Sazuna/UAT_keywords huggingface dataset:
A Giant Loop of Ionized Gas Emerging from the Tumultuous Central Region of IC 5063. The biconical radiation pattern extending from an active galactic nucleus (AGN) may strongly photoionize the circumnuclear interstellar medium (ISM) and stimulate emission from the narrow-line region (NLR). Observations of the NLR may provide clues to the structure of dense material that preferentially obscures the bicone at certain angles, and may reveal the presence of processes in the ISM tied to AGN accretion and feedback. Ground-based integral field units may study these processes via well-understood forbidden diagnostic lines such as [O III] and [S II], but scales of ~tens of parsecs remain challenging to spatially resolve at these wavelengths for all but the nearest AGN. We present recent narrow-filter Hubble Space Telescope observations of diagnostic forbidden ([O III], [S II]) and Balmer (Hα, Hβ) lines in the NLR of IC 5063. This AGN's jet inclination into the plane of the galaxy provides an important laboratory for strong AGN-host interactions. We find evidence for a low-ionization loop which emits brightly in [S II] and [N II], and which may arise from plume-like hot outflows that ablate ISM from the galactic plane before escaping laterally. We also present spatially resolved Baldwin-Phillips-Terlevich diagnostic maps of the IC 5063 NLR. These maps suggest a sharp transition to lower-ionization states outside the jet path, and that such emission is dominated by ~10-40 pc clumps and filamentary structure at large (≫25°) angles from the bicone axis. Such emission may arise from precursorless shocks when AGN outflows impact low-density hot plasma in the cross cone. * Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. These observations are associated with programs #8598 and #15609.

Keywords: Seyfert galaxies, Active galaxies
Total Solar Irradiance Variability on the Evolutionary Timescale and its Impact on the Earth's Mean Surface Temperature. The Sun is the primary source of energy for the Earth. The small changes in total solar irradiance (TSI) can affect our climate on the longer timescale. In the evolutionary timescale, the TSI varies by a large amount and hence its influence on the Earth's mean surface temperature (Ts) also increases significantly. We develop a mass loss dependent analytical model of TSI in the evolutionary timescale and evaluated its influence on the Ts. We determined the numerical solution of TSI for the next 8.23 Gyr to be used as an input to evaluate the Ts which formulated based on a zero-dimensional energy balance model. We used the present-day albedo and bulk atmospheric emissivity of the Earth and Mars as initial and final boundary conditions, respectively. We found that the TSI increases by 10% in 1.42 Gyr, by 40% in about 3.4 Gyr, and by 120% in about 5.229 Gyr from now, while the Ts shows an insignificant change in 1.644 Gyr and increases to 298.86 K in about 3.4 Gyr. The Ts attains the peak value of 2319.2 K as the Sun evolves to the red giant and emits the enormous TSI of 7.93 × 106 W m-2 in 7.676 Gys. At this temperature Earth likely evolves to be a liquid planet. In our finding, the absorbed and emitted flux equally increases and approaches the surface flux in the main sequence, and they are nearly equal beyond the main sequence, while the flux absorbed by the cloud shows the opposite trend.

Keywords: Planetary science, Planetary atmospheres, Planetary climates, Solar evolution
Rovibrationally Resolved Photodissociation of AlH via Excited Electronic States. Photodissociation processes are of great importance for modeling interstellar chemistry since it is a key destruction pathway for small molecules. Here, we present a detailed ab initio study of AlH photodissociation. Potential energy curves and transition dipole moments for AlH are obtained by using the internally contracted multireference configuration interaction method and the Davidson correction (icMRCI+Q), as well as the aug-cc-pV6Z basis set. Except for the X1Σ+, A1Π, and C1Σ+ states, five higher excited 31Σ+, 21Π, 31Π, 41Σ+, and 41Π states are considered in order to investigate the photodissociation pathways in the vacuum ultraviolet region. State-resolved cross sections of transitions from all the rovibrational levels of the X1Σ+ state to seven singlet excited states are computed for photon wavelengths ranging from 500 Å to the threshold. Photodissociation cross sections in local thermal equilibrium (LTE) are obtained at temperatures from 500 to 10,000 K. Applications of the LTE cross sections to compute photodissociation rates in the standard interstellar radiation field and blackbody radiation field are briefly discussed.

