bluuebunny/crossref_metadata_2025_split huggingface dataset:
Defining value in health care: a scoping review of the literature
Authors: Landon Susan n , Padikkala Jane , Horwitz Leora i 
Published: November 2021

Abstract

Background
As health-care spending rises internationally, policymakers have increasingly begun to look to improve health-care value. However, the precise definition of health-care value remains ambiguous.

Methods
We conducted a scoping review of the literature to understand how value has been defined in the context of health care. We searched PubMed, Embase, Google Scholar, PolicyFile and Scopus between February and March 2020 to identify articles eligible for inclusion. Publications that defined value (including high or low value) using an element of cost and an element of outcomes were included in this review. No restrictions were placed on the date of publication. Articles were limited to those published in English.

Results
Out of 1750 publications screened, 46 met inclusion criteria. Among the 46 included articles, 22 focused on overall value, 19 on low value and 5 on high value. We developed a framework to categorize definitions based on three core domains: components, perspective and scope. Differences across these three domains contributed to significant variations in definitions of value.

Conclusions
How value is defined has the potential to influence measurement and intervention strategies in meaningful ways. To effectively improve value in health-care systems, we must understand what is meant by value and the merits of different definitions.
Playing with Religion: Delight at the Border between Epistemological Worlds
Authors: Dunn Mary 
Published: November 2021

AbstractThis article builds on conversations that began here in the Journal of the American Academy of Religion in 2019 on Jonathan Z. Smith’s legacy to the study of religion. Specifically, in this article I take up and elaborate on Heather Blair’s tentative proposal for thinking about religious studies as a kind of play. Beginning with Blair and engaging with the work of Sam Gill, Tyler Roberts, Robert Orsi, and others, I put forward a strong argument for adopting a playful approach to the study of religion. A programmatic alternative to reading religion against the grain and between the lines, a ludic approach to religious studies enables the scholar to engage with religion in ways that fruitfully combine at least provisional commitment to its rules with ironic disavowal, inviting the scholar to play between the incommensurate epistemologies of enchanted religious worlds, on the one hand, and the disenchanted modern academy, on the other. It is here, I argue, in this frictive space between these mutually exclusive and logically incompatible positions that religious studies finds its niche (or should), trafficking—and delighting—in the creative insights generated by the oscillation between fit and no-fit.
Dark Energy Survey Year 3 results: galaxy–halo connection from galaxy–galaxy lensing
Authors: Zacharegkas G , Chang C , Prat J , Pandey S , Ferrero I , Blazek J , Jain B , Crocce M , DeRose J , Palmese A , Seitz S , Sheldon E , Hartley W G , Wechsler R H , Dodelson S , Fosalba P , Krause E , Park Y , Sánchez C , Alarcon A , Amon A , Bechtol K , Becker M R , Bernstein G M , Campos A , Carnero Rosell A , Carrasco Kind M , Cawthon R , Chen R , Choi A , Cordero J , Davis C , Diehl H T , Doux C , Drlica-Wagner A , Eckert K , Elvin-Poole J , Everett S , Ferté A , Gatti M , Giannini G , Gruen D , Gruendl R A , Harrison I , Herner K , Huff E M , Jarvis M , Kuropatkin N , Leget P-F , MacCrann N , McCullough J , Myles J , Navarro-Alsina A , Porredon A , Raveri M , Rollins R P , Roodman A , Ross A J , Rykoff E S , Secco L F , Sevilla-Noarbe I , Shin T , Troxel M A , Tutusaus I , Varga T N , Yanny B , Yin B , Zhang Y , Zuntz J , Abbott T M C , Aguena M , Allam S , Andrade-Oliveira F , Annis J , Bacon D , Bertin E , Brooks D , Burke D L , Carretero J , Castander F J , Costanzi M , da Costa L N , Pereira M E S , Desai S , Dietrich J P , Doel P , Evrard A E , Flaugher B , Frieman J , García-Bellido J , Gaztanaga E , Gschwend J , Gutierrez G , Hinton S R , Hollowood D L , Honscheid K , Hoyle B , James D J , Kuehn K , Lima M , Maia M A G , Marshall J L , Melchior P , Menanteau F , Miquel R , Muir J , Ogando R L C , Paz-Chinchón F , Pieres A , Sanchez E , Serrano S , Smith M , Suchyta E , Tarle G , Thomas D , To C , Wilkinson R D , (DES Collaboration)  
Published: November 2021

