Abstract We apply the angular two-point correlation function (TPCF) to the spatial distributions of young star clusters (YSCs) in four nearby star forming galaxies (NGC 628, NGC 4449, M51, and M83) in order to investigate their underlying hierarchical structuring. Using newly constructed catalogs of YSCs in the emerging phase (eYSCs), identified in the infrared with JWST, and optical YSCs detected in archival Hubble Space Telescope data, we compute the TPCFs for various cluster samples and age bins across the four galaxies, as part of the Feedback in Emerging extrAgalactic Star ClusTers (FEAST) program. We find clear evidence of hierarchical structuring, especially in eYSCs and YSCs with ages <10 Myr (referred to as oYSCs), which show similar TPCFs within each galaxy. NGC 628 exhibits a clear distinction between the TPCFs of eYSCs and oYSCs, implying a shorter randomization timescale. In contrast, clusters aged 10–300 Myr exhibit progressively more random spatial distributions, becoming effectively random after ∼100 Myr, consistent with earlier studies. The two-dimensional fractal index D 2 values of the YSCs’ underlying distributions are calculated from model fits to the TPCFs. Our values of D 2 derived from the youngest YSC populations align better with the expected value of D 2 ∼ 1.3 for a universal star formation process compared to previous findings.

White dwarfs (WDs) are the final fate of about 97% of the stars in our galaxy, making them vital tracers of stellar history. A fraction of WDs exist in cataclysmic variable (CV) systems, accreting matter from a nearby companion star. A subset of CVs undergo episodic rapid mass transfer, termed dwarf novae (DNe) outbursts. Some accreting WDs exhibit near sinusoidal photometric variations, interpreted as g mode pulsations. However, identifying pulsation modes in accreting WDs remains challenging due to the paucity of available observed modes. In this work, we present a comprehensive computation of the observable g mode frequencies across a range of WD parameters, varying the WD mass, size of the newly accreted layer and core temperature. We also introduce a novel method for mode identification based on the time evolution of pulsation periods following an accretion episode. Our mode identification method does not rely on the direct detection of the consecutive radial mode orders, frequently required in isolated WDs. Moreover, this work improves upon our previous WD modeling efforts. We use a more realistic core temperature in addition to thermohaline mixing and element diffusion enabled during the accretion phase.

Abstract The Cool Planets Imaging Coronagraph (CPI-C) on Chinese Space Station Survey Telescope (CSST) is proposed to direct image the cool planets around nearby solar-type stars (within 40 pc). The core scientific objective of CPI-C is to conduct high-contrast directly imaging surveys of exoplanets ranging in size from Neptune-like to Jupiter-like, located at separations of 0.5 to 5 AU from their host stars, and to perform systematic spectroscopic analysis of the detected planets through high-precision multi-band photometry. CPI-C employs a step-transmission apodization technique to suppress the diffraction noises from the telescope pupil and a precise phase correction technique to eliminate the speckle noises due to imperfections of the optical surfaces. The contrast requirement is better than $10^{-8}$ at an inner working angle (IWA) of $3-4\lambda/D$, in the visible wavelength from 600 nm to 900 nm. CPI-C will be the first space-based instrument capable of directly imaging the reflection light from the cool exoplanets in the visible wavelength, enabling the measurement of key physical parameters such as the effective temperature, surface gravity, radius, mass, and other key parameters. The potential observation results will significantly contribute to further understand the formation and evolution mechanisms of planets, which will also lay a solid foundation for future confirmation of the Earth-twins in the next generation space flagship missions.

Abstract Iota Aquarii is a nearby B-type star that has accrued a large amount of evidence for a close companion. Here we report on a VLTI/GRAVITY observation in which we detected a 1.2 M ⊙ companion at a projected separation ρ = 7.1 mas ↔ 0.38 au. We conclude that this is the same companion that has been previously reported from direct spectral detection, but that its reported mass (1.00 ± 0.03 M ⊙ ) had been somewhat underestimated. However, the Gaia–Hipparcos proper motion change and parallax discrepancy are not readily explained by the companion; if due to another hierarchical outer companion, it would have to be either a M ≲ 0.5 M ⊙ red dwarf or a white dwarf to remain undetected.

