bluuebunny/crossref_metadata_2025_split huggingface dataset:
No Evidence for a Metallicity-dependent Enhancement of Distant Giant Companions to Close-in Small Planets in the California Legacy Survey
Authors: Van Zandt Judah , Petigura Erik A. 
Published: November 2024

Abstract
Understanding the relationship between close-in small (CS) planets and distant giants (DGs) is central to understanding the formation of planetary systems like our own. Most studies of this connection have found evidence for a positive correlation, though significant statistical and systematic uncertainties remain due to differences in sample size, target selection bias, and even the definitions of CS and DG planets. Recently, M. L. Bryan & E. J. Lee conducted a study of 184 stars hosting super-Earths (

M
sin
i
=
1
−
20

M
⊕

or R = 1 − 4 R
⊕) to determine the effect of stellar metallicity on the prevalence of DG companions (

M
sin
i
=
0.5
−
20

M
J

, a = 1−10 au). They found that such giants are twice as common in the presence of inner planets, but only in metal-rich systems: P(DG∣CS, [Fe/H] > 0) =

28.0

−
4.6

+
4.9

%

versus P(DG∣[Fe/H] > 0) =

14.3

−
1.8

+
2.0

%

. Further, they found that this correlation disappears for metal-poor stars: P(DG∣CS, [Fe/H] ≤ 0) =

4.5

−
1.9

+
2.6

%

versus P(DG∣[Fe/H] ≤ 0) =

5.0

−
1.3

+
1.6

%

. We conducted an analogous study to test whether this effect was present in the California Legacy Survey sample. Using the same planet definitions, we did not find evidence for an enhancement in metal-rich systems: P(DG∣CS, [Fe/H] > 0) =

14

−
8

+
11

%

versus P(DG∣[Fe/H] > 0) =

17.9

−
2.4

+
2.5

%

. We also found a 2σ tension between our conditional rate and a 2x enhancement. We brought our results into closer agreement with M. L. Bryan & E. J. Lee by repeating our analysis with different planet definitions. For example, considering only CS planets with

1
≤
M
sin
i
≤
10

M

⊕

and DG planets with

0.5
≤
M
sin
i
≤
20

M

J

gives P(DG∣CS, [Fe/H] > 0) =

48

−
17

+
17

%

and P(DG∣[Fe/H] > 0) =

21.8

−
2.7

+
2.9

%

, consistent with a 2x enhancement. However, we find that this 2x enhancement is also present when we apply the same planet definitions to the overall sample, challenging the idea that metallicity is responsible. Our sample, though only ∼1/6 the size of M. L. Bryan & E. J. Lee, was assembled and analyzed self-consistently. The discrepancy between our findings and theirs may arise from a variety of sources, underscoring the need for large exoplanet surveys to overcome both small number statistics and sample inhomogeneities.
The SAGA Survey. V. Modeling Satellite Systems around Milky Way–Mass Galaxies with Updated UniverseMachine
Authors: Wang Yunchong , Nadler Ethan O. , Mao Yao-Yuan , Wechsler Risa H. , Abel Tom , Behroozi Peter , Geha Marla , Asali Yasmeen , de los Reyes Mithi A. C. , Kado-Fong Erin , Kallivayalil Nitya , Tollerud Erik J. , Weiner Benjamin , Wu John F. 
Published: November 2024

Abstract
Environment plays a critical role in shaping the assembly of low-mass galaxies. Here, we use the UniverseMachine (UM) galaxy–halo connection framework and Data Release 3 of the Satellites Around Galactic Analogs (SAGA) Survey to place dwarf galaxy star formation and quenching into a cosmological context. UM is a data-driven forward model that flexibly parameterizes galaxy star formation rates (SFRs) using only halo mass and assembly history. We add a new quenching model to UM, tailored for galaxies with m
⋆ ≲ 109
M
⊙, and constrain the model down to m
⋆ ≳ 107
M
⊙ using new SAGA observations of 101 satellite systems around Milky Way (MW)–mass hosts and a sample of isolated field galaxies in a similar mass range from the Sloan Digital Sky Survey. The new best-fit model, “UM-SAGA,” reproduces the satellite stellar mass functions, average SFRs, and quenched fractions in SAGA satellites while keeping isolated dwarfs mostly star-forming. The enhanced quenching in satellites relative to isolated field galaxies leads the model to maximally rely on halo assembly to explain the observed environmental quenching. Extrapolating the model down to m
⋆ ∼ 106.5
M
⊙ yields a quenched fraction of ≳30% for isolated field galaxies and ≳80% for satellites of MW-mass hosts at this stellar mass. Spectroscopic surveys can soon test this specific prediction to reveal the relative importance of internal feedback, cessation of mass and gas accretion, satellite-specific gas processes, and reionization for the evolution of faint low-mass galaxies.
A Hierarchical Bayesian Approach to Point-source Analysis in High-energy Neutrino Telescopes
Authors: Capel Francesca , Kuhlmann Julian , Haack Christian , Ha Minh Martin , Niederhausen Hans , Schumacher Lisa 
Published: November 2024

