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HI content in galaxies in loose groups
Gas deficiency in cluster spirals is well known and ram-pressurestripping is considered the main gas removal mechanism. In some compactgroups too gas deficiency is reported. However, gas deficiency in loosegroups is not yet well established. Lower dispersion of the membervelocities and the lower density of the intragroup medium in small loosegroups favour tidal stripping as the main gas removal process in them.Recent releases of data from the HI Parkes All-Sky Survey (HIPASS) andcatalogues of nearby loose groups with associated diffuse X-ray emissionhave allowed us to test this notion. In this paper, we address thefollowing questions: (i) do galaxies in groups with diffuse X-rayemission statistically have lower gas content compared to the ones ingroups without diffuse X-ray emission? (ii) does HI deficiency vary withthe X-ray luminosity, LX, of the loose group in a systematicway? We find that (i) galaxies in groups with diffuse X-ray emission, onaverage, are HI deficient, and have lost more gas compared to those ingroups without X-ray emission; the latter are found not to havesignificant HI deficiency; (ii) no systematic dependence of the HIdeficiency with LX is found. Ram-pressure-assisted tidalstripping and evaporation by thermal conduction are the two possiblemechanisms to account for this excess gas loss.
| High-Resolution H I Observations of the Galaxy NGC 404: A Dwarf S0 with Abundant Interstellar Gas
As part of a detailed study of the gas content in a sample of early-typegalaxies, we present 21 cm H I line maps of the S0 galaxy NGC 404 at aspatial resolution of 15.2"'×14.4"(α×δ) and a velocity resolution of 2.6 kms-1. The H I has been traced out to a radiusR~8R25 or 48 disk scale lengths, making it one of the largestH I extents reported (800" or 12.6 kpc at the assumed distance of 3.3Mpc). Approximately 75% of the H I resides in a doughnut, which is seenclose to face-on with inner and outer radii of ~R25 and~4R25, respectively. The optical galaxy fits snugly withinthe hole of the doughnut. The remaining 25% of the neutral gas is foundin an annulus concentric with the doughnut and with a somewhat largerellipticity, extending from a radius of ~4R25 to~8R25. A total H I mass of1.52+/-0.04×108Msolar is found, whichimplies an MHI/LB=0.22 in solar units. We arguethat most, if not all, of this gas is of external origin, most likelyfrom the merger of a dwarf irregular galaxy with MB~-15.5mag. The velocity field shows a steeply declining observed rotationcurve, compatible with Keplerian decline. However, because the galaxy isclose to face-on, there is a degeneracy in the determination of theintrinsic rotation curve and inclination. We therefore analyzed twoextreme cases, producing tilted-ring model fits forcing either aKeplerian or a flat rotation curve through the observations; bothapproaches result in equally plausible fits. In both model fits, theposition angle of the kinematical major axis of the annulus is distinctfrom that of the doughnut and ranges from 160° to 120° (for thedoughnut these values are 100° to 60°). Assuming a distance of3.3 Mpc, a total mass of 3×1010Msolar isfound on the basis of the Keplerian rotation curve. This implies aglobal MT/LB ratio of ~44 in solar units, which ishigh and likely a reflection of the low blue luminosity of the galaxy(~15 times lower than the average S0 luminosity). Values for a flatrotation curve are a factor of 4 higher.
