Search

We present the discovery and characterization of six short-period, transiting giant planets from NASA's Transiting Exoplanet Survey Satellite (TESS) -- TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642), TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), & TOI-2497 (TIC 97568467). All six planets orbit bright host stars (8.9, Comment: 20 Pages, 6 Figures, 8 Tables, Accepted by MNRAS

We report the discovery and confirmation of the planetary system TOI-1288. This late G dwarf harbours two planets: TOI-1288 b and TOI-1288 c. We combine TESS space-borne and ground-based transit photometry with HARPS-N and HIRES high-precision Doppler measurements, which we use to constrain the masses of both planets in the system and the radius of planet b. TOI-1288~b has a period of $2.699835^{+0.000004}_{-0.000003}$ d, a radius of $5.24 \pm 0.09$ R$_\oplus$, and a mass of $42 \pm 3$ M$_\oplus$, making this planet a hot transiting super-Neptune situated right in the Neptunian desert. This desert refers to a paucity of Neptune-sized planets on short period orbits. Our 2.4-year-long Doppler monitoring of TOI-1288 revealed the presence of a Saturn-mass planet on a moderately eccentric orbit ($0.13^{+0.07}_{-0.09}$) with a minimum mass of $84 \pm 7$ M$_\oplus$ and a period of $443^{+11}_{-13}$ d. The 5 sectors worth of TESS data do not cover our expected mid-transit time for TOI-1288 c, and we do not detect a transit for this planet in these sectors., 16 pages, 17 figures, under review MNRAS

Full list of authors: Yee, Samuel W.; Winn, Joshua N.; Hartman, Joel D.; Bouma, Luke G.; Zhou, George; Quinn, Samuel N.; Latham, David W.; Bieryla, Allyson; Rodriguez, Joseph E.; Collins, Karen A.; Alfaro, Owen; Barkaoui, Khalid; Beard, Corey; Belinski, Alexander A.; Benkhaldoun, Zouhair; Benni, Paul; Bernacki, Krzysztof; Boyle, Andrew W.; Butler, R. Paul; Caldwell, Douglas A.; Chontos, Ashley; Christianse, Jessie L.; Cia, David R.; Coll, Kevin I.; Conti, Dennis M.; Crane, Jeffrey D.; Daylan, Tansu; Dressing, Courtney D.; Eastman, Jason D.; Essack, Zahra; Evans, Phil; Everett, Mark E.; Fajardo-Acosta, Sergio; Fores-Toribio, Raquel; Furlan, Elise; Ghachoui, Mourad; Gillon, Michael; Hellier, Coel; Helm, Ian; Howard, Andrew W.; Howell, Steve B.; Isaacson, Howard; Jehin, Emmanuel; Jenkin, Jon M.; Jensen, Eric L. N.; Kielkopf, John F.; Laloum, Didier; Leonhardes-Barboza, Naunet; Lewin, Pablo; Logsdon, Sarah E.; Lubin, Jack; Lund, Michael B.; MacDougall, Mason G.; Mann, Andrew W.; Maslennikova, Natalia A.; Massey, Bob; McLeod, Kim K.; Munoz, Jose A.; Newman, Patrick; Orlov, Valeri; Plavchan, Peter; Popowicz, Adam; Pozuelos, Francisco J.; Pritchard, Tyler A.; Radford, Don J.; Reefe, Michael; Ricker, George R.; Rudat, Alexander; Safonov, Boris S.; Schwarz, Richard P.; Schweiker, Heidi; Scott, Nicholas J.; Seager, S.; Shectman, Stephen A.; Stockdale, Chris; Tan, Thiam-Guan; Teske, Johanna K.; Thomas, Neil B.; Timmermans, Mathilde; Vanderspek, Roland; Vermilion, David; Watanabe, David; Weiss, Lauren M.; West, Richard G.; Van Zandt, Judah; Zejmo, Michal; Ziegler, Carl.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., NASA's Transiting Exoplanet Survey Satellite (TESS) mission promises to improve our understanding of hot Jupiters by providing an all-sky, magnitude-limited sample of transiting hot Jupiters suitable for population studies. Assembling such a sample requires confirming hundreds of planet candidates with additional follow-up observations. Here we present 20 hot Jupiters that were detected using TESS data and confirmed to be planets through photometric, spectroscopic, and imaging observations coordinated by the TESS Follow-up Observing Program. These 20 planets have orbital periods shorter than 7 days and orbit relatively bright FGK stars (10.9 < G < 13.0). Most of the planets are comparable in mass to Jupiter, although there are four planets with masses less than that of Saturn. TOI-3976b, the longest-period planet in our sample (P = 6.6 days), may be on a moderately eccentric orbit (e = 0.18 ± 0.06), while observations of the other targets are consistent with them being on circular orbits. We measured the projected stellar obliquity of TOI-1937A b, a hot Jupiter on a 22.4 hr orbit with the Rossiter–McLaughlin effect, finding the planet's orbit to be well aligned with the stellar spin axis (∣λ∣ = 4fdg0 ± 3fdg5). We also investigated the possibility that TOI-1937 is a member of the NGC 2516 open cluster but ultimately found the evidence for cluster membership to be ambiguous. These objects are part of a larger effort to build a complete sample of hot Jupiters to be used for future demographic and detailed characterization work. © 2023. The Author(s). Published by the American Astronomical Society., J.H. acknowledges funding from NASA grant 80NSSC21K0335. This work was supported by an LSSTC Catalyst Fellowship awarded by LSST Corporation to T.D. with funding from the John Templeton Foundation grant ID No. 62192. K.K.M. acknowledges support from the New York Community Trustâs Fund for Astrophysical Research. N.L.-B. thanks the NASA Massachusetts Space Grant for support. A.A.B., N.A.M., and B.S.S. acknowledge the support of the Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). A.P. acknowledges grant BK-246/RAu-11/2022. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco)., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).

