Sazuna/UAT_keywords huggingface dataset:
A Massive Quiescent Galaxy Confirmed in a Protocluster at z = 3.09. We report a massive quiescent galaxy at ${z}_{\mathrm{spec}}={3.0922}_{-0.004}^{+0.008}$ spectroscopically confirmed at a protocluster in the SSA22 field by detecting the Balmer and Ca II absorption features with the multi-object spectrometer for infrared exploration on the Keck I telescope. This is the most distant quiescent galaxy confirmed in a protocluster to date. We fit the optical to mid-infrared photometry and spectrum simultaneously with spectral energy distribution (SED) models of parametric and nonparametric star formation histories (SFHs). Both models fit the observed SED well and confirm that this object is a massive quiescent galaxy with a stellar mass of $\mathrm{log}({\text{}}{M}_{\star }/{\text{}}{M}_{\odot })={11.26}_{-0.04}^{+0.03}$ and ${11.54}_{-0.00}^{+0.03}$ , and a star formation rate of SFR/M⊙ yr-1 &lt; 0.3 and $={0.01}_{-0.01}^{+0.03}$ for parametric and nonparametric models, respectively. The SFH from the former modeling is described as an instantaneous starburst whereas that of the latter modeling is longer-lived, but both models agree with a sudden quenching of the star formation at ~0.6 Gyr ago. This massive quiescent galaxy is confirmed in an extremely dense group of galaxies predicted as a progenitor of a brightest cluster galaxy formed via multiple mergers in cosmological numerical simulations. We discover three new plausible [O III]λ5007 emitters at 3.0791 ≤ zspec ≤ 3.0833 serendipitously detected around the target. Two of them just between the target and its nearest massive galaxy are possible evidence of their interactions. They suggest the future great size and stellar mass evolution of this massive quiescent galaxy via mergers.

Keywords: Giant elliptical galaxies, Galaxy evolution, Protoclusters, Galaxy environments
Validation of the PDFI_SS Method for Electric Field Inversions Using a Magnetic Flux Emergence Simulation. Knowledge of electric fields in the photosphere is required to calculate the electromagnetic energy flux through the photosphere and set up boundary conditions for data-driven magnetohydrodynamic (MHD) simulations of solar eruptions. Recently, the PDFI_SS method for inversions of electric fields from a sequence of vector magnetograms and Doppler velocity measurements was improved to incorporate spherical geometry and a staggered-grid description of variables. The method was previously validated using synthetic data from anelastic MHD (ANMHD) simulations. In this paper, we further validate the PDFI_SS method, using approximately 1 hr long MHD simulation data of magnetic flux emergence from the upper convection zone into the solar atmosphere. We reconstruct photospheric electric fields and calculate the Poynting flux, and we compare those to the actual values from the simulations. We find that the accuracy of the PDFI_SS reconstruction is quite good during the emergence phase of the simulated ephemeral active region evolution and decreases during the shearing phase. Analyzing our results, we conclude that the more complex nature of the evolution (compared to the previously studied ANMHD case) that includes the shearing evolution phase is responsible for the obtained accuracy decrease.

Keywords: Solar active region velocity fields, Solar active region magnetic fields, Solar atmosphere, Solar magnetic flux emergence, Solar photosphere, Solar active regions
Life in Elliptical Galaxies: Hot Spheroids, Fast Stars, Deadly Comets?. Elliptical galaxies have dynamically hot (σ1D ~100-300 km s-1) populations of stars, and presumably, smaller objects like comets. Because interstellar minor bodies are moving much faster, they hit planets harder and more often than in the local Galaxy. I estimate the rates for Chicxulub-scale impacts on an Earth-size planet in elliptical galaxies as a potential habitability constraint on intelligent life. Around most stars in a normal elliptical galaxy, these planets receive only ~0.01-0.1 Gyr-1, although hazardous rates may be common in certain compact early-type galaxies and red nuggets. About ~5% of the stellar mass is in a region where the rate is &gt; 10 Gyr-1, large enough to dominate the mass extinction rate. This suggests that elliptical galaxies have an exclusion zone of order one hundred parsecs in radius around their centers for the evolution of intelligent life.

