bluuebunny/crossref_metadata_2025_split huggingface dataset:
Flight of the Bumblebee: the Early Excess Flux of Type Ia Supernova 2023bee Revealed by TESS, Swift, and Young Supernova Experiment Observations
Authors: Wang Qinan , Rest Armin , Dimitriadis Georgios , Ridden-Harper Ryan , Siebert Matthew R. , Magee Mark , Angus Charlotte R. , Auchettl Katie , Davis Kyle W. , Foley Ryan J. , Fox Ori D. , Gomez Sebastian , Jencson Jacob E. , Jones David O. , Kilpatrick Charles D. , Pierel Justin D. R. , Piro Anthony L. , Polin Abigail , Politsch Collin A. , Rojas-Bravo César , Shahbandeh Melissa , Villar V. Ashley , Zenati Yossef , Ashall C. , Chambers Kenneth C. , Coulter David A. , de Boer Thomas , DiLullo Nico , Gall Christa , Gao Hua , Hsiao Eric Y. , Huber Mark E. , Izzo Luca , Khetan Nandita , LeBaron Natalie , Magnier Eugene A. , Mandel Kaisey S. , McGill Peter , Miao Hao-Yu , Pan Yen-Chen , Stevens Catherine P. , Swift Jonathan J. , Taggart Kirsty , Yang Grace 
Published: February 2024

Abstract
We present high-cadence ultraviolet through near-infrared observations of the Type Ia supernova (SN Ia) 2023bee at D = 32 ± 3 Mpc, finding excess flux in the first days after explosion, particularly in our 10 minutes cadence TESS light curve and Swift UV data. Compared to a few other normal SNe Ia with early excess flux, the excess flux in SN 2023bee is redder in the UV and less luminous. We present optical spectra of SN 2023bee, including two spectra during the period where the flux excess is dominant. At this time, the spectra are similar to those of other SNe Ia but with weaker Si ii, C ii, and Ca ii absorption lines, perhaps because the excess flux creates a stronger continuum. We compare the data to several theoretical models on the origin of early excess flux in SNe Ia. Interaction with either the companion star or close-in circumstellar material is expected to produce a faster evolution than observed. Radioactive material in the outer layers of the ejecta, either from double detonation explosion or from a 56Ni clump near the surface, cannot fully reproduce the evolution either, likely due to the sensitivity of early UV observable to the treatment of the outer part of ejecta in simulation. We conclude that no current model can adequately explain the full set of observations. We find that a relatively large fraction of nearby, bright SNe Ia with high-cadence observations have some amount of excess flux within a few days of explosion. Considering potential asymmetric emission, the physical cause of this excess flux may be ubiquitous in normal SNe Ia.
Constraining Stellar Rotation at the Zero-age Main Sequence with TESS
Authors: Douglas S. T. , Cargile P. A. , Matt S. P. , Breimann A. A. , Pérez Chávez J. A. , Huang C. X. , Wright N. J. , Zhou G. 
Published: February 2024

Abstract
The zero-age main sequence (ZAMS) is a critical phase for stellar angular momentum evolution, as stars transition from contraction-dominated spin-up to magnetic wind-dominated spin-down. We present the first robust observational constraints on rotation for FGK stars at ≈40 Myr. We have analyzed TESS light curves for 1410 members of five young open clusters with ages between 25 and 55 Myr: IC 2391, IC 2602, NGC 2451A, NGC 2547, and Collinder 135. In total, we measure 868 rotation periods, including 96 new, high-quality periods for stars around 1 M
⊙. This is an increase of ten times the existing literature sample at the ZAMS. We then use the τ
2 method to compare our data to models for stellar angular momentum evolution. Although the ages derived from these rotation models do not match isochronal ages, we show that these observations can clearly discriminate between different models for stellar wind torques. Finally, τ
2 fits indicate that magnetic braking and/or internal angular momentum transport significantly impact rotational evolution even on the pre-main sequence.
CMZoom. IV. Incipient High-mass Star Formation throughout the Central Molecular Zone
Authors: Hatchfield H Perry , Battersby Cara , Barnes Ashley T. , Butterfield Natalie , Ginsburg Adam , Henshaw Jonathan D. , Longmore Steven N. , Lu Xing , Svoboda Brian , Walker Daniel , Callanan Daniel , Mills Elisabeth A. C. , Ho Luis C. , Kauffmann Jens , Kruijssen J. M. Diederik , Ott Jürgen , Pillai Thushara , Zhang Qizhou 
Published: February 2024

