bluuebunny/crossref_metadata_2025 huggingface dataset:
The POKEMON Speckle Survey of Nearby M Dwarfs. II. Observations of 1125 Targets
Authors: Clark Catherine A. , van Belle Gerard T. , Horch Elliott P. , Lund Michael B. , Ciardi David R. , von Braun Kaspar , Winters Jennifer G. , Everett Mark E. , Hartman Zachary D. , Llama Joe
Published: January 2024

Stellar multiplicity is correlated with many stellar properties, yet multiplicity measurements have proven difficult for the M dwarfs—the most common type of star in our galaxy—due to their faintness and the fact that a reasonably complete inventory of later M dwarfs did not exist until recently. We have therefore carried out the Pervasive Overview of “Kompanions” of Every M dwarf in Our Neighborhood (POKEMON) survey, which made use of the Differential Speckle Survey Instrument on the 4.3 m Lowell Discovery Telescope, along with the NN-EXPLORE Exoplanet Stellar Speckle Imager on the 3.5 m WIYN telescope. The POKEMON sample is volume limited from M0V through M9V out to 15 pc, with additional brighter targets at larger distances. In total, 1125 targets were observed. New discoveries were presented in the first paper in the series. In this second paper in the series, we present all detected companions, gauge our astrometric and photometric precision, and compare our filtered and filterless speckle observations. We find that the majority (58.9%) of the companions we detect in our speckle images are not resolved in Gaia, demonstrating the need for high-resolution imaging in addition to long-term astrometric monitoring. Additionally, we find that the majority (73.2%) of simulated stellar companions would be detectable by our speckle observations. Specifically within 100 au, we find that 70.3% of simulated companions are recovered. Finally, we discuss future directions of the POKEMON survey.
Kepler-discovered Multiple-planet Systems near Period Ratios Suggestive of Mean-motion Resonances Are Young
Authors: Hamer Jacob H. , Schlaufman Kevin C.
Published: January 2024

Before the launch of the Kepler Space Telescope, models of low-mass planet formation predicted that convergent type I migration would often produce systems of low-mass planets in low-order mean-motion resonances. Instead, Kepler discovered that systems of small planets frequently have period ratios larger than those associated with mean-motion resonances and rarely have period ratios smaller than those associated with mean-motion resonances. Both short-timescale processes related to the formation or early evolution of planetary systems and long-timescale secular processes have been proposed as explanations for these observations. Using a thin disk stellar population’s Galactic velocity dispersion as a relative age proxy, we find that Kepler-discovered multiple-planet systems with at least one planet pair near a period ratio suggestive of a second-order mean-motion resonance have a colder Galactic velocity dispersion and are therefore younger than both single-transiting and multiple-planet systems that lack planet pairs consistent with mean-motion resonances. We argue that a nontidal secular process with a characteristic timescale no less than a few hundred Myr is responsible for moving systems of low-mass planets away from second-order mean-motion resonances. Among systems with at least one planet pair near a period ratio suggestive of a first-order mean-motion resonance, only the population of systems likely affected by tidal dissipation inside their innermost planets has a small Galactic velocity dispersion and is therefore young. We predict that period ratios suggestive of mean-motion resonances are more common in young systems with 10 Myr ≲ τ ≲ 100 Myr and become less common as planetary systems age.
Disappearing Galaxies: The Orientation Dependence of JWST-bright, HST-dark, Star-forming Galaxy Selection
Authors: Cochrane R. K. , Anglés-Alcázar D. , Cullen F. , Hayward C. C.
Published: January 2024

Galaxies that are invisible in deep optical–near-infrared imaging but detected at longer wavelengths have been the focus of several recent observational studies, with speculation that they could constitute a substantial missing population and even dominate the cosmic star formation rate density at z ≳ 4. The depths now achievable with JWST at the longest wavelengths probed by the Hubble Space Telescope (HST), coupled with the transformative resolution at longer wavelengths, are already enabling detailed, spatially resolved characterization of sources that were invisible to HST, often known as “HST-dark” galaxies. However, until now, there has been little theoretical work to compare against. We present the first simulation-based study of this population, using highly resolved galaxies from the Feedback in Realistic Environments project, with multiwavelength images along several lines of sight forward-modeled using radiative transfer. We naturally recover a population of modeled sources that meet commonly used selection criteria (H
AB > 27 mag and H
AB − F444W > 2.3). These simulated HST-dark galaxies lie at high redshifts (z = 4–7), have high levels of dust attenuation (A

V
= 2–4), and display compact recent star formation (R
1/2,4.4 μm ≲ 1 kpc). Orientation is very important: for all but one of the 17 simulated galaxy snapshots with HST-dark sight lines, there exist other sight lines that do not meet the criteria. This result has important implications for comparisons between observations and models that do not resolve the detailed star-dust geometry, such as semianalytic models or coarsely resolved hydrodynamical simulations. Critically, we demonstrate that HST-dark sources are not an unexpected or exotic population, but a subset of high-redshift, highly dust-attenuated sources viewed along certain lines of sight.
A Pathway for Collisional Planetesimal Growth in the Ice-dominant Regions of Protoplanetary Disks
Authors: Yunerman Elizabeth , Powell Diana , Murray-Clay Ruth
Published: January 2024

