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Several theoretical proposals describe horizonless compact objects that can mimic black holes in their gravitational wave signatures; however, their spin-induced quadrupole moments (SIQMs) may reveal their distinct nature. Using the tight bounds on the SIQM of GW241011, we place constraints on the nature of its primary. Across exotic compact object models considered in this Letter, we find that rotating boson stars with quartic self-interactions cannot explain the nature of the primary, whereas models of sufficiently large compactness, <inline-formula><mml:math><mml:mi>C</mml:mi><mml:mo>≳</mml:mo><mml:mn>0.24</mml:mn></mml:math></inline-formula>, may still be viable contenders.