bluuebunny/crossref_metadata_2025_split huggingface dataset:
Trixagus atticus Reitter et T. minutas Rey, deux espèces méconnues d'Europe occidentale présentes en France (Coleoptera Throscidae)
Authors: Leseigneur Lucien 
Published: February 2017

Trixagus atticus Reitter and T. minutus Rey, two unrecognized species from western Europe present in France (Coleoptera, Throscidae)
Summary. — Trixagus atticus Reitter, which was described from Greece, has a large distribution. It was recently discovered in several countries of western Europe and in Cyprus. Trixagus minutus Rey, which was synonymized with T. obtusus (Curtis) by all authors is a valid species which belongs to the atticus group. T. ciliaris Rey is kept as synonym of T. obtusus (Curtis). The case of T. pusillus (Heer) is examined but unresolved, the original specimens being missing. Lectotypes of T. minutus and T. ciliaris are designated.
Biodiversité et écologie : quelques réflexions théoriques et pratiques
Authors: Lebreton Philippe 
Published: February 2017

Biodiversity and ecology : some theoretical and practical ideas.
Biodiversity is a concept which has received recently a great deal of publicity but is more complex than sometimes thought. Present at every level of biological organisation, biodiversity can be defined as the quantity and the quality of information contained in any biosystem, from genetic material through to lanscapes. Examples are examined using the pine genus (Pinus) in Europe and regional bird communities : these demonstrate the need to complete the quantitative concept of richness by qualitative notions of rarity and local occurence.
Two cases taken within natural pares of the Rhône-Alpes region (France) also underline the need to situate biodiversity in an overall and evolving context. The first case concerns the (re) introduction of the alpine ibex in the Vercors pre-Alps, the second the «garden» management of the heaths (between meadow and woodlands areas) on the tops of the Pilat hills (West bank of the Rhône valley). In conclusion, biodiversity provides an excellent criterion for assessing environmental management in the context of what is now termed «sustainable development».
Uniform Contribution of Supernova Explosions to the Chemical Enrichment of Abell 3112 out to R200
Authors: Ezer Cemile , Bulbul Esra , Ercan E. Nihal , Smith Randall K. , Bautz Mark W. , Loewenstein Mike , McDonald Mike , Miller Eric D. 
Published: February 2017

Abstract
The spatial distribution of the metals residing in the intra-cluster medium (ICM) of galaxy clusters records all the information on a cluster’s nucleosynthesis and chemical enrichment history. We present measurements from a total of 1.2 Ms Suzaku XIS and 72 ks Chandra observations of the cool-core galaxy cluster Abell 3112 out to its virial radius (∼1470 kpc). We find that the ratio of the observed supernova type Ia explosions to the total supernova explosions has a uniform distribution at a level of 12%–16% out to the cluster’s virial radius. The observed fraction of type Ia supernova explosions is in agreement with the corresponding fraction found in our Galaxy and the chemical enrichment of our Galaxy. The non-varying supernova enrichment suggests that the ICM in cluster outskirts was enriched by metals at an early stage before the cluster itself was formed during a period of intense star formation activity. Additionally, we find that the 2D delayed detonation model CDDT produce significantly worse fits to the X-ray spectra compared to simple 1D W7 models. This is due to the relative overestimate of Si, and the underestimate of Mg in these models with respect to the measured abundances.
Testing the Presence of Multiple Photometric Components in Nearby Early-type Galaxies Using SDSS
Authors: Oh Semyeong , Greene Jenny E. , Lackner Claire N. 
Published: February 2017

Abstract
We investigate two-dimensional image decomposition of nearby, morphologically selected early-type galaxies (ETGs). We are motivated by recent observational evidence of significant size growth of quiescent galaxies and theoretical development advocating a two-phase formation scenario for ETGs. We find that a significant fraction of nearby ETGs show changes in isophotal shape that require multi-component models. The characteristic sizes of the inner and outer component are ∼3 and ∼15 kpc. The inner component lies on the mass–size relation of ETGs at z ∼ 0.25–0.75, while the outer component tends to be more elliptical and hints at a stochastic buildup process. We find real physical differences between single- and double-component ETGs, with double-component galaxies being younger and more metal-rich. The fraction of double-component ETGs increases with increasing σ and decreases in denser environments. We hypothesize that double-component systems were able to accrete gas and small galaxies until later times, boosting their central densities, building up their outer parts, and lowering their typical central ages. In contrast, the oldest galaxies, perhaps due to residing in richer environments, have no remaining hints of their last accretion episode.
CO Spectral Line Energy Distributions in Galactic Sources: Empirical Interpretation of Extragalactic Observations∗
Authors: Indriolo Nick , Bergin E. A. , Goicoechea J. R. , Cernicharo J. , Gerin M. , Gusdorf A. , Lis D. C. , Schilke P. 
Published: February 2017

