bluuebunny/crossref_metadata_2025_split huggingface dataset:
NEAR-INFRARED SPECTROSCOPY OF NEARBY SEYFERT GALAXIES: IS THERE EVIDENCE FOR SHOCK EXCITATION IN NARROW-LINE REGIONS?
Authors: Terao K. , Nagao T. , Hashimoto T. , Yanagisawa K. , Matsuoka K. , Toba Y. , Ikeda H. , Taniguchi Y. 
Published: December 2016

ABSTRACT
One of the important unsettled problems regarding active galactic nuclei (AGNs) is the major ionization mechanism of gas clouds in AGN narrow-line regions (NLRs). In order to investigate this issue, we present our J-band spectroscopic observations of a sample of 26 nearby Seyfert galaxies. In our study, we use the flux ratio of the following two forbidden emission lines, [Fe ii]1.257 μm and [P ii]1.188 μm, because it is known that this ratio is sensitive to the ionization mechanism. We obtain the [Fe ii]/[P ii] flux ratio or its lower limit for 19 objects. In addition to our data, we compile this flux ratio (or its lower limit) for 23 nearby Seyfert galaxies from the literature. Based on the collected data, we find that three Seyfert galaxies show very large lower limits of the [Fe ii]/[P ii] flux ratios (≳10): NGC 2782, NGC 5005, and Mrk 463. It is thus suggested that the contribution of the fast shock in the gas excitation is significantly large for them. However, more than half of the Seyfert galaxies in our sample show moderate [Fe ii]/[P ii] flux ratios (∼2), which is consistent with pure photoionization by power-law ionizing continuum emission. We also find that the [Fe ii]/[P ii] flux ratio shows no clear correlation with the radio loudness, suggesting that the radio jet is not the primary origin of shocks in NLRs of Seyfert galaxies.
YOUNG STELLAR POPULATIONS IN MYStIX STAR-FORMING REGIONS: CANDIDATE PROTOSTARS
Authors: Romine Gregory , Feigelson Eric D. , Getman Konstantin V. , Kuhn Michael A. , Povich Matthew S. 
Published: December 2016

ABSTRACT
The Massive Young Star-Forming Complex in Infrared and X-ray (MYStIX) project provides a new census on stellar members of massive star-forming regions within 4 kpc. Here the MYStIX Infrared Excess catalog and Chandra-based X-ray photometric catalogs are mined to obtain high-quality samples of Class I protostars using criteria designed to reduce extragalactic and Galactic field star contamination. A total of 1109 MYStIX Candidate Protostars (MCPs) are found in 14 star-forming regions. Most are selected from protoplanetary disk infrared excess emission, but 20% are found from their ultrahard X-ray spectra from heavily absorbed magnetospheric flare emission. Two-thirds of the MCP sample is newly reported here. The resulting samples are strongly spatially associated with molecular cores and filaments on Herschel far-infrared maps. This spatial agreement and other evidence indicate that the MCP sample has high reliability with relatively few “false positives” from contaminating populations. But the limited sensitivity and sparse overlap among the infrared and X-ray subsamples indicate that the sample is very incomplete with many “false negatives.” Maps, tables, and source descriptions are provided to guide further study of star formation in these regions. In particular, the nature of ultrahard X-ray protostellar candidates without known infrared counterparts needs to be elucidated.
LABORATORY FREQUENCY REDISTRIBUTION FUNCTION FOR THE POLARIZED Λ-TYPE THREE-TERM ATOM
Authors: Casini R. , Manso Sainz R. 
Published: December 2016

ABSTRACT
We present the frequency redistribution function for a polarized three-term atom of the Λ-type in the collisionless regime, and we specialize it to the case where both the initial and final terms of the three-state transition are metastable (i.e., with infinitely sharp levels). This redistribution function represents a generalization of the well-known R
II function to the case where the lower terms of the transition can be polarized and carry atomic coherence, and it can be applied to the investigation of polarized line formation in tenuous plasmas, where collisional rates may be low enough that anisotropy-induced atomic polarization survives even in the case of metastable levels.
MASTER OPTICAL POLARIZATION VARIABILITY DETECTION IN THE MICROQUASAR V404 CYG/GS 2023+33
Authors: Lipunov Vladimir M. , Gorbovskoy E. , Kornilov V. , Krushinskiy V. , Vlasenko D. , Tiurina N. , Balanutsa P. , Kuznetsov A. , Budnev N. , Gress O. , Tlatov A. , Rebolo Lopez R. , Serra-Ricart M. , Buckley D. A. H. , Israelyan G. , Lodieu N. , Ivanov K. , Yazev S. , Sergienko Yu. , Gabovich A. , Yurkov V. , Levato H. , Saffe C. , Podesta R. , Mallamaci C. , Lopez C. 
Published: December 2016

