Confirmation of Planet-mass Objects in Extragalactic Systems
Quasar microlensing serves as a unique probe of discrete objects within galaxies and galaxy clusters. Recent advancement of the technique shows that it can constrain planet-scale objects beyond our native galaxy by studying their induced microlensing signatures, the energy shift of emission lines originating in the vicinity of the black hole of high redshift background quasars. We employ this technique to exert effective constraints on the planet-mass object distribution within two additional lens systems, Q J0158−4325 (zl = 0.317) and SDSS J1004+4112 (zl = 0.68), using Chandra observations of the two gravitationally lensed quasars. The observed variations of the emission line peak energy can be explained as microlensing of the FeKα emission region induced by planet-mass microlenses. To corroborate this, we perform microlensing simulations to determine the probability of a caustic transiting the source region and compare this with the observed line shift rates. Our analysis yields constraints on the substellar population, with masses ranging from Moon (10−8 M⊙) to Jupiter (10−3 M⊙) sized bodies, within these galaxy or cluster scale structures, with total mass fractions of ∼3 × 10−4 and ∼1 × 10−4 with respect to halo mass for Q J0158−4325 and SDSS J1004+4112, respectively. Our analysis suggests that unbound planet-mass objects are universal in galaxies, and we surmise the objects to be either free-floating planets or primordial black holes. We present the first ever constraints on the substellar mass distribution in the intracluster light of a galaxy cluster. Our results provide the most stringent limit on the mass fraction of primordial black holes at the mass range.