bluuebunny/crossref_metadata_2025_split huggingface dataset:
Mass transfer and tidally tilted pulsation in the Algol-type system TZ Dra
Authors: Kahraman Aliçavuş F , Handler G , Aliçavuş F , De Cat P , Bedding T R , Lampens P , Ekinci Ö , Gümüș D , Leone F 
Published: December 2021

ABSTRACT
Oscillating eclipsing Algols (oEAs) are remarkable systems that allow us to determine accurate fundamental stellar parameters (mass, radius) and probe the stellar interiors through pulsations. TZ Dra is an oEA system containing a δ Scuti component. To examine particular characteristics of such close systems including pulsations and mass transfer, we present a detailed photometric and spectroscopic study of TZ Dra. With the analysis of high-resolution spectra, the orbital parameters were determined by the radial velocity analysis and the atmospheric parameters were derived for the primary component. The binary modelling and the pulsational frequency analysis was carried out using the Transiting Exoplanet Survey Satellite data set. The H α line profiles show the signature of mass transfer from the cool to the hot binary component. The conclusion of mass transfer/mass-loss in the system was supported by the analysis of the orbital period changes. As a result, it was found that there is $3.52 \times 10^{-9}\, {\rm M}_\odot$ yr−1 mass-loss from the system most probably through the hotspot and stellar winds. Additionally, most pulsation frequencies originating from the primary component were found to be spaced by harmonics of the orbital frequencies in particular, 12 doublets spaced by 2forb were detected from which we infer that this star is a tidally tilted pulsator. A mean p-mode frequency spacing of ≈7.2 d−1 was found as well.
What is the halo mass function in a fuzzy dark matter cosmology?
Authors: Kulkarni Mihir , Ostriker Jeremiah P 
Published: December 2021

ABSTRACT
Fuzzy dark matter (FDM) or wave dark matter is an alternative theory designed to solve the small-scale problems faced by the standard cold dark matter proposal for the primary material component of the Universe. It is made up of ultra-light axions having mass $\sim 10^{-22}\, {\rm eV}$ that typically have de Broglie wavelength of several kpc, alleviating some of the apparent small-scale discrepancies faced by the standard ΛCDM paradigm. In this paper, we calculate the halo mass function for the FDM using a sharp-k window function and compare it with one calculated using numerical simulations, finding the peak mass at roughly $10^{10}\, {M_{\odot }}$ for a particle mass of $2\times 10^{-22}\, {\rm eV}$. We also constrain the mass of FDM particle to be $^{\gtrsim}_{\sim} 2\times 10^{-22}\, {\rm eV}$ using the observations of high-redshift (z ∼ 10) lensed galaxies from CLASH survey.
WALLABY pilot survey: H i gas disc truncation and star formation of galaxies falling into the Hydra I cluster
Authors: Reynolds T N , Catinella B , Cortese L , Westmeier T , Meurer G R , Shao L , Obreschkow D , Román J , Verdes-Montenegro L , Deg N , Dénes H , For B-Q , Kleiner D , Koribalski B S , Lee-Waddell K , Murugeshan C , Oh S-H , Rhee J , Spekkens K , Staveley-Smith L , Stevens A R H , van der Hulst J M , Wang J , Wong O I , Holwerda B W , Bosma A , Madrid J P , Bekki K 
Published: December 2021

ABSTRACT
We present results from our analysis of the Hydra I cluster observed in neutral atomic hydrogen (H i) as part of the Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY). These WALLABY observations cover a 60-square-degree field of view with uniform sensitivity and a spatial resolution of 30 arcsec. We use these wide-field observations to investigate the effect of galaxy environment on H i gas removal and star formation quenching by comparing the properties of cluster, infall, and field galaxies extending up to ∼5R200 from the cluster centre. We find a sharp decrease in the H i-detected fraction of infalling galaxies at a projected distance of ∼1.5R200 from the cluster centre from $\sim 85{{\ \rm per\ cent}}$ to $\sim 35{{\ \rm per\ cent}}$. We see evidence for the environment removing gas from the outskirts of H i-detected cluster and infall galaxies through the decrease in the H i to r-band optical disc diameter ratio. These galaxies lie on the star-forming main sequence, indicating that gas removal is not yet affecting the inner star-forming discs and is limited to the galaxy outskirts. Although we do not detect galaxies undergoing galaxy-wide quenching, we do observe a reduction in recent star formation in the outer disc of cluster galaxies, which is likely due to the smaller gas reservoirs present beyond the optical radius in these galaxies. Stacking of H i non-detections with H i masses below $M_{\rm {HI}}\lesssim 10^{8.4}\, \rm {M}_{\odot }$ will be required to probe the H i of galaxies undergoing quenching at distances ≳60 Mpc with WALLABY.
The large-scale environment of thermonuclear and core-collapse supernovae
Authors: Tsaprazi Eleni , Jasche Jens , Goobar Ariel , Peiris Hiranya V , Andreoni Igor , Coughlin Michael W , Fremling Christoffer U , Graham Matthew J , Kasliwal Mansi , Kulkarni Shri R , Mahabal Ashish A , Riddle Reed , Sollerman Jesper , Tzanidakis Anastasios 
Published: December 2021

