Sazuna/UAT_keywords huggingface dataset:
Element Nucleosynthetic Origins from Abundance Spatial Distributions beyond the Milky Way. An element's astrophysical origin should be reflected in the spatial distribution of its abundance, yielding measurably different spatial distributions for elements with different nucleosynthetic sites. However, most extragalactic multielement analyses of gas-phase abundances to date have been limited to small numbers of sight lines, making statistical characterization of differences in spatial distributions of elements impossible. Here we use integrated field spectroscopic data covering the full face of the nearby dwarf galaxy NGC 5253 sampled at 3.5 pc resolution to produce maps of the abundances of oxygen, nitrogen, and sulfur using independent direct methods. We find strong evidence for differences in the elements' spatial statistics that mirror their predicted nucleosynthetic origins: the spatial distributions of oxygen and sulfur, both predominantly produced in core-collapse supernovae, indicate that initial injection occurs on larger scales than for nitrogen, which is predominantly produced by asymptotic giant branch stars. All elements are well correlated, but oxygen and sulfur are much better correlated with each other than with nitrogen, consistent with recent results for stellar abundances in the Milky Way. These findings both open a new avenue to test nucleosynthetic models and make predictions for the structure of stellar chemical abundance distributions.

Keywords: Chemical enrichment, Chemical abundances, Interstellar medium
The Cosmic Microwave Background Optical Depth Constrains the Duration of Reionization. Recently, it was pointed out that invoking a large value of the cosmic microwave background (CMB) optical depth, τCMB = 0.09, could help resolve tensions between Dark Energy Survey Instrument DR2 baryon acoustic oscillation data and the CMB. This is larger than the value of τCMB = 0.058 measured from the Planck low-ℓ polarization data. Traditionally, τCMB is thought of as a constraint on reionization's midpoint. However, recent observations and modeling of the Lyα forest of high-z quasars at 5 &lt; z &lt; 6 have tightly constrained the timing of the last 10%─20% of reionization, adding nuance to this interpretation. Here, we point out that fixing reionization's endpoint, in accordance with the latest Lyα forest constraints, renders τCMB a sensitive probe of the duration of reionization, as well as its midpoint. We compare low and high values of τCMB to upper limits on the patchy kinematic Sunyaev─Zel'dovich (pkSZ) effect, another CMB observable that constrains reionization's duration, and find that a value of τCMB = 0.09 is in ≍2σ tension with existing limits on the pkSZ from the South Pole Telescope (SPT). The strength of this tension is sensitive to the choices involved in modeling the other CMB foregrounds in the SPT measurement, and in the modeling of the pkSZ signal itself.

Keywords: Observational cosmology, Reionization, Cosmic microwave background radiation
Observed Antiparallel Correlation between Spiral Galaxy and Cosmic Filament Spins. Understanding the origin of galactic angular momentum and its connection to the cosmic web remains a pivotal issue in galaxy formation. Using kinematic data from the MaNGA survey, we investigate the alignment between the spin directions of spiral galaxies and their host cosmic filaments. By incorporating filament spin measurements derived from redshift asymmetry across filament spines, we reveal a mass-dependent antiparallel correlation: low-mass spiral galaxies ( log10(M*/M⊙)≲10 ) exhibit a statistically significant antiparallel alignment between their stellar/gas spins and filament spins, while high-mass spirals show no such trend. Spatial analysis further indicates that high-mass spirals preferentially reside near filament spines, whereas low-mass spirals occupy filament outskirts. These findings extend previous alignment studies that neglected directional spin correlations and provide new insights into how cosmic environments shape galactic angular momentum. The observed antiparallel trend suggests a critical role for filament spin in regulating the angular momentum acquisition of low-mass spirals. This antiparallel alignment is significantly enhanced for low-mass spirals residing in dynamically cold filaments, highlighting the importance of filament properties in shaping galaxy spin.