Keywords: Radiative processes, Interstellar molecules, Astrochemistry
Spiral Structure Boosts Star Formation in Disk Galaxies. We investigate the impact of spiral structure on global star formation using a sample of 2226 nearby bright disk galaxies. Examining the relationship between spiral arms, star formation rate (SFR), and stellar mass, we find that arm strength correlates well with the variation of SFR as a function of stellar mass. Arms are stronger above the star-forming galaxy main sequence (MS) and weaker below it: arm strength increases with higher $\mathrm{log}(\mathrm{SFR}/{\mathrm{SFR}}_{\mathrm{MS}})$ , where SFRMS is the SFR along the MS. Likewise, stronger arms are associated with higher specific SFR. We confirm this trend using the optical colors of a larger sample of 4378 disk galaxies, whose position on the blue cloud also depends systematically on spiral arm strength. This link is independent of other galaxy structural parameters. For the subset of galaxies with cold gas measurements, arm strength positively correlates with H I and H2 mass fraction, even after removing the mutual dependence on $\mathrm{log}(\mathrm{SFR}/{\mathrm{SFR}}_{\mathrm{MS}})$ , consistent with the notion that spiral arms are maintained by dynamical cooling provided by gas damping. For a given gas fraction, stronger arms lead to higher $\mathrm{log}(\mathrm{SFR}/{\mathrm{SFR}}_{\mathrm{MS}})$ , resulting in a trend of increasing arm strength with shorter gas depletion time. We suggest a physical picture in which the dissipation process provided by gas damping maintains spiral structure, which, in turn, boosts the star formation efficiency of the gas reservoir.

Keywords: Spiral galaxies, Galaxy structure, Spiral arms, Star formation, Galaxy evolution, Interstellar medium
The Diversity of Environments around Luminous Quasars at Redshift z   6. Significant clustering around the rarest luminous quasars is a feature predicted by dark matter theory combined with number density matching arguments. However, this expectation is not reflected by observations of quasars residing in a diverse range of environments. Here we assess the tension in the diverse clustering of visible i-band dropout galaxies around luminous z ~ 6 quasars. Our approach uses a simple empirical method to derive the median luminosity-to-halo mass relation, Lc(Mh), for both quasars and galaxies under the assumption of lognormal luminosity scatter, ΣQ and ΣG. We show that higher ΣQ reduces the average halo mass hosting a quasar of a given luminosity, thus introducing at least a partial reversion to the mean in the number count distribution of nearby Lyman-break galaxies. We generate a large sample of mock Hubble Space Telescope fields of view centered across rare z ~ 6 quasars by resampling pencil beams traced through the dark matter component of the BlueTides cosmological simulation. We find that diverse quasar environments are expected for ΣQ &gt; 0.4, consistent with numerous observations and theoretical studies. However, we note that the average number of galaxies around the central quasar is primarily driven by galaxy evolutionary processes in neighboring halos, as embodied by our parameter ΣG, instead of a difference in the large-scale structure around the central quasar host, embodied by ΣQ. We conclude that models with ΣG &gt; 0.3 are consistent with current observational constraints on high-z quasars, and that such a value is comparable to the scatter estimated from hydrodynamical simulations of galaxy formation.

Keywords: Supermassive black holes, Clustering, Quasars
Broadband High-energy Emission of the Gamma-Ray Binary System LS 5039: Spectral and Temporal Features Using NuSTAR and Fermi Observations. We report a detailed analysis of the hard X-ray and GeV gamma-ray spectra of LS 5039, one of the brightest gamma-ray binary system in the Galaxy. The Nuclear Spectroscopic Telescope Array (NuSTAR) observation covering its entire orbit in 2016 allowed us for the first time to study the orbital variability of the spectrum above 10 keV. The hard X-ray spectrum is well described with a single power-law component up to 78 keV. The X-ray flux showed a slight deviation from those observed previously with Suzaku in 2007. The fast X-ray brightening observed with Suzaku, around the inferior conjunction, was not observed in this observation. We also analyzed 11 yr of Fermi Large Area Telescope data of LS 5039. The GeV spectrum around the inferior conjunction was well described with two nonthermal components: a power law with a photon index of ~3 and a cutoff power law with a cutoff energy of ~2 GeV. The orbital flux variability also changed gradually around a few GeV. These results indicate that there are two emission components in the GeV band, and the dominant component above ~1 GeV does not depend on the orbital phase. By combining these results, we update the spectral energy distribution of LS 5039 with the highest available statistics. Theoretical models proposed so far cannot explain the obtained multiwavelength spectrum, especially the emission from ~1 to ~400 MeV, and we discuss the possibility that particle acceleration in LS 5039 is different from the shock acceleration.

