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1. Weak lensing combined with the kinetic Sunyaev Zel'dovich effect: A study of baryonic feedback

Author: Bigwood, L., Amon, A., Schneider, A., Salcido, J., McCarthy, I. G., Preston, C., Sanchez, D., Sijacki, D., Schaan, E., Ferraro, S., Battaglia, N., Chen, A., Dodelson, S., Roodman, A., Pieres, A., Ferte, A., Alarcon, A., Drlica-Wagner, A., Choi, A., Navarro-Alsina, A., Campos, A., Ross, A. J., Rosell, A. Carnero, Yin, B., Yanny, B., Sanchez, C., Chang, C., Davis, C., Doux, C., Gruen, D., Rykoff, E. S., Huff, E. M., Sheldon, E., Tarsitano, F., Andrade-Oliveira, F., Bernstein, G. M., Giannini, G., Diehl, H. T., Huang, H., Harrison, I., Sevilla-Noarbe, I., Tutusaus, I., Elvin-Poole, J., McCullough, J., Zuntz, J., Blazek, J., DeRose, J., Cordero, J., Prat, J., Myles, J., Eckert, K., Bechtol, K., Herner, K., Secco, L. F., Gatti, M., Raveri, M., Kind, M. Carrasco, Becker, M. R., Troxel, M. A., Jarvis, M., MacCrann, N., Friedrich, O., Alves, O., Leget, P. -F., Chen, R., Rollins, R. P., Wechsler, R. H., Gruendl, R. A., Cawthon, R., Allam, S., Bridle, S. L., Pandey, S., Everett, S., Shin, T., Hartley, W. G., Fang, X., Zhang, Y., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Carretero, J., Castander, F. J., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lee, S., Marshall, J. L., Mena-Fernandez, J., Miquel, R., Muir, J., Paterno, M., Malagon, A. A. Plazas, Porredon, A., Romer, A. K., Samuroff, S., Sanchez, E., Cid, D. Sanchez, Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Weaverdyck, N., Weller, J., Wiseman, P., and Yamamoto, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev-Zel'dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, `baryonification'. First, using WL only, we compare the $S_8$ constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of $S_8$ and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters and shifts $S_8$ to $S_8=0.823^{+0.019}_{-0.020}$, a higher value than attained using the WL-only analysis. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.
Published: 2024

2. Dark Energy Survey Year 3 Results: Constraints on extensions to $\Lambda$CDM with weak lensing and galaxy clustering

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Alves, O., Amon, A., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Birrer, S., Blazek, J., Bocquet, S., Brandao-Souza, A., Bridle, S. L., Brooks, D., Burke, D. L., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, C., Davis, T. M., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Farahi, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Giani, L., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamaus, N., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huang, H., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Leget, P. -F., Lemos, P., Leonard, C. D., Liddle, A. R., Lima, M., Lin, H., MacCrann, N., Marshall, J. L., McCullough, J., Mena-Fernández, J., Menanteau, F., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paterno, M., Paz-Chinchón, F., Percival, W. J., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Scolnic, D., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Yin, B., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We constrain extensions to the $\Lambda$CDM model using measurements from the Dark Energy Survey's first three years of observations and external data. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data and blind analyses of real data to validate the robustness of our results. In many cases, constraining power is limited by the absence of nonlinear predictions that are reliable at our required precision. The models are: dark energy with a time-dependent equation of state, non-zero spatial curvature, sterile neutrinos, modifications of gravitational physics, and a binned $\sigma_8(z)$ model which serves as a probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find $(w_{\rm p}, w_a)= (-0.99^{+0.28}_{-0.17},-0.9\pm 1.2)$ at 68% confidence with $z_{\rm p}=0.24$ from the DES measurements alone, and $(w_{\rm p}, w_a)= (-1.03^{+0.04}_{-0.03},-0.4^{+0.4}_{-0.3})$ with $z_{\rm p}=0.21$ for the combination of all data considered. Curvature constraints of $\Omega_k=0.0009\pm 0.0017$ and effective relativistic species $N_{\rm eff}=3.10^{+0.15}_{-0.16}$ are dominated by external data. For massive sterile neutrinos, we improve the upper bound on the mass $m_{\rm eff}$ by a factor of three compared to previous analyses, giving 95% limits of $(\Delta N_{\rm eff},m_{\rm eff})\leq (0.28, 0.20\, {\rm eV})$. We also constrain changes to the lensing and Poisson equations controlled by functions $\Sigma(k,z) = \Sigma_0 \Omega_{\Lambda}(z)/\Omega_{\Lambda,0}$ and $\mu(k,z)=\mu_0 \Omega_{\Lambda}(z)/\Omega_{\Lambda,0}$ respectively to $\Sigma_0=0.6^{+0.4}_{-0.5}$ from DES alone and $(\Sigma_0,\mu_0)=(0.04\pm 0.05,0.08^{+0.21}_{-0.19})$ for the combination of all data. Overall, we find no significant evidence for physics beyond $\Lambda$CDM., Comment: Updated to match published version and fix a citation reference. 46 pages, 25 figures, data available at https://dev.des.ncsa.illinois.edu/releases/y3a2/Y3key-extensions
Published: 2022
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3. Constraining the Baryonic Feedback with Cosmic Shear Using the DES Year-3 Small-Scale Measurements

Author: Chen, A., Aricò, G., Huterer, D., Angulo, R., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., DeRose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., MacCrann, N., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and To, C.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package \texttt{Baccoemu} to accelerate the evaluation of the baryonic nonlinear matter power spectrum. We design our analysis pipeline to focus on the constraints of the baryonic suppression effects, utilizing the implication given by a principal component analysis on the Fisher forecasts. Our constraint on the baryonic effects can then be used to better model and ameliorate the effects of baryons in producing cosmological constraints from the next generation large-scale structure surveys. We detect the baryonic suppression on the cosmic shear measurements with a $\sim 2 \sigma$ significance. The characteristic halo mass for which half of the gas is ejected by baryonic feedback is constrained to be $M_c > 10^{13.2} h^{-1} M_{\odot}$ (95\% C.L.). The best-fit baryonic suppression is $\sim 5\%$ at $k=1.0 {\rm Mpc}\ h^{-1}$ and $\sim 15\%$ at $k=5.0 {\rm Mpc} \ h^{-1}$. Our findings are robust with respect to the assumptions about the cosmological parameters, specifics of the baryonic model, and intrinsic alignments., Comment: 20 pages, 10 figures. DES Collaboration, Year-3 analysis
Published: 2022
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4. Lensing Without Borders. I. A Blind Comparison of the Amplitude of Galaxy-Galaxy Lensing Between Independent Imaging Surveys

Author: Leauthaud, A., Amon, A., Singh, S., Gruen, D., Lange, J. U., Huang, S., Robertson, N. C., Varga, T. N., Luo, Y., Heymans, C., Hildebrandt, H., Blake, C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Bhargava, S., Blazek, J., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Choi, A., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, C., De Vicente, J., DeRose, J., Diehl, H. T., Dietrich, J. P., Doel, P., Eckert, K., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gatti, M., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hollowood, D. L., Honscheid, K., Jain, B., James, D. J., Jarvis, M., Joachimi, B., Kannawadi, A., Kim, A. G., Krause, E., Kuehn, K., Kuijken, K., Kuropatkin, N., Lima, M., MacCrann, N., Maia, M. A. G., Makler, M., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Miyatake, H., Mohr, J. J., Moraes, B., More, S., Surhud, M., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Malagon, A. A. Plazas, Prat, J., Rau, M. M., Rhodes, J., Rodriguez-Monroy, M., Roodman, A., Ross, A. J., Samuroff, S., Sanchez, C., Sanchez, E., Scarpine, V., Schlegel, D. J., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sifon, C., Smith, M., Speagle, J. S., Suchyta, E., Tarle, G., Thomas, D., Tinker, J., To, C., Troxel, M. A., Van Waerbeke, L., Vielzeuf, P., and Wright, A. H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Lensing Without Borders is a cross-survey collaboration created to assess the consistency of galaxy-galaxy lensing signals ($\Delta\Sigma$) across different data-sets and to carry out end-to-end tests of systematic errors. We perform a blind comparison of the amplitude of $\Delta\Sigma$ using lens samples from BOSS and six independent lensing surveys. We find good agreement between empirically estimated and reported systematic errors which agree to better than 2.3$\sigma$ in four lens bins and three radial ranges. For lenses with $z_{\rm L}>0.43$ and considering statistical errors, we detect a 3-4$\sigma$ correlation between lensing amplitude and survey depth. This correlation could arise from the increasing impact at higher redshift of unrecognised galaxy blends on shear calibration and imperfections in photometric redshift calibration. At $z_{\rm L}>0.54$ amplitudes may additionally correlate with foreground stellar density. The amplitude of these trends is within survey-defined systematic error budgets which are designed to include known shear and redshift calibration uncertainty. Using a fully empirical and conservative method, we do not find evidence for large unknown systematics. Systematic errors greater than 15% (25%) ruled out in three lens bins at 68% (95%) confidence at $z<0.54$. Differences with respect to predictions based on clustering are observed to be at the 20-30% level. Our results therefore suggest that lensing systematics alone are unlikely to fully explain the "lensing is low" effect at $z<0.54$. This analysis demonstrates the power of cross-survey comparisons and provides a promising path for identifying and reducing systematics in future lensing analyses., Comment: 41 page, 20 figures
Published: 2021
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5. Cosmic Shear in Harmonic Space from the Dark Energy Survey Year 1 Data: Compatibility with Configuration Space Results

Author: Camacho, H., Andrade-Oliveira, F., Troja, A., Rosenfeld, R., Faga, L., Gomes, R., Doux, C., Fang, X., Lima, M., Miranda, V., Eifler, T. F., Friedrich, O., Gatti, M., Bernstein, G. M., Blazek, J., Bridle, S. L., Choi, A., Davis, C., DeRose, J., Gaztanaga, E., Gruen, D., Hartley, W. G., Hoyle, B., Jarvis, M., MacCrann, N., Prat, J., Rau, M. M., Samuroff, S., Sánchez, C., Sheldon, E., Troxel, M. A., Vielzeuf, P., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Reil, K., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a cosmic shear analysis in harmonic space using the first year of data collected by the Dark Energy Survey (DES-Y1). We measure the cosmic weak lensing shear power spectra using the Metacalibration catalogue and perform a likelihood analysis within the framework of CosmoSIS. We set scale cuts based on baryonic effects contamination and model redshift and shear calibration uncertainties as well as intrinsic alignments. We adopt as fiducial covariance matrix an analytical computation accounting for the mask geometry in the Gaussian term, including non-Gaussian contributions. A suite of 1200 lognormal simulations is used to validate the harmonic space pipeline and the covariance matrix. We perform a series of stress tests to gauge the robustness of the harmonic space analysis. Finally, we use the DES-Y1 pipeline in configuration space to perform a similar likelihood analysis and compare both results, demonstrating their compatibility in estimating the cosmological parameters $S_8$, $\sigma_8$ and $\Omega_m$. The methods implemented and validated in this paper will allow us to perform a consistent harmonic space analysis in the upcoming DES data., Comment: 16 pages, 11 figures. This version matches the published one
Published: 2021
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6. Dark Energy Survey Year 3 results: Marginalisation over redshift distribution uncertainties using ranking of discrete realisations

Author: Cordero, Juan P., Harrison, Ian, Rollins, Richard P., Bernstein, G. M., Bridle, S. L., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Camacho, H., Campos, A., Choi, A., DeRose, J., Dodelson, S., Eckert, K., Eifler, T. F., Everett, S., Fang, X., Friedrich, O., Gruen, D., Gruendl, R. A., Hartley, W. G., Huff, E. M., Krause, E., Kuropatkin, N., MacCrann, N., McCullough, J., Myles, J., Pandey, S., Raveri, M., Rosenfeld, R., Rykoff, E. S., Sánchez, C., Sánchez, J., Sevilla-Noarbe, I., Sheldon, E., Troxel, M., Wechsler, R., Yanny, B., Yin, B., Zhang, Y., Aguena, M., Allam, S., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L., Pereira, M. E. da Silva, De Vicente, J., Diehl, H. T., Dietrich, J., Doel, P., Elvin-Poole, J., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D., Kuehn, K., Lahav, O., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagón, A. Plazas, Sánchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., and Varga, T. N.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Cosmological information from weak lensing surveys is maximised by dividing source galaxies into tomographic sub-samples for which the redshift distributions are estimated. Uncertainties on these redshift distributions must be correctly propagated into the cosmological results. We present hyperrank, a new method for marginalising over redshift distribution uncertainties in cosmological analyses, using discrete samples from the space of all possible redshift distributions. This is demonstrated in contrast to previous highly simplified parametric models of the redshift distribution uncertainty. In hyperrank the set of proposed redshift distributions is ranked according to a small (in this work between one and four) number of summary values, which are then sampled along with other nuisance parameters and cosmological parameters in the Monte Carlo chain used for inference. This can be regarded as a general method for marginalising over discrete realisations of data vector variation with nuisance parameters, which can consequently be sampled separately to the main parameters of interest, allowing for increased computational efficiency. We focus on the case of weak lensing cosmic shear analyses and demonstrate our method using simulations made for the Dark Energy Survey (DES). We show the method can correctly and efficiently marginalise over a range of models for the redshift distribution uncertainty. Finally, we compare hyperrank to the common mean-shifting method of marginalising over redshift uncertainty, validating that this simpler model is sufficient for use in the DES Year 3 cosmology results presented in companion papers., Comment: Accepted for publication in MNRAS. 17 pages, 12 figures, comments welcome Replacement: Added small comments suggested by referee
Published: 2021
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7. Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Bhargava, S., Birrer, S., Blazek, J., Brandao-Souza, A., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. da Silva, Davis, C., Davis, T. M., De Vicente, J., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Evrard, A. E., Fang, X., Farahi, A., Fernandez, E., Ferrero, I., Ferté, A., Fosalba, P., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Leget, P. -F., Lemos, P., Liddle, A. R., Lidman, C., Lima, M., Lin, H., MacCrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., McCullough, J., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tucker, D. L., Tutusaus, I., Varga, T. N., Walker, A. R., Weaverdyck, N., Wechsler, R., Weller, J., Yanny, B., Yin, B., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first cosmology results from large-scale structure in the Dark Energy Survey (DES) spanning 5000 deg$^2$. We perform an analysis combining three two-point correlation functions (3$\times$2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions. The analysis was designed to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results. We model the data within the flat $\Lambda$CDM and $w$CDM cosmological models. We find consistent cosmological results between the three two-point correlation functions; their combination yields clustering amplitude $S_8=0.776^{+0.017}_{-0.017}$ and matter density $\Omega_{\mathrm{m}} = 0.339^{+0.032}_{-0.031}$ in $\Lambda$CDM, mean with 68% confidence limits; $S_8=0.775^{+0.026}_{-0.024}$, $\Omega_{\mathrm{m}} = 0.352^{+0.035}_{-0.041}$, and dark energy equation-of-state parameter $w=-0.98^{+0.32}_{-0.20}$ in $w$CDM. This combination of DES data is consistent with the prediction of the model favored by the Planck 2018 cosmic microwave background (CMB) primary anisotropy data, which is quantified with a probability-to-exceed $p=0.13$ to $0.48$. When combining DES 3$\times$2pt data with available baryon acoustic oscillation, redshift-space distortion, and type Ia supernovae data, we find $p=0.34$. Combining all of these data sets with Planck CMB lensing yields joint parameter constraints of $S_8 = 0.812^{+0.008}_{-0.008}$, $\Omega_{\mathrm{m}} = 0.306^{+0.004}_{-0.005}$, $h=0.680^{+0.004}_{-0.003}$, and $\sum m_{\nu}<0.13 \;\mathrm{eV\; (95\% \;CL)}$ in $\Lambda$CDM; $S_8 = 0.812^{+0.008}_{-0.008}$, $\Omega_{\mathrm{m}} = 0.302^{+0.006}_{-0.006}$, $h=0.687^{+0.006}_{-0.007}$, and $w=-1.031^{+0.030}_{-0.027}$ in $w$CDM. (abridged), Comment: See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 3x2pt cosmology release. Matches version accepted in PRD
Published: 2021
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8. Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Data Calibration