ABSTRACT
The new generation of wide-field time-domain surveys has made it feasible to study the clustering of supernova (SN) host galaxies in the large-scale structure (LSS) for the first time. We investigate the LSS environment of SN populations, using 106 dark matter density realisations with a resolution of ∼3.8 Mpc, constrained by the 2M+ + galaxy survey. We limit our analysis to redshift z &lt; 0.036, using samples of 498 thermonuclear and 782 core-collapse SNe from the Zwicky Transient Facility’s Bright Transient Survey and Census of the Local Universe catalogues. We detect clustering of SNe with high significance; the observed clustering of the two SNe populations is consistent with each other. Further, the clustering of SN hosts is consistent with that of the Sloan Digital Sky Survey (SDSS) Baryon Oscillation Spectroscopic Survey DR12 spectroscopic galaxy sample in the same redshift range. Using a tidal shear classifier, we classify the LSS into voids, sheets, filaments, and knots. We find that both SNe and SDSS galaxies are predominantly found in sheets and filaments. SNe are significantly under-represented in voids and over-represented in knots compared to the volume fraction in these structures. This work opens the potential for using forthcoming wide-field deep SN surveys as a complementary LSS probe.
Evolution of the Sun’s activity and the poleward transport of remnant magnetic flux in Cycles 21–24
Authors: Mordvinov Alexander V , Karak Bidya Binay , Banerjee Dipankar , Golubeva Elena M , Khlystova Anna I , Zhukova Anastasiya V , Kumar Pawan 
Published: December 2021

ABSTRACT
Detailed study of the solar magnetic field is crucial to understand its generation, transport, and reversals. The timing of the reversals may have implications on space weather and thus identification of the temporal behaviour of the critical surges that lead to the polar field reversals is important. We analyse the evolution of solar activity and magnetic flux transport in Cycles 21–24. We identify critical surges of remnant flux that reach the Sun’s poles and lead to the polar field reversals. We reexamine the polar field build-up and reversals in their causal relation to the Sun’s low-latitude activity. We further identify the major remnant flux surges and their sources in the time-latitude aspect. We find that special characteristics of individual 11-yr cycles are generally determined by the spatiotemporal organization of emergent magnetic flux and its unusual properties. We find a complicated restructuring of high-latitude magnetic fields in Cycle 21. The global rearrangements of solar magnetic fields were caused by surges of trailing and leading polarities that occurred near the activity maximum. The decay of non-Joy and anti-Hale active regions resulted in the remnant flux surges that disturbed the usual order in magnetic flux transport. We finally show that the leading-polarity surges during cycle minima sometimes link the following cycle and a collective effect of these surges may lead to secular changes in the solar activity. The magnetic field from a Babcock–Leighton dynamo model generally agrees with these observations.
Cronomoons: origin, dynamics, and light-curve features of ringed exomoons
Authors: Sucerquia Mario , Alvarado-Montes Jaime A , Bayo Amelia , Cuadra Jorge , Cuello Nicolás , Giuppone Cristian A , Montesinos Matías , Olofsson J , Schwab Christian , Spitler Lee , Zuluaga Jorge I 
Published: December 2021

