bluuebunny/crossref_metadata_2025_split huggingface dataset:
Distribution of Water Vapor in Molecular Clouds. II
Authors: Melnick Gary J. , Tolls Volker , Snell Ronald L. , Kaufman Michael J. , Bergin Edwin A. , Goicoechea Javier R. , Goldsmith Paul F. , González-Alfonso Eduardo , Hollenbach David J. , Lis Dariusz C. , Neufeld David A. 
Published: March 2020

Abstract
The depth-dependent abundance of both gas-phase and solid-state water within dense, quiescent, molecular clouds is important to both the cloud chemistry and gas cooling. Where water is in the gas phase, it is free to participate in the network of ion-neutral reactions that lead to a host of oxygen-bearing molecules, and its many ortho- and para-energy levels make it an effective coolant for gas temperatures greater than 20 K. Where water is abundant as ice on grain surfaces, and unavailable to cool the gas, significant amounts of oxygen are removed from the gas phase, suppressing the gas-phase chemical reactions that lead to a number of oxygen-bearing species, including O2. Models of far-UV (FUV)-illuminated clouds predict that the gas-phase water abundance peaks in the range

∼ 3 and 8 mag of the cloud surface, depending on the gas density and FUV field strength. Deeper within such clouds, water is predicted to exist mainly as ice on grain surfaces. More broadly, these models are used to analyze a variety of other regions, including outflow cavities associated with young stellar objects and the surface layers of protoplanetary disks. In this paper, we report the results of observational tests of FUV-illuminated cloud models toward the Orion Molecular Ridge and Cepheus B using data obtained from the Herschel Space Observatory and the Five College Radio Astronomy Observatory. Toward Orion, 2220 spatial positions were observed along the face-on Orion Ridge in the H2O 1

– 101 557 GHz and NH3
J, K = 1,0–0,0 572 GHz lines. Toward Cepheus B, two strip scans were made in the same lines across the edge-on ionization front. These new observations demonstrate that gas-phase water exists primarily within a few magnitudes of dense cloud surfaces, strengthening the conclusions of an earlier study based on a much smaller data set, and indirectly supports the prediction that water ice is quite abundant in dense clouds.
A Deep View into the Nucleus of the Sagittarius Dwarf Spheroidal Galaxy with MUSE. II. Kinematic Characterization of the Stellar Populations
Authors: Alfaro-Cuello M. , Kacharov N. , Neumayer N. , Bianchini P. , Mastrobuono-Battisti A. , Lützgendorf N. , Seth A. C. , Böker T. , Kamann S. , Leaman R. , Watkins L. L. , van de Ven G. 
Published: March 2020

Abstract
The Sagittarius dwarf spheroidal galaxy is in an advanced stage of disruption but still hosts its nuclear star cluster (NSC), M54, at its center. In this paper, we present a detailed kinematic characterization of the three stellar populations present in M54: young metal-rich (YMR); intermediate-age metal-rich (IMR); and old metal-poor (OMP), based on the spectra of ∼6500 individual M54 member stars extracted from a large Multi-Unit Spectroscopic Explorer (MUSE)/Very Large Telescope data set. We find that the OMP population is slightly flattened with a low amount of rotation (∼0.8 km s−1) and with a velocity dispersion that follows a Plummer profile. The YMR population displays a high amount of rotation (∼5 km s−1) and a high degree of flattening, with a lower and flat velocity dispersion profile. The IMR population shows a high but flat velocity dispersion profile, with some degree of rotation (∼2 km s−1). We complement our MUSE data with information from Gaia DR2 and confirm that the stars from the OMP and YMR populations are comoving in 3D space, suggesting that they are dynamically bound. While dynamical evolutionary effects (e.g., energy equipartition) are able to explain the differences in velocity dispersion between the stellar populations, the strong differences in rotation indicate different formation paths for the populations, as supported by an N-body simulation tailored to emulate the YMR–OMP system. This study provides additional evidence for the M54 formation scenario proposed in our previous work, where this NSC formed via GC accretion (OMP) and in situ formation from gas accretion in a rotationally supported disk (YMR).
Newly Improved Ionization Corrections for the Neutral Interstellar Medium: Enabling Accurate Abundance Determinations in Star-forming Galaxies throughout the Universe*
Authors: Hernandez Svea , Aloisi Alessandra , James Bethan L. , Ferland Gary J. , Fox Andrew J. , Tosi Monica , Tumlinson Jason 
Published: March 2020

