We present the TESS-based discoveries of planetary systems orbiting the late G dwarfs TOI-2494 and TOI-5143, each of which harbors a hot giant planet and a smaller interior planet. TOI-2494 hosts a transiting mini-Neptune (P = 2.41 days, RP=2.35-0.15+0.16 R circle plus) and a hot Saturn (P = 8.38 days) with grazing transits, while TOI-5143 hosts a transiting mini-Neptune (P = 2.38 days, RP=2.73-0.17+0.19 R circle plus) and a hot Jupiter (P = 5.21 days) with grazing transits. We measure the masses of TOI-2494 c (80 +/- 19 M circle plus) and TOI-5143 c (208 +/- 14 M circle plus), place upper limits on the masses of the smaller planets, and explore the architectures of the planetary systems. TOI-2494 c and TOI-5143 c join a small but growing number of short-period giant planets known to be flanked by smaller companions. While the absence of close neighbors to most hot Jupiters would be consistent with disruptive dynamical evolution, the presence of nearby small planets in some hot Jupiter systems points to a separate, dynamically quiet formation pathway. In support of this conclusion, we present preliminary evidence that hot giant planets with small nearby companions tend to have low mutual orbital inclinations, consistent with the mutual inclination distribution of the dynamically quiet population of compact systems of multiple super-Earths and mini-Neptunes.

Despite decades of research on hot Jupiters, there are still several theories for their formation. Perhaps hot Jupiters form in several ways. Atmospheric and dynamical studies have the capability to constrain the formation scenarios. However, potential targets have to be well characterized before these observations can further constrain the theories. We present the confirmation and characterization of five hot and warm Jupiters discovered by the TESS space mission. Using TESS data combined with ground-based observations, we determine the masses, radii, and other parameters of TOI-2040 b, TOI-2049 b, TOI-2578 b, TOI-4427 b, and TOI-4458 b. Three of the planets have equilibrium temperatures of about 1800 K while two have temperatures of about 1000 K. Particularly interesting for future atmospheric characterizations are TOI-2578 b and TOI-4427 b, because of their low density and large transmission spectroscopy metric. TOI-4458 b is of special interest because it is in the northern PLATO field. It appears that TOI-2040 b has a small, but measurable eccentricity.

Most known planets are found around metal-rich host stars, which has made it difficult to determine whether a lower metallicity limit for planet formation exists and how the properties of planets born in low-metallicity environments may differ from those with metal-rich origins. We present the discovery and characterization of TOI-7169 b (TIC 372048733 b), a hot Jupiter that is orbiting a spectroscopically-confirmed metal-poor ([Fe/H] = -0.72 +/- 0.05) host star. Based on photometry from TESS and follow-up ground-based imaging, we measure an orbital period of 3.4373125 d and a planetary radius of 1.475 +/- 0.029 R_Jup. We use TRES spectroscopy to determine a mass for TOI-7169 b of 0.41 +/- 0.14 M_Jup. The planet is therefore inflated, with a low density of 0.159 +0.055/-0.054 g/cm^3. We also characterize the host star, showing that TOI-7169 is ancient (12.3 +/- 0.6 Gyr) and alpha-enhanced ([alpha/Fe] 0.3), but with a Galactocentric orbit that is confined to the thin disk. TOI-7169 is perhaps the oldest and most metal-poor star currently known to host a transiting giant planet. Future transmission spectroscopy probing the atmosphere of TOI-7169 b may provide insight into the effect of metallicity on the physical properties of giant planets.

