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1. Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Modeling Uncertainty

Author

Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., DeRose, J., Myles, J., Ferté, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., MacCrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sánchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Alsina, A. Navarro, Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and To, C.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This work and its companion paper, Amon et al. (2021), present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter $S_8\equiv\sigma_8\sqrt{\Omega_\textrm{m}/0.3}$ at the 3% level in $\Lambda$CDM: $S_8=0.759^{+0.025}_{-0.023}$ (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the $\Lambda$CDM analysis: $S_8=0.772^{+0.018}_{-0.017}$ (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak-lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of $\Lambda$CDM is found to be in statistical agreement with Planck 2018, although favors a lower $S_8$ than the CMB-inferred value by $2.3\sigma$ (a $p$-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3$\sigma$ in the plane of $S_8\times\Omega_\textrm{m}$ caused by uncertainties in the theoretical models., Comment: Minor modifications, results unchanged. Matches version published in PRD. DES Y3 cosmology data products in https://des.ncsa.illinois.edu/releases/y3a2

Published
2021
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2. redMaPPer I: Algorithm and SDSS DR8 Catalog

Author

Rykoff, E. S., Rozo, E., Busha, M. T., Cunha, C. E., Finoguenov, A., Evrard, A., Hao, J., Koester, B. P., Leauthaud, A., Nord, B., Pierre, M., Reddick, R., Sadibekova, T., Sheldon, E. S., and Wechsler, R. H.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe redMaPPer, a new red-sequence cluster finder specifically designed to make optimal use of ongoing and near-future large photometric surveys. The algorithm has multiple attractive features: (1) It can iteratively self-train the red-sequence model based on minimal spectroscopic training sample, an important feature for high redshift surveys; (2) It can handle complex masks with varying depth; (3) It produces cluster-appropriate random points to enable large-scale structure studies; (4) All clusters are assigned a full redshift probability distribution P(z); (5) Similarly, clusters can have multiple candidate central galaxies, each with corresponding centering probabilities; (6) The algorithm is parallel and numerically efficient: it can run a Dark Energy Survey-like catalog in ~500 CPU hours; (7) The algorithm exhibits excellent photometric redshift performance, the richness estimates are tightly correlated with external mass proxies, and the completeness and purity of the corresponding catalogs is superb. We apply the redMaPPer algorithm to ~10,000 deg^2 of SDSS DR8 data, and present the resulting catalog of ~25,000 clusters over the redshift range 0.08

Published
2013
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3. The L_X--M relation of Clusters of Galaxies

Author

Rykoff, E. S., Evrard, A. E., McKay, T. A., Becker, M. R., Johnston, D. E., Koester, B. P., Nord, B., Rozo, E., Sheldon, E. S., Stanek, R., and Wechsler, R. H.

Subjects
Astrophysics
Abstract

We present a new measurement of the scaling relation between X-ray luminosity and total mass for 17,000 galaxy clusters in the maxBCG cluster sample. Stacking sub-samples within fixed ranges of optical richness, N_200, we measure the mean 0.1-2.4 keV X-ray luminosity, , from the ROSAT All-Sky Survey. The mean mass, , is measured from weak gravitational lensing of SDSS background galaxies (Johnston et al. 2007). For 9 <= N_200 < 200, the data are well fit by a power-law, /10^42 h^-2 erg/s = (12.6+1.4-1.3 (stat) +/- 1.6 (sys)) (/10^14 h^-1 M_sun)^1.65+/-0.13. The slope agrees to within 10% with previous estimates based on X-ray selected catalogs, implying that the covariance in L_X and N_200 at fixed halo mass is not large. The luminosity intercent is 30%, or 2\sigma, lower than determined from the X-ray flux-limited sample of Reiprich & Bohringer (2002), assuming hydrostatic equilibrium. This difference could arise from a combination of Malmquist bias and/or systematic error in hydrostatic mass estimates, both of which are expected. The intercept agrees with that derived by Stanek et al. (2006) using a model for the statistical correspondence between clusters and halos in a WMAP3 cosmology with power spectrum normalization sigma_8 = 0.85. Similar exercises applied to future data sets will allow constraints on the covariance among optical and hot gas properties of clusters at fixed mass., Comment: 5 pages, 1 figure, MNRAS accepted

Published
2008
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4. Measuring the mean and scatter of the X-ray luminosity -- optical richness relation for maxBCG galaxy clusters

Author

Rykoff, E. S., McKay, T. A., Becker, M. R., Evrard, A., Johnston, D. E., Koester, B. P., Rozo, E., Sheldon, E. S., and Wechsler, R. H.

