bluuebunny/crossref_metadata_2025_split huggingface dataset:
Insights into the Properties of Type Ibn/Icn Supernovae and Their Progenitor Channels through X-Ray Emission
Authors: Inoue Yusuke , Maeda Keiichi 
Published: February 2025

Abstract
Type Ibn/Icn supernovae (SNe Ibn/Icn), which are characterized by narrow helium or carbon lines that originated in hydrogen-poor dense circumstellar medium (CSM), provide new insights into the final evolution of massive stars. While SNe Ibn/Icn are expected to emit strong X-rays through the strong supernova (SN)-CSM interaction, the X-ray emission modeling effort has been limited so far. In the present study, we provide broad-band X-ray light curve (LC) predictions for SNe Ibn/Icn. We find that the soft X-ray LC provides information about the CSM compositions, while the hard X-ray LC is a robust measure of the CSM density, the explosion energy, and the ejecta mass. In addition, considering the evolution of the ionization state in the unshocked CSM, a bright soft X-ray is expected in the first few days since the explosion, which encourages rapid X-ray follow-up observations as a tool to study the nature of SNe Ibn/Icn. Applying our model to the soft X-ray LCs of SNe Ibn 2006jc and 2022ablq, we derive that the CSM potentially contains a larger fraction of carbon and oxygen for SN 2006jc than 2022ablq, highlighting the power of the soft X-ray modeling to address the nature of the CSM. We also discuss detectability and observational strategy, with which the currently operating telescopes such as NuSTAR and Swift can offer an irreplaceable opportunity to explore the nature of these enigmatic rapid transients and their still-unclarified progenitor channel(s).
Striking a Chord with Spectral Sirens: Multiple Features in the Compact Binary Population Correlate with H0
Authors: Mali Utkarsh , Essick Reed 
Published: February 2025

Abstract
Spectral siren measurements of the Hubble constant (H
0) rely on correlations between observed detector-frame masses and luminosity distances. Features in the source-frame mass distribution can induce these correlations. It is crucial, then, to understand (i) which features in the source-frame mass distribution are robust against model (re)parameterization, (ii) which features carry the most information about H
0, and (iii) whether distinct features independently correlate with cosmological parameters. We study these questions using real gravitational-wave observations from the LIGO-Virgo-KAGRA Collaborations' third observing run. Although constraints on H
0 are weak, we find that current data reveals several prominent features in the mass distribution, including peaks in the binary black hole source-frame mass distribution near ∼9M
⊙ and ∼32M
⊙ and a roll-off at masses above ∼46M⊙. For the first time using real data, we show that all of these features carry cosmological information and that the peak near ∼32M
⊙ consistently correlates with H
0 most strongly. Introducing model-independent summary statistics, we show that these statistics independently correlate with H
0, exactly what is required to limit systematics within future spectral siren measurements from the (expected) astrophysical evolution of the mass distribution.
Associations between Scattering Screens and Interstellar Medium Filaments
Authors: Stock Ashley M. , van Kerkwijk Marten H. 
Published: February 2025

