bluuebunny/crossref_metadata_2025_split huggingface dataset:
A warm dark matter cosmogony may yield more low-mass galaxy detections in 21-cm surveys than a cold dark matter one
Authors: Oman Kyle A , Frenk Carlos S , Crain Robert A , Lovell Mark R , Pfeffer Joel 
Published: July 2024

ABSTRACT
The 21-cm spectral line widths, $w_{50}$, of galaxies are an approximate tracer of their dynamical masses, such that the dark matter halo mass function is imprinted in the number density of galaxies as a function of $w_{50}$. Correcting observed number counts for survey incompleteness at the level of accuracy needed to place competitive constraints on warm dark matter (WDM) cosmological models is very challenging, but forward-modelling the results of cosmological hydrodynamical galaxy formation simulations into observational data space is more straightforward. We take this approach to make predictions for an ALFALFA-like survey from simulations using the EAGLE galaxy formation model in both cold (CDM) and WDM cosmogonies. We find that for WDM cosmogonies more galaxies are detected at the low-$w_{50}$ end of the 21-cm velocity width function than in the CDM cosmogony, contrary to what might naïvely be expected from the suppression of power on small scales in such models. This is because low-mass galaxies form later and retain more gas in WDM cosmogonies (with EAGLE). While some shortcomings in the treatment of cold gas in the EAGLE model preclude placing definitive constraints on WDM scenarios, our analysis illustrates that near-future simulations with more accurate modelling of cold gas will likely make strong constraints possible, especially in conjunction with new 21-cm surveys such as WALLABY.
Study of consecutive eclipses of pulsar J0024-7204O
Authors: Abbate F , Possenti A , Ridolfi A , Buchner S , Geyer M , Kramer M , Zhang L , Corongiu A , Camilo F , Bailes M 
Published: July 2024

ABSTRACT
The eclipses seen in the radio emission of some pulsars can be invaluable to study the properties of the material from the companion stripped away by the pulsar. We present a study of six consecutive eclipses of PSR J0024–7204O in the globular cluster 47 Tucanae as seen by the MeerKAT radio telescope in the UHF (544–1088 MHz) band. A high scintillation state boosted the signal during one of the orbits and allowed a detailed study of the eclipse properties. We measure significant dispersion measure (DM) variations and detect strong scattering that seems to be the dominating mechanism of the eclipses at these frequencies. A complete drop in the linear polarization together with a small increase in the rotation measure suggests the presence of a magnetic field of $\sim 2$ mG. The study of multiple eclipses allowed us to measure difference in the lengths of the eclipses and DM differences of $\sim 0.01$ pc cm$^{-3}$ in consecutive orbits. One orbit, in particular, shows a delay in recovery of the linear polarization and a visible delay in the arrival of the pulses caused by a stronger scattering event. We suggest that these are caused by a higher variance of density fluctuations during the event.
Observational clues to the magnetic evolution of magnetars
Authors: Makishima Kazuo , Uchida Nagomi , Enoto Teruaki 
Published: July 2024

ABSTRACT
Utilizing four archival X-ray data sets taken with the Hard X-ray Detector onboard Suzaku, timing studies were performed on three magnetars, 1E 1841−045 (observed in 2006), SGR 0501+4516 (2008), and 1RXS J170849.0−400910 (2009 and 2010). Their pulsations were reconfirmed, typically in an energy range of 12–50 keV. The 11.783 s pulses of 1E 1841−045 and those of SGR 0501+4516 at 5.762 s were periodically phase modulated, with a long period of $\approx 23.4$ and $\approx 16.4$ ks, respectively. The pulse-phase modulation was also observed, at $\approx 46.5$ ks, from two data sets of 1RXS J170849.0−400910. In all these cases, the modulation amplitude was 6 per cent to 16 per cent of the pulse cycle. Including previously confirmed four objects, this characteristic timing behaviour is now detected from seven magnetars in total, and interpreted as a result of free precession of neutron stars that are deformed to an asphericity of $\sim 10^{-4}$. Assuming that the deformation is due to magnetic stress, these magnetars are inferred to harbour toroidal magnetic fields of $B_{\rm t}\sim 10^{16}$ G. By comparing the estimated $B_{\rm t}$ of these objects with their poloidal dipole field $B_{\rm d}$, the $B_{\rm t}/B_{\rm d}$ ratio is found to increase with their characteristic age. Therefore, the toroidal fields of magnetars are likely to last longer than their poloidal fields. This explains the presence of some classes of neutron stars that have relatively weak $B_{\rm d}$ but are suspected to hide strong $B_{\rm t}$ inside them.
Different spectra of cosmic ray H, He, and heavier nuclei escaping compact star clusters
Authors: Blasi Pasquale , Morlino Giovanni 
Published: July 2024

