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1. A joint SZ–X-ray–optical analysis of the dynamical state of 288 massive galaxy clusters.

Author

Zenteno, A, Hernández-Lang, D, Klein, M, Vergara Cervantes, C, Hollowood, D L, Bhargava, S, Palmese, A, Strazzullo, V, Romer, A K, Mohr, J J, Jeltema, T, Saro, A, Lidman, C, Gruen, D, Ojeda, V, Katzenberger, A, Aguena, M, Allam, S, Avila, S, and Bayliss, M

Subjects
STELLAR luminosity function, DARK energy, GAS distribution, GALAXY clusters, CLUSTER sampling, REDSHIFT, GALACTIC evolution
Abstract

We use imaging from the first three years of the Dark Energy Survey to characterize the dynamical state of 288 galaxy clusters at 0.1 ≲ z ≲ 0.9 detected in the South Pole Telescope (SPT) Sunyaev–Zeldovich (SZ) effect survey (SPT-SZ). We examine spatial offsets between the position of the brightest cluster galaxy (BCG) and the centre of the gas distribution as traced by the SPT-SZ centroid and by the X-ray centroid/peak position from Chandra and XMM data. We show that the radial distribution of offsets provides no evidence that SPT SZ-selected cluster samples include a higher fraction of mergers than X-ray-selected cluster samples. We use the offsets to classify the dynamical state of the clusters, selecting the 43 most disturbed clusters, with half of those at z ≳ 0.5, a region seldom explored previously. We find that Schechter function fits to the galaxy population in disturbed clusters and relaxed clusters differ at z > 0.55 but not at lower redshifts. Disturbed clusters at z > 0.55 have steeper faint-end slopes and brighter characteristic magnitudes. Within the same redshift range, we find that the BCGs in relaxed clusters tend to be brighter than the BCGs in disturbed samples, while in agreement in the lower redshift bin. Possible explanations includes a higher merger rate, and a more efficient dynamical friction at high redshift. The red-sequence population is less affected by the cluster dynamical state than the general galaxy population. [ABSTRACT FROM AUTHOR]

Published
2020
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2. Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters.

Author

Palmese, A, Annis, J, Burgad, J, Farahi, A, Soares-Santos, M, Welch, B, da Silva Pereira, M, Lin, H, Bhargava, S, Hollowood, D L, Wilkinson, R, Giles, P, Jeltema, T, Romer, A K, Evrard, A E, Hilton, M, Vergara Cervantes, C, Bermeo, A, Mayers, J, and DeRose, J

Subjects
DARK energy, STELLAR mass, GALAXY clusters, PROXY, VECTOR spaces, X-ray scattering
Abstract

We introduce a galaxy cluster mass observable, μ⋆, based on the stellar masses of cluster members, and we present results for the Dark Energy Survey (DES) Year 1 (Y1) observations. Stellar masses are computed using a Bayesian model averaging method, and are validated for DES data using simulations and COSMOS data. We show that μ⋆ works as a promising mass proxy by comparing our predictions to X-ray measurements. We measure the X-ray temperature–μ⋆ relation for a total of 129 clusters matched between the wide-field DES Y1 redMaPPer catalogue and Chandra and XMM archival observations, spanning the redshift range 0.1 < |$z$| < 0.7. For a scaling relation that is linear in logarithmic space, we find a slope of α = 0.488 ± 0.043 and a scatter in the X-ray temperature at fixed μ⋆ of |$\sigma _{{\rm ln} T_\mathrm{ X}|\mu _\star }= 0.266^{+0.019}_{-0.020}$| for the joint sample. By using the halo mass scaling relations of the X-ray temperature from the Weighing the Giants program, we further derive the μ⋆-conditioned scatter in mass, finding |$\sigma _{{\rm ln} M|\mu _\star }= 0.26^{+ 0.15}_{- 0.10}$|⁠. These results are competitive with well-established cluster mass proxies used for cosmological analyses, showing that μ⋆ can be used as a reliable and physically motivated mass proxy to derive cosmological constraints. [ABSTRACT FROM AUTHOR]

Published
2020
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3. Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters.

Author

Farahi, A, Chen, X, Evrard, A E, Hollowood, D L, Wilkinson, R, Bhargava, S, Giles, P, Romer, A K, Jeltema, T, Hilton, M, Bermeo, A, Mayers, J, Vergara Cervantes, C, Rozo, E, Rykoff, E S, Collins, C, Costanzi, M, Everett, S, Liddle, A R, and Mann, R G

Subjects
X-rays, REGRESSION analysis, CONFIDENCE intervals, VARIANCES, GALAXY clusters, CLUSTER sampling, DARK energy
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, T X, with optical richness, λRM, for clusters in the redshift range 0.2 < z < 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 > 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 T X 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 T X–mass relation and the covariance of T X 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. [ABSTRACT FROM AUTHOR]

Published
2019
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4. Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function.