Abstract We discuss the most recent observations made with the Southern Connecticut Stellar Interferometer, which is a three-station stellar intensity interferometer located on the campus of Southern Connecticut State University, in New Haven, Connecticut. Two different kinds of observations are presented. We first analyze observations of Vega taken in a three-telescope mode. (Previously, the instrument had only two operational stations.) We show that, while the efficiency remains nearly identical to that reported in our last paper, the addition of the third station allows more photon data to be recorded simultaneously, and therefore we can build up the photon-bunching peak in the data stream in fewer hours on sky for an unresolved source. In the second part of the paper, we report our observations to date of the nearby red giant star Arcturus, most of which occurred in the first half of 2025. These show that, as a partially resolved source at the baselines we used, we detect fewer correlations in the photon-bunching peak than for an unresolved source of comparable brightness. Combining the data with speckle imaging observations taken at Apache Point Observatory, we derive a new measurement of Arcturus’ diameter that extends the temporal baseline of interferometric observations of the star and is consistent with previous analyses made by other investigators.

The long gamma-ray burst GRB,180728A at a redshift of z=0.1171 stands out due to its high isotropic energy of E_ erg, in contrast with most events at redshift z<0.2, but it is comparable to the bulk of luminous bursts more common at higher redshift. γ,iso 51 We aim to study the properties of GRB,180728A's prompt emission, afterglow, and associated supernova (SN 2018fip), comparing them with other GRB-SN events. This study employs a dense photometric and spectroscopic follow-up of the afterglow and the SN up to 80 days after the burst. We used image subtraction to remove the presence of a nearby bright star, and modelled both the afterglow and the supernova. This event lies on the E_ 000$ km s plane occupied by classical collapsar events, and the prompt emission is one of the most energetic at z<0.2 after GRB 030329 and GRB 221009A. The afterglow of GRB,180728A is less luminous than that of most long GRBs, showing a shallow early phase that steepens after about 5 hours (0.2 days). The GRB exploded in an irregular low-mass blue star-forming galaxy, which is typical of low-z collapsar events. Because of the relatively faint afterglow, the light curve bump of SN,2018fip dominates the optical emission already after approximately 3 days and is one of the best sampled to date. The strong suppression below sim4000 Å and a largely featureless continuum in the early 6--9 day spectra favour aspherical two-component ejecta with a high-velocity collimated component ($>20 , -1 ), that is dominant early on and a more massive low-velocity component that dominates at much later epochs. Our findings indicate that asymmetries need to be considered in order to better understand GRB-SNe. In any case, SN,2018fip shares many characteristics with typical GRB-SNe. Its kinetic energy is below the common range of 10^52--10^53 erg and does not correlate with the high energy of the GRB, highlighting the complexity and diversity of the GRB-SN energy budget partition.

Abstract The discovery of heavy radioactive elements (e.g., $^{60}\mathrm{Fe}$) on Earth suggests that supernova explosions may have occurred near our planet within the past million years, potentially having a significant impact on the ecological environment. This finding has motivated the search for nearby neutron stars in the Solar neighborhood. In a recent study, a candidate for one of the closest neutron stars to Earth, LAMOST J235456.73+335625.9 (hereafter J2354), was reported. \textcolor{red}{Based on dynamical mass measurements under different inclination angle assumptions, the inferred mass range for the unseen compact companion in the system is $1.4$--$1.6$ $M_{\odot}$.} Hence, the unseen companion in J2354 is either a massive cold white dwarf or a neutron star. Here we model the flux variations of J2354 as a combination of ellipsoidal modulation and surface spots. We test both cold spot and hot spot models, setting the number of spots to two in each case, and constrain the spot properties through light curve fitting. In the cold spot scenario, the spots are mostly visible at phases $0.5$--$0.75$, whereas in the hot spot scenario, the spots appear predominantly at phases $0.25$--$0.5$. The hot spot model shows better agreement with the observed H$\alpha$ phase variation than the cold spot model. Furthermore, \textcolor{red}{the thermal radiation of} a massive but cold white dwarf \textcolor{red}{cannot} produce the level of localized heating required to explain the hot spot \textcolor{red}{unless additional heating mechanisms are involved}; in contrast, a neutron star can naturally provide such heating through energetic winds. Our results \textcolor{red}{are consistent with} the neutron star interpretation of the compact object in J2354.

