bluuebunny/crossref_metadata_2025_split huggingface dataset:
WD 0141−675: a case study on how to follow-up astrometric planet candidates around white dwarfs
Authors: Rogers Laura K , Debes John , Anslow Richard J , Bonsor Amy , Casewell S L , Dos Santos Leonardo A , Dufour Patrick , T. Gänsicke Boris , Gentile Fusillo Nicola , Koester Detlev , Nielsen Louise Dyregaard , Penoyre Zephyr , Rickman Emily L , Sahlmann Johannes , Tremblay Pier-Emmanuel , Vanderburg Andrew , Xu Siyi , Dennihy Erik , Farihi Jay , Hermes J J , Hodgkin Simon , Kilic Mukremin , Kowalski Piotr M , Sanderson Hannah , Toonen Silvia 
Published: October 2023

ABSTRACT
This work combines spectroscopic and photometric data of the polluted white dwarf WD 0141−675, which has a now retracted astrometric super-Jupiter candidate, and investigates the most promising ways to confirm Gaia astrometric planetary candidates and obtain follow-up data. Obtaining precise radial velocity measurements for white dwarfs is challenging due to their intrinsic faint magnitudes, lack of spectral absorption lines, and broad spectral features. However, dedicated radial velocity campaigns are capable of confirming close-in giant exoplanets (a few MJup) around polluted white dwarfs, where additional metal lines aid radial velocity measurements. Infrared emission from these giant exoplanets is shown to be detectable with JWST Mid-Infrared Instrument (MIRI) and will provide constraints on the formation of the planet. Using the initial Gaia astrometric solution for WD 0141−675 as a case study, if there were a planet with a 33.65 d period or less with a nearly edge-on orbit, (1) ground-based radial velocity monitoring limits the mass to &lt;15.4 MJup, and (2) space-based infrared photometry shows a lack of infrared excess and in a cloud-free planetary cooling scenario, a substellar companion would have to be &lt;16 MJup and be older than 3.7 Gyr. These results demonstrate how radial velocities and infrared photometry can probe the mass of the objects producing some of the astrometric signals, and rule out parts of the brown dwarf and planet mass parameter space. Therefore, combining astrometric data with spectroscopic and photometric data is crucial to both confirm and characterize astrometric planet candidates around white dwarfs.
The Quasar Feedback Survey: characterizing CO excitation in quasar host galaxies
Authors: Molyneux S J , Calistro Rivera G , De Breuck C , Harrison C M , Mainieri V , Lundgren A , Kakkad D , Circosta C , Girdhar A , Costa T , Mullaney J R , Kharb P , Arrigoni Battaia F , Farina E P , Alexander D M , Ward S R , Silpa S , Smit R 
Published: October 2023

ABSTRACT
We present a comprehensive study of the molecular gas properties of 17 Type 2 quasars at z &lt; 0.2 from the Quasar Feedback Survey (L$_{\rm [O~{\small III}]}$ &gt; 1042.1 $\rm ergs^{-1}$), selected by their high [O iii] luminosities and displaying a large diversity of radio jet properties, but dominated by LIRG-like galaxies. With these data, we are able to investigate the impact of AGN and AGN feedback mechanisms on the global molecular interstellar medium. Using Atacama Pathfinder EXperiment and ALMA ACA observations, we measure the total molecular gas content using the CO(1-0) emission and homogeneously sample the carbon monoxide (CO) spectral line energy distributions, observing CO transitions (Jup = 1, 2, 3, 6, 7). We observe high r21 ratios (r21 = L’CO(2-1)/L’CO(1-0)) with a median r21 = 1.06, similar to local (U)LIRGs (with r21 ∼ 1) and higher than normal star-forming galaxies (with r21 ∼ 0.65). Despite the high r21 values, for the seven targets with the required data, we find low excitation in CO(6-5) & CO(7-6) (r61 and r62 &lt; 0.6 in all but one target), unlike high-redshift quasars in the literature, which are far more luminous and show higher line ratios. The ionized gas traced by [O iii] exhibits systematically higher velocities than the molecular gas traced by CO. We conclude that any effects of quasar feedback (e.g. via outflows and radio jets) do not have a significant instantaneous impact on the global molecular gas content and excitation and we suggest that it only occurs on more localized scales.
Isochrone fitting of Galactic globular clusters – V. NGC 6397 and NGC 6809 (M55)
Authors: Gontcharov George A , Bonatto Charles J , Ryutina Olga S , Savchenko Sergey S , Mosenkov Aleksandr V , Il’in Vladimir B , Khovritchev Maxim Yu , Marchuk Alexander A , Poliakov Denis M , Smirnov Anton A , Seguine Jonah 
Published: October 2023

