bluuebunny/crossref_metadata_2025_split huggingface dataset:
BRIGHT GALAXIES AT HUBBLE’S REDSHIFT DETECTION FRONTIER: PRELIMINARY RESULTS AND DESIGN FROM THE REDSHIFT z ∼ 9–10 BoRG PURE-PARALLEL HST SURVEY
Authors: Calvi V. , Trenti M. , Stiavelli M. , Oesch P. , Bradley L. D. , Schmidt K. B. , Coe D. , Brammer G. , Bernard S. , Bouwens R. J. , Carrasco D. , Carollo C. M. , Holwerda B. W. , MacKenty J. W. , Mason C. A. , Shull J. M. , Treu T. 
Published: January 2016

ABSTRACT
We present the first results and design from the redshift z ∼ 9–10 Brightest of the Reionizing Galaxies Hubble Space Telescope survey BoRG[z9–10], aimed at searching for intrinsically luminous unlensed galaxies during the first 700 Myr after the Big Bang. BoRG[z9–10] is the continuation of a multi-year pure-parallel near-IR and optical imaging campaign with the Wide Field Camera 3. The ongoing survey uses five filters, optimized for detecting the most distant objects and offering continuous wavelength coverage from λ = 0.35 μm to λ = 1.7 μm. We analyze the initial ∼130 arcmin2 of area over 28 independent lines of sight (∼25% of the total planned) to search for

galaxies using a combination of Lyman-break and photometric redshift selections. From an effective comoving volume of (5–25) × 105 Mpc3 for magnitudes brighter than

in the

-band respectively, we find five galaxy candidates at

8.3–10 detected at high confidence (

), including a source at

8.4 with

(

), which, if confirmed, would be the brightest galaxy identified at such early times (

). In addition, BoRG[z9–10] data yield four galaxies with

. These new Lyman-break galaxies with

are ideal targets for follow-up observations from ground and space-based observatories to help investigate the complex interplay between dark matter growth, galaxy assembly, and reionization.
IDCS J1426.5+3508: THE MOST MASSIVE GALAXY CLUSTER AT z > 1.5
Authors: Brodwin Mark , McDonald Michael , Gonzalez Anthony H. , Stanford S. A. , Eisenhardt Peter R. , Stern Daniel , Zeimann Gregory R. 
Published: January 2016

ABSTRACT
We present a deep (100 ks) Chandra observation of IDCS J1426.5+3508, a spectroscopically confirmed, infrared-selected galaxy cluster at z = 1.75. This cluster is the most massive galaxy cluster currently known at z > 1.5, based on existing Sunyaev–Zel’dovich (SZ) and gravitational lensing detections. We confirm this high mass via a variety of X-ray scaling relations, including T
X–M, f

g
–M, Y
X–M, and L
X–M, finding a tight distribution of masses from these different methods, spanning M
500 = 2.3–3.3 × 1014
M
⊙, with the low-scatter Y
X-based mass

=

M
⊙. IDCS J1426.5+3508 is currently the only cluster at z > 1.5 for which X-ray, SZ, and gravitational lensing mass estimates exist, and these are in remarkably good agreement. We find a relatively tight distribution of the gas-to-total mass ratio, employing total masses from all of the aforementioned indicators, with values ranging from f
gas,500 = 0.087–0.12. We do not detect metals in the intracluster medium (ICM) of this system, placing a 2σ upper limit of

. This upper limit on the metallicity suggests that this system may still be in the process of enriching its ICM. The cluster has a dense, low-entropy core, offset by ∼30 kpc from the X-ray centroid, which makes it one of the few “cool core” clusters discovered at z > 1, and the first known cool core cluster at z > 1.2. The offset of this core from the large-scale centroid suggests that this cluster has had a relatively recent (≲500 Myr) merger/interaction with another massive system.
ON THE ACTIVE REGION BRIGHT GRAINS OBSERVED IN THE TRANSITION REGION IMAGING CHANNELS OF IRIS
Authors: Skogsrud H. , Voort L. Rouppe van der , Pontieu B. De 
Published: January 2016

