bluuebunny/crossref_metadata_2025_split huggingface dataset:
Self-efficacy and quality of life after low-intensity neuropsychological rehabilitation: A pre-post intervention study
Authors: Brands Ingrid , Custers Maud , van Heugten Caroline 
Published: February 2017

BACKGROUND: Being highly self-efficacious is a key factor in successful chronic disease self-management. It is unknown whether neuropsychological rehabilitation improves self-efficacy in managing the consequences of brain injury. OBJECTIVE: To investigate whether levels of general and brain injury specific self-efficacy and quality of life (QoL) increased after neuropsychological rehabilitation and whether cognitive performance was associated with self-efficacy. METHODS: We conducted a retrospective clinical cohort study of 62 patients with acquired brain injury and cognitive complaints with measurements before start and after completion of treatment. QoL was measured with the visual analogue scale (EQ VAS) of the EuroQol (EQ-5D); self-efficacy with the TBI Self-efficacy Questionnaire (SEsx) and the General Self-efficacy Scale (GSES). Cognitive performance was measured as a compound score of tests for memory, attention and information processing speed. RESULTS: Self-efficacy for managing brain injury-specific symptoms and QoL increased significantly after neuropsychological rehabilitation. Both general and brain injury-specific self-efficacy were positively associated with QoL after completion of the programme. Cognitive performance was not associated with self-efficacy for managing brain injury-specific symptoms nor with general self-efficacy. CONCLUSIONS: Self-efficacy and QoL improve after treatment. Further research is needed to identify the specific ingredients responsible for improvement of self-efficacy in patients with cognitive complaints.
Le chômage des jeunes : quel diagnostic ?
Authors: Batard Pierre-Édouard , Ferrari Nicolas , Saillard Emmanuel 
Published: February 2017

Analysing Youth Unemployment.
The youth unemployment rate gives a very incomplete view of the difficulties facing young people entering the French labour market. The main obstacles are the general rigidities that penalise newentrants whatever their age. However, some young entrants– notably dropouts– experience specific problems. Short-term contracts have lasting but ambiguous effects on integration into the labour force. On the positive side, entering the labour market with a temporary contract may raise the probability of remaining employed in the medium/ long term. On the negative side, a succession of short-term contracts may make it harder to find a stable job. Lastly, young people are often forced to enter the labour market by accepting a job for which they are overqualified.
Can We Reconcile the TA Excess and Hotspot with Auger Observations?
Authors: Globus Noemie , Allard Denis , Parizot Etienne , Lachaud Cyril , Piran Tsvi 
Published: February 2017

Abstract
The Telescope Array (TA) shows a 20° hotspot as well as an excess of ultra-high-energy cosmic-rays (UHECRs) above 50 EeV when compared with the Auger spectrum. We consider the possibility that both the TA excess and hotspot are due to a dominant source in the northern sky. We carry out detailed simulations of UHECR propagation in both the intergalactic medium and the Galaxy, using different values for the intergalactic magnetic field. We consider two general classes of sources: transients and steady, adopting a mixed UHECR composition that is consistent with the one found by Auger. The spatial location of the sources is drawn randomly. We generate Auger-like and TA-like data sets from which we determine the spectrum, the sky maps, and the level of anisotropy. We find that, while steady sources are favored over transients, it is unlikely to account for all the currently available observational data. While we reproduce fairly well the Auger spectrum for the vast majority of the simulated data sets, most of the simulated data sets with a spectrum compatible with that of TA (at most a few percent depending on density model tested) show a much stronger anisotropy than the one observed. We find that the rare cases in which both the spectrum and the anisotropy are consistent require a steady source within ∼10 Mpc, to account for the flux excess, and a strong extragalactic magnetic field ∼10 nG, to reduce the excessive anisotropy.
Nebular Emission Line Ratios in z ≃ 2–3 Star-forming Galaxies with KBSS-MOSFIRE: Exploring the Impact of Ionization, Excitation, and Nitrogen-to-Oxygen Ratio∗
Authors: Strom Allison L. , Steidel Charles C. , Rudie Gwen C. , Trainor Ryan F. , Pettini Max , Reddy Naveen A. 
Published: February 2017

Abstract
We present a detailed study of the rest-optical (3600–7000 Å) nebular spectra of ∼380 star-forming galaxies at

