Sazuna/UAT_keywords huggingface dataset:
Measurement of the Relativistic Sunyaev-Zeldovich Correction in RX J1347.5-1145. We present a measurement of the relativistic corrections to the thermal Sunyaev-Zel'dovich (SZ) effect spectrum, the rSZ effect, toward the massive galaxy cluster RX J1347.5-1145 by combining submillimeter images from Herschel-SPIRE with millimeter wavelength Bolocam maps. Our analysis simultaneously models the SZ effect signal, the population of cosmic infrared background galaxies, and the galactic cirrus dust emission in a manner that fully accounts for their spatial and frequency-dependent correlations. Gravitational lensing of background galaxies by RX J1347.5-1145 is included in our methodology based on a mass model derived from the Hubble Space Telescope observations. Utilizing a set of realistic mock observations, we employ a forward modeling approach that accounts for the non-Gaussian covariances between the observed astrophysical components to determine the posterior distribution of SZ effect brightness values consistent with the observed data. We determine a maximum a posteriori (MAP) value of the average Comptonization parameter of the intracluster medium (ICM) within R 2500 to be &lt;y&gt;2500 = 1.56 × 10-4, with corresponding 68% credible interval [1.42, 1.63] × 10-4, and a MAP ICM electron temperature of &lt;T sz&gt;2500 = 22.4 keV with 68% credible interval spanning [10.4, 33.0] keV. This is in good agreement with the pressure-weighted temperature obtained from Chandra X-ray observations, &lt;T x,pw&gt;2500 = 17.4 ± 2.3 keV. We aim to apply this methodology to comparable existing data for a sample of 39 galaxy clusters, with an estimated uncertainty on the ensemble mean &lt;T sz&gt;2500 at the ≃ 1 keV level, sufficiently precise to probe ICM physics and to inform X-ray temperature calibration.

Keywords: Galaxy clusters, Radio astronomy, Intracluster medium, Sunyaev-Zeldovich effect
Statistics of Water-group Band Ion Cyclotron Waves in Saturn's Inner Magnetosphere Based on 13 yr of Cassini Measurements. Based on Cassini observations from 2004 to 2016, we perform a comprehensive analysis of the statistical distribution of the occurrence rate, averaged amplitude, wave normal angle (WNA), ellipticity, and power spectral intensity of ion cyclotron waves in Saturn's inner magnetosphere. Our results show that ion cyclotron waves mainly occur between the orbits of Enceladus and Dione near the equatorial region (∣λ∣ &lt; 20°), with higher occurrence rates in the northern hemisphere than the southern hemisphere. The averaged wave amplitudes vary between 0.1 and 2 nT with a strong day-night asymmetry and a pronounced minimum at the equator. Saturnian ion cyclotron waves are predominantly left-handed polarized with small WNAs near the equator and become linearly polarized with larger WNAs at higher latitudes. The major wave power occurs frequently at frequencies of 0.5-1.2 ${f}_{{w}^{+}}$ , where ${f}_{{w}^{+}}$ is the equatorial gyrofrequency of H2O+ ions, with the strongest intensity (&gt;~10 nT2 Hz-1) at L ~ 6.5 statistically present in the midnight sector.

Keywords: Planetary magnetospheres, Saturn, Planetary science
The Wind Temperature and Mass-loss Rate of Arcturus (K1.5 III). In this paper we aim to constrain the wind temperature, outflow and turbulent velocities, ionization state, and mass-loss rate of the single red giant Arcturus (α Boo K1.5 III) using high spectral resolution Hubble Space Telescope Space Telescope Imaging Spectrograph profiles of Si III 1206.5 Å , O I 1304 Å and 1306 Å, C II 1334 Å and 1335 Å, and Mg II h 2802 Å. The use of the E140-H setting for α Boo allows the Si III 1206.5 Å line to be cleanly extracted from the echelle format for the first time. The ratios of the wind optical depths of lines from different species constrain the temperature at the base of the wind to T wind ~ 15,400 K. The mass-loss rate derived is 2.5 × 10-11 $\,{{M}_{\odot }\,{\rm{yr}}}^{-1}$ for Epoch 2018-2019, smaller than previous semiempirical estimates. These results can be reconciled with multiwavelength Very Large Array radio continuum fluxes for Epoch 2011-2012 by increasing the temperature to T wind ~ 18,000 K, or increasing the mass-loss rate to 4.0 × 10-11 $\,{{M}_{\odot }\,{\rm{yr}}}^{-1}$ . Interpreting the wind acceleration and turbulence in terms of a steady WKB Alfvén wave-driven wind reveals that the wave energy damping length increases with increasing radius, opposite to the trend expected for ion-neutral damping of monochromatic waves, confirming a previous result by Kuin and Ahmad derived for ζ Aur binaries. This implies that a spectrum of waves is required in this framework with wave periods in the range of hours to days, consistent with the photospheric granulation timescale. Constraints on a radial magnetic field (B) at 1.2 R * are an upper limit of B ≤ 2 G from the implied wave heating, and B ≥ 0.3 G to avoid excessive wave amplitudes.