ABSTRACT
We fit various colour–magnitude diagrams (CMDs) of the Galactic globular clusters NGC 6397 and NGC 6809 (M55) by isochrones from the Dartmouth Stellar Evolution Database (DSED) and Bag of Stellar Tracks and Isochrones (BaSTI) for α–enhanced [α/Fe] = +0.4. For the CMDs, we use data sets from Hubble Space Telescope, Gaia, Visible and Infrared Survey Telescope for Astronomy, and other sources utilizing 32 and 23 photometric filters for NGC 6397 and NGC 6809, respectively, from the ultraviolet to mid-infrared. We obtain the following characteristics for NGC 6397 and NGC 6809, respectively: metallicities [Fe/H] = −1.84 ± 0.02 ± 0.1 and −1.78 ± 0.02 ± 0.1 (statistic and systematic uncertainties); distances 2.45 ± 0.02 ± 0.06 and 5.24 ± 0.02 ± 0.18 kpc; ages 12.9 ± 0.1 ± 0.8 and 13.0 ± 0.1 ± 0.8 Gyr; reddenings E(B − V) = 0.178 ± 0.006 ± 0.01 and 0.118 ± 0.004 ± 0.01 mag; extinctions AV = 0.59 ± 0.01 ± 0.02 and 0.37 ± 0.01 ± 0.04 mag; and extinction-to-reddening ratio $R_\mathrm{V}=3.32^{+0.32}_{-0.28}$ and $3.16^{+0.66}_{-0.56}$. Our estimates agree with most estimates from the literature. BaSTI gives systematically higher [Fe/H] and lower reddenings than DSED. Despite nearly the same metallicity, age, and helium enrichment, these clusters show a considerable horizontal branch (HB) morphology difference, which must therefore be described by another parameter. This parameter must predominantly explain why the least massive HB stars (0.58–0.63 solar masses) are only found within NGC 6809. Probably they have been lost by the core-collapse cluster NGC 6397 during its dynamical evolution and mass segregation. In contrast, NGC 6809 has a very low central concentration and, hence, did not undergo this process.
The role of magma oceans in maintaining surface water on rocky planets orbiting M-dwarfs
Authors: Moore Keavin , Cowan Nicolas B , Boukaré Charles-Édouard 
Published: October 2023

ABSTRACT
Earth-like planets orbiting M-dwarf stars, M-Earths, are currently the best targets to search for signatures of life. Life as we know it requires water. The habitability of M-Earths is jeopardized by water loss to space: high flux from young M-dwarf stars can drive the loss of 3–20 Earth oceans from otherwise habitable planets. We develop a 0-D box model for Earth-mass terrestrial exoplanets, orbiting within the habitable zone, which tracks water loss to space and exchange between reservoirs during an early surface magma ocean phase and the longer deep-water cycling phase. A key feature is the duration of the surface magma ocean, assumed concurrent with the runaway greenhouse. This time-scale can discriminate between desiccated planets, planets with desiccated mantles but substantial surface water, and planets with significant water sequestered in the mantle. A longer-lived surface magma ocean helps M-Earths retain water: dissolution of water in the magma provides a barrier against significant loss to space during the earliest, most active stage of the host M-dwarf, depending on the water saturation limit of the magma. Although a short-lived basal magma ocean can be beneficial to surface habitability, a long-lived basal magma ocean may sequester significant water in the mantle at the detriment of surface habitability. We find that magma oceans and deep-water cycling can maintain or recover habitable surface conditions on Earth-like planets at the inner edge of the habitable zone around late M-dwarf stars – these planets would otherwise be desiccated if they form with less than ∼10 terrestrial oceans of water.
A multiwavelength study of Swift J0503.7-2819: a chimeric magnetic CV
Authors: Pradeep Kala G , Singh Kulinder Pal , Dewangan G C , Aydi Elias , Barrett P E , Buckley D A H , Girish V , Page K L , Potter S B , Schlegel E M 
Published: October 2023

