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The ISOPHOT 170 μm Serendipity Survey II. The catalog of optically identified galaxies%
The ISOPHOT Serendipity Sky Survey strip-scanning measurements covering≈15% of the far-infrared (FIR) sky at 170 μm were searched forcompact sources associated with optically identified galaxies. CompactSerendipity Survey sources with a high signal-to-noise ratio in at leasttwo ISOPHOT C200 detector pixels were selected that have a positionalassociation with a galaxy identification in the NED and/or Simbaddatabases and a galaxy counterpart visible on the Digitized Sky Surveyplates. A catalog with 170 μm fluxes for more than 1900 galaxies hasbeen established, 200 of which were measured several times. The faintest170 μm fluxes reach values just below 0.5 Jy, while the brightest,already somewhat extended galaxies have fluxes up to ≈600 Jy. For thevast majority of listed galaxies, the 170 μm fluxes were measured forthe first time. While most of the galaxies are spirals, about 70 of thesources are classified as ellipticals or lenticulars. This is the onlycurrently available large-scale galaxy catalog containing a sufficientnumber of sources with 170 μm fluxes to allow further statisticalstudies of various FIR properties.Based on observations with ISO, an ESA project with instruments fundedby ESA Member States (especially the PI countries: France, Germany, TheNetherlands and the UK) and with the participation of ISAS and NASA.Members of the Consortium on the ISOPHOT Serendipity Survey (CISS) areMPIA Heidelberg, ESA ISO SOC Villafranca, AIP Potsdam, IPAC Pasadena,Imperial College London.Full Table 4 and Table 6 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/422/39
| 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.
| 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.
| Seeking the Local Convergence Depth. IV. Tully-Fisher Observations of 35 Abell Clusters
We present Tully-Fisher observations for 35 rich Abell clusters ofgalaxies. Results from I-band photometry and optical rotation curve workconstitute the bulk of this paper. This is the third such datainstallment of an all-sky survey of 52 clusters in the distance range~50 to 200 h^-1 Mpc. The complete data set provides the basis fordetermining an accurate Tully-Fisher template relation and forestimating the amplitude and direction of the local bulk flow on a 100h^-1 Mpc scale.
| 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.
| Kinematics of the Hercules supercluster
The Hercules supercluster consists of the Abell clusters A2147, A2151,and A2152. Previous studies of the kinematics have been confounded bythe difficulty of correctly assigning galaxies to the individualclusters, which are not well separated. Our study has a total of 468available velocities for galaxies in the region, 175 of them new. Thereare 414 galaxies in the supercluster, about three times the number usedin the previous supercluster study. We verify the existence of the threeindividual clusters and compute their individual dynamical parameters.We investigate several techniques for assigning galaxy membership toclusters in this crowded field. We use the KMM mixture-modelingalgorithm to separate the galaxies into clusters; we find that A2152 hasa higher mean velocity than previous studies have reported. A2147 andA2152 also have lower velocity dispersions: 821 and 715 km/s,respectively. The assignment of galaxies to either A2152 or A2147requires velocity and position information. We study the kinematics ofthe supercluster using the two-body formalism of Beers et al. (1982) andconclude that A2147 and A2151 are probably bound to each other and thatthe supercluster as a whole may also be bound. The mass of thesupercluster, if bound, is (7.6 +/- 2.0) 10 exp 15/h M(solar); with thesupercluster luminosity, (1.4 +/- 0.2) 10 exp 13/sq h L(solar), thisyields 0.34 +/- 0.1.
| 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
| A VLA Survey of the Hercules Cluster.I.The HI Data
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....113.1939D&db_key=AST
| 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.
| Integrated photoelectric magnitudes and color indices of bright galaxies in the Johnson UBV system
The photoelectric total magnitudes and color indices published in theThird Reference Catalogue of Bright Galaxies (RC3) are based on ananalysis of approximately equals 26,000 B, 25,000 B-V, and 17,000 U-Bmultiaperture measurements available up to mid 1987 from nearly 350sources. This paper provides the full details of the analysis andestimates of internal and external errors in the parameters. Thederivation of the parameters is based on techniques described by theVaucouleurs & Corwin (1977) whereby photoelectric multiaperture dataare fitted by mean Hubble-type-dependent curves which describe theintegral of the B-band flux and the typical B-V and U-B integrated colorgradients. A sophisticated analysis of the residuals of thesemeasurements from the curves was made to allow for the random andsystematic errors that effect such data. The result is a homogeneous setof total magnitudes BTA total colors(B-V)T and (U-B)T, and effective colors(B-V)e and (U-B)e for more than 3000 brightgalaxies in RC3.
