pinecone/core-2020-05-10-deduplication huggingface dataset:
Isotopic 32 S/ 33 S ratio as a diagnostic of presolar grains from novae

Measurements of sulphur isotopes in presolar grains can help to identify the astrophysical sites in which these grains were formed. A more precise thermonuclear rate of the 33 S( p,γ ) 34 Cl reaction is required, however, to assess the diagnostic ability of sulphur isotopic ratios. We have studied the 33 S( 3 He,d) 34 Cl proton-transfer reaction at 25 MeV using a high-resolution quadrupole–dipole–dipole–dipole magnetic spectrograph. Deuteron spectra were measured at ten scattering angles between 10° and 55°. Twenty-four levels in 34 Cl over Ex=4.6–5.9 MeV were observed, including three levels for the first time. Proton spectroscopic factors were extracted for the first time for levels above the 33 S + p threshold, spanning the energy range required for calculations of the thermonuclear 33 S( p,γ ) 34 Cl rate in classical nova explosions. We have determined a new 33 S( p,γ ) 34 Cl rate using a Monte Carlo method and have performed new hydrodynamic nova simulations to determine the impact on nova nucleosynthesis of remaining nuclear physics uncertainties in the reaction rate. We find that these uncertainties lead to a factor of ≤5 variation in the 33 S( p,γ ) 34 Cl rate over typical nova peak temperatures, and variation in the ejected nova yields of S Ca isotopes by ≤20% . In particular, the predicted 32 S/ 33 S ratio is 110–130 for the nova model considered, compared to 110–440 with previous rate uncertainties. As recent type II supernova models predict ratios of 130–200, the 32 S/ 33 S ratio may be used to distinguish between grains of nova and supernova origin
Paleoearthquakes of the Düzce fault (North Anatolian Fault Zone): implications for earthquake recurrence

The November 12, 1999, Mw 7.1 earthquake, ruptured the Düzce segment of the North Anatolian Fault Zone and produced ca. 40 km-long surface ruptures. 
To learn about recurrence of large surface faulting earthquakes on this fault, we undertook paleoseismological trench investigations. We found evidence for repeated surface faulting paleoearthquakes pre-dating the 1999 event. Dating was based on radiocarbon and 210Pb analyses as well as on archaeological considerations. By merging information obtained from all the trenches we reconstructed the seismic history of the Düzce fault for the past millennium. We correlated coeval events between different trench sites under the assumption that, similarly to the 1999 event, paleoearthquakes ruptured the whole Düzce fault. Besides the 1999 earthquake, prior surface faulting earthquakes are dated as follows: AD1685-1900 (possibly end of 19th century); AD1685-1900 (possibly close to AD 1700); AD1185-1640; AD685-1220 (possibly AD800-1000). Thus, the AD1719, AD1878 and AD1894 historical earthquakes, may have ruptured the Düzce fault and not the faults they are usually associated to or, alternatively, a cascade of events occurred on the Düzce and nearby faults (similarly to the Izmit and Düzce 1999 earthquakes). 
Five events since AD 685-1220 (possibly AD800-1000), would yield an average recurrence time for the Düzce fault, of 200-325 yr (possibly 250-300 yr). The three most recent earthquakes, including 1999, occurred within 300 yr and may be suggestive of clustering. Assuming that the average 1999 slip is characteristic for this fault, the above recurrence times yield slip rates of 6.7-13.5 mm/yr
The XMM-Newton serendipitous survey - IV. Optical identification of the XMM-Newton medium sensitivity survey (XMS)

Aims.X-ray sources at intermediate fluxes (a few $\times$ 10-14 erg cm-2 s-1) with a sky density of ~100 deg-2 are responsible for a significant fraction of the cosmic X-ray background at various energies below 10 keV. The aim of this paper is to provide an unbiased and quantitative description of the X-ray source population at these fluxes and in various X-ray energy bands.\ud
Methods.We present the XMM-Newton Medium sensitivity Survey (XMS), including a total of 318 X-ray sources found among the serendipitous content of 25 XMM-Newton target fields. The XMS comprises four largely overlapping source samples selected at soft (0.5-2 keV), intermediate (0.5-4.5 keV), hard (2-10 keV) and ultra-hard (4.5-7.5 keV) bands, the first three of them being flux-limited.\ud
Results.We report on the optical identification of the XMS samples, complete to 85-95%. At the flux levels sampled by the XMS we find that the X-ray sky is largely dominated by Active Galactic Nuclei. The fraction of stars in soft X-ray selected samples is below 10%, and only a few per cent for hard selected samples. We find that the fraction of optically obscured objects in the AGN population stays constant at around 15-20% for soft and intermediate band selected X-ray sources, over 2 decades of flux. The fraction of obscured objects amongst the AGN population is larger (~35-45%) in the hard or ultra-hard selected samples, and constant across a similarly wide flux range. The distribution in X-ray-to-optical flux ratio is a strong function of the selection band, with a larger fraction of sources with high values in hard selected samples. Sources with X-ray-to-optical flux ratios in excess of 10 are dominated by obscured AGN, but with a significant contribution from unobscured AGN.Peer-reviewedPublisher Version4361
Half of the most luminous quasars may be obscured : investigating the nature of wise-selected hot dust-obscured galaxies

