Phantom matter (PM) offers a promising solution to the cosmological tensions between the Hubble parameter $ H_0 $ and the growth of large-scale structures (LSS). In this study, the authors explore a simplified version of the $ \Lambda $ XCDM model, which incorporates PM as a component of dark energy (DE). Unlike conventional phantom DE, PM satisfies the strong energy condition, characterized by positive pressure and negative energy density. This behavior allows PM to act as a transient 'phantom vacuum' that tunnels into the late universe before transitioning into a new de Sitter era, potentially enabling earlier structure formation. Using data from SNIa, cosmic chronometers, transverse BAO, large-scale structure, and Planck 2018 CMB, the authors find that the PM scenario significantly reduces the tensions between $ H_0 $ and LSS growth. The value of $ H_0 $ derived from their analysis is compatible with SH0ES measurements within less than $ 0.25\sigma $, and the LSS growth tension is nonexistent. Statistical information criteria strongly favor the PM solution, with the wXCDM model showing a $ \gtrsim 3\sigma $ preference over the $ \Lambda $ CDM model for low redshifts. The wXCDM model, which includes PM as a transient component and quintessence-like behavior for the subsequent phase, provides a better fit to the data than the $ \Lambda $ CDM. The PM component behaves as a phantom matter with $ w_X \lesssim -1 $, while the Y component behaves as quintessence with $ w_Y \gtrsim -1 $. The analysis shows that the PM phase is transient, with its influence diminishing as the universe transitions into a stable de Sitter phase. The results suggest that the composite DE models, particularly the wXCDM, offer a more accurate description of the universe's evolution than the standard $ \Lambda $ CDM model. The findings support the idea that the DE may be a composite fluid, with PM playing a key role in resolving the cosmological tensions.Phantom matter (PM) offers a promising solution to the cosmological tensions between the Hubble parameter $ H_0 $ and the growth of large-scale structures (LSS). In this study, the authors explore a simplified version of the $ \Lambda $ XCDM model, which incorporates PM as a component of dark energy (DE). Unlike conventional phantom DE, PM satisfies the strong energy condition, characterized by positive pressure and negative energy density. This behavior allows PM to act as a transient 'phantom vacuum' that tunnels into the late universe before transitioning into a new de Sitter era, potentially enabling earlier structure formation. Using data from SNIa, cosmic chronometers, transverse BAO, large-scale structure, and Planck 2018 CMB, the authors find that the PM scenario significantly reduces the tensions between $ H_0 $ and LSS growth. The value of $ H_0 $ derived from their analysis is compatible with SH0ES measurements within less than $ 0.25\sigma $, and the LSS growth tension is nonexistent. Statistical information criteria strongly favor the PM solution, with the wXCDM model showing a $ \gtrsim 3\sigma $ preference over the $ \Lambda $ CDM model for low redshifts. The wXCDM model, which includes PM as a transient component and quintessence-like behavior for the subsequent phase, provides a better fit to the data than the $ \Lambda $ CDM. The PM component behaves as a phantom matter with $ w_X \lesssim -1 $, while the Y component behaves as quintessence with $ w_Y \gtrsim -1 $. The analysis shows that the PM phase is transient, with its influence diminishing as the universe transitions into a stable de Sitter phase. The results suggest that the composite DE models, particularly the wXCDM, offer a more accurate description of the universe's evolution than the standard $ \Lambda $ CDM model. The findings support the idea that the DE may be a composite fluid, with PM playing a key role in resolving the cosmological tensions.