bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Dark Energy Survey Year 3 high-redshift sample: selection, characterization, and analysis of galaxy clustering
Authors: Sánchez C , Alarcon A , Bernstein G M , Sanchez J , Pandey S , Raveri M , Prat J , Weaverdyck N , Sevilla-Noarbe I , Chang C , Baxter E , Omori Y , Jain B , Alves O , Amon A , Bechtol K , Becker M R , Blazek J , Choi A , Campos A , Rosell A Carnero , Kind M Carrasco , Crocce M , Cross D , DeRose J , Diehl H T , Dodelson S , Drlica-Wagner A , Eckert K , Eifler T F , Elvin-Poole J , Everett S , Fang X , Fosalba P , Gruen D , Gruendl R A , Harrison I , Hartley W G , Huang H , Huff E M , Kuropatkin N , MacCrann N , McCullough J , Myles J , Krause E , Porredon A , Rodriguez-Monroy M , Rykoff E S , Secco L F , Sheldon E , Troxel M A , Yanny B , Yin B , Zhang Y , Zuntz J , Abbott T M C , Aguena M , Allam S , Andrade-Oliveira F , Bertin E , Bocquet S , Brooks D , Burke D L , Carretero J , Castander F J , Cawthon R , Conselice C , Costanzi M , Pereira M E S , Desai S , Doel P , Doux C , Ferrero I , Flaugher B , Frieman J , García-Bellido J , Gutierrez G , Herner K , Hinton S R , Hollowood D L , Honscheid K , James D J , Kuehn K , Marshall J L , Mena-Fernández J , Menanteau F , Miquel R , Ogando R L C , Palmese A , Paz-Chinchón F , Pieres A , Malagón A A Plazas , Sanchez E , Scarpine V , Schubnell M , Smith M , Suchyta E , Tarle G , Thomas D , To C ,   (DES Collaboration)
Published: August 2023

ABSTRACT
The fiducial cosmological analyses of imaging surveys like DES typically probe the Universe at redshifts z &lt; 1. We present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around z ∼ 0.9, 1.2, and 1.5, which extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions. The analysis of galaxy clustering measurements, with a total signal to noise S/N ∼ 70 after scale cuts, yields robust cosmological constraints on a combination of the fraction of matter in the Universe Ωm and the Hubble parameter h, $\Omega _m h = 0.195^{+0.023}_{-0.018}$, and 2–3 per cent measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, bσ8. A companion paper (in preparation) will present the cross-correlations of these high-z samples with cosmic microwave background lensing from Planck and South Pole Telescope, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work.
Effects of massive central objects on the degree of energy equipartition of globular clusters
Authors: Aros Francisco I , Vesperini Enrico 
Published: August 2023

ABSTRACT
We present an analysis of the degree of energy equipartition in a sample of 101 Monte Carlo numerical simulations of globular clusters (GCs) hosting either a system of stellar-mass black holes (BHS), an intermediate-mass black hole (IMBH) or neither of them. For the first time, we systematically explore the signatures that the presence of BHS or IMBHs produces on the degree of energy equipartition and if these signatures could be found in current observations. We show that a BHS can halt the evolution towards energy equipartition in the cluster centre. We also show that this effect grows stronger with the number of stellar-mass black holes in the GC. The signatures introduced by IMBHs depend on how dominant their masses are to the GCs and for how long the IMBH has co-evolved with its host GCs. IMBHs with a mass fraction below 2 per cent of the cluster mass produce a similar dynamical effect to BHS, halting the energy equipartition evolution. IMBHs with a mass fraction larger than 2 per cent can produce an inversion of the observed mass-dependence of the velocity dispersion, where the velocity dispersion grows with mass. We compare our results with observations of Galactic GCs and show that the observed range of the degree of energy equipartition in real clusters is consistent with that found in our analysis. In particular, we show that some Galactic GCs fall within the anomalous behaviour expected for systems hosting a BHS or an IMBH and are promising candidates for further dynamical analysis.
Frequency of the dark matter subhalo collisions and bifurcation sequence arising formation of dwarf galaxies
Authors: Otaki Koki , Mori Masao 
Published: August 2023