Abstract Understanding planetary habitability requires a comparative approach that explores the divergent evolutionary outcomes of Earth and Venus. The Habitable Worlds Observatory (HWO) will be uniquely positioned to conduct a statistical and physical census of terrestrial exoplanets spanning the Venus Zone (VZ) and the Habitable Zone, enabling the detection and atmospheric characterization of post-runaway greenhouse worlds (“exoVenuses”). We present an updated list of VZ exoplanets, which raises the number of known candidates to 370. We describe a science case and an observing strategy for VZ exoplanets that integrates precursor exoplanet detection data and stellar characterization with HWO direct imaging, spectroscopy across the UV/optical/IR, and spectropolarimetry. Our proposed framework emphasizes a pathway toward the diagnosis of sulfur chemistry (SO 2 ) and aerosol physics (H 2 SO 4 clouds/hazes), planetary redox states (O 2 /O 3 false positives from hydrogen loss), and cloud microphysics detection (rainbow polarization). We quantify implications for HWO requirements, including UV access to 0.2–0.4 μ m, optical/NIR coverage to ≳1.5 μ m, inner working angle (IWA) reaching 0.3–1.5 au around nearby Sun-like stars, and the SNR/resolution needed for key features. Finally, we outline a community-driven path to producing robust demographic inferences and target selection for optimizing HWO observations.

The age of the Local Bubble (LB) constrains the timescale on which the interstellar medium in the solar neighborhood evolves. Previous estimates placed the age of the LB at ≳ 14, , and attributed its expansion to ∼ 15-20 supernovae (SNe), yet a companion paper suggests this age may be overestimated. Myr We place new constraints on the age of the LB and reevaluate the question of whether its expansion triggered or suppressed local star formation. We reconstructed the LB’s geometry and momentum using publicly available 3D dust maps and compared them to the high-quality sample of simulated SN remnants in the SISSI project. Independent constraints on the star formation history and SN rate were obtained from a Gaia DR3–based census of nearby star clusters. We find that sim7- 59 SNe over to respectively, are required to explain both the LB's momentum and size and confirm that such a high SN rate can be sustained by local star clusters. Our analysis yields a substantially smaller LB age than previous estimates, requiring a correspondingly larger number of SNe, driving its expansion. We show that this result is in tension with the conclusion that the LB is powered solely by SNe from the Scorpius–Centaurus OB association, which ceased star formation around the time the LB formed. If our estimates are correct, it follows that the majority of star formation in the solar neighborhood happened before the formation of the LB and was not triggered by its expansion. Instead, the SNe that powered the LB appear to overall have quenched the ongoing star formation process. This does not rule out that star formation in the clouds, located near its current edge, could have been affected by the LB expansion.

Axion-like particles (ALPs) are hypothetical pseudoscalar bosons that arise in many extensions of the Standard Model and can be well-motivated dark-matter candidates. Nearby massive stars in the late stages of stellar evolution provide a promising environment for enhanced ALP production due to their high core temperatures and densities. In this work, we aim to search for a combined signal of ALP-induced hard X-ray and soft γ-ray emission from 18 nearby pre-supernova stars. We intend to use the full public INTEGRAL/SPI 22-year database to create individual datasets and link the resulting spectra for a coherent analysis. We used a maximum-likelihood approach to extract the fluxes of the selected nearby stars from 20--2000,keV. From stellar-evolution models, we obtain the expected spectral shapes of ALPs producing processes peaking in the 50--500,keV range, depending on the age and mass of the star. We then constructed a joint likelihood that acknowledges the uncertainties in individual stellar parameters toward a combined estimate for the coupling constants g_aγ and g_ae as a function of the ALP mass m_a. We find that the hard X-ray and soft γ-ray fluxes of all selected stars are consistent with zero within uncertainties. We provide upper limits on the continuum flux as well as the 511,keV and 1809,keV lines from these sources. The combined estimate of the upper limit of the product aγ g_ ae is $(0.008 - 2) 10^ -24 GeV ^ -1 $ (95% C.I.) and the ALP-photon coupling g_ aγ = (0.13 - 1.26) 10^ -11 GeV ^ -1 (95% C.I.) up to a mass of m_a łeqq 10^ -11 eV for different times to core-collapse and different magnetic-field models. Our results are among the strongest limits on the ALP coupling constants in the literature. We also provide conservative limits on the coupling constants, g_ aγ g_ ae , of $(0.27 - 1.25) 10^ -24 GeV ^ -1 $ (95% C.I.) by assuming all stars but one to be in the early He-burning phase. This work shows that soft γ-ray observations are required to efficiently probe the ALP parameter space, as well as massive-star evolution models in general.

