Cosmological constraints derived from galaxy clusters rely on accurate predictions of cluster observable properties , in which feedback from active galactic nuclei ( AGN ) is a critical component .
In order to model the physical effects due to supermassive black holes ( SMBH ) on cosmological scales , subgrid modeling is required , and a variety of implementations have been developed in the literature .
However , theoretical uncertainties due to model and parameter variations are not yet well understood , limiting the predictive power of simulations including AGN feedback .
By performing a detailed parameter sensitivity study in a single cluster using several commonly-adopted AGN accretion and feedback models with FLASH , we quantify the model uncertainties in predictions of cluster integrated properties .
We find that quantities that are more sensitive to gas density have larger uncertainties ( \sim 20 \% for M _ { gas } and a factor of \sim 2 for L _ { X } at R _ { 500 } ) , whereas T _ { X } , Y _ { SZ } , and Y _ { X } are more robust ( \sim 10 - 20 \% at R _ { 500 } ) .
To make predictions beyond this level of accuracy would require more constraints on the most relevant parameters : the accretion model , mechanical heating efficiency , and size of feedback region .
By studying the impact of AGN feedback on the scaling relations , we find that an anti-correlation exists between M _ { gas } and T _ { X } , which is another reason why Y _ { SZ } and Y _ { X } are excellent mass proxies .
This anti-correlation also implies that AGN feedback is likely to be an important source of intrinsic scatter in the M _ { gas } – T _ { X } and L _ { X } – T _ { X } relations .