ABSTRACT
In recent years, technical and theoretical work to detect moons and rings around exoplanets has been attempted. The small mass/size ratios between moons and planets means this is very challenging, having only one exoplanetary system where spotting an exomoon might be feasible (i.e. Kepler-1625b i). In this work, we study the dynamical evolution of ringed exomoons, dubbed cronomoons after their similarity with Cronus (Greek for Saturn), and after Chronos (the epitome of time), following the Transit Timing Variations and Transit Duration Variation that they produce on their host planet. Cronomoons have extended systems of rings that make them appear bigger than they actually are when transiting in front of their host star. We explore different possible scenarios that could lead to the formation of such circumsatellital rings, and through the study of the dynamical/thermodynamic stability and lifespan of their dust and ice ring particles, we found that an isolated cronomoon can survive for time-scales long enough to be detected and followed up. If these objects exist, cronomoons’ rings will exhibit gaps similar to Saturn’s Cassini Division and analogous to the asteroid belt’s Kirkwood gaps but instead raised due to resonances induced by the host planet. Finally, we analyse the case of Kepler-1625b i under the scope of this work, finding that the controversial giant moon could instead be an Earth-mass cronomoon. From a theoretical perspective, this scenario can contribute to a better interpretation of the underlying phenomenology in current and future observations.
Drivers of asymmetry in synthetic H i emission-line profiles of galaxies in the eagle simulation
Authors: Manuwal Aditya , Ludlow Aaron D , Stevens Adam R H , Wright Ruby J , Robotham Aaron S G 
Published: December 2021

ABSTRACT
We study the shapes of spatially integrated $\rm{H}\, \small {{I}}$ emission-line profiles of galaxies in the eagle simulation using three separate measures of the profile’s asymmetry. We show that the subset of eagle galaxies whose gas fractions and stellar masses are consistent with those in the xGASS survey also have similar $\rm{H}\, \small {{I}}$ line asymmetries. Central galaxies with symmetric $\rm{H}\, \small {{I}}$ line profiles typically correspond to rotationally supported $\rm{H}\, \small {{I}}$ and stellar discs, but those with asymmetric line profiles may or may not correspond to dispersion-dominated systems. Galaxies with symmetric $\rm{H}\, \small {{I}}$ emission lines are, on average, more gas rich than those with asymmetric lines, and also exhibit systematic differences in their specific star formation rates, suggesting that turbulence generated by stellar or AGN feedback may be one factor contributing to $\rm{H}\, \small {{I}}$ line asymmetry. The line asymmetry also correlates strongly with the dynamical state of a galaxy’s host dark matter halo: older, more relaxed haloes host more-symmetric galaxies than those hosted by unrelaxed ones. At fixed halo mass, asymmetric centrals tend to be surrounded by a larger number of massive subhaloes than their symmetric counterparts, and also experience higher rates of gas accretion and outflow. At fixed stellar mass, central galaxies have, on average, more symmetric $\rm{H}\, \small {{I}}$ emission lines than satellites; for the latter, ram pressure and tidal stripping are significant sources of asymmetry.
Detecting low-mass haloes with strong gravitational lensing I: the effect of data quality and lensing configuration
Authors: Despali Giulia , Vegetti Simona , White Simon D M , Powell Devon M , Stacey Hannah R , Fassnacht Christopher D , Rizzo Francesca , Enzi Wolfgang 
Published: December 2021

ABSTRACT
This paper aims to quantify how the lowest halo mass that can be detected with galaxy-galaxy strong gravitational lensing depends on the quality of the observations and the characteristics of the observed lens systems. Using simulated data, we measure the lowest detectable NFW mass at each location of the lens plane, in the form of detailed sensitivity maps. In summary, we find that: (i) the lowest detectable mass Mlow decreases linearly as the signal-to-noise ratio (SNR) increases and the sensitive area is larger when we decrease the noise; (ii) a moderate increase in angular resolution (0.07″ versus 0.09″) and pixel scale (0.01″ versus 0.04″) improves the sensitivity by on average 0.25 dex in halo mass, with more significant improvement around the most sensitive regions; (iii) the sensitivity to low-mass objects is largest for bright and complex lensed galaxies located inside the caustic curves and lensed into larger Einstein rings (i.e rE ≥ 1.0″). We find that for the sensitive mock images considered in this work, the minimum mass that we can detect at the redshift of the lens lies between 1.5 × 108 and $3\times 10^{9}\, \mathrm{M}_{\odot }$. We derive analytic relations between Mlow, the SNR and resolution and discuss the impact of the lensing configuration and source structure. Our results start to fill the gap between approximate predictions and real data and demonstrate the challenging nature of calculating precise forecasts for gravitational imaging. In light of our findings, we discuss possible strategies for designing strong lensing surveys and the prospects for HST, Keck, ALMA, Euclid and other future observations.
Rapid build-up of the stellar content in the protocluster core SPT2349−56 at z = 4.3
Authors: Hill Ryley , Chapman Scott , Phadke Kedar A , Aravena Manuel , Archipley Melanie , Ashby Matthew L N , Béthermin Matthieu , Canning Rebecca E A , Gonzalez Anthony , Greve Thomas R , Gururajan Gayathri , Hayward Christopher C , Hezaveh Yashar , Jarugula Sreevani , MacIntyre Duncan , Marrone Daniel P , Miller Tim , Rennehan Douglas , Reuter Cassie , Rotermund Kaja M , Scott Douglas , Spilker Justin , Vieira Joaquin D , Wang George , Weiß Axel 
Published: December 2021

