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|The 1000 Brightest HIPASS Galaxies: Newly Cataloged Galaxies|
The H I Parkes All-Sky Survey (HIPASS) is a blind 21 cm survey forextragalactic neutral hydrogen, covering the whole southern sky. TheHIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and containsthe 1000 H I-brightest (peak flux density) galaxies. Here we present the138 HIPASS BGC galaxies that had no redshift measured prior to theParkes multibeam H I surveys. Of the 138 galaxies, 87 are newlycataloged. Newly cataloged is defined as having no optical (or infrared)counterpart in the NASA/IPAC Extragalactic Database. Using the DigitizedSky Survey, we identify optical counterparts for almost half of thenewly cataloged galaxies, which are typically of irregular or Magellanicmorphological type. Several H I sources appear to be associated withcompact groups or pairs of galaxies rather than an individual galaxy.The majority (57) of the newly cataloged galaxies lie within 10° ofthe Galactic plane and are missing from optical surveys as a result ofconfusion with stars or dust extinction. This sample also includes newlycataloged galaxies first discovered by Henning et al. in the H I shallowsurvey of the zone of avoidance. The other 30 newly cataloged galaxiesescaped detection because of their low surface brightness or opticalcompactness. Only one of these, HIPASS J0546-68, has no obvious opticalcounterpart, as it is obscured by the Large Magellanic Cloud. We findthat the newly cataloged galaxies with |b|>10° are generally lowerin H I mass and narrower in velocity width compared with the totalHIPASS BGC. In contrast, newly cataloged galaxies behind the Milky Wayare found to be statistically similar to the entire HIPASS BGC. Inaddition to these galaxies, the HIPASS BGC contains four previouslyunknown H I clouds.
|Kinematics of the local universe. VII. New 21-cm line measurements of 2112 galaxies|
This paper presents 2112 new 21-cm neutral hydrogen line measurementscarried out with the meridian transit Nan\c cay radiotelescope. Amongthese data we give also 213 new radial velocities which complement thoselisted in three previous papers of this series. These new measurements,together with the HI data collected in LEDA, put to 6 700 the number ofgalaxies with 21-cm line width, radial velocity, and apparent diameterin the so-called KLUN sample. Figure 5 and Appendices A and B forcorresponding comments are available in electronic form at thehttp://www.edpsciences.com
|Total magnitude, radius, colour indices, colour gradients and photometric type of galaxies|
We present a catalogue of aperture photometry of galaxies, in UBVRI,assembled from three different origins: (i) an update of the catalogueof Buta et al. (1995) (ii) published photometric profiles and (iii)aperture photometry performed on CCD images. We explored different setsof growth curves to fit these data: (i) The Sersic law, (ii) The net ofgrowth curves used for the preparation of the RC3 and (iii) A linearinterpolation between the de Vaucouleurs (r(1/4) ) and exponential laws.Finally we adopted the latter solution. Fitting these growth curves, wederive (1) the total magnitude, (2) the effective radius, (3) the colourindices and (4) gradients and (5) the photometric type of 5169 galaxies.The photometric type is defined to statistically match the revisedmorphologic type and parametrizes the shape of the growth curve. It iscoded from -9, for very concentrated galaxies, to +10, for diffusegalaxies. Based in part on observations collected at the Haute-ProvenceObservatory.
|A southern sky survey of the peculiar velocities of 1355 spiral galaxies|
The paper presents data from photometric and spectroscopic observationsof 1355 southern spiral galaxies and uses them to determine theirdistances and peculiar velocities via the Tully-Fisher (TF) relation.I-band CCD surface photometry was carried out using the 1-m and 3.9-mtelescopes at Siding Spring Observatory. H-alpha rotation curves for 965galaxies and 551 H I profiles are presented. The physical parameters,photometric and velocity data, distances, and peculiar velocities of thegalaxies are presented in tabular form. The mean distance, systemicvelocity, and average peculiar velocity of 24 clusters in the sample aregiven. TF diagrams are presented for each cluster.
|Colors and the evolution of amorphous galaxies|
UBVRI and H-alpha photometric observations are presented for 16amorphous galaxies and a comparison sample of Magellanic irregular (Im)and Sc spiral galaxies. These data are analyzed in terms ofstar-formation rates and histories in amorphous galaxies. Amorphousgalaxies have mean global colors and star-formation rates per unit areathat are similar to those in giant Im systems, despite differences inspatial distributions of star-forming centers in these two galacticstructural classes. Amorphous galaxies differ from giant Im systems inhaving somewhat wider scatter in relationships between B - V and U - Bcolors, and between U - B and L(H-alpha)/L(B). This scatter isinterpreted as resulting from rapid variations in star-formation ratesduring the recent past, which could be a natural consequence of theconcentration of star-forming activity into centrally located,supergiant young stellar complexes in many amorphous galaxies. While theunusual spatial distribution and intensity of star formation in someamorphous galaxies is due to interactions with other galaxies, severalamorphous galaxies are relatively isolated and thus the processes mustbe internal. The ultimate evolutionary fate of rapidly evolvingamorphous galaxies remains unknown.
|Southern Galaxy Catalogue.|
|The Antlia cluster of galaxies and its environment - The Hydra I-Centaurus supercluster|
The small Antlia cluster of galaxies was investigated by measuring manyradial velocities for galaxies from the Lauberts catalog in the Antliaregion. Apart from the Antlia cluster itself, four more small groupswere identified. These five systems form a tiny but not bound Antliamini-supercluster. The mini-supercluster consists of small groups andclusters and of a dispersed component of field galaxies. The five galaxysystems are also part of the large Hydra I-Centaurus supercluster. Thislarge supercluster belongs now to the class of well observed ones. Ithas a chain-like filamentary structure. This supercluster seems to beconnected to the Local Supercluster via two very extended but very loosegroups. The total structure is the triangle-shaped Virgo-HydraI-Centaurus supercluster.
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