| The complex structure of Abell 2151 (Hercules)
We analyzed the space distribution of 117 galaxies in an area of 0.9 degradius centered on NGC 6045 in the Hercules cluster in the velocityrange 9000 to 14,000 km/s. By taking advantage of 74 morphologies basedon CCD images, we succeed in isolating a cluster of galaxies with anaverage velocity of 11,467 km/s located to the NE of the assumedcentroid of A2151, where early and late type galaxies share the samedynamical properties. The implications of this result for the nature andidentification of the x-ray source is briefly discussed.
| Hα velocity fields and rotation curves of galaxies in clusters
Hα maps (continuum and line), velocity contour maps and rotationcurves are presented for 15 galaxies in six different clusters: A 262, A1367, Cancer, Coma (A 1656), Hercules (A 2151) and Pegasus I. These datahave been obtained from two-dimensional Hα observations at theCanada-France-Hawaii Telescope equipped with PALILA, a scanningPerot-Fabry interferometer. They complement the set of 21 galaxiesalready observed with the same instrumentation (Amram et al. 1992a).
| Colors, Luminosities, and Masses of Disk Galaxies
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993ApJ...419..469G&db_key=AST
| Dark matter and dynamics in the Hercules Cluster (A2151)
New 21-cm observations of faint spiral galaxies in the Hercules cluster(A2151) are presented in order to investigate the dynamics throughoutthe cluster core, out to a projected radius of 1.8/h Mpc. The globaldynamical mass of Hercules is calculated using the virial theorem andthe projected mass estimator. These masses lie in the range 3-9 x 10 exp14 solar masses. The importance of subclustering in A2151 by eye isexamined via the statistical test of Dressler & Shectman (1988), andby considering the effects of the detected substructure on the dynamicalmass determination. The clumpy distribution is interpreted as a signthat the galaxies in the cluster have not reached dynamical equilibriumin the gravitational potential.
| A near-infrared imaging survey of interacting galaxies - The small angular-size ARP systems
Near-IR images of a large sample of interacting galaxies selected fromthe Atlas of Peculiar Galaxies by Arp (1966) have been obtained.Approximately 180 systems have been imaged in at least two, and usuallythree of the standard JHK bands. The survey and the observing and datareduction procedures, are described, and contour plots and aperturephotometry are presented. Future papers will analyze the imaging data bygroupings based on interaction type, stage, and progenitors. The goalsof the analysis are to explore the relationships between galaxyinteractions, activity, and morphology by studying the structure of thenear-IR luminosity distribution, where extinction effects are muchreduced relative to the optical and the major stellar mass component ofgalaxies dominates the observed light.
| Detection of excess rotation measure due to intracluster magnetic fields in clusters of galaxies
The Faraday rotation measures of a sample of extragalactic radio sourcesprojected within a third of an Abell radius of a galaxy cluster werecompared with those of sources located further from cluster centers. Theresult strongly indicates that the distribution of the residual rotationmeasure (RRM) in the former population is broadened, at a confidencelevel exceeding 99 percent. The broadening is detectable out to1/h50 Mpc. The best present estimate of the excess Faradayrotation measure varies from 100 + or - 36 rad/sq m in the central sixthof an Abell radius to 36 + or - 15 rad/sq m further out. The combinationof these results with electron densities determined from X-ray data forsome of the clusters suggests that magnetic field strengths in clustergas are of order 1 microgauss.
