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Journal articles on the topic 'Mass-Richness Relation'

Author: Grafiati
Published: 4 June 2021
Last updated: 12 February 2022

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1

Andreon, S., and J. Bergé. "Richness-mass relation self-calibration for galaxy clusters." Astronomy & Astrophysics 547 (November 2012): A117. http://dx.doi.org/10.1051/0004-6361/201220115.

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2

Ford, Jes, Hendrik Hildebrandt, Ludovic Van Waerbeke, Thomas Erben, Clotilde Laigle, Martha Milkeraitis, and Christopher B. Morrison. "Cluster magnification and the mass–richness relation in CFHTLenS." Monthly Notices of the Royal Astronomical Society 439, no. 4 (February 21, 2014): 3755–64. http://dx.doi.org/10.1093/mnras/stu225.

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3

Hearin, Andrew P., Andrew R. Zentner, Jeffrey A. Newman, and Andreas A. Berlind. "Mind the gap: tightening the mass–richness relation with magnitude gaps." Monthly Notices of the Royal Astronomical Society 430, no. 2 (January 30, 2013): 1238–46. http://dx.doi.org/10.1093/mnras/sts699.

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4

Andreon, S., and P. Congdon. "The insignificant evolution of the richness-mass relation of galaxy clusters." Astronomy & Astrophysics 568 (August 2014): A23. http://dx.doi.org/10.1051/0004-6361/201423616.

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5

Sereno, Mauro, Stefano Ettori, Giorgio F. Lesci, Federico Marulli, Matteo Maturi, Lauro Moscardini, Mario Radovich, Fabio Bellagamba, and Mauro Roncarelli. "CoMaLit – VI. Intrinsic scatter in stacked relations. The weak lensing AMICO galaxy clusters in KiDS-DR3." Monthly Notices of the Royal Astronomical Society 497, no. 1 (July 7, 2020): 894–905. http://dx.doi.org/10.1093/mnras/staa1902.

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ABSTRACT Unbiased and precise mass calibration of galaxy clusters is crucial to fully exploit galaxy clusters as cosmological probes. Stacking of weak lensing (WL) signal allows us to measure observable–mass relations down to less massive haloes without extrapolation. We propose a Bayesian inference method to constrain the intrinsic scatter of the mass proxy in stacked analyses. The scatter of the stacked data is rescaled with respect to the individual scatter based on the number of binned clusters. We apply this method to the galaxy clusters detected with the AMICO (Adaptive Matched Identifier of Clustered Objects) algorithm in the third data release of the Kilo-Degree Survey. The results confirm the optical richness as a low-scatter mass proxy. Based on the optical richness and the calibrated WL mass–richness relation, mass of individual objects down to $\sim\! 10^{13}\, \mathrm{M}_\odot$ can be estimated with a precision of ∼20 per cent.
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Grandis, S., J. J. Mohr, M. Costanzi, A. Saro, S. Bocquet, M. Klein, M. Aguena, et al. "Exploring the contamination of the DES-Y1 cluster sample with SPT-SZ selected clusters." Monthly Notices of the Royal Astronomical Society 504, no. 1 (March 25, 2021): 1253–72. http://dx.doi.org/10.1093/mnras/stab869.

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ABSTRACT We perform a cross validation of the cluster catalogue selected by the red-sequence Matched-filter Probabilistic Percolation algorithm (redMaPPer) in Dark Energy Survey year 1 (DES-Y1) data by matching it with the Sunyaev–Zel’dovich effect (SZE) selected cluster catalogue from the South Pole Telescope SPT-SZ survey. Of the 1005 redMaPPer selected clusters with measured richness $\hat{\lambda }\gt 40$ in the joint footprint, 207 are confirmed by SPT-SZ. Using the mass information from the SZE signal, we calibrate the richness–mass relation using a Bayesian cluster population model. We find a mass trend λ ∝ MB consistent with a linear relation (B ∼ 1), no significant redshift evolution and an intrinsic scatter in richness of σλ = 0.22 ± 0.06. By considering two error models, we explore the impact of projection effects on the richness–mass modelling, confirming that such effects are not detectable at the current level of systematic uncertainties. At low richness SPT-SZ confirms fewer redMaPPer clusters than expected. We interpret this richness dependent deficit in confirmed systems as due to the increased presence at low richness of low-mass objects not correctly accounted for by our richness-mass scatter model, which we call contaminants. At a richness $\hat{\lambda }=40$, this population makes up ${\gt}12{{\ \rm per\ cent}}$ (97.5 percentile) of the total population. Extrapolating this to a measured richness $\hat{\lambda }=20$ yields ${\gt}22{{\ \rm per\ cent}}$ (97.5 percentile). With these contamination fractions, the predicted redMaPPer number counts in different plausible cosmologies are compatible with the measured abundance. The presence of such a population is also a plausible explanation for the different mass trends (B ∼ 0.75) obtained from mass calibration using purely optically selected clusters. The mean mass from stacked weak lensing (WL) measurements suggests that these low-mass contaminants are galaxy groups with masses ∼3–5 × 1013 M⊙ which are beyond the sensitivity of current SZE and X-ray surveys but a natural target for SPT-3G and eROSITA.
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Capasso, R., J. J. Mohr, A. Saro, A. Biviano, N. Clerc, A. Finoguenov, S. Grandis, et al. "Mass calibration of the CODEX cluster sample using SPIDERS spectroscopy – I. The richness–mass relation." Monthly Notices of the Royal Astronomical Society 486, no. 2 (March 30, 2019): 1594–607. http://dx.doi.org/10.1093/mnras/stz931.

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Abstract We use galaxy dynamical information to calibrate the richness–mass scaling relation of a sample of 428 galaxy clusters that are members of the CODEX sample with redshifts up to z ∼ 0.7. These clusters were X-ray selected using the ROSAT All-Sky Survey (RASS) and then cross-matched to associated systems in the redMaPPer (the red sequence Matched-filter Probabilistic Percolation) catalogue from the Sloan Digital Sky Survey. The spectroscopic sample we analyse was obtained in the SPIDERS program and contains ∼7800 red member galaxies. Adopting NFW mass and galaxy density profiles and a broad range of orbital anisotropy profiles, we use the Jeans equation to calculate halo masses. Modelling the scaling relation as $\lambda \propto \text{A}_{\lambda } {M_{\text{200c}}}^{\text{B}_{\lambda }} ({1+z})^{\gamma _{\lambda }}$, we find the parameter constraints $\text{A}_{\lambda }=38.6^{+3.1}_{-4.1}\pm 3.9$, $\text{B}_{\lambda }=0.99^{+0.06}_{-0.07}\pm 0.04$, and $\gamma _{\lambda }=-1.13^{+0.32}_{-0.34}\pm 0.49$, where we present systematic uncertainties as a second component. We find good agreement with previously published mass trends with the exception of those from stacked weak lensing analyses. We note that although the lensing analyses failed to account for the Eddington bias, this is not enough to explain the differences. We suggest that differences in the levels of contamination between pure redMaPPer and RASS + redMaPPer samples could well contribute to these differences. The redshift trend we measure is more negative than but statistically consistent with previous results. We suggest that our measured redshift trend reflects a change in the cluster galaxy red sequence (RS) fraction with redshift, noting that the trend we measure is consistent with but somewhat stronger than an independently measured redshift trend in the RS fraction. We also examine the impact of a plausible model of correlated scatter in X-ray luminosity and optical richness, showing it has negligible impact on our results.
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8

Simet, Melanie, Tom McClintock, Rachel Mandelbaum, Eduardo Rozo, Eli Rykoff, Erin Sheldon, and Risa H. Wechsler. "Weak lensing measurement of the mass–richness relation of SDSS redMaPPer clusters." Monthly Notices of the Royal Astronomical Society 466, no. 3 (December 15, 2016): 3103–18. http://dx.doi.org/10.1093/mnras/stw3250.

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9

Rozo, Eduardo, Eli Rykoff, Benjamin Koester, Brian Nord, Hao-Yi Wu, August Evrard, and Risa Wechsler. "EXTRINSIC SOURCES OF SCATTER IN THE RICHNESS-MASS RELATION OF GALAXY CLUSTERS." Astrophysical Journal 740, no. 2 (September 27, 2011): 53. http://dx.doi.org/10.1088/0004-637x/740/2/53.