Abstract
In this work, we constrain the star-forming properties of all possible sites of incipient high-mass star formation in the Milky Way’s Galactic Center. We identify dense structures using the CMZoom 1.3 mm dust continuum catalog of objects with typical radii of ∼0.1 pc, and measure their association with tracers of high-mass star formation. We incorporate compact emission at 8, 21, 24, 25, and 70 μm from the Midcourse Space Experiment, Spitzer, Herschel, and SOFIA, cataloged young stellar objects, and water and methanol masers to characterize each source. We find an incipient star formation rate (SFR) for the Central Molecular Zone (CMZ) of ∼0.08 M
⊙ yr−1 over the next few 105 yr. We calculate upper and lower limits on the CMZ’s incipient SFR of ∼0.45 and ∼0.05 M
⊙ yr−1,respectively, spanning roughly equal to and several times greater than other estimates of CMZ’s recent SFR. Despite substantial uncertainties, our results suggest the incipient SFR in the CMZ may be higher than previously estimated. We find that the prevalence of star formation tracers does not correlate with source volume density, but instead ≳75% of high-mass star formation is found in regions above a column density ratio (N
SMA/N
Herschel) of ∼1.5. Finally, we highlight the detection of atoll sources, a reoccurring morphology of cold dust encircling evolved infrared sources, possibly representing H ii regions in the process of destroying their envelopes.
The Factory and the Beehive. V. Chromospheric and Coronal Activity and Its Dependence on Rotation in Praesepe and the Hyades
Authors: Núñez Alejandro , Agüeros Marcel A. , Curtis Jason L. , Covey Kevin R. , Douglas Stephanie T. , Chu Sabine R. , DeLaurentiis Stanislav , Wang Minzhi (Luna) , Drake Jeremy J. 
Published: February 2024

Abstract
Low-mass (≲1.2 M
⊙) main-sequence stars lose angular momentum over time, leading to a decrease in their magnetic activity. The details of this rotation–activity relation remain poorly understood, however. Using observations of members of the ≈700 Myr old Praesepe and Hyades open clusters, we aim to characterize the rotation–activity relation for different tracers of activity at this age. To complement published data, we obtained new optical spectra for 250 Praesepe stars, new X-ray detections for 10, and new rotation periods for 28. These numbers for Hyads are 131, 23, and 137, respectively. The latter increases the number of Hyads with periods by 50%. We used these data to measure the fractional Hα and X-ray luminosities, L
Hα
/L
bol and L
X/L
bol, and to calculate Rossby numbers R
o. We found that at ≈700 Myr almost all M dwarfs exhibit Hα emission, with binaries having the same overall color–Hα equivalent width distribution as single stars. In the R
o–L
Hα
/L
bol plane, unsaturated single stars follow a power law with index β = −5.9 ± 0.8 for R
o > 0.3. In the R
o–L
X/L
bol plane, we see evidence for supersaturation for single stars with R
o ≲ 0.01, following a power law with index

