bluuebunny/crossref_metadata_2025_split huggingface dataset:
Beliefs and Perceived Barriers Regarding Psychedelic-assisted Therapy in a Pilot Study of Service Members and Veterans With a History of Traumatic Brain Injury
Authors: Gray Joshua C , Murphy Mikela , Carter Sierra E , Johnson Matthew W , Wolfgang Aaron S , Roy Michael J , Maples-Keller Jessica L 
Published: December 2022

ABSTRACT

Introduction
Posttraumatic stress disorder (PTSD) and depression are common in service members and veterans, and the response to currently available treatments is often modest at best. Recent studies suggest potential benefit with psychedelic-assisted therapies (PATs), particularly 3,4-methylenedioxymethamphetamine-assisted therapy for PTSD and psilocybin-assisted therapy for depression. This study examined beliefs and perceived barriers regarding PAT among service members and veterans to inform the delivery of these treatments if they are approved by the FDA.

Materials and Methods
Twenty-one service members and veterans (67% male, 81% White, and 43% active duty) with a history of traumatic brain injury and co-occurring cognitive and psychological symptoms completed a measure assessing baseline knowledge and views of PAT, read a brief psychoeducation regarding PAT, and then responded to questions related to their beliefs and perceived barriers to PAT.

Results
Before psychoeducation, participants reported a neutral view of psychedelic drugs (M = 2.76; range: 1-5), PAT (M = 3.33), and interest in PAT (M = 3.10). After psychoeducation, participants reported a significantly more positive view of psychedelic drugs (M = 3.24, P = .014) and interest in PAT (M = 3.67, P = .016). Overall, participants indicated that they would support PAT availability in medical settings if proven beneficial (M = 4.52; 5 = “agree strongly”) and they would support a loved one engaging in PAT (M = 4.29). The most frequently reported health concerns were concern of long-term effects (43%), fear of losing their mind (33%), fear of personality changes (33%), and fear of traumatic brain injury complications (24%). The most frequently endorsed barriers were time commitment, transportation, financial concerns, work, and childcare (33%-19%), with 48% reporting no barriers.

Conclusions
This is the first study to explore beliefs and perceived barriers regarding PAT among service members and veterans. These results indicate that military populations may be interested in PAT, particularly if psychoeducation and outreach regarding these treatments occurred. If FDA approved, it will be important to facilitate command support and address logistical barriers to ensure appropriate access within military contexts.
The Uchuu-universe machine data set: galaxies in and around clusters
Authors: Aung Han , Nagai Daisuke , Klypin Anatoly , Behroozi Peter , Abdullah Mohamed H , Ishiyama Tomoaki , Prada Francisco , Pérez Enrique , López Cacheiro Javier , Ruedas José 
Published: December 2022

ABSTRACT
We present the public data release of the Uchuu-UM galaxy catalogues by applying the UniverseMachine algorithm to assign galaxies to the dark matter haloes in the Uchuu N-body cosmological simulation. It includes a variety of baryonic properties for all galaxies down to ∼5 × 108 M⊙ with haloes in a mass range of 1010 &lt; Mhalo/M⊙ &lt; 5 × 1015 up to redshift z = 10. Uchuu-UM includes more than 104 cluster-size haloes in a volume of 8(h−1Gpc)3, reproducing observed stellar mass functions across the redshift range of z = 0−7, galaxy quenched fractions, and clustering statistics at low redshifts. Compared to the previous largest UM catalogue, the Uchuu-UM catalogue includes significantly more massive galaxies hosted by large-mass dark matter haloes. Overall, the number density profile of galaxies in dark matter haloes follows the dark matter profile, with the profile becoming steeper around the splashback radius and flattening at larger radii. The number density profile of galaxies tends to be steeper for larger stellar masses and depends on the colour of galaxies, with red galaxies having steeper slopes at all radii than blue galaxies. The quenched fraction exhibits a strong dependence on the stellar mass and increases towards the inner regions of clusters. The publicly available Uchuu-UM galaxy catalogue presented here can serve to model ongoing and upcoming large galaxy surveys.
X-ray and UV radiation in the planet-forming T-Tauri system PDS 70. Signs of accretion and coronal activity
Authors: Joyce Simon R G , Pye John P , Nichols Jonathan D , Alexander Richard , Güdel Manuel , Barrado David 
Published: December 2022

