- ID:
- ivo://CDS.VizieR/J/AJ/147/52
- Title:
- Structures in the Chandra Deep Field-South
- Short Name:
- J/AJ/147/52
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a comprehensive structure detection analysis of the 0.3deg^2^ area of the MUSYC-ACES field, which covers the Chandra Deep Field-South (CDFS). Using a density-based clustering algorithm on the MUSYC and ACES photometric and spectroscopic catalogs, we find 62 overdense regions up to redshifts of 1, including clusters, groups, and filaments. We also present the detection of a relatively small void of ~10Mpc^2^ at z~0.53. All structures are confirmed using the DBSCAN method, including the detection of nine structures previously reported in the literature. We present a catalog of all structures present, including their central position, mean redshift, velocity dispersions, and classification based on their morphological and spectroscopic distributions. In particular, we find 13 galaxy clusters and 6 large groups/small clusters. Comparison of these massive structures with published XMM-Newton imaging (where available) shows that 80% of these structures are associated with diffuse, soft-band (0.4-1keV) X-ray emission, including 90% of all objects classified as clusters. The presence of soft-band X-ray emission in these massive structures (M_200_{>=}4.9x10^13^M_{sun}_) provides a strong independent confirmation of our methodology and classification scheme. In the closest two clusters identified (z<0.13) high-quality optical ur photometric sample contains 5522 galaxies imaging from the Deep2c field of the Garching-Bonn Deep Survey reveals the cD galaxies and demonstrates that they sit at the center of the detected X-ray emission. Nearly 60% of the clusters, groups, and filaments are detected in the known enhanced density regions of the CDFS at z=~0.13, 0.52, 0.68, and 0.73. Additionally, all of the clusters, bar the most distant, are found in these overdense redshift regions. Many of the clusters and groups exhibit signs of ongoing formation seen in their velocity distributions, position within the detected cosmic web, and in one case through the presence of tidally disrupted central galaxies exhibiting trails of stars. These results all provide strong support for hierarchical structure formation up to redshifts of 1.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/369/1131
- Title:
- Structures in the GA region
- Short Name:
- J/MNRAS/369/1131
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- To further our understanding of the Great Attractor (GA), we have undertaken a redshift survey using the 2dF on the AAT. Clusters and filaments in the GA region were targeted with 25 separate pointings resulting in approximately 2600 new redshifts. Targets included poorly studied X-ray clusters from the CIZA catalogue as well as the Cen-Crux and PKS 1343-601 clusters, both of which lie close to the classic GA centre. For nine clusters in the region, we report velocity distributions as well as virial and projected mass estimates. The virial mass of CIZA J1324.75736, now identified as a separate structure from the Cen-Crux cluster, is found to be ~3x10^14^M_{sun}_ in good agreement with the X-ray inferred mass. In the PKS 1343-601 field, five redshifts are measured of which four are new. An analysis of redshifts from this survey, in combination with those from the literature, reveals the dominant structure in the GA region to be a large filament, which appears to extend from Abell S0639 (l=281{deg}, b=+11{deg}) to (l~5{deg}, b~-50{deg}), encompassing the Cen-Crux, CIZA J1324.75736, Norma and Pavo II clusters. Behind the Norma Cluster at cz~15000km/s, the masses of four rich clusters are calculated. These clusters (Triangulum-Australis, Ara, CIZA J1514.64558 and CIZA J1410.44246) may contribute to a continued large- scale flow beyond the GA. The results of these observations will be incorporated into a subsequent analysis of the GA flow.
1013. Study of Abell 119
- ID:
- ivo://CDS.VizieR/J/AJ/105/788
- Title:
- Study of Abell 119
- Short Name:
- J/AJ/105/788
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report 60 new radial velocities, as well as new photographic and CCD photometry.
- ID:
- ivo://CDS.VizieR/J/ApJ/669/714
- Title:
- Subaru weak-lensing survey. I.
- Short Name:
- J/ApJ/669/714
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of an ongoing weak-lensing survey conducted with the Subaru Telescope whose initial goal is to locate and study the distribution of shear-selected structures, or halos. Using a Suprime-Cam imaging survey spanning 21.82deg^2^, we present a catalog of 100 candidate halos located from lensing-convergence maps. Our sample is reliably drawn from that subset of our survey area (totaling 16.72deg^2^) uncontaminated by bright stars and edge effects and is limited at a convergence signal-to-noise ratio of 3.69. To validate the sample, detailed spectroscopic measures have been made for 26 candidates using the Subaru multiobject spectrograph, FOCAS. All are confirmed as clusters of galaxies, but two arise as the superposition of multiple clusters viewed along the line of sight. Including data available in the literature and an ongoing Keck spectroscopic campaign, a total of 41 halos now have reliable redshifts.
