bluuebunny/crossref_metadata_2025_split huggingface dataset:
How to Craft a Just Economy (not Enforce a Mad Utopia): Response to Michael Black
Authors: Powell Bill 
Published: December 2017

Most people see ‘capitalism’ and ‘socialism’ as opposed, but for ‘distributists’, like G. K. Chesterton and Hilaire Belloc, they are both fatally flawed. Instead, distributists ‘believe that ownership in the means of livelihood is normal to man, and necessary to liberty.’ At present, the ownership of productive property is concentrated in too few hands, which causes all sorts of problems, including the latest round of Wall Street failures and bailouts. The question is, how can we achieve a better distribution of property without going down the Utopian road of coercion (and nightmare)? At the heart of distributist theory is the conviction that widespread ownership is what most people actually want. Distributists don’t want to coerce anyone into becoming owners; we want to remove the coercions that currently prevent most people from becoming owners. In theory, all adults in Western societies are already free to become their own economic masters; in reality, a myriad of coercive tactics keep most economic control in a few hands. Although we should work on the political side to end these coercions (for instance, the current government tax breaks, bailouts, and outright subsidies to large corporations), the main distributist focus is always on widespread, personal action. We can do much more than we’re doing with the freedoms we still have, especially our choices in how we shop and how we work.
Evolutionary history of two pollen self‐incompatibility factors reveals alternate routes to self‐compatibility within Solanum
Authors: Markova Dragomira N. , Petersen Jennifer J. , Yam Sarah E. , Corral Adryanna , Valle Matthew J. , Li Wentao , Chetelat Roger T. 
Published: December 2017

PREMISE OF THE STUDY:Self‐incompatibility (SI) prevents self‐fertilization and reduces inbreeding. While SI is common in plants, transitions to self‐compatibility (SC) occur frequently. Little is known about the genetic changes and evolutionary steps underlying these shifts.METHODS:In the Solanaceae, SI is gametophytic, with specificity determined by S‐RNases in the pistil and S‐locus F‐box proteins (SLFs) in pollen. We examined the role of two pollen factors, Cullin1 (CUL1) and SLF‐23, in SI → SC transitions in wild tomato species from the Arcanum species group (Solanum arcanum, S. neorickii, and S. chmielewskii). Pollen compatibility was assessed on tester lines that reject pollen lacking functional SLF‐23 or CUL1. Complementation tests, gene sequencing, and phylogenetic analyses were used to characterize both functional and nonfunctional alleles.KEY RESULTS:We found evidence for multiple independent SI → SC transitions. In S. arcanum and S. chmielewskii, SC is caused by loss of pistil S‐RNase activity, while in S. neorickii SC is associated with expression of a functional SLF‐23 that recognizes the S9 type S‐RNase expressed in its pistils. Interestingly, we found identical deletion mutations in CUL1 exon 7 of S. chmielewskii as previously seen in S. habrochaites.CONCLUSIONS:Mating system transitions in the Arcanum group have occurred via both pistil loss‐of‐function and pollen gain‐of‐function SC mutations. Mutations common to S. chmielewskii and S. habrochaites must have arisen in a common ancestor, possibly to the entire tomato clade, then became fixed in different lineages after loss of pistil‐side SI function.
Photometric Redshifts with the LSST: Evaluating Survey Observing Strategies
Authors: Graham Melissa L. , Connolly Andrew J. , Ivezić Željko , Schmidt Samuel J. , Jones R. Lynne , Jurić Mario , Daniel Scott F. , Yoachim Peter 
Published: December 2017

