extended radio sources with off-axis emission. In Roberts et al. we made radio images of 52 of these sources with resolution of about 1 arcsecond using archival Very Large Array data. Fifty-one of the 52 were observed at 1.4 GHz, seven were observed at 1.4 and 5 GHz, and one was observed only at 5 GHz. Our higher resolution VLA images along with FIRST survey images of the sources in the sample reveal that extended extragalactic radio sources with small axial ratios are largely (60%) cases of double radio sources with twin lobes that have off-axis extensions, usually with inversion-symmetric structure. The available radio images indicate that at most 20% of sources might be genuine X-shaped radio sources that could have formed by a restarting of beams in a new direction following an interruption and axis flip. The remaining 20% are in neither of these categories.

These images indicate that at most a small fraction of the candidates might be genuine X-shaped radio sources that were formed by a restarting of beams in a new direction following a major merger, or by spin drift caused by BH-BH interaction. This suggests that fewer than 1.3% of extended radio sources appear to be candidates for genuine axis reorientations (“spin flips”), or 2.2% if possible “axis drift” sources are included, much smaller than the 7% suggested by Leahy & Parma. Thus, the associated GWB may be substantially smaller than previous estimates. These results can be used to normalize detailed calculations of the SMBH coalescence rate and the GWB.
Astrochemical models of water
Authors: Aikawa Yuri
Published: October 2016

We will review the chemical reaction network models of water and its D/H ratio coupled with the dynamics of star formation. Infrared observations show that water ice is abundant even in molecular clouds with relatively low visual extinction (~ 3 mag), which indicates that water ice is formed in early stage of molecular clouds. We thus start from a possible formation site of molecular clouds, i.e. the converging flow of diffuse gas. Then we proceed to dense cloud cores and its gravitational collapse, during which a significant deuterium enrichment occurs. The gas and ice accrete onto the circumstellar disks, which evolve to protoplanetary disks in T Tauri phase. If the disks are turbulent, water could be photodissociated in the disk surface and re-formed in deeper layers. The cycle continues until the dust grains with ice mantle are decoupled from the turbulence and settle to the midplane. The water D/H ratio could thus vary within the disk.
Search for water and life's building blocks in the universe: A summary
Authors: Bergin Edwin A.
Published: October 2016

Water and organics need to be supplied to terrestrial worlds like our own to provide the essential compounds required for the origin of life. These molecules form initially during the earliest stages of stellar birth, are supplied by collapse to the planet-forming disk predominantly as ice, and may undergo significant processing during this collapse and within large planetesimals that are heated via radioactive decay. Water and organic carriers can be quite volatile, thus their survival as ices within rocks is not preordained. In this focus meeting our goal is to bring together astronomers, cosmochemists, planetary scientists, chemical physicists, and spectroscopists who each explore individual aspects of this problem. In this summary we discuss some of the main themes that appeared in the meeting. Ultimately, cross-field collaboration is needed to provide greater understanding of the likelihood that terrestrial worlds form with these key compounds readily available on their surfaces – and are hence habitable if present at the right distance from the star.
Detection of rotational CO emission from the red-supergiants in the Large Magellanic Cloud
Authors: Matsuura Mikako , Sargent B. , Swinyard Bruce , Yates J.A. , Royer P. , Barlow M.J. , Boyer M.L. , Decin L. , Khouri Theo , Meixner Margaret , van Loon J.Th. , Woods P.M.
Published: October 2016

It is yet well understood how mass-loss rates from evolved stars depend on metallicities. With a half of the solar metallicity and the distance of only 50 kpc, the evolved stars of the Large Magellanic Cloud (LMC) are an ideal target for studying mass loss at low metallicity. We have obtained spectra of red-supergiants in the LMC, using the Hershel Space Observatory, detecting CO thermal lines fro J=6–5 up to 15–14 lines. Modelling CO lines with non-LTE Radiative transfer code suggests that CO lines intensities can be well explained with high gas-to-dust ratio, with no obvious reduction in mass-loss rate at the LMC. We conclude that the luminosities of the stars are primary factors on mass-loss rates, rather than the metallicity.
Asteroseismology of GD358 with complex core carbon and oxygen profiles
Authors: Bischoff-Kim Agnès , Provencal Judith L.
Published: October 2016