Keywords: Search for extraterrestrial intelligence, Astrobiology, Elliptical galaxies, Habitable planets
Fine Structures of an EUV Wave Event from Multi-viewpoint Observations. In this study, we investigate an extreme ultraviolet (EUV) wave event on 2010 February 11, which occurred as a limb event from the Earth viewpoint and a disk event from the Solar Terrestrial Relations Observatory-Behind viewpoint. We use the data obtained by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory in various EUV channels. The EUV wave event was launched by a partial prominence eruption. Compared with some EUV wave events in previous works, this EUV wave event contains a faster wave with a speed of ~445 ± 6 km s-1, which we call a coronal Moreton wave, and a slower wave with a speed of ~298 ± 5 km s-1, which we call the Extreme Ultraviolet Imaging Telescope (EIT) wave. The coronal Moreton wave is identified as a fast-mode wave and the EIT wave is identified as an apparent propagation due to successive field-line stretching. We also observe a stationary front associated with the fast-mode EUV wave. This stationary front is explained as mode conversion from the coronal Moreton wave to a slow-mode wave near a streamer.

Keywords: Solar coronal mass ejections, Solar coronal waves, Solar prominences
Radioactive Planet Formation. Young stellar objects are observed to have large X-ray fluxes and are thought to produce commensurate luminosities in energetic particles (cosmic rays). This particle radiation, in turn, can synthesize short-lived radioactive nuclei through spallation. With a focus on 26Al, this paper estimates the expected abundances of radioactive nuclei produced by spallation during the epoch of planet formation. In this model, cosmic rays are accelerated near the inner truncation radii of circumstellar disks, rX ≈ 0.1 au, where intense magnetic activity takes place. For planets forming in this region, radioactive abundances can be enhanced over the values inferred for the early solar system (from meteoritic measurements) by factors of ~10-20. These short-lived radioactive nuclei influence the process of planet formation and the properties of planets in several ways. The minimum size required for planetesimals to become fully molten decreases with increasing levels of radioactive enrichment, and such melting leads to loss of volatile components, including water. Planets produced with an enhanced radioactive inventory have significant internal luminosity, which can be comparable to that provided by the host star; this additional heating affects both atmospheric mass loss and chemical composition. Finally, the habitable zone of red dwarf stars is coincident with the magnetic reconnection region, so that planets forming at those locations will experience maximum exposure to particle radiation and subsequent depletion of volatiles.

Keywords: Nucleosynthesis, Cosmic ray nucleosynthesis, Exoplanet astronomy, Exoplanet evolution, Exoplanet structure, Exoplanet formation
Bayesian Nonparametric Inference of the Neutron Star Equation of State via a Neural Network. We develop a new nonparametric method to reconstruct the equation of state (EoS) of a neutron star with multimessenger data. As a universal function approximator, the feed-forward neural network (FFNN) with one hidden layer and a sigmoidal activation function can approximately fit any continuous function. Thus, we are able to implement the nonparametric FFNN representation of the EoSs. This new representation is validated by its capability of fitting the theoretical EoSs and recovering the injected parameters. Then, we adopt this nonparametric method to analyze the real data, including the mass-tidal deformability measurement from the binary neutron star merger gravitational-wave event GW170817 and mass-radius measurement of PSR J0030+0451 by NICER. We take the publicly available samples to construct the likelihood and use the nested sampling to obtain the posteriors of the parameters of the FFNN according to the Bayesian theorem, which in turn can be translated to the posteriors of the EoS parameters. Combining all of these data for a canonical 1.4 M⊙ neutron star, we get a radius ${R}_{1.4}={11.83}_{-1.08}^{+1.25}$ km and tidal deformability ${{\rm{\Lambda }}}_{1.4}={323}_{-165}^{+334}$ (90% confidence interval). Furthermore, we find that in the high-density region (≥3ρsat), the 90% lower limits of ${c}_{{\rm{s}}}^{2}/{c}^{2}$ (where cs is the sound speed and c is the velocity of light in vacuum) are above 1/3, which means that the so-called conformal limit (i.e., ${c}_{{\rm{s}}}^{2}/{c}^{2}\lt 1/3$ ) is not always valid in the neutron stars.