| Associations between quasi-stellar objects and galaxies
A table is presented here listing all close pairs of QSOs and galaxiesthat were found in a computer-aided search of catalogs of QSOs andbright galaxies and an extensive search of the literature. There is alarge excess of pairs with separations of 2 arcmin lor less, or about 60kpc, over the numbers expected if the configurations were accidental.The angular separation for 392 pairs adds to the evidence for physicalassociation, and it is shown that selection effects are not important. Ageneral rule is stated that QSOs tend to lie in the vicinity of normalgalaxies much more often than is expected by chance whether or not thegalaxies and the QSOs have the same redshifts. It is emphasized thatthis rule cannot be explained in terms of gravitational microlensing,and it is concluded that some part of the redshift of all classes ofactive nuclei is not associated with the expansion of the universe.
| The Tully-Fisher relation in different environments
The Tully-Fisher relation (TFR) in different environments wasinvestigated in 13 galaxy samples spanning a large range in galaxydensities, using two statistical tests to compare the TFR of differentsamples. Results of the analysis of TFR parameters in severalenvironments showed that, when samples of similar data-accuracy andmagnitude-range were compared, there was no significant differencebetween the galaxy samples. It is suggested that a comparison of sampleswith very different data accuracy or those biased by incompletenesseffects may lead to misleading results.
| The faint end of the Zwicky magnitude scale - CCD isophotal magnitudes versus Zwicky magnitudes
Zwicky magnitudes are compared to blue isophotal magnitudes derived fromsurface photometry of digital galaxy images to study the isophotalnature of the Zwicky magnitude scale at the faint end. The approximateisophote that corresponds to the magnitude tabulated in the Catalog ofGroups and Clusters of Galaxies (Zwicky et al. 1961-1968). It is foundthat, in the mean, the Zwicky magnitude closely corresponds to the bluemagnitude measured with the B = 26.0 mag/sq arcsec isophote. The scatteris 0.31 mag and the distribution of isophotal surface brightness is verybroad, however, making the Zwicky magnitudes only accurate to about 30percent when used a luminosity indicator. It is shown that relativedifferences in Zwicky magnitude do not provide an accurate gage of thetrue relative luminosities of galaxies.
| The distribution of mass for spiral galaxies in clusters and in the field
A comparison is made between the mass distributions of spiral galaxiesin clusters and in the field using Burstein's mass-type methodology.Both the H-alpha emission-line rotation curves and more extended H Irotation curves are used. The fitting technique for determining masstypes used by Burstein and coworkers has been replaced by an objectivechi-sq method. Mass types are shown to be a function of both the Hubbletype and luminosity, contrary to earlier results. The present data showa difference in the distribution of mass types for spiral galaxies inthe field and in clusters, in the sense that mass type I galaxies, wherethe inner and outer velocity gradients are similar, are generally foundin the field rather than in clusters. This can be understood in terms ofthe results of Whitmore, Forbes, and Rubin (1988), who find that therotation curves of galaxies in the central region of clusters aregenerally failing, while the outer galaxies in a cluster and fieldgalaxies tend to have flat or rising rotation curves.
| Rotation curves for spiral galaxies in clusters and in the field
This paper compares the H-alpha emission-line rotation curves and the HI rotation curves of spiral galaxies in clusters with their counterpartsin the field, using the following three criteria: the inner and outervelocity gradients, the mass-to-light ratio (M/L) gradients, and theBurstein's mass-type methodology. Results show a good correlationbetween the outer gradient of the rotation curve and the galaxy'sdistance from the center of the cluster; namely, the inner galaxies tendto have falling rotation curves, while the outer galaxies and fieldgalaxies tend to have flat or rising rotation curves. In addition, acorrelation was found between the M/L gradient across a galaxy and thegalaxy's position in the cluster, with the outer galaxies having steeperM/L gradients. Contrary to earlier reports, the mass types for fieldspirals were found to be a function of both Hubble-type and luminosity.These correlations indicate that the inner cluster environment can stripaway some fraction of the mass in the outer halo of a spiral galaxy.
