adsabs/SciX_UAT_keywords huggingface dataset:
The Resolved Sunyaev-Zel'dovich Profiles of Nearby Galaxy Groups

Many of the baryons in galaxy groups are thought to have been driven out to large distances (≳R500) by feedback, but there are few constraining observations of this extended gas. This work presents the resolved Sunyaev-Zel'dovich (SZ) profiles for a stacked sample of 10 nearby galaxy groups within the mass range ${\mathrm{log}}_{10}({M}_{500}[{M}_{\odot }])=13.6\mbox{--}13.9$ . We measured the SZ profiles using the publicly available y-map from the Planck Collaboration as well as our own y-maps constructed from more recent versions of Planck data. The y-map extracted from the latest data release yielded a significant SZ detection out to 3 R500. In addition, the stacked profile from these data was consistent with simulations that included AGN feedback. Our best-fit model using the latest Planck data suggested a baryon fraction ≈5.6% within R500. This is significantly lower than the cosmic value of ≈16%, supporting the idea that baryons have been driven to large radii by AGN feedback. Lastly, we discovered a significant (~3σ) "bump" feature near ~2 R500 that is most likely the signature of internal accretion shocks.

Keywords: galaxy groups; sunyaev-zeldovich effect; intracluster medium; active galactic nuclei
Visual Orbits and Alignments of Planet-hosting Binary Systems

Roughly half of Solar-type planet hosts have stellar companions, so understanding how these binary companions affect the formation and evolution of planets is an important component to understanding planetary systems overall. Measuring the dynamical properties of planet host binaries enables a valuable test of planet formation in multistar systems and requires knowledge of the binary orbital parameters. Using high-resolution imaging, we have measured the relative astrometry and visual orbits of 13 binary systems where one of the stars is known to host a transiting exoplanet. Our results indicate that the mutual inclination between the orbits of the binary hosts and the transiting planets are well aligned. Our results for close binary systems (a < 100 au) complement past work for wide planet host binaries from Gaia.

Keywords: binary stars; exoplanet systems; planet hosting stars; astrometric binary stars
Orbits of the Irregular Satellites of Uranus and Neptune

We report on an ephemerides update for the irregular satellites of Uranus and Neptune, including Nereid. Our data set contains ground-based and Voyager 2 position measurements of the satellites. Some of the new observations were reduced with respect to the GAIA star catalog and represent high-quality, modern astrometry. The orbital fits are based on the numerically integrated equations of motion. We summarized results in terms of state vectors, orbital uncertainties, and mean elements. A large number of the irregulars have not been followed up in over a decade, and our study shows that their orbits still contain significant uncertainties.

Keywords: irregular satellites; orbit determination; uranian satellites; neptunian satellites
The Intrinsic Statistical Properties and Correlations of Short Gamma-Ray Bursts

The intrinsic statistical properties and correlations of short gamma-ray bursts (SGRBs) have not been fully determined, due to the limitations of observations. In this paper, we compile a more extensive sample of 82 SGRBs with measured redshifts and present a comprehensive study of their intrinsic characteristics. We obtain the median values of the intrinsic duration (T 90,z), peak energy (E p,z), isotropic energy (E iso), and peak luminosity (L iso) as 0.47 s, 466 keV, 8.21 ×1050 erg, and 3.22 × 1051 erg s-1, respectively. We update the spectrum-energy correlations, and report ${E}_{{\rm{p}},{\rm{z}}}\propto {E}_{\mathrm{iso}}^{0.36\pm 0.05}$ and ${E}_{{\rm{p}},{\rm{z}}}\propto {L}_{\mathrm{iso}}^{0.33\pm 0.04}$ , which further confirm the previous results that the E p,z-E iso correlations of SGRBs and long gamma-ray bursts (LGRBs) are different and that this correlation can be used to distinguish GRB types. We report for the first time that there is a tighter correlation between the isotropic energy of the prompt emission of SGRBs and the star formation rate of their host galaxies, which reads $\mathrm{sSFR}\propto {E}_{\mathrm{iso}}^{0.38\pm 0.11}$ . Using the measured jet break time (t jet) of 11 SGRBs, we tentatively investigate the E iso-E p,z-t jet,z and L iso-E p,z-t jet,z correlations of SGRBs and find that three-parameter correlations of SGRBs also exist and are different from those of LGRBs. Based on the E iso-E p,z-t jet,z correlation, we estimate the t jet,z values of other SGRBs and calculate the opening angles of SGRBs. We find that the median value of the SGRB opening angle is 7.°5, which is larger than that of LGRBs.