The solar neighborhood is dominated by stars smaller, colder, and fainter than the Sun: the M dwarfs. If we are to understand the context in which the Sun formed and evolved, then we must investigate the system architectures of our low-mass neighbors. We have therefore carried out the Pervasive Overview of Kompanions of Every M Dwarf in Our Neighborhood (POKEMON) speckle survey of nearby M dwarf primaries. We created the survey with the goal of observing a volume-limited (north of -30 degrees) sample of M dwarf primaries through M9 out to 15 pc at diffraction-limited resolution. Pre-Gaia parallax measurements yielded a catalog of 454 nearby M dwarf primaries. However, the precise astrometry from Gaia indicated that there are additional low-mass sources within 15 pc. Here we present the POKEMON-Distance Limited Catalog, a supplemental catalog that consists of speckle observations for the 66 additional M dwarf primaries identified by Gaia, increasing the number of ultracool dwarf (later than M6.5) primaries in the POKEMON catalog by a factor of 1.6. In our observations we detect four likely bound companions. After carrying out a literature search for additional companions, we update the projected separation distribution and find a peak at 7.91 au (sigma log(a) = 1.1, SElog(a) = 0.10). We also update the M dwarf stellar multiplicity and companion rates, and find values of 22.7% +/- 1.8% and 27.5% +/- 2.0%, respectively. These results emphasize the utility of Gaia for identifying low-mass, nearby sources, and we find that ensuing characterization of these sources by SPHEREx will continue to clarify the nature of the solar neighborhood.

We report the discovery of a low-mass transiting brown dwarf orbiting TOI-6884 (TIC 156514476, T-mag = 11.4) from NASA's Transiting Exoplanet Survey Satellite (TESS) mission. The TESS light curves initially suggested an orbital period of similar to 14.42 days; however, our high-precision ground-based radial velocity measurements and multi-epoch time-series photometry reveal this to be a harmonic alias. We determine the true orbital period to be 4.808264(-0.000014)(+0.000015) days and confirm the substellar nature of the companion. TOI-6884b has a mass of 26.32(-0.93)(+0.98)MJ, a radius of 0.927(-0.52)(+0.51)RJ, and resides on a nearly circular orbit (e=0.067(-0.012)(+0.010)). Its host star is a late F-type slightly evolved star with M-* =1.410(-0.069)(+0.075)M(circle dot), R-* =1.840(-0.073)(+0.072) R-circle dot, log g=4.057(-0.039)(+0.045), [Fe/H]=0.094(-0.068)(+0.073) dex, and T-eff=6330(-160)(+180) K. TOI-6884b is a key addition to the small population of well-characterized transiting brown dwarfs orbiting host stars that have left the main sequence. The detection of such systems will contribute to our understanding of dynamical histories and structural evolution of short-period substellar companions around evolved stars.

One of the key goals of the Habitable Worlds Observatory (HWO) is to directly image about 25 potentially habitable exoplanets and determine their properties. This challenge will require a large survey of nearby, bright stars: ∼100 according to the Astro2020 Decadal Survey. To ensure the success of the mission and to help guide design decisions, the stellar multiplicity of the target stars must be well-understood. To this end, we present optical speckle imaging of stars in the NASA Exoplanet Exploration Program provisional HWO star list, which is currently the Tier 1 target list for the HWO Target Stars and Systems Sub-Working Group. We obtained new observations using ‘Alopeke and Zorro at Gemini Observatory and queried the Exoplanet Follow-up Observing Program Archive for archival observations, resulting in speckle imaging data for 80 of the 164 stars. We confirmed one candidate companion detected previously by Gaia (HD 90089) and obtained an ambiguous detection of a known companion (HD 212330). To examine our sensitivity to companions, we simulated stellar companions down to ∼0.1 M _⊙ for each target and found that 75%–85% would be detected in our speckle images; the remaining simulated companions are either too faint or too close-in, and will require follow-up using other methods such as long-term spectroscopic measurements and space-based techniques. This work represents a first step toward surveying potential HWO targets for close-in stellar companions and helping to inform the target selection process for the HWO direct-imaging survey, bringing us closer toward the discovery of potential habitable worlds.

