bluuebunny/crossref_metadata_2025_split huggingface dataset:
ON THE NON-KOLMOGOROV NATURE OF FLARE-PRODUCTIVE SOLAR ACTIVE REGIONS
Authors: Mandage Revati S. , McAteer R. T. James 
Published: December 2016

ABSTRACT
A magnetic power spectral analysis is performed on 53 solar active regions, observed from 2011 August to 2012 July. Magnetic field data obtained from the Helioseismic and Magnetic Imager, inverted as Active Region Patches, are used to study the evolution of the magnetic power index as each region rotates across the solar disk. Active regions are classified based on the numbers and sizes of solar flares they produce in order to study the relationship between flare productivity and the magnetic power index. The choice of window size and inertial range plays a key role in determining the correct magnetic power index. The overall distribution of magnetic power indices has a range of 1.0–2.5. Flare-quiet regions peak at a value of 1.6. However, flare-productive regions peak at a value of 2.2. Overall, the histogram of the distribution of power indices of flare-productive active regions is well separated from flare-quiet active regions. Only 12% of flare-quiet regions exhibit an index greater than 2, whereas 90% of flare-productive regions exhibit an index greater than 2. Flare-quiet regions exhibit a high temporal variance (i.e., the index fluctuates between high and low values), whereas flare-productive regions maintain an index greater than 2 for several days. This shows the importance of including the temporal evolution of active regions in flare prediction studies, and highlights the potential of a 2–3 day prediction window for space weather applications.
MAPPING THE REAL-SPACE DISTRIBUTIONS OF GALAXIES IN SDSS DR7. I. TWO-POINT CORRELATION FUNCTIONS
Authors: Shi Feng , Yang Xiaohu , Wang Huiyuan , Zhang Youcai , Mo H. J. , van den Bosch Frank C. , Li Shijie , Liu Chengze , Lu Yi , Tweed Dylan , Yang Lei 
Published: December 2016

ABSTRACT
Using a method to correct redshift-space distortion (RSD) for individual galaxies, we mapped the real-space distributions of galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7). We use an ensemble of mock catalogs to demonstrate the reliability of our method. Here, in the first paper in a series, we focus mainly on the two-point correlation function (2PCF) of galaxies. Overall the 2PCF measured in the reconstructed real space for galaxies brighter than

agrees with the direct measurement to an accuracy better than the measurement error due to cosmic variance, if the reconstruction uses the correct cosmology. Applying the method to the SDSS DR7, we construct a real-space version of the main galaxy catalog, which contains 396,068 galaxies in the North Galactic Cap with redshifts in the range 0.01 ≤ z ≤ 0.12. The Sloan Great Wall, the largest known structure in the nearby universe, is not as dominant an overdense structure as it appears to be in redshift space. We measure the 2PCFs in reconstructed real space for galaxies of different luminosities and colors. All of them show clear deviations from single power-law forms, and reveal clear transitions from one-halo to two-halo terms. A comparison with the corresponding 2PCFs in redshift space nicely demonstrates how RSDs boost the clustering power on large scales (by about 40%–50% at scales

) and suppress it on small scales (by about 70%–80% on a scale of

).
SPHERICAL HARMONIC ANALYSES OF INTENSITY MAPPING POWER SPECTRA
Authors: Liu Adrian , Zhang Yunfan , Parsons Aaron R. 
Published: December 2016

ABSTRACT
Intensity mapping is a promising technique for surveying the large-scale structure of our universe from z = 0 to z ∼ 150, using the brightness temperature field of spectral lines to directly observe previously unexplored portions of our cosmic timeline. Examples of targeted lines include the 21 cm hyperfine transition of neutral hydrogen, rotational lines of carbon monoxide, and fine-structure lines of singly ionized carbon. Recent efforts have focused on detections of the power spectrum of spatial fluctuations, but have been hindered by systematics such as foreground contamination. This has motivated the decomposition of data into Fourier modes perpendicular and parallel to the line of sight, which has been shown to be a particularly powerful way to diagnose systematics. However, such a method is well-defined only in the limit of a narrow-field, flat-sky approximation. This limits the sensitivity of intensity mapping experiments, as it means that wide surveys must be separately analyzed as a patchwork of smaller fields. In this paper, we develop a framework for analyzing intensity mapping data in a spherical Fourier–Bessel basis, which incorporates curved sky effects without difficulty. We use our framework to generalize a number of techniques in intensity mapping data analysis from the flat sky to the curved sky. These include visibility-based estimators for the power spectrum, treatments of interloper lines, and the “foreground wedge” signature of spectrally smooth foregrounds.
IC 3639—A NEW BONA FIDE COMPTON-THICK AGN UNVEILED BY NuSTAR
Authors: Boorman Peter G. , Gandhi P. , Alexander D. M. , Annuar A. , Ballantyne D. R. , Bauer F. , Boggs S. E. , Brandt W. N. , Brightman M. , Christensen F. E. , Craig W. W. , Farrah D. , Hailey C. J. , Harrison F. A. , Hönig S. F. , Koss M. , LaMassa S. M. , Masini A. , Ricci C. , Risaliti G. , Stern D. , Zhang W. W. 
Published: December 2016

