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178 results on '"Fausti Neto, A"'

1. Dark Energy Survey Year 1 results: Weak lensing shape catalogues

Author: Zunt, J, Sheldon, E, Samuroff, S, Troxel, MA, Jarvis, M, MacCrann, N, Gruen, D, Prat, J, Sánchez, C, Choi, A, Bridle, SL, Bernstein, GM, Dodelson, S, Drlica-Wagner, A, Fang, Y, Gruendl, RA, Hoyle, B, Huff, EM, Jain, B, Kirk, D, Kacprzak, T, Krawiec, C, Plazas, AA, Rollins, RP, Rykoff, ES, Sevilla-Noarbe, I, Soergel, B, Varga, TN, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Bechtol, K, Benoit-Lévy, A, Bertin, E, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Davis, C, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Eifler, TF, Estrada, J, Evrard, AE, Fausti Neto, A, Fernandez, E, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gschwend, J, Gutierrez, G, Hartley, WG, Honscheid, K, James, DJ, Jeltema, T, Johnson, MWG, Johnson, MD, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Maia, MAG, March, M, Martini, P, Melchior, P, Menanteau, F, Miller, CJ, Miquel, R, Mohr, JJ, Neilsen, E, Nichol, RC, Ogando, RLC, Roe, N, Romer, AK, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Smith, M, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, and Swanson, MEC
Subjects: astro-ph.CO, Astronomical And Space Sciences, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present two galaxy shape catalogues from the Dark Energy Survey Year 1 data set, covering 1500 deg2 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 amaximum-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 1σ uncertainties in multiplicative shear calibration to be 0.013 and 0.025 for the METACALIBRATION and IM3SHAPE catalogues, respectively.
Published: 2018

2. A measurement of CMB cluster lensing with SPT and DES year 1 data

Author: Baxter, EJ, Raghunathan, S, Crawford, TM, Fosalba, P, Hou, Z, Holder, GP, Omori, Y, Patil, S, Rozo, E, Abbott, TMC, Annis, J, Aylor, K, Benoit-Lévy, A, Benson, BA, Bertin, E, Bleem, L, Buckley-Geer, E, Burke, DL, Carlstrom, J, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chang, CL, Cho, HM, Crites, AT, Crocce, M, Cunha, CE, da Costa, LN, D'Andrea, CB, Davis, C, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Dodelson, S, Doel, P, Drlica-Wagner, A, Estrada, J, Everett, WB, Fausti Neto, A, Flaugher, B, Frieman, J, García-Bellido, J, George, EM, Gaztanaga, E, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Halverson, NW, Harrington, NL, Hartley, WG, Holzapfel, WL, Honscheid, K, Hrubes, JD, Jain, B, James, DJ, Jarvis, M, Jeltema, T, Knox, L, Krause, E, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lahav, O, Lee, AT, Leitch, EM, Li, TS, Lima, M, Luong-Van, D, Manzotti, A, March, M, Marrone, DP, Marshall, JL, Martini, P, McMahon, JJ, Melchior, P, Menanteau, F, Meyer, SS, Miller, CJ, Miquel, R, Mocanu, LM, Mohr, JJ, Natoli, T, Nord, B, Ogando, RLC, Padin, S, Plazas, AA, Pryke, C, Rapetti, D, Reichardt, CL, Romer, AK, Roodman, A, Ruhl, JE, Rykoff, E, Sako, M, Sanchez, E, Sayre, JT, and Scarpine, V
Subjects: gravitational lensing: weak, galaxies: clusters: general, cosmic background radiation, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: Clusters of galaxies gravitationally lens the cosmic microwave background (CMB) radiation, resulting in a distinct imprint in the CMB on arcminute scales. Measurement of this effect offers a promising way to constrain the masses of galaxy clusters, particularly those at high redshift. We use CMB maps from the South Pole Telescope Sunyaev-Zel'dovich (SZ) survey to measure the CMB lensing signal around galaxy clusters identified in optical imaging from first year observations of the Dark Energy Survey. The cluster catalogue used in this analysis contains 3697 members with mean redshift of z = 0.45. We detect lensing of the CMB by the galaxy clusters at 8.1s significance. Using the measured lensing signal, we constrain the amplitude of the relation between cluster mass and optical richness to roughly 17 per cent precision, finding good agreement with recent constraints obtained with galaxy lensing. The error budget is dominated by statistical noise but includes significant contributions from systematic biases due to the thermal SZ effect and cluster miscentring.
Published: 2018

