  Binary star systems are important for understanding stellar structure and
evolution, and are especially useful when oscillations can be detected and
analysed with asteroseismology. However, only four systems are known in which
solar-like oscillations are detected in both components. Here, we analyse the
fifth such system, HD 176465, which was observed by Kepler. We carefully
analysed the system's power spectrum to measure individual mode frequencies,
adapting our methods where necessary to accommodate the fact that both stars
oscillate in a similar frequency range. We also modelled the two stars
independently by fitting stellar models to the frequencies and complementary
parameters. We are able to cleanly separate the oscillation modes in both
systems. The stellar models produce compatible ages and initial compositions
for the stars, as is expected from their common and contemporaneous origin.
Combining the individual ages, the system is about 3.0$\pm$0.5 Gyr old. The two
components of HD 176465 are young physically-similar oscillating solar
analogues, the first such system to be found, and provide important constraints
for stellar evolution and asteroseismology.
