Sazuna/UAT_keywords huggingface dataset:
Halfway to the Peak: Ice Absorption Bands at z ≈ 0.5 with JWST MIRI/MRS. This paper presents the first combined detections of CO2, CO, XCN, and water ices beyond the local Universe. We find gas-phase CO in addition to the solid phase CO. Our source, SSTXFLS J172458.3+591545, is a z = 0.494 star-forming galaxy that also hosts a deeply obscured AGN. The profiles of its ice features are consistent with those of other Galactic and local galaxy sources, and the implied ice mantle composition is similar to that of even more obscured sources. The ice features indicate the presence of a compact nucleus in our Galaxy and allow us to place constraints on its density and temperature (n &gt; 105 cm‑3 and T = 20–90 K). We infer the visual extinction towards this nucleus to be AV ≈ 6–7. An observed plot of τSi versus τCO2/τSi can be viewed as a probe for both the total dustiness of a system as well as the clumpiness of the dust along the line of sight. This paper highlights the potential of using JWST MIRI spectra to study the dust composition and geometric distribution of sources beyond the local Universe.

Keywords: Dust composition, Active galaxies
Hunting for High-mass X-Ray Binaries in the Galactic Center with NuSTAR. The central 2 × 0.8 deg2 region of our Galaxy contains ∼10,000 X-ray point sources that were detected by a series of Chandra observations over the last two decades. However, the limited bandpass of Chandra below 8 keV hampered their spectroscopic classification. In 2016, the initial NuSTAR Galactic center (GC) survey detected 77 X-ray sources above 10 keV. The hard X-ray detections indicate magnetic cataclysmic variables, low-mass X-ray binaries, high-mass X-ray binaries (HMXBs), or even pulsars. The possibility of HMXB detections is particularly interesting given the dearth of identified HMXBs in the GC. We conducted a search for bright (Ks ≲ 16 mag) near-infrared (NIR) counterparts to the hard X-ray sources—utilizing their Chandra positions—in order to identify HMXB candidates. We identified seven NuSTAR sources with NIR counterpart candidates whose magnitudes are consistent with HMXBs at the GC. We assessed the likelihood of random association for these seven sources, and determined that two have a nonrandom association with a probability exceeding 99.98%, making them strong HMXB candidates. We analyzed broadband NuSTAR, Chandra, and XMM-Newton spectral data for these two candidates, one of which was previously identified as a red supergiant. We find that the X-ray spectra are consistent with HMXBs. If confirmed through follow-up NIR spectroscopic studies, our findings will open a new window into our understanding of the intrinsic luminosity distribution of HMXBs in our Galaxy in general and the GC HMXB population in particular.

Keywords: X-ray identification, X-ray point sources, Galactic center, High mass x-ray binary stars
Status Report on the Chicago-Carnegie Hubble Program (CCHP): Measurement of the Hubble Constant Using the Hubble and James Webb Space Telescopes. We present the latest results from the Chicago-Carnegie Hubble Program to measure the Hubble constant, using data from the James Webb Space Telescope (JWST). The overall program aims to calibrate three independent methods: (1) tip of the red giant branch (TRGB) stars, (2) J-region asymptotic giant branch (JAGB) stars, and (3) Cepheids. To date, our program includes 10 nearby galaxies, hosting 11 Type Ia supernovae (SNe Ia) suitable for measuring the Hubble constant (H0). It also includes the galaxy NGC 4258, whose geometric distance provides the zero-point calibration. In this paper, we discuss our results from the TRGB and JAGB methods. Our current best (highest-precision) estimate is H0 = 70.39 ± 1.22 (stat) ± 1.33 (sys) ± 0.70 (σSN), based on the TRGB method alone, with a total of 24 SN Ia calibrators from both Hubble Space Telescope and JWST data. Based on our new JWST data only, and tying into SNe Ia, we find values of H0 = 68.81 ± 1.79 (stat) ± 1.32 (sys) for the TRGB, and H0 = 67.80 ± 2.17 (stat) ± 1.64 (sys) km s−1 Mpc−1 for the JAGB method. The distances measured using the TRGB and the JAGB methods agree, on average, at a level better than 1%, and with the SHoES Cepheid distances at just over the 1% level. Our results are consistent with the current standard Lambda cold dark matter (ΛCDM) model, without the need for the inclusion of additional new physics. Future JWST data will be required to increase the precision and accuracy of the local distance scale.

