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1161. WISE Massive & Distant Clusters (MaDCoWS). II.
ID:
ivo://CDS.VizieR/J/ApJS/213/25
Title:
WISE Massive & Distant Clusters (MaDCoWS). II.
Short Name:
J/ApJS/213/25
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present optical and infrared imaging and optical spectroscopy of galaxy clusters which were identified as part of an all-sky search for high-redshift galaxy clusters, the Massive and Distant Clusters of WISE Survey (MaDCoWS). The initial phase of MaDCoWS combined infrared data from the all-sky data release of the Wide-field Infrared Survey Explorer (WISE) with optical data from the Sloan Digital Sky Survey to select probable z~1 clusters of galaxies over an area of 10000deg^2^. Our spectroscopy confirms 19 new clusters at 0.7<z<1.3, half of which are at z>1, demonstrating the viability of using WISE to identify high-redshift galaxy clusters. The next phase of MaDCoWS will use the greater depth of the AllWISE data release to identify even higher redshift cluster candidates.
1162. WISE W1/W2 Tully-Fisher relation calibrator data
ID:
ivo://CDS.VizieR/J/ApJ/792/129
Title:
WISE W1/W2 Tully-Fisher relation calibrator data
Short Name:
J/ApJ/792/129
Date:
21 Oct 2021
Publisher:
CDS
Description:
In order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminosities-capable of providing such distance measures-to the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 (3.4 {mu}m) and W2 (4.6 {mu}m) filters. We find a correlation of line width to absolute magnitude (known as the Tully-Fisher relation, TFR) of M_W1_^b,i,k,a^=-20.35-9.56(logW_mx_^i^-2.5) (0.54 mag rms) and M_W2_^b,i,k,a^=-19.76-9.74(logW_mx_^i^-2.5) (0.56 mag rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully & Courtois (2012ApJ...749...78T). We derive M_l_^b,i,k^=-21.34-8.95(logW_mx_^i^-2.5) (0.46 mag rms). The WISE TFRs show evidence of curvature. Quadratic fits give M_W1_^b,i,k,a^=-20.48-8.36(logW_mx_^i^-2.5)+3.60(loglogW_mx_^i^-2.5)^2^ (0.52 mag rms) and M_W2_^b,i,k,a^=-19.91-8.40(logW_mx_^i^-2.5)+ 4.32(loglogW_mx_^i^ -2.5)^2^ (0.55 mag rms). We apply an I-band -WISE color correction to lower the scatter and derive M_Cw1_=-20.22-9.12(logW_mx_^i^-2.5) and M_Cw2_=-19.63-9.11(logW_mx_^i^-2.5) (both 0.46 mag rms). Using our three independent TFRs (W1 curved, W2 curved, and I band), we calibrate the UNION2 Type Ia supernova sample distance scale and derive H_0_=74.4+/-1.4(stat)+/-2.4(sys) km/s/Mpc with 4% total error.
1163. WMAP observations of Planck ESZ clusters
ID:
ivo://CDS.VizieR/J/ApJ/771/137
Title:
WMAP observations of Planck ESZ clusters
Short Name:
J/ApJ/771/137
Date:
21 Oct 2021
Publisher:
CDS
Description:
We examine the Sunyaev-Zeldovich (SZ) effect in the seven year Wilkinson Microwave Anisotropy Probe (WMAP) data by cross-correlating it with the Planck Early-release Sunyaev-Zeldovich catalog (Cat. VIII/88/esz). Our analysis proceeds in two parts. We first perform a stacking analysis in which the filtered WMAP data are averaged at the locations of the 175 Planck clusters. We then perform a regression analysis to compare the mean amplitude of the SZ signal, Y_500_, in the WMAP data to the corresponding amplitude in the Planck data. The aggregate Planck clusters are detected in the seven year WMAP data with a signal-to-noise ratio of 16.3. In the regression analysis, we find that the SZ amplitude measurements agree to better than 25%: a=1.23+/-0.18 for the fit Y_500_^wmap^=aY_500_^planck^.