ABSTRACT
On 2015 June 15, the Swift space observatory discovered that the Galactic black hole candidate V404 Cyg was undergoing another active X-ray phase, after 25 years of inactivity. The 12 telescopes of the MASTER Global Robotic Net located at six sites across four continents were the first ground-based observatories to start optical monitoring of the microquasar after its gamma-ray wake up at 18h 34m 09s U.T. on 2015 June 15. In this paper, we report, for the first time, the discovery of variable optical linear polarization, changing by 4%–6% over a timescale of ∼1 hr, on two different epochs. We can conclude that the additional variable polarization arises from the relativistic jet generated by the black hole in V404 Cyg. The polarization variability correlates with optical brightness changes, increasing when the flux decreases.
A SYSTEMATIC STUDY OF MID-INFRARED EMISSION FROM CORE-COLLAPSE SUPERNOVAE WITH SPIRITS
Authors: Tinyanont Samaporn , Kasliwal Mansi M. , Fox Ori D. , Lau Ryan , Smith Nathan , Williams Robert , Jencson Jacob , Perley Daniel , Dykhoff Devin , Gehrz Robert , Johansson Joel , Van Dyk Schuyler D. , Masci Frank , Cody Ann Marie , Prince Thomas 
Published: December 2016

ABSTRACT
We present a systematic study of mid-infrared emission from 141 nearby supernovae (SNe) observed with Spitzer/IRAC as part of the ongoing SPIRITS survey. We detect 8 Type Ia and 36 core-collapse SNe. All Type Ia/Ibc SNe become undetectable within three years of explosion, whereas 22 ± 11% of Type II SNe continue to be detected. Five Type II SNe are detected even two decades after discovery (SN 1974E, 1979C, 1980K, 1986J, and 1993J). Warm dust luminosity, temperature, and a lower limit on mass are obtained by fitting the two IRAC bands, assuming an optically thin dust shell. We derive warm dust masses between 10−6 and 10−2
M
⊙ and dust color temperatures between 200 and 1280 K. This observed warm dust could be pre-existing or newly created, but in either case represents a lower limit to the dust mass because cooler dust may be present. We present three case studies of extreme SNe. SN 2011ja (II-P) was over-luminous ([4.5] = −15.6 mag) at 900 days post explosion with increasing hot dust mass, suggesting either an episode of dust formation or intensifying circumstellar material (CSM) interactions heating up pre-existing dust. SN 2014bi (II-P) showed a factor of 10 decrease in dust mass over one month, suggesting either dust destruction or reduced dust heating. The IR luminosity of SN 2014C (Ib) stayed constant over 800 days, possibly due to strong CSM interaction with an H-rich shell, which is rare among stripped-envelope SNe. The observations suggest that this CSM shell originated from an LBV-like eruption roughly 100 years pre-explosion. The observed diversity demonstrates the power of mid-IR observations of a large sample of SNe.
ALMA BAND 8 CONTINUUM EMISSION FROM ORION SOURCE I
Authors: Hirota Tomoya , Machida Masahiro N. , Matsushita Yuko , Motogi Kazuhito , Matsumoto Naoko , Kim Mi Kyoung , Burns Ross A. , Honma Mareki 
Published: December 2016

ABSTRACT
We have measured continuum flux densities of a high-mass protostar candidate, a radio source I in the Orion KL region (Orion Source I) using the Atacama Large Millimeter/Submillimeter Array (ALMA) at band 8 with an angular resolution of 0.″1. The continuum emission at 430, 460, and 490 GHz associated with Source I shows an elongated structure along the northwest–southeast direction perpendicular to the so-called low-velocity bipolar outflow. The deconvolved size of the continuum source, 90 au × 20 au, is consistent with those reported previously at other millimeter/submillimeter wavelengths. The flux density can be well fitted to the optically thick blackbody spectral energy distribution, and the brightness temperature is evaluated to be 700–800 K. It is much lower than that in the case of proton–electron or H− free–free radiations. Our data are consistent with the latest ALMA results by Plambeck & Wright, in which the continuum emission was proposed to arise from the edge-on circumstellar disk via thermal dust emission, unless the continuum source consists of an unresolved structure with a smaller beam filling factor.
PRE-ERUPTION OSCILLATIONS IN THIN AND LONG FEATURES IN A QUIESCENT FILAMENT
Authors: Joshi Anand D. , Hanaoka Yoichiro , Suematsu Yoshinori , Morita Satoshi , Yurchyshyn Vasyl , Cho Kyung-Suk 
Published: December 2016

