Sazuna/UAT_keywords huggingface dataset:
Nature versus Nurture: Investigating the Effects of Measurement Uncertainties in the Assessment of Potential Trends between Planetary and Stellar Properties. Correlations between planetary and stellar properties, particularly age, can provide insight on planetary formation and evolution processes. However, the underlying source of such trends can be unclear, and measurement uncertainties and small sample sizes can leave doubt as to whether an observed trend truly exists. We use a Bayesian framework to examine how uncertainties in measured parameters influence the odds ratios of competing hypotheses for the source of an observed trend. We analyze three reported trends from the literature. In each application, while uncertainties do affect the numerical value of the odds ratios, our conclusions remain the same whether or not uncertainties are taken into account: hot Jupiter eccentricities are circularized over time, obliquities of hot Jupiter hosts are driven by stellar temperature, and there is not enough evidence to favor a trend of 2:1 orbital resonances with age over a chance relation. Updated samples for the 2:1 resonance and obliquity cases do not change the original conclusions. Simulated 2:1 resonance data show that sample size may be more important than measurement precision for drawing a firm conclusion. However, if 2:1 resonances get disrupted on a wide range of timescales, an age trend will be inherently difficult to confirm over a chance relation, even with a large sample. For some applications, full incorporation of measurement uncertainties may be too computationally expensive, making it preferable to use the framework without uncertainties and perform additional tests to examine the effects of highly uncertain measurements.

Keywords: Exoplanet dynamics, Bayesian statistics, Exoplanet astronomy, Exoplanet formation, Hierarchical models
Retrieving the C and O Abundances of HR 7672 AB: A Solar-type Primary Star with a Benchmark Brown Dwarf. A benchmark brown dwarf (BD) is a BD whose properties (e.g., mass and chemical composition) are precisely and independently measured. Benchmark BDs are valuable in testing theoretical evolutionary tracks, spectral synthesis, and atmospheric retrievals for substellar objects. Here, we report results of atmospheric retrieval on a synthetic spectrum and a benchmark BD, HR 7672 B, with petitRADTRANS. First, we test the retrieval framework on a synthetic PHOENIX BT-Settl spectrum with a solar composition. We show that the retrieved C and O abundances are consistent with solar values, but the retrieved C/O is overestimated by 0.13-0.18, which is about four times higher than the formal error bar. Second, we perform retrieval on HR 7672 B using high spectral-resolution data (R = 35,000) from the Keck Planet Imager and Characterizer and near-infrared photometry. We retrieve [C/H], [O/H], and C/O to be -0.24 ± 0.05, -0.19 ± 0.04, and 0.52 ± 0.02. These values are consistent with those of HR 7672 A within 1.5σ. As such, HR 7672 B is among only a few benchmark BDs (along with Gl 570 D and HD 3651 B) that have been demonstrated to have consistent elemental abundances with their primary stars. Our work provides a practical procedure of testing and performing atmospheric retrieval, and sheds light on potential systematics of future retrievals using high- and low-resolution data.

Keywords: Exoplanet atmospheric composition , Brown dwarfs, Chemical abundances
The Hubble PanCET Program: Emission Spectrum of Hot Jupiter HAT-P-41b. We present the most complete emission spectrum for inflated hot Jupiter HAT-P-41b combining new Hubble Space Telescope Wide Field Camera/G141 spectrum from the Hubble Panchromatic Comparative Exoplanet Treasury program with archival Spitzer eclipse observations. We found a near blackbody-like emission spectrum, which is best fitted with an isothermal temperature-pressure (TP) profile, that agrees well with the dayside heat redistribution scenario assuming zero Bond albedo. The noninverted TP profile is consistent with the nondetection of near-UV/optical absorbers in the transit spectra. We do not find any evidence for significant H- opacity nor a metal-rich atmosphere. HAT-P-41b is an ideal target that sits in the transitioning parameter space between hot and ultra-hot Jupiters, and future James Webb Space Telescope observations will help us to better constrain the thermal structure and chemical composition.

