pinecone/core-2020-05-10-deduplication huggingface dataset:
A scalable dataflow accelerator for real time onboard hyperspectral image classification

© Springer International Publishing Switzerland 2016.Real-time hyperspectral image classification is a necessary primitive in many remotely sensed image analysis applications. Previous work has shown that Support Vector Machines (SVMs) can achieve high classification accuracy, but unfortunately it is very computationally expensive. This paper presents a scalable dataflow accelerator on FPGA for real-time SVM classification of hyperspectral images.To address data dependencies, we adapt multi-class classifier based on Hamming distance. The architecture is scalable to high problem dimensionality and available hardware resources. Implementation results show that the FPGA design achieves speedups of 26x, 1335x, 66x and 14x compared with implementations on ZYNQ, ARM, DSP and Xeon processors. Moreover, one to two orders of magnitude reduction in power consumption is achieved for the AVRIS hyperspectral image datasets
Analyzing Locality of Mobile Messaging Traffic using the MATAdOR
  Framework

Mobile messaging services have gained a large share in global
telecommunications. Unlike conventional services like phone calls, text
messages or email, they do not feature a standardized environment enabling a
federated and potentially local service architecture. We present an extensive
and large-scale analysis of communication patterns for four popular mobile
messaging services between 28 countries and analyze the locality of
communication and the resulting impact on user privacy. We show that server
architectures for mobile messaging services are highly centralized in single
countries. This forces messages to drastically deviate from a direct
communication path, enabling hosting and transfer countries to potentially
intercept and censor traffic. To conduct this work, we developed a measurement
framework to analyze traffic of such mobile messaging services. It allows to
conduct automated experiments with mobile messaging applications, is
transparent to those applications and does not require any modifications to the
applications.Comment: To appear at Passive and Active Measurements Conference 201
Mental Lexicon Growth Modelling Reveals the Multiplexity of the English
  Language

In this work we extend previous analyses of linguistic networks by adopting a
multi-layer network framework for modelling the human mental lexicon, i.e. an
abstract mental repository where words and concepts are stored together with
their linguistic patterns. Across a three-layer linguistic multiplex, we model
English words as nodes and connect them according to (i) phonological
similarities, (ii) synonym relationships and (iii) free word associations. Our
main aim is to exploit this multi-layered structure to explore the influence of
phonological and semantic relationships on lexicon assembly over time. We
propose a model of lexicon growth which is driven by the phonological layer:
words are suggested according to different orderings of insertion (e.g. shorter
word length, highest frequency, semantic multiplex features) and accepted or
rejected subject to constraints. We then measure times of network assembly and
compare these to empirical data about the age of acquisition of words. In
agreement with empirical studies in psycholinguistics, our results provide
quantitative evidence for the hypothesis that word acquisition is driven by
features at multiple levels of organisation within language.Comment: 14 pages, published in the Proceedings of the 7th Workshop on Complex
  Networks CompleNet 2016. Complex Systems VII, Volume 644 of the series
  Studies in Computational Intelligence pp 267-279, 201
Modeling and Analysis of Dependability and Interdependency Failures in Smart Grids: Study on how the wide usage of ICT changes the Dependability in the future Power Grid