| Near-infrared observations of galaxies in Pisces-Perseus. V. On the origin of bulges
We investigate the scaling relations of bulge and disk structuralparameters for a sample of 108 disk galaxies. Structural parameters ofindividual galaxies are obtained from two-dimensional bulge/diskdecomposition of their H-band surface brightness distributions. Bulgesare modelled with a generalized exponential (Sérsic) withvariable integer shape index n. We find that bulge effectivescalelengths reB and luminosity MBincrease with increasing n, but disk properties are independent of bulgeshape. As Hubble type T increases, bulges become less luminous and theirmean effective surface brightness <μeB>gets fainter; disk <μeD> shows a similar,but much weaker, trend. When bulge parameters(<μeB>, reB,MB) are compared with disk ones(<μeD>, reD,MD), they are tightly correlated for n=1 bulges. Thecorrelations gradually worsen with increasing n such that n=4 bulgesappear virtually independent of their disks. The Kormendy relation,<μeB> vs. reB, isshown to depend on bulge shape n; the two parameters are tightlycorrelated in n=4 bulges (r=0.8), and increasingly less so as ndecreases; disk <μeD> andreD are well correlated (r=0.7). Bulge-to-disksize ratios reB/reD areindependent of Hubble type, but smaller for exponential bulges; the meanreB/reD for n=1 bulges is 4times smaller than that for n=4, with a spread which is 9 times smaller.Strongly barred SB galaxies with exponential bulges are more luminousthan their unbarred counterparts. Exponential bulges appear to beclosely related to their underlying disks, while bulges with higher nvalues are less so; n=4 bulges and their disks apparently have norelation. We interpret our results as being most consistent with asecular evolutionary scenario, in which dissipative processes in thedisk are responsible for building up the bulges in most spirals.Based on observations at the TIRGO, NOT, and VATT telescopes. TIRGO(Gornergrat, CH) is operated by IRA-CNR, Arcetri, Firenze. NOT (LaPalma, Canary Islands) is operated by NOTSA, the Nordic ObservatoryScientific Association. VATT (Mt. Graham, AZ) is operated by VORG, theVatican Observatory Research Group.Full Table 1 is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/414/905.
| A Search for H I in Five Elliptical Galaxies with Fine Structure
We report on VLA H I spectral line observations of five early-typegalaxies classified as optically peculiar because of the presence ofjets, ripples, or other optical fine structure. We detect H I within theprimary beam (30' half-power beamwidth) in four of the five systems.However, in only one case is this gas associated with the targetedelliptical galaxy. In the other cases the H I is associated with anearby gas-rich disk or dwarf galaxy. The one H I detection is for NGC7626, where we tentatively detect an H I cloud lying between 20 and 40kpc southwest of the galaxy center. Its origin is unclear. Our failureto detect obvious tidal H I features suggests that if thesefine-structure elliptical galaxies are remnants of disk galaxy mergers,either the progenitors were gas-poor or they are well evolved and anygaseous tidal features have dispersed and/or been converted into otherphases. Our targeted systems all reside in groups or clusters, and itseems likely that tidal H I is shorter lived in these environments thansuggested by studies of more isolated merger remnants.
| Spectroscopy of Low Surface Brightness Galaxies with the Hobby-Eberly Telescope
We have obtained low-resolution spectra of 19 red and blue low surfacebrightness (LSB) galaxies, using the Marcario Low-ResolutionSpectrograph on the 9.2 m Hobby-Eberly Telescope. These galaxies form avery heterogeneous class, whose spectra qualitatively resemble those ofhigh surface brightness galaxies covering the full range of spectra seenin galaxies of Hubble types from E to Irr. We use a combination ofemission-line (EW(Hα), [N II] λ6584/Hα) andabsorption-line (Mg b, Hβ, ) based diagnostics toinvestigate the star formation and chemical enrichment histories ofthese galaxies. These are diverse, with some galaxies having lowmetallicity and very young mean stellar ages and other galaxies showingold, supersolar-metallicity stellar populations. In contrast with someprevious studies, which found a strong trend of decreasing metallicitywith decreasing central surface brightness, we find a population ofgalaxies with low surface brightness and near-solar metallicity.Correlations between several of the gas-phase and stellar population ageand metallicity indicators are used to place constraints on plausibleevolutionary scenarios for LSB galaxies. The redshift range spanned bythese galaxies is broad, with radial velocities from 3400 kms-1 to more than 65,000 km s-1. A subset of thesample galaxies have published H I redshifts and gas masses based onobservations with the Arecibo 305 m single-dish radio telescope, whichplace these galaxies far off of the mean Tully-Fisher relation. Our newoptical redshifts do not agree with the published H I redshifts forthese galaxies. Most of the discrepancies can be explained by beamconfusion in the Arecibo observations, causing erroneous H I detectionsfor some of the galaxies.
