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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.
| Arcsecond Positions of UGC Galaxies
We present accurate B1950 and J2000 positions for all confirmed galaxiesin the Uppsala General Catalog (UGC). The positions were measuredvisually from Digitized Sky Survey images with rms uncertaintiesσ<=[(1.2")2+(θ/100)2]1/2,where θ is the major-axis diameter. We compared each galaxymeasured with the original UGC description to ensure high reliability.The full position list is available in the electronic version only.
| Supernova 1997da in IC 1216
IAUC 6711 available at Central Bureau for Astronomical Telegrams.
| 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
| 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).
| Transport de particules et atmospheres d'etoiles magnetiques
We present the results of a spectral study of 17 galaxies with UV excessfrom the lists of [1-3]. We determine the equivalent widths of lines,the relative intensities of emission lines for 3 galaxies, the electrondensities of the gas components of 9 galaxies, and the gas masses of 2galaxies. It is shown that the gas component of Galaxy No. 235 hasextremely low excitability. In the spectrum of this galaxy the lines[Fell] 4951, 4947 are seen to be distinct, not merging with the line[OIII] 4959. The line H in the spectrum of Galaxy No. 128 has twoemission peaks, which seem to have been formed by an absorptioncomponent midway between the lines. The line H in the spectrum of GalaxyNo. 350 is detected both in emission and absorption, the absorptioncomponent lying in the longwave part of the line.
| Spectral observations of new galaxies with ultraviolet excess.
The results are given of spectral observations of 42 galaxies withultraviolet excess. Spectra were obtained with the 6-m telescope of theSpecial Astrophysical Observatory of the USSR Academy of Sciences withUAGS the spectrograph in conjunction with a scanner. Emission lines areobserved in the spectra of 27 galaxies; one object, No. 82, exhibits thefeatures of Seyfert galaxies. In the spectrum of galaxy No. 188 linesare not observed in the fairly wide wavelength interval 3550-7130 A.
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