ABSTRACT
The Interface Region Imaging Spectrograph (IRIS) provides spectroscopy and narrow band slit-jaw (SJI) imaging of the solar chromosphere and transition region at unprecedented spatial and temporal resolutions. Combined with high-resolution context spectral imaging of the photosphere and chromosphere as provided by the Swedish 1 m Solar Telescope (SST), we can now effectively trace dynamic phenomena through large parts of the solar atmosphere in both space and time. IRIS SJI 1400 images from active regions, which primarily sample the transition region with the Si iv 1394 and 1403 Å lines, reveal ubiquitous bright “grains” which are short-lived (two to five minute) bright roundish small patches of sizes 0.″5–1.″7 that generally move limbward with velocities up to about 30 km s−1. In this paper, we show that many bright grains are the result of chromospheric shocks impacting the transition region. These shocks are associated with dynamic fibrils (DFs), most commonly observed in Hα. We find that the grains show the strongest emission in the ascending phase of the DF, that the emission is strongest toward the top of the DF, and that the grains correspond to a blueshift and broadening of the Si iv lines. We note that the SJI 1400 grains can also be observed in the SJI 1330 channel which is dominated by C ii lines. Our observations show that a significant part of the active region transition region dynamics is driven from the chromosphere below rather than from coronal activity above. We conclude that the shocks that drive DFs also play an important role in the heating of the upper chromosphere and lower transition region.
NON-EQUILIBRIUM HELIUM IONIZATION IN AN MHD SIMULATION OF THE SOLAR ATMOSPHERE
Authors: Golding Thomas Peter , Leenaarts Jorrit , Carlsson Mats 
Published: January 2016

ABSTRACT
The ionization state of the gas in the dynamic solar chromosphere can depart strongly from the instantaneous statistical equilibrium commonly assumed in numerical modeling. We improve on earlier simulations of the solar atmosphere that only included non-equilibrium hydrogen ionization by performing a 2D radiation-magnetohydrodynamics simulation featuring non-equilibrium ionization of both hydrogen and helium. The simulation includes the effect of hydrogen Lyα and the EUV radiation from the corona on the ionization and heating of the atmosphere. Details on code implementation are given. We obtain helium ion fractions that are far from their equilibrium values. Comparison with models with local thermodynamic equilibrium (LTE) ionization shows that non-equilibrium helium ionization leads to higher temperatures in wavefronts and lower temperatures in the gas between shocks. Assuming LTE ionization results in a thermostat-like behavior with matter accumulating around the temperatures where the LTE ionization fractions change rapidly. Comparison of DEM curves computed from our models shows that non-equilibrium ionization leads to more radiating material in the temperature range 11–18 kK, compared to models with LTE helium ionization. We conclude that non-equilibrium helium ionization is important for the dynamics and thermal structure of the upper chromosphere and transition region. It might also help resolve the problem that intensities of chromospheric lines computed from current models are smaller than those observed.
CHANDRA OBSERVATIONS OF THE ELUSIVE PULSAR WIND NEBULA AROUND PSR B0656+14
Authors: Bîrzan L. , Pavlov G. G. , Kargaltsev O. 
Published: January 2016

ABSTRACT
PSR B0656+14 is a middle-aged pulsar with a characteristic age

kyr and spin-down power

erg s−1. Using Chandra data, we searched for a pulsar wind nebula (PWN). We found evidence of an extended emission in a 3.″5–15″ annulus around the pulsar, with a luminosity

erg s−1 (at the distance of 288 pc), which is a fraction of ∼0.05 of the nonthermal pulsar luminosity. If the extended emission is mostly due to a PWN, its X-ray effiency,