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10

Phriksee, Anirut, Eric Jullo, Marceau Limousin, HuanYuan Shan, Alexis Finoguenov, Siramas Komonjinda, Suwicha Wannawichian, and Utane Sawangwit. "Weak lensing analysis of codex clusters using dark energy camera legacy survey: mass–richness relation." Monthly Notices of the Royal Astronomical Society 491, no. 2 (November 4, 2019): 1643–55. http://dx.doi.org/10.1093/mnras/stz3049.

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ABSTRACT We present the weak-lensing analysis of 279 CODEX clusters using imaging data from 4200 deg2 of the DECam Legacy Survey (DECaLS) Data Release 3. The cluster sample results from a joint selection in X-ray, optical richness in the range 20 ≤ λ < 110, and redshift in the range 0.1 ≤ z ≤ 0.2. We model the cluster mass (M200c) and the richness relation with the expression $\left\langle M_{\rm 200c} | \lambda \right\rangle \propto M_{0} \, (\lambda / 40)^{F_{\lambda }}$. By measuring the CODEX cluster sample as an individual cluster, we obtain the best-fitting values, $M_{0} = 3.24^{+0.29}_{-0.27} \times 10^{14} \text{M}_{\odot }$, and $F_{\lambda } = 1.00 ^{+0.22}_{-0.22}$ for the richness scaling index, consistent with a power-law relation. Moreover, we separate the cluster sample into three richness groups; λ = 20–30, 30–50, and 50–110, and measure the stacked excess surface mass density profile in each group. The results show that both methods are consistent. In addition, we find an excellent agreement between our weak lensing based scaling relation and the relation obtained with dynamical masses estimated from cluster member velocity dispersions measured by the SDSS-IV/SPIDERS team. This suggests that the cluster dynamical equilibrium assumption involved in the dynamical mass estimates is statistically robust for a large sample of clusters.
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11

Wang, Jing. "The H i size-mass relation of galaxies." Proceedings of the International Astronomical Union 11, S321 (March 2016): 284. http://dx.doi.org/10.1017/s174392131600911x.

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AbstractWe revisit the well known H i size-mass relation of galaxies with an unprecedented large sample of over 500 galaxies (Wang et al. 2016). We find that the relation and the scatter about the relation do not depend on the galaxy type, optical luminosity or H i richness. It indicates a fundamental unrecognised mechanism that drives the distribution of H i in different galaxies.
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12

Capasso, R., J. J. Mohr, A. Saro, A. Biviano, N. Clerc, A. Finoguenov, S. Grandis, et al. "Erratum: Mass calibration of the CODEX cluster sample using SPIDERS spectroscopy – I. The richness–mass relation." Monthly Notices of the Royal Astronomical Society 488, no. 1 (July 5, 2019): 481. http://dx.doi.org/10.1093/mnras/stz1826.

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13

Gonzalez, Elizabeth Johana, Facundo Rodriguez, Diego García Lambas, Manuel Merchán, Gael Foëx, and Martín Chalela. "Weak-lensing measurement of the mass–richness relation using the SDSS data base." Monthly Notices of the Royal Astronomical Society 465, no. 2 (November 2, 2016): 1348–57. http://dx.doi.org/10.1093/mnras/stw2803.

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14

Simet, Melanie, Tom McClintock, Rachel Mandelbaum, Eduardo Rozo, Eli Rykoff, Erin Sheldon, and Risa H. Wechsler. "Erratum: Weak Lensing Measurement of the Mass–Richness Relation of SDSS redMaPPer Clusters." Monthly Notices of the Royal Astronomical Society 480, no. 4 (August 31, 2018): 5385. http://dx.doi.org/10.1093/mnras/sty2318.

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15

Bauer, Anne H., Charles Baltay, Nancy Ellman, Jonathan Jerke, David Rabinowitz, and Richard Scalzo. "THE MASS-RICHNESS RELATION OF MaxBCG CLUSTERS FROM QUASAR LENSING MAGNIFICATION USING VARIABILITY." Astrophysical Journal 749, no. 1 (March 22, 2012): 56. http://dx.doi.org/10.1088/0004-637x/749/1/56.

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16

Ider Chitham, J., J. Comparat, A. Finoguenov, N. Clerc, C. Kirkpatrick, S. Damsted, A. Kukkola, et al. "Cosmological constraints from CODEX galaxy clusters spectroscopically confirmed by SDSS-IV/SPIDERS DR16." Monthly Notices of the Royal Astronomical Society 499, no. 4 (October 14, 2020): 4768–84. http://dx.doi.org/10.1093/mnras/staa3044.

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ABSTRACT This paper presents a cosmological analysis based on the properties of X-ray selected clusters of galaxies from the CODEX survey which have been spectroscopically followed up within the SPIDERS programme as part of the sixteenth data release (DR16) of SDSS-IV. The cosmological sub-sample contains a total of 691 clusters over an area of 5350 deg2 with newly measured optical properties provided by a reanalysis of the CODEX source catalogue using redMaPPer and the DESI Legacy Imaging Surveys (DR8). Optical richness is used as a proxy for the cluster mass, and the combination of X-ray, optical, and spectroscopic information ensures that only confirmed virialized systems are considered. Clusters are binned in observed redshift, $\tilde{z} \in \left[0.1, 0.6 \right)$ and optical richness, $\tilde{\lambda } \in \left[25, 148 \right)$ and the number of clusters in each bin is modelled as a function of cosmological and richness–mass scaling relation parameters. A high-purity sub-sample of 691 clusters is used in the analysis and best-fitting cosmological parameters are found to be $\Omega _{m_{0}}=0.34^{+0.09}_{-0.05}$ and $\sigma _8=0.73^{+0.03}_{-0.03}$. The redshift evolution of the self-calibrated richness–mass relation is poorly constrained due to the systematic uncertainties associated with the X-ray component of the selection function (which assumes a fixed X-ray luminosity–mass relation with h = 0.7 and $\Omega _{m_{0}}=0.30$). Repeating the analysis with the assumption of no redshift evolution is found to improve the consistency between both cosmological and scaling relation parameters with respect to recent galaxy cluster analyses in the literature.
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17

Chiu, I.-Non, Keiichi Umetsu, Ryoma Murata, Elinor Medezinski, and Masamune Oguri. "The richness-to-mass relation of CAMIRA galaxy clusters from weak-lensing magnification in the Subaru Hyper Suprime-Cam survey." Monthly Notices of the Royal Astronomical Society 495, no. 1 (April 28, 2020): 428–50. http://dx.doi.org/10.1093/mnras/staa1158.

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ABSTRACT We present a statistical weak-lensing magnification analysis on an optically selected sample of 3029 CAMIRA (Cluster finding Algorithm based on Multiband Identification of Red-sequence gAlaxies) galaxy clusters with richness N &gt; 15 at redshift 0.2 ≤ z &lt; 1.1 in the Subaru Hyper Suprime-Cam survey. We use two distinct populations of colour-selected, flux-limited background galaxies, namely the low-z and high-z samples at mean redshifts of ≈1.1 and ≈1.4, respectively, from which to measure the weak-lensing magnification signal by accounting for cluster contamination as well as masking effects. Our magnification bias measurements are found to be uncontaminated according to validation tests against the ‘null-test’ samples for which the net magnification bias is expected to vanish. The magnification bias for the full CAMIRA sample is detected at a significance level of 9.51σ, which is dominated by the high-z background. We forward-model the observed magnification data to constrain the normalization of the richness-to-mass (N–M) relation for the CAMIRA sample with informative priors on other parameters. The resulting scaling relation is N∝ (M500)0.92 ± 0.13(1 + z)−0.48 ± 0.69, with a characteristic richness of N = 17.72 ± 2.60 and intrinsic lognormal scatter of 0.15 ± 0.07 at M500 = 1014 h−1 M⊙. With the derived N–M relation, we provide magnification-calibrated mass estimates of individual CAMIRA clusters, with the typical uncertainty of ≈39 and ≈32 per cent at richness of ≈20 and ≈40, respectively. We further compare our magnification-inferred N–M relation with those from the shear-based results in the literature, finding good agreement.
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18

Sayad, E., S. M. Hosseini, V. Hosseini, and M. H. Salehe-Shooshtari. "Soil macrofauna in relation to soil and leaf litter properties in tree plantations." Journal of Forest Science 58, No. 4 (April 27, 2012): 170–80. http://dx.doi.org/10.17221/58/2011-jfs.

