  Among the low-mass pre-main sequence stars, a small group called FU
Orionis-type objects (FUors) are notable for undergoing powerful accretion
outbursts. V1057 Cyg, a classical example of an FUor, went into outburst around
1969-1970, after which it faded rapidly, making it the fastest fading FUor
known. Around 1995, a more rapid increase in fading occurred. Since that time,
strong photometric modulations have been present. We present nearly 10 years of
source monitoring at Piszk\'estet\H{o} Observatory, complemented with
optical/near-infrared photometry and spectroscopy from the Nordic Optical
Telescope, Bohyunsan Optical Astronomy Observatory, Transiting Exoplanet Survey
Satellite, and the Stratospheric Observatory for Infrared Astronomy. Our light
curves show continuation of significant quasi-periodic variability in
brightness over the past decade. Our spectroscopic observations show strong
wind features, shell features, and forbidden emission lines. All of these
spectral lines vary with time. We also report the first detection of [S II], [N
II], and [O III] lines in the star.
