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Discovery of counter-rotating gas in the galaxies NGC 1596 and 3203 and the incidence of gas counter-rotation in S0 galaxies
We have identified two new galaxies with gas counter-rotation (NGC 1596and 3203) and have confirmed similar behaviour in another one (NGC 128),this using results from separate studies of the ionized-gas and stellarkinematics of a well-defined sample of 30 edge-on disc galaxies. Gascounter-rotators thus represent 10 +/- 5 per cent of our sample, but thefraction climbs to 21 +/- 11 per cent when only lenticular (S0) galaxiesare considered and to 27 +/- 13 per cent for S0 galaxies with detectedionized gas only. Those fractions are consistent with but slightlyhigher than previous studies. A compilation from well-defined studies ofS0 galaxies in the literature yields fractions of 15 +/- 4 and 23 +/- 5per cent, respectively. Although mainly based on circumstantialevidence, we argue that the counter-rotating gas originates primarilyfrom minor mergers and tidally induced transfer of material from nearbyobjects. Assuming isotropic accretion, twice those fractions of objectsmust have undergone similar processes, underlining the importance of(minor) accretion for galaxy evolution. Applications of gascounter-rotators to barred galaxy dynamics are also discussed.
| A new catalogue of ISM content of normal galaxies
We have compiled a catalogue of the gas content for a sample of 1916galaxies, considered to be a fair representation of ``normality''. Thedefinition of a ``normal'' galaxy adopted in this work implies that wehave purposely excluded from the catalogue galaxies having distortedmorphology (such as interaction bridges, tails or lopsidedness) and/orany signature of peculiar kinematics (such as polar rings,counterrotating disks or other decoupled components). In contrast, wehave included systems hosting active galactic nuclei (AGN) in thecatalogue. This catalogue revises previous compendia on the ISM contentof galaxies published by \citet{bregman} and \citet{casoli}, andcompiles data available in the literature from several small samples ofgalaxies. Masses for warm dust, atomic and molecular gas, as well asX-ray luminosities have been converted to a uniform distance scale takenfrom the Catalogue of Principal Galaxies (PGC). We have used twodifferent normalization factors to explore the variation of the gascontent along the Hubble sequence: the blue luminosity (LB)and the square of linear diameter (D225). Ourcatalogue significantly improves the statistics of previous referencecatalogues and can be used in future studies to define a template ISMcontent for ``normal'' galaxies along the Hubble sequence. The cataloguecan be accessed on-line and is also available at the Centre desDonnées Stellaires (CDS).The catalogue is available in electronic form athttp://dipastro.pd.astro.it/galletta/ismcat and at the CDS via anonymousftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/405/5
| A catalogue and analysis of X-ray luminosities of early-type galaxies
We present a catalogue of X-ray luminosities for 401 early-typegalaxies, of which 136 are based on newly analysed ROSAT PSPC pointedobservations. The remaining luminosities are taken from the literatureand converted to a common energy band, spectral model and distancescale. Using this sample we fit the LX:LB relationfor early-type galaxies and find a best-fit slope for the catalogue of~2.2. We demonstrate the influence of group-dominant galaxies on the fitand present evidence that the relation is not well modelled by a singlepower-law fit. We also derive estimates of the contribution to galaxyX-ray luminosities from discrete-sources and conclude that they provideLdscr/LB~=29.5ergs-1LBsolar-1. Wecompare this result with luminosities from our catalogue. Lastly, weexamine the influence of environment on galaxy X-ray luminosity and onthe form of the LX:LB relation. We conclude thatalthough environment undoubtedly affects the X-ray properties ofindividual galaxies, particularly those in the centres of groups andclusters, it does not change the nature of whole populations.