Keywords: Exoplanet atmospheres
A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939. This study calculated astrophysical parameters, as well as kinematic and galactic orbital parameters, of the open clusters NGC 1664 and NGC 6939. The work is based on CCD ultraviolet, blue, and visual (UBV) and Gaia photometric and astrometric data from ground- and space-based observations. Considering Gaia Early Data Release 3 (EDR3) astrometric data, we determined membership probabilities of stars located in both of the clusters. We used two-color diagrams to determine the E(B - V) color excesses for NGC 1664 and NGC 6939 as 0.190 ± 0.018 and 0.380 ± 0.025 mag, respectively. Photometric metallicities for the two clusters were estimated as [Fe/H] = -0.10 ± 0.02 dex for NGC 1664 and as [Fe/H] = -0.06 ± 0.01 dex for NGC 6939. Using the reddening and metallicity calculated in the study, we obtained distance moduli and ages of the clusters by fitting PARSEC isochrones to the color-magnitude diagrams based on the most likely member stars. Isochrone fitting distances are 1289 ± 47 pc and 1716 ± 87 pc, which coincide with ages of 675 ± 50 Myr and 1.5 ± 0.2 Gyr for NGC 1664 and NGC 6939, respectively. We also derived the distances to the clusters using Gaia trigonometric parallaxes and compared these estimates with the literature. We concluded that the results are in good agreement with those given by the current study. Present-day mass function slopes were calculated as Γ = -1.22 ± 0.33 and Γ = -1.18 ± 0.21 for NGC 1664 and NGC 6939, respectively, which are compatible with the Salpeter slope. Analyzes showed that both of clusters are dynamically relaxed. The kinematic and dynamic orbital parameters of the clusters were calculated, indicating that the birthplaces of the clusters are outside the solar circle.

Keywords: Hertzsprung Russell diagram, Stellar kinematics, Galaxy kinematics, Open star clusters, Star clusters
Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds. Mira variables are asymptotic giant-branch pulsating stars with long pulsation periods and large amplitudes in optical bands. By applying the random forest algorithm to the I-band light curves for the Miras in the Magellanic Clouds, we have classified these Miras into regular Miras and nonregular Miras. Nonregular Miras exhibit a long-term variation in addition to their primary pulsation periods. Our results confirm that the period-luminosity relation for maximum light has a small dispersion, but only occurs on the regular oxygen-rich Miras, which we recommend to be applied in future distance-scale work. We have also collected multiband photometry for these Miras to perform a spectral energy distribution fitting with stellar and dust components, showing that a significant fraction of dust is present around the nonregular Miras. According to our results, we believe that the periodic long-term variations seen in the nonregular Miras might be due to the presence of dust.

Keywords: Periodic variable stars, Mira variable stars, Long period variable stars, Pulsating variable stars
The MKID Pipeline: A Data Reduction and Analysis Pipeline for UVOIR MKID Data. We present the Microwave Kinetic Inductance Detector (MKID) Pipeline, which is a general use science data pipeline for the reduction and analysis of ultraviolet, optical, and infrared MKID data sets. This paper provides an introduction to the nature of MKID data sets, it gives an overview of the calibration steps that are included in the pipeline, and it introduces the implementation of the software.

Keywords: Publicly available software, Time series analysis, Astronomy data reduction
The Energetics of the Central Engine in the Powerful Quasar 3C 298. The compact steep-spectrum radio source 3C 298 (redshift of 1.44) has the largest 178 MHz luminosity in the Third Cambridge Revised Catalogue (3CR); its radio lobes are among the most luminous in the universe. The plasma state of the radio lobes is modeled with the aid of interferometric radio observations (in particular, the new Low Frequency Array observation and archival MERLIN data) and archival single-station data. It is estimated that the long-term time-averaged jet power required to fill these lobes with leptonic plasma is $\overline{Q}\,\approx 1.28\pm 0.51\times {10}^{47}\,\mathrm{erg}\,{{\rm{s}}}^{-1}$ , rivaling the largest time-averaged jet powers from any quasar. Supporting this notion of extraordinary jet power is a 0.5-10 keV luminosity of ≈ 5.2 × 1046 erg s-1, comparable to luminous blazars, yet there is no other indication of strong relativistic beaming. We combine two new high signal-to-noise ratio optical spectroscopic observations from the Hobby-Eberly Telescope with archival Hubble Space Telescope, Two Micron All Sky Survey, and Galaxy Evolutionary Explorer data to compute a bolometric luminosity from the accretion flow of L bol ≈ 1.55 ± 0.15 × 1047 erg s-1. The ratio, $\overline{Q}/{L}_{\mathrm{bol}}\approx 1$ , is the approximate upper limit for quasars. Characteristic of a large $\overline{Q}/{L}_{\mathrm{bol}}$ , we find an extreme-ultraviolet (EUV) spectrum that is very steep (the "EUV deficit" of powerful radio quasars relative to radio-quiet quasars), and this weak ionizing continuum is likely a contributing factor to the relatively small equivalent widths of the broad emission lines in this quasar.