ABSTRACT
The cold dark matter model predicts galaxies have 100 times more dark matter mass than stars. Nevertheless, recent observations report the existence of dark-matter-deficient galaxies with less dark matter than expected. To solve this problem, we investigate the physical processes of galaxy formation in head-on collisions between gas-containing dark matter subhaloes (DMSHs). Analytical estimation of the collision frequency between DMSHs associated with a massive host halo indicates that collisions frequently occur within one-tenth of the virial radius of the host halo, with a collision time-scale of about $10\, \mathrm{Myr}$, and the most frequent relative velocity increases with increasing radius. Using analytical models and numerical simulations, we show the bifurcation channel of the formation of dark-matter-dominated and dark-matter-deficient galaxies. In the case of low-velocity collisions, a dark-matter-dominated galaxy is formed by the merging of two DMSHs. In the case of moderate-velocity collisions, the two DMSHs penetrate each other. However, the gas medium collides, and star formation begins as the gas density increases, forming a dwarf galaxy without dark matter at the collision surface. In the case of high-velocity collisions, shock-breakout occurs due to the shock waves generated at the collision surface reaching the gas surface, and no galaxy forms. For example, the simulation demonstrates that a pair of DMSHs with a mass of $10^9\, \mathrm{M_\odot }$ containing gas of 0.1 solar metallicity forms a dark-matter-deficient galaxy with a stellar mass of $10^7\, \mathrm{M_\odot }$ for a relative velocity of $200\, \mathrm{km\, s^{-1}}$.
Orbital structure evolution in self-consistent N-body simulations
Authors: Valencia-Enríquez Diego , Puerari Ivânio , Chaves-Velasquez Leonardo 
Published: August 2023

ABSTRACT
The bar structure in disc galaxies models is formed by different families of orbits; however, it is not clear how these families of orbits support the bar throughout its secular evolution. Here, we analyse the orbital structure on three stellar disc N-body models embedded in a live dark matter halo. During the evolution of the models, discs naturally form a bar that buckles out of the galactic plane at different ages of the galaxy evolution generating boxy, X, peanut, and/or elongated shapes. To understand how the orbit families hold the bar structure, we evaluate the orbital evolution using the frequency analysis on phase space coordinates for all disc particles at different time intervals. We analyse the density maps morphology of the 2:1 family as the bar potential evolves. We showed that the families of orbits providing bar support exhibit variations during different stages of its evolutionary process, specifically prior to and subsequent to the buckling phase, likewise in the secular evolution of the bar. The disc-dominated model develops an internal boxy structure after the first Gyr. Afterwards, the outer part of the disc evolves into a peanut-shape, which lasts till the end of the simulation. The intermediary model develops the boxy structure only after 2 Gyr of evolution. The peanut shape appears 2 Gyr later and evolves slowly. The halo-dominated model develops the boxy structure much later, around 3 Gyr, and the peanut morphology is just incipient at the end of the simulation.
Star formation in the centre of NGC 1808 as observed by ALMA
Authors: Chen Guangwen , Bendo George J , Fuller Gary A , Henkel Christian , Kong Xu 
Published: August 2023

ABSTRACT
We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of 85.69- and 99.02-GHz continuum emission and H42α and H40α lines emission from the central 1 kpc of NGC 1808. These forms of emission are tracers of photoionizing stars but unaffected by dust obscuration that we use to test the applicability of other commonly star formation metrics. An analysis of the spectral energy distributions shows that free–free emission contributes about 60–90 per cent of the continuum emission in the 85–100-GHz frequency range, dependent on the region. The star formation rate (SFR) derived from the ALMA free–free emission is 3.1 ± 0.3 M⊙ yr−1. This is comparable to the SFRs measured from the infrared emission, mainly because most of the bolometric energy from the heavily obscured region is emitted as infrared emission. The radio 1.5-GHz emission yields an SFR 25 per cent lower than the ALMA value, probably because of the diffusion of the electrons producing the synchrotron emission beyond the star-forming regions. The SFRs measured from the extinction-corrected H α line emission are about 40–65 per cent of the SFR derived from the ALMA data, likely because this metric was not calibrated for high-extinction regions. Some SFRs based on extinction-corrected ultraviolet emission are similar to those from ALMA and infrared data, but given that the ultraviolet terms in the extinction correction equations are very small, these metrics seem inappropriate to apply to this dusty starburst.
Empirical extinction coefficients for the Swift-UVOT optical-through-ultraviolet passbands
Authors: Yi Fang , Haibo Yuan , Ruoyi Zhang , Jian Gao , Shuai Xu 
Published: August 2023