Abstract
The relative populations in rotational transitions of CO can be useful for inferring gas conditions and excitation mechanisms at work in the interstellar medium. We present CO emission lines from rotational transitions observed with Herschel/HIFI in the star-forming cores Orion S, Orion KL, Sgr B2(M), and W49N. Integrated line fluxes from these observations are combined with those from Herschel/PACS observations of the same sources to construct CO spectral line energy distributions (SLEDs) from 5 ≤ J

u
≤ 48. These CO SLEDs are compared to those reported in other galaxies, with the intention of empirically determining which mechanisms dominate excitation in such systems. We find that CO SLEDs in Galactic star-forming cores cannot be used to reproduce those observed in other galaxies, although the discrepancies arise primarily as a result of beam filling factors. The much larger regions sampled by the Herschel beams at distances of several megaparsecs contain significant amounts of cooler gas, which dominate the extragalactic CO SLEDs, in contrast to observations of Galactic star-forming regions, which are focused specifically on cores containing primarily hot molecular gas.
Self-consistent Black Hole Accretion Spectral Models and the Forgotten Role of Coronal Comptonization of Reflection Emission
Authors: Steiner James F. , García Javier A. , Eikmann Wiebke , McClintock Jeffrey E. , Brenneman Laura W. , Dauser Thomas , Fabian Andrew C. 
Published: February 2017

Abstract
Continuum and reflection spectral models have each been widely employed in measuring the spins of accreting black holes. However, the two approaches have not been implemented together in a photon-conserving, self-consistent framework. We develop such a framework using the black hole X-ray binary GX 339–4 as a touchstone source, and we demonstrate three important ramifications. (1) Compton scattering of reflection emission in the corona is routinely ignored, but is an essential consideration given that reflection is linked to the regimes with strongest Comptonization. Properly accounting for this causes the inferred reflection fraction to increase substantially, especially for the hard state. Another important impact of the Comptonization of reflection emission by the corona is the downscattered tail. Downscattering has the potential to mimic the relativistically broadened red wing of the Fe line associated with a spinning black hole. (2) Recent evidence for a reflection component with a harder spectral index than the power-law continuum is naturally explained as Compton-scattered reflection emission. (3) Photon conservation provides an important constraint on the hard state’s accretion rate. For bright hard states, we show that disk truncation to large scales

is unlikely as this would require accretion rates far in excess of the observed

of the brightest soft states. Our principal conclusion is that when modeling relativistically broadened reflection, spectral models should allow for coronal Compton scattering of the reflection features, and when possible, take advantage of the additional constraining power from linking to the thermal disk component.
Observation of a Short Period Quasi-periodic Pulsation in Solar X-Ray, Microwave, and EUV Emissions
Authors: Kumar Pankaj , Nakariakov Valery M. , Cho Kyung-Suk 
Published: February 2017

Abstract
This paper presents the multiwavelength analysis of a 13 s quasi-periodic pulsation (QPP) observed in hard X-ray (12–300 keV) and microwave (4.9–34 GHz) emissions during a C-class flare that occurred on 2015 September 21. Atmospheric Image Assembly (AIA) 304 and 171 Å images show an emerging loop/flux tube (L1) moving radially outward, which interacts with the preexisting structures within the active region (AR). The QPP was observed during the expansion of and rising motion of L1. The Nobeyama Radioheliograph microwave images in 17/34 GHz channels reveal a single radio source that was co-spatial with a neighboring loop (L2). In addition, using AIA 304 Å images, we detected intensity oscillations in the legs of L2 with a period of about 26 s. A similar oscillation period was observed in the GOES soft X-ray flux derivative. This oscillation period seems to increase with time. We suggest that the observed QPP is most likely generated by the interaction between L2 and L3 observed in the AIA hot channels (131 and 94 Å). The merging speed of loops L2 and L3 was ∼35 km s−1. L1 was destroyed possibly by its interaction with preexisting structures in the AR, and produced a cool jet with the speed of ∼106–118 km s−1 associated with a narrow CME (∼770 km s−1). Another mechanism of the QPP in terms of a sausage oscillation of the loop (L2) is also possible.
Precise Calculations of Astrophysically Important Allowed and Forbidden Transitions of Xe viii
Authors: Bhowmik Anal , Dutta Narendra Nath , Roy Sourav 
Published: February 2017

