bluuebunny/crossref_metadata_2025_split huggingface dataset:
Strategies to Increase Workforce Diversity in Pediatric Infectious Diseases
Authors: Rogo Tanya , Holland Sabina , Fassiotto Magali , Maldonado Yvonne , Joseph Tuhina , Ramilo Octavio , Byrd Katrina , Delair Shirley 
Published: December 2022

Abstract
The number of physicians who are underrepresented in medicine within the pediatric infectious diseases workforce remains disproportionate compared to the US population. Physician workforce diversity plays an important role in reducing health care disparities. Pathways to careers in pediatric infectious diseases require that a diverse pool of students enter medicine and subsequently choose pediatric residency followed by subspecialty training. Efforts must be made to expose learners to pediatric infectious diseases earlier in the education timeline. Along with recruitment and creation of pathways, cultures of inclusivity must be created and fostered within institutions of learning along the entire spectrum of medical training.
Morgagni hernia: an uncommon pathology in adults
Authors: Rajkumar Karnan , Kulkarni Sayali , Talishinskiy Toghrul 
Published: December 2022

Abstract
Typically, diaphragmatic hernias occur as congenital defects and are considered a rare presentation when seen in adults. They occur as developmental defects and stem from embryonic components of the diaphragm not fusing completely. There are two types of diaphragmatic hernias, classified based on the location of herniation through the diaphragmatic defect. Bochdalek hernias present as defects in the left postero-lateral diaphragm, whereas Morgagni hernias present as anterior defects of the diaphragm. The more common defect of the two are Bochdalek hernias making Morgagni hernias a rare presentation. This case describes the presentation of a hernia through an anterior defect in the diaphragm, otherwise classified as a Morgagni hernia.
Soundness and completeness results for LEA and probability semantics
Authors: Moore Eoin 
Published: December 2022

Abstract
In Artemov (2020, J. Logic Comput., 30, 61–76), a logical system called the logic of evidence aggregation (LEA) was introduced, along with an intended semantics for it called probability semantics. The goal was to describe probabilistic evidence aggregation in the setting of formal logic. However, as noted in that paper, LEA is not complete with respect to probability semantics. This leaves the tasks open to find sound and complete semantics for LEA and a proper axiomatization for probability semantics. In this paper, we do both. We define a class of basic models called deductive basic models. We show LEA is sound and complete with respect to the class of deductive basic models. We also define an axiomatic system LEA$_+$ extending LEA and show it is sound and complete with respect to probability semantics. Along the way, we develop an intermediate system LEA$_-$ which, it turns out, is equivalent to propositional lax logic with a classical logic base. Sequent systems and decidability results for LEA$_-$ and LEA$_+$ are also presented.
Detecting planetary mass companions near the water frost-line using JWST interferometry
Authors: Ray Shrishmoy , Hinkley Sasha , Sallum Steph , Bonavita Mariangela , Squicciarini Vito , Carter Aarynn L , Lazzoni Cecilia 
Published: December 2022

ABSTRACT
JWST promises to be the most versatile infrared observatory for the next two decades. The Near Infrared and Slitless Spectrograph (NIRISS) instrument, when used in the Aperture Masking Interferometry (AMI) mode, will provide an unparalleled combination of angular resolution and sensitivity compared to any existing observatory at mid-infrared wavelengths. Using simulated observations in conjunction with evolutionary models, we present the capability of this mode to image planetary mass companions around nearby stars at small orbital separations near the circumstellar water frost-line for members of the young, kinematic moving groups β Pictoris, TW Hydrae, as well as the Taurus–Auriga association. We show that for appropriately chosen stars, JWST/NIRISS operating in the AMI mode can image sub-Jupiter companions near the water frost-lines with ∼68 per cent confidence. Among these, M-type stars are the most promising. We also show that this JWST mode will improve the minimum inner working angle by as much as ∼50 per cent in most cases when compared to the survey results from the best ground-based exoplanet direct imaging facilities (e.g. VLT/SPHERE). We also discuss how the NIRISS/AMI mode will be especially powerful for the mid-infrared characterization of the numerous exoplanets expected to be revealed by Gaia. When combined with dynamical masses from Gaia, such measurements will provide a much more robust characterization of the initial entropies of these young planets, thereby placing powerful constraints on their early thermal histories.
An analysis of the effect of data processing methods on magnetic propeller models in short GRBs
Authors: Meredith Tomos R L , Wynn Graham A , Evans Philip A 
Published: December 2022

