Only DY Persei itself was known in our galaxy until 2008 when systematic catalogue searches for R CrB variables discovered a 17th magnitude (at maximum) example.
[1] Since then automated searches have confirmed another four, including one of magnitude 5.9 at maximum.
[2] There are also several candidates that have not yet been observed to fade, and several DY Per stars in the Large Magellanic Cloud.
[3] Although DY Persei variables have been considered a subset of the R CrB variables because of their irregular fades and carbon-rich spectra, they may simply be an unusual type of carbon star unrelated to the more massive and more luminous R CrB variables.
The fades may be caused by obscuring ejection events rather than carbon condensation in the atmospheres of the stars.