Such data are routinely collected with some large field imaging cameras that use multiple detectors and a separate filter for each of the detectors. The uncertainty in measured line parameters can be sharply reduced by using repeated observations of the same target field with filters that have overlapping passbands but differ slightly in central wavelength or wavelength dependence of the effective filter curve. This leads to substantial uncertainties in redshifts and fluxes that are derived from the observations with one specific narrowband filter.Īims. In most cases, the width of such filters is broader than typical line widths, and the throughput of the filters varies substantially within the bandpass.

High redshift star-forming galaxies are discovered routinely because of a flux excess in narrowband filters caused by an emission line. Tasca 3ĭark Cosmology Centre, Niels Bohr Institute, University ofĬopenhagen Southern Observatory, Karl-Schwarzschild-Straße 2, 85748Īix-Marseille Université, CNRS, LAM (Laboratoire d’AstrophysiqueĬontext. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes

Wavelength redshift equation