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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.
|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.
|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.
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