The Pau Survey: An Improved Photo-Z Sample In The Cosmos Field

We present - and make publicly available - accurate and precise photometric redshifts in the ACS footprint from the COSMOS field for objects with i(AB) <= 23. The redshifts are computed using a combination of narrow-band photometry from PAUS, a survey with 40 narrow bands spaced at 100 angstrom intervals covering the range from 4500 to 8500 angstrom, and 26 broad, intermediate, and narrow bands covering the UV, visible and near-infrared spectrum from the COSMOS2015 catalogue. We introduce a new method that models the spectral energy distributions as a linear combination of continuum and emission-line templates and computes its Bayes evidence, integrating over the linear combinations. The correlation between the UV luminosity and the Oii line is measured using the 66 available bands with the zCOSMOS spectroscopic sample, and used as a prior which constrains the relative flux between continuum and emission-line templates. The flux ratios between the Oii line and H-alpha, H-beta and are similarly measured and used to generate the emission-line templates. Comparing to public spectroscopic surveys via the quantity Delta(z) equivalent to (z(photo) - z(spec))/(1 + z(spec)), we find the photometric redshifts to be more precise than previous estimates, with sigma(68)(Delta(z)) approximate to (0.003, 0.009) for galaxies at magnitude i(AB) similar to 18 and i(AB) similar to 23, respectively, which is three times and 1.66 times tighter than COSMOS2015. Additionally, we find the redshifts to be very accurate on average, yielding a median of the Delta(z) distribution compatible with vertical bar median(Delta(z))vertical bar <= 0.001 at all redshifts and magnitudes considered. Both the added PAUS data and new methodology contribute significantly to the improved results. The catalogue produced with the technique presented here is expected to provide a robust redshift calibration for current and future lensing surveys, and allows one to probe galaxy formation physics in an unexplored luminosity-redshift regime, thanks to its combination of depth, completeness, and excellent redshift precision and accuracy.