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Observations and modelling of the interacting galaxies NGC 3395 and 3396
We present both observations and modelling of the atomic hydrogen in theclosely interacting galaxies NGC 3395 and 3396. The observations weremade with the VLA in both C- and D-arrays. We detect a large `tail' ofHi extending to a projected distance of 63kpc (10arcmin) south-west ofthe pair, as well as two smaller galaxies, IC 2604, 14arcmin to thesouth-west, and IC 2608, 14arcmin to the south-east. However, thesegalaxies appear to have had at most a minor influence on the dynamics ofNGC 3395/6. By means of N-body simulation we show that the tail is gasthat has been stripped from NGC 3395 during a prograde encounter withNGC 3396, and that the pair has had one previous close approach. It isshown that the galaxies are within 5x10^7yr of their second perigalacticpassage. Comparison of the time-scales for starburst activity with thosefrom the simulations shows that the current starbursts are a result ofthe current close approach and not the first one. The interactionbetween NGC 3395 and 3396 has flattened the rotation curve of NGC 3396owing to the parameters of the interaction. This naturally explains themore nucleated radio continuum structure observed in this galaxy, assignificant infall and a subsequent central starburst would be expectedin this scenario. The velocity structure and line profiles of the Hi arebest explained if both cloud-cloud collisions between the two gas discsand tidal forces have been important.
| An image database. II. Catalogue between δ=-30deg and δ=70deg.
A preliminary list of 68.040 galaxies was built from extraction of35.841 digitized images of the Palomar Sky Survey (Paper I). For eachgalaxy, the basic parameters are obtained: coordinates, diameter, axisratio, total magnitude, position angle. On this preliminary list, weapply severe selection rules to get a catalog of 28.000 galaxies, wellidentified and well documented. For each parameter, a comparison is madewith standard measurements. The accuracy of the raw photometricparameters is quite good despite of the simplicity of the method.Without any local correction, the standard error on the total magnitudeis about 0.5 magnitude up to a total magnitude of B_T_=17. Significantsecondary effects are detected concerning the magnitudes: distance toplate center effect and air-mass effect.
| New HI Observations for Possible Group Member Galaxies
We present new HI-observations made at the Nancay radiotelescope for 120spiral galaxies. These galaxies have been selected because of theirpossible membership to groups of the LGG catalog. For each object wegive the heliocentric HI-velocity, HI-linewidths at 20% and 50% of themaximum intensity and the HI-flux.
| La Base de Données Extragalactiques de Lyon-Meudon revisitée
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| KISO survey for ultraviolet-excess galaxies. IX
A set of identification charts is presented for UV-excess galaxiesdetected on multicolor plates for ten survey fields. The charts are partof the Kiso UV galaxy catalog (Takase and Miyauchi-Isobe, 1988). Thisset of charts brings the total number of objects in the catalog to 583,covering a 300-sq deg sky area down to a photographic magnitude of about18. The parameters presented include morphological classifications,image sizes, and degree of UV-excess.
| The Case low-dispersion Northern Sky Survey. V.
Positions, estimated magnitudes, and finding charts (when necessary) areprovided for 143 blue and/or emission-line galaxies, probable H IIregions in 11 galaxies, 149 blue and/or emission-line stellar objectsincluding QSO candidates, and 36 known and suspected blue stars in theR.A. region between 10 h 10 m and 12 h 15 m and declination between +33.0 and .38.0 deg (1950). The objects, whose blue magnitudes are mostlywithin the range 15-18, were identified on low-dispersionobjective-prism plates taken with the Burrel Schmidt telescope at KittPeak.
| Photographs of nebulae with the 60-inch reflector, 1917-1919.
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