bluuebunny/crossref_metadata_2025_split huggingface dataset:
L. Sulla imperator et imperator iterum : pour une réévaluation de la chronologie des émissions monétaires de Sylla (RRC 367-368 et 359)
Authors: Assenmaker Pierre 
Published: February 2017

Cet article aborde sous un angle nouveau le problème de la chronologie des émissions syllaniennes aux légendes L. SVL(L) A IM(P)(E) (RRC 367-368) et L. SVLLA IMPER ITERV(M) (RRC 359). La première partie est consacrée à la signification du titre d’imperator, qui désigne Sylla a priori comme «commandant détenteur de l’imperium » . Le classement traditionnel des séries implique une utilisation arbitraire de l’itération, qui n’est pas la plus vraisemblable. La suite de l’article propose donc une réévaluation des éléments fondant les datations communément adoptées.
Au terme de cet examen, l’hypothèse suivante est mise à l’épreuve : l’émission L. Sulla imperator aurait été produite vers 90-89, durant la guerre sociale, et les monnaies L. Sulla imperator iterum à partir de la fin de l’année 84 (au plus tôt), pour financer la campagne en Italie.
In the interface of caesalpinioids and mimosoids: Comparative floral development elucidates shared characters in Dimorphandra mollis and Pentaclethra macroloba (Leguminosae)
Authors: De Barros Thais C. , Pedersoli Giseli D. , Paulino Juliana V. , Teixeira Simone P. 
Published: February 2017

PREMISE OF THE STUDY:Pentaclethra and Dimorphandra (Leguminosae) have long been considered a possible enigmatic link between caesalpinioids and mimosoids because they both have an imbricate calyx and heteromorphic androecium, floral features that are rare among mimosoids but common among caesalpinioids. This study compared the developing flowers of Dimorphandra mollis and Pentaclethra macroloba to determine whether the shared floral conditions also have the same ontogenetic origin.METHODS:Buds of different sizes and flowers were processed for surface (scanning electron microscopy) and histological (light microscopy) examination.KEY RESULTS:The floral meristem initiates five sepal primordia in a modified helical order in both species. The median sagittal sepal is adaxial. The overlap of the sepals during elongation culminates with the formation of the imbricate calyx. Heteromorphic androecia arise in the intermediate stages of development. In P. macroloba, the fertile pollen‐bearing stamens are antesepalous, robust and short, and the anthers carry a robust apical gland; the staminodes are long and white with a vestigial apical gland. In contrast, in D. mollis the fertile pollen‐bearing stamens are antepetalous without glands and as long as the staminodes. The staminodes are thinner with an expanded apical region.CONCLUSIONS:The imbricate calyx and the heteromorphic androecium in the studied species originated via distinct pathways, favoring the hypothesis of homoplasy of these conditions. The pathways observed in P. macroloba are more similar to those observed in caesalpinioids than to those observed in mimosoids, indicating that although the floral development differs between the species studied, it supports the basal placement of Pentaclethra among mimosoids.
Evolution of Occator Crater on (1) Ceres
Authors: Nathues A. , Platz T. , Thangjam G. , Hoffmann M. , Mengel K. , Cloutis E. A. , Corre L. Le , Reddy V. , Kallisch J. , Crown D. A. 
Published: February 2017

Abstract
The dwarf planet Ceres (diameter 939 km) is the largest object in the main asteroid belt. Recent investigations suggest that Ceres is a thermally evolved, volatile-rich body with potential geological activity, a body which was never completely molten but possibly differentiated into a rocky core, an ice-rich mantle, and which may contain remnant internal liquid water. Thermal alteration and exogenic material infall contribute to producing a (dark) carbonaceous chondritic-like surface containing ammoniated phyllosilicates. Here we report imaging and spectroscopic analyses of Occator crater derived from the Framing Camera and the Visible and Infrared Spectrometer onboard Dawn. We found that the central bright spot (Cerealia Facula) of Occator is ∼30 Myr younger than the crater itself. The central spot is located in a central pit which contains a dome that is spectrally homogenous, exhibiting absorption features that are consistent with carbonates. Multiple radial fractures across the dome indicate an extrusive formation process. Our results lead us to conclude that the floor region was subject to past endogenic activity. Dome and bright material in its vicinity formed likely due to a long-lasting, periodic, or episodic ascent of bright material from a subsurface reservoir rich in carbonates. Originally triggered by an impact event, gases, possibly dissolved from a subsurface water/brine layer, enabled material rich in carbonates to ascend through fractures and be deposited onto the surface.
One Law to Rule Them All: The Radial Acceleration Relation of Galaxies
Authors: Lelli Federico , McGaugh Stacy S. , Schombert James M. , Pawlowski Marcel S. 
Published: February 2017

