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A porous Co‐based metal‐oxide foam catalyst is fabricated via the dynamic hydrogen bubble template electrodeposition method followed by calcination (6 h at 300 °C thermal treatment). Electrolysis results demonstrate excellent performance of this catalyst in the electrochemical nitrate reduction reaction (NO3−RR ${\\mathrm{NO}}_3^ - {\\mathrm{RR}}$ ), attaining near‐unity Faradaic efficiency (97.8% ± 3.6% at jNH3,lim = –59.5 ± 2.3 mA cm−2) at a low (over)potential of –0.2 V vs RHE, which represents maximum achievable performance in 0.1 mol L−1 nitrate solutions (pH 13.7) under transport‐limiting conditions in the absence of extra convection. Digital simulations show that, without forced convection, the catalyst's electrochemically active surface area changes dynamically due to rapid nitrate depletion inside the 3D foam. Electrolyte replenishment, triggered by vigorous hydrogen evolution, is shown to restore the active surface in the foam interior. This self‐convection enables high ammonia partial current densities exceeding hundreds of mA cm−2 (e.g., jNH3 = –220 ± 18 mA cm−2 at –0.6 V vs RHE, with FENH3 = 80.2% ± 2.2%). Operando XAS, XRD, Raman spectroscopy, and electrochemical analysis reveal the in situ evolution of a “tandem” composite catalyst during electrolysis, where β‐Co(OH)2 and metallic Co function both as the active phases for NO3−RR ${\\mathrm{NO}}_3^ - {\\mathrm{RR}}$ , with β‐Co(OH)2 remaining kinetically stabilized under the cathodic operating conditions. A porous cobalt‐based metal‐oxide foam catalyst is synthesized using the DHBT technique, followed by calcination. It demonstrates exceptional activity for e‐NO3RR, reaching near‐unity ammonia selectivity at low overpotentials. Dynamic surface area changes due to NO3‐ depletion are mitigated by “self‐convection” during hydrogen evolution. Operando analyses reveal the formation of highly active “tandem catalyst”— β‐Co(OH)2 and metallic Co serving as a stable active phase under reaction conditions.

Extraintestinal manifestations (EIMs) are frequently observed in IBDs and contribute considerably to morbidity and mortality. They have long been considered a difficult to treat entity due to limited therapy options, but the increasing use of anti-tumour necrosis factors has dramatically changed the therapeutic approach to EIM in recent years. Newly emerging therapies such as JAK inhibitors and anti-interleukin 12/23 will further shape the available armamentarium. Clinicians dealing with EIMs in everyday IBD practice may be puzzled by the numerous available biological agents and small molecules, their efficacy for EIMs and their potential off-label indications. Current guidelines on EIMs in IBD do not include treatment algorithms to help practitioners in the treatment decision-making process. Herein, we summarise knowledge on emerging biological treatment options and small molecules for EIMs, highlight current research gaps, provide therapeutic algorithms for EIM management and shed light on future strategies in the context of IBD-related EIMs.

To the Editor: The Case Record discussed by Hoppin et al. (Oct. 12 issue), 1 which describes the condition of a severely obese 15-year-old girl, concludes with a diagnosis of “severe childhood obesity with obstructive sleep apnea, hypertension, impaired glucose tolerance progressing to type 2 diabetes mellitus, the polycystic ovary syndrome, and nonalcoholic steatohepatitis.” However, this case seems to present an unsolved medical problem. A number of the clinical signs may have been the consequence of an unexplained metabolic syndrome, probably related to the severe obesity. Why was this child so severely obese by the age of 3 years that she . . .

The CHaracterising ExOPlanet Satellite (CHEOPS) is a partnership between the European Space Agency and Switzerland with important contributions by 10 additional ESA member States. It is the first S-class mission in the ESA Science Programme. CHEOPS has been flying on a Sun-synchronous low Earth orbit since December 2019, collecting millions of short-exposure images in the visible domain to study exoplanet properties. A small yet increasing fraction of CHEOPS images show linear trails caused by resident space objects crossing the instrument field of view. To characterize the population of satellites and orbital debris observed by CHEOPS, all and every science images acquired over the past 3 years have been scanned with a Hough transform algorithm to identify the characteristic linear features that these objects cause on the images. Thousands of trails have been detected. This statistically significant sample shows interesting trends and features such as an increased occurrence rate over the past years as well as the fingerprint of the Starlink constellation. The cross-matching of individual trails with catalogued objects is underway as we aim to measure their distance at the time of observation and deduce the apparent magnitude of the detected objects. As space agencies and private companies are developing new space-based surveillance and tracking activities to catalogue and characterize the distribution of small debris, the CHEOPS experience is timely and relevant. With the first CHEOPS mission extension currently running until the end of 2026, and a possible second extension until the end of 2029, the longer time coverage will make our dataset even more valuable to the community, especially for characterizing objects with recurrent crossings.