Direct-to-consumer genetic tests have become increasingly popular in the United States within the last few years. However, these tests pose many risks to the consumer, most notably privacy risks. A subset of these privacy risks involves the issue of company mergers, acquisitions, and sales. Many companies in the direct-to-consumer genetic testing market have privacy policies that contain a variation of a “business transfer” clause. These clauses specify that in the event the company goes through a business transition such as a sale, merger, or acquisition, the consumer’s personal information—including the consumer’s DNA—will be among the assets transferred. This Article explores the risks associated with these business transfer clauses as they relate to the consumer, and presents a solution to mitigate said risks. The solution lies in FTC v. Toysmart, wherein a toy company that filed for bankruptcy was restricted in selling its assets—which included its customers’ personal data— only to entities with the same interests as the toy company. This Article urges that the default interpretation standard of business transfer clauses track similarly such that a direct-to-consumer genetic testing company may only be sold to, merged with, or acquired by a company with the same or like interests.

Some legal theorists say that legal entrapment to commit a crime is incoherent. So far, there is no satisfactorily precise statement of this objection in the literature: it is obscure even as to the type of incoherence that is purportedly involved. (Perhaps consequently, substantial assessment of the objection is also absent.) We aim to provide a new statement of the objection that is more precise and more rigorous than its predecessors. We argue that the best form of the objection asserts that, in attempting to entrap, law-enforcement agents lapse into a form of practical incoherence that involves the attempt simultaneously to pursue contrary ends. We then argue that the objection, in this form, encompasses all cases of legal entrapment only if it is supplemented by appeal to the premise that law-enforcement agents have an absolute duty never to create crimes.

We report the discovery of ten short-period giant planets (TOI-2193A b, TOI-2207 b, TOI-2236 b, TOI-2421 b, TOI-2567 b, TOI-2570 b, TOI-3331 b, TOI-3540A b, TOI-3693 b, TOI-4137 b). All of the planets were identified as planet candidates based on periodic flux dips observed by NASA's Transiting Exoplanet Survey Satellite (TESS). The signals were confirmed to be from transiting planets using ground-based time-series photometry, high angular resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The ten newly discovered planets orbit relatively bright F and G stars ($G < 12.5$,~$T_\mathrm{eff}$ between 4800 and 6200 K). The planets' orbital periods range from 2 to 10~days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421 b is notable for being a Saturn-mass planet and TOI-2567 b for being a ``sub-Saturn'', with masses of $0.322\pm 0.073$ and $0.195\pm 0.030$ Jupiter masses, respectively. In most cases, we have little information about the orbital eccentricities. Two exceptions are TOI-2207 b, which has an 8-day period and a detectably eccentric orbit ($e = 0.17\pm0.05$), and TOI-3693 b, a 9-day planet for which we can set an upper limit of $e < 0.052$. The ten planets described here are the first new planets resulting from an effort to use TESS data to unify and expand on the work of previous ground-based transit surveys in order to create a large and statistically useful sample of hot Jupiters., 44 pages, 15 tables, 21 figures; revised version submitted to AJ

SEA, DMD, JEH and DM thank the ERC (EU FP7 Consolidator Grant 614290 “EXONMR”) for funding. SEA would like to thank the Royal Society and the Wolfson Foundation for a merit award. The National High Magnetic Field Laboratory is supported by National Science Foundation Cooperative Agreement DMR-1644779 and the State of Florida. We present an NMR crystallographic investigation of two as-made forms of the recently characterised gallophosphate GaPO-34A, which has an unusual framework composition with a Ga : P ratio of 7 : 6 and contains both hydroxide and fluoride anions and either 1-methylimidazolium or pyridinium as the structure-directing agent. We combine previously reported X-ray crystallographic data with solid-state NMR spectroscopy and periodic density functional theory (DFT) calculations to show that the structure contains at least three distinct types of disorder (occupational, compositional and dynamic). The occupational disorder arises from the presence of six anion sites per unit cell, but a total occupancy of these of five, leading to full occupancy of four sites and partial occupancy of the fifth and sixth (which are related by symmetry). The mixture of OH and F present leads to compositional disorder on the occupied anion sites, although the occupancy of some sites by F is calculated to be energetically unfavorable and signals relating to F on these sites are not observed by NMR spectroscopy, confirming that the compositional disorder is not random. Finally, a combination of high-field 71Ga NMR spectroscopy and variable-temperature 13C and 31P NMR experiments shows that the structure directing agents are dynamic on the microsecond timescale, which can be supported by averaging the 31P chemical shifts calculated with the SDA in different orientations. This demonstrates the value of an NMR crystallographic approach, particularly in the case of highly disordered crystalline materials, where the growth of large single crystals for conventional structure determination may not be possible owing to the extent of disorder present. Postprint