| The H I Line Width/Linear Diameter Relationship as an Independent Test of the Hubble Constant
The relationship between corrected H I line widths and linear diameters(LW/LD) for spiral galaxies is used as an independent check on the valueof the Hubble constant. After calibrating the Tully-Fisher (TF) relationin both the B and I bands, the B-band relation is used for galaxies ofmorphological/luminosity types Sc I, Sc I.2, Sc I.3, Sab, Sb, Sb I-II,and Sb II to derive the LW/LD relation. We find that for this sample thescatter in the LW/LD is smallest with a Hubble constant of 90-95 kms-1 Mpc-1. Lower values of the Hubble constantproduce a separation in the LW/LD relation that is a function ofmorphological type. Since a Hubble constant of 90-95 is significantlylarger than the final Key Project value of 72 km s-1Mpc-1, a comparison of TF, surface brightness fluctuation(SBF), and fundamental plane (FP) is made. This comparison indicatesthat the Key Project TF distances to 21 clusters may be too large. For asample of 11 clusters, the Key Project TF distances provide anunweighted mean Hubble constant of 77 km s-1Mpc-1, while a combination of the FP, SBF, and our TFdistances for the same 11 clusters gives H0=91 kms-1 Mpc-1. A more subtle result in our data is amorphological dichotomy in the Hubble constant. The data suggest that ScI galaxies follow a Hubble constant of 90-95 while Sb galaxies follow aHubble constant closer to 75 km s-1 Mpc-1.Possible explanations for this result are considered, but it is shownthat this Sb/Sc I Hubble flow discrepancy is also present in the VirgoCluster and is consistent with previous investigations that indicatethat some galaxies carry a component of age-related intrinsic redshift.
| The UZC-SSRS2 Group Catalog
We apply a friends-of-friends algorithm to the combined Updated ZwickyCatalog and Southern Sky Redshift Survey to construct a catalog of 1168groups of galaxies; 411 of these groups have five or more members withinthe redshift survey. The group catalog covers 4.69 sr, and all groupsexceed the number density contrast threshold, δρ/ρ=80. Wedemonstrate that the groups catalog is homogeneous across the twounderlying redshift surveys; the catalog of groups and their membersthus provides a basis for other statistical studies of the large-scaledistribution of groups and their physical properties. The medianphysical properties of the groups are similar to those for groupsderived from independent surveys, including the ESO Key Programme andthe Las Campanas Redshift Survey. We include tables of groups and theirmembers.
| Low Surface Brightness Galaxies and the Tully-Fisher Relation
We present Very Large Array (VLA) H I imaging of four low surfacebrightness (LSB) galaxies ([OBC97] P01-3, [OBC97] C06-1, [OBC97] C04-1,[OBC97] C04-2),1 which were thought tostrongly deviate from the Tully-Fisher (TF) relation based on Arecibosingle-dish observations. We do not detect three of the four targetedlow surface brightness galaxies (LSBs) in H I down to a 4 σ limitof 0.08 Jy km s-1. We find that two of the four of these LSBshave bright galaxies at projected distances of 2.6′ and2.9′, which have contaminated the Arecibo signal. A furtherexamination of the Arecibo sample shows that five out of the sixgalaxies that were found to deviate from the TF relation have nearbybright galaxies (within 3.5′ and within the observed H I velocityrange), and we conclude that possibly all but one of the non-TF galaxiesare contaminated by H I from nearby galaxies. The sixth galaxy was notdetected by us. A new observation by Arecibo did not confirm the earlierdetection. We present the H I properties, kinematics, and rotationcurves of three bright galaxies NGC 7631, KUG 2318+078, NGC 2595 whichhappened to be in the LSB fields and of two LSB galaxies, one of thetargeted ones C04-2 and one (UGC 12535 or P01-1) that was found in thefield of P01-3. The two detected LSB galaxies fall within 2 σ onthe TF relation. The integrated profiles of the bright galaxies areconsistent with the Arecibo results both in velocity range andamplitude, which indicates that most of the extreme deviators from theTF relation must have been affected by bright companions in this earlierH I survey. A more recent determination of the sidelobe structure of theArecibo beam supports our conclusion and shows that the degree ofsidelobe contamination was much larger than could have been initiallypredicted. If the now unknown velocities of these nondetected LSB's arewithin our probed velocity range then the limit to their H I mass isroughly 108 Msolar assuming H0=75 kms-1 Mpc-1. Hence, we have corrected the resultsfound in O'Neil et al. (2000a) and have reconstructed the TF relation.These new observations then show (1) a reconstructed TF relation thathas relatively large scatter at all values of rotational velocity(possibly indicating the true range in disk galaxy properties) and (2)the presence of at least some red, gas-poor, LSB disks that indeed maybe in an advanced evolutionary state as the faded remnants of theirformer high surface brightness actively star-forming state.