β

sup

=

0.5

−
0.1

+
0.2

, supporting the hypothesis that the coronae of these stars are being centrifugally stripped. We found that the critical R
o value at which activity saturates is smaller for L
X/L
bol than for L
Hα
/L
bol. Finally, we observed an almost 1:1 relation between L
Hα
/L
bol and L
X/L
bol, suggesting that both the corona and the chromosphere experience similar magnetic heating.
Validation of Elemental and Isotopic Abundances in Late-M Spectral Types with the Benchmark HIP 55507 AB System
Authors: Xuan Jerry W. , Wang Jason , Finnerty Luke , Horstman Katelyn , Grimm Simon , Peck Anne E. , Nielsen Eric , Knutson Heather A. , Mawet Dimitri , Isaacson Howard , Howard Andrew W. , Liu Michael C. , Walker Sam , Phillips Mark W. , Blake Geoffrey A. , Ruffio Jean-Baptiste , Zhang Yapeng , Inglis Julie , Wallack Nicole L. , Sanghi Aniket , Gonzales Erica J. , Dai Fei , Baker Ashley , Bartos Randall , Bond Charlotte Z. , Bryan Marta L. , Calvin Benjamin , Cetre Sylvain , Delorme Jacques-Robert , Doppmann Greg , Echeverri Daniel , Fitzgerald Michael P. , Jovanovic Nemanja , Liberman Joshua , López Ronald A. , Martin Emily C. , Morris Evan , Pezzato Jacklyn , Ruane Garreth , Sappey Ben , Schofield Tobias , Skemer Andrew , Venenciano Taylor , Wallace J. Kent , Wang Ji , Wizinowich Peter , Xin Yinzi , Agrawal Shubh , Do Ó Clarissa R. , Hsu Chih-Chun , Phillips Caprice L. 
Published: February 2024

Abstract
M dwarfs are common host stars to exoplanets but often lack atmospheric abundance measurements. Late-M dwarfs are also good analogs to the youngest substellar companions, which share similar T
eff ∼ 2300–2800 K. We present atmospheric analyses for the M7.5 companion HIP 55507 B and its K6V primary star with Keck/KPIC high-resolution (R ∼ 35,000) K-band spectroscopy. First, by including KPIC relative radial velocities between the primary and secondary in the orbit fit, we improve the dynamical mass precision by 60% and find

M

B

=

88.0

−
3.2

+
3.4

M

Jup

, putting HIP 55507 B above the stellar–substellar boundary. We also find that HIP 55507 B orbits its K6V primary star with

a
=

38

−
3

+
4

au and e = 0.40 ± 0.04. From atmospheric retrievals of HIP 55507 B, we measure [C/H] = 0.24 ± 0.13, [O/H] = 0.15 ± 0.13, and C/O = 0.67 ± 0.04. Moreover, we strongly detect 13CO (7.8σ significance) and tentatively detect

H

2

18

O

(3.7σ significance) in the companion’s atmosphere and measure

12

CO

/

13

CO
=

98

−
22

+
28

and

H

2

16

O

/

H

2

18

O
=

240

−
80

+
145

after accounting for systematic errors. From a simplified retrieval analysis of HIP 55507 A, we measure

12

CO

/

13

CO
=

79

−
16

+
21

and

C

16

O

/

C

18

O
=

288

−
70

+
125

for the primary star. These results demonstrate that HIP 55507 A and B have consistent 12C/13C and 16O/18O to the <1σ level, as expected for a chemically homogeneous binary system. Given the similar flux ratios and separations between HIP 55507 AB and systems with young substellar companions, our results open the door to systematically measuring 13CO and

H

2

18

O

abundances in the atmospheres of substellar or even planetary-mass companions with similar spectral types.
Disruption of Dark Matter Minihalos in the Milky Way Environment: Implications for Axion Miniclusters and Early Matter Domination
Authors: Shen Xuejian , Xiao Huangyu , Hopkins Philip F. , Zurek Kathryn M. 
Published: February 2024