Dental, oral, and maxillofacial diseases are some of the most common problems in small animal veterinary practice. These conditions create significant pain as well as localized and potentially systemic infection. As such, the World Small Animal Veterinary Association (WSAVA) believes that un- and under treated oral and dental diseases pose a significant animal welfare concern. Dentistry is an area of veterinary medicine which is still widely ignored and is subject to many myths and misconceptions. Effective teaching of veterinary dentistry in the veterinary school is the key to progression in this field of veterinary medicine, and to the improvement of welfare for all our patients globally. These guidelines were developed to provide veterinarians with the information required to understand best practices for dental therapy and create realistic minimum standards of care. Using the three-tiered continuing education system of WSAVA, the guidelines make global equipment and therapeutic recommendations and highlight the anaesthetic and welfare requirements for small animal patients. This document contains information on common oral and dental pathologies, diagnostic procedures (an easily implementable and repeatable scoring system for dental health, dental radiography and radiology) and treatments (periodontal therapy, extractions). Further, there are sections on anaesthesia and pain management for dental procedures, home dental care, nutritional information, and recommendations on the role of the universities in improving veterinary dentistry. A discussion of the deleterious effects of anaesthesia free dentistry (AFD) is included, as this procedure is ineffective at best and damaging at worst. Throughout the document the negative effects of undiagnosed and/or treated dental disease on the health and well-being of our patients, and how this equates to an animal welfare issue, is discussed.

Ventures are often hesitant to accept corporate venture capital due to concerns of intellectual property misappropriation. This is likely to be especially true with startup stage ventures operating in weak intellectual property rights regimes. Drawing on transaction costs economics and game theory, we examine how corporate investors might alleviate concerns of misappropriation by establishing credible commitments to their corporate venture capital program, which discourages opportunistic behavior. We submit that corporate investors can demonstrate credible commitments through prior investment quantity and prior investment continuity, therefore increasing the chances of forming a corporate venture capital–venture investment relationship. Our findings—using data from 11,136 ventures, 300 corporate venture capital investors, and 1782 investments across 18 years—demonstrate that ventures are more likely to pair with corporate venture capital investors that have made a credible commitment to their corporate venture capital program. Also, we find evidence that both quantity and continuity possess an enhanced effect on alleviating fears of misappropriation when a startup venture operates in the same industry as a potential corporate venture capital partner; this is because the corporate venture capital investor possesses both the absorptive capacity to understand the venture’s intellectual property and complementary capabilities to beat them to market.

A synthesis method for the preparation of mixed manganese–ruthenium oxides is presented along with a detailed characterisation of the solids produced. The use of 1 M aqueous sulfuric acid mediates the redox reaction between KRuO\(_4\), KMnO\(_4\) and Mn\(^{2+}\) to form ternary oxides. At reaction temperature of 100°C the products are mixtures of α-MnO\(_2\) (hollandite-type) and β-MnO\(_2\) (rutile-type), with some evidence of Ru incorporation in each from their expanded unit cell volumes. At reaction temperature of 200°C solid-solutions β-Mn\(_{1−x}\)Ru\(_x\)O\(_2\) are formed and materials with x ≤ 0.6 have been studied. The amount of Ru included in the oxide is greater than expected from the ratio of metals used in the synthesis, as determined by elemental analysis, implying that some Mn remains unreacted in solution. Powder X-ray diffraction (XRD) shows that while the unit cell volume expands in a linear manner, following Vegard's law, the tetragonal lattice parameters, and the a/c ratio, do not follow the extrapolated trends: this anisotropic behaviour is consistent with the different local coordination of the metals in the end members. Powder XRD patterns show increased peak broadening with increasing ruthenium content, which is corroborated by electron microscopy that shows nanocrystalline material. X-ray absorption near-edge spectra show that the average oxidation state of Mn in the solid solutions is reduced below +4 while that of Ru is increased above +4, suggesting some redistribution of charge. Analysis of the extended X-ray absorption fine structure provides complementary local structural information, confirming the formation of a solid solution, while X-ray photoelectron spectroscopy shows that the surface oxidation states of both Ru and Mn are on average lower than +4, suggesting a disordered surface layer may be present in the materials.

Funding Acknowledgements Type of funding sources: Public grant(s) – EU funding. Main funding source(s): PIC from European Union"s Horizon 2020 Marie Skłodowska-Curie Actions ITN Background The wall thickness of the left ventricle (LV) is an important parameter in the diagnosis of hypertension and more specifically in hypertrophic cardiomyopathy. A user-dependent manual assessment of distances on 2D echocardiographic images is the current clinical gold-standard. Purpose The automation of LV wall thickness measurements in 2D echocardiography in order to improve robustness and reduce time of clinical reports where wall thickness is required, such as hypertrophy and the presence of Basal Septal Hypertrophy (BSH)(1). Methods A dataset of 4-chamber (4CH) echocardiograms on 118 patients with a diagnosis of hypertension (2) is used for this study. The images were segmented automatically (3) extracting the blood pool and the myocardium. Based on the curvature of the complete myocardial contour, the valve annular regions are removed leaving the endocardial and the epicardial walls as independent structures. The wall thickness along the myocardium is calculated as the distance from each endocardial border pixel to the closest epicardial point (see Figure 1). A high pass gaussian filter was applied to remove high frequency noise. Ultimately, the basal-to-mid septal wall thickness ratio that defines BSH (ratio ≥ 1.4) was computed as the maximal of basal-septal segment divided by minimum of mid-septal segment. In order to validate the method for BSH detection, the wall thickness septal ratio was carefully measured by a clinical expert following the guidelines (2). The statistical agreement was accessed via linear correlation and Bland-Altman analysis. Results The automatic assessment of LV wall thickness along the myocardium is feasible in 2D echocardiography. The septal ratio showed an excellent agreement with manual measurements (R2 = 0.94, bias=-0.01, see Figure 2), leading to a detection of BSH in n = 19 vs the n = 18 detected manually (1 false-negative and 2 false-positives). In comparison to the intra and inter-observer variabilities of 12% and 42% respectively in the manual measurement (4), the automatic method had no variability for a given image acquisition. Conclusions The automatic measurement of myocardial wall thickness from a 2D echocardiographic images is accurate and reproducible. The implementation of the methodology in clinical practise has the potential to improve and automate the assessment of hypertrophic cardiac conditions. Abstract Figure. Pipeline for automatic measurement of WT Abstract Figure. Agreement of BSH WT ratio

Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other mechanisms (e.g., primordial misalignment or planet-star interactions) are more important in sculpting the obliquity distribution. Here we present the stellar obliquity measurement of TOI-1268 (TIC-142394656, $V_{\rm mag} {\sim} 10.9$), a young K-type dwarf hosting an 8.2-day period, Saturn-sized planet. TOI-1268's lithium abundance and rotation period suggest the system age between the ages of Pleiades cluster (${\sim}120$ Myr) and Praesepe cluster (${\sim}670$ Myr). Using the newly commissioned NEID spectrograph, we constrain the stellar obliquity of TOI-1268 via the Rossiter-McLaughlin (RM) effect from both radial velocity (RV) and Doppler Tomography (DT) signals. The 3$\sigma$ upper bounds of the projected stellar obliquity $|\lambda|$ from both models are below 60$^\circ$. The large host star separation ($a/R_\star {\sim} 17$), combined with the system's young age, makes it unlikely that the planet has realigned its host star. The stellar obliquity measurement of TOI-1268 probes the architecture of a young gas giant beyond the reach of tidal realignment ($a/R_\star {\gtrsim} 10$) and reveals an aligned or slightly misaligned system., Comment: 14 pages, 6 figures, 1 table, accepted for publication in ApJL; see independent work by Subjak et al. for RV follow-up of TOI-1268

N.S., R.W. and B.-O.D. acknowledge support from the Swiss National Science Foundation (PP00P2-163967 and PP00P2-190080). M.N.G. acknowledges support from MIT's Kavli Institute as a Juan Carlos Torres Fellow and from the European Space Agency (ESA) as an ESA Research Fellow. A.A.B., B.S.S.and I.A.S. acknowledge the support of the Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). L.D. is an F.R.S.-FNRS Postdoctoral Researcher. B.V.R. thanks the Heising-Simons Foundation for support. This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to M.T. and E.J. acknowledges DGAPA for his postdoctoral fellowship. Y.G.M.C. acknowledges support from UNAM-DGAPA PAPIIT BG-101321. D.D. acknowledges support from the TESS Guest Investigator Program grant 80NSSC19K1727 and NASA Exoplanet Research Program grant 18-2XRP18_2-0136. We acknowledge support from the Centre for Space and Habitability (CSH) of the University of Bern. Part of this work received support from the National Centre for Competence in Research PlanetS, supported by the Swiss National Science Foundation (SNSF). Funding for the TESS mission is provided by NASA's Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). This work is based upon observations carried out at the Observatorio Astronomico Nacional on the Sierra de San Pedro Martir (OAN-SPM), Baja California, Mexico. We warmly thank the entire technical staff of the Observatorio Astronomico Nacional at San Pedro Martir in Mexico for their unfailing support to SAINT-EX operations, namely: E. Cadena, T. Calvario, E. Colorado, F. Diaz, A. Franco, B. Garcia, C. Guerrero, G. Guisa, F. Guillen, A. Landa, L. Figueroa, B. Hernandez, J. Herrera, E. Lopez, E. Lugo, B. Martinez, G. Melgoza, F. Montalvo, J.M. Nunez, J.L. Ochoa, I. Plauchu, F. Quiroz, H. Riesgo, H. Serrano, T. Verdugo, I. Zavala. The research leading to these results has received funding from the European Research Council (ERC) under the FP/2007-2013 ERC grant agreement nffi 336480, and under the European Union's Horizon 2020 research and innovation programme (grants agreements nffi 679030 and 803193/BEBOP); from an Actions de Recherche Concertee (ARC) grant, financed by the Wallonia-Brussels Federation, from the Balzan Prize Foundation, from the BEL-SPO/BRAIN2.0 research program (PORTAL project), from the Science and Technology Facilities Council (STFC; grant nffi ST/S00193X/1), and from F.R.S-FNRS (Research Project ID T010920F). This work was also partially supported by a grant from the Simons Foundation (PI: Queloz, grant number 327127), as well as by the MERAC foundation (PI: Triaud). PI: Gillon is F.R.S.-FNRS Senior Research Associate. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant PDR T.0120.21, with the participation of the Swiss National Science Fundation (SNF). M.G. and E.J. are F.R.S.-FNRS Senior Research Associate. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). M.S.I.P. is funded by NSF. Some of the observations in the paper made use of the High-Resolution Imaging instrument(s) `Alopeke (and/or Zorro). `Alopeke (and/or Zorro) was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Data were reduced using a software pipeline originally written by Elliott Horch and Mark Everett. `Alopeke (and/or Zorro) was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation, on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigacion y Desarrollo (Chile), Ministerio de Ciencia, Tecnologia e Innovacion (Argentina), Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of exoplanet (Foreman-Mackey et al. 2021a,b) and its dependencies (Agol et al. 2020; Kumar et al. 2019; Astropy Collaboration 2013, 2018; Kipping 2013; Luger et al. 2019; Salvatier et al. 2016; Theano Development Team 2016). Additional use of software packages AstroImageJ (Collins et al. 2017) and TAPIR (Jensen 2013)., Context. Thanks to the relative ease of finding and characterizing small planets around M-dwarf stars, these objects have become cornerstones in the field of exoplanet studies. The current paucity of planets in long-period orbits around M dwarfs makes such objects particularly compelling as they provide clues about the formation and evolution of these systems. Aims. In this study we present the discovery of TOI-2257 b (TIC 198485881), a long-period (35 d) sub-Neptune orbiting an M3 star at 57.8 pc. Its transit depth is about 0.4%, large enough to be detected with medium-size, ground-based telescopes. The long transit duration suggests the planet is in a highly eccentric orbit (e similar to 0.5), which would make it the most eccentric planet known to be transiting an M-dwarf star. Methods. We combined TESS and ground-based data obtained with the 1.0-meter SAINT-EX, 0.60-meter TRAPPIST-North, and 1.2-meter FLWO telescopes to find a planetary size of 2.2 R-circle plus and an orbital period of 35.19 days. In addition, we make use of archival data, high-resolution imaging, and vetting packages to support our planetary interpretation. Results. With its long period and high eccentricity, TOI-2257 b falls into a novel slice of parameter space. Despite the planet's low equilibrium temperature (similar to 256 K), its host star's small size (R-* = 0.311 +/- 0.015) and relative infrared brightness (K-mag = 10.7) make it a suitable candidate for atmospheric exploration via transmission spectroscopy., Swiss National Science Foundation (SNSF), European Commission PP00P2-163967 PP00P2-190080, MIT's Kavli Institute, European Space Agency European Commission, Ministry of Science and Higher Education of the Russian Federation 075-15-2020-780 (N13.1902.21.0039), Heising-Simons Foundation, French Community of Belgium, DGAPA, Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica (PAPIIT) Universidad Nacional Autonoma de Mexico BG-101321, TESS Guest Investigator Program 80NSSC19K1727, NASA Exoplanet Research Program 18-2XRP18_2-0136, Centre for Space and Habitability (CSH) of the University of Bern, European Research Council (ERC) 336480, Actions de Recherche Concertee (ARC) grant - Wallonia-Brussels Federation, UK Research & Innovation (UKRI), Science & Technology Facilities Council (STFC), Science and Technology Development Fund (STDF) ST/S00193X/1, Fonds de la Recherche Scientifique - FNRS T010920F, Simons Foundation 327127, MERAC foundation, Fonds de la Recherche Scientifique - FNRS PDR T.0120.21, National Science Foundation (NSF), NASA Exoplanet Exploration Program NASA's Science Mission Directorate, European Research Council (ERC) 679030 803193/BEBOP, Balzan Prize Foundation BEL-SPO/BRAIN2.0 research program (PORTAL project)

