Aims: Our goal is to calculate the circular velocity curve of the Milky Way, along with corresponding uncertainties that quantify various sources of systematic uncertainty in a self-consistent manner. Methods: The observed rotational velocities are described as circular velocities minus the asymmetric drift. The latter is described by the radial

Massive stars are progenitors of supernovae, neutron stars and black holes. During the hydrogen-core burning phase, their convective cores are the prime drivers of their evolution, but inferences of core masses are subject to unconstrained boundary mixing processes. Moreover, uncalibrated transport mechanisms can lead to strong envelope mixing and

We compute the axion-pion scattering a π →π π , relevant for the axion thermalization rate in the early Universe, within unitarized next-to-leading-order chiral perturbation theory. The latter extends the range of validity of the chiral expansion of axion-pion scattering and thus provides a crucial ingredient for the reliable determination of the

The main objective of this work is to characterize relevant properties of the hot spots obtained in the interaction between ion beams of V23+ and a spherical pure precompressed deuterium-tritium plasmas in the field of ion fast ignition scheme. In particular, we focus our analysis on the determination of the length, average temperature and maximum

We perform a search for galaxy-galaxy strong lens systems using a convolutional neural network (CNN) applied to imaging data from the first public data release of the DECam Local Volume Exploration Survey, which contains ~520 million astronomical sources covering ~4000 deg2 of the southern sky to a 5σ point-source depth of g = 24.3, r = 23.9, i =

Zodiacal light (ZL) is sunlight scattered by interplanetary dust particles (IDPs) at optical wavelengths. The spatial distribution of IDPs in the Solar System may hold an important key to understanding the evolution of the Solar System and material transportation within it. The number density of IDPs can be expressed as n (r ) ∼r-α , and the