| X-ray luminosities of galaxies in groups
We have derived the X-ray luminosities of a sample of galaxies ingroups, making careful allowance for contaminating intragroup emission.The LX:LB and LX:LFIRrelations of spiral galaxies in groups appear to be indistinguishablefrom those in other environments, however the elliptical galaxies fallinto two distinct classes. The first class is central-dominant groupgalaxies, which are very X-ray luminous and may be the focus of groupcooling flows. All other early-type galaxies in groups belong to thesecond class, which populates an almost constant band ofLX/LB over the range9.8
| Nearby Optical Galaxies: Selection of the Sample and Identification of Groups
In this paper we describe the Nearby Optical Galaxy (NOG) sample, whichis a complete, distance-limited (cz<=6000 km s-1) andmagnitude-limited (B<=14) sample of ~7000 optical galaxies. Thesample covers 2/3 (8.27 sr) of the sky (|b|>20deg) andappears to have a good completeness in redshift (97%). We select thesample on the basis of homogenized corrected total blue magnitudes inorder to minimize systematic effects in galaxy sampling. We identify thegroups in this sample by means of both the hierarchical and thepercolation ``friends-of-friends'' methods. The resulting catalogs ofloose groups appear to be similar and are among the largest catalogs ofgroups currently available. Most of the NOG galaxies (~60%) are found tobe members of galaxy pairs (~580 pairs for a total of ~15% of objects)or groups with at least three members (~500 groups for a total of ~45%of objects). About 40% of galaxies are left ungrouped (field galaxies).We illustrate the main features of the NOG galaxy distribution. Comparedto previous optical and IRAS galaxy samples, the NOG provides a densersampling of the galaxy distribution in the nearby universe. Given itslarge sky coverage, the identification of groups, and its high-densitysampling, the NOG is suited to the analysis of the galaxy density fieldof the nearby universe, especially on small scales.
| Distances to Galaxies from the Correlation between Luminosities and Line Widths. III. Cluster Template and Global Measurement of H0
The correlation between the luminosities and rotation velocities ofgalaxies can be used to estimate distances to late-type galaxies. It isan appropriate moment to reevaluate this method given the great deal ofnew information available. The major improvements described hereinclude: (1) the template relations can now be defined by large,complete samples, (2) the samples are drawn from a wide range ofenvironments, (3) the relations are defined by photometric informationat the B, R, I, and K' bands, (4) the multiband information clarifiesproblems associated with internal reddening, (5) the template zeropoints are defined by 24 galaxies with accurately known distances, and(6) the relations are applied to 12 clusters scattered across the skyand out to velocities of 8000 km s-1. The biggest change fromearlier calibrations are associated with point 5. Roughly a 15% increasein the distance scale has come about with the fivefold increase in thenumber of zero-point calibrators. The overall increase in the distancescale from the luminosity-line width methodology is about 10% afterconsideration of all factors. Modulo an assumed distance to the LargeMagellanic Cloud of 50 kpc and no metallicity corrections to the Cepheidcalibration, the resulting value of the Hubble constant isH0=77+/-8 km s-1 Mpc-1, where the erroris the 95% probable statistical error. Cumulative systematic errorsinternal to this analysis should not exceed 10%. Uncertainties in thedistance scale ladder external to this analysis are estimated at ~10%.If the Cepheid calibration is shifted from the LMC to NGC 4258 with adistance established by observations of circumnuclear masers, thenH0 is larger by 12%.
