bluuebunny/crossref_metadata_2025_split huggingface dataset:
Better Together: How Clustering Can Attenuate Hedonic Decline
Authors: Chen Jinjie , Redden Joseph P 
Published: October 2023

Abstract
How should consumers sequence the different stimuli they consume: cluster each stimulus together, or intermix them to break things up? Surprisingly, prior literature has provided little insight into this question, even though consumers face it on a regular basis. We propose that clustering each stimulus type together can prolong enjoyment (vs. intermixing the types). Six studies confirm that clustering slows hedonic decline, and process evidence shows this happens because clustering leads people to attend more to the different details offered by a stimulus during repeated exposures. We also establish two boundary conditions for this effect: clustering does not slow hedonic decline in the presence of regular intervening distractions, or for impoverished stimuli lacking rich details. The present work is among the first to examine the interplay of consumption sequence and hedonic decline, and the findings provide consumers and firms with practical guidance on how to consider sequencing experiences to enjoy them longer.
Diversification, vertical integration and economic resilience: evidence from intercity truck flows during COVID-19 in China
Authors: Fang Da , Guo Yan , Zhang Haochen 
Published: October 2023

AbstractThis article examines economic resilience by combining high-frequency truck flows and the lockdown policy shock during COVID-19 in China. We discover that the truck flows in regions with higher levels of diversification and vertical integration see a smaller decrease in response to the COVID-19 shock. Dynamically, such moderating effects of diversification and vertical integration get smaller with the recovery of interregional economic linkages. Diversification and integration also mitigate the negative impact from nonlocal infection cases. The association between the industrial structure attributes and economic resilience is more prominent in regions with lower centrality in the nationwide intercity truck flow network.
Geopolitical decoupling and global production networks: the case of Ukrainian industries after the 2014 Crimean annexation
Authors: Blažek Jiří , Lypianin Anton 
Published: October 2023

Abstract
This study investigates the decoupling of Ukrainian aerospace, defense and electro-engineering industries resulting from the Russian Crimean annexation in 2014. Conceptually, we contribute to global value chain/global production network research by developing the notion of geopolitical decoupling, thus augmenting the existing 2-fold typology. Moreover, the article elaborates a typology of recoupling. Empirically, we investigate patterns of decoupling from Russia and recoupling via alternative production networks as well as patterns of decoupling/recoupling according to the position of companies in the production hierarchy. We found a neat pattern of decoupling from Russia according to tier but profoundly different dynamics of recoupling with the European Union and Asia.
Assessment of intrafractional motion of the cervix–uterus by MR-guided radiotherapy system
Authors: Nagao Ayaka , Okamoto Hiroyuki , Nakayama Hiroki , Chiba Takahito , Fujiyama Daisuke , Kuwahara Junichi , Sakasai Tatsuya , Kashihara Tairo , Kaneda Tomoya , Inaba Koji , Okuma Kae , Murakami Naoya , Igaki Hiroshi 
Published: October 2023

Abstract
The uterus is known as one of the moving organs. We evaluated the movement of the uterus during irradiation and the effects of changes in the surrounding organs using a magnetic resonance (MR)-guided radiotherapy system. Seven patients with cervical cancer underwent pre- and posttreatment MR imaging to assess changes in the positioning of the uterus and cervix as well as the alterations in bladder and rectal volume. The study revealed that the movements of the uterus were greater than that of the cervix and showed a tendency to correlate with the bladder rather than the rectum. We also examined whether intrafractional motion could lead to insufficient dose coverage of the clinical target volume (CTV), specifically focusing on the D98% of the CTV in the uterine body and cervix. The impact of intrafractional motion on the D98% varied among patients, with one out of the seven patients experiencing an average dosimetric change of −2.6 Gy in the uterus, although larger planning target volume margins of 1.5 cm were applied, therefore, indicating the need for individualized optimal margins in each case. Online adaptive radiotherapy offers the advantage of modifying the treatment plan when irradiating moving organs, such as the uterus. However, it should be noted that this approach may result in longer overall treatment times compared with the traditional methods. Therefore, we must carefully consider the influence of intrafractional organ motions when opting for such a treatment.
Surgical treatment for a giant venous malformation of the parotid area
Authors: Urabe Ryotaro , Miyamae Makoto , Minegishi Yoshiki , Nakai Kunihiro 
Published: October 2023