Keywords: gamma-ray bursts
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 <y>2500 = 1.56 × 10-4, with corresponding 68% credible interval [1.42, 1.63] × 10-4, and a MAP ICM electron temperature of <T sz>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, <T x,pw>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 <T sz>2500 at the ≃ 1 keV level, sufficiently precise to probe ICM physics and to inform X-ray temperature calibration.

Keywords: galaxy clusters; sunyaev-zeldovich effect; radio astronomy; intracluster medium
Probing the Shock Breakout Signal of SN 2024ggi from the Transformation of Early Flash Spectroscopy

We present early-time, hour-to-day cadence spectroscopy of the nearby Type II supernova (SN II) 2024ggi, which was discovered at a phase when the SN shock had just emerged from the red supergiant (RSG) progenitor star. Over the first few days after the first light, SN 2024ggi exhibited prominent narrow emission lines formed through intense and persistent photoionization of the nearby circumstellar material (CSM). In the first 63 hr, spectral lines of He, C, N, and O revealed a rapid rise in ionization as a result of the progressive sweeping up of the CSM by the shock. The duration of the IIn-like spectra indicates a dense and relatively confined CSM distribution extending up to ∼4 × 1014 cm. Spectral modeling reveals that a CSM mass-loss rate at this region exceeding 5 × 10‑3 M ⊙ yr‑1 is required to reproduce low-ionization emissions, which dramatically exceeds that of an RSG. Analyzing the Hα emission shift implies the velocity of the unshocked outer CSM to be between 20 and 40 km s‑1, matching the typical wind velocity of an RSG. The differences between the inner and outer layers of the CSM and an RSG progenitor highlight a complex mass-loss history before the explosion of SN 2024ggi.

Keywords: type ii supernovae; supernovae; core-collapse supernovae
Shock Properties and Associated Characteristics of Solar Energetic Particles in the 2017 September 10 Ground-level Enhancement Event

The solar eruption on 2017 September 10 was accompanied by a fast coronal mass ejection (~3000 km s-1) and produced a ground-level enhancement (GLE) event at Earth. Multiple-viewpoint remote sensing observations are used to find the three-dimensional (3D) structure of the shock. We determine the shock parameters by combining the 3D shock kinematics and the solar wind properties obtained from a global magnetohydrodynamic (MHD) simulation, in order to compare them with the characteristics of the solar energetic particles (SEPs). We extract the magnetic connectivities of the observers from the MHD simulation and find that L1 was magnetically connected to the shock flank (rather than the nose). Further analysis shows that this shock flank propagates through the heliospheric current sheet (HCS). The weak magnetic field and relatively dense plasma around the HCS result in a large Mach number of the shock, which leads to efficient particle acceleration even at the shock flank. We conclude that the interaction between the shock and HCS provides a potential mechanism for production of the GLE event. The comparison between the shock properties and the characteristics of SEPs suggests an efficient particle acceleration in a wide spatial range by the shock propagating through the highly inhomogeneous coronal medium.

Keywords: solar flares; solar coronal mass ejection shocks; solar energetic particles
The Yarkovsky Effect on the Long-term Evolution of Binary Asteroids