We present a semi-analytic model for the growth, drift, desorption, and fragmentation of millimeter- to meter-sized particles in protoplanetary disks. Fragmentation occurs where particle collision velocities exceed critical fragmentation velocities. Using this criterion, we produce fragmentation regions in disk orbital radius–particle size phase space for particles with a range of material properties, structures, and compositions (including SiO2, Mg2SiO4, H2O, CO2, and CO). For reasonable disk conditions, compact aggregate H2O, CO2, and CO ice particles do not reach destructive relative velocities and are thus not likely to undergo collisional fragmentation. Uncoated silicate particles are more susceptible to collisional destruction and are expected to fragment in the inner disk, consistent with previous work. We then calculate the growth, drift, and sublimation of small particles, initially located in the outer disk. We find that ice-coated particles can avoid fragmentation as they grow and drift inward under a substantial range of disk conditions, as long as the particles are aggregates composed of 0.1 μm-sized monomers. Such particles may undergo runaway growth in disk regions abundant in H2O or CO2 ice, depending on the assumed disk temperature structure. These results indicate that icy collisional growth to planetesimally relevant sizes may happen efficiently throughout a disk’s lifetime, and is particularly robust at early times when the disk’s dust-to-gas ratio is comparable to that of the interstellar medium.
Synthetic Observations of the Infalling Rotating Envelope: Links between the Physical Structure and Observational Features
Authors: Mori Shoji , Aikawa Yuri , Oya Yoko , Yamamoto Satoshi , Sakai Nami
Published: January 2024

We performed synthetic observations of the Ulrich, Cassen, and Moosman (UCM) model to understand the relation between the physical structures of the infalling envelope around a protostar and their observational features in molecular lines, adopting L1527 as an example. We also compared the physical structure and synthetic position–velocity (P–V) diagrams of the UCM model and a simple ballistic (SB) model. There are multiple ways to compare synthetic data with observational data. We first calculated the correlation coefficient. The UCM model and the SB model show similarly good correlation with the observational data. While the correlation reflects the overall similarity between the cube datasets, we can alternatively compare specific local features, such as the centrifugal barrier in the SB model or the centrifugal radius in the UCM model. We evaluated systematic uncertainties in these methods. In the case of L1527, the stellar mass values estimated using these methods are all lower than the value derived from previous Keplerian analysis of the disk. This may indicate that the gas infall motion in the envelope is retarded by, e.g., magnetic fields. We also showed analytically that, in the UCM model, the spin-up feature of the P–V diagram is due to the infall velocity rather than the rotation. The line-of-sight velocity V is thus ∝x
−0.5, where x is the offset. If the infall is retarded, rotational velocity should dominate so that V is proportional to x
−1, as is often observed in the protostellar envelope.
Dual-band Observations of the Asymmetric Ring around CIDA 9A: Dead or Alive?
Authors: Harsono Daniel , Long Feng , Pinilla Paola , Rota Alessia A. , Manara Carlo F. , Herczeg Gregory J. , Johnstone Doug , Rosotti Giovanni , Lodato Giuseppe , Menard Francois , Tazzari Marco , Shi Yangfan
Published: January 2024

While the most exciting explanation of the observed dust asymmetries in protoplanetary disks is the presence of protoplanets, other mechanisms can also form the dust features. This paper presents dual-wavelength Atacama Large Millimeter/submillimeter Array observations of a large asymmetric dusty ring around the M-type star CIDA 9A. We detect a dust asymmetry in both 1.3 and 3.1 mm data. To characterize the asymmetric structure, a parametric model is used to fit the observed visibilities. We report a tentative azimuthal shift of the dust emission peaks between the observations at the two wavelengths. This shift is consistent with a dust trap caused by a vortex, which may be formed by an embedded protoplanet or other hydrodynamical instabilities, such as a dead zone. Deep high-spatial-resolution observations of dust and molecular gas are needed to constrain the mechanisms that formed the observed millimeter cavity and dust asymmetry in the protoplanetary disk around CIDA 9A.
LATIS: Constraints on the Galaxy–Halo Connection at z ∼ 2.5 from Galaxy–Galaxy and Galaxy–Lyα Clustering
Authors: Newman Andrew B. , Qezlou Mahdi , Chartab Nima , Rudie Gwen C. , Blanc Guillermo A. , Bird Simeon , Benson Andrew J. , Kelson Daniel D. , Lemaux Brian C.
Published: January 2024

The connection between galaxies and dark matter halos is often quantified using the stellar mass–halo mass (SMHM) relation. Optical and near-infrared imaging surveys have led to a broadly consistent picture of the evolving SMHM relation based on measurements of galaxy abundances and angular correlation functions. Spectroscopic surveys at z ≳ 2 can also constrain the SMHM relation via the galaxy autocorrelation function and through the cross-correlation between galaxies and Lyα absorption measured in transverse sight lines; however, such studies are very few and have produced some unexpected or inconclusive results. We use ∼3000 spectra of z ∼ 2.5 galaxies from the Lyα Tomography IMACS Survey (LATIS) to measure the galaxy–galaxy and galaxy–Lyα correlation functions in four bins of stellar mass spanning 109.2 ≲ M
*/M
⊙ ≲ 1010.5. Parallel analyses of the MultiDark N-body and ASTRID hydrodynamic cosmological simulations allow us to model the correlation functions, estimate covariance matrices, and infer halo masses. We find that results of the two methods are mutually consistent and broadly accord with standard SMHM relations. This consistency demonstrates that we are able to measure and model Lyα transmission fluctuations δ

F
in LATIS accurately. We also show that the galaxy–Lyα cross-correlation, a free by-product of optical spectroscopic galaxy surveys at these redshifts, can constrain halo masses with similar precision to galaxy–galaxy clustering.
Chandra X-Ray Observatory Observations of 13 Fermi LAT Sources
Authors: Rangelov Blagoy , Yang Hui , Williams Brice , Kargaltsev Oleg , Hare Jeremy , Martinic Kean
Published: January 2024