We present the discovery and confirmation of the ultrashort period (USP) planet TOI-2431 b orbiting a nearby (d similar to 36 pc) late K star (T-eff = 4109 +/- 28 K) using observations from the Transiting Exoplanet Survey Satellite (TESS), precise radial velocities (RVs) with NEID and Habitable-zone Planet Finder (HPF) spectrographs, as well as ground-based high-contrast imaging from NESSI. TOI-2431 b has a period of 5 hours and 22 minutes, making it one of the shortest-period exoplanets known to date. TOI-2431 b has a radius of 1.534 +/- 0.033 R-circle plus and a mass of 6.2 +/- 1.6 M-circle plus, where the exact mass precision shows a slight dependence on the choice of prior. This suggests TOI-2431 b has a density compatible with an Earth-like composition and due to its high irradiation, it is likely to be a "lava-world" with a T-eq = 2063 +/- 30 K. We estimate that the current orbital period is only 30% larger than the Roche-limit orbital period and that it has an expected orbital decay timescale of only similar to 31 Myr. Finally, due to the brightness of the host star (V = 10.9, K = 7.6), we find that TOI-2431 b has a high emission spectroscopy metric (ESM) of 27, making it one of the best USP systems for atmospheric phase-curve analyses.

We report the confirmation and analysis of TOI-5349 b, a transiting, warm, Saturn-like planet orbiting an early M dwarf with a period of ∼3.3 days, which we confirmed as part of the Searching for GEMS survey. TOI-5349 b was initially identified in photometry from NASA’s Transiting Exoplanet Survey Satellite mission and subsequently confirmed using high-precision radial velocity (RV) measurements from the Habitable-zone Planet Finder and MAROON-X spectrographs, and from ground-based transit observations obtained using the 0.6 m telescope at Red Buttes Observatory and the 1.0 m telescope at the Table Mountain Facility of Pomona College. From a joint fit of the RV and photometric data, we determine the planet’s mass and radius to be 0.40 ± 0.02 M J ( 127 . 4 − 5.7 + 5.9 M ⊕ ) and 0.91 ± 0.02 R J (10.2 ± 0.3 R ⊕ ), respectively, resulting in a bulk density of ρ p = 0.66 ± 0.06 g cm −3 (∼0.96 the density of Saturn). We determine that the host star is a metal-rich M1-type dwarf with a mass and radius of 0.61 ± 0.02 M ⊙ and 0.58 ± 0.01 R ⊙ , and an effective temperature of T eff = 3751 ± 59 K. Our analysis highlights an emerging pattern, exemplified by TOI-5349, in which transiting Giant Exoplanets around M dwarf Stars (GEMS) often have Saturn-like masses and densities and orbit metal-rich stars. With the growing sample of GEMS planets, comparative studies of short-period gas giants orbiting M dwarfs and Sun-like stars are needed to investigate how metallicity and disk conditions shape the formation and properties of these planets.

We report the confirmation and characterization of four transiting giant planets orbiting early-M dwarfs discovered by the Searching for Giant Exoplanets around M-dwarf Stars (GEMS) survey: TOI-7189 b, TOI-7265B b, TOI-7393 b, and TOI-7394B b. Joint modeling of TESS and ground-based photometry with precision radial velocities from the Habitable-zone Planet Finder and NEID spectrographs yields self-consistent orbital and physical parameters for all systems. The planets have short orbital periods (P = 1.25-4.17 days), masses spanning from 0.5 M_ J to 2.1 M_ J, and radii comparable to Jupiter (0.95 R_ J < R_p < 1.02 R_ J). TOI-7189 b (0.50 M_ J), TOI-7265B b (0.71 M_ J), and TOI-7393 b (0.61 M_ J) are Saturn-like in mass and density, whereas TOI-7394B b is a dense super-Jupiter (2.10 M_ J, ρ_p ≈ 2.4 g cm^-3) on a 1.25-day orbit. All hosts are early-M dwarfs with a narrow range of stellar properties, enabling a controlled comparison of giant-planet outcomes around low-mass stars. Three systems orbit super-solar metallicity stars, while TOI-7393 ([Fe/H] = -0.35 ± 0.16) is the most metal-poor GEMS host identified to date, and exhibits kinematics consistent with the thin/thick-disk transition, suggestive of an older stellar population. Together, these systems reveal substantial diversity in the masses and bulk properties of short-period giant planets orbiting early-M dwarfs, demonstrating that markedly different planetary outcomes can arise around stars with otherwise similar fundamental properties.

