bluuebunny/crossref_metadata_2025_split huggingface dataset:
CALCULATIONS WITH SPECTROSCOPIC ACCURACY: ENERGIES AND TRANSITION RATES IN THE NITROGEN ISOELECTRONIC SEQUENCE FROM Ar XII TO Zn XXIV
Authors: Wang K. , Si R. , Dang W. , Jönsson P. , Guo X. L. , Li S. , Chen Z. B. , Zhang H. , Long F. Y. , Liu H. T. , Li D. F. , Hutton R. , Chen C. Y. , Yan J. 
Published: June 2019

ABSTRACT
Combined relativistic configuration interaction and many-body perturbation calculations are performed for the 359 fine-structure levels of the 2s
2 2p
3, 2 s2p
4, 2p
5, 2s
2 2p
2 3l, 2 s2p
3 3l, 2p
4 3l, and 2s
2 2p
2 4l configurations in N-like ions from Ar xii to Zn xxiv. Complete and consistent data sets of energies, wavelengths, radiative rates, oscillator strengths, and line strengths for all possible electric dipole, magnetic dipole, electric quadrupole, and magnetic quadrupole transitions among the 359 levels are given for each ion. The present work significantly increases the amount of accurate data for ions in the nitrogen-like sequence, and the accuracy of the energy levels is high enough to enable the identification and interpretation of observed spectra involving the n = 3, 4 levels, for which experimental values are largely scarce. Meanwhile, the results should be of great help for modeling and diagnosing astrophysical and fusion plasmas.
The Detectability and Characterization of the TRAPPIST-1 Exoplanet Atmospheres with JWST
Authors: Lustig-Yaeger Jacob , Meadows Victoria S. , Lincowski Andrew P. 
Published: June 2019

Abstract
The James Webb Space Telescope (JWST) will offer the first opportunity to characterize terrestrial exoplanets with sufficient precision to identify high mean molecular weight atmospheres, and TRAPPIST-1's seven known transiting Earth-sized planets are particularly favorable targets. To assist community preparations for JWST observations, we use simulations of plausible post-ocean-loss and habitable environments for the TRAPPIST-1 exoplanets, and test simulations of all bright object time-series spectroscopy modes and all Mid-Infrared Instrument photometry filters to determine optimal observing strategies for atmospheric detection and characterization using both transmission and emission observations. We find that transmission spectroscopy with the Near-Infrared Spectrograph Prism is optimal for detecting terrestrial, CO2-containing atmospheres, potentially in fewer than 10 transits for all seven TRAPPIST-1 planets, if they lack high-altitude aerosols. If the TRAPPIST-1 planets possess Venus-like H2SO4 aerosols, up to 12 times more transits may be required to detect an atmosphere. We present optimal instruments and observing modes for the detection of individual molecular species in a given terrestrial atmosphere and an observational strategy for discriminating between evolutionary states. We find that water may be prohibitively difficult to detect in both Venus-like and habitable atmospheres, due to its presence lower in the atmosphere where transmission spectra are less sensitive. Although the presence of biogenic O2 and O3 will be extremely challenging to detect, abiotically produced oxygen from past ocean loss may be detectable for all seven TRAPPIST-1 planets via O2–O2 collisionally induced absorption at 1.06 and 1.27 μm, or via NIR O3 features for the outer three planets. Our results constitute a suite of hypotheses on the nature and detectability of highly evolved terrestrial exoplanet atmospheres that may be tested with JWST.
Spitzer Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M Dwarf
Authors: Jung Youn Kil , Gould Andrew , Udalski Andrzej , Sumi Takahiro , Yee Jennifer C. , Shvartzvald Yossi , Zang Weicheng ,   and, Han Cheongho , Albrow Michael D. , Chung Sun-Ju , Hwang Kyu-Ha , Ryu Yoon-Hyun , Shin In-Gu , Zhu Wei , Cha Sang-Mok , Kim Dong-Jin , Kim Hyoun-Woo , Kim Seung-Lee , Lee Chung-Uk , Lee Dong-Joo , Lee Yongseok , Park Byeong-Gon , Pogge Richard W. ,   (The KMTNet Collaboration), Mróz Przemek , Szymański Michał K. , Skowron Jan , Poleski Radek , Soszyński Igor , Pietrukowicz Paweł , Kozłowski Szymon , Ulaczyk Krzystof , Rybicki Krzysztof A. , Iwanek Patryk , Wrona Marcin ,   (The OGLE Collaboration), Beichman Charles A. , Bryden Geoffery , Novati Sebastiano Calchi , Carey Sean , Gaudi B. Scott , Henderson Calen B. ,   (The Spitzer Team), Abe Fumio , Barry Richard , Bennett David P. , Bond Ian A. , Bhattacharya Aparna , Donachie Martin , Fukui Akihiko , Hirao Yuki , Itow Yoshitaka , Kondo Iona , Koshimoto Naoki , Li Man Cheung Alex , Matsubara Yutaka , Miyazaki Shota , Muraki Yasushi , Nagakane Masayuki , Ranc Clément , Rattenbury Nicholas J. , Suematsu Haruno , Sullivan Denis J. , Suzuki Daisuke , Tristram Paul J. , Yonehara Atsunori ,   (The MOA Collaboration), Jacklin Savannah , Penny Matthew T. , Stassun Keivan G. ,   (The UKIRT Microlensing Team), Fouqué Pascal , Mao Shude , Wang Tianshu ,   (The CFHT Microlensing Collaboration)
Published: June 2019