, is lower than those of most other known PWNe, but similar to that of the middle-aged Geminga pulsar. The small radial extent and nearly round shape of the putative PWN can be expained if the pulsar is receding (or approaching) in the direction close to the line of sight. The very soft spectrum of the extended emission (

) is much softer than those of typical PWNe; this could be explained by contribution from a faint dust scattering halo, which may dominate in the outer part of the extended emission.
THE INTERPLAY BETWEEN CHEMISTRY AND NUCLEATION IN THE FORMATION OF CARBONACEOUS DUST IN SUPERNOVA EJECTA
Authors: Lazzati Davide , Heger Alexander 
Published: January 2016

ABSTRACT
Core-collapse supernovae (CCSNe) are considered to be important contributors to the primitive dust enrichment of the interstellar medium in the high-redshift universe. Theoretical models of dust formation in stellar explosions have so far provided controversial results and a generally poor fit to the observations of dust formation in local supernovae. We present a new methodology for the calculation of carbonaceous dust formation in young supernova remnants. Our new technique uses both the nucleation theory and a chemical reaction network to allow us to compute the dust growth beyond the molecular level as well as consider the chemical erosion of the forming grains. We find that carbonaceous dust forms efficiently in the core of the ejecta, but takes several years to condensate, longer than previously estimated. It forms unevenly and remains concentrated in the inner part of the remnant. These results support the role of CCSNe as dust factories and provide new insight into the observations of SN 1987A, in which large amounts of dust have been detected to form on a timescale of years after core-collapse.
DISCOVERY OF A STELLAR OVERDENSITY IN ERIDANUS–PHOENIX IN THE DARK ENERGY SURVEY
Authors: Li T. S. , Balbinot E. , Mondrik N. , Marshall J. L. , Yanny B. , Bechtol K. , Drlica-Wagner A. , Oscar D. , Santiago B. , Simon J. D. , Vivas A. K. , Walker A. R. , Wang M. Y. , Abbott T. M. C. , Abdalla F. B. , Benoit-Lévy A. , Bernstein G. M. , Bertin E. , Brooks D. , Burke D. L. , Rosell A. Carnero , Kind M. Carrasco , Carretero J. , Costa L. N. da , DePoy D. L. , Desai S. , Diehl H. T. , Doel P. , Estrada J. , Finley D. A. , Flaugher B. , Frieman J. , Gruen D. , Gruendl R. A. , Gutierrez G. , Honscheid K. , James D. J. , Kuehn K. , Kuropatkin N. , Lahav O. , Maia M. A. G. , March M. , Martini P. , Ogando R. , Plazas A. A. , Reil K. , Romer A. K. , Roodman A. , Sanchez E. , Scarpine V. , Schubnell M. , Sevilla-Noarbe I. , Smith R. C. , Soares-Santos M. , Sobreira F. , Suchyta E. , Swanson M. E. C. , Tarle G. , Tucker D. , Zhang Y. ,   (The DES Collaboration)
Published: January 2016

ABSTRACT
We report the discovery of an excess of main-sequence turnoff stars in the direction of the constellations of Eridanus and Phoenix from the first-year data of the Dark Energy Survey (DES). The Eridanus–Phoenix (EriPhe) overdensity is centered around

and

and spans at least 30° in longitude and 10° in latitude. The Poisson significance of the detection is at least

. The stellar population in the overdense region is similar in brightness and color to that of the nearby globular cluster NGC 1261, indicating that the heliocentric distance of EriPhe is about

. The extent of EriPhe in projection is therefore at least ∼4 kpc by ∼3 kpc. On the sky, this overdensity is located between NGC 1261 and a new stellar stream discovered by DES at a similar heliocentric distance, the so-called Phoenix Stream. Given their similar distance and proximity to each other, it is possible that these three structures may be kinematically associated. Alternatively, the EriPhe overdensity is morphologically similar to the Virgo overdensity and the Hercules–Aquila cloud, which also lie at a similar Galactocentric distance. These three overdensities lie along a polar plane separated by ∼120° and may share a common origin. Spectroscopic follow-up observations of the stars in EriPhe are required to fully understand the nature of this overdensity.
HIGH PRECISION ROVIBRATIONAL SPECTROSCOPY OF OH+
Authors: Markus Charles R. , Hodges James N. , Perry Adam J. , Kocheril G. Stephen , Müller Holger S. P. , McCall Benjamin J. 
Published: January 2016