ABSTRACT
We present analysis of observational data from the Swift Burst Analyser for a sample of 15 short gamma-ray bursts with extended emission (SGRBEEs) which have been processed such that error propagation from Swift’s count-rate-to-flux conversion factor is applied to the flux measurements. We apply this propagation to data presented by the Burst Analyser at 0.3–10 keV and also at 15–50 keV, and identify clear differences in the morphologies of the light curves in the different bands. In performing this analysis with data presented at both 0.3–10 keV, at 15–50 keV, and also at a combination of both bands, we highlight the impact of extrapolating data from their native bandpasses on the light curve. We then test these data by fitting to them a magnetar-powered model for SGRBEEs, and show that while the model is consistent with the data in both bands, the model’s derived physical parameters are generally very loosely constrained when this error propagation is included and are inconsistent across the two bands. In this way, we highlight the importance of the Swift data processing methodology to the details of physical model fits to SGRBEEs.
First semi-empirical test of the white dwarf mass–radius relationship using a single white dwarf via astrometric microlensing
Authors: McGill Peter , Anderson Jay , Casertano Stefano , Sahu Kailash C , Bergeron Pierre , Blouin Simon , Dufour Patrick , Smith Leigh C , Evans N Wyn , Belokurov Vasily , Smart Richard L , Bellini Andrea , Calamida Annalisa , Dominik Martin , Kains Noé , Klüter Jonas , Nielsen Martin Bo , Wambsganss Joachim 
Published: December 2022

ABSTRACT
In November 2019, the nearby single, isolated DQ-type white dwarf LAWD 37 (WD 1142-645) aligned closely with a distant background source and caused an astrometric microlensing event. Leveraging astrometry from Gaia and followup data from the Hubble Space Telescope, we measure the astrometric deflection of the background source and obtain a gravitational mass for LAWD 37. The main challenge of this analysis is in extracting the lensing signal of the faint background source whilst it is buried in the wings of LAWD 37’s point spread function. Removal of LAWD 37’s point spread function induces a significant amount of correlated noise which we find can mimic the astrometric lensing signal. We find a deflection model, including correlated noise caused by the removal of LAWD 37’s point spread function best explains the data and yields a mass for LAWD 37 of $0.56\pm 0.08\, {\rm M}_{\odot }$. This mass is in agreement with the theoretical mass–radius relationship and cooling tracks expected for CO core white dwarfs. Furthermore, the mass is consistent with no or trace amounts of hydrogen that is expected for objects with helium-rich atmospheres like LAWD 37. We conclude that further astrometric followup data on the source is likely to improve the inference on LAWD 37’s mass at the ≈3 per cent level and definitively rule out purely correlated noise explanations of the data. This work provides the first semi-empirical test of the white dwarf mass–radius relationship using a single, isolated white dwarf and supports current model atmospheres of DQ white dwarfs and white dwarf evolutionary theory.
On the masses, age, and architecture of the VHS J1256−1257AB b system
Authors: Dupuy Trent J , Liu Michael C , Evans Elise L , Best William M J , Pearce Logan A , Sanghi Aniket , Phillips Mark W , Bardalez Gagliuffi Daniella C 
Published: December 2022

ABSTRACT
VHS J1256−1257 AB is an ultracool dwarf binary that hosts a wide-separation planetary-mass companion that is a key target of the JWST Exoplanet Early Release Science programme. Using Keck adaptive optics imaging and aperture masking interferometry, we have determined the host binary’s orbit (a = 1.96 ± 0.03 au, P = 7.31 ± 0.02 yr, e = 0.883 ± 0.003) and measured its dynamical total mass (0.141 ± 0.008 M⊙). This total mass is consistent with VHS J1256−1257 AB being a brown dwarf binary or pair of very low-mass stars. In addition, we measured the orbital motion of VHS J1256−1257 b with respect to the barycentre of VHS J1256−1257 AB, finding that the wide companion’s orbit is also eccentric ($e=0.68^{+0.11}_{-0.10}$), with a mutual inclination of 115○ ± 14○ with respect to the central binary. This orbital architecture is consistent with VHS J1256−1257 b attaining a significant mutual inclination through dynamical scattering and thereafter driving Kozai–Lidov cycles to pump the eccentricity of VHS J1256−1257 AB. We derive a cooling age of 140 ± 20 Myr for VHS J1256−1257 AB from low-mass stellar/substellar evolutionary models. At this age, the luminosity of VHS J1256−1257 b is consistent with both deuterium-inert and deuterium-fusing evolutionary tracks. We thus find a bimodal probability distribution for the mass of VHS J1256−1257 b, either 12.0 ± 0.1 MJup or 16 ± 1 MJup, from these models. Future spectroscopic data to measure isotopologues such as HDO and CH3D could break this degeneracy and provide a strong test of substellar models at the deuterium-fusion mass boundary.
The tracking tapered gridded estimator for the power spectrum from drift scan observations
Authors: Chatterjee Suman , Bharadwaj Somnath , Choudhuri Samir , Sethi Shiv , Patwa Akash Kumar 
Published: December 2022