The Wide-field Infrared Survey Explorer mission has unveiled a rare population of high-redshift (z = 1–4.6), dusty, hyper-luminous galaxies, with infrared luminosities Lir>1013L⊙, and sometimes exceeding 1014 L⊙. Previous work has shown that their dust temperatures and overall far-infrared spectral energy distributions (SEDs) are significantly hotter than expected to be powered by star formation. We present here an analysis of the rest-frame optical through mid-infrared SEDs for a large sample of these so-called "hot, dust-obscured galaxies" (Hot DOGs). We find that the SEDs of Hot DOGs are generally well modeled by the combination of a luminous, yet obscured active galactic nuclei (AGNs) that dominates the rest-frame emission at $\lambda \gt 1\;\mu {\rm m}$ and the bolometric luminosity output, and a less luminous host galaxy that is responsible for the bulk of the rest optical/UV emission. Even though the stellar mass of the host galaxies may be as large as 10[Superscript: 11]–10[Superscript: 12] M⊙, the AGN emission, with a range of luminosities comparable to those of the most luminous QSOs known, require that either Hot DOGs have black hole masses significantly in excess of the local relations, or that they radiate significantly above the Eddington limit, at a level at least 10 times more efficiently than z ~ 2 QSOs. We show that, while rare, the number density of Hot DOGs is comparable to that of equally luminous but unobscured (i.e., Type 1) QSOs. This may be at odds with the trend suggested at lower luminosities for the fraction of obscured AGNs to decrease with increasing luminosity. That trend may, instead, reverse at higher luminosities. Alternatively, Hot DOGs may not be the torus-obscured counterparts of the known optically selected, largely unobscured, hyper-luminous QSOs, and may represent a new component of the galaxy evolution paradigm. Finally, we discuss the environments of Hot DOGs and statistically show that these objects are in regions as dense as those of known high-redshift proto-clusters.Peer-reviewedPublisher Versio
The plant cytoskeleton, NET3C, and VAP27 mediate the link between the plasma membrane and endoplasmic reticulum.

The cortical endoplasmic reticulum (ER) network in plants is a highly dynamic structure, and it contacts the plasma membrane (PM) at ER-PM anchor/contact sites. These sites are known to be essential for communication between the ER and PM for lipid transport, calcium influx, and ER morphology in mammalian and fungal cells. The nature of these contact sites is unknown in plants [1 and 2], and here, we have identified a complex that forms this bridge. This complex includes (1) NET3C, which belongs to a plant-specific superfamily (NET) of actin-binding proteins [3], (2) VAP27, a plant homolog of the yeast Scs2 ER-PM contact site protein [4 and 5], and (3) the actin and microtubule networks. We demonstrate that NET3C and VAP27 localize to puncta at the PM and that NET3C and VAP27 form homodimers/oligomers and together form complexes with actin and microtubules. We show that F-actin modulates the turnover of NET3C at these puncta and microtubules regulate the exchange of VAP27 at the same sites. Based on these data, we propose a model for the structure of the plant ER-PM contact sites
Ab initio potential energy surfaces, bound states, and electronic spectrum of the Ar–SH complex.

New ab initiopotential energy surfaces for the Π2ground electronic state of the Ar–SH complex are presented, calculated at the RCCSD(T)/aug-cc-pV5Z level. Weakly bound rotation-vibration levels are calculated using coupled-channel methods that properly account for the coupling between the two electronic states. The resulting wave functions are analyzed and a new adiabatic approximation including spin-orbit coupling is proposed. The ground-statewave functions are combined with those obtained for the excited Σ+2 state [D. M. Hirst, R. J. Doyle, and S. R. Mackenzie, Phys. Chem. Chem. Phys.6, 5463 (2004)] to produce transition dipole moments. Modeling the transition intensities as a combination of these dipole moments and calculated lifetime values [A. B. McCoy, J. Chem. Phys.109, 170 (1998)] leads to a good representation of the experimental fluorescence excitation spectrum [M.-C. Yang, A. P. Salzberg, B.-C. Chang, C. C. Carter, and T. A. Miller, J. Chem. Phys.98, 4301 (1993)]
Increasing Autumn drought over Southern China associated with ENSO regime shift