ABSTRACT
We analyze high-quality NuSTAR observations of the local (z = 0.011) Seyfert 2 active galactic nucleus (AGN) IC 3639, in conjunction with archival Suzaku and Chandra data. This provides the first broadband X-ray spectral analysis of the source, spanning nearly two decades in energy (0.5–30 keV). Previous X-ray observations of the source below 10 keV indicated strong reflection/obscuration on the basis of a pronounced iron fluorescence line at 6.4 keV. The hard X-ray energy coverage of NuSTAR, together with self-consistent toroidal reprocessing models, enables direct broadband constraints on the obscuring column density of the source. We find the source to be heavily Compton-thick (CTK) with an obscuring column in excess of

cm−2, unconstrained at the upper end. We further find an intrinsic 2–10 keV luminosity of

to 90% confidence, almost 400 times the observed flux, and consistent with various multiwavelength diagnostics. Such a high ratio of intrinsic to observed flux, in addition to an Fe-Kα fluorescence line equivalent width exceeding 2 keV, is extreme among known bona fide CTK AGNs, which we suggest are both due to the high level of obscuration present around IC 3639. Our study demonstrates that broadband spectroscopic modeling with NuSTAR enables large corrections for obscuration to be carried out robustly and emphasizes the need for improved modeling of AGN tori showing intense iron fluorescence.
CHEMICAL EVOLUTION OF RED MSX SOURCES IN THE SOUTHERN SKY
Authors: Yu Naiping , Xu Jinlong 
Published: December 2016

ABSTRACT
Red Midcourse Space Experiment (MSX) Sources (RMSs) are regarded as excellent candidates of massive star-forming regions. In order to characterize the chemical properties of massive star formation, we made a systematic study of 87 RMSs in the southern sky, using archival data taken from the Atacama Pathfinder Experiment Telescope Large Area Survey of the Galaxy (ATLASGAL), the Australia Telescope Compact Array, and the Millimetre Astronomy Legacy Team Survey at 90 GHz (MALT90). According to previous multiwavelength observations, our sample could be divided into two groups: massive young stellar objects and H ii regions. Combined with the MALT90 data, we calculated the column densities of N2H+, C2H, HC3N, and HNC and found that they are not much different from previous studies made in other massive star-forming regions. However, their abundances are relatively low compared to infrared dark clouds (IRDCs). The abundances of N2H+ and HNC in our sample are at least 1 mag lower than those found in IRDCs, indicating chemical depletions in the relatively hot gas. Besides, the fractional abundances of N2H+, C2H, and HC3N seem to decrease as a function of their Lyman continuum fluxes (N

L
), indicating that these molecules could be destroyed by UV photons when H ii regions have formed inside. We also find that the C2H abundance decreases faster than HC3N with respect to N

L
. The abundance of HNC has a tight correlation with that of N2H+, indicating that it may be also preferentially formed in cold gas. We regard our RMSs as being in a relatively late evolutionary stage of massive star formation.
DEMONSTRATING DIVERSITY IN STAR-FORMATION HISTORIES WITH THE CSI SURVEY*
Authors: Dressler Alan , Kelson Daniel D. , Abramson Louis E. , Gladders Michael D. , Oemler Augustus , Poggianti Bianca M. , Mulchaey John S. , Vulcani Benedetta , Shectman Stephen A. , Williams Rik J. , McCarthy Patrick J. 
Published: December 2016

ABSTRACT
We present coarse but robust star-formation histories (SFHs) derived from spectrophotometric data of the Carnegie-Spitzer-IMACS Survey, for 22,494 galaxies at

with stellar masses of 109
M
⊙ to 1012
M
⊙. Our study moves beyond “average” SFHs and distribution functions of specific star-formation rates (sSFRs) to individually measured SFHs for tens of thousands of galaxies. By comparing star-formation rates (SFRs) with timescales of