Keywords: Galaxy formation, Galaxy environments, Large-scale structure of the universe, Galaxy kinematics, Cosmic web
Optical+Near-IR Analysis of a Newly Confirmed Einstein Ring at z ∼ 1 from the Kilo-Degree Survey: Dark Matter Fraction, Total and Dark Matter Density Slope, and Initial Mass Function. We report the spectroscopic confirmation of a bright blue Einstein ring in the Kilo-Degree Survey (KiDS) footprint: the Einstein "blue eye." Spectroscopic data from X-Shooter at the Very Large Telescope (VLT) show that the lens is a typical early-type galaxy (ETG) at zl = 0.9906, while the background source is a Lyα emitter at zs = 2.823. The reference lens modeling was performed on a high-resolution Y-band adaptive-optics image from HAWK-I at VLT. Assuming a singular isothermal ellipsoid total mass density profile, we inferred an Einstein radius REin = 10.47 ± 0.06 kpc. The average slope of the total mass density inside the Einstein radius, as determined by a joint analysis of lensing and isotropic Jeans equations, is  γtot=2.14−0.07+0.06 , showing no systematic deviation from the slopes of lower-redshift galaxies. This can be the evidence of ETGs developing through dry mergers plus moderate dissipationless accretion. Stellar population analysis with eight-band (griZYJHKs) photometries from KiDS and VIKING shows that the total stellar mass of the lens is M* = (3.95 ± 0.35) × 1011 M⊙ (Salpeter initial mass function (IMF)), implying a dark matter fraction inside the effective radius of fDM = 0.307 ± 0.151. We finally explored the dark matter halo slope and found a strong degeneracy with the dynamic stellar mass. Dark matter adiabatic contraction is needed to explain the posterior distribution of the slope, unless an IMF heavier than Salpeter is assumed. *Based on observations with OmegaCam@VST, VIRCAM@VISTA, HAWK-I, and XSHOOTER@VLT (Prog. ID: 107.22S8).

Keywords: Galaxy formation, Galaxy dynamics, Gravitational lensing, Galaxy evolution, Dark matter
A New High-latitude H I Cloud Complex Entrained in the Northern Fermi Bubble. We report the discovery of 11 high-velocity H I clouds at Galactic latitudes of 25°–30°, likely embedded in the Milky Way's nuclear wind. The clouds are detected with deep Green Bank Telescope 21 cm observations of a 3 .° 2 × 6 .° 2 field around QSO 1H1613-097, located behind the northern Fermi Bubble. Our measurements reach 3σ limits on NHI as low as 3.1 × 1017 cm‑2, more than twice as sensitive as previous H I studies of the bubbles. The clouds span ‑180 ≤ vLSR ≤ ‑90 km s‑1 and are the highest-latitude 21 cm high-velocity cloud detected inside the bubbles. Eight clouds are spatially resolved, showing coherent structures with sizes of 4–28 pc, peak column densities of log(NHI/cm2) = 17.9–18.7, and H I masses up to 1470 M⊙. Several exhibit internal velocity gradients. Their presence at such high latitudes is surprising, given the short expected survival times for clouds expelled from the Galactic center. These objects may be fragments of a larger cloud disrupted by interaction with the surrounding hot gas.

Keywords: Galactic center, High-velocity clouds, Neutral hydrogen clouds, Circumgalactic medium, Milky Way evolution, Milky Way Galaxy
An Extremely Metal-poor Lyα Emitter Candidate at z = 6 Revealed through Absorption Spectroscopy. We report the discovery of a Lyα emitter (LAE) candidate in the immediate foreground of the quasar PSO J158-14 at zQSO = 6.0685 at a projected distance ∼29 pkpc that is associated with an extremely metal-poor absorption system. This system was found in archival observations of the quasar field with the Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) and was previously missed in searches of absorption systems using quasar absorption line spectroscopy, as it imparts no detectable metal absorption lines on the background quasar spectrum. The detected Lyα emission line at a redshift of zLAE = 6.0323 is well aligned with the outer edge of the quasar's proximity zone and can plausibly cause its observed damping wing if it is associated with a proximate subdamped Lyα absorption system with a column density of  logNHI/cm−2≍19.7 . A &gt;10 hr medium-resolution spectrum of the quasar observed with the Magellan/Folded-port InfraRed Echellette (FIRE) and VLT/X-Shooter spectrographs reveals a metallicity constraint of [Z/H] &lt; −3. Such low metallicity makes this system an extremely metal-poor galaxy candidate and provides an exciting site to study possible signatures of Population III stars.