Author: Amon, A., Gruen, D., Troxel, M. A., MacCrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., DeRose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferté, A., Raveri, M., Lemos, P., Campos, A., Prat, J., Sánchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P. -F., Liddle, A. R., McCullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., 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., Kron, R., 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, Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., and Weller, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This work, together with its companion paper, Secco and Samuroff et al. (2021), presents the Dark Energy Survey Year 3 cosmic shear measurements and cosmological constraints based on an analysis of over 100 million source galaxies. With the data spanning 4143 deg$^2$ on the sky, divided into four redshift bins, we produce the highest significance measurement of cosmic shear to date, with a signal-to-noise of 40. We conduct a blind analysis in the context of the $\Lambda$CDM model and find a 3% constraint of the clustering amplitude, $S_8\equiv \sigma_8 (\Omega_{\rm m}/0.3)^{0.5} = 0.759^{+0.025}_{-0.023}$. A $\Lambda$CDM-Optimized analysis, which safely includes smaller scale information, yields a 2% precision measurement of $S_8= 0.772^{+0.018}_{-0.017}$ that is consistent with the fiducial case. The two low-redshift measurements are statistically consistent with the Planck Cosmic Microwave Background result, however, both recovered $S_8$ values are lower than the high-redshift prediction by $2.3\sigma$ and $2.1\sigma$ ($p$-values of 0.02 and 0.05), respectively. The measurements are shown to be internally consistent across redshift bins, angular scales and correlation functions. The analysis is demonstrated to be robust to calibration systematics, with the $S_8$ posterior consistent when varying the choice of redshift calibration sample, the modeling of redshift uncertainty and methodology. Similarly, we find that the corrections included to account for the blending of galaxies shifts our best-fit $S_8$ by $0.5\sigma$ without incurring a substantial increase in uncertainty. We examine the limiting factors for the precision of the cosmological constraints and find observational systematics to be subdominant to the modeling of astrophysics. Specifically, we identify the uncertainties in modeling baryonic effects and intrinsic alignments as the limiting systematics., Comment: 42 pages, 19 figures
Published: 2021
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9. 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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10. Probing gravity with the DES-CMASS sample and BOSS spectroscopy

Author: Lee, S., Huff, E. M., Choi, A., Elvin-Poole, J., Hirata, C., Honscheid, K., MacCrann, N., Ross, A. J., Troxel, M. A., Eifler, T. F., Kong, H., Ferté, A., Blazek, J., Huterer, D., Amara, A., Campos, A., Chen, A., Dodelson, S., Lemos, P., Leonard, C. D., Miranda, V., Muir, J., Raveri, M., Secco, L. F., Weaverdyck, N., Zuntz, J., Bridle, S. L., Davis, C., DeRose, J., Gatti, M., Prat, J., Rau, M. M., Samuroff, S., Sánchez, C., Vielzeuf, P., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Varga, T. N., and Weller, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The DES-CMASS sample (DMASS) is designed to optimally combine the weak lensing measurements from the Dark Energy Survey (DES) and redshift-space distortions (RSD) probed by the CMASS galaxy sample from the Baryonic Oscillation Spectroscopic Survey (BOSS). In this paper, we demonstrate the feasibility of adopting DMASS as the equivalent of BOSS CMASS for a joint analysis of DES and BOSS in the framework of modified gravity. We utilize the angular clustering of the DMASS galaxies, cosmic shear of the DES METACALIBRATION sources, and cross-correlation of the two as data vectors. By jointly fitting the combination of the data with the RSD measurements from the BOSS CMASS sample and Planck data, we obtain the constraints on modified gravity parameters $\mu_0 = -0.37^{+0.47}_{-0.45}$ and $\Sigma_0 = 0.078^{+0.078}_{-0.082}$. We do not detect any significant deviation from General Relativity. Our constraints of modified gravity measured with DMASS are tighter than those with the DES Year 1 redMaGiC galaxy sample with the same external data sets by $29\%$ for $\mu_0$ and $21\%$ for $\Sigma_0$, and comparable to the published results of the DES Year 1 modified gravity analysis despite this work using fewer external data sets. This improvement is mainly because the galaxy bias parameter is shared and more tightly constrained by both CMASS and DMASS, effectively breaking the degeneracy between the galaxy bias and other cosmological parameters. Such an approach to optimally combine photometric and spectroscopic surveys using a photometric sample equivalent to a spectroscopic sample can be applied to combining future surveys having a limited overlap such as DESI and LSST., Comment: 16 pages, 8 figures, Matches version accepted by MNRAS
Published: 2021
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11. The Dark Energy Survey Data Release 2

Author: DES Collaboration, Abbott, T. M. C., Adamow, M., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Banerji, M., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Choi, A., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Davis, T. M., De Vicente, J., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., García-Bellido, J., Gelman, L., Gerdes, D. W., Giannantonio, T., Gill, M., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Jeltema, T., Johnson, M. D., Kent, S., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lin, H., MacCrann, N., Maia, M. A. G., Manning, T., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Neilsen, E., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas, A. A., Pond, C., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Rykoff, E. S., Sako, M., Sanchez, E., Santiago, B., Serrano, S., Sevilla-Noarbe, I., Smith, J. Allyn., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tremblay, P. E., Troxel, M. A., Tucker, D. L., Turner, D. J, Varga, T. N., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wilkinson, R. D., Yanny, B., Zhang, Y., Nikutta, R., Fitzpatrick, M., Jacques, A., Scott, A., Olsen, K., Huang, L., Herrera, D., Juneau, S., Nidever, D., Weaver, B. A., Adean, C., Correia, V., de Freitas, M., Freitas, F. N., Singulani, C., and Vila-Verde, G.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the second public data release of the Dark Energy Survey, DES DR2, based on optical/near-infrared imaging by the Dark Energy Camera mounted on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. DES DR2 consists of reduced single-epoch and coadded images, a source catalog derived from coadded images, and associated data products assembled from 6 years of DES science operations. This release includes data from the DES wide-area survey covering ~5000 deg2 of the southern Galactic cap in five broad photometric bands, grizY. DES DR2 has a median delivered point-spread function full-width at half maximum of g= 1.11, r= 0.95, i= 0.88, z= 0.83, and Y= 0.90 arcsec photometric uniformity with a standard deviation of < 3 mmag with respect to Gaia DR2 G-band, a photometric accuracy of ~10 mmag, and a median internal astrometric precision of ~27 mas. The median coadded catalog depth for a 1.95 arcsec diameter aperture at S/N= 10 is g= 24.7, r= 24.4, i= 23.8, z= 23.1 and Y= 21.7 mag. DES DR2 includes ~691 million distinct astronomical objects detected in 10,169 coadded image tiles of size 0.534 deg2 produced from 76,217 single-epoch images. After a basic quality selection, benchmark galaxy and stellar samples contain 543 million and 145 million objects, respectively. These data are accessible through several interfaces, including interactive image visualization tools, web-based query clients, image cutout servers and Jupyter notebooks. DES DR2 constitutes the largest photometric data set to date at the achieved depth and photometric precision., Comment: Accepted version. Copyright AAS. Reproduced with permission. 29 pages, 13 figures. Visit https://des.ncsa.illinois.edu/releases/dr2
Published: 2021
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12. DES Y3 results: Blending shear and redshift biases in image simulations

Author: MacCrann, N., Becker, M. R., McCullough, J., Amon, A., Gruen, D., Jarvis, M., Choi, A., Troxel, M. A., Sheldon, E., Yanny, B., Herner, K., Dodelson, S., Zuntz, J., Eckert, K., Rollins, R. P., Varga, T. N., Bernstein, G. M., Gruendl, R. A., Harrison, I., Hartley, W. G., Sevilla-Noarbe, I., Pieres, A., Bridle, S. L., Myles, J., Alarcon, A., Everett, S., Sánchez, C., Huff, E. M., Tarsitano, F., Gatti, M., Secco, L. F., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Wilkinson, R. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: As the statistical power of galaxy weak lensing reaches percent level precision, large, realistic and robust simulations are required to calibrate observational systematics, especially given the increased importance of object blending as survey depths increase. To capture the coupled effects of blending in both shear and photometric redshift calibration, we define the effective redshift distribution for lensing, $n_{\gamma}(z)$, and describe how to estimate it using image simulations. We use an extensive suite of tailored image simulations to characterize the performance of the shear estimation pipeline applied to the Dark Energy Survey (DES) Year 3 dataset. We describe the multi-band, multi-epoch simulations, and demonstrate their high level of realism through comparisons to the real DES data. We isolate the effects that generate shear calibration biases by running variations on our fiducial simulation, and find that blending-related effects are the dominant contribution to the mean multiplicative bias of approximately $-2\%$. By generating simulations with input shear signals that vary with redshift, we calibrate biases in our estimation of the effective redshfit distribution, and demonstrate the importance of this approach when blending is present. We provide corrected effective redshift distributions that incorporate statistical and systematic uncertainties, ready for use in DES Year 3 weak lensing analyses., Comment: Submitted to MNRAS. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release. Version accepted by mnras
Published: 2020
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13. Dark Energy Survey Year 3 Results: Redshift Calibration of the Weak Lensing Source Galaxies

Author: Myles, J., Alarcon, A., Amon, A., Sánchez, C., Everett, S., DeRose, J., McCullough, J., Gruen, D., Bernstein, G. M., Troxel, M. A., Dodelson, S., Campos, A., MacCrann, N., Yin, B., Raveri, M., Amara, A., Becker, M. R., Choi, A., Cordero, J., Eckert, K., Gatti, M., Giannini, G., Gschwend, J., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Kuropatkin, N., Lin, H., Masters, D., Miquel, R., Prat, J., Roodman, A., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Wechsler, R. H., Yanny, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Eifler, T. F., Elvin-Poole, J., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Krause, E., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Mohr, J. J., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Rodriguez-Monroy, M., Samuroff, S., Sanchez, E., Scarpine, V., Secco, L. F., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., and Wester, W.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Determining the distribution of redshifts of galaxies observed by wide-field photometric experiments like the Dark Energy Survey is an essential component to mapping the matter density field with gravitational lensing. In this work we describe the methods used to assign individual weak lensing source galaxies from the Dark Energy Survey Year 3 Weak Lensing Source Catalogue to four tomographic bins and to estimate the redshift distributions in these bins. As the first application of these methods to data, we validate that the assumptions made apply to the DES Y3 weak lensing source galaxies and develop a full treatment of systematic uncertainties. Our method consists of combining information from three independent likelihood functions: Self-Organizing Map $p(z)$ (SOMPZ), a method for constraining redshifts from galaxy photometry; clustering redshifts (WZ), constraints on redshifts from cross-correlations of galaxy density functions; and shear ratios (SR), which provide constraints on redshifts from the ratios of the galaxy-shear correlation functions at small scales. Finally, we describe how these independent probes are combined to yield an ensemble of redshift distributions encapsulating our full uncertainty. We calibrate redshifts with combined effective uncertainties of $\sigma_{\langle z \rangle}\sim 0.01$ on the mean redshift in each tomographic bin., Comment: See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release. 30 pages, 18 figures
Published: 2020
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14. Dark Energy Survey Year 3 Results: Point-Spread Function Modeling