Context. The number of super-Earth and Earth-mass planet discoveries has increased significantly in the last two decades thanks to the Doppler radial velocity and planetary transit observing techniques. Either technique can detect planet candidates on its own, but the power of a combined photometric and spectroscopic analysis is unique for an insightful characterization of the planets, which in turn has repercussions for our understanding of the architecture of planetary systems and, therefore, their formation and evolution. Aims. Two transiting planet candidates with super-Earth radii around the nearby (d = 70.64 ± 0.06 pc) K7–M0 dwarf star TOI-1238 were announced by NASA’s Transiting Exoplanet Survey Satellite (TESS), which observed the field of TOI-1238 in four different sectors. We aim to validate their planetary nature using precise radial velocities taken with the CARMENES spectrograph. Methods. We obtained 55 CARMENES radial velocity measurements that span the 11 months between 9 May 2020 and 5 April 2021. For a better characterization of the parent star’s activity, we also collected contemporaneous optical photometric observations at the Joan Oró and Sierra Nevada observatories and retrieved archival photometry from the literature. We performed a combined TESS+CARMENES photometric and spectroscopic analysis by including Gaussian processes and Keplerian orbits to account for the stellar activity and planetary signals simultaneously. Results. We estimate that TOI-1238 has a rotation period of 40 ± 5 d based on photometric and spectroscopic data. The combined analysis confirms the discovery of two transiting planets, TOI-1238 b and c, with orbital periods of 0.764597−0.000011+0.000013 d and 3.294736−0.000036+0.000034 d, masses of 3.76−1.07+1.15 M⊕ and 8.32−1.88+1.90 M⊕, and radii of 1.21−0.10+0.11 R⊕ and 2.11−0.14+0.14 R⊕. They orbit their parent star at semimajor axes of 0.0137 ± 0.0004 au and 0.036 ± 0.001 au, respectively.The two planets are placed on opposite sides of the radius valley for M dwarfs and lie between the star and the inner border of TOI-1238’s habitable zone. The inner super-Earth TOI-1238 b is one of the densest ultra-short-period planets ever discovered (ρ = 11.7−3.4+4.2 g cm−3). The CARMENES data also reveal the presence of an outer, non-transiting, more massive companion with an orbital period and radial velocity amplitude of ≥600 d and ≥70 m s−1, which implies a likely mass of M ≥ 2 √(1− e2) MJup and a separation ≥1.1 au from its parent star. © ESO 2022., CARMENES is an instrument for the Centro Astronómico Hispano-Alemán de Calar Alto (CAHA, Almería, Spain). CARMENES is funded by the German Max-Planck- Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Científicas (CSIC), the European Union through FEDER/ERF funds, and the members of the CARMENES Consortium (Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Andalucía, Landessternwarte Koönigstuhl, Institut de Ciències de l’Espai, Insitut für Astrophysik Göttingen, Universidad, Complutense de Madrid, Thüringer Landessternwarte Tautenburg, Instituto de Astrofísica de Canarias, Hamburger Sternwarte, Centro de Astrobiología and Centro Astronómico Hispano-Alemán), with additional contributions by the Spanish Ministry of Economy, the state of Baden-Wüttemberg, the German Science Foundation (DFG), the Klaus Tschira Foundation (KTS), and by the Junta de Andalucía. This work was based on data from the CARMENES data archive at CAB (CSIC-INTA). This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA’s Science Mission Directorate. This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. Some of the observations in the paper made use of the High-Resolution Imaging instrument ‘Alopeke obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. ‘Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. ‘Alopeke was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed bythe Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). Data were partly collected with the 90 cm telescope at the Sierra Nevada Observatory (SNO) operated by the Instituto de Astrofí fica de Andalucí a (IAA-CSIC). We acknowledge the telescope operators from Observatori Astronómic del Montsec, Sierra Nevada Observatory, and Centro Astronómico Hispano-Alemán de Calar Alto (CAHA). E.G.A., M.R.Z.O., J.A.C., J.S.F, and D.M. acknowledge financial support from the Spanish Ministry of Science and Innovation through project PID2019-109522GBC5[1:4]. E.G.A also acknowledges support from AEI Project No. MDM-2017-0737 Unidad de Excelencia “María de Maeztu” – Centro de Astrobiología (CSIC-INTA). V.M.P. acknowledges financial support from NASA through grant NNX17AG24G. S.V.J. acknowledges the support of the DFG priority program SPP 1992 “Exploring the Diversity of Extrasolar Planets (JE 701/5-1)”. M.J.L.-G., E.R., C.R.-L., and P.J.A. acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación through projects PID2019-109522GB-C52, PID2019-107061GB-C64, PID2019-110689RB-100 and the Centre of Excellence Severo Ochoa Instituto de Astrofísica de Andalucía (SEV-2017-0709). G.M. received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 895525. S.S. and S.R. acknowledgesupport by the DFG Research Unit FOR 2544 Blue Planets around Red Stars, project no. RE 2694/4-1.