Keywords: Population III stars, Quasar absorption line spectroscopy, Quasars, Damped Lyman-alpha systems, Lyman-alpha galaxies, Metallicity
Highly Polarized Type III Storm Observed with Parker Solar Probe. The Parker Solar Probe (PSP) spacecraft observed a large coronal mass ejection (CME) on 2022 September 5, shortly before closest approach during the 13th PSP solar encounter. For several days following the CME, PSP detected a storm of Type III radio bursts. Stokes parameter analysis of the radio emission indicates that the Type III storm was highly circularly polarized (with fractional polarization up to ∼0.4). Left-hand circularly polarized (LHC) emission dominated at the start of the storm, transitioning to right-hand circularly polarized (RHC) emission at the crossing of the heliospheric current sheet on September 6. We analyze the properties of this Type III storm. The drift rate of the Type IIIs indicates a constant beam speed of ∼0.1c, typical for Type III-producing electron beams. The sense of polarization is consistent with fundamental emission generated primarily in the O-mode. The stable and well organized post-CME magnetic field neatly separates the LHC- and RHC-dominated intervals of the storm, with minimal overlap between the senses of polarization. The proximity of PSP to the source region, both in radial distance and in heliographic longitude, makes this event an ideal case study to connect in situ plasma measurements with remote observations of radio emission.

Keywords: Space vehicle instruments, Radio bursts, Solar radio emission
Recurrent Cometary Activity Discovered on Quasi-Hilda Jupiter Family Comet 362P/(457175) 2008 GO<SUB>98</SUB>. We report the discovery of recurrent activity on quasi-Hilda comet (QHC) 362P/(457175) 2008 GO98. The first activity epoch was discovered during the perihelion passage of 362P in 2016, so we were motivated to observe it for recurrent cometary activity near its next perihelion passage (UT 2024 July 20). We obtained observations with the Lowell Discovery Telescope, the Astrophysical Research Consortium telescope, and the Vatican Advanced Technology Telescope and identified a second activity epoch when 362P had a true anomaly (ν) as early as 318 .° 1. We conducted archival searches of six repositories and identified images obtained with Canada–France–Hawaii Telescope MegaCam, Dark Energy Camera, Pan-STARRS 1, SkyMapper, Zwicky Transient Facility, and Las Cumbres Observatory Global Telescope network data. Using these data, we identified activity from a previously unreported time span, and we did not detect activity when 362P was away from perihelion, specifically 83∘ &lt; ν &lt; 318∘. Detection of activity near perihelion and absence of activity away from perihelion suggest thermally driven activity and volatile sublimation. Our dynamical simulations suggest 362P is a QHC, and it will remain in a combined Jupiter-family comet (JFC) and quasi-Hilda orbit over the next 1 kyr though it will become increasingly chaotic nearing the end of this timeframe. Our reverse simulations suggest 362P may have migrated from the orbit of a long-period comet (∼53%) or Centaur (∼32%); otherwise it remained a JFC (∼15%) over the previous 100 kyr. We recommend additional telescope observations from the community as 362P continues outbound from its perihelion on UT 2024 July 20, as well as continued observations for a third activity epoch.

Keywords: Comet tails, Comet dynamics, Hilda group
New Clues on the Extended He II Ionization in IZw18 from GTC/MEGARA and JWST/MIRI. IZw18 is one of the lowest-metallicity star-forming galaxies known at z ∼ 0, considered a unique local analogue of the first galaxies. The origin of its hard ionizing continuum, expected to be a common feature in the early Universe and traced by He II emission lines, remains intensely debated and challenging to explain. Here we combine optical Gran Telescopio Canarias MEGARA and mid-infrared (JWST/MIRI) integral field spectroscopic observations for IZw18 to shed new light on the high-ionization phenomenon. This Letter reports the first detection of the high-ionization [Ne V]14.32 μm line in IZw18. Its emission is spatially extended and coincident with the He II peak, revealing the presence of highly energetic ionizing sources that surpass mechanisms previously proposed on the basis of He II alone. Our kinematic studies highlight that the He IIλ4686-emitting gas displays higher velocity dispersions and a different velocity pattern compared with the Hβ emission, suggesting the presence of energetic processes such as shocks or stellar-driven feedback. Additionally, integrated spectra show asymmetric blueshifted profiles in the He IIλ4686 line, possibly indicating early-stage stellar-driven outflows potentially facilitating future ionizing photon leakage. Our spatial analysis also reveals differences in structure between the emission of Hβ and He IIλ4686, with the He IIλ4686 peak offset by a projected distance of 140 pc from the peak Hβ emission. This indicates distinct locations for the most extreme ionizing sources compared to moderate ionizing sources. Our findings underscore the complex interplay of physical processes in extremely metal-poor environments with highly ionized gas, offering new insights into the conditions prevailing in the early galaxies.