The transition from the current electrical power grid towards a smart grid is driven\ud
by new technologies and services. Traditional dedicated power grid components\ud
are exchanged with more powerful and highly configurable devices that are interconnected\ud
and help monitoring and controlling the power grid. The power grid is\ud
a critical infrastructure with high dependability requirements. The pervasive use\ud
of information and communication technology (ICT) to support the operation in\ud
the smart grid creates a complex interdependent system in which the dependability\ud
of the ICT systems plays an important role for the overall dependability. Additionally,\ud
interdependent system-of-systems feature new failure modes not found in\ud
simple systems. Therefore, it becomes crucial to understand and address the dependability\ud
issues in the smart grid in order not to risk a decreasing dependability\ud
with the introduction of new technology.\ud
The objective of this thesis has been to analyze how the dependability of the\ud
power grid changes with the introduction of smart grid technologies, to propose\ud
new dependability models and propose operational support mechanisms for the\ud
control center to detect and master the expected dependability issues in the smart\ud
grid. The first step of the research was to conduct literature studies to find new dependability\ud
challenges in the smart grid. Based on that, the consequences of these\ud
new challenges are assessed with the help of analytical models and simulations.\ud
My findings show that there are several challenges such as cascading and escalating\ud
failures, latent errors and a risk of automation waiting when transitioning\ud
towards a smart grid. The qualitative and quantitative analysis show that these\ud
effects can have a strong impact on the total dependability of the smart grid and\ud
need to be considered. The analysis also shows that smart services like demand\ud
response or automatic detection and isolation of failures can help improving the\ud
dependability if implemented with the right supporting measures. As a conclusion\ud
from the analysis, I give a list of guidelines for the control center on how to\ud
address the future challenges. One of the central advices from this thesis to the\ud
electrical utilities is, that they should try to thoroughly understand their specific interdependencies by analyzing their systems, processes and organizational structure.\ud
The next step is then to create awareness inside the company and invest in\ud
preparedness and mitigation strategies.\ud
Overall, this thesis contributes to the discussion on new dependability challenges\ud
in the smart grid, the definition of realistic use cases illustrating how they\ud
might affect the system, the quantification of their consequences, and the discussion\ud
on how the utilities might address these new challenges
ESPRESSO on VLT: An Instrument for Exoplanet Research

ESPRESSO (Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic
Observations) is a VLT ultra-stable high resolution spectrograph that will be
installed in Paranal Observatory in Chile at the end of 2017 and offered to the
community by 2018. The spectrograph will be located at the Combined-Coud\'e
Laboratory of the VLT and will be able to operate with one or (simultaneously)
several of the four 8.2 m Unit Telescopes (UT) through four optical Coud\'e
trains. Combining efficiency and extreme spectroscopic precision, ESPRESSO is
expected to gaining about two magnitudes with respect to its predecessor HARPS.
We aim at improving the instrumental radial-velocity precision to reach the 10
cm s$^-1$ level, thus opening the possibility to explore new frontiers in the
search for Earth-mass exoplanets in the habitable zone of quiet, nearby G to
M-dwarfs. ESPRESSO will be certainly an important development step towards
high-precision ultra-stable spectrographs on the next generation of giant
telescopes such as the E-ELT.Comment: Invited Revie
Exoplanet Atmosphere Measurements from Transmission Spectroscopy and
  other Planet-Star Combined Light Observations

It is possible to learn a great deal about exoplanet atmospheres even when we
cannot spatially resolve the planets from their host stars. In this chapter, we
overview the basic techniques used to characterize transiting exoplanets -
transmission spectroscopy, emission and reflection spectroscopy, and full-orbit
phase curve observations. We discuss practical considerations, including
current and future observing facilities and best practices for measuring
precise spectra. We also highlight major observational results on the
chemistry, climate, and cloud properties of exoplanets.Comment: Accepted review chapter; Handbook of Exoplanets, eds. Hans J. Deeg
  and Juan Antonio Belmonte (Springer-Verlag). 22 pages, 6 figure
Radiative Transfer for Exoplanet Atmospheres

Remote sensing of the atmospheres of distant worlds motivates a firm
understanding of radiative transfer. In this review, we provide a pedagogical
cookbook that describes the principal ingredients needed to perform a radiative
transfer calculation and predict the spectrum of an exoplanet atmosphere,
including solving the radiative transfer equation, calculating opacities (and
chemistry), iterating for radiative equilibrium (or not), and adapting the
output of the calculations to the astronomical observations. A review of the
state of the art is performed, focusing on selected milestone papers.
Outstanding issues, including the need to understand aerosols or clouds and
elucidating the assumptions and caveats behind inversion methods, are
discussed. A checklist is provided to assist referees/reviewers in their
scrutiny of works involving radiative transfer. A table summarizing the
methodology employed by past studies is provided.Comment: 7 pages, no figures, 1 table. Filled in missing information in
  references, main text unchange
Exoplanet phase curves: observations and theory