Author: Jarvis, M., Bernstein, G. M., Amon, A., Davis, C., Léget, P. F., Bechtol, K., Harrison, I., Gatti, M., Roodman, A., Chang, C., Chen, R., Choi, A., Desai, S., Drlica-Wagner, A., Gruen, D., Gruendl, R. A., Hernandez, A., MacCrann, N., Meyers, J., Navarro-Alsina, A., Pandey, S., Plazas, A. A., Secco, L. F., Sheldon, E., Troxel, M. A., Vorperian, S., Wei, K., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bhargava, S., Bridle, S. L., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Diehl, H. T., Doel, P., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., and Collaboration, DES
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We introduce a new software package for modeling the point-spread function (PSF) of astronomical images, called Piff (PSFs In the Full FOV), which we apply to the first three years (known as Y3) of the Dark Energy Survey (DES) data. We describe the relevant details about the algorithms used by Piff to model the PSF, including how the PSF model varies across the field of view (FOV). Diagnostic results show that the systematic errors from the PSF modeling are very small over the range of scales that are important for the DES Y3 weak lensing analysis. In particular, the systematic errors from the PSF modeling are significantly smaller than the corresponding results from the DES year one (Y1) analysis. We also briefly describe some planned improvements to Piff that we expect to further reduce the modeling errors in future analyses., Comment: 19 pages, accepted/published by MNRAS. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release
Published: 2020
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15. Dark Energy Survey Year 3 Results: Optimizing the Lens Sample in Combined Galaxy Clustering and Galaxy-Galaxy Lensing Analysis

Author: Porredon, A., Crocce, M., Fosalba, P., Elvin-Poole, J., Rosell, A. Carnero, Cawthon, R., Eifler, T. F., Fang, X., Ferrero, I., Krause, E., MacCrann, N., Weaverdyck, N., Abbott, T. M. C., Aguena, M., Allam, S., Amon, A., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Kind, M. Carrasco, Carretero, J., Castander, F. J., Choi, A., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Ferté, A., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jarvis, M., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Pandey, S., Paz-Chinchón, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate potential gains in cosmological constraints from the combination of galaxy clustering and galaxy-galaxy lensing by optimizing the lens galaxy sample selection using information from Dark Energy Survey (DES) Year 3 data and assuming the DES Year 1 Metacalibration sample for the sources. We explore easily reproducible selections based on magnitude cuts in $i$-band as a function of (photometric) redshift, $z_{\rm phot}$, and benchmark the potential gains against those using the well established redMaGiC sample. We focus on the balance between density and photometric redshift accuracy, while marginalizing over a realistic set of cosmological and systematic parameters. Our optimal selection, the MagLim sample, satisfies $i < 4 \, z_{\rm phot} + 18$ and has $\sim 30\%$ wider redshift distributions but $\sim 3.5$ times more galaxies than redMaGiC. Assuming a wCDM model and equivalent scale cuts to mitigate nonlinear effects, this leads to $40\%$ increase in the figure of merit for the pair combinations of $\Omega_m$, $w$, and $\sigma_8$, and gains of $16\%$ in $\sigma_8$, $10\%$ in $\Omega_m$, and $12\%$ in $w$. Similarly, in LCDM we find an improvement of $19\%$ and $27\%$ on $\sigma_8$ and $\Omega_m$, respectively. We also explore flux-limited samples with a flat magnitude cut finding that the optimal selection, $i < 22.2$, has $\sim 7$ times more galaxies and $\sim 20\%$ wider redshift distributions compared to MagLim, but slightly worse constraints. We show that our results are robust with respect to the assumed galaxy bias and photometric redshift uncertainties with only moderate further gains from increased number of tomographic bins or the inclusion of bin cross-correlations, except in the case of the flux-limited sample, for which these gains are more significant., Comment: 24 pages, 15 figures. See http://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release. Updated references
Published: 2020
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16. Dark Energy Survey Year 3 Results: Photometric Data Set for Cosmology

Author: Sevilla-Noarbe, I., Bechtol, K., Kind, M. Carrasco, Rosell, A. Carnero, Becker, M. R., Drlica-Wagner, A., Gruendl, R. A., Rykoff, E. S., Sheldon, E., Yanny, B., Alarcon, A., Allam, S., Amon, A., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Burke, D. L., Carretero, J., Choi, A., Diehl, H. T., Everett, S., Flaugher, B., Gaztanaga, E., Gschwend, J., Harrison, I., Hartley, W. G., Hoyle, B., Jarvis, M., Johnson, M. D., Kessler, R., Kron, R., Kuropatkin, N., Leistedt, B., Li, T. S., Menanteau, F., Morganson, E., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Pond, C., Rodriguez-Monroy, M., Allyn-Smith, J., Stringer, K. M., Troxel, M. A., Tucker, D. L., de Vicente, J., Wester, W., Zhang, Y., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bhargava, S., Bridle, S. L., Brooks, D., Brout, D., Castander, F. J., Cawthon, R., Chang, C., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. E., Davis, T. M., Desai, S., Dietrich, J. P., Doel, P., Eckert, K., Evrard, A. E., Ferrero, I., Fosalba, P., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huff, E. M., Huterer, D., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Mohr, J. J., Morgan, R., Neilsen, E., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wechsler, R. H., Weller, J., and Wilkinson, R. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We describe the Dark Energy Survey (DES) photometric data set assembled from the first three years of science operations to support DES Year 3 cosmology analyses, and provide usage notes aimed at the broad astrophysics community. Y3 Gold improves on previous releases from DES, Y1 Gold and Data Release 1 (DES DR1), presenting an expanded and curated data set that incorporates algorithmic developments in image detrending and processing, photometric calibration, and object classification. Y3 Gold comprises nearly 5000 square degrees of grizY imaging in the south Galactic cap, including nearly 390 million objects, with depth reaching S/N ~ 10 for extended objects up to $i_{AB}\sim 23.0$, and top-of-the-atmosphere photometric uniformity $< 3$ mmag. Compared to DR1, photometric residuals with respect to Gaia are reduced by $50\%$, and per-object chromatic corrections are introduced. Y3 Gold augments DES DR1 with simultaneous fits to multi-epoch photometry for more robust galaxy color measurements and corresponding photometric redshift estimates. Y3 Gold features improved morphological star-galaxy classification with efficiency $>98\%$ and purity $>99\%$ for galaxies with $19 < i_{AB} < 22.5$. Additionally, it includes per-object quality information, and accompanying maps of the footprint coverage, masked regions, imaging depth, survey conditions, and astrophysical foregrounds that are used to select the cosmology analysis samples. This paper will be complemented by online resources., Comment: see https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release
Published: 2020
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17. DES Y1 results: Splitting growth and geometry to test $\Lambda$CDM

Author: Muir, J., Baxter, E., Miranda, V., Doux, C., Ferté, A., Leonard, C. D., Huterer, D., Jain, B., Lemos, P., Raveri, M., Nadathur, S., Campos, A., Chen, A., Dodelson, S., Elvin-Poole, J., Lee, S., Secco, L. F., Troxel, M. A., Weaverdyck, N., Zuntz, J., Brout, D., Choi, A., Crocce, M., Davis, T. M., Gruen, D., Krause, E., Lidman, C., MacCrann, N., Möller, A., Prat, J., Ross, A. J., Sako, M., Samuroff, S., Sáchez, C., Scolnic, D., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We analyze Dark Energy Survey (DES) data to constrain a cosmological model where a subset of parameters -- focusing on $\Omega_m$ -- are split into versions associated with structure growth (e.g. $\Omega_m^{\rm grow}$) and expansion history (e.g. $\Omega_m^{\rm geo}$). Once the parameters have been specified for the $\Lambda$CDM cosmological model, which includes general relativity as a theory of gravity, it uniquely predicts the evolution of both geometry (distances) and the growth of structure over cosmic time. Any inconsistency between measurements of geometry and growth could therefore indicate a breakdown of that model. Our growth-geometry split approach therefore serves as both a (largely) model-independent test for beyond-$\Lambda$CDM physics, and as a means to characterize how DES observables provide cosmological information. We analyze the same multi-probe DES data as arXiv:1811.02375 : DES Year 1 (Y1) galaxy clustering and weak lensing, which are sensitive to both growth and geometry, as well as Y1 BAO and Y3 supernovae, which probe geometry. We additionally include external geometric information from BOSS DR12 BAO and a compressed Planck 2015 likelihood, and external growth information from BOSS DR12 RSD. We find no significant disagreement with $\Omega_m^{\rm grow}=\Omega_m^{\rm geo}$. When DES and external data are analyzed separately, degeneracies with neutrino mass and intrinsic alignments limit our ability to measure $\Omega_m^{\rm grow}$, but combining DES with external data allows us to constrain both growth and geometric quantities. We also consider a parameterization where we split both $\Omega_m$ and $w$, but find that even our most constraining data combination is unable to separately constrain $\Omega_m^{\rm grow}$ and $w^{\rm grow}$. Relative to $\Lambda$CDM, splitting growth and geometry weakens bounds on $\sigma_8$ but does not alter constraints on $h$., Comment: 35 pages, 18 figures. Updated to match published version
Published: 2020
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18. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations

Author: To, C., Krause, E., Rozo, E., Wu, H., Gruen, D., Wechsler, R. H., Eifler, T. F., Rykoff, E. S., Costanzi, M., Becker, M. R., Bernstein, G. M., Blazek, J., Bocquet, S., Bridle, S. L., Cawthon, R., Choi, A., Crocce, M., Davis, C., DeRose, J., Drlica-Wagner, A., Elvin-Poole, J., Fang, X., Farahi, A., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Hartley, W. G., Hoyle, B., Jarvis, M., MacCrann, N., McClintock, T., Miranda, V., Pereira, M. E. S., Park, Y., Porredon, A., Prat, J., Rau, M. M., Ross, A. J., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Troxel, M. A., Varga, T. N., Vielzeuf, P., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C., Conselice, C., da Costa, L. N., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Huterer, D., James, D. J., Jeltema, T., Kron, R., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Myles, J., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Weller, J., and Wester, W.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Combining multiple observational probes is a powerful technique to provide robust and precise constraints on cosmological parameters. In this letter, we present the first joint analysis of cluster abundances and auto/cross correlations of three cosmic tracer fields measured from the first year data of the Dark Energy Survey: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis of cluster abundances, three cluster cross-correlations, and auto correlations of galaxy density, we obtain $\Omega_{\rm{m}}=0.305^{+0.055}_{-0.038}$ and $\sigma_8=0.783^{+0.064}_{-0.054}$. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat $\nu\Lambda$CDM model. We thus combine cluster abundances and all two-point correlations from three cosmic tracer fields and find improved constraints on cosmological parameters as well as on the cluster observable--mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multi-probe analyses of upcoming wide imaging surveys., Comment: 14 pages, 7 figures, 2 tables; submitted to PRL; comments are welcome
Published: 2020
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19. $\mu_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses

Author: Pereira, M. E. S., Palmese, A., Varga, T. N., McClintock, T., Soares-Santos, M., Burgad, J., Annis, J., Farahi, A., Lin, H., Choi, A., DeRose, J., Esteves, J., Gatti, M., Gruen, D., Hartley, W. G., Hoyle, B., Jeltema, T., MacCrann, N., Roodman, A., Sánchez, C., Shin, T., von der Linden, A., Zuntz, J., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Wechsler, R. H., Weller, J., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the weak lensing mass calibration of the stellar mass based $\mu_{\star}$ 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 $\mu_{\star}$ at high redshifts, $z>0.33$. In a blinded analysis, we use $\sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 \leqslant z<0.65$ and $\mu_{\star}$ up to $\sim 5.5 \times 10^{13} M_{\odot}$, 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 NFW halo profile, halo triaxiality and projection effects. We use the inferred masses to estimate the joint mass--$\mu_{\star}$--$z$ 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 $G_z= -1.14 \pm 0.37$. We discuss the use of $\mu_{\star}$ as a complementary mass proxy to the well-studied richness $\lambda$ for: $i)$ exploring the regimes of low $z$, $\lambda<20$ and high $\lambda$, $z \sim 1$; $ii)$ testing systematics such as projection effects for applications in cluster cosmology., Comment: 20 pages, 10 figures, submitted to MNRAS
Published: 2020
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20. The impact of spectroscopic incompleteness in direct calibration of redshift distributions for weak lensing surveys

Author: Hartley, W. G., Chang, C., Samani, S., Rosell, A. Carnero, Davis, T. M., Hoyle, B., Gruen, D., Asorey, J., Gschwend, J., Lidman, C., Kuehn, K., King, A., Rau, M. M., Wechsler, R. H., DeRose, J., Hinton, S. R., Whiteway, L., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Bertin, E., Bridle, S. L., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Kent, S., Krause, E., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Chinchon, F. Paz, 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., Tarle, G., Troxel, M. A., Tucker, D. L., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Obtaining accurate distributions of galaxy redshifts is a critical aspect of weak lensing cosmology experiments. One of the methods used to estimate and validate redshift distributions is apply weights to a spectroscopic sample so that their weighted photometry distribution matches the target sample. In this work we estimate the \textit{selection bias} in redshift that is introduced in this procedure. We do so by simulating the process of assembling a spectroscopic sample (including observer-assigned confidence flags) and highlight the impacts of spectroscopic target selection and redshift failures. We use the first year (Y1) weak lensing analysis in DES as an example data set but the implications generalise to all similar weak lensing surveys. We find that using colour cuts that are not available to the weak lensing galaxies can introduce biases of $\Delta~z\sim0.015$ in the weighted mean redshift of different redshift intervals. To assess the impact of incompleteness in spectroscopic samples, we select only objects with high observer-defined confidence flags and compare the weighted mean redshift with the true mean. We find that the mean redshift of the DES Y1 weak lensing sample is typically biased at the $\Delta~z=0.005-0.05$ level after the weighting is applied. The bias we uncover can have either sign, depending on the samples and redshift interval considered. For the highest redshift bin, the bias is larger than the uncertainties in the other DES Y1 redshift calibration methods, justifying the decision of not using this method for the redshift estimations. We discuss several methods to mitigate this bias., Comment: 20 pages, 12 figures. Our main result is shown in Fig. 6. MNRAS, Volume 496, Issue 4, pp.4769-4786. Catalogue data used in this publication can be found here: http://star.ucl.ac.uk/~whartley/simspec/
Published: 2020
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21. Detection of cross-correlation between gravitational lensing and gamma rays