Keywords: Observational cosmology
Merger-driven Turbulence and Coherent Transport in the Intracluster Medium. The distribution of metals and temperature in the intracluster medium (ICM) provides key insights into galaxy cluster evolution, revealing information about chemical enrichment and heating and cooling processes, respectively. To access this information, it is crucial to understand the transport processes in the ICM. Here, we systematically study the transport mechanisms in the ICM with tracer particle resimulations of the Omega500 cosmological hydrosimulation, using a sample of four galaxy clusters of comparable masses but different mass assembly histories. Through the analysis of particle pair dispersion statistics, we find a time-dependent scaling index linked to the cluster's dynamical state. It reaches or exceeds Richardson scaling briefly during major mergers but remains much lower in relaxed clusters. We identify a coherent transport mode during major mergers that causes directional flow in the ICM. Although coherent transport can move particles to outer regions, the particles transported to the cluster outskirts compose only a small fraction of the density there; thus, the anisotropy it creates in the overall density distribution is limited. Moreover, strong turbulence generated by mergers quickly disperses these particles, further limiting this effect. We also provide useful statistics on the radial evolution of the ICM and the fraction of particles that ever reached the inner regions as a function of radius. Our results show that major mergers primarily drive particle transport, linking ICM transport to merger-driven dynamics, and highlighting the interplay between coherent and turbulent transport.

Keywords: Galaxy clusters, Hydrodynamical simulations, Intracluster medium, Astronomical simulations
Spin-polarized Electrons from Magnetically Aligned Grains and Chiral Symmetry Breaking: Effects of Cosmic Rays in Protostellar Environments. Low-energy spin-polarized electrons (SPEs) are thought to cause symmetry breaking and could explain the origin of homochirality of prebiotic molecules such as amino acids and sugars. Here we study the effect of cosmic rays (CRs) on the emission of SPEs from aligned grains in dense protostellar environments and explore their effects on chiral asymmetry of prebiotic molecules. We first show that icy grains in protostellar environments can align with magnetic fields due to magnetically enhanced radiative torque mechanism. We then study the production of thermal electrons by CR ionization of H2 and the CR-induced UV radiation using the attenuated CR spectra in dense cores obtained from a continuous slowing down model. Next, we show that thermal electrons with initial random spins captured by aligned grains will become spin-polarized due to the Barnett effect, converting unpolarized electrons into SPEs. We calculate the rate of photoemission of such SPEs by CRs-induced UV radiation and secondary electron emission from aligned grains and find that the photoemission by CRs-induced UV radiation is dominant. Finally, we calculate the total production rate of SPEs inside aligned dust grains by CRs. We estimate the alignment degree of SPEs from superparmagnetic (SPM) grains and find that it is only significant for SPM grains having large iron clusters and fast rotation. We suggest that low-energy secondary SPEs from aligned superparamagnetic grains with large iron inclusions induced by CRs might cause the chiral asymmetry of chiral prebiotic molecules formed in the ice mantle of aligned grains (analogously to UV circularly polarized light). We propose that amino acids and sugars of chiral asymmetry detected in meteorite/asteroids/comets might be formed in icy grain mantles with superparamagnetic inclusions under the irradiation of SPEs released from aligned grains by CRs in protostellar environments.

Keywords: Complex organic molecules, Star forming regions, Interstellar magnetic fields, Interstellar dust processes, Pre-biotic astrochemistry, Cosmic rays
The Link between Galaxy Structure Properties and Star Formation in Local Galaxies. To investigate the role of morphology in galaxy evolution, we analyze the relationships between galaxy structure, star formation, and H I gas content. Using multiband images from the DESI Legacy Imaging Surveys, we perform detailed structural decompositions on a representative local galaxy sample from xGASS. Structural components and color properties are examined as functions of deviations from the star formation main sequence (ΔSFRMS) and H I gas deficiency (ΔfH I). We find that bulge fractions decrease with higher ΔSFRMS and lower stellar mass, indicating that star-forming galaxies are predominantly disk dominated while quiescent galaxies are bulge dominated. The slope of the color (g ‑ r) versus ΔSFRMS relationship decreases from low to high stellar masses and from outer to inner regions, with greater color variation in massive galaxies. Color gradients are predominantly negative, becoming shallower in lower-mass galaxies and in the outer disk regions. We also identify inflection points in the color gradient and bulge fraction relations with ΔSFRMS, with main-sequence galaxies having the lowest bulge fractions and steepest color gradients. At fixed stellar mass, we observe only a slight correlation between bulge fraction and H I deficiency. However, outer disk colors show a stronger dependence on H I content than inner regions, and color gradients flatten as ΔfH I increases. These results suggest that H I gas is more closely linked to star-forming, disk-dominated systems, supporting the idea that gas accretion fuels star formation primarily in galaxy disks.