In the latest data release from the Fermi Gamma-ray Space Telescope (the 4th Fermi LAT 14 yr Catalog, or 4FGL), more than 50% of the Galactic sources are yet to be identified. We observed 13 unidentified Fermi LAT sources with the Chandra X-Ray Observatory to explore their nature. We report the results of the classification of X-ray sources in the fields of these γ-ray sources and discuss the implications for their nature. We use multiwavelength (MW) data for a machine-learning classification, accompanied by a more detailed spectral/variability analysis for brighter sources. Eight 4FGL sources have γ-ray pulsars within their position error ellipses. We consider three of these pulsars (PSR J1906+0722, PSR J1105–6037, and PSR J1358–6025) to be detected in X-rays, while PSR J1203–6242 shows a hint of X-ray emission. Within the positional uncertainties of three of the 4FGL sources, we detect X-ray sources that may be yet unknown pulsars, depending on the MW association. In addition to point sources, we discovered two extended sources, one of which is likely to be a bow-shock pulsar-wind nebula associated with PSR J1358–6025. Finally, we classify other X-ray sources detected in these observations and report the most interesting classifications.
Evidence of Third Dredge-up in Post-AGB Stars in Galactic Globular Clusters
Authors: Dixon William V.
Published: January 2024

To better understand the mixing and mass loss experienced by low-mass stars as they ascend the asymptotic giant branch (AGB), I have gathered from the literature the abundances of CNO and s-process elements in post-AGB stars in Galactic globular clusters. These species are mixed to the surface during third dredge-up (3DU) events, so their abundance should increase as the star ascends the AGB. Of the 17 stars in this sample, CNO abundances are available for 11. Of these, four are enhanced in CNO relative to the red giant branch stars from which they descended, which I take as evidence of 3DU on the AGB. The enhancement is mainly in the form of carbon. Of the six stars for which only heavy-element abundances are available, one shows s-process enhancements that previous authors have interpreted as evidence of 3DU. Combining these 17 stars with other recent samples reveals that most globular-cluster post-AGB stars have luminosities

log
(
L

/

L

⊙

)
∼
3.25

. They are the progeny of blue horizontal-branch (HB) stars in clusters with intermediate metallicity ([Fe/H] ∼ −1.5). A second group consists of sub-luminous stars associated with high-metallicity clusters ([Fe/H] ∼ −1.0) with red HBs. They may be burning helium, rather than hydrogen. A third group of hot, super-luminous stars is evolving quickly across the Hertzsprung–Russell diagram. Some of them may be merger remnants.
Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. I. Discovery of Prominence Eruptions Associated with Superflares
Authors: Namekata Kosuke , Airapetian Vladimir S. , Petit Pascal , Maehara Hiroyuki , Ikuta Kai , Inoue Shun , Notsu Yuta , Paudel Rishi R. , Arzoumanian Zaven , Avramova-Boncheva Antoaneta A. , Gendreau Keith , Jeffers Sandra V. , Marsden Stephen , Morin Julien , Neiner Coralie , Vidotto Aline A. , Shibata Kazunari
Published: January 2024

Young solar-type stars frequently produce superflares, serving as a unique window into the young Sun-Earth environments. Large solar flares are closely linked to coronal mass ejections (CMEs) associated with filament/prominence eruptions, but observational evidence for stellar superflares remains scarce. Here, we present a 12-day, multiwavelength campaign observation of young solar-type star EK Draconis (G1.5V, 50–120 Myr age) utilizing the Transiting Exoplanet Survey Satellite, the Neutron star Interior Composition ExploreR, and the Seimei telescope. The star has previously exhibited blueshifted Hα absorptions as evidence for a filament eruption associated with a superflare. Our simultaneous optical and X-ray observations identified three superflares of 1.5 × 1033–1.2 × 1034 erg. We report the first discovery of two prominence eruptions on a solar-type star, observed as blueshifted Hα emissions at speeds of 690 and 430 km s−1 and masses of 1.1 × 1019 and 3.2 × 1017 g, respectively. The faster, massive event shows a candidate of post-flare X-ray dimming with the amplitude of up to ∼10%. Several observational aspects consistently point to the occurrence of a fast CME associated with this event. The comparative analysis of the estimated length scales of flare loops, prominences, possible dimming region, and starspots provides the overall picture of the eruptive phenomena. Furthermore, the energy partition of the observed superflares in the optical and X-ray bands is consistent with flares from the Sun, M-dwarfs, and close binaries, yielding the unified empirical relations. These discoveries provide profound implications of the impact of these eruptive events on early Venus, Earth, and Mars and young exoplanets.
A Numerical Study of the Effects of a Corotating Interaction Region on Cosmic-Ray Transport. II. Features of Cosmic-Ray Composition and Rigidity
Authors: Luo Xi , Potgieter Marius S. , Zhang Ming , Shen Fang
Published: January 2024

