- ID:
- ivo://CDS.VizieR/J/AJ/111/42
- Title:
- Galaxies in Abell 168
- Short Name:
- J/AJ/111/42
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- V- and I- band CCD photometry of the central 0.18 square degree of Abell 168 was observed in November and December 1993 at the 1.05m Kiso Schmidt telescope (f/3.1). The CCD chip has 1000x1018 pixels, the pixel size is 0.752arcsec, giving a field of view of 12.0x12.7 arcmin. The total observed region was covered by 7 individual CCD fields. Note that some revisions were made by the author (TOMITA Akihiko) compared to the original publication.
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- ID:
- ivo://CDS.VizieR/J/AZh/76/83
- Title:
- Galaxies in and near the cluster A1185
- Short Name:
- J/AZh/76/83
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7,3.9,7.6, and 31 cm, together with data published in other study. At the cluster center some of the galaxies have either flat or inverted spectra.
- ID:
- ivo://CDS.VizieR/J/ApJS/78/1
- Title:
- Galaxies in 7 clusters 0.35<z<0.55
- Short Name:
- J/ApJS/78/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present photometry and spectroscopy for seven deep fields containing distant clusters of galaxies with 0.35<z<0.55. Positions and photometric parameters, including r-magnitudes g-r and r-i colors, surface brightnesses, and photometric profile types are given for about 2000 galaxies. Low-resolution spectroscopy is obtained from which redshifts are determined for 289 objects, of which 190 are cluster members.
- ID:
- ivo://CDS.VizieR/VII/180
- Title:
- Galaxies in Fornax Cluster and five nearby groups
- Short Name:
- VII/180
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.
- ID:
- ivo://CDS.VizieR/J/MNRAS/395/1213
- Title:
- Galaxies in the field of MACS J1206.2-0847
- Short Name:
- J/MNRAS/395/1213
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We discuss the X-ray and optical properties of the massive galaxy cluster MACSJ1206.2-0847 (z=0.4385), discovered in the Massive Cluster Survey (MACS). Our Chandra observation of the system yields a total X-ray luminosity of 2.4x10^45^erg/s (0.1-2.4keV) and a global gas temperature of 11.6+/-0.7keV, very high values typical of MACS clusters. In both optical and X-ray images, MACSJ1206.2-0847 appears close to relaxed in projection, with a pronounced X-ray peak at the location of the brightest cluster galaxy (BCG); we interpret this feature as the remnant of a cold core. A spectacular giant gravitational arc, 15-arcsec in length, bright (V~21) and unusually red (R-K=4.3), is seen 20-arcsec west of the BCG; we measure a redshift of z=1.036 for the lensed galaxy. From our Hubble Space Telescope image of the cluster, we identify the giant arc and its counter image as a sevenfold imaged system. An excess of X-ray emission in the direction of the arc coincides with a mild galaxy overdensity and could be the remnant of a minor merger with a group of galaxies. We derive estimates of the total cluster mass as well as of the mass of the cluster core using X-ray, dynamical and gravitational-lensing techniques. For the mass enclosed by the giant arc (r<119kpc), our strong-lensing analysis based on Hubble Space Telescope imaging yields a very high value of 1.1x10^14^M_{sun}_, inconsistent with the much lower X-ray estimate of 0.5x10^14^M_{sun}_. Similarly, the virial estimate of 4x10^15^M_{sun}_ for the total cluster mass, derived from multi-object spectroscopy with Canada-France-Hawaii Telescope (CFHT) and the VLT of 38 cluster members, is significantly higher than the corresponding X-ray estimate of 1.7x10^15^M_{sun}_. We take the discrepancy between X-ray and other mass estimates to be indicative of pronounced substructure along the line of sight during an ongoing merger event, an interpretation that is supported by the system's very high velocity dispersion of 1580km/s.
- ID:
- ivo://CDS.VizieR/J/other/AstBu/73.124
- Title:
- Galaxies in the Local Supercluster band
- Short Name:
- J/other/AstBu/73
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate the distribution and velocity field of galaxies situated in a band of 100x20 degrees centered on M87 and oriented along the Local supercluster plane. Our sample amounts 2158 galaxies with radial velocities less than 2000 km/s. Of them, 1119 galaxies (52%) have distance and peculiar velocity estimates. About 3/4 of early-type galaxies are concentrated within the Virgo cluster core, most of the late-type galaxies in the band locate outside the virial radius. Distribution of gas-rich dwarfs with M_HI_> M* looks to be insensitive to the Virgo cluster presence. Among 50 galaxy groups in the equatorial supercluster band 6 groups have peculiar velocities about 500-1000km/s comparable with virial motions in rich clusters. The most cryptic case is a flock of nearly 30 galaxies around NGC4278 (Coma I cloud), moving to us with the mean peculiar velocity of -840km/s. This cloud (or filament?) resides at a distance of 16.1Mpc from us and approximately 5Mpc away from the Virgo center. Galaxies around Virgo cluster exhibit Virgocentric infall with an amplitude of about 500 km/s. Assuming the spherically symmetric radial infall, we estimate the radius of the zero-velocity surface to be R0=(7.0+/-0.3)Mpc that yields the total mass of Virgo cluster to be (7.4+/-0.9)x10^14^ solar masses, in tight agreement with its virial mass estimates. We conclude that the Virgo outskirts does not contain significant amounts of dark mater beyond its virial core.