Keywords: Galaxy structure, Galaxy bulges, Star formation, Galaxy evolution
Exploring the Spectral Energy Distributions of Luminous Broad Absorption Line Quasars at High Redshift. We present the multiwavelength spectral energy distributions (SEDs) for 65 luminous broad absorption line (BAL) quasars with redshifts 1.55 ≲ z ≲ 3.50 from the Gemini Near Infrared Spectrograph─Distant Quasar Survey (GNIRS-DQS). We integrate data from a variety of ground- and space-based observatories to construct a comprehensive spectral profile of these objects from radio through X-rays. In addition, we present a mid-infrared to X-ray composite SED of these sources. Our data set represents the most uniform sample of BAL quasars, providing a statistically robust set of SEDs. Our findings indicate that the BAL quasars in the GNIRS-DQS sample exhibit significant reddening in the ultraviolet-optical continuum relative to their non-BAL counterparts, consistent with previous studies. Notably, our analysis reveals no significant differences in the mid- or near-infrared spectral regime between BAL and non-BAL quasars. In line with previous work, we find no strong evidence that BAL and non-BAL quasars possess fundamentally different SEDs, also consistent with recent findings that both groups display similar rest-frame optical emission-line properties.

Keywords: Active galactic nuclei, Broad-absorption line quasar, Quasars
Exploring the Anisotropic Gravitational Wave Background from All-sky Mock Gravitational Wave Event Catalogs. Anisotropic stochastic gravitational wave background (SGWB) serves as a potential probe of the large-scale structure (LSS) of the universe. In this work, we explore the anisotropic SGWB from local (z &lt; ∼ 0.085) merging stellar mass compact binaries, specifically focusing on merging stellar binary black holes, merging neutron star–black hole binaries, and merging binary neutron stars. The analysis employs seven all-sky mock lightcone gravitational wave event catalogs, which are derived from the Millennium simulation combined with a semianalytic model of galaxy formation and a binary population synthesis model. We calculate the angular power spectra Cℓ at multipole moments ℓ, expressed as log10[ℓ(ℓ + 1)Cℓ/(2π)], based on the skymaps of the overdensity δGW in the anisotropic SGWB. The spectra for all three source types exhibit an approximately linear increase with log10ℓ at higher ℓ (e.g., ℓ &gt; ∼ 30–300) in seven catalogs, with a characteristic slope of ∼2. The spectra of seven catalogs exhibit considerable variations, arising from fluctuations in spatial distribution, primarily in the radial distribution, of nearby sources (e.g., &lt;50 Mpc h‑1). After subtracting these nearby sources, the variations become much smaller and the spectra for the three source types become closely aligned (within discrepancies of a factor of ∼2 across ℓ = 1–1000 for all catalogs). We also find that including farther sources results in a rapid decrease in the anisotropy.