Author: Ammazzalorso, S., Gruen, D., Regis, M., Camera, S., Ando, S., Fornengo, N., Bechtol, K., Bridle, S. L., Choi, A., Eifler, T. F., Gatti, M., MacCrann, N., Omori, Y., Samuroff, S., Sheldon, E., Troxel, M. A., Zuntz, J., Kind, M. Carrasco, Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Everett, S., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kent, S., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, C., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: In recent years, many gamma-ray sources have been identified, yet the unresolved component hosts valuable information on the faintest emission. In order to extract it, a cross-correlation with gravitational tracers of matter in the Universe has been shown to be a promising tool. We report here the first identification of a cross-correlation signal between gamma rays and the distribution of mass in the Universe probed by weak gravitational lensing. We use the Dark Energy Survey Y1 weak lensing catalogue and the Fermi Large Area Telescope 9-year gamma-ray data, obtaining a signal-to-noise ratio of 5.3. The signal is mostly localised at small angular scales and high gamma-ray energies, with a hint of correlation at extended separation. Blazar emission is likely the origin of the small-scale effect. We investigate implications of the large-scale component in terms of astrophysical sources and particle dark matter emission., Comment: 24 pages, 10 figures, v2: text re-arranged, typos corrected, slight improvement in the detection significance, matching version accepted for publication in PRL
Published: 2019
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22. Monte Carlo Control Loops for cosmic shear cosmology with DES Year 1

Author: Kacprzak, T., Herbel, J., Nicola, A., Sgier, R., Tarsitano, F., Bruderer, C., Amara, A., Refregier, A., Bridle, S. L., Drlica-Wagner, A., Gruen, D., Hartley, W. G., Hoyle, B., Secco, L. F., Zuntz, J., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., and Weller, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Weak lensing by large-scale structure is a powerful probe of cosmology and of the dark universe. This cosmic shear technique relies on the accurate measurement of the shapes and redshifts of background galaxies and requires precise control of systematic errors. The Monte Carlo Control Loops (MCCL) is a forward modelling method designed to tackle this problem. It relies on the Ultra Fast Image Generator (UFig) to produce simulated images tuned to match the target data statistically, followed by calibrations and tolerance loops. We present the first end-to-end application of this method, on the Dark Energy Survey (DES) Year 1 wide field imaging data. We simultaneously measure the shear power spectrum $C_{\ell}$ and the redshift distribution $n(z)$ of the background galaxy sample. The method includes maps of the systematic sources, Point Spread Function (PSF), an Approximate Bayesian Computation (ABC) inference of the simulation model parameters, a shear calibration scheme, and the fast estimation of the covariance matrix. We find a close statistical agreement between the simulations and the DES Y1 data using an array of diagnostics. In a non-tomographic setting, we derive a set of $C_\ell$ and $n(z)$ curves that encode the cosmic shear measurement, as well as the systematic uncertainty. Following a blinding scheme, we measure the combination of $\Omega_m$, $\sigma_8$, and intrinsic alignment amplitude $A_{\rm{IA}}$, defined as $S_8D_{\rm{IA}} = \sigma_8(\Omega_m/0.3)^{0.5}D_{\rm{IA}}$, where $D_{\rm{IA}}=1-0.11(A_{\rm{IA}}-1)$. We find $S_8D_{\rm{IA}}=0.895^{+0.054}_{-0.039}$, where systematics are at the level of roughly 60\% of the statistical errors. We discuss these results in the context of earlier cosmic shear analyses of the DES Y1 data. Our findings indicate that this method and its fast runtime offer good prospects for cosmic shear measurements with future wide-field surveys., Comment: 31 pages, 15 figures, 2 tables
Published: 2019
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23. Dark Energy Survey Year 1 Results: Wide field mass maps via forward fitting in harmonic space

Author: Mawdsley, B., Bacon, D., Chang, C., Melchior, P., Rozo, E., Seitz, S., Jeffrey, N., Gatti, M., Gaztanaga, E., Gruen, D., Hartley, W. G., Hoyle, B., Samuroff, S., Sheldon, E., Troxel, M. A., Zuntz, J., Abbott, T. M. C., Annis, J., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Car- rasco, Carretero, J., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Vikram, V., and Walker, A. R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present new wide-field weak lensing mass maps for the Year 1 Dark Energy Survey data, generated via a forward fitting approach. This method of producing maps does not impose any prior constraints on the mass distribution to be reconstructed. The technique is found to improve the map reconstruction on the edges of the field compared to the conventional Kaiser-Squires method, which applies a direct inversion on the data; our approach is in good agreement with the previous direct approach in the central regions of the footprint. The mapping technique is assessed and verified with tests on simulations; together with the Kaiser-Squires method, the technique is then applied to data from the Dark Energy Survey Year 1 data and the differences between the two methods are compared. We also produce the first DES measurements of the convergence Minkowski functionals and compare them to those measured in simulations., Comment: 19 pages, 16 figures. Submitted to MNRAS
Published: 2019
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24. Phenotypic redshifts with self-organizing maps: A novel method to characterize redshift distributions of source galaxies for weak lensing

Author: Buchs, R., Davis, C., Gruen, D., DeRose, J., Alarcon, A., Bernstein, G. M., Sánchez, C., Myles, J., Roodman, A., Allen, S., Amon, A., Choi, A., Masters, D. C., Miquel, R., Troxel, M. A., Wechsler, R. H., Abbott, T. M. C., Annis, J., Avila, S., Bechtol, K., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., D'Andrea, C. B., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruend, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Ogando, R. L. C., Plazas, A. A., Rykoff, E. S., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Vikram, V.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Wide-field imaging surveys such as the Dark Energy Survey (DES) rely on coarse measurements of spectral energy distributions in a few filters to estimate the redshift distribution of source galaxies. In this regime, sample variance, shot noise, and selection effects limit the attainable accuracy of redshift calibration and thus of cosmological constraints. We present a new method to combine wide-field, few-filter measurements with catalogs from deep fields with additional filters and sufficiently low photometric noise to break degeneracies in photometric redshifts. The multi-band deep field is used as an intermediary between wide-field observations and accurate redshifts, greatly reducing sample variance, shot noise, and selection effects. Our implementation of the method uses self-organizing maps to group galaxies into phenotypes based on their observed fluxes, and is tested using a mock DES catalog created from N-body simulations. It yields a typical uncertainty on the mean redshift in each of five tomographic bins for an idealized simulation of the DES Year 3 weak-lensing tomographic analysis of $\sigma_{\Delta z} = 0.007$, which is a 60% improvement compared to the Year 1 analysis. Although the implementation of the method is tailored to DES, its formalism can be applied to other large photometric surveys with a similar observing strategy., Comment: 24 pages, 11 figures; matches version accepted to MNRAS
Published: 2019
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25. Dark Energy Survey Year 1 Results: Constraints on Intrinsic Alignments and their Colour Dependence from Galaxy Clustering and Weak Lensing

Author: Samuroff, S., Blazek, J., Troxel, M. A., MacCrann, N., Krause, E., Leonard, C. D., Prat, J., Gruen, D., Dodelson, S., Eifler, T. F., Gatti, M., Hartley, W. G., Hoyle, B., Larsen, P., Zuntz, J., Abbott, T. M. C., Allam, S., Annis, J., Bernstein, G. M., Bertin, E., Bridle, S. L., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DePoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., and Vikram, V.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a joint analysis of intrinsic alignments and cosmology using tomographic weak lensing, galaxy clustering and galaxy-galaxy lensing measurements from Year 1 (Y1) of the Dark Energy Survey. We define early- and late-type subsamples, which are found to pass a series of systematics tests, including for spurious photometric redshift error and point spread function correlations. We analyse these split data alongside the fiducial mixed Y1 sample using a range of intrinsic alignment models. In a fiducial Nonlinear Alignment Model (NLA) analysis, assuming a flat \lcdm~cosmology, we find a significant difference in intrinsic alignment amplitude, with early-type galaxies favouring $A_\mathrm{IA} = 2.38^{+0.32}_{-0.31}$ and late-type galaxies consistent with no intrinsic alignments at $0.05^{+0.10}_{-0.09}$. We find weak evidence of a diminishing alignment amplitude at higher redshifts in the early-type sample. The analysis is repeated using a number of extended model spaces, including a physically motivated model that includes both tidal torquing and tidal alignment mechanisms. In multiprobe likelihood chains in which cosmology, intrinsic alignments in both galaxy samples and all other relevant systematics are varied simultaneously, we find the tidal alignment and tidal torquing parts of the intrinsic alignment signal have amplitudes $A_1 = 2.66 ^{+0.67}_{-0.66}$, $A_2=-2.94^{+1.94}_{-1.83}$, respectively, for early-type galaxies and $A_1 = 0.62 ^{+0.41}_{-0.41}$, $A_2 = -2.26^{+1.30}_{-1.16}$ for late-type galaxies. In the full (mixed) Y1 sample the best constraints are $A_1 = 0.70 ^{+0.41}_{-0.38}$, $A_2 = -1.36 ^{+1.08}_{-1.41}$. For all galaxy splits and IA models considered, we report cosmological parameter constraints that are consistent with the results of Troxel et al. (2017) and Dark Energy Survey Collaboration (2017)., Comment: 31 pages, 23 figures; accepted by MNRAS
Published: 2018
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26. Cosmological Constraints from Multiple Probes in the Dark Energy Survey

Author: DES Collaboration, Abbott, T. M. C., Alarcon, A., Allam, S., Andersen, P., Andrade-Oliveira, F., Annis, J., Asorey, J., Avelino, A., Avila, S., Bacon, D., Banik, N., Bassett, B. A., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Burke, D. L., Calcino, J., Camacho, H., Campos, A., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Challis, P., Chan, K. C., Chang, C., Childress, M., Clocchiatti, A., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Davis, T. M., De Vicente, J., DePoy, D. L., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Estrada, J., Evrard, A. E., Fernandez, E., Filippenko, A. V., Flaugher, B., Foley, R. J., Fosalba, P., Frieman, J., Galbany, L., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoormann, J. K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Kasai, E., Kent, S., Kessler, R., Kim, A. G., Kirshner, R. P., Kokron, N., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lasker, J., Lemos, P., Lewis, G. F., Li, T. S., Lidman, C., Lima, M., Lin, H., Macaulay, E., MacCrann, N., Maia, M. A. G., Mandel, K. S., March, M., Marriner, J., Marshall, J. L., Martini, P., McMahon, R. G., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morganson, E., Muir, J., Möller, A., Neilsen, E., Nichol, R. C., Nord, B., Ogando, R. L. C., Palmese, A., Pan, Y. -C., Peiris, H. V., Percival, W. J., Plazas, A. A., Porredon, A., Prat, J., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sharp, R., Sheldon, E., Smith, M., Soares-Santos, M., Sobreira, F., Sommer, N. E., Swann, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, B. E., Uddin, S. A., Vielzeuf, P., Walker, A. R., Wang, M., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Zhang, B., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The combination of multiple observational probes has long been advocated as a powerful technique to constrain cosmological parameters, in particular dark energy. The Dark Energy Survey has measured 207 spectroscopically--confirmed Type Ia supernova lightcurves; the baryon acoustic oscillation feature; weak gravitational lensing; and galaxy clustering. Here we present combined results from these probes, deriving constraints on the equation of state, $w$, of dark energy and its energy density in the Universe. Independently of other experiments, such as those that measure the cosmic microwave background, the probes from this single photometric survey rule out a Universe with no dark energy, finding $w=-0.80^{+0.09}_{-0.11}$. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of $\Omega_b=0.069^{+0.009}_{-0.012}$ that is independent of early Universe measurements. These results demonstrate the potential power of large multi-probe photometric surveys and pave the way for order of magnitude advances in our constraints on properties of dark energy and cosmology over the next decade., Comment: 8 pages, 2 figures; v3 matches version accepted by PRL
Published: 2018
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27. Dark Energy Survey Year 1 Results: Constraints on Extended Cosmological Models from Galaxy Clustering and Weak Lensing