We continue the numerical modeling of a corotating interaction region (CIR) and the effects it has on solar-rotational recurrent variations of galactic cosmic rays (GCRs). A magnetohydrodynamic model is adapted to simulate the background solar wind plasma with a CIR structure in the inner heliosphere, which is incorporated into a comprehensive Parker-type transport model. The focus is on the simulation of the effects of a CIR on GCR protons and the two helium isotopes as a function of heliolongitude. This is to establish whether the difference in composition affects how they are modulated by the CIR in terms of their distribution in longitude. It is demonstrated that particle diffusion and drift influence the effects of the CIR with increasing rigidity from 100 MV up to 15 GV. It is found that protons and helium isotopes are modulated differently with longitude by the CIR and that particle drift influences the modulation effects in longitude. These differences dissipate with increasing rigidity. The final results are focused on the simulated amplitude of these GCR flux variations as a function of rigidity. The amplitude displays a power-law behavior above ∼1 GV with an index similar to the power index of the rigidity dependence of the assumed diffusion coefficients. The simulations further show that below this rigidity, the amplitude at first flattens off, displaying a plateau-like profile, but it then increases systematically with decreasing rigidity below ∼0.3 GV. Again, a power-law behavior is displayed, but it is completely different from that above 1 GV.
JWST Confirms the Nature of CID-42
Authors: Li Junyao , Zhuang Ming-Yang , Shen Yue
Published: January 2024

The galaxy CID-42 (CXOC J100043.1+020637.2) at z = 0.359 has been proposed to contain a promising candidate for a gravitational-wave recoiling supermassive black hole (SMBH), a slingshot SMBH from a triple-SMBH interaction, or a kiloparsec-scale dual active galactic nucleus (AGN). These claims were primarily based on a pair of bright cores separated by ∼0.″5 resolved in optical Hubble Space Telescope (HST) imaging. Existing HST, Chandra, and ground-based imaging and spectroscopy are unable to confirm either scenario. With improved spatial resolution, depth, and IR wavelength coverage, NIRCam multiband imaging from the COSMOS-Web JWST treasury program well resolved the two cores in CID-42, revealing a significant stellar bulge for both cores (with stellar masses of ∼1010
M
⊙ for both). JWST imaging further revealed that only the SE core contains an unobscured AGN point source, based on both image decomposition and spectral energy distribution fitting. There is no evidence for AGN activity in the NW core based on the current data. These new observations unambiguously rule out the gravitational-wave-recoiling and slingshot-SMBH scenarios and establish CID-42 as a low-redshift merging pair of galaxies, with likely only one active AGN in the system. These results demonstrate the unparalleled capabilities of JWST (even with imaging alone) in studying the galactic-scale environment of merging galaxies and SMBHs.
Volume Density Structure of the Central Molecular Zone NGC 253 through ALCHEMI Excitation Analysis
Authors: Tanaka Kunihiko , Mangum Jeffrey G. , Viti Serena , Martín Sergio , Harada Nanase , Sakamoto Kazushi , Muller Sebastien , Yoshimura Yuki , Nakanishi Kouichiro , Herrero-Illana Rubén , Emig Kimberly L. , Mühle S. , Kaneko Hiroyuki , Tosaki Tomoka , Behrens Erica , Rivilla Víctor M. , Colzi Laura , Nishimura Yuri , Humire P. K. , Bouvier Mathilde , Huang Ko-Yun , Butterworth Joshua , Meier David S. , van der Werf Paul P.
Published: January 2024

We present a spatially resolved excitation analysis for the central molecular zone (CMZ) of the starburst galaxy NGC 253 using the data from the Atacama Large Millimeter/submillimeter Array Comprehensive High-resolution Extragalactic Molecular Inventory, whereby we explore parameters distinguishing NGC 253 from the quiescent Milky Way’s Galactic center (GC). Non-LTE analyses employing a hierarchical Bayesian framework are applied to Band 3–7 transitions from nine molecular species to delineate the position–position–velocity distributions of column density (

N

H

2

), volume density (

n

H

2

), and temperature (T
kin) at 27 pc resolution. Two distinct components are detected: a low-density component with

(

n

H

2

,

T

kin

)
∼
(

10

3.3

cm

−
3

,
85

K
)

and a high-density component with

(

n

H

2

,

T

kin

)

∼
(

10

4.4

cm

−
3

,
110

K
)

, separated at

n

H

2

∼

10

3.8

cm

−
3

. NGC 253 has ∼10 times the high-density gas mass and ∼3 times the dense-gas mass fraction of the GC. These properties are consistent with their HCN/CO ratio but cannot alone explain the factor of ∼30 difference in their star formation efficiencies (SFEs), contradicting the dense-gas mass to star formation rate scaling law. The

n

H

2

histogram toward NGC 253 exhibits a shallow declining slope up to

n

H

2

∼

10

6

cm

−
3

, while that of the GC steeply drops in

n

H

2

≳

10

4.5

cm

−
3

and vanishes at 105 cm−3. Their dense-gas mass fraction ratio becomes consistent with their SFEs when the threshold

n

H

2

for the dense gas is taken at ∼104.2−4.6 cm−3. The rich abundance of gas above this density range in the NGC 253 CMZ, or its scarcity in the GC, is likely to be the critical difference characterizing the contrasting star formation in the centers of the two galaxies.
Constraints on Coasting Cosmological Models from Gravitational-wave Standard Sirens
Authors: Raffai Peter , Pálfi Mária , Dálya Gergely , Gray Rachel
Published: January 2024

We present the first test of coasting cosmological models with gravitational-wave (GW) standard sirens observed in the first three observing runs of the LIGO–Virgo–KAGRA detector network. We apply the statistical galaxy catalog method adapted to coasting cosmologies and infer constraints on the H
0 Hubble constant for the three fixed values of the curvature parameter

k
=

−
1
,
0
,
+
1

in

H

0

2

c

−
2

units. The maximum posteriors and 68.3% highest density intervals we obtained from a combined analysis of 46 dark siren detections and a single bright siren detection are