Phase curves are the best technique to probe the three dimensional structure
of exoplanets' atmospheres. In this chapter we first review current exoplanets
phase curve observations and the particular challenges they face. We then
describe the different physical mechanisms shaping the atmospheric phase curves
of highly irradiated tidally locked exoplanets. Finally, we discuss the
potential for future missions to further advance our understanding of these new
worlds.Comment: Fig.5 has been updated. Table 1 and corresponding figures have been
  updated with new values for WASP-103b and WASP-18b. Contains a table
  sumarizing phase curve observation
Small Telescope Exoplanet Transit Surveys: XO

The XO project aims at detecting transiting exoplanets around bright stars
from the ground using small telescopes. The original configuration of XO
(McCullough et al. 2005) has been changed and extended as described here. The
instrumental setup consists of three identical units located at different
sites, each composed of two lenses equipped with CCD cameras mounted on the
same mount. We observed two strips of the sky covering an area of 520 deg$^2$
for twice nine months. We build lightcurves for ~20,000 stars up to magnitude
R~12.5 using a custom-made photometric data reduction pipeline. The photometric
precision is around 1-2% for most stars, and the large quantity of data allows
us to reach a millimagnitude precision when folding the lightcurves on
timescales that are relevant to exoplanetary transits. We search for periodic
signals and identify several hundreds of variable stars and a few tens of
transiting planet candidates. Follow-up observations are underway to confirm or
reject these candidates. We found two close-in gas giant planets so far, in
line with the expected yield.Comment: Invited review, 25 pages, 16 figure
SPECULOOS exoplanet search and its prototype on TRAPPIST

One of the most significant goals of modern science is establishing whether
life exists around other suns. The most direct path towards its achievement is
the detection and atmospheric characterization of terrestrial exoplanets with
potentially habitable surface conditions. The nearest ultracool dwarfs (UCDs),
i.e. very-low-mass stars and brown dwarfs with effective temperatures lower
than 2700 K, represent a unique opportunity to reach this goal within the next
decade. The potential of the transit method for detecting potentially habitable
Earth-sized planets around these objects is drastically increased compared to
Earth-Sun analogs. Furthermore, only a terrestrial planet transiting a nearby
UCD would be amenable for a thorough atmospheric characterization, including
the search for possible biosignatures, with near-future facilities such as the
James Webb Space Telescope. In this chapter, we first describe the physical
properties of UCDs as well as the unique potential they offer for the detection
of potentially habitable Earth-sized planets suitable for atmospheric
characterization. Then, we present the SPECULOOS ground-based transit survey,
that will search for Earth-sized planets transiting the nearest UCDs, as well
as its prototype survey on the TRAPPIST telescopes. We conclude by discussing
the prospects offered by the recent detection by this prototype survey of a
system of seven temperate Earth-sized planets transiting a nearby UCD,
TRAPPIST-1.Comment: Submitted as a chapter in the "Handbook of Exoplanets" (editors: H.
  Deeg & J.A. Belmonte; Section Editor: N. Narita). 16 pages, 4 figure
Bayesian Methods for Exoplanet Science

Exoplanet research is carried out at the limits of the capabilities of
current telescopes and instruments. The studied signals are weak, and often
embedded in complex systematics from instrumental, telluric, and astrophysical
sources. Combining repeated observations of periodic events, simultaneous
observations with multiple telescopes, different observation techniques, and
existing information from theory and prior research can help to disentangle the
systematics from the planetary signals, and offers synergistic advantages over
analysing observations separately. Bayesian inference provides a
self-consistent statistical framework that addresses both the necessity for
complex systematics models, and the need to combine prior information and
heterogeneous observations. This chapter offers a brief introduction to
Bayesian inference in the context of exoplanet research, with focus on time
series analysis, and finishes with an overview of a set of freely available
programming libraries.Comment: Invited revie
Circumstellar discs: What will be next?

