We present 2241 exoplanet candidates identified with data from the Transiting Exoplanet Survey Satellite (TESS) during its 2 yr Prime Mission. We list these candidates in the TESS Objects of Interest (TOI) Catalog, which includes both new planet candidates found by TESS and previously known planets recovered by TESS observations. We describe the process used to identify TOIs, investigate the characteristics of the new planet candidates, and discuss some notable TESS planet discoveries. The TOI catalog includes an unprecedented number of small planet candidates around nearby bright stars, which are well suited for detailed follow-up observations. The TESS data products for the Prime Mission (sectors 1-26), including the TOI catalog, light curves, full-frame images, and target pixel files, are publicly available at the Mikulski Archive for Space Telescopes.

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Qualitative studies suggest that patients with primary biliary cirrhosis (PBC) experience significant problems with memory and concentration. Studies of nonhepatic disease have linked hypotension and cognitive impairment. In this study, we determined the prevalence of cognitive symptoms in PBC, examined the relationship between symptoms and overt cognitive impairment and structural brain lesions, and explored the role of autonomic dysfunction. The prevalence of cognitive symptoms was determined in 198 patients with PBC. Twenty-eight representative early-stage female patients with PBC and 11 matched controls underwent formal cognitive testing at baseline and after 2 years of follow-up. Autonomic nervous system function was assessed according to heart rate variability and baroreflex sensitivity. Eleven subjects with PBC had structural brain lesions quantified via magnetic resonance imaging. Cognitive symptoms were frequent in our PBC population, with 53% of patients experiencing moderate or severe problems with concentration and/or memory, which were unrelated in their severity to biochemical and histological makers of liver disease severity, suggesting that this symptom burden is largely or entirely unrelated to hepatic encephalopathy. Perceived cognitive symptoms correlated with objectively assessed cognitive impairment (r 2 ‫؍‬ 0.2, P < 0.05). Cognitive deficits were seen in the PBC cohort compared with controls, with significant decline detected over 2 years of follow-up. Correlations were seen between cognitive performance (full-scale intelligence quotient) and systolic blood pressure (P ‫؍‬ 0.01, r 2 ‫؍‬ 0.2) with decline in cognitive function associated with autonomic abnormalities. Structural brain lesions were found in PBC, the density of which correlated with degree of cognitive impairment (P ‫؍‬ 0.01, r 2 ‫؍‬ 0.5) and autonomic function (P ‫؍‬ 0.03, r 2 ‫؍‬ 0.2). Conclusion: Cognitive symptoms are prevalent in PBC independent of liver disease severity and are associated with poorer performance on objective cognitive testing. Cognitive impairment is, in turn, associated with structural brain lesions and autonomic dysfunction, which may predict risk of cognitive decline. (HEPATOLOGY 2008;48:541-549.) P rimary biliary cirrhosis (PBC) is a chronic cholestatic liver disease with an autoimmune etiology. 1 In addition to the risk of progressive liver disease, culminating in biliary cirrhosis with its associated complications, patients frequently experience non-stage-associated symptoms that can often lead to significant impairment of their quality of life. [2][3][4][5][6] Research into the non-end-stage disease-associated factors that lead to impairment of quality of life in PBC has, to date, largely focused on fatigue; a symptom which affects a significant proportion of patients and which is associated with impairment in normal physical functioning. 7-10 However, patient reports, and qualitative studies performed in the derivation of a PBC-specific quality of life measure, the PBC-40, suggest the existence of...

The Automated Planet Finder (APF) is a facility purpose-built for the discovery and characterization of extrasolar planets through high cadence Doppler velocimetry of the reflex barycentric accelerations of their host stars. Located atop Mt. Hamilton, the APF facility consists of a 2.4-m telescope and its Levy Spectrometer, an optical echelle spectrometer optimized for precision Doppler velocimetry. APF features a fixed format spectral range from 374 nm -970 nm, and delivers a "Throughput" (resolution * slit width product) of 114,000 arc-seconds, with spectral resolutions up to 150,000.Overall system efficiency (fraction of photons incident on the primary mirror that are detected by the science CCD) on blaze at 560 nm in planet-hunting mode is 15%. Firstlight tests on the RV standard stars HD 185144 and HD 9407 demonstrate sub-m s −1 precision (RMS per observation) held over a 3-month period. This paper reviews the basic features of the telescope, dome, and spectrometer, and gives a brief summary of first-light performance.