Abstract
We report the discovery of a Spitzer microlensing planet OGLE-2018-BLG-0596Lb, with preferred planet-host mass ratio q ∼ 2 × 10−4. The planetary signal, which is characterized by a short (∼1 day) “bump” on the rising side of the lensing light curve, was densely covered by ground-based surveys. We find that the signal can be explained by a bright source that fully envelops the planetary caustic, i.e., a “Hollywood” geometry. Combined with the source proper motion measured from Gaia, the Spitzer satellite parallax measurement makes it possible to precisely constrain the lens physical parameters. The preferred solution, in which the planet perturbs the minor image due to lensing by the host, yields a Uranus-mass planet with a mass of M
p = 13.9 ± 1.6 M
⊕ orbiting a mid M-dwarf with a mass of M
h = 0.23 ± 0.03 M
⊙. There is also a second possible solution that is substantially disfavored but cannot be ruled out, for which the planet perturbs the major image. The latter solution yields M
p = 1.2 ± 0.2 M
⊕ and M
h = 0.15 ± 0.02 M
⊙. By combining the microlensing and Gaia data together with a Galactic model, we find in either case that the lens lies on the near side of the Galactic bulge at a distance D
L ∼ 6 ± 1 kpc. Future adaptive optics observations may decisively resolve the major image/minor image degeneracy.
Io’s Volcanic Activity from Time Domain Adaptive Optics Observations: 2013–2018
Authors: de Kleer Katherine , de Pater Imke , Molter Edward M. , Banks Elizabeth , Davies Ashley Gerard , Alvarez Carlos , Campbell Randy , Aycock Joel , Pelletier John , Stickel Terry , Kacprzak Glenn G. , Nielsen Nikole M. , Stern Daniel , Tollefson Joshua 
Published: June 2019

Abstract
We present measurements of the near-infrared brightness of Io’s hot spots derived from 2 to 5 μm imaging with adaptive optics on the Keck and Gemini N telescopes. The data were obtained on 271 nights between 2013 August and the end of 2018, and include nearly 1000 detections of over 75 unique hot spots. The 100 observations obtained between 2013 and 2015 have been previously published in de Kleer & de Pater the observations since the start of 2016 are presented here for the first time, and the analysis is updated to include the full five-year data set. These data provide insight into the global properties of Io’s volcanism. Several new hot spots and bright eruptions have been detected, and the preference for bright eruptions to occur on Io’s trailing hemisphere noted in the 2013–2015 data is strengthened by the larger data set and remains unexplained. The program overlapped in time with Sprint-A/EXCEED and Juno observations of the Jovian system, and correlations with transient phenomena seen in other components of the system have the potential to inform our understanding of the impact of Io’s volcanism on Jupiter and its neutral/plasma environment.
BOOSTING LYα AND He ii λ1640 LINE FLUXES FROM POPULATION III GALAXIES: STOCHASTIC IMF SAMPLING AND DEPARTURES FROM CASE-B
Authors: Mas-Ribas Lluís , Dijkstra Mark , Forero-Romero Jaime E. 
Published: June 2019