| A Dynamical Study of Galaxies in the Hickson Compact Groups
To investigate dynamical properties of spiral galaxies in the Hicksoncompact groups (HCGs), we present rotation curves of 30 galaxies in 20HCGs. We found as follows: (1) There is no significant relation betweendynamical peculiarity and morphological peculiarity in HCG spiralgalaxies. (2) There is no significant relation between the dynamicalproperties and the frequency distribution of nuclear activities in HCGspiral galaxies. (3) There are no significant correlations between thedynamical properties of HCG spiral galaxies and any group properties(i.e., size, velocity dispersion, galaxy number density, and crossingtime). (4) Asymmetric and peculiar rotation curves are more frequentlyseen in the HCG spiral galaxies than in field spiral galaxies or incluster ones. However, this tendency is more obviously seen in late-typeHCG spiral galaxies. These results suggest that the dynamical propertiesof HCG spiral galaxies do not strongly correlate with the morphology,the nuclear activity, and the group properties. Our results also suggestthat more frequent galaxy collisions occur in the HCGs than in the fieldand in the clusters.
| Arcsecond Positions of UGC Galaxies
We present accurate B1950 and J2000 positions for all confirmed galaxiesin the Uppsala General Catalog (UGC). The positions were measuredvisually from Digitized Sky Survey images with rms uncertaintiesσ<=[(1.2")2+(θ/100)2]1/2,where θ is the major-axis diameter. We compared each galaxymeasured with the original UGC description to ensure high reliability.The full position list is available in the electronic version only.
| The I-Band Tully-Fisher Relation for SC Galaxies: 21 Centimeter H I Line Data
A compilation of 21 cm line spectral parameters specifically designedfor application of the Tully-Fisher (TF) distance method is presentedfor 1201 spiral galaxies, primarily field Sc galaxies, for which opticalI-band photometric imaging is also available. New H I line spectra havebeen obtained for 881 galaxies. For an additional 320 galaxies, spectraavailable in a digital archive have been reexamined to allow applicationof a single algorithm for the derivation of the TF velocity widthparameter. A velocity width algorithm is used that provides a robustmeasurement of rotational velocity and permits an estimate of the erroron that width taking into account the effects of instrumental broadeningand signal-to-noise. The digital data are used to establish regressionrelations between measurements of velocity widths using other commonprescriptions so that comparable widths can be derived throughconversion of values published in the literature. The uniform H I linewidths presented here provide the rotational velocity measurement to beused in deriving peculiar velocities via the TF method.
| The I-Band Tully-Fisher Relation for SC Galaxies: Optical Imaging Data
Properties derived from the analysis of photometric I-band imagingobservations are presented for 1727 inclined spiral galaxies, mostly oftypes Sbc and Sc. The reduction, parameter extraction, and errorestimation procedures are discussed in detail. The asymptotic behaviorof the magnitude curve of growth and the radial variation in ellipticityand position angle are used in combination with the linearity of thesurface brightness falloff to fit the disk portion of the profile. TotalI-band magnitudes are calculated by extrapolating the detected surfacebrightness profile to a radius of eight disk scale lengths. Errors inthe magnitudes, typically ~0.04 mag, are dominated by uncertainties inthe sky subtraction and disk-fitting procedures. Comparison is made withthe similar imaging database of Mathewson, Ford, & Buchhorn, both aspresented originally by those authors and after reanalyzing theirdigital reduction files using identical disk-fitting procedures. Directcomparison is made of profile details for 292 galaxies observed incommon. Although some differences occur, good agreement is found,proving that the two data sets can be used in combination with onlyminor accommodation of those differences. The compilation of opticalproperties presented here is optimized for use in applications of theTully-Fisher relation as a secondary distance indicator in studies ofthe local peculiar velocity field.
