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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.
| An HI Survey of the Bootes Void. II. The Analysis
We discuss the results of a VLA [Napier et al., Proc. IEEE71,1295(1983)] H I survey of the Bootes void and compare thedistribution and H I properties of the void galaxies to those ofgalaxies found in a survey of regions of mean cosmic density. The Bootessurvey covers 1100 Mpc^3^ or ~ 1% of the volume of the void and consistsof 24 cubes of typically 2 Mpc x 2 Mpc x 1280 km s^-1^, centered onoptically known galaxies. Sixteen targets were detected in H I; 18previously uncataloged objects were discovered directly in H I. Thecontrol samples consists of 12 cubes centered on IRAS-selected galaxieswith FIR luminosities similar to those of the Bootes targets and locatedin regions of one to two times the cosmic mean density. In addition tothe 12 targets 29 companions were detected in H I. We find that thenumber of galaxies within 1 Mpc of the targets is the same to within afactor of 2 for void and control samples, and thus that the small scaleclustering of galaxies is the same in regions that differ by a factor of~6 in density on larger scales. A dynamical analysis of the galaxies inthe void suggests that on scales of a few Mpc the galaxies aregravitationally bound, forming interacting galaxy pairs, loose pairs,and loose groups. One group is compact enough to qualify as a Hicksoncompact group (hereafter referred to as HCG [Hickson, APJ, 255 , 382(1982)]. The galaxies found in the void are mostly late-type, gas-richsystems. A careful scrutiny of their H I and optical properties showsthem to be very similar to field galaxies of the same morphologicaltype. This, combined with our finding that the small scale clustering ofthe galaxies in the voids is the same as in the field, suggests that itis the near environment that mostly affects the evolution of galaxies.
| Large-Scale Structures in the Zone of Avoidance: The Galactic Anticenter Region
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...449..527L&db_key=AST
| Apparent magnitudes of galaxies behind the Milky Way
There are many Infrared Astronomy Satellite (IRAS) Uppsala GeneralCatalogue of Galaxies (UGC) and IRAS/Catalogue of Galaxies and ofClusters of Galaxies (CGCG) galaxies with measured redshifts in theMilky Way region at absolute value of b less than 15 deg. We compare themagnitudes of these galaxies with those of IRAS/UGC and IRAS/CGCGgalaxies located at b = 30 deg to 45 deg having similar redshift values.Eighteen redshifts of the latter objects were newly measured by us. Thebrightnesses of the galaxies systematically decrease with Galacticlatitude at the Milky Way region. It is shown that IRAS galaxies withincz less than 10000 km/sec are mostly detected in the regions behind theMilky Way with N(H I) less than 5 x 1021/sq cm if theredshifts are measured down to 21 mag in blue magnitude.
| The extended 12 micron galaxy sample
We have selected an all-sky (absolute value of b greater than or equalto 25 deg) 12 micron flux-limited sample of 893 galaxies from the IRASFaint Source Catalog, Version 2 (FSC-2). We have obtained accurate totalfluxes in the IRAS wavebands by using the ADDSCAN procedure for allobjects with FSC-2 12 micron fluxes greater than 0.15 Jy and increasingflux densities from 12 to 60 microns, and defined the sample by imposinga survey limit of 0.22 Jy on the total 12 micron flux. Its completenessis verified, by means of the classical log N - log S andV/Vmax tests, down to 0.30 Jy, below which we have measuredthe incompleteness down to the survey limit, using the log N - log Splot, for our statistical analysis. We have obtained redshifts (mostlyfrom catalogs) for virtually all (98.4%) the galaxies in the sample.Using existing catalogs of active galaxies, we defined a subsample of118 objects consisting of 53 Seyfert 1s and quasars, 63 Seyfert 2s, andtwo blazars (approximately 13% of the full sample), which is the largestunbiased sample of Seyfert galaxies ever assembled. Since the 12 micronflux has been shown to be about one-fifth of the bolometric flux forSeyfert galaxies and quasars, the subsample of Seyferts (includingquasars and blazars) is complete not only to 0.30 Jy at 12 microns butalso with respect to a bolometric flux limit of approximately 2.0 x10-10 ergs/s/sq cm. The average value of V/Vmaxfor the full sample, corrected for incompleteness at low fluxes, is 0.51+/- 0.04, expected for a complete sample of uniformly distributedgalaxies, while the value for the Seyfert galaxy subsample is 0.46 +/-0.10. We have derived 12 microns and far-infrared luminosity functionsfor the AGNs, as well as for the entire sample. We extracted from oursample a complete subsample of 235 galaxies flux-limited (8.3 Jy) at 60microns. The 60 micron luminosity function computed for this subsampleis in satisfactory agreement with the ones derived from the brightgalaxy sample (BGS) and the deep high-galactic latitude sample, bothselected at 60 microns.
| New galaxies with high surface brightness in the Nilson system
Using Arkelian's criteria (1974, 1975), data for 47 new High SurfaceBrightness Galaxies (HSBG) in the system of the Uppsala GeneralCatalogue of Galaxies are presented. Of the 193 Arkelian galaxies listedin the catalog, 46 were also found to be HSBGs in the Nilson system(1973). The present list contains 19 Zwicky (1971) compact galaxies (40percent), two of which are listed as HSBGs by Nilson.
| Seven poor clusters of galaxies
The measurement of 83 new redshifts from galaxies in the region of sevenof the poor clusters of galaxies identified by Morgan et al (1975) andAlbert et al (1977) has been followed by an estimation of cluster massesthrough the application of both the virial theorem and the projected masmethod. For each system, these two estimates are consistent. For the twoclusters with highest X-ray luminosities, the line-of-sight velocitydispersions are about 700 km/sec, while for the five other clusters, thedispersions are of the order of less than about 370 km/sec. The D or cDgalaxy in each poor cluster is at the kinematic center of each system.
| Observations of galaxies of high surface brightness at 102 MHz
Forty-four of the galaxies of high surface brightness listed byArakelyan have been observed at 102-MHz frequency with the Pushchinocophased antenna array by the interplanetary-scintillation method. Tenof these objects have been detected at flux-density levels above 1-2 Jy.Seven of them have scintillating components not greater than 1 arcsecacross. The galaxy Ark 448 shows 100 percent scintillation; Ark 451,nearly 100 percent. Spectra are established for the scintillatingcomponents. Almost all the scintillators either are E or S0 galaxies, orappear highly compact at photographic wavelengths.
| Accurate Optical Positions of Arakelian Galaxies
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1981AJ.....86..820K&db_key=AST
| Galaxies of high surface brightness
Two lists are presented which contain 621 galaxies whose surfacebrightness, as derived from their apparent magnitudes, is at least 22.0magnitudes from an area of 1 sq arcsec. The lists were compiled in anattempt to verify observationally a possible correlation between surfacebrightness and nuclear activity. Four percent of all the galaxies in anarea of 4.5 sr at declinations higher than -3 deg and galactic latitudesgreater than 20 deg are listed, including 30 Markarian, 29 Zwicky, and 7blue Haro galaxies. A morphological study of 130 of the galaxiesindicates that about half are elliptical or lenticular, 50 are compactor peculiar, and that there is an excess of elliptical and lenticularobjects in comparison with a random sample. Notes on the morphologicaltypes and colors of the galaxies are provided along with identificationcharts.
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