Keywords: Neutron stars, Nonparametric inference, Gravitational waves
Self-calibrating Interloper Bias in Spectroscopic Galaxy-clustering Surveys. Contamination of interloper galaxies due to misidentified emission lines can be a big issue in spectroscopic galaxy-clustering surveys, especially in future high-precision observations. We propose a statistical method based on the cross correlations of the observational data between two redshift bins to efficiently reduce this effect, and it can also derive the interloper fraction fi in a redshift bin with a high level of accuracy. The ratio of cross and autoangular correlation functions or power spectra between redshift bins are suggested to estimate fi, and the key equations are derived for theoretical discussion. In order to explore and prove the feasibility and effectiveness of this method, we also run simulations, generate mock data, and perform cosmological constraints considering systematics based on the observation of China Space Station Telescope. We find that this method can effectively reduce the interloper effect, and accurately constrain the cosmological parameters for fi &lt; 1% ~ 10%, which is suitable for most future surveys. This method can also be applied to other kinds of galaxy-clustering surveys like line intensity mapping.

Keywords: Cosmology, Cosmological parameters, Large-scale structure of the universe
The Bluest Changing-Look QSO SDSS J224113-012108. In this manuscript, we report a new changing-look QSO (CLQSO) SDSS J2241 at z = 0.059. Based on the multi-epoch Sloan Digital Sky Survey spectra from 2011 to 2017, the flux ratio of broad Hα to broad Hβ has changed from 7 in 2011 to 2.7 in 2017, leading SDSS J2241 with a spectral index αλ ~ -5.21 ± 0.02 (λ &lt; 4000) in 2017 to be, so far, the bluest CLQSO. Based on the SDSS spectrum in 2011, the host galaxy contribution with a stellar velocity dispersion of ~86 km s-1 can be well determined, leading to the M-sigma relation expected central black hole (BH) mass of ~3 × 106 M⊙. However, based on properties of the broad Hα emission, the virial BH mass is ~108 M⊙, about two magnitudes larger than the mass found through the M-sigma relation. The different BH masses found using different methods indicate that SDSS J2241 is one unique CLQSO. The long-term photometric light curve shows interesting variability that is not expected assuming the Damped Random Walk process commonly applied to active galactic nuclei but probably connected to a central tidal disruption event. Furthermore, based on continuum emission properties in 2017 with no dust obscuration, the moving dust clouds scenario alone cannot be preferred to explain the CLQSO SDSS J2241, because the expected intrinsic reddening-corrected continuum emission was unreasonably higher than the unobscured continuum emission in 2017.

Keywords: Active galaxies, Active galactic nuclei, Emission line galaxies, Quasars
The Evolutionary Effects of the Radius and Moment of Inertia of Rapidly Rotating Neutron Stars. A newly born millisecond magnetar is thought to be the central engine of some gamma-ray bursts (GRBs), especially those that present long-lasting X-ray plateau emissions. By solving the field equations, we find that when the rotational speed of the magnetar is approaching the breakup limit, its radius R and moment of inertia I undergo an obvious evolution as the magnetar spins down. Meanwhile, the values of R and I sensitively depend on the adoption of a neutron star (NS) equation of state (EoS) and the NS baryonic mass. With different EoSs and baryonic mass considered, the magnetic dipole radiation luminosity (Ldip) could be variant within one to two orders of magnitude. We thus suggest that when using the X-ray plateau data of GRBs to diagnose the properties of the nascent NSs, EoS and NS mass information should be invoked as simultaneously constrained parameters. On the other hand, due to the evolution of R and I, the temporal behavior of Ldip becomes more complicated. For instance, if the spin-down process is dominated by gravitational wave emission due to the NS asymmetry caused by magnetic field distortion ( $\epsilon \propto {B}_{p}^{2}$ ), the segment Ldip ∝ t0 could be followed by Ldip ∝ t-γ with γ larger than 3. This case could naturally interpret the so-called internal X-ray plateau feature shown in some GRB afterglows, which means the sharp decay following the plateau unnecessarily corresponds to the collapse of the NS. This may explain why some internal X-ray plateaus are followed by late-time central engine activity, manifested through flares and second shallow plateaus.