Keywords: X-ray binary stars, Gamma-ray sources, Compact binary stars, High mass x-ray binary stars, X-ray sources
Variation of the Interplanetary Shocks in the Inner Heliosphere. Observations of the solar wind plasma and interplanetary magnetic field in the ecliptic plane by the Voyager 1 and 2 spacecraft are utilized to study the variation of the interplanetary shocks (with magnetosonic Mach number &gt;1) encountered in the inner heliosphere, between ~1 and ~15 au from the Sun. The overwhelming majority (~76%) of the shocks are fast forward (FF) moving at an average shock speed (Vsh) of ~458 km s-1 away from the Sun, and only ~24% are fast reverse (FR) shocks with an average Vsh of ~323 km s-1 toward the Sun. About ~89% of the shocks are quasi-perpendicular with an average shock angle (θBn) of ~72° relative to the ambient magnetic field, and only ~11% are quasi-parallel with an average θBn of ~32°. While the interplanetary coronal mass ejections are the major (~89%) driver of the FF shocks, a significant part (~41%) of the FR shocks are associated with the corotating interaction regions. The shock occurrence rate, with a peak at the heliocentric distance (Rh) of ~5 au, exhibits a clear decrease with the increasing Rh. While the shock strength and propagation angle do not exhibit any systematic change with Rh, Vsh increases with the increasing Rh at a rate of ~11 km s-1 au-1.

Keywords: Interplanetary shocks, Solar wind, Interplanetary magnetic fields, Solar coronal mass ejections, Corotating streams
High-resolution Extinction Map in the Direction of the Strongly Obscured Bulge Fossil Fragment Liller 1. We used optical images acquired with the Wide Field Camera of the Advanced Camera for Surveys on board the Hubble Space Telescope and near-infrared data from Gemini Multi-conjugate Adaptive Optics System (GeMS)/Gemini South Adaptive Optics Imager (GSAOI) to construct a high-resolution extinction map in the direction of the bulge stellar system Liller 1. In spite of its appearance of a globular cluster, Liller 1 has been recently found to harbor two stellar populations with remarkably different ages, and it is the second complex stellar system with similar properties (after Terzan 5) discovered in the bulge, thus defining a new class of objects: the Bulge Fossil Fragments. Because of its location in the inner bulge of the Milky Way, very close to the Galactic plane, Liller 1 is strongly affected by large and variable extinction. The simultaneous study of both the optical and the near-infrared color-magnitude diagrams revealed that the extinction coefficient RV in the direction of Liller 1 has a much smaller value than commonly assumed for diffuse interstellar medium (RV = 2.5, instead of 3.1), in agreement with previous findings along different light paths to the Galactic bulge. The derived differential reddening map has a spatial resolution ranging from 1″ to 3″ over a field of view of about 90″ × 90″. We found that the absorption clouds show patchy substructures with extinction variations as large as δE(B - V) ~ 0.9 mag. * Based on observations collected with the NASA/ESA HST (Prop. GO 15231), obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. Based on observations (Prop. GS-2013-Q-23) obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). Based on observations gathered with the ESO-VISTA telescope (program ID 179.B-2002).