ABSTRACT
Cosmic ray acceleration at the termination shock of compact star clusters has recently received much attention, mainly because of the detection of gamma-ray emission from some of such astrophysical sources. Here we focus on the acceleration of nuclei at the termination shock and we investigate the role played by proton energy losses and spallation reactions of nuclei, especially downstream of the shock. We show that for a reasonable choice of the mean gas density in the cavity excavated by the cluster wind, dominated by the presence of dense clouds, the spectrum of He nuclei escaping the bubble is systematically harder than the spectrum of hydrogen, in a manner that appears to be qualitatively consistent with the observed and yet unexplained phenomenon of discrepant hardening. We also find that, in this scenario, the spallation reactions of heavier nuclei are likely to be so severe that their spectra becomes very hard and with a low normalization, meaning that it is unlikely that heavy nuclei escaping star clusters can provide a sizeable contribution to the spectrum of cosmic rays at the Earth. Limitations and implications of this scenario are discussed.
The thermalization of γ-rays in radioactive expanding ejecta: a simple model and its application for Kilonovae and Ia SNe
Authors: Guttman Or , Shenhar Ben , Sarkar Arnab , Waxman Eli 
Published: July 2024

ABSTRACT
A semi-analytic approximation is derived for the time-dependent fraction $f_\gamma (t)$ of the energy deposited by radioactive decay $\gamma$-rays in a homologously expanding plasma of general structure. An analytic approximation is given for spherically symmetric plasma distributions. Applied to Kilonovae (KNe) associated with neutron stars mergers and Type Ia supernovae, our semi-analytic and analytic approximations reproduce, with a few per cent and 10 per cent accuracy, respectively, the energy deposition rates, $\dot{Q}_{\rm dep}$, obtained in numeric Monte Carlo calculations. The time $t_\gamma$ beyond which $\gamma$-ray deposition is inefficient is determined by an effective frequency-independent $\gamma$-ray opacity $\kappa _{\gamma ,\text{eff}}$, $t_\gamma = \sqrt{\kappa _{\gamma ,\text{eff}}\langle \Sigma \rangle t^2}$, where $\langle \Sigma \rangle \propto t^{-2}$ is the average plasma column density. For $\beta$-decay dominated energy release, $\kappa _{\gamma ,\text{eff}}$ is typically close to the effective Compton scattering opacity, $\kappa _{\gamma ,\text{eff}} \approx 0.025$ cm$^{2}$ g$^{-1}$ with a weak dependence on composition. For KNe, $\kappa _{\gamma ,\text{eff}}$ depends mainly on the initial electron fraction $Y_e$, $\kappa _{\gamma ,\text{eff}} \approx 0.03(0.05)$ cm$^{2}$ g$^{-1}$ for $Y_e \gtrsim (\lesssim) 0.25$ (in contrast with earlier work that found $\kappa _{\gamma ,\text{eff}}$ larger by 1–2 orders of magnitude for low $Y_e$), and is insensitive to the (large) nuclear physics uncertainties. Determining $t_\gamma$ from observations will therefore measure the ejecta $\langle \Sigma \rangle t^2$, providing a stringent test of models. For $\langle \Sigma \rangle t^2=2\times 10^{11}~{\rm g\, {cm}^{-2}\, s^2}$, a typical value expected for KNe, $t_\gamma \approx 1$ d.
Atmospheric parameters and chemical abundances within 100 pc: a sample of G, K, and M main-sequence stars
Authors: López-Valdivia Ricardo , Adame Lucía , Zagala Lagunas Eduardo , Román-Zúñiga Carlos G , Hernández Jesús , Sánchez Edilberto , Fernández-Trincado José G , Carigi Leticia , Kounkel Marina , Lane Richard R , Stassun Keivan G , Villanova Sandro 
Published: July 2024