| Structure and kinematics of the peculiar galaxy NGC 128
This is a multiband photometric and spectroscopic study of the peculiarS0 galaxy NGC 128. We present results from broad (Band R) and narrow (Hα ) band optical CCD photometry, near (NIR)and far (FIR) infrared observations, long slit spectroscopy, andFabry-Perot interferometry (CIGALE). The peculiar peanut shapemorphology of the galaxy is observed both at optical and near-infraredwavelengths. The stellar disk is thick and distorted (arc-bended), witha color asymmetry along the major axis due to the presence of a largeamount of dust, estimated through NIR and FIR data of ~ 6\ 10(6\)M_ȯ, in the region of interaction with the companion galaxyNGC 127. The color maps are nearly uniform over thewhole galaxy, but for the major axis asymmetry, and a small gradienttoward the center indicating the presence of a redder disk-likecomponent. The Hα image indeed reveals the existence of a tiltedgaseous ``disk'' around the center, oriented with the major axis towardthe companion galaxy NGC 127. Long slit and CIGALE data confirm thepresence of gas in a disk-like component counter-rotating and inclinedapproximately of 50(deg) to the line of sight. The mass of the gas diskin the inner region is ~ 2.7\ 10(4) \ M_ȯ. The stellar velocityfield is cylindrical up to the last measured points of the derivedrotation curves, while the velocity dispersion profiles are typical foran S0 galaxy, but for an extended constant behaviour along the minoraxis. Based on observations taken at ESO La Silla and at the SpecialAstrophysical Observatory (SAO) of the Russian Academy of Sciences(RAS).
| Interferometer (12) CO observations of the box-shaped bulge spiral NGC 4013
The nucleus of the box-shaped galaxy NGC 4013 has been observed with theIRAM interferometer in the J=1-0 and J=2-1 lines of (12) CO. Our mapsshow the existence of a fast-rotating (130 km s(-1) ) molecular gas diskof radius r ~ 2arcsec (110 pc). Several arguments support the existenceof a bar potential in NGC 4013. The figure-of-eight pattern of the majoraxis p-v plot, the ring-like distribution of gas, and the existence ofgas emission at non-circular velocities are best accounted by a bar. Wehave also detected gas at high z distances from the plane (z ~200-300pc=4arcsec -5arcsec ). The latter component is related to asystem of 4 Hα filaments of diffuse ionized gas that come out fromthe nucleus. The galactic fountain model seems the best to account forthe Hα and CO filaments. Although the peanut distortion can bespontaneously formed by a stellar bar in the disk, gas at high z mighthave been ejected after a nuclear starburst. The Hα filamentsstart in the plane of the disk at r ~ 200 pc(4arcsec ), and reachseveral Kpc height at r ~ 600 pc(10arcsec ), coinciding with the maximumpeanut distortion where the strength of the restoring forces of theplane have a minimum. We have critically examined other alternativesjudged less probable: the existence of a CO warp (connected to the HIwarping disk), the accretion of gas along stable inclined orbits and,finally, a vertical gas response near the resonances of the peanut (thelatter is tested by numerical simulations). Although a link between thebar and the box-shaped bulge in NGC 4013 is suggested we find noticeabledifferences between the results of previous numerical simulations andthe present observations. The discrepancy concerns the parameters of thebar generating the peanut. We see in NGC 4013 the existence of a strongILR region. The inclusion of a dissipative component, which remains tobe thoroughly studied, may change the evolution of the stellar peanut:although in simulations the peanut appears initially near a marginalILR, the inflow of gas driven by the bar, can make two ILRs appear.
| Total magnitude, radius, colour indices, colour gradients and photometric type of galaxies
We present a catalogue of aperture photometry of galaxies, in UBVRI,assembled from three different origins: (i) an update of the catalogueof Buta et al. (1995) (ii) published photometric profiles and (iii)aperture photometry performed on CCD images. We explored different setsof growth curves to fit these data: (i) The Sersic law, (ii) The net ofgrowth curves used for the preparation of the RC3 and (iii) A linearinterpolation between the de Vaucouleurs (r(1/4) ) and exponential laws.Finally we adopted the latter solution. Fitting these growth curves, wederive (1) the total magnitude, (2) the effective radius, (3) the colourindices and (4) gradients and (5) the photometric type of 5169 galaxies.The photometric type is defined to statistically match the revisedmorphologic type and parametrizes the shape of the growth curve. It iscoded from -9, for very concentrated galaxies, to +10, for diffusegalaxies. Based in part on observations collected at the Haute-ProvenceObservatory.
| A counter-rotating tilted gas disc in the peanut galaxy NGC 128.