Subjects
Astrophysics
Abstract

Determining the scaling relations between galaxy cluster observables requires large samples of uniformly observed clusters. We measure the mean X-ray luminosity--optical richness (L_X--N_200) relation for an approximately volume-limited sample of more than 17,000 optically-selected clusters from the maxBCG catalog spanning the redshift range 0.1

Published
2007
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5. A Gravitationally Lensed Quasar with Quadruple Images Separated by 14.62 Arcseconds

Author

Inada, N., Oguri, M., Pindor, B., Hennawi, J. F., Chiu, K., Zheng, W., Ichikawa, S. -I., Gregg, M. D., Becker, R. H., Suto, Y., Strauss, M. A., Turner, E. L., Keeton, C. R., Annis, J., Castander, F. J., Eisenstein, D. J., Frieman, J. A., Fukugita, M., Gunn, J. E., Johnston, D. E., Kent, S. M., Nichol, R. C., Richards, G. T., Rix, H. -W., Sheldon, E. S., Bahcall, N. A., Brinkmann, J., Ivezic, Z., Lamb, D. Q., McKay, T. A., Schneider, D. P., and York, D. G.

Subjects
Astrophysics
Abstract

Gravitational lensing is a powerful tool for the study of the distribution of dark matter in the Universe. The cold-dark-matter model of the formation of large-scale structures predicts the existence of quasars gravitationally lensed by concentrations of dark matter so massive that the quasar images would be split by over 7 arcsec. Numerous searches for large-separation lensed quasars have, however, been unsuccessful. All of the roughly 70 lensed quasars known, including the first lensed quasar discovered, have smaller separations that can be explained in terms of galaxy-scale concentrations of baryonic matter. Although gravitationally lensed galaxies with large separations are known, quasars are more useful cosmological probes because of the simplicity of the resulting lens systems. Here we report the discovery of a lensed quasar, SDSS J1004+4112, which has a maximum separation between the components of 14.62 arcsec. Such a large separation means that the lensing object must be dominated by dark matter. Our results are fully consistent with theoretical expectations based on the cold-dark-matter model., Comment: 10 pages, 3 figures, to appear in the 18th&25th Dec issue of Nature (Letters to Nature)

Published
2003
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6. Observations and Theoretical Implications of the Large Separation Lensed Quasar SDSS J1004+4112

Author

Oguri, M., Inada, N., Keeton, C. R., Pindor, B., Hennawi, J. F., Gregg, M. D., Becker, R. H., Chiu, K., Zheng, W., Ichikawa, S. -I., Suto, Y., Turner, E. L., Annis, J., Bahcall, N. A., Brinkmann, J., Castander, F. J., Eisenstein, D. J., Frieman, J. A., Goto, T., Gunn, J. E., Johnston, D. E., Kent, S. M., Nichol, R. C., Richards, G. T., Rix, H. -W., Schneider, D. P., Sheldon, E. S., and Szalay, A. S.

Subjects
Astrophysics
Abstract

We study the recently discovered gravitational lens SDSS J1004+4112, the first quasar lensed by a cluster of galaxies. It consists of four images with a maximum separation of 14.62''. The system has been confirmed as a lensed quasar at z=1.734 on the basis of deep imaging and spectroscopic follow-up observations. We present color-magnitude relations for galaxies near the lens plus spectroscopy of three central cluster members, which unambiguously confirm that a cluster at z=0.68 is responsible for the large image separation. We find a wide range of lens models consistent with the data, but they suggest four general conclusions: (1) the brightest cluster galaxy and the center of the cluster potential well appear to be offset by several kpc; (2) the cluster mass distribution must be elongated in the North--South direction, which is consistent with the observed distribution of cluster galaxies; (3) the inference of a large tidal shear (~0.2) suggests significant substructure in the cluster; and (4) enormous uncertainty in the predicted time delays between the images means that measuring the delays would greatly improve constraints on the models. We also compute the probability of such large separation lensing in the SDSS quasar sample, on the basis of the CDM model. The lack of large separation lenses in previous surveys and the discovery of one in SDSS together imply a mass fluctuation normalization \sigma_8=1.0^{+0.4}_{-0.2} (95% CL), if cluster dark matter halos have an inner slope -1.5. Shallower profiles would require higher values of \sigma_8. Although the statistical conclusion might be somewhat dependent on the degree of the complexity of the lens potential, the discovery is consistent with the predictions of the abundance of cluster-scale halos in the CDM scenario. (Abridged), Comment: 21 pages, 24 figures, 5 tables, accepted for publication in ApJ

