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Inspired by the conundrum of the gravitational event, GW190814 which bringsto light the coalescence of a 23 $ M_{\odot}$ black hole with a yet to bedetermined secondary component, we look to modelling compact objects within theframework of $f(\mathcal{Q})$ gravity by employing the method of gravitationaldecoupling. We impose a quadratic equation of state (EOS) for the interiormatter distribution which in the appropriate limit reduces to the MIT bagmodel. The governing field equations arising from gravitational decouplingbifurcates into the $\rho=\theta^0_0$ and $p_r=\theta^1_1$ sectors leading totwo distinct classes of solutions. Both families of solutions are subjected torigorous tests qualifying them to describe a plethora of compact objectsincluding neutron stars, strange stars and the possible progenitor of thesecondary component of GW190814. Using observational data of mass-radiusrelations for compact objects LMC X-4, Cen X-3, PSR J1614-2230 and PSRJ0740+6620 we show that it is possible to generate stellar masses and radiibeyond 2.0 $ M_{\odot}$ for neutron stars. Our findings reveal that the most {suitable and versatile model in this framework is the quadratic EOS}, whichaccounts for a range of low mass stars as well as typical stellar candidatesdescribing the secondary component of GW190814.

The effect of gravitational decoupling on constraining the mass and  radius for the secondary component of GW190814 and other self-bound strange  stars in f(Q)-gravity theory