H

0

=

68.1

−
5.6

+
8.5

,

67.5

−
5.2

+
8.3

,

67.1

−
5.8

+
6.6

km

s

−
1

Mpc

−
1

, respectively. All our constraints on H
0 are consistent within 1σ with the H
0 measured with the differential age method, which provides a constraint on H
0 in coasting cosmologies independently from k. Our results constrain all cosmological models with a(t) ∝ t linear expansion in the luminosity distance and redshift range of the 47 LIGO–Virgo detections, i.e., d
L ≲ 5Gpc and z ≲ 0.8, which practically include all (both strictly linear and quasi-linear) models in the coasting model family. As we have found, the coasting models and the Lambda cold dark matter (or ΛCDM) model fit equally well to the applied set of GW detections.
Efficiency of Turbulent Reacceleration by Solenoidal Turbulence and Its Application to the Origin of Radio Megahalos in Cluster Outskirts
Authors: Nishiwaki Kosuke , Brunetti Gianfranco , Vazza Franco , Gheller Claudio
Published: January 2024

Recent radio observations with the Low Frequency Array (LOFAR) discovered diffuse emission extending beyond the scale of classical radio halos. The presence of such megahalos indicates that the amplification of the magnetic field and acceleration of relativistic particles are working in the cluster outskirts, presumably due to the combination of shocks and turbulence that dissipate energy in these regions. Cosmological magnetohydrodynamical (MHD) simulations of galaxy clusters suggest that solenoidal turbulence has a significant energy budget in the outskirts of galaxy clusters. In this paper, we explore the possibility that this turbulence contributes to the emission observed in megahalos through second-order Fermi acceleration of relativistic particles and magnetic field amplification by the dynamo. We focus on the case of A2255 and find that this scenario can explain the basic properties of the diffuse emission component that is observed under assumptions that are used in previous literature. More specifically, we conduct a numerical follow-up, solving the Fokker–Planck equation by using a snapshot of an MHD simulation and deducing the synchrotron brightness integrated along the lines of sight. We find that a volume-filling emission, ranging between 30% and almost 100% of the projected area, depending on our assumptions on the particle diffusion and transport, can be detected at LOFAR sensitivities. Assuming a magnetic field B ∼ 0.2 μG, as derived from a dynamo model applied to the emitting region, we find that the observed brightness can be matched when ∼1% of the solenoidal turbulent energy flux is channeled into particle acceleration.
A Multiwavelength Study of the Symbiotic Mira HM Sge with SOFIA and HST
Authors: Goldman Steven R. , Sankrit Ravi , Montiel Edward , Garner Sean , Wolthuis Nathan , Karnath Nicole
Published: January 2024

We have targeted the dusty symbiotic Mira system HM Sge with four instruments from the IR to the UV. We have used these observations along with archival observations to study how the system has been evolving after its 1975 nova-like outburst. We have detected rovibrational water emission in a symbiotic system for the first time using new EXES high-spectral-resolution infrared spectroscopy. The features, detected in emission, have velocities consistent with the systemic velocity but do not show any clear evidence of high-velocity outflows. Mid-infrared photometry and grism spectroscopy show that the oxygen-rich asymptotic giant branch dust and dust output have shown little to no change over the past 39 years. In the optical/UV, we detect three main [N ii] nebular features that were detected 22 years ago. Two of these features show a small amount of movement, corresponding to average outflows speeds of 38 and 78 km s−1 since they were previously observed; some previously detected [N ii] features are no longer visible. New UV spectroscopy has shown that the nebular environment continues to steadily relax after the system’s 1975 outburst. The data suggest, however, that the temperature of the hot component has increased from 200,000 K in 1989 to greater than 250,000 K now. Our new and archival observations suggest that the evolution of the system after its outburst is swift with little to no major changes after a period of a couple of years.
Long-term Variations in the Orbital Period of Hot Jupiters from Transit-timing Analysis Using TESS Survey Data
Authors: Wang Wenqin , Zhang Zixin , Chen Zhangliang , Wang Yonghao , Yu Cong , Ma Bo
Published: January 2024

Many hot Jupiters may experience orbital decays, which are manifested as long-term transit-timing variations. We have analyzed 7068 transits from the Transiting Exoplanet Survey Satellite (TESS) for a sample of 326 hot Jupiters. These new mid-transit-time data allow us to update ephemerides for these systems. By combining the new TESS transit-timing data with archival data, we searched for possible long-term variations in the orbital period in these hot Jupiters using a linear and a quadratic ephemeris model. We identified 26 candidates that exhibit possible long-term variations of the orbital period, including 18 candidates with decreasing orbital periods and eight candidates with increasing orbital periods. Among them, 12 candidates failed our leave-one-out cross validation test and thus should be considered to be marginal candidates. In addition to tidal interaction, alternative mechanisms such as apsidal precession, the Rømer effect, and the Applegate effect could also contribute to the variations during the observed period. The ephemerides derived in this work are useful for scheduling follow-up observations for these hot Jupiters in the future. The Python code (PdotQuest, https://github.com/AeoN400/PdotQuest) used to generate the ephemerides is made available online.
Predicting Solar Proton Events of Solar Cycles 22–24 Using GOES Proton and Soft-X-Ray Flux Features
Authors: Ali Aatiya , Sadykov Viacheslav , Kosovichev Alexander , Kitiashvili Irina N. , Oria Vincent , Nita Gelu M. , Illarionov Egor , O’Keefe Patrick M. , Francis Fraila , Chong Chun-Jie , Kosovich Paul , Marroquin Russell D.
Published: January 2024