, and 108 years, we find a wide diversity of SFHs: “old galaxies” that formed most or all of their stars early, galaxies that formed stars with declining or constant SFRs over a Hubble time, and genuinely “young galaxies” that formed most of their stars since z = 1. This sequence is one of decreasing stellar mass, but remarkably, each type is found over a mass range of a factor of 10. Conversely, galaxies at any given mass follow a wide range of SFHs, leading us to conclude that (1) halo mass does not uniquely determine SFHs, (2) there is no “typical” evolutionary track, and (3) “abundance matching” has limitations as a tool for inferring physics. Our observations imply that SFHs are set at an early epoch, and that—for most galaxies—the decline and cessation of star formation occurs over a Hubble time, without distinct “quenching” events. SFH diversity is inconsistent with models where galaxy mass, at any given epoch, grows simply along relations between SFR and stellar mass, but is consistent with a two-parameter lognormal form, lending credence to this model from a new and independent perspective.
INVESTIGATING THE MASS SEGREGATION PROCESS IN GLOBULAR CLUSTERS WITH BLUE STRAGGLER STARS: THE IMPACT OF DARK REMNANTS
Authors: Alessandrini Emiliano , Lanzoni Barbara , Ferraro Francesco R. , Miocchi Paolo , Vesperini Enrico 
Published: December 2016

ABSTRACT
We present the results of a set of N-body simulations aimed at exploring how the process of mass segregation (as traced by the spatial distribution of blue straggler stars, BSSs) is affected by the presence of a population of heavy dark remnants (as neutron stars and black holes (BHs)). To this end, clusters characterized by different initial concentrations and different fractions of dark remnants have been modeled. We find that an increasing fraction of stellar-mass BHs significantly delay the mass segregation of BSSs and the visible stellar component. In order to trace the evolution of BSS segregation, we introduce a new parameter (A
+), which can be easily measured when the cumulative radial distribution of these stars and a reference population are available. Our simulations show that A
+ might also be used as an approximate indicator of the time remaining to the core collapse of the visible component.
PREDICTION OF GEOMAGNETIC STORM STRENGTH FROM INNER HELIOSPHERIC IN SITU OBSERVATIONS
Authors: Kubicka M. , Möstl C. , Amerstorfer T. , Boakes P. D. , Feng L. , Eastwood J. P. , Törmänen O. 
Published: December 2016

ABSTRACT
Prediction of the effects of coronal mass ejections (CMEs) on Earth strongly depends on knowledge of the interplanetary magnetic field southward component, B

z
. Predicting the strength and duration of B

z
inside a CME with sufficient accuracy is currently impossible, forming the so-called B

z
problem. Here, we provide a proof-of-concept of a new method for predicting the CME arrival time, speed, B

z
, and resulting disturbance storm time (Dst) index on Earth based only on magnetic field data, measured in situ in the inner heliosphere (<1 au). On 2012 June 12–16, three approximately Earthward-directed and interacting CMEs were observed by the Solar Terrestrial Relations Observatory imagers and Venus Express (VEX) in situ at 0.72 au, 6° away from the Sun–Earth line. The CME kinematics are calculated using the drag-based and WSA–Enlil models, constrained by the arrival time at VEX, resulting in the CME arrival time and speed on Earth. The CME magnetic field strength is scaled with a power law from VEX to Wind. Our investigation shows promising results for the Dst forecast (predicted: −96 and −114 nT (from 2 Dst models); observed: −71 nT), for the arrival speed (predicted: 531 ± 23 km s−1; observed: 488 ± 30 km s−1), and for the timing (6 ± 1 hr after the actual arrival time). The prediction lead time is 21 hr. The method may be applied to vector magnetic field data from a spacecraft at an artificial Lagrange point between the Sun and Earth or to data taken by any spacecraft temporarily crossing the Sun–Earth line.
SOLAR ATMOSPHERIC MAGNETIC ENERGY COUPLING: BROAD PLASMA CONDITIONS AND SPECTRUM REGIMES
Authors: Orange N. Brice , Chesny David L. , Gendre Bruce , Morris David C. , Oluseyi Hakeem M. 
Published: December 2016

