In this work , we examine the possibility of using the diffuse supernova neutrino background ( DSNB ) to test the Chaplygin gas ( CG ) models of the Universe .
With a typical supernova rate R _ { \mathrm { SN } } ( z ) and supernova neutrino spectrum \mathrm { d } N ( E _ { \nu } ) / \mathrm { d } E _ { \nu } , the DSNB flux spectrum n ( E _ { \nu } ) in three categories of CG models , the generalized CG ( GCG ) , modified CG ( MCG ) and extended CG ( ECG ) models , are studied .
It is found that generally the flux spectra take a form similar to a Fermi-Dirac distribution with a peak centered around 3.80-3.97 MeV .
The spectrum shape and peak positions are primarily determined by R _ { \mathrm { SN } } ( z ) and \mathrm { d } N ( E _ { \nu } ) / \mathrm { d } E _ { \nu } and only slightly affected by the CG models .
However , the height of the spectra in each category of the CG models can vary dramatically for different models , with variances of 13.2 % , 23.6 % and 14.9 % for GCG , MCG and ECG categories respectively .
The averaged total flux in each category are also different , with the ECG model average 10.0 % and 12.7 % higher than that of the GCG and MCG models .
These suggest that the DSNB flux spectrum height and total flux can be used to constrain the CG model parameters , and if the measured to a sub-10 % accuracy , might be used to rule out some models .