ABSTRACT
Galaxy–galaxy lensing is a powerful probe of the connection between galaxies and their host dark matter haloes, which is important both for galaxy evolution and cosmology. We extend the measurement and modelling of the galaxy–galaxy lensing signal in the recent Dark Energy Survey Year 3 cosmology analysis to the highly non-linear scales (∼100 kpc). This extension enables us to study the galaxy–halo connection via a Halo Occupation Distribution (HOD) framework for the two lens samples used in the cosmology analysis: a luminous red galaxy sample (redmagic) and a magnitude-limited galaxy sample (maglim). We find that redmagic (maglim) galaxies typically live in dark matter haloes of mass log10(Mh/M⊙) ≈ 13.7 which is roughly constant over redshift (13.3−13.5 depending on redshift). We constrain these masses to ${\sim}15{{\ \rm per\ cent}}$, approximately 1.5 times improvement over the previous work. We also constrain the linear galaxy bias more than five times better than what is inferred by the cosmological scales only. We find the satellite fraction for redmagic (maglim) to be ∼0.1−0.2 (0.1−0.3) with no clear trend in redshift. Our constraints on these halo properties are broadly consistent with other available estimates from previous work, large-scale constraints, and simulations. The framework built in this paper will be used for future HOD studies with other galaxy samples and extensions for cosmological analyses.
Gaia EDR3 bright star parallax zero-point using stellar clusters
Authors: Flynn C , Sekhri R , Venville T , Dixon M , Duffy A , Mould J , Taylor E N 
Published: November 2021

ABSTRACT
We examine the zero-point of parallaxes in the Gaia EDR3 (Early Data Release 3, Gaia Collaboration (2021a)), using stars in open and globular clusters. Our aim is to check for zero-point systematics between bright stars G &lt; 12 (which includes some important distance scale calibrators) and faint stars G &gt; 14, for which the parallax scale has been very well tied to the extragalactic frame using active galactic nuclei and quasars (AGN/QSOs) observed by Gaia (Lindegren et al. 2021). Cluster stars are distinguished from field stars using conservative spatial and proper motion cuts. The median parallax cluster stars fainter the G = 14 are compared with the parallaxes of bright stars (G &lt; 14) to search for zero-point systematics. We confirm that the Lindegren et al. (2021) parallax corrections bring cluster stars into very good agreement over a wide range of magnitude and colour. We find small residual colour-dependent offsets for the bright stars (G &lt; 11). Specifically, we find a median parallax offset of $\approx 10\, \mu$as between the reddest stars (BP − RP &gt; 1) compared to those stars with colours similar to the AGN/QSOs (0.5 &lt; BP − RP &lt; 1) that serve as the primary zero-point calibrators for EDR3. These findings are similar to those found in other recent independent checks of the zero-point scale, and have significant implications for calibrating the extragalactic distance scale to stars in the Milky Way.
Evolution towards energy equipartition in star clusters: effects of the tidal field, primordial binaries, and internal velocity anisotropy
Authors: Pavlík Václav , Vesperini Enrico 
Published: November 2021

ABSTRACT
This paper is the second in a series investigating the evolution of star clusters towards energy equipartition (EEP). Here, we focus on the effects of the external tidal field of the host galaxy, initial anisotropy in the velocity distribution, and primordial binary star population. The results of our N-body simulations show that regardless of the strength of the tidal field or the fraction of primordial binaries: (i) the evolution towards EEP in the intermediate and outer regions of initially anisotropic systems is more rapid than for isotropic systems; (ii) this evolution also proceeds at different rates for the tangential and radial components of the velocity dispersion; and (iii) the outer regions of the initially isotropic systems show a tendency to evolve towards a state of ‘inverted’ EEP in which low-mass stars have smaller velocity dispersion than high-mass stars. We also find that the clusters with primordial binaries stay even farther from EEP than systems containing only single stars. Finally, we show that all these results also hold when the degree of EEP is calculated using quantities measured in projection as it is done in observational studies, and that our findings could be tested with current and upcoming observational data.
Hiding in plain sight: observing planet-starspot crossings with the James Webb Space Telescope
Authors: Bruno Giovanni , Lewis Nikole K , Valenti Jeff A , Pagano Isabella , Wilson Tom J , Schlawin Everett , Lothringer Joshua , Lanza Antonino F , Fraine Jonathan , Scandariato Gaetano , Micela Giuseppina , Cracchiolo Gianluca 
Published: November 2021

