bluuebunny/crossref_metadata_2025_split huggingface dataset:
Differences between Stable and Unstable Architectures of Compact Planetary Systems
Authors: Volk Kathryn , Malhotra Renu 
Published: May 2024

Abstract
We present a stability analysis of a large set of simulated planetary systems of three or more planets based on architectures of multiplanet systems discovered by Kepler and K2. We propagated 21,400 simulated planetary systems up to 5 billion orbits of the innermost planet; approximately 13% of these simulations ended in a planet–planet collision within that time span. We examined trends in dynamical stability based on dynamical spacings, orbital period ratios, and mass ratios of nearest-neighbor planets as well as the system-wide planet mass distribution and the spectral fraction describing the system’s short-term evolution. We find that instability is more likely in planetary systems with adjacent planet pairs that have period ratios less than 2 and in systems of greater variance of planet masses. Systems with planet pairs at very small dynamical spacings (less than ∼10–12 mutual Hill radii) are also prone to instabilities, but instabilities also occur at much larger planetary separations. We find that a large spectral fraction (calculated from short integrations) is a reasonable predictor of longer-term dynamical instability; systems that have a large number of Fourier components in their eccentricity vectors are prone to secular chaos and subsequent eccentricity growth and instabilities.
JWST Observations of Starbursts: Polycyclic Aromatic Hydrocarbon Emission at the Base of the M82 Galactic Wind
Authors: Bolatto Alberto D. , Levy Rebecca C. , Tarantino Elizabeth , Boyer Martha L. , Fisher Deanne B. , Cronin Serena A. , Leroy Adam K. , Klessen Ralf S. , Smith J. D. , Berg Danielle A. , Böker Torsten , Boogaard Leindert A. , Ostriker Eve C. , Thompson Todd A. , Ott Juergen , Lenkić Laura , Lopez Laura A. , Dale Daniel A. , Veilleux Sylvain , van der Werf Paul P. , Glover Simon C. O. , Sandstrom Karin M. , Skillman Evan D. , Chisholm John , Villanueva Vicente , Lai Thomas S.-Y. , Lopez Sebastian , Mills Elisabeth A. C. , Emig Kimberly L. , Armus Lee , Mayya Divakara , Meier David S. , De Looze Ilse , Herrera-Camus Rodrigo , Walter Fabian , Relaño Mónica , Koziol Hannah B. , Marvil Joshua , Jiménez-Donaire María J. , Martini Paul 
Published: May 2024

Abstract
We present new observations of the central 1 kpc of the M82 starburst obtained with the James Webb Space Telescope near-infrared camera instrument at a resolution θ ∼ 0.″05–0.″1 (∼1–2 pc). The data comprises images in three mostly continuum filters (F140M, F250M, and F360M), and filters that contain [Fe ii] (F164N), H2
v = 1 → 0 (F212N), and the 3.3 μm polycyclic aromatic hydrocarbon (PAH) feature (F335M). We find prominent plumes of PAH emission extending outward from the central starburst region, together with a network of complex filamentary substructures and edge-brightened bubble-like features. The structure of the PAH emission closely resembles that of the ionized gas, as revealed in Paschen α and free–free radio emission. We discuss the origin of the structure, and suggest the PAHs are embedded in a combination of neutral, molecular, and photoionized gas.
Predicting the Spectroscopic Features of Galaxies by Applying Manifold Learning on Their Broadband Colors: Proof of Concept and Potential Applications for Euclid, Roman, and Rubin LSST
Authors: Jafariyazani Marziye , Masters Daniel , Faisst Andreas L. , Teplitz Harry I. , Ilbert Olivier 
Published: May 2024

Abstract
Entering the era of large-scale galaxy surveys, which will deliver unprecedented amounts of photometric and spectroscopic data, there is a growing need for more efficient, data-driven, and less model-dependent techniques to analyze the spectral energy distribution of galaxies. In this work, we demonstrate that by taking advantage of manifold learning approaches, we can estimate spectroscopic features of large samples of galaxies from their broadband photometry when spectroscopy is available only for a fraction of the sample. This will be done by applying the self-organizing map algorithm on broadband colors of galaxies and mapping partially available spectroscopic information into the trained maps. In this pilot study, we focus on estimating the 4000 Å break in a magnitude-limited sample of galaxies in the Cosmic Evolution Survey (COSMOS) field. We also examine this method to predict the Hδ

