Sazuna/UAT_keywords huggingface dataset:
Evidence for a Supergalactic Structure of Magnetic Deflection Multiplets of Ultra-high-energy Cosmic Rays. Evidence for a large-scale supergalactic cosmic-ray multiplet (arrival directions correlated with energy) structure is reported for ultra-high-energy cosmic-ray (UHECR) energies above 1019 eV using 7 years of data from the Telescope Array (TA) surface detector and updated to 10 years. Previous energy-position correlation studies have made assumptions regarding magnetic field shapes and strength, and UHECR composition. Here the assumption tested is that, because the supergalactic plane is a fit to the average matter density of the local large-scale structure, UHECR sources and intervening extragalactic magnetic fields are correlated with this plane. This supergalactic deflection hypothesis is tested by the entire field-of-view (FOV) behavior of the strength of intermediate-scale energy-angle correlations. These multiplets are measured in spherical cap section bins (wedges) of the FOV to account for coherent and random magnetic fields. The structure found is consistent with supergalactic deflection, the previously published energy spectrum anisotropy results of the TA (the Hotspot and Coldspot), and toy-model simulations of a supergalactic magnetic sheet. The seven year data posttrial significance of this supergalactic structure of multiplets appearing by chance, on an isotropic sky, is found by Monte Carlo simulation to be 4.2σ. The 10 years of data posttrial significance is 4.1σ. Furthermore, the starburst galaxy M82 is shown to be a possible source of the TA Hotspot, and an estimate of the supergalactic magnetic field using UHECR measurements is presented.

Keywords: Extragalactic magnetic fields, High energy astrophysics, Astrophysical magnetism, Cosmic ray astronomy, Cosmic ray sources, Ultra-high-energy cosmic radiation, Cosmic rays
The Kinematics of Massive Quiescent Galaxies at 1.4 &lt; z &lt; 2.1: Dark Matter Fractions, IMF Variation, and the Relation to Local Early-type Galaxies. We study the dynamical properties of massive quiescent galaxies at 1.4 &lt; z &lt; 2.1 using deep Hubble Space Telescope WFC3/F160W imaging and a combination of literature stellar velocity dispersion measurements and new near-infrared spectra obtained using the K-band Multi Object Spectrograph (KMOS) on the ESO Very Large Telescope. We use these data to show that the typical dynamical-to-stellar mass ratio has increased by ∼0.2 dex from z = 2 to the present day, and we investigate this evolution in the context of possible changes in the stellar initial mass function (IMF) and/or fraction of dark matter contained within the galaxy effective radius, fDM[&lt;re]. Comparing our high-redshift sample to their likely descendants at low redshift, we find that fDM[&lt;re] has increased by a factor of more than 4 since z ≍ 1.8, from fDM[&lt;re] = 6.6% ± 1.0% to ∼24%. The observed increase appears robust to changes in the methods used to estimate dynamical masses or match progenitors and descendants. We quantify possible variation of the stellar IMF through the offset parameter α, defined as the ratio of dynamical mass in stars to the stellar mass estimated using a Chabrier IMF. We demonstrate that the correlation between stellar velocity dispersion and α reported among quiescent galaxies at low redshift is already in place at z = 2, and we argue that subsequent evolution through (mostly minor) merging should act to preserve this relation while contributing significantly to galaxies' overall growth in size and stellar mass. * Based on observations obtained at the Very Large Telescope (VLT) of the European Southern Observatory (ESO), Paranal, Chile (ESO program IDs 092.A-0091, 093.A-0079, 093.A-0187, and 094.A-0287).

