Large- and small-scale structure in the continuum energy distributions of quasi-stellar objects and Seyfert 1 galaxies

Details Large- and small-scale structure in the continuum energy distributions of quasi-stellar objects and Seyfert 1 galaxies Large- and small-scale structure in the continuum energy distributions of quasi-stellar objects and Seyfert 1 galaxies

Jul 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...239..475g&link_type=abstract

Astrophysical Journal, Part 1, vol. 239, July 15, 1980, p. 475-482.

Astronomy and Astrophysics

Astrophysics

44

Astronomical Photometry, Continuous Spectra, Quasars, Seyfert Galaxies, Spectral Energy Distribution, Absorption Spectra, Balmer Series, Black Body Radiation, Emission Spectra, Iron, Line Spectra, Photoelectric Emission, Spectrophotometry, Spectrum Analysis, Thermal Emission

Scientific paper

Moderate-resolution spectrophotometric observations of more than 40 Seyfert 1 galaxies and QSOs have been analyzed to study large- and small-scale structure in the continuum energy distributions of such objects. We find that for essentially all of the Seyferts and QSOs in our sample, the continuous spectra in the rest wavelength range λ4000 7000 Å are well-fitted by a simple power law. However, we confirm the previous finding that the continuum shortward of 4000 very often rises above this power law and is characterized by a broad "hump" of emission. Consideration of three obvious explanations Balmer continuum emission, two-photon emission, and thermal emission from a blackbody shows that none can easily explain the observed shape and strength of the hump. Attention is also called to several small-scale features which are repeatedly found in the continuum between 2000 and 3500 A. Although a few individual emission lines such as C II λ2326, He II λ3203, and O III λ3135 are observed in some objects, much of the rest of the bumps and wiggles in this wavelength region are not readily identified. Both absorption- and emission-line interpretations of the remaining structure are possible. However, the most convincing identification is made with several resonance-line multiplets of Fe II, observed in emission.

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