ABSTRACT
We calculated empirical reddening and extinction coefficients with respect to the dust reddening map of Schlegel et al. (1998) for the Swift-UVOT passbands, using the ‘star pair’ method and photometric data from the UVOT Serendipitous Source Catalogue and 2MASS as well as spectroscopic data from LAMOST Data Release 7. The reddening coefficients for the UVW2 − UVM2, UVM2 − UVW1, UVW1 − U, U − B, and B − V colours are −1.39, 2.08, 0.78, 0.72, and 0.84, respectively. The extinction coefficients for the UVW2, UVM2, UVW1, U, B, and V bands are 5.60, 6.99, 4.91, 4.13, 3.41, and 2.57, respectively. The numbers are consistent with predictions by the Fitzpatrick’s extinction law of R(V) = 3.0. Temperature-dependent variations of the coefficients are found and discussed, particularly for the ultraviolet passbands. We recommend using the new reddening and extinction coefficients in future when dereddening the Swift-UVOT data.
Photometric long-term variations of dwarf novae during quiescence
Authors: Vogt N , Vega-Manubens I 
Published: August 2023

ABSTRACT
Using the Catalina Sky Survey and Gaia alert data bases, we have carried out a systematic search for long-term variability of the brightness of dwarf novae in quiescence. A small, but significant portion of them revealed variability on time-scales between 2 and 14 yr which can be fitted, in some of the targets, by linear slopes of 0.14 mag yr−1 on average and up to 0.6 mag yr−1 in extreme cases. Another group of dwarf novae showed quasi-periodic variations in their quiescent brightness, with periods of 3.7 yr on average and up to 13 yr in extreme cases, and mean amplitudes of 0.5 mag, reaching up to 1.3 mag. The observed slopes could be understood as portions of a quasi-sinusoidal variability with larger periods, not covered by our data. SU UMa stars have, on average, smaller slope values and longer periods, compared to other dwarf novae. These variations could be interpreted as caused by magnetic activity of the secondary companion star, similar to the 11-yr solar cycle, but one could consider also other origins of this phenomenon.
Beyond diffusion: a generalized mean-field theory of turbulent dust transport in protoplanetary discs
Authors: Binkert Fabian 
Published: August 2023

ABSTRACT
Turbulence in protoplanetary discs, when present, plays a critical role in transporting dust particles embedded in the gaseous disc component. When using a field description of dust dynamics, a diffusion approach is traditionally used to model this turbulent dust transport. However, it has been shown that classical turbulent diffusion models are not fully self-consistent. Several shortcomings exist, including the ambiguous nature of the diffused quantity and the non-conservation of angular momentum. Orbital effects are also neglected without an explicit prescription. In response to these inconsistencies, we present a novel Eulerian turbulent dust transport model for isotropic and homogeneous turbulence on the basis of a mean-field theory. Our model is based on density-weighted averaging applied to the pressureless fluid equations and uses appropriate turbulence closures. Our model yields novel dynamic equations for the turbulent dust mass flux and recovers existing turbulent transport models in special limiting cases, thus providing a more general and self-consistent description of turbulent particle transport. Importantly, our model ensures the conservation of global angular and linear momentum unconditionally and implicitly accounts for the effects of orbital dynamics in protoplanetary discs. Furthermore, our model correctly describes the vertical settling–diffusion equilibrium solutions for both small and large particles. Hence, this work presents a generalized Eulerian turbulent dust transport model, establishing a comprehensive framework for more detailed studies of turbulent dust transport in protoplanetary discs.
Steady states of the Parker instability: the effects of rotation
Authors: Tharakkal Devika , Shukurov Anvar , Gent Frederick A , Sarson Graeme R , Snodin Andrew 
Published: August 2023