Keywords: High-redshift galaxies, Galaxy kinematics, Galaxy evolution
Correlation of Structure and Stellar Properties of Galaxies in Stripe 82. Establishing a correlation (or lack thereof) between the bimodal color distribution of galaxies and their structural parameters is crucial to understand the origin of bimodality. To achieve that, we have performed a 2D mass-based structural decomposition (bulge+disk) of all disk galaxies (total = 1263) in the Herschel imaging area of the Stripe 82 region using Ks-band images from the VICS82 survey. The scaling relations thus derived are found to reflect the internal kinematics and are employed in combination to select an indubitable set of classical- and pseudo-bulge-hosting disk galaxies. The rest of the galaxies (&lt;20%) are marked as disks with "ambiguous" bulges. Pseudo- and classical bulge-disk galaxies exhibit clear bimodality in terms of all stellar parameters (M*, specific star formation rate, r - Ks). All pseudo-bulge-disk galaxies are blue and star forming, and all classical bulge-disk galaxies are red and quiescent with less than 5% digressions. Ambiguous bulge-disk galaxies are intermediate to pseudo- and classical bulge-disk galaxies in the distribution of all structural and stellar parameters. ${\rm{\Delta }}\langle {\mu }_{\mathrm{eb}}\rangle $ —based on the placement of bulges on the Kormendy relation—is found to be the most efficient single structural indicator of both bulge type and stellar activity. The placement of ambiguous bulge-disk galaxies on scaling relations and the fundamental plane, in addition to their peculiar stellar properties, suggests that they are dominantly part of the green valley.

Keywords: Galaxy structure, Galaxy bulges, Star formation, Galaxy stellar content
A Numerical Study of the Effects of Corotating Interaction Regions on Cosmic-Ray Transport. The intensity of galactic cosmic rays (GCRs) is modulated by solar activity on various timescales. In this study, we performed comprehensive numerical modeling of the solar rotational recurrent variation in GCRs caused by a corotation interaction region (CIR). A recently developed magnetohydrodynamic numerical model is adapted to simulate the background solar wind plasma with a CIR structure present in the inner heliosphere. As for the outer heliospheric plasma background, from 27 to 80 au, the Parker interplanetary magnetic field model is utilized. The output of these plasma and magnetic field models is incorporated into a comprehensive Parker-type transport model for GCRs. The local interstellar spectrum for galactic protons is transported to 80 au, specifying the outer boundary condition. The obtained solutions of this hybrid model, for studying the CIR effect, are as follows: (1) the onset of the decrease in the GCR intensity inside the CIR coincides with the increase of the solar wind speed with the intensity depression accompanied by a magnetic field and plasma density enhancement. Additionally, the CIR effect weakens with increasing heliocentric radial distance. (2) This decrease in GCR intensity also appears at different heliolatitudes and varies with changing latitude; the amplitude of the GCR depression exhibits a maximum in the low-latitude region. (3) The CIR affects GCR transport at different energy levels as well. Careful analysis has revealed a specific energy dependence of the amplitude of the recurrent GCR variation in the range of 30-2000 MeV.

Keywords: Galactic cosmic rays, Solar wind, Corotating streams
Unified Simulations of Planetary Formation and Atmospheric Evolution. II. Rapid Disk Clearing by Photoevaporation Yields Low-mass Super-Earth Atmospheres. Super-Earths possess low-mass H2/He atmospheres (typically less than 10% by mass). However, the origins of super-Earth atmospheres have not yet been ascertained. We investigate the role of rapid disk clearing by photoevaporation during the formation of super-Earths and their atmospheres. We perform unified simulations of super-Earth formation and atmospheric evolution in evolving disks that consider both photoevaporative winds and magnetically driven disk winds. For the growth mode of planetary cores, we consider two cases in which planetary embryos grow with and without pebble accretion. Our main findings are summarized as follows. (i) The time span of atmospheric accretion is shortened by rapid disk dissipation due to photoevaporation, which prevents super-Earth cores from accreting massive atmospheres. (ii) Even if planetary cores grow rapidly by embryo accretion in the case without pebble accretion, the onset of runaway gas accretion is delayed because the isolation mass for embryo accretion is small. Together with rapid disk clearing, the accretion of massive atmospheres can be avoided. (iii) After rapid disk clearing, a number of high-eccentricity embryos can remain in outer orbits. Thereafter, such embryos may collide with the super-Earths, leading to efficient impact erosion of accreted atmospheres. Therefore, we find that super-Earths with low-mass H2/He atmospheres are naturally produced by N-body simulations that consider realistic disk evolution.