ABSTRACT
The protocluster SPT2349−56 at $z = 4.3$ contains one of the most actively star-forming cores known, yet constraints on the total stellar mass of this system are highly uncertain. We have therefore carried out deep optical and infrared observations of this system, probing rest-frame ultraviolet to infrared wavelengths. Using the positions of the spectroscopically confirmed protocluster members, we identify counterparts and perform detailed source deblending, allowing us to fit spectral energy distributions in order to estimate stellar masses. We show that the galaxies in SPT2349−56 have stellar masses proportional to their high star formation rates, consistent with other protocluster galaxies and field submillimetre galaxies (SMGs) around redshift 4. The galaxies in SPT2349−56 have on average lower molecular gas-to-stellar mass fractions and depletion time-scales than field SMGs, although with considerable scatter. We construct the stellar-mass function for SPT2349−56 and compare it to the stellar-mass function of $z = 1$ galaxy clusters, finding consistent shapes between the two. We measure rest-frame galaxy ultraviolet half-light radii from our HST-F160W imaging, finding that on average the galaxies in our sample are similar in size to typical star-forming galaxies at these redshifts. However, the brightest HST-detected galaxy in our sample, found near the luminosity-weighted centre of the protocluster core, remains unresolved at this wavelength. Hydrodynamical simulations predict that the core galaxies will quickly merge into a brightest cluster galaxy, thus our observations provide a direct view of the early formation mechanisms of this class of object.
Matching Bayesian and frequentist coverage probabilities when using an approximate data covariance matrix
Authors: Percival Will J , Friedrich Oliver , Sellentin Elena , Heavens Alan 
Published: December 2021

ABSTRACT
Observational astrophysics consists of making inferences about the Universe by comparing data and models. The credible intervals placed on model parameters are often as important as the maximum a posteriori probability values, as the intervals indicate concordance or discordance between models and with measurements from other data. Intermediate statistics (e.g. the power spectrum) are usually measured and inferences are made by fitting models to these rather than the raw data, assuming that the likelihood for these statistics has multivariate Gaussian form. The covariance matrix used to calculate the likelihood is often estimated from simulations, such that it is itself a random variable. This is a standard problem in Bayesian statistics, which requires a prior to be placed on the true model parameters and covariance matrix, influencing the joint posterior distribution. As an alternative to the commonly used independence Jeffreys prior, we introduce a prior that leads to a posterior that has approximately frequentist matching coverage. This is achieved by matching the covariance of the posterior to that of the distribution of true values of the parameters around the maximum likelihood values in repeated trials, under certain assumptions. Using this prior, credible intervals derived from a Bayesian analysis can be interpreted approximately as confidence intervals, containing the truth a certain proportion of the time for repeated trials. Linking frequentist and Bayesian approaches that have previously appeared in the astronomical literature, this offers a consistent and conservative approach for credible intervals quoted on model parameters for problems where the covariance matrix is itself an estimate.
Early rRNA processing is a stress-dependent regulatory event whose inhibition maintains nucleolar integrity
Authors: Szaflarski Witold , Leśniczak-Staszak Marta , Sowiński Mateusz , Ojha Sandeep , Aulas Anaïs , Dave Dhwani , Malla Sulochan , Anderson Paul , Ivanov Pavel , Lyons Shawn M 
Published: December 2021