GD 358 is the brightest (mv=13.7) and best studied helium atmosphere white dwarf pulsator. We present an analysis based on over 1000 hours of observations spanning 2007-2014 as well as archival data going back to 1982. From the complete data set, we identify a total of 27 independent frequencies and fit 14 of them as m=0 modes in our asteroseismic analysis. We add GD358 to a set of helium atmosphere white dwarfs fitted with similar models. With this consistent set, we can see a trend in the thickness of the pure helium layer that are quantitatively consistent with time-dependent diffusion calculations.
Sound speed and oscillation frequencies for solar models evolved with Los Alamos ATOMIC opacities
Authors: Guzik Joyce A. , Fontes C. J. , Walczak P. , Wood S. R. , Mussack K. , Farag E.
Published: October 2016

Los Alamos National Laboratory has calculated a new generation of radiative opacities (OPLIB data using the ATOMIC code) for elements with atomic number Z = 1-30 with improved physics input, updated atomic data, and finer temperature grid to replace the Los Alamos LEDCOP opacities released in the year 2000. We calculate the evolution of standard solar models including these new opacities, and compare with models evolved using the Lawrence Livermore National Laboratory OPAL opacities (Iglesias & Rogers 1996). We use the solar abundance mixture of Asplund et al. 2009. The Los Alamos ATOMIC opacities (Colgan et al. 2013a, 2013b, 2015) have steeper opacity derivatives than those of OPAL for temperatures and densities of the solar interior radiative zone. We compare the calculated nonadiabatic solar oscillation frequencies and solar interior sound speed to observed frequencies and helioseismic inferences. The calculated sound-speed profiles are similar for models evolved using either the updated Iben evolution code (see Guzik & Mussack 2010), or the MESA evolution code (Paxton et al. 2015). The LANL ATOMIC opacities partially mitigate the ‘solar abundance problem’.
Light curve modeling of the short-period W UMa star GSC 02049-01164
Authors: Fox-Machado Lester , Echevarria Juan , González-Buitrago Diego , Michel Raul
Published: October 2016

The preliminary results of an analysis of the time-series photometric data of binary star GSC 02049-01164 (ROTSE1 J164341.65+251748.1) are presented. GSC 02049-01164 was observed for eight consecutive nights with the 0.84-m telescope of the San Pedro Martir Observatory in Mexico. The light curve of GSC 02049-01164 is typical of those of W UMa type binary stars. In an effort to gain a better understanding of the binary system and determine its physical properties we have analyzed the light curve with the software PHOEBE V.0 0.31a. We have found that GSC 02049-01164 binary system has a mass ratio of ~ 0.42, an inclination of ~ 85 degrees, a semi-major axis of ~ 2.24 R⊙. It is likely that the two stellar components are in contact, with a degree of overcontact of 13%. The physical parameters of the stellar components have been derived.
An analysis of the solar-like oscillations in the red giant star KIC 5701829 observed withKepler
Authors: Fox-Machado Lester , Deras Dan
Published: October 2016

The preliminary results of an analysis of the red giant star KIC 5701829 observed for 29 days in short-cadence mode with theKeplersatellite are reported. The oscillation spectrum of this star is characterized by the presence of a well-defined solar-like oscillation pattern due to acoustic modes. The characterization of the power spectrum has been performed following three basics steps commonly used in the analysis of solar-like oscillations: fitting and correcting for the background, estimating the frequency of maximum power (νmax) and the large separation (Δν), and extracting individual frequencies. We have found that the frequency of maximum oscillation power, νmax, and the mean large frequency separation, Δν, are around, 143 and 12 μHz, respectively. The global asteroseismic parameters along with atmospheric parameters from the literature allow us to infer about evolutionary status of the star.
The Schmidt Law Decoded and Explained
Authors: Madore Barry F.
Published: October 2016