ABSTRACT
Intensity mapping with the redshifted 21-cm line is an emerging tool in cosmology. Drift scan observations, where the antennas are fixed to the ground and the telescope’s pointing centre (PC) changes continuously on the sky due to earth’s rotation, provide broad sky coverage and sustained instrumental stability needed for 21-cm intensity mapping. Here, we present the Tracking Tapered Grided Estimator (TTGE) to quantify the power spectrum of the sky signal estimated directly from the visibilities measured in drift scan radio interferometric observations. The TTGE uses the data from the different PC to estimate the power spectrum of the signal from a small angular region located around a fixed tracking centre (TC). The size of this angular region is decided by a suitably chosen tapering window function that serves to reduce the foreground contamination from bright sources located at large angles from the TC. It is possible to cover the angular footprint of the drift scan observations using multiple TC, and combine the estimated power spectra to increase the signal-to-noise ratio. Here, we have validated the TTGE using simulations of $154 \, {\rm MHz}$ Murchison Wide-field Array drift scan observations. We show that the TTGE can recover the input model angular power spectrum Cℓ within $20 {{\ \rm per\ cent}}$ accuracy over the ℓ range 40 &lt; ℓ &lt; 700.
Ironing the folds: the phase space chevrons of a GSE-like merger as a dark matter subhalo detector
Authors: Davies Elliot Y , Vasiliev Eugene , Belokurov Vasily , Evans N Wyn , Dillamore Adam M 
Published: December 2022

ABSTRACT
Recent work uncovered features in the phase space of the Milky Way’s stellar halo which may be attributed to the last major merger. When stellar material from a satellite is accreted onto its host, it phase mixes and appears finely substructured in phase space. For a high-eccentricity merger, this substructure most clearly manifests as numerous wrapping chevrons in (vr, r) space, corresponding to stripes in (E, θr) space. We introduce the idea of using this substructure as an alternative subhalo detector to cold stellar streams. We simulate an N-body merger akin to the GSE and assess the impact of subhaloes on these chevrons. We examine how their deformation depends on the mass, pericentre, and number of subhaloes. To quantify the impact of perturbers in our simulations, we utilize the appearance of chevrons in (E, θr) space to introduce a new quantity – the ironing parameter. We show that: (1) a single flyby of a massive (∼1010 M⊙) subhalo with pericentre comparable to, or within, the shell’s apocentre smooths out the substructure, (2) a single flyby of a low mass (≲ 108 M⊙) has negligible effect, (3) multiple flybys of subhalos derived from a subhalo mass function between 107 and 1010 M⊙ cause significant damage if deep within the potential, (4) the effects of known perturbers (e.g. Sagittarius) should be detectable and offer constraints on their initial mass. The sensitivity to the populations of subhaloes suggests that we should be able to place an upper limit on the Milky Way’s subhalo mass function.
Forecast analysis on interacting dark energy models from future generation PICO and DESI missions
Authors: Joseph Albin , Saha Rajib 
Published: December 2022

