  Objects transiting near or within the disruption radius of both main sequence
(e.g. KOI 1843) and white dwarf (WD 1145+017) stars are now known. Upon
fragmentation or disintegration, these planets or asteroids may produce
co-orbital configurations of nearly equal-mass objects. However, as evidenced
by the co-orbital objects detected by transit photometry in the WD 1145+017
system, these bodies are largely unconstrained in size, mass, and total number
(multiplicity). Motivated by potential future similar discoveries, we perform
N-body simulations to demonstrate if and how debris masses and multiplicity may
be bounded due to second-to-minute deviations and the resulting accumulated
phase shifts in the osculating orbital period amongst multiple co-orbital equal
point masses. We establish robust lower and upper mass bounds as a function of
orbital period deviation, but find the constraints on multiplicity to be weak.
We also quantify the fuzzy instability boundary, and show that mutual
collisions occur in less than 5%, 10% and 20% of our simulations for masses of
10^{21}, 10^{22} and 10^{23} kg. Our results may provide useful initial rough
constraints on other stellar systems with multiple co-orbital bodies.