Keywords: Gravitational wave astronomy, Cosmic anisotropy, Gravitational waves, Gravitational wave sources
Effects of Planetary Parameters on Disequilibrium Chemistry in Irradiated Planetary Atmospheres: From Gas Giants to Sub-Neptunes. A primary goal of characterizing exoplanet atmospheres is to constrain planetary bulk properties, such as their metallicity, C/O ratio, and intrinsic heat. However, there are significant uncertainties in many aspects of atmospheric physics, such as the strength of vertical mixing. Here, we use PICASO and the photochem model to explore how atmospheric chemistry is influenced by planetary properties such as metallicity, C/O ratio, Tint, Teq, and Kzz in hydrogen-dominated atmospheres. We vary the Teq of the planets between 400 and 1600 K, across "cold," "warm," and "hot" objects. We also explore an extensive range of Tint values between 30 and 500 K, representing sub-Neptunes to massive gas giants. We find that gases such as CO and CO2 show a drastically different dependence on Kzz and C/O for planets with cold interiors (e.g., sub-Neptunes) compared to planets with hotter interiors (e.g., Jupiter mass planets) for the same Teq. We also find that gases such as CS and CS2 can carry a significant portion of the S-inventory in the upper atmosphere near Teq ≤ 600 K, below which SO2 ceases to be abundant. For solar C/O, we show that the CO/CH4 ratio in the upper atmospheres of planets can become ≤1 for planets with low Teq, but only if their interiors are cold (Tint ≤ 100 K). We find that photochemical haze precursor molecules in the upper atmosphere show very complex dependence on C/O, Kzz, Teq, and Tint for planets with cold interiors (e.g., sub-Neptunes). We also briefly explore fully coupling PICASO and photochem to generate self-consistent radiative–convective–photochemical-equilibrium models.

Keywords: Exoplanet atmospheric composition , Exoplanet atmospheric dynamics, Exoplanet evolution, Exoplanet atmospheres, Exoplanet atmospheric structure
Low-acceleration Gravitational Anomaly from Bayesian 3D Modeling of Wide Binary Orbits: Methodology and Results with Gaia Data Release 3. Isolated wide binary stars provide natural laboratories to directly probe gravity for Newtonian acceleration of gN ≲ 10‑9 m s‑2. Recent statistical analyses of wide binaries have been performed only with sky-projected relative velocities vp in the pairs. A new method of Bayesian orbit modeling exploiting three relative velocity components including the radial (line-of-sight) component vr is developed to measure the gravitational anomaly parameter  Γ≡log10γg≡log10Geff/GN  where Geff is the effective gravitational constant for pseudo-Newtonian elliptical orbits, while GN is Newton's constant. The method infers individual probability distributions of Γ and then combines the independent distributions to obtain a consolidated distribution in a specific range of gN. Here the method is described and applied to a sample of 312 wide binaries in a broad dynamic range of 10‑11.0 ≲ gN ≲ 10‑6.7 m s‑2 with vr uncertainties in the range  168&lt;σvr&lt;380  m s‑1 selected from the Gaia Data Release 3 database. The following results are obtained: Γ = 0.000 ± 0.011 or γg = 1.00 ± 0.05 (Nbinary = 125) for the high-acceleration regime (10‑7.9 ≲ gN ≲ 10‑6.7 m s‑2) agreeing well with Newton, but Γ = 0.085 ± 0.040 or  γg=1.48‑0.23+0.33  (35) for the modified Newtonian dynamics (MOND) regime (10‑11.0 ≲ gN ≲ 10‑9.5 m s‑2) and Γ = 0.063 ± 0.015 or  γg=1.34‑0.08+0.10  (111) for the MOND + transition regime (10‑11.0 ≲ gN ≲ 10‑8.5 m s‑2). These results show that a gravitational anomaly is evident for gN ≲ 10‑9 m s‑2 and Γ in the MOND regime (≲10‑9.5 m s‑2) agrees with the first-tier prediction (Γ ≈ 0.07 or γg ≈ 1.4) of MOND gravity theories.

Keywords: Binary stars, Gravitation, Non-standard theories of gravity, Wide binary stars, Modified Newtonian dynamics
Discovery of Evolution of the Temporal Features of X-Ray Bursts from SGR J1935+2154. SGR J1935+2154 has undergone eight active episodes since its discovery in 2014. In this study, our focus is on the evolution of the temporal characteristics including burst duration, minimum variation timescale (MVT), and waiting time across these active episodes observed by Fermi/Gamma-ray Burst Monitor (GBM). We find a linear increase in the logarithmic mean of burst duration over time, with a deviation during the fourth and eighth active episodes containing X-ray burst (XRB)‑Fast Radio Burst (FRB) 200428 and XRB‑radio burst 221021 association events. We also find a possible increasing burst frequency, with the fourth active episode exhibiting an exceptionally high burst rate. Therefore, XRB‑FRB 200428 is potentially triggered by energetic events such as a large crust, magnetic reconnection, or glitches. The MVT analysis reveals deviations in the sixth and seventh active episodes with ∼3σ. These results may suggest evolving magnetospheric field geometry, neutron star crust, and energy release mechanisms of SGR J1935+2154. Finally, our findings predict that longer XRB durations indicate the highly likely occurrence of XRB and radio burst association events, warranting focused multiwavelength observations during such episodes, which will also be further confirmed or disproved by future observations.