ABSTRACT
The next-generation cosmic microwave background (CMB) satellite missions are expected to provide robust constraints on a wide range of cosmological parameters with unprecedented precision. But these constraints on the parameters could weaken if we do not attribute dark energy to a cosmological constant. The cosmological models involving interaction between dark energy and dark matter can give rise to comparable energy densities at the present epoch, thereby alleviating the so-called cosmic coincidence problem. In the present paper, we perform a forecast analysis to test the ability of the future generation high-sensitive CMB, and baryon acoustic oscillation (BAO) experiments to constrain phenomenological interacting dark energy models. We consider cosmic variance limited future CMB experiment Probe of Inflation and Cosmic Origins (PICO) along with BAO information from the Dark Energy Spectroscopic Instrument (DESI), to constrain the parameters of the interacting dark sector. Based on the stability of the cosmological perturbations, we consider two possibilities for the interaction scenario. We investigate the impact of both coupling constant and equation of state parameter of dark energy on CMB temperature power spectrum, matter power spectrum, and fσ8. We have used simulated temperature and polarization data from PICO within the multipole ranges (ℓ = 2–4000), and as expected, we do see PICO alone produces better constraints than Planck on the ΛCDM parameters. With the integration of PICO and DESI missions, we observe a significant improvement in the constraints on several cosmological parameters, especially the equation of state parameter of dark energy. However, we note that additional data are required to constrain a small positive coupling constant.
NGC 7538 IRS 2 in [Ne ii]: shell and cavity kinematics of a compact H ii region
Authors: Beilis Dan , Beck Sara , Lacy John 
Published: December 2022

ABSTRACT
NGC 7538 IRS 2 is a compact H ii region and recent star formation source, with a shell morphology, lying on the border of the visible H ii region NGC 7538. We present a spectral cube of the [Ne ii] 12.8 $\mu$m emission line obtained with the TEXES spectrometer on Gemini North with velocity resolution ∼4 km s−1 and angular resolution ∼0.3 arcsec. The kinematics of the data cube show ionized gas flowing along multiple cavity walls. We have simulated the kinematics and structure of IRS 2 with a model of superimposed cavities created by outflows from embedded stars in a cloud with density gradients. Most of the cavities, including the largest that dominates IRS 2 structure, are associated with B-type stars; the outflow of the bright ionizing O star binary IRS 2a/b is small in extent and lies in a high-density clump. The IRS 2 model shows that the behaviour of an H ii region is not a matter of only the most massive star present; cloud clumpiness and activity of lower mass stars may determine the structure and kinematics.
Semi-analytic forecasts for Roman – the beginning of a new era of deep-wide galaxy surveys
Authors: Yung L Y Aaron , Somerville Rachel S , Finkelstein Steven L , Behroozi Peter , Davé Romeel , Ferguson Henry C , Gardner Jonathan P , Popping Gergö , Malhotra Sangeeta , Papovich Casey , Rhoads James E , Bagley Micaela B , Hirschmann Michaela , Koekemoer Anton M 
Published: December 2022

ABSTRACT
The Nancy Grace Roman Space Telescope, NASA’s next flagship observatory, will redefine deep-field galaxy survey with a field of view two orders of magnitude larger than Hubble and an angular resolution of matching quality. These future deep-wide galaxy surveys necessitate new simulations to forecast their scientific output and to optimize survey strategies. In this work, we present five realizations of 2-deg2 light cones, containing a total of ≳25 million simulated galaxies with −16 ≳ MUV ≳ −25 spanning z ∼ 0 to 10. This data set enables a new set of experiments with the impacts of survey size on the derived galaxy formation and cosmological constraints. The intrinsic and observable galaxy properties are predicted using a well-established, physics-based semi-analytic modelling approach. We provide forecasts for number density, cosmic SFR, field-to-field variance, and angular two-point correlation functions, and demonstrate how the future wide-field surveys will be able to improve these measurements relative to current generation surveys. We also present a comparison between these light cones and others that have been constructed with empirical models. The mock light cones are designed to facilitate the exploration of multi-instrument synergies and connecting with current generation instruments and legacy surveys. In addition to Roman, we also provide photometry for a number of other instruments on upcoming facilities, including Euclid and Rubin, as well as the instruments, that are part of many legacy surveys. Full object catalogues and data tables for the results presented in this work are made available through a web-based, interactive portal.
Extending Ultra-Diffuse Galaxy abundances to Milky Way analogues
Authors: Karunakaran Ananthan , Zaritsky Dennis 
Published: December 2022