Abstract
Pulsar scintillation can be used to measure small-scale structure in the Galaxy, but little is known about the specific interstellar medium (ISM) features that cause scintillation. We searched for ISM counterparts to all scintillation screens for which absolute distances and scattering orientations have been measured—a sample of 12 pulsars and 22 screens. For one pulsar, PSR J0737–3039A, we reanalyze its scintillation screen and find evidence for a highly anisotropic screen. Comparisons with tracers of ionized media did not find any new associations. Instead, for seven of the pulsars analyzed, aligned H i filaments are seen for at least one of their screens, for a total of 12 out of 22 screens. This result seems unlikely to be due to chance: Comparing with random trials, we estimate a likelihood of finding 12 or more screens with aligned emission by chance of only 0.004%. Estimating the significance of the amount of aligned emission (in standard deviations over the mean), the probability of finding as much observed aligned emission by chance is larger, at 1.7%, but still indicative of a real correlation. Since H i filaments are preferentially associated with cold neutral gas, and thus unlikely to cause scintillation, this may indicate that both the filaments and the screens are aligned preferentially by the same mechanisms, such as magnetic fields or shocks.
The Lyman Continuum Escape Fraction of Star-forming Galaxies at 2.4 ≲ z ≲ 3.0 from UVCANDELS
Authors: Wang Xin , Teplitz Harry I. , Smith Brent M. , Windhorst Rogier A. , Rafelski Marc , Mehta Vihang , Alavi Anahita , Ji Zhiyuan , Brammer Gabriel , Colbert James , Grogin Norman , Hathi Nimish P. , Koekemoer Anton M. , Prichard Laura , Scarlata Claudia , Sunnquist Ben , Arrabal Haro Pablo , Conselice Christopher , Gawiser Eric , Guo Yicheng , Hayes Matthew , Jansen Rolf A. , Lucas Ray A. , O’Connell Robert , Robertson Brant , Rutkowski Michael , Siana Brian , Vanzella Eros , Ashcraft Teresa , Bagley Micaela , Baronchelli Ivano , Barro Guillermo , Blanche Alex , Broussard Adam , Carleton Timothy , Chartab Nima , Cheng Yingjie , Codoreanu Alex , Cohen Seth , Dai Y. Sophia , Darvish Behnam , Davé Romeel , DeGroot Laura , De Mello Duilia , Dickinson Mark , Emami Najmeh , Ferguson Henry , Ferreira Leonardo , Finkelstein Keely , Finkelstein Steven , Gardner Jonathan P. , Gburek Timothy , Giavalisco Mauro , Grazian Andrea , Gronwall Caryl , Hemmati Shoubaneh , Howell Justin , Iyer Kartheik , Kaviraj Sugata , Kurczynski Peter , Lazar Ilin , MacKenty John , Mantha Kameswara Bharadwaj , Martin Alec , Martin Garreth , McCabe Tyler , Mobasher Bahram , Nedkova Kalina , Olsen Charlotte , Otteson Lillian , Ravindranath Swara , Redshaw Caleb , Sattari Zahra , Soto Emmaris , Yung L. Y. Aaron , Zabelle Bonnabelle ,   the UVCANDELS team
Published: February 2025

Abstract
The UltraViolet Imaging of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey Fields (UVCANDELS) survey is a Hubble Space Telescope (HST) Cycle-26 Treasury Program, allocated in total 164 orbits of primary Wide-Field Camera 3 Ultraviolet and VISible light F275W imaging with coordinated parallel Advanced Camera for Surveys F435W imaging, on four of the five premier extragalactic survey fields: GOODS-N, GOODS-S, EGS, and COSMOS. We introduce this survey by presenting a comprehensive analysis of the absolute escape fraction (

f

esc

abs

) of Lyman continuum radiation through stacking the UV images of a population of star-forming galaxies with secure redshifts at 2.4 ≤ z ≤ 3.0. Our stacking benefits from the catalogs of high-quality spectroscopic redshifts compiled from archival ground-based data and HST slitless spectroscopy, carefully vetted by dedicated visual inspection efforts. We develop a robust stacking method to apply to 10 samples of in total 56 galaxies, and perform detailed Monte Carlo simulations of the intergalactic medium (IGM) attenuation, to take into account the sample variance of the mean IGM transmission when measuring

f

esc

abs

. The full stack at z ≈ 2.44 from 28 galaxies places a stringent 1σ upper limit of

f

esc

abs

≲
5
%

, whereas the full stack at z ≈ 2.72 of an equal number of galaxies gives an upper limit of

f

esc

abs

≲
26
%

at 1σ confidence level. These new F275W and F435W imaging mosaics from UVCANDELS have been made publicly available on the Barbara A. Mikulski Archive for Space Telescopes.
Differentiating the Acceleration Mechanisms in the Slow and Alfvénic Slow Solar Wind
Authors: Rivera Yeimy J. , Badman Samuel T. , Verniero J. L. , Varesano Tania , Stevens Michael L. , Stawarz Julia E. , Reeves Katharine K. , Raines Jim M. , Raymond John C. , Owen Christopher J. , Livi Stefano A. , Lepri Susan T. , Landi Enrico , Halekas Jasper. S. , Ervin Tamar , Dewey Ryan M. , De Marco Rossana , D’Amicis Raffaella , Dakeyo Jean-Baptiste , Bale Stuart D. , Alterman B. L. 
Published: February 2025

