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The Dwarf Galaxy Population in Nearby Groups: The Data
We used V and I CCD photometry to search for low surface brightnessdwarf galaxies in the central (<0.5 h-1 Mpc) region of thegroups NGC 6868, NGC 5846, HCG 42, and the poor cluster IC 4765. We usedthe exponential profile fit parameters to identify 80 low surfacebrightness dwarf galaxy candidates with 17 magMV>-11.4), V-I<1.5 mag,μ0>22.5 V mag arcsec-2, h>1.5", anddiameters larger than 1.2 h-1 kpc. Twenty of these galaxiesare extended low surface brightness galaxies that were detected only onsmoothed images, after masking all high surface brightness objects. Thecompleteness in the sample detection is ~80% for V<~20 and 22.5 V magarcsec-2<μ0<24.5 V magarcsec-2. For galaxies with V>20 mag andμ0>24.5 V mag arcsec-2, the completeness isbelow 50% but increases to ~80% when we search for galaxies in smoothedimages. The detected galaxies are highly concentrated toward the centerof the groups (inner 250 h-1 kpc). The best-fit power-lawslope of the surface density distribution is, on average, β~-1.5,in agreement with the values found for satellite dwarfs around isolatedE/S0 galaxies and in X-ray-bright groups. The selected dwarf galaxies donot show a clear correlation in the MV-μ0plane, suggesting that the correlation noted by other studies could beproduced by selection effects. We also find that these galaxies follow awell-defined color-magnitude relation, extending for more than 10 mag(from bright elliptical galaxies to faint dwarfs). A similar relation isknown to be valid for galaxy clusters, but it is the first time that ithas been demonstrated in the sparse environments of groups. Thespectroscopic follow-up shows that only 78 of the 409 galaxies withmeasured velocities are group members. Of these, five are low surfacebrightness dwarf galaxies. In addition, new structures along the groups'lines of sight were discovered. These new structures are groups and poorclusters that extend to ~0.3 in redshift space.Based on data collected with the 1.3 m Warsaw telescope and 2.5 m DuPont telescope at Las Campanas Observatory, Chile.

A new catalogue of ISM content of normal galaxies
We have compiled a catalogue of the gas content for a sample of 1916galaxies, considered to be a fair representation of ``normality''. Thedefinition of a ``normal'' galaxy adopted in this work implies that wehave purposely excluded from the catalogue galaxies having distortedmorphology (such as interaction bridges, tails or lopsidedness) and/orany signature of peculiar kinematics (such as polar rings,counterrotating disks or other decoupled components). In contrast, wehave included systems hosting active galactic nuclei (AGN) in thecatalogue. This catalogue revises previous compendia on the ISM contentof galaxies published by \citet{bregman} and \citet{casoli}, andcompiles data available in the literature from several small samples ofgalaxies. Masses for warm dust, atomic and molecular gas, as well asX-ray luminosities have been converted to a uniform distance scale takenfrom the Catalogue of Principal Galaxies (PGC). We have used twodifferent normalization factors to explore the variation of the gascontent along the Hubble sequence: the blue luminosity (LB)and the square of linear diameter (D225). Ourcatalogue significantly improves the statistics of previous referencecatalogues and can be used in future studies to define a template ISMcontent for ``normal'' galaxies along the Hubble sequence. The cataloguecan be accessed on-line and is also available at the Centre desDonnées Stellaires (CDS).The catalogue is available in electronic form athttp://dipastro.pd.astro.it/galletta/ismcat and at the CDS via anonymousftp to\ cdsarc.u-strasbg.fr ( or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/405/5

Nearby Optical Galaxies: Selection of the Sample and Identification of Groups
In this paper we describe the Nearby Optical Galaxy (NOG) sample, whichis a complete, distance-limited (cz<=6000 km s-1) andmagnitude-limited (B<=14) sample of ~7000 optical galaxies. Thesample covers 2/3 (8.27 sr) of the sky (|b|>20deg) andappears to have a good completeness in redshift (97%). We select thesample on the basis of homogenized corrected total blue magnitudes inorder to minimize systematic effects in galaxy sampling. We identify thegroups in this sample by means of both the hierarchical and thepercolation ``friends-of-friends'' methods. The resulting catalogs ofloose groups appear to be similar and are among the largest catalogs ofgroups currently available. Most of the NOG galaxies (~60%) are found tobe members of galaxy pairs (~580 pairs for a total of ~15% of objects)or groups with at least three members (~500 groups for a total of ~45%of objects). About 40% of galaxies are left ungrouped (field galaxies).We illustrate the main features of the NOG galaxy distribution. Comparedto previous optical and IRAS galaxy samples, the NOG provides a densersampling of the galaxy distribution in the nearby universe. Given itslarge sky coverage, the identification of groups, and its high-densitysampling, the NOG is suited to the analysis of the galaxy density fieldof the nearby universe, especially on small scales.