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Soil communities exert strong influences on the processing of organic matter and nutrients. Plantations of trees, especially of nitrogen fixing ones, may affect the soil macrofauna through litter quality and quantity. This study was conducted in a randomized block design with three blocks consisting of Populus euphratica, Eucalyptus camaldulensis, Eucalyptus microtheca, Acacia farnesiana, Acacia salicina, Acacia saligna, Acacia stenophylla and Dalbergia sissoo monoculture plantations that were established in 1992. Soils and soil macrofauna were sampled in November 2006. Leaf litterfall was collected from November 2006 to November 2007 at bi-weekly intervals. Macroinvertebrate abundance and biomass were consistently higher in A. salicina plantations than in the others, whereas they were lowest in E. camaldulensis. Tree species and nitrogen fixing trees significantly influenced the soil macrofauna richness. The results suggest that the earthworm distribution is regulated by leaf litter quality (Ca, C and N) whereas the macrofauna richness is regulated by leaf litter mass, soil organic carbon and leaf litter Mg. Totally, it was revealed that the tree species clearly affected macrofauna whereas nitrogen fixation did not. &nbsp;
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19

Costanzi, M., E. Rozo, M. Simet, Y. Zhang, A. E. Evrard, A. Mantz, E. S. Rykoff, et al. "Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release." Monthly Notices of the Royal Astronomical Society 488, no. 4 (July 17, 2019): 4779–800. http://dx.doi.org/10.1093/mnras/stz1949.

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ABSTRACT We implement the first blind analysis of cluster abundance data to derive cosmological constraints from the abundance and weak lensing signal of redMaPPer clusters in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness–mass relation of the clusters. For a flat Λ cold dark matter cosmological model with massive neutrinos, we find $S_8 \equiv \sigma _{8}(\Omega _\mathrm{ m}/0.3)^{0.5}=0.79^{+0.05}_{-0.04}$. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES), the Kilo-Degree Survey (KiDS), and with the cosmic microwave background (CMB) anisotropies as measured by Planck. We demonstrate that the cosmological posteriors are robust against variation of the richness–mass relation model and to systematics associated with the calibration of the selection function. In combination with baryon acoustic oscillation data and big bang nucleosynthesis data (Cooke et al.), we constrain the Hubble rate to be h = 0.66 ± 0.02, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness–mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.
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20

Erfanianfar, G., A. Finoguenov, K. Furnell, P. Popesso, A. Biviano, S. Wuyts, C. A. Collins, et al. "Stellar mass–halo mass relation for the brightest central galaxies of X-ray clusters since z ∼ 0.65." Astronomy & Astrophysics 631 (November 2019): A175. http://dx.doi.org/10.1051/0004-6361/201935375.

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We present the brightest cluster galaxies (BCGs) catalog for SPectroscoic IDentification of eROSITA Sources (SPIDERS) DR14 cluster program value-added catalog. We list the 416 BCGs identified as part of this process, along with their stellar mass, star formation rates (SFRs), and morphological properties. We identified the BCGs based on the available spectroscopic data from SPIDERS and photometric data from SDSS. We computed stellar masses and SFRs of the BCGs on the basis of SDSS, WISE, and GALEX photometry using spectral energy distribution fitting. Morphological properties for all BCGs were derived by Sersic profile fitting using the software package SIGMA in different optical bands (g,r,i). We combined this catalog with the BCGs of galaxy groups and clusters extracted from the deeper AEGIS, CDFS, COSMOS, XMM-CFHTLS, and XMM-XXL surveys to study the stellar mass–halo mass relation using the largest sample of X-ray groups and clusters known to date. This result suggests that the mass growth of the central galaxy is controlled by the hierarchical mass growth of the host halo. We find a strong correlation between the stellar mass of BCGs and the mass of their host halos. This relation shows no evolution since z ∼ 0.65. We measure a mean scatter of 0.21 and 0.25 for the stellar mass of BCGs in a given halo mass at low (0.1 < z < 0.3) and high (0.3 < z < 0.65) redshifts, respectively. We further demonstrate that the BCG mass is covariant with the richness of the host halos in the very X-ray luminous systems. We also find evidence that part of the scatter between X-ray luminosity and richness can be reduced by considering stellar mass as an additional variable.
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21

Farahi, A., X. Chen, A. E. Evrard, D. L. Hollowood, R. Wilkinson, S. Bhargava, P. Giles, et al. "Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters." Monthly Notices of the Royal Astronomical Society 490, no. 3 (September 26, 2019): 3341–54. http://dx.doi.org/10.1093/mnras/stz2689.

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ABSTRACT Using archival X-ray observations and a lognormal population model, we estimate constraints on the intrinsic scatter in halo mass at fixed optical richness for a galaxy cluster sample identified in Dark Energy Survey Year-One (DES-Y1) data with the redMaPPer algorithm. We examine the scaling behaviour of X-ray temperatures, TX, with optical richness, λRM, for clusters in the redshift range 0.2 &lt; z &lt; 0.7. X-ray temperatures are obtained from Chandra and XMM observations for 58 and 110 redMaPPer systems, respectively. Despite non-uniform sky coverage, the TX measurements are $\gt 50{{\ \rm per\ cent}}$ complete for clusters with λRM &gt; 130. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, $\sigma _{\ln T \, |\, \lambda }= 0.275 \pm 0.019$. Joined with constraints for TX scaling with halo mass from the Weighing the Giants program and richness–temperature covariance estimates from the LoCuSS sample, we derive the richness-conditioned scatter in mass, $\sigma _{\ln M \, |\, \lambda }= 0.30 \pm 0.04\, _{({\rm stat})} \pm 0.09\, _{({\rm sys})}$, at an optical richness of approximately 100. Uncertainties in external parameters, particularly the slope and variance of the TX–mass relation and the covariance of TX and λRM at fixed mass, dominate the systematic error. The $95{{\ \rm per\ cent}}$ confidence region from joint sample analysis is relatively broad, $\sigma _{\ln M \, |\, \lambda }\in [0.14, \, 0.55]$, or a factor 10 in variance.
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22

Murata, Ryoma, Takahiro Nishimichi, Masahiro Takada, Hironao Miyatake, Masato Shirasaki, Surhud More, Ryuichi Takahashi, and Ken Osato. "Constraints on the Mass–Richness Relation from the Abundance and Weak Lensing of SDSS Clusters." Astrophysical Journal 854, no. 2 (February 20, 2018): 120. http://dx.doi.org/10.3847/1538-4357/aaaab8.

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23

Tudorica, A., H. Hildebrandt, M. Tewes, H. Hoekstra, C. B. Morrison, A. Muzzin, G. Wilson, et al. "Weak lensing magnification of SpARCS galaxy clusters." Astronomy & Astrophysics 608 (December 2017): A141. http://dx.doi.org/10.1051/0004-6361/201731267.

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Context. Measuring and calibrating relations between cluster observables is critical for resource-limited studies. The mass–richness relation of clusters offers an observationally inexpensive way of estimating masses. Its calibration is essential for cluster and cosmological studies, especially for high-redshift clusters. Weak gravitational lensing magnification is a promising and complementary method to shear studies, that can be applied at higher redshifts. Aims. We aim to employ the weak lensing magnification method to calibrate the mass–richness relation up to a redshift of 1.4. We used the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS) galaxy cluster candidates (0.2 < z < 1.4) and optical data from the Canada France Hawaii Telescope (CFHT) to test whether magnification can be effectively used to constrain the mass of high-redshift clusters. Methods. Lyman-break galaxies (LBGs) selected using the u-band dropout technique and their colours were used as a background sample of sources. LBG positions were cross-correlated with the centres of the sample of SpARCS clusters to estimate the magnification signal, which was optimally-weighted using an externally-calibrated LBG luminosity function. The signal was measured for cluster sub-samples, binned in both redshift and richness. Results. We measured the cross-correlation between the positions of galaxy cluster candidates and LBGs and detected a weak lensing magnification signal for all bins at a detection significance of 2.6–5.5σ. In particular, the significance of the measurement for clusters with z> 1.0 is 4.1σ; for the entire cluster sample we obtained an average M200 of 1.28 -0.21+0.23 × 1014 M⊙. Conclusions. Our measurements demonstrated the feasibility of using weak lensing magnification as a viable tool for determining the average halo masses for samples of high redshift galaxy clusters. The results also established the success of using galaxy over-densities to select massive clusters at z > 1. Additional studies are necessary for further modelling of the various systematic effects we discussed.
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Gilbank, David G., L. Felipe Barrientos, Erica Ellingson, Kris Blindert, H. K. C. Yee, T. Anguita, M. D. Gladders, et al. "Spectroscopic characterization of galaxy clusters in RCS-1: spectroscopic confirmation, redshift accuracy, and dynamical mass–richness relation." Monthly Notices of the Royal Astronomical Society 476, no. 2 (February 9, 2018): 1991–2012. http://dx.doi.org/10.1093/mnras/sty355.

