Sazuna/UAT_keywords huggingface dataset:
The Discovery of the Long-Period, Eccentric Planet Kepler-88 d and System Characterization with Radial Velocities and Photodynamical Analysis. We present the discovery of Kepler-88 d ( ${P}_{d}\,= $1403\pm 14\,\mathrm{days}, $M\sin {i}_{d}=965\pm 44\,{M}_{\oplus }=3.04\pm 0.13\,{M}_{{\rm{J}}}, ${e}_{d}=0.41\pm 0.03 ) based on six years of radial velocity (RV) follow-up from the W. M. Keck Observatory High Resolution Echelle Spectrometer spectrograph. Kepler-88 has two previously identified planets. Kepler-88 b (KOI-142.01) transits in the NASA Kepler photometry and has very large transit timing variations (TTVs). Nesvorný et al. performed a dynamical analysis of the TTVs to uniquely identify the orbital period and mass of the perturbing planet (Kepler-88 c), which was later was confirmed with RVs from the Observatoire de Haute-Provence (OHP). To fully explore the architecture of this system, we performed photodynamical modeling on the Kepler photometry combined with the RVs from Keck and OHP and stellar parameters from spectroscopy and Gaia. Planet d is not detectable in the photometry, and long-baseline RVs are needed to ascertain its presence. A photodynamical model simultaneously optimized to fit the RVs and Kepler photometry yields the most precise planet masses and orbital properties yet for b and c: ${P}_{b}=10.91647\pm 0.00014\,\mathrm{days}${M}_{b}=9.5\pm 1.2\,{M}_{\oplus }, ${P}_{c}=22.2649\pm 0.0007\,\mathrm{days}, and ${M}_{c}=214.0\pm 5.3\,{M}_{\oplus } . The photodynamical solution also finds that planets b and c have low eccentricites and low mutual inclination, are apsidally anti-aligned, and have conjunctions on the same hemisphere of the star. Continued RV follow-up of systems with small planets will improve our understanding of the link between inner planetary system architectures and giant planets.

Keywords: Exoplanet astronomy, Exoplanet detection methods, Exoplanet systems, Exoplanets
TESS Reveals HD 118203 b to be a Transiting Planet. The exoplanet HD 118203 b, orbiting a bright (V = 8.05) host star, was discovered using the radial velocity method by da Silva et al., but was not previously known to transit. Transiting Exoplanet Survey Satellite (TESS) photometry has revealed that this planet transits its host star. Nine planetary transits were observed by TESS, allowing us to measure the radius of the planet to be ${1.136}_{-0.028}^{+0.029}{R}_{J}$ , and to calculate the planet mass to be ${2.166}_{-0.079}^{+0.074}{M}_{J}$ . The host star is slightly evolved with an effective temperature of ${T}_{\mathrm{eff}}={5683}_{-85}^{+84}$ K and a surface gravity of $\mathrm{log}\,g={3.889}_{0.018}^{0.017}$ . With an orbital period of ${6.134985}_{-0.000030}^{+0.000029}$ days and an eccentricity of 0.314 ± 0.017, the planet occupies a transitional regime between circularized hot Jupiters and more dynamically active planets at longer orbital periods. The host star is among the 10 brightest known to have transiting giant planets, providing opportunities for both planetary atmospheric and asteroseismic studies.

Keywords: Exoplanet astronomy, Transit photometry, Exoplanet systems
HD 165054: An Astrometric Calibration Field for High-contrast Imagers in Baade's Window. We present a study of the HD 165054 astrometric calibration field that has been periodically observed with the Gemini Planet Imager (GPI). HD 165054 is a bright star within Baade's Window, a region of the galactic plane with relatively low extinction from interstellar dust. HD 165054 was selected as a calibrator target due to the high number density of stars within this region (∼3 stars per square arcsecond with H &lt; 22), necessary because of the small field of view of the GPI. Using nine epochs spanning over five years, we have fit a standard five-parameter astrometric model to the astrometry of seven background stars within close proximity to HD 165054 (ρ &lt; 2″). We achieved a proper motion precision of ∼0.3 mas yr-1 and constrained the parallax of each star to be ≲1 mas. Our measured proper motions and parallax limits are consistent with the background stars being a part of the galactic bulge. Using these measurements, we find no evidence of any systematic trend of either the plate scale or the north angle offset of GPI between 2014 and 2019. We compared our model describing the motions of the seven background stars to observations of the same field in 2014 and 2018 obtained with Keck/NIRC2, an instrument with excellent astrometric calibration. We find that the predicted position of the background sources is consistent with that measured by NIRC2, within the uncertainties of the calibration of the two instruments. In the future, we will use this field as a standard astrometric calibrator for the upgrade of GPI and potentially for other high-contrast imagers.