ABSTRACT
The molecular ion OH+ has long been known to be an important component of the interstellar medium. Its relative abundance can be used to indirectly measure cosmic ray ionization rates of hydrogen, and it is the first intermediate in the interstellar formation of water. To date, only a limited number of pure rotational transitions have been observed in the laboratory making it necessary to indirectly calculate rotational levels from high-precision rovibrational spectroscopy. We have remeasured 30 transitions in the fundamental band with MHz-level precision, in order to enable the prediction of a THz spectrum of OH+. The ions were produced in a water cooled discharge of O2, H2, and He, and the rovibrational transitions were measured with the technique Noise Immune Cavity Enhanced Optical Heterodyne Velocity Modulation Spectroscopy. These values have been included in a global fit of field free data to a 3Σ− linear molecule effective Hamiltonian to determine improved spectroscopic parameters which were used to predict the pure rotational transition frequencies.
THE DISCOVERY OF LENSED RADIO AND X-RAY SOURCES BEHIND THE FRONTIER FIELDS CLUSTER MACS J0717.5+3745 WITH THE JVLA AND CHANDRA
Authors: Weeren R. J. van , Ogrean G. A. , Jones C. , Forman W. R. , Andrade-Santos F. , Bonafede A. , Brüggen M. , Bulbul E. , Clarke T. E. , Churazov E. , David L. , Dawson W. A. , Donahue M. , Goulding A. , Kraft R. P. , Mason B. , Merten J. , Mroczkowski T. , Murray S. S. , Nulsen P. E. J. , Rosati P. , Roediger E. , Randall S. W. , Sayers J. , Umetsu K. , Vikhlinin A. , Zitrin A. 
Published: January 2016

ABSTRACT
We report on high-resolution JVLA and Chandra observations of the Hubble Space Telescope (HST) Frontier Cluster MACS J0717.5+3745. MACS J0717.5+3745 offers the largest contiguous magnified area of any known cluster, making it a promising target to search for lensed radio and X-ray sources. With the high-resolution 1.0–6.5 GHz JVLA imaging in A and B configuration, we detect a total of 51 compact radio sources within the area covered by the HST imaging. Within this sample, we find seven lensed sources with amplification factors larger than two. None of these sources are identified as multiply lensed. Based on the radio luminosities, the majority of these sources are likely star-forming galaxies with star-formation rates (SFRs) of 10–50

yr−1 located at

. Two of the lensed radio sources are also detected in the Chandra image of the cluster. These two sources are likely active galactic nuclei, given their 2–10 keV X-ray luminosities of ∼1043–44 erg s−1. From the derived radio luminosity function, we find evidence for an increase in the number density of radio sources at

, compared to a

sample. Our observations indicate that deep radio imaging of lensing clusters can be used to study star-forming galaxies, with SFRs as low as ∼10 M
⊙ yr−1, at the peak of cosmic star formation history.
INFLOW GENERATED X-RAY CORONA AROUND SUPERMASSIVE BLACK HOLES AND A UNIFIED MODEL FOR X-RAY EMISSION
Authors: Wang Lile , Cen Renyue 
Published: January 2016

ABSTRACT
Three-dimensional hydrodynamic simulations are performed, which cover the spatial domain from hundreds of Schwarzschild radii to 2 pc around the central supermassive black hole of mass

, with detailed radiative cooling processes. The existence of a significant amount of shock heated, high temperature (

