- ID:
- ivo://CDS.VizieR/VIII/29A
- Title:
- 1400-MHz Survey of 1478 Abell Clusters of Galaxies
- Short Name:
- VIII/29A
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness>=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10>=17.0; richness<=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.
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- ID:
- ivo://CDS.VizieR/J/A+AS/74/315
- Title:
- 327 MHz Survey of the A262 cluster region
- Short Name:
- J/A+AS/74/315
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This catalog contains a survey at 327 MHz of the A262 cluster region. The survey was performed with the WSRT Telescope in the redundancy mode, and covers a circular region of 21 square degrees towards A262 (RA = 01h49m50s, decl = 35d54'20" -- B1950). The synthesized beam width is 56" x 93" (RA x DEC). 309 sources were detected, with a detection limit of 7 mJy (~5 sigma) at the field center. Nine of these galaxies have been identified with galaxies of the A262 cluster.
- ID:
- ivo://CDS.VizieR/J/A+A/406/867
- Title:
- Mid-IR galaxies in Virgo cluster. III.
- Short Name:
- J/A+A/406/867
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present ISOCAM imaging data at 6.75 and 15{mu}m for 145 galaxies in the Virgo cluster and in the Coma/A1367 supercluster. Of these, 99 form a complete, optically-selected, volume-limited sample including galaxies in the core and in the periphery of the Virgo cluster, suitable for statistical analysis. 34 of the Virgo galaxies were resolved by ISOCAM: for these objects we present mid-IR images, radial light and colour profiles, as well as effective and isophotal radii, surface brightness and light concentration indices.
- ID:
- ivo://CDS.VizieR/J/ApJ/800/80
- Title:
- MIR properties of galaxies in A2199 at z~0.03
- Short Name:
- J/ApJ/800/80
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study the mid-infrared (MIR) properties of the galaxies in the A2199 supercluster at z=0.03 to understand the star formation activity of galaxy groups and clusters in the supercluster environment. Using the Wide-field Infrared Survey Explorer (WISE) data, we find no dependence of mass-normalized integrated star formation rates of galaxy groups/clusters on their virial masses. We classify the supercluster galaxies into three classes in the MIR color-luminosity diagram: MIR blue cloud (massive, quiescent, and mostly early-type), MIR star-forming sequence (mostly late-type), and MIR green valley galaxies. These MIR green valley galaxies are distinguishable from the optical green valley galaxies in the sense that they belong to the optical red sequence. We find that the fraction of each MIR class does not depend on the virial mass of each group/cluster. We compare the cumulative distributions of surface galaxy number density and cluster/group-centric distance for the three MIR classes. MIR green valley galaxies show the distribution between MIR blue cloud and MIR star-forming (SF) sequence galaxies. However, if we fix galaxy morphology, early- and late-type MIR green valley galaxies show different distributions. Our results suggest a possible evolutionary scenario of these galaxies: (1) late-type MIR SF sequence galaxies --> (2) late-type MIR green valley galaxies --> (3) early-type MIR green valley galaxies --> (4) early-type MIR blue cloud galaxies. In this sequence, the star formation of galaxies is quenched before the galaxies enter the MIR green valley, and then morphological transformation occurs in the MIR green valley.
- ID:
- ivo://CDS.VizieR/J/AJ/110/2131
- Title:
- M/L for Draco and UMi. I.
- Short Name:
- J/AJ/110/2131
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.
- ID:
- ivo://CDS.VizieR/J/ApJS/229/20
- Title:
- MMT/Hectospec redshift survey for Abell 2029
- Short Name:
- J/ApJS/229/20
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Based on an extensive redshift survey for galaxy clusters Abell 2029 and Coma, we measure the luminosity functions (LFs) and stellar mass functions (SMFs) for the entire cluster member galaxies. Most importantly, we measure the velocity dispersion functions (VDFs) for quiescent members. The MMT/Hectospec redshift survey for galaxies in A2029 identifies 982 spectroscopic members; for 838 members, we derive the central velocity dispersion from the spectroscopy. Coma is the only other cluster surveyed as densely. The LFs, SMFs, and VDFs for A2029 and Coma are essentially identical. The SMFs of the clusters are consistent with simulations. The A2029 and Coma VDFs for quiescent galaxies have a significantly steeper slope than those of field galaxies for velocity dispersion 100km/s. The cluster VDFs also exceed the field at velocity dispersion 250km/s. The differences between cluster and field VDFs are potentially important tests of simulations and of the formation of structure in the universe.