Keywords: Direct imaging, Astrometry, Astronomy data reduction, Astronomical instrumentation
Suspended and Restored Activities of a Nearby Supermassive Black Hole. The discovery of spectral type transition of active galactic nuclei (AGNs), the so-called "changing-look" (CL) phenomenon, challenges the widely accepted AGN paradigm, not only in the orientation-based unified model, but also in the standard disk model. In past decades, only a couple of nearby repeat changing-look active galactic nuclei (CL-AGNs) have been identified. Here we report spectroscopic observations of UGC 3223 over the course of 18 yr, from 2001 onwards. Combining the spectrum taken in 1987 by Stirpe, we have witnessed its type transitions from $1.5\to 2.0\to 1.8$ over 32 yr, and captured a long-lived (at least 10 yr) thorough "turn-off" state with a spectrum typical of a Seyfert 2 galaxy. The long-term thorough turn-off state probably suggests a once-dormant and an awakening central engine in UGC 3223. We argue that the (dis)appearance of the broad Balmer emission lines can be explained by the disk-wind broad-line region model given the evolution of the calculated Eddington ratio of accretion of the supermassive black hole.

Keywords: Active galactic nuclei, Emission line galaxies
WIYN Open Cluster Study LXXX: HDI CCD UBVRI Photometry of the Old Open Cluster NGC 7142 and Comparison to M67. We present UBVRI photometry of 8702 stars in a 0°5 × 0°5 field in the direction of NGC 7142, taken with the Half Degree Imager at the WIYN 0.9 m telescope, to improve knowledge of this cluster's basic parameters. Our photometry spans the ranges 10.6-20.4 mag in U, 10.6-22.0 mag in B, 10.0-21.8 mag in V, 9.2-20.7 mag in R, and 8.5-19.9 mag in I. Using color-color diagrams that employ all four color combinations that include U, versus B - V, we derive a reddening-metallicity relation for the cluster, with preferred values E(B - V) = 0.338 ± 0.031 mag for the left-edge fiducial of the main sequence and [Fe/H] = 0.0 ± 0.1 dex, where the Hyades cluster has been used as an unreddened reference cluster, the extinction relations of Cardelli have been employed, and the metallicity dependence of the Yonsei-Yale (Y2) isochrones has been assumed. Comparison of our data to the Y2 isochrones in multiple color-magnitude diagrams (CMDs) yields distance-metallicity and age-metallicity relations, with preferred values of $m-M=12.65\pm 0.23$ mag and age = ${4.0}_{+1.3}^{-0.7}$ Gyr. Re-evaluation of the parameters of M67 using Stetson's UBVI photometry yields [Fe/H] = -0.02 ± 0.05 dex, E(B - V) = 0.04 ± 0.01 mag, m - M = 9.75 ± 0.03 mag, and age = 3.85 ± 0.17 Gyr; we thus find the metallicity and age of the two clusters to be indistinguishable. A semi-independent analysis adopting the parameters of M67 and shifting the fiducials of the two clusters in six CMDs until they match strongly corroborates the values listed above. The differences between our inferred parallaxes and the Gaia DR2 values are 87 ± 60 μas for NGC 7142 and 48 ± 15 μas for M67, consistent with previous studies. * The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, the National Optical Astronomy Observatory and the University of Missouri.