This study evaluates the effectiveness of Frequency Domain Electromagnetic (FDEM) and Electrical Resistivity Tomography (ERT) in detecting buried metallic and plastic objects in high-conductivity clay. The investigation was conducted at a controlled Geophysical Test Site (GTS) with two parallel lines of buried objects: five metallic (steel) drums and five plastic drums (empty and water-filled), buried at 0.5–2.0 m depths. FDEM effectively detected metallic objects, showing conductivity values of 230–280 mS/m, well above the 202 mS/m background clay conductivity. Deeper metallic objects (2 m) exhibited higher phase values (~16), and those aligned parallel to the survey line produced stronger anomalies. However, FDEM had limited sensitivity to plastic objects, except when water-filled drums (Objects 8 and 9) increased conductivity (~195–215 mS/m). ERT successfully detected both metallic and plastic objects. However, metallic objects appeared as high-resistivity anomalies (~4 Ω·m) due to current deflection effects. Depth misplacement was observed, with objects buried at 1.5–2.0 m appearing shallower (~1.0 m) due to the dipole-dipole array’s vertical resolution limitations in shallow depth and inversion constraints. These findings highlight the importance of multi-method geophysical surveys. FDEM is optimal for metallic object detection, while ERT provides broader material characterization. Future research should refine inversion techniques and electrode configurations to improve depth resolution and accuracy, enhancing geophysical surveys for environmental, engineering, and archaeological applications.

The population of Jupiter-sized exoplanets with orbital periods between 10 and 200 days (WJs) exhibits a broad range of orbital eccentricities and system architectures, suggesting a diversity of formation and migration pathways. In this work, we report the detection and characterization of two new eccentric WJs, TOI-2147 b and TOI-6019 b, initially identified as planet candidates by the Transiting Exoplanet Survey Satellite (TESS). We combined TESS photometry with ground-based follow-up observations, including multiband photometry from LCOGT and MuSCAT2, high-angular-resolution speckle imaging, and high-precision radial velocity measurements from the high-resolution Manfred Hirt Planet Finder Spectrograph (MaHPS). Using these data, we were able to confirm the planetary nature of both candidates. TOI-2147 b has a radius of 10.5 ± 0.3 R_⊕ and a mass of 116 ± 22 M_⊕. It orbits its slightly metal-poor ([Fe/H] = -0.29^+0.07_-0.08) G-type host star on an eccentric orbit (e = 0.29 ± 0.07) with a period of 26.2 days. TOI-6019 b has a radius of 12.3 ± 0.3 R_⊕ and a mass of 149 ± 15 M_⊕. It orbits a slightly evolved, solar-metallicity G-type sub-giant with a period of 14.5 days on a significantly eccentric orbit (e = 0.48^+0.05_-0.04). Both planets have bulk densities below that of Jupiter, indicating mildly inflated radii, with interior structure modeling using GASTLI. This suggests that tidal heating from the nonzero eccentricities likely contributes to this inflation and disfavors large atmospheric metal enrichment. No significant signals from additional companions were detected in the radial velocity time series or transit timing variations. Together with the elevated eccentricities, this is consistent with a high-eccentricity migration origin for both systems.