ABSTRACT
We extend the Ultra-Diffuse Galaxy (UDG) abundance relation, NUDG − M200, to lower halo mass hosts $(M_{200}\sim 10^{11.6-12.2}\, \mathrm{M}_{\odot })$. We select UDG satellites from published catalogues of dwarf satellite galaxies around Milky Way analogues, namely the Exploration of Local Volume Satellites (ELVES) survey, the Satellite Around Galactic Analogs (SAGA) survey, and a survey of Milky Way-like systems conducted using the Hyper-Suprime Cam. Of the 516 satellites around a total of 75 Milky Way-like hosts, we find that 41 satellites around 33 hosts satisfy the UDG criteria. The distributions of host halo masses peak around $M_{200}\sim 10^{12}\, \mathrm{M}_{\odot }$, independent of whether the host has a UDG satellite or not. We use literature UDG abundances and those derived here to trace the NUDG − M200 relation over three orders of magnitude down to $M_{200}=10^{11.6}\, \mathrm{M}_{\odot }$ and find the best-fitting linear relation of $N_{\mathrm{ UDG}} = (38\pm 5) (\frac{M_{200}}{10^{14}})^{0.89\,\,\pm ~ 0.04}$. This sub-linear slope is consistent with earlier studies of UDG abundances as well as abundance relations for brighter dwarf galaxies, excluding UDG-formation mechanisms that require high-density environments. However, we highlight the need for further homogeneous characterization of UDGs across a wide range of environments to properly understand the NUDG − M200 relation.
A single centre in-depth analysis of death with a functioning kidney graft and reasons for overall graft failure
Authors: Mayrdorfer Manuel , Liefeldt Lutz , Osmanodja Bilgin , Naik Marcel G , Schmidt Danilo , Duettmann Wiebke , Hammett Charlotte , Schrezenmeier Eva , Friedersdorff Frank , Wu Kaiyin , Halleck Fabian , Budde Klemens 
Published: December 2022

ABSTRACT

Background
High numbers of unknown classifications and inconsistent methodologies in previous studies make the interpretation of causes leading to graft loss difficult. In addition, data on a holistic view looking at both death with a functioning graft (DWFG) and death-censored graft failure (DCGF) are sparse.

Methods
In this single-centre study we included 1477 adult kidney transplants performed between 1997 and 2017, of which all 286 DWFGs until the end of observation were analysed and causes for death assigned. Additionally, the results were compared with the causes of 303 DCGFs of the same cohort to evaluate the impact of causes for overall graft loss.

Results
The most frequent causes for DWFG were cardiovascular disease (CVD) in 30.8%, malignancy in 28.3% and infections in 21%. Only 9.4% of reasons for DWFG were unknown. Sudden death occurred in 40% (35/88) of patients classified as DWFG due to CVD. Overall graft loss was related to the effect of immunosuppression in 36.2% [infection 20.9% (123/589), malignancy 15.3% (90/589)] and CVD in 22.4% (132/589). In 27.4% (161/589), graft failure was associated with underimmunosuppression (rejection). For infections (60 DWFG, 63 DCGF) and CVD (88 DWFG, 44 DCGF), a considerable overlap was observed between DWFG and DCGF. For patients &gt;70 years of age at transplantation, medical events accounted for 78% of overall graft losses and only 6.5% were associated with rejection.

Conclusions
DWFG and DCGF share more causes for graft loss than previously reported and sudden death plays an underestimated role in death with a functioning graft.
Evidence of differing staging strategies between adult and juvenile Semipalmated Sandpipers highlights the importance of small staging sites in Atlantic Canada
Authors: Linhart Rebeca C , Hamilton Diana J , Paquet Julie , Gratto-Trevor Cheri L 
Published: December 2022

AbstractSemipalmated Sandpipers (Calidris pusilla) are Arctic-breeding shorebirds that use staging sites in Atlantic Canada during their southbound migration to South America. The upper Bay of Fundy is recognized as a critical staging area, but hundreds of smaller sites outside the Bay of Fundy also host staging Semipalmated Sandpipers and have received comparatively little attention. Using the Motus Wildlife Tracking System, we tracked adult and juvenile Semipalmated Sandpipers and identified different staging strategies used by sandpipers tagged inside and outside the Bay of Fundy. Birds tagged in the Bay of Fundy remained there, while birds tagged along the Northumberland Strait, a tidal water body along the eastern coast of New Brunswick and northern Nova Scotia displayed multiple strategies. Most birds tagged along the Northumberland Strait used sites outside the Bay of Fundy exclusively, while a smaller proportion moved to the Bay of Fundy. Length of stay was shorter for birds using only sites outside the Bay of Fundy compared to birds using Bay sites or transferring between them. Choice of departure conditions also varied; birds using the Bay were more selective of specific wind conditions, favoring north and northwesterly winds. We found juvenile Semipalmated Sandpipers stayed 3 days longer in the region than adults and appeared to use a broader variety of sites. Our results highlight the importance of implementing conservation measures for smaller, lesser-known staging sites in Atlantic Canada, many of which are at an increased risk of loss and degradation due to climate change, coastal development, pollution, and human disturbance.