We introduce an updated To&Krause2021 model for joint analyses of cluster abundances and large-scale two-point correlations of weak lensing and galaxy and cluster clustering (termed CL + 3 × 2 pt analysis) and validate that this model meets the systematic accuracy requirements of analyses with the statistical precision of the final Dark Energy

Context. The millimetre spectrum of Galactic regions and galaxies is rich in continuum and molecular lines. This diversity is mostly explored using either broad-band photometry or high-resolution heterodyne spectroscopy. Aims. We aim to map the millimetre continuum emission of Galactic regions with an intermediate spectral resolution between

Determining the distribution of water throughout the main asteroid belt can inform us about the formation and evolution of the early Solar System. A powerful method for probing water abundance involves the observation and characterization of carbon-rich (C-complex) asteroids in the "3-μm region," which contains the fundamental OH stretching mode

Introduction: Trans-Neptunian Objects (TNOs) harbor materials from the early solar nebula (e.g., Gladman et al. 2008; Tegler et al. 2016). Observations from the NIRSpec instrument onboard the James Webb Space Telescope (JWST) included >50 TNOs during Cycle 1 for the large program "Discovering the Compositions of TNOs" (DiSCo-TNOs; #2418; PI: N

Primitive C-complex asteroids, primarily located in the main asteroid belt, are commonly associated with carbonaceous chondrites (CCs) due to their low geometric albedo (typically pv<10%) and similar spectral shape [e.g. 1]. The presence of hydrated minerals and organics in CCs attests to the accretion of volatiles by their parent body in the early

We present the results of time-resolved photometry, abundance analysis, and Doppler imaging of an Ap star, HD 100357. The TESS photometry revealed rotational modulation with a period of 1.6279247 d. Upon inspecting the residuals after removing the rotational period and its harmonics, we found additional frequencies around 15.8054 d $^{-1}$, which