ABSTRACT
Planet formation takes place in protoplanetary discs around young T-Tauri stars. PDS 70 is one of the first confirmed examples of a system where the planets are currently forming in gaps in the disc, and can be directly imaged. One of the main early influences on planet formation is the lifetime of the protoplanetary disc, which is limited by the intense stellar X-ray and UV radiation. Stellar coronal activity and accretion of material onto the star are both potential sources of XUV radiation. Previous Swift observations detected UV emission, which were consistent with a low rate of accretion. We present follow up observations with the XMM-Newton observatory, which observed PDS 70 simultaneously in X-ray and UV in order to determine intensity of XUV radiation in the system, and identify if the source is coronal, accretion, or both. We detect a strong source in both X-ray and UV, with an average X-ray 0.2–12 keV luminosity of 1.37 × 1030 erg s−1, and a possible flare which increased the luminosity to 2.8 × 1030 erg s−1. The UV flux density is in excess of what would be expected from chromospheric emission, and supports the interpretation that PDS 70 has continuing weak accretion less than ∼10−10 M⊙ yr−1. The implications of the detected X-ray and UV radiation are that the disc is likely to be in the final stages of dispersal, and will be completely evaporated in the next million years, bringing an end to the primary planet formation process.
Limb darkening measurements from TESS and Kepler light curves of transiting exoplanets
Authors: Maxted Pierre F L 
Published: December 2022

ABSTRACT
Inaccurate limb-darkening models can be a significant source of error in the analysis of the light curves for transiting exoplanet and eclipsing binary star systems. To test the accuracy of published limb-darkening models, I have compared limb-darkening profiles predicted by stellar atmosphere models to the limb-darkening profiles measured from high-quality light curves of 43 FGK-type stars in transiting exoplanet systems observed by the Kepler and TESS missions. The comparison is done using the parameters $h^{\prime }_1 = I_{\lambda }({2}/{3})$ and $h^{\prime }_2 = h^{\prime }_1 - I_{\lambda }({1}/{3})$, where Iλ(μ) is the specific intensity emitted in the direction μ, the cosine of the angle between the line of sight and the surface normal vector. These parameters are straightforward to interpret and insensitive to the details of how they are computed. I find that most (but not all) tabulations of limb-darkening data agree well with the observed values of $h^{\prime }_1$ and $h^{\prime }_2$. There is a small but significant offset $\Delta h^{\prime }_1 \approx 0.006$ compared to the observed values that can be ascribed to the effect of a mean vertical magnetic field strength ≈100 G that is expected in the photospheres of these inactive solar-type stars but that is not accounted for by typical stellar model atmospheres. The implications of these results for the precision of planetary radii measured by the PLATO mission are discussed briefly.
Fraction of stars in clusters for the LEGUS dwarf galaxies
Authors: Cook D O , Lee J C , Adamo A , Calzetti D , Chandar R , Whitmore B C , Aloisi A , Cignoni M , Dale D A , Elmegreen B G , Fumagalli M , Grasha K , Johnson K E , Kennicutt R C , Kim H , Linden S T , Messa M , Östlin G , Ryon J E , Sacchi E , Thilker D A , Tosi M , Wofford A 
Published: December 2022

ABSTRACT
We study the young star cluster populations in 23 dwarf and irregular galaxies observed by the Hubble Space Telescope (HST) Legacy ExtraGalactic Ultraviolet Survey (LEGUS), and examine relationships between the ensemble properties of the cluster populations and those of their host galaxies: star formation rate (SFR) density (ΣSFR). A strength of this analysis is the availability of SFRs measured from temporally resolved star formation histories that provide the means to match cluster and host galaxy properties on several time-scales (1–10, 1–100, and 10–100 Myr). Nevertheless, studies of this kind are challenging for dwarf galaxies due to the small numbers of clusters in each system. We mitigate these issues by combining the clusters across different galaxies with similar ΣSFR properties. We find good agreement with a well-established relationship ($M_{V}^{\mathrm{ brightest}}$–SFR), but find no significant correlations between ΣSFR and the slopes of the cluster luminosity function, mass function, nor the age distribution. We also find no significant trend between the fraction of stars in bound clusters at different age ranges (Γ1–10, Γ10–100, and Γ1–100) and ΣSFR of the host galaxy. Our data show a decrease in Γ over time (from 1–10 to 10–100 Myr) suggesting early cluster dissolution, though the presence of unbound clusters in the youngest time bin makes it difficult to quantify the degree of dissolution. While our data do not exhibit strong correlations between ΣSFR and ensemble cluster properties, we cannot rule out that a weak trend might exist given the relatively large uncertainties due to low number statistics and the limited ΣSFR range probed.
Gas-phase metallicity break radii of star-forming galaxies in IllustrisTNG
Authors: Garcia Alex M , Torrey Paul , Hemler Z S , Hernquist Lars , Kewley Lisa J , Nelson Erica J , Grasha Kathryn , Zovaro Henry R M , Chen Qian-Hui 
Published: December 2022