Abstract
In the corona, plasma is accelerated to hundreds of kilometers per second and heated to temperatures hundreds of times hotter than the Sun's surface before it escapes to form the solar wind. Decades of space-based experiments have shown that the energization process does not stop after it escapes. Instead, the solar wind continues to accelerate, and it cools far more slowly than a freely expanding adiabatic gas. Recent work suggests that fast solar wind requires additional momentum beyond what can be provided by the observed thermal pressure gradients alone, whereas it is sufficient for the slowest wind. The additional acceleration for fast wind can be provided through an Alfvén wave pressure gradient. Beyond this fast/slow categorization, however, a subset of slow solar wind exhibits high Alfvénicity that suggests that Alfvén waves could play a larger role in its acceleration compared to conventional slow wind outflows. Through a well-timed conjunction between Solar Orbiter and Parker Solar Probe (PSP), we trace the energetics of slow wind to compare with a neighboring Alfvénic slow solar wind stream. An analysis that integrates remote and heliospheric properties and modeling of the two distinct solar wind streams finds that Alfvénic slow solar wind behaves like fast wind, where a wave pressure gradient is required to reconcile its full acceleration, while non-Alfvénic slow wind can be driven by its nonadiabatic electron and proton thermal pressure gradients. Derived coronal conditions of the source region indicate good model compatibility, but extended coronal observations are required to effectively trace solar wind energetics below PSP's orbit.
Neutrino-dominated Relativistic Viscous Accretion Flows around Rotating Black Holes with Shocks
Authors: Kumar Amit , Chakrabarti Sayan , Das Santabrata 
Published: February 2025

Abstract
We investigate the relativistic, viscous, advective neutrino-dominated accretion flows (NDAFs) around rotating stellar-mass black holes, incorporating neutrino cooling. By adopting an effective potential to describe the spacetime geometry around the rotating black holes, we self-consistently solve the governing NDAF equations to obtain global transonic accretion solutions. Our findings indicate that, depending on the model parameters, namely, energy (ε), angular momentum (λ), accretion rate (

m

̇

), viscosity (α), and black hole spin (a
k), NDAFs may harbor standing shocks where the Rankine–Hugoniot shock conditions are satisfied. Utilizing these shock-induced NDAF solutions, we compute the neutrino luminosity (L

ν
) and neutrino annihilation luminosity (

L

ν

ν

¯

) across a wide range of model parameters. We further calculate maximum neutrino luminosity (

L

ν

max

) and neutrino annihilation luminosity (

L

ν

ν

¯

max

), resulting in

L

ν

max

∼
1

0

51
−
53

erg s−1 (1048−51 erg s−1) and

L

ν

ν

¯

max

∼
1

0

48
−
52

erg s−1 (1042−49 erg s−1) for a
k = 0.99 (0.0). These findings suggest that shocked NDAF solutions are potentially promising to explain the energy output of gamma-ray bursts (GRBs). We employ our NDAF model formalism to elucidate

L

ν

ν

¯

obs

for five GRBs with known redshifts and estimate their accretion rate (

m

̇

) based on the spin (a
k) of the central source of the GRBs studied here.
APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Pinsonneault Marc H. , Zinn Joel C. , Tayar Jamie , Serenelli Aldo , García Rafael A. , Mathur Savita , Vrard Mathieu , Elsworth Yvonne P. , Mosser Benoit , Stello Dennis , Bell Keaton J. , Bugnet Lisa , Corsaro Enrico , Gaulme Patrick , Hekker Saskia , Hon Marc , Huber Daniel , Kallinger Thomas , Cao Kaili , Johnson Jennifer A. , Liagre Bastien , Patton Rachel A. , Santos Ângela R. G. , Basu Sarbani , Beck Paul G. , Beers Timothy C. , Chaplin William J. , Cunha Katia , Frinchaboy Peter M. , Girardi Léo , Godoy-Rivera Diego , Holtzman Jon A. , Jönsson Henrik , Mészáros Szabolcs , Reyes Claudia , Rix Hans-Walter , Shetrone Matthew , Smith Verne V. , Spoo Taylor , Stassun Keivan G. , Wang Ji 
Published: February 2025

Abstract
In the third APOKASC catalog, we present data for the complete sample of 15,808 evolved stars with APOGEE spectroscopic parameters and Kepler asteroseismology. We used 10 independent asteroseismic analysis techniques and anchor our system on fundamental radii derived from Gaia L and spectroscopic T
eff. We provide evolutionary state, asteroseismic surface gravity, mass, radius, age, and the data used to derive them for 12,418 stars. This includes 10,036 exceptionally precise measurements, with median fractional uncertainties in