Keywords: Globular star clusters, Galactic bulge, Reddening law, Extinction, Star clusters
TIC 454140642: A Compact, Coplanar, Quadruple-lined Quadruple Star System Consisting of Two Eclipsing Binaries. We report the discovery of a compact, coplanar, quadruple-lined, eclipsing quadruple star system from Transiting Exoplanet Survey Satellite data, TIC 454140642, also known as TYC 0074-01254-1. The target was first detected in Sector 5 with a 30-minute cadence in full-frame images and then observed in Sector 32 with a 2-minute cadence. The light curve exhibits two sets of primary and secondary eclipses with periods of PA = 13.624 days (binary A) and PB = 10.393 days (binary B). Analysis of archival and follow-up data shows clear eclipse-timing variations and divergent radial velocities, indicating dynamical interactions between the two binaries and confirming that they form a gravitationally bound quadruple system with a 2 + 2 hierarchy. The Aa+Ab binary, Ba+Bb binary, and A-B system are aligned with respect to each other within a fraction of a degree: the respective mutual orbital inclinations are 0°25 (A versus B), 0°37 (A versus A-B), and 0°47 (B versus A-B). The A-B system has an orbital period of 432 days-the second shortest of the confirmed quadruple systems-and an orbital eccentricity of 0.3.

Keywords: Multiple stars, Astronomy data modeling, Astronomy data analysis, Eclipsing binary stars, Transit photometry
Physical Characterization of Serendipitously Uncovered Millimeter-wave Line-emitting Galaxies at z   2.5 behind the Local Luminous Infrared Galaxy VV 114. We present a detailed investigation of millimeter-wave line emitters ALMA J010748.3-173028 (ALMA-J0107a) and ALMA J010747.0-173010 (ALMA-J0107b), which were serendipitously uncovered in the background of the nearby galaxy VV 114 with spectral scan observations at λ = 2-3 mm. Via Atacama Large Millimeter/submillimeter Array (ALMA) detection of CO(4-3), CO(3-2), and [C I](1-0) lines for both sources, their spectroscopic redshifts are unambiguously determined to be z = 2.4666 ± 0.0002 and z = 2.3100 ± 0.0002, respectively. We obtain the apparent molecular gas masses Mgas of these two line emitters from [C I] line fluxes as (11.2 ± 3.1) × 1010 M⊙ and (4.2 ± 1.2) × 1010 M⊙, respectively. The observed CO(4-3) velocity field of ALMA-J0107a exhibits a clear velocity gradient across the CO disk, and we find that ALMA-J0107a is characterized by an inclined rotating disk with a significant turbulence, that is, a deprojected maximum rotation velocity to velocity dispersion ratio ${v}_{\max }/{\sigma }_{v}$ of 1.3 ± 0.3. We find that the dynamical mass of ALMA-J0107a within the CO-emitting disk computed from the derived kinetic parameters, (1.1 ± 0.2) × 1010 M⊙, is an order of magnitude smaller than the molecular gas mass derived from dust continuum emission, (3.2 ± 1.6) × 1011 M⊙. We suggest this source is magnified by a gravitational lens with a magnification of μ ≳ 10, which is consistent with the measured offset from the empirical correlation between CO-line luminosity and width.

Keywords: Starburst galaxies, Galaxy kinematics, Interstellar medium, Submillimeter astronomy, High-redshift galaxies
Nearby SN-associated GRB 190829A: Environment, Jet Structure, and VHE Gamma-Ray Afterglows. We present a self-consistent paradigm to interpret the striking features of nearby low-luminosity GRB 190829A. Its prompt gamma-ray lightcurve has two separated pulses. We propose that the interaction of the hard prompt gamma-ray photons ( ${E}_{p}={624}_{-303}^{+2432}$ keV) of its initial pulse with the dusty medium (AV = 2.33) not only results in the second soft gamma-ray pulse (Ep ~ 12 keV) but also makes a pre-accelerated e± -rich medium shell via the γγ annihilation. In this paradigm, we show that the observed radio, optical, and X-ray afterglow lightcurves are well-fitted with the forward shock model. Its jet is almost isotropic (θj &gt; 1.0 rad) with a Lorentz factor of ~35, and the electron density of the e± -rich medium shell is ~15 cm-3, which is about seven times higher than the electron density of its normal surrounding medium. The GRB ejecta catches up with and propagates into the e± -rich medium shell at a region of R = (4.07-6.46) × 1016 cm. This results in a bright afterglow bump at ~103 seconds after the GRB trigger. The predicted very high energy (VHE) gamma-ray emission from the synchrotron self-Compton process agrees with the H.E.S.S. observation. The derived broadband spectral energy distribution shows that GRB 190829A like nearby GRBs would be promising targets of the VHE gamma-ray telescopes, such as H.E.S.S., MAGIC, and CTA (Cerenkov Telescope Arrays).