ABSTRACT
We present radial gas-phase metallicity profiles, gradients, and break radii at redshift z = 0–3 from the TNG50-1 star-forming galaxy population. These metallicity profiles are characterized by an emphasis on identifying the steep inner gradient and flat outer gradient. From this, the break radius, Rbreak, is defined as the region where the transition occurs. We observe the break radius having a positive trend with mass that weakens with redshift. When normalized by the stellar half-mass radius, the break radius has a weaker relation with both mass and redshift. To test if our results are dependent on the resolution or adopted physics of TNG50-1, the same analysis is performed in TNG50-2 and Illustris-1. We find general agreement between each of the simulations in their qualitative trends; however, the adopted physics between TNG and Illustris differ and therefore the breaks, normalized by galaxy size, deviate by a factor of ∼2. In order to understand where the break comes from, we define two relevant time-scales: an enrichment time-scale and a radial gas mixing time-scale. We find that Rbreak occurs where the gas mixing time-scale is ∼10 times as long as the enrichment time-scale in all three simulation runs, with some weak mass and redshift dependence. This implies that galactic discs can be thought of in two-parts: a star-forming inner disc with a steep gradient and a mixing-dominated outer disc with a flat gradient, with the break radius marking the region of transition between them.
ExoMol line lists – XLVII. Rovibronic spectrum of aluminium monochloride (AlCl)
Authors: Yurchenko Sergei N , Nogué Emma , Azzam Ala’a A A , Tennyson Jonathan 
Published: December 2022

ABSTRACT
A line list for two isotopologues of aluminium monochloride, Al35Cl and Al37Cl, is presented covering the wavelength range &lt;0.2 µm, J up to 400, and applicable for temperatures up to 5000 K. The line lists are built using an empirical spectroscopic model consisting of potential energy curves, spin–orbit coupling curves, electronic angular momentum curves, and Born–Oppenheimer breakdown correction curves combined with ab initio dipole moments and cover the four lowest electronic states, ${X}\, ^1\Sigma ^+$, ${A}\, ^1\Pi$, ${a}\, ^3\Pi$, and ${b}\, ^3\Sigma ^+$. Considerable problems with the assignments of some laboratory rovibronic spectra are identified. Treatment of the states lying in the continuum is discussed. The YNAT line list is available from the ExoMol data base at www.exomol.com.
The Sherwood–Relics simulations: overview and impact of patchy reionization and pressure smoothing on the intergalactic medium
Authors: Puchwein Ewald , Bolton James S , Keating Laura C , Molaro Margherita , Gaikwad Prakash , Kulkarni Girish , Haehnelt Martin G , Iršič Vid , Šoltinský Tomáš , Viel Matteo , Aubert Dominique , Becker George D , Meiksin Avery 
Published: December 2022