An Einstein X-Ray Survey of Optically Selected Galaxies. I. Data
We present the results of a complete Einstein imaging proportionalcounter X-ray survey of optically selected galaxies from theShapley-Ames Catalog, the Uppsala General Catalogue, and the EuropeanSouthern Observatory Catalog. Well-defined optical criteria are used toselect the galaxies, and X-ray fluxes are measured at the opticallydefined positions. The result is a comprehensive list of X-ray detectionand upper limit measurements for 1018 galaxies. Of these, 827 haveeither independent distance estimates or radial velocities. Associatedoptical, redshift, and distance data have been assembled for thesegalaxies, and their distances come from a combination of directlypredicted distances and those predicted from the Faber-Burstein GreatAttractor/Virgocentric infall model. The accuracy of the X-ray fluxeshas been checked in three different ways; all are consistent with thederived X-ray fluxes being of <=0.1 dex accuracy. In particular,there is agreement with previously published X-ray fluxes for galaxiesin common with a 1991 study by Roberts et al. and a 1992 study byFabbiano et al. The data presented here will be used in further studiesto characterize the X-ray output of galaxies of various morphologicaltypes and thus to enable the determination of the major sourcescontributing to the X-ray emission from galaxies.

The Butcher-Oemler Effect at Low Redshift: Spectroscopy of Five Nearby Clusters of Galaxies
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....113..492C&db_key=AST

General study of group membership. II - Determination of nearby groups
We present a whole sky catalog of nearby groups of galaxies taken fromthe Lyon-Meudon Extragalactic Database. From the 78,000 objects in thedatabase, we extracted a sample of 6392 galaxies, complete up to thelimiting apparent magnitude B0 = 14.0. Moreover, in order to considersolely the galaxies of the local universe, all the selected galaxieshave a known recession velocity smaller than 5500 km/s. Two methods wereused in group construction: a Huchra-Geller (1982) derived percolationmethod and a Tully (1980) derived hierarchical method. Each method gaveus one catalog. These were then compared and synthesized to obtain asingle catalog containing the most reliable groups. There are 485 groupsof a least three members in the final catalog.

Dynamics of clusters of galaxies with central dominant galaxies. I - Galaxy redshifts
Optical redshifts are presented for a sample of 638 galaxies in thefields of the clusters Abell 85, DC 0107-46, Abell 496, Abell 2052, andDC 1842-63. The velocity histograms and wedge diagrams show evidence fora foreground sheet of galaxies in Abell 85 and background sheets ofgalaxies in DC 0107-46 and Abell 2052. The foreground group projectedagainst the center of Abell 85 found by Beers et al. (1991) isconfirmed. No evidence of substructure was found in Abell 496, Abell2052, and DC 1842-63. The clusters have global velocity dispersionsranging from 551 km/s for DC 1842-63 to 714 km/s for A496, and flatdispersion profiles. Mass estimates using the virial theorem and theprojected mass method range from 2.3 x 10 exp 14 solar masses for DC0107-46 to 1.1 x 10 exp 15 solar masses for A85.

Multicolour photometry of the cluster of galaxies Sersic 129-01
Photometry is presented of 907 galaxies brighter that b(26.25) = 20.5 ina 1.83 x 1.83 deg area centered on the southern cluster Sersic 129-01 inthe u, b, r and i bands. The slopes and zero-points of thecolor-absolute magnitude diagrams agree well with other clustersincluding Coma and the rich cluster Shapley 8 suggesting they areindependent of cluster environment. The (u-b) against (b-i) diagramdistinguishes well between morphological types. The reddening obtainedby a number of methods disagrees with that of Griersmith (1982). A massof 7.4 x 10 to the 13th solar masses is found for the ellipticaldominated component of the cluster and (M/L)b = 59.

Photometric properties of galaxies in the cluster DC 1842-63
Results are presented from photometric and kinematic observations of thecluster DC 1842-63, including total magnitudes for 174 galaxies, surfacephotometry and bulge-to-disk ratios for 31 galaxies, and redshiftsmeasurements for 20 galaxies. The mean cluster velocity is found to be4437 + or - 78 km/s with a cluster velocity dispersion of 507 km/s. TheX-ray luminosity of the cluster is shown to be 3.0 X 10 to the 43rderg/s in the 0.5 and 4.5 keV band.

A redshift map of the Triangulum Australe-Ara region - Further indication that Centaurus and Pavo are one and the same supercluster
Existing redshifts for the region RA 15 h 30 m to 18 h 40 m, Dec. -50deg to -70 deg, have been supplemented by new observations. Aconspicuous excess of galaxies with velocity of about 4700 km/s forms anapparent link between Centaurus and Pavo. A number of possible nearbyvoids are identified.

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Right ascension:18h42m49.40s
Aparent dimensions:1.175′ × 0.977′

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ICIC 4749

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