ν

max

, Δν, mass, radius, and age of 0.6%, 0.6%, 3.8%, 1.8%, and 11.1%, respectively. We provide more limited data for 1624 additional stars that either have lower-quality data or are outside of our primary calibration domain. Using lower red giant branch (RGB) stars, we find a median age for the chemical thick disk of 9.14 ± 0.05(ran) ± 0.9(sys) Gyr with an age dispersion of 1.1 Gyr, consistent with our error model. We calibrate our red clump (RC) mass loss to derive an age consistent with the lower RGB and provide asymptotic GB and RGB ages for luminous stars. We also find a sharp upper-age boundary in the chemical thin disk. We find that scaling relations are precise and accurate on the lower RGB and RC, but they become more model dependent for more luminous giants and break down at the tip of the RGB. We recommend the use of multiple methods, calibration to a fundamental scale, and the use of stellar models to interpret frequency spacings.
ExoMolHR: A Relational Database of Empirical High-resolution Molecular Spectra
Authors: Zhang Jingxin , Hill Christian , Tennyson Jonathan , Yurchenko Sergei N. 
Published: February 2025

Abstract
ExoMolHR is an empirical, high-resolution molecular spectrum calculator for the high-temperature molecular line lists available from the ExoMol molecular database. Uncertainties, where available, in recommended ExoMol data sets are used to select highly accurate spectral lines. These lines largely rely on empirical energy levels generated through the MARVEL procedure, which is being systematically used to improve the energy and transition data provided by the ExoMol database. The freely accessible ExoMolHR database provides line positions with calculated intensities for a user-specified wavenumber/wavelength range and temperature. Spectra can be plotted on the ExoMolHR website https://www.exomol.com/exomolhr/ or downloaded as a .csv file. Cross sections can be calculated using the Python program PyExoCross. The ExoMolHR database currently provides 24,307,135 spectral lines for 33 molecules and 58 isotopologues; these numbers will increase as the ExoMol database is updated.
Pearls on a String: Dark and Bright Galaxies on a Strikingly Straight and Narrow Filament
Authors: Arabsalmani M. , Roychowdhury S. , Schneider B. , Springel V. , Floc’h E. Le , Bournaud F. , Burkert A. , Cuillandre J.-C. , Duc P.-A. , Emsellem E. , Galárraga-Espinosa D. , Pian E. , Renaud F. , Zwaan M. A. 
Published: February 2025

Abstract
We identify a chain of galaxies along an almost straight line in the nearby Universe with a projected length of ~5 Mpc. The galaxies are distributed within projected distances of only 7–105 kpc from the axis of the identified filament. They have redshifts in a very small range of z = 0.0361−0.0370 so that their radial velocities are consistent with galaxy proper motions. The filament galaxies are mainly star forming and have stellar masses in a range of 109.1−1010.7
M
⊙. We search for systems with similar geometrical properties in the full-sky mock galaxy catalog of the MillenniumTNG simulations and find that, although such straight filaments are unusual and rare, they are predicted by ΛCDM simulations (4% incidence). We study the cold H i gas in a 1.3 Mpc section of the filament through H i 21 cm emission line observations and detect 11 H i sources, many more than expected from the H i mass function in a similar volume. They have H i masses 108.5−109.5
M
⊙ and are mostly within ~120 kpc projected distance from the filament axis. None of these H i sources has a confirmed optical counterpart. Their darkness together with their large H i 21 cm line widths indicates that they contain gas that might not yet be virialized. These clouds must be marking the peaks of the dark matter and H i distributions over large scales within the filament. The presence of such gas clouds around the filament spines is predicted by simulations, but this is the first time that the existence of such clouds in a filament is observationally confirmed.
The Early Post-outburst Infrared Spectrum of the Stellar Merger V1309 Scorpii (Nova Scorpii 2008)
Authors: Rudy Richard J. , Russell Ray W. , Lynch David K. , Sitko Michael L. 
Published: February 2025

Abstract
In this paper we present a 0.8–2.4 μm spectrum of the stellar merger V1309 Scorpii (Nova Scorpii 2008). The spectrum was acquired within three days of discovery and a day before maximum light and has the appearance of a F supergiant. It is dominated by H i line absorptions and closely mimicks that of a classical novae with a massive ejected shell shortly after outburst. The spectrum also displays Fe ii features—all in emission—and absorption lines due to C i, S i and Ca ii. Weak molecular absorption from carbon monoxide may also be present.
Mesa Redonda Complex (Villaverde del Río, Seville): a tell above the Lower Guadalquivir Valley
Authors: Diaz-Zorita Bonilla Marta , Bartelheim Martin , Chala-Aldana Döbereiner , Escudero Carrillo Javier , García Fernández Francisco José , Ferrer Albelda Eduardo , Garrido González Pablo , Daza Pastrana Fernando 
Published: February 2025