ABSTRACT
We present multiwavelength temporal and spectral characteristics of a magnetic cataclysmic variable (MCV) Swift J0503.7-2819, using far ultraviolet and X-ray data from AstroSat, supplemented with optical data from the Southern African Large Telescope and X-ray data from the XMM-Newton and Swift observatories. The X-ray modulations at 4897.6657 s and 3932.0355 s are interpreted as the orbital (PΩ) and spin (Pω) period, respectively, and are consistent with prior reports. With a spin-orbit period ratio of 0.8 and PΩ falling below the period gap (2–3 h) of CVs, Swift J0503.7-2819 would be the newest addition to the growing population of nearly synchronous MCVs, which we call EX Hya-like systems. Hard X-ray luminosity of &lt;2.5 × 1032 erg s−1, as measured with the Swift Burst Alert Telescope, identifies it to be a low-luminosity intermediate polar, similar to other EX Hya-like systems. The phenomenology of the light curves and the spectral characteristics rule out a purely disc-fed/stream-fed model and instead reveal the presence of complex accretion structures around the white dwarf. We propose a ring-like accretion flow, akin to EX Hya, using period ratio, stability arguments, and observational features. An attempt is made to differentiate between the asynchronous polar/nearly synchronous intermediate polar nature of Swift J0503.7-2819. Further, we note that with the advent of sensitive surveys, a growing population of MCVs that exhibit characteristics of both polars and intermediate polars is beginning to be identified, likely forming a genealogical link between the two conventional classes of MCVs.
Collisional excitation of PO+ by para-H2: potential energy surface, scattering calculations, and astrophysical applications
Authors: Tonolo F , Bizzocchi L , Rivilla V M , Lique F , Melosso M , Puzzarini C 
Published: October 2023

ABSTRACT
We report the derivation of rate coefficients for the rotational (de-)excitation of PO+ induced by collisions with H2. The calculations were performed on a 4D potential energy surface, obtained on top of highly accurate ab initio energy points. Preliminary tests pointed out the low influence of the coupling between j = 0 and the higher rotational levels of H2 on the cross-sections values, thus allowing to neglect the rotational structure of H2. On this basis, state-to-state collisional rate coefficients were derived for temperatures ranging from 5 to 200 K. Radiative transfer calculations have been used to model the recent observation of PO+ in the G+0.693–0.027 molecular cloud, in order to evaluate the possible impact of non-LTE models on the determination of its physical conditions. The derived column density was found to be approximately ∼ 3.7 × 1011 cm−2, which is 60% (a factor of ∼ 1.7) smaller than the previously LTE-derived value. Extensive simulations show that PO+ low-j rotational lines exhibit maser behaviour at densities between 104 and 106 cm−3, thus highlighting the importance of a proper treatment of the molecular collisions to accurately model PO+ emissions in the interstellar medium.
An improved dynamical Poisson equation solver for self-gravity
Authors: Maeda Ryunosuke , Inoue Tsuyoshi , Inutsuka Shu-ichiro 
Published: October 2023

ABSTRACT
Since self-gravity is crucial in the structure formation of the Universe, many hydrodynamics simulations with the effect of self-gravity have been conducted. The multigrid method is widely used as a solver for the Poisson equation of the self-gravity; however, the parallelization efficiency of the multigrid method becomes worse when we use a massively parallel computer, and it becomes inefficient with more than 104 cores, even for highly tuned codes. To perform large-scale parallel simulations (&gt;104 cores), developing a new gravity solver with good parallelization efficiency is beneficial. In this article, we develop a new self-gravity solver using the telegraph equation with a damping coefficient, κ. Parallelization is much easier than the case of the elliptic Poisson equation since the telegraph equation is a hyperbolic partial differential equation. We analyse convergence tests of our telegraph equations solver and determine that the best non-dimensional damping coefficient of the telegraph equations is $\tilde{\kappa } \simeq 2.5$. We also show that our method can maintain high parallelization efficiency even for massively parallel computations due to the hyperbolic nature of the telegraphic equation by weak-scaling tests. If the time-step of the calculation is determined by heating/cooling or chemical reactions, rather than the Courant–Friedrichs–Lewy (CFL) condition, our method may provide the method for calculating self-gravity faster than other previously known methods such as the fast Fourier transform and multigrid iteration solvers because gravitational phase velocity determined by the CFL condition using these time-scales is much larger than the fluid velocity plus sound speed.
Posterior sampling of the initial conditions of the universe from non-linear large scale structures using score-based generative models
Authors: Legin Ronan , Ho Matthew , Lemos Pablo , Perreault-Levasseur Laurence , Ho Shirley , Hezaveh Yashar , Wandelt Benjamin 
Published: October 2023

