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The dynamics of S0 galaxies and their Tully-Fisher relation
This paper investigates the detailed dynamical properties of arelatively homogeneous sample of disc-dominated S0 galaxies, with a viewto understanding their formation, evolution and structure. By using highsignal-to-noise ratio long-slit spectra of edge-on systems, we have beenable to reconstruct the complete line-of-sight velocity distributions ofstars along the major axes of the galaxies. From these data, we havederived both model distribution functions (the phase density of theirstars) and the approximate form of their gravitational potentials. Thederived distribution functions are all consistent with these galaxiesbeing simple disc systems, with no evidence for a complex formationhistory. Essentially no correlation is found between the characteristicmass scalelengths and the photometric scalelengths in these galaxies,suggesting that they are dark-matter dominated even in their innerparts. Similarly, no correlation is found between the mass scalelengthsand asymptotic rotation speed, implying a wide range of dark matter haloproperties. By comparing their asymptotic rotation speeds with theirabsolute magnitudes, we find that these S0 galaxies are systematicallyoffset from the Tully-Fisher relation for later-type galaxies. Theoffset in luminosity is what one would expect if star formation had beensuddenly switched off a few Gyr ago, consistent with a simple picture inwhich these S0s were created from ordinary later-type spirals which werestripped of their star-forming interstellar medium when they encountereda dense cluster environment.
| 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 (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| A search for counter-rotating stars in S0 galaxies.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996MNRAS.283..543K&db_key=AST
| 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.
| A comparative study of morphological classifications of APM galaxies
We investigate the consistency of visual morphological classificationsof galaxies by comparing classifications for 831 galaxies from sixindependent observers. The galaxies were classified on laser print copyimages or on computer screen using scans made with the Automated PlateMeasuring (APM) machine. Classifications are compared using the RevisedHubble numerical type index T. We find that individual observers agreewith one another with rms combined dispersions of between 1.3 and 2.3type units, typically about 1.8 units. The dispersions tend to decreaseslightly with increasing angular diameter and, in some cases, withincreasing axial ratio (b/a). The agreement between independentobservers is reasonably good but the scatter is non-negligible. In spiteof the scatter, the Revised Hubble T system can be used to train anautomated galaxy classifier, e.g. an artificial neural network, tohandle the large number of galaxy images that are being compiled in theAPM and other surveys.
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