  KIC 12557548 b is first of a growing class of intriguing disintegrating
planet candidates, which lose mass in the form of a metal rich vapor that
condenses into dust particles. Here, we follow up two perplexing observations
of the system: 1) the transits appeared shallower than average in 2013 and 2014
and 2) the parameters derived from a high resolution spectrum of the star
differed from other results using photometry and low resolution spectroscopy.
We observe 5 transits of the system with the 61-inch Kuiper telescope in 2016
and show that they are consistent with photometry from the Kepler spacecraft in
2009-2013, suggesting that the dusty tail has returned to normal length and
mass. We also evaluate high resolution archival spectra from the Subaru HDS
spectrograph and find them to be consistent with a main-sequence Teff=4440 +/-
70 K star in agreement with the photometry and low resolution spectroscopy.
This disfavors the hypothesis that planet disintegration affected the analysis
of prior high resolution spectra of this star. We apply Principal Component
Analysis to the Kepler long cadence data to understand the modes of
disintegration. There is a tentative 491 day periodicity of the second
principal component, which corresponds to possible long-term evolution of the
dust grain sizes, though the mechanism on such long timescales remains unclear.