| Near-infrared observations of galaxies in Pisces-Perseus. I. vec H-band surface photometry of 174 spiral
We present near-infrared, H-band (1.65 $() μm), surface photometry of174 spiral galaxies in the area of the Pisces-Perseus supercluster. Theimages, acquired with the ARNICA camera mounted on various telescopes,are used to derive radial profiles of surface brightness, ellipticities,and position angles, together with global parameters such as H-bandmagnitudes and diameters Radial profiles in tabular form and images FITSfiles are also available upon request from gmorio@arcetri.astro.it.}.The mean relation between H-band isophotal diameter D_{21.5} and theB-band D25 implies a B-H color of the outer disk bluer than3.5; moreover, D_{21.5}/D25 depends on (global) color andabsolute luminosity. The correlations among the various photometricparameters suggest a ratio between isophotal radius D_{21.5}/2 and diskscale length of ~ m3.5 and a mean disk central brightness ~ meq 17.5H-mag arcsec^{-2}. We confirm the trend of the concentration indexC31$ with absolute luminosity and, to a lesser degree, withmorphological type. We also assess the influence of non-axisymmetricstructures on the radial profiles and on the derived parameters. Basedon observations at the TIRGO, NOT, and VATT telescopes. TIRGO(Gornergrat, CH) is operated by CAISMI-CNR, Arcetri, Firenze. NOT (LaPalma, Canary Islands) is operated by NOTSA, the Nordic ObservatoryScientific Association. VATT (Mt. Graham, Az) is operated by VORG, theVatican Observatory Research Group Table 3 and Fig. 4 are only availablein electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html.
| The intra-cluster medium influence on spiral galaxies
We made a detailed analysis of the sample of 39 cluster spiral galaxiesof various types observed at Hα wavelength by Amram et al. (1992to 1996), with a scanning Fabry-Perot. We plotted the outer gradient oftheir rotation curves as a function of the deprojected cluster-centricdistance. The rotation curves of late type galaxies markedly rise farfrom the cluster center. This suggests evolutionary effects, since earlytypes show no special trend. We suggest that the evolution processwithin a cluster leads late type galaxies to exhibit flatter curves whenthey get closer to the center, on their way to evolving into early typegalaxies.
| Near-infrared observations of galaxies in Pisces-Perseus. III. Global scaling relations of disks and bulges
We determine the parameters of scaling relations analogous to theFundamental Plane of elliptical galaxies for the bulges and disks of asample of 40 spiral galaxies. To this end we derive structuralparameters (scalelengths and surface brightnesses) from near infrared Hband images, and kinematical parameters (rotational velocities) fromoptical rotation curves. In the case of the disks, we test the accuracyof the derived relation as a distance indicator by comparing its scatterto that of the H band Tully-Fisher relation for the same sample, andfind that the accuracy attained by the latter is slightly higher (thedispersion is 19% versus 23% for this sample). It is speculated that thedifference is due to the more robust character of global parameters,rather than those associated with the inner parts of disks. It alsoapperas that (a) either the stellar mass-to-light ratios of bulge anddisk increase with the size of the components, or (b) the bulge and diskrelative contributions to the overall rotation of the galaxy (and, as aconsequence, to its total mass) become steadily smaller with increasingsize.
| Groups of galaxies. III. Some empirical characteristics.