Keywords: Exoplanet dynamics, Planet formation, Exoplanet formation, Exoplanet atmospheres
Impact of an Active Sgr A* on the Synthesis of Water and Organic Molecules throughout the Milky Way. Sgr A*, the supermassive black hole (SMBH) in our Galaxy, is dormant today, but it should have gone through multiple gas-accretion episodes in the past billions of years to grow to its current mass of 4 × 106 M⊙. Each episode temporarily ignites the SMBH and turns the Galactic Center into an active galactic nucleus (AGN). Recently, we showed that the AGN could produce large amounts of hard X-rays that can penetrate the dense interstellar medium in the Galactic plane. Here we further study the impact of X-rays on the molecular chemistry in our Galaxy. We use a chemical-reaction network to simulate the evolution of several molecular species, including H2O, CH3OH, and H2CO, both in the gas phase and on the surface of dust grains. We find that X-ray irradiation could significantly enhance the abundances of these species. The effect is most significant in young, high-density molecular clouds and could be prominent at a Galactic distance of 8 kpc or smaller. The imprint in the chemical abundance is visible even several million years after the AGN turns off.

Keywords: Interstellar molecules, Astrochemistry, Galaxy abundances, X-ray active galactic nuclei, Interstellar medium
The Star Formation Rate-Radius Connection: Data and Implications for Wind Strength and Halo Concentration. This paper is one in a series that explores the importance of radius as a second parameter in galaxy evolution. The topic investigated here is the relationship between star formation rate (SFR) and galaxy radius ( ${R}_{{\rm{e}}}$ ) for main-sequence star-forming galaxies. The key observational result is that, over a wide range of stellar mass and redshift in both CANDELS and SDSS, there is little correlation between SFR and ${R}_{{\rm{e}}}$ at fixed stellar mass. The Kennicutt-Schmidt law, or any similar density-related star formation law, then implies that smaller galaxies must have lower gas fractions than larger galaxies (at fixed ${M}_{* }$ ), and this is supported by observations of gas in local star-forming galaxies. We investigate the implications by adopting the equilibrium "bathtub" model: the ISM gas mass is assumed to be constant over time, and the net SFR is the difference between the accretion rate of gas onto the galaxy from the halo and the outflow rate due to winds. To match the observed null correlation between SFR and radius, the bathtub model requires that smaller galaxies at fixed mass have weaker galactic winds. Our hypothesis is that galaxies are a two-parameter family whose properties are set mainly by halo mass and concentration. These determine the radius and gas accretion rate, which in turn predict how wind strength needs to vary with ${R}_{{\rm{e}}}$ to keep the SFR constant.

Keywords: Galaxy structure, Star formation, Galaxy evolution
Recombination Lines and Molecular Gas from Hypercompact H II regions in W51 A. We present a detailed characterization of the population of compact radio-continuum sources in W51 A using subarcsecond Very Large Array and Atacama Large Millimeter/submillimeter Array observations. We analyze their 2 cm continuum, the recombination lines (RLs) H77α and H30α, and the lines of ${{\rm{H}}}_{2}\mathrm{CO}({3}_{\mathrm{0,3}}-{2}_{\mathrm{0,2}})$ , ${{\rm{H}}}_{2}\mathrm{CO}({3}_{\mathrm{2,1}}-{2}_{\mathrm{2,0}})$ , and $\mathrm{SO}({6}_{5}-{5}_{4})$ . We derive diameters for 10/20 sources in the range D ∼ 10-3 to ∼10-2 pc, thus placing them in the regime of hypercompact H II regions (HC H II's). Their continuum-derived electron densities are in the range ne ∼ 104 -105 cm-3, lower than typically considered for HC H II's. We combined the RL measurements and independently derived ne, finding the same range of values but significant offsets for individual measurements between the two methods. We find that most of the sources in our sample are ionized by early B-type stars, and a comparison of ne versus D shows that they follow the inverse relation previously derived for ultracompact (UC) and compact H II's. When determined, the ionized-gas kinematics is always (7/7) indicative of outflow. Similarly, 5 and 3 out of the 8 HC H II's still embedded in a compact core show evidence for expansion and infall motions in the molecular gas, respectively. We hypothesize that there could be two different types of hypercompact (D &lt; 0.05 pc) H II regions: those that essentially are smaller, expanding UC H II's; and those that are also hyperdense (ne &gt; 106 cm-3), probably associated with O-type stars in a specific stage of their formation or early life.