This prospective chapter gives our view on the evolution of the study of
circumstellar discs within the next 20 years from both observational and
theoretical sides. We first present the expected improvements in our knowledge
of protoplanetary discs as for their masses, sizes, chemistry, the presence of
planets as well as the evolutionary processes shaping these discs. We then
explore the older debris disc stage and explain what will be learnt concerning
their birth, the intrinsic links between these discs and planets, the hot dust
and the gas detected around main sequence stars as well as discs around white
dwarfs.Comment: invited review; comments welcome (32 pages
Exoplanet Research with the Stratospheric Observatory for Infrared
  Astronomy (SOFIA)

When the Stratospheric Observatory for Infrared Astronomy (SOFIA) was
conceived and its first science cases defined, exoplanets had not been
detected. Later studies, however, showed that optical and near-infrared
photometric and spectrophotometric follow-up observations during planetary
transits and eclipses are feasible with SOFIA's instrumentation, in particular
with the HIPO-FLITECAM and FPI+ optical and near infrared (NIR) instruments.
Additionally, the airborne-based platform SOFIA has a number of unique
advantages when compared to other ground- and space-based observatories in this
field of research. Here we will outline these theoretical advantages, present
some sample science cases and the results of two observations from SOFIA's
first five observation cycles -- an observation of the Hot Jupiter HD 189733b
with HIPO and an observation of the Super-Earth GJ 1214b with FLIPO and FPI+.
Based on these early products available to this science case, we evaluate
SOFIA's potential and future perspectives in the field of optical and infrared
exoplanet spectrophotometry in the stratosphere.Comment: Invited review chapter, accepted for publication in "Handbook of
  Exoplanets" edited by H.J. Deeg and J.A. Belmonte, Springer Reference Work
The Rossiter-McLaughlin effect in Exoplanet Research

The Rossiter-McLaughlin effect occurs during a planet's transit. It provides
the main means of measuring the sky-projected spin-orbit angle between a
planet's orbital plane, and its host star's equatorial plane. Observing the
Rossiter-McLaughlin effect is now a near routine procedure. It is an important
element in the orbital characterisation of transiting exoplanets. Measurements
of the spin-orbit angle have revealed a surprising diversity, far from the
placid, Kantian and Laplacian ideals, whereby planets form, and remain, on
orbital planes coincident with their star's equator. This chapter will review a
short history of the Rossiter-McLaughlin effect, how it is modelled, and will
summarise the current state of the field before describing other uses for a
spectroscopic transit, and alternative methods of measuring the spin-orbit
angle.Comment: Review to appear as a chapter in the "Handbook of Exoplanets", ed. H.
  Deeg & J.A. Belmont
Signatures of Star-planet interactions

Planets interact with their host stars through gravity, radiation and
magnetic fields, and for those giant planets that orbit their stars within
$\sim$10 stellar radii ($\sim$0.1 AU for a sun-like star), star-planet
interactions (SPI) are observable with a wide variety of photometric,
spectroscopic and spectropolarimetric studies. At such close distances, the
planet orbits within the sub-alfv\'enic radius of the star in which the
transfer of energy and angular momentum between the two bodies is particularly
efficient. The magnetic interactions appear as enhanced stellar activity
modulated by the planet as it orbits the star rather than only by stellar
rotation. These SPI effects are informative for the study of the internal
dynamics and atmospheric evolution of exoplanets. The nature of magnetic SPI is
modeled to be strongly affected by both the stellar and planetary magnetic
fields, possibly influencing the magnetic activity of both, as well as
affecting the irradiation and even the migration of the planet and rotational
evolution of the star. As phase-resolved observational techniques are applied
to a large statistical sample of hot Jupiter systems, extensions to other
tightly orbiting stellar systems, such as smaller planets close to M dwarfs
become possible. In these systems, star-planet separations of tens of stellar
radii begin to coincide with the radiative habitable zone where planetary
magnetic fields are likely a necessary condition for surface habitability.Comment: Accepted for publication in the handbook of exoplanet
Models of Star-Planet Magnetic Interaction