ABSTRACT
Transiting exoplanets orbiting active stars frequently occult starspots and faculae on the visible stellar disc. Such occultations are often rejected from spectrophotometric transits, as it is assumed they do not contain relevant information for the study of exoplanet atmospheres. However, they can provide useful constraints to retrieve the temperature of active features and their effect on transmission spectra. We analyse the capabilities of the James Webb Space Telescope in the determination of the spectra of occulted starspots, despite its lack of optical wavelength instruments on board. Focusing on K and M spectral types, we simulate starspots with different temperatures and in different locations of the stellar disc, and find that starspot temperatures can be determined to within a few hundred kelvins using NIRSpec/Prism and the proposed NIRCam/F150W2+F322W2’s broad wavelength capabilities. Our results are particularly promising in the case of K and M dwarfs of mag$_K \lesssim 12.5$ with large temperature contrasts.
Optimal 1D Ly α forest power spectrum estimation – II. KODIAQ, SQUAD, and XQ-100
Authors: Karaçaylı Naim Göksel , Padmanabhan Nikhil , Font-Ribera Andreu , Iršič Vid , Walther Michael , Brooks David , Gaztañaga Enrique , Kehoe Robert , Levi Michael , Ntelis Pierros , Palanque-Delabrouille Nathalie , Tarlé Gregory 
Published: November 2021

ABSTRACT
We measure the 1D Ly α power spectrum P1D from Keck Observatory Database of Ionized Absorption toward Quasars (KODIAQ), The Spectral Quasar Absorption Database (SQUAD), and XQ-100 quasars using the optimal quadratic estimator. We combine KODIAQ and SQUAD at the spectrum level, but perform a separate XQ-100 estimation to control its large resolution corrections in check. Our final analysis measures P1D at scales k &lt; 0.1 s km−1 between redshifts $z$ = 2.0–4.6 using 538 quasars. This sample provides the largest number of high-resolution, high-S/N observations; and combined with the power of optimal estimator it provides exceptional precision at small scales. These small-scale modes (k ≳ 0.02 s km−1), unavailable in Sloan Digital Sky Survey and Dark Energy Spectroscopic Instrument analyses, are sensitive to the thermal state and reionization history of the intergalactic medium, as well as the nature of dark matter. As an example, a simple Fisher forecast analysis estimates that our results can improve small-scale cut-off sensitivity by more than a factor of 2.
The role of thermal and non-thermal processes in the ISM of the Magellanic Clouds
Authors: Hassani H , Tabatabaei F , Hughes A , Chastenet J , McLeod A F , Schinnerer E , Nasiri S 
Published: November 2021

ABSTRACT
Radio continuum emission is a dust-unbiased tracer of both thermal and non-thermal processes in the interstellar medium. We present new maps of the free–free and synchrotron emission in the Magellanic Clouds (MCs) at 0.166, 1.4, and 4.8 GHz with no prior assumption about the radio non-thermal spectrum. The maps were constructed using a de-reddened H α map as a template for the thermal radio emission, which we subtract from maps of the total radio continuum emission. To de-redden the H α emission, it is important to know the fraction of dust surface density that attenuates the H α emission along the line of sight, fd. This fraction is obtained by comparing the dust opacity obtained through the infrared emission spectrum and the Balmer decrement method. In star-forming regions, the median fd is about 0.1, which is lower than that in diffuse regions by a factor of three. We obtain a global thermal radio fraction, fth, of 30 per cent (35 per cent) in the LMC (SMC) at 1.4 GHz. Furthermore, we present maps of the equipartition magnetic field strength with average values of $\simeq \, 10.1\, \mu$G in the LMC and $\simeq \, 5.5\, \mu$G in the SMC. The magnetic field is proportional to the star-formation rate to the power of 0.24 and 0.20 for the LMC and SMC, respectively. This study shows that non-thermal processes control the interstellar medium in the MCs.
Are blazars above the blazar sequence a significant source of IceCube neutrinos?
Authors: Savard Katherine , Ruan John J , Haggard Daryl 
Published: November 2021