ABSTRACT
We present the Sherwood–Relics simulations, a new suite of large cosmological hydrodynamical simulations aimed at modelling the intergalactic medium (IGM) during and after the cosmic reionization of hydrogen. The suite consists of over 200 simulations that cover a wide range of astrophysical and cosmological parameters. It also includes simulations that use a new lightweight hybrid scheme for treating radiative transfer effects. This scheme follows the spatial variations in the ionizing radiation field, as well as the associated fluctuations in IGM temperature and pressure smoothing. It is computationally much cheaper than full radiation hydrodynamics simulations, and circumvents the difficult task of calibrating a galaxy formation model to observational constraints on cosmic reionization. Using this hybrid technique, we study the spatial fluctuations in IGM properties that are seeded by patchy cosmic reionization. We investigate the relevant physical processes and assess their impact on the z &gt; 4 Lyman-α forest. Our main findings are: (i) consistent with previous studies patchy reionization causes large-scale temperature fluctuations that persist well after the end of reionization, (ii) these increase the Lyman-α forest flux power spectrum on large scales, and (iii) result in a spatially varying pressure smoothing that correlates well with the local reionization redshift. (iv) Structures evaporated or puffed up by photoheating cause notable features in the Lyman-α forest, such as flat-bottom or double-dip absorption profiles.
Seeking the growth of the first black hole seeds with JWST
Authors: Trinca Alessandro , Schneider Raffaella , Maiolino Roberto , Valiante Rosa , Graziani Luca , Volonteri Marta 
Published: December 2022

ABSTRACT
In this paper, we provide predictions for the black hole (BH) population that would be observable with planned JWST surveys at 5 ≤ z ≤ 15. We base our study on the recently developed Cosmic Archaeology Tool, which allows us to model BH seeds formation and growth while being consistent with the general population of active galactic nuclei (AGNs) and galaxies observed at 4 ≤ z ≤ 7. We find that JWST planned surveys will provide a complementary view on active BHs at z &gt; 5, with JADES-Medium/-Deep being capable of detecting the numerous BHs that populate the faint-end of the distribution, COSMOS-Web sampling a large enough area to detect the rarest brightest systems, and CEERS/PRIMER bridging the gap between these two regimes. The relatively small field of view of the above surveys preferentially selects BHs with masses 6 ≤ Log(MBH/M⊙) &lt; 8 at 7 ≤ z &lt; 10, residing in relatively metal poor (Log(Z/Z⊙) ≥ −2) and massive (8 ≤ Log(M*/M⊙) &lt; 10) galaxies. At z ≥ 10, only JADES-Deep will have the sensitivity to detect growing BHs with masses 4 ≤ Log(MBH/M⊙) &lt; 6, hosted by more metal poor (−3 ≤ Log(Z/Z⊙) &lt; −2) and less massive (6 ≤ Log(M*/M⊙) &lt; 8) galaxies. In our model, the latter population corresponds to heavy BH seeds formed by the direct collapse of supermassive stars in their earliest phases of mass growth. Detecting these systems would provide invaluable insights on the nature and early growth of the first BH seeds.
Has the dust clump in the debris disc of Beta Pictoris moved?
Authors: Han Y , Wyatt M C , Dent W R F 
Published: December 2022

ABSTRACT
The edge-on debris disc of the nearby young star Beta Pictoris shows an unusual brightness asymmetry in the form of a clump. The clump has been detected in both the mid-infrared (IR) and CO, and its origin has so far remained uncertain. Here, we present new mid-IR observations of Beta Pic to track any motion of the dust clump. Together with previous observations, the data span a period of 12 yr. We measured any projected displacement of the dust clump over the 12-yr period to be $0.2^{+1.3}_{-1.4}$ au away from the star based on the median and 1σ uncertainty, and constrain this displacement to be &lt;11 au at the 3σ level. This implies that the observed motion is incompatible with Keplerian motion at the 2.8σ level. It has been posited that a planet migrating outwards may trap planetesimals into a 2:1 resonance, resulting in the observed clump at pericentre of their orbits that trails the planet. The observed motion is also incompatible with such resonant motion at the 2.6σ level. While Keplerian motion and resonant motion is still possible, the data suggest that the dust clump is more likely stationary. Such a stationary dust clump could originate from the collision or tidal disruption of a planet-sized body, or from secular perturbations due to a planet that create regions with enhanced densities in the disc.
Reversible time-step adaptation for the integration of few-body systems
Authors: Boekholt Tjarda C N , Vaillant Timothée , Correia Alexandre C M 
Published: December 2022