A
index given our available spectroscopic measurements. We use observed galaxy colors (u,g,r,i,z,Y,J,H), as well as spectroscopic measurements for a fraction of the sample from the LEGA-C and zCOSMOS spectroscopic surveys to estimate this feature for our parent photometric sample. We recover the D4000 feature for galaxies that only have broadband colors with uncertainties about twice the uncertainty of the employed spectroscopic surveys. Using these measurements, we observe a positive correlation between D4000 and the stellar mass of the galaxies in our sample with weaker D4000 features for higher-redshift galaxies at fixed stellar masses. These can be explained by the downsizing scenario for the formation of galaxies and the decrease in their specific star formation rate as well as the aging of their stellar populations over this time period.
Toward Early-type Eclipsing Binaries as Extragalactic Milestones. III. Physical Properties of the O-type Eclipsing Binary OGLE LMC-ECL-21568 in a Quadruple System*
,

†
Authors: Taormina Mónica , Kudritzki R.-P. , Pilecki B. , Pietrzyński G. , Thompson I. B. , Puls J. , Górski M. , Zgirski B. , Graczyk D. , Gieren W. , Hajdu G. 
Published: May 2024

Abstract
We present the results from a complex study of an eclipsing O-type binary (Aa+Ab) with the orbital period of P
A = 3.2254367 days that forms part of a higher-order multiple system in a configuration of (A+B)+C. We derived masses of the Aa+Ab binary of M
1 = 19.02 ± 0.12 and M
2 = 17.50 ± 0.13 M
⊙, the radii of R
1 = 7.70 ± 0.05 and R
2 = 6.64 ± 0.06 R
⊙, and temperatures of T
1 = 34,250 ± 500 K and T
2 = 33,750 ± 500 K. From the analysis of the radial velocities, we found a spectroscopic orbit of A in the outer A+B system with P
A+B = 195.8 days (P
A+B/P
A ≈ 61). In the O − C analysis, we confirmed this orbit and found another component orbiting the A+B system with P
AB+C = 2550 days (P
AB+C/P
A+B ≈ 13). From the total mass of the inner binary and its outer orbit, we estimated the mass of the third object, M
B ≳ 10.7 M
⊙. From the light travel time effect fit to the O − C data, we obtained the limit for the mass of the fourth component, M
C ≳ 7.3 M
⊙. These extra components contribute about 20%–30% (increasing with wavelength) to the total system light. From the comparison of model spectra with the multiband photometry, we derived a distance modulus of 18.59 ± 0.06 mag, a reddening of 0.16 ± 0.02 mag, and an RV
of 3.2. This work is part of our ongoing project, which aims to calibrate the surface brightness–color relation for early-type stars.
Forecasts for Galaxy Formation and Dark Matter Constraints from Dwarf Galaxy Surveys
Authors: Nadler Ethan O. , Gluscevic Vera , Driskell Trey , Wechsler Risa H. , Moustakas Leonidas A. , Benson Andrew , Mao Yao-Yuan 
Published: May 2024

Abstract
The abundance of faint dwarf galaxies is determined by the underlying population of low-mass dark matter (DM) halos and the efficiency of galaxy formation in these systems. Here, we quantify potential galaxy formation and DM constraints from future dwarf satellite galaxy surveys. We generate satellite populations using a suite of Milky Way (MW)–mass cosmological zoom-in simulations and an empirical galaxy–halo connection model, and assess sensitivity to galaxy formation and DM signals when marginalizing over galaxy–halo connection uncertainties. We find that a survey of all satellites around one MW-mass host can constrain a galaxy formation cutoff at peak virial masses of

M

50

=

10

8

M

⊙

at the 1σ level; however, a tail toward low

M

50

prevents a 2σ measurement. In this scenario, combining hosts with differing bright satellite abundances significantly reduces uncertainties on

M

50

at the 1σ level, but the 2σ tail toward low

M

50

persists. We project that observations of one (two) complete satellite populations can constrain warm DM models with m
WDM ≈ 10 keV (20 keV). Subhalo mass function (SHMF) suppression can be constrained to ≈70%, 60%, and 50% that in cold dark matter (CDM) at peak virial masses of 108, 109, and 1010
M
⊙, respectively; SHMF enhancement constraints are weaker (≈20, 4, and 2 times that in CDM, respectively) due to galaxy–halo connection degeneracies. These results motivate searches for faint dwarf galaxies beyond the MW and indicate that ongoing missions like Euclid and upcoming facilities including the Vera C. Rubin Observatory and Nancy Grace Roman Space Telescope will probe new galaxy formation and DM physics.
WawHelioIonMP: A Semiempirical Tool for the Determination of Latitudinal Variation in the Ionization Rate of Interstellar Hydrogen and the Solar Wind
Authors: Porowski C. , Bzowski M. 
Published: May 2024