Keywords: Stellar ages, Johnson photometry, Interstellar reddening, Open star clusters, Stellar distance, Metallicity
California-Kepler Survey. IX. Revisiting the Minimum-mass Extrasolar Nebula with Precise Stellar Parameters. We investigate a possible correlation between the solid surface density Σ of the minimum-mass extrasolar nebula (MMEN) and the host star mass M⋆ and metallicity [Fe/H]. Leveraging on the precise host star properties from the California-Kepler Survey (CKS), we found that ${\rm{\Sigma }}={50}_{-20}^{+33}\,{\rm{g}}\,{\mathrm{cm}}^{-2}$ (a/1 au)-1.75±0.07 (M⋆/M⊙)1.04±0.22 100.22±0.05[Fe/H] for Kepler-like systems (1-4R⊕; a &lt; 1 au). The strong M⋆ dependence is reminiscent of previous dust continuum results that the solid disk mass scales with M⋆. The weaker [Fe/H] dependence shows that sub-Neptune planets, unlike giant planets, form readily in lower metallicity environment. The innermost region (a &lt; 0.1 au) of an MMEN maintains a smooth profile despite a steep decline of planet occurrence rate: a result that favors the truncation of disks by corotating magnetospheres with a range of rotation periods, rather than the sublimation of dust. The Σ of Kepler multitransiting systems shows a much stronger correlation with M⋆ and [Fe/H] than singles. This suggests that the dynamically hot evolution that produced single systems also partially removed the memory of formation in disks. Radial-velocity planets yielded a MMEN very similar to CKS planets; transit-timing-variation planets' postulated convergent migration history is supported by their poorly constrained MMEN. We found that lower mass stars have a higher efficiency of forming/retaining planets: for Sun-like stars, about 20% of the solid mass within ∼1 au are converted/preserved as sub-Neptunes, compared to 70% for late-K to early-M stars. This may be due to the lower binary fraction, lower giant-planet occurrence, or the longer disk lifetime of lower mass stars.

Keywords: Exoplanet formation
Searching the Entirety of Kepler Data. II. Occurrence Rate Estimates for FGK Stars. We present exoplanet occurrence rates estimated with approximate Bayesian computation for planets with radii between 0.5 and 16 R⊕ and orbital periods between 0.78 and 400 days orbiting FGK dwarf stars. We base our results on an independent planet catalog compiled from our search of all ∼200,000 stars observed over the Kepler mission, with precise planetary radii supplemented by Gaia DR2-incorporated stellar radii. We take into account detection and vetting efficiency, planet radius uncertainty, and reliability against transit-like noise signals in the data. By analyzing our FGK occurrence rates as well as those computed after separating F-, G-, and K-type stars, we explore dependencies on stellar effective temperature, planet radius, and orbital period. We reveal new characteristics of the photoevaporation-driven "radius gap" between ∼1.5 and 2 R⊕, indicating that the bimodal distribution previously revealed for P &lt; 100 days exists only over a much narrower range of orbital periods, above which sub-Neptunes dominate and below which super-Earths dominate. Finally, we provide several estimates of the "eta-Earth" value—the frequency of potentially habitable, rocky planets orbiting Sun-like stars. For planets with sizes 0.75-1.5 R⊕ orbiting in a conservatively defined habitable zone (0.99-1.70 au) around G-type stars, we place an upper limit (84.1th percentile) of &lt;0.18 planets per star.

Keywords: Bayesian statistics, Exoplanet catalogs, Exoplanets, Astrostatistics, Transit photometry, Habitable planets
Periodic Narrowband Radio Wave Emissions and Inward Plasma Transport at Saturn's Magnetosphere. The abrupt brightening of an Energetic Neutral Atom (ENA) blob or cloud has been interpreted as plasma injection in the Kronian magnetosphere (termed ENA injection herein). Morphologically, there appears to be two types of abrupt ENA cloud brightening: (1) the brightening of a large cloud usually seen at distances &gt;10-12 Rs (Rs ∼ 60,268 km) in the midnight or postmidnight region; (2) the brightening of a smaller cloud usually seen at distances &lt;10-12 Rs around 21-03 magnetic local time. Among many radio waves observed at Saturn, type 2 ENA injections correlate best with the 5 kHz narrowband (NB) waves. Using Cassini Ion and Neutral Camera (INCA) and Radio and Plasma Wave Science (RPWS) data, we examine the periodicities of the type 2 ENA injections and the 5 kHz NB emissions as well as their cross-correlations, which have been previously used to measure the lag times or phase differences. Because correlational analysis can only establish linear relationships, we also use mutual information to establish linear and nonlinear relationships. On average, the peak of the 5 kHz NB emission lags those of the type 2 ENA injection by about a few minutes to 2 hr. The injection of hot plasma to the inner magnetosphere can lead to temperature anisotropy, which can generate electrostatic upper hybrid waves, which upon encountering the high-density gradient at the outer edge of the Enceladus density torus, can mode convert to Z mode and then to O mode. The 5 kHz NB waves commonly propagate in the O mode.