Keywords: Quasars
The Open Cluster Chemical Abundances and Mapping Survey. V. Chemical Abundances of CTIO/Hydra Clusters Using The Cannon. Open clusters are key chemical and age tracers of Milky Way evolution. While open clusters provide significant constraints on galaxy evolution, their use has been limited due to discrepancies in measuring abundances from different studies. We analyze medium-resolution (R ~ 19,000) Cerro Tololo Inter-American Observatory/Hydra spectra of giant stars in 58 open clusters using The Cannon to determine [Fe/H], [Mg/Fe], [Si/Fe], [Al/Fe], and [O/Fe]. This work adds an additional 55 primarily southern hemisphere open clusters calibrated to the Sloan Digital Sky Survey/Apache Point Observatory Galactic Evolution Experiment DR16 metallicity system. This uniform analysis is compared to previous studies [Fe/H] measurements for 23 clusters and we present spectroscopic metallicities for the first time for 35 open clusters.

Keywords: Open star clusters, Galactic abundances, Chemical abundances, Milky Way evolution
Uncertainty in Grain Size Estimations of Volatiles on Trans-Neptunian Objects and Kuiper Belt Objects. We analyze the uncertainty in grain size estimation of pure methane (CH4) and nitrogen saturated with methane (N2:CH4) ices, the most abundant volatile materials on trans-Neptunian objects (TNOs) and Kuiper Belt objects (KBOs). We compare the single scattering albedo, which determines the grain size estimation of outer solar system regolith, of these ices using the Mie scattering model and two other Hapke approximations (Hapke 1993) in radiative transfer scattering models (RTMs) at near-infrared (NIR) wavelengths (1-5 μm). The equivalent slab (Hapke slab) approximation model predicts results much closer to Mie scattering over the NIR wavelengths at a wide range of grain sizes. In contrast, even though the internal scattering model predicts an approximate particle diameter close to the Mie model for particles with a 10 μm radii, it exhibits higher discrepancies in the predicted estimation for larger grain sizes (e.g., 100 and 1000 μm radii). Owing to the Rayleigh effect on single-scattering properties, neither Hapke approximate models could predict an accurate grain size estimation for the small particles (radii ≤5 μm). We recommend that future studies should favor the Hapke slab approximation when employing RTMs for estimating grain sizes of the vast number of TNOs and KBOs in the outer solar system.

Keywords: Plutoids, Classical Kuiper belt objects, Surface ices, Radiative transfer, Trans-Neptunian objects
Revisiting WASP-47 with ESPRESSO and TESS. WASP-47 hosts a remarkable planetary system containing a hot Jupiter (WASP-47 b; P = 4.159 days) with an inner super-Earth (WASP-47 e; P = 0.7896 days), a close-orbiting outer Neptune (WASP-47 d; P = 9.031 days), and a long-period giant planet (WASP-47 c; P = 588.4 days). We use the new Transiting Exoplanet Survey Satellite (TESS) photometry to refine the orbital ephemerides of the transiting planets in the system, particularly the hot Jupiter WASP-47 b, for which we find an update equating to a 17.4 minute shift in the transit time. We report new radial-velocity measurements from the Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO) spectrograph for WASP-47, which we use to refine the masses of WASP-47 d and WASP-47 e, with a high-cadence observing strategy aimed to focus on the super-Earth WASP-47 e. We detect a periodic modulation in the K2 photometry that corresponds to a 32.5 ± 3.9 day stellar rotation, and find further stellar activity signals in our ESPRESSO data consistent with this rotation period. For WASP-47 e we measure a mass of 6.77 ± 0.57 M ⊕ and a bulk density of 6.29 ± 0.60 g cm-3, giving WASP-47 e the second most precisely measured density to date of any super-Earth. The mass and radius of WASP-47 e, combined with the exotic configuration of the planetary system, suggest the WASP-47 system formed through a mechanism different to systems with multiple small planets or more typical isolated hot Jupiters.

