Non-stellar radiation in radio galaxies at 3.5 microns

Details Non-stellar radiation in radio galaxies at 3.5 microns Non-stellar radiation in radio galaxies at 3.5 microns

May 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.214..109l&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 214, May 1, 1985, p. 109-118.

Astronomy and Astrophysics

Astronomy

23

Astronomical Spectroscopy, Radio Galaxies, Red Shift, Stellar Radiation, Cosmic Dust, Emission Spectra, Galactic Nuclei, H Beta Line, Infrared Spectra, Spectral Line Width, Visible Spectrum

Scientific paper

JHKLL' observations of 24 3CR radio galaxies forming a statistically complete sample at redshifts between 0.01 and 0.20 are presented and discussed. Over a third of the sample show significant non-stellar radiation components at 3.5 μm, but only those galaxies with strong optical emission lines are found to have infrared excesses. The remaining galaxies in which the emission lines are weak or absent have continua from 1 to 3.5 μm that are purely stellar in origin. In the galaxies with excesses, the strength of the excess is loosely correlated with the strength of the Hβ line and with the nuclear core radio luminosity and X-ray luminosity in the sense that the more luminous objects have stronger infrared excesses. It is inferred that the narrow-line objects probably have steeper non-stellar continua than the broad-line radio galaxies, and it is suggested that the non-stellar emission in the narrow-lined objects is produced by thermally reradiating dust associated with gas in the radio galaxies.

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