ABSTRACT
We model the Parker instability in vertically stratified isothermal gas using non-ideal MHD three-dimensional simulations. Rotation, especially differential, more strongly and diversely affects the nonlinear state than the linear stage (where we confirm the most important conclusions of analytical models), and stronger than any linear analyses predict. Steady-state magnetic fields are stronger and cosmic ray energy density is higher than in comparable non-rotating systems. Transient gas outflows induced by the nonlinear instability persist longer, of order 2 Gyr, with rotation. Stratification combined with (differential) rotation drives helical flows, leading to mean-field dynamo. Consequently, the nonlinear state becomes oscillatory (while both the linear instability and the dynamo are non-oscillatory). The horizontal magnetic field near the mid-plane reverses its direction propagating to higher altitudes as the reversed field spreads buoyantly. The spatial pattern of the large-scale magnetic field may explain the alternating magnetic field directions in the halo of the edge-on galaxy NGC 4631. Our model is unique in producing a large-scale magnetic structure similar to such observation. Furthermore, our simulations show that the mean kinetic helicity of the magnetically driven flows has the sign opposite to that in the conventional non-magnetic flows. This has profound consequences for the nature of the dynamo action and large-scale magnetic field structure in the coronae of spiral galaxies that remain to be systematically explored and understood. We show that the energy density of cosmic rays and magnetic field strength are not correlated at scales of order 1 kiloparsec.
Giant molecular cloud G18.1-0.3+51 associated with H ii regions and supernova remnant in the 3-kpc expanding ring
Authors: Sofue Yoshiaki 
Published: August 2023

ABSTRACT
Analysing the high-resolution CO line survey of the Galactic plane with the Nobeyama 45-m telescope (FUGIN), we show that the star-forming complex G18.15-0.30+51 (G18) at radial velocity of 51 km s−1 is a tight triple association of a giant molecular cloud (GMC), H ii regions, and a supernova remnant (SNR). The radial velocity of G18 allows three possible kinematic distances of d = 3.9 ± 0.2 kpc for near solution or 12 ± 0.2 kpc for far solution, if we assume circular Galactic rotation, or d = 6.1 ± 0.1 kpc, if it is moving with the 3-kpc expanding ring at an expanding velocity of 50 km s−1. The H i line absorption of radio continuum from the H ii region constrains the distance to 5.6 ≲ dSNR ≤ 7.6 kpc. The Σ−D (radio brightness–diameter) relation yields the distance to the SNR of $d_{\rm SNR}=10.1^{+11.5}_{-4.7}$ kpc, allowing for a minimum distance of 5.4 kpc. From these, we uniquely determined the distance of G18 to be 6.07 ± 0.13 kpc in the 3-kpc expanding ring with the SNR being physically associated. The molecular mass of the GMC is estimated to be Mmol ∼ 3 × 105 M⊙. The ratio of virial to luminous molecular masses is greater than unity in the central region and decreases outward to ≲0.2 at the cloud edge, indicating that the central region is dynamic, while the entire cloud is stable. We discuss the origin of the G18 triple system and propose a sustainable GMC model with continuous star formation.
First light and reionization epoch simulations (FLARES) X iii: the lyman-continuum emission of high-redshift galaxies
Authors: Seeyave Louise T C , Wilkins Stephen M , Kuusisto Jussi K , Lovell Christopher C , Irodotou Dimitrios , Simmonds Charlotte , Vijayan Aswin P , Thomas Peter A , Roper William J , Byrne Conor M , Jones Gareth T , Turner Jack C , Conselice Christopher J 
Published: August 2023