3. Galaxy Populations in Massive Galaxy Clusters to z=1.1: Color Distribution, Concentration, Halo Occupation Number and Red Sequence Fraction

Author: Hennig, C., Mohr, J. J., Zenteno, A., Desai, S., Dietrich, J. P., Bocquet, S., Strazzullo, V., Saro, A., Abbott, T. M. C., Abdalla, F. B., Bayliss, M., Benoit-Levy, A., Bernstein, R. A., Bertin, E., Brooks, D., Capasso, R., Capozzi, D., Carnero, A., Kind, M. Carrasco, Carretero, J., Chiu, I., D'Andrea, C. B., daCosta, L. N., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Fausti-Neto, A., Fosalba, P., Frieman, J., Gangkofner, C., Gonzalez, A., Gruen, D., Gruendl, R. A., Gupta, N., Gutierrez, G., Honscheid, K., Hlavacek-Larrondo, J., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., March, M., Marshall, J. L., Martini, P., McDonald, M., Melchior, P., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R., Plazas, A. A., Reichardt, C., Romer, A. K., Rozo, E., Rykoff, E. S., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Stalder, B., Stanford, S. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Walker, A. R., and Zhang, Y.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the galaxy populations in 74 Sunyaev Zeldovich Effect (SZE) selected clusters from the South Pole Telescope (SPT) survey that have been imaged in the science verification phase of the Dark Energy Survey (DES). The sample extends up to $z\sim 1.1$ with $4 \times 10^{14} M_{\odot}\le M_{200}\le 3\times 10^{15} M_{\odot}$. Using the band containing the 4000~\AA\ break and its redward neighbor, we study the color-magnitude distributions of cluster galaxies to $\sim m_*+2$, finding: (1) the intrinsic rest frame $g-r$ color width of the red sequence (RS) population is $\sim$0.03 out to $z\sim0.85$ with a preference for an increase to $\sim0.07$ at $z=1$ and (2) the prominence of the RS declines beyond $z\sim0.6$. The spatial distribution of cluster galaxies is well described by the NFW profile out to $4R_{200}$ with a concentration of $c_{\mathrm{g}} = 3.59^{+0.20}_{-0.18}$, $5.37^{+0.27}_{-0.24}$ and $1.38^{+0.21}_{-0.19}$ for the full, the RS and the blue non-RS populations, respectively, but with $\sim40$\% to 55\% cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region $N_{200}$ exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The red sequence (RS) fraction within $R_{200}$ is $(68\pm3)$\% at $z=0.46$, varies from $\sim$55\% at $z=1$ to $\sim$80\% at $z=0.1$, and exhibits intrinsic variation among clusters of $\sim14$\%. We discuss a model that suggests the observed redshift trend in RS fraction favors a transformation timescale for infalling field galaxies to become RS galaxies of 2 to 3~Gyr., Comment: 22 pages, 14 figures, submitted to MNRAS
Published: 2016
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4. The Dark Energy Survey view of the Sagittarius stream: Discovery of two faint stellar system candidates