In the two most recent decades, more frequent drought struck southern China during autumn, causing an unprecedented water crisis. We found that the increasing autumn drought is largely attributed to an ENSO regime shift. Compared to traditional eastern-Pacific (EP) El Niño, central-Pacific (CP) El Niño events have occurred more frequently, with maximum sea surface temperature anomalies located near the dateline. Southern China usually experiences precipitation surplus during the autumn of EP El Niño years, while the CP El Niño tends to produce precipitation deficits. Since the CP El Niño has occurred more frequently while EP El Niño has become less common after the early 1990s, there has been a significant increase in the frequency of autumn drought. This has implications for increasing precipitation shortages over southern China in a warming world, in which CP El Niño events have been suggested to become more common
Performance of an acoustic emission monitoring system to detect subsurface ground movement at Flat Cliffs, North Yorkshire, UK

This paper was presented at IAEG XII Congress - Engineering Geology for Society and Territory, Turin, 15th-19th September 2014. The final publication is available at http://link.springer.com/book/10.1007/978-3-319-09057-3This paper describes the performance of an innovative acoustic emission sub-surface slope displacement monitoring system installed in a large coastal landslide complex at Flat Cliffs, North Yorkshire, northeast England. Cliff instability is in-dicated by repeat deformation of an access road that serves a settlement of about 50 houses. As part of an extensive ground investigation, a sensor that can quantify acoustic emission was installed adjacent to a standard inclinometer, and continuous monitoring of acoustic emission has since taken place. The acoustic sensor has detected periods of slope deformation that are confirmed by manual surveys of the inclinometer. Performance is demonstrated using time series of acoustic measurements compared with ground deformations and triggering rain-fall events
An extreme planetary system around HD 219828 : one long-period super Jupiter to a hot-Neptune host star

Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims. We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods. We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results. We announce the discovery of a long period (P = 13.1 yr) massive (m sini = 15.1 MJup) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions. The HD 219828 system is extreme and unique in several aspects. First, among all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.Publisher PDFPeer reviewe
Pion-nucleon correlations in finite nuclei in a relativistic framework:
  effects on the shell structure

The relativistic particle-vibration coupling (RPVC) model is extended by the
inclusion of spin- and isospin-flip excitation modes into the phonon space,
introducing a new mechanism of dynamical interaction between nucleons with
different isospin in the nuclear medium. Protons and neutrons exchange by
collective modes which are formed by isovector $\pi$ and $\rho$-mesons, in
turn, softened considerably because of coupling to nucleons of the medium.
These modes are investigated within the proton-neutron relativistic random
phase approximation (pn-RRPA) and relativistic proton-neutron time blocking
approximation (pn-RTBA). The appearance of isospin-flip states with sizable
transition probabilities at low energies points out that they are likely to
couple to the single-particle degrees of freedom and, in addition to isoscalar
low-lying phonons, to modify their spectroscopic characteristics. Such a
coupling is quantified for the shell structure of $^{100,132}$Sn and found
significant for the location of the dominant single-particle states.Comment: Article; 9 pages, 6 figure
OIFITS 2: the 2nd version of the Data Exchange Standard for Optical
  (Visible/IR) Interferometry

This paper describes version 2 of the OI Exchange Format (OIFITS), the
standard for exchanging calibrated data from optical (visible/infrared)
interferometers. This IAU-endorsed standard has been in use for 10 years at
most of the past and current optical interferometer projects, including COAST,
NPOI, IOTA, CHARA, VLTI, PTI and the Keck interferometer. Software is available
for reading, writing and merging OI Exchange Format files. This version 2
provides definitions of additional data tables (e.g. for polarisation
measurements), addressing the needs of future interferometric instruments. Also
included are data columns for a more rigorous description of measurement errors
and their correlations. In that, this document is a step towards the design of
a common data model for optical interferometry. Finally, the main OIFITS header
is expanded with several new keywords summarising the content to allow data
base searches.Comment: 12 pages, 13 tables. Initially published in Astronomy and
  Astrophysics. This is a normative document, intended to be versioned here on
  ArXiv. This is version #4, with minor changes wrt. the publication in A&A,
  clarifying the some header formats and describing more clearly the OI_CORR
  tabl
A proposed new diagnostic for Herbig disc geometry: FWHM versus J of CO
  ro-vibrational lines