This chapter discusses the problematic issue of occult breast carcinoma. In considering the predicament of occult breast carcinoma, five clinical situations are similarly reviewed and discussed: management of breast carcinoma presenting as axillary nodal metastases in the absence of a clinically evident primary; carcinoma in the patient who presents with an incidental, serous nipple discharge in the absence of a palpable breast mass; carcinoma occurring in a benign fibroadenoma; hemorrhage into the breast resulting from trauma obscuring underlying carcinoma; and finally, Paget’s disease of the breast. In addition to melanoma and squamous cell carcinoma of the lung, other primary sites of origin to be considered when axillary nodal metastases are shown to contain metastatic adenocarcinoma are thyroid, renal cell, stomach, pancreas, colon, and ovary. After a careful history and physical examination, bilateral mammography should be the first screening test performed. Adenofibromas represent one of the two major classes of fibroepithelial tumors of the breast.

Submitted to European Journal of Political Theory: https://journals.sagepub.com/home/ept# We characterize, more precisely than before, what Rawls calls the “analytical” method of drawing up a list of basic liberties. This method employs one or more general conditions that, under any just social order whatever, putative entitlements must meet for them to be among the basic liberties encompassed, within some just social order, by Rawls’s first principle of justice (i.e., the liberty principle). We argue that the general conditions that feature in Rawls’s own account of the analytical method, which employ the notion of necessity, are too stringent. They ultimately fail to deliver as basic certain particular liberties that should be encompassed within any fully adequate scheme of liberties. To address this under-generation problem, we provide an amended general condition. This replaces Rawls’s necessity condition with a probabilistic condition and it appeals to the standard liberal prohibition on arbitrary coercion by the state. We defend our new approach both as apt to feature in applications of the analytical method and as adequately grounded in justice as fairness as Rawls articulates the theory’s fundamental ideas.

We report the discovery of an ultrahot Jupiter with an extremely short orbital period of $0.67247414\,\pm\,0.00000028$ days ($\sim$16 hr). The $1.347 \pm 0.047$ $R_{\rm Jup}$ planet, initially identified by the Transiting Exoplanet Survey Satellite (TESS) mission, orbits TOI-2109 (TIC 392476080): a $T_{\rm eff} \sim 6500$ K F-type star with a mass of $1.447 \pm 0.077$ $M_{\rm Sun}$, a radius of $1.698 \pm 0.060$ $R_{\rm Sun}$, and a rotational velocity of $v\sin i_* = 81.9 \pm 1.7$ km s$^{-1}$. The planetary nature of TOI-2109b was confirmed through radial velocity measurements, which yielded a planet mass of $5.02 \pm 0.75$ $M_{\rm Jup}$. Analysis of the Doppler shadow in spectroscopic transit observations indicates a well-aligned system, with a sky-projected obliquity of $\lambda = 1\overset{\circ}{.}7 \pm 1\overset{\circ}{.}7$. From the TESS full-orbit light curve, we measured a secondary eclipse depth of $731 \pm 46$ ppm, as well as phase-curve variations from the planet's longitudinal brightness modulation and ellipsoidal distortion of the host star. Combining the TESS-band occultation measurement with a $K_s$-band secondary eclipse depth ($2012 \pm 80$ ppm) derived from ground-based observations, we find that the dayside emission of TOI-2109b is consistent with a brightness temperature of $3631 \pm 69$ K, making it the second hottest exoplanet hitherto discovered. By virtue of its extreme irradiation and strong planet-star gravitational interaction, TOI-2109b is an exceptionally promising target for intensive follow-up studies using current and near-future telescope facilities to probe for orbital decay, detect tidally driven atmospheric escape, and assess the impacts of H$_2$ dissociation and recombination on the global heat transport., Comment: 30 pages, 17 figures, published in AJ