Not Available
| The Interchangeability of CO and H I in the Tully-Fisher Relation
We investigate the viability and precision of using ^12CO (J = 1 -->0) emission lines from galaxies in lieu of 21 cm emission in theTully-Fisher distance indicator (TF). Here we combine CO data gatheredspecifically for Tully-Fisher analysis with I-band photometry (both newand from the literature) for cluster galaxies between 3500 and 8000 kms^-1 and compare the luminosity-line width relation using CO with theresults of recent, large TF surveys using H i and Hα. We cull someCO data as suggested by previously published numerical simulations andfind that CO line widths, with corrections for turbulence andnoise-broadening on the order of 35 km s^-1, behave identically to H iand Hα in luminosity-line width analyses. We also examine therelation between CO line shapes and other parameters of the galaxies.
| Observations of (C-12)O (J = 1-0) in 44 cluster galaxies
We present (C-12)O (J = 10) (2.6 mm, 115 GHz) spectra from 44 galaxiesin clusters between 3500 and 8000 km/s. The data were obtained using theNRAO 12 m telescope at Kitt Peak. Forty galaxies are detected. We deducemolecular gas masses from the line integrated intensities and upperlimits for the four nondetections. Although the sample's first inclusioncriterion is that a source have 60 m flux greater than 350 mJy, thegalaxies in this survey are found to be neither ultraluminous in the FIRnor particularly rich in molecular gas, nor do they exhibit evidence ofinteractions. Neither the molecular gas mass nor the far-IR luminosityshows variations as functions of the galaxies' proximity to the clustercores. Because the CO line widths and central velocities agree overallwith the 21 cm widths and redshifts for these galaxies, we argue that COspectra could be used in lieu of H I spectra for Tully-Fishercalculations.
| Reexamination of the nonsymmetric gravitational theory with rotation curves of galaxies.
Not Available
| Catalogue of HI maps of galaxies. I.
A catalogue is presented of galaxies having large-scale observations inthe HI line. This catalogue collects from the literature the informationthat characterizes the observations in the 21-cm line and the way thatthese data were presented by means of maps, graphics and tables, forshowing the distribution and kinematics of the gas. It containsfurthermore a measure of the HI extension that is detected at the levelof the maximum sensitivity reached in the observations. This catalogueis intended as a guide for references on the HI maps published in theliterature from 1953 to 1995 and is the basis for the analysis of thedata presented in Paper II. The catalogue is only available inelectronic form at the CDS via anonymous ftp 130.79.128.5 orhttp://cdsweb.u-strasbg.fr/Abstract.html
| 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 catalogue of spatially resolved kinematics of galaxies: Bibliography
We present a catalogue of galaxies for which spatially resolved data ontheir internal kinematics have been published; there is no a priorirestriction regarding their morphological type. The catalogue lists thereferences to the articles where the data are published, as well as acoded description of these data: observed emission or absorption lines,velocity or velocity dispersion, radial profile or 2D field, positionangle. Tables 1, 2, and 3 are proposed in electronic form only, and areavailable from the CDS, via anonymous ftp to cdsarc.u-strasbg.fr (to130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html
| Homogeneous Velocity-Distance Data for Peculiar Velocity Analysis. III. The Mark III Catalog of Galaxy Peculiar Velocities
This is the third in a series of papers in which we assemble and analyzea homogeneous catalog of peculiar velocity data. In Papers I and II, wedescribed the Tully-Fisher (TF) redshift-distance samples thatconstitute the bulk of the catalog and our methodology for obtainingmutually consistent TF calibrations for these samples. In this paper, wesupply further technical details of the treatment of the data andpresent a subset of the catalog in tabular form. The full catalog, knownas the Mark III Catalog of Galaxy Peculiar Velocities, is available inaccessible on-line databases, as described herein. The electroniccatalog incorporates not only the TF samples discussed in Papers I andII but also elliptical galaxy Dn- sigma samples originally presentedelsewhere. The relative zero pointing of the elliptical and spiral datasets is discussed here. The basic elements of the Mark III Catalog arethe observables for each object (redshift, magnitude, velocity width,etc.) and inferred distances derived from the TF or Dn- sigma relations.Distances obtained from both the forward and inverse TF relations aretabulated for the spirals. Malmquist bias--corrected distances arecomputed for each catalog object using density fields obtained from theIRAS 1.2 Jy redshift survey. Distances for both individual objects andgroups are provided. A variety of auxiliary data, including distancesand local densities predicted from the IRAS redshift surveyreconstruction method, are tabulated as well. We study the distributionsof TF residuals for three of our samples and conclude that they are wellapproximated as Gaussian. However, for the Mathewson et al. sample wedemonstrate a significant decrease in TF scatter with increasingvelocity width. We test for, but find no evidence of, a correlationbetween TF residuals and galaxy morphology. Finally, we derivetransformations that map the apparent magnitude and velocity width datafor each spiral sample onto a common system. This permits theapplication of analysis methods that assume that a unique TF relationdescribes the entire sample.