ABSTRACT
The recent association of two flaring blazars (TXS 0506+056 and 3HSP J095507.9+355101) with IceCube neutrinos strongly suggests that blazars are at least one source of high-energy neutrinos. A peculiar characteristic of these two blazars is that they both appear to lie above the well-known blazar sequence, and they move further above the blazar sequence during the neutrino emission. Although the reason for this peculiarity is unclear, it may indicate a link between blazar SED properties and neutrino emission. Here, we test whether blazars lying above the blazar sequence are overrepresented in IceCube neutrino error regions. We spatially cross-match IceCube error regions with a sample of γ-ray blazars from the Fermi-LAT 4LAC catalogue, as a function of the blazars’ distance in synchrotron peak frequency above the blazar sequence. We do not find a statistically significant excess of counterparts, and thus conclude that the current data cannot confirm that the sources above the blazar sequence are a significant source of IceCube neutrinos. However, we show that the inclusion of more recently detected IceCube events increases the likelihood of an excess of blazars above the blazar sequence, and suggest that this excess may reach statistical significance in the future as the sample of IceCube neutrino detections increases.
Uncertainty-aware learning for improvements in image quality of the Canada–France–Hawaii Telescope
Authors: Gilda Sankalp , Draper Stark C , Fabbro Sébastien , Mahoney William , Prunet Simon , Withington Kanoa , Wilson Matthew , Ting Yuan-Sen , Sheinis Andrew 
Published: November 2021

ABSTRACTWe leverage state-of-the-art machine learning methods and a decade’s worth of archival data from Canada–France–Hawaii Telescope (CFHT) to predict observatory image quality (IQ) from environmental conditions and observatory operating parameters. Specifically, we develop accurate and interpretable models of the complex dependence between data features and observed IQ for CFHT’s wide-field camera, MegaCam. Our contributions are several-fold. First, we collect, collate, and reprocess several disparate data sets gathered by CFHT scientists. Second, we predict probability distribution functions of IQ and achieve a mean absolute error of ∼0.07 arcsec for the predicted medians. Third, we explore the data-driven actuation of the 12 dome ‘vents’ installed in 2013–14 to accelerate the flushing of hot air from the dome. We leverage epistemic and aleatoric uncertainties in conjunction with probabilistic generative modelling to identify candidate vent adjustments that are in-distribution (ID); for the optimal configuration for each ID sample, we predict the reduction in required observing time to achieve a fixed signal-to-noise ratio. On average, the reduction is $\sim 12{{\ \rm per\ cent}}$. Finally, we rank input features by their Shapley values to identify the most predictive variables for each observation. Our long-term goal is to construct reliable and real-time models that can forecast optimal observatory operating parameters to optimize IQ. We can then feed such forecasts into scheduling protocols and predictive maintenance routines. We anticipate that such approaches will become standard in automating observatory operations and maintenance by the time CFHT’s successor, the Maunakea Spectroscopic Explorer, is installed in the next decade.
The mean free path approximation and stellar collisions in star clusters: numerical exploration of the analytic rates and the role of perturbations on binary star mergers
Authors: Reinoso Bastián , Leigh Nathan W C , Barrera-Retamal Carlos M , Schleicher Dominik , Klessen Ralf S , Stutz Amelia M 
Published: November 2021

