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We analyze Hubble's approach to cosmology. In 1929 he accepted a finite expanding universe in order to explain the redshifts of distant galaxies. Later on he turned to an infinite stationary universe due to observational constraints. We show, by quoting his works, that he remained cautiously against the big bang until the end of his life., Comment: Paper accepted for presentation at the Second Crisis in Cosmology Conference, to be held on 2008 September 7-11, Port Angeles, Washington, USA, Portuguese version at http://www.fisica.ufmg.br/~dsoares/ensino/Hubble-pt.doc

A classification scheme for close pairs of galaxies is proposed. The scheme is motivated by the fact that the majority of apparent close pairs are in fact wide pairs in three-dimensional space. This is demonstrated by means of numerical simulations of random samples of binary galaxies and the scrutiny of the resulting projected and spatial separation distributions. Observational strategies for classifying close pairs according to the scheme are suggested. As a result, physical (i.e., bound and spatially) close pairs are identified., Comment: 16 pages, 5 figures, accepted for publication in The Astronomical Journal, added text corrections on proofs

We introduce a network growth model in which the preferential attachment probability includes the fitness vertex and the Euclidean distance between nodes. We grow a planar network around its barycenter. Each new site is fixed in space by obeying a power law distribution., Comment: 7 pages, 6 figures. To appear in Progress of Theoretical Physics Supplement - Japan

We study in this work the properties of the $Q_{mf}$ network which is constructed from an anisotropic partition of the square, the multifractal tiling. This tiling is build using a single parameter $\rho$, in the limit of $\rho \to 1$ the tiling degenerates into the square lattice that is associated with a regular network. The $Q_{mf}$ network is a space-filling network with the following characteristics: it shows a power-law distribution of connectivity for $k>7$ and it has an high clustering coefficient when compared with a random network associated. In addition the $Q_{mf}$ network satisfy the relation $N \propto \ell^{d_f}$ where $\ell$ is a typical length of the network (the average minimal distance) and $N$ the network size. We call $d_f$ the fractal dimension of the network. In tne limit case $\rho \to 1$ we have $d_{f} \to 2$., Comment: 10 pages, 5 figures and 1 table

Detailed BVRI-Halpha photometry has been obtained for the ring galaxy HRG 2302. This is probably a still interacting system which shows two principal components: the target, which is a knotted ringed-disk, and the intruder, an elongated galaxy with two substructures probably caused by the interaction. The existence of H II emission regions is suggested by Halpha images and medium dispersion spectra of the three brightest parts of this system. Analysis of a color-color diagram suggests recent star formation, in agreement with the behavior of interacting galaxies with nuclear emission. HRG 2302 has been previously classified as a Polar Ring galaxy (Faundez-Abans & de Oliveira-Abans 1998a), but we have reclassified it as Elliptical-Knotted, based on the morphological substructures found. This work reveals, for the first time, the existence of at least 15 fainter galaxies in the field within ~4 arcmin around HRG 2302, giving positions and integrated standard magnitudes for all of them., Comment: 10 pages, accepted by Astronomy and Astrophysics

Binary galaxies are modeled as point-masses obeying the non-Newtonian MOND and Mannheim-Kazanas (MKG) theories of gravity. Random samples of such systems are generated by means of Monte Carlo simulations of binary orbits. Model pairs have total masses and mass ratios similar to pairs in the cataloged sample used in the analysis. General features of synthetic samples are derived from a comparison with observed data of galaxy pairs in $R \times \Delta V/(L_1+L_2)^{1/2} $ space. Both MOND and Mannheim-Kazanas binaries either on circular or low-eccentricity orbits cannot be the source of observations because they require extremely high $M/L$ values ($\approx$ 45 solar units). Both MOND and MKG binaries on high-eccentricity orbits and reasonable $M/L$ values (5 solar units) produce envelopes of $R \times \Delta V/(L_1+L_2)^{1/2}$ consistent with the observations, but the distribution of separations is inconsistent with the observed data, unless strong selection effects are at work. A definite answer to the issue whether one or another model is suitable to explain real binary galaxy dynamics will be only possible when {\it a large sample containing a significant fraction of wide pairs, determined with velocity-blind selection procedures, is investigated} under a rigorous statistical analysis, taking into account sample selection biases and contamination by non-physical pairs., Comment: Uuencoded compressed tar file with text and figures. Revised version accepted for Astronomy & Astrophysics on 28 February 1996

A catalogue of binary galaxies with 621 pairs has been determined by applying a surface density enhancement procedure to {\it The Surface Photometry Catalogue of the ESO-Uppsala Galaxies}. The method does not require any redshift information. An additional restriction, based on objective criteria that take into account the completeness of the source catalogue, led to a sample of 189 isolated pairs which are listed. We have obtained the optical luminosity function of binary galaxies in the catalogue, from which we estimate that the luminosity density of galaxies in binaries is $\sim$4% of that found for field galaxies. The general properties of our sample are similar to those from CPG and CMG., Comment: 16pages text+1table+4figures, uuencoded tar file with 6 postscript files, 400 kb, accepted by A&ASS (sept./94), preprint IAG/USP-1994

The rotation curves of 20 spiral galaxies are examined in the light of a toy model (Soares 1992) which has as the main feature the assignment of a high M/L ratio (=30; Ho=50 km/s/Mpc) to the visible matter. The observed rotation of all galaxies can be accommodated without the assumption of a dark halo. Moreover, the suggestion is made that the fact that almost all available rotational velocity measurements are derived from emission lines emitted by galaxian gas (either neutral or ionized) makes them inappropriate as tracers of the galaxy gravitational potential. To account for that, the model introduces an effective potential meant to describe the hydrodynamics inside a gaseous disk. The general morphology of the curves (i.e., the presence of a plateau in V(r) X r) is interpreted in this framework as a consequence of the hydrodynamical characteristics of galaxian disks. The Tully-Fisher relation is expressed in terms of model parameters and used as an additional constraint in the process of fitting the model to the observed rotation of the galaxies., Comment: 12 pages, LaTeX, accepted by RevMexAA 01-94