ABSTRACT
To date, we have access to enormous inventories of stellar spectra that allow the extraction of atmospheric parameters and chemical abundances essential in stellar studies. However, characterizing such a large amount of data is complex and requires a good understanding of the studied object to ensure reliable and homogeneous results. In this study, we present a methodology to measure homogenously the basic atmospheric parameters and detailed chemical abundances of over 1600 thin disc main-sequence stars in the 100 pc solar neighbourhood, using APOGEE-2 infrared spectra. We employed the code tonalli to determine the atmospheric parameters using a prior on $\log {g}$. The $\log {g}$ prior in tonalli implies an understanding of the treated population and helps to find physically coherent answers. Our atmospheric parameters agree within the typical uncertainties (100 K in $\mathrm{T_{eff}}$, 0.15 dex in $\log {g}$ and [M/H]) with previous estimations of ASPCAP and Gaia DR3. We use our temperatures to determine a new infrared colour–temperature sequence, in good agreement with previous works, that can be used for any main-sequence star. Additionally, we used the bacchus code to determine the abundances of Mg, Al, Si, Ca, and Fe in our sample. The five elements (Mg, Al, Si, Ca, Fe) studied have an abundance distribution centred around slightly subsolar values in agreement with previous results for the solar neighbourhood. The over 1600 main-sequence stars’ atmospheric parameters and chemical abundances presented here are useful in follow-up studies of the solar neighbourhood or as a training set for data-driven methods.
Nebular nitrogen line emission in stripped-envelope supernovae – a new progenitor mass diagnostic
Authors: Barmentloo Stan , Jerkstrand Anders , Iwamoto Koichi , Hachisu Izumi , Nomoto Ken’ichi , Sollerman Jesper , Woosley Stan 
Published: July 2024

ABSTRACT
Nitrogen is produced by CNO-cycling in massive stars, and can be ejected in significant amounts in supernova explosions. While in H-rich SNe, its [N ii] 6548, 6583 emission becomes obscured by strong H$\alpha$, in explosions of He stars, this nitrogen emission becomes more visible. We here explore the formation of this line, using the sumo code to compute spectra for a grid of 1D models with parametrized mixing informed from new 2D simulations. Because the mass fraction of nitrogen in the ejecta decreases with larger He-core masses, as more of the He/N zone gets processed by shell helium burning and is lost to winds, the [N ii] luminosity relative to the overall optical flux probes the He-core mass. By comparing to large samples of data, we find that low-mass He cores ($M_{\rm preSN}\lesssim \ 3\ \mathrm{ M}_\odot$) are exclusively associated with Type IIb SNe, with the exception of Type Ib SN 2007Y. Seeing no strong nitrogen emission in other Type Ib SNe, the implication is either an origin from low-mass stars with the He/N layer (but not the He/C) layer peeled away, or from higher mass He cores. We also see no clear nitrogen emission in Type Ic SNe. We discuss the diagnostic potential of this new line metric, and also dependencies on mass-loss rate and metallicity.
Imaging and quantification of human and viral circular RNAs
Authors: Jaijyan Dabbu Kumar , Yang Shaomin , Ramasamy Santhamani , Gu Alison , Zeng Mulan , Subbian Selvakumar , Tyagi Sanjay , Zhu Hua 
Published: July 2024

Abstract
We present a robust approach for cellular detection, imaging, localization, and quantification of human and viral encoded circular RNAs (circRNA) using amplified fluorescence in situ hybridization (ampFISH). In this procedure, a pair of hairpin probes bind next to each other at contiguous stretches of sequence and then undergo a conformational reorganization which initiates a target-dependent hybridization chain reaction (HCR) resulting in deposition of an amplified fluorescent signal at the site. By harnessing the capabilities of both ampFISH and single-molecule FISH (smFISH), we selectively identified and imaged circular RNAs and their linear counterparts derived from the human genome, SARS-CoV-2 (an RNA virus), and human cytomegalovirus (HCMV, a DNA virus). Computational image processing facilitated accurate quantification of circular RNA molecules in individual cells. The specificity of ampFISH for circular RNA detection was confirmed through an in situ RNase R treatment that selectively degrades linear RNAs without impacting circular RNAs. The effectiveness of circular RNA detection was further validated by using ampFISH probes with mismatches and probe pairs that do not bind to the continuous sequence in their target RNAs but instead bind at segregated sites. An additional specificity test involved probes against the negative strands of the circular RNA sequence, absent in the cell. Importantly, our technique allows simultaneous detection of circular RNAs and their linear counterparts within the same cell with single molecule sensitivity, enabling explorations of circular RNA biogenesis, subcellular localization, and functions.
HYENA detects oncogenes activated by distal enhancers in cancer
Authors: Yu Anqi , Yesilkanal Ali E , Thakur Ashish , Wang Fan , Yang Yang , Phillips William , Wu Xiaoyang , Muir Alexander , He Xin , Spitz Francois , Yang Lixing 
Published: July 2024