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25

Saro, A., S. Bocquet, E. Rozo, B. A. Benson, J. Mohr, E. S. Rykoff, M. Soares-Santos, et al. "Constraints on the richness–mass relation and the optical-SZE positional offset distribution for SZE-selected clusters." Monthly Notices of the Royal Astronomical Society 454, no. 3 (October 12, 2015): 2305–19. http://dx.doi.org/10.1093/mnras/stv2141.

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26

Rozo, Eduardo, Eli S. Rykoff, August Evrard, Matthew Becker, Timothy McKay, Risa H. Wechsler, Benjamin P. Koester, et al. "CONSTRAINING THE SCATTER IN THE MASS-RICHNESS RELATION OF maxBCG CLUSTERS WITH WEAK LENSING AND X-RAY DATA." Astrophysical Journal 699, no. 1 (June 16, 2009): 768–81. http://dx.doi.org/10.1088/0004-637x/699/1/768.

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27

Myles, J., D. Gruen, A. B. Mantz, S. W. Allen, R. G. Morris, E. Rykoff, M. Costanzi, et al. "Spectroscopic quantification of projection effects in the SDSS redMaPPer galaxy cluster catalogue." Monthly Notices of the Royal Astronomical Society 505, no. 1 (May 3, 2021): 33–44. http://dx.doi.org/10.1093/mnras/stab1243.

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ABSTRACT Projection effects, whereby galaxies along the line of sight to a galaxy cluster are mistakenly associated with the cluster halo, present a significant challenge for optical cluster cosmology. We use statistically representative spectral coverage of luminous galaxies to investigate how projection effects impact the low-redshift limit of the Sloan Digital Sky Survey (SDSS) redMaPPer galaxy cluster catalogue. Spectroscopic redshifts enable us to differentiate true cluster members from false positives and determine the fraction of candidate cluster members viewed in projection. Our main results can be summarized as follows: first, we show that a simple double-Gaussian model can be used to describe the distribution of line-of-sight velocities in the redMaPPer sample; secondly, the incidence of projection effects is substantial, accounting for ∼16 per cent of the weighted richness for the lowest richness objects; thirdly, projection effects are a strong function of richness, with the contribution in the highest richness bin being several times smaller than for low-richness objects; fourthly, our measurement has a similar amplitude to state-of-the-art models, but finds a steeper dependence of projection effects on richness than these models; and fifthly, the slope of the observed velocity dispersion–richness relation, corrected for projection effects, implies an approximately linear relationship between the true, three-dimensional halo mass and three-dimensional richness. Our results provide a robust, empirical description of the impact of projection effects on the SDSS redMaPPer cluster sample and exemplify the synergies between optical imaging and spectroscopic data for studies of galaxy cluster astrophysics and cosmology.
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Radovich, Mario, Crescenzo Tortora, Fabio Bellagamba, Matteo Maturi, Lauro Moscardini, Emanuella Puddu, Mauro Roncarelli, et al. "AMICO galaxy clusters in KiDS-DR3: galaxy population properties and their redshift dependence." Monthly Notices of the Royal Astronomical Society 498, no. 3 (September 7, 2020): 4303–15. http://dx.doi.org/10.1093/mnras/staa2705.

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ABSTRACT A catalogue of galaxy clusters was obtained in an area of 414 $\deg ^2$ up to a redshift z ∼ 0.8 from the Data Release 3 of the Kilo-Degree Survey (KiDS-DR3), using the Adaptive Matched Identifier of Clustered Objects (amico) algorithm. The catalogue and the calibration of the richness–mass relation were presented in two companion papers. Here, we describe the selection of the cluster central galaxy and the classification of blue and red cluster members, and analyse the main cluster properties, such as the red/blue fraction, cluster mass, brightness, and stellar mass of the central galaxy, and their dependence on redshift and cluster richness. We use the Illustris-TNG simulation, which represents the state-of-the-art cosmological simulation of galaxy formation, as a benchmark for the interpretation of the results. A good agreement with simulations is found at low redshifts (z ≤ 0.4), while at higher redshifts the simulations indicate a lower fraction of blue galaxies than what found in the KiDS-amico catalogue: we argue that this may be due to an underestimate of star-forming galaxies in the simulations. The selection of clusters with a larger magnitude difference between the two brightest central galaxies, which may indicate a more relaxed cluster dynamical status, improves the agreement between the observed and simulated cluster mass and stellar mass of the central galaxy. We also find that at a given cluster mass the stellar mass of blue central galaxies is lower than that of the red ones.
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Chiu, I.-Non, Teppei Okumura, Masamune Oguri, Aniket Agrawal, Keiichi Umetsu, and Yen-Ting Lin. "A clustering-based self-calibration of the richness-to-mass relation of CAMIRA galaxy clusters out to z ≈ 1.1 in the Hyper Suprime-Cam survey." Monthly Notices of the Royal Astronomical Society 498, no. 2 (August 17, 2020): 2030–53. http://dx.doi.org/10.1093/mnras/staa2440.

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ABSTRACT We perform a self-calibration of the richness-to-mass (N–M) relation of CAMIRA galaxy clusters with richness N ≥ 15 at redshift 0.2 ≤ z &lt; 1.1 by modelling redshift-space two-point correlation functions. These correlation functions are the autocorrelation function ξcc of CAMIRA clusters, the autocorrelation function ξgg of the CMASS galaxies spectroscopically observed in the Baryon Oscillation Spectroscopic Survey, and the cross-correlation function ξcg between these two samples. We focus on constraining the normalization AN of the N–M relation with a forward-modelling approach, carefully accounting for the redshift-space distortion, the Finger-of-God effect, and the uncertainty in photometric redshifts of CAMIRA clusters. The modelling also takes into account the projection effect on the halo bias of CAMIRA clusters. The parameter constraints are shown to be unbiased according to validation tests using a large set of mock catalogues constructed from N-body simulations. At the pivotal mass $M_{500}=10^{14}\, h^{-1}\, \mathrm{M}_{\odot }$ and the pivotal redshift zpiv = 0.6, the resulting normalization AN is constrained as $13.8^{+5.8}_{-4.2}$, $13.2^{+3.4}_{-2.7}$, and $11.9^{+3.0}_{-1.9}$ by modelling ξcc, ξcc + ξcg, and ξcc + ξcg + ξgg, with average uncertainties at levels of 36, 23, and $21{{\ \rm per\ cent}}$, respectively. We find that the resulting AN is statistically consistent with those independently obtained from weak-lensing magnification and from a joint analysis of shear and cluster abundance, with a preference for a lower value at a level of ≲ 1.9σ. This implies that the absolute mass scale of CAMIRA clusters inferred from clustering is mildly higher than those from the independent methods. We discuss the impact of the selection bias introduced by the cluster finding algorithm, which is suggested to be a subdominant factor in this work.
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Gannon, Jonah S., Duncan A. Forbes, Aaron J. Romanowsky, Anna Ferré-Mateu, Warrick J. Couch, and Jean P. Brodie. "On the stellar kinematics and mass of the Virgo ultradiffuse galaxy VCC 1287." Monthly Notices of the Royal Astronomical Society 495, no. 3 (May 8, 2020): 2582–98. http://dx.doi.org/10.1093/mnras/staa1282.