A simple diagnostic testing procedure is described to help non-expert practitioners search for unmarked graves at historic burial sites using ground-penetrating radar. The methodology, which includes real-time video-assisted documentation of GPR apparatus trajectories, is illustrated with data from a historic cemetery in Texas, USA. The acquired radargrams are classified, from which unmarked-grave decisions are made under strict, moderate, and lax thresholds. Since there is no gold standard, an alternative strategy for decision-making is adopted assuming the distribution of radar signatures generated by the marked graves is the same as the distribution generated by the unmarked graves. About half of the marked graves generated no discernible radar signature, so this proportion of the unmarked graves is likely to be missed. About one-third of the marked graves generated the tell-tale signature of a deep-seated hyperbola so this proportion of the unmarked graves is likely to be found. The remaining signals are complex and ambiguous. The uncertainty is due to the wide variety of radar signatures that are expressed by burials. The diagnostic testing procedure allows a non-expert practitioner to develop acuity in recognizing unmarked-grave signatures and hone a decision-making capability that leads to improved stakeholder trust.

We present the confirmation of TOI-5573 b, a Saturn-sized exoplanet on an 8.79 days orbit around an early M dwarf (3790 K, 0.59 R ⊙ , 0.61 M ⊙ , 12.30 Jmag). TOI-5573 b has a mass of 11 2 − 19 + 18 M ⊕ (0.35 ± 0.06 M Jup ) and a radius of 9.75 ± 0.47 R ⊕ (0.87 ± 0.04 R Jup ), resulting in a density of 0.6 6 − 0.13 + 0.16 g cm −3 , akin to that of Saturn. The planet was initially discovered by the Transiting Exoplanet Survey Satellite (TESS) and confirmed using a combination of 11 transits from four TESS Sectors (20, 21, 47, and 74), ground-based photometry from the Red Buttes Observatory, and high-precision radial velocity data from the Habitable-zone Planet Finder and NN-EXPLORE Exoplanet Investigations with Doppler spectrographs, achieving a 5 σ precision on the planet’s mass. TOI-5573 b is one of the coolest Saturn-like exoplanets discovered around an M-dwarf, with an equilibrium temperature of only 528 ± 10 K, making it a valuable target for atmospheric characterization. Saturn-like exoplanets around M dwarfs likely form through core accretion, with increased disk opacity slowing gas accretion and limiting their mass. The host star’s supersolar metallicity supports core accretion, but uncertainties in M-dwarf metallicity estimates complicate definitive conclusions. Compared to other GEMS (Giant Exoplanets around M-dwarf Stars) orbiting metal-rich stars, TOI-5573 b aligns with the observed pattern that giant planets preferentially form around M-dwarfs with supersolar metallicity. Further high-resolution spectroscopic observations are needed to explore the role of stellar metallicity in shaping the formation and properties of giant exoplanets like TOI-5573 b.

We present the discovery of 30 transiting giant planets that were initially detected using data from NASA's Transiting Exoplanet Survey Satellite mission. These new planets orbit relatively bright (G <= 12.5) FGK host stars with orbital periods between 1.6 and 8.2 days, and have radii between 0.9 and 1.7 Jupiter radii. We performed follow-up ground-based photometry, high angular resolution imaging, high-resolution spectroscopy, and radial velocity monitoring for each of these objects to confirm that they are planets and determine their masses and other system parameters. The planets' masses span more than an order of magnitude (0.17 M-J < M-p < 3.3 M-J). For two planets, TOI-3593 b and TOI-4961 b, we measured significant nonzero eccentricities of 0.11(-0.03)(+0.05) and 0.18(-0.05)(+0.04 ), respectively, while for the other planets, the data typically provide a 1 sigma upper bound of 0.15 on the eccentricity. These discoveries represent a major step toward assembling a complete, magnitude-limited sample of transiting hot Jupiters around FGK stars.

