Mathematics – Logic
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21441404n&link_type=abstract
American Astronomical Society, AAS Meeting #214, #414.04; Bulletin of the American Astronomical Society, Vol. 41, p.681
Mathematics
Logic
Scientific paper
Many of the cosmological tests to be performed by planned dark energy experiments will require extremely well-characterized photometric redshift measurements. The true mean redshift of the objects in each photo-z bin must be known to better than 0.002(1+z) if errors in cosmological measurements are not to be degraded. A conventional approach is to calibrate these photometric redshifts with large sets of spectroscopic redshifts; however, at the depths probed by Stage III surveys (such as DES), let alone Stage IV (LSST, JDEM, Euclid), existing large redshift samples have all been highly (25-60%) incomplete, with a strong dependence of success rate on both redshift and galaxy properties; even a 1% failure rate would have catastrophic impact on dark energy inference. A powerful alternative approach is to exploit the clustering of galaxies to perform photometric redshift calibrations. Measuring the angular cross-correlation between objects in some photometric redshift bin and objects with known spectroscopic redshift, as a function of the spectroscopic z allows the true redshift distribution of a photometric sample to be reconstructed in detail, even if it includes objects too faint for spectroscopy or if spectroscopic samples are highly incomplete. In this poster, we present updated forecasts for the accuracy of this calibration technique for future dark energy experiments, based upon error models for correlation function measurements that are more realistic than those used previously.
Matthews Daniel J.
Newman Jeffrey
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