The archaeological site of Mesa Redonda (Villaverde del Río, Seville) was the subject of archaeological research at the end of the 1970s, and only recently has new research been carried out. In this paper we present the results of both the old and the new archaeological work conducted in 2019-2021. We have named this site the Mesa Redonda Complex, because of the wider period of use and because it includes many different sites. According to the results of the archaeological survey, test pits and geoelectric prospection, the archaeological site offers a multi-layered continuous use of the summit from the Bronze Age to the Islamic Middle Ages (12th century AD). Due to its size and long diachronic sequence, in this case covering at least four millennia, the structure of the site complies with the definition of an archaeological tell. Mesa Redonda is strategically located between the Guadalquivir Valley and Sierra Morena, overlooking the fertile lands of the valley with abundant agropastoral resources.
Une nouvelle cartographie de l’accueil du néo-réalisme en France
Authors: Gheller Enrico 
Published: February 2025

À partir de quelques critiques négatives consacrées au film Ladri di biciclette (le Voleur de bicyclette, Vittorio De Sica, 1948), cette étude se propose d’esquisser une « cartographie » alternative de la réception du néo-réalisme en France et de complexifier l’idée d’un accueil bienveillant de ce mouvement. Pour ce faire, elle identifie trois domaines critiques ayant exprimé des lectures problématiques, sceptiques ou franchement négatives. Ces domaines critiques « hérétiques » s’opposent en quelque sorte aux interprétations « canoniques » soutenues par André Bazin et Georges Sadoul et constituent autant de communautés interprétatives négligées par l’histoire officielle.
Lumière d’été de Jean Grémillon : Haute-Provence sur Dordogne
Authors: Albera François 
Published: February 2025

En 1942 Jean Grémillon, Jacques Prévert et Pierre Laroche entreprennent un film, Lumière d’été, qui sortira en mai 1943 alors que la France est occupée par les armées nazies et que la Résistance s’organise en vue de la Libération. Le film se situe dans un autre temps, antérieur à la guerre et pourtant retentit fortement des événements contemporains, dont il traite de manière décalée. Le tournage se situant en partie sur le chantier d’un grand barrage sur la Dordogne, lui-même foyer de résistance, le film qui utilise comme figurants les ouvriers et les habitants de la vallée en viendra jusqu’à nos jours à représenter dans la région un véritable « lieu de mémoire » et à faire l’objet d’une appropriation en dépit du fait que son récit situe les événements dans une autre région de France.
CircRNA-0013747 Promotes Mesangial Cell Proliferation in Immunoglobulin A Nephropathy through Modulation of the Warburg Effect
Authors: Zou Huimei , Deng Wenli , Xu Lifen , Shi Mingjun , Liu Lingling , Gong Lei , Cui Daolin , Zhang Fan 
Published: February 2025

Abstract
Immunoglobulin A nephropathy (IgAN) is characterized by aberrant mesangial cell (MC) proliferation, which is a critical determinant of glomerular sclerosis and renal dysfunction. Previous studies have highlighted the role of pyruvate kinase M2 (PKM2)- mediated aerobic glycolysis in promoting MC growth and the progression of kidney diseases. However, the precise mechanisms underlying PKM2 dysregulation in IgAN remain unclear. Circular RNAs (circRNAs), a class of noncoding RNAs, have emerged as pivotal regulators in various diseases, yet their role in IgAN has not been fully elucidated. In this study, we investigated the expression and functional significance of circRNA_0013747 in IgAN, focusing on its interaction with microRNA-330-3p (miR-330-3p) and its downstream effects on PKM2-mediated aerobic glycolysis. Our results demonstrated a significant upregulation of circRNA_0013747 in kidney biopsy samples from IgAN patients. Functional analyses revealed that circRNA_0013747 promoted MC proliferation and activated PKM2-mediated aerobic glycolysis. Importantly, these effects were attenuated by the upregulation of miR-330-3p, which was found to physically interact with circRNA_0013747, thereby inhibiting its function. Mechanistically, circRNA_0013747 acted as a sponge for miR-330-3p, relieving its suppressive effects on PKM2 expression. These findings suggest that circRNA_0013747 enhances glycolysis and proliferation in MCs through modulation of the miR-330-3p/PKM2 signaling axis. These results offer novel insights into the pathogenesis of IgAN and could contribute to new therapeutic approaches for this disease. Specifically, targeting circRNA_0013747 or modulating its interaction with miR-330-3p may provide a means to inhibit MC proliferation and aerobic glycolysis, thereby slowing the progression of IgAN and preserving renal function. Such therapeutic strategies hold the promise of substantial benefits for patients with IgAN and could pave the path toward developing more potent treatments for a wider range of renal diseases.