Abstract
Studies measuring the chemical abundances of the neutral gas in star-forming galaxies (SFGs) require ionization correction factors (ICFs) to accurately measure their metal contents. In the work presented here, we calculate newly improved ICFs for a sample of SFGs. These new corrections include both the contaminating ionized gas along the line of sight (

) and unaccounted for higher ionization stages in the neutral gas (

). We make use of recently acquired spectroscopic observations taken with the Cosmic Origins Spectrograph on board Hubble to measure column densities for Fe ii and Fe iii. Using the Fe iii/Fe ii ratios as well as other physical properties (i.e., log[

], N(H i), T, and Z), we generate ad hoc photoionization models with CLOUDY to quantify the corrections required for each of the targets. We identify a luminosity threshold of log[

] ∼ 40.75 erg s−1 above which the

values for nitrogen are relatively higher (

−0.7) than those for the rest of the elements (

). This behavior indicates that, for the high UV luminosity objects, N ii is found in non-negligible quantities in the neutral gas, making these

corrections critical for determining the true abundances in the interstellar medium. In addition, we calculate ICFs from a uniform grid of models covering a wide range of physical properties typically observed in studies of SFGs and extragalactic H ii regions. We provide the community with tabulated ICF values for the neutral gas abundances measured from a variety of environments and applicable to chemical studies of the high-redshift universe.
The Evolving AGN Duty Cycle in Galaxies Since z ∼ 3 as Encoded in the X-Ray Luminosity Function
Authors: Delvecchio I. , Daddi E. , Aird J. , Mullaney J. R. , Bernhard E. , Grimmett L. P. , Carraro R. , Cimatti A. , Zamorani G. , Caplar N. , Vito F. , Elbaz D. , Rodighiero G. 
Published: March 2020

Abstract
We present a new modeling of the X-ray luminosity function (XLF) of active galactic nuclei (AGNs) out to z ∼ 3, dissecting the contributions of main-sequence (MS) and starburst (SB) galaxies. For each galaxy population, we convolved the observed galaxy stellar mass (M
⋆) function with a grid of M
⋆-independent Eddington ratio (λ
EDD) distributions, normalized via empirical black hole accretion rate (BHAR) to star formation rate (SFR) relations. Our simple approach yields an excellent agreement with the observed XLF since z ∼ 3. We find that the redshift evolution of the observed XLF can only be reproduced through an intrinsic flattening of the λ
EDD distribution and with a positive shift of the break λ*, consistent with an antihierarchical behavior. The AGN accretion history is predominantly made by massive (1010 < M
⋆ < 1011
M
⊙) MS galaxies, while SB-driven BH accretion, possibly associated with galaxy mergers, becomes dominant only in bright quasars, at log(L
X/erg s−1) > 44.36 + 1.28 × (1 + z). We infer that the probability of finding highly accreting (λ
EDD > 10%) AGNs significantly increases with redshift, from 0.4% (3.0%) at z = 0.5%–6.5% (15.3%) at z = 3 for MS (SB) galaxies, implying a longer AGN duty cycle in the early universe. Our results strongly favor a M
⋆-dependent ratio between BHAR and SFR, as BHAR/SFR ∝

, supporting a nonlinear BH buildup relative to the host. Finally, this framework opens potential questions on super-Eddington BH accretion and different λ
EDD prescriptions for understanding the cosmic BH mass assembly.
Radio Sources Associated with Optical Galaxies and Having Unresolved or Extended Morphologies (ROGUE). I. A Catalog of SDSS Galaxies with FIRST Core Identifications
Authors: Kozieł-Wierzbowska Dorota , Goyal Arti , Żywucka Natalia 
Published: March 2020