Keywords: Star formation, Giant molecular clouds, Radio astronomy, H II regions
Generalized General Relativistic Magnetohydrodynamic Equations for Plasmas of Active Galactic Nuclei in the Era of the Event Horizon Telescope. The generalized general relativistic magnetohydrodynamic (generalized GRMHD) equations have been used to study specific relativistic plasma phenomena, such as relativistic magnetic reconnection or wave propagation modified by nonideal MHD effects. However, the Θ term in the generalized Ohm's law, which expresses the energy exchange between two fluids composing a plasma, has yet to be determined in these equations. In this paper, we determine the Θ term based on the generalized relativistic Ohm's law itself. This provides closure of the generalized GRMHD equations, yielding a closed system of the equations of relativistic plasma. According to this system of equations, we reveal the characteristic scales of nonideal MHD phenomena and clarify the applicable condition of the ideal GRMHD equations. We evaluate the characteristic scales of the nonideal MHD phenomena in the M87* plasma using the Event Horizon Telescope observational data.

Keywords: Black hole physics, High energy astrophysics, Plasma physics, Active galactic nuclei, General relativity, Magnetic fields
Characterizing Quasar C IV Emission-line Measurements from Time-resolved Spectroscopy. We use multiepoch quasar spectroscopy to determine how accurately single-epoch spectroscopy can locate quasars in emission-line parameter space in order to inform investigations where time-resolved spectroscopy is not available. We explore the improvements in emission-line characterization that result from using nonparametric information from many lines as opposed to a small number of parameters for a single line, utilizing reconstructions based on an independent component analysis applied to the data from the Sloan Digital Sky Survey Reverberation Mapping project. We find that most of the quasars are well described by just two components, while more components signal a quasar likely to yield a successful reverberation mapping analysis. In single-epoch spectroscopy the apparent variability of equivalent width is exaggerated because it is dependent on the continuum. Multiepoch spectroscopy reveals that single-epoch results do not significantly change where quasars are located in C IV parameter space and do not have a significant impact on investigations of the global Baldwin effect. Quasars with emission-line properties indicative of higher L/LEdd are less variable, consistent with models with enhanced accretion disk density. Narrow absorption features at the systemic redshift may be indicative of orientation (including radio-quiet quasars) and may appear in as much as 20% of the quasar sample. Future work applying these techniques to lower-luminosity quasars will be important for understanding the nature of accretion disk winds.

Keywords: Black hole physics, Quasars
On the Magnetic Fields, Beaming Fractions, and Fastness Parameters of Pulsating Ultraluminous X-Ray Sources. The discovery of pulsating ultraluminous X-ray sources (PULX) suggests that neutron stars are presumably common within the ultraluminous X-ray source (ULX) population though the majority of the population members currently lack pulsations. These systems are likely to host neutron stars accreting mass at super-Eddington (supercritical) rates from their massive companion in high-mass X-ray binaries. Taking into account the spherization of the accretion flow in the supercritical regime, the beaming of X-ray emission, and the reduction of the scattering cross section in a strong magnetic field, we infer the ranges for the neutron-star surface magnetic dipole field strengths, beaming fractions, and fastness parameters in the PULX M82 X-2, ULX NGC 5907, ULX NGC 7793 P13, NGC 300 ULX1, M51 ULX-7, NGC 1313 X-2, and Swift J0243.6+6124 from a set of conditions based on a variety of combinations of different spin and luminosity states. Using the observed spin-up rates under the critical luminosity condition, we estimate the surface-field strengths in the ∼1011-1013 G range for all PULX. In general, the results of our analysis under the subcritical luminosity condition indicate surface-field strengths in the ∼1011-1015 G range. We argue that PULX do not require magnetar-strength surface dipole fields if beaming is taken into account, yet the fields are strong enough for the neutron stars in ULX to magnetically channel the accretion flow in supercritical accretion disks.