Abstract The brown dwarf desert describes a range of orbital periods ( ${\lt}5$ yr) in which fewer brown dwarf-mass companions have been observed around Sun-like stars, when compared to planets and low mass stellar companions. It is therefore theorised that brown dwarf companions are unlikely to form or remain in this period range. The Gaia space telescope is uniquely sensitive to companions in this period range, making it an ideal tool to conduct a survey of the brown dwarf desert. In this study, we use Bayesian inference to analyse data from nearby ( ${\lt}200$ pc) Sun-like stars in Gaia ’s DR3 catalogue, assuming single companions. From this, we identify 2 673 systems (2.41% of the sample) with possible brown dwarf companions in this period range. Accounting for observational biases, we find that $10.4^{+0.8}_{-0.6}$ % of nearby Sun-like stars have astrometric errors consistent with a brown dwarf-mass companion with a period less than 5 yr, significantly higher than previous studies which reported occurrence rates of ${\lt}1$ %. However, we acknowledge the limitations of DR3 and are unable to make a definitive statement without epoch data. By simulating epoch data with multiple companions, we find that, while some of the data can be explained by multiple low-mass brown dwarf companions and high-mass planets ( ${\gt}10$ M $_{\mathrm{J}}$ ), high-mass brown dwarfs ( ${\gt}50$ M $_{\mathrm{J}}$ ) in this period range are comparatively rare. Finally, we used our studies of the brown dwarf distribution to predict the number of companions in the brown dwarf desert we can expect to discover in DR4.

The nearby star Fomalhaut is orbited by a compact source, Fomalhautb, which has previously been interpreted as either a dust-enshrouded exoplanet or a dust cloud generated by the collision of two planetesimals. Such collisions are rarely observed but their debris can appear in direct imaging. We report Hubble Space Telescope observations that show the appearance in 2023 of a second point source around Fomalhaut, resembling the appearance of Fomalhautb twenty years earlier. We interpret this additional source as a dust cloud produced by a recent impact between two planetesimals. The positions and motion of two impact-generated dust clouds over twenty years provide constraints on the collisional dynamics in the debris belt.

Abstract The upcoming Roman Coronagraph will be the first high-contrast instrument in space capable of high-order wave front sensing and control technologies, a critical technology demonstration for the proposed Habitable Worlds Observatory (HWO) that aims to directly image and characterize habitable exoEarths. The nominal Roman Coronagraph observing plan involves alternating observations of a science target and a bright, nearby reference star. High contrast is achieved using wave front sensing and control, also known as “digging a dark hole,” where performance depends on the properties of the reference star, requiring V < 3, a resolved stellar diameter <2 mas, and no stellar multiplicity. The imposed brightness and diameter criteria limit the sample of reference star candidates to high-mass main-sequence and post-main-sequence objects, where multiplicity rates are high. A future HWO coronagraph may have similarly restrictive criteria in reference star selection. From an exhaustive literature review of 95 stars, we identify an initial list of 40 primary and 18 reserve reference star candidates relevant to both the Roman Coronagraph and HWO. We present results from an initial survey of these candidates with high-resolution adaptive optics imaging and speckle interferometry and identify no new companions. We discuss the need for higher-contrast observations to sufficiently vet these reference star candidates prior to Roman Coronagraph observations, along with the implications of reference star criteria on observation planning for Roman and HWO.

Abstract We modeled the trajectories of material ejected from 20 nearby debris disk stars, including ϵ Eridani (Ran), Vega, Fomalhaut, and β Pictoris, within a simulated Milky Way potential in order to quantify their contribution to the population of interstellar material entering the solar system. Our simulations show that material from each of these 20 systems is currently to be expected within our planetary system. We calculate expected fluxes of both macroscopic interstellar objects (ISOs, ≥100 m), which could be detected by telescopic surveys, and smaller meteoroids (≥200 μ m), which could manifest as meteors in Earth’s atmosphere. We estimate that the ISO population originating from these debris disks and currently within the inner solar system is on the order of ∼2, only a fraction of the expected total ISO population but nonetheless likely to be discovered by Rubin. Meteors in Earth’s atmosphere from these systems are expected as well, but current methods, both radar and video, might require decades to collect even a single event. Our sample is found to be rich in relatively low excess velocity particles compared to the broader expected ISO population, which might make them harder to distinguish observationally from bound objects in some cases. These results provide a framework for linking detections of interstellar material to their astrophysical origins, offering new opportunities to probe the composition and dynamical history of nearby planetary systems.