Abstract
This report discusses the surgical treatment of a giant parotid venous malformation (VM) that had grown beyond the dimensions of the parotid gland, causing significant displacement. Special attention was paid to identifying the facial nerve, which was found to traverse the surface of the VM. Although, in our case, the facial nerve ran superficially on the VM, it is possible that a portion of it penetrated the mass. A two-stage excision and revision surgery strategy was employed due to the complexity of assessing deformities after removing the giant lesion. During the initial surgery, the displaced superficial lobe of the parotid gland was repositioned to its original location and carefully laid over the facial nerve, ensuring its safety during the subsequent procedure.
An emulator-based halo model in modified gravity – I. The halo concentration–mass relation and density profile
Authors: Ruan Cheng-Zong , Cuesta-Lazaro Carolina , Eggemeier Alexander , Li Baojiu , Baugh Carlton M , Arnold Christian , Bose Sownak , Hernández-Aguayo César , Zarrouk Pauline , Davies Christopher T 
Published: October 2023

ABSTRACT
In this series of papers, we present an emulator-based halo model for the non-linear clustering of galaxies in modified gravity cosmologies. In the first paper, we present emulators for the following halo properties: the halo mass function, concentration–mass relation and halo-matter cross-correlation function. The emulators are trained on data extracted from the forge and bridge suites of N-body simulations, respectively, for two modified gravity (MG) theories: f(R) gravity, and the DGP model, varying three standard cosmological parameters Ωm0, H0, σ8, and one MG parameter, either $\bar{f}_{R0}$ or rc. Our halo property emulators achieve an accuracy of ${\lesssim}1\ \hbox{per cent}$ on independent test data sets. We demonstrate that the emulators can be combined with a galaxy–halo connection prescription to accurately predict the galaxy–galaxy and galaxy–matter correlation functions using the halo model framework.
Constraints on pre-SN outbursts from the progenitor of SN 2023ixf using the large binocular telescope
Authors: Neustadt J M M , Kochanek C S , Smith M Rizzo 
Published: October 2023

ABSTRACT
The progenitor of SN 2023ixf was an ∼104.8 to $10^{5.0}\, \text{L}_\odot$ star (∼9 to $14\, \text{M}_\odot$ at birth) obscured by a dusty $\dot{M} \simeq 10^{-5}\, \text{M}_\odot \rm \, yr^{-1}$ wind with a visual optical depth of τV ≃ 13. This is required by the progenitor spectral energy distribution, the post-SN X-ray and H α luminosities, and the X-ray column density estimates. In Large Binocular Telescope (LBT) data spanning 5600 to 400 d before the supernova (SN), there is no evidence for optical variability at the level of $\sim 10^3\, \text{L}_\odot$ in R band, roughly three times the predicted luminosity of the obscured progenitor. This constrains direct observation of any pre-SN optical outbursts where there are LBT observations. However, models of the effects of any pre-SN outburst on the dusty wind show that an outburst of essentially any duration exceeding ∼5 times the luminosity of the progenitor would have detectable effects on the dust optical depth for decades. While the dust obscuration here is high, all red supergiants have dusty winds, and the destruction (or formation) of dust by even short-lived transients will always have long-term effects on the observed brightness of the star because changes in the dust optical depths after a luminous transient occur very slowly.
Evolution of low-frequency quasi-periodic oscillations in GX 339-4 during its 2021 outburst using AstroSat data
Authors: Mondal Santanu , Salgundi Anirudh , Chatterjee Debjit , Jana Arghajit , Chang H-K , Naik Sachindra 
Published: October 2023

ABSTRACT
The black hole X-ray binary GX 339-4 showed an X-ray outburst during 2021. The AstroSat captured this outburst when the source entered into the intermediate flux state while the count rate was declining. The source showed an alternating flux profile in a time-scale of ≲100 ks, where the hard energy band was more variable than the soft band. The energy-dependent timing study showed that the observed quasi-periodic oscillation (QPO) was prominent in the low-energy bands, with its nearly sub-harmonic and harmonic components. These components appear and disappear with time, as observed in the orbit-wise QPO study. The Q-value, fractional rms, and 4.8–5.6 Hz frequency infer the QPOs as type-B and the spectral state as soft intermediate. The rms spectra of all orbits exhibiting QPOs show an increase in amplitude till ∼10 keV, beyond which it starts decreasing. This may indicate that ∼10 keV photons contributed relatively more in QPOs than other energy band photons. The Lorentzian normalization of the type-B QPO in different energy bands is consistent with the 10 keV peak. The energy-dependent time lag is complex and could be associated with the Comptonizing corona or jet. Finally, we discuss possible reasons behind the origin of different timing properties observed.
Close encounters of star–black hole binaries with single stars
Authors: Ryu Taeho , de Mink Selma E , Farmer Rob , Pakmor Rüdiger , Perna Rosalba , Springel Volker 
Published: October 2023