Abstract
The present work reports transition line parameters for Xe viii, which are potentially important for astrophysics in view of recent observations of multiply ionized xenon in hot white dwarfs. The relativistic coupled-cluster method is employed here to calculate the E1, E2, and M1 transition line parameters with high accuracy. The E1 oscillator strengths and probabilities of E2 and M1 transitions are determined using theoretical amplitudes and experimental energy values. The calculated branching ratios and the lifetimes are supplemented to the transition parameters. The accurate presentation of these calculated data is crucial for density estimation in several stellar and interstellar media.
Intermediate-mass Asymptotic Giant Branch Stars and Sources of 26Al, 60Fe, 107Pd, and 182Hf in the Solar System
Authors: Wasserburg G. J. , Karakas Amanda I. , Lugaro Maria 
Published: February 2017

Abstract
We explore the possibility that the short-lived radionuclides

l,

e,

d, and

f inferred to be present in the proto-solar cloud originated from 3–8

asymptotic giant branch (AGB) stars. Models of AGB stars with initial mass above

are prolific producers of

l owing to hot bottom burning (HBB). In contrast,

e,

d, and

f are produced by neutron captures:

d and

f in models

and

e in models with higher mass. We mix stellar yields from solar-metallicity AGB models into a cloud of solar mass and composition to investigate whether it is possible to explain the abundances of the four radioactive nuclides at the Sun’s birth using one single value of the mixing ratio between the AGB yields and the initial cloud material. We find that AGB stars that experience efficient HBB (

) cannot provide a solution because they produce too little

f and

d relative to

l and

e. Lower-mass AGB stars cannot provide a solution because they produce too little

l relative to

d and

f. A self-consistent solution may be found for AGB stars with masses in between (4–5.5

), provided that HBB is stronger than in our models and the

(α, n)

neutron source is mildly activated. If stars of

are the source of the radioactive nuclides, then some basis for their existence in proto-solar clouds needs to be explored, given that the stellar lifetimes are longer than the molecular cloud lifetimes.
A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3
Authors: Temim Tea , Dwek Eli , Arendt Richard G. , Borkowski Kazimierz J. , Reynolds Stephen P. , Slane Patrick , Gelfand Joseph D. , Raymond John C. 
Published: February 2017

Abstract
While theoretical models of dust condensation predict that most refractory elements produced in core-collapse supernovae (SNe) efficiently condense into dust, a large quantity of dust has so far only been observed in SN 1987A. We present an analysis of observations from the Spitzer Space Telescope, Herschel Space Observatory, Stratospheric Observatory for Infrared Astronomy, and AKARI of the infrared shell surrounding the pulsar wind nebula in the supernova remnant G54.1+0.3. We attribute a distinctive spectral feature at 21 μm to a magnesium silicate grain species that has been invoked in modeling the ejecta-condensed dust in Cas A, which exhibits the same spectral signature. If this species is responsible for producing the observed spectral feature and accounts for a significant fraction of the observed infrared continuum, we find that it would be the dominant constituent of the dust in G54.1+0.3, with possible secondary contributions from other compositions, such as carbon, silicate, or alumina grains. The total mass of SN-formed dust required by this model is at least 0.3 M
⊙. We discuss how these results may be affected by varying dust grain properties and self-consistent grain heating models. The spatial distribution of the dust mass and temperature in G54.1+0.3 confirms the scenario in which the SN-formed dust has not yet been processed by the SN reverse shock and is being heated by stars belonging to a cluster in which the SN progenitor exploded. The dust mass and composition suggest a progenitor mass of 16–27 M
⊙ and imply a high dust condensation efficiency, similar to that found for Cas A and SN 1987A. The study provides another example of significant dust formation in a Type IIP SN explosion and sheds light on the properties of pristine SN-condensed dust.
Investigating the Effect of Cosmic Opacity on Standard Candles
Authors: Hu J. , Yu H. , Wang F. Y. 
Published: February 2017