1164. WSRT Virgo HI filament survey
ID:
ivo://CDS.VizieR/J/A+A/527/A90
Title:
WSRT Virgo HI filament survey
Short Name:
J/A+A/527/A90
Date:
21 Oct 2021
Publisher:
CDS
Description:
Observations of neutral hydrogen can provide a wealth of information about the kinematics of galaxies. To learn more about the large-scale structures and accretion processes, the extended environment of galaxies have to be observed. Numerical simulations predict a cosmic web of extended structures and gaseous filaments. To observe the direct vicinity of galaxies, column densities have to be achieved that probe the regime of Lyman limit systems. Typically, HI observations are limited to a brightness sensitivity of N_HI_~10^19^cm^-2^, but this has to be improved by ~2 orders of magnitude. With the Westerbork Synthesis Radio Telescope (WSRT), we mapped the galaxy filament connecting the Virgo Cluster with the Local Group. About 1500 square degrees on the sky was surveyed with Nyquist sampled pointings. By using the WSRT antennas as single-dish telescopes instead of the more conventional interferometer, we were very sensitive to extended emission. The survey consists of a total of 22000 pointings, and each pointing was observed for two minutes with 14 antennas.
1165. WSRT Virgo HI filament survey. II.
ID:
ivo://CDS.VizieR/J/A+A/528/A28
Title:
WSRT Virgo HI filament survey. II.
Short Name:
J/A+A/528/A28
Date:
21 Oct 2021
Publisher:
CDS
Description:
The extended environment of galaxies contains a wealth of information about the formation and life cycle of galaxies which are regulated by accretion and feedback processes. Observations of neutral hydrogen are routinely used to image the high brightness disks of galaxies and to study their kinematics. Deeper observations will give more insight into the distribution of diffuse gas in the extended halo of the galaxies and the inter-galactic medium, where numerical simulations predict a cosmic web of extended structures and gaseous filaments. To observe the extended environment of galaxies, column density sensitivities have to be achieved that probe the regime of Lyman limit systems. HI observations are typically limited to a brightness sensitivity of NHI~10^19^cm^-2^, but this must be improved upon by ~2 orders of magnitude.
1166. WSRT ZoA Perseus-Pisces. HI catalogue
ID:
ivo://CDS.VizieR/J/MNRAS/460/923
Title:
WSRT ZoA Perseus-Pisces. HI catalogue
Short Name:
J/MNRAS/460/923
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present results of a blind 21cm HI-line imaging survey of a galaxy overdensity located behind the Milky Way at l, b ~= 160{deg}, 0.5{deg}. The overdensity corresponds to a zone-of-avoidance crossing of the Perseus-Pisces Supercluster filament. Although it is known that this filament contains an X-ray galaxy cluster (3C 129) hosting two strong radio galaxies, little is known about galaxies associated with this potentially rich cluster because of the high Galactic dust extinction. We mapped a sky area of ~9.6 deg^2^ using the Westerbork Synthesis Radio Telescope in a hexagonal mosaic of 35 pointings observed for 12h each, in the radial velocity range cz=2400-16600km/s. The survey has a sensitivity of 0.36mJy/beam rms at a velocity resolution of 16.5km/s. We detected 211 galaxies, 62 per cent of which have a near-infrared counterpart in the UKIDSS Galactic Plane Survey. We present a catalogue of the HI properties and an HI atlas containing total intensity maps, position-velocity diagrams, global HI profiles and UKIDSS counterpart images. For the resolved galaxies we also present HI velocity fields and radial HI surface density profiles. A brief analysis of the structures outlined by these galaxies finds that 87 of them lie at the distance of the Perseus-Pisces Supercluster (cz~4000-8000km/s) and seem to form part of the 3C 129 cluster. Further 72 detections trace an overdensity at a velocity of cz~=10000km/s and seem to coincide with a structure predicted from mass density reconstructions in the first 2MASS Redshift Survey.
1167. WWFI g'-band obs. of bright cluster galaxies
ID:
ivo://CDS.VizieR/J/ApJS/247/43
Title:
WWFI g'-band obs. of bright cluster galaxies
Short Name:
J/ApJS/247/43
Date:
21 Oct 2021
Publisher:
CDS
Description:
Observations of 170 local (z<~0.08) galaxy clusters in the northern hemisphere have been obtained with the Wendelstein Telescope Wide Field Imager (WWFI). We correct for systematic effects such as point-spread function broadening, foreground star contamination, relative bias offsets, and charge persistence. Background inhomogeneities induced by scattered light are reduced down to {Delta}SB>31 g' mag/arcsec^2^ by large dithering and subtraction of night-sky flats. Residual background inhomogeneities brighter than SB_{sigma}_<27.6 g' mag/arcsec^2^ caused by galactic cirrus are detected in front of 23% of the clusters. However, the large field of view allows discrimination between accretion signatures and galactic cirrus. We detect accretion signatures in the form of tidal streams in 22%, shells in 9.4%, and multiple nuclei in 47% of the brightest cluster galaxies (BCGs) and find two BCGs in 7% of the clusters. We measure semimajor-axis surface brightness profiles of the BCGs and their surrounding intracluster light (ICL) down to a limiting surface brightness of SB=30 g' mag/arcsec^2^. The spatial resolution in the inner regions is increased by combining the WWFI light profiles with those that we measured from archival Hubble Space Telescope images or deconvolved WWFI images. We find that 71% of the BCG+ICL systems have surface brightness (SB) profiles that are well described by a single Sersic function, whereas 29% require a double Sersic function to obtain a good fit. We find that BCGs have scaling relations that differ markedly from those of normal ellipticals, likely due to their indistinguishable embedding in the ICL.