Solar energetic particle (SEP) events and their major subclass, solar proton events (SPEs), can have unfavorable consequences on numerous aspects of life and technology, making them one of the most harmful effects of solar activity. Garnering knowledge preceding such events by studying operational data flows is essential for their forecasting. Considering only solar cycle (SC) 24 in our previous study, we found that it may be sufficient to only utilize proton and soft X-ray (SXR) parameters for SPE forecasts. Here, we report a catalog recording ≥10 MeV ≥10 particle flux unit SPEs with their properties, spanning SCs 22–24, using NOAA’s Geostationary Operational Environmental Satellite flux data. We report an additional catalog of daily proton and SXR flux statistics for this period, employing it to test the application of machine learning (ML) on the prediction of SPEs using a support vector machine (SVM) and extreme gradient boosting (XGBoost). We explore the effects of training models with data from one and two SCs, evaluating how transferable a model might be across different time periods. XGBoost proved to be more accurate than SVMs for almost every test considered, while also outperforming operational SWPC NOAA predictions and a persistence forecast. Interestingly, training done with SC 24 produces weaker true skill statistic and Heidke skill scores2, even when paired with SC 22 or SC 23, indicating transferability issues. This work contributes toward validating forecasts using long-spanning data—an understudied area in SEP research that should be considered to verify the cross cycle robustness of ML-driven forecasts.
Baryon-induced Collapse of Dark Matter Cores into Supermassive Black Holes
Authors: Argüelles C. R. , Rueda J. A. , Ruffini R.
Published: January 2024

Nonlinear structure formation for fermionic dark matter particles leads to dark matter density profiles with a degenerate compact core surrounded by a diluted halo. For a given fermion mass, the core has a critical mass that collapses into a supermassive black hole (SMBH). Galactic dynamics constraints suggest a ∼100 keV/c
2 fermion, which leads to ∼107
M
⊙ critical core mass. Here, we show that baryonic (ordinary) matter accretion drives an initially stable dark matter core to SMBH formation and determines the accreted mass threshold that induces it. Baryonic gas density ρ

b
and velocity v

b
inferred from cosmological hydrosimulations and observations produce sub-Eddington accretion rates triggering the baryon-induced collapse in less than 1 Gyr. This process produces active galactic nuclei in galaxy mergers and the high-redshift Universe. For TXS 2116–077, merging with a nearby galaxy, the observed 3 × 107
M
⊙ SMBH, for

Q

b

=

ρ

b

/

v

b

3

=
0.125

M

⊙

/

(
100

km

s

−
1

pc
)

3

, forms in ≈0.6 Gyr, consistent with the 0.5–2 Gyr merger timescale and younger jet. For the farthest central SMBH detected by the Chandra X-ray satellite in the z = 10.3 UHZ1 galaxy observed by the James Webb Space Telescope (JWST), the mechanism leads to a 4 × 107
M
⊙ SMBH in 87–187 Myr, starting the accretion at z = 12–15. The baryon-induced collapse can also explain the ≈107–108
M
⊙ SMBHs revealed by JWST at z ≈ 4–6. After its formation, the SMBH can grow to a few 109
M
⊙ in timescales shorter than 1 Gyr via sub-Eddington baryonic mass accretion.
Case Report: Lip Augmentation with Injection of a Novel PEG-crosslinked Hyaluronic Acid Hydrogel
Authors: Edwards Cleo
Published: January 2024

BACKGROUND: Lip augmentation with hyaluronic acid (HA) hydrogels is one of the most common esthetic procedures worldwide, but requires products with an optimal balance of elasticity and cohesivity to volumize while integrating with the surrounding tissue. This case report describes the results of lip augmentation with a novel, 24 mg/mL HA hydrogel cross-linked with poly (ethylene glycol) diglycidyl (PEGDE-HA 24), and supplemented with l-proline and glycine to limit post-injection swelling.
METHODS: In three separate treatment sessions (Weeks 0, 2, and 10), a 29-year-old woman requesting lip augmentation was injected with PEGDE-HA 24 as multiple superficial injections using a tenting technique. Photographs were taken before treatment and at 2-weeks, 1-month, and 5-months after the initial injection. The subject provided post-treatment updates on her experience with the hydrogel in terms of the results achieved and any adverse events experienced.
RESULTS: A total of 1.0 mL PEGDE-HA 24 was injected: treatment session 1 (0.3 mL); session 2 (0.4 mL); and session 3 (0.3 mL). The day after each injection the subject reported that her lips were sensitive, but not painful. The level of post-injection bruising and swelling diminished with each subsequent injection and healed rapidly. No other adverse events were reported. The subject was very satisfied with the results describing them as attractive and natural looking for up to 5 months.
CONCLUSIONS: This case report demonstrated that 1 mL of PEGDE-HA 24 was effective and well tolerated for volume augmentation of the lip. The subject was very satisfied with her experience of the hydrogel and natural-looking results were achieved.
False Prolongation of Activated Partial Thromboplastin Time with Aminoglycoside Antimicrobial Agents: A Case Report
Authors: Doi Hiroki , Osawa Michiko , Ozaki Ayane , Sato Seiko , Fujita Takashi , Akiyama Hidehiko , Ito Hiroyasu
Published: January 2024