- ID:
- ivo://CDS.VizieR/J/A+AS/139/141
- Title:
- Galaxies in the Perseus Cluster
- Short Name:
- J/A+AS/139/141
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A new catalogue of 660 galaxies within a field of about 10 square degrees in the Perseus cluster region is presented. The catalogue contains accurate positions, isophotal magnitudes, angular radii, position angles, radial velocities, morphological types, and detailed informations on morphological peculiarities. If available, cross identifications and radial velocities are also given. The catalogue is estimated to be complete to a 25mag isophotal B magnitude of about 18.
- ID:
- ivo://CDS.VizieR/J/A+A/640/A30
- Title:
- Galaxies in the Perseus cluster field
- Short Name:
- J/A+A/640/A30
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate the galaxies brighter than B~20 in the field of the Perseus cluster. The galaxies were selected on Schmidt CCD images in B and Halpha in combination with SDSS images. The survey field roughly covers the virial radius of the cluster. The galaxy sample is used for analysing cluster properties, such as radial profiles, indications of sub-structure, virial mass, and viral radius and is applied for a study of the cluster galaxy population with an emphasis on morphological types and peculiarities, star formation rates and active galactic nuclei.
- ID:
- ivo://CDS.VizieR/J/MNRAS/437/1858
- Title:
- Galaxies in the RX J1347.5-1145 cluster
- Short Name:
- J/MNRAS/437/1858
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a revised strong lensing mass reconstruction of the galaxy cluster RX J1347.5-1145. The X-ray luminous cluster at redshift z=0.451 has already been studied intensively in the past. Based on information of two such previous (strong-) lensing studies by Halkola et al. (2008A&A...481...65H) and Bradac et al. (2008ApJ...681..187B), as well as by incorporating newly available data from the Cluster Lensing And Supernova survey with Hubble, we identified four systems of multiply lensed images (anew) in the redshift range 1.75<=z<=4.19. One multiple image system consists of in total eight multiply lensed images of the same source. The analysis based on a parametric mass model derived with the software GLAFIC suggests that the high image multiplicity is due to the source (z_phot_=4.19) being located on a so-called 'swallowtail' caustic. In addition to the parametric mass model, we also employed a non-parametric approach using the software pixelens in order to reconstruct the projected mass of the cluster using the same strong lensing data input. Both reconstructed mass models agree in revealing several mass components and a highly elliptic shape of the mass distribution. Furthermore, the projected mass inside, for example, a radius R~35arcsec~200kpc of the cluster for a source at redshift z=1.75 is M(<R)~(2.19^+0.01^_-0.02_)*10^14^M_{sun}_ as estimated by GLAFIC. Within the same radius pixelens predicts a mass of M(<R)~(2.47+/-0.01)*10^14^M_{sun}_which exceeds the GLAFIC estimate by ~13 per cent. The difference could be related to the fundamental degeneracy involved when constraining dark matter substructures with gravitationally lensed arcs.
- ID:
- ivo://CDS.VizieR/J/MNRAS/429/2264
- Title:
- Galaxies in the UMa cluster complex
- Short Name:
- J/MNRAS/429/2264
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A nearby friable cloud in Ursa Majoris contains 270 galaxies with radial velocities 500<V_LG_<1500km/s inside the area of RA=[11.0h,13.0h] and DE=[+40{deg},+60{deg}]. At present, 97 galaxies of them have individual distance estimates. We use these data to clarify the structure and kinematics of the UMa complex. According to Makarov & Karachentsev (2011MNRAS.412.2498M, Cat. J/MNRAS/412/2498), most of the UMa galaxies belong to seven bound groups, which have the following median parameters: velocity dispersion of 58k/s, harmonic projected radius of 300kpc, virial mass of 2x10^12^M{sun} and virial mass-to-K-band luminosity ratio of 27M{sun}/L{sun}. Almost a half of the UMa cloud population are gas-rich dwarfs (Ir, Im, BCD) with active star formation seen in the GALEX UV-survey. The UMa groups reside within 15-19Mpc from us, being just at the same distance as the Virgo cluster. The total virial mass of the UMa groups is 4x10^13^M{sun}, yielding the average density of dark matter in the UMa cloud to be {Omega}m=0.08, i.e. a factor of 3 lower than the cosmic average. This is despite the fact that the UMa cloud resides in a region of the Universe that is an apparent overdensity. A possible explanation for this is that most mass in the Universe lies in the empty space between clusters. Herewith, the mean distances and velocities of the UMa groups follow nearly undisturbed Hubble flow without a sign of the 'Z-wave' effect caused by infall towards a massive attractor. This constrains the total amount of dark matter between the UMa groups within the cloud volume.
