Aims: We present results from MUSE observations of the nearly face-on disk galaxy NGC 7742. This galaxy hosts a spectacular nuclear ring of enhanced star formation, which is unusual in that it is hosted by a non-barred galaxy, and because this star formation is most likely fuelled by externally accreted gas that counter-rotates with respect to its

An analysis of the bottom baryon decay Λb→J /ψ (→μ+μ- )Λ (→p π- ) is performed to measure the Λb polarization and three angular parameters in data from p p collisions at √{s }=7 and 8 TeV, collected by the CMS experiment at the Large Hadron Collider. The Λb polarization is measured to be 0.00 ±0.06 (stat )±0.06 (syst ) and the parity-violating

Data from heavy ion collisions suggest that the evolution of a parton shower is modified by interactions with the color charges in the dense partonic medium created in these collisions, but it is not known where in the shower evolution the modifications occur. The momentum ratio of the two leading partons, resolved as subjets, provides information

A measurement is presented of the associated production of a single top quark and a Z boson. The study uses data from proton-proton collisions at √{ s } = 13TeV recorded by the CMS experiment, corresponding to an integrated luminosity of 35.9 fb-1. Using final states with three leptons (electrons or muons), the tZq production cross section is

Normalized differential cross sections for top quark pair production are measured in the dilepton (e+e-, μ + μ -, and μ ∓e±) decay channels in proton-proton collisions at a center-of-mass energy of 13 TeV. The measurements are performed with data corresponding to an integrated luminosity of 2.1 fb-1 using the CMS detector at the LHC. The cross

In this paper we present MASCARA-2 b, a hot Jupiter transiting the mV = 7.6 A2 star HD 185603. Since early 2015, MASCARA has taken more than 1.6 million flux measurements of the star, corresponding to a total of almost 3000 h of observations, revealing a periodic dimming in the flux with a depth of 1.3%. Photometric follow-up observations were