BACKGROUND: Activated partial thromboplastin time (APTT) is a clotting time assay for screening bleeding tendency, evaluating coagulation factor production capacity, assessing preoperatively, monitoring anticoagulant drugs, and searching for blood coagulation abnormalities such as hemophilia and antiphospholipid syndrome.
CASE PRESENTATION: Here, we present a 77-year-old male patient with dyspnea who was suspected to have a drug-resistant Pseudomonas aeruginosa infection and pulmonary mycosis. The patient had no history of bleeding tendencies or anticoagulant medication use. The laboratory test results revealed an abnormally prolonged activated partial thromboplastin time (APTT) of 120.3 s using the Coagpia® APTT-N reagent. The APTT test is frequently used to evaluate blood clotting function and assess for bleeding disorders. Prolonged APTT can indicate coagulation factor deficiencies or the presence of certain conditions such as von Willebr and disease, hemophilia, and disseminated intravascular syndrome. However, APTT standardization has not been achieved, causing discrepancies in test results due to variations in the reagents used. The prolonged APTT, in this case, was initially suspected to be caused by contamination or other artifacts, but repeat blood collections and cross-mixing tests revealed the Coagpia® APTT-N reagent as the cause of false prolongation. The reagent was changed to HemosIL SynthASil APTT, which revealed a normal APTT result. The patient had been receiving the aminoglycoside antimicrobial agent tobramycin, and the blood sample taken at the peak tobramycin level demonstrated the longest APTT time. The APTT shortened over time, corresponding to the decrease in tobramycin blood levels.
CONCLUSION: Overall, this paper reports a case of false APTT prolongation due to a specific APTT reagent in the presence of aminoglycoside antimicrobial agents. The findings underscore the difficulties in standar PTT testing and the importance of considering reagent performance characteristics in result interpretations.
Assessing the diversity of nematodes in the Store Mosse National Park (Sweden) using metabarcoding
Authors: Ahmed Mohammed , Slos Dieter , Holovachov Oleksandr
Published: January 2024

The Store Mosse National Park in the south of Sweden was surveyed for nematode diversity and distribution using DNA metabarcoding. Fifty samples were collected from five vegetation types in the park across a range of habitats (e.g. soil, litter, lichens, sphagnum and roots). The other habitats, aside from soil and litter, were sampled in order to capture the diversity of nematodes that may be uniquely associated with them. Nematodes were characterised using the V7-V8 variable domain (~ 350 bp) of the 18S ribosomal RNA gene. We identified 46 families, 76 genera (21 new to Swedish fauna) and 60 species (31 new to Swedish fauna). Some nematodes showed strong associations with their habitats, especially at the species level. Although soil and litter supported the most diverse nematode communities, our results support a strong justification for sampling across different media types to quantify nematode diversity accurately. Soil and litter communities showed high levels of stability with balanced distribution of all the various trophic and coloniser-persister groups.
Politiques d’attractivité des territoires
Authors: Loisy Marine , Réau Bertrand
Published: January 2024

La crise liée à la pandémie de Covid-19 a permis de rendre plus attractifs des territoires jusque-là peu ou pas touristiques. Densité moindre, nouvel environnement quotidien et nouveau rythme de vie couplé parfois à un changement professionnel ont convaincu certaines personnes d’une installation à plus long terme. Le département de la Nièvre, par exemple, a profité de l’élaboration de sa stratégie touristique territoriale pour orienter ses actions vers l’accueil de nouvelles populations résidentes. Cet article a pour objectif de proposer une analyse croisée des productions institutionnelles et scientifiques relatives à l’attractivité nouvelle de certains territoires, notamment ruraux. Plus spécifiquement, il permet de questionner ce que l’organisation des territoires en matière d’attractivité (touristique, résidentielle et de loisirs) fait à l’articulation des temps sociaux en interrogeant les (ré) organisations observables, notamment, au sein des sphères professionnelles, familiales et de loisirs.
Compte rendu de la journée d’études « Travail de plateforme et reproduction sociale »
Authors: Benvegnù Carlotta
Published: January 2024

Journée d’études organisée par A. Koechlin (Centre d’étude des techniques, des connaissances et des pratiques [Cetcopra], Université Paris 1 Panthéon-Sorbonne) et L. Baronian (Centre d’économie de l’Université Sorbonne Paris Nord [CEPN]), le lundi 14 février 2022 au campus Condorcet (Paris), financée par le projet européen H2020- Platform labour in urban spaces (Plus).
The Parent-Child Meeting Space
Authors: Morange Arnaud
Published: January 2024

Un espace de rencontre est un dispositif visant à maintenir le lien entre un ou plusieurs enfants et l’un de leurs parents, lorsque la justice a décidé d’une résidence exclusive. Il entre dans le champ de la protection de l’enfance et répond aux évolutions sociétales relatives à la famille. Il concerne plus de 30 000 enfants chaque année en France. Des professionnels du travail social sont en charge de sa mise en œuvre. Cet article résulte d’une recherche qualitative conduite entre 2017 et 2020 auprès des acteurs de douze espaces de rencontre situés dans l’Hexagone. Le vécu des parents et des intervenants concernés y est analysé. Nous en déduisons l’intérêt du dispositif, tout en pointant ses paradoxes.
Inguinal hernia leading to omental torsion: Role of CT in differentiating from other clinical mimics - a case report and literature review
Authors: Mansoor Ali , Shaukat Rabia
Published: January 2024