Abstract
Standard candles can probe the evolution of dark energy over a large redshift range. But the cosmic opacity can degrade the quality of standard candles. In this paper, we use the latest observations, including Type Ia supernovae (SNe Ia) from the “joint light-curve analysis” sample and Hubble parameters, to probe the opacity of the universe. A joint fitting of the SNe Ia light-curve parameters, cosmological parameters, and opacity is used in order to avoid the cosmological dependence of SNe Ia luminosity distances. The latest gamma-ray bursts are used in order to explore the cosmic opacity at high redshifts. The cosmic reionization process is considered at high redshifts. We find that the sample supports an almost transparent universe for flat ΛCDM and XCDM models. Meanwhile, free electrons deplete photons from standard candles through (inverse) Compton scattering, which is known as an important component of opacity. This Compton dimming may play an important role in future supernova surveys. From analysis, we find that about a few per cent of the cosmic opacity is caused by Compton dimming in the two models, which can be corrected.
Diffusion of Oxygen Isotopes in Thermally Evolving Planetesimals and Size Ranges of Presolar Silicate Grains
Authors: Wakita Shigeru , Nozawa Takaya , Hasegawa Yasuhiro 
Published: February 2017

Abstract
Presolar grains are small particles found in meteorites through their isotopic compositions, which are considerably different from those of materials in the solar system. If some isotopes in presolar grains diffused out beyond their grain sizes when they were embedded in parent bodies of meteorites, their isotopic compositions could be washed out, and hence the grains could no longer be identified as presolar grains. We explore this possibility for the first time by self-consistently simulating the thermal evolution of planetesimals and the diffusion length of 18O in presolar silicate grains. Our results show that presolar silicate grains smaller than ∼0.03 μm cannot keep their original isotopic compositions even if the host planetesimals experienced a maximum temperature as low as 600 °C. Since this temperature corresponds to that experienced by petrologic type 3 chondrites, isotopic diffusion can constrain the size of presolar silicate grains discovered in such chondrites to be larger than ∼0.03 μm. We also find that the diffusion length of 18O reaches ∼0.3–2 μm in planetesimals that were heated up to 700–800°C. This indicates that, if the original size of presolar grains spans a range from ∼0.001 μm to ∼0.3 μm like that in the interstellar medium, then the isotopic records of the presolar grains may be almost completely lost in such highly thermalized parent bodies. We propose that isotopic diffusion could be a key process to control the size distribution and abundance of presolar grains in some types of chondrites.
Tomographic Findings After Implantation of Ferrara Intrastromal Corneal Ring Segments in Keratoconus
Authors: Lyra João Marcelo , Lyra Daniela , Ribeiro Guilherme , Torquetti Leonardo , Ferrara Paulo , Machado Aydano 
Published: February 2017

PURPOSE:
To analyze and compare changes to the anterior and posterior corneal surfaces after Ferrara intracorneal ring segment (ICRS) (AJL, Boecillo, Spain) implantation and to correlate those changes with visual outcomes.

METHODS:
This retrospective case series study comprised consecutive patients with keratoconus implanted with the Ferrara ICRS. Computed tomography scans of the two corneal surfaces were obtained preoperatively and postoperatively with a rotating Scheimpflug imaging system. The Wilcoxon test was used to compare groups, and the Pearson's correlation coefficient was used to measure the strength of the correlation between variables.

RESULTS:
The study evaluated 241 eyes in 182 patients with keratoconus. Both corneal surfaces showed statistically significant decreases in average steep keratometry (K2) values, corneal astigmatism, elevation at the apex and at the thinnest point, maximum elevation in the central 4-mm area, and elevation inside the 3- and 4-mm zones and at the 3-mm ring. Regarding anterior surface parameters, a significant decrease was observed in flat keratometry (K1), whereas asphericity increased. On the posterior corneal surface, no significant changes in K1 and asphericity were observed. Poor correlation was found between visual outcomes and changes in tomographic parameters. The best correlation was obtained for anterior corneal astigmatism.

CONCLUSIONS:
ICRS implantation led to statistically significant changes in both anterior and posterior corneal surfaces. However, correlation between visual outcomes and tomographic parameters was poor.

[
J Refract Surg.
2017;33(2):110–115.]
A Critical Evaluation of Refractive Outcomes Following LASIK for Moderate to High Astigmatism Using Two Excimer Laser Platforms
Authors: Patel Sudi , Bohac Maja , Biscevic Alma , Koncarevic Mateja , Anticic Marija , Gabric Nikica 
Published: February 2017

PURPOSE:
To calculate the surgically induced astigmatism (SIA) following LASIK and identify any association between SIA and the target induced astigmatism (TIA) at 1 year postoperatively.