1168. WWFI g'-band obs. of bright galaxy clusters
ID:
ivo://CDS.VizieR/J/ApJS/252/27
Title:
WWFI g'-band obs. of bright galaxy clusters
Short Name:
J/ApJS/252/27
Date:
21 Oct 2021
Publisher:
CDS
Description:
We explore several ways to dissect brightest cluster galaxies (BCGs) and their surrounding intracluster light (ICL) using a surface brightness (SB) cut, a luminosity cut, excess light above a de Vaucouleurs profile, or a double Sersic decomposition. Assuming that all light above M{<}-21.85g'mag is attributable to the ICL, we find that an average fraction of f_ICL_^MT^=71+/-22% of all diffuse light centered on the BCG belongs to the ICL. Likewise, if we assume that all light fainter than SB>27g'mag/arcsec^2^ belongs to the ICL, the average ICL fraction is f_ICL_^SB27^=34+/-19% . After fitting a de Vaucouleurs profile to the inner parts of the SB profile, we detect excess light at large radii, corresponding to an average ICL fraction of f_ICL_^DV^=48+/-20% . Finally, by decomposing the SB profile into two Sersic functions, we find an average ICL fraction of f_ICL_^Sx^=52+/-21% associated with the outer Sersic component. Our measured ICL and BCG+ICL luminosities agree well with predictions from high-resolution simulations where the outer Sersic component traces the unrelaxed, accreted stellar material. BCG and ICL properties defined in this way are correlated with cluster parameters to study the coevolution of BCGs, ICL, and their host clusters. We find positive correlations between BCG+ICL brightness and cluster mass, cluster velocity dispersion, cluster radius, and integrated satellite brightness, confirming that BCG/ICL growth is indeed coupled with cluster growth. On average, the ICL is better aligned than the BCG with the host cluster in terms of position angle, ellipticity, and centering. That makes it a potential dark-matter tracer.
1169. XBACs, the sample
ID:
ivo://CDS.VizieR/J/MNRAS/281/799
Title:
XBACs, the sample
Short Name:
J/MNRAS/281/799
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|>=20{deg}), the nominal redshift range of the ACO catalogue of z<=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.
1170. X-CLASS/GROND catalogue
ID:
ivo://CDS.VizieR/J/MNRAS/468/662
Title:
X-CLASS/GROND catalogue
Short Name:
J/MNRAS/468/662
Date:
21 Oct 2021
Publisher:
CDS
Description:
The XMM Cluster Archive Super Survey (X-CLASS) is a serendipitously detected X-ray-selected sample of 845 galaxy clusters based on 2774 XMM archival observations and covering an approximately 90deg^2^ spread across the high-Galactic latitude (|b|>20{deg}) sky. The primary goal of this survey is to produce a well-selected sample of galaxy clusters on which cosmological analyses can be performed. This paper presents the photometric redshift follow-up of a high signal-to-noise ratio subset of 265 of these clusters with declination {delta}<+20{deg} with Gamma-Ray Burst Optical and Near-Infrared Detector (GROND), a 7-channel (grizJHK) simultaneous imager on the MPG 2.2-m telescope at the ESO La Silla Observatory. We use a newly developed technique based on the red sequence colour-redshift relation, enhanced with information coming from the X-ray detection to provide photometric redshifts for this sample. We determine photometric redshifts for 232 clusters, finding a median redshift of z=0.39 with an accuracy of {Delta}z=0.02(1+z) when compared to a sample of 76 spectroscopically confirmed clusters. We also compute X-ray luminosities for the entire sample and find a median bolometric luminosity of 7.2x10^43^erg/s and a median temperature of 2.9 keV. We compare our results to those of the XMM-XCS and XMM-XXL surveys, finding good agreement in both samples. The X-CLASS catalogue is available online at http://xmm-lss.in2p3.fr:8080/l4sdb/.

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