Abstract
We study the link between baryons and dark matter (DM) in 240 galaxies with spatially resolved kinematic data. Our sample spans 9 dex in stellar mass and includes all morphological types. We consider (1) 153 late-type galaxies (LTGs; spirals and irregulars) with gas rotation curves from the SPARC database, (2) 25 early-type galaxies (ETGs; ellipticals and lenticulars) with stellar and H i data from ATLAS

3
D

or X-ray data from Chandra, and (3) 62 dwarf spheroidals (dSphs) with individual-star spectroscopy. We find that LTGs, ETGs, and “classical” dSphs follow the same radial acceleration relation: the observed acceleration (

g

obs

) correlates with that expected from the distribution of baryons (

g

bar

) over 4 dex. The relation coincides with the 1:1 line (no DM) at high accelerations but systematically deviates from unity below a critical scale of ∼10−10 m s−2. The observed scatter is remarkably small (

≲
0.13

dex) and largely driven by observational uncertainties. The residuals do not correlate with any global or local galaxy property (e.g., baryonic mass, gas fraction, and radius). The radial acceleration relation is tantamount to a natural law: when the baryonic contribution is measured, the rotation curve follows, and vice versa. Including ultrafaint dSphs, the relation may extend by another 2 dex and possibly flatten at

g

bar

≲

10

−
12

m s−2, but these data are significantly more uncertain. The radial acceleration relation subsumes and generalizes several well-known dynamical properties of galaxies, like the Tully–Fisher and Faber–Jackson relations, the “baryon-halo” conspiracies, and Renzo’s rule.
Limits on Polarized Leakage for the PAPER Epoch of Reionization Measurements at 126 and 164 MHz
Authors: Moore David F. , Aguirre James E. , Kohn Saul A. , Parsons Aaron R. , Ali Zaki S. , Bradley Richard F. , Carilli Chris L. , DeBoer David R. , Dexter Matthew R. , Gugliucci Nicole E. , Jacobs Daniel C. , Klima Pat , Liu Adrian , MacMahon David H. E. , Manley Jason R. , Pober Jonathan C. , Stefan Irina I. , Walbrugh William P. 
Published: February 2017

Abstract
Polarized foreground emission is a potential contaminant of attempts to measure the fluctuation power spectrum of highly redshifted 21 cm H i emission from the epoch of reionization. Using the Donald C. Backer Precision Array for Probing the Epoch of Reionization, we present limits on the observed power spectra of all four Stokes parameters in two frequency bands, centered at 126 MHz (z = 10.3) and 164 MHz (z = 7.66), for a three-month observing campaign of a deployment involving 32 antennas, for which results on the unpolarized power spectrum have been reported at z = 7.7 (by Parsons et al.) and at

(by Jacobs et al.). The power spectra in this paper are processed in the same way as by those authors, and show no definitive detection of polarized power. This nondetection is consistent with what is known about polarized sources, combined with the suppression of polarized power by fluctuations in the ionospheric rotation measure, which can strongly affect Stokes Q and U. We are able to show that the net effect of polarized leakage is a negligible contribution at the levels of the limits reported by Parsons et al. and Jacobs et al.
Void Profile from Planck Lensing Potential Map
Authors: Chantavat Teeraparb , Sawangwit Utane , Wandelt Benjamin D. 
Published: February 2017

Abstract
We use the lensing potential map from Planck CMB lensing reconstruction analysis and the “Public Cosmic Void Catalog” to measure the stacked void lensing potential. We have made an attempt to fit the HSW void profile parameters from the stacked lensing potential. In this profile, four parameters are needed to describe the shape of voids with different characteristic radii R

V
. However, we have found that after reducing the background noise by subtracting the average background, there is a residue lensing power left in the data. The inclusion of the environment shifting parameter,

, is necessary to get a better fit to the data with the residue lensing power. We divide the voids into two redshift bins: cmass1 (