, obtained with Keck/Multi-object Spectrometer for Infrared Exploration (MOSFIRE) as part of the Keck Baryonic Structure Survey (KBSS). The KBSS-MOSFIRE sample is representative of star-forming galaxies at these redshifts, with stellar masses

and star formation rates SFR = 3–1000

yr−1. We focus on robust measurements of many strong diagnostic emission lines for individual galaxies: [O ii]λλ3727, 3729, [Ne iii]λ3869, Hβ, [O iii]

4960, 5008, [N ii]λλ 6549, 6585, Hα, and [S ii]λλ6718, 6732. Comparisons with observations of typical local galaxies from the Sloan Digital Sky Survey and between subsamples of KBSS-MOSFIRE show that high-redshift galaxies exhibit a number of significant differences in addition to the well-known offset in log([O iii]

/Hβ) and log([N ii]

/Hα). We argue that the primary difference between H ii regions in

galaxies and those at

is an enhancement in the degree of nebular excitation, as measured by [O iii]/Hβ and

[([O iii]

+[O ii]

)/Hβ]. At the same time, KBSS-MOSFIRE galaxies are ∼10 times more massive than

galaxies with similar ionizing spectra and have higher N/O (likely accompanied by higher O/H) at fixed excitation. These results indicate the presence of harder ionizing radiation fields at fixed N/O and O/H relative to typical

galaxies, consistent with Fe-poor stellar population models that include massive binaries, and highlight a population of massive, high-specific star formation rate galaxies at high redshift with systematically different star formation histories than galaxies of similar stellar mass today.
A New Compton-thick AGN in Our Cosmic Backyard: Unveiling the Buried Nucleus in NGC 1448 with NuSTAR
Authors: Annuar A. , Alexander D. M. , Gandhi P. , Lansbury G. B. , Asmus D. , Ballantyne D. R. , Bauer F. E. , Boggs S. E. , Boorman P. G. , Brandt W. N. , Brightman M. , Christensen F. E. , Craig W. W. , Farrah D. , Goulding A. D. , Hailey C. J. , Harrison F. A. , Koss M. J. , LaMassa S. M. , Murray S. S. , Ricci C. , Rosario D. J. , Stanley F. , Stern D. , Zhang W. 
Published: February 2017

Abstract
NGC 1448 is one of the nearest luminous galaxies (L
8–1000μm > 109
L
⊙) to ours (z = 0.00390), and yet the active galactic nucleus (AGN) it hosts was only recently discovered, in 2009. In this paper, we present an analysis of the nuclear source across three wavebands: mid-infrared (MIR) continuum, optical, and X-rays. We observed the source with the Nuclear Spectroscopic Telescope Array (NuSTAR), and combined these data with archival Chandra data to perform broadband X-ray spectral fitting (≈0.5–40 keV) of the AGN for the first time. Our X-ray spectral analysis reveals that the AGN is buried under a Compton-thick (CT) column of obscuring gas along our line of sight, with a column density of N
H(los) ≳ 2.5 × 1024 cm−2. The best-fitting torus models measured an intrinsic 2–10 keV luminosity of L

(3.5–7.6) × 1040 erg s−1, making NGC 1448 one of the lowest luminosity CTAGNs known. In addition to the NuSTAR observation, we also performed optical spectroscopy for the nucleus in this edge-on galaxy using the European Southern Observatory New Technology Telescope. We re-classify the optical nuclear spectrum as a Seyfert on the basis of the Baldwin–Philips–Terlevich diagnostic diagrams, thus identifying the AGN at optical wavelengths for the first time. We also present high spatial resolution MIR observations of NGC 1448 with Gemini/T-ReCS, in which a compact nucleus is clearly detected. The absorption-corrected 2–10 keV luminosity measured from our X-ray spectral analysis agrees with that predicted from the optical [O iii]λ5007 Å emission line and the MIR 12 μm continuum, further supporting the CT nature of the AGN.
A Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19)*
Authors: Johnson Christian I. , Caldwell Nelson , Rich R. Michael , Mateo Mario , Bailey, III John I. , Clarkson William I. , Olszewski Edward W. , Walker Matthew G. 
Published: February 2017