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ABSTRACT Here, we present a kinematical analysis of the Virgo cluster ultradiffuse galaxy (UDG) VCC 1287 based on data taken with the Keck Cosmic Web Imager (KCWI). We confirm VCC 1287’s association both with the Virgo cluster and its globular cluster (GC) system, measuring a recessional velocity of 1116 ± 2 km s−1. We measure a stellar velocity dispersion (19 ± 6 km s−1) and infer both a dynamical mass ($1.11^{+0.81}_{-0.81} \times 10^{9} \ \mathrm{M_{\odot }}$) and mass-to-light ratio (M/L) ($13^{+11}_{-11}$) within the half-light radius (4.4 kpc). This places VCC 1287 slightly above the well-established relation for normal galaxies, with a higher M/L for its dynamical mass than normal galaxies. We use our dynamical mass, and an estimate of GC system richness, to place VCC 1287 on the GC number–dynamical mass relation, finding good agreement with a sample of normal galaxies. Based on a total halo mass derived from GC counts, we then infer that VCC 1287 likely resides in a cored or low-concentration dark matter halo. Based on the comparison of our measurements to predictions from simulations, we find that strong stellar feedback and/or tidal effects are plausibly the dominant mechanisms in the formation of VCC 1287. Finally, we compare our measurement of the dynamical mass with those for other UDGs. These dynamical mass estimates suggest relatively massive haloes and a failed galaxy origin for at least some UDGs.
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Campa, Julia, Juan Estrada, and Brenna Flaugher. "Measuring the Scatter of the Mass–Richness Relation in Galaxy Clusters in Photometric Imaging Surveys by Means of Their Correlation Function." Astrophysical Journal 836, no. 1 (February 3, 2017): 9. http://dx.doi.org/10.3847/1538-4357/836/1/9.

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Scervino, Renata Picolo, and Lya Carolina da Silva Mariano Pereira. "Natural regeneration, composition and structure in a secondary Atlantic Forest fragment and in an abandoned Eucalyptus saligna Smith. (Myrtaceae) commercial plantation / Regeneração natural, composição e estrutura em um fragmento em sucessão secundária de Mata Atlântica e em reflorestamento comercial de Eucalyptus saligna Smith. (Myrtaceae) abandonado à regeneração." Brazilian Journal of Animal and Environmental Research 4, no. 2 (June 16, 2021): 2571–85. http://dx.doi.org/10.34188/bjaerv4n2-082.

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The litter horizon on forests ecosystems acts on the nutrient cycling and on the soil’s microclimate conditions. However, to reforestation ecosystems the litter attributes can conduct to alterations that can diminish the seedling establishment, as well can act on the herbivory rates. In this context, this study aimed to verify the differences and relationships between woody species diversity, the herbivory index, the litter attributes, and the canopy openness among a fragment of Atlantic Forest on secondary succession and commercial plantation of Eucalyptus saligna Smith abandoned to regeneration. This study was conducted at the Klabin’s Company “Ecological Reserve”, at Telêmaco Borba – PR, Brazil. There weren’t observed differences on the species richness and abundance among the studied sites. Litter mass and thickness were higher in E. saligna environment. However, the litter attributes only presented relationship with the woody vegetation at the Atlantic Forest site, such as abundance and species richness with litter mass (r2=0.53 and r2=0.40, respectively) and abundance with litter thickness (r2=0.63). The herbivory index was greater on the forest patch. The canopy openness was superior in the E. saligna site. At this site, the herbivory index presented a positive relation with the canopy openness (r2=0.48) and a negative with abundance (r2=0.48). Abundance also presented a negative relation with the canopy openness (r2=0.58) in the E. saligna environment. The litter horizon on the E. saligna plantation doesn’t seem to offer restrictions to regeneration of the woody vegetation. However, at this site, the higher canopy openness and the herbivory pressure over the woody vegetation may lead to a lower rate of secondary succession compared to the Atlantic Forest fragment.
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Grandis, S., M. Klein, J. J. Mohr, S. Bocquet, M. Paulus, T. M. C. Abbott, M. Aguena, et al. "Validation of selection function, sample contamination and mass calibration in galaxy cluster samples." Monthly Notices of the Royal Astronomical Society 498, no. 1 (August 11, 2020): 771–98. http://dx.doi.org/10.1093/mnras/staa2333.

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ABSTRACT We construct and validate the selection function of the MARD-Y3 galaxy cluster sample. This sample was selected through optical follow-up of the 2nd ROSAT faint source catalogue with Dark Energy Survey year 3 data. The selection function is modelled by combining an empirically constructed X-ray selection function with an incompleteness model for the optical follow-up. We validate the joint selection function by testing the consistency of the constraints on the X-ray flux–mass and richness–mass scaling relation parameters derived from different sources of mass information: (1) cross-calibration using South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) clusters, (2) calibration using number counts in X-ray, in optical and in both X-ray and optical while marginalizing over cosmological parameters, and (3) other published analyses. We find that the constraints on the scaling relation from the number counts and SPT-SZ cross-calibration agree, indicating that our modelling of the selection function is adequate. Furthermore, we apply a largely cosmology independent method to validate selection functions via the computation of the probability of finding each cluster in the SPT-SZ sample in the MARD-Y3 sample and vice versa. This test reveals no clear evidence for MARD-Y3 contamination, SPT-SZ incompleteness or outlier fraction. Finally, we discuss the prospects of the techniques presented here to limit systematic selection effects in future cluster cosmological studies.
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van der Burg, Remco F. J., Henk Hoekstra, Adam Muzzin, Cristóbal Sifón, Massimo Viola, Malcolm N. Bremer, Sarah Brough, et al. "The abundance of ultra-diffuse galaxies from groups to clusters." Astronomy & Astrophysics 607 (November 2017): A79. http://dx.doi.org/10.1051/0004-6361/201731335.

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In recent years, many studies have reported substantial populations of large galaxies with low surface brightness in local galaxy clusters. Various theories that aim to explain the presence of such ultra-diffuse galaxies (UDGs) have since been proposed. A key question that will help to distinguish between models is whether UDGs have counterparts in host haloes with lower masses, and if so, what their abundance as a function of halo mass is. We here extend our previous study of UDGs in galaxy clusters to galaxy groups. We measure the abundance of UDGs in 325 spectroscopically selected groups from the Galaxy And Mass Assembly (GAMA) survey. We make use of the overlapping imaging from the ESO Kilo-Degree Survey (KiDS), from which we can identify galaxies with mean surface brightnesses within their effective radii down to ~25.5 mag arcsec-2 in the r band. We are able to measure a significant overdensity of UDGs (with sizes reff ≥ 1.5 kpc) in galaxy groups down to M200 = 1012 M⊙, a regime where approximately only one in ten groups contains a UDG that we can detect. We combine measurements of the abundance of UDGs in haloes that cover three orders of magnitude in halo mass, finding that their numbers scale quite steeply with halo mass: NUDG(R < R200) ∝ M2001.11±0.07. To better interpret this, we also measure the mass-richness relation for brighter galaxies down to Mr* + 2.5 in the same GAMA groups, and find a much shallower relation of NBright(R < R200) ∝ M2000.78±0.05. This shows that compared to bright galaxies, UDGs are relatively more abundant in massive clusters than in groups. We discuss the implications, but it is still unclear whether this difference is related to a higher destruction rate of UDGs in groups or if massive haloes have a positive effect on UDG formation.
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Pereira, M. E. S., A. Palmese, T. N. Varga, T. McClintock, M. Soares-Santos, J. Burgad, J. Annis, et al. "μ⋆ masses: weak-lensing calibration of the Dark Energy Survey Year 1 redMaPPer clusters using stellar masses." Monthly Notices of the Royal Astronomical Society 498, no. 4 (September 7, 2020): 5450–67. http://dx.doi.org/10.1093/mnras/staa2687.

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ABSTRACT We present the weak-lensing mass calibration of the stellar-mass-based μ⋆ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time, we are able to perform a calibration of μ⋆ at high redshifts, z &gt; 0.33. In a blinded analysis, we use ∼6000 clusters split into 12 subsets spanning the ranges 0.1 ≤ z &lt; 0.65 and μ⋆ up to ${\sim} 5.5 \times 10^{13} \, \mathrm{M}_{\odot }$, and infer the average masses of these subsets through modelling of their stacked weak-lensing signal. In our model, we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, cluster-member contamination of the source sample, deviations from the Navarro–Frenk–White halo profile, halo triaxiality, and projection effects. We use the inferred masses to estimate the joint mass–μ⋆–z scaling relation given by $\langle M_{200c} | \mu _{\star },z \rangle = M_0 (\mu _{\star }/5.16\times 10^{12} \, \mathrm{M_{\odot }})^{F_{\mu _{\star }}} ((1+z)/1.35)^{G_z}$. We find $M_0= (1.14 \pm 0.07) \times 10^{14} \, \mathrm{M_{\odot }}$ with $F_{\mu _{\star }}= 0.76 \pm 0.06$ and Gz = −1.14 ± 0.37. We discuss the use of μ⋆ as a complementary mass proxy to the well-studied richness λ for: (i) exploring the regimes of low z, λ &lt; 20 and high λ, z ∼ 1; and (ii) testing systematics such as projection effects for applications in cluster cosmology.
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Forbes, Duncan A., Adebusola Alabi, Aaron J. Romanowsky, Jean P. Brodie, and Nobuo Arimoto. "Globular clusters in Coma cluster ultra-diffuse galaxies (UDGs): evidence for two types of UDG?" Monthly Notices of the Royal Astronomical Society 492, no. 4 (January 22, 2020): 4874–83. http://dx.doi.org/10.1093/mnras/staa180.