) and cmass2 (

). Our best-fit parameters are

,

,

,

,

for the cmass1 sample with 123 voids and

,

,

,

,

for the cmass2 sample with 393 voids at 68% C.L. The addition of the environment shifting parameter is consistent with the conjecture that the Sloan Digital Sky Survey voids reside in an underdense region.
Scaling Relations of Mass, Velocity, and Radius for Disk Galaxies
Authors: Schulz Earl 
Published: February 2017

Abstract
I demonstrate four tight correlations of total baryonic mass, velocity, and radius for a set of nearby disk galaxies: the mass–velocity relation

the mass–radius relation

; the radius–velocity relation

and the mass–radius–velocity relation

. The mass–velocity relation is the familiar Baryonic Tully–Fisher relation, and versions of the other three relations, using magnitude rather than baryonic mass, are also well known. These four observed correlations follow from a pair of more fundamental relations. First, the centripetal acceleration at the edge of the stellar disk is proportional to the acceleration predicted by Newtonian physics, and second, this acceleration is a constant that is related to Milgrom’s constant. The two primary relations can be manipulated algebraically to generate the four observed correlations and allow little room for dark matter inside the radius of the stellar disk. The primary relations do not explain the velocity of the outer gaseous disks of spiral galaxies, which do not trace the Newtonian gravitational field of the observed matter.
IRIS, Hinode, SDO, and RHESSI Observations of a White Light Flare Produced Directly by Non-thermal Electrons
Authors: Lee Kyoung-Sun , Imada Shinsuke , Watanabe Kyoko , Bamba Yumi , Brooks David H. 
Published: February 2017

Abstract
An X1.6 flare occurred in active region AR 12192 on 2014 October 22 at 14:02 UT and was observed by Hinode, IRIS, SDO, and RHESSI. We analyze a bright kernel that produces a white light (WL) flare with continuum enhancement and a hard X-ray (HXR) peak. Taking advantage of the spectroscopic observations of IRIS and Hinode/EIS, we measure the temporal variation of the plasma properties in the bright kernel in the chromosphere and corona. We find that explosive evaporation was observed when the WL emission occurred, even though the intensity enhancement in hotter lines is quite weak. The temporal correlation of the WL emission, HXR peak, and evaporation flows indicates that the WL emission was produced by accelerated electrons. To understand the WL emission process, we calculated the energy flux deposited by non-thermal electrons (observed by RHESSI) and compared it to the dissipated energy estimated from a chromospheric line (Mg ii triplet) observed by IRIS. The deposited energy flux from the non-thermal electrons is about (3–7.7) × 1010 erg cm−2 s−1 for a given low-energy cutoff of 30–40 keV, assuming the thick-target model. The energy flux estimated from the changes in temperature in the chromosphere measured using the Mg ii subordinate line is about (4.6–6.7) × 109 erg cm−2 s−1: ∼6%–22% of the deposited energy. This comparison of estimated energy fluxes implies that the continuum enhancement was directly produced by the non-thermal electrons.
Formation of Galactic Prominence in the Galactic Central Region
Authors: Peng Chih-Han , Matsumoto Ryoji 
Published: February 2017

Abstract
We carried out 2.5-dimensional resistive MHD simulations to study the formation mechanism of molecular loops observed by Fukui et al. in the Galactic central region. Since it is hard to form molecular loops by lifting up dense molecular gas, we study the formation mechanism of molecular gas in rising magnetic arcades. This model is based on the in situ formation model of solar prominences, in which prominences are formed by cooling instability in helical magnetic flux ropes formed by imposing converging and shearing motion at footpoints of the magnetic arch anchored to the solar surface. We extended this model to Galactic center scale (a few hundreds of parsecs). Numerical results indicate that magnetic reconnection taking place in the current sheet that formed inside the rising magnetic arcade creates dense blobs confined by the rising helical magnetic flux ropes. Thermal instability taking place in the flux ropes forms dense molecular filaments floating at high Galactic latitude. The mass of the filament increases with time and can exceed

10

5

M

⊙

.
Dynamical Formation of Low-mass Merging Black Hole Binaries like GW151226
Authors: Chatterjee Sourav , Rodriguez Carl L. , Kalogera Vicky , Rasio Frederic A. 
Published: February 2017