Abstract
The latitudinal structure of the solar wind varies during the cycle of solar activity. Analysis of this variation is important for understanding the solar activity and interpretation of observations of heliospheric energetic neutral hydrogen atoms and interstellar neutral (ISN) atoms inside the heliosphere, which yield information on the heliosphere and its interaction with the interstellar medium. Existing methods of retrieving this information from indirect remote-sensing measurements of phenomena, including the heliospheric backscatter glow and interplanetary scintillations of remote radio sources, are challenging to apply in real time. Here, we propose a method WawHelioIonMP of approximate retrieval of latitudinal profiles of the ionization rates of ISN H using a machine-learning-based interpretation of the helioglow. Assuming that we know their history during two past solar cycles and have observations of the helioglow for close-to-circumsolar circles with a radius close to 90°, we derive statistically an algebraic relation between the ionization profiles and lightcurves. With the relation reversed, we are then able to derive the ionization rate profiles based on observed light curves, such as those planned for the GLObal solar Wind Structure (GLOWS) experiment on the forthcoming NASA mission Interstellar Mapping and Acceleration Probe (IMAP). The application of this method is straightforward and rapid because complex simulations are no longer needed. We present the method of retrieval of the profiles of the ionization rates, leaving the discussion of details of the decomposition of the retrieved ionization rate profiles into profiles of the solar wind speed and density to a future paper.
Investigations of Massive Filaments and Star Formation (INFANT). I. Core Identification and Core Mass Function
Authors: Cheng 程 Yu 宇 , Lu 吕 Xing 行 , Sanhueza Patricio , Liu Hauyu Baobab , Zhang Qizhou , Galván-Madrid Roberto , Wang Ke , Nakamura Fumitaka , Liu Tie , Feng Siyi , Li Shanghuo , Jiao Sihan , Tanaka Kei E. I. , Liu Xunchuan , Li Pak Shing , Luo Qiuyi , Gu Qilao , Lin Yuxin , Guzmán Andrés E. 
Published: May 2024

Abstract
Filamentary structures are ubiquitously found in high-mass star-forming clouds. To investigate the relationship between filaments and star formation, we carry out the INFANT (Investigations of Massive Filaments and Sar Formation) survey, a multiscale, multiwavelength survey of massive filamentary clouds with Atacama Large Millimeter/submillimeter Array (ALMA) band 3/band 6 and Very Large Array K band. In this first paper, we present the ALMA band 6 continuum observations toward a sample of eight high-mass star-forming filaments. We covered each target with an approximately rectangular mosaic field of view with two 12 m array configurations, achieving an angular resolution of ∼0.″6 (2700 au at 4.5 kpc) and a continuum rms of ∼0.1 mJy beam−1 (∼0.06 M
⊙ in gas mass assuming 15 K). We identify cores using the getsf and astrodendro and find the former is more robust in terms of both identification and measuring flux densities. We identify in total 183 dense cores (15–36 cores in each cloud) and classify their star formation states via outflow and warm gas tracers. The protostellar cores are statistically more massive than the prestellar cores, possibly indicating further accretion onto cores after the formation of protostars. For the high-mass end (

M

core

> 1.5 M
⊙) of the core mass function (CMF) we derive a power-law index of −1.15 ± 0.12 for the whole sample and −1.70 ± 0.25 for the prestellar population. We also find a steepening trend in CMF with cloud evolution (−0.89 ± 0.15 for the young group versus. −1.44 ± 0.25 for the evolved group) and discuss its implications for cluster formation.
Extrapolation of Type Ia Supernova Spectra into the Near-infrared Using Principal Component Analysis
Authors: Burrow Anthony , Baron E. , Burns Christopher R. , Hsiao Eric Y. , Lu Jing , Ashall Chris , Brown Peter J. , DerKacy James M. , Folatelli G. , Galbany Lluís , Hoeflich P. , Krisciunas Kevin , Morrell N. , Phillips M. M. , Shappee Benjamin J. , Stritzinger Maximilian D. , Suntzeff Nicholas B. 
Published: May 2024