ABSTRACT
Multibody dynamical interactions of binaries with other objects are one of the main driving mechanisms for the evolution of star clusters. It is thus important to bring our understanding of three-body interactions beyond the commonly employed point-particle approximation. To this end, we here investigate the hydrodynamics of three-body encounters between star–black hole (BH) binaries and single stars, focusing on the identification of final outcomes and their long-term evolution and observational properties, using the moving-mesh hydrodynamics code AREPO. This type of encounter produces five types of outcomes: stellar disruption, stellar collision, weak perturbation of the original binary, binary member exchange, and triple formation. The two decisive parameters are the binary phase angle, which determines which two objects meet at the first closest approach, and the impact parameter, which sets the boundary between violent and non-violent interactions. When the impact parameter is smaller than the semimajor axis of the binary, tidal disruptions and star-BH collisions frequently occur when the BH and the incoming star first meet, while the two stars mostly merge when the two stars meet first instead. In both cases, the BHs accrete from an accretion disc at super-Eddington rates, possibly generating flares luminous enough to be observed. The stellar collision products either form a binary with the BH or remain unbound to the BH. Upon collision, the merged stars are hotter and larger than the main sequence stars of the same mass at similar age. Even after recovering their thermal equilibrium state, stellar collision products, if isolated, would remain hotter and brighter than main sequence stars until becoming giants.
An ALMA Survey of M-dwarfs in the Beta Pictoris Moving Group with two new debris disc detections
Authors: Cronin-Coltsmann Patrick F , Kennedy Grant M , Kral Quentin , Lestrade Jean-François , Marino Sebastian , Matrà Luca , Wyatt Mark C 
Published: October 2023

ABSTRACT
Previous surveys in the far-infrared have found very few, if any, M-dwarf debris discs among their samples. It has been questioned whether M-dwarf discs are simply less common than earlier types, or whether the low detection rate derives from the wavelengths and sensitivities available to those studies. The highly sensitive, long-wavelength Atacama Large Millimetre/submillimetre Array (ALMA) can shed light on the problem. This paper presents a survey of M-dwarf stars in the young and nearby Beta Pictoris Moving Group with ALMA at Band 7 (880 μm). From the observational sample, we detect two new sub-mm excesses that likely constitute unresolved debris discs around GJ 2006 A and AT Mic A and model distributions of the disc fractional luminosities and temperatures. From the science sample of 36 M-dwarfs including AU Mic, we find a disc detection rate of 4/36 or 11.1$^{+7.4}_{-3.3}$ per cent that rises to 23.1$^{+8.3}_{-5.5}$ per cent when adjusted for completeness. We conclude that this detection rate is consistent with the detection rate of discs around G- and K-type stars and that the disc properties are also likely consistent with earlier type stars. We additionally conclude that M-dwarf stars are not less likely to host debris discs, but instead their detection requires longer wavelength and higher sensitivity observations than have previously been employed.
NEATH – II. N2H+ as a tracer of imminent star formation in quiescent high-density gas
Authors: Priestley F D , Clark P C , Glover S C O , Ragan S E , Fehér O , Prole L R , Klessen R S 
Published: October 2023