Abstract
Using numerical models for star clusters spanning a wide range in ages and metallicities (Z) we study the masses of binary black holes (BBHs) produced dynamically and merging in the local universe (z ≲ 0.2). After taking into account cosmological constraints on star formation rate and metallicity evolution, which realistically relate merger delay times obtained from models with merger redshifts, we show here for the first time that while old, metal-poor globular clusters can naturally produce merging BBHs with heavier components, as observed in GW150914, lower-mass BBHs like GW151226 are easily formed dynamically in younger, higher-metallicity clusters. More specifically, we show that the mass of GW151226 is well within 1σ of the mass distribution obtained from our models for clusters with Z/Z⊙ ≳ 0.5. Indeed, dynamical formation of a system like GW151226 likely requires a cluster that is younger and has a higher metallicity than typical Galactic globular clusters. The LVT151012 system, if real, could have been created in any cluster with Z/Z⊙ ≲ 0.25. On the other hand, GW150914 is more massive (beyond 1σ) than typical BBHs from even the lowest-metallicity (Z/Z⊙ = 0.005) clusters we consider, but is within 2σ of the intrinsic mass distribution from our cluster models with Z/Z⊙ ≲ 0.05; of course, detection biases also push the observed distributions toward higher masses.
Searching for Rapid Orbital Decay of WASP-18b
Authors: Wilkins Ashlee N. , Delrez Laetitia , Barker Adrian J. , Deming Drake , Hamilton Douglas , Gillon Michael , Jehin Emmanuel 
Published: February 2017

Abstract
The WASP-18 system, with its massive and extremely close-in planet, WASP-18b (M

p
= 10.3M

J
, a = 0.02 au, P = 22.6 hr), is one of the best-known exoplanet laboratories to directly measure Q′, the modified tidal quality factor and proxy for efficiency of tidal dissipation, of the host star. Previous analysis predicted a rapid orbital decay of the planet toward its host star that should be measurable on the timescale of a few years, if the star is as dissipative as is inferred from the circularization of close-in solar-type binary stars. We have compiled published transit and secondary eclipse timing (as observed by WASP, TRAPPIST, and Spitzer) with more recent unpublished light curves (as observed by TRAPPIST and Hubble Space Telescope) with coverage spanning nine years. We find no signature of a rapid decay. We conclude that the absence of rapid orbital decay most likely derives from Q′ being larger than was inferred from solar-type stars and find that Q′ ≥ 1 × 106, at 95% confidence; this supports previous work suggesting that F stars, with their convective cores and thin convective envelopes, are significantly less tidally dissipative than solar-type stars, with radiative cores and large convective envelopes.
Prospective Surveillance of Antiviral Resistance in Hospitalized Infants Less than 12 Months of Age with A(H3N2) Influenza Infection and Treated with Oseltamivir
Authors: Rath Barbara , Chen Xi , Spies Vera , Muehlhans Susann , Obermeier Patrick , Tief Franziska , Seeber Lea , Karsch Katharina , Milde Jeanette , Skopnik Heino , Schweiger Brunhilde , Duwe Susanne C 
Published: February 2017

Background Infants exhibit elevated influenza virus loads and prolonged viral shedding, which may increase the risk for resistance development, especially in cases of suboptimal exposure to antiviral therapy. Methods We performed a prospective surveillance of hospitalized infants undergoing oseltamivir therapy during the 2008–2009 and 2011–2012 influenza seasons at two paediatric hospitals in Germany. A total of 37 infants less than 1 year of age with laboratory confirmed influenza A(H3N2) infection received oseltamivir as per physician's order for 5 days (2008–2009 season: 2 mg/kg twice daily; 2011–2012 season: 2.0 mg/kg; 2.5 mg/kg and 3.0 mg/kg twice daily for infants <1 month; 2–3 months and 4–12 months, respectively). Virus load, the susceptibility to neuraminidase inhibitors (NAIs), and the presence of molecular markers of resistance to NAIs was assessed for influenza viruses recovered from respiratory samples collected at baseline and during follow-up visits. Results Overall, 73% of the infants continued to shed viral RNA detectable by reverse transcription (RT)-PCR after dose number 10 of oseltamivir; 12 infants shed viruses, 2 of them (both 9 months of age) shed resistant viruses. Resistance was characterized by ≥1,000-fold increase of 50% inhibitory concentration (IC50) for oseltamivir, up to 50-fold for zanamivir and elevated Km values when compared to susceptible A(H3N2) strains. Sanger sequencing revealed the selection of the NA-R292K substitution in both instances (after dose number 10 on day 6). Conclusions Our data suggest that it may be relevant to monitor antiviral resistance systematically in all infants, considering that the European Medicines Agency has recently extended the licensure for oseltamivir to include full-term infants.
Infans adoptée, adolescente adoptante
Authors: de Kernier Nathalie 
Published: February 2017