Abstract
Many theories of dark matter beyond the weakly interacting massive particles paradigm feature an enhanced matter power spectrum on subparsec scales, leading to the formation of dense dark matter minihalos. Future local observations are promising to search for and constrain such substructures. The survival probability of these dense minihalos in the Milky Way environment is crucial for interpreting local observations. In this work, we investigate two environmental effects: stellar disruption and (smooth) tidal disruption. These two mechanisms are studied using semianalytic models and idealized N-body simulations. For stellar disruption, we perform a series of N-body simulations of isolated minihalo–star encounters to test and calibrate analytic models of stellar encounters before applying the model to the realistic Milky Way disk environment. For tidal disruption, we perform N-body simulations to confirm the effectiveness of the analytic treatment. Finally, we propose a framework to combine the hierarchical assembly and infall of minihalos to the Milky Way with the late-time disruption mechanisms. We make predictions for the mass functions of minihalos in the Milky Way. The mass survival fraction (at M
mh ≥ 10−12
M
⊙) of dense dark matter minihalos, e.g., for axion miniclusters and minihalos from early matter domination, is ∼60% with the relatively low-mass, compact population surviving. The survival fraction is insensitive to the detailed model parameters. We discuss various implications of the framework and future direct detection prospects.
MINDS. JWST/MIRI Reveals a Dynamic Gas-rich Inner Disk inside the Cavity of SY Cha
Authors: Schwarz Kamber R. , Henning Thomas , Christiaens Valentin , Gasman Danny , Samland Matthias , Perotti Giulia , Jang Hyerin , Grant Sierra L. , Tabone Benoît , Morales-Calderón Maria , Kamp Inga , van Dishoeck Ewine F. , Güdel Manuel , Lagage Pierre-Olivier , Barrado David , Caratti o Garatti Alessio , Glauser Adrian M. , Ray Tom P. , Vandenbussche Bart , Waters L. B. F. M. , Arabhavi Aditya M. , Kanwar Jayatee , Olofsson Göran , Rodgers-Lee Donna , Schreiber Jürgen , Temmink Milou 
Published: February 2024

Abstract
SY Cha is a T Tauri star surrounded by a protoplanetary disk with a large cavity seen in the millimeter continuum but has the spectral energy distribution of a full disk. Here we report the first results from JWST/Mid-InfraRed Instrument (MIRI) Medium Resolution Spectrometer (MRS) observations taken as part of the MIRI mid-INfrared Disk Survey (MINDS) GTO Program. The much improved resolution and sensitivity of MIRI-MRS compared to Spitzer enables a robust analysis of the previously detected H2O, CO, HCN, and CO2 emission as well as a marginal detection of C2H2. We also report the first robust detection of mid-infrared OH and rovibrational CO emission in this source. The derived molecular column densities reveal the inner disk of SY Cha to be rich in both oxygen- and carbon-bearing molecules. This is in contrast to PDS 70, another protoplanetary disk with a large cavity observed with JWST, which displays much weaker line emission. In the SY Cha disk, the continuum, and potentially the line, flux varies substantially between the new JWST observations and archival Spitzer observations, indicative of a highly dynamic inner disk.
Typical X-Ray Outburst Light Curves of Aql X-1
Authors: Çoban Ömer Faruk , Ertan Ünal 
Published: February 2024

Abstract
We show that the typical X-ray outburst light curve of Aql X-1 can be reproduced by accretion onto a neutron star in the frame of the disk instability model without invoking partial accretion or the propeller effect. The knee and the subsequent sharp decay in the X-ray light curve can be generated naturally by taking into account the weak dependence of the disk aspect ratio, h/r, on the disk mass-flow rate,

M

̇

in

, in the X-ray irradiation flux calculation. This

M

̇

in

dependence of h/r only slightly modifies the irradiation temperature profile along the hot disk in comparison to that obtained with a constant h/r. Nevertheless, this small difference has a significant cumulative effect on the hot disk radius, leading to a much faster decrease in the size of the hot disk and thereby to a sharper decay in the X-ray outburst light curve. The same model also produces the long-term evolution of Aql X-1, consistent with its observed outburst recurrence time and typical light curve. Our results imply that the source accretes matter from the disk in the quiescent state as well. We also estimate that the dipole moment of the source μ ≲ 4 × 1026 G cm3 (B ≲ 4 × 108 G at the surface).
The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: Deka P. P. , Gupta N. , Jagannathan P. , Sekhar S. , Momjian E. , Bhatnagar S. , Wagenveld J. , Klöckner H.-R. , Jose J. , Balashev S. A. , Combes F. , Hilton M. , Borgaonkar D. , Chatterjee A. , Emig K. L. , Gaunekar A. N. , Józsa G. I. G. , Klutse D. Y. , Knowles K. , Krogager J.-K. , Mohapatra A. , Moodley K. , Muller Sébastien , Noterdaeme P. , Petitjean P. , Salas P. , Sikhosana S. 
Published: February 2024