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ABSTRACT Ultra-diffuse galaxies (UDGs) reveal extreme properties. Here, we compile the largest study to date of 85 globular cluster (GC) systems around UDGs in the Coma cluster, using new deep ground-based imaging of the known UDGs and existing imaging from the Hubble Space Telescope of their GC systems. We find that the richness of GC systems in UDGs generally exceeds that found in normal dwarf galaxies of the same stellar mass. These GC-rich UDGs imply haloes more massive than expected from the standard stellar mass–halo mass relation. The presence of such overly massive haloes presents a significant challenge to the latest simulations of UDGs in cluster environments. In some exceptional cases, the mass in the GC system is a significant fraction of the stellar content of the host galaxy. We find that rich GC systems tend to be hosted in UDGs of lower luminosity, smaller size, and fainter surface brightness. Similar trends are seen for normal dwarf galaxies in the Coma cluster. A toy model is presented in which the GC-rich UDGs are assumed to be ‘failed’ galaxies within massive haloes that have largely old, metal-poor, alpha-element-enhanced stellar populations. On the other hand, GC-poor UDGs are more akin to normal, low surface brightness dwarfs that occupy less massive dark matter haloes. Additional data on the stellar populations of UDGs with GC systems will help to further refine and test this simplistic model.
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37

Sarron, F., N. Martinet, F. Durret, and C. Adami. "Evolution of the cluster optical galaxy luminosity function in the CFHTLS: breaking the degeneracy between mass and redshift." Astronomy & Astrophysics 613 (May 2018): A67. http://dx.doi.org/10.1051/0004-6361/201731981.

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Obtaining large samples of galaxy clusters is important for cosmology: cluster counts as a function of redshift and mass can constrain the parameters of our Universe. They are also useful in order to understand the formation and evolution of clusters. We develop an improved version of the Adami & MAzure Cluster FInder (AMACFI), now the Adami, MAzure & Sarron Cluster FInder (AMASCFI), and apply it to the 154 deg2 of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) to obtain a large catalogue of 1371 cluster candidates with mass M200 > 1014 M⊙ and redshift z ≤ 0.7. We derive the selection function of the algorithm from the Millennium simulation, and cluster masses from a richness–mass scaling relation built from matching our candidates with X-ray detections. We study the evolution of these clusters with mass and redshift by computing the i′-band galaxy luminosity functions (GLFs) for the early-type (ETGs) and late-type galaxies (LTGs). This sample is 90% pure and 70% complete, and therefore our results are representative of a large fraction of the cluster population in these redshift and mass ranges. We find an increase in both the ETG and LTG faint populations with decreasing redshift (with Schechter slopes αETG = −0.65 ± 0.03 and αLTG = −0.95 ± 0.04 at z = 0.6, and αETG = −0.79 ± 0.02 and αLTG = −1.26 ± 0.03 at z = 0.2) and also a decrease in the LTG (but not the ETG) bright end. Our large sample allows us to break the degeneracy between mass and redshift, finding that the redshift evolution is more pronounced in high-mass clusters, but that there is no significant dependence of the faint end on mass for a given redshift. These results show that the cluster red sequence is mainly formed at redshift z > 0.7, and that faint ETGs continue to enrich the red sequence through quenching of brighter LTGs at z ≤ 0.7. The efficiency of this quenching is higher in large-mass clusters, while the accretion rate of faint LTGs is lower as the more massive clusters have already emptied most of their environment at higher redshifts.
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Colares, Renato, Thuany Machado, Filipe Machado Patel, Natália da Silva Brunelli, Letícia Costa Viana, Rafael Martins, Pedro Augusto dos Santos Longo, and Mainara Figueiredo Cascaes. "REDE ECOLÓGICA DOS GASTRÓPODES ASSOCIADOS AO BANCO DE ALGAS DA PRAIA DA RIBANCEIRA, SANTA CATARINA, BRASIL." Oecologia Australis 25, no. 01 (March 15, 2021): 47–58. http://dx.doi.org/10.4257/oeco.2021.2501.05.

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Among the rocky shores’ biota, the networks of interaction between macroalgae and associated organisms, especially gastropods, stand out. In order to contribute to the understanding of the ecology of rocky shores, this study aims to evaluate the relation between macroalgae and associated gastropods in Ribanceira Beach, Imbituba, Santa Catarina, Brazil. The survey of algae samples took place in a wet season, using 20 cm x 20 cm quadrants, allocated in 18 transects distributed equally in the infra and mesolittoral zones, with five points each. In the laboratory, algae were screened and associated gastropods identified. Concepts of network theory were applied for a better understanding of interactions among organisms, where connectance descriptors, niche overlap and centrality index for each species were calculated. Multivariate techniques were used to assess the significance of intertidal zones, morphofunctional group and other variables in the composition of the associated gastropods. The sampling resulted in a total of 1.466 gastropods, distributed in 14 species and nine families. In relation to the macroalgae, 14 species were identified, with seven presenting associated gastropods. The ecological network showed low connectance and niche overlap for both levels (gastropods and macroalgae), suggesting the existence of many specific interactions. The centrality values highlighted Eulithidium affine (C.B. Adams, 1850) and Sargassum cymosum C. Agardh as key species in the studied network. The mass and morphofunctional group of the macroalgae sampled showed influence in the composition of the associated community. Cortical algae, especially S. cymosum, stood out with high levels of species richness and species density of associated gastropods, suggesting importance in the structural complexity of macroalgae for gastropods. The non-significant effect of the tidal zone for the gastropod composition was highlighted, suggesting that the nesting and foraging stability provided by the macroalgae allows the same gastropod species to occur in both infralittoral and mesolittoral zones.
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Martinache, C., A. Rettura, H. Dole, M. Lehnert, B. Frye, B. Altieri, A. Beelen, et al. "Spitzer Planck Herschel Infrared Cluster (SPHerIC) survey: Candidate galaxy clusters at 1.3 < z < 3 selected by high star-formation rate." Astronomy & Astrophysics 620 (December 2018): A198. http://dx.doi.org/10.1051/0004-6361/201833198.

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There is a lack of large samples of spectroscopically confirmed clusters and protoclusters at high redshifts, z > 1.5. Discovering and characterizing distant (proto-)clusters is important for yielding insights into the formation of large-scale structure and on the physical processes responsible for regulating star-formation in galaxies in dense environments. The Spitzer Planck Herschel Infrared Cluster (SPHerIC) survey was initiated to identify these characteristically faint and dust-reddened sources during the epoch of their early assembly. We present Spitzer/IRAC observations of 82 galaxy (proto-)cluster candidates at 1.3 < zp < 3.0 that were vetted in a two step process: (1) using Planck to select by color those sources with the highest star-formation rates, and (2) using Herschel at higher resolution to separate out the individual red sources. The addition of the Spitzer data enables efficient detection of the central and massive brightest red cluster galaxies (BRCGs). We find that BRCGs are associated with highly significant, extended and crowded regions of IRAC sources which are more overdense than the field. This result corroborates our hypothesis that BRCGs within the Planck–Herschel sources trace some of the densest and actively star-forming proto-clusters in the early Universe. On the basis of a richness-mass proxy relation, we obtain an estimate of their mean masses which suggests our sample consists of some of the most massive clusters at z ≈ 2 and are the likely progenitors of the most massive clusters observed today.
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Li, Xiang, Zewen Li, Yan He, Pan Li, Hongwei Zhou, and Nianyi Zeng. "Regional distribution of Christensenellaceae and its associations with metabolic syndrome based on a population-level analysis." PeerJ 8 (August 4, 2020): e9591. http://dx.doi.org/10.7717/peerj.9591.