Published
2003
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7. The Galaxy-mass Correlation Function Measured from Weak Lensing in the SDSS

Author

Sheldon, E. S., Johnston, D. E., Frieman, J. A., Scranton, R., McKay, T. A., Connolly, A. J., Budavari, T., Zehavi, I., Bahcall, N., Brinkmann, J., and Fukugita, M.

Subjects
Astrophysics
Abstract

We present galaxy-galaxy lensing measurements over scales 0.025 to 10 Mpc/h in the Sloan Digital Sky Survey. Using a flux-limited sample of 127,001 lens galaxies with spectroscopic redshifts and mean luminosity = L_* and 9,020,388 source galaxies with photometric redshifts, we invert the lensing signal to obtain the galaxy-mass correlation function xi_{gm}. We find xi_{gm} is consistent with a power-law, xi_{gm} = (r/r_0)^{-gamma}, with best-fit parameters gamma = 1.79 +/- 0.06 and r_0 = (5.4+/-0.7)(0.27/Omega_m)^{1/gamma} Mpc/h. At fixed separation, the ratio xi_{gg}/xi_{gm} = b/r where b is the bias and r is the correlation coefficient. Comparing to the galaxy auto-correlation function for a similarly selected sample of SDSS galaxies, we find that b/r is approximately scale independent over scales 0.2-6.7 Mpc/h, with mean = (1.3+/-0.2)(Omega_m/0.27). We also find no scale dependence in b/r for a volume limited sample of luminous galaxies (-23.0 < M_r < -21.5). The mean b/r for this sample is _{Vlim} = (2.0+/-0.7)(Omega_m/0.27). We split the lens galaxy sample into subsets based on luminosity, color, spectral type, and velocity dispersion, and see clear trends of the lensing signal with each of these parameters. The amplitude and logarithmic slope of xi_{gm} increases with galaxy luminosity. For high luminosities (L ~5 L_*), xi_{gm} deviates significantly from a power law. These trends with luminosity also appear in the subsample of red galaxies, which are more strongly clustered than blue galaxies., Comment: 20 pages, 21 figures, prepared with emulateapj, Accepted to AJ, corrected some major typos

Published
2003
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8. Physical Evidence for Dark Energy

Author

Scranton, R., Connolly, A. J., Nichol, R. C., Stebbins, A., Szapudi, I., Eisenstein, D. J., Afshordi, N., Budavari, T., Csabai, I., Frieman, J. A., Gunn, J. E., Johnston, D., Loh, Y., Lupton, R. H., Miller, C. J., Sheldon, E. S., Sheth, R. S., Szalay, A. S., Tegmark, M., and Xu, Y.

Subjects
Astrophysics, High Energy Physics - Experiment
Abstract

We present measurements of the angular cross-correlation between luminous red galaxies from the Sloan Digital Sky Survey and the cosmic microwave background temperature maps from the Wilkinson Microwave Anisotropy Probe. We find a statistically significant achromatic positive correlation between these two data sets, which is consistent with the expected signal from the late Integrated Sachs-Wolfe (ISW) effect. We do not detect any anti-correlation on small angular scales as would be produced from a large Sunyaev-Zel'dovich (SZ) effect, although we do see evidence for some SZ effect for our highest redshift samples. Assuming a flat universe, our preliminary detection of the ISW effect provides independent physical evidence for the existence of dark energy., Comment: Submitted to Phys. Rev. Letters (6 pages)