Keywords: Starburst galaxies, Blue compact dwarf galaxies, Photoionization, Stellar feedback, Galaxy physics, Emission line galaxies, H II regions, Galaxy kinematics, Interstellar medium, Ionization, Metallicity, Galaxies
Gas-poor Hosts and Gas-rich Companions of z ≍ 3.5 Radio Active Galactic Nuclei: ALMA Insights into Jet Triggering and Feedback. Cold gaseous systems play important roles in galaxy evolution by possibly providing fuel to ignite active galactic nuclei (AGN) activity and star formation. In this work, we analyze [C II]158 μm and continuum observations from the Atacama Large Millimeter/submillimeter Array for a sample of four radio AGN at z ≍ 3.5, focusing on eight associated companion cloud systems discovered within projected distances of tens of kiloparsecs or less. The spatial distribution of these companions indicates that the majority of cold gas is not located at the AGN position, i.e., not in their host galaxies. With the assistance of [C II] at 0 .″ 2 resolution, we further confirm the gas-poor nature of the hosts by reanalyzing archival [C I] (a tracer of H2) at ∼2″ resolution. Our sample has [C II] luminosities in a range of 2.8 × 108 &lt; L[C II]/L⊙ &lt; 4.2 × 109. The L[C II]/LIR ratio, ∼9.4 × 10−4, is consistent with sources discussed in the literature. Our findings show the gas-poor radio AGN hosts have nearby gas-rich companions. We propose that these companions may be stripped clouds resulting from merger processes, which could be a trigger of radio-loud AGN. They may also be a signature of negative AGN feedback (e.g., shock heating) on these infalling companions and on the host galaxy. In general, our analysis shows that powerful AGN at and before Cosmic Noon are impacting and being impacted by cold gaseous clouds in their circumgalactic or protointracluster media.

Keywords: AGN host galaxies, Active galaxies, Galactic and extragalactic astronomy, Radio loud quasars, Circumgalactic medium
Multi-instrument Search for Gamma-Ray Counterpart of X-Ray Transients Detected by EP/WXT. As a soft X-ray imager with an unprecedentedly large field of view, Einstein Probe (EP)/Wide-field X-ray Telescope (WXT) has detected many (fast) X-ray transients, whose nature is very intriguing. Whether there is a gamma-ray counterpart for the X-ray transient provides important implications for its origin. Some of them have been reported to be associated with gamma-ray bursts; however, a systematic study on the gamma-ray emission of these X-ray transients is lacking. In this work, we implemented a comprehensive targeted search for gamma-ray counterparts to 63 X-ray transients reported by EP/WXT during its first year of operation, using the dedicated multiple-instrument search pipeline, Energetic Transients Joint Analysis System for Multi-Instrument (ETJASMIN), with GECAM-B, GECAM-C, Fermi/GBM, and Insight-HXMT data. We find that 14 out of 63 (22%) EP/WXT X-ray transients have gamma-ray counterparts. For other transients, the ETJASMIN pipeline provided the upper limit of the gamma-ray emission, which is more stringent than that given by an individual instrument. Moreover, we investigated the properties of the X-ray transients and their gamma-ray counterparts and explored the relation between the X-ray transient and the gamma-ray counterpart.