ABSTRACT
We revisit calculations of nebular hydrogen Lyα and He ii
λ1640 line strengths for Population III (Pop III) galaxies, undergoing continuous, and bursts of, star formation. We focus on initial mass functions (IMFs) motivated by recent theoretical studies, which generally span a lower range of stellar masses than earlier works. We also account for case-B departures and the stochastic sampling of the IMF. In agreement with previous work, we find that departures from case-B can enhance the Lyα flux by a factor of a few, but we argue that this enhancement is driven mainly by collisional excitation and ionization, and not due to photoionization from the n = 2 state of atomic hydrogen. The increased sensitivity of the Lyα flux to the high-energy end of the galaxy spectrum makes it more subject to stochastic sampling of the IMF. The latter introduces a dispersion in the predicted nebular line fluxes around the deterministic value by as much as a factor of ∼4. In contrast, the stochastic sampling of the IMF has less impact on the emerging Lyman Werner photon flux. When case-B departures and stochasticity effects are combined, nebular line emission from Pop III galaxies can be up to one order of magnitude brighter than predicted by “standard” calculations that do not include these effects. This enhances the prospects for detection with future facilities such as the James Webb Space Telescope and large, ground-based telescopes.
Resonant Relaxation in Globular Clusters
Authors: Meiron Yohai , Kocsis Bence 
Published: June 2019

Abstract
Resonant relaxation has been discussed as an efficient process that changes the angular momenta of stars orbiting around a central supermassive black hole due to the fluctuating gravitational field of the stellar cluster. Other spherical stellar systems, such as globular clusters, exhibit a restricted form of this effect where enhanced relaxation rate only occurs in the directions of the angular momentum vectors, but not in their magnitudes; this is called vector resonant relaxation (VRR). To explore this effect, we performed a large set of direct N-body simulations, with up to 512k particles (where k =1024) and ∼500 dynamical times. Contrasting these simulations, which naturally include the collective effects, with Spitzer-style Monte Carlo simulations, which by design only exhibit two-body relaxation, we show that the temporal behavior of the angular momentum vectors in N-body simulations cannot be explained by two-body relaxation alone. VRR operates efficiently in globular clusters with N > 104. The fact that VRR operates in globular clusters may open a way to use powerful tools in statistical physics for their description. In particular, since the distribution of orbital planes relaxes much more rapidly than the distribution of the magnitude of angular momentum and the radial action, the relaxation process reaches an internal statistical equilibrium in the corresponding part of phase space while the whole cluster is generally out of equilibrium, in a state of quenched disorder. We point out the need to include effects of VRR in Monte Carlo simulations of globular clusters.
Nonparametric Dark Energy Reconstruction Using the Tomographic Alcock–Paczynski Test
Authors: Zhang Zhenyu , Gu Gan , Wang Xiaoma , Li Yun-He , Sabiu Cristiano G. , Park Hyunbae , Miao Haitao , Luo Xiaolin , Fang Feng , Li Xiao-Dong 
Published: June 2019

Abstract
The tomographic Alcock–Paczynski (AP) method can result in tight cosmological constraints by using small and intermediate clustering scales of the large-scale structure of the galaxy distribution. By focusing on the redshift dependence, the AP distortion can be distinguished from the distortions produced by the redshift space distortions. In this work, we combine the tomographic AP method with other recent observational data sets of SN Ia+BAO+CMB+H
0 to reconstruct the dark energy equation-of-state w in a nonparametric form. The result favors a dynamical DE at z ≲ 1, and shows a mild deviation (≲2σ) from w = −1 at z = 0.5–0.7. We find the addition of the AP method improves the low-redshift (z ≲ 0.7) constraint by ∼50%.
The Generalized Nonlinear Ohm's Law: How a Strong Electric Field Influences Nonideal MHD Effects in Dusty Protoplanetary Disks
Authors: Okuzumi Satoshi , Mori Shoji , Inutsuka Shu-ichiro 
Published: June 2019

