We present a measure of the hard (2Y8 keV ) X-ray luminosity function (XLF) of AGNs up to z $ 5. At high redshifts, the wide area coverage of the Chandra Multiwavength Project is crucial to detect rare and luminous (L X > 10 44 ergs s À1 ) AGNs. The inclusion of samples from deeper published surveys, such as the Chandra Deep Fields, allows us to span the lower L X range of the XLF. Our sample is selected from both the hard (z < 3, f 2Y8 keV > 6:3 ; 10 À16 ergs cm À2 s À1 ) and soft (z > 3, f 0:5Y2:0 keV > 1:0 ; 10 À16 ergs cm À2 s À1 ) energy band detections. Within our optical magnitude limits (r 0 ; i 0 < 24), we achieve an adequate level of completeness (>50%) regarding X-ray source identification (i.e., redshift). We find that the luminosity function is similar to that found in previous X-ray surveys up to z $ 3 with an evolution dependent on both luminosity and redshift. At z > 3, there is a significant decline in the numbers of AGNs with an evolution rate similar to that found by studies of optically selected QSOs. Based on our XLF, we assess the resolved fraction of the cosmic X-ray background, the cumulative mass density of SMBHs, and the comparison of the mean accretion rate onto SMBHs and the star formation history of galaxies as a function of redshift. A coevolution scenario up to z $ 2 is plausible, although at higher redshifts the accretion rate onto SMBHs drops more rapidly. Finally, we highlight the need for better statistics of high-redshift AGNs at z k 3, which is achievable with the upcoming Chandra surveys.

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