- ID:
- ivo://CDS.VizieR/J/ApJ/903/151
- Title:
- MMT spectroscopic redshift catalog of the A521 field
- Short Name:
- J/ApJ/903/151
- Date:
- 21 Mar 2022 05:59:04
- Publisher:
- CDS
- Description:
- A521 has been a subject of extensive panchromatic studies from X-ray to radio. The cluster possesses a number of remarkable features, including a bright radio relic with a steep spectrum, more than three distinct galaxy groups forming a filament, and two disturbed X-ray peaks at odds with the distant position and tilted orientation of the radio relic. These lines of evidence indicate a complex merger. In this paper, we present a multiwavelength study of A521 based on Subaru optical, Hubble Space Telescope infrared, Chandra X-ray, Giant Metrewave Radio Telescope radio, and Multiple Mirror Telescope optical spectroscopic observations. Our weak-lensing (WL) analysis with improved systematics control reveals that A521 is mainly composed of three substructures aligned in the northwest to southeast orientation. These WL mass substructures are remarkably well-aligned with the cluster optical luminosity distribution constructed from our new enhanced cluster member catalog. These individual substructure masses are determined by simultaneously fitting three Navarro-Frenk-White profiles. We find that the total mass of A521 modeled by the superposition of the three halos is 13.0_-1.3_^+1.0^x10^14^M{odot}, a factor of 2 higher than the previous WL measurement. With these WL mass constraints combined with X-ray and radio features, we consider two merging scenarios, carry out the corresponding numerical simulations, and discuss the strengths and weaknesses of each case.
- ID:
- ivo://CDS.VizieR/J/A+A/540/A96
- Title:
- Molecular gas in Hickson Compact Groups
- Short Name:
- J/A+A/540/A96
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study the effect of the extreme environment in Hickson Compact Groups (HCGs) on the molecular gas mass, M_H2_, and the star formation rate (SFR) of galaxies as a function of atomic hydrogen (HI) content and evolutionary phase of the group. We selected a redshift-limited (D<100Mpc) sample of 88 galaxies in 20 HCGs with available atomic hydrogen (HI) VLA maps, covering a wide range of HI deficiencies and evolutionary phases of the groups containing at least one spiral galaxy. We observed the CO(1-0) and CO(2-1) lines with the IRAM 30m telescope for 47 galaxies. Together with literature data, our sample contains CO(1-0) spectra for 86 galaxies. We derived the far-infrared (FIR) luminosity L_FIR_ from IRAS data and used it as a tracer of the star formation rate (SFR). We calculated the HI mass, M_HI_ L_FIR_ and M_H2_ deficiencies, based on the values expected from L_B_ and L_K_ in isolated galaxies from the AMIGA sample. We limited our statistical analysis to spiral galaxies, since the large number of upper limits did not allow drawing strong conclusions about M_H2_ and L_FIR_ in early-type galaxies.
- ID:
- ivo://CDS.VizieR/J/MNRAS/432/3141
- Title:
- Morphological classification of PM2GC galaxies
- Short Name:
- J/MNRAS/432/3141
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study the galaxy stellar mass function in different environments in the local Universe, considering both the total mass function and that of individual galaxy morphological types. We compare the mass functions of galaxies with log_10_M*/M_{sun}_>=10.25 in the general field and in galaxy groups, binary and single galaxy systems from the Padova-Millennium Galaxy and Group Catalogue at z=0.04-0.1 with the mass function of galaxy clusters of the WIde-field Nearby Galaxy-Cluster Survey at z=0.04-0.07. Strikingly, the variations of the mass function with global environment, overall, are small and subtle. The shapes of the mass functions of the general field and clusters are indistinguishable, and only small, statistically insignificant variations are allowed in groups. Only the mass function of our single galaxies, representing the least massive haloes and comprising less than a third of the general field population, is proportionally richer in low-mass galaxies than other environments. The most notable environmental effect is a progressive change in the upper galaxy mass, with very massive galaxies found only in the most massive environments. This environment-dependent mass cut-off is unable to affect the Schechter parameters and the Kolmogorov-Smirnov test, and can only be revealed by an ad hoc analysis. Finally, we show how, in each given environment, the mass function changes with morphological type, and that galaxies of the same morphological type can have different mass functions in different environments.
- ID:
- ivo://CDS.VizieR/VII/174
- Title:
- Morphological type catalog in 55 rich galaxy clusters
- Short Name:
- VII/174
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.