ABSTRACT
We investigate the eruption of a quiescent filament located close to an active region. Large-scale activation was observed in only half of the filament in the form of pre-eruption oscillations. Consequently only this half erupted nearly 30 hr after the oscillations commenced. Time-slice diagrams of 171 Å images from the Atmospheric Imaging Assembly were used to study the oscillations. These were observed in several thin and long features connecting the filament spine to the chromosphere below. This study traces the origin of such features and proposes their possible interpretation. Small-scale magnetic flux cancellation accompanied by a brightening was observed at the footpoint of the features shortly before their appearance, in images recorded by the Helioseismic and Magnetic Imager. A slow rise of the filament was detected in addition to the oscillations, indicating a gradual loss of equilibrium. Our analysis indicates that a change in magnetic field connectivity between two neighbouring active regions and the quiescent filament resulted in a weakening of the overlying arcade of the filament, leading to its eruption. It is also suggested that the oscillating features are filament barbs, and the oscillations are a manifestation during the pre-eruption phase of the filaments.
THE PHYSICAL ENVIRONMENT AROUND IRAS 17599–2148: INFRARED DARK CLOUD AND BIPOLAR NEBULA
Authors: Dewangan L. K. , Ojha D. K. , Zinchenko I. , Janardhan P. , Ghosh S. K. , Luna A. 
Published: December 2016

ABSTRACT
We present a multiscale and multiwavelength study to investigate the star formation process around IRAS 17599–2148, which is part of an elongated filamentary structure (EFS) (extension ∼21 pc) seen in the Herschel maps. Using the Herschel data analysis, at least six massive clumps (M
clump ∼ 777–7024 M
⊙) are found in the EFS with a range of temperature and column density of ∼16–39 K and ∼(0.6–11) × 1022 cm−2 (A

V
∼ 7–117 mag), respectively. The EFS hosts cold gas regions (i.e., infrared dark cloud) without any radio detection and a bipolar nebula (BN) linked with the H ii region IRAS 17599–2148, tracing two distinct environments inferred through the temperature distribution and ionized emission. Based on virial analysis and higher values of self-gravitating pressure, the clumps are found unstable against gravitational collapse. We find 474 young stellar objects (YSOs) in the selected region, and ∼72% of these YSOs are found in the clusters distributed mainly toward the clumps in the EFS. These YSOs might have spontaneously formed due to processes not related to the expanding H ii region. At the edges of BN, four additional clumps are also associated with YSO clusters, which appear to be influenced by the expanding H ii region. The most massive clump in the EFS contains two compact radio sources traced in the Giant Metre-wave Radio Telescope 1.28 GHz map and a massive protostar candidate, IRS 1, prior to an ultracompact H ii phase. Using the Very Large Telescope/NACO near-infrared images, IRS 1 is resolved with a jet-like feature within a 4200 au scale.
DESIGN OF LABORATORY EXPERIMENTS TO STUDY PHOTOIONIZATION FRONTS DRIVEN BY THERMAL SOURCES
Authors: Drake R. P. , Hazak G. , Keiter P. A. , Davis J. S. , Patterson C. R , Frank A. , Blackman E. G. , Busquet Michel 
Published: December 2016

ABSTRACT
This paper analyzes the requirements of a photoionization-front experiment that could be driven in the laboratory, using thermal sources to produce the necessary flux of ionizing photons. It reports several associated conclusions. Such experiments will need to employ the largest available facilities, capable of delivering many kJ to MJ of energy to an X-ray source. They will use this source to irradiate a volume of neutral gas, likely of N, on a scale of a few mm to a few cm, increasing with source energy. For a gas pressure of several to ten atmospheres at room temperature, and a source temperature near 100 eV, one will be able to drive a photoionization front through a system of tens to hundreds of photon mean free paths. The front should make the familiar transition from the so-called R-Type to D-Type as the radiation flux diminishes with distance. The N is likely to reach the He-like state. Preheating from the energetic photons appears unlikely to become large enough to alter the essential dynamics of the front beyond some layer near the surface. For well-chosen experimental conditions, competing energy transport mechanisms are small.
DEEP CHANDRA OBSERVATIONS OF THE PULSAR WIND NEBULA CREATED BY PSR B0355+54
Authors: Klingler Noel , Rangelov Blagoy , Kargaltsev Oleg , Pavlov George G. , Romani Roger W. , Posselt Bettina , Slane Patrick , Temim Tea , Ng C.-Y. , Bucciantini Niccolò , Bykov Andrei , Swartz Douglas A. , Buehler Rolf 
Published: December 2016