Aims. CO ro-vibrational lines observed from Herbig group II discs are seen to
be often broad while the same lines observed from group I discs are often
narrow. This difference is not well understood. In this paper we explore the
underlying cause for this difference and provide a pathway for a better
understanding of the geometry and structure of the inner discs around Herbig
Ae/Be stars. Methods. High-spectral-resolution infrared spectra of CO
ro-vibrational emission from six Herbig Ae/Be candidate stars were taken with
CRIRES (CRyogenic high-resolution InfraRed Echelle Spectrograph) at the VLT
(Very Large Telescope). From these spectra, we produce individual and co-added
CO ro-vibrational line profiles. We investigate line profile shape differences,
and we explore the FWHM (Full Width Half Maximum) variations with J quantum
number in the context of disc geometry. Furthermore, we put our new sources
into the context of earlier observed sources to study a large sample. For
comparison, we also investigate the FWHM variations with J of modelled CO
ro-vibrational lines from two typical disc geometries produced with the
thermo-chemical disc modelling code ProDiMo. Results. - abbreviated - Comparing
dust and gas inner disc geometries (inferred by SED and CO ro-vibrational
emission) for the expanded sample of observed Herbig discs, we find no clear
correspondence between the SED groups of the sources and their inner CO radius.
Conclusions. The FWHM versus J is a potential new gas diagnostic for the inner
disc with e.g. a constant FWHM versus J indicating the presence of a large gas
hole or gap. Both models and observations indicate the potential of this new
diagnostic. - abbreviated -Comment: accepted for publication in A&
SIM$(1)$--VSR Maxwell-Chern-Simons electrodynamics

In this paper we propose a very special relativity (VSR)-inspired
generalization of the Maxwell-Chern-Simons (MCS) electrodynamics. This proposal
is based upon the construction of a proper study of the SIM$(1)$--VSR
gauge-symmetry. It is shown that the VSR nonlocal effects present a significant
and health departure from the usual MCS theory. The classical dynamics is
analysed in full detail, by studying the solution for the electric field and
static energy for this configuration. Afterwards, the interaction energy
between opposite charges are derived and we show that the VSR effects play an
important part in obtaining a (novel) finite expression for the static
potential.Comment: 15 pages, 2 figures; to appear in PL
Comments on the symmetry of AdS$_6$ solutions in String/M-theory and
  Killing spinor equations

It was recently pointed out in \cite{Kim:2015hya} that AdS$_6$ solutions in
IIB theory enjoy an extended symmetry structure and the consistent truncation
to $D=4$ internal space leads to a nonlinear sigma model with target
$SL(3,\mathbb{R})/SO(2,1)$. We continue to study the purely bosonic $D=4$
effective action, and elucidate how the addition of scalar potential term still
allows Killing spinor equations in the absence of gauge fields. In particular,
the potential turns out to be a single diagonal component of the coset
representative. Furthermore, we perform a general analysis of the integrability
conditions of Killing spinor equations and establish that the effective action
can be in fact generalized to arbitrary sizes and signatures, e.g. with target
$SL(n,\mathbb{R})/SO(p,n-p)$ and the scalar potential expressible by a single
diagonal component of the coset representative. We also comment on a similar
construction and its generalizations of effective $D=5$ purely bosonic
non-linear sigma model action related to AdS$_6$ in M-theory.Comment: v2: 17 pages, version published in PL
Quantum Cognition Beyond Hilbert Space I: Fundamentals

The formalism of quantum theory in Hilbert space has been applied with
success to the modeling and explanation of several cognitive phenomena, whereas
traditional cognitive approaches were problematical. However, this 'quantum
cognition paradigm' was recently challenged by its proven impossibility to
simultaneously model 'question order effects' and 'response replicability'. In
Part I of this paper we describe sequential dichotomic measurements within an
operational and realistic framework for human cognition elaborated by
ourselves, and represent them in a quantum-like 'extended Bloch representation'
where the Born rule of quantum probability does not necessarily hold. In Part
II we apply this mathematical framework to successfully model question order
effects, response replicability and unpacking effects, thus opening the way
toward quantum cognition beyond Hilbert space.Comment: 10 pages, 2 figure
Optical and ultraviolet observations of a strong flare in the young, single K2 dwarf LQ Hya

We present high-resolution optical echelle spectra and IUE observations during a strong flare on 1993 December 22 in the very active, young, rapidly rotating, single K2 dwarf LQ Hya. The initial impulsive phase of the flare, which started sometime between 2:42 ut and 4:07 ut, was characterized by strong optical continuum enhancement and blueshifted emission lines with broad wings. The optical chromospheric lines reached their maximum intensity at ≈ 5:31 ut, by which time the blueshift vanished and the optical continuum enhancement had sharply decreased. Thereafter, the line emission slowly decreased and the lines redshift in a gradual phase that lasted at least two more hours. The Mg II lines behaved similarly. Quiescent C IV flux levels were not recovered until 21 h later, though a data gap and a possible second flare make the interpretation uncertain. In addition to the typically flare-enhanced emission lines (e.g., H α and H β), we observe He I D_3 going into emission, plus excess emission (after subtraction of the quiescent spectrum) in other He I and several strong neutral metal lines (e.g., Mg I b). Flare enhancement of the far-ultraviolet continuum generally agrees with an Si I recombination model. We estimate the total flare energy, and discuss the broad components, asymmetries and Doppler shifts seen in some of the emission lines