Abstract
Somatic structural variations (SVs) in cancer can shuffle DNA content in the genome, relocate regulatory elements, and alter genome organization. Enhancer hijacking occurs when SVs relocate distal enhancers to activate proto-oncogenes. However, most enhancer hijacking studies have only focused on protein-coding genes. Here, we develop a computational algorithm ‘HYENA’ to identify candidate oncogenes (both protein-coding and non-coding) activated by enhancer hijacking based on tumor whole-genome and transcriptome sequencing data. HYENA detects genes whose elevated expression is associated with somatic SVs by using a rank-based regression model. We systematically analyze 1146 tumors across 25 types of adult tumors and identify a total of 108 candidate oncogenes including many non-coding genes. A long non-coding RNA TOB1-AS1 is activated by various types of SVs in 10% of pancreatic cancers through altered 3-dimensional genome structure. We find that high expression of TOB1-AS1 can promote cell invasion and metastasis. Our study highlights the contribution of genetic alterations in non-coding regions to tumorigenesis and tumor progression.
DNA abasic sites act as rational therapeutic targets to synergize temozolomide response in both MMR-proficient and deficient cancer
Authors: Bora Achyut , Pal Ritesh , Mandi Chandra Sova , Dutta Sanjay 
Published: July 2024

Abstract
Temozolomide (TMZ) is widely used in cancer treatment, yet resistance to this agent limits its therapeutic effectiveness, particularly in mismatch-repair (MMR) deficient cancer. Concurrently, the Base Excision Repair (BER) pathway exerts a mitigating role. Our results demonstrated that the increasing TMZ concentrations correlate with an elevated accumulation of DNA abasic sites via the BER pathway in both MMR-proficient and deficient cancer cells, implicating abasic sites as promising targets to enhance the TMZ response. Amino-quinoxaline small molecules (RA-1) have been developed, whose hydrophobic core facilitates selective binding to apurinic/apyrimidinic (AP) sites, particularly adenine as the complementary nucleobase opposite to the AP-sites via base stacking. RA-1 effectively cleaves TMZ-induced DNA abasic sites in-vitro at minimal concentrations through Schiff-base formation. Remarkably, the combination of TMZ and RA-1 exerts a notable synergistic effect on both types of cells. The underlying mechanism of this synergy is rooted in the cleavage of TMZ-induced DNA abasic sites, which impairs the BER pathway, leading to the formation of DNA double-strand breaks. Consequently, the ATM-Chk2/ATR-Chk1 signalling pathways are activated, prompting S-phase arrest and ultimately driving apoptosis. These findings provide a compelling rationale for targeting DNA abasic sites to synergistically augment TMZ responses in both MMR-proficient and deficient cancer cells.
The Long-Term Impact of the Tips From Former Smokers® Campaign on Calls to 1-800-QUIT-NOW, 2012–2023
Authors: Mann Nathan H , Murphy-Hoefer Rebecca L , Davis Kevin C , Von Jaglinsky Annette S , Rodes Robert M , Beistle Diane M 
Published: July 2024

Abstract

Introduction
There is substantial evidence that mass media campaigns increase calls to quitlines as well as smoking cessation. In 2012, the Centers for Disease Control and Prevention launched the first federally funded national tobacco education campaign, Tips From Former Smokers® (ie, Tips). From 2012 through 2023, Tips aired advertisements on television. To date, no studies have examined the long-term effect of a national smoking cessation campaign on quitline calls. This study examined the long-term impact of Tips television ads on calls to 1-800-QUIT-NOW from 2012 through 2023.

Methods
Exposure to the Tips campaign was measured using weekly gross rating points (GRPs) for television ads in each U.S. designated market area. We obtained data on calls to 1-800-QUIT-NOW from the National Cancer Institute and used linear regression to model calls to 1-800-QUIT-NOW, from 2012 through 2023, as a function of weekly media market-level GRPs for Tips television ads. Using the regression model results, we calculated predicted values of calls to 1-800-QUIT-NOW across observed GRP values to determine the total calls to 1-800-QUIT-NOW that were attributable to the Tips campaign during 2012–2023.

Results
Tips GRPs were positively and significantly associated with calls to 1-800-QUIT-NOW across all years (b = 39.94, p &lt; .001). Based on this association, we estimate the Tips campaign generated nearly 2.1 million additional calls to 1-800-QUIT-NOW during 2012–2023.

Conclusions
Exposure to the Tips campaign has consistently and significantly increased calls to tobacco quitlines.