A synthesis method for the preparation of mixed manganese-ruthenium oxides is presented along with a detailed characterisation of the solids produced. The use of 1 M aqueous sulfuric acid mediates the redox reaction between KRuO4, KMnO4 and Mn2+ to form ternary oxides. At reaction temperature of 100 °C the products are mixtures of α-MnO2 (hollandite-type) and β-MnO2 (rutile-type), with some evidence of Ru incorporation in each from their expanded unit cell volumes. At reaction temperature of 200 °C solid-solutions β-Mn1-xRuxO2 are formed and materials with x ≤ 0.6 have been studied. The amount of Ru included in the oxide is greater than expected from the ratio of metals used in the synthesis, as determined by elemental analysis, implying that some Mn remains unreacted in solution. Powder X-ray diffraction (XRD) shows that while the unit cell volume expands in a linear manner, following Vegard's law, the tetragonal lattice parameters, and the a/c ratio, do not follow the extrapolated trends: this anisotropic behaviour is consistent with the different local coordination of the metals in the end members. Powder XRD patterns show increased peak broadening with increasing ruthenium content, which is corroborated by electron microscopy that shows nanocrystalline material. X-ray absorption near-edge spectra show that the average oxidation state of Mn in the solid solutions is reduced below +4 while that of Ru is increased above +4, suggesting some redistribution of charge. Analysis of the extended X-ray absorption fine structure provides complementary local structural information, confirming the formation of a solid solution, while X-ray photoelectron spectroscopy shows that the surface oxidation states of both Ru and Mn are on average lower than +4, suggesting a disordered surface layer may be present in the materials.

Despite extensive research on organizational virtue, our understanding about factors that promote virtue within organizations remains unclear. Drawing on upper echelon theory, we examine the relationship between five top management team (TMT) characteristics and organizational virtue orientation (OVO)—the integrated set of values and beliefs that support ethical traits and virtuous behaviors of an organization. Specifically, we utilize prospectuses of initial public offering (IPO) firms and 10-K post-IPO filings to explore how TMT composition with respect to member age, tenure, education, functional background, and gender influences OVO. Additionally, we examine the moderating effects of organizational size, and argue that the more expansive structures and processes associated with larger organizations diminish the main relationships. Our findings, using two sources of data, are consistent, but somewhat mixed in their support for our hypotheses. Overall, TMT characteristics do appear to influence OVO, but in more complex and counterintuitive ways than initially expected.

We present the discovery of TOI-1518b -- an ultra-hot Jupiter orbiting a bright star $V = 8.95$. The transiting planet is confirmed using high-resolution optical transmission spectra from EXPRES. It is inflated, with $R_p = 1.875\pm0.053\,R_{\rm J}$, and exhibits several interesting properties, including a misaligned orbit (${240.34^{+0.93}_{-0.98}}$ degrees) and nearly grazing transit ($b =0.9036^{+0.0061}_{-0.0053}$). The planet orbits a fast-rotating F0 host star ($T_{\mathrm{eff}} \simeq 7300$ K) in 1.9 days and experiences intense irradiation. Notably, the TESS data show a clear secondary eclipse with a depth of $364\pm28$ ppm and a significant phase curve signal, from which we obtain a relative day-night planetary flux difference of roughly 320 ppm and a 5.2$\sigma$ detection of ellipsoidal distortion on the host star. Prompted by recent detections of atomic and ionized species in ultra-hot Jupiter atmospheres, we conduct an atmospheric cross-correlation analysis. We detect neutral iron (${5.2\sigma}$), at $K_p = 157^{+68}_{-44}$ km s$^{-1}$ and $V_{\rm sys} = -16^{+2}_{-4}$ km s$^{-1}$, adding another object to the small sample of highly irradiated gas-giant planets with Fe detections in transmission. Detections so far favor particularly inflated gas giants with radii $\gtrsim 1.78\,R_{\rm J}$; although this may be due to observational bias. With an equilibrium temperature of $T_{\rm eq}=2492\pm38$ K and a measured dayside brightness temperature of $3237\pm59$ K (assuming zero geometric albedo), TOI-1518b is a promising candidate for future emission spectroscopy to probe for a thermal inversion., Comment: 25 pages, 11 figures, accepted to AJ