Abstract
We present the catalog of Radio sources associated with Optical Galaxies and having Unresolved or Extended morphologies I (ROGUE I), consisting of 32,616 spectroscopically selected galaxies. It is the largest handmade catalog of this kind, obtained by cross-matching galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 7 and radio sources from both the First Images of Radio Sky at Twenty Centimetre (FIRST) survey and the NRAO Very Large Array Sky Survey, without imposing a limit on the radio flux densities. The catalog provides a visual classification of radio and optical morphologies of galaxies presenting a FIRST core within 3″ of the optical position. The radio morphological classification is performed by examining the radio–optical overlays of linear sizes equal to 1 Mpc at the source distance, while the 120″ image snapshots from the SDSS database are used for optical classification. The results of our search are as follows: (i) single-component unresolved and elongated radio sources constitute the major group in the ROGUE I catalog (∼90%), and ∼8% exhibit extended morphologies; (ii) samples of 269, 730, and 115 Fanaroff–Riley (FR) type I, II, and hybrid galaxies, respectively, are presented; (iii) we report 55 newly discovered giant/possible giant, 16 double–double, 9 X-shaped, and 25 Z-shaped radio sources; (iv) on the optical front, most galaxies have elliptical morphologies (∼62%) while spirals form the second major category (∼17%) followed by distorted (∼12%) and lenticular (∼7%) morphologies; and (v) division between the FR I and the FR II sources in the radio–optical luminosity plane is blurred, in tune with recent studies.
Relativistic MR-MP Energy Levels for K-like Fe
Authors: Santana Juan A. , Ishikawa Yasuyuki , Beiersdorfer Peter 
Published: March 2020

Abstract
Relativistic Multi-Reference Møller-Plesset (MR-MP) many-body perturbation theory calculations are reported for the ground and excited states of Fe viii. Energies are provided for states coming from the configurations

(l = s, p, d, and f) with

, p ≤ 3, and q ≤ 1. The MR-MP results were compared with the recommended observed values in the CHIANTI-v8 database and with previous ab-initio calculations. The MR-MP calculations reproduce 90% of the available observed values within 3500 cm−1. The previous accurate ab-initio calculations reproduce only 50% of the observed values within 3500 cm−1. The electronic structure of Fe viii is very complex and our MR-MP results show that accurate calculations require the inclusion of not only 3s
2–3d
2, 3p
2–3d
2, and 3s3p–3d
2 promotions but also of all electron correlations via perturbation theory.
Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog
Authors: Kremer Kyle , Ye Claire S. , Rui Nicholas Z. , Weatherford Newlin C. , Chatterjee Sourav , Fragione Giacomo , Rodriguez Carl L. , Spera Mario , Rasio Frederic A. 
Published: March 2020

Abstract
We present a set of 148 independent N-body simulations of globular clusters (GCs) computed using the code CMC (Cluster Monte Carlo). At an age of ∼10–13 Gyr, the resulting models cover nearly the full range of cluster properties exhibited by the Milky Way GCs, including total mass, core and half-light radii, metallicity, and galactocentric distance. We use our models to investigate the role that stellar-mass black holes play in the process of core collapse. Furthermore, we study how dynamical interactions affect the formation and evolution of several important types of sources in GCs, including low-mass X-ray binaries, millisecond pulsars, blue stragglers, cataclysmic variables, Type Ia supernovae, calcium-rich transients, and merging compact binaries. While our focus here is on old, low-metallicity GCs, our CMC simulations follow the evolution of clusters over a Hubble time, and they include a wide range of metallicities (up to solar), so that our results can also be used to study younger and higher-metallicity star clusters. Finally, the output from these simulations is available for download at https://cmc.ciera.northwestern.edu/home/.
The Rapid Imaging Planetary Spectrograph: Observations of Mercury’s Sodium Exosphere in Twilight
Authors: Schmidt Carl A. , Baumgardner Jeffrey , Moore Luke , Bida Thomas A. , Swindle Ryan , Lierle Patrick 
Published: March 2020

Abstract
Ground-based observations of Mercury’s exosphere are intrinsically difficult due to its proximity to the Sun and must be made in daylight or during brief windows at twilight. While the dimmer twilight background is far preferred, high airmass seeing and haze through Earth’s atmosphere, windshake, and guiding all present formidable challenges toward spatially resolving the exosphere’s structure. This study explores how such effects can be mitigated using results from a new instrument for high cadence spectroscopy, the Rapid Imaging Planetary Spectrograph. While high cadence observations do not significantly improve upon the resolution floor imposed by atmospheric seeing, the method does mitigate obstacles such as telescope tracking inaccuracy, windshake, and flux calibration. Whereas daytime observing has been the predominant methodology in past exosphere studies, the twilight observations performed here easily resolve distinct brightness enhancements near 50°–60° latitude, just equatorward of magnetic cusp regions. The exosphere in these locations is diagnostic of space weather effects such as charged particle precipitation. The structure in the sodium exosphere generally appears both more extended and brighter over the southern cusp, which has a broader open magnetic field line region. However, a northern enhancement during one observation confirms that the exosphere responds dynamically to environmental drivers, presumably changes in the solar wind dynamic pressure and/or interplanetary magnetic field.
The Solar Wind Prevents Reaccretion of Debris after Mercury’s Giant Impact
Authors: Spalding Christopher , Adams Fred C. 
Published: March 2020

