  Multi-wavelength monitoring of Mrk 335 with Swift between 2007-2019 are used
to construct annual spectral energy distributions and track year-to-year
changes. Non-contemporaneous archival data prior to 2007 are used to build a
bright state SED. In this work, the changes are examined and quantified to
build the foundation for future SED modelling. The yearly SEDs trace a downward
trend on the average, with the X-ray portion varying significantly and
acquiring further lower values in the past two years when compared to the
optical/UV portion of SED. The bolometric Eddington ratios derived using
optical/UV to X-ray SEDs and the calculated X-ray luminosities show a gradual
decrease over the monitoring period. Changes in the parameters over time are
examined. Principal component analysis suggests that the primary variability is
in the X-ray properties of Mrk 335. When looking at the broader picture of Mrk
335 and its behaviour, the X-rays, accounting most of the variability in the
13-year data, are possibly driven by physical processes related to the corona
or absorption whereas the modest optical-UV variations suggest their origin
within the accretion disc. These results are consistent with the previous
interpretation of Mrk 335 using the timing analyses on the monitoring data and
spectral modelling of deep observations.