Abstract
Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this “iron-complex” cluster class, and we provide here a chemical and kinematic analysis of >300 red giant branch and asymptotic giant branch member stars using high-resolution spectra obtained with the Magellan–M2FS and VLT–FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = −2 to −1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg–Al anti-correlation may only be present in stars with [Fe/H] ≳ −1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the s-process must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [α/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster’s large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to ω Cen and M54.
Exploring 21 cm-Lyα Emitter Synergies for SKA
Authors: Hutter Anne , Dayal Pratika , Müller Volker , Trott Cathryn M. 
Published: February 2017

Abstract
We study the signatures of reionization and ionizing properties of early galaxies in the cross-correlations between the 21 cm emission from the spin-flip transition of neutral hydrogen (H i) and the underlying galaxy population. In particular, we focus on a sub-population of galaxies visible as Lyα Emitters (LAEs). With both observables simultaneously derived from a

hydrodynamical simulation (GADGET-2) snapshot post-processed with a radiative transfer code (pCRASH) and a dust model, we perform a parameter study and aim to constrain both the average intergalactic medium (IGM) ionization state (

) and the reionization topology (outside-in versus inside-out). We find that, in our model, LAEs occupy the densest and most-ionized regions resulting in a very strong anti-correlation between the LAEs and the 21 cm emission. A 1000 hr Square Kilometer Array (SKA)-LOW1—Subaru Hyper Suprime-Cam experiment can provide constraints on

, allowing us to distinguish between IGM ionization levels of 50%, 25%, 10%, and fully ionized at scales

comoving Mpc (assuming foreground avoidance for SKA). Our results support the inside-out reionization scenario where the densest knots (under-dense voids) are ionized first (last) for

. Further, 1000 hr SKA-LOW1 observations should be able to confirm the inside-out scenario by detecting a lower 21 cm brightness temperature (by about 2–10 mK) in the densest regions (≳2 arcmin scales) hosting LAEs, compared to lower-density regions devoid of them.
Galaxy and Mass Assembly (GAMA): Exploring the WISE Web in G12
Authors: Jarrett T. H. , Cluver M. E. , Magoulas C. , Bilicki M. , Alpaslan M. , Bland-Hawthorn J. , Brough S. , Brown M. J. I. , Croom S. , Driver S. , Holwerda B. W. , Hopkins A. M. , Loveday J. , Norberg P. , Peacock J. A. , Popescu C. C. , Sadler E. M. , Taylor E. N. , Tuffs R. J. , Wang L. 
Published: February 2017

Abstract
We present an analysis of the mid-infrared Wide-field Infrared Survey Explorer (WISE) sources seen within the equatorial GAMA G12 field, located in the North Galactic Cap. Our motivation is to study and characterize the behavior of WISE source populations in anticipation of the deep multiwavelength surveys that will define the next decade, with the principal science goal of mapping the 3D large-scale structures and determining the global physical attributes of the host galaxies. In combination with cosmological redshifts, we identify galaxies from their WISE W1 (3.4 μm) resolved emission, and we also perform a star-galaxy separation using apparent magnitude, colors, and statistical modeling of star counts. The resulting galaxy catalog has ≃590,000 sources in 60 deg2, reaching a W1 5σ depth of 31 μJy. At the faint end, where redshifts are not available, we employ a luminosity function analysis to show that approximately 27% of all WISE extragalactic sources to a limit of 17.5 mag (31 μJy) are at high redshift,

. The spatial distribution is investigated using two-point correlation functions and a 3D source density characterization at 5 Mpc and 20 Mpc scales. For angular distributions, we find that brighter and more massive sources are strongly clustered relative to fainter sources with lower mass; likewise, based on WISE colors, spheroidal galaxies have the strongest clustering, while late-type disk galaxies have the lowest clustering amplitudes. In three dimensions, we find a number of distinct groupings, often bridged by filaments and superstructures. Using special visualization tools, we map these structures, exploring how clustering may play a role with stellar mass and galaxy type.
Atmospheric Habitable Zones in Y Dwarf Atmospheres
Authors: Yates Jack S. , Palmer Paul I. , Biller Beth , Cockell Charles S. 
Published: February 2017