Abstract
In this paper we present and characterize a nearest-neighbors color-matching photometric redshift estimator that features a direct relationship between the precision and accuracy of the input magnitudes and the output photometric redshifts. This aspect makes our estimator an ideal tool for evaluating the impact of changes to LSST survey parameters that affect the measurement errors of the photometry, which is the main motivation of our work (i.e., it is not intended to provide the “best” photometric redshifts for LSST data). We show how the photometric redshifts will improve with time over the 10 year LSST survey and confirm that the nominal distribution of visits per filter provides the most accurate photo-z results. The LSST survey strategy naturally produces observations over a range of airmass, which offers the opportunity of using an SED- and z-dependent atmospheric affect on the observed photometry as a color-independent redshift indicator. We show that measuring this airmass effect and including it as a prior has the potential to improve the photometric redshifts and can ameliorate extreme outliers, but that it will only be adequately measured for the brightest galaxies, which limits its overall impact on LSST photometric redshifts. We furthermore demonstrate how this airmass effect can induce a bias in the photo-z results, and caution against survey strategies that prioritize high-airmass observations for the purpose of improving this prior. Ultimately, we intend for this work to serve as a guide for the expectations and preparations of the LSST science community with regard to the minimum quality of photo-z as the survey progresses.
On the Spatially Resolved Star Formation History in M51. I. Hybrid UV+IR Star Formation Laws and IR Emission from Dust Heated by Old Stars
Authors: Eufrasio R. T. , Lehmer B. D. , Zezas A. , Dwek E. , Arendt R. G. , Basu-Zych A. , Wiklind T. , Yukita M. , Fragos T. , Hornschemeier A. E. , Markwardt L. , Ptak A. , Tzanavaris P. 
Published: December 2017

Abstract
We present Lightning, a new spectral energy distribution fitting procedure, capable of quickly and reliably recovering star formation history (SFH) and extinction parameters. The SFH is modeled as discrete steps in time. In this work, we assumed lookback times of 0–10 Myr, 10–100 Myr, 0.1–1 Gyr, 1–5 Gyr, and 5–13.6 Gyr. Lightning consists of a fully vectorized inversion algorithm to determine SFH step intensities and combines this with a grid-based approach to determine three extinction parameters. We apply our procedure to the extensive far-UV-to-far-IR photometric data of M51, convolved to a common spatial resolution and pixel scale, and make the resulting maps publicly available. We recover, for M51a, a peak star formation rate (SFR) between 0.1 and 5 Gyr ago, with much lower star formation activity over the past 100 Myr. For M51b, we find a declining SFR toward the present day. In the outskirt regions of M51a, which includes regions between M51a and M51b, we recover an SFR peak between 0.1 and 1 Gyr ago, which corresponds to the effects of the interaction between M51a and M51b. We utilize our results to (1) illustrate how UV+IR hybrid SFR laws vary across M51 and (2) provide first-order estimates for how the IR luminosity per unit stellar mass varies as a function of the stellar age. From the latter result, we find that IR emission from dust heated by stars is not always associated with young stars and that the IR emission from M51b is primarily powered by stars older than 5 Gyr.
Transient Spiral Arms from Far Out-of-equilibrium Gravitational Evolution
Authors: Benhaiem David , Joyce Michael , Sylos Labini Francesco 
Published: December 2017

Abstract
We describe how a simple class of out-of-equilibrium, rotating, and asymmetrical mass distributions evolve under their self-gravity to produce a quasi-planar spiral structure surrounding a virialized core, qualitatively resembling a spiral galaxy. The spiral structure is transient, but can survive tens of dynamical times, and further reproduces qualitatively noted features of spiral galaxies such as the predominance of trailing two-armed spirals and large pitch angles. As our models are highly idealized, a detailed comparison with observations is not appropriate, but generic features of the velocity distributions can be identified to be the potential observational signatures of such a mechanism. Indeed, the mechanism leads generically to a characteristic transition from predominantly rotational motion, in a region outside the core, to radial ballistic motion in the outermost parts. Such radial motions are excluded in our Galaxy up to 15 kpc, but could be detected at larger scales in the future by GAIA. We explore the apparent motions seen by external observers of the velocity distributions of our toy galaxies, and find that it is difficult to distinguish them from those of a rotating disk with sub-dominant radial motions at levels typically inferred from observations. These simple models illustrate the possibility that the observed apparent motions of spiral galaxies might be explained by non-trivial non-stationary mass and velocity distributions without invoking a dark matter halo or modification of Newtonian gravity. In this scenario the observed phenomenological relation between the centripetal and gravitational acceleration of the visible baryonic mass could have a simple explanation.
The Sleeping Monster: NuSTAR Observations of SGR 1806–20, 11 Years After the Giant Flare
Authors: Younes George , Baring Matthew G. , Kouveliotou Chryssa , Harding Alice , Donovan Sophia , Göğüş Ersin , Kaspi Victoria , Granot Jonathan 
Published: December 2017