ABSTRACT
Solar variability investigations that include magnetic energy coupling are paramount to solving many key solar/stellar physics problems, particularly for understanding the temporal variability of magnetic energy redistribution and heating processes. Using three years of observations from the Solar Dynamics Observatory’s Atmospheric Imaging Assembly and Heliosemic Magnetic Imager, we measured radiative and magnetic fluxes from gross features and at full-disk scales, respectively. Magnetic energy coupling analyses support radiative flux descriptions via the plasma heating connectivity of dominant (magnetic) and diffuse components, specifically of the predominantly closed-field corona. Our work shows that this relationship favors an energetic redistribution efficiency across large temperature gradients, and potentially sheds light on the long-standing issue of diffuse unresolved low corona emission. The close connection between magnetic energy redistribution and plasma conditions revealed by this work lends significant insight into the field of stellar physics, as we have provided possible means for probing distant sources in currently limited and/or undetectable radiation distributions.
PULSAR MAGNETOSPHERES: BEYOND THE FLAT SPACETIME DIPOLE
Authors: Gralla Samuel E. , Lupsasca Alexandru , Philippov Alexander 
Published: December 2016

ABSTRACT
Most studies of the pulsar magnetosphere have assumed a pure magnetic dipole in flat spacetime. However, recent work suggests that the effects of general relativity are in fact of vital importance and that realistic pulsar magnetic fields will have a significant nondipolar component. We introduce a general analytical method for studying the axisymmetric force-free magnetosphere of a slowly rotating star of arbitrary magnetic field, mass, radius, and moment of inertia, including all the effects of general relativity. We confirm that spacelike current is generically present in the polar caps (suggesting a pair production region), irrespective of the stellar magnetic field. We show that general relativity introduces a

correction to the formula for the dipolar component of the surface magnetic field inferred from spindown. Finally, we show that the location and shape of the polar caps can be modified dramatically by even modestly strong higher moments. This can affect emission processes occurring near the star and may help explain the modified beam characteristics of millisecond pulsars.
THE PROPERTIES OF THE CIRCUMGALACTIC MEDIUM IN RED AND BLUE GALAXIES: RESULTS FROM THE COS-GASS+COS-HALOS SURVEYS
Authors: Borthakur Sanchayeeta , Heckman Timothy , Tumlinson Jason , Bordoloi Rongmon , Kauffmann Guinevere , Catinella Barbara , Schiminovich David , Davé Romeel , Moran Sean M. , Saintonge Amelie 
Published: December 2016

ABSTRACT
We use the combined data from the COS-GASS and COS-Halos surveys to characterize the Circum-Galactic Medium (CGM) surrounding typical low-redshift galaxies in the mass range

, and over a range of impact parameters extending to just beyond the halo virial radius (R
vir). We find the radial scale length of the distributions of the equivalent widths of the Lyα and Si iii absorbers to be ∼1 and ∼0.4 R
vir, respectively. The radial distribution of equivalent widths is relatively uniform for the blue galaxies, but highly patchy (i.e., it has a low covering fraction) for the red galaxies. We also find that the Lyα and Si iii equivalent widths show significant positive correlations with the specific star formation rate (sSFR) of the galaxy. We find a surprising lack of correlations between the halo mass (virial velocity) and either the velocity dispersions or velocity offsets of the Lyα lines. The ratio of the velocity offset to the velocity dispersion for the Lyα absorbers has a mean value of ∼4, suggesting that a given line of sight is intersecting a dynamically coherent structure in the CGM, rather than a sea of orbiting clouds. The kinematic properties of the CGM are similar in the blue and red galaxies, although we find that a significantly larger fraction of the blue galaxies have large Lyα velocity offsets (>200 km s−1). We show that—if the CGM clouds represent future fuel for star formation—our new results could imply a large drop in the sSFR across the galaxy mass-range we probe.
HERSCHEL OBSERVATIONS OF DUSTY DEBRIS DISKS
Authors: Vican Laura , Schneider Adam , Bryden Geoff , Melis Carl , Zuckerman B. , Rhee Joseph , Song Inseok 
Published: December 2016

ABSTRACT
We present results from two Herschel observing programs using the Photodetector Array Camera and Spectrometer. During three separate campaigns, we obtained Herschel data for 24 stars at 70, 100, and 160 μm. We chose stars that were already known or suspected to have circumstellar dust based on excess infrared (IR) emission previously measured with the InfraRed Astronomical Satellite (IRAS) or Spitzer and used Herschel to examine long-wavelength properties of the dust. Fifteen stars were found to be uncontaminated by background sources and possess IR emission most likely due to a circumstellar debris disk. We analyzed the properties of these debris disks to better understand the physical mechanisms responsible for dust production and removal. Seven targets were spatially resolved in the Herschel images. Based on fits to their spectral energy distributions, nine disks appear to have two temperature components. Of these nine, in three cases, the warmer dust component is likely the result of a transient process rather than a steady-state collisional cascade. The dust belts at four stars are likely stirred by an unseen planet and merit further investigation.
Naître, grandir, vieillir avec un handicap
Authors: Salmona Sarah 
Published: December 2016