Keywords: Hubble Space Telescope, Stellar mass loss, Stellar winds, Alfven waves, Stellar spectral lines
The Circumstellar Environments of Double-peaked, Calcium-strong Transients 2021gno and 2021inl. We present panchromatic observations and modeling of calcium-strong supernovae (SNe) 2021gno in the star-forming host-galaxy NGC 4165 and 2021inl in the outskirts of elliptical galaxy NGC 4923, both monitored through the Young Supernova Experiment transient survey. The light curves of both, SNe show two peaks, the former peak being derived from shock cooling emission (SCE) and/or shock interaction with circumstellar material (CSM). The primary peak in SN 2021gno is coincident with luminous, rapidly decaying X-ray emission (L  x  = 5 × 1041 erg s-1) detected by Swift-XRT at δ t = 1 day after explosion, this observation being the second-ever detection of X-rays from a calcium-strong transient. We interpret the X-ray emission in the context of shock interaction with CSM that extends to r &lt; 3 × 1014 cm. Based on X-ray modeling, we calculate a CSM mass M CSM = (0.3-1.6) × 10-3 M ⊙ and density n = (1-4) × 1010 cm-3. Radio nondetections indicate a low-density environment at larger radii (r &gt; 1016 cm) and mass-loss rate of $\dot{M}\lt {10}^{-4}$ M ⊙ yr-1. SCE modeling of both primary light-curve peaks indicates an extended-progenitor envelope mass M  e  = 0.02-0.05 M ⊙ and radius R  e  = 30-230 R ⊙. The explosion properties suggest progenitor systems containing either a low-mass massive star or a white dwarf (WD), the former being unlikely given the lack of local star formation. Furthermore, the environments of both SNe are consistent with low-mass hybrid He/C/O WD + C/O WD mergers.

Keywords: White dwarf stars, X-ray transient sources, Supernovae, X-ray telescopes
Magnetic Field Observations in the Very Local Interstellar Medium by Voyagers 1 and 2. Observations of the magnetic field B in the very local interstellar medium (VLISM) were made by Voyager 1 (V1) in the northern hemisphere from 2012 to mid-2021 and by Voyager 2 (V2) in the southern hemisphere from 2018 through 2020. Near 2019.4, V2 observed an abrupt increase in B associated with a pressure front near the heliopause. During 2020, V2 observed an abrupt increase in B at a jump in B that was preceded by electron plasma oscillations and cosmic rays, indicating that it was a shock. The shock was followed by a decrease in B ending ~50 days later. V2 observed large-scale waves in all three components of B , before and after the shock. The largest- and intermediate-amplitude waves were in the BN and BR component, respectively, indicating that the waves were predominantly transverse several au from the heliopause. It was shown previously that waves near the heliopause were predominantly longitudinal at V1 and V2. Thus, V2 observed a mode transformation process within 10 au of the heliopause in the southern hemisphere, like that observed by V1 in the northern hemisphere. The elevation and azimuthal angles observed by V1 and V2 varied linearly with increasing distance in the VLISM. Voyager 1 observed jumps in B at two shocks and a pressure front, each followed by a decrease in B in a ramp. V1 also observed a fourth jump in B, at 2020.4, but B continued to increase until at least year 2021.5. This long-lasting increase in B was not anticipated.