Abstract
We report the analysis of five Nuclear Spectroscopic Telescope Array (NuSTAR) observations of SGR 1806−20 spread over a year from 2015 April to 2016 April, more than 11 years following its giant flare (GF) of 2004. The source spin frequency during the NuSTAR observations follows a linear trend with a frequency derivative

Hz s−1, implying a surface dipole equatorial magnetic field

G. Thus, SGR 1806−20 has finally returned to its historical minimum torque level measured between 1993 and 1998. The source showed strong timing noise for at least 12 years starting in 2000, with

increasing one order of magnitude between 2005 and 2011, following its 2004 major bursting episode and GF. SGR 1806−20 has not shown strong transient activity since 2009, and we do not find short bursts in the NuSTAR data. The pulse profile is complex with a pulsed fraction of

with no indication of energy dependence. The NuSTAR spectra are well fit with an absorbed blackbody,

, plus a power law,

. We find no evidence for variability among the five observations, indicating that SGR 1806−20 has reached a persistent and potentially its quiescent X-ray flux level after its 2004 major bursting episode. Extrapolating the NuSTAR model to lower energies, we find that the 0.5–10 keV flux decay follows an exponential form with a characteristic timescale

days. Interestingly, the NuSTAR flux in this energy range is a factor of ∼2 weaker than the long-term average measured between 1993 and 2003, a behavior also exhibited in SGR 1900+14. We discuss our findings in the context of the magnetar model.
Testing the Isotropic Universe Using the Gamma-Ray Burst Data of Fermi/GBM
Authors: Řípa Jakub , Shafieloo Arman 
Published: December 2017

Abstract
The sky distribution of gamma-ray bursts (GRBs) has been intensively studied by various groups for more than two decades. Most of these studies test the isotropy of GRBs based on their sky number density distribution. In this work, we propose an approach to test the isotropy of the universe through inspecting the isotropy of the properties of GRBs such as their duration, fluences, and peak fluxes at various energy bands and different timescales. We apply this method on the Fermi/Gamma-ray Burst Monitor (GBM) data sample containing 1591 GRBs. The most noticeable feature we found is near the Galactic coordinates

,

, and radius

. The inferred probability for the occurrence of such an anisotropic signal (in a random isotropic sample) is derived to be less than a percent in some of the tests while the other tests give results consistent with isotropy. These are based on the comparison of the results from the real data with the randomly shuffled data samples. Considering the large number of statistics we used in this work (some of which are correlated with each other), we can anticipate that the detected feature could be a result of statistical fluctuations. Moreover, we noticed a considerably low number of GRBs in this particular patch, which might be due to some instrumentation or observational effects that can consequently affect our statistics through some systematics. Further investigation is highly desirable in order to clarify this result, e.g., utilizing a larger future Fermi/GBM data sample as well as data samples of other GRB missions and also looking for possible systematics.
IN-SYNC. VII. Evidence for a Decreasing Spectroscopic Binary Fraction (from 1 to 100 Myr) within the IN-SYNC Sample
Authors: Jaehnig Karl , Bird Jonathan C. , Stassun Keivan G. , Rio Nicola Da , Tan Jonathan C. , Cotaar Michiel , Somers Garrett 
Published: December 2017

Abstract
We study the occurrence of spectroscopic binaries in young star-forming regions using the INfrared Spectroscopy of Young Nebulous Clusters (IN-SYNC) survey, carried out in SDSS-III with the APOGEE spectrograph. Multi-epoch observations of thousands of low-mass stars in Orion A, NGC 2264, NGC 1333, IC 348, and the Pleiades have been carried out, yielding H-band spectra with a nominal resolution of R = 22,500 for sources with H < 12 mag. Radial velocity precisions of ∼0.3

were achieved, which we use to identify radial velocity variations indicative of undetected companions. We use Monte Carlo simulations to assess the types of spectroscopic binaries to which we are sensitive, finding sensitivity to binaries with orbital periods

days, for stars with

and

< 100

. Using Bayesian inference, we find evidence for a decline in the spectroscopic binary fraction, by a factor of 3–4, from the age of our pre-main-sequence (PMS) sample to the Pleiades age . The significance of this decline is weakened if spot-induced radial-velocity jitter is strong in the sample, and is only marginally significant when comparing any one of the PMS clusters against the Pleiades. However, the same decline in both sense and magnitude is found for each of the five PMS clusters, and the decline reaches a statistical significance of greater than 95% confidence when considering the PMS clusters jointly. Our results suggest that dynamical processes disrupt the widest spectroscopic binaries (

days) as clusters age, indicating that this occurs early in the stars’ evolution, while they still reside within their nascent clusters.
The Extremely Luminous Quasar Survey in the SDSS Footprint. I. Infrared-based Candidate Selection
Authors: Schindler Jan-Torge , Fan Xiaohui , McGreer Ian D. , Yang Qian , Wu Jin , Jiang Linhua , Green Richard 
Published: December 2017