Author

Zhang, Y, Miller, C J, Rooney, P, Bermeo, A, Romer, A K, Vergara Cervantes, C, Rykoff, E S, Hennig, C, Das, R, McKay, T, Song, J, Wilcox, H, Bacon, D, Bridle, S L, Collins, C, Conselice, C, Hilton, M, Hoyle, B, Kay, S, and Liddle, A R

Abstract

Using ∼100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red-sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the LF simultaneously in redshift (0.1 < z < 1.05) and cluster mass (⁠|$13.5 \le \rm {log_{10}}(M_{200crit}) \sim \lt 15.0$|⁠). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schechter function, including its characteristic break (m *) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m * with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to |${\sim } 20{{\ \rm per\ cent}}$| precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis. [ABSTRACT FROM AUTHOR]

Published
2019
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5. A joint SZ-X-ray-optical analysis of the dynamical state of 288 massive galaxy clusters

Author

Matthew B. Bayliss, Eli S. Rykoff, M. Smith, Daniel Gruen, J. Gschwend, A. Roodman, A. Carnero Rosell, D. W. Gerdes, A. Katzenberger, M. E. C. Swanson, V. Scarpine, Sunayana Bhargava, Samuel Hinton, J. Carretero, G. Gutierrez, Matthias Klein, E. Suchyta, Felipe Menanteau, V. Ojeda, August E. Evrard, C. Vergara Cervantes, Marcos Lima, D. L. Burke, Michael Schubnell, Shantanu Desai, Peter Doel, Josh Frieman, A. A. Plazas, M. Carrasco Kind, Alistair R. Walker, Kyler Kuehn, H. T. Diehl, Marcelle Soares-Santos, F. Paz-Chinchón, I. Sevilla-Noarbe, D. Hernandez-Lang, R. Capasso, S. Allam, Robert A. Gruendl, Antonella Palmese, D. L. Hollowood, David J. James, K. Honscheid, R. D. Wilkinson, S. Serrano, Tesla E. Jeltema, M. A. G. Maia, Pablo Fosalba, T. N. Varga, David J. Brooks, W. G. Hartley, L. N. da Costa, R. L. C. Ogando, C. Lidman, J. De Vicente, Michel Aguena, Daniel Thomas, E. Buckley-Geer, Joseph J. Mohr, B. Floyd, Peter Melchior, A. Saro, A. K. Romer, T. F. Eifler, F. J. Castander, V. Strazzullo, Ofer Lahav, E. J. Sanchez, Santiago Avila, Ramon Miquel, M. March, G. Tarle, Alfredo Zenteno, Juan Garcia-Bellido, B. Flaugher, E. Bertin, Mike McDonald, J. R. Gonzalez, M. Costanzi, Zenteno, A., Hernández-Lang, D., Klein, M., Vergara Cervantes, C., Hollowood, D. L., Bhargava, S., Palmese, A., Strazzullo, V., Romer, A. K., Mohr, J. J., Jeltema, T., Saro, A., Lidman, C., Gruen, D., Ojeda, V., Katzenberger, A., Aguena, M., Allam, S., Avila, S., Bayliss, M., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capasso, R., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Floyd, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gonzalez, J. R., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lima, M., Mcdonald, M., Maia, M. A. G., March, M., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wilkinson, R. D., Des, Collaboration, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, galaxies: luminosity function, mass function, galaxies: clusters: general, 01 natural sciences, 0103 physical sciences, Cluster (physics), clusters: general [galaxies], Brightest cluster galaxy, education, 010303 astronomy & astrophysics, Galaxy cluster, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: luminosity function, South Pole Telescope, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), Cluster sampling, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use imaging from the first three years of the Dark Energy Survey to characterize the dynamical state of 288 galaxy clusters at $0.1 \lesssim z \lesssim 0.9$ detected in the South Pole Telescope (SPT) Sunyaev-Zeldovich (SZ) effect survey (SPT-SZ). We examine spatial offsets between the position of the brightest cluster galaxy (BCG) and the center of the gas distribution as traced by the SPT-SZ centroid and by the X-ray centroid/peak position from Chandra and XMM data. We show that the radial distribution of offsets provides no evidence that SPT SZ-selected cluster samples include a higher fraction of mergers than X-ray-selected cluster samples. We use the offsets to classify the dynamical state of the clusters, selecting the 43 most disturbed clusters, with half of those at $z \gtrsim 0.5$, a region seldom explored previously. We find that Schechter function fits to the galaxy population in disturbed clusters and relaxed clusters differ at $z>0.55$ but not at lower redshifts. Disturbed clusters at $z>0.55$ have steeper faint-end slopes and brighter characteristic magnitudes. Within the same redshift range, we find that the BCGs in relaxed clusters tend to be brighter than the BCGs in disturbed samples, while in agreement in the lower redshift bin. Possible explanations includes a higher merger rate, and a more efficient dynamical friction at high redshift. The red-sequence population is less affected by the cluster dynamical state than the general galaxy population., 21 pages, 12 Figures, 4 Tables. Accepted for publication in MNRAS