Keywords: Gamma-ray observatories, X-ray transient sources, Gamma-ray bursts
The Hα Line as a Probe of Chromospheric Magnetic Fields. We explore the diagnostic potential of the Hα line for probing the chromospheric magnetic field using a realistic 3D radiative magnetohydrodynamic (rMHD) model. The Stokes profiles of the Hα line are synthesized through full 3D radiative transfer under the field-free approximation, alongside the Ca II 8542 Å and Fe I 6173 Å lines for comparison. The line-of-sight (LOS) magnetic fields are inferred using the weak-field approximation for the Hα and Ca II 8542 Å lines, while the Fe I 6173 Å line is analyzed through Milne-Eddington inversion techniques. The comparison between the inferred LOS magnetic field maps and the magnetic fields in the rMHD model revealed that the Hα line core primarily probes the chromospheric magnetic field at  logτ500  = ‑5.7, which corresponds to higher layers than the Ca II 8542 Å line core, which is most sensitive to conditions at  logτ500  = ‑5.1. On average, the Stokes V profiles of the Hα line core form 500 km higher than those of the Ca II 8542 Å line core. The Hα polarization signals persist after adding noise, and with noise at the level of 10‑3Ic, most simulated magnetic structures remain visible. These findings suggest that spectropolarimetric observations of the Hα line can provide complementary insights into the stratification of the magnetic field at higher altitudes, especially when recorded simultaneously with widely used chromospheric diagnostics such as the Ca II 8542 Å line.

Keywords: Solar chromosphere, Spectropolarimetry, Solar magnetic fields
Discovery of Diffuse Radio Emission in a Massive z = 1.709 Cool Core Cluster: A Candidate Radio Minihalo. Clusters of galaxies host spectacular diffuse radio sources, extending over scales from 100 kpc to several Mpcs. These sources, with extremely faint surface brightness (μJy/arcsec2 level), are not tied to individual galaxies but trace synchrotron emission from large-scale magnetic fields and relativistic particles within the intracluster environment. Here, we report the discovery of a candidate radio minihalo in SpARCS104922.6+564032.5, the most distant cool-core galaxy cluster identified to date at z = 1.709, using deep LOFAR 120–168 MHz observations. We show that this emission originates from diffuse cluster-associated processes rather than unresolved active galactic nuclei or star-forming galaxies. The diffuse radio emission coincides spatially with the X-ray emission of the hot intracluster medium and has a radio power of  P150MHz=49.8‑11.7+14.7×1024  W Hz‑1, exhibiting striking similarities to low-redshift radio minihalos. This discovery doubles the redshift of previously known minihalos, challenging models of inverse Compton losses and indicating the presence of strong magnetic fields, enhanced turbulence in high-redshift clusters, or active hadronic processes that require a cosmic-ray-to-thermal-energy ratio of 0.07 within 200 kpc, assuming a clumped distribution with spatial correlations among the gas, cosmic rays, and magnetic field that partially compensate for cosmological redshift dimming. It further implies that magnetic fields are efficiently amplified to ∼10 μG levels within an Mpc3 volume during the epoch of cluster formation before z ∼ 2. These findings provide critical insights into high-redshift cluster physics and emphasize the transformative potential of next-generation radio surveys, such as those with the Square Kilometre Array and next-generation Very Large Array (ngVLA), in exploring the early evolution of galaxy clusters.

Keywords: Galaxy clusters, Cooling flows, High-redshift galaxy clusters, Extragalactic radio sources, Interferometers, Non-thermal radiation sources, Active galactic nuclei
Follow-up Exploration of the TWA 7 Planet─Disk System with JWST NIRCam. The young M star TWA 7 hosts a bright and near face-on debris disk, which has been imaged from the optical to the submillimeter. The disk displays multiple complex substructures such as three disk components, a large dust clump, and spiral arms, suggesting the presence of planets to actively sculpt these features. The evidence for planets in this disk was further strengthened with the recent detection of a point source compatible with a Saturn-mass planet companion using JWST/MIRI at 11 μm, at the location a planet was predicted to reside based on the disk morphology. In this Letter, we present new observations of the TWA 7 system with JWST/NIRCam in the F200W and F444W filters. The disk is detected at both wavelengths and presents many of the same substructures as previously imaged, although we do not robustly detect the southern spiral arm. Furthermore, we detect two faint potential companions in the F444W filter at the 2σ─3σ level. While one of these companions needs further follow-up to determine its nature, the other one coincides with the location of the planet candidate imaged with MIRI, providing further evidence that this source is a sub-Jupiter-mass planet companion rather than a background galaxy. Such discoveries make TWA 7 only the second system, after β Pictoris, in which a planet predicted by the debris disk morphology has been detected.

Keywords: High contrast techniques, Debris disks, Exoplanet systems, Near infrared astronomy