  We report new spectroscopic and photometric observations of the
main-sequence, detached, eccentric, double-lined eclipsing binary V541 Cyg (P =
15.34 days, e = 0.468). Using these observations together with existing
measurements we determine the component masses and radii to better than 1%
precision: M1 = 2.335 +0.017/-0.013 MSun, M2 = 2.260 +0.016/-0.013 MSun, R1 =
1.859 +0.012/-0.009 RSun, and R2 = 1.808 +0.015/-0.013 RSun. The nearly
identical B9.5 stars have estimated temperatures of 10650 +/- 200 K and 10350
+/- 200 K. A comparison of these properties with current stellar evolution
models shows excellent agreement at an age of about 190 Myr and [Fe/H]
approximately -0.18. Both components are found to be rotating at the
pseudo-synchronous rate. The system displays a slow periastron advance that is
dominated by General Relativity (GR), and has previously been claimed to be
slower than predicted by theory. Our new measurement, dw/dt = 0.859
+0.042/-0.017 deg/century, has an 88% contribution from GR and agrees with the
expected rate within the uncertainties. We also clarify the use of the gravity
darkening coefficients in the light-curve fitting program EBOP, a version of
which we use here.