Like the Bode-Titius Law before it, the Schmidt Law is not properly understood, given that it has never been reduced to, or predicted from first principles. Star formation is complicated. And, it is almost certainly a multi-scale process that has multiple immediate causes (quiescent, periodic and impulsive in their time dependence; local, global and cosmic/external in their origin) resulting in the same end product: stars. Philosophers of science would say that the theory of star formation is “massively underdetermined by the observations” of stars alone.
The image plane approach to cosmic telescopes
Authors: Oguri Masamune
Published: October 2016

Studies of high-redshift galaxies behind the cores of mass clusters require the correction of gravitational lensing effects. We present our approach to estimate shapes, magnitudes, and the selection effect of high-redshift galaxies in the image plane, which allows us to include not only lensing magnifications but also lensing distortions and image multiplications. For this purpose we construct new mass models for the Frontier Fields clusters using the public software glafic. We present some results on faint-end slopes of the luminosity function and the size evolution of high-redshift galaxies from the analysis of Frontier Fields clusters.
Systematics errors in strong lens modeling
Authors: Johnson Traci L. , Sharon Keren , Bayliss Matthew B.
Published: October 2016

We investigate how varying the number of multiple image constraints and the available redshift information can influence the systematic errors of strong lens models, specifically, the image predictability, mass distribution, and magnifications of background sources. This work will not only inform upon Frontier Field science, but also for work on the growing collection of strong lensing galaxy clusters, most of which are less massive and are capable of lensing a handful of galaxies.
Probing the Cosmic Frontier of Galaxies
Authors: Oesch Pascal A.
Published: October 2016

Understanding when and how the first galaxies formed and what sources reionized the universe are key goals of extragalactic astronomy. Thanks to deep surveys with the powerful WFC3/IR camera on the HST, the observational frontier of galaxy build-up now lies at only ~450 Myr after the Big Bang, at redshifts z ~10-12. In combination with deep data from Spitzer/IRAC we can now probe the evolution of the stellar mass density over 96% of cosmic history. However, detecting and characterizing galaxies at these early epochs is challenging even for HST and the sample sizes at the earliest redshifts are still very small. The Hubble Frontier Fields provide a prime new dataset to improve upon our current, sparse sampling of the UV luminosity function at z>8 from blank fields to answer some of the most pressing open questions. For instance, even the evolution of the cosmic star-formation rate density at z>8 is still debated. While our measurements based on blank field data indicate that galaxies with SFR>0.7 Msol/yr disappear quickly from the cosmic record between z~8 and z~10, other previous results, e.g., from the CLASH survey favor a more moderate decline. Here, we briefly review the recent progress in studying galaxy build-up out to z~10 from the combined blank field and existing Frontier Field datasets and discuss their implications for primordial galaxy formation and cosmic reionization.
Reconciling the rules of international humanitarian law with the rules of European human rights law
Authors: Landais Claire , Bass Léa
Published: October 2016

States party to the European Convention for the Protection of Human Rights and Fundamental Freedoms that engage in military operations abroad face an increased risk to be held responsible for violations of the Convention, given the relatively recent case law adopted by the European Court of Human Rights. This article examines some of the issues raised by the concurrent applicability of international humanitarian law and European human rights law. It also seeks to identify ways to reconcile these two different, but not incompatible, branches of international law.
Kite Receives 2016 Ronald Greeley Early Career Award in Planetary Science
Authors:   AGU
Published: October 2016

Edwin Kite will receive the 2016 Ronald Greeley Early Career Award in Planetary Science at the 2016 American Geophysical Union Fall Meeting, to be held 12–16 December in San Francisco, Calif. The award recognizes significant early-career contributions to planetary science.
Brain structure in pediatric Tourette syndrome
Authors:   and The Tourette Association of America Neuroimaging Consortium, Greene D J , Williams III A C , Koller J M , Schlaggar B L , Black K J
Published: October 2016