Abstract
We propose a novel approach to the detection of point-like sources of high-energy neutrinos. Motivated by evidence for emerging sources in existing data, we focus on the characterization and interpretation of these sources rather than the rejection of the background-only hypothesis. The hierarchical Bayesian model is implemented in the Stan platform, enabling computation of the posterior distribution with a Hamiltonian Monte Carlo algorithm. We simulate a population of weak neutrino sources detected by the IceCube experiment and use the resulting data set to demonstrate and validate our framework. We show that even for the challenging case of sources at the threshold of detection and using limited prior information, it is possible to correctly infer the source properties. Additionally, we demonstrate how modeling flexible connections between similar sources can be used to recover the contribution of sources that would not be detectable individually. While a direct comparison of our method to existing approaches is challenged by the fundamental differences in frequentist and Bayesian frameworks, we draw parallels where possible. In particular, we highlight how including more complexity into the source modeling can increase the sensitivity to sources and their populations.
The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources*
Authors: Acebron Ana , Grillo Claudio , Suyu Sherry H. , Angora Giuseppe , Bergamini Pietro , Caminha Gabriel B. , Ertl Sebastian , Mercurio Amata , Nonino Mario , Rosati Piero , Wang Han , Bolamperti Andrea , Meneghetti Massimo , Schuldt Stefan , Vanzella Eros 
Published: November 2024

Abstract
Overcoming both modeling and computational challenges, we present, for the first time, the extended surface-brightness distribution model of a strongly lensed source in a complex galaxy-cluster-scale system. We exploit the high-resolution Hubble Space Telescope (HST) imaging and extensive Multi Unit Spectroscopic Explorer spectroscopy to build an extended strong-lensing model, in a full multiplane formalism, of SDSS J1029+2623, a lens cluster at z = 0.588 with three multiple images of a background quasar (z = 2.1992). Going beyond typical cluster strong-lensing modeling techniques, we include as observables both the positions of 26 pointlike multiple images from seven background sources, spanning a wide redshift range between 1.02 and 5.06, and the extended surface-brightness distribution of the strongly lensed quasar host galaxy, over ∼78,000 HST pixels. In addition, we model the light distribution of seven objects, angularly close to the strongly lensed quasar host, over ∼9300 HST pixels. Our extended lens model reproduces well both the observed intensity and morphology of the quasar host galaxy in the HST F160W band (with a 0.″03 pixel scale). The reconstructed source shows a single, compact, and smooth surface-brightness distribution, for which we estimate an intrinsic magnitude of 23.3 ± 0.1 in the F160W band and a half-light radius of (2.39 ± 0.03) kpc. The increased number of observables enables the accurate determination of the total mass of line-of-sight halos lying angularly close to the extended arc. This work paves the way for a new generation of galaxy cluster strong-lens models, where additional, complementary lensing observables are directly incorporated as model constraints.
Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Waratkar Gaurav , Bhalerao Varun , Bhattacharya Dipankar 
Published: November 2024

Abstract
GW150914 marked the start of the gravitational wave (GW) era with the direct detection of a binary black hole (BBH) merger by the LIGO-Virgo GW detectors. The event was tentatively associated with a signal detected by the Fermi Gamma-ray Burst Monitor (GBM), which hinted toward electromagnetic emission associated with compact object coalescence. The detection of a short gamma-ray burst (GRB) associated with GW170817, along with several multiwavelength detections, truly established that compact object mergers are indeed multimessenger events. The CadmiumZincTelluride Imager (CZTI) on board AstroSat can search for X-ray counterparts of the GW events and has detected over 650 GRBs in the 8.5 yr since it was launched. We present results from our searches for counterparts coincident with GW triggers from the first three LIGO-Virgo-KAGRA (LVK) GW Transient Catalogs. For 71 out of 90 GW events for which AstroSat-CZTI data was available, we undertook a systematic search for temporally coincident transients in the 20–200 keV band and detected no X-ray counterparts. We evaluate the upper limits on the maximum possible flux from the source in a 100 s window centered around each trigger, consistent with the GW localization of the event. Thanks to the sensitivity of CZTI, these upper limits are competitive with those from other spacecraft. We use these upper limits to constrain theoretical models that predict high-energy counterparts to BBH mergers. We also discuss the probability of nondetections of BBH mergers at different luminosities and the implications of such nondetections from the ongoing fourth observing run of the LVK detectors.
Low [O/Fe] Ratio in a Luminous Galaxy at the Early Cosmic Epoch (z > 10): Signature of Short Delay Time or Bright Hypernovae/Pair-instability Supernovae?
Authors: Nakane Minami , Ouchi Masami , Nakajima Kimihiko , Harikane Yuichi , Tominaga Nozomu , Takahashi Koh , Kashino Daichi , Yanagisawa Hiroto , Watanabe Kuria , Nomoto Ken’ichi , Isobe Yuki , Nishigaki Moka , Ishigaki Miho N. , Ono Yoshiaki , Takeda Yui 
Published: November 2024