Abstract
The planet Mercury possesses an anomalously large iron core, and a correspondingly high bulk density. Numerous hypotheses have been proposed in order to explain such a large iron content. A long-standing idea holds that Mercury once possessed a larger silicate mantle that was removed by a giant impact early in the the solar system’s history. A central problem with this idea has been that material ejected from Mercury is typically reaccreted onto the planet after a short (∼Myr) timescale. Here, we show that the primordial solar wind would have provided sufficient drag upon ejected debris to remove them from Mercury-crossing trajectories before reimpacting the planet’s surface. Specifically, the young Sun likely possessed a stronger wind, fast rotation, and strong magnetic field. Depending upon the time of the giant impact, the ram pressure associated with this wind would push particles outward into the solar system, or inward toward the Sun, on sub-Myr timescales, depending upon the size of ejected debris. Accordingly, the giant impact hypothesis remains a viable pathway toward the removal of planetary mantles, both on Mercury and extrasolar planets, particularly those close to young stars with strong winds.
ISCHEMIC CONTRACTURE OF THE FOOT AND ANKLE: PRINCIPLES OF MANAGEMENT AND PREVENTION
Authors: Botte Michael J , Santi Mark D , Prestianni Cheryl A , Abrams Reid A 
Published: March 2020

ABSTRACT
A variety of clinical presentations can be encountered following compartment syndrome of the leg and foot Deformity and functional impairment in the foot and ankle secondary to ischemia are determined by: 1) which leg compartments have been affected and to what degree extrinsic flexor or extensor "overpuU" is exhibited, 2) degree of nerve injury sustained causing weakness or paralysis of extrinsic or intrinsic foot and ankle muscles, 3) which foot compartments have been affected and to what degree intrinsic "overpull" is exhibited, and 4) degree of sensory nerve injury leading to anesthesia, hypoesthesia, or hyperesthesia of the foot Nonoperative therapy attempts to obtain or preserve joint mobility, increase strength, and provide corrective bracing and accommodative foot wear. Operative management is undertaken for treatment of residual nerve compression or refractory problematic deformities. Established surgical protocols are performed in a stepwise fashion, and include: 1) release of residual or secondary nerve compression; 2) release of fixed contractures, using infarct excision, myotendinous lengthening, muscle recession, or tenotomy; 3) tendon transfers or arthrodesis to increase function; and 4) osteotomy or amputation for severe, non-salvageable deformities.
Comparison of a New, Filter-Free Stereopsis Test (BEST) With the Randot Stereotest in a Pediatric Cohort
Authors: Lagstein Oded , Hecht Idan , Anteby Irene 
Published: March 2020

Purpose:
To evaluate the Bernell Evaluation of Stereopsis Test (BEST) (Bernell Corporation, Mishawaka, IN), a new lenticular technology and filter-free test to measure stereopsis in children, and compare it to the Randot Stereotest (Randot) (Stereo Optical, Inc., Chicago, IL).

Methods:
This was a retrospective review of the medical records of children examined at the Center for Pediatric Ophthalmology at Hadassah-Hebrew University Medical Center from July to November 2018. All children were evaluated with the Randot and BEST in a random order.

Results:

The study included 100 children (53% female, 64% orthophoric) with a mean age of 8.52 ± 3.18 years (range: 3.3 to 17.8 years) and mean best corrected visual acuity of 0.178 ± 0.16 logMAR (range: 0 to 0.7 logMAR). The mean BEST stereoacuity was 1.772 ± 0.27 log seconds of arc (arcsec), whereas the mean Randot stereo-acuity was 1.778 ± 0.39 log arcsec (
P
= .835). The Bland– Altman analysis revealed an overall bias of 0.0073 log arcsec (95% confidence interval: 0.04219 to 0.05679 log arcsec), with limits of agreement of −0.4816 to 0.4962 log arcsec (0.3299 to 3.1347 arcsec). A significant proportional bias was noted because the difference between the tests was significantly larger in higher log arcsec values (
t
= 5.566,
P
< .001). Age, gender, strabismus, and visual acuity did not affect the differences between the stereoacuity tests (
P
> .05). Both tests were influenced by strabismus but not monocular amblyopia.