Abstract
The MeerKAT Absorption Line Survey (MALS) has observed 391 telescope pointings at the L band (900–1670 MHz) at δ ≲ +20°. We present radio continuum images and a catalog of 495,325 (240,321) radio sources detected at a signal-to-noise ratio (S/N) > 5 over an area of 2289 deg2 (1132 deg2) at 1006 MHz (1381 MHz). Every MALS pointing contains a central bright radio source (S
1 GHz ≳ 0.2 Jy). The median spatial resolution is 12″ (8″). The median rms noise away from the pointing center is 25 μJy beam−1 (22 μJy beam−1) and is within ∼15% of the achievable theoretical sensitivity. The flux density scale ratio and astrometric accuracy deduced from multiply observed sources in MALS are <1% (8% scatter) and 1″, respectively. Through comparisons with NVSS and FIRST at 1.4 GHz, we establish the catalog’s accuracy in the flux density scale and astrometry to be better than 6% (15% scatter) and 0.″8, respectively. The median flux density offset is higher (9%) for an alternate beam model based on holographic measurements. The MALS radio source counts at 1.4 GHz are in agreement with literature. We estimate spectral indices (α) of a subset of 125,621 sources (S/N > 8), confirm the flattening of spectral indices with decreasing flux density, and identify 140 ultra-steep-spectrum (α < −1.3) sources as prospective high-z radio galaxies (z > 2). We have identified 1308 variable and 122 transient radio sources comprising primarily active galactic nuclei that demonstrate long-term (26 yr) variability in their observed flux densities. The MALS catalogs and images are publicly available at https://mals.iucaa.in.
Fierce Feedback in an Obscured, Sub-Eddington State of the Seyfert 1.2 Markarian 817
Authors: Zak Miranda K. , Miller Jon M. , Behar Ehud , Brandt W. N. , Brenneman Laura , Draghis Paul A. , Kammoun Elias , Koss Michael J. , Reynolds Mark T. , Zoghbi Abderahmen 
Published: February 2024

Abstract
Mrk 817 is a bright and variable Seyfert 1.2 active galactic nucleus (AGN). X-ray monitoring of Mrk 817 with the Neil Gehrels Swift Observatory in 2022 revealed that the source flux had declined to a lower level than recorded at any prior point in the then 19 yr mission. We present an analysis of deep XMM-Newton and NuSTAR observations obtained in this low flux state. The spectra reveal a complex X-ray wind consisting of neutral and ionized absorption zones. Three separate velocity components are detected as part of a structured ultrafast outflow (UFO), with

v

/

c

=

0.043

−
0.003

+
0.007

,

v

/

c

=

0.079

−
0.0008

+
0.003

, and

v

/

c

=

0.074

−
0.005

+
0.004

. These projected velocities suggest that the wind likely arises at radii that are much smaller than the optical broad-line region. In order for each component of the outflow to contribute significant feedback, the volume filling factors must be greater than f ≃ 0.009, f ≃ 0.003, and f ≃ 0.3, respectively. For plausible, data-driven volume filling factors, these limits are passed, and the total outflow likely delivers the fierce feedback required to reshape its host environment, despite a modest radiative Eddington fraction of λ ≃ 0.008–0.016 (this range reflects plausible masses). UFOs are often detected at or above the Eddington limit; this result signals that black hole accretion has the potential to shape host galaxies even at modest Eddington fractions and over a larger fraction of a typical AGN lifetime. We discuss our findings in terms of models for disk winds and black hole feedback in this and other AGN.
Atmospheric Loss in Giant Impacts Depends on Preimpact Surface Conditions
Authors: Lock Simon J. , Stewart Sarah T. 
Published: February 2024