Abstract
We present an [O/Fe] ratio of a luminous galaxy GN-z11 at z = 10.60 derived with the deep public JWST/NIRSpec data. We fit the medium-resolution grating (G140M, G235M, and G395M) data with the model spectra consisting of BPASS-stellar and Cloudy-nebular spectra in the rest-frame UV wavelength ranges with Fe absorption lines, carefully masking the other emission and absorption lines in the same manner as previous studies conducted for lower-redshift (z ∼ 2–6) galaxies with oxygen abundance measurements. We obtain an Fe-rich abundance ratio

[
O

/

Fe
]
=
−

0.37

−
0.22

+
0.43

, which is confirmed with the independent deep prism data as well as by the classic 1978 index method. This [O/Fe] measurement is lower than that measured for star-forming galaxies at z ∼ 2–3. Because z = 10.60 is an early epoch after the Big Bang (∼430 Myr) and the first star formation (likely ∼200 Myr), it is difficult to produce Fe by Type Ia supernovae (SNe Ia), which requires sufficient delay time for white-dwarf formation and gas accretion. The Fe-rich abundance ratio in GN-z11 suggests that the delay time is short or that the major Fe enrichment is not accomplished by SNe Ia but by bright hypernovae (BrHNe) and/or pair-instability supernovae (PISNe), where the yield models of BrHNe and PISNe explain Fe, Ne, and O abundance ratios of GN-z11. The [O/Fe] measurement is not too low to rule out the connection between GN-z11 and globular clusters (GCs) previously suggested by the nitrogen abundance but rather supports the connection with a GC population at high [N/O] if a metal dilution process exists.
Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Golomb Jacob , Isi Maximiliano , Farr Will M. 
Published: November 2024

Abstract
Gravitational-wave observations of binary black holes have revealed unexpected structure in the black hole mass distribution. Previous studies employ physically motivated phenomenological models and infer the parameters that control the features of the mass distribution that are allowed in their model, associating the constraints on those parameters with their physical motivations a posteriori. In this work, we take an alternative approach in which we introduce a model parameterizing the underlying stellar and core-collapse physics and obtaining the remnant black hole distribution as a derived by-product. In doing so, we constrain the stellar physics necessary to explain the astrophysical distribution of black hole properties under a given model. We apply this to the mapping between initial mass and remnant black hole mass, accounting for mass-dependent mass loss using a simple parameterized description. Allowing the parameters of the initial mass–remnant mass relationship to evolve with redshift permits correlated and physically reasonable changes to features in the mass function. We find that the current data are consistent with no redshift evolution in the core–remnant mass relationship, but place only weak constraints on the change of these parameters. This procedure can be applied to modeling any physical process underlying the astrophysical distribution. We illustrate this by applying our model to the pulsational pair instability supernova (PPISN) process, previously proposed as an explanation for the observed excess of black holes at ∼35 M
⊙. Placing constraints on the reaction rates necessary to explain the PPISN parameters, we concur with previous results in the literature that the peak observed at ∼35 M
⊙ is unlikely to be a signature from the PPISN process as presently understood.
Radio Morphology of Gamma-Ray Sources: Double-lobed Radio Sources
Authors: Paliya Vaidehi S. , Saikia D. J. , Domínguez Alberto , Stalin C. S. 
Published: November 2024