Keywords: Neutron stars, Magnetars, Gamma-ray bursts
Kinetic Imprints of Ion Acceleration in Collisionless Magnetic Reconnection. Fast collisionless magnetic reconnection implies fast energy conversion. The main form of energy conversion in magnetic reconnection concerns bulk ion acceleration with resulting ion jets. Based on theoretical analysis and MMS data, we examine the kinetic imprints of ion in the context of fast reconnection rates. The ion kinetic imprints we analyze in MMS observations include ion beams toward the X-line and distorted velocity distributions in reconnection jets. The distorted ion velocity distributions lead to a bipolar reversal in an off-diagonal element of the pressure tensor across the X-line, supporting an enhancement of the ion-scale reconnection electric field.

Keywords: Planetary magnetospheres, Solar magnetic reconnection, Space plasmas
Measurements of the Hubble Constant: Tensions in Perspective. Measurement of the distances to nearby galaxies has improved rapidly in recent decades. The ever-present challenge is to reduce systematic effects, especially as greater distances are probed and the uncertainties become larger. In this paper, we combine several recent calibrations of the tip of the red giant branch (TRGB) method. These calibrations are internally self-consistent at the 1% level. New Gaia Early Data Release 3 data provide an additional consistency check at a (lower) 5% level of accuracy, a result of the well-documented Gaia angular covariance bias. The updated TRGB calibration applied to a sample of Type Ia supernovae from the Carnegie Supernova Project results in a value of the Hubble constant of H0 = 69.8 ± 0.6 (stat) ± 1.6 (sys) km s-1 Mpc-1. No statistically significant difference is found between the value of H0 based on the TRGB and that determined from the cosmic microwave background. The TRGB results are also consistent to within 2σ with the SHoES and Spitzer plus Hubble Space Telescope (HST) Key Project Cepheid calibrations. The TRGB results alone do not demand additional new physics beyond the standard (ΛCDM) cosmological model. They have the advantage of simplicity of the underlying physics (the core He flash) and small systematic uncertainties (from extinction, metallicity, and crowding). Finally, the strengths and weaknesses of both the TRGB and Cepheids are reviewed, and prospects for addressing the current discrepancy with future Gaia, HST, and James Webb Space Telescope observations are discussed. Resolving this discrepancy is essential for ascertaining if the claimed tension in H0 between the locally measured and CMB-inferred values is physically motivated. * Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program Nos. 13472, 13691, 9477, and 10399.

Keywords: Cosmology, Observational cosmology, Hubble constant, Cepheid variable stars, Red giant stars, Stellar distance
Spitzer's Last Look at Extragalactic Explosions: Long-term Evolution of Interacting Supernovae. Here we present new, yet final, mid-infrared (mid-IR) data for supernovae (SNe) based on measurements with the Spitzer Space Telescope. Comparing our recent 3.6 and 4.5 μm photometry with previously published mid-IR and further multiwavelength data sets, we were able to draw some conclusions about the origin and heating mechanism of the dust in these SNe or in their environments, as well as about possible connection with circumstellar matter (CSM) originating from pre-explosion mass-loss events in the progenitor stars. We also present new results regarding both certain SN classes and single objects. We highlight the mid-IR homogeneity of SNe Ia-CSM, which may be a hint of their common progenitor type and of their basically uniform circumstellar environments. Regarding single objects, it is worth highlighting the late-time interacting Type Ib SNe 2003gk and 2004dk, for which we present the first-ever mid-IR data, which seem to be consistent with clues of ongoing CSM interaction detected in other wavelength ranges. Our current study suggests that long-term mid-IR follow-up observations play a key role in a better understanding of both pre- and post-explosion processes in SNe and their environments. While Spitzer is not available anymore, the expected unique data from the James Webb Space Telescope, as well as long-term near-IR follow-up observations of dusty SNe, can bring us closer to the hidden details of this topic.