Abstract
Studies of the most luminous quasars at high redshift directly probe the evolution of the most massive black holes in the early universe and their connection to massive galaxy formation. However, extremely luminous quasars at high redshift are very rare objects. Only wide-area surveys have a chance to constrain their population. The Sloan Digital Sky Survey (SDSS) has so far provided the most widely adopted measurements of the quasar luminosity function at

. However, a careful re-examination of the SDSS quasar sample revealed that the SDSS quasar selection is in fact missing a significant fraction of

quasars at the brightest end. We identified the purely optical-color selection of SDSS, where quasars at these redshifts are strongly contaminated by late-type dwarfs, and the spectroscopic incompleteness of the SDSS footprint as the main reasons. Therefore, we designed the Extremely Luminous Quasar Survey (ELQS), based on a novel near-infrared JKW2 color cut using Wide-field Infrared Survey Explorer mission (WISE) AllWISE and 2MASS all-sky photometry, to yield high completeness for very bright (

) quasars in the redshift range of

. It effectively uses random forest machine-learning algorithms on SDSS and WISE photometry for quasar–star classification and photometric redshift estimation. The ELQS will spectroscopically follow-up ∼230 new quasar candidates in an area of ∼12,000 deg2 in the SDSS footprint to obtain a well-defined and complete quasar sample for an accurate measurement of the bright-end quasar luminosity function (QLF) at

. In this paper, we present the quasar selection algorithm and the quasar candidate catalog.
Ion–Ion Equilibration and Particle Distributions in a 3000 km s−1 Shock in SN 1006
Authors: Raymond J. C. , Winkler P. F. , Blair W. P. , Laming J. M. 
Published: December 2017

Abstract
SN 1006 is the most attractive target for investigating the physics of collisionless shock waves faster than 2000

. We obtained UV and optical spectra and an Hα image of a 3000

shock driven by a clump of ejecta that has overtaken the blast wave. It is 500 km s–1 faster than the filament studied earlier. We find kinetic temperatures of H, He, C, and N that are consistent with being mass proportional, suggesting little or no energy transfer among species. We also find evidence that the electron temperature is less than 10% of the proton temperature and that the velocity distribution of H atoms is non-Maxwellian. We measure a proper motion of 0.″34 ± 0.″01 yr−1 for the bow shock, which implies a distance to SN 1006 of 1.85 ± 0.25 kpc, and we discuss the role of plasma turbulence in determining the shape of the velocity distribution.
Copious Amounts of Dust and Gas in a z = 7.5 Quasar Host Galaxy
Authors: Venemans Bram P. , Walter Fabian , Decarli Roberto , Bañados Eduardo , Carilli Chris , Winters Jan Martin , Schuster Karl , da Cunha Elisabete , Fan Xiaohui , Farina Emanuele Paolo , Mazzucchelli Chiara , Rix Hans-Walter , Weiss Axel 
Published: December 2017

Abstract
We present IRAM/NOEMA and JVLA observations of the quasar J1342+0928 at z = 7.54 and report detections of copious amounts of dust and [C ii] emission in the interstellar medium (ISM) of its host galaxy. At this redshift, the age of the universe is 690 Myr, about 10% younger than the redshift of the previous quasar record holder. Yet, the ISM of this new quasar host galaxy is significantly enriched by metals, as evidenced by the detection of the [C ii] 158 μm cooling line and the underlying far-infrared (FIR) dust continuum emission. To the first order, the FIR properties of this quasar host are similar to those found at a slightly lower redshift (

), making this source by far the FIR-brightest galaxy known at

. The [C ii] emission is spatially unresolved, with an upper limit on the diameter of 7 kpc. Together with the measured FWHM of the [C ii] line, this yields a dynamical mass of the host of