Keywords: Space plasmas, Magnetohydrodynamics, Magnetospheric radio emissions, Multi-periodic pulsation, Neutral hydrogen clouds, Lomb-Scargle periodogram, Planetary magnetospheres
Precision Photometric and Astrometric Calibration Using Alternating Satellite Speckles. Photometric and astrometric calibration of high-contrast images is essential for the characterization of companions at small angular separation from their stellar host. The main challenge to performing accurate relative photometry and astrometry of high-contrast companions with respect to the host star is that the central starlight cannot be directly used as a reference, as it is either blocked by a coronagraphic mask or saturating the detector. Our approach is to add fiducial incoherent faint copies of the host star in the image plane and alternate the pattern of these copies between exposures. Subtracting two frames with different calibration patterns removes measurement bias due to static and slowly varying incoherent speckle halo components, while ensuring that calibration references are inserted on each frame. Each calibration pattern is achieved by high-speed modulation of a pupil-plane deformable mirror to ensure incoherence. We implemented the technique on-sky on the Subaru Coronagraphic Extreme Adaptive Optics instrument with speckles which were of the order of 103 times fainter than the central host. The achieved relative photometric and astrometric measurement precisions for 10 s exposure were respectively 5% and 20 milliarcsecond. We also demonstrate, over a 540 s measurement span, that residual photometric and astrometric errors are uncorrelated in time, indicating that residual noise averages as the inverse square root of the number of exposures in longer time-series data sets.

Keywords: Coronagraphic imaging, Astronomical techniques, Artificial satellites, Astronomical instrumentation, Astrometry, Photometry, Direct imaging
The Gemini Planet Imager View of the HD 32297 Debris Disk. We present new H-band scattered light images of the HD 32297 edge-on debris disk obtained with the Gemini Planet Imager. The disk is detected in total and polarized intensity down to a projected angular separation of 0"15, or 20 au. On the other hand, the large-scale swept-back halo remains undetected, likely a consequence of its markedly blue color relative to the parent body belt. We analyze the curvature of the disk spine and estimate a radius of ≍100 au for the parent body belt, smaller than past scattered light studies but consistent with thermal emission maps of the system. We employ three different flux-preserving post-processing methods to suppress the residual starlight and evaluate the surface brightness and polarization profile along the disk spine. Unlike past studies of the system, our high-fidelity images reveal the disk to be highly symmetric and devoid of morphological and surface brightness perturbations. We find the dust scattering properties of the system to be consistent with those observed in other debris disks, with the exception of HR 4796. Finally, we find no direct evidence for the presence of a planetary-mass object in the system.

Keywords: Circumstellar dust, Debris disks
First Images of the Protoplanetary Disk around PDS 201. Scattered light imaging has revealed nearly a dozen circumstellar disks around young Herbig Ae/Be stars—enabling studies of structures in the upper disk layers as potential signs of ongoing planet formation. We present the first images of the disk around the variable Herbig Ae star PDS 201 (V* V351 Ori) and an analysis of the images and spectral energy distribution through 3D Monte Carlo radiative transfer simulations and forward modeling. The disk is detected in three data sets with the Large Binocular Telescope Interferometer/Large Binocular Telescope mid-infrared camera at the Large Binocular Telescope, including direct observations in the Ks and L' filters, and an L' observation with the 360° vector apodizing phase plate coronagraph. The scattered light disk extends to a very large radius of ∼250 au, which places it among the largest of such disks. Exterior to the disk, we establish detection limits on substellar companions down to ∼5 MJup at ≳1"5 (≳500 au), assuming the Baraffe et al. models. The images show a radial gap extending to ∼0"4 (∼140 au at a distance of 340 pc) that is also evident in the spectral energy distribution. The large gap is a possible signpost of multiple high-mass giant planets at orbital distances (∼60-100 au) that are unusually massive and widely separated compared to those of planet populations previously inferred from protoplanetary disk substructures.

Keywords: Early-type variable stars, Variable stars, Protoplanetary disks, Exoplanets
TOI-1338: TESS' First Transiting Circumbinary Planet. We report the detection of the first circumbinary planet (CBP) found by Transiting Exoplanet Survey Satellite (TESS). The target, a known eclipsing binary, was observed in sectors 1 through 12 at 30 minute cadence and in sectors 4 through 12 at 2 minute cadence. It consists of two stars with masses of 1.1 M☉ and 0.3 M☉ on a slightly eccentric (0.16), 14.6 day orbit, producing prominent primary eclipses and shallow secondary eclipses. The planet has a radius of ∼6.9 R⊕ and was observed to make three transits across the primary star of roughly equal depths (∼0.2%) but different durations—a common signature of transiting CBPs. Its orbit is nearly circular (e ≍ 0.09) with an orbital period of 95.2 days. The orbital planes of the binary and the planet are aligned to within ∼1°. To obtain a complete solution for the system, we combined the TESS photometry with existing ground-based radial-velocity observations in a numerical photometric-dynamical model. The system demonstrates the discovery potential of TESS for CBPs and provides further understanding of the formation and evolution of planets orbiting close binary stars.