Omental torsion is a very rare cause of acute abdomen. Clinically, it mimics other common pathologies such as acute appendicitis, acute diverticulitis and acute cholecystitis. It is therefore no surprise, that it was rarely diagnosed pre operatively before the advent and easy availability of modern imaging techniques. CT scan, in particular, can diagnose omental torsion with confidence pre operatively. This can make conservative treatment possible in cases of primary omental torsion and guide regarding the appropriate treatment in cases of secondary torsion. We present a case of a young male patient who presented to Emergency departments with symptoms of acute abdomen. Clinical and laboratory findings were non-specific for any specific cause of acute abdomen. CT scan, however, showed omental fat stranding with whirlpool sign representing omental torsion which was seen to be secondary to left inguinal hernia. Patient was operated in emergency and necrotic omentum was resected and hernia repaired. Post-operative recovery was uneventful.
What Is an Algorithm?
Authors: de Miguel Julia , Velázquez-Iturbide J. Ángel
Published: January 2024

Algorithms have emerged in past years as an object of public interest and debate. However, this term is used to name very different conceptions. The chapter presents the different definitions of the term “algorithm,” especially the traditional conception of algorithms as used in informatics and the novel conception of (intelligent) algorithms that have emerged in the last years. The main contribution of the chapter is the characterization of both types of algorithms in terms of the problems they are intended to solve. Furthermore, the chapter contributes by analyzing other uses of the word “algorithm” where it is an inadequate term. Finally, the chapter discusses misconceptions on algorithms present in other disciplines, which is an obstacle to mutual understanding and a source of mismatch between the disciplines.
Six-month Outcomes and Predictors Following Non-ST Elevation Myocardial Infarction Managed by Internists
Authors: Daniel Jaifrin , Hansdak Samuel George , Iyadurai Ramya , Ralph Ravikar , Gunasekaran Karthik , Miraclin T Angel , Jayaseelan Visalakshi , Sudarsanam Thambu David
Published: January 2024

Background:

Acute coronary syndrome (ACS) is associated with significant morbidity and mortality. There is an increase in the proportion of non-ST elevation myocardial infarction/unstable angina (NSTEMI/UA) but there is a sparsity of data about the long-term outcome of patients with NSTEMI managed by internists. The long-term outcome and predictors of mortality of individuals with NSTEMI, managed by internists were the subject of the present study.

Methods:

This is a prospective observational cohort study of patients admitted under the internal medicine units with ACS. One hundred forty participants were recruited from April 2016 to July 2017. The various clinical outcomes and all-cause mortality at discharge, 1 month and 6 months were recorded.

Results:

During the study, 132 patients had NTSEMI/UA while 8 had ST-elevation myocardial infarction; 53.2% were men. The mean age was 63.6 ± 11.8 years for NSTEMI/UA. The mean duration of onset of symptoms to primary care was 29.14 ± 34.6 h; 39 (27.9%) presented beyond 48 h. The most frequent comorbidities observed were diabetes mellitus 96 (68.6%), hypertension 94 (67.1%), and dyslipidemia 44 (31.4%). Fifty-two (37.1%) required respiratory support. All patients received Antiplatelet agents and statins. Mortality rates were 9.1%, 13.4%, and 16.1% at discharge, 1-month, and 6 month following admission. The median survival was 161 (147–175) days. Dyslipidemia (hazard ratio [HR]: 0.55, 95% confidence interval [CI]: 0.26, 1.15, P = 0.110) and smoking (HR: 2.16, 95% CI: 1.16–4.02, P = 0.015) were identified as risk factors which predicted mortality.

Conclusions:

Mortality rates following NSTEMI, managed by internists at our tertiary care hospital was similar to various national and international registries. Smoking and dyslipidemia were predictors of mortality.
Comparative Study on Umbilical Cord Serum Prolactin Levels of Normal Preterm Neonates and Preterm Neonates with Respiratory Distress Syndrome
Authors: Sehra Ram Narain , Krishnan R. Gokul , Verma Suniti
Published: January 2024

Introduction:

Respiratory distress syndrome (RDS) is the most common cause of respiratory distress, morbidity, and mortality associated with premature delivery. Prolactin is present in very high concentrations in amniotic fluid, and prolactin receptors are present in lung preparations. Prolactin acts as a direct trigger of lecithin synthesis or in a “chain reaction” along the hypothalamic–pituitary–adrenal axis. Thus, prolactin seems to have a role in lung maturation along with many other factors through a complex mechanism.

Aim:

The aim of this study was to evaluate and compare the umbilical cord serum prolactin levels of preterm infants with and without RDS.

Materials and Methods:

This was a hospital-based comparative observational study carried out at neonatal units of the department of pediatric medicine in a tertiary care center from April 2019 to May 2020. Out of a total of 80 preterm infants, 40 developed RDS and other 40 served as controls. Umbilical cord blood prolactin levels in neonates were measured in both groups and compared. Chi-square test and an unpaired Student’s t-test were used for statistical analysis. Probability was considered significant if <0.05.

Results:

The mean weight of babies was 1312.50 ± 134.30 g in the normal preterm group and 1285.80 ± 314.76 g in the preterm RDS group (P = 0.622). The mean gestational age was 32.1 ± 1.39 weeks in the normal preterm group and 31.77 ± 2.10 weeks in the preterm RDS group (P = 0.418). The mean serum prolactin levels were slightly high in the female preterm RDS group (P = 0.533). The mean cord prolactin levels in all the gestational ages were higher in normal preterm as compared to preterm with RDS (P < 0.05).

Conclusions:

Prolactin level was significantly associated with gestational age and birth weight. Low prolactin levels were significantly associated with the development of RDS in preterm babies. The easily available cord blood can be used to measure prolactin levels at birth to predict RDS.