Aims. We present the first observations of the HD 92945 debris disk obtained with the James Webb Space Telescope (JWST), targeting this nearby K0V star located at 21.54 pc from the Sun. The main objectives are to characterize the disk’s morphology in the near infrared, compare it with previous data from ALMA and HST, and place new constraints on the presence and properties of potential planetary companions shaping the disk. Methods. High-contrast coronagraphic imaging was performed using JWST/NIRCam in the F200W and F444W filters. Advanced postprocessing techniques were employed, including reference differential imaging (RDI) with custom-built point spread function (PSF) libraries, and forward modeling of the disk using synthetic PSFs and MCMC optimization. After subtracting the disk contribution, the residuals were analyzed to identify candidate point sources. From these, we derived contrast curves and constructed detection probability maps for substellar companions. Results. The disk is clearly detected in both NIRCam filters and reveals a broad, inclined structure with a gap, consistent with previous scattered-light and ALMA observations. The modeling confirms the presence of a gap at ∼80 au and shows a scale height and scattering properties compatible with a dynamically active disk. A significant brightness asymmetry is observed in the southwestern inner ring at both 2 and 4.4 μm, consistent with previous ALMA results. Observing this feature across different wavelengths and epochs strongly supports a scenario where one or more unseen planetary companions are perturbing the disk. No comoving sources are detected, and all candidate objects in the field are consistent with background stars or galaxies. The derived detection limits exclude planets more massive than ∼0.4-0.5 M Jup beyond 100 au and more massive than ∼1 M Jup beyond 20-40 au. This, in turn, rules out the possibility of a single planet placed beyond ∼ 20 au as responsible for the astrometric signal observed by Gaia. These results, combined with the observed disk features, support a scenario in which a single or multiple sub-Jupiter planets dynamically shape the system through mechanisms such as secular apsidal resonances, providing a coherent explanation for the gap, the asymmetric brightness distribution and the astrometric signal.

Abstract The dominant sources of photoionizing radiation in the extreme-ultraviolet (EUV) incident on the exterior of the local interstellar clouds include two nearby early B-type stars, ϵ CMa (124 ± 2 pc) and β CMa (151 ± 5 pc), three hot dwarfs, and the Local Hot Bubble (LHB). Line emission (170–912 Å) from highly ionized metals (Fe, Ne, Mg) in million-degree LHB plasma may be responsible for the elevated ionization fractions of helium ( n He II / n He ≈ 0.4) compared to hydrogen ( n H II / n H ≈ 0.2) in the local clouds. We update the stellar parameters and ionizing flux for β CMa, after correcting the EUV spectra for intervening H i column density, N H I = (1.9 ± 0.1) × 10 18 cm −2 , and its hotter effective temperature, T eff ≈ 25,000 K versus 21,000 K for ϵ CMa. These two stars produce a combined H-ionizing photon flux Φ H ≈ 6800 ± 1400 cm −2 s −1 at the external surface of the local clouds. The hot bubble could produce comparable fluxes, Φ H = 2000–9000 cm −2 s −1 , depending on the amount of metal depletion into dust grains that survive sputtering. The radial velocities and proper motions of β CMa and ϵ CMa indicate that both stars passed within 10 ± 1 pc of the Sun 4.4 ± 0.1 Myr ago, with 100–200 times higher local ionizing fluxes. At that time, the local clouds were likely farther from the Sun, owing to their transverse motion. Over the past few Myr, EUV radiation from these two stars left a wake of highly ionized gas in a hot, low-density cavity produced by past supernova explosions in the Sco-Cen OB association and connected with the LHB.

Abstract Obtaining a complete census of gas in the local interstellar medium (LISM; <100 pc) is challenging given the limited available tracers of the warm, partially ionized medium. Medium- to high-resolution UV absorption spectroscopy toward individual nearby stars is the primary method used, and incomplete spatial sampling of this complex medium makes a global map of the material difficult. Using H I column density measurements derived from H I Ly α spectroscopy toward 164 stars inside 100 pc, we have generated 2D spatially interpolated N (H I ) maps for different distance shells. Based on the area-weighted sky averages, we find that sight lines inside 10 pc typically have log 10 [ N (H I )/cm −2 ] ∼ 17.9. For greater distance shells, log 10 [ N (H I )/cm −2 ] increases to 18.3 (10–20 pc), then to 18.4 (20–70 pc), and finally to 18.6 (70–100 pc). This last increase is likely associated with the detection of the Local Bubble boundary, thus making the plateau of column density from 20 to 70 pc notable and suggestive of the rarity of warm LISM material beyond ∼10–20 pc. We estimate that the uncertainties associated with N (H I ) values inferred from the interpolated sky maps are approximately inversely correlated with the number of samples in each distance shell, and are in the range of 0.20–0.48 dex, compared to the 0.01–0.30 dex typically determined from direct Ly α observations. We discuss the impact of these uncertainties on interstellar medium corrections of extreme-UV and Ly α observations for nearby stars. Denser spatial sampling of the sky via UV absorption spectroscopy of nearby stars is required to improve the accuracy of these N (H I ) estimates.

