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Physical Coupling of Kazarian Galaxies with Surrounding Galaxies
Results from a statistical study of Kazarian galaxies and the objectssurrounding them are presented. It is shown that: (1) the sample ofKazarian galaxies up to 16m.0 is complete. (2) Roughly 35.7% of theKazarian galaxies are members of clusters, 14.0% of groups, and 13.6% ofbinary systems, while 36.7% are single galaxies. (3) Of the 580 Kazariangalaxies, roughly 61.2% are infrared, 8.8% radio, and 2.8% x-raysources. (4) The relative numbers of Kazarian galaxies for completesamples of I, R, and X in the different groups are systematically higherthan the corresponding numbers for samples of all Kazarian galaxies.
| Galaxy coordinates. II. Accurate equatorial coordinates for 17298 galaxies
Using images of the Digitized Sky Survey we measured coodinates for17298 galaxies having poorly defined coordinates. As a control, wemeasured with the same method 1522 galaxies having accurate coordinates.The comparison with our own measurements shows that the accuracy of themethod is about 6 arcsec on each axis (RA and DEC).
| Spectrophotometric investigation of eight galaxies with a UV excess.
The results of a spectroscopic and morphological investigation ofgalaxies with a UV excess Nos. 27, 28, 93, 101, 109, 164, 204, and 217from the lists of [M. A. Kazarian, 15, 5, 193 (1979)] are given. Theequivalent widths, relative intensities, and half- widths of lines aredetermined. The masses of galaxies Nos. 28, 93, 101, 164, 204, and 217are also determined.
| Morphological classification of new galaxies with a UV excess
The results of a morphological classification of 580 galaxies with a UVexcess, included in the lists in [M. A. Kazarian, Astrofizika,15, 5(1979); ibid.,15, 193 (1979); M. A. Kazarian and É. S. Kazarian,ibid.,16, 17 (1980); ibid.,18, 512 (1982); ibid.,19, 213 (1983)], arepresented. For this we have developed a set of symbols, using the typesE, S, and Ir introduced by Hubble, as well as symbols introduced byother authors and us. This set enabled us to make the morphologicalclassification. Direct photographs obtained on the 2.6-m and 6-mtelescopes were used to classify 141 of the galaxies (over 24%), whilePalomar Atlas charts were used for the remaining 439 galaxies. Thesegalaxies were divided into two groups based on classificationconditions, and data on each group are given in Tables 1 and 2,respectively. The results for each group, given in Table 3, show thatwith the transition from early types, such as C and E, to later types,such as S and Ir, the relative number of galaxies going into one group(Table 1), in which the classification was based on direct photographs,increases in comparison with the number going into the other group(Table 2).
| Corrections and additions to the third reference catalogue of bright galaxies
List of corrections and additions to the Third Reference Catalogue ofBright Galaxies (RC3) are given. The corrected version of the catalogue(RC3.9b), dated April 1994, is currently available through the nationaldata centers.
| UBV photometry of two physical systems of galaxies with ultraviolet excess
Detailed photographic UBV photometry of two physical systems of galaxieswith ultraviolet excess (Nos. 27, 28, 29 and Nos. 346, 347, 348) fromKazarian's lists (1979, 1980), is reported. The distribution of thesurface brightness B/sq arcsec and the color indices U-B and B-V alongthe semimajor axes of galaxies Nos. 28 and 348 is given, together withthe (U-B, B-V) diagrams. In both groups, it is noted that the galaxieshave similarities in a number of photometric characteristics. Theultraviolet excess in the investigated galaxies has, in all probability,a stellar origin and, as a rule, is localized in the nuclear regions. Itis noted that in galaxy No. 346 there are seven bright condensationswhich, on the basis of the absolute magnitudes and colors, aresuperassociations (giant H II regions).
| Spectra of Seyfert galaxies and Seyfert galaxy candidates
New spectral classifications of a number of Seyfert galaxies, as well asof other objects that are not but were earlier suspected of beingSeyfert galaxies, are presented. Measured redshifts for all theseobjects are also given. Mrk 266 SW and Mrk 1066, two galaxies near thelower end of the Seyfert 2's and close to Liners (low-ionization nuclearemission-line regions), are studied spectrophotometrically. Theirrelative emission-line spectra agree much better with published modelsfor photoionization by a low-luminosity power-law-like radiation sourcethan by shock-wave heating. The spectra of Mrk 883 and Mrk 1320, whichare borderline Seyfert galaxies, of Mrk 984, a double emission-linegalaxy, and Mrk 1459, a galaxy photoionized by a hot-star population,are briefly discussed.
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