Abstract
The extragalactic γ-ray sky is dominated by relativistic jets aligned to the observer’s line of sight, i.e., blazars. A few of their misaligned counterparts, e.g., radio galaxies, are also detected with the Fermi-Large Area Telescope (LAT), albeit in a small number (∼50), indicating the crucial role played by the jet viewing angle in detecting γ-ray emission from jets. These γ-ray emitting misaligned active galactic nuclei (AGN) provide us with a unique opportunity to understand the high-energy emission production mechanisms from a different viewpoint than the more common blazars. With this goal in mind, we have systematically studied the radio morphology of γ-ray emitting sources present in the fourth data release of the fourth catalog of Fermi-LAT detected γ-ray sources to identify misaligned AGN. By utilizing the high-resolution and sensitive MHz and GHz frequency observations delivered by the Very Large Array Sky Survey, Low-Frequency Array Two-metre Sky Survey, Faint Images of the Radio Sky at Twenty Centimeters, and Rapid ASKAP Continuum Survey, here we present a catalog of 149 γ-ray detected misaligned AGN, thus approximately tripling the number of known objects of this class. Our sample includes a variety of radio morphologies, e.g., edge-darkened and edge-brightened, hybrids, wide-angle-tailed, bent jets, and giants. Since the γ-ray emission is thought to be highly sensitive to the jet viewing angle, such an enlarged sample of γ-ray detected misaligned radio sources will permit us to explore the origin of high-energy emission in relativistic jets and radio lobes and study AGN unification, in general.
Understanding the Effects of Micrometeoroid Bombardment on Graphite-rich Mercury Analogs through Laboratory Experiments and Electron Microscopy Analysis
Authors: Bott Nicolas , Thompson Michelle S. , Loeffler Mark J. , Vander Kaaden Kathleen E. , McCubbin Francis M. 
Published: November 2024

Abstract
Space weathering alters the spectral, microstructural, and chemical characteristics of the surface of Mercury, and an effective way to understand it is in the laboratory. To simulate energetic micrometeoroid impacts on the surface of Mercury, we irradiated pellets containing forsteritic olivine and graphite with a pulsed laser. Our analysis with scanning electron microscopy showed two morphological textures: one that is melt-rich and one consisting of fluffy, C-rich globules. Performing transmission electron microscopy on these textures, we identified the presence of new microstructural and chemical features resulting from simulated space weathering, including C-rich inclusions in the melt and vesiculated textures in the C-rich globules. Separate analysis of Si wafers, which were suspended near the target to collect the vapor and melt ejected during irradiation, show a variety of ejected material, including forsterite grains, melt splash, and C-rich particles. These observations suggest the possibility that space weathering products on the surface of Mercury may be different than on other airless bodies, which will be further explored by the BepiColombo mission.
Les débarquements de la seconde guerre mondiale et la géomorphologie dynamique littorale : naissance d’une discipline au sein de l’institut d’océanographie du Scripps en Californie
Authors: Suanez Serge 
Published: November 2024

Au début de la seconde guerre mondiale, alors que les Etats-Majors des armées anglo-américaines préparent les débarquements de troupes de fantassins en Europe et dans le Pacifique, ils font le constat que les connaissances en matière d'hydrodynamisme côtier et de fonctionnement morphosédimentaire littoral sont insuffisantes pour mener à bien ces opérations amphibies. Pendant 4 ans (1940-1944), de jeunes ingénieurs du civil et militaires vont mener des expérimentations de terrain et en laboratoire afin de résoudre de nombreuses problématiques en lien avec le déferlement des vagues, les courants côtiers, et la migration des corps sédimentaires immergés. Ces travaux précurseurs, réalisés en grande partie au sein de l'institut océanographique du Scripps (SIO) de l'université de Californie, donnent naissance à la géomorphologie dynamique littorale en tant que discipline de recherche.
Vers une typo-chronologie des tombes à inhumation de la Préhistoire à l’orée du xxe siècle sur le territoire suisse
Authors: Gallay Audrey , Steiner Lucie , Thorimbert Sophie , Tremblay Lara 
Published: November 2024

Afin de poser les bases d’une première typo-chronologie intercantonale des tombes à inhumation de la Préhistoire au xxe s. sur le territoire suisse, un groupe de travail constitué de 23 intervenants de 8 cantons situés à l’ouest du pays a rassemblé un corpus de 1 283 sépultures, pour la plupart inédites, fouillées dans les 30 dernières années. L’analyse préliminaire d’une sélection de 817 contenants bien datés a permis d’identifier 44 types, regroupés selon les matériaux employés : bois, pierre, métal, terre cuite ou assemblages mixtes. La vaste fourchette chronologique prise en compte met en évidence des phénomènes de permanences pour certains types, mais aussi des récurrences et des particularités propres à certaines périodes, qui ouvrent de nombreuses pistes de recherche.
Les pratiques funéraires en Alsace du Néolithique à l’époque moderne. Lecture typo-chronologique des sépultures à inhumation
Authors: Mauduit Amandine , Chenal Fanny , Pélissier Amélie , Barrand-Emam Hélène 
Published: November 2024