En revisitant des temps de psychothérapie d’une adolescente adoptée bébé, consultant à la suite d’une tentative de suicide, le processus analytique est vu comme analogue à un processus d’adoption réciproque, incluant les parents adoptifs confiant l’adolescente en thérapie. Le travail analytique favorise chez l’adolescente l’adoption de parties d’elle clivées, l’amenant à se réapproprier son histoire. Devenir adulte impliquera la possibilité de choisir ses affiliations : à son tour, elle pourra adopter.
Lost in transition
Authors: Monzani Stefano 
Published: February 2017

Si l’adoption à l’adolescence se passe souvent sans de graves écueils, il existe néanmoins des situations où la collusion entre les aspects traumatiques liés au passé de l’enfant et sa réactivation à l’adolescence, et la vulnérabilité des parents, empêchent toute affiliation, toute greffe. L’auteur a appelé ces situations de grande détresse individuelle et familiale, états de survivance, en référence aux écrits de J. Altounian.
Les images « trash » sur réseaux sociaux : souffrance ou passage pubertaire ?
Authors: Papot Vincent , Haza Marion 
Published: February 2017

Grâce aux médias sociaux, l’adolescent expérimente sa relation aux autres et à lui-même. Parfois, ces expressions identitaires par l’image dérivent. Même si les contenus que l’adolescent partage peuvent choquer, l’hypothèse d’une « déviance » a ses limites. Ainsi, sur Internet ce qui distingue la souffrance psychique d’une publication typiquement adolescente serait la capacité du jeune à s’inscrire après-coup dans un croisement narcissique et objectal, au cœur du « désir d’extimité ».
The Activating Human NK Cell Receptor KIR2DS2 Recognizes a β2-Microglobulin–Independent Ligand on Cancer Cells
Authors: Thiruchelvam-Kyle Lavanya , Hoelsbrekken Sigurd E. , Saether Per C. , Bjørnsen Elisabeth Gyllensten , Pende Daniela , Fossum Sigbjørn , Daws Michael R. , Dissen Erik 
Published: February 2017

Abstract
The functions of activating members of the killer cell Ig-like receptor (KIR) family are not fully understood, as the ligands for these receptors are largely unidentified. In this study, we report that KIR2DS2 reporter cells recognize a ligand expressed by cancer cell lines. All cancer targets recognized by KIR2DS2 were also recognized by KIR2DL2 and KIR2DL3 reporters. Trogocytosis of membrane proteins from the cancer targets was observed with responding reporter cells, indicating the formation of KIR2DS2 ligand–specific immunological synapses. HLA-C typing of target cells showed that KIR2DS2 recognition was independent of the HLA C1 or C2 group, whereas targets cells that were only recognized by KIR2DL3 expressed C1 group alleles. Anti–HLA class I Abs blocked KIR2DL3 responses toward C1-expressing targets, but they did not block KIR2DS2 recognition of cancer cells. Small interfering RNA knockdown of β2-microglobulin reduced the expression of class I H chain on the cancer targets by &gt;97%, but it did not reduce the KIR2DS2 reporter responses, indicating a β2-microglobulin–independent ligand for KIR2DS2. Importantly, KIR2DL3 responses toward some KIR2DS2 ligand–expressing cells were also undiminished after β2-microglobulin knockdown, and they were not blocked by anti–HLA class I Abs, suggesting that KIR2DL3, in addition to the traditional HLA-C ligands, can bind to the same β2-microglobulin–independent ligand as KIR2DS2. These observations indicate the existence of a novel, presently uncharacterized ligand for the activating NK cell receptor KIR2DS2. Molecular identification of this ligand may lead to improved KIR-HLA mismatching in hematopoietic stem cell transplantation therapy for leukemia and new, more specific NK cell–based cancer therapies.