ABSTRACT
Star formation activity in molecular clouds is often found to be correlated with the amount of material above a column density threshold of ${\sim} 10^{22} \, {\rm cm}^{-2}$. Attempts to connect this column density threshold to a volume density above which star formation can occur are limited by the fact that the volume density of gas is difficult to reliably measure from observations. We post-process hydrodynamical simulations of molecular clouds with a time-dependent chemical network, and investigate the connection between commonly observed molecular species and star formation activity. We find that many molecules widely assumed to specifically trace the dense, star-forming component of molecular clouds (e.g. HCN, HCO+, CS) actually also exist in substantial quantities in material only transiently enhanced in density, which will eventually return to a more diffuse state without forming any stars. By contrast, N2H+ only exists in detectable quantities above a volume density of $10^4 \, {\rm cm}^{-3}$, the point at which CO, which reacts destructively with N2H+, begins to deplete out of the gas phase on to grain surfaces. This density threshold for detectable quantities of N2H+ corresponds very closely to the volume density at which gas becomes irreversibly gravitationally bound in the simulations: the material traced by N2H+ never reverts to lower densities, and quiescent regions of molecular clouds with visible N2H+ emission are destined to eventually form stars. The N2H+ line intensity is likely to directly correlate with the star formation rate averaged over time-scales of around a Myr.
Investigating the orbital evolution of the eccentric HMXB GX 301–2 using long-term X-ray light curves
Authors: Manikantan Hemanth , Kumar Manish , Paul Biswajit , Rana Vikram 
Published: October 2023

ABSTRACT
We report the orbital decay rate of the high-mass X-ray binary GX 301–2 from an analysis of its long-term X-ray light curves and pulsed flux histories from CGRO/BATSE, RXTE/ASM, Swift/BAT, Fermi/GBM, and MAXI by timing the pre-periastron flares over a span of almost 30 yr. The time of arrival of the pre-periastron flares exhibits an energy dependence (hard lag) and the orbital period decay was estimated after correcting for it. This method of orbital decay estimation is unaffected by the fluctuations in the spin rate of the X-ray pulsar associated with variations in the mass accretion rate. The resulting $\dot{P}_\textrm {orb}$ = −(1.98 ± 0.28) × 10−6 s s−1 indicates a rapid evolution time-scale of $|P_\textrm {orb}/\dot{P}_\textrm {orb}|\sim 0.6\times 10^{5}$ yr, making it the high mass X-ray binary with the fastest orbital decay. Our estimate of $\dot{P}$orb is off by a factor of ∼2 from the previously reported value of −(3.7 ± 0.5) × 10−6 s s−1 estimated from pulsar TOA analysis. We discuss various possible mechanisms that could drive this rapid orbital decay and also suggest that GX 301–2 is a prospective Thorne–Żytkow candidate.
Resolved low-J12CO excitation at 190 parsec resolution across NGC 2903 and NGC 3627
Authors: den Brok J S , Leroy A K , Usero A , Schinnerer E , Rosolowsky E , Koch E W , Querejeta M , Liu D , Bigiel F , Barnes A T , Chevance M , Colombo D , Dale D A , Glover S C O , Jimenez-Donaire M J , Teng Y-H , Williams T G 
Published: October 2023

ABSTRACT
The low-J rotational transitions of 12CO are commonly used to trace the distribution of molecular gas in galaxies. Their ratios are sensitive to excitation and physical conditions in the molecular gas. Spatially resolved studies of CO ratios are still sparse and affected by flux calibration uncertainties, especially since most do not have high angular resolution or do not have short-spacing information and hence miss any diffuse emission. We compare the low-J CO ratios across the disc of two massive, star-forming spiral galaxies NGC 2903 and NGC 3627 to investigate whether and how local environments drive excitation variations at GMC scales. We use Atacama Large Millimeter Array (ALMA) observations of the three lowest-J CO transitions at a common angular resolution of 4 arcsec (190 pc). We measure median line ratios of $R_{21}=0.67^{+0.13}_{-0.11}$, $R_{32}=0.33^{+0.09}_{-0.08}$, and $R_{31}=0.24^{+0.10}_{-0.09}$ across the full disc of NGC 3627. We see clear CO line ratio variation across the galaxy consistent with changes in temperature and density of the molecular gas. In particular, towards the centre, R21, R32, and R31 increase by 35 per cent, 50 per cent, and 66 per cent, respectively, compared to their average disc values. The overall line ratio trends suggest that CO(3–2) is more sensitive to changes in the excitation conditions than the two lower J transitions. Furthermore, we find a similar radial R32 trend in NGC 2903, albeit a larger disc-wide average of $\langle R_{32}\rangle =0.47^{+0.14}_{-0.08}$. We conclude that the CO low-J line ratios vary across environments in such a way that they can trace changes in the molecular gas conditions, with the main driver being changes in temperature.
Beyond the 3rd moment: a practical study of using lensing convergence CDFs for cosmology with DES Y3
Authors: Anbajagane D , Chang C , Banerjee A , Abel T , Gatti M , Ajani V , Alarcon A , Amon A , Baxter E J , Bechtol K , Becker M R , Bernstein G M , Campos A , Rosell A Carnero , Kind M Carrasco , Chen R , Choi A , Davis C , DeRose J , Diehl H T , Dodelson S , Doux C , Drlica-Wagner A , Eckert K , Elvin-Poole J , Everett S , Ferté A , Gruen D , Gruendl R A , Harrison I , Hartley W G , Huff E M , Jain B , Jarvis M , Jeffrey N , Kacprzak T , Kokron N , Kuropatkin N , Leget P-F , MacCrann N , McCullough J , Myles J , Navarro-Alsina A , Pandey S , Prat J , Raveri M , Rollins R P , Roodman A , Rykoff E S , Sánchez C , Secco L F , Sevilla-Noarbe I , Sheldon E , Shin T , Troxel M A , Tutusaus I , Whiteway L , Yanny B , Yin B , Zhang Y , Abbott T M C , Allam S , Aguena M , Alves O , Andrade-Oliveira F , Annis J , Bacon D , Blazek J , Brooks D , Cawthon R , da Costa L N , Pereira M E S , Davis T M , Desai S , Doel P , Ferrero I , Frieman J , Giannini G , Gutierrez G , Hinton S R , Hollowood D L , Honscheid K , James D J , Kuehn K , Lahav O , Marshall J L , Mena-Fernández J , Menanteau F , Miquel R , Palmese A , Pieres A , Malagón A A Plazas , Reil K , Sanchez E , Smith M , Swanson M E C , Tarle G , Wiseman P ,   (DES Collaboration)
Published: October 2023