Keywords: Exoplanet astronomy, Radial velocity, Transit photometry, Stellar activity
Dynamical Architecture of the HD 107148 Planetary System. We present an independent Doppler validation and dynamical orbital analysis of the two-planet system HD 107148, which was recently announced in Rosenthal et al. Our detailed analyses are based on literature HIRES data and newly obtained HARPS and CARMENES radial-velocity (RV) measurements as part of our survey in search for additional planets around single-planet systems. We perform a periodogram analysis of the available HIRES and HARPS precise RVs and stellar activity indicators. We do not find any apparent correlation between the RV measurements and the stellar activity indicators, thus linking the two strong periodicities to a moderately compact multiplanet system. We carry out orbital fitting analysis by testing various one- and two-planet orbital configurations and studying the posterior probability distribution of the fitted parameters. Our results solidify the existence of a Saturn-mass planet (HD 107148b, discovered first) with a period of P b ~ 77.2 days and a second, eccentric (e c ~ 0.4), Neptune-mass exoplanet (HD 107148c) with an orbital period of P c ~ 18.3 days. Finally, we investigate the two-planet system's long-term stability and overall orbital dynamics with the posterior distribution of our preferred orbital configuration. Our N-body stability simulations show that the system is long-term stable and exhibits large secular osculations in eccentricity but in no particular mean motion resonance configuration. The HD 107148 system, consisting of a solar-type main-sequence star with two giant planets in a rare configuration, features a common proper-motion white dwarf companion and is therefore a valuable target for understanding the formation and evolution of planetary systems.

Keywords: Exoplanet dynamics, Radial velocity, Exoplanet systems, Exoplanet astronomy, Exoplanet detection methods
Plaskett 1.8 m Observations of Starlink Satellites. We present observations of 23 Starlink satellites in the g' bandpass, obtained from the Dominion Astrophysical Observatory's Plaskett 1.8 m telescope. The targets include a mixture of satellites with and without brightness mitigation measures (i.e., visors). At the time of the observations (2021 July 16), Starlink satellites were sunlit throughout the night, and, even with strict elevation and azimuth limits, there were over 800 candidate Starlink arcs. The satellites altogether have a median range corrected brightness (550 km) of ${\overline{H}}_{g}^{550}=5.3$ mag. Dividing the targets into those without and with visors, their median range corrected magnitudes are ${\overline{H}}_{g}^{550}(\mathrm{no}\,\mathrm{visor})=5.1$ and ${\overline{H}}_{g}^{550}(\mathrm{visor})=5.7$ mag, respectively. While the visor sample is dimmer in aggregate, the range corrected brightness distribution ranged from ${H}_{g}^{550}=4.3$ mag to 9.4 mag. The two brightest satellites have similar H  g  550 to within the uncertainty, but one is visored and the other nonvisored. The dimmest satellite we observed is one without mitigations. The intrinsic brightness dispersion among the full sample is σ  g  = 0.5 mag.

Keywords: Artificial satellites, Astronomical site protection
An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO. In order to assess the multiplicity statistics of stars across spectral types and populations in a volume-limited sample, we censused nearby stars for companions with Robo-AO. We report on observations of 1157 stars of all spectral types within 25 pc with decl. &gt;-13° searching for tight companions. We detected 154 companion candidates with separations ranging from ~0.″15 to 4.″0 and magnitude differences up to ∆m ${}_{i^{\prime} }\leqslant 7$ using the robotic adaptive optics instrument Robo-AO. We confirmed physical association from Gaia EDR3 astrometry for 53 of the companion candidates, 99 remain to be confirmed, and two were ruled out as background objects. We complemented the high-resolution imaging companion search with a search for comoving objects with separations out to 10,000 au in Gaia EDR3, which resulted in an additional 147 companions registered. Of the 301 total companions reported in this study, 49 of them are new discoveries. Out of the 191 stars with significant acceleration measurements in the Hipparcos-Gaia catalog of accelerations, we detect companions around 115 of them, with the significance of the acceleration increasing as the companion separation decreases. From this survey, we report the following multiplicity fractions (compared to literature values): 40.9% ± 3.0% (44%) for FGK stars and 28.2% ± 2.3% (27%) for M stars, as well as higher-order fractions of 5.5% ± 1.1% (11%) and 3.9% ± 0.9% (5%) for FGK stars and M-type stars, respectively.