ABSTRACTIn this paper, we compute predictions for the number of stellar collisions derived from analytic models based on the mean free path (MFP) approximation and compare them to the results of N-body simulations. Our goal is to identify the cluster conditions under which the MFP approximation remains valid. Adopting a range of particle numbers (100 ≤ N ≤ 5000) and different combinations of particle masses and radii, we explore three different channels leading to stellar collisions, all of which are expected to occur in realistic stellar environments. At high densities, binaries form from isolated three-body interactions of single stars. Hence, we consider collisions between single stars and collisions involving binary stars, after they form in our simulations. For the latter, we consider two channels for mergers, namely direct stellar collisions during chaotic single–binary interactions and perturbation-driven mergers of binaries due to random walks in eccentricity approaching unity. In the densest systems considered here, a very massive object is formed at the cluster centre, causing local stellar orbits to become increasingly Keplerian and the assumptions going into our analytic model to break down. Before reaching this limit, we obtain excellent agreement between our theoretical predictions and the simulations: The analytic rates are typically accurate to within one standard deviation for the entire parameter space considered here, but the agreement is best for short integration times. Our results have direct implications for blue straggler formation in dense star clusters, and stellar mergers in galactic nuclei hosting massive black holes.
Probing Transit Timing Variations of three hot Jupiters: HATP-36b, HATP-56b, and WASP-52b
Authors: Sonbas E , Karaman N , Özdönmez A , Er H , Dhuga K S , Göğüş E , Nasiroglu I , Zejmo M 
Published: November 2021

ABSTRACT
We report the results of new transit observations for the three hot Jupiter-like planets, HATP-36b, HATP-56b, and WASP-52b, respectively. Transit timing variations (TTVs) are presented for these systems based on observations that span the period 2016–2020. The data were collected with the 0.6-m telescope at Adiyaman University (ADYU60, Turkey) and the 1.0 m telescope at TÜBİTAK National Observatory (TUG, Turkey). Global fits were performed to the combined light curves for each system along with the corresponding radial velocity (RV) data taken from the literature. The extracted parameters (for all three systems) are found to be consistent with the values from previous studies. Through fits to the combined mid-transit times data from our observations and the data available in the literature, an updated linear ephemeris is obtained for each system. Although a number of potential outliers are noted in the respective O-C diagrams, the majority of the data are consistent within the 3σ confidence level implying a lack of convincing evidence for the existence of additional objects in the systems studied.
Spectroscopy of an extreme [O iii] emitting active galactic nucleus at
z
= 3.212: implications for the reionization era
Authors: Tang Mengtao , Stark Daniel P , Ellis Richard S , Charlot Stéphane , Feltre Anna , Shapley Alice E , Endsley Ryan 
Published: November 2021

ABSTRACT
Reionization-era galaxies often display intense nebular emission lines, both in rest-frame optical ([O iii] + H β) and ultraviolet (UV; C iii], C iv). How such strong nebular emission is powered remains unclear, with both active galactic nuclei (AGNs) and hot stars considered equally viable. The UV continuum slopes of these early systems tend to be very blue (β &lt; −2), reflecting minimal dust obscuration, young ages, and low metallicities. This contrasts with narrow-lined AGNs at $z$ ∼ 2−3, whose UV slopes are significantly redder (β &gt; −1) than typical star-forming systems in the reionization era. To investigate the properties of AGNs in the reionization era, we have conducted a search for potential examples of rare analogues with blue continua at intermediate redshift ($z$ ∼ 2−3). Our goals are to determine whether AGNs with intense line emission and blue continua exist and thereby to establish the range of rest-frame UV and optical line ratios in this population. In this paper, we report the detection of an X-ray luminous AGN at $z$ = 3.21 (UDS-24561) with extreme [O iii] + H β line emission (equivalent width = 1300 Å) and a blue UV continuum slope (β = −2.34). MMT/Binospec and Keck/MOSFIRE spectra indicate rest-frame UV line ratios consistent with AGN photoionization models and rest-frame optical lines with both a narrow component [full width at half-maximum (FWHM) $=154\, {\rm km\, s}^{-1}$] and extended broad wings (FWHM $=977\, {\rm km\, s}^{-1}$), consistent with outflowing gas. We describe how such objects can be identified in future James Webb Space Telescope emission line surveys in the reionization era, thereby providing a valuable census of AGN activity at $z$ &gt; 6 and understanding their contribution to cosmic reionization.