Keywords: Interstellar magnetic fields
Primordial Helium-3 Redux: The Helium Isotope Ratio of the Orion Nebula. We report the first direct measurement of the helium isotope ratio, 3He/4He, outside of the Local Interstellar Cloud, as part of science-verification observations with the upgraded CRyogenic InfraRed Echelle Spectrograph. Our determination of 3He/4He is based on metastable He I* absorption along the line of sight toward Θ2A Ori in the Orion Nebula. We measure a value 3He/4He = (1.77 ± 0.13) × 10-4, which is just ~40% above the primordial relative abundance of these isotopes, assuming the Standard Model of particle physics and cosmology, (3He/4He)p = (1.257 ± 0.017) × 10-4. We calculate a suite of galactic chemical evolution simulations to study the Galactic build up of these isotopes, using the yields from Limongi &amp; Chieffi for stars in the mass range M = 8-100 M ☉ and Lagarde et al. for M = 0.8-8 M ☉. We find that these simulations simultaneously reproduce the Orion and protosolar 3He/4He values if the calculations are initialized with a primordial ratio ${\left({}^{3}\mathrm{He}{/}^{4}\mathrm{He}\right)}_{{\rm{p}}}=(1.043\pm 0.089)\times {10}^{-4}$ . Even though the quoted error does not include the model uncertainty, this determination agrees with the Standard Model value to within ~2σ. We also use the present-day Galactic abundance of deuterium (D/H), helium (He/H), and 3He/4He to infer an empirical limit on the primordial 3He abundance, ${\left({}^{3}\mathrm{He}/{\rm{H}}\right)}_{{\rm{p}}}\leqslant (1.09\pm 0.18)\times {10}^{-5}$ , which also agrees with the Standard Model value. We point out that it is becoming increasingly difficult to explain the discrepant primordial 7Li/H abundance with nonstandard physics, without breaking the remarkable simultaneous agreement of three primordial element ratios (D/H, 4He/H, and 3He/4He) with the Standard Model values. *Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program(s) 107.22U1.001, 194.C-0833.

Keywords: Cosmology, Cosmochemistry, Galaxy chemical evolution, Quasar absorption line spectroscopy, Interstellar line absorption, Astronomy data analysis, Astrochemistry, Astronomical techniques, Interstellar absorption, Interstellar medium, Spectroscopy, Big Bang nucleosynthesis
The Criterion for Chaos in Three-planet Systems. We establish the criterion for chaos in three-planet systems, for systems similar to those discovered by the Kepler spacecraft. Our main results are as follows: (i) The simplest criterion, which is based on overlapping mean motion resonances (MMRs), only agrees with numerical simulations at a very crude level. (ii) Much greater accuracy is attained by considering neighboring MMRs that do not overlap. We work out the widths of the chaotic zones around each of the neighbors, and also provide simple approximate expressions for the widths. (iii) Even greater accuracy is provided by the overlap of three-body resonances (3BRs), which accounts for the fine-grained structure seen in maps from N-body simulations, and also predicts Lyapunov times. From previous studies, it is unclear whether interplanetary chaos should be attributed to the overlap of MMRs or of 3BRs. We show that the two apparently contradictory viewpoints are in fact consistent: both predict the same criterion for chaos. (iv) We compare the predicted criterion with high-resolution maps of chaos from N-body simulations, and show that they agree at a high level of detail.

Keywords: Exoplanet dynamics, Celestial mechanics, Orbits, Orbital resonances
The Temporal and Spatial Behaviors of CME Occurrence Rate at Different Latitudes. The statistical study of the coronal mass ejections (CMEs) is a hot topic in solar physics. To further reveal the temporal and spatial behaviors of the CMEs at different latitudes and heights, we analyzed the correlation and phase relationships between the occurrence rate of CMEs, the coronal brightness index (CBI), and the 10.7 cm solar radio flux (F10.7). We found that the occurrence rate of the CMEs correlates with the CBI relatively stronger at high latitudes (≥60°) than at low latitudes (≤50°). At low latitudes, the occurrence rate of the CMEs correlates relatively weaker with the CBI than the F10.7. There is a relatively stronger correlation relationship between CMEs, the F10.7, and the CBI during Solar Cycle 24 (SC24) than Solar Cycle 23 (SC23). During SC23, the high-latitude CME occurrence rate lags behind the F10.7 by 3 months, and during SC24, the low-latitude CME occurrence rate leads the low-latitude CBI by 1 month. The correlation coefficient values turn out to be larger when the very faint CMEs are removed from the samples of the CDAW catalog. Based on our results, we may speculate that the source regions of the high/low-latitude CMEs may vary in height, and the process of magnetic energy accumulation and dissipation is from the lower to the upper atmosphere of the Sun. The temporal offsets between different indicators could help us better understand the physical processes responsible for the solar-terrestrial interactions.

