Optical and 2 micron surface photometry of NGC 185

Details Optical and 2 micron surface photometry of NGC 185 Optical and 2 micron surface photometry of NGC 185

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...297..652p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 297, Oct. 15, 1985, p. 652-661. Research supported by the University of Wyo

Astronomy and Astrophysics

Astronomy

13

Astronomical Photometry, Dwarf Galaxies, Elliptical Galaxies, Infrared Astronomy, Astronomical Models, Isophotes, Optical Thickness, Photoabsorption, Ubv Spectra

Scientific paper

Photoelectric UBV surface photometry, photovoltaic K surface photometry, and six-filter CCD surface photometry (4250, 5000, 6000, 6700, 7700, and 8700 A) of NGC 185, a small peculiar elliptical companion galaxy to M 31, are obtained using the Wyoming 2.3 m telescope. The optical depth, luminosity distance into the galaxy, density, and mass have been determined for a prominent absorption region in the vicinity of the nucleus. It is found the optical depths of this dust cloud, normalized to tauv, are different as a function of wavelength from the accepted galactic optical depth ratios. On subtracting an Oemler model from the optical images of NGC 185, a diffuse remnant results whose colors are almost identical to those of the remnant similarly obtained for NGC 205, but the NGC 185 remnant is much fainter. It is unclear whether the faintness of the NGC 185 remnant has any physical significance. It is argued that NGC 185 is in a quiescent phase of its evolution, as there is a noticeable paucity of prominent young stars in its central regions.

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