Abstract
The production of ribosomes is an energy-intensive process owing to the intricacy of these massive macromolecular machines. Each human ribosome contains 80 ribosomal proteins and four non-coding RNAs. Accurate assembly requires precise regulation of protein and RNA subunits. In response to stress, the integrated stress response (ISR) rapidly inhibits global translation. How rRNA is coordinately regulated with the rapid inhibition of ribosomal protein synthesis is not known. Here, we show that stress specifically inhibits the first step of rRNA processing. Unprocessed rRNA is stored within the nucleolus, and when stress resolves, it re-enters the ribosome biogenesis pathway. Retention of unprocessed rRNA within the nucleolus aids in the maintenance of this organelle. This response is independent of the ISR or inhibition of cellular translation but is independently regulated. Failure to coordinately control ribosomal protein translation and rRNA production results in nucleolar fragmentation. Our study unveils how the rapid translational shut-off in response to stress coordinates with rRNA synthesis production to maintain nucleolar integrity.
Development and external validation of a diagnostic model for biopsy-proven acute interstitial nephritis using electronic health record data
Authors: Moledina Dennis G , Eadon Michael T , Calderon Frida , Yamamoto Yu , Shaw Melissa , Perazella Mark A , Simonov Michael , Luciano Randy , Schwantes-An Tae-Hwi , Moeckel Gilbert , Kashgarian Michael , Kuperman Michael , Obeid Wassim , Cantley Lloyd G , Parikh Chirag R , Wilson F Perry 
Published: December 2021

ABSTRACT

Background
Patients with acute interstitial nephritis (AIN) can present without typical clinical features, leading to a delay in diagnosis and treatment. We therefore developed and validated a diagnostic model to identify patients at risk of AIN using variables from the electronic health record.

Methods
In patients who underwent a kidney biopsy at Yale University between 2013 and 2018, we tested the association of &gt;150 variables with AIN, including demographics, comorbidities, vital signs and laboratory tests (training set 70%). We used least absolute shrinkage and selection operator methodology to select prebiopsy features associated with AIN. We performed area under the receiver operating characteristics curve (AUC) analysis with internal (held-out test set 30%) and external validation (Biopsy Biobank Cohort of Indiana). We tested the change in model performance after the addition of urine biomarkers in the Yale AIN study.

Results
We included 393 patients (AIN 22%) in the training set, 158 patients (AIN 27%) in the test set, 1118 patients (AIN 11%) in the validation set and 265 patients (AIN 11%) in the Yale AIN study. Variables in the selected model included serum creatinine {adjusted odds ratio [aOR] 2.31 [95% confidence interval (CI) 1.42–3.76]}, blood urea nitrogen:creatinine ratio [aOR 0.40 (95% CI 0.20–0.78)] and urine dipstick specific gravity [aOR 0.95 (95% CI 0.91–0.99)] and protein [aOR 0.39 (95% CI 0.23–0.68)]. This model showed an AUC of 0.73 (95% CI 0.64–0.81) in the test set, which was similar to the AUC in the external validation cohort [0.74 (95% CI 0.69–0.79)]. The AUC improved to 0.84 (95% CI 0.76–0.91) upon the addition of urine interleukin-9 and tumor necrosis factor-α.

Conclusions
We developed and validated a statistical model that showed a modest AUC for AIN diagnosis, which improved upon the addition of urine biomarkers. Future studies could evaluate this model and biomarkers to identify unrecognized cases of AIN.
FRUITFULL-like genes regulate flowering time and inflorescence architecture in tomato
Authors: Jiang Xiaobing , Lubini Greice , Hernandes-Lopes José , Rijnsburger Kim , Veltkamp Vera , de Maagd Ruud A , Angenent Gerco C , Bemer Marian 
Published: December 2021

Abstract
The timing of flowering and the inflorescence architecture are critical for the reproductive success of tomato (Solanum lycopersicum), but the gene regulatory networks underlying these traits have not been fully explored. Here, we show that the tomato FRUITFULL-like (FUL-like) genes FUL2 and MADS-BOX PROTEIN 20 (MBP20) promote the vegetative-to-reproductive transition and repress inflorescence branching by inducing floral meristem (FM) maturation. FUL1 fulfils a less prominent role and appears to depend on FUL2 and MBP20 for its upregulation in the inflorescence- and floral meristems. MBP10, the fourth tomato FUL-like gene, has probably lost its function. The tomato FUL-like proteins cannot homodimerize in in vitro assays, but heterodimerize with various other MADS-domain proteins, potentially forming distinct complexes in the transition meristem and FM. Transcriptome analysis of the primary shoot meristems revealed various interesting downstream targets, including four repressors of cytokinin signaling that are upregulated during the floral transition in ful1 ful2 mbp10 mbp20 mutants. FUL2 and MBP20 can also bind in vitro to the upstream regions of these genes, thereby probably directly stimulating cell division in the meristem upon the transition to flowering. The control of inflorescence branching does not occur via the cytokinin oxidase/dehydrogenases (CKXs) but may be regulated by repression of transcription factors such as TOMATO MADS-box gene 3 (TM3) and APETALA 2b (AP2b).