| Rotation curves for spiral galaxies in clusters. II - Variations as a function of cluster position
Inner and outer velocity gradients, residuals from synthetic rotationcurves for field spirals, and M/L gradients are used to study therotation curves of spiral galaxies. A good correlation is found betweenthe outer gradient of the rotation curve and the galaxy's distance fromthe cluster center, with a similar effect noted in the residuals betweenthe observed and synthetic rotation curves. A correlation is also shownto exist between the M/L gradient across a galaxy and the galaxy'sposition in the cluster. The results suggest that the inner clusterenvironment may strip away some fraction of the mass in the outer haloof a spiral galaxy or may not allow the halo to form.
| Rotation curves for spiral galaxies in clusters. I - Data, global properties, and a comparison with field galaxies
Rotational velocities have been obtained for 21 galaxies in the largespiral-rich clusters Cancer, Hercules, Peg I, and DC 1842-63. It isnoted that the larger, brighter, more massive spirals which are rare inthe field are absent in the cluster spirals. Falling rotation curveshave been found. The amplitudes of the rotation curves for the nine Saand Sb galaxies considered are shown to be lower than those of theirfield counterparts. The results indicate that galaxies which are H Ideficient have rotation curves which are most depressed in comparisonwith field spirals of equivalent Hubble type and luminosity.
| Isophotal diameters of cluster spirals
The applicability of isophotal diameters for measuring the sizes ofgalaxies is examined by comparing diameters derived using surfacephotometry with those derived from the Uppsala General Catalogue ofGalaxies (UGC). The sample studied consisted of a subset of galaxiesfrom the CCD survey of Bothun (1981). The surface photometry techniqueused is described, and the surface brightness profiles were extractedfrom the data using the galaxy surface photometry package of Cawson(1983). Isophotal diameters were derived and compared with those fromthe UGC. The differences between the data are 2.4 arcsec for the galaxydiameter, 0.03 for the galaxy ellipticities, and 0.05 mag for the galaxymagnitudes; it is observed that the isophotal diameters determined bysurface photometry are more accurate than those tabulated by UGC. The21-cm line width/diameter relation and the absolute magnitude/surfacebrightness relation are analyzed using the isophotal diameter data.
| Far-infrared properties of cluster galaxies
Far-infrared properties are derived for a sample of over 200 galaxies inseven clusters: A262, Cancer, A1367, A1656 (Coma), A2147, A2151(Hercules), and Pegasus. The IR-selected sample consists almost entirelyof IR normal galaxies, with Log of L(FIR) = 9.79 solar luminosities, Logof L(FIR)/L(B) = 0.79, and Log of S(100 microns)/S(60 microns) = 0.42.None of the sample galaxies has Log of L(FIR) greater than 11.0 solarluminosities, and only one has a FIR-to-blue luminosity ratio greaterthan 10. No significant differences are found in the FIR properties ofHI-deficient and HI-normal cluster galaxies.
| A catalog of galaxies in Hercules from the Palomar Sky Survey and the Minnesota Automated Plate Scanner
The development of galaxies catalogs from the Palomar Sky Survey usingthe Minnesota Automated Plate Scanner (APS) is examined. The design andoperation of APS are described. The algorithm used to distinguish starsfrom galaxies is discussed, and the completeness and confusion of thealgorithm as a function of magnitude are estimated. The quality of thephotometric calibration for galaxy magnitudes and surface-brightnessthresholds is evaluated. The relation between the distribution of colorsand morphological types is studied. The luminosity functions forHercules galaxies are calculated and presented. The catalog generatedusing the APS is 80 percent complete; photometry good to 0.23 mag rms ispossible; and J-F colors are good to 0.17 mag rms.
| Cluster population incompleteness bias and the value of H(0) from the Tully-Fisher B0(T) relation
Data on the Virgo cluster and ten more distant clusters are the basis ofan evaluation of the influence of the cluster population incompletenessbias on the B-band Tully-Fisher relation. The data are well fitted by atheoretical curve that is obtained for a Hubble constant value of 72 +or - 5 km/sec per Mpc in the de Vaucouleurs local scale, confirming theconstant's previous determination in light of a study of the Malmquistbias for field galaxies. The true value for the Hubble constant isconcluded to lie within the 50-75 range, depending on the primarycalibration.
| The Distance to the Hercules Supercluster. II. Application of Tertiary Indicators and an Estimate of the Hubble Constant
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1986ApJS...62..283B&db_key=AST
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