Published
2020
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6. Dark Energy Surveyed Year 1 results: calibration of cluster mis-centring in the redMaPPer catalogues

Author

W. G. Hartley, C. Stern, Devon L. Hollowood, John P. Stott, Ramon Miquel, A. Bermeo, B. Flaugher, Martin Sahlén, Chris A. Collins, Eli S. Rykoff, Elisabeth Krause, Tesla E. Jeltema, Yanxi Zhang, Shantanu Desai, C. J. Miller, Arya Farahi, A. A. Plazas, J. Gschwend, Marcelle Soares-Santos, M. E. C. Swanson, M. Costanzi, Xi Chen, Vinu Vikram, J. P. Dietrich, R. H. Schindler, Juan Garcia-Bellido, W. C. Wester, E. Bertin, David J. Brooks, M. Klein, A. Carnero Rosell, J. Carretero, Peter Melchior, Sunayana Bhargava, M. Smith, Eduardo Rozo, Jennifer L. Marshall, Daniel Gruen, G. Gutierrez, S. W. Allen, D. L. Burke, Peter Doel, R. D. Wilkinson, Maria Manolopoulou, S. Allam, Robert A. Gruendl, Pablo Fosalba, K. Honscheid, H. T. Diehl, V. Scarpine, S. Everett, G. Tarle, August E. Evrard, Ricardo L. C. Ogando, Julian A. Mayers, J. De Vicente, Ben Hoyle, Daniel Thomas, Felipe Menanteau, Robert G. Mann, M. A. G. Maia, A. von der Linden, G. Morris, Risa H. Wechsler, E. Suchyta, Matt Hilton, S. Serrano, M. Carrasco Kind, C. Vergara Cervantes, Marcos Lima, I. Sevilla-Noarbe, Enrique Gaztanaga, N. Kuropatkin, M. Splettstoesser, Adam Mantz, L. N. da Costa, Joshua A. Frieman, Douglas L. Tucker, Kyler Kuehn, Paul Giles, A. K. Romer, Santiago Avila, Keith Bechtol, F. J. Castander, Pedro T. P. Viana, E. J. Sanchez, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Zhang, Y., Jeltema, T., Hollowood, D. L., Everett, S., Rozo, E., Farahi, A., Bermeo, A., Bhargava, S., Giles, P., Romer, A. K., Wilkinson, R., Rykoff, E. S., Mantz, A., Diehl, H. T., Evrard, A. E., Stern, C., Gruen, D., von der Linden, A., Splettstoesser, M., Chen, X., Costanzi, M., Allen, S., Collins, C., Hilton, M., Klein, M., Mann, R. G., Manolopoulou, M., Morris, G., Mayers, J., Sahlen, M., Stott, J., Vergara Cervantes, C., Viana, P. T. P., Wechsler, R. H., Allam, S., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., Hoyle, B., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Wester, W., and Des, Collaboration

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: general, dark energy, X-rays: galaxies: clusters, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, media_common.cataloged_instance, clusters: general [galaxies], European union, Astronomy observatory, 010303 astronomy & astrophysics, media_common, QB, Physics, 010308 nuclear & particles physics, European research, GALÁXIAS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Research council, Astrophysics of Galaxies (astro-ph.GA), Fundamental physics, Christian ministry, galaxies: clusters [X-rays], National laboratory, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The center determination of a galaxy cluster from an optical cluster finding algorithm can be offset from theoretical prescriptions or $N$-body definitions of its host halo center. These offsets impact the recovered cluster statistics, affecting both richness measurements and the weak lensing shear profile around the clusters. This paper models the centering performance of the \RM~cluster finding algorithm using archival X-ray observations of \RM-selected clusters. Assuming the X-ray emission peaks as the fiducial halo centers, and through analyzing their offsets to the \RM~centers, we find that $\sim 75\pm 8 \%$ of the \RM~clusters are well centered and the mis-centered offset follows a Gamma distribution in normalized, projected distance. These mis-centering offsets cause a systematic underestimation of cluster richness relative to the well-centered clusters, for which we propose a descriptive model. Our results enable the DES Y1 cluster cosmology analysis by characterizing the necessary corrections to both the weak lensing and richness abundance functions of the DES Y1 redMaPPer cluster catalog., Code used in this analysis is available from https://github.com/yyzhang/center_modeling_y1