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At a distance of 1.8 parsecs 1 , Barnard's star (Gl 699) is a red dwarf with the largest apparent motion of any known stellar object. It is the closest single star to the Sun, second only to the a Centauri triple stellar system. Barnard's star is also among the least magnetically active red dwarfs known 2,3 and has an estimated age older than our Solar System. Its properties have made it a prime target for planet searches employing techniques such as radial velocity 4,5,6 , astrometry 7,8 , and direct imaging 9 , all with different sensitivity limits but ultimately leading to disproved or null results. Here we report that the combination of numerous measurements from high-precision radial velocity instruments reveals the presence of a low-amplitude but significant periodic signal at 233 days. Independent photometric and spectroscopic monitoring, as well as the analysis of instrumental systematic effects, show that this signal is best explained as arising from a planetary companion. The candidate planet around Barnard's star is a cold super-Earth with a minimum mass of 3.2 Earth masses orbiting near its snow-line. The combination of all radial velocity datasets spanning 20 years additionally reveals a long-term modulation that could arise from a magnetic activity cycle or from a more distant planetary object. Because of its proximity to the Sun, the proposed planet has a maximum angular separation of 220 milliarcseconds from Barnard's star, making it an excellent target for complementary direct imaging and astrometric observations.Barnard's star is the second closest red dwarf to the Solar System, after Proxima Centauri, and thus an ideal target to search for exoplanets with potential for further characterisation 10 . Its very low X-ray flux, lack of Ha emission, low chromospheric emission indices, slow rotation rate, slightly sub-solar metallicity, and membership of the thick disc kinematic population indicate an extremely low magnetic activity level and suggest an age older than the Sun. Because of its apparent brightness and very low variability, Barnard's star is often regarded as a benchmark for intermediate M-type dwarfs. Its basic properties are summarized in Table 1.An early analysis of archival radial velocity datasets of Barnard's star up to 2015 indicated the presence of at least one significant signal with a period of ~230 days but with rather poor sampling. To elucidate its presence and nature we undertook an intensive monitoring campaign with the CARMENES spectrometer 11 , collecting precise radial velocity measurements on every possible night during 2016-2017, and we obtained overlapping observations with the ESO/HARPS and HARPS-N instruments. The combined Doppler monitoring effort of Barnard's star, including archival and newly acquired observations, resulted in 771 radial velocity epochs (nightly averages) with typical individual precisions of 0.9 to 1.8 m s -1 , obtained over a timespan exceeding 20 years from seven different facilities and yielding eight independent datasets (ED Table 1).While e...

Transiting Exoplanet Survey Satellite (TESS ) observations have revealed a compact multi-planet system around the sixth-magnitude star HR 858 (TIC 178155732, TOI 396), located 32 parsecs away. Three planets, each about twice the size of Earth, transit this slightly-evolved, late F-type star, which is also a member of a visual binary. Two of the planets may be in mean motion resonance. We analyze the TESS observations, using novel methods to model and remove instrumental systematic errors, and combine these data with follow-up observations taken from a suite of ground-based telescopes to characterize the planetary system. The HR 858 planets are enticing targets for precise radial velocity observations, secondary eclipse spectroscopy, and measurements of the Rossiter-McLaughlin effect.

Gliese 876 harbors one of the most dynamically rich and well-studied exoplanetary systems. The nearby M4V dwarf hosts four known planets, the outer three of which are trapped in a Laplace meanmotion resonance. A thorough characterization of the complex resonant perturbations exhibited by the orbiting planets, and the chaotic dynamics therein, is key to a complete picture of the system's formation and evolutionary history. Here we present a reanalysis of the system using six years of new radial velocity (RV) data from four instruments. This new data augments and more than doubles the size of the decades-long collection of existing velocity measurements. We provide updated estimates of the system parameters by employing a computationally efficient Wisdom-Holman N-body symplectic integrator, coupled with a Gaussian Process (GP) regression model to account for correlated stellar noise. Experiments with synthetic RV data show that the dynamical characterization of the system can differ depending on whether a white noise or correlated noise model is adopted. Despite there being a region of stability for an additional planet in the resonant chain, we find no evidence for one. Our new parameter estimates place the system even deeper into resonance than previously thought and suggest that the system might be in a low energy, quasi-regular double apsidal corotation resonance. This result and others will be used in a subsequent study on the primordial migration processes responsible for the formation of the resonant chain.