ASTROMETRIC REDSHIFTS FOR QUASARS

The wavelength dependence of atmospheric refraction causes differential chromatic refraction (DCR), whereby objects imaged at different optical/ultraviolet wavelengths are observed at slightly different positions in the plane of the detector. Strong spectral features induce changes in the effective wavelengths of broad-band filters that are capable of producing significant positional offsets with respect to standard DCR corrections. We examine such offsets for broad-emission-line (type 1) quasars from the Sloan Digital Sky Survey (SDSS) spanning 0 < z < 5 and an airmass range of 1.0-1.8. These offsets are in good agreement with those predicted by convolving a composite quasar spectrum with the SDSS bandpasses as a function of redshift and airmass. This astrometric information can be used to break degeneracies in photometric redshifts of quasars (or other emission-line sources) and, for extreme cases, may be suitable for determining 'astrometric redshifts'.On the SDSS's southern equatorial stripe, where it is possible to average many multi-epoch measurements, more than 60% of the quasars have emission-line-induced astrometric offsets larger than the SDSS's relative astrometric errors of 25-35 mas. Folding these astrometric offsets into photometric redshift estimates yields an improvement of 9% within Δz ± 0.1. Future multi-epoch synoptic surveys such as LSST and Pan-STARRS could benefit from intentionally making ∼10 observations at relatively high airmass (AM ∼ 1.4) in order to improve their photometric redshifts for quasars.