Keywords: Neutron stars, X-ray binary stars, Accretion, Pulsars
GASP XXX. The Spatially Resolved SFR-Mass Relation in Stripping Galaxies in the Local Universe. The study of the spatially resolved star formation rate-mass ( ${{\rm{\Sigma }}}_{\mathrm{SFR}}$ - ${{\rm{\Sigma }}}_{* }$ ) relation gives important insights on how galaxies assemble at different spatial scales. Here, we present an analysis of the ${{\rm{\Sigma }}}_{\mathrm{SFR}}$ - ${{\rm{\Sigma }}}_{* }$ of 40 local cluster galaxies undergoing ram-pressure stripping drawn from the GAs Stripping Phenomena in galaxies (GASP) sample. Considering their integrated properties, these galaxies show an SFR enhancement with respect to undisturbed galaxies of similar stellar mass; we now exploit spatially resolved data to investigate the origin and location of the excess. Even on ∼1kpc scales, stripping galaxies present a systematic enhancement of ${{\rm{\Sigma }}}_{\mathrm{SFR}}$ (∼0.35 dex at ${{\rm{\Sigma }}}_{* }$ = ${10}^{8}{M}_{\odot }\,{\mathrm{kpc}}^{-2}$ ) at any given ${{\rm{\Sigma }}}_{* }$ compared to their undisturbed counterparts. The excess is independent of the degree of stripping and of the amount of star formation in the tails, and it is visible at all galactocentric distances within the disks, suggesting that the star formation is most likely induced by compression waves from ram pressure. Such excess is larger for less massive galaxies and decreases with increasing mass. As stripping galaxies are characterized by ionized gas beyond the stellar disk, we also investigate the properties of 411 star-forming clumps found in the galaxy tails. At any given stellar mass density, these clumps are systematically forming stars at a higher rate than in the disk, but differences are reconciled when we just consider the mass formed in the last few 108 yr ago, suggesting that on these timescales, the local mode of star formation is similar in the tails and in the disks.

Keywords: Galaxy clusters, Galaxy formation, Emission line galaxies, Star formation, Galaxy evolution, Galaxies
Fast Magnetosonic Waves and Flows in a Solar Prominence Foot: Observations and Modeling. We study recent observations of propagating fluctuations in a prominence foot with Hinode Solar Optical Telescope (SOT) high-resolution observations in Ca II and Hα emission, which we identify as nonlinear fast magnetosonic waves. Here we analyze further the observations of propagating waves and flows with Interface Region Imaging Spectrograph Mg II slit jaw images, in addition to Hinode/SOT Ca II images. We find that the waves have typical periods in the range of 5-11 minutes and wavelengths in the plane of the sky (POS) of about 2000 km, while the flows in narrow threads have a typical speed in the POS of ∼16-46 km s-1. We also detect apparent kink oscillations in the threads with flowing material, and apply coronal seismology to estimate the magnetic field strength in the range of 5-17 G. Using 2.5D MHD we model the combined effects of nonlinear waves and flows on the observed dynamics of the prominence material, and reproduce the propagating and refracting fast magnetosonic waves, as well as standing kink-mode waves in flowing material along the magnetic field. The modeling results are in good qualitative agreement with the observations of the various waves and flows in the prominence foot, further confirming coronal seismology analysis and improving the understanding of the fine-scale dynamics of the prominence material.

Keywords: Alfven waves, Solar prominences, Magnetohydrodynamical simulations
Wave Pressure and Energy Cascade Rate of Kink Waves Computed with Elsässer Variables. Numerical simulations have revealed a new type of turbulence of unidirectional waves in a plasma that is perpendicularly structured, named uniturbulence. For this new type of turbulence, the transverse structuring modifies the upward propagating wave to have both Elsässer variables, leading to the well-known perpendicular cascade. In this paper, we study an analytical description of the nonlinear evolution of kink waves in a cylindrical flux tube that are prone to uniturbulence. We show that they lead to a nonlinear cascade for both propagating and standing waves. We calculate explicit expressions for the wave pressure and energy cascade rate. The computed damping rate $\tau /P$ depends on the density contrast of the flux tube and the background plasma and is inversely proportional to the amplitude of the kink wave. The dependence on the density contrast shows that it plays a role especially in the lower solar corona. These expressions may be added in Alfvén wave driven models of the solar atmosphere (such as the Alfvén Wave Solar Model (AWSOM)), modifying it to UAWSOM (Uniturbulence and the Alfvén Wave Solar Model).

Keywords: Interplanetary turbulence, Solar coronal heating, Solar coronal waves, Solar coronal holes, Solar corona, Active solar corona