Keywords: Observational astronomy, Multiple stars, Binary stars, Close binary stars, Astronomy data analysis, Solar neighborhood, Direct imaging, Astronomical methods, High angular resolution
Architectures of Compact Super-Earth Systems Shaped by Instabilities. Compact nonresonant systems of sub-Jovian planets are the most common outcome of the planet formation process. Despite exhibiting broad overall diversity, these planets also display dramatic signatures of intrasystem uniformity in their masses, radii, and orbital spacings. Although the details of their formation and early evolution are poorly known, sub-Jovian planets are expected to emerge from their natal nebulae as multiresonant chains, owing to planet-disk interactions. Within the context of this scenario, the architectures of observed exoplanet systems can be broadly replicated if resonances are disrupted through postnebular dynamical instabilities. Here, we generate an ad hoc sample of resonant chains and use a suite of N-body simulations to show that instabilities can not only reproduce the observed period ratio distribution, but that the resulting collisions also modify the mass uniformity in a way that is consistent with the data. Furthermore, we demonstrate that primordial mass uniformity, motivated by the sample of resonant chains coupled with dynamical sculpting, naturally generates uniformity in orbital period spacing similar to what is observed. Finally, we find that almost all collisions lead to perfect mergers, but some form of postinstability damping is likely needed to fully account for the present-day dynamically cold architectures of sub-Jovian exoplanets.

Keywords: Exoplanet dynamics, Exoplanet astronomy, Exoplanet formation, Orbital resonances
PetroFit: A Python Package for Computing Petrosian Radii and Fitting Galaxy Light Profiles. PetroFit is an open-source Python package based on Astropy and Photutils that can calculate Petrosian profiles and fit galaxy images. It offers end-to-end tools for making accurate photometric measurements, estimating morphological properties, and fitting 2D models to galaxy images. Petrosian metric radii can be used for model parameter estimation and aperture photometry to provide accurate total fluxes. Correction tools are provided for improving Petrosian radii estimates affected by galaxy morphology. PetroFit also provides tools for sampling Astropy-based models (including custom profiles and multicomponent models) onto image grids and enables point-spread function convolution to account for the effects of seeing. These capabilities provide a robust means of modeling and fitting galaxy light profiles. We have made the PetroFit package publicly available on GitHub ( PetroFit/petrofit ) and PyPi (pip install petrofit).

Keywords: CCD photometry, Regression, Astronomy software, Galaxies
Semidetached Mass-transfer Massive Binaries in the Nearby Galaxy M31. Semidetached binaries provide a valuable test of the evolutionary models of interacting binaries where the mass is transferring from one component to the other, and the evolutions of both components will be changed. Many results of semidetached binaries have been obtained in the Milky Way, while there are few studies in the Andromeda galaxy (M31). By analyzing the light curves of 12 eclipsing binaries observed by Vilardell et al., we determined the fundamental parameters of these systems using the Wilson and Devinney method. It is discovered that they are semidetached binaries where the less massive components have filled their Roche lobes, while the more massive ones are detached from the lobes. We calculated their times of light minimum for the first time. The primary stars in those semidetached binaries have different mass ratios and fill-out factors and they are good sources to investigate the binary evolution in M31. It is found that the mass ratio is correlated with the fill-out factor of the primary. Systems with higher mass ratios tend to have lower fill-out factors. These results can be explained that the mass transfer from the less massive component to the more massive one. Moreover, the photometric solutions reveal that the secondary components are more evolved than the primary ones indicating that they are formed from originally detached binary systems via a case A mass transfer. These binaries have experienced the mass-reverse evolution and are at the late stage of a case A evolution in the nearby galaxy M31.

Keywords: Eclipsing binary stars, Andromeda Galaxy, Early stellar evolution, Close binary stars