We measure the evolution of galaxy clustering out to a redshift of z \simeq 1.5 using data from two MUSYC fields , the Extended Hubble Deep Field South ( EHDF-S ) and the Extended Chandra Deep Field South ( ECDF-S ) .
We use photometric redshift information to calculate the projected-angular correlation function , \omega ( \sigma ) , from which we infer the projected correlation function \Xi ( \sigma ) .
We demonstrate that this technique delivers accurate measurements of clustering even when large redshift measurement errors affect the data .
To this aim we use two mock MUSYC fields extracted from a \Lambda CDM simulation populated with GALFORM semi-analytic galaxies which allow us to assess the degree of accuracy of our estimates of \Xi ( \sigma ) and to identify and correct for systematic effects in our measurements .
We study the evolution of clustering for volume limited subsamples of galaxies selected using their photometric redshifts and rest-frame r -band absolute magnitudes .
We find that the real-space correlation length r _ { 0 } of bright galaxies , M _ { r } < -21 ( rest-frame ) can be accurately recovered out to z \simeq 1.5 , particularly for ECDF-S given its near-infrared photometric coverage .
For these samples , the correlation length is consistent with a constant value of r _ { 0 } = ( 2.6 \pm 0.3 ) h ^ { -1 } Mpc for the ECDF-S field , and r _ { 0 } = ( 3.0 \pm 0.4 ) h ^ { -1 } Mpc for the EHDF-S field from a median redshift z _ { med } = 0.37 to z _ { med } = 1.15 .
There is mild evidence for a luminosity dependent clustering in both fields at the low redshift samples ( up to < z > = 0.57 ) , where the correlation length is higher for brighter galaxies by up to 1 Mpc / h between median rest-frame r-band absolute magnitudes of \sim - 18 to \sim - 21.5 .
As a result of the photometric redshift measurement , each galaxy is assigned a best-fit template ; we restrict to E and E +20 \% Sbc types to construct subsamples of early type galaxies ( ETGs ) .
These ETGs are separated into samples at different redshift intervals so that their passively evolved luminosities ( to z = 0 ) are comparable .
Our ETG samples show a strong increase in r _ { 0 } as the redshift increases , making it unlikely ( 95 \% level ) that ETGs at median redshift z _ { med } = 1.15 are the direct progenitors of ETGs at z _ { med } = 0.37 with equivalent passively evolved luminosities .