Keywords: Gamma-ray bursts
Search for Galactic Civilizations Using Historical Supernovae. We study an interstellar signaling scheme that was originally proposed by Seto and efficiently links intentional transmitters to extraterrestrial intelligence (ETI) searchers through a conspicuous astronomical burst, without prior communication. Based on the geometrical and game theoretic viewpoints, the scheme can be refined so that intentional signals can be sent and received after observing a reference burst, in contrast to the original proposal (before observing a burst). Given this inverted temporal structure, Galactic supernovae recorded in the past 2000 yr can be regarded as interesting guideposts for an ETI search. While the best use period of SN 393 has presumably passed ~100 yr ago, some of the historical supernovae might allow us to compactify the ETI survey regions down to less than one present of 4π, around two rings in the sky.

Keywords: Supernova remnants, Search for extraterrestrial intelligence, Technosignatures
ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin. ASASSN-14ms may represent the most luminous Type Ibn supernova (SN Ibn) ever detected, with an absolute U-band magnitude brighter than -22.0 mag and a total bolometric luminosity &gt;1.0 × 1044 erg s-1 near maximum light. The early-time spectra of this SN are characterized by a blue continuum on which are superimposed narrow P Cygni profile lines of He I, suggesting the presence of slowly moving (~1000 km s-1), He-rich circumstellar material (CSM). At 1-2 months after maximum brightness, the He I line profiles become only slightly broader, with blueshifted velocities of 2000-3000 km s-1, consistent with the CSM shell being continuously accelerated by the SN light and ejecta. Like most SNe Ibn, the light curves of ASASSN-14ms show rapid post-peak evolution, dropping by ~7 mag in the V band over three months. Such a rapid post-peak decline and high luminosity can be explained by interaction between SN ejecta and helium-rich CSM of 0.9 M⊙ at a distance of ~1015 cm. The CSM around ASASSN-14ms is estimated to originate from a pre-explosion event with a mass-loss rate of 6.7 M⊙ yr-1 (assuming a velocity of ~1000 km s-1), which is consistent with abundant He-rich material violently ejected during the late Wolf-Rayet (WN9-11 or Opfe) stage. After examining the light curves for a sample of SNe Ibn, we find that the more luminous ones tend to have slower post-peak decline rates, reflecting that the observed differences may arise primarily from discrepancies in the CSM distribution around the massive progenitors.

Keywords: Circumstellar dust, Stellar mass loss
The Diffusion Coefficient of the Splashback Mass Function as a Probe of Cosmology. We present an analytic model for the splashback mass function of dark matter halos, which is parameterized by a single coefficient and constructed in the framework of the generalized excursion set theory and the self-similar spherical infall model. The value of the single coefficient that quantifies the diffusive nature of the splashback boundary is determined at various redshifts by comparing the model with the numerical results from the Erebos N-body simulations for the Planck and the WMAP7 cosmologies. Showing that the analytic model with the best-fit coefficient provides excellent matches to the numerical results in the mass range of 5 ≤ M/(1012 h-1 M⊙) &lt; 103, we employ the Bayesian and Akaike Information Criterion tests to confirm that our model is most preferred by the numerical results compared to previous models at redshifts of 0.3 ≤ z ≤ 3 for both of the cosmologies. We also found that the diffusion coefficient decreases almost linearly with redshift, converging to zero at a certain threshold redshift, zc, whose value significantly differs between the Planck and WMAP7 cosmologies. Our result implies that the splashback mass function of dark matter halos at z ≥ zc is well described by a parameter-free analytic formula and that zc may have the potential to independently constrain the initial conditions of the universe.

Keywords: Cosmological models, Large-scale structure of the universe