ABSTRACT
We report on Chandra X-ray Observatory (CXO) observations of the pulsar wind nebula (PWN) associated with PSR B0355+54 (eight observations with a 395 ks total exposure, performed over an eight month period). We investigated the spatial and spectral properties of the emission coincident with the pulsar, compact nebula (CN), and extended tail. We find that the CN morphology can be interpreted in a way that suggests a small angle between the pulsar spin axis and our line of sight, as inferred from the radio data. On larger scales, emission from the

(

pc) tail is clearly seen. We also found hints of two faint extensions nearly orthogonal to the direction of the pulsar’s proper motion. The spectrum extracted at the pulsar position can be described with an absorbed power-law + blackbody model. The nonthermal component can be attributed to magnetospheric emission, while the thermal component can be attributed to emission from either a hot spot (e.g., a polar cap) or the entire neutron star surface. Surprisingly, the spectrum of the tail shows only a slight hint of cooling with increasing distance from the pulsar. This implies either a low magnetic field with fast flow speed, or particle reacceleration within the tail. We estimate physical properties of the PWN and compare the morphologies of the CN and the extended tail with those of other bow shock PWNe observed with long CXO exposures.
MAGNETAR HEATING
Authors: Beloborodov Andrei M. , Li Xinyu 
Published: December 2016

ABSTRACT
We examine four candidate mechanisms that could explain the high surface temperatures of magnetars. (1) Heat flux from the liquid core heated by ambipolar diffusion. It could sustain the observed surface luminosity

erg s−1 if core heating offsets neutrino cooling at a temperature

K. This scenario is viable if the core magnetic field exceeds 1016 G and the heat-blanketing envelope of the magnetar has a light-element composition. However, we find that the lifetime of such a hot core should be shorter than the typical observed lifetime of magnetars. (2) Mechanical dissipation in the solid crust. This heating can be quasi-steady, powered by gradual (or frequent) crustal yielding to magnetic stresses. We show that it obeys a strong upper limit. As long as the crustal stresses are fostered by the field evolution in the core or Hall drift in the crust, mechanical heating is insufficient to sustain persistent

erg s−1. The surface luminosity is increased in an alternative scenario of mechanical deformations triggered by external magnetospheric flares. (3) Ohmic dissipation in the crust, in volume or current sheets. This mechanism is inefficient because of the high conductivity of the crust. Only extreme magnetic configurations with crustal fields

G varying on a 100 meter scale could provide

erg s−1. (4) Bombardment of the stellar surface by particles accelerated in the magnetosphere. This mechanism produces hot spots on magnetars. Observations of transient magnetars show evidence of external heating.
CHEMICAL TAGGING CAN WORK: IDENTIFICATION OF STELLAR PHASE-SPACE STRUCTURES PURELY BY CHEMICAL-ABUNDANCE SIMILARITY
Authors: Hogg David W. , Casey Andrew R. , Ness Melissa , Rix Hans-Walter , Foreman-Mackey Daniel , Hasselquist Sten , Ho Anna Y. Q. , Holtzman Jon A. , Majewski Steven R. , Martell Sarah L. , Mészáros Szabolcs , Nidever David L. , Shetrone Matthew 
Published: December 2016

ABSTRACT
Chemical tagging promises to use detailed abundance measurements to identify spatially separated stars that were, in fact, born together (in the same molecular cloud) long ago. This idea has not yielded much practical success, presumably because of the noise and incompleteness in chemical-abundance measurements. We have succeeded in substantially improving spectroscopic measurements with The Cannon, which has now delivered 15 individual abundances for

stars observed as part of the APOGEE spectroscopic survey, with precisions around 0.04 dex. We test the chemical-tagging hypothesis by looking at clusters in abundance space and confirming that they are clustered in phase space. We identify (by the k-means algorithm) overdensities of stars in the 15-dimensional chemical-abundance space delivered by The Cannon, and plot the associated stars in phase space. We use only abundance-space information (no positional information) to identify stellar groups. We find that clusters in abundance space are indeed clusters in phase space, and we recover some known phase-space clusters and find other interesting structures. This is the first-ever project to identify phase-space structures at the survey-scale by blind search purely in abundance space; it verifies the precision of the abundance measurements delivered by The Cannon; the prospects for future data sets appear very good.
La résilience, une nouvelle approche de la dimension émotionnelle
Authors: Bernard Marie-Josée , Fayolle Alain 
Published: December 2016