Previous studies of brain structure in Tourette syndrome (TS) have produced mixed results, and most had modest sample sizes. In the present multicenter study, we used structural magnetic resonance imaging (MRI) to compare 103 children and adolescents with TS to a well-matched group of 103 children without tics. We applied voxel-based morphometry methods to test gray matter (GM) and white matter (WM) volume differences between diagnostic groups, accounting for MRI scanner and sequence, age, sex and total GM+WM volume. The TS group demonstrated lower WM volume bilaterally in orbital and medial prefrontal cortex, and greater GM volume in posterior thalamus, hypothalamus and midbrain. These results demonstrate evidence for abnormal brain structure in children and youth with TS, consistent with and extending previous findings, and they point to new target regions and avenues of study in TS. For example, as orbital cortex is reciprocally connected with hypothalamus, structural abnormalities in these regions may relate to abnormal decision making, reinforcement learning or somatic processing in TS.
The fungal-specific β-glucan-binding lectin FGB1 alters cell-wall composition and suppresses glucan-triggered immunity in plants
Authors: Wawra Stephan , Fesel Philipp , Widmer Heidi , Timm Malte , Seibel Jürgen , Leson Lisa , Kesseler Leona , Nostadt Robin , Hilbert Magdalena , Langen Gregor , Zuccaro Alga
Published: October 2016

β-glucans are well-known modulators of the immune system in mammals but little is known about β-glucan triggered immunity in planta. Here we show by isothermal titration calorimetry, circular dichroism spectroscopy and nuclear magnetic resonance spectroscopy that the FGB1 gene from the root endophyte Piriformospora indica encodes for a secreted fungal-specific β-glucan-binding lectin with dual function. This lectin has the potential to both alter fungal cell wall composition and properties, and to efficiently suppress β-glucan-triggered immunity in different plant hosts, such as Arabidopsis, barley and Nicotiana benthamiana. Our results hint at the existence of fungal effectors that deregulate innate sensing of β-glucan in plants.
Dynamic microfluidic control of supramolecular peptide self-assembly
Authors: Arnon Zohar A. , Vitalis Andreas , Levin Aviad , Michaels Thomas C. T. , Caflisch Amedeo , Knowles Tuomas P. J. , Adler-Abramovich Lihi , Gazit Ehud
Published: October 2016

The dynamic nature of supramolecular polymers has a key role in their organization. Yet, the manipulation of their dimensions and polarity remains a challenge. Here, the minimalistic diphenylalanine building block was applied to demonstrate control of nano-assemblies growth and shrinkage using microfluidics. To fine-tune differential local environments, peptide nanotubes were confined by micron-scale pillars and subjected to monomer flows of various saturation levels to control assembly and disassembly. The small-volume device allows the rapid adjustment of conditions within the system. A simplified kinetic model was applied to calculate parameters of the growth mechanism. Direct real-time microscopy analysis revealed that different peptide derivatives show unidirectional or bidirectional axial dimension variation. Atomistic simulations show that unidirectional growth is dictated by the differences in the axial ends, as observed in the crystalline order of symmetry. This work lays foundations for the rational control of nano-materials dimensions for applications in biomedicine and material science.
mTORC1 and mTORC2 regulate skin morphogenesis and epidermal barrier formation
Authors: Ding Xiaolei , Bloch Wilhelm , Iden Sandra , Rüegg Markus A. , Hall Michael N. , Leptin Maria , Partridge Linda , Eming Sabine A.
Published: October 2016

Mammalian target of rapamycin (mTOR), a regulator of growth in many tissues, mediates its activity through two multiprotein complexes, mTORC1 or mTORC2. The role of mTOR signalling in skin morphogenesis and epidermal development is unknown. Here we identify mTOR as an essential regulator in skin morphogenesis by epidermis-specific deletion of Mtor in mice (mTOREKO). mTOREKO mutants are viable, but die shortly after birth due to deficits primarily during the early epidermal differentiation programme and lack of a protective barrier development. Epidermis-specific loss of Raptor, which encodes an essential component of mTORC1, confers the same skin phenotype as seen in mTOREKO mutants. In contrast, newborns with an epidermal deficiency of Rictor, an essential component of mTORC2, survive despite a hypoplastic epidermis and disruption in late stage terminal differentiation. These findings highlight a fundamental role for mTOR in epidermal morphogenesis that is regulated by distinct functions for mTORC1 and mTORC2.
Self-motion evokes precise spike timing in the primate vestibular system
Authors: Jamali Mohsen , Chacron Maurice J. , Cullen Kathleen E.
Published: October 2016