We present an upgraded version of TRICERATOPS , a software package designed to calculate false positive probabilities for planet candidates identified by the Transiting Exoplanet Survey Satellite (TESS). This enhanced framework now incorporates ground-based light curves in separate bandpasses, which are routinely obtained as part of the candidate vetting process. We apply this upgraded framework to explore the planetary nature of 14 TESS planet candidates, combining primarily J- band light curves acquired with the 200 inch Hale Telescope at Palomar Observatory with complementary archival observations from the Las Cumbres Observatory Global Telescope, the Fred Lawrence Whipple Observatory, and the Teide Observatory, along with existing TESS data and contrast curves from high-resolution imaging. As a result of this analysis we statistically validate (false positive probability < 1.5% and nearby false positive probability < 0.1%) six new planets in five systems: TOI-1346 b, TOI-1346 c, TOI-2719 b, TOI-4155 b, TOI-6000 b, and TOI-6324 b. For these systems, we provide updated estimates of their stellar and planetary properties derived from the TESS and ground-based observations. These new systems contain planets with radii between 0.9 and 6 R _⊕ and orbital periods between 0.3 and 5.5 days. Finally, we use our upgraded version of TRICERATOPS to quantify the relative importance of multiwavelength transit photometry and high-resolution imaging for exoplanet candidate validation, and discuss which kinds of candidates typically benefit the most from ground-based multicolor transit observations.

Barrier islands serve as natural buffers against coastal hazards, hosting freshwater lenses (FWLs) crucial for ecosystems and human water supplies. These groundwater resources are vulnerable to natural disturbances, such as saltwater intrusion and drought, and anthropogenic impacts, notably urban development and canal dredging. This study integrates comprehensive geophysical (TDEM), topographic (DEM and GNSS), and hydrogeological (groundwater level and salinity) measurements to investigate controls on the spatial variability of FWLs across developed and undeveloped regions of Padre Island (Texas, USA)-the world's longest barrier island. Results indicate that proximity to saltwater bodies and urban development (buildings, streets, and pavements) significantly increase FWL salinity (decrease resistivity) and decrease its thickness due to enhanced pathways for saltwater intrusion and reduced infiltration from impervious surfaces. FWL resistivity (mean 33 +/- 18 Omega m) and thickness (8 +/- 5 m) are generally lower near saltwater bodies and significantly reduced in developed sections compared to undeveloped areas. Urban development, including increased impervious surfaces, canal construction, and dune modification, significantly reduces FWL thickness and quality by enhancing seawater intrusion pathways and decreasing groundwater recharge. Moderate to strong positive correlations were found between ground elevation and FWL properties, specifically elevation versus resistivity (r approximate to 0.58) and elevation versus lens thickness (r approximate to 0.82). Higher elevation areas (>2 m) sustain thicker (similar to 9 m) and fresher (similar to 34 Omega m) FWL primarily by reducing evaporative losses, limited saltwater intrusion due to deeper freshwater tables, reduced inundations, and high dune recharge. Larger dune volumes (>16,800 m(3)) strongly correlate with thicker lenses (r approximate to 0.51), likely reflecting enhanced rainwater infiltration and localized recharge over sparsely vegetated dunes. Geological factors also significantly affect lens characteristics; locations where the low-permeability clay aquitard lies deeper support thicker (average similar to 10 m) and fresher (similar to 36 Omega m) lenses. This integrated approach highlights critical natural and anthropogenic controls influencing barrier island freshwater resources, emphasizing the need to jointly consider surface geomorphology, subsurface geology, and development impacts for sustainably managing coastal groundwater.

Ground-penetrating radar (GPR) methods are particularly effective at detecting subsurface features with contrasting electromagnetic properties in archaeological contexts. At the undeveloped prehistoric site of Don Up Mung in northeastern Thailand, GPR surveys were conducted to identify potential burial features within the complex stratigraphic sequences characteristic of multiphase settlements. To assess this potential, we employed a MAL & Aring; Easy Locator Pro WideRange HDR GPR system across a 7.5 x 8 m grid adjacent to a previously excavated area containing confirmed burials dated to 571-404 cal. bce. Radar signatures were systematically classified into six distinct trait classes based on their reflection patterns, and local statistic was applied to identify significant spatial clustering. Results revealed prominent GPR anomalies at depths of 0.4-1.2 m (10-30 ns of radar two-way travel time). The significance maps identified two primary clusters of high-amplitude reflections in the southwestern portion and one cluster of low-amplitude reflections in the eastern portion of the survey area. Despite limitations imposed by the spatial offset between survey and excavation areas, the correspondence between anomaly depths and documented burial horizons provides compelling evidence for burial identification. This research establishes a systematic framework that combines GPR signature classification with point pattern analysis to enhance prehistoric burial detection capabilities in similar geological settings, offering valuable guidance for future archaeological investigations at the site.