Cet article présente le concept de résilience comme une clef de compréhension du choix d’entreprendre et montre son utilité pour faire face aux difficultés parfois sévères inhérentes à cette aventure. Il fait référence à « l’ancrage » historique de la résilience dans la littérature de l’entrepreneuriat, notamment à partir des travaux de Shapero. L’article montre comment la résilience mobilise à la fois la dimension émotionnelle, cognitive et psychologique de l’individu. Entreprendre est ici envisagé comme une façon de rebondir dans un parcours de vie et la résilience permet de mieux saisir l’impact des événements sur les individus. Nous présentons les caractéristiques d’une dynamique de rebond et la façon dont certains entrepreneurs développent des talents spécifiques pour faire face à l’adversité et les mobilisent dans des situations critiques. Nous proposons une perspective sur l’évolution actuelle de l’approche de la résilience dans le champ de l’entrepreneuriat et des repères utiles pour en saisir les principes. Enfin cet article permet d’ouvrir de nouvelles voies pour mieux accompagner les personnes et les projets dans des phases critiques.
Des étudiants heureux et proactifs grâce à l’apprentissage autodirigé
Authors: Verzat Caroline , O’Shea Noreen , Jore Maxime 
Published: December 2016

L’une des composantes reconnues et mesurables de l’esprit d’entreprendre est la proactivité. Peut-elle être développée par un dispositif pédagogique ? Quels sont ses liens avec le plaisir d’apprendre ? La recherche présentée ici compare les résultats de deux approches testées sur 281 étudiants dans le cadre d’un séminaire de 15 heures en début d’année de master en entrepreneuriat. Dans le premier cas (design autodirigé), les étudiants ont été invités à concevoir eux-mêmes un projet signifiant pour eux l’esprit d’entreprendre, à le réaliser de manière autonome et à l’auto-évaluer sur des critères négociés, l’enseignant jouant le rôle de coach. Dans le second cas (design dirigé), l’enseignant a guidé étroitement le processus d’acquisition de connaissances en faisant réaliser par les étudiants un protocole de recherche sur l’esprit d’entreprendre. In fine , il a évalué les présentations de manière traditionnelle. Les résultats montrent que l’approche autodirigée développe la pro-activité des étudiants de manière significative. Deux facteurs supplémentaires inter-reliés interviennent spécifiquement dans la pédagogie autodirigée : l’efficacité groupale de nature créative et ludique et des émotions positives associées.
Leaders, écoutez ce que vous murmurent les chevaux...
Authors: Toutain Olivier , Ballereau Valérie , Blache Julien 
Published: December 2016

Pour explorer la question des processus subjectifs dans l’apprentissage entrepreneurial, nous avons observé une formation au leadership basée sur le coaching équin (accompagnement des personnes par l’interaction avec un cheval). Objectif : observer si la relation avec l’animal facilite la prise de conscience et le contrôle des processus subjectifs dans la prise de décision entrepreneuriale. Les résultats montrent que le type de communication directe nécessaire avec le cheval favorise cette prise de conscience des processus subjectifs. Les enseignements du « horse coaching » sont transférables dans d’autres contextes d’apprentissage, à condition de respecter certaines règles dans le montage du dispositif de formation
Naître, grandir, vieillir avec un handicap
Authors: Korff-Sausse Simone 
Published: December 2016

Le temps détermine les étapes qui scandent la temporalité de la vie, en nous imposant des transitions qui exigent des remaniements identitaires, correspondant aux âges de la vie. La survenue d’un handicap bouscule la temporalité, aussi bien pour l’enfant handicapé que pour ses parents. Les parents n’arrivent pas à anticiper sur un futur possible pour cet enfant. Leur enfant n’a pas d’âge. Et eux non plus. Le temps s’arrête. Pour les enfants, l’angoisse liée à la temporalité est particulièrement présente, dans certaines situations, comme celle des maladies évolutives ou celles où les enfants ont frôlé la mort. La personne en situation de handicap ainsi que ses proches sont « hors temps ». Le but du travail psychanalytique sera de réintroduire dans cette temporalité figée, une mobilité qui garantit les passages possibles entre passé, présent et futur.