. Using standard assumptions about the dust temperature and emissivity, the NOEMA measurements give a dust mass of

. The brightness of the [C ii] luminosity, together with the high dust mass, imply active ongoing star formation in the quasar host. Using [C ii]–SFR scaling relations, we derive star formation rates of 85–545

yr−1 in the host, consistent with the values derived from the dust continuum. Indeed, an episode of such past high star formation is needed to explain the presence of ∼108
M
☉ of dust implied by the observations.
Direct Measurement of Anisotropic and Asymmetric Wave Vector Spectrum in Ion-scale Solar Wind Turbulence
Authors: Roberts O. W. , Narita Y. , Escoubet C. P. 
Published: December 2017

Abstract
This analysis represents the first time that a simultaneous measurement of parallel and perpendicular spectral indices at both inertial and kinetic scales has been made directly in wave vector space, using a single interval of solar wind plasma. An interferometric wave vector analysis method is applied to four-point magnetometer data from the Cluster spacecraft to study for the first time the anisotropic and axially asymmetric energy spectrum directly in the three-dimensional wave vector space in the solar wind on spatial scales for the fluid picture (at about 6000 km) down to the ion kinetic regime (at about 400 km) without invoking Taylor’s frozen-in flow hypothesis. At fluid scales, the spectral index is found to transition from −2 along the large-scale magnetic field direction to a spectral index approaching −5/3 in the perpendicular direction. The wave number for the spectral break between ion inertial and kinetic scales occurs at larger scales in the parallel projection, compared to the perpendicular. At ion kinetic scales, the spectrum in the parallel direction is difficult to measure, while the two perpendicular directions are also anisotropic and vary between −8/3 and −11/3. This suggests that a single anisotropic process where symmetry is broken in a single direction cannot account for the results.
The First Detection of a Pulsar with ALMA
Authors: Mignani R. P. , Paladino R. , Rudak B. , Zajczyk A. , Corongiu A. , de Luca A. , Hummel W. , Possenti A. , Geppert U. , Burgay M. , Marconi G. 
Published: December 2017

Abstract
Although there is a general consensus on the fact that pulsars’ radio emission is coherent in nature, whereas the emission from the optical to high-energy γ-rays is due to incoherent processes, it has not been established yet at which wavelengths the transition occurs, which is key information for all emission models of pulsar magnetospheres. Of course, to address this issue, covering the spectral region between the GHz radio frequencies and the mid-infrared (IR) is crucial. We used the Atacama Large Millimeter/submillimeter Array (ALMA) to observe the Vela pulsar (PSR B0833−45), one of the very few observed in radio and from the mid-IR up to the very high-energy γ-rays. We detected Vela at frequencies of 97.5, 145, 233, and 343.5 GHz, which makes it the first pulsar ever detected with ALMA. Its energy density spectrum follows a power law of spectral index α = −0.93 ± 0.16. This corresponds to very high brightness temperatures—from 1017 to 1015 K—suggesting that a coherent radiative process still contributes to the millimeter/submillimeter emission. Therefore, this is the first indication of coherent emission in pulsars extending to the submillmeter range. At the same time, we identified an extended structure, preliminarily detected in ground-based near-IR observations, at a distance of ∼1.″4 from the pulsar, possibly interpreted as a counter-jet protruding from the pulsar.
Intermezzo. Des animaux friands d’histoires
Authors: Legrain Laurent 
Published: December 2017

Cet intermezzo synthétise les résultats d’une déambulation libre et heureuse dans des disciplines sœurs de l’anthropologie comme la psychologie du développement et la linguistique. Je m’attache à établir un fondement commun – et humain – à la menterie. C’est dans l’histoire du développement du langage que je trouve le fondement de cette compétence au mensonge ainsi que notre irrésistible tendance à nous laisser tromper.
Intermezzo. Hudal. De l’erreur aux tromperies en passant par l’art bien balancé de l’éternel brodeur
Authors: Legrain Laurent 
Published: December 2017

Dans cet intermezzo, j’analyse plusieurs des sens donnés au hudal mongol – souvent traduit par « mensonge ». Sous nos latitudes, les sens subsumés sous le hudal mongol portent des appellations variées : erreur, affabulation, fourberie, baratin, blague. Je place ces usages du langage en relation avec certaines formes d’organisations sociales.