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The link between the gut microbiota and metabolic syndrome (MetS) has attracted widespread attention. Christensenellaceae was recently described as an important player in human health, while its distribution and relationship with MetS in Chinese population is still unknown. This study sought to observe the association between Christensenellaceae and metabolic indexes in a large sample of residents in South China. A total of 4,781 people from the GGMP project were included, and the fecal microbiota composition of these individuals was characterized by 16S rRNA sequencing and analyzed the relation between Christensenellaceae and metabolism using QIIME (Quantitative Insight Into Microbial Ecology, Version 1.9.1). The results demonstrated that microbial richness and diversity were increased in the group with a high abundance of Christensenellaceae, who showed a greater complexity of the co-occurrence network with other bacteria than residents who lacked Christensenellaceae. The enriched bacterial taxa were predominantly represented by Oscillospira, Ruminococcaceae, RF39, Rikenellaceae and Akkermansia as the Christensenellaceae abundance increased, while the abundances of Veillonella, Fusobacterium and Klebsiella were significantly reduced. Furthermore, Christensenellaceae was negatively correlated with the pathological features of MetS, such as obesity, hypertriglyceridemia and body mass index (BMI). We found reduced levels of lipid biosynthesis and energy metabolism pathways in people with a high abundance of Christensenellaceae, which may explain the negative relationship between body weight and Christensenellaceae. In conclusion, we found a negative correlation between Christensenellaceae and MetS in a large Chinese population and reported the geographical distribution of Christensenellaceae in the GGMP study. The association data from this population-level research support the investigation of strains within Christensenellaceae as potentially beneficial gut microbes.
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van Uitert, Edo, David G. Gilbank, Henk Hoekstra, Elisabetta Semboloni, Michael D. Gladders, and Howard K. C. Yee. "Weak-lensing-inferred scaling relations of galaxy clusters in the RCS2: mass-richness, mass-concentration, mass-bias, and more." Astronomy & Astrophysics 586 (January 26, 2016): A43. http://dx.doi.org/10.1051/0004-6361/201526719.

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42

Fuzia, Brittany J., Lalitwadee Kawinwanichakij, Nicola Mehrtens, Simone Aiola, Nicholas Battaglia, Robin Ciardullo, Mark Devlin, et al. "The Atacama Cosmology Telescope: SZ-based masses and dust emission from IR-selected cluster candidates in the SHELA survey." Monthly Notices of the Royal Astronomical Society 502, no. 3 (January 25, 2021): 4026–38. http://dx.doi.org/10.1093/mnras/stab193.

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ABSTRACT We examine the stacked thermal Sunyaev–Zel’dovich (SZ) signals for a sample of galaxy group and cluster candidates from the 24 deg2 infrared Spitzer-HETDEX Exploratory Large Area (SHELA) survey. We identify the objects in combination with optical data using the redMaPPer algorithm, and divide them into three richness bins (λ in 10–20, 20–30, and 30–76 with average photometric redshifts of 0.80, 0.73, and 0.70, respectively). All richness bins show evidence for dust emission, which we fit using stacked profiles from Herschel Stripe 82 data. We fit for synchrotron emission using stacked profiles created by binning source fluxes from NRAO VLA Sky Survey data. We can confidently detect the SZ decrement only in the highest richness bin, finding MSZ,500 = $8.7^{+1.7}_{-1.3} \times 10^{13}\, \mathrm{ M}_\odot$. Neglecting the correction for dust and synchrotron depresses the inferred mass by 26 per cent, indicating a partial fill-in of the SZ decrement from dust and synchrotron emission. We compare our corrected SZ masses to two redMaPPer mass–richness scaling relations and find that the SZ mass is lower than predicted by the richness. For the lower richness bins, mass bias factors as low as 1 − b = 0.6 are not enough to bring the mass limits into agreement. We discuss possible explanations for this discrepancy. The SHELA richnesses may differ from previous richness measurements due to the inclusion of infrared data in redMaPPer. To connect the SZ signal to the mass, we use a universal gas pressure profile that is calibrated to massive clusters at low redshift. It may not be applicable to our lower mass, higher redshift sample.
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Yang, Wei, Chengwu Li, Rui Xu, and Xunchang Li. "Experimental Investigation on Time-Frequency Characteristics of Microseismic Signals in the Damage Evolution Process of Coal and Rock." Energies 13, no. 4 (February 13, 2020): 809. http://dx.doi.org/10.3390/en13040809.

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The deformation and failure of coal and rock materials is the primary cause of many engineering disasters. How to accurately and effectively monitor and forecast the damage evolution process of coal and rock mass, and form a set of prediction methods and prediction indicators is an urgent engineering problems to be solved in the field of rock mechanics and engineering. As a form of energy dissipation in the deformation process of coal and rock, microseismic (MS) can indirectly reflect the damage of coal and rock. In order to analyze the relationship between the damage degree of coal and rock and time-frequency characteristics of MS, the deformation and fracture process of coal and rock materials under different loading modes was tested. The time-frequency characteristics and generation mechanism of MS were analyzed under different loading stages. Meanwhile, the influences of properties of coal and rock materials on MS signals were studied. Results show that there is an evident mode cutoff point between high-frequency and low-frequency MS signals. The properties of coal and rock, such as the development degree of the original fracture, particle size and dense degree have a decisive influence on the amplitude, frequency, energy and other characteristic parameters of MS signals. The change of MS parameters is closely related to material damage, but has no strong relation with the loading rate. The richness of MS signals before the main fracture depends on the homogeneity of materials. With the increase of damage, the energy release rate increases, which can lead to the widening of MS signals spectrum. The stiffness and natural frequency of specimens decreases correspondingly. Meanwhile, the main reason that the dominant frequency of MS detected by sensors installed on the surface of coal and rock materials is mainly low-frequency is friction loss and the resonance effect. In addition, the spectrum and energy evolution of MS can be used as a characterization method of the damage degree of coal and rock materials. Furthermore, the results can provide important reference for prediction and early warning of some rock engineering disasters.
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Markov, Alexander. "SCHUBERT'S «THE TROUT» IN RUSSIAN POETRY." Izvestia of Smolensk State University, no. 1 (49) (May 26, 2020): 5–18. http://dx.doi.org/10.35785/2072-9464-2020-49-1-5-18.

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Franz Schubert is one of the well-known western composers in Russian poetry due to the fact that poets have been attracted by his laconic plots, relation to legends, melodramaticism and deep symbolism going beyond historical symbolism. In Russian poetry the small play «The Trout» acquired a meaning different from the composer’s intensions. It began to be understood not as a moral tale of caution and temptation and not as a hymn to youth and young feelings, but as a call for freedom of improvisation. The article, based on material from Russian poetry of the XXth century, immigrant and modern poetry, examines the reasons for the bias in the understanding of the play. The article thoroughly analyzes rhetoric of the text «The Trout» and features of its perception in modern and contemporary lyrics. The author indicates factors of meaning bias such as a biographical subtext of «The Trout» creation, Schubert’s general image mainly as a romantic composer, an implicit competition between poets lived at the same time for the correct understanding of musical rhetoric. The research methods include reconstruction of the composer's reputation in Russian culture, a comparative historical analysis and hermeneutics of a poetic text, and specification of musical allusions. Thanks to the individualization and analysis of the stages found in the transformation of the «The Trout» perception in Russian poetry, it is proved that the musical work perception is associated with a special understanding of media nature like the play brevity, its distribution, the first publication in the newspaper its use in parodies and mass culture has made the author understand «The Trout» as a democratic work with its own media principles. In addition, the richness of Schubert’s legendary and ballad plots and the need to artificially build Schubert’s world within a short lyrical work have turned «The Trout» into an exemplary key of the plot. The ballad starts to be interpreted through poetic form as the opposite to the work with morality; musical intonation is understood as a gesture of gaining freedom contrary to the literal content of the ballad.
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Melo, Juliana, Ana Isabel Ribeiro, Susana Aznar, Andreia Pizarro, and Maria Paula Santos. "Urban Green Spaces, Greenness Exposure and Species Richness in Residential Environments and Relations with Physical Activity and BMI in Portuguese Adolescents." International Journal of Environmental Research and Public Health 18, no. 12 (June 18, 2021): 6588. http://dx.doi.org/10.3390/ijerph18126588.