Published
2019
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7. Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters

Author

Peter Doel, Elisabeth Krause, David J. James, Alistair R. Walker, Pablo Fosalba, H. T. Diehl, Douglas L. Tucker, J. Carretero, Jochen Weller, Pedro T. P. Viana, Kyler Kuehn, E. J. Sanchez, Paul Giles, I. Sevilla-Noarbe, Eli S. Rykoff, David Brooks, M. E. C. Swanson, N. Kuropatkin, Shantanu Desai, J. P. Dietrich, Ramon Miquel, Adam Mantz, L. N. da Costa, Mathew Smith, M. Carrasco Kind, A. Bermeo, C. Vergara Cervantes, Daniel Thomas, Marcos Lima, E. Buckley-Geer, Xi Chen, V. Scarpine, R. L. C. Ogando, Tesla E. Jeltema, Sunayana Bhargava, Michael Schubnell, Joshua A. Frieman, G. Gutierrez, Robert G. Mann, Jennifer L. Marshall, J. Gschwend, K. Honscheid, Enrique Gaztanaga, M. Costanzi, Yanxi Zhang, Julian A. Mayers, A. K. Romer, August E. Evrard, Arya Farahi, Flavia Sobreira, S. Serrano, Felipe Menanteau, B. Flaugher, John P. Stott, Gregory Tarle, R. D. Wilkinson, A. Carnero Rosell, S. Everett, P. Rooney, D. L. Burke, Juan Garcia-Bellido, Martin Sahlén, Chris A. Collins, Eduardo Rozo, J. Annis, Robert A. Gruendl, Vinu Vikram, J. De Vicente, E. Suchyta, Matt Hilton, Santiago Avila, Devon L. Hollowood, Andrew R. Liddle, Francisco J. Castander, A. A. Plazas, Daniel Gruen, D. W. Gerdes, M. A. G. Maia, Peter Melchior, Farahi, A., Chen, X., Evrard, A. E., Hollowood, D. L., Wilkinson, R., Bhargava, S., Giles, P., Romer, A. K., Jeltema, T., Hilton, M., Bermeo, A., Mayers, J., Vergara Cervantes, C., Rozo, E., Rykoff, E. S., Collins, C., Costanzi, M., Everett, S., Liddle, A. R., Mann, R. G., Mantz, A., Rooney, P., Sahlen, M., Stott, J., Viana, P. T. P., Zhang, Y., Annis, J., Avila, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., da Costa, L. N., de Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, 0103 physical sciences, 010306 general physics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, Scaling, STFC, ComputingMilieux_MISCELLANEOUS, QC, Galaxy cluster, QB, Confidence region, Physics, clusters: general - X-rays: galaxies: clusters [Galaxies], RCUK, Astronomy and Astrophysics, Covariance, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Log-normal distribution, astro-ph.CO, Galaxies: clusters: general - X-rays: galaxies: clusters, galaxies: clusters [X-rays], Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using archival X-ray observations and a log-normal 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 behavior of X-ray temperatures, $T_X$, with optical richness, $\lambda_{RM}$, for clusters in the redshift range $0.2 50\%$ complete for clusters with $\lambda_{RM} > 130$. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, $\sigma_{\ln Tx | \lambda} = 0.275 \pm 0.019$. Joined with constraints for $T_X$ 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 70. Uncertainties in external parameters, particularly the slope and variance of the $T_X$--mass relation and the covariance of $T_X$ and $\lambda_{RM}$ at fixed mass, dominate the systematic error. The $95\%$ confidence region from joint sample analysis is relatively broad, $\sigma_{\ln M | \lambda} \in [0.14, \, 0.55]$, or a factor ten in variance., Comment: 14 pages. Main results are Figure 3, 5, and 6, Table 2, and Equation 9. Submitted to MNRAS. Comments welcome

Published
2019
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