Malgré la soupe et les verres de lait, mon corps et moi avons eu bien du mal à grandir au même rythme. Comment s’élever lorsque le handicap vous retient dans l’enfance et la dépendance ? Comment faire avancer celui qui ne pense qu’à reculer ? Nous avons rencontré beaucoup d’obstacles, mon corps et moi, mais nous avons compris qu’au cours d’une vie, rien ne pouvait en réalité empêcher un être de grandir et de devenir. Mon corps ne suivait pas bien la courbe mais mon esprit voulait gravir des montagnes. J’ai bien essayé de laisser ce corps capricieux sur le bas-côté mais je n’arrivais pas à faire un pas sans lui. Il a bien fallu nous réconcilier et ne faire plus qu’un pour pouvoir aller toujours plus loin…
Naître, grandir, vieillir avec un handicap
Authors: Vanden Driessche Luc 
Published: December 2016

L’auteur réfléchit sur son expérience professionnelle dans différents services et institutions dédiés au handicap mental pour montrer comment l’autonomisation psychique est mobilisée lors du passage d’une structure à une autre. L’angoisse qui peut en être générée se présente avec des intensités variables, allant de l’inquiétude passagère jusqu’aux manifestations psychopathologiques. Mais elle est aussi motrice, révélatrice d’un moment de franchissement très fécond pour la suite. Cette réflexion vaut pour les établissements pour adultes : modifications des liens à la famille, sollicitations relationnelles et sexuelles, entrée dans le monde du travail. Elle vaut également pour les adolescents et pour les enfants devant les acquisitions ou les difficultés dans les grandes étapes du développement, l’entrée dans un petit groupe, l’intégration scolaire. L’accompagnement doit ici s’accorder à la temporalité propre du sujet et considérer tous ces moments d’articulation dans leur efficacité symbolique et en faire, quand c’est possible, des opportunités pour la séparation psychique et la construction de l’identité.
Les collaborateurs issus de l’immigration dans les entreprises françaises : le cas de 10 comités exécutifs du CAC 40
Authors: Penin Pauline 
Published: December 2016

L’objet de cet article est de mesurer la proportion de collaborateurs issus de l’immigration parmi les membres des comités exécutifs. Pour cela nous avons utilisé la « méthode patronymique » afin de reconstituer les origines géographiques supposées des collaborateurs en fonction de leurs noms et prénoms. Les individus qui dirigent les organisations sont d’ailleurs des « sujets d’études » de cette diversité managériale. Problématique sociétale devenue domaine privilégié d’intervention politique et d’action patronale tout autant que sujet légitime d’investigation scientifique, la diversité pose question, et méritent que l’on s’y attarde tant elle est pourvue d’implications profondes dans le cadre de l’entreprise.
Les notions de qualité et de performance de la justice administrative
Authors: Cluzel-Métayer Lucie , Sauviat Agnès 
Published: December 2016

Résumé	La justice administrative est soumise aux exigences de performance imposées par la loi organique relative aux lois de finances, elle est aussi animée par la question de la recherche de la qualité. Les notions de performance et de qualité s’entrecroisent sans pour autant être comparables, elles peuvent s’affronter mais ne sont pas dissociables. À une opposition conceptuelle certaine qui conduit à occulter la qualité au profit de la performance imposée comme mode d’allocation des crédits budgétaires se substitue une complémentarité qui conduit à faire de la qualité un moteur de l’évolution de la justice administrative contemporaine finalement stimulée par la performance et qui font de la qualité une attente objective tout autant qu’une réalité fonctionnelle.
Bilan et perspective d’évolution de la qualité du procès administratif : le point de vue d’un avocat
Authors: Sagalovitsch Éric 
Published: December 2016

Résumé	Les réformes de ces trente dernières années ont contribué à la modernisation du procès administratif. Si la communication à l’avocat du sens des conclusions du rapporteur public avant l’audience et la faculté offerte à l’avocat de prendre la parole après le rapporteur public ont constitué deux avancées majeures, le statut actuel des conclusions du rapporteur public n’est pas satisfaisant. Si la phase d’instruction pourrait être améliorée sur certains points, la nouvelle organisation des audiences et le dialogue pratiqué lors des audiences de référés pourraient permettre quant à eux d’ériger la phase de l’audience du procès administratif comme un modèle particulièrement adapté à la justice du XXI e siècle.