Keywords: Solar activity, Magnetic fields, Solar coronal mass ejections
Deriving Thermonuclear Supernova Properties from Gamma-Ray Line Measurements. We illustrate methods for deriving properties of thermonuclear, or Type Ia, supernovae, including synthesized 56Ni mass, total ejecta mass, ejecta kinetic energy, and 56Ni distribution in velocity, from gamma-ray line observations. We simulate data from a small number of published SNe Ia models for a simple gamma-ray instrument, and measure their underlying properties from straightforward analyses. Assuming spherical symmetry and homologous expansion, we calculate exact line profiles for all 56Co and 56Ni lines at all times, requiring only the variation of mass density and 56Ni mass fraction with expansion velocity as input. By parameterizing these quantities, we iterate the parameters to fit the simulated data. We fit the full profiles of multiple lines, or we integrate over the lines and fit line fluxes only versus time. Line profile fits are more robust, but in either case, we can recover accurately the values of the aforementioned properties of the models simulated, given sufficient signal to noise in the lines. A future gamma-ray mission with line sensitivity approaching 10-6 photons cm-2 s-1 would measure these properties for many SNe Ia, and with unprecedented precision and accuracy for a few per year. Our analyses applied to the reported 56Co lines from SN 2014J favor a low 56Ni mass and low ejecta mass, relative to other estimates.

Keywords: Type Ia supernovae, Gamma-ray lines
Circumnuclear Medium around the Central AGN in a Cool-core Cluster, Abell 1644-South. We present the circumnuclear multiphase gas properties of the brightest cluster galaxy (BCG) in the center of Abell 1644-South (A1644-S). A1644-S is the main cluster in a merging system, which is well known for X-ray hot gas sloshing in its core. The sharply peaked X-ray profile of A1644-S implies the presence of a strongly cooling gas core. In this study, we analyze ALMA 12CO (1-0) data, JVLA H I data, and KaVA 22 GHz data for the central region of A1644-S to probe the potential origin of the cool gas and its role in (re)powering the central active galactic nucleus (AGN). We find CO clumps distributed in an arc shape along the X-ray gas sloshing, which is suggestive of a connection between the cold gas and the hot intracluster medium (ICM). H I and CN are detected in absorption against the AGN continuum emission. The absorption dip is observed at the systemic velocity of the BCG with an extended, redshifted tail. Based on the spatial and spectral configurations of the H I, CN, and CO gases, it is inferred that cool gas spirals into the core of the BCG, which is then fed to the central AGN. Indeed, our KaVA observation reveals a parsec-scale bipolar jet, implying that this AGN could have been (re)powered quite recently. Combining this, we suggest that some cold gas in A1644-S could have been formed from the cooling of the ICM, triggering the activity of the central AGN in the early development of a cool-core cluster.

Keywords: Molecular gas, Cooling flows, Radio jets, Interstellar atomic gas, Brightest cluster galaxies
Turbulent Cosmic Ray-Mediated Shocks in the Hot Ionized Interstellar Medium. The structure of shocks and turbulence are strongly modified during the acceleration of cosmic rays (CRs) at a shock wave. The pressure and the collisionless viscous stress decelerate the incoming thermal gas and thus modify the shock structure. A CR streaming instability ahead of the shock generates the turbulence on which CRs scatter. The turbulent magnetic field in turn determines the CR diffusion coefficient and further affects the CR energy spectrum and pressure distribution. The dissipation of turbulence contributes to heating the thermal gas. Within a multicomponent fluid framework, CRs and thermal gas are treated as fluids and are closely coupled to the turbulence. The system equations comprise the gas dynamic equations, the CR pressure evolution equation, and the turbulence transport equations, and we adopt typical parameters for the hot ionized interstellar medium. It is shown that the shock has no discontinuity but possesses a narrow but smooth transition. The self-generated turbulent magnetic field is much stronger than both the large-scale magnetic field and the preexisting turbulent magnetic field. The resulting CR diffusion coefficient is substantially suppressed and is more than three orders smaller near the shock than it is far upstream. The results are qualitatively consistent with certain observations.