Abstract
The magnetohydrodynamics (MHD) of protoplanetary disks are strongly subject to the nonideal MHD effects arising from the low ionization fraction of the disk gas. A strong electric field induced by gas motions can heat ionized gas particles and can thereby affect the ionization balance in the disks. Our previous studies revealed that in dusty protoplanetary disks, the ohmic conductivity decreases with increasing electric field strength until the electrical breakdown of the disk gas occurs. In this study, we extend our previous work to more general cases where both electric and magnetic fields affect the motion of plasma particles, allowing us to study the impacts of plasma heating on all nonideal MHD effects: ohmic, Hall, and ambipolar diffusion. We find that the upper limit on the electric current we previously derived applies even in the presence of magnetic fields. Although the Hall and ambipolar resistivities can either increase or decrease with electric field strength depending on the abundance of charged dust grains, the ohmic resistivity always increases with electric field strength. An order-of-magnitude estimate suggests that a large-scale electric current generated by gas motions in the inner part of protoplanetary disks could exceed the upper limit. This implies that MHD motions of the inner disk, such as the motion driven by the Hall-shear instability, could either get suppressed or trigger electrical breakdown (lightning discharge). This may have important implications for gas accretion and chondrule formation in the inner part of protoplanetary disks.
Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
Authors: Okuzumi Satoshi , Tazaki Ryo 
Published: June 2019

Abstract
Recent (sub)millimeter polarimetric observations toward the young star HL Tau have successfully detected polarization emission from its circumstellar disk. The polarization pattern observed at 0.87 mm is uniform and parallel to the disk’s minor axis, consistent with the self-scattering of thermal emission by dust particles whose maximum radius is ≈100 μm. However, this maximum size is considerably smaller than anticipated from dust evolution models that assume a high sticking efficiency for icy particles. Here we show that the unexpectedly small particle size can be explained if CO2 ice covers the particles in the outer region of the HL Tau disk. CO2 ice is one of the most major interstellar ices, and laboratory experiments show that it is poorly sticky. Based on dust evolution models accounting for CO2 ice mantles, as well as aggregate sintering, we simulate the polarimetric observation of HL Tau at 0.87 mm. We find that the models with CO2 ice mantles better match the observation. These models also predict that only particles lying between the H2O and CO2 snow lines can grow to millimeter to centimeter sizes and that their rapid inward drift results in a local dust gap similar to the 10 au gap of the HL Tau disk. We also suggest that the millimeter spectral index for the outer part of the HL Tau disk is largely controlled by the optical thickness of this region and does not necessarily indicate dust growth to millimeter sizes.
Peculiarities of the Dynamics of Solar NOAA Active Region 12673
Authors: Getling A. V. 
Published: June 2019

Abstract
The dynamics of active region (AR) 12673 is qualitatively studied using observational data obtained with the Helioseismic and Magnetic Imager of the Solar Dynamics Observatory on 2017 August 31–September 8. This AR was remarkable for its complex structure and extraordinary flare productivity. The sunspot group in this AR consisted of (1) an old, well-developed and highly stable, coherent sunspot, which had also been observed two solar rotations earlier, and (2) a rapidly developing cluster of umbral and penumbral fragments. Cluster (2) formed two elongated, arc-shaped chains of spot elements, skirting around the major sunspot (1), with two chains of magnetic elements spatially coinciding with the arcs. AR components (1) and (2) were in relative motion, cluster (2) overtaking spot (1) in westward motion, and their relative velocity agrees in order of magnitude with the velocity jump over the near-surface shear layer, or leptocline. The pattern of motion of the features about the main spot bears amazing resemblance to the pattern of a fluid flow about a roundish body. This suggests that spot (1) was dynamically coupled with the surface layers, while cluster (2) developed in deeper layers of the convection zone. The magnetic-flux emergence in cluster (2) appeared to be associated with fluid motions similar to roll convection. The mutual approach of components (1) and (2) gave rise to light bridges in the umbrae of sunspots with the magnetic field having the same sign on both sides of the bridge.
The Living Atlases Community of Practice
Authors: Lecoq Marie-Elise , Archambeau Anne-Sophie , Figueira Rui , Martin David , Pamerlon Sophie , Robertson Tim , Vignes Lebbe Régine , Villaverde Cristina 
Published: June 2019

