Context : The population of near-Earth asteroids ( NEAs ) shows a large variety of objects in terms of physical and dynamical properties .
They are subject to planetary encounters and to strong solar wind and radiation effects .
Their study is also motivated by practical reasons regarding space exploration and long-term probability of impact with the Earth .

Aims : We aim to spectrally characterize a significant sample of NEAs with sizes in the range of \sim 0.25 - 5.5 km ( categorized as large ) , and search for connections between their spectral types and the orbital parameters .

Methods : Optical spectra of NEAs were obtained using the Isaac Newton Telescope ( INT ) equipped with the IDS spectrograph .
These observations are analyzed using taxonomic classification and by comparison with laboratory spectra of meteorites .

Results : A total number of 76 NEAs were observed .
We spectrally classified 44 of them as Q/S-complex , 16 as B/C-complex , eight as V-types , and another eight belong to the remaining taxonomic classes .
Our sample contains 27 asteroids categorized as potentially hazardous and 31 possible targets for space missions including ( 459872 ) 2014 EK24 , ( 436724 ) 2011 UW158 , and ( 67367 ) 2000 LY27 .
The spectral data corresponding to ( 276049 ) 2002 CE26 and ( 385186 ) 1994 AW1 shows the 0.7 \mu m feature which indicates the presence of hydrated minerals on their surface .
We report that Q-types have the lowest perihelia ( a median value and absolute deviation of 0.797 \pm 0.244 AU ) and are systematically larger than the S-type asteroids observed in our sample .
We explain these observational evidences by thermal fatigue fragmentation as the main process for the rejuvenation of NEA surfaces .

Conclusions : In general terms , the taxonomic distribution of our sample is similar to the previous studies and matches the broad groups of the inner main belt asteroids .
Nevertheless , we found a wide diversity of spectra compared to the standard taxonomic types .