We present a new technique to constrain the gravitational potential of a galaxy from the observed stellar mass surface density alone under a number of assumptions. It uses the classical Eddington inversion method to compute the phase-space distribution function (DF) needed for stars to reside in a given gravitational potential. In essence, each

While several thousand exoplanets are now confirmed, the number of known transiting warm Jupiters (10 d < period < 200 d) remains relatively small. These planets are generally believed to have formed outside the snowline and migrated to their current orbits. Because they are sufficiently distant from their host stars, they mitigate proximity

Aims. Mrk 421 was in its most active state around early 2010, which led to the highest TeV gamma-ray flux ever recorded from any active galactic nuclei (AGN). We aim to characterize the multiwavelength behavior during this exceptional year for Mrk 421, and evaluate whether it is consistent with the picture derived with data from other less

Context. Small bodies in Earth-like orbits, the Arjunas, are good targets for scientific exploration, and space mining or in situ resource utilization (ISRU) trials as they enable low-cost missions. The subset of these objects that experience recurrent temporarily captured flyby or orbiter episodes are among the best ranked in terms of

In the third APOKASC catalog, we present data for the complete sample of 15,808 evolved stars with APOGEE spectroscopic parameters and Kepler asteroseismology. We used 10 independent asteroseismic analysis techniques and anchor our system on fundamental radii derived from Gaia L and spectroscopic T eff. We provide evolutionary state, asteroseismic

We present results over an 11-year Solar cycle of cosmic antiprotons based on 1.1 × 10 6 events in the rigidity range from 1.00 to 41.9 GV. The p ¯ fluxes exhibit distinct properties. The magnitude of the p ¯ flux temporal variation is significantly smaller than those of p, e -, and e +. A hysteresis between the p ¯ fluxes and the p fluxes is