Other
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21933105m&link_type=abstract
American Astronomical Society, AAS Meeting #219, #331.05
Other
Scientific paper
The combination of photometric and spectroscopic surveys in the same region of sky provides powerful tools for studying cosmology and galaxy evolution. We have previously demonstrated that via cross-correlation techniques, photometric redshifts for future dark energy surveys can be calibrated to the necessary accuracy using spectroscopy only of the brightest objects at a given z. Another area where such complementary datasets can be particularly useful is in the analysis of high-redshift galaxy samples. A key challenge in identifying high redshift galaxies photometrically is distinguishing them from lower-redshift (z 2) interlopers with similar broadband colors. In the past these interlopers have generally been identified via extremely deep imaging at other bands or via spectroscopy. However, for the faint dropout samples now being identified using WFC3, both of these avenues become less practical. A powerful alternative is to exploit the clustering of galaxies to determine the interloper fraction. Low redshift interlopers will cluster with easier-to-identify, bright low-redshift objects, whereas true high-redshift galaxies will not. Hence, by measuring the two-point angular cross-correlation between objects in a sample of high-z candidates and objects with known spectroscopic redshifts, we can constrain the interloper fraction for samples too faint for spectroscopy. With coarse priors on galaxy biasing (e.g. assuming observed trends of bias with color and luminosity extend to fainter galaxies at low redshift), the interloper fraction can be determined even if spectroscopic samples do not cover the full redshift range of the high-z candidates. This technique can be useful for measuring interloper fractions in new surveys of the high-redshift universe such as the CANDELS Multi-Cycle Treasury Program on the Hubble Space Telescope.
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