La recherche archéologique alsacienne est emprunte d’un dynamisme historique. L’intérêt pour les sites funéraires est très ancien et a donné lieu, pour l’ensemble de la chronologie, à de nombreuses synthèses remontant parfois au xixe s. Bien que réactualisés, certains de ces travaux anciens font encore foi de nos jours. Ce dynamisme régional persiste et de nombreux projets de recherche collectifs, portés par les différents acteurs locaux, ont déjà été réalisés ou sont aujourd’hui encore en cours. Nous proposons, sur la base de ces nombreux travaux, de brosser un panorama des caractéristiques constitutives des sépultures à inhumation alsaciennes pour l’ensemble de la chronologie, du Néolithique à l’époque moderne.
Typo-chronologie des tombes à inhumation dans le nord de la France
Authors: Oudry Sophie , Durin Cécile , Gryspeirt Noémie 
Published: November 2024

Le colloque de Tours de 2009 a été l’occasion de mener pour la première fois une enquête territoriale sur la typo-chronologie des tombes à inhumation dans le nord de la France. Malgré des lacunes dans quelques zones géographiques et à certaines périodes et une représentativité variable des données à notre disposition, nous avons pu établir un premier bilan depuis les plus anciennes sépultures connues dans la région au Néolithique ancien jusqu’aux plus récentes, datées du milieu du xixe s. De grandes tendances dans l’évolution des architectures funéraires au sens large se dégagent d’ores et déjà, ce qui est très prometteur pour l’avenir, lorsque de nouvelles fouilles viendront alimenter le corpus de sépultures étudiées.
Mourir à Arpi (Pouilles, Italie du Sud) : typo-chronologie des sépultures à inhumation entre le vie et le ier siècle avant J.-C.
Authors: Leone Marcella , Munzi Priscilla 
Published: November 2024

Le site daunien d’Arpi est implanté dans la plaine alluviale du Tavoliere des Pouilles. Les premières attestations d’une occupation remontent à l’âge du Fer, mais c’est surtout à partir du ive s. que l’agglomération prend progressivement de l’importance. Le site est défini par un agger qui renferme une superficie de 1 000 ha et protège une aire destinée à accueillir non seulement l’habitat, mais aussi les nécropoles et des espaces réservés à l’agriculture et aux pâturages. Le croisement des informations fournies par la topographie des tombes, leur typologie, leur mobilier, leur chronologie et les données anthropologiques, complète les connaissances sur les transformations urbaines et sociales d’une des plus grandes agglomérations dauniennes entre le vie av. J.-C. et le ier s. ap. J.-C.
Chrono-typologie des tombes à inhumation dans les quatre départements lorrains, depuis la Préhistoire jusqu’à l’époque contemporaine. Essai de traitement massif et proposition d’évolution des pratiques dans la longue durée
Authors: Lefebvre Arnaud , Sanson Luc 
Published: November 2024

Un tableau de saisie réunissant près de 5 000 tombes fouillées en Lorraine par différents opérateurs archéologiques, cumulé à la méthode des sommes des densités de probabilité pour effectuer un séquençage chronologique a permis de proposer une évolution des typologies des tombes à inhumations en Lorraine, depuis le Néolithique jusqu’à la période contemporaine. L’effectif varie beaucoup en fonction des séquences chronologiques, ainsi que la répartition spatiale qui donne l’image des secteurs d’intervention archéologique préférentiels. Pourtant, la vision d’une évolution des types de tombes dynamique peut être proposée et peut également être mise en relation avec les régions limitrophes, comme la Champagne-Ardenne, la Bourgogne et la Franche-Comté.
La nécropole romaine de Nikaia, iie-ve siècles ap. J.-C. : un aperçu (Nice/Alpes-Maritimes)
Authors: Chevaux Brice , Civetta Aude , Jossier Bérangère , Mercurin Romuald 
Published: November 2024

Entre 2015 et 2019, les opérations d’archéologie préventive conduites par le service de l’Archéologie de Nice Côte-d’Azur à Nice (Alpes-Maritimes) ont permis de localiser la ou une des nécropoles de l’agglomération antique de Nikaia. Faisant suite à une occupation funéraire de la période massaliète (iie s. av. J.-C.), un ensemble de 35 sépultures à inhumation d’adultes et d’immatures, dont les datations s’échelonnent entre les iie et ve s., a ainsi pu être documenté.