We explore the Yarkovsky effect on small binary asteroids. While significant attention has been given to the binary YORP effect, the Yarkovsky effect is often overlooked. We develop an analytical model for the binary Yarkovsky effect, considering both the Yarkovsky–Schach and planetary Yarkovsky components, and verify it against thermophysical numerical simulations. We find that the Yarkovsky force could change the mutual orbit when the asteroid's spin period is unequal to the orbital period. Our analysis predicts new evolutionary paths for binaries. For a prograde asynchronous secondary, the Yarkovsky force will migrate the satellite toward the location of the synchronous orbit on ∼100 kyr timescales, which could be faster than other synchronization processes such as YORP and tides. For retrograde secondaries, the Yarkovsky force always migrates the secondary outward, which could produce asteroid pairs with opposite spin poles. Satellites spinning faster than the Roche limit orbit period (e.g., from ∼4 hr to ∼10 hr) will migrate inward until they disrupt, reshape, or form a contact binary. We also predict a short-lived equilibrium state for asynchronous secondaries where the Yarkovsky force is balanced by tides. We provide calculations of the Yarkovsky-induced drift rate for known asynchronous binaries. If the NASA DART impact broke Dimorphos from synchronous rotation, we predict that Dimorphos's orbit will shrink by cm yr‑1, which can be measured by the Hera mission. We also speculate that the Yarkovsky force may have synchronized the Dinkinesh–Selam system after a possible merger of Selam's two lobes.

Keywords: asteroids; planetary rings; solar system
Inferences from Surface Brightness Fluctuations of Zwicky 3146 via the Sunyaev-Zel'dovich Effect and X-Ray Observations

The galaxy cluster Zwicky 3146 is a sloshing cool-core cluster at z = 0.291 that in Sunyaev-Zel'dovich (SZ) imaging does not appear to exhibit significant pressure substructure in the intracluster medium. We perform a surface brightness fluctuation analysis via Fourier amplitude spectra on SZ (MUSTANG-2) and X-ray (XMM-Newton) images of this cluster. These surface brightness fluctuations can be deprojected to infer pressure and density fluctuations from the SZ and X-ray data, respectively. In the central region (Ring 1, r < 100″ = 440 kpc, in our analysis), we find fluctuation spectra that suggest injection scales around 200 kpc (~140 kpc from pressure fluctuations and ~250 kpc from density fluctuations). When comparing the pressure and density fluctuations in the central region, we observe a change in the effective thermodynamic state from large to small scales, from isobaric (likely due to the slow sloshing) to adiabatic (due to more vigorous motions). By leveraging scalings from hydrodynamical simulations, we find an average 3D Mach number ≈0.5. We further compare our results to other studies of Zwicky 3146 and, more broadly, to other studies of fluctuations in other clusters.

Keywords: galaxy clusters; intracluster medium
Precise Dynamical Masses and Orbital Fits for β Pic b and β Pic c

We present a comprehensive orbital analysis to the exoplanets β Pictoris b and c that resolves previously reported tensions between the dynamical and evolutionary mass constraints on β Pic b. We use the Markov Chain Monte Carlo orbit code orvara to fit 15 years of radial velocities and relative astrometry (including recent GRAVITY measurements), absolute astrometry from Hipparcos and Gaia, and a single relative radial velocity measurement between β Pic A and b. We measure model-independent masses of ${9.3}_{-2.5}^{+2.6}$ <!-- --> MJup for β Pic b and 8.3 ± 1.0 MJup for β Pic c. These masses are robust to modest changes to the input data selection. We find a well-constrained eccentricity of 0.119 ± 0.008 for β Pic b, and an eccentricity of ${0.21}_{-0.09}^{+0.16}$ <!-- --> for β Pic c, with the two orbital planes aligned to within ∼0°5. Both planets' masses are within ∼1σ of the predictions of hot-start evolutionary models and exclude cold starts. We validate our approach on N-body synthetic data integrated using REBOUND. We show that orvara can account for three-body effects in the β Pic system down to a level ∼5 times smaller than the GRAVITY uncertainties. Systematics in the masses and orbital parameters from orvara's approximate treatment of multiplanet orbits are a factor of ∼5 smaller than the uncertainties we derive here. Future GRAVITY observations will improve the constraints on β Pic c's mass and (especially) eccentricity, but improved constraints on the mass of β Pic b will likely require years of additional radial velocity monitoring and improved precision from future Gaia data releases.