Abstract
Earth likely acquired much of its inventory of volatile elements during the main stage of its formation. Some of Earth’s proto-atmosphere must therefore have survived the giant impacts, collisions between planet-sized bodies, that dominate the latter phases of accretion. Here, we use a suite of 1D hydrodynamic simulations and impedance-match calculations to quantify the effect that preimpact surface conditions (such as atmospheric pressure and the presence of an ocean) have on the efficiency of atmospheric and ocean loss from protoplanets during giant impacts. We find that—in the absence of an ocean—lighter, hotter, and lower-pressure atmospheres are more easily lost. The presence of an ocean can significantly increase the efficiency of atmospheric loss compared to the no-ocean case, with a rapid transition between low- and high-loss regimes as the mass ratio of atmosphere to ocean decreases. However, contrary to previous thinking, the presence of an ocean can also reduce atmospheric loss if the ocean is not sufficiently massive, typically less than a few times the atmospheric mass. Volatile loss due to giant impacts is thus highly sensitive to the surface conditions on the colliding bodies. To allow our results to be combined with 3D impact simulations, we have developed scaling laws that relate loss to the ground velocity and surface conditions. Our results demonstrate that the final volatile budgets of planets are critically dependent on the exact timing and sequence of impacts experienced by their precursor planetary embryos, making atmospheric properties a highly stochastic outcome of accretion.
« Les institutions internationales ne sont plus adaptées »
Authors: Mbembe Achille , Lafortune Guillaume , Hervieu-Léger Benoît 
Published: February 2024

Bâti au mitan du XX e siècle, le système financier international peine à tenir l’enjeu du développement durable dans un monde plombé par les inégalités. Quelles pistes feraient bouger les lignes ? Dialogue entre le politologue et historien Achille Mbembe et Guillaume Lafortune, vice-président du réseau des Nations unies de solutions pour le développement durable.
Les grandes espérances : la Grande-Bretagne et l’inclusion de la Russie soviétique et post-soviétique dans le système de sécurité européen (1984-1994)
Authors: Guderzo Massimiliano , Guderzo Massimiliano 
Published: February 2024

L’article veut contribuer au thème de l’inclusion/exclusion de la Russie dans les organisations régionales à la fin de la guerre froide et peu après, avec une référence particulière à l’intégration européenne et atlantique. Quels ont été la perception et le rôle de Londres face aux initiatives de Mikhaïl Gorbatchev dans les années où l’Union soviétique pouvait encore être perçue comme une superpuissance, bien qu’en déclin, puis face à la Fédération de Russie dans les premières années de l’administration Eltsine ? Des éléments de continuité ou de discontinuité ont-ils prévalu dans la transition Thatcher-Major en 1990 ? Dans quelle mesure la politique britannique a-t‑elle influencé les politiques européennes dans la sphère atlantique et au moment très délicat de la constitution de l’Union européenne ? L’article vise aussi à étudier l’hypothèse qui voit dans l’échec du décollage d’un sujet fédéral européen fort au début des années 1990 l’une des principales causes du désordre international des trente dernières années.
Du théâtre à l’écran. Desideria et la satire sociale dans le cinéma chilien dans les années 1940
Authors: Núñez Fabián 
Published: February 2024

Desideria est le personnage le plus célèbre créé par Ana González qui a donné la parole à une catégorie sociale nouvellement formée au Chili : les employées de maison. Notre objectif est de raconter la genèse du personnage et d’analyser le film P’al otro lao.
El humor en el cine chicano contemporáneo. Parodia y transnacionalismo en la trilogía de El Mariachi de Robert Rodriguez
Authors: Gregorio Fernández Noelia 
Published: February 2024

Este artículo analiza los aspectos paródicos en cuanto a la representación del personaje masculino en la trilogía de El Mariachi de Robert Rodriguez, como estrategia alternativa a los estereotipos cinematográficos del latino en el cine.
Paul Leduc a toujours été là
Authors: Rodríguez Israel 
Published: February 2024

Paul leduc était un cinéaste qui a toujours conservé son indépendance, refusant constamment les aides d’état. Il a choisi de développer une œuvre critique et militante. Elle est le portrait des luttes sociales et politiques du Mexique et de l’Amérique latine des dernières décennies du XXe siècle.