Magnetic interactions between a planet and its environment are known to lead
to phenomena such as aurorae and shocks in the solar system. The large number
of close-in exoplanets that were discovered triggered a renewed interest in
magnetic interactions in star-planet systems. Multiple other magnetic effects
were then unveiled, such as planet inflation or heating, planet migration,
planetary material escape, and even modification of the host star properties.
We review here the recent efforts in modelling and understanding magnetic
interactions between stars and planets in the context of compact systems. We
first provide simple estimates of the effects of magnetic interactions and then
detail analytical and numerical models for different representative scenarii.
We finally lay out a series of future developments that are needed today to
better understand and constrain these fascinating interactions.Comment: 23 pages, 10 figures, accepted as a chapter in the Handbook of
  Exoplanet
Stellar Coronal and Wind Models: Impact on Exoplanets

Surface magnetism is believed to be the main driver of coronal heating and
stellar wind acceleration. Coronae are believed to be formed by plasma confined
in closed magnetic coronal loops of the stars, with winds mainly originating in
open magnetic field line regions. In this Chapter, we review some basic
properties of stellar coronae and winds and present some existing models. In
the last part of this Chapter, we discuss the effects of coronal winds on
exoplanets.Comment: Chapter published in the "Handbook of Exoplanets", Editors in Chief:
  Juan Antonio Belmonte and Hans Deeg, Section Editor: Nuccio Lanza. Springer
  Reference Work
Accretion of Planetary Material onto Host Stars

Accretion of planetary material onto host stars may occur throughout a star's
life. Especially prone to accretion, extrasolar planets in short-period orbits,
while relatively rare, constitute a significant fraction of the known
population, and these planets are subject to dynamical and atmospheric
influences that can drive significant mass loss. Theoretical models frame
expectations regarding the rates and extent of this planetary accretion. For
instance, tidal interactions between planets and stars may drive complete
orbital decay during the main sequence. Many planets that survive their stars'
main sequence lifetime will still be engulfed when the host stars become red
giant stars. There is some observational evidence supporting these predictions,
such as a dearth of close-in planets around fast stellar rotators, which is
consistent with tidal spin-up and planet accretion. There remains no clear
chemical evidence for pollution of the atmospheres of main sequence or red
giant stars by planetary materials, but a wealth of evidence points to active
accretion by white dwarfs. In this article, we review the current understanding
of accretion of planetary material, from the pre- to the post-main sequence and
beyond. The review begins with the astrophysical framework for that process and
then considers accretion during various phases of a host star's life, during
which the details of accretion vary, and the observational evidence for
accretion during these phases.Comment: 18 pages, 5 figures (with some redacted), invited revie
On the Detection of Extrasolar Moons and Rings

Since the discovery of a planet transiting its host star in the year 2000,
thousands of additional exoplanets and exoplanet candidates have been detected,
mostly by NASA's Kepler space telescope. Some of them are almost as small as
the Earth's moon. As the solar system is teeming with moons, more than a
hundred of which are in orbit around the eight local planets, and with all of
the local giant planets showing complex ring systems, astronomers have
naturally started to search for moons and rings around exoplanets in the past
few years. We here discuss the principles of the observational methods that
have been proposed to find moons and rings beyond the solar system and we
review the first searches. Though no exomoon or exoring has been unequivocally
validated so far, theoretical and technological requirements are now on the
verge of being mature for such discoveries.Comment: invited review, 17 pages, 4 figures (3 col, 1 b/w