Keywords: exoplanet astronomy; exoplanet dynamics; exoplanet systems; exoplanet formation; radial velocity; pulsating variable stars; brown dwarfs; exoplanet evolution
Temporal and Latitudinal Variations in Ca-K Plage and Network Area: An Implication for Meridional Flows

The Ca-K spectroheliograms obtained at the Kodaikanal observatory are used to generate a uniform time series using the equal-contrast technique for studying the long- and short-term variations in the solar chromosphere. The percentages of plage, enhanced network, and active and quiet network areas at various latitudes is compared with the activity at 35° latitude and also with the sunspot number for the period of 1907-1984. The values of the phase differences indicate that the activity begins at ~45° latitude and shifts progressively to a lower latitude at a speed of ~9.4 m s-1 . The shift speed slows down gradually and reaches ~3 m s-1 at ~5° latitude. No phase difference between the variations of Ca-K activity at 55°, 65°, and 75° latitude belts implies that changes in the activity are happening simultaneously. The analysis shows that the activity at polar latitude belts is anticorrelated with the sunspot number. This study indicates that a multicell meridional flow pattern could exist in the latitude direction. One type of cell could transport the magnetic elements from mid- to low-latitude belts through meridional flows, and the other cell type could be operating in the polar region.

Keywords: solar cycle; plages; solar activity
New Light on Dark Extended Lenses with the Roman Space Telescope

The Roman Space Telescope's Galactic Bulge Time Domain Survey will constitute the most sensitive microlensing survey of the Galactic bulge to date, opening up new opportunities to search for dark matter (DM). Many extensions of the Standard Model predict the formation of extended DM substructures, such as DM subhalos, boson/axion stars, and halo-dressed primordial black holes. We demonstrate that for such targets, Roman will be sensitive to a broad parameter space up to 4 orders of magnitude below existing constraints. Our analysis can be readily applied to other extended DM configurations as well.

Keywords: dark matter; gravitational microlensing
The PFS View of TOI-677 b: A Spin–Orbit Aligned Warm Jupiter in a Dynamically Hot System

TOI-677 b is part of an emerging class of "tidally detached" gas giants (a/R ⋆ ≳ 11) that exhibit large orbital eccentricities and yet low stellar obliquities. Such sources pose a challenge for models of giant planet formation, which must account for the excitation of high eccentricities without large changes in the orbital inclination. In this work, we present a new Rossiter–McLaughlin measurement of the tidally detached warm Jupiter TOI-677 b, obtained using high-precision radial velocity observations with Magellan's Planet Finder Spectrograph (PFS). Combined with previously published observations from the Very Large Telescope's ESPRESSO spectrograph, we derive one of the most precisely constrained sky-projected spin–orbit angle measurements to date for an exoplanet. The combined fit offers a refined set of self-consistent parameters, including a low sky-projected stellar obliquity of $\lambda ={3\buildrel{\circ}\over{.} 2}_{-{1.}^{\circ }5}^{+{1.}^{\circ }6}$ and a moderately high eccentricity of $e={0.460}_{-0.018}^{+0.019}$ , which further constrain the puzzling architecture of this system. We examine several potential scenarios that may have produced the current TOI-677 orbital configuration, ultimately concluding that TOI-677 b most likely had its eccentricity excited through disk–planet interactions. This system adds to a growing population of aligned warm Jupiters on eccentric orbits around hot (T eff > 6100 K) stars. *This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.

Keywords: planetary theory; exoplanet tides; exoplanet migration; planetary dynamics; exoplanets; hot jupiters; exoplanet systems; star-planet interactions; planetary alignment; exoplanet evolution; exoplanet astronomy; exoplanet dynamics
Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies

The star formation rate (SFR) in galactic disks depends on both the quantity of the available interstellar medium (ISM) gas and its physical state. Conversely, the ISM's physical state depends on the SFR, because the "feedback" energy and momentum injected by recently formed massive stars is crucial to offsetting losses from turbulent dissipation and radiative cooling. The ISM's physical state also responds to the gravitational field that confines it, with increased weight driving higher pressure. In a quasi-steady state, it is expected that the mean total pressure of different thermal phases will match each other, that the component pressures and total pressure will satisfy thermal and dynamical equilibrium requirements, and that the SFR will adjust as needed to provide the requisite stellar radiation and supernova feedback. The pressure-regulated, feedback-modulated (PRFM) theory of the star-forming ISM formalizes these ideas, leading to a prediction that the SFR per unit area, ΣSFR, will scale nearly linearly with ISM weight ${ \mathcal W }$ . In terms of the large-scale gas surface density Σgas, stellar plus dark matter density ρ sd, and effective ISM velocity dispersion σ eff, an observable weight estimator is ${ \mathcal W }\approx {P}_{\mathrm{DE}}=\pi G{{\rm{\Sigma }}}_{\mathrm{gas}}^{2}/2+{{\rm{\Sigma }}}_{\mathrm{gas}}{(2G{\rho }_{\mathrm{sd}})}^{1/2}{\sigma }_{\mathrm{eff}}$ , and this is predicted to match the total midplane pressure P tot. Using a suite of multiphase magnetohydrodynamic simulations run with the TIGRESS computational framework, we test the principles of the PRFM model and calibrate the total feedback yield ϒtot = P tot/ΣSFR ~ 1000 km s-1, as well as its components. We compare the results from TIGRESS to theory, previous numerical simulations, and observations, finding excellent agreement.

Keywords: interstellar medium; star formation; stellar feedback; magnetohydrodynamical simulations
A Statistical Analysis of Spiral-shaped Wave Patterns in Sunspot Umbrae

Spiral-shaped wave patterns (SWPs) observed in sunspot umbrae represent the superposition of axisymmetric patterns and nonaxisymmetric patterns of umbral oscillations. These patterns give us physical information about the source of oscillations below the surface. Here we present the statistics of their observational properties determined from the 304 Å line-intensity data obtained with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. From the 2013 to 2018 data set, we examined each of the 496 sunspots near the disk center for 2 hr. As a result, we identified 241 SWPs from 140 sunspots, which corresponds to the detection rate of 0.24 per hour in each sunspot. Most of the SWPs had one spiral arm, 48 SWPs had two arms, and only one had three. The oscillation period was estimated at 151 ± 27 s and the lifetime, at 770 ± 250 s, being comparable to those of conventional umbral oscillations. The rotation period of the SWPs was estimated at 190 ± 69 s for the one-armed SWPs and 299 ± 115 s for the two-armed SWPs. We found that the properties of the SWPs have no dependence on hemisphere, latitude, and sunspot size. From the apparent radial speeds of the SWPs and a simple model of wave propagation, we infer that the SWPs may be generated between 2 and 11 Mm below the photosphere with a mean value of about 6 Mm.

Keywords: solar chromosphere; sunspots; solar oscillations; magnetohydrodynamics
WISEA J052305.94-015356.1: A New EsdT Candidate

I present WISEA J052305.94-015356.1 as a new candidate extremely metal-poor T subdwarf (esdT), based on its distinctive infrared colors and high proper motion (~500 mas yr-1). Spectroscopic follow-up is now needed to confirm it is a member of this newly discovered class of substellar objects.

Keywords: brown dwarfs; t subdwarfs
A Model-based Technique for Ad Hoc Correction of Instrumental Polarization in Solar Spectropolarimetry

We present a new approach for correcting instrumental polarization by modeling the nondepolarizing effects of a complex series of optical elements to determine physically realizable Mueller matrices. Provided that the Mueller matrix of the optical system can be decomposed into a general elliptical diattenuator and general elliptical retarder, it is possible to model the crosstalk between both the polarized and unpolarized states of the Stokes vector and then use the acquired science observations to determine the best-fit free parameters. Here we implement a minimization for solar spectropolarimetric measurements containing photospheric spectral lines sensitive to the Zeeman effect using physical constraints provided by polarized line and continuum formation. This model-based approach is able to provide an accurate correction even in the presence of large amounts of polarization crosstalk and conserves the physically meaningful magnitude of the Stokes vector, a significant improvement over previous ad hoc techniques.

Keywords: solar physics; spectropolarimetry; calibration; solar magnetic fields