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NGC 3281D



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The Cusp/Core Problem in Galactic Halos: Long-Slit Spectra for a Large Dwarf Galaxy Sample
We derive inner dark matter halo density profiles for a sample of 165low-mass galaxies using rotation curves obtained from high-quality,long-slit optical spectra assuming minimal disks and spherical symmetry.For ρ(r)~r-α near the galaxy center, we measuremedian inner slopes ranging from αm=0.22+/-0.08 to0.28+/-0.06 for various subsamples of the data. This is similar tovalues found by other authors and in stark contrast to the intrinsiccusps (αint~1) predicted by simulations of haloassembly in cold dark matter (CDM) cosmologies. To elucidate therelationship between αm and αint inour data, we simulate long-slit observations of model galaxies with haloshapes broadly consistent with the CDM paradigm. Simulations withαint=1/2 and 1 recover both the observed distributionof αm and correlations between αm andprimary observational parameters such as distance and disk inclination,whereas those with αint=5/4 are marginally consistentwith the data. Conversely, the hypothesis that low-mass galaxies haveαint=3/2 is rejected. While the simulations do notimply that the data favor intrinsic cusps over cores, they demonstratethat the discrepancy between αm andαint~1 for our sample does not necessarily imply agenuine conflict between our results and CDM predictions; rather, theapparent cusp/core problem may be reconciled by considering the impactof observing and data-processing techniques on rotation curves derivedfrom long-slit spectra.

Box- and peanut-shaped bulges. I. Statistics
We present a classification for bulges of a complete sample of ~ 1350edge-on disk galaxies derived from the RC3 (Third Reference Catalogue ofBright Galaxies, de Vaucouleurs et al. \cite{rc3}). A visualclassification of the bulges using the Digitized Sky Survey (DSS) inthree types of b/p bulges or as an elliptical type is presented andsupported by CCD images. NIR observations reveal that dust extinctiondoes almost not influence the shape of bulges. There is no substantialdifference between the shape of bulges in the optical and in the NIR.Our analysis reveals that 45% of all bulges are box- and peanut-shaped(b/p). The frequency of b/p bulges for all morphological types from S0to Sd is > 40%. In particular, this is for the first time that such alarge frequency of b/p bulges is reported for galaxies as late as Sd.The fraction of the observed b/p bulges is large enough to explain theb/p bulges by bars. Partly based on observations collected at ESO/LaSilla (Chile), DSAZ/Calar Alto (Spain), and Lowell Observatory/Flagstaff(AZ/U.S.A.). Tables 6 and 7 are only available in electronic form at CDSvia anonymous ftp to cdsarc.u-strasbg.fr ( or viahttp://cdsweb.u-strasbg.fr/Abstract.html

Parameters of 2447 Southern Spiral Galaxies for Use in the Tully-Fisher Relation
I-band luminosities, rotational velocities, and redshifts of 1092 spiralgalaxies have been measured by CCD photometry and Hα spectroscopyusing the 1 m and 2.3 m telescopes at Siding Spring Observatory,respectively. The results are tabulated. Luminosity profiles andHα rotation curves are given for the galaxies. When these resultsare combined with similar data for 1355 spiral galaxies publishedpreviously (Mathewson, Ford, & Buchhorn, hereafter Paper I), itprovides a large, uniform, and unique data set with which to measure,via the Tully-Fisher relation, the peculiar velocities of galaxies inthe local universe to a distance of 11,000 km s^-1^ (Mathewson &Ford). Taking advantage of the opportunity for publishing this data inmachine-readable form, in the CD-ROM, we have also included similar datafor the 1355 galaxies in Paper I.

Southern Galaxy Catalogue.
Not Available

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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Observation and Astrometry data

Right ascension:10h34m18.90s
Aparent dimensions:2.042′ × 0.447′

Catalogs and designations:
Proper Names   (Edit)
NGC 2000.0NGC 3281D

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