Abstract
We use a simple organism lifecycle model to explore the viability of an atmospheric habitable zone (AHZ), with temperatures that could support Earth-centric life, which sits above an environment that does not support life. To illustrate our model, we use a cool Y dwarf atmosphere, such as WISE J085510.83–0714442.5, whose 4.5–5.2 μm spectrum shows absorption features consistent with water vapor and clouds. We allow organisms to adapt to their atmospheric environment (described by temperature, convection, and gravity) by adopting different growth strategies that maximize their chance of survival and proliferation. We assume a constant upward vertical velocity through the AHZ. We found that the organism growth strategy is most sensitive to the magnitude of the atmospheric convection. Stronger convection supports the evolution of more massive organisms. For a purely radiative environment, we find that evolved organisms have a mass that is an order of magnitude smaller than terrestrial microbes, thereby defining a dynamical constraint on the dimensions of life that an AHZ can support. Based on a previously defined statistical approach, we infer that there are of the order of 109 cool Y brown dwarfs in the Milky Way, and likely a few tens of these objects are within 10 pc from Earth. Our work also has implications for exploring life in the atmospheres of temperate gas giants. Consideration of the habitable volumes in planetary atmospheres significantly increases the volume of habitable space in the galaxy.
Observational Evidence Linking Interstellar UV Absorption to PAH Molecules
Authors: Blasberger Avi , Behar Ehud , Perets Hagai B. , Brosch Noah , Tielens Alexander G. G. M. 
Published: February 2017

Abstract
The 2175 Å UV extinction feature was discovered in the mid-1960s, yet its physical origin remains poorly understood. One suggestion is absorption by polycyclic aromatic hydrocarbon (PAH) molecules, which is supported by theoretical molecular structure computations and by laboratory experiments. PAHs are positively detected by their 3.3, 6.2, 7.7, 8.6, 11.3, and 12.7 μm IR emission bands, which are specified by their modes of vibration. A definitive empirical link between the 2175 Å UV extinction and the IR PAH emission bands, however, is still missing. We present a new sample of hot stars that have both 2175 Å absorption and IR PAH emission. We find significant shifts of the central wavelength of the UV absorption feature, up to 2350 Å, but predominantly in stars that also have IR PAH emission. These UV shifts depend on stellar temperature in a fashion that is similar to the shifts of the 6.2 and 7.7 μm IR PAH bands, that is, the features are increasingly more redshifted as the stellar temperature decreases, but only below ∼15 kK. Above 15 kK both UV and IR features retain their nominal values. Moreover, we find a suggestive correlation between the UV and IR shifts. We hypothesize that these similar dependences of both the UV and IR features on stellar temperature hint at a common origin of the two in PAH molecules and may establish the missing link between the UV and IR observations. We further suggest that the shifts depend on molecular size, and that the critical temperature of ∼15 kK above which no shifts are observed is related to the onset of UV-driven hot-star winds and their associated shocks.
Interaction of Two Filaments in a Long Filament Channel Associated with Twin Coronal Mass Ejections
Authors: Zheng Ruisheng , Zhang Qingmin , Chen Yao , Wang Bing , Du Guohui , Li Chuanyang , Yang Kai 
Published: February 2017

Abstract
Using the high-quality observations of the Solar Dynamics Observatory, we present the interaction of two filaments (F1 and F2) in a long filament channel associated with twin coronal mass ejections (CMEs) on 2016 January 26. Before the eruption, a sequence of rapid cancellation and emergence of the magnetic flux has been observed, which likely triggered the ascending of the west filament (F1). The east footpoints of rising F1 moved toward the east far end of the filament channel, accompanied by post-eruption loops and flare ribbons. This likely indicated a large-scale eruption involving the long filament channel, which resulted from the interaction between F1 and the east filament (F2). Some bright plasma flew over F2, and F2 stayed at rest during the eruption, likely due to the confinement of its overlying lower magnetic field. Interestingly, the impulsive F1 pushed its overlying magnetic arcades to form the first CME, and F1 finally evolved into the second CME after the collision with the nearby coronal hole. We suggest that the interaction of F1 and the overlying magnetic field of F2 led to the merging reconnection that forms a longer eruptive filament loop. Our results also provide a possible picture of the origin of twin CMEs and show that the large-scale magnetic topology of the coronal hole is important for the eventual propagation direction of CMEs.
Charge States and FIP Bias of the Solar Wind from Coronal Holes, Active Regions, and Quiet Sun
Authors: Fu Hui , Madjarska Maria S. , Xia LiDong , Li Bo , Huang ZhengHua , Wangguan Zhipeng 
Published: February 2017