The accurate representation of self-motion requires the efficient processing of sensory input by the vestibular system. Conventional wisdom is that vestibular information is exclusively transmitted through changes in firing rate, yet under this assumption vestibular neurons display relatively poor detection and information transmission. Here, we carry out an analysis of the system’s coding capabilities by recording neuronal responses to repeated presentations of naturalistic stimuli. We find that afferents with greater intrinsic variability reliably discriminate between different stimulus waveforms through differential patterns of precise (∼6 ms) spike timing, while those with minimal intrinsic variability do not. A simple mathematical model provides an explanation for this result. Postsynaptic central neurons also demonstrate precise spike timing, suggesting that higher brain areas also represent self-motion using temporally precise firing. These findings demonstrate that two distinct sensory channels represent vestibular information: one using rate coding and the other that takes advantage of precise spike timing.
Coupling optogenetic stimulation with NanoLuc-based luminescence (BRET) Ca++ sensing
Authors: Yang Jie , Cumberbatch Derrick , Centanni Samuel , Shi Shu-qun , Winder Danny , Webb Donna , Johnson Carl Hirschie
Published: October 2016

Optogenetic techniques allow intracellular manipulation of Ca++ by illumination of light-absorbing probe molecules such as channelrhodopsins and melanopsins. The consequences of optogenetic stimulation would optimally be recorded by non-invasive optical methods. However, most current optical methods for monitoring Ca++ levels are based on fluorescence excitation that can cause unwanted stimulation of the optogenetic probe and other undesirable effects such as tissue autofluorescence. Luminescence is an alternate optical technology that avoids the problems associated with fluorescence. Using a new bright luciferase, we here develop a genetically encoded Ca++ sensor that is ratiometric by virtue of bioluminescence resonance energy transfer (BRET). This sensor has a large dynamic range and partners optimally with optogenetic probes. Ca++ fluxes that are elicited by brief pulses of light to cultured cells expressing melanopsin and to neurons-expressing channelrhodopsin are quantified and imaged with the BRET Ca++ sensor in darkness, thereby avoiding undesirable consequences of fluorescence irradiation.
Mesenchymal state of intimal cells may explain higher propensity to ascending aortic aneurysm in bicuspid aortic valves
Authors: Maleki Shohreh , Kjellqvist Sanela , Paloschi Valentina , Magné Joelle , Branca Rui Miguel Mamede , Du Lei , Hultenby Kjell , Petrini Johan , Fuxe Jonas ,   MIBAVA Leducq Consortium, Dietz Harry C. , Loeys Bart , Van Laer Lut , McCallion Andrew S. , Mertens Luc , Mital Seema , Mohamed Salah A. , Andelfinger Gregor , Lehtiö Janne , Franco-Cereceda Anders , Eriksson Per , Björck Hanna M.
Published: October 2016

Individuals with a bicuspid aortic valve (BAV) are at significantly higher risk of developing aortic complications than individuals with tricuspid aortic valves (TAV) and defective signaling during the embryonic development and/or life time exposure to abnormal hemodynamic have been proposed as underlying factors. However, an explanation for the molecular mechanisms of aortopathy in BAV has not yet been provided. We combined proteomics, RNA analyses, immunohistochemistry, and electron microscopy to identify molecular differences in samples of non-dilated ascending aortas from BAV (N = 62) and TAV (N = 54) patients. Proteomic analysis was also performed for dilated aortas (N = 6 BAV and N = 5 TAV) to gain further insight into the aortopathy of BAV. Our results collectively showed the molecular signature of an endothelial/epithelial-mesenchymal (EndMT/EMT) transition-like process, associated with instability of intimal cell junctions and activation of RHOA pathway in the intima and media layers of ascending aorta in BAV patients. We propose that an improper regulation of EndMT/EMT during the spatiotemporally related embryogenesis of semilunar valves and ascending aorta in BAV individuals may result in aortic immaturity and instability prior to dilation. Exasperation of EndMT/EMT state in post embryonic life and/or exposure to non-physiological hemodynamic could lead to the aneurysm of ascending aorta in BAV individuals.