Keywords: Infrared astronomy, Circumstellar matter, Infrared telescopes, Circumstellar dust, Supernovae
X-Ray Sources in the 1.75 Ms Ultra Narrow Deep Field Observed by XMM-Newton. In this work, we present the results of the survey carried out on one of the deepest X-ray fields observed by the XMM-Newton satellite. The 1.75 Ms Ultra Narrow Deep Field (XMM175UNDF) survey is made by 13 observations taken over 2 yr with a total exposure time of 1.75 Ms (1.372 Ms after flare-filtered) in a field of 30' × 30' centered around the blazar 1ES 1553+113. We stacked the 13 observations reaching flux limits of 4.03 × 10-16, 1.3 × 10-15, and 9.8 × 10-16 erg s-1 cm-2 in the soft (0.2-2 keV), hard (2-12 keV), and full (0.2-12 keV) bands, respectively. Using a conservative threshold of Maximum Likelihood significance of ML ≥ 6, corresponding to 3σ, we detected 301 point-sources for which we derived positions, fluxes in different bands, and hardness ratios. Thanks to an optical follow-up that was carried out using the 10.4m the Gran Telescopio Canarias on the same field in the u'g'r'i'z' bands, combined with WISE/2MASS IR data, we identified 244 optical/IR counterpart candidates for our X-ray sources and estimated their X-ray luminosities, redshift distribution, X-ray/optical-X-ray/IR flux ratios, and absolute magnitudes. Finally, we divided this subsample into 40 non-active sources and 204 active galactic nuclei, of which 139 are classified as Seyfert galaxies and 41 as Quasars.

Keywords: X-ray active galactic nuclei, X-ray surveys, Catalogs
The Evolution of Compressible Solar Wind Turbulence in the Inner Heliosphere: PSP, THEMIS, and MAVEN Observations. The first computations of the compressible energy transfer rate from ~0.2 up to ~1.7 au is obtained using Parker Solar Probe (PSP), Time History of Events and Macroscale Interactions during Substorms (THEMIS), and Mars Atmosphere and Volatile EvolutioN (MAVEN) observations. Using a recently derived exact relation for isothermal magnetohydrodynamics turbulence, the compressible energy cascade rate, εC, is computed for hundred of events at different heliocentric distances, for time intervals when the spacecrafts were in the pristine solar wind. The observational results show moderate increases of εC with respect to the incompressible cascade rate, εI. Depending on the level of compressibility in the plasma, which reaches up to 25% at PSP's perihelion, the different terms in the exact compressible relation are shown to have different impacts on the total cascade rate, εC. Finally, the observational results are connected with the local ion temperature and the solar wind heating problem.

Keywords: Slow solar wind, Solar wind, Interplanetary physics, Fast solar wind
An Exquisitely Deep View of Quenching Galaxies through the Gravitational Lens: Stellar Population, Morphology, and Ionized Gas. This work presents an in-depth analysis of four gravitationally lensed red galaxies at z = 1.6-3.2. The sources are magnified by factors of 2.7-30 by foreground clusters, enabling spectral and morphological measurements that are otherwise challenging. Our sample extends below the characteristic mass of the stellar mass function and is thus more representative of the quiescent galaxy population at z &gt; 1 than previous spectroscopic studies. We analyze deep VLT/X-SHOOTER spectra and multiband Hubble Space Telescope photometry that cover the rest-frame UV-to-optical regime. The entire sample resembles stellar disks as inferred from lensing-reconstructed images. Through stellar population synthesis analysis, we infer that the targets are young (median age = 0.1-1.2 Gyr) and formed 80% of their stellar masses within 0.07-0.47 Gyr. Mg II λλ 2796, 2803 absorption is detected across the sample. Blueshifted absorption and/or redshifted emission of Mg II are found in the two youngest sources, indicative of a galactic-scale outflow of warm (T ~ 104 K) gas. The [O III] λ5007 luminosity is higher for the two young sources (median age less than 0.4 Gyr) than the two older ones, perhaps suggesting a decline in nuclear activity as quenching proceeds. Despite high-velocity (v ≍ 1500 km s-1) galactic-scale outflows seen in the most recently quenched galaxies, warm gas is still present to some extent long after quenching. Altogether, our results indicate that star formation quenching at high redshift must have been a rapid process (&lt;1 Gyr) that does not synchronize with bulge formation or complete gas removal. Substantial bulge growth is required if they are to evolve into the metal-rich cores of present-day slow rotators.

Keywords: Supermassive black holes, Galaxy chemical evolution, Stellar populations, Galaxy structure, Galaxy stellar content, Galaxy ages, Warm ionized medium, Active galactic nuclei, Galaxy evolution, Galaxy quenching, Metallicity, Galaxy processes