The power and configurability of the the Atlas of Living Australia tools have enabled more and more institutions and participants of the Global Biodiversity Information Facility adapt and install biodiversity platforms. For six years, we have demonstrated that the community around this platform was needed and ready for its adoption. During the symposium organized for the SPNHC+TDWG 2018, we started a discussion that has led us to the creation of a more structured and sustainable community of practice.
We want to create a community that follows the structure of open-source technical projects such as Linux or Apache foundation. After the GBIF Governing Board (GB25), the Kilkenny accord was agreed among 8 country or institution partners and early adopters of ALA platform to outline the scope of the new Living Atlases community. Thanks to this accord, we have begun to set up a new structure based on the Community of Practice (CoP) model. In summary, the governance will be held by a Management committee and a Technical advisory committee. Adding to these, the Living Atlases community will have two coordinators with technical and administrative duties.
This presentation will briefly summarise the community history leading up to the agreement of the Kilkenny accord and provide information and context of the key points contained. Then, we will present and launch the new Living Atlases Community of Practice . Through this presentation, we aim to collect lessons learned and good practices from other CoP in topics like governance, communications, sustainability, among others to incorporate them in the consolidation process of the Living Atlases community.
The Global Omics Observatory Network: Shaping standards for long-term molecular observation
Authors: Buttigieg Pier Luigi , Janssen Felix , Macklin James , Pitz Kathleen 
Published: June 2019

Founded in early 2018 through a collaboration between the EU Horizon 2020 AtlantOS project and Agriculture and Agri-Food Canada, the Global Omics Observatory Network (GLOMICON) is federating long-term ecological observatories employing "omic" (e.g. metagenomcis, metatranscriptomics, metabolomics) techniques to assess biodiversity across scales. GLOMICON is the consolidation of a series of meetings and ad hoc efforts (e.g. the multi-omic sessions at TDWG 2017) and seeks to mainstream multi-omic observation in existing observatory systems. GLOMICON currently networks &gt;40 organisations observing biodiversity from urban and agricultural systems to the depths of the polar ocean. Coordination through GLOMICON allows the long-term observatory community to develop and align their needs, thus approaching standards bodies including the Genomic Standards Consortium (GSC), the Biodiversity Information Standards (TDWG) organisation, and the Earth Science Information Partners (ESIP) with a common voice. Further, as more ecological observatories begin to adopt molecular techniques, GLOMICON offers a community building best practices to facilitate their operationalisation. Vitally, GLOMICON interfaces with established observation networks via organisations such as UNESCO/IOC Global Ocean Observing System through its Biology and Ecosystems Panel. Such interactions have provided invaluable guidance on how to approach global standardisation in a firmly operational and multi-stakeholder environment, while ensuring innovative science can thrive.
In this contribution, we will deliver a briefing on GLOMICON's current priorities and efforts to shape molecular standards to become fit-for-purpose in observatory-grade settings. In particular, we will focus on our interactions with other key omic observing networks, including the Genomic Observatories Network, and our joint strategies to progress towards an distributed yet integrated system. We will also note practical steps the network has taken to systematise protocols and best practices, (bio)informatics routines, observatory parameters, and global intercalibration through sample exchange. Lastly, we will note the network's upcoming priorities, which feature the need to develop strategies for sustainability and the extension of coordination efforts between national, regional, and global Earth observation systems.