Abstract
We present a method of extrapolating the spectroscopic behavior of Type Ia supernovae (SNe Ia) in the near-infrared (NIR) wavelength regime up to 2.30 μm using optical spectroscopy. Such a process is useful for accurately estimating K-corrections and other photometric quantities of SNe Ia in the NIR. A principal component analysis is performed on data consisting of Carnegie Supernova Project I & II optical and NIR FIRE spectra to produce models capable of making these extrapolations. This method differs from previous spectral template methods by not parameterizing models strictly by photometric light-curve properties of SNe Ia, allowing for more flexibility of the resulting extrapolated NIR flux. A difference of around −3.1% to −2.7% in the total integrated NIR flux between these extrapolations and the observations is seen here for most test cases including Branch core-normal and shallow-silicon subtypes. However, larger deviations from the observation are found for other tests, likely due to the limited high-velocity and broad-line SNe Ia in the training sample. Maximum-light principal components are shown to allow for spectroscopic predictions of the color-stretch light-curve parameter, s
BV, within approximately ±0.1 units of the value measured with photometry. We also show these results compare well with NIR templates, although in most cases the templates are marginally more fitting to observations, illustrating a need for more concurrent optical+NIR spectroscopic observations to truly understand the diversity of SNe Ia in the NIR.
What if the Universe Expands Linearly? A Local General Relativity to Solve the “Zero Active Mass” Problem
Authors: Monjo Robert 
Published: May 2024

Abstract
Modern cosmology presents important challenges such as the Hubble Tension, El Gordo’s collision, or the impossible galaxies (z > 10). Slight modifications to the standard model propose new parameters (e.g., the early and dynamical dark energy). On the other hand, alternatives such as the coasting universes (e.g., the hyperconical model and the spatially flat R

h
= ct universe) are statistically compatible with most of the observational tests, but still present theoretical problems in matching the observed matter contents since they predict a “zero active gravitational mass.” To solve these open issues, we suggest that general relativity might be not valid at cosmic scales, but it would be valid at local scales. This proposal is addressed from two main features of the embedding hyperconical model: (1) the background metric would be independent of the matter content, and (2) the observed cosmic acceleration would be fictitious and because of a distorted stereographic projection of coordinates that produce an apparent radial inhomogeneity from homogeneous manifolds. Finally, to support the discussion, standard observational tests were updated here, showing that the hyperconical model is adequately fitted to Type Ia supernovae, quasars, galaxy clusters, baryon acoustic oscillations, and cosmic chronometer data sets.
Monitoring AGNs with Hβ Asymmetry. IV. First Reverberation Mapping Results of 14 Active Galactic Nuclei
Authors: Zastrocky T. E. , Brotherton Michael S. , Du Pu , McLane Jacob N. , Olson Kianna A. , Dale D. A. , Kobulnicky H. A. , Maithil Jaya , Nguyen My L. , Chick William T. , Kasper David H. , Hand Derek , Adelman C. , Carter Z. , Murphree G. , Oeur M. , Roth T. , Schonsberg S. , Caradonna M. J. , Favro J. , Ferguson A. J. , Gonzalez I. M. , Hadding L. M. , Hagler H. D. , Rogers C. J. , Stack T. R. , Chapman Franklin , Bao Dong-Wei , Fang Feng-Na , Zhai Shuo , Yang Sen , Chen Yong-Jie , Bai Hua-Rui , Fu Yi-Xin , Liu Jun-Rong , Yao Zhu-Heng , Peng Yue-Chang , Songsheng Yu-Yang , Li Yan-Rong , Bai Jin-Ming , Hu Chen , Xiao Ming , Ho Luis C. , Wang Jian-Min 
Published: May 2024

Abstract
We report first-time reverberation-mapping results for 14 active galactic nuclei (AGNs) from the ongoing Monitoring AGNs with Hβ Asymmetry campaign (MAHA). These results utilize optical spectra obtained with the Long Slit Spectrograph on the Wyoming Infrared 2.3 m Telescope between 2017 November and 2023 May. MAHA combines long-duration monitoring with high cadence. We report results from multiple observing seasons for nine of the 14 objects. These results include Hβ time lags, supermassive black hole masses, and velocity-resolved time lags. The velocity-resolved lags allow us to investigate the kinematics of the broad-line region.
Pros and Cons of Air-Dried and Conventional Wet-Fixed Pap Smears: An Institutional Study
Authors: Mary A Queen , Das Subhashish , Sheela SR 
Published: May 2024

Introduction:
Wet-fixed smear study routinely used to identify several pre-cancerous and cancerous tumours. By contrasting cellular preservation and staining quality in rehydration smears with wet-fixed smears, the current study aims to establish the effects of rehydration on air-dried smears.

Materials and Methods:
One hundred paired samples are compared. Wet fixing was done in the first place. Air-dried samples are rehydrated for 30 s with regular saline and then placed in 95% ethanol for 30 min. Both smears will undergo screening, evaluation and grading for numerous cytomorphological factors after Pap staining. The 2014 Bethesda system was used to report the cervical smear results.