Keywords: Magnetars
A Multiwavelength Technique for Estimating Galaxy Cluster Mass Accretion Rates. The mass accretion rate of galaxy clusters is a key factor in determining their structure, but a reliable observational tracer has yet to be established. We present a state-of-the-art machine learning model for constraining the mass accretion rate of galaxy clusters from only X-ray and thermal Sunyaev─Zeldovich observations. Using idealized mock observations of galaxy clusters from the MillenniumTNG simulation, we train a machine learning model to estimate the mass accretion rate. The model constrains 68% of the mass accretion rates of the clusters in our data set to within 33% of the true value without significant bias, a ∼58% reduction in the scatter over existing constraints. We demonstrate that the model uses information from both radial surface brightness density profiles and asymmetries.

Keywords: Galaxy clusters, Convolutional neural networks, Neural networks
The Discovery of Two Quadruple Star Systems with the Second and Third Shortest Outer Periods. We present the discovery of two quadruple star systems—TIC 285853156 and TIC 392229331—each consisting of two bound eclipsing binary stars. Among the most compact quadruples known, TIC 392229331 and TIC 285853156 have the second and third shortest outer orbital periods (145 days and 152 days, respectively) after BU Canis Minoris (122 days). We demonstrate that both systems are long-term dynamically stable despite substantial outer orbital eccentricities (0.33 for TIC 285853156 and 0.56 for TIC 392229331). We previously reported these systems in V. B. Kostov et al. and V. B Kostov et al. as 2 + 2 hierarchical quadruple candidates producing two sets of primary and secondary eclipses in TESS data, as well as prominent eclipse timing variations on both binary components. We combine all available TESS data and new spectroscopic observations into a comprehensive photodynamical model, proving that the component binary stars are gravitationally bound in both systems and finding accurate stellar and orbital parameters for both systems, including very precise determinations of the outer periods. TIC 285853156 and TIC 392229331 represent the latest addition to the small population of well-characterized proven quadruple systems dynamically interacting on detectable timescales.

Keywords: Eclipsing binary stars, Multiple stars
CHILES. IX. Observational and Simulated H I Content and Star Formation of Blue Galaxies in Different Cosmic Web Environments. We examine the redshift evolution of the relationship between the neutral atomic hydrogen (H I) content and star formation properties of blue galaxies, along with their location in the cosmic web. Using the COSMOS H I Large Extragalactic Survey (CHILES) and the IllustrisTNG (TNG100) cosmological simulation, and the DISPERSE algorithm, we identify the filamentary structure in both observations and simulations, measure the distance of galaxies to the nearest filament spine Dfil, and calculate the mean H I gas fraction and the relative specific star formation rate (sSFR) of blue galaxies in three different cosmic web environments—0 &lt; Dfil/Mpc &lt; 2 (filament cores), 2 &lt; Dfil/Mpc &lt; 4 (filament outskirts), and 4 &lt; Dfil/Mpc &lt; 20 (voids). We find that, although there are some similarities between CHILES and TNG, there exist significant discrepancies in the dependence of H I and star formation on the cosmic web and on redshift. TNG overpredicts the observed H I fraction and relative sSFR at z = 0–0.5, with the tension being strongest in the voids. CHILES observes a decline in the H I fraction from filament cores to voids, exactly the opposite of the trend predicted by TNG. CHILES observes an increase in H I fraction at z = 0.5 → 0 in the voids, while TNG predicts an increase in this time in all environments. Further dividing the sample into stellar mass bins, we find that the H I in  log(M*/M⊙)&gt;10  galaxies is better reproduced by TNG than H I in  log(M*/M⊙)=9‑10  galaxies.

Keywords: Extragalactic astronomy, Radio astronomy, Astronomical simulations, Galaxy environments