) coronal gas in the inner (

) region is generally found. It is shown that the composite bremsstrahlung emission spectrum due to coronal gas of various temperatures is in reasonable agreement with the overall ensemble spectrum of active galactic nuclei (AGNs) and hard X-ray background. Taking into account inverse Compton processes, in the context of the simulation-produced coronal gas, our model can readily account for the wide variety of AGN spectral shapes, which can now be understood physically. The distinguishing feature of our model is that X-ray coronal gas is, for the first time, an integral part of the inflow gas and its observable characteristics are physically coupled to the concomitant inflow gas. One natural prediction of our model is the anti-correlation between accretion disk luminosity and spectral hardness: as the luminosity of SMBH accretion disk decreases, the hard X-ray luminosity increases relative to the UV/optical luminosity.
DISTINGUISHING A HYPOTHETICAL ABIOTIC PLANET–MOON SYSTEM FROM A SINGLE INHABITED PLANET
Authors: Li Tong , Tian Feng , Wang Yuwei , Wei Wanjing , Huang Xiaomeng 
Published: January 2016

ABSTRACT
It has recently been suggested that an exomoon with a CH4 atmosphere, orbiting an abiotic Earth-mass planet with an O2-rich atmosphere, can produce a false positive biosignature at a low–moderate spectral resolution (R = λ/Δλ ≤ 2000). If this were true, inferring the presence of life on exoplanets will be beyond our reach in the next several decades. Here we use a line-by-line radiative transfer model to compute the relevant reflection spectrum between 1 and 3.3 μm. We show that it is possible to separate the combined spectra of such planet–moon systems from an inhabited planet by multiple-band NIR observations. We suggest that future observations near the 2.3 μm CH4 absorption band at a resolution of 100 and an SNR of 10 or more may be a good way to distinguish an abiotic planet–moon system from a inhabited single planet.
L'anorexie mentale
Authors: Antoine Pascal 
Published: January 2016

La difficulté à se défaire des préoccupations alimentaires et corporelles, les obsessions et les rituels, les erreurs de perception corporelle, la rigidité dans les interactions et les routines sont autant d’observations cliniques qui permettent d’interroger l’existence d’un fonctionnement intellectuel ou d’un style cognitif particulier dans l’anorexie mentale. Derrière cette question, à laquelle les neuropsychologues répondent de plus en plus précisément, d’autres enjeux émergent : ce style cognitif est-il lié à la perte de poids ou préexistant à l’apparition des troubles ? Des patterns spécifiques d’activité cérébrale sont-ils associés ? Peut-on aider les patients à adopter un style cognitif plus adaptatif par des techniques éprouvées de remédiation cognitive ?	La rencontre clinique dans le champ de l’anorexie mentale se heurte à l’affaiblissement physique, psychique mais également intellectuel des patients, et ce d’autant plus lorsque l’IMC est faible. La pensée apparaît confuse et la fatigabilité importante, ce qui diminue la réflexivité des patients et la portée des interactions. Par ailleurs, l’anorexie mentale reste mystérieuse en bien des aspects, notamment étiologiques. Elle ne bénéficie pas non plus de proposition psychothérapeutique dont le niveau d’efficacité en fasse un élément incontournable du dispositif de soin. Face à ces manques et à ces constats cliniques, étiologiques et thérapeutiques, les travaux se sont multipliés depuis une trentaine d’années et se sont accélérés plus récemment pour tenter d’identifier les processus sous-jacents à l’apparition puis au maintien de la maladie ainsi que ses marqueurs biologiques. Cette voie tout à fait originale est ouverte par la psychopathologie cognitive et la neuropsychologie clinique, et ce chapitre en propose une synthèse. Pour éviter toute ambiguïté, notamment relative à l’influence potentielle d’un IMC faible ou très faible, les recherches fondées sur des personnes issues de la population générale avec des niveaux élevés de restriction cognitive n’ont pas été intégrées. Les travaux recensés, sans être exhaustifs, sont ceux exclusivement acquis auprès de patients relevant d’un diagnostic d’anorexie mentale. Après un aperçu rapide de la littérature sur l’intelligence, ce chapitre couvrira les domaines cognitifs classiquement abordés en neuropsychologie, le domaine particulier des perceptions corporelles, avant d’aborder la question de la prise en charge neuropsychologique : la remédiation cognitive.
L'anorexie mentale
Authors: Antoine Pascal 
Published: January 2016