ABSTRACT The nearby binary star system 99 Herculis (99 Her) is host to the only known polar-aligned circumbinary debris disc. We investigate the hypothesis that the narrow structure of this circumbinary disc is sculpted by the gravitational influence of one or more unseen polar circumbinary planets. We first establish the theoretically viable parameter space for a sculpting planet by considering dynamical stability and clearing mechanisms, including the chaotic zone, Hill’s radius, diffusion, and polar alignment time-scales. We then use N-body simulations to test three specific architectures: a single planet interior to the disc, a single planet exterior, and a two-planet system bracketing the disc. Our simulations demonstrate that single-planet models are insufficient to reproduce the observed morphology, as they can only truncate one edge of the disc while leaving the other dynamically extended. In contrast, the two-planet shepherding model successfully carves both the inner and outer edges, confining the debris into a narrow, stable polar ring consistent with observations. We conclude that the structure of the 99 Her debris disc is most plausibly explained by the presence of two shepherding, polar circumbinary planets. We present a specific, testable model for this unique system, which elucidates the pivotal role of planetary bodies in sculpting the architecture of debris discs.

ABSTRACT We present new radial velocity measurements of 13 selected intermediate mass stars (2–6 M ⊙ ). The measurements were performed between 29 April and 6 September 2024 at the University Observatory Jena using the échelle spectrograph FLECHAS. The radial velocity of eight stars was found to be constant during our spectroscopic monitoring, namely: 17 Dra A, HD 148374, HD 169487 A, 57 Cnc, And, HD 11031, And, and Cas. In contrast, the radial velocity of five stars showed significant variability throughout or spectroscopic observation, namely: 7 CrB A, 7 CrB B, HD 214007, Her, and HD 201433 A. In all these cases, Keplerian orbital solutions were fitted to the observational data and the orbital elements of these spectroscopic binary systems were determined. In addition, we searched for wide companions of our targets using the third data release from ESA's Gaia mission, in order to determine the multiplicity status of these stars and contribute to the census of bright, nearby multiple stars.

Abstract Observations over the past few decades have found that planets are common around nearby stars in our Galaxy, but little is known about planets that formed outside the Milky Way. We describe the design and early implementation of a survey to test whether planets also exist orbiting the remnant stars of ancient dwarf galaxies that merged with the Milky Way, and if so, how they differ from their Milky Way counterparts. VOYAGERS ( Views Of Yore —Ancient Gaia-enceladus Exoplanet Revealing Survey ) is a radial velocity (RV) search using precision spectrographs to discover exoplanets orbiting very low metallicity (−2.8 < [Fe/H] ≤ −0.8) stars born in the dwarf galaxy Enceladus, which merged with the Milky Way galaxy about 10 Gyr ago. A sample of 22 candidates have been screened from a catalog of Gaia–Enceladus–Sausage (GES) members using a combination of stellar properties and reconnaissance observations from the TRES spectrograph. Precision RV measurements have been initiated using the NEID, HARPS-N, and CARMENES spectrographs. We plan to focus most upcoming observations on 10 main sequence targets. Data collection is well underway, with 778 observations on 22 candidates (385 of which are on 10 focus targets), but far from complete. This survey is designed to be sensitive to sub-Neptune mass planets with periods up to hundreds of days. We note that the RV analysis gives mass multiplied by sin ( inclination ) or the minimum mass for exoplanets. The expected survey yield is three planets, assuming that occurrence rates are similar to those in the Milky Way and taking into account the degeneracy with inclination in our yield models. Our survey is designed to detect at least one exoplanet if occurrence rates are similar to known Milky Way exoplanets or, if no exoplanets are discovered, to rule out a Milky Way-like planet population in GES with 95% confidence level.