ABSTRACT
Widefield surveys probe clustered scalar fields – such as galaxy counts, lensing potential, etc. – which are sensitive to different cosmological and astrophysical processes. Constraining such processes depends on the statistics that summarize the field. We explore the cumulative distribution function (CDF) as a summary of the galaxy lensing convergence field. Using a suite of N-body light-cone simulations, we show the CDFs’ constraining power is modestly better than the second and third moments, as CDFs approximately capture information from all moments. We study the practical aspects of applying CDFs to data, using the Dark Energy Survey (DES Y3) data as an example, and compute the impact of different systematics on the CDFs. The contributions from the point spread function and reduced shear approximation are $\lesssim 1~{{\ \rm per\ cent}}$ of the total signal. Source clustering effects and baryon imprints contribute 1–10 per cent. Enforcing scale cuts to limit systematics-driven biases in parameter constraints degrade these constraints a noticeable amount, and this degradation is similar for the CDFs and the moments. We detect correlations between the observed convergence field and the shape noise field at 13σ. The non-Gaussian correlations in the noise field must be modelled accurately to use the CDFs, or other statistics sensitive to all moments, as a rigorous cosmology tool.
Efficient 3′-pairing renders microRNA targeting less sensitive to mRNA seed accessibility
Authors: Kosek David M , Banijamali Elnaz , Becker Walter , Petzold Katja , Andersson Emma R 
Published: October 2023

Abstract
MicroRNAs (miRNAs) are short RNAs that post-transcriptionally regulate gene expression by binding to specific sites in mRNAs. Site recognition is primarily mediated by the seed region (nucleotides g2–g8 in the miRNA), but pairing beyond the seed (3′-pairing) is important for some miRNA:target interactions. Here, we use SHAPE, luciferase reporter assays and transcriptomics analyses to study the combined effect of 3′-pairing and secondary structures in mRNAs on repression efficiency. Using the interaction between miR-34a and its SIRT1 binding site as a model, we provide structural and functional evidence that 3′-pairing can compensate for low seed-binding site accessibility, enabling repression of sites that would otherwise be ineffective. We show that miRNA 3′-pairing regions can productively base-pair with nucleotides far upstream of the seed-binding site and that both hairpins and unstructured bulges within the target site are tolerated. We use SHAPE to show that sequences that overcome inaccessible seed-binding sites by strong 3′-pairing adopt the predicted structures and corroborate the model using luciferase assays and high-throughput modelling of 8177 3′-UTR targets for six miRNAs. Finally, we demonstrate that PHB2, a target of miR-141, is an inaccessible target rescued by efficient 3′-pairing. We propose that these results could refine predictions of effective target sites.