Abstract
Connecting in situ measured solar-wind plasma properties with typical regions on the Sun can provide an effective constraint and test to various solar wind models. We examine the statistical characteristics of the solar wind with an origin in different types of source regions. We find that the speed distribution of coronal-hole (CH) wind is bimodal with the slow wind peaking at ∼400 km s−1 and the fast at ∼600 km s−1. An anti-correlation between the solar wind speeds and the O7+/O6+ ion ratio remains valid in all three types of solar wind as well during the three studied solar cycle activity phases, i.e., solar maximum, decline, and minimum. The

range and its average values all decrease with the increasing solar wind speed in different types of solar wind. The

range (0.06–0.40, first ionization potential (FIP) bias range 1–7) for active region wind is wider than for CH wind (0.06–0.20, FIP bias range 1–3), while the minimum value of

(∼ 0.06) does not change with the variation of speed, and it is similar for all source regions. The two-peak distribution of CH wind and the anti-correlation between the speed and O7+/O6+ in all three types of solar wind can be explained qualitatively by both the wave-turbulence-driven and reconnection-loop-opening (RLO) models, whereas the distribution features of

in different source regions of solar wind can be explained more reasonably by the RLO models.
Magnetospheric Multiscale Observations of Electron Vortex Magnetic Hole in the Turbulent Magnetosheath Plasma
Authors: Huang S. Y. , Sahraoui F. , Yuan Z. G. , He J. S. , Zhao J. S. , Contel O. Le , Deng X. H. , Zhou M. , Fu H. S. , Shi Q. Q. , Lavraud B. , Pang Y. , Yang J. , Wang D. D. , Li H. M. , Yu X. D. , Pollock C. J. , Giles B. L. , Torbert R. B. , Russell C. T. , Goodrich K. A. , Gershman D. J. , Moore T. E. , Ergun R. E. , Khotyaintsev Y. V. , Lindqvist P.-A. , Strangeway R. J. , Magnes W. , Bromund K. , Leinweber H. , Plaschke F. , Anderson B. J. , Burch J. L. 
Published: February 2017

Abstract
We report on the observations of an electron vortex magnetic hole corresponding to a new type of coherent structure in the turbulent magnetosheath plasma using the Magnetospheric Multiscale mission data. The magnetic hole is characterized by a magnetic depression, a density peak, a total electron temperature increase (with a parallel temperature decrease but a perpendicular temperature increase), and strong currents carried by the electrons. The current has a dip in the core region and a peak in the outer region of the magnetic hole. The estimated size of the magnetic hole is about 0.23 ρ
i (∼30 ρ
e) in the quasi-circular cross-section perpendicular to its axis, where ρ
i and ρ
e are respectively the proton and electron gyroradius. There are no clear enhancements seen in high-energy electron fluxes. However, there is an enhancement in the perpendicular electron fluxes at 90° pitch angle inside the magnetic hole, implying that the electrons are trapped within it. The variations of the electron velocity components V
em and V
en suggest that an electron vortex is formed by trapping electrons inside the magnetic hole in the cross-section in the M–N plane. These observations demonstrate the existence of a new type of coherent structures behaving as an electron vortex magnetic hole in turbulent space plasmas as predicted by recent kinetic simulations.
A new device to mount portable energy-dispersive X-ray fluorescence spectrometers (p-ED-XRF) for semi-continuous analyses of split (sediment) cores and solid samples
Authors: Hoelzmann Philipp , Klein Torsten , Kutz Frank , Schütt Brigitta 
Published: February 2017

Abstract. Portable energy-dispersive X-ray fluorescence spectrometers (p-ED-XRF) have become increasingly popular in sedimentary laboratories to quantify the chemical composition of a range of materials such as sediments, soils, solid samples, and artefacts. Here, we introduce a low-cost, clearly arranged unit that functions as a sample chamber (German industrial property rights no. 20 2014 106 048.0) for p-ED-XRF devices to facilitate economic, non-destructive, fast, and semi-continuous analysis of (sediment) cores or other solid samples. The spatial resolution of the measurements is limited to the specifications of the applied p-ED-XRF device – in our case a Thermo Scientific Niton XL3t p-ED-XRF spectrometer with a maximum spatial resolution of 0.3 cm and equipped with a charge-coupled device (CCD) camera to document the measurement spot. We demonstrate the strength of combining p-ED-XRF analyses with this new sample chamber to identify Holocene facies changes (e.g. marine vs. terrestrial sedimentary facies) using a sediment core from an estuarine environment in the context of a geoarchaeological investigation at the Atlantic coast of southern Spain.