| Optical Rotation Curves and Linewidths for Tully-Fisher Applications
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.2402C&db_key=AST
| The I band Tully-Fisher relation for cluster galaxies: data presentation.
Observational parameters which can be used for redshift-independentdistance determination using the Tully-Fisher (TF) technique are givenfor \ntot spiral galaxies in the fields of 24 clusters or groups. I bandphotometry for the full sample was either obtained by us or compiledfrom published literature. Rotational velocities are derived either from21 cm spectra or optical emission line long-slit spectra, and convertedto a homogeneous scale. In addition to presenting the data, a discussionof the various sources of error on TF parameters is introduced, and thecriteria for the assignment of membership to each cluster are given.
| The universal rotation curve of spiral galaxies - I. The dark matter connection
We use a homogeneous sample of about 1100 optical and radio rotationcurves (RCs) and relative surface photometry to investigate the mainmass structure properties of spirals, over a range of 6 mag and out to<~1.5 and 2 optical radii (for the optical and radio data,respectively). We confirm the strong dependence on luminosity for boththe profile and the amplitude of RCs claimed by Persic & Salucci.Spiral RCs show the striking feature that a single global parameter,e.g. luminosity, dictates the rotational velocity at any radius for anyobject, so revealing the existence of a universal RC. At highluminosities, there is a slight discrepancy between the profiles of RCsand those predicted from the luminous matter (LM) distributions: thisimplies a small, yet detectable, amount of dark matter (DM). At lowluminosities, the failure of the LM prediction is much more severe, andthe DM is the only relevant mass component. We show that the universalRC implies a number of scaling properties between dark and luminousgalactic structure parameters: (i) the DM/LM mass ratio scales inverselywith luminosity; (ii) the central halo density scales as L^-0.7 (iii)the halo core radius is comparable to the optical radius, but shrinksfor low luminosities; (iv) the total halo mass scales as L^0.5. Suchscaling properties can be represented as a curve in the(luminosity)-(DM/LM mass ratio)-(DM core radius)-(DM central density)space, which provides a geometrical description of the tight couplingbetween the dark and the luminous matter in spiral galaxies.
| Parameters of 2447 Southern Spiral Galaxies for Use in the Tully-Fisher Relation
I-band luminosities, rotational velocities, and redshifts of 1092 spiralgalaxies have been measured by CCD photometry and Hα spectroscopyusing the 1 m and 2.3 m telescopes at Siding Spring Observatory,respectively. The results are tabulated. Luminosity profiles andHα rotation curves are given for the galaxies. When these resultsare combined with similar data for 1355 spiral galaxies publishedpreviously (Mathewson, Ford, & Buchhorn, hereafter Paper I), itprovides a large, uniform, and unique data set with which to measure,via the Tully-Fisher relation, the peculiar velocities of galaxies inthe local universe to a distance of 11,000 km s^-1^ (Mathewson &Ford). Taking advantage of the opportunity for publishing this data inmachine-readable form, in the CD-ROM, we have also included similar datafor the 1355 galaxies in Paper I.
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