Open AccessThe KX method for producing K ‐band flux‐limited samples of quasars
Author(s) -
Warren S. J.,
Hewett P. C.,
Foltz C. B.
Publication year - 2000
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2000.03206.x
Subject(s) - quasar , physics , astrophysics , galaxy , population , extinction (optical mineralogy) , ovv quasar , astronomy , flux (metallurgy) , stars , wavelength , spectral line , optics , demography , materials science , sociology , metallurgy
The longstanding question of the extent to which the quasar population is affected by dust extinction, within host galaxies or galaxies along the line of sight, remains open. More generally, the spectral energy distributions of quasars vary significantly, and flux‐limited samples defined at different wavelengths include different quasars. Surveys employing flux measurements at widely separated wavelengths are necessary to characterize fully the spectral properties of the quasar population. The availability of panoramic near‐infrared detectors on large telescopes provides the opportunity to undertake surveys capable of establishing the importance of extinction by dust on the observed population of quasars. We introduce an efficient method for selecting K ‐band, flux‐limited samples of quasars, termed ‘KX’ by analogy with the UVX method. This method exploits the difference between the power‐law nature of quasar spectra and the convex spectra of stars: quasars are relatively brighter than stars at both short wavelengths (the UVX method) and long wavelengths (the KX method). We consider the feasibility of undertaking a large‐area KX survey for damped Ly α galaxies and gravitational lenses using the planned UKIRT wide‐field near‐infrared camera.