La difficulté à prendre conscience des troubles, l’étouffement des éprouvés corporels et émotionnels, la rigidité du fonctionnement psychique et la résistance à s’engager dans une relation thérapeutique sont typiques des patients avec une anorexie mentale. Les psychothérapeutes développent actuellement plusieurs courants qui tiennent compte de ces défis imposés par la maladie : ces différentes approches, motivationnelles, d’acceptation et d’engagement ou de pleine conscience, favorisent l’émergence du changement, l’évolution de l’attitude envers le symptôme ou le traitement et le réinvestissement de son existence.
Pratiques stratégiques des multinationales françaises en Chine : analyse des facteurs culturels
Authors: Gao Huiyi 
Published: January 2016

La propagation des multinationales françaises en Chine se heurte au problème de la transposition de leurs pratiques du management stratégique au contexte local. Les résultats d’une étude de 4 cas confirment les divergences liées à la pensée holistique, aux concepts du pouvoir et de responsabilité et aux facteurs psychosociaux. Les défis soulevés s’organisent autour de deux axes : agir en prenant en compte la logique chinoise et dynamiser les interactions entre des acteurs tant internes qu’externes.
Parler de management et de gestion éthique. Un exemple : le recueil des directives anticipées
Authors: Bréhaux Karine , Frémond-Lejeune Corinne 
Published: January 2016

Les directives anticipées, en référence à la loi de 2005, dite Loi de Léonetti, constituent un dispositif d’expression, par anticipation, de la volonté du patient quant à sa fin de vie, pour le cas où il ne serait plus en capacité de le faire. Une étude a été menée dans un centre hospitalier sur la phase de recueil. Comme toute activité, ce processus est soumis à des dangers. Face à eux ou en situation dangereuse, la méthode d’Analyse Globale des Risques (AGR), appliquée au sujet, permet d’identifier et de caractériser les scénarios conduisant à des évènements redoutés afin de définir des actions de réduction des risques assorties ou non de paramètres de sécurisation. Elles sont soumises à validation des dirigeants sur la base des risques majeurs et d’un bilan financier. Le coordonnateur de la gestion des risques associés aux soins de l’établissement conduit la démarche et anime le groupe d’experts du système étudié. Cette étude a permis d’identifier 332 scénarios dont 42,77 % associés à un risque tolérable sous contrôle et 11,14 % à un risque non acceptable, définis ainsi par la matrice de criticité, outil managérial de décision. Parmi ces derniers, trois risques majeurs ont été identifiés sur la base des valeurs maximales des risques moyens. Deux d’entre eux étaient associés à l’étape d’évaluation des capacités du patient à exprimer ses volontés et le troisième était associé à l’étape de recueil de la décision du patient de rédiger ou non ses directives anticipées. Deux actions de réduction des risques, de nature préventive et économiquement rentables, chacune consolidée par un paramètre de sécurité ont été retenues en guise de traitement. L’élaboration d’un projet managérial énonce des valeurs partagées et cette étude permet de les décliner objectivement : rendre compatible les évolutions de l’hôpital avec la démarche éthique, rappeler les valeurs communes du service public hospitalier en les corrélant avec les droits des personnes et les valeurs éthiques (égalité, neutralité, médiation, respect de la réglementation, respect du consentement de la personne). Cela nécessite de développer des principes de management éthique participatif où de nouveaux profils de managers (à la fois directeur d’établissement et éthicien ?) seraient appréciés et où le coordonnateur de la gestion des risques associés aux soins de l’établissement pourrait être un nouveau manager créatif.