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BVRI surface photometry of mixed morphology pairs of galaxies. II. The second data set
In order to analyze the photometric signature of gravitationalinteractions in spiral and elliptical galaxies, we present results ofmulticolor broad band (BVRI) surface photometry for a second set of 10mixed pairs drawn from the Karachentsev Catalogue of Isolated Pairs ofGalaxies (KPG). We report total magnitudes and colors, as well assurface brightness, color and geometric (ɛ, PA anda4/a) profiles. Most of this subsample have photometricparameters homogeneously derived for the first time. Internal andexternal data comparisons show consistency within the estimated errors.We find 1 true (E+S) pair and 4 probable (E+S) pairs ((E/S0+S) cases) inthe present sample. The remaining objects include 3 lenticular-spiral(S0+S) systems, 1 spiral-spiral (S+S) pair and 1 probable spiral-spiralpair ((S0/Sa+S) case). Four lenticular galaxies show evidence ofunderlying (perhaps induced) structures like bars/arms. Among the spiralcomponents, an over-representation of early (Sa-Sb) types was found. Abrief discussion on the existence of a Holmberg Effect is alsopresented.Based on data obtained at the 0.84 m telescope of the ObservatorioAstronómico Nacional (OAN), San Pedro Mártir, BajaCalifornia, México, operated by the Instituto deAstronomía, UNAM.Tables 1-3 and Figs. 3-12 are only available in electronic form athttp://www.edpsciences.org
| 21-cm line observations of galaxies from Kazarian's lists
The 21-cm neutral hydrogen line has been measured for the first time in39 non-Seyfert type galaxies from Kazarian list, with the Nancayradiotelescope. The line profiles, widths at 20% and 50% of the peakintensity, radial velocities as well as total fluxes are presented. Thevalues of radial velocity are in fairly good agreement with thoseobtained from optical spectra. The width values at 20% of the peak varyin wide range from 113 km s^{-1} (KAZ 579) to 608 km s^{-1} for KAZ 566.Nine of our objects remained undetected, whether their HI-flux was toofaint, the integration time too short, or the frequency sighted wrong.However, for part of them, there were positive hint of detection.Comments on individual objects are given. Tables 1 and 3 are onlyavailable in electronic form at CDS. Table 2 is also available inelectronic form at CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html
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