Published
2003

10. Dark Energy Survey Year 3 results: Cosmology from cosmic shear and robustness to modeling uncertainty

Author

Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferté, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sánchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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, Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferte, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sanchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Plazas Malagon, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), National Science Foundation (US), European Commission, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, University of Chicago, University of Pennsylvania, Carnegie Mellon University, Northeastern University, University of Arizona, École Polytechnique Fédérale de Lausanne (EPFL), Stanford University, University of Michigan, The Ohio State University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, University of California, California Institute of Technology, University College London, Duke University, University of Cambridge, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, ETH Zürich, Northern Illinois University, University of Zürich, Argonne National Laboratory, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, University of Hawai'i, University of Wisconsin-Madison, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnológicas (CIEMAT), Instituto de Astrofísica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, University of Manchester, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Fermi National Accelerator Laboratory, Max Planck Institute für Extraterrestrial Physics, Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, Université de Genève, Université de Paris, Laboratoire de Physique de Clermont, Laboratoire de Physique Nucléaire et de Hautes Énergies, The University of Tokyo, Ohio State University, Brookhaven National Laboratory, Ludwig-Maximilians Universität München, NSF's National Optical-Infrared Astronomy Research Laboratory, University of Portsmouth, Institut d'Astrophysique de Paris, University of Sussex, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Max Planck Institute for Extraterrestrial Physics, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas A and M University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and UAM. Departamento de Física Teórica

Subjects
luminous red galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, Sky surveys, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Gravitational lenses, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, Weak, baryonic feedback, 010303 astronomy & astrophysics, redshift inference, intrinsic galaxy shapes, Gravitational Lensing, 010308 nuclear & particles physics, Física, COSMOLOGIA, Dark Energy, 13. Climate action, 2-point correlation-functions, photometric data set, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Secco, L.F., et al. (DES Collaboration), This work and its companion paper, Amon et al. [Phys. Rev. D 105, 023514 (2022)PRVDAQ2470-001010.1103/PhysRevD.105.023514], present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter S8σ8ωm/0.3 at the 3% level in ΛCDM: S8=0.759-0.023+0.025 (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the ΛCDM analysis: S8=0.772-0.017+0.018 (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of ΛCDM is found to be in statistical agreement with Planck 2018, although favors a lower S8 than the CMB-inferred value by 2.3σ (a p-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3σ in the plane of S8×ωm caused by uncertainties in the theoretical models., The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.

Published
2022
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27. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey : measurements of the growth of structure and expansion rate at z = 0.57 from anisotropic clustering

Author

Reid, B. A., Samushia, L., White, M., Percival, W. J., Manera, M., Padmanabhan, N., Ross, A. J., Sánchez, A. G., Bailey, S., Bizyaev, D., Bolton, A. S., Brewington, H., Brinkmann, J., Brownstein, J. R., Cuesta, A. J., Eisenstein, D. J., Gunn, J. E., Honscheid, K., Malanushenko, E., Malanushenko, V., Maraston, C., McBride, C. K., Muna, D., Nichol, R. C., Oravetz, D., Pan, K., de Putter, R., Roe, N. A., Ross, N. P., Schlegel, D. J., Schneider, D. P., Seo, H.-J., Shelden, A., Sheldon, E. S., Simmons, A., Skibba, R. A., Snedden, S., Swanson, M. E. C., Thomas, D., Tinker, J., Tojeiro, R., Verde, L., Wake, D. A., Weaver, B. A., Weinberg, D. H., Zehavi, I., Zhao, G.-B., and University of St Andrews. School of Physics and Astronomy

Subjects
QC Physics, haloes [Galaxies], statistics [Galaxies], Cosmological parameters, QB Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Large-scale structure of the Universe, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