Keywords: Shocks, Cosmic rays
Insight-HXMT Study of the Inner Accretion Disk in the Black Hole Candidate EXO 1846-031. We study the spectral evolution of the black hole candidate EXO 1846-031 during its 2019 outburst, in the 1-150 keV band, with the Hard X-ray Modulation Telescope. The continuum spectrum is well modeled with an absorbed disk-blackbody plus cutoff power law, in the hard, intermediate, and soft states. In addition, we detect an ≈6.6 keV Fe emission line in the hard intermediate state. Throughout the soft intermediate and soft states, the fitted inner disk radius remains almost constant; we suggest that it has settled at the innermost stable circular orbit (ISCO). However, in the hard and hard intermediate states, the apparent inner radius was unphysically small (smaller than the ISCO), even after accounting for the Compton scattering of some of the disk photons by the corona in the fit. We argue that this is the result of a high hardening factor, f col ≈ 2.0-2.7, in the early phases of the outburst evolution, well above the canonical value of 1.7 suitable for a steady disk. We suggest that the inner disk radius was already close to the ISCO in the low/hard state. Furthermore, we propose that this high value of the hardening factor in the relatively hard state was probably caused by the additional illuminating of the coronal irradiation onto the disk. Additionally, we estimate the spin parameter using the continuum-fitting method, over a range of plausible black hole masses and distances. We compare our results with the spin measured using the reflection-fitting method and find that the inconsistency of the two results is partly caused by different choices of f col.

Keywords: Accretion, Black hole physics, High energy astrophysics
Heating or Cooling: Study of Advective Heat Transport in the Inflow and the Outflow of Optically Thin Advection-dominated Accretion Flows. Advection is believed to be the dominant cooling mechanism in optically thin advection-dominated accretion flows (ADAFs). When outflow is considered, however, the first impression is that advection should be of opposite sign in the inflow and the outflow, due to the opposite direction of radial motion. Then how is the energy balance achieved simultaneously? We investigate the problem in this paper, analyzing the profiles of different components of advection with self-similar solutions of ADAFs in spherical coordinates (r θ ϕ). We find that for n &lt; 3γ/2 - 1, where n is the density index in ρ ∝ r -n  and γ is the heat capacity ratio, the radial advection is a heating mechanism in the inflow and a cooling mechanism in the outflow. It becomes 0 for n = 3γ/2 - 1, and turns to a cooling mechanism in the inflow and a heating mechanism in the outflow for n &gt; 3γ/2 - 1. The energy conservation is only achieved when the latitudinal (θ direction) advection is considered, which takes an appropriate value to maintain energy balance, so that the overall effect of advection, no matter the parameter choices, is always a cooling mechanism that cancels out the viscous heating everywhere. For the extreme case of n = 3/2, latitudinal motion stops, viscous heating is balanced solely by radial advection, and no outflow is developed.

Keywords: Accretion, High energy astrophysics, Hydrodynamics
Radial Trapping of Thermal Rossby Waves within the Convection Zones of Low-mass Stars. We explore how thermal Rossby waves propagate within the gravitationally stratified atmosphere of a low-mass star with an outer convective envelope. Under the conditions of slow, rotationally constrained dynamics, we derive a local dispersion relation for atmospheric waves in a fully compressible stratified fluid. This dispersion relation describes the zonal and radial propagation of acoustic waves and gravito-inertial waves. Thermal Rossby waves are just one class of prograde-propagating gravito-inertial wave that manifests when the buoyancy frequency is small compared to the rotation rate of the star. From this dispersion relation, we identify the radii at which waves naturally reflect and demonstrate how thermal Rossby waves can be trapped radially in a waveguide that permits free propagation in the longitudinal direction. We explore this trapping further by presenting analytic solutions for thermal Rossby waves within an isentropically stratified atmosphere that models a zone of efficient convective heat transport. We find that, within such an atmosphere, waves of short zonal wavelength have a wave cavity that is radially thin and confined within the outer reaches of the convection zone near the star's equator. The same behavior is evinced by the thermal Rossby waves that appear at convective onset in numerical simulations of convection within rotating spheres. Finally, we suggest that stable thermal Rossby waves could exist in the lower portion of the Sun's convection zone, despite that region's unstable stratification. For long wavelengths, the Sun's rotation rate is sufficiently rapid to stabilize convective motions, and the resulting overstable convective modes are identical to thermal Rossby waves.

Keywords: Stellar convective zones, Solar rotation, Internal waves, Hydrodynamics, Helioseismology, Solar convective zone, Solar oscillations, Stellar oscillations, Stellar rotation, Asteroseismology, Polytropes