We have obtained V, R_c_, I_c_ HRCAM images and TIGER spectrography ofthe central region of the peanut galaxy NGC 128. The colour imagesreveal the presence of a red disc tilted by about 26 degres with respectto the major-axis of the galaxy. This tilted disc is made of dust andgas, as revealed by the 2D TIGER map of the ionized gas distribution.The TIGER stellar and gas velocity fields show that the angular momentumvectors of the stellar and gaseous components are reversed. We thereforesuggest that the gas orbits belong to the so-called anomalous family,which is evidence for a tumbling triaxial potential (a bar) associatedwith the peanut morphology. The bar formation has very probably beentriggered through the interaction with its nearby companion NGC 127,from which the dissipative component is being accreted along retrogradeorbits.
| A multiparametric analysis of the Einstein sample of early-type galaxies. 1: Luminosity and ISM parameters
We have conducted bivariate and multivariate statistical analysis ofdata measuring the luminosity and interstellar medium of the Einsteinsample of early-type galaxies (presented by Fabbiano, Kim, &Trinchieri 1992). We find a strong nonlinear correlation betweenLB and LX, with a power-law slope of 1.8 +/- 0.1,steepening to 2.0 +/- if we do not consider the Local Group dwarfgalaxies M32 and NGC 205. Considering only galaxies with logLX less than or equal to 40.5, we instead find a slope of 1.0+/- 0.2 (with or without the Local Group dwarfs). Although E and S0galaxies have consistent slopes for their LB-LXrelationships, the mean values of the distribution functions of bothLX and LX/LB for the S0 galaxies arelower than those for the E galaxies at the 2.8 sigma and 3.5 sigmalevels, respectively. We find clear evidence for a correlation betweenLX and the X-ray color C21, defined by Kim,Fabbiano, & Trinchieri (1992b), which indicates that X-rayluminosity is correlated with the spectral shape below 1 keV in thesense that low-LX systems have relatively large contributionsfrom a soft component compared with high-LX systems. We findevidence from our analysis of the 12 micron IRAS data for our samplethat our S0 sample has excess 12 micron emission compared with the Esample, scaled by their optical luminosities. This may be due toemission from dust heated in star-forming regions in S0 disks. Thisinterpretation is reinforced by the existence of a strongL12-L100 correlation for our S0 sample that is notfound for the E galaxies, and by an analysis of optical-IR colors. Wefind steep slopes for power-law relationships between radio luminosityand optical, X-ray, and far-IR (FIR) properties. This last point arguesthat the presence of an FIR-emitting interstellar medium (ISM) inearly-type galaxies is coupled to their ability to generate nonthermalradio continuum, as previously argued by, e.g., Walsh et al. (1989). Wealso find that, for a given L100, galaxies with largerLX/LB tend to be stronger nonthermal radiosources, as originally suggested by Kim & Fabbiano (1990). We notethat, while LB is most strongly correlated withL6, the total radio luminosity, both LX andLX/LB are more strongly correlated with L6CO, the core radio luminosity. These points support the argument(proposed by Fabbiano, Gioia, & Trinchieri 1989) that radio cores inearly-type galaxies are fueled by the hot ISM.
| General study of group membership. II - Determination of nearby groups
We present a whole sky catalog of nearby groups of galaxies taken fromthe Lyon-Meudon Extragalactic Database. From the 78,000 objects in thedatabase, we extracted a sample of 6392 galaxies, complete up to thelimiting apparent magnitude B0 = 14.0. Moreover, in order to considersolely the galaxies of the local universe, all the selected galaxieshave a known recession velocity smaller than 5500 km/s. Two methods wereused in group construction: a Huchra-Geller (1982) derived percolationmethod and a Tully (1980) derived hierarchical method. Each method gaveus one catalog. These were then compared and synthesized to obtain asingle catalog containing the most reliable groups. There are 485 groupsof a least three members in the final catalog.