ABSTRACT
Reconstructing the initial conditions of the universe is a key problem in cosmology. Methods based on simulating the forward evolution of the universe have provided a way to infer initial conditions consistent with present-day observations. However, due to the high complexity of the inference problem, these methods either fail to sample a distribution of possible initial density fields or require significant approximations in the simulation model to be tractable, potentially leading to biased results. In this work, we propose the use of score-based generative models to sample realizations of the early universe given present-day observations. We infer the initial density field of full high-resolution dark matter N-body simulations from the present-day density field and verify the quality of produced samples compared to the ground truth based on summary statistics. The proposed method is capable of providing plausible realizations of the early universe density field from the initial conditions posterior distribution marginalized over cosmological parameters and can sample orders of magnitude faster than current state-of-the-art methods.
Use, access, and initial outcomes of off-label ivosidenib in patients with IDH1 mutant glioma
Authors: Peters Katherine B , Alford Candice , Heltemes Amy , Savelli Alicia , Landi Daniel B , Broadwater Gloria , Desjardins Annick , Johnson Margaret O , Low Justin T , Khasraw Mustafa , Ashley David M , Friedman Henry S , Patel Mallika P 
Published: October 2023

Abstract

Background
Isocitrate dehydrogenase (IDH) is commonly mutated (mIDH) in gliomas, and this mutant enzyme produces the oncometabolite 2-hydroxyglutarate (2HG). 2HG promotes gliomagenesis and is implicated in epileptogenesis. Ivosidenib (IVO), a small molecule oral mIDH1 inhibitor, is FDA-approved for mIDH1 newly diagnosed and relapsed/refractory acute myeloid leukemia. Moreover, IVO has efficacy in clinical trials for recurrent mIDH1 gliomas. Given the lack of targeted treatments for gliomas, we initiated off-label IVO for mIDH glioma patients in October 2020.

Methods
Retrospectively, we sought to assess early outcomes in our patients and describe their experience on IVO from October 2020 through February 2022. Our objective was to report on the following variables of off-label use of IVO: radiographic response, seizure control, tolerability, and access to the medication. All patients initially received single-agent IVO dosed at 500 mg orally once daily.

Results
The cohort age range was 21–74 years. Tumor types included astrocytoma (n = 14) and oligodendroglioma (n = 16), with most being grade 2 (n = 21). The best radiographic response in nonenhancing disease (n = 22) was 12 stable diseases, 5 minor responses, 3 partial responses, and 2 progressive diseases. Seizure frequency was stable to improved for most patients (70%, n = 21). IVO was well-tolerated, with the most common toxicities being diarrhea, elevated creatine kinase, and QTc interval prolongation. Most patients (66.7%, n = 20) received drugs via the patient assistance program, with insurance initially covering a third of patients and with ongoing use, later covering 60%.

Conclusions
Targeted therapies like IVO are options for mIDH glioma patients and can provide positive oncologic and neurological outcomes.
A narrative review of clinic–community food provision interventions aimed at improving diabetes outcomes among food-insecure adults: examining the role of nutrition education
Authors: Schier Heather E , Chetty Krithika S , Garrity Katharine , Westrick Miranda , Copeland Kristen A , Miller Abigail , Gunther Carolyn 
Published: October 2023

Abstract

Background
Food provision interventions (eg, produce/food prescriptions, food pharmacies, food voucher programs) that bridge clinic and community settings for improved nutritional health outcomes of at-risk patients have gained momentum. Little is known about the role of nutrition education and potential augmented impact on patient outcomes.

Objective
To describe intervention designs and outcomes of direct food provision clinic–community programs aimed at improving diabetes-related outcomes (glycated hemoglobin [HbA1c] levels) among patients with type 2 diabetes (T2DM) or prediabetes and food insecurity, and to compare nutrition education components across interventions.

Methods
The PubMed and Academic Search Complete databases were systematically searched for original peer-reviewed articles (published during 2011–2022) that described the impact of clinic–community food provision programs (ie, produce/food prescriptions, food pharmacies, and food voucher programs) onHbA1c values among adults diagnosed with T2DM or prediabetes and who screened positive for food insecurity or low income. Study designs, intervention approaches, program implementation, and intervention outcomes were described.