Results:
When evaluated for numerous cellular properties, statistically significant similarities can be seen between two groups, one with wet-fixed smears and the other with rehydrated air-dried smears. The results of the cytological diagnosis comparison between the two groups can be shown in the agreement. Rehydrated air-dried smear interpretation and staining quality are significantly superior to traditional wet smears.

Conclusions:
Rehydration air-dried techniques can be used instead of traditional wet fixation methods and are as effective when used alone or with traditional wet-fixed smears.
Repurposing the Anti-Depression Drug Sertraline against Catheter-Associated Urinary Tract Infections
Authors: Poyil Muhammad Musthafa , Khan Mohammed Sarosh , Gowri Meiyazhagan 
Published: May 2024

Introduction:
Catheter-associated urinary tract infections (CAUTIs) account for one-third of the nosocomial infections. As drug repurposing is an excellent method to develop new antimicrobials, the present study is a trial to repurpose the anti-depression drug sertraline against two of the major CAUTI causing, biofilm forming bacteria viz., Enterococcus faecalis and Escherichia coli.

Materials and Methods:
Agar diffusion and microdilution methods were used in repurposing sertraline against E. faecalis and E. coli, to find out the antibacterial activity and the minimal inhibitory concentration of the drug. The anti-biofilm activity of the drug was also studied.

Results:
Sertraline (concentrations given within brackets) produced growth inhibition zones against E. faecalis as: 23 mm (125 μg), 24 mm (150 μg) and 26 mm (200 μg) and against E. coli as: 14 mm (125 μg), 15 mm (150 μg) and 17 mm (200 μg), respectively. Against both of the pathogens, the minimal inhibitory concentration of the drug was found to be 75 μg/ml, and at this concentration, the drug prevented the colony formation by these bacteria on polystyrene surfaces. The drug reduced the biofilms of E. faecalis and E. coli by 62% and 69%, respectively.

Conclusion:
When repurposed against E. faecalis and E. coli sertraline showed promising antibacterial, anti-biofilm and anti-adhesive activities, repurposing being one of the easiest ways to develop new drugs against bacterial pathogens, the authors suggest for further studies on repurposing sertraline for its clinical applications.
Andrology laboratory technique for analysis of semen in men with azoospermia
Authors: Japari Andrian , Moorthy Dharani , Rambhatla Amarnath 
Published: May 2024

Abstract
Discovery of spermatozoa during the 17th century led to developing technologies for semen analysis in the early 1900s, and then, standard techniques were implemented during the 20th century. Semen analysis has a pivotal role in the male infertility evaluation, and azoospermia is an important finding. Azoospermia is identified in 15% of infertile men. However, the accurate laboratory assessment of azoospermia poses certain technical challenges. Laboratories currently perform semen assessment with great variability; thus, a standard method should be used. Planning suitable management and determining the cause of infertility require a precise evaluation of azoospermia. This review aims to address the definition of azoospermia and highlight laboratory methods in the assessments of azoospermia. Basic methods such as centrifugation, repeat pellet analysis, and staining and advanced methods such as genetic testing and biomarkers have been discussed. These methods have helped in standardizing the protocol for accurate azoospermia assessments with less variability.
Type 2 diabetes mellitus and thyroid dysfunction, revisiting the intersections: A review article
Authors: Ezeani Ignatius Ugochukwu , Ogbonna Stanley U 
Published: May 2024

Abstract
There is an overwhelming evidence of the relationship between type 2 diabetes mellitus (T2DM) and thyroid dysfunction. The literature is robustly littered with data demonstrating the intersection of these two most common endocrine conditions. However, the extent of these intersections still remains complex, conflicting, and unclear. Therefore, we aimed to review the current literature on these intersections with an emphasis on interrelationship between thyroid dysfunction and T2DM. Several mechanisms have been postulated; some of which include but are not limited to blunting of the nocturnal thyroid-stimulating hormone (TSH) peak impairment of the TSH response to TRH from the hypothalamus, impairment of peripheral conversion from T4 to T3, increased hepatocyte plasma membrane concentrations of glucose transporter in the liver, which leads to an increased hepatic glucose output and abnormal glucose metabolism, to the perturbed genetic expression of a group of genes along with physiological abnormality. Insulin resistance has been shown to be associated with thyroid dysfunction (hyperthyroidism) in patients with T2DM. In other words, insulin resistance links both conditions. Several studies have evidenced an incontrovertible role of thyroid dysfunction as an intertwined cohort of T2DM. A plethora of guidelines have been exhaustively evaluated highlighting their key messages while synthesizing the relationship existing between them. The different treatment options available inexorably validate the importance of the intersection between these two endocrine conditions.