| An X-ray catalog and atlas of galaxies
An X-ray catalog and atlas of galaxies observed with the EinsteinObservatory imaging instruments (IPC and HRI) are presented. The catalogcomprises 493 galaxies, including targets of pointed observations, andRSA or RC2 galaxies serendipitously included in Einstein fields. A totalof 450 of these galaxies were imaged well within the instrumentalfields, resulting in 238 detections and 2123 sigma upper limits. Theother galaxies were either at the edge of the visible field of view orconfused with other X-ray sources. For these a rough measure of theirX-ray emission is also given. The atlas shows X-ray contour maps ofdetected galaxies superposed on optical photographs and givesazimuthally averaged surface brightness profiles of galaxies detectedwith a high signal-to-noise ratio.
| Satellite galaxies as probes of the gravitational potentials of large spirals
An aspect of the missing mass problem in galaxies, not easy to address,is whether the dynamical mass distribution is spherical or greatlyflattened, following the light. Rotation curves of spirals out of theplane of the disk cannot, by definition, be measured. A way around thisproblem might be to use satellite galaxies orbiting within a fewHolmberg radii of their parents. In this paper, the difficulties impliedin using a satellite are addressed in this way: to what extent is itpossible to solve uniquely for its orbital parameters? A practical setof solutions which can constrain an orbit is derived using the tidalradius of the satellite to scale the gravitational pull of the parent.Although data of the quality needed exist as yet for very few systems,it is shown, using M31, NGC 128, and NGC 1023 and their respectivesatellites, how the dynamics of the interactions can be explored.
| Observations of galaxies in groups at 102 MHz
Observations of 325 galaxies in groups were carried out at a frequencyof 102 MHz via the scintillation method. Radio emission was found in 42of these components. Eleven of these have a meridional component.
| Gravitational amplification of brightest cluster galaxies by foreground clusters
It is suggested that the Hubble diagram of brightest cluster galaxies(BCG) is strongly affected by gravitational amplifications due toforeground clusters of galaxies. Galaxies from Kristian et al.'s (1978)sample are placed with respect to foreground Zwicky clusters and theirdeviations from the mean magnitude-redshift relation are compared to thepredictions of Ricci gravitational amplification formula. It is foundthat the gravitational brightness increase reaches some tenth ofmagnitudes for these BCGs and that it has induced a strong selectioneffect artificially increasing the deceleration parameter q0.Once these effects are accounted for the Hubble diagram value ofq0 might agree with the low values obtained for the densityparameter sigma0 (0.1-0.2) without any need for rapidevolution.
| A comparison of distance scales for early-type galaxies
The distance scales of elliptical and lenticular galaxies areintercompared, based on the velocity dispersion indicator derived from arevised Faber-Jackson relation. The scales are found to be in nearperfect agreement with scales derived from the luminosity index and fromthe 21 cm line width indicator. The scales are also in excellentagreement with the distance scale derived by Michard (1979). Additionsare offered for the general catalog of 424 early-type galaxies, and aseries of reduction equations is presented which reduces the externalerrors in the distance moduli.
| Radio observations of galaxies of the Byurakan classification at 102 MHz
Interplanetary-scintillation observations at 102 MHz have been made of131 galaxies of the Biurakan classification (1975). It is found thatgalaxies with more pronounced nuclei have higher activity in the radiorange and that scintillating components (with angular dimensions about0.1 arcsec) are more frequently found in them. The scintillatingcomponents have steep spectra.
| A new classification system for galaxies
A galaxy classification system is proposed in which normal spirals andlenticulars form parallel sequences within which 'early' and 'late'systems are distinguished by means of their disk-to-bulge ratios. Asequence of 'anemic spirals', which occur most frequently in richclusters, is found to have characteristics that are intermediate betweenthose of vigorous gas-rich normal spirals and gas-poor systems of typeS0. The differences between normal spirals (Sa-Sb-Sc), anemic spirals(Aa-Ab-Ac), and lenticulars (S0a-S0b-S0c) are tentatively interpreted interms of the influence of environment on the evolution of flattenedgalaxies.
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