Keywords: Exoplanet astronomy, Eclipsing binary stars
The Most Metal-poor Stars in Omega Centauri (NGC 5139). The most massive and complex globular clusters in the Galaxy are thought to have originated as the nuclear cores of now tidally disrupted dwarf galaxies, but the connection between globular clusters and dwarf galaxies is tenuous with the M54/Sagittarius system representing the only unambiguous link. The globular cluster Omega Centauri (ω Cen) is more massive and chemically diverse than M 54, and is thought to have been the nuclear star cluster of either the Sequoia or Gaia-Enceladus galaxy. Local Group dwarf galaxies with masses equivalent to these systems often host significant populations of very metal-poor stars ([Fe/H] &lt; -2.5), and one might expect to find such objects in ω Cen. Using high-resolution spectra from Magellan-M2FS, we detected 11 stars in a targeted sample of 395 that have [Fe/H] ranging from -2.30 to -2.52. These are the most metal-poor stars discovered in the cluster, and are five times more metal-poor than ω Cen's dominant population. However, these stars are not so metal-poor as to be unambiguously linked to a dwarf galaxy origin. The cluster's metal-poor tail appears to contain two populations near [Fe/H] ∼ -2.1 and -2.4, which are very centrally concentrated but do not exhibit any peculiar kinematic signatures. Several possible origins for these stars are discussed. ∗ This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

Keywords: Globular star clusters, Population II stars, Metallicity, Chemical abundances
Two Transiting Hot Jupiters from the WASP Survey: WASP-150b and WASP-176b. We report the discovery of two transiting exoplanets from the WASP survey, WASP-150b and WASP-176b. WASP-150b is an eccentric (e = 0.38) hot Jupiter on a 5.6 day orbit around a V = 12.03, F8 main-sequence host. The host star has a mass and radius of 1.4 ${M}_{\odot }$ and 1.7 ${R}_{\odot }$ respectively. WASP-150b has a mass and radius of 8.5 ${M}_{{\rm{J}}}$ and 1.1 RJ, leading to a large planetary bulk density of 6.4 ρJ. WASP-150b is found to be ∼3 Gyr old, well below its circularization timescale, supporting the eccentric nature of the planet. WASP-176b is a hot Jupiter planet on a 3.9 day orbit around a V = 12.01, F9 sub-giant host. The host star has a mass and radius of 1.3 M⊙ and 1.9 R⊙. WASP-176b has a mass and radius of 0.86 MJ and 1.5 RJ, respectively, leading to a planetary bulk density of 0.23 ρJ.

Keywords: Radial velocity, Exoplanet detection methods, Exoplanet systems, Photometry
OGLE-2018-BLG-0677Lb: A Super-Earth Near the Galactic Bulge. We report the analysis of the microlensing event OGLE-2018-BLG-0677. A small feature in the light curve of the event leads to the discovery that the lens is a star-planet system. Although there are two degenerate solutions that could not be distinguished for this event, both lead to a similar planet-host mass ratio. We perform a Bayesian analysis based on a Galactic model to obtain the properties of the system and find that the planet corresponds to a super-Earth/sub-Neptune with a mass of ${M}_{\mathrm{planet}}={3.96}_{-2.66}^{+5.88}{M}_{\oplus }$ . The host star has a mass of ${M}_{\mathrm{host}}={0.12}_{-0.08}^{+0.14}\,{M}_{\odot }$ . The projected separation for the inner and outer solutions are ${0.63}_{-0.17}^{+0.20}$ au and ${0.72}_{-0.19}^{+0.23}$ au respectively. At ${\rm{\Delta }}{\chi }^{2}={\chi }^{2}(1{\rm{L}}1{\rm{S}})-{\chi }^{2}(2{\rm{L}}1{\rm{S}})=46$ , this is by far the lowest Δχ2 for any securely detected microlensing planet to date, a feature that is closely connected to the fact that it is detected primarily via a "dip" rather than a "bump."

Keywords: Gravitational microlensing exoplanet detection, Exoplanets, Super Earths, Exoplanet detection methods, Astrostatistics strategies