We analyse the anisotropic clustering of massive galaxies from the Sloan Digital Sky Survey III Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) sample, which consists of 264 283 galaxies in the redshift range 0.43 < z < 0.7 spanning 3275 deg2. Both peculiar velocities and errors in the assumed redshift–distance relation (‘Alcock–Paczynski effect’) generate correlations between clustering amplitude and orientation with respect to the line of sight. Together with the sharp baryon acoustic oscillation (BAO) standard ruler, our measurements of the broad-band shape of the monopole and quadrupole correlation functions simultaneously constrain the comoving angular diameter distance (2190 ± 61 Mpc) to z = 0.57, the Hubble expansion rate at z = 0.57 (92.4 ± 4.5 km s−1 Mpc−1) and the growth rate of structure at that same redshift (dσ8/d ln a = 0.43 ± 0.069). Our analysis provides the best current direct determination of both DA and H in galaxy clustering data using this technique. If we further assume a Λcold dark matter expansion history, our growth constraint tightens to dσ8/d ln a = 0.415 ± 0.034. In combination with the cosmic microwave background, our measurements of DA, H and dσ8/d ln a all separately require dark energy at z > 0.57, and when combined imply ΩΛ = 0.74 ± 0.016, independent of the Universe's evolution at z < 0.57. All of these constraints assume scale-independent linear growth, and assume general relativity to compute both 퓞 (10 per cent) non-linear model corrections and our errors. In our companion paper, Samushia et al., we explore further cosmological implications of these observations. Publisher PDF

Published
2012

35. redMaPPer. I. ALGORITHM AND SDSS DR8 CATALOG

Author

Rykoff, E. S., primary, Rozo, E., additional, Busha, M. T., additional, Cunha, C. E., additional, Finoguenov, A., additional, Evrard, A., additional, Hao, J., additional, Koester, B. P., additional, Leauthaud, A., additional, Nord, B., additional, Pierre, M., additional, Reddick, R., additional, Sadibekova, T., additional, Sheldon, E. S., additional, and Wechsler, R. H., additional

Published
2014
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36. Baryon acoustic oscillations in the Lyαforest of BOSS quasars

Author

Busca, N. G., primary, Delubac, T., additional, Rich, J., additional, Bailey, S., additional, Font-Ribera, A., additional, Kirkby, D., additional, Le Goff, J.-M., additional, Pieri, M. M., additional, Slosar, A., additional, Aubourg, É., additional, Bautista, J. E., additional, Bizyaev, D., additional, Blomqvist, M., additional, Bolton, A. S., additional, Bovy, J., additional, Brewington, H., additional, Borde, A., additional, Brinkmann, J., additional, Carithers, B., additional, Croft, R. A. C., additional, Dawson, K. S., additional, Ebelke, G., additional, Eisenstein, D. J., additional, Hamilton, J.-C., additional, Ho, S., additional, Hogg, D. W., additional, Honscheid, K., additional, Lee, K.-G., additional, Lundgren, B., additional, Malanushenko, E., additional, Malanushenko, V., additional, Margala, D., additional, Maraston, C., additional, Mehta, K., additional, Miralda-Escudé, J., additional, Myers, A. D., additional, Nichol, R. C., additional, Noterdaeme, P., additional, Olmstead, M. D., additional, Oravetz, D., additional, Palanque-Delabrouille, N., additional, Pan, K., additional, Pâris, I., additional, Percival, W. J., additional, Petitjean, P., additional, Roe, N. A., additional, Rollinde, E., additional, Ross, N. P., additional, Rossi, G., additional, Schlegel, D. J., additional, Schneider, D. P., additional, Shelden, A., additional, Sheldon, E. S., additional, Simmons, A., additional, Snedden, S., additional, Tinker, J. L., additional, Viel, M., additional, Weaver, B. A., additional, Weinberg, D. H., additional, White, M., additional, Yèche, C., additional, and York, D. G., additional

Published
2013
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37. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Release 9 spectroscopic galaxy sample