Conclusions:
BEST stereoacuity measurements were comparable to those of the Randot, with no significant difference in crude values, minimal bias, and narrow limits of agreement. A larger, clinically insignificant variability between tests was noted with lower stereoacuity values, because children achieved better scores with the BEST. The BEST may be a valuable tool in the arsenal of the ophthalmologist.

[
J Pediatr Ophthalmol Strabismus
. 2020;57(2):129–135.]
IRF8 Regulates Gram-Negative Bacteria–Mediated NLRP3 Inflammasome Activation and Cell Death
Authors: Karki Rajendra , Lee Ein , Sharma Bhesh R. , Banoth Balaji , Kanneganti Thirumala-Devi 
Published: March 2020

Abstract
Inflammasomes are intracellular signaling complexes that are assembled in response to a variety of pathogenic or physiologic stimuli to initiate inflammatory responses. Ubiquitously present LPS in Gram-negative bacteria induces NLRP3 inflammasome activation that requires caspase-11. We have recently demonstrated that IFN regulatory factor (IRF) 8 was dispensable for caspase-11–mediated NLRP3 inflammasome activation during LPS transfection; however, its role in Gram-negative bacteria–mediated NLRP3 inflammasome activation remains unknown. In this study, we found that IRF8 promotes NLRP3 inflammasome activation in murine bone marrow–derived macrophages (BMDMs) infected with Gram-negative bacteria such as Citrobacter rodentium, Escherichia coli, or Pseudomonas aeruginosa mutant strain ΔpopB. Moreover, BMDMs deficient in IRF8 showed substantially reduced caspase-11 activation and gasdermin D cleavage, which are required for NLRP3 inflammasome activation. Mechanistically, IRF8-mediated phosphorylation of IRF3 was required for Ifnb transcription, which in turn triggered the caspase-11–dependent NLRP3 inflammasome activation in the infected BMDMs. Overall, our findings suggest that IRF8 promotes NLRP3 inflammasome activation during infection with Gram-negative bacteria.
El animador como artista, el artista como animador. Una recapitulación
Authors: Cholodenko Alan 
Published: March 2020

<p>Alan Cholodenko (Nueva Jersey, 1940) no solo es uno de los teóricos más importantes de la animación, sino que ha hecho de la animación una forma de entender la vida. No hay arte sin ánima, sin deseo de insuflar vida; ni hay animación que no sea, en el fondo, ‘lifedeath’, vida/muerte, (re)animación. Con un pensamiento de corte postestructuralista, seguidor de sus mentores Jean Baudrillard y Jacques Derrida, Alan Cholodenko ha construido una sólida filosofía de la animación cuyo centro es el ‘aparato animático’ (‘the animatic apparatus’), un término esencial para comprender la revolución que implica las tecnologías de la imagen que vertebran la ciencia, la cultura y la sociedad actuales. En “El animador como artista, el artista como animador”, un artículo tan personal como penetrante, se expone el eje fundamental de su pensamiento en torno al dibujo como gesto seductor y deconstructivo.</p>
Explaining Economic Inequality Using the Film, The Queen of Versailles
Authors: Booker Teresa A. 
Published: March 2020

In introductory classes on race and ethnicity, terms like wealth, economic inequality, and SES (socio-economic status) often take center stage during one chapter or another. There are numerous text books on this subject. But, I've had more success explaining these terms by using different media. To illustrate such important themes to non-economics majors, I often show and discuss The Queen of Versailles, a 2012 documentary that depicts the Siegel family’s 2-year meteoric decent from wealth (being worth billions of dollars) to rags (being worth “only” tens of millions of dollars).
Intersectional Approaches to Teaching about Privileges
Authors: Siliman Shadia , Kearns Katherine 
Published: March 2020

The 'privilege walk' is a classroom activity at many colleges and universities deployed to create a visual, embodied, and concreterepresentation of students' earned and unearned social advantages. In this article, we engage in a systematic reflection to interpret the privilege walk through an intersectional lens, and we elaborate on our concerns around the use of the activity. We claim thatthe privilege walk ultimately cultivates a two-dimensional, rather than an intersectional, understanding of privilege and oppression. We then offer alternativeswhich adapt the core concept of the privilege walk activity, adding intersectionality to its structure and learning outcomes in order to challengestudents to recognize their positionalities. We describe our own privilege walk adaptations and we reflect on our observations of the outcomes as well as opportunities for further consideration. Through this reflection, we invite colleagues to a pedagogical and interdisciplinary conversation about their alternatives to the privilege walk.