METHODS:
The SIA was calculated using the TIA and residual astigmatism values for [A] myopic astigmatism and [B] mixed astigmatism treated with either the [I] WaveLight Allegretto EyeQ 400-Hz (Alcon Laboratories, Inc. Fort Worth, TX) or [II] Schwind Amaris 750S (Schwind eye-tech-solutions, Kleinostheim, Germany) platforms. The TIA and corresponding SIA results were analyzed using various techniques.

RESULTS:

Key findings were the negative SIA power (y
1
) was significantly correlated with negative TIA power (x
1
) and sine of the TIA axis (x
2
) as follows: [A] I, y
1
= 0.829x
1
–0.403x
2
–0.325 (
F
= 87.76,
r
= 0.804,
P
< .001, n = 127); II, y
1
= 0.891x
1
–0.037x
2
–0.192 (
F
= 240.06,
r
= 0.901,
P
< .001, n = 119) and [B] I, y
1
= 1.063x
1
+0.233x
2
+0.411 (
F
= 990.99,
r
= 0.881,
P
< .001, n = 61); II, y
1
= 1.029x
1
–0.115x
2
+0.322 (
F
= 270.12,
r
= 0.908,
P
< 0.001, n = 111). The sine of negative SIA axis (y
2
) was significantly correlated with negative TIA power (x
1
) and TIA axis (x
2
) as follows: [A] I, y
2
= 0.951x
2
–0.007x
1
+0.008 (
F
= 446.58,
r
= 0.950,
P
< .001, n = 127); II, y
2
= 0.856x
2
+0.007x
1
+0.105 (
F
= 277.18,
r
= 0.912,
P
< .001, n = 119) and [B] I, y
2
= 0.953x
2
+0.009x
1
+0.075 (
F
= 362.6,
r
= 0.963,
P
< .001, n = 61); II, y
2
= 0.977x
2
–0.004x
1
+0.002 (
F
= 2910.9,
r
= 0.990,
P
< .001, n = 111).

CONCLUSIONS:
The predicted SIA power was up to 12% less than expected in cases of −6.00 diopters cylinder treated for myopic astigmatism using the Allegretto platform. The mean predicted angle of error (the angle between the SIA and TIA axes) was less than 4°, increasing to 12° for against-the-rule astigmatism. The Allegretto platform tended toward a clockwise axis rotational error, whereas the Amaris platform tended toward the opposite.

[
J Refract Surg.
2017;33(2):104–109.]
An Algorithm to Predict the Biomechanical Stiffening Effect in Corneal Cross-linking
Authors: Kling Sabine , Hafezi Farhad 
Published: February 2017

PURPOSE:
To develop an algorithm to predict the stiffening effect of CXL and to verify the accuracy with results obtained from experimental measurements.

METHODS:

The algorithm considers different variables: the reaction kinetics of riboflavin diffusion and riboflavin photodegradation to determine the effective riboflavin concentration in different stromal layers; the oxygen diffusion and ultraviolet (UV) absorption to determine the amount of reactive oxygen species as a function of time and stromal depth. For the experimental comparison, corneas were deepithelialized, followed by riboflavin instillation for 30 minutes and UV irradiation. Different pulsed and continuous-light conditions were analyzed with irradiances ranging from 3 to 100 mW/cm
2
and irradiation times from 8 to 30 minutes. Stress-relaxation measurements were performed in fresh-enucleated porcine (n = 66) and rabbit (n = 2) eyes directly after treatment, using a load of 0.6 MPa.

RESULTS:

A clear linear relationship was observed between the concentration of newly induced cross-links and the experimentally observed stiffening factor (
R
2
= 0.9432). An additional 1 mol/m
3
of cross-links increased the mechanical stress resistance of the cornea by 50.4%. The efficacy of standard CXL in murine, lapine, and porcine corneas was inversely related to corneal thickness. The stiffening effect after CXL decreased by 4.1% per 100
µ
m (
R
2
= 0.9961).

CONCLUSIONS:
The proposed model, supported by data in porcine, murine, and lapine corneas, suggests a possibility of also predicting the biomechanical CXL efficacy in human corneas. The biomechanical efficacy of CXL may be increased by prolonged UV irradiation at reduced irradiances or by a higher oxygen pressure in the environment. Pulsed CXL does not accelerate CXL or increase its efficacy when compared to standard CXL of the same irradiation duration. This model might be used to calculate customized irradiation settings for high-risk cases, but also topography-guided CXL treatments.

[
J Refract Surg.
2017;33(2):128–136.]