Author

Anderson, L., primary, Aubourg, E., additional, Bailey, S., additional, Bizyaev, D., additional, Blanton, M., additional, Bolton, A. S., additional, Brinkmann, J., additional, Brownstein, J. R., additional, Burden, A., additional, Cuesta, A. J., additional, da Costa, L. A. N., additional, Dawson, K. S., additional, de Putter, R., additional, Eisenstein, D. J., additional, Gunn, J. E., additional, Guo, H., additional, Hamilton, J.-C., additional, Harding, P., additional, Ho, S., additional, Honscheid, K., additional, Kazin, E., additional, Kirkby, D., additional, Kneib, J.-P., additional, Labatie, A., additional, Loomis, C., additional, Lupton, R. H., additional, Malanushenko, E., additional, Malanushenko, V., additional, Mandelbaum, R., additional, Manera, M., additional, Maraston, C., additional, McBride, C. K., additional, Mehta, K. T., additional, Mena, O., additional, Montesano, F., additional, Muna, D., additional, Nichol, R. C., additional, Nuza, S. E., additional, Olmstead, M. D., additional, Oravetz, D., additional, Padmanabhan, N., additional, Palanque-Delabrouille, N., additional, Pan, K., additional, Parejko, J., additional, Paris, I., additional, Percival, W. J., additional, Petitjean, P., additional, Prada, F., additional, Reid, B., additional, Roe, N. A., additional, Ross, A. J., additional, Ross, N. P., additional, Samushia, L., additional, Sanchez, A. G., additional, Schlegel, D. J., additional, Schneider, D. P., additional, Scoccola, C. G., additional, Seo, H.-J., additional, Sheldon, E. S., additional, Simmons, A., additional, Skibba, R. A., additional, Strauss, M. A., additional, Swanson, M. E. C., additional, Thomas, D., additional, Tinker, J. L., additional, Tojeiro, R., additional, Magana, M. V., additional, Verde, L., additional, Wagner, C., additional, Wake, D. A., additional, Weaver, B. A., additional, Weinberg, D. H., additional, White, M., additional, Xu, X., additional, Yeche, C., additional, Zehavi, I., additional, and Zhao, G.-B., additional

Published
2012
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38. The Sloan Digital Sky Survey quasar catalog: ninth data release

Author

Pâris, I., primary, Petitjean, P., additional, Aubourg, É., additional, Bailey, S., additional, Ross, N. P., additional, Myers, A. D., additional, Strauss, M. A., additional, Anderson, S. F., additional, Arnau, E., additional, Bautista, J., additional, Bizyaev, D., additional, Bolton, A. S., additional, Bovy, J., additional, Brandt, W. N., additional, Brewington, H., additional, Browstein, J. R., additional, Busca, N., additional, Capellupo, D., additional, Carithers, W., additional, Croft, R. A. C., additional, Dawson, K., additional, Delubac, T., additional, Ebelke, G., additional, Eisenstein, D. J., additional, Engelke, P., additional, Fan, X., additional, Filiz Ak, N., additional, Finley, H., additional, Font-Ribera, A., additional, Ge, J., additional, Gibson, R. R., additional, Hall, P. B., additional, Hamann, F., additional, Hennawi, J. F., additional, Ho, S., additional, Hogg, D. W., additional, Ivezić, Ž., additional, Jiang, L., additional, Kimball, A. E., additional, Kirkby, D., additional, Kirkpatrick, J. A., additional, Lee, K.-G., additional, Le Goff, J.-M., additional, Lundgren, B., additional, MacLeod, C. L., additional, Malanushenko, E., additional, Malanushenko, V., additional, Maraston, C., additional, McGreer, I. D., additional, McMahon, R. G., additional, Miralda-Escudé, J., additional, Muna, D., additional, Noterdaeme, P., additional, Oravetz, D., additional, Palanque-Delabrouille, N., additional, Pan, K., additional, Perez-Fournon, I., additional, Pieri, M. M., additional, Richards, G. T., additional, Rollinde, E., additional, Sheldon, E. S., additional, Schlegel, D. J., additional, Schneider, D. P., additional, Slosar, A., additional, Shelden, A., additional, Shen, Y., additional, Simmons, A., additional, Snedden, S., additional, Suzuki, N., additional, Tinker, J., additional, Viel, M., additional, Weaver, B. A., additional, Weinberg, D. H., additional, White, M., additional, Wood-Vasey, W. M., additional, and Yèche, C., additional

Published
2012
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39. The LX–M relation of clusters of galaxies

Author

Rykoff, E. S., primary, Evrard, A. E., additional, McKay, T. A., additional, Becker, M. R., additional, Johnston, D. E., additional, Koester, B. P., additional, Nord, B., additional, Rozo, E., additional, Sheldon, E. S., additional, Stanek, R., additional, and Wechsler, R. H., additional

Published
2008
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43. The.

