Showing 261–280 of 1,145 results
/ Date/ Name
Dec 14, 2023Amplitude analysis of the $B^{0}\to K^{*0}μ^+μ^-$ decayDec 13, 2023IPA: Class 0 Protostars Viewed in CO Emission Using JWSTDec 8, 2023Seamless: Multilingual Expressive and Streaming Speech TranslationDec 6, 2023Bayesian estimation of cross-coupling and reflection systematics in 21cm array visibility dataDec 6, 2023The Initial Mass Function Based on the Full-sky 20-pc Census of $\sim$3,600 Stars and Brown DwarfsNov 30, 2023Evaluating the feasibility of short-integration scans based on the 2022 VGOS-R&D programNov 27, 2023The UV luminosity function at 0.6 < z < 1 from UVCANDELSNov 24, 2023Overview Of The 2023 Icassp Sp Clarity Challenge: Speech Enhancement For Hearing AidsNov 17, 2023A model-independent measurement of the CKM angle $γ$ in partially reconstructed $B^{\pm} \to D^{*} h^{\pm}$ decays with $D \to K_{S}^{0} h^{+}h^{-}$ $(h=π, K)$Nov 13, 2023Particle Identification at VAMOS++ with Machine Learning TechniquesNov 9, 2023Simulation of high-contrast polarimetric observations of debris disks with the Roman Coronagraph InstrumentNov 9, 2023Isoscaling in Dilute Warm Nuclear SystemsNov 8, 2023TESS photometry of the nova eruption in V606 Vul: asymmetric photosphere and multiple ejections?Nov 7, 2023Automated Mathematical Discovery and Verification: Minimizing Pentagons in the PlaneOct 25, 2023The GAPS programme at TNG XLIX. TOI-5398, the youngest compact multi-planet system composed of an inner sub-Neptune and an outer warm SaturnOct 23, 2023The FLASH pilot survey: an HI absorption search against MRC 1-Jy radio sourcesOct 21, 2023Discovery of a collimated jet from the low luminosity protostar IRAS 16253$-$2429 in a quiescent accretion phase with the JWSTOct 9, 2023Magnetic Field Properties inside the Jet of Mrk 421: Multiwavelength Polarimetry Including the Imaging X-ray Polarimetry ExplorerOct 6, 2023DeepSpeed4Science Initiative: Enabling Large-Scale Scientific Discovery through Sophisticated AI System TechnologiesOct 6, 2023Measurement of the CKM angle $γ$ using the $B^{\pm}\rightarrow D^{*} h^{\pm}$ channels