- ID:
- ivo://CDS.VizieR/J/MNRAS/384/1611
- Title:
- Submm observations in gravitational lenses
- Short Name:
- J/MNRAS/384/1611
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z>>2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes <2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (>50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850>6mJy contribute only 10 per cent.
- ID:
- ivo://CDS.VizieR/J/A+A/470/39
- Title:
- Substructures in WINGS clusters
- Short Name:
- J/A+A/470/39
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We search for and characterize substructures in the projected distribution of galaxies observed in the wide field CCD images of the 77 nearby clusters of the WIde-field Nearby Galaxy-cluster Survey (WINGS). This sample is complete in X-ray flux in the redshift range 0.04<z<0.07. We search for substructures in WINGS clusters with DEDICA, an adaptive-kernel procedure. We test the procedure on Monte-Carlo simulations of the observed frames and determine the reliability for the detected structures.
- ID:
- ivo://CDS.VizieR/J/MNRAS/376/1073
- Title:
- Sunyaev-Zel'dovich effect in galaxy clusters
- Short Name:
- J/MNRAS/376/1073
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In a search for evidence of the short wavelength increment in the Sunyaev-Zel'dovich (SZ) effect, we have analysed archival galaxy cluster data from the Submillimetre Common User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope, resulting in the most complete pointed survey of clusters at 850{mu}m to date. SCUBA's 850{mu}m passband overlaps the peak of the SZ increment. The sample consists of 44 galaxy clusters in the range 0<z<1.3. Maps of each of the clusters have been made and sources have been extracted; as an ancillary product, we generate the most thorough galaxy cluster point source list yet from SCUBA. 17 of these clusters are free of obvious active galactic nuclei (AGN) and have data deep enough to provide interesting measurements of the expected SZ signal.
- ID:
- ivo://CDS.VizieR/J/ApJS/253/3
- Title:
- Sunyaev-Zel'dovich galaxy clusters surveyed by ACT
- Short Name:
- J/ApJS/253/3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a catalog of 4195 optically confirmed Sunyaev-Zel'dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13211deg^2^ of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04<z<1.91 (median z=0.52). The catalog contains 222 z>1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M_500c_>3.8x10^14^M_{sun}_, evaluated at z=0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2.4'. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566deg^2^), the Hyper Suprime-Cam Subaru Strategic Program (469deg^2^), and the Kilo Degree Survey (825deg^2^). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10Gyr.
- ID:
- ivo://CDS.VizieR/J/A+A/459/L1
- Title:
- Supercluster sample from SDSS DR4
- Short Name:
- J/A+A/459/L1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We compile a supercluster sample using the Sloan Digital Sky Survey Data Release 4, and reanalyse supercluster samples found for the 2dF Galaxy Redshift Survey and for simulated galaxies of the Millennium Run. We find for all supercluster samples Density Field (DF) clusters, which represent high-density peaks of the class of Abell clusters, and use median luminosities of richness class 1 DF-clusters to calculate relative luminosity functions. We show that the fraction of very luminous superclusters in real samples is about five times greater than in simulated samples. Superclusters are generated by large-scale density perturbations that evolve very slowly. The absence of very luminous superclusters in simulations can be explained either by incorrect treatment of large-scale perturbations, or by some yet unknown processes in the very early Universe.
1020. Superclusters and voids
- ID:
- ivo://CDS.VizieR/J/MNRAS/269/301
- Title:
- Superclusters and voids
- Short Name:
- J/MNRAS/269/301
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study the whole-sky distribution of rich clusters of galaxies up to the distance z~0.1 and present catalogues of superclusters and cluster-defined voids. The data on clusters, superclusters and voids show the presence of the characteristic scale of 130h^-1^Mpc in the supercluster-void network, found earlier by Broadhurst et al. (1990Natur.343..726B) from a one-dimensional study. This scale has been detected in the distribution of clusters of richnesses R=0 and R>=1. We perform tests to study the influence of projection effects. The clusters that do not belong to superclusters are located in the vicinity of superclusters and form their outlying parts. We compare the distribution of ACO clusters with that of APM clusters. The APM clusters determine a smaller scale: 100h^-1^Mpc. We discuss the possible reasons for this difference.