Author

Rykoff, E. S., Evrard, A. E., McKay, T. A., Becker, M. R., Johnston, D. E., Koester, B. P., Nord, B., Rozo, E., Sheldon, E. S., Stanek, R., and Wechsler, R. H.

Subjects
X-ray astronomy, X-rays, STELLAR luminosity function, GRAVITATIONAL lenses, MICROLENSING (Astrophysics)
Abstract

We present a new measurement of the scaling relation between X-ray luminosity and total mass for 17 000 galaxy clusters in the maxBCG cluster sample. Stacking subsamples within fixed ranges of optical richness, N200, we measure the mean 0.1–2.4 keV X-ray luminosity, , from the ROSAT All-Sky Survey. The mean mass, , is measured from weak gravitational lensing of SDSS background galaxies. For , the data are well fitted by a power law, . The slope agrees to within 10 per cent with previous estimates based on X-ray selected catalogues, implying that the covariance in and N200 at a fixed halo mass is not large. The luminosity intercept is 30 per cent, or 2σ, lower than that determined from the X-ray flux-limited sample of Reiprich & Böhringer, assuming hydrostatic equilibrium. This slight difference could arise from a combination of Malmquist bias and/or systematic error in hydrostatic mass estimates, both of which are expected. The intercept agrees with that derived by Stanek et al. using a model for the statistical correspondence between clusters and haloes in a WMAP3 cosmology with power spectrum normalization . Similar exercises applied to future data sets will allow constraints on the covariance among optical and hot gas properties of clusters at a fixed mass. [ABSTRACT FROM AUTHOR]

Published
2008
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44. Raynaud, Gaston, La Chastelaine de Vergi (Book Review)

Author

Sheldon, E. S.

Subjects
Europeans, Comparative literature, French poetry, Romance literature, French literature
Abstract

This is the first volume of a new series of Old French and Provençal texts of earîier date than 1500, with the general title Les Classiques français du moyen âge. The series is under the direction of M. Mario Roques, Directeur adjoint à l'École pratique des Hautes Études. The announcement signed by him and setting forth the plan of the series contemplates the publication of all the really important works (thé word "classiques"is to be taken in a wide sensé), without full vocabularies or commentaries: "il existe aujourd'hui assez de recueils philologiques, d'ouvrages généraux, d'etudes particulières, de dictionnaires, auxquels il est légitime d'envoyer; mais il serait indispensable que ces textes fussent édités avec assez de rigueur et munis d'indications historiques et critiques suffisantes pour que le travail scientifique y trouvât immédiatement une base certaine; il faudrait encore que ces éditions fussent d'un prix modique...enfin que la publication fût assez rapide pour fournir au bout de peu d'années une véritable bibliothèque riche et variée." This is a most interesting and attractive plan, and we may all hope that it will be carried out with the success it well deserves.

Published
1911
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45. Letter from E. S. Sheldon

Author

Sheldon, E. S.

Subjects
recommendation, grammar, french, Edward B Schlatter, romance philology, old french
Abstract

Letter of recommendation for Edward B. Schlatter.

Published
1904

46. The concordance to Dante's minor Italian works.

Author

Sheldon, E. S., Sheldon, E.S. (Edward Stevens), 1851-1925., Sheldon, E. S., and Sheldon, E.S. (Edward Stevens), 1851-1925.

Abstract

We have determined this item to be in the public domain according to US copyright law through information in the bibliographic record and/or US copyright renewal records. The digital version is available for all educational uses worldwide. Please contact HathiTrust staff at hathitrust-help@umich.edu with any questions about this item., Dante Alighieri, 1265-1321., (OCoLC)320172745., Sdr-ia-srlf3054742., Http://hdl.handle.net/2027/uc2.ark:/13960/t6pz54w0h.

Published
1904

49. The Amelioration of Our Spelling: Discussion

Author

Thomas, Calvin, primary, Greene, H. E., additional, Scott, F. N., additional, Emerson, O. F., additional, Cohn, A., additional, Babbitt, E. H., additional, Gregor, L. R., additional, Sheldon, E. S., additional, Bright, J. W., additional, Mead, W. E., additional, Jessen, K. D., additional, and Higginson, T. W., additional

Published
1902
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