Surgical injury to the recurrent laryngeal nerve (RLN) is a significant complication of head and neck surgery due to the potential for significant, permanent functional disability. Originally recommended by Lahey in 1938, intraoperative identification and protection of the nerve, remains the gold standard for minimizing RLN injury. Over time however, less invasive mechanisms for monitoring and protecting the RLN during surgical procedures have been developed. One such method is the endotracheal Nerve Integrity Monitoring (NIM) system. Several techniques to determine accurate positioning of the NIMs device have been proposed, some are simpler, less invasive, and more accurate than others. This clinical prospective study of 176 patients showed a novel method to determine correct positioning of the NIM device using a train of four (TOF) electric stimulation. TOF electrical stimulation resulted in contraction of the musculature and vocal cords overlying the NIMs device. As such, it provided more accurate positioning of the NIM device compared to a commonly used Tap Test method, which taps the larynx, (p

We studied prevalence and predictors of meaningful self-reflection among surgical residents and with prompting/structured interventions, sought to improve/sustain resident skills.Residents from six programs recorded 1032 narrative self-reflective comments (120 residents), using a web-based platform. If residents identified something learned or to be improved, self-reflection was deemed meaningful. Independent variables PGY level, resident/surgeon gender, study site/Phase1: July2014-August2015 vs. Phase2: September2015-September2016) were analyzed.Meaningful self-reflection was documented in 40.6% (419/1032) of entries. PGY5's meaningfully self-reflected less than PGY1-4's, 26.1% vs. 49.6% (p = 0.002). In multivariate analysis, resident narratives during Phase 2 were 4.7 times more likely to engage in meaningful self-reflection compared to Phase1 entries (p 0.001). Iterative changes during Phase2 showed a 236% increase in meaningful self-reflection, compared to Phase1.Surgical residents uncommonly practice meaningful self-reflection, even when prompted, and PGY5/chief residents reflect less than more junior residents. Substantial/sustained improvements in resident self-reflection can occur with both training and interventions.

Background Gender and/or gender-stereotypes might influence surgical education. We hypothesized that female surgeons might focus their learning and teaching differently from male surgeons. Methods Residents and surgeons (multi-institutional) individually recorded preoperatively discussed learning objectives (LO) for matching cases. Narratives were classified as knowledge-based, skill-based, or attitude-based. Multinomial logistic regression analyses, LO = dependent variable; independent variables = resident/surgeon gender, PGY level, timing of entry-to-procedure date, and quarters-of-year. Results 727 LOs from 125 residents (41% female) and 49 surgeons (20% female) were classified. Female residents were 1.4 times more likely to select knowledge over skill. With female surgeons, residents were 1.6 and 2.1 times more likely to select knowledge over skill and attitude over skill than if the surgeon was male. PGY 4/5 residents chose attitude-based LOs over junior residents. Conclusion Resident, surgeon gender and year-of-training influence learning objectives. Whether this reflects gender stereotyping by residents or differences in attending teaching styles awaits further exploration.

Resident and curriculum evaluation require tracking surgical resident operative performance, yet what and when to measure remains unclear.From a multi-institutional database, we reviewed 611 resident/surgeon-paired assessments of ACGME Milestones and modified OPRS ratings for different cases and postgraduate years.Faculty Milestone ratings increased with each PGY (p=0.001) and correlated with resident self-ratings (ICC = 0.83). Mean OPRS scores increased in small increments with substantial intra-year variability. Progression among individual OPRS subcategories was not apparent from more global analyses. Interestingly, male faculty offered lower ratings than female faculty.Milestones and modified mean OPRS ratings suggest residents are learning, yet lack sufficient discrimination for promotion or curricular analysis. Differential progression through OPRS subcategories suggests a taxonomy of surgical learning that can be tailored to focus on different skills at each point in the training continuum. The effect of faculty gender on resident ratings awaits further study.

We present the discoveries of KELT-25b (TIC 65412605, TOI-626.01) and KELT-26b (TIC 160708862, TOI-1337.01), two transiting companions orbiting relatively bright, early A-stars. The transit signals were initially detected by the KELT survey, and subsequently confirmed by \textit{TESS} photometry. KELT-25b is on a 4.40-day orbit around the V = 9.66 star CD-24 5016 ($T_{\rm eff} = 8280^{+440}_{-180}$ K, $M_{\star}$ = $2.18^{+0.12}_{-0.11}$ $M_{\odot}$), while KELT-26b is on a 3.34-day orbit around the V = 9.95 star HD 134004 ($T_{\rm eff}$ =$8640^{+500}_{-240}$ K, $M_{\star}$ = $1.93^{+0.14}_{-0.16}$ $M_{\odot}$), which is likely an Am star. We have confirmed the sub-stellar nature of both companions through detailed characterization of each system using ground-based and \textit{TESS} photometry, radial velocity measurements, Doppler Tomography, and high-resolution imaging. For KELT-25, we determine a companion radius of $R_{\rm P}$ = $1.64^{+0.039}_{-0.043}$ $R_{\rm J}$, and a 3-sigma upper limit on the companion's mass of $\sim64~M_{\rm J}$. For KELT-26b, we infer a planetary mass and radius of $M_{\rm P}$ = $1.41^{+0.43}_{-0.51}$ $M_{\rm J}$ and $R_{\rm P}$ = $1.940^{+0.060}_{-0.058}$ $R_{\rm J}$. From Doppler Tomographic observations, we find KELT-26b to reside in a highly misaligned orbit. This conclusion is weakly corroborated by a subtle asymmetry in the transit light curve from the \textit{TESS} data. KELT-25b appears to be in a well-aligned, prograde orbit, and the system is likely a member of a cluster or moving group., 24 pages, 18 figures, 8 tables