Author: DES Collaboration, Abbott, T. M. C., Abdalla, F. B., Avila, S., Banerji, M., Baxter, E., Bechtol, K., Becker, M. R., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Evrard, A. E., Fernandez, E., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Lemos, P., Leonard, C. D., Li, T. S., Liddle, A. R., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Nichol, R. C., Nord, B., Ogando, R. L. C., Plazas, A. A., Raveri, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Samuroff, S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Vikram, V., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology
Abstract: We present constraints on extensions of the minimal cosmological models dominated by dark matter and dark energy, $\Lambda$CDM and $w$CDM, by using a combined analysis of galaxy clustering and weak gravitational lensing from the first-year data of the Dark Energy Survey (DES Y1) in combination with external data. We consider four extensions of the minimal dark energy-dominated scenarios: 1) nonzero curvature $\Omega_k$, 2) number of relativistic species $N_{\rm eff}$ different from the standard value of 3.046, 3) time-varying equation-of-state of dark energy described by the parameters $w_0$ and $w_a$ (alternatively quoted by the values at the pivot redshift, $w_p$, and $w_a$), and 4) modified gravity described by the parameters $\mu_0$ and $\Sigma_0$ that modify the metric potentials. We also consider external information from Planck CMB measurements; BAO measurements from SDSS, 6dF, and BOSS; RSD measurements from BOSS; and SNIa information from the Pantheon compilation. Constraints on curvature and the number of relativistic species are dominated by the external data; when these are combined with DES Y1, we find $\Omega_k=0.0020^{+0.0037}_{-0.0032}$ at the 68% confidence level, and $N_{\rm eff}<3.28\, (3.55)$ at 68% (95%) confidence. For the time-varying equation-of-state, we find the pivot value $(w_p, w_a)=(-0.91^{+0.19}_{-0.23}, -0.57^{+0.93}_{-1.11})$ at pivot redshift $z_p=0.27$ from DES alone, and $(w_p, w_a)=(-1.01^{+0.04}_{-0.04}, -0.28^{+0.37}_{-0.48})$ at $z_p=0.20$ from DES Y1 combined with external data; in either case we find no evidence for the temporal variation of the equation of state. For modified gravity, we find the present-day value of the relevant parameters to be $\Sigma_0= 0.43^{+0.28}_{-0.29}$ from DES Y1 alone, and $(\Sigma_0, \mu_0)=(0.06^{+0.08}_{-0.07}, -0.11^{+0.42}_{-0.46})$ from DES Y1 combined with external data, consistent with predictions from GR., Comment: 22 pages, 7 figures, matches the published version
Published: 2018
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28. Dark Energy Survey Year 1 Results: Joint Analysis of Galaxy Clustering, Galaxy Lensing, and CMB Lensing Two-point Functions

Author: Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Allam, S., Annis, J., Avila, S., Aylor, K., Banerji, M., Banik, N., Baxter, E. J., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Blazek, J., Bleem, L., Bleem, L. E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chang, C. L., Cho, H-M., Choi, A., Chown, R., Crawford, T. M., Crites, A. T., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., de Haan, T., DeRose, J., Desai, S., De Vicente, J., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Everett, W. B., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Knox, L., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lee, A. T., Leitch, E. M., Li, T. S., Lima, M., Lin, H., Luong-Van, D., MacCrann, N., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Muir, J., Natoli, T., Nicola, A., Nord, B., Omori, Y., Padin, S., Pandey, S., Plazas, A. A., Porredon, A., Prat, J., Pryke, C., Rau, M. M., Reichardt, C. L., Rollins, R. P., Romer, A. K., Roodman, A., Ross, A. J., Rozo, E., Ruhl, J. E., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vanderlinde, K., Vieira, J. D., Vielzeuf, P., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Williamson, R., Wu, W. L. K., Yanny, B., Zahn, O., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a joint analysis of the auto and cross-correlations between three cosmic fields: the galaxy density field, the galaxy weak lensing shear field, and the cosmic microwave background (CMB) weak lensing convergence field. These three fields are measured using roughly 1300 sq. deg. of overlapping optical imaging data from first year observations of the Dark Energy Survey and millimeter-wave observations of the CMB from both the South Pole Telescope Sunyaev-Zel'dovich survey and Planck. We present cosmological constraints from the joint analysis of the two-point correlation functions between galaxy density and galaxy shear with CMB lensing. We test for consistency between these measurements and the DES-only two-point function measurements, finding no evidence for inconsistency in the context of flat $\Lambda$CDM cosmological models. Performing a joint analysis of five of the possible correlation functions between these fields (excluding only the CMB lensing autospectrum) yields $S_{8}\equiv \sigma_8\sqrt{\Omega_{\rm m}/0.3} = 0.782^{+0.019}_{-0.025}$ and $\Omega_{\rm m}=0.260^{+0.029}_{-0.019}$. We test for consistency between these five correlation function measurements and the Planck-only measurement of the CMB lensing autospectrum, again finding no evidence for inconsistency in the context of flat $\Lambda$CDM models. Combining constraints from all six two-point functions yields $S_{8}=0.776^{+0.014}_{-0.021}$ and $\Omega_{\rm m}= 0.271^{+0.022}_{-0.016}$. These results provide a powerful test and confirmation of the results from the first year DES joint-probes analysis., Comment: 20 pages, 7 figures
Published: 2018
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29. Dark Energy Survey Year 1 Results: tomographic cross-correlations between DES galaxies and CMB lensing from SPT+Planck

Author: Omori, Y., Giannantonio, T., Porredon, A., Baxter, E., Chang, C., Crocce, M., Fosalba, P., Alarcon, A., Banik, N., Blazek, J., Bleem, L. E., Bridle, S. L., Cawthon, R., Choi, A., Chown, R., Crawford, T., Dodelson, S., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Friedrich, O., Gruen, D., Holder, G. P., Huterer, D., Jain, B., Jarvis, M., Kirk, D., Kokron, N., Krause, E., MacCrann, N., Muir, J., Prat, J., Reichardt, C. L., Ross, A. J., Rozo, E., Rykoff, E. S., Sánchez, C., Secco, L. F., Simard, G., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Avila, S., Aylor, K., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Cho, H-M., Crites, A. T., Cunha, C. E., da Costa, L. N., de Haan, T., Davis, C., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Everett, W. B., Doel, P., Estrada, J., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., George, E. M., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lee, A. T., Leitch, E. M., Lima, M., Luong-Van, D., Manzotti, A., Marrone, D. P., Marshall, J. L., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miller, C. J., Miquel, R., Mocanu, L. M., Mohr, J. J., Natoli, T., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Sanchez, E., Scarpine, V., Schaffer, K. K., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Vanderlinde, K., Vieira, J. D., Walker, A. R., Wu, W. L. K., and Zahn, O.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the cross-correlation between redMaGiC galaxies selected from the Dark Energy Survey (DES) Year-1 data and gravitational lensing of the cosmic microwave background (CMB) reconstructed from South Pole Telescope (SPT) and Planck data over 1289 sq. deg. When combining measurements across multiple galaxy redshift bins spanning the redshift range of $0.15
Published: 2018
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30. Dark Energy Survey Year 1 Results: Cross-correlation between DES Y1 galaxy weak lensing and SPT+Planck CMB weak lensing

Author: Omori, Y., Baxter, E., Chang, C., Kirk, D., Alarcon, A., Bernstein, G. M., Bleem, L. E., Cawthon, R., Choi, A., Chown, R., Crawford, T. M., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T. F., Fosalba, P., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Gruen, D., Hartley, W. G., Holder, G. P., Hoyle, B., Huterer, D., Jain, B., Jarvis, M., Krause, E., MacCrann, N., Miquel, R., Prat, J., Rau, M. M., Reichardt, C. L., Rozo, E., Samuroff, S., Sánchez, C., Secco, L. F., Sheldon, E., Simard, G., Troxel, M. A., Vielzeuf, P., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Aylor, K., Benson, B. A., Bertin, E., Bridle, S. L., Brooks, D., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Cho, H-M., Crites, A. T., Crocce, M., Cunha, C. E., da Costa, L. N., de Haan, T., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Everett, W. B., Fernandez, E., Flaugher, B., Frieman, J., García-Bellido, J., George, E. M., Gruendl, R. A., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hollowood, D. L., Honscheid, K., Holzapfel, W. L., Hou, Z., Hrubes, J. D., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Lee, A. T., Leitch, E. M., Luong-Van, D., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Mocanu, L. M., Mohr, J. J., Natoli, T., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Sanchez, E., Scarpine, V., Schaffer, K. K., Schindler, R., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J. D., Vikram, V., Walker, A. R., Weller, J., Williamson, R., Wu, W. L. K., and Zahn, O.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one (Y1) data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg$^{2}$. With the combined measurements from four source galaxy redshift bins, we reject the hypothesis of no lensing with a significance of $10.8\sigma$. When employing angular scale cuts, this significance is reduced to $6.8\sigma$, which remains the highest signal-to-noise measurement of its kind to date. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial $\Lambda$CDM model, finding $A = 0.99 \pm 0.17$. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the $\Lambda$CDM model, we obtain the marginalized constraints of $\Omega_{\rm m}=0.261^{+0.070}_{-0.051}$ and $S_{8}\equiv \sigma_{8}\sqrt{\Omega_{\rm m}/0.3} = 0.660^{+0.085}_{-0.100}$. These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT and Planck data., Comment: 15 pages, 6 figures
Published: 2018
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31. Dark Energy Survey Year 1 Results: Measurement of the Galaxy Angular Power Spectrum

Author: Camacho, H., Kokron, N., Andrade-Oliveira, F., Rosenfeld, R., Lima, M., Lacasa, F., Sobreira, F., da Costa, L. N., Avila, S., Chan, K. C., Crocce, M., Ross, A. J., Troja, A., García-Bellido, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bernstein, R. A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Cunha, C. E., D'Andrea, C. B., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Estrada, J., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Krause, E., Kuehn, K., Kuropatkin, N., Lin, H., Marshall, J. L., Miquel, R., Percival, W. J., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use data from the first-year (Y1) observations of the DES collaboration to measure the galaxy angular power spectrum (APS), and search for its BAO feature using a template-fitting method. We test our methodology in a sample of 1800 DES Y1-like mock catalogs. The APS is measured with the pseudo-$C_\ell$ method, using pixelized maps constructed from the mock catalogs and the DES mask. The covariance matrix of the $C_\ell$'s in these tests are also obtained from the mock catalogs. We use templates to model the measured spectra and estimate template parameters firstly from the $C_\ell$'s of the mocks using two different methods, a maximum likelihood estimator and a MCMC, finding consistent results with a good reduced $\chi^2$. Robustness tests are performed to estimate the impact of different choices of settings used in our analysis. After these tests on mocks, we apply our method to a galaxy sample constructed from DES Y1 data specifically for LSS studies. This catalog comprises galaxies within an effective area of 1318 deg$^2$ and $0.6
Published: 2018
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32. Dark Energy Survey Year 1 Results: Weak Lensing Mass Calibration of redMaPPer Galaxy Clusters

Author: McClintock, T., Varga, T. N., Gruen, D., Rozo, E., Rykoff, E. S., Shin, T., Melchior, P., DeRose, J., Seitz, S., Dietrich, J. P., Sheldon, E., Zhang, Y., von der Linden, A., Jeltema, T., Mantz, A., Romer, A. K., Allen, S., Becker, M. R., Bermeo, A., Bhargava, S., Costanzi, M., Everett, S., Farahi, A., Hamaus, N., Hartley, W. G., Hollowood, D. L., Hoyle, B., Israel, H., Li, P., MacCrann, N., Morris, G., Palmese, A., Plazas, A. A., Pollina, G., Rau, M. M., Simet, M., Soares-Santos, M., Troxel, M. A., Cervantes, C. Vergara, Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Doel, P., Drlica-Wagner, A., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kirk, D., Krause, E., Kuehn, K., Lahav, O., Li, T. S., Lima, M., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Nord, B., Ogando, R. L. C., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We constrain the mass--richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing. We split clusters into $4\times3$ bins of richness $\lambda$ and redshift $z$ for $\lambda\geq20$ and $0.2 \leq z \leq 0.65$ and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as $\langle M_{\rm 200m}|\lambda,z\rangle = M_0 (\lambda/40)^F ((1+z)/1.35)^G$, we constrain the normalization of the scaling relation at the 5.0 per cent level as $M_0 = [3.081 \pm 0.075 ({\rm stat}) \pm 0.133 ({\rm sys})] \cdot 10^{14}\ {\rm M}_\odot$ at $\lambda=40$ and $z=0.35$. The richness scaling index is constrained to be $F=1.356 \pm 0.051\ ({\rm stat})\pm 0.008\ ({\rm sys})$ and the redshift scaling index $G=-0.30\pm 0.30\ ({\rm stat})\pm 0.06\ ({\rm sys})$. These are the tightest measurements of the normalization and richness scaling index made to date. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentering, cluster member dilution of the source sample, systematic uncertainties in the modeling of the halo--mass correlation function, halo triaxiality, and projection effects. We discuss prospects for reducing this systematic error budget, which dominates the uncertainty on $M_0$. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid and WFIRST., Comment: 28 pages, 15 figures; matches MNRAS referee response version
Published: 2018
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33. Weak Lensing Analysis of SPT selected Galaxy Clusters using Dark Energy Survey Science Verification Data

Author: Stern, C., Dietrich, J. P., Bocquet, S., Applegate, D., Mohr, J. J., Bridle, S. L., Kind, M. Carrasco, Gruen, D., Jarvis, M., Kacprzak, T., Saro, A., Sheldon, E., Troxel, M. A., Zuntz, J., Benson, B. A., Capasso, R., Chiu, I., Desai, S., Rapetti, D., Reichardt, C. L., Saliwanchik, B., Schrabback, T., Gupta, N., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carretero, J., Castander, F. J., D'Andrea, C. B., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Doel, P., Estrada, J., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D., Jeltema, T., Kirk, D., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Melchior, P., Menanteau, F., Miquel, R., Plazas, A. A., Romer, A. K., Sanchez, E., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Walker, A. R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present weak lensing (WL) mass constraints for a sample of massive galaxy clusters detected by the South Pole Telescope (SPT) via the Sunyaev-Zeldovich effect (SZE). We use $griz$ imaging data obtained from the Science Verification (SV) phase of the Dark Energy Survey (DES) to fit the WL shear signal of 33 clusters in the redshift range $0.25 \le z \le 0.8$ with NFW profiles and to constrain a four-parameter SPT mass-observable relation. To account for biases in WL masses, we introduce a WL mass to true mass scaling relation described by a mean bias and an intrinsic, log-normal scatter. We allow for correlated scatter within the WL and SZE mass-observable relations and use simulations to constrain priors on nuisance parameters related to bias and scatter from WL. We constrain the normalization of the $\zeta-M_{500}$ relation, $A_\mathrm{SZ}=12.0_{-6.7}^{+2.6}$ when using a prior on the mass slope $B_\mathrm{SZ}$ from the latest SPT cluster cosmology analysis. Without this prior, we recover $A_\mathrm{SZ}=10.8_{-5.2}^{+2.3}$ and $B_\mathrm{SZ}=1.30_{-0.44}^{+0.22}$. Results in both cases imply lower cluster masses than measured in previous work with and without WL, although the uncertainties are large. The WL derived value of $B_\mathrm{SZ}$ is $\approx 20\%$ lower than the value preferred by the most recent SPT cluster cosmology analysis. The method demonstrated in this work is designed to constrain cluster masses and cosmological parameters simultaneously and will form the basis for subsequent studies that employ the full SPT cluster sample together with the DES data., Comment: Revised version in response to referee report
Published: 2018
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34. A gravitational-wave standard siren measurement of the Hubble constant

