On presente des criteres permettant de distinguer des pulsars de type I et II. Les pulsars de type II seraient statistiquement d'un modele calotte polaire
In this paper, the variation of C_z~2, the dispersion of velocities in z-axis, with r is obtained by direct integration. We also obtain the variation of the radial dispersion of velocities with r through the stability of the density wave in three-dimensional dishlike galaxies. In the solar neighborhood, the theoretical values of C_r and C_z are in fair agreement with the observed values. And toward the centre of the galaxies, the value of C_r/C_z approaches to 1.
Fourty-four objects selected for ultraviolet excess have been identified spectroscopically. The objects lie in two Palomar 1.2 m Schmidt fields in the north galactic polar cap, one of 7.7 sq deg centered on Kapteyn Selected Area 29, the other of 36 sq deg centered on SA 55. The objects are characterized by Color Classes (CC) 1A, 1, 1B, 1C, 2, and 3. Quasars comprise 75 percent of the CC 1A objects and 44 percent of the objects in the SA 29 field. Twelve quasars in the SA 29 field comprise a complete sample to B = 18.5 mag, and given an uncorrected surface density of 1.6 quasars/sq deg. This value is essentially that derived by Sandage (1969). Corrections are applied to account for the lack of high redshift quasars. An empirical correction is derived to account for lack of simultaneity in selection and photometry. A corrected lower limit to the surface density is estimated to be 1.85 quasars/sq deg to B = 18.5 mag.
In this paper, we present observations of absorption line spectrum of QSO 1225+317 with resolution of 18 km . Four possible new heavy element line systems are identified. The properties of Lyman forest lines are discussed.
Les auteurs ont deja propose la separation des pulsars en deux types. Ils examinent ici la distribution Z et les caracteristiques d'âge des candidats de type II avec P 1,3 s
In this paper we studied the orientation of the spin vectors (SVs) for 302 field galaxies in the Local Supercluster (LSC). All galaxies in our sample are selected from the Photometric Atlas of Northern Bright Galaxies after an exclusion of the members of the clusters and groups of galaxies with at least five members within the LSC. The SV orientation of these field galaxies is found to be anistropic, which is well shown in Χ2 tests of the azimuthal angle and area distributions. The histograms of the polar angle distribution exhibit a weak tendency that the field galaxies in the LSC preferentially have their SVs parallel to the LSC plane. Comparison with the results for the Virgo cluster members shows that the post-formation epoch dynamics did perturb the galactic SV orientation. This is supported by two facts: (i) There is a significant hump at high polar angle for the Virgo members while no similar hump is found in our sample. (ii) The SV projections on the LSC plane for the field galaxies show their excess direction significantly deviated from the direction pointing towards the Virgo center, unlike the Virgo cluster members.
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