Deconvolution of quasar images from point-spread function Application to 3C 273, PKS 2135 + 147, and PKS 0812 + 020

Details Deconvolution of quasar images from point-spread function Application to 3C 273, PKS 2135 + 147, and PKS 0812 + 020 Deconvolution of quasar images from point-spread function Application to 3C 273, PKS 2135 + 147, and PKS 0812 + 020

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.103..165b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 103, no. 1, Aug. 1984, p. 165-187.

Astronomy and Astrophysics

Astrophysics

6

Astronomical Photography, Convolution Integrals, Point Spread Functions, Quasars, Astronomical Photometry, Astronomical Spectroscopy, Brightness Distribution, Image Resolution

Scientific paper

The photometric structure of the resolved quasars 3C 273, PKS 2135 + 147, and PKS 0812 + 020 has been restored by an effective deconvolution procedure from observed photographic profiles and PFSs given by Wyckoff et al. (1981). Three well-defined components have been found in quasars: (1) the central pointlike source, containing about 75 percent of the total light, (2) an intermediate region of about 10 kpc radius, whose luminosity seems to depend on the quasar's absolute luminosity, and (3) an external region with dimensions and behavior of the brightness profile typical of giant elliptical and cD galaxies. The appearance of the photographic images of quasars with underlying nebulosities is discussed on the grounds of reliable extended PFSs and distances. An extensive discussion is devoted to the numerical aspects of deconvolution, which belongs to the class of ill-posed inverse problems. The regularization method, which avoids the numerical instabilities arising in such problems as well in the estimation of many nonlinear parameters, is also described.

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