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, A. K. W., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colla, A., Collette, C. G., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R. T., De Rossi, C., DeSalvo, R., de Varona, O., Devenson, J., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Álvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C. -J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. 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B., Bechtol, K., Benoit-Lévy, A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Estrada, J., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gutierrez, G., Hartley, W. G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Zhang, Y., Haislip, J. B., Kouprianov, V. V., Reichart, D. E., Tartaglia, L., Sand, D. J., Valenti, S., Yang, S., Arcavi, Iair, Hosseinzadeh, Griffin, Howell, D. Andrew, McCully, Curtis, Poznanski, Dovi, Vasylyev, Sergiy, Tanvir, N. R., Levan, A. J., Hjorth, J., Cano, Z., Copperwheat, C., de Ugarte-Postigo, A., Evans, P. A., Fynbo, J. P. U., González-Fernández, C., Greiner, J., Irwin, M., Lyman, J., Mandel, I., McMahon, R., Milvang-Jensen, B., O'Brien, P., Osborne, J. P., Perley, D. A., Pian, E., Palazzi, E., Rol, E., Rosetti, S., Rosswog, S., Rowlinson, A., Schulze, S., Steeghs, D. T. H., Thöne, C. C., Ulaczyk, K., Watson, D., Wiersema, K., Lipunov, V. M., Gorbovskoy, E., Kornilov, V. G., Tyurina, N ., Balanutsa, P., Vlasenko, D., Gorbunov, I., Podesta, R., Levato, H., Saffe, C., Buckley, D. A. H., Budnev, N. M., Gress, O., Yurkov, V., Rebolo, R., and Serra-Ricart, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The detection of GW170817 in both gravitational waves and electromagnetic waves heralds the age of gravitational-wave multi-messenger astronomy. On 17 August 2017 the Advanced LIGO and Virgo detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than 2 seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source. This sky region was subsequently observed by optical astronomy facilities, resulting in the identification of an optical transient signal within $\sim 10$ arcsec of the galaxy NGC 4993. These multi-messenger observations allow us to use GW170817 as a standard siren, the gravitational-wave analog of an astronomical standard candle, to measure the Hubble constant. This quantity, which represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Our measurement combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using electromagnetic data. This approach does not require any form of cosmic "distance ladder;" the gravitational wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be $70.0^{+12.0}_{-8.0} \, \mathrm{km} \, \mathrm{s}^{-1} \, \mathrm{Mpc}^{-1}$ (maximum a posteriori and 68% credible interval). This is consistent with existing measurements, while being completely independent of them. Additional standard-siren measurements from future gravitational-wave sources will provide precision constraints of this important cosmological parameter., Comment: 26 pages, 5 figures, Nature in press. For more information see https://dcc.ligo.org/LIGO-P1700296/public
Published: 2017
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35. Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey Data II: Hierarchical Bayesian Modeling of the Red-Sequence Galaxy Luminosity Function

Author: Zhang, Y., Miller, C. J., Rooney, P., Bermeo, A., Romer, A. K., cervantes, C. Vergara, 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., Liddle, A. R., Mann, R. G., Mehrtens, N., Mayers, J., Nichol, R. C., Sahlen, M., Stott, J., Viana, P. T. P., Wechsler, R. H., Abbott, T., Abdalla, F. B., Allam, S., Benoit-levy, A., Brooks, D., Buckley-geer, E., Burke, D. L., rosell, A. Carnero, kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., Dandrea, C. B., Da costa, L. N., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Flaugher, B., Fosalba, P., Garcia-bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Schubnell, M., Sevilla-noarbe, I., Smith, M., Soares-santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Walker, A. R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Using $\sim 100$ 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 luminosity function simultaneously in redshift ($0.1
Published: 2017

36. Density split statistics: Cosmological constraints from counts and lensing in cells in DES Y1 and SDSS data

Author: Gruen, D., Friedrich, O., Krause, E., DeRose, J., Cawthon, R., Davis, C., Elvin-Poole, J., Rykoff, E. S., Wechsler, R. H., Alarcon, A., Bernstein, G. M., Blazek, J., Chang, C., Clampitt, J., Crocce, M., De Vicente, J., Gatti, M., Gill, M. S. S., Hartley, W. G., Hilbert, S., Hoyle, B., Jain, B., Jarvis, M., Lahav, O., MacCrann, N., McClintock, T., Prat, J., Rollins, R. P., Ross, A. J., Rozo, E., Samuroff, S., Sánchez, C., Sheldon, E., Troxel, M. A., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Walker, A. R., Weller, J., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We derive cosmological constraints from the probability distribution function (PDF) of evolved large-scale matter density fluctuations. We do this by splitting lines of sight by density based on their count of tracer galaxies, and by measuring both gravitational shear around and counts-in-cells in overdense and underdense lines of sight, in Dark Energy Survey (DES) First Year and Sloan Digital Sky Survey (SDSS) data. Our analysis uses a perturbation theory model (see companion paper Friedrich at al.) and is validated using N-body simulation realizations and log-normal mocks. It allows us to constrain cosmology, bias and stochasticity of galaxies w.r.t. matter density and, in addition, the skewness of the matter density field. From a Bayesian model comparison, we find that the data weakly prefer a connection of galaxies and matter that is stochastic beyond Poisson fluctuations on <=20 arcmin angular smoothing scale. The two stochasticity models we fit yield DES constraints on the matter density $\Omega_m=0.26^{+0.04}_{-0.03}$ and $\Omega_m=0.28^{+0.05}_{-0.04}$ that are consistent with each other. These values also agree with the DES analysis of galaxy and shear two-point functions (3x2pt) that only uses second moments of the PDF. Constraints on $\sigma_8$ are model dependent ($\sigma_8=0.97^{+0.07}_{-0.06}$ and $0.80^{+0.06}_{-0.07}$ for the two stochasticity models), but consistent with each other and with the 3x2pt results if stochasticity is at the low end of the posterior range. As an additional test of gravity, counts and lensing in cells allow to compare the skewness $S_3$ of the matter density PDF to its LCDM prediction. We find no evidence of excess skewness in any model or data set, with better than 25 per cent relative precision in the skewness estimate from DES alone., Comment: 33 pages, 22 figures; matches published version
Published: 2017
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37. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cosmic Shear

Author: Troxel, M. A., MacCrann, N., Zuntz, J., Eifler, T. F., Krause, E., Dodelson, S., Gruen, D., Blazek, J., Friedrich, O., Samuroff, S., Prat, J., Secco, L. F., Davis, C., Ferté, A., DeRose, J., Alarcon, A., Amara, A., Baxter, E., Becker, M. R., Bernstein, G. M., Bridle, S. L., Cawthon, R., Chang, C., Choi, A., De Vicente, J., Drlica-Wagner, A., Elvin-Poole, J., Frieman, J., Gatti, M., Hartley, W. G., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Kacprzak, T., Kirk, D., Kokron, N., Krawiec, C., Lahav, O., Liddle, A. R., Peacock, J., Rau, M. M., Refregier, A., Rollins, R. P., Rozo, E., Rykoff, E. S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Stebbins, A., Varga, T. N., Vielzeuf, P., Wang, M., Wechsler, R. H., Yanny, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Fernandez, E., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gschwend, J., Gutierrez, G., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Nord, B., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use 26 million galaxies from the Dark Energy Survey (DES) Year 1 shape catalogs over 1321 deg$^2$ of the sky to produce the most significant measurement of cosmic shear in a galaxy survey to date. We constrain cosmological parameters in both the flat $\Lambda$CDM and $w$CDM models, while also varying the neutrino mass density. These results are shown to be robust using two independent shape catalogs, two independent \photoz\ calibration methods, and two independent analysis pipelines in a blind analysis. We find a 3.5\% fractional uncertainty on $\sigma_8(\Omega_m/0.3)^{0.5} = 0.782^{+0.027}_{-0.027}$ at 68\% CL, which is a factor of 2.5 improvement over the fractional constraining power of our DES Science Verification results. In $w$CDM, we find a 4.8\% fractional uncertainty on $\sigma_8(\Omega_m/0.3)^{0.5} = 0.777^{+0.036}_{-0.038}$ and a dark energy equation-of-state $w=-0.95^{+0.33}_{-0.39}$. We find results that are consistent with previous cosmic shear constraints in $\sigma_8$ -- $\Omega_m$, and see no evidence for disagreement of our weak lensing data with data from the CMB. Finally, we find no evidence preferring a $w$CDM model allowing $w\ne -1$. We expect further significant improvements with subsequent years of DES data, which will more than triple the sky coverage of our shape catalogs and double the effective integrated exposure time per galaxy., Comment: 32 pages, 19 figures; matches PRD referee response version
Published: 2017
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38. Dark Energy Survey Year 1 Results: Galaxy clustering for combined probes

Author: Elvin-Poole, J., Crocce, M., Ross, A. J., Giannantonio, T., Rozo, E., Rykoff, E. S., Avila, S., Banik, N., Blazek, J., Bridle, S. L., Cawthon, R., Drlica-Wagner, A., Friedrich, O., Kokron, N., Krause, E., MacCrann, N., Prat, J., Sanchez, C., Secco, L. F., Sevilla-Noarbe, I., Troxel, M. A., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Asorey, J., Bechtol, K., Becker, M. R., Benoit-Levy, A., Bernstein, G. M., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., DAndrea, C. B., da Costa, L. N., Davis, T. M., Davis, C., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Eifler, T. F., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoormann, J. K., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., King, A., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lewis, G., Li, T. S., Lidman, C., Lima, M., Lin, H., Macaulay, E., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moller, A., Nichol, R. C., Nord, B., ONeill, C. R., Percival, W. J., Petravick, D., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sheldon, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Uddin, S. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Yuan, F., Zhang, B., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the clustering of DES Year 1 galaxies that are intended to be combined with weak lensing samples in order to produce precise cosmological constraints from the joint analysis of large-scale structure and lensing correlations. Two-point correlation functions are measured for a sample of $6.6 \times 10^{5}$ luminous red galaxies selected using the \textsc{redMaGiC} algorithm over an area of $1321$ square degrees, in the redshift range $0.15 < z < 0.9$, split into five tomographic redshift bins. The sample has a mean redshift uncertainty of $\sigma_{z}/(1+z) = 0.017$. We quantify and correct spurious correlations induced by spatially variable survey properties, testing their impact on the clustering measurements and covariance. We demonstrate the sample's robustness by testing for stellar contamination, for potential biases that could arise from the systematic correction, and for the consistency between the two-point auto- and cross-correlation functions. We show that the corrections we apply have a significant impact on the resultant measurement of cosmological parameters, but that the results are robust against arbitrary choices in the correction method. We find the linear galaxy bias in each redshift bin in a fiducial cosmology to be $b(z$=$0.24)=1.40 \pm 0.08$, $b(z$=$0.38)=1.61 \pm 0.05$, $b(z$=$0.53)=1.60 \pm 0.04$ for galaxies with luminosities $L/L_*>$$0.5$, $b(z$=$0.68)=1.93 \pm 0.05$ for $L/L_*>$$1$ and $b(z$=$0.83)=1.99 \pm 0.07$ for $L/L_*$$>1.5$, broadly consistent with expectations for the redshift and luminosity dependence of the bias of red galaxies. We show these measurements to be consistent with the linear bias obtained from tangential shear measurements., Comment: 20 pages, 13 figures. Version accepted by PRD, minor changes to text, covariance matrix updated, conclusions unchanged
Published: 2017
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39. Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