ABSTRACT
The history of reionization is highly dependent on the ionizing properties of high-redshift galaxies. It is therefore important to have a solid understanding of how the ionizing properties of galaxies are linked to physical and observable quantities. In this paper, we use the First Light and Reionization Epoch Simulations (Flares) to study the Lyman-continuum (LyC, i.e. hydrogen-ionizing) emission of massive ($M_*\gt 10^8\, \mathrm{M_\odot }$) galaxies at redshifts z = 5 − 10. We find that the specific ionizing emissivity (i.e. intrinsic ionizing emissivity per unit stellar mass) decreases as stellar mass increases, due to the combined effects of increasing age and metallicity. Flares predicts a median ionizing photon production efficiency (i.e. intrinsic ionizing emissivity per unit intrinsic far-UV luminosity) of $\log _{10}(\xi _{\rm ion}\rm {/erg^{-1}Hz})=25.40^{+0.16}_{-0.17}$, with values spanning the range $\log _{10}(\xi _{\rm ion}\rm {/erg^{-1}Hz})=25-25.75$. This is within the range of many observational estimates, but below some of the extremes observed. We compare the production efficiency with observable properties, and find a weak negative correlation with the UV-continuum slope, and a positive correlation with the [O iii] equivalent width. We also consider the dust-attenuated production efficiency (i.e. intrinsic ionizing emissivity per unit dust-attenuated far-UV luminosity), and find a median of $\log _{10}(\xi _{\rm ion}\rm {/erg^{-1}Hz})\sim 25.5$. Within our sample of $M_*\gt 10^8\, \mathrm{M_\odot }$ galaxies, it is the stellar populations in low mass galaxies that contribute the most to the total ionizing emissivity. Active galactic nuclei (AGN) emission accounts for 10 − 20 per cent of the total emissivity at a given redshift, and extends the LyC luminosity function by ∼0.5 dex.
Experiences of diagnosis and treatment for upper limb Complex Regional Pain Syndrome: a qualitative analysis
Authors: Griffiths Grace S , Thompson Bronwyn L , Snell Deborah L , Dunn Jennifer A 
Published: August 2023

Abstract

Introduction
Complex Regional Pain Syndrome (CRPS) most frequently affects the upper limb, with high associated disability. Delays to diagnosis and appropriate treatment can adversely impact prognosis and quality of life, but little is known about the healthcare experiences of people with CRPS. This study aimed to explore lived experiences of diagnosis and treatment for people with upper limb CRPS.

Methods
Participants were recruited through online support groups and multiple public and private healthcare settings in the Greater Wellington Region, New Zealand. Semi-structured interviews were conducted with participants who had experienced upper limb CRPS for more than three months and less than three years. Interviews were transcribed verbatim and analysed using reflexive thematic analysis.

Results
Thirteen participants (11 female, 2 male) aged between 43 and 68 years were interviewed. Duration of CRPS ranged from 7 months to 2.5 years. Five themes were identified. Participants initially engaged in healthcare out of a desire to return to being the person they were before having CRPS. Three interacting experiences epitomised the overall healthcare experience: (1) not knowing what is going on, (2) not being taken seriously, and (3) healthcare as adding another layer of load. Meanwhile, participants used multiple approaches in an attempt to not let CRPS stop them from continuing to live their lives.

Conclusions
Participants in this study felt that credible information, validation, and simplification from healthcare providers and systems would support their process of navigating towards a meaningful life and self-concept in the presence of CRPS.
Dynamic Equilibrium with Costly Short-Selling and Lending Market
Authors: Atmaz Adem , Basak Suleyman , Ruan Fangcheng 
Published: August 2023

Abstract
We develop a dynamic model of costly stock short-selling and lending market and obtain implications that simultaneously support many empirical regularities related to short-selling. In our model, investors’ belief disagreement leads to shorting demand, whereby short-sellers pay shorting fees to borrow stocks from lenders. Our main novel results are as follows. Short interest is positively related to shorting fee and predicts stock returns negatively. Higher short-selling risk can be associated with lower stock returns and less short-selling activity. Stock volatility is increased under costly short-selling. An application to GameStop episode yields implications consistent with observed patterns.