  RW Aur is a young binary star that experienced a deep dimming in 2010-11 in
component A and a second even deeper dimming from summer 2014 to summer 2016.
We present new unresolved multi-band photometry during the 2014-16 eclipse, new
emission line spectroscopy before and during the dimming, archive infrared
photometry between 2014-15, as well as an overview of literature data.
  Spectral observations were carried out with the Fibre-fed RObotic Dual-beam
Optical Spectrograph on the Liverpool Telescope. Photometric monitoring was
done with the Las Cumbres Observatory Global Telescope Network and James
Gregory Telescope. Our photometry shows that RW Aur dropped in brightness to R
= 12.5 in March 2016. In addition to the long-term dimming trend, RW Aur is
variable on time scales as short as hours. The short-term variation is most
likely due to an unstable accretion flow. This, combined with the presence of
accretion-related emission lines in the spectra suggest that accretion flows in
the binary system are at least partially visible during the eclipse.
  The equivalent width of [O I] increases by a factor of ten in 2014,
coinciding with the dimming event, confirming previous reports. The
blue-shifted part of the $H\alpha$ profile is suppressed during the eclipse. In
combination with the increase in mid-infrared brightness during the eclipse
reported in the literature and seen in WISE archival data, and constraints on
the geometry of the disk around RW Aur A we arrive at the conclusion that the
obscuring screen is part of a wind emanating from the inner disk.