Author: DES Collaboration, Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Aleksić, J., Allam, S., Allen, S., Amara, A., Annis, J., Asorey, J., Avila, S., Bacon, D., Balbinot, E., Banerji, M., Banik, N., Barkhouse, W., Baumer, M., Baxter, E., Bechtol, K., Becker, M. R., Benoit-Lévy, A., Benson, B. A., Bernstein, G. M., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Buckley-Geer, E., Burke, D. L., Busha, M. T., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, N., Childress, M., Choi, A., Conselice, C., Crittenden, R., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., Davis, T. M., Davis, C., De Vicente, J., DePoy, D. L., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elliott, A. E., Elsner, F., Elvin-Poole, J., Estrada, J., Evrard, A. E., Fang, Y., Fernandez, E., Ferté, A., Finley, D. A., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., García-Bellido, J., Garcia-Fernandez, M., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. D., Johnson, M. W. G., Kacprzak, T., Kent, S., Kim, A. G., King, A., Kirk, D., Kokron, N., Kovacs, A., Krause, E., Krawiec, C., Kremin, A., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lacasa, F., Lahav, O., Li, T. S., Liddle, A. R., Lidman, C., Lima, M., Lin, H., MacCrann, N., Maia, M. A. G., Makler, M., Manera, M., March, M., Marshall, J. L., Martini, P., McMahon, R. G., Melchior, P., Menanteau, F., Miquel, R., Miranda, V., Mudd, D., Muir, J., Möller, A., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R. L. C., Palmese, A., Peacock, J., Peiris, H. V., Peoples, J., Percival, W. J., Petravick, D., Plazas, A. A., Porredon, A., Prat, J., Pujol, A., Rau, M. M., Refregier, A., Ricker, P. M., Roe, N., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rozo, E., Rykoff, E. S., Sako, M., Salvador, A. I., Samuroff, S., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Smith, M., Smith, J., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Tucker, B. E., Uddin, S. A., Varga, T. N., Vielzeuf, P., Vikram, V., Vivas, A. K., Walker, A. R., Wang, M., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Yanny, B., Yuan, F., Zenteno, A., Zhang, B., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present cosmological results from a combined analysis of galaxy clustering and weak gravitational lensing, using 1321 deg$^2$ of $griz$ imaging data from the first year of the Dark Energy Survey (DES Y1). We combine three two-point functions: (i) the cosmic shear correlation function of 26 million source galaxies in four redshift bins, (ii) the galaxy angular autocorrelation function of 650,000 luminous red galaxies in five redshift bins, and (iii) the galaxy-shear cross-correlation of luminous red galaxy positions and source galaxy shears. To demonstrate the robustness of these results, we use independent pairs of galaxy shape, photometric redshift estimation and validation, and likelihood analysis pipelines. To prevent confirmation bias, the bulk of the analysis was carried out while blind to the true results; we describe an extensive suite of systematics checks performed and passed during this blinded phase. The data are modeled in flat $\Lambda$CDM and $w$CDM cosmologies, marginalizing over 20 nuisance parameters, varying 6 (for $\Lambda$CDM) or 7 (for $w$CDM) cosmological parameters including the neutrino mass density and including the 457 $\times$ 457 element analytic covariance matrix. We find consistent cosmological results from these three two-point functions, and from their combination obtain $S_8 \equiv \sigma_8 (\Omega_m/0.3)^{0.5} = 0.783^{+0.021}_{-0.025}$ and $\Omega_m = 0.264^{+0.032}_{-0.019}$ for $\Lambda$CDM for $w$CDM, we find $S_8 = 0.794^{+0.029}_{-0.027}$, $\Omega_m = 0.279^{+0.043}_{-0.022}$, and $w=-0.80^{+0.20}_{-0.22}$ at 68% CL. The precision of these DES Y1 results rivals that from the Planck cosmic microwave background measurements, allowing a comparison of structure in the very early and late Universe on equal terms. Although the DES Y1 best-fit values for $S_8$ and $\Omega_m$ are lower than the central values from Planck ..., Comment: Matches published version. Results essentially unchanged, except updated covariance matrix leads to improved chi^2 (colored text removed)
Published: 2017
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40. Dark Energy Survey Year 1 Results: The Impact of Galaxy Neighbours on Weak Lensing Cosmology with im3shape

Author: Samuroff, S., Bridle, S. L., Zuntz, J., Troxel, M. A., Gruen, D., Rollins, R. P., Bernstein, G. M., Eifler, T. F., Huff, E. M., Kacprzak, T., Krause, E., MacCrann, N., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Crocce, M., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Doel, P., Neto, A. Fausti, Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kirk, D., Kuehn, K., Kuhlmann, S., Li, T. S., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Nord, B., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., and Tucker, D. L.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use a suite of simulated images based on Year 1 of the Dark Energy Survey to explore the impact of galaxy neighbours on shape measurement and shear cosmology. The hoopoe image simulations include realistic blending, galaxy positions, and spatial variations in depth and PSF properties. Using the im3shape maximum-likelihood shape measurement code, we identify four mechanisms by which neighbours can have a non-negligible influence on shear estimation. These effects, if ignored, would contribute a net multiplicative bias of $m \sim 0.03 - 0.09$ in the DES Y1 im3shape catalogue, though the precise impact will be dependent on both the measurement code and the selection cuts applied. This can be reduced to percentage level or less by removing objects with close neighbours, at a cost to the effective number density of galaxies $n_\mathrm{eff}$ of 30%. We use the cosmological inference pipeline of DES Y1 to explore the cosmological implications of neighbour bias and show that omitting blending from the calibration simulation for DES Y1 would bias the inferred clustering amplitude $S_8\equiv \sigma_8 (\Omega _\mathrm{m} /0.3)^{0.5}$ by $2 \sigma$ towards low values. Finally, we use the hoopoe simulations to test the effect of neighbour-induced spatial correlations in the multiplicative bias. We find the impact on the recovered $S_8$ of ignoring such correlations to be subdominant to statistical error at the current level of precision., Comment: 20 pages, submitted to MNRAS
Published: 2017
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41. Dark Energy Survey Year 1 Results: Weak Lensing Shape Catalogues

Author: Zuntz, J., Sheldon, E., Samuroff, S., Troxel, M. A., Jarvis, M., MacCrann, N., Gruen, D., Prat, J., Sánchez, C., Choi, A., Bridle, S. L., Bernstein, G. M., Dodelson, S., Drlica-Wagner, A., Fang, Y., Gruendl, R. A., Hoyle, B., Huff, E. M., Jain, B., Kirk, D., Kacprzak, T., Krawiec, C., Plazas, A. A., Rollins, R. P., Rykoff, E. S., Sevilla-Noarbe, I., Soergel, B., Varga, T. N., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Evrard, A. E., Neto, A. Fausti, Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., March, M., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Ogando, R. L. C., Roe, N., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present two galaxy shape catalogues from the Dark Energy Survey Year 1 data set, covering 1500 square degrees with a median redshift of $0.59$. The catalogues cover two main fields: Stripe 82, and an area overlapping the South Pole Telescope survey region. We describe our data analysis process and in particular our shape measurement using two independent shear measurement pipelines, METACALIBRATION and IM3SHAPE. The METACALIBRATION catalogue uses a Gaussian model with an innovative internal calibration scheme, and was applied to $riz$-bands, yielding 34.8M objects. The IM3SHAPE catalogue uses a maximum-likelihood bulge/disc model calibrated using simulations, and was applied to $r$-band data, yielding 21.9M objects. Both catalogues pass a suite of null tests that demonstrate their fitness for use in weak lensing science. We estimate the 1$\sigma$ uncertainties in multiplicative shear calibration to be $0.013$ and $0.025$ for the METACALIBRATION and IM3SHAPE catalogues, respectively., Comment: 36 Pages, 29 figures. This version accepted for publication in MNRAS
Published: 2017
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42. Weak-lensing mass calibration of redMaPPer galaxy clusters in Dark Energy Survey Science Verification data

Author: Melchior, P., Gruen, D., McClintock, T., Varga, T. N., Sheldon, E., Rozo, E., Amara, A., Becker, M. R., Benson, B. A., Bermeo, A., Bridle, S. L., Clampitt, J., Dietrich, J. P., Hartley, W. G., Hollowood, D., Jain, B., Jarvis, M., Jeltema, T., Kacprzak, T., MacCrann, N., Rykoff, E. S., Saro, A., Suchyta, E., Troxel, M. A., Zuntz, J., Bonnett, C., Plazas, A. A., Abbott, T. M. C., Abdalla, F. B., Annis, J., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Eifler, T. F., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kirk, D., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Ogando, R., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., Weller, J., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use weak-lensing shear measurements to determine the mean mass of optically selected galaxy clusters in Dark Energy Survey Science Verification data. In a blinded analysis, we split the sample of more than 8,000 redMaPPer clusters into 15 subsets, spanning ranges in the richness parameter $5 \leq \lambda \leq 180$ and redshift $0.2 \leq z \leq 0.8$, and fit the averaged mass density contrast profiles with a model that accounts for seven distinct sources of systematic uncertainty: shear measurement and photometric redshift errors; cluster-member contamination; miscentering; deviations from the NFW halo profile; halo triaxiality; and line-of-sight projections. We combine the inferred cluster masses to estimate the joint scaling relation between mass, richness and redshift, $\mathcal{M}(\lambda,z) \varpropto M_0 \lambda^{F} (1+z)^{G}$. We find $M_0 \equiv \langle M_{200\mathrm{m}}\,|\,\lambda=30,z=0.5\rangle=\left[ 2.35 \pm 0.22\ \rm{(stat)} \pm 0.12\ \rm{(sys)} \right] \cdot 10^{14}\ M_\odot$, with $F = 1.12\,\pm\,0.20\ \rm{(stat)}\, \pm\, 0.06\ \rm{(sys)}$ and $G = 0.18\,\pm\, 0.75\ \rm{(stat)}\, \pm\, 0.24\ \rm{(sys)}$. The amplitude of the mass-richness relation is in excellent agreement with the weak-lensing calibration of redMaPPer clusters in SDSS by Simet et al. (2016) and with the Saro et al. (2015) calibration based on abundance matching of SPT-detected clusters. Our results extend the redshift range over which the mass-richness relation of redMaPPer clusters has been calibrated with weak lensing from $z\leq 0.3$ to $z\leq0.8$. Calibration uncertainties of shear measurements and photometric redshift estimates dominate our systematic error budget and require substantial improvements for forthcoming studies., Comment: 22 pages, 14 figures, accepted by MNRAS
Published: 2016
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43. Galaxy bias from galaxy-galaxy lensing in the DES Science Verification Data

Author: Prat, J., Sánchez, C., Miquel, R., Kwan, J., Blazek, J., Bonnett, C., Amara, A., Bridle, S. L., Clampitt, J., Crocce, M., Fosalba, P., Gaztanaga, E., Giannantonio, T., Hartley, W. G., Jarvis, M., MacCrann, N., Percival, W. J., Ross, A. J., Sheldon, E., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Annis, J., Benoit-Lévy, A., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Neto, A. Fausti, Flaugher, B., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J. L., Melchior, P., Menanteau, F., Nord, B., Plazas, A. A., Reil, K., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Walker, A. R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a measurement of galaxy-galaxy lensing around a magnitude-limited ($i_{AB} < 22.5$) sample of galaxies from the Dark Energy Survey Science Verification (DES-SV) data. We split these lenses into three photometric-redshift bins from 0.2 to 0.8, and determine the product of the galaxy bias $b$ and cross-correlation coefficient between the galaxy and dark matter overdensity fields $r$ in each bin, using scales above 4 Mpc/$h$ comoving, where we find the linear bias model to be valid given our current uncertainties. We compare our galaxy bias results from galaxy-galaxy lensing with those obtained from galaxy clustering (Crocce et al. 2016) and CMB lensing (Giannantonio et al. 2016) for the same sample of galaxies, and find our measurements to be in good agreement with those in Crocce et al. (2016), while, in the lowest redshift bin ($z\sim0.3$), they show some tension with the findings in Giannantonio et al. (2016). We measure $b\cdot r$ to be $0.87\pm 0.11$, $1.12 \pm 0.16$ and $1.24\pm 0.23$, respectively for the three redshift bins of width $\Delta z = 0.2$ in the range $0.2
Published: 2016
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44. Inference from the small scales of cosmic shear with current and future Dark Energy Survey data

Author: MacCrann, N., Aleksić, J., Amara, A., Bridle, S. L., Bruderer, C., Chang, C., Dodelson, S., Eifler, T. F., Huff, E. M., Huterer, D., Kacprzak, T., Refregier, A., Suchyta, E., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Allam, S., Annis, J., Armstrong, R., Benoit-Lévy, A., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Flaugher, B., Fosalba, P., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Jarvis, M., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Plazas, A. A., Romer, A. K., Rykoff, E. S., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Sheldon, E., Soares-Santos, M., Swanson, M. E. C., Tarle, G., Thomas, D., and Vikram, V.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Cosmic shear is sensitive to fluctuations in the cosmological matter density field, including on small physical scales, where matter clustering is affected by baryonic physics in galaxies and galaxy clusters, such as star formation, supernovae feedback and AGN feedback. While muddying any cosmological information that is contained in small scale cosmic shear measurements, this does mean that cosmic shear has the potential to constrain baryonic physics and galaxy formation. We perform an analysis of the Dark Energy Survey (DES) Science Verification (SV) cosmic shear measurements, now extended to smaller scales, and using the Mead et al. 2015 halo model to account for baryonic feedback. While the SV data has limited statistical power, we demonstrate using a simulated likelihood analysis that the final DES data will have the statistical power to differentiate among baryonic feedback scenarios. We also explore some of the difficulties in interpreting the small scales in cosmic shear measurements, presenting estimates of the size of several other systematic effects that make inference from small scales difficult, including uncertainty in the modelling of intrinsic alignment on nonlinear scales, `lensing bias', and shape measurement selection effects. For the latter two, we make use of novel image simulations. While future cosmic shear datasets have the statistical power to constrain baryonic feedback scenarios, there are several systematic effects that require improved treatments, in order to make robust conclusions about baryonic feedback., Comment: 14 pages, 10 figures
Published: 2016
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45. Cosmology constraints from shear peak statistics in Dark Energy Survey Science Verification data

Author: Kacprzak, T., Kirk, D., Friedrich, O., Amara, A., Refregier, A., Marian, L., Dietrich, J. P., Suchyta, E., Aleksić, J., Bacon, D., Becker, M. R., Bonnett, C., Bridle, S. L., Chang, C., Eifler, T. F., Hartley, W., Huff, E. M., Krause, E., MacCrann, N., Melchior, P., Nicola, A., Samuroff, S., Sheldon, E., Troxel, M. A., Weller, J., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Armstrong, R., Benoit-Lévy, A., Bernstein, R. A., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Evrard, A. E., Neto, A. Fausti, Flaugher, B., Fosalba, P., Frieman, J., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., March, M., Marshall, J. L., Martini, P., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Walker, A. R., and Zhang, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Shear peak statistics has gained a lot of attention recently as a practical alternative to the two point statistics for constraining cosmological parameters. We perform a shear peak statistics analysis of the Dark Energy Survey (DES) Science Verification (SV) data, using weak gravitational lensing measurements from a 139 deg$^2$ field. We measure the abundance of peaks identified in aperture mass maps, as a function of their signal-to-noise ratio, in the signal-to-noise range $0<\mathcal S / \mathcal N<4$. To predict the peak counts as a function of cosmological parameters we use a suite of $N$-body simulations spanning 158 models with varying $\Omega_{\rm m}$ and $\sigma_8$, fixing $w = -1$, $\Omega_{\rm b} = 0.04$, $h = 0.7$ and $n_s=1$, to which we have applied the DES SV mask and redshift distribution. In our fiducial analysis we measure $\sigma_{8}(\Omega_{\rm m}/0.3)^{0.6}=0.77 \pm 0.07$, after marginalising over the shear multiplicative bias and the error on the mean redshift of the galaxy sample. We introduce models of intrinsic alignments, blending, and source contamination by cluster members. These models indicate that peaks with $\mathcal S / \mathcal N>4$ would require significant corrections, which is why we do not include them in our analysis. We compare our results to the cosmological constraints from the two point analysis on the SV field and find them to be in good agreement in both the central value and its uncertainty. We discuss prospects for future peak statistics analysis with upcoming DES data., Comment: 21 pages, 14 figures, submitted to MNRAS
Published: 2016
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46. Cross-correlation of gravitational lensing from DES Science Verification data with SPT and Planck lensing