Implications
Quitlines provide evidence-based support to help people quit smoking. They have been shown to increase the likelihood of successfully quitting. Mass media campaigns have promoted quitlines, and quitline calls have increased significantly with media promotion. The long-term effect of campaigns—like the Centers for Disease Control and Prevention’s Tips From Former Smokers® (ie, Tips)—on quitline calls has not been determined. From 2012 through 2023, exposure to the Tips campaign is estimated to have generated nearly 2.1 million additional calls to 1-800-QUIT-NOW. This study supports the continued use of mass media to promote quitlines.
Put the Vanc Down, Flip It and Reverse It: Comparison of Vancomycin and Daptomycin Health Care Utilization and Cost in Outpatient Parenteral Antimicrobial Therapy
Authors: Streifel Amber C , Luis Katie , Nakrani Monark , Yu Diana , Sikka Monica K , Varley Cara D , Douglass Alyse , Mayer Heather , Young Kathleen , Lewis James S 
Published: July 2024

Abstract
Vancomycin and daptomycin are frequently used in outpatient parenteral antimicrobial therapy (OPAT). We analyze health care utilization and cost to the health care system for vancomycin vs daptomycin in the outpatient setting and find that vancomycin results in significantly higher health care utilization and similar cost per course compared with daptomycin in OPAT.
A kinematic analysis of the giant molecular complex W3: Possible evidence for cloud–cloud collisions that triggered OB star clusters in W3 Main and W3(OH)
Authors: Yamada Rin I , Sano Hidetoshi , Tachihara Kengo , Enokiya Rei , Nishimura Atsushi , Fujita Shinji , Kohno Mikito , Bieging John H , Fukui Yasuo 
Published: July 2024

Abstract
W3 is one of the most outstanding regions of high-mass star formation in the outer solar circle, and includes two active star-forming clouds: W3 Main and W3(OH). Based on a new analysis of the ${^{12}\text{CO}(J = 2-1)}$ data obtained at $38^{\prime \prime }$ resolution, we have found three clouds that have molecular masses from 2000 to $8000\, {M_\odot }$ at velocities $-50\:\rm{km\: s^{-1}}$, $-43\:\rm{km\:s^{-1}}$, and $-39\:\rm{km\:s^{-1}}$. The $-43\:\rm{km\:s^{-1}}$ cloud is the most massive one, overlapping with the $-39\:\rm{km\:s^{-1}}$ cloud and the $-50\:\rm{km\:s^{-1}}$ cloud toward W3 Main and W3(OH), respectively. In W3 Main and W3(OH), we have found typical signatures of a cloud–cloud collision, i.e., the complementary distribution with/without a displacement between the two clouds and/or a V-shape in the position–velocity diagram. We frame a hypothesis that a cloud–cloud collision triggered the high-mass star formation in each region. The collision in W3 Main involves the $-39\:\rm{km\:s^{-1}}$ cloud and the $-43\:\rm{km\:s^{-1}}$ cloud. The collision likely produced a cavity in the $-43\:\rm{km\:s^{-1}}$ cloud that has a size similar to the $-39\:\rm{km\:s^{-1}}$ cloud and triggered the formation of young high-mass stars in IC 1795 $2\:$Myr ago. We suggest that the $-39\:\rm{km\:s^{-1}}$ cloud is still triggering the high-mass objects younger than $1\:$Myr currently embedded in W3 Main. On the other hand, another collision between the $-50\:\rm{km\:s^{-1}}$ cloud and the $-43\:\rm{km\:s^{-1}}$ cloud likely formed the heavily embedded objects in W3(OH) within $\sim\! 0.5\:$Myr ago. The present results favour an idea that cloud–cloud collisions are common phenomena not only in the inner solar circle but also in the outer solar circle, where the number of reported cloud–cloud collisions is yet limited (Fukui et al. 2021, PASJ, 73, S1).
Partisans neither expect nor receive reputational rewards for sharing falsehoods over truth online
Authors: Ghezae Isaias , Jordan Jillian J , Gainsburg Izzy B , Mosleh Mohsen , Pennycook Gordon , Willer Robb , Rand David G 
Published: July 2024

Abstract
A frequently invoked explanation for the sharing of false over true political information is that partisans are motivated by their reputations. In particular, it is often argued that by indiscriminately sharing news that is favorable to one's political party, regardless of whether it is true—or perhaps especially when it is not true—partisans can signal loyalty to their group, and improve their reputations in the eyes of their online networks. Across three survey studies (total N = 3,038), and an analysis of over 26,000 tweets, we explored these hypotheses by measuring the reputational benefits that people anticipate and receive from sharing different content online. In the survey studies, we showed participants actual news headlines that varied in (ⅰ) veracity, and (ⅱ) favorability to their preferred political party. Across all three studies, participants anticipated that sharing true news would bring more reputational benefits than sharing false news. Critically, while participants also expected greater reputational benefits for sharing news favorable to their party, the perceived reputation value of veracity was no smaller for more favorable headlines. We found a similar pattern when analyzing engagement on Twitter: among headlines that were politically favorable to a user's preferred party, true headlines elicited more approval than false headlines.