ABSTRACT
The time-step criterion plays a crucial role in direct N-body codes. If not chosen carefully, it will cause a secular drift in the energy error. Shared, adaptive time-step criteria commonly adopt the minimum pairwise time-step, which suffers from discontinuities in the time evolution of the time-step. This has a large impact on the functioning of time-step symmetrization algorithms. We provide new demonstrations of previous findings that a smooth and weighted average over all pairwise time-steps in the N-body system, improves the level of energy conservation. Furthermore, we compare the performance of 27 different time-step criteria, by considering three methods for weighting time-steps and nine symmetrization methods. We present performance tests for strongly chaotic few-body systems, including unstable triples, giant planets in a resonant chain, and the current Solar System. We find that the harmonic symmetrization methods (methods A3 and B3 in our notation) are the most robust, in the sense that the symmetrized time-step remains close to the time-step function. Furthermore, based on our Solar System experiment, we find that our new weighting method based on direct pair-wise averaging (method W2 in our notation), is slightly preferred over the other methods.
A dynamics-based density profile for dark haloes – II. Fitting function
Authors: Diemer Benedikt 
Published: December 2022

ABSTRACT
The density profiles of dark matter haloes are commonly described by fitting functions such as the NFW or Einasto models, but these approximations break down in the transition region where haloes become dominated by newly accreting matter. Here, we present a simple accurate new fitting function that is inspired by the asymptotic shapes of the separate orbiting and infalling halo components. The orbiting term is described as a truncated Einasto profile, ρorb ∝ exp [ − 2/α (r/rs)α − 1/β (r/rt)β], with a five-parameter space of normalization, physically distinct scale and truncation radii, and α and β, which control how rapidly the profiles steepen. The infalling profile is modelled as a power law in overdensity that smoothly transitions to a constant at the halo centre. We show that these formulae fit the averaged total profiles in simulations to about 5 per cent accuracy across almost all of an expansive parameter space in halo mass, redshift, cosmology, and accretion rate. When fixing α = 0.18 and β = 3, the formula becomes a three-parameter model that fits individual haloes better than the Einasto profile on average. By analogy with King profiles, we show that the sharp truncation resembles a cut-off in binding energy.
Comparing energy and entropy formulations for cosmic ray hydrodynamics
Authors: Weber Matthias , Thomas Timon , Pfrommer Christoph 
Published: December 2022

ABSTRACT
Cosmic rays (CRs) play an important role in many astrophysical systems. Acting on plasma scales to galactic environments, CRs are usually modelled as a fluid, using the CR energy density as the evolving quantity. This method comes with the flaw that the corresponding CR evolution equation is not in conservative form as it contains an adiabatic source term that couples CRs to the thermal gas. In the absence of non-adiabatic changes, instead evolving the CR entropy density is a physically equivalent option that avoids this potential numerical inconsistency. In this work, we study both approaches for evolving CRs in the context of magnetohydrodynamic (MHD) simulations using the massively parallel moving-mesh code Arepo. We investigate the performance of both methods in a sequence of shock-tube tests with various resolutions and shock Mach numbers. We find that the entropy-conserving scheme performs best for the idealized case of purely adiabatic CRs across the shock while both approaches yield similar results at lower resolution. In this set-up, both schemes operate well and almost independently of the shock Mach number. Taking active CR acceleration at the shock into account, the energy-based method proves to be numerically much more stable and significantly more accurate in determining the shock velocity, in particular at low resolution, which is more typical for astrophysical large-scale simulations. For a more realistic application, we simulate the formation of several isolated galaxies at different halo masses and find that both numerical methods yield almost identical results with differences far below common astrophysical uncertainties.
Orbits of the TOI-1338 and TIC-172900988 systems
Authors: Gakis Dionysios , Gourgouliatos Konstantinos N 
Published: December 2022

ABSTRACT
Recent observations by TESS revealed the existence of circumbinary planets in the systems of TOI-1338 and TIC-172900988. The purpose of this work is to model the planetary orbits in these two systems and study them under the perspective of previous theoretical models. Each planet’s distance from the barycentre through time is simulated using N-body integrations and is compared with outcomes from a semi-analytic, a geometric and a Keplerian-based approach. Furthermore, we infer the most prominent frequencies of both planets’ orbits induced by the central binaries. We confirm that both systems appear to be stable. Lastly, we examine the implications of an additional candidate planet in TOI-1338 system finding that an extra, 48 M⊕ planet that has been hinted from observations could be located at 0.8 au without generating any radical changes to the orbits of the other members of the system.