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Environmental factors play an important role in obesity-related behaviors. Evidence indicates significant associations between weight and urban green spaces in adults, but it is not clear whether this relationship applies to adolescents. Therefore, our aim was to determine the associations between urban green spaces, greenness exposure and species richness in residential environments with physical activity and body mass index. Sixty-two adolescents between 12 and 18 years of age answered a self-administered questionnaire, providing information on height, weight, age, sex and home address. Data on socioeconomic deprivation were obtained from the European Index of Deprivation for Small Portuguese Areas. Physical activity levels were assessed using accelerometers. Urban green space counts and the normalized difference vegetation index values were measured using buffers along the roads with distances of 300, 500, 1000 and 1500 m from each participant’s residence. To quantify the species richness, the species richness index was used. Linear regression models were fitted to analyze whether urban green spaces, exposure to green spaces and species richness counts for each distance were associated with physical activity and self-reported body mass index. We did not find significant associations between the independent variables and the probability of overweight or obesity. The relationship between environmental variables, adolescents’ physical activity and body weight seems to be complex and further studies may contribute to better understanding of the topic.
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Klein, M., S. Grandis, J. J. Mohr, M. Paulus, T. M. C. Abbott, J. Annis, S. Avila, et al. "A new RASS galaxy cluster catalogue with low contamination extending to z ∼ 1 in the DES overlap region." Monthly Notices of the Royal Astronomical Society 488, no. 1 (May 29, 2019): 739–69. http://dx.doi.org/10.1093/mnras/stz1463.

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ABSTRACT We present the MARD-Y3 catalogue of between 1086 and 2171 galaxy clusters (52 per cent and 65 per cent new) produced using multicomponent matched filter (MCMF) follow-up in 5000 deg2 of DES-Y3 optical data of the ∼20 000 overlapping ROSAT All-Sky Survey source catalogue (2RXS) X-ray sources. Optical counterparts are identified as peaks in galaxy richness as a function of redshift along the line of sight towards each 2RXS source within a search region informed by an X-ray prior. All peaks are assigned a probability fcont of being a random superposition. The clusters lie at 0.02 &lt; z &lt; 1.1 with more than 100 clusters at z &gt; 0.5. Residual contamination is 2.6 per cent and 9.6 per cent for the cuts adopted here. For each cluster we present the optical centre, redshift, rest frame X-ray luminosity, M500 mass, coincidence with NWAY infrared sources, and estimators of dynamical state. About 2 per cent of MARD-Y3 clusters have multiple possible counterparts, the photo-z’s are high quality with σΔz/(1 + z) = 0.0046, and ∼1 per cent of clusters exhibit evidence of X-ray luminosity boosting from emission by cluster active galactic nuclei. Comparison with other catalogues (MCXC, RM, SPT-SZ, Planck) is performed to test consistency of richness, luminosity, and mass estimates. We measure the MARD-Y3 X-ray luminosity function and compare it to the expectation from a fiducial cosmology and externally calibrated luminosity- and richness–mass relations. Agreement is good, providing evidence that MARD-Y3 has low contamination and can be understood as a simple two step selection – X-ray and then optical – of an underlying cluster population described by the halo mass function.
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KRASNOV, B. R., G. I. SHENBROT, S. G. MEDVEDEV, V. S. VATSCHENOK, and I. S. KHOKHLOVA. "Host–habitat relations as an important determinant of spatial distribution of flea assemblages (Siphonaptera) on rodents in the Negev Desert." Parasitology 114, no. 2 (February 1997): 159–73. http://dx.doi.org/10.1017/s0031182096008347.

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We studied flea assemblages on rodents in different habitats of the Ramon erosion cirque in the Negev Desert to examine whether host–habitat relations influence flea spatial distribution. Eleven flea species parasitizing 12 rodent species were recorded. There was significant positive relationship between flea species richness and body mass of the host species; no relationships were found between relative richness of flea assemblage and either the number of habitats occupied by the host species or the size of host geographical range. The differences in pattern of flea parasitism among habitat types within host species were determined by both environmental features of a habitat and the specific pattern of habitat use by rodents. There was replacement of Xenopsylla conformis by Xenopsylla ramesis on Meriones crassus and Gerbillus dasyurus among different habitats. The results of ordination of the flea collections from each individual host demonstrated that the flea assemblages were segregated mainly along 4 axes, which explained 86% of total variance. Each of the ordination axes corresponded with a change in flea species composition. The directions of these changes were (1) among-hosts within a habitat and (2) among-habitats within a host.
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Chen, Chuanhong, and Xueyan Li. "The effect of online shopping festival promotion strategies on consumer participation intention." Industrial Management & Data Systems 120, no. 12 (July 17, 2020): 2375–95. http://dx.doi.org/10.1108/imds-11-2019-0628.

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PurposeThe purpose of this paper is to explore the effect of consumers' perceived product promotion and atmosphere promotion strategies on their participation intention, and the possible interaction between product promotion and atmosphere promotion strategies on their participation intention in online shopping festivals.Design/methodology/approachThis paper conceptualized consumer perception of product promotion strategies of online shopping festivals as Perceived Temptation of Price Promotion, Perceived Categories Richness of Promotion and Perceived Fun of Promotion Activities and atmosphere promotion strategies as Perceived Contagiousness of Mass Participation. Based on the Stimulus-Response Theory, this study constructed an influencing model of promotion strategies on consumer participation intention in online shopping festivals. Structural equation modeling with partial least squares was used for analyzing the data from a sample of 495 consumers to test the proposed hypotheses.FindingsThe results showed that Perceived Temptation of Price Promotion, Perceived Categories Richness of Promotion, Perceived Fun of Promotion Activities and Perceived Contagiousness of Mass Participation significantly and positively affect consumer Participation Intention; Perceived Contagiousness of Mass Participation plays a moderating role in the effect of Perceived Temptation of Price Promotion on Participation Intention.Originality/valueThis study is the first empirical attempt to examine the moderating role of atmosphere promotion between product promotion and consumer participation intention in online shopping festivals. The findings provide theoretical basis and practical guidance for e-commerce platforms and merchants for improving their online shopping festival promotion strategies.
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Rettura, A., R. Chary, J. Krick, and S. Ettori. "Mass–Richness Relations for X-Ray and SZE-selected Clusters at 0.4 < z < 2.0 as Seen by Spitzer at 4.5 μm." Astrophysical Journal 867, no. 1 (October 25, 2018): 12. http://dx.doi.org/10.3847/1538-4357/aad818.

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Zohren, Hannah, Tim Schrabback, Remco F. J. van der Burg, Monique Arnaud, Jean-Baptiste Melin, Jan Luca van den Busch, Henk Hoekstra, and Matthias Klein. "Optical follow-up study of 32 high-redshift galaxy cluster candidates from Planck with the William Herschel Telescope." Monthly Notices of the Royal Astronomical Society 488, no. 2 (July 5, 2019): 2523–42. http://dx.doi.org/10.1093/mnras/stz1838.

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Abstract The Planck satellite has detected cluster candidates via the Sunyaev Zel’dovich (SZ) effect, but the optical follow-up required to confirm these candidates is still incomplete, especially at high redshifts and for SZ detections at low significance. In this work, we present our analysis of optical observations obtained for 32 Planck cluster candidates using ACAM on the 4.2-m William Herschel Telescope. These cluster candidates were pre-selected using SDSS, WISE, and Pan-STARRS images to likely represent distant clusters at redshifts z ≳ 0.7. We obtain photometric redshift and richness estimates for all of the cluster candidates from a red-sequence analysis of r-, i-, and z-band imaging data. In addition, long-slit observations allow us to measure the redshifts of a subset of the clusters spectroscopically. The optical richness is often lower than expected from the inferred SZ mass when compared to scaling relations previously calibrated at low redshifts. This likely indicates the impact of Eddington bias and projection effects or noise-induced detections, especially at low-SZ significance. Thus, optical follow-up not only provides redshift measurements, but also an important independent verification method. We find that 18 (7) of the candidates at redshifts z &gt; 0.5 (z &gt; 0.8) are at least half as rich as expected from scaling relations, thereby clearly confirming these candidates as massive clusters. While the complex selection function of our sample due to our pre-selection hampers its use for cosmological studies, we do provide a validation of massive high-redshift clusters particularly suitable for further astrophysical investigations.
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