We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by \\(\\sim\\) 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 \\(\\pm\\) 0.08 R\\(_\\oplus\\) and a period of 10.924709 \\(\\pm\\) 0.000032 days, whilst HD 15906 c has a radius of 2.93\\(^{+0.07}_{-0.06}\\) R\\(_\\oplus\\) and a period of 21.583298\\(^{+0.000052}_{-0.000055}\\) days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 \\(\\pm\\) 13 K and 532 \\(\\pm\\) 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm (\\(\\lesssim\\) 700 K) sub-Neptune sized planets transiting a bright star (G \\(\\leq\\) 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution.

We report the discovery and characterisation of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in TESS photometry. To characterise the system, we performed and retrieved CHEOPS, TESS, and ground-based photometry, HARPS high-resolution spectroscopy, and Gemini speckle imaging. We characterise the host star and determine \\(T_{\\rm eff, \\star}=4734\\pm67\\) K, \\(R_{\\star}=0.726\\pm0.007\\) \\(R_{\\odot}\\), and \\(M_{\\star}=0.748\\pm0.032\\) \\(M_{\\odot}\\). We present a novel detrending method based on PSF shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of \\(P_{\\rm b}=6.44387\\pm0.00003\\) d, a radius of \\(R_{\\rm b}=2.59\\pm0.04\\) \\(R_{\\oplus}\\), and a mass of \\(M_{\\rm b}=13.5_{-1.8}^{+1.7}\\) \\(M_{\\oplus}\\), whilst TOI-1064 c has an orbital period of \\(P_{\\rm c}=12.22657^{+0.00005}_{-0.00004}\\) d, a radius of \\(R_{\\rm c}=2.65\\pm0.04\\) \\(R_{\\oplus}\\), and a 3\\(\\sigma\\) upper mass limit of 8.5 \\({\\rm M_{\\oplus}}\\). From the high-precision photometry we obtain radius uncertainties of \\(\\sim\\)1.6%, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterised sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further RVs are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b are important for planets in this region of mass-radius space, and it allows us to identify a trend in bulk density-stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets.

The CHaracterising ExOPlanet Satellite (CHEOPS) was selected in 2012, as the first small mission in the ESA Science Programme and successfully launched in December 2019. CHEOPS is a partnership between ESA and Switzerland with important contributions by ten additional ESA Member States. CHEOPS is the first mission dedicated to search for transits of exoplanets using ultrahigh precision photometry on bright stars already known to host planets. As a follow-up mission, CHEOPS is mainly dedicated to improving, whenever possible, existing radii measurements or provide first accurate measurements for a subset of those planets for which the mass has already been estimated from ground-based spectroscopic surveys and to following phase curves. CHEOPS will provide prime targets for future spectroscopic atmospheric characterisation. Requirements on the photometric precision and stability have been derived for stars with magnitudes ranging from 6 to 12 in the V band. In particular, CHEOPS shall be able to detect Earth-size planets transiting G5 dwarf stars in the magnitude range between 6 and 9 by achieving a photometric precision of 20 ppm in 6 hours of integration. For K stars in the magnitude range between 9 and 12, CHEOPS shall be able to detect transiting Neptune-size planets achieving a photometric precision of 85 ppm in 3 hours of integration. This is achieved by using a single, frame-transfer, back-illuminated CCD detector at the focal plane assembly of a 33.5 cm diameter telescope. The 280 kg spacecraft has a pointing accuracy of about 1 arcsec rms and orbits on a sun-synchronous dusk-dawn orbit at 700 km altitude. The nominal mission lifetime is 3.5 years. During this period, 20% of the observing time is available to the community through a yearly call and a discretionary time programme managed by ESA.