Results
Ten studies representing 8 distinct programs were identified. There was a high degree of variation in the studies’ design, implementation, and evaluation. Across the 8 programs, 6 included nutrition education; of these, 1 used a theoretical framework, and 3 incorporated goal setting. Nutrition education covered multiple topical contents, including general nutrition knowledge, fruit and vegetable consumption, and accessing resources (eg, enrolling in the Supplemental Nutrition Assistance Program). Furthermore, the education was delivered through various formats (from 1-on-1 to group-based sessions), educators (community health workers, registered dietitians, physicians), and durations (from a single session to biweekly). All programs with a nutrition education component reported reduced participant HbA1c, and 4 demonstrated an increase in fruit and vegetable purchases or improved dietary quality. The remaining 2 programs that did not include nutrition education yielded mixed results.

Conclusion
The majority of programs included a nutrition education component; however, there was a high degree of heterogeneity in terms of content, educator, and duration. Patients who participated in programs that included nutrition education had consistent reductions in HbA1c. These observational trends warrant further exploration to conclusively determine the impact of nutrition education on patient outcomes participating in clinic–community food provision programs.
RNA/DNA ratios as estimate of metabolic and functional traits in diatom species from the northwestern Adriatic Sea
Authors: Casabianca Silvia , Capellacci Samuela , Ricci Fabio , Ravera Giorgia , Signa Geraldina , Scardi Michele , Penna Antonella 
Published: October 2023

Abstract
Different phytoplankton biomass estimations can provide information about abundance variation, but they are not able to describe the metabolic activity of species or groups within assemblages. Conversely, molecular traits are key for the metabolic dynamics in pelagic ecosystems. To investigate if the RNA/DNA and taxon-specific 18S ribosomal RNA (rRNA)/ribosomal DNA (rDNA) ratios could be used to assess and be indicators of metabolic activity in marine phytoplankton species, two Adriatic diatom species, Chaetoceros socialis and Skeletonema marinoi, were studied. Significant correlations between abundance, chlorophyll a, carbon content and proteins were found in individual and co-cultured growth experiments (from rs = 0.570 to rs = 0.986, P &lt; 0.001). The biomass trend followed a logistic curve without providing additional information regarding diatom metabolic activity. In both experiments, the RNA/DNA and taxon-specific 18S rRNA/rDNA ratios of C. socialis and S. marinoi showed maximum values at the beginning of the growth phase, i.e as 23.2 ± 1.5 and 15.3 ± 0.8, and 16.2 ± 1.6 and 30.1 ± 5.4 after 2 and 6 days, respectively, in individual cultures, with a subsequent significant decrease in these values for both species in individual and co-culture experiments. Our results showed that these molecular rRNA/rDNA ratios expressed an activation of metabolism before the abundance increases, even in the presence of interspecific interaction between C. socialis and S. marinoi.
Abundance and biomass of copepods and cladocerans in Atlantic and Arctic domains of the Barents Sea ecosystem
Authors: Skjoldal Hein Rune , Aarflot Johanna Myrseth 
Published: October 2023

Abstract
Zooplankton in the Barents Sea have been monitored annually with a standard procedure with determination of size-fractioned biomass since the mid-1980s. Biomass of copepods and cladocerans was estimated based on measured abundance and individual weights taken from literature. Calanus species were dominant, making up ~85% of the estimated biomass of copepods. The second most important taxon was Oithona spp. (~0.5 g dry weight (dw) m−2, ~10%), followed by Metridia spp. (~0.15 g dw m−2, 2–3%) and Pseudocalanus spp. (0.10–0.15 g dw m−2, 1–5%). Estimated biomass of cladoceran taxa (Evadne and Podon) was low (0.01 g dw m−2). Calanus spp. contributed most of the biomass of the medium size fraction (1–2 mm), whereas small copepod species (Oithona, Pseudocalanus and others) contributed to the small size fraction (&lt;1 mm). Estimated biomass of Calanus spp. and of the sum of small copepod species were both positively correlated with measured total zooplankton biomass (R2 = 0.72 and 0.34, respectively). The biomass ratio of small copepod species to Calanus was similar in Atlantic and Arctic water masses (~0.15–0.2) but tended to increase with decreasing total biomass. This suggests a shift to relatively larger roles of small copepods as Calanus and total biomass decrease.