Author: Kirk, D., Omori, Y., Benoit-Lévy, A., Cawthon, R., Chang, C., Larsen, P., Amara, A., Bacon, D., Crawford, T. M., Dodelson, S., Fosalba, P., Giannantonio, T., Holder, G., Jain, B., Kacprzak, T., Lahav, O., MacCrann, N., Nicola, A., Refregier, A., Sheldon, E., Story, K. T., Troxel, M. A., Vieira, J. D., Vikram, V., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Becker, M. R., Benson, B. A., Bernstein, G. M., Bernstein, R. A., Bleem, L. E., Bonnett, C., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Frieman, J., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Honscheid, K., James, D. J., Jarvis, M., Kent, S., Kuehn, K., Kuropatkin, N., Lima, M., March, M., Martini, P., Melchior, P., Miller, C. J., Miquel, R., Nichol, R. C., Ogando, R., Plazas, A. A., Reichardt, C. L., Roodman, A., Rozo, E., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Simard, G., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Wechsler, R. H., and Weller, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the cross-correlation between weak lensing of galaxy images and of the cosmic microwave background (CMB). The effects of gravitational lensing on different sources will be correlated if the lensing is caused by the same mass fluctuations. We use galaxy shape measurements from 139 deg$^{2}$ of the Dark Energy Survey (DES) Science Verification data and overlapping CMB lensing from the South Pole Telescope (SPT) and Planck. The DES source galaxies have a median redshift of $z_{\rm med} {\sim} 0.7$, while the CMB lensing kernel is broad and peaks at $z{\sim}2$. The resulting cross-correlation is maximally sensitive to mass fluctuations at $z{\sim}0.44$. Assuming the Planck 2015 best-fit cosmology, the amplitude of the DES$\times$SPT cross-power is found to be $A = 0.88 \pm 0.30$ and that from DES$\times$Planck to be $A = 0.86 \pm 0.39$, where $A=1$ corresponds to the theoretical prediction. These are consistent with the expected signal and correspond to significances of $2.9 \sigma$ and $2.2 \sigma$ respectively. We demonstrate that our results are robust to a number of important systematic effects including the shear measurement method, estimator choice, photometric redshift uncertainty and CMB lensing systematics. Significant intrinsic alignment of galaxy shapes would increase the cross-correlation signal inferred from the data; we calculate a value of $A = 1.08 \pm 0.36$ for DES$\times$SPT when we correct the observations with a simple IA model. With three measurements of this cross-correlation now existing in the literature, there is not yet reliable evidence for any deviation from the expected LCDM level of cross-correlation, given the size of the statistical uncertainties and the significant impact of systematic errors, particularly IAs. We provide forecasts for the expected signal-to-noise of the combination of the five-year DES survey and SPT-3G., Comment: 13 pages, 6 figures
Published: 2015
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47. Mapping and simulating systematics due to spatially-varying observing conditions in DES Science Verification data

Author: Leistedt, B., Peiris, H. V., Elsner, F., Benoit-Lévy, A., Amara, A., Bauer, A. H., Becker, M. R., Bonnett, C., Bruderer, C., Busha, M. T., Kind, M. Carrasco, Chang, C., Crocce, M., da Costa, L. N., Gaztanaga, E., Huff, E. M., Lahav, O., Palmese, A., Percival, W. J., Refregier, A., Ross, A. J., Rozo, E., Rykoff, E. S., Sánchez, C., Sadeh, I., Sevilla-Noarbe, I., Sobreira, F., Suchyta, E., Swanson, M. E. C., Wechsler, R. H., Abdalla, F. B., Allam, S., Banerji, M., Bernstein, G. M., Bernstein, R. A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Carretero, J., Cunha, C. E., D'Andrea, C. B., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Neto, A. Fausti, Flaugher, B., Fosalba, P., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Jarvis, M., Kent, S., Kuehn, K., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Miller, C. J., Miquel, R., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Roodman, A., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Smith, R. C., Soares-Santos, M., Tarle, G., Thaler, J., Thomas, D., Vikram, V., Walker, A. R., Wester, W., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Spatially-varying depth and characteristics of observing conditions, such as seeing, airmass, or sky background, are major sources of systematic uncertainties in modern galaxy survey analyses, in particular in deep multi-epoch surveys. We present a framework to extract and project these sources of systematics onto the sky, and apply it to the Dark Energy Survey (DES) to map the observing conditions of the Science Verification (SV) data. The resulting distributions and maps of sources of systematics are used in several analyses of DES SV to perform detailed null tests with the data, and also to incorporate systematics in survey simulations. We illustrate the complementarity of these two approaches by comparing the SV data with the BCC-UFig, a synthetic sky catalogue generated by forward-modelling of the DES SV images. We analyse the BCC-UFig simulation to construct galaxy samples mimicking those used in SV galaxy clustering studies. We show that the spatially-varying survey depth imprinted in the observed galaxy densities and the redshift distributions of the SV data are successfully reproduced by the simulation and well-captured by the maps of observing conditions. The combined use of the maps, the SV data and the BCC-UFig simulation allows us to quantify the impact of spatial systematics on $N(z)$, the redshift distributions inferred using photometric redshifts. We conclude that spatial systematics in the SV data are mainly due to seeing fluctuations and are under control in current clustering and weak lensing analyses. The framework presented here is relevant to all multi-epoch surveys, and will be essential for exploiting future surveys such as the Large Synoptic Survey Telescope (LSST), which will require detailed null-tests and realistic end-to-end image simulations to correctly interpret the deep, high-cadence observations of the sky., Comment: 13 pages, 12 figures
Published: 2015
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48. The DES Science Verification Weak Lensing Shear Catalogues

Author: Jarvis, M., Sheldon, E., Zuntz, J., Kacprzak, T., Bridle, S. L., Amara, A., Armstrong, R., Becker, M. R., Bernstein, G. M., Bonnett, C., Chang, C., Das, R., Dietrich, J. P., Drlica-Wagner, A., Eifler, T. F., Gangkofner, C., Gruen, D., Hirsch, M., Huff, E. M., Jain, B., Kent, S., Kirk, D., MacCrann, N., Melchior, P., Plazas, A. A., Refregier, A., Rowe, B., Rykoff, E. S., Samuroff, S., Sánchez, C., Suchyta, E., Troxel, M. A., Vikram, V., Abbott, T., Abdalla, F. B., Allam, S., Annis, J., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Clampitt, J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Neto, A. Fausti, Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., March, M., Martini, P., Miquel, R., Mohr, J. J., Neilsen, E., Nord, B., Ogando, R., Reil, K., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Walker, A. R., and Wechsler, R. H.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present weak lensing shear catalogues for 139 square degrees of data taken during the Science Verification (SV) time for the new Dark Energy Camera (DECam) being used for the Dark Energy Survey (DES). We describe our object selection, point spread function estimation and shear measurement procedures using two independent shear pipelines, IM3SHAPE and NGMIX, which produce catalogues of 2.12 million and 3.44 million galaxies respectively. We detail a set of null tests for the shear measurements and find that they pass the requirements for systematic errors at the level necessary for weak lensing science applications using the SV data. We also discuss some of the planned algorithmic improvements that will be necessary to produce sufficiently accurate shear catalogues for the full 5-year DES, which is expected to cover 5000 square degrees., Comment: Accepted by MNRAS; 38 pages, 29 figures; v3: minor edits based on referee's comments, switched to mnras style, added figure 8, updated info about released catalogs
Published: 2015
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49. Cosmic Shear Measurements with DES Science Verification Data

Author: Becker, M. R., Troxel, M. A., MacCrann, N., Krause, E., Eifler, T. F., Friedrich, O., Nicola, A., Refregier, A., Amara, A., Bacon, D., Bernstein, G. M., Bonnett, C., Bridle, S. L., Busha, M. T., Chang, C., Dodelson, S., Erickson, B., Evrard, A. E., Frieman, J., Gaztanaga, E., Gruen, D., Hartley, W., Jain, B., Jarvis, M., Kacprzak, T., Kirk, D., Kravtsov, A., Leistedt, B., Rykoff, E. S., Sabiu, C., Sanchez, C., Seo, H., Sheldon, E., Wechsler, R. H., Zuntz, J., Abbott, T., Abdalla, F. B., Allam, S., Armstrong, R., Banerji, M., Bauer, A. H., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Neto, A. Fausti, Fernandez, E., Finley, D. A., Flaugher, B., Fosalba, P., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., March, M., Martini, P., Melchior, P., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Vikram, V., Walker, A. R., and Collaboration, The DES
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present measurements of weak gravitational lensing cosmic shear two-point statistics using Dark Energy Survey Science Verification data. We demonstrate that our results are robust to the choice of shear measurement pipeline, either ngmix or im3shape, and robust to the choice of two-point statistic, including both real and Fourier-space statistics. Our results pass a suite of null tests including tests for B-mode contamination and direct tests for any dependence of the two-point functions on a set of 16 observing conditions and galaxy properties, such as seeing, airmass, galaxy color, galaxy magnitude, etc. We furthermore use a large suite of simulations to compute the covariance matrix of the cosmic shear measurements and assign statistical significance to our null tests. We find that our covariance matrix is consistent with the halo model prediction, indicating that it has the appropriate level of halo sample variance. We compare the same jackknife procedure applied to the data and the simulations in order to search for additional sources of noise not captured by the simulations. We find no statistically significant extra sources of noise in the data. The overall detection significance with tomography for our highest source density catalog is 9.7sigma. Cosmological constraints from the measurements in this work are presented in a companion paper (DES et al. 2015)., Comment: measurements and covariance matrices in machine readable format are available as ancillary data on the arXiv; high-resolution versions of figures can be downloaded from http://deswl.github.io
Published: 2015
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50. Cosmology from Cosmic Shear with DES Science Verification Data

Author: The Dark Energy Survey Collaboration, Abbott, T., Abdalla, F. B., Allam, S., Amara, A., Annis, J., Armstrong, R., Bacon, D., Banerji, M., Bauer, A. H., Baxter, E., Becker, M. R., Benoit-Lévy, A., Bernstein, R. A., Bernstein, G. M., Bertin, E., Blazek, J., Bonnett, C., Bridle, S. L., Brooks, D., Bruderer, C., Buckley-Geer, E., Burke, D. L., Busha, M. T., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C., Clampitt, J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., DePoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Efstathiou, G., Eifler, T. F., Erickson, B., Estrada, J., Evrard, A. E., Neto, A. Fausti, Fernandez, E., Finley, D. A., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Gangkofner, C., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W., Hirsch, M., Honscheid, K., Huff, E. M., Jain, B., James, D. J., Jarvis, M., Kacprzak, T., Kent, S., Kirk, D., Krause, E., Kravtsov, A., Kuehn, K., Kuropatkin, N., Kwan, J., Lahav, O., Leistedt, B., Li, T. S., Lima, M., Lin, H., MacCrann, N., March, M., Marshall, J. L., Martini, P., McMahon, R. G., Melchior, P., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Nicola, A., Nord, B., Ogando, R., Palmese, A., Peiris, H. V., Plazas, A. A., Refregier, A., Roe, N., Romer, A. K., Roodman, A., Rowe, B., Rykoff, E. S., Sabiu, C., Sadeh, I., Sako, M., Samuroff, S., Sánchez, C., Sanchez, E., Seo, H., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Troxel, M. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the first constraints on cosmology from the Dark Energy Survey (DES), using weak lensing measurements from the preliminary Science Verification (SV) data. We use 139 square degrees of SV data, which is less than 3\% of the full DES survey area. Using cosmic shear 2-point measurements over three redshift bins we find $\sigma_8 (\Omega_{\rm m}/0.3)^{0.5} = 0.81 \pm 0.06$ (68\% confidence), after marginalising over 7 systematics parameters and 3 other cosmological parameters. We examine the robustness of our results to the choice of data vector and systematics assumed, and find them to be stable. About $20$\% of our error bar comes from marginalising over shear and photometric redshift calibration uncertainties. The current state-of-the-art cosmic shear measurements from CFHTLenS are mildly discrepant with the cosmological constraints from Planck CMB data; our results are consistent with both datasets. Our uncertainties are $\sim$30\% larger than those from CFHTLenS when we carry out a comparable analysis of the two datasets, which we attribute largely to the lower number density of our shear catalogue. We investigate constraints on dark energy and find that, with this small fraction of the full survey, the DES SV constraints make negligible impact on the Planck constraints. The moderate disagreement between the CFHTLenS and Planck values of $\sigma_8 (\Omega_{\rm m}/0.3)^{0.5}$ is present regardless of the value of $w$., Comment: Finally updating to the published version. 20 pages, 12 figures. Additional information at http://deswl.github.io/
Published: 2015
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