Stellar systems consisting of three or more stars are not an uncommon occurrence in the Galaxy. Nearly 50% of solar-type wide binaries with separations >1000 au are actually higher-order multiples with one component being a close binary. Additionally, the higher-order multiplicity fraction appears to be correlated with the physical separation of the widest component. These facts have motivated some of our current theories behind how the widest stellar systems formed, which can have separations on the order of or larger than protostellar cores. However, it is unclear if the correlation between wide binary separation and higher-order multiplicity extends to low-mass binaries. We present initial results of an ongoing speckle imaging survey of nearby low-mass wide binaries. We find an overall higher-order multiplicity fraction for our sample of 42.0% ± 10.9%. If we include systems where Gaia indicates that a companion is likely present, this fraction increases to 62.0% ± 14.2%. This is consistent with previous results from both higher-mass stars and a previous result for low-mass wide binaries. However, we do not detect the expected increase in higher-order multiplicity fraction with separation, as was seen with previous studies. We briefly explore why higher-order multiplicity statistics could be different in low-mass stars, and what the significance might be for models of wide binary formation.

Potato (Solanum tuberosum) is widely recognized as the leading vegetable crop in the United States, with millions of tons produced annually. Despite many advancements in cultivars, crop production still suffers from meager progress in the assessment of early maturity. One potential solution to this problem is Ground- Penetrating Radar (GPR), a near-surface geophysical tool that has recently been applied to agriculture for assessment of root systems by detecting dielectric variations in sub-surface and soil layers by means of electromagnetic waves emitted into the ground. This study seeks to assess GPR's capability to serve as anon- destructive proximal-sensing technique for quantifying potato tuber biomass by estimating the size of potatoes by measuring changes in the reflected GPR signal. Two methods, thresholding analysis and continuous wavelet transform (CWT), were employed in this study to extract features from GPR responses to predict tuber biomass. The dataset was collected in a controlled sandbox system. Thresholding analysis on the interpolated amplitude values yielded significant results, being able to predict tuber biomass with an accuracy of r = 0.82 and R2 = 0.64 based upon Multiple Linear regression. CWT was somewhat less successful, yet still significant, with a prediction accuracy of r = 0.6 and R2 = 0.32. These results indicate that GPR technology is suitable as a decision-support tool for potato breeders seeking to monitor tuber growth.

Sub-Neptunes-volatile-rich exoplanets smaller than Neptune-are intrinsically the most common type of planet known. However, the formation and nature of these objects, as well as the distinctions between subclasses (if any), remain unclear. Two powerful tools to tease out the secrets of these worlds are measurements of (i) atmospheric composition and structure revealed by transit and/or eclipse spectroscopy, and (ii) mass, radius, and density revealed by transit photometry and Doppler spectroscopy. Here, we present OrCAS, a survey to better elucidate the origins, compositions, and atmospheres of sub-Neptunes. This radial velocity survey uses a repeatable, quantifiable metric to select targets suitable for subsequent transmission spectroscopy and address key science themes about the atmospheric and internal compositions and architectures of these systems. Our survey targets 26 systems with transiting sub-Neptune planet candidates, with the overarching goal of increasing the sample of such planets suitable for subsequent atmospheric characterization. This paper lays out our survey's science goals, defines our target prioritization metric, and performs light-curve fits and statistical validation using existing TESS photometry and ground-based follow-up observations. Our survey serves to continue expanding the sample of small exoplanets with well-measured properties orbiting nearby bright stars, ensuring fruitful studies of these systems for many years to come.