Author: Luque, E, Pieres, A, Santiago, B, Yanny, B, Vivas, AK, Queiroz, A, Drlica-Wagner, A, Morganson, E, Balbinot, E, Marshall, JL, Li, TS, Fausti Neto, A, da Costa, LN, Maia, MAG, Bechtol, K, Kim, AG, Bernstein, GM, Dodelson, S, Whiteway, L, Diehl, HT, Finley, DA, Abbott, T, Abdalla, FB, Allam, S, Annis, J, Benoit-Ĺevy, A, Bertin, E, Brooks, D, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Cunha, CE, D'Andrea, CB, Desai, S, Doel, P, Evrard, AE, Flaugher, B, Fosalba, P, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gutierrez, G, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Martini, P, Miquel, R, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, and Walker, AR
Subjects: globular clusters: general, galaxies: dwarf, astro-ph.GA, astro-ph.SR, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We report the discovery of two new candidate stellar systems in the constellation of Cetus using the data from the first two years of the Dark Energy Survey (DES). The objects, DES J0111-1341 and DES J0225+0304, are located at a heliocentric distance of ~25 kpc and appear to have old and metal-poor populations. Their distances to the Sagittarius orbital plane, ~1.73 kpc (DES J0111-1341) and ~0.50 kpc (DES J0225+0304), indicate that they are possibly associated with the Sagittarius dwarf stream. The half-light radius (rh ≃ 4.55 pc) and luminosity (MV ≃ +0.3) of DES J0111-1341 are consistent with it being an ultrafaint stellar cluster, while the half-light radius (rh ≃ 18.55 pc) and luminosity (MV ≃ -1.1) of DES J0225+0304 place it in an ambiguous region of size-luminosity space between stellar clusters and dwarf galaxies. Determinations of the characteristic parameters of the Sagittarius stream, metallicity spread (-2.18 ≲ [Fe/H] ≲ -0.95) and distance gradient (23 kpc ≲ D⊙ ≲ 29 kpc), within the DES footprint in the Southern hemisphere, using the same DES data, also indicate a possible association between these systems. If these objects are confirmed through spectroscopic follow-up to be gravitationally bound systems and to share a Galactic trajectory with the Sagittarius stream, DES J0111-1341 and DES J0225+0304 would be the first ultrafaint stellar systems associated with the Sagittarius stream. Furthermore, DES J0225+0304 would also be the first confirmed case of an ultrafaint satellite of a satellite.
Published: 2017

5. Joint analysis of galaxy-galaxy lensing and galaxy clustering: Methodology and forecasts for Dark Energy Survey

Author: Park, Y, Krause, E, Dodelson, S, Jain, B, Amara, A, Becker, MR, Bridle, SL, Clampitt, J, Crocce, M, Fosalba, P, Gaztanaga, E, Honscheid, K, Rozo, E, Sobreira, F, Sánchez, C, Wechsler, RH, Abbott, T, Abdalla, FB, Allam, S, Benoit-Lévy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Da Costa, LN, Depoy, DL, Desai, S, Dietrich, JP, Doel, P, Eifler, TF, Fausti Neto, A, Fernandez, E, Finley, DA, Flaugher, B, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, James, DJ, Kent, S, Kuehn, K, Kuropatkin, N, Lima, M, Maia, MAG, Marshall, JL, Melchior, P, Miller, CJ, Miquel, R, Nichol, RC, Ogando, R, Plazas, AA, Roe, N, Romer, AK, Rykoff, ES, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Vikram, V, Walker, AR, Weller, J, and Zuntz, J
Abstract: The joint analysis of galaxy-galaxy lensing and galaxy clustering is a promising method for inferring the growth function of large-scale structure. Anticipating a near future application of this analysis to Dark Energy Survey (DES) measurements of galaxy positions and shapes, we develop a practical approach to modeling the assumptions and systematic effects affecting the joint analysis of small-scale galaxy-galaxy lensing and large-scale galaxy clustering. Introducing parameters that characterize the halo occupation distribution (HOD), photometric redshift uncertainties, and shear measurement errors, we study how external priors on different subsets of these parameters affect our growth constraints. Degeneracies within the HOD model, as well as between the HOD and the growth function, are identified as the dominant source of complication, with other systematic effects being subdominant. The impact of HOD parameters and their degeneracies necessitate the detailed joint modeling of the galaxy sample that we employ. We conclude that DES data will provide powerful constraints on the evolution of structure growth in the Universe, conservatively/optimistically constraining the growth function to 7.9%/4.8% with its first-year data that cover over 1000 square degrees, and to 3.9%/2.3% with its full five-year data that will survey 5000 square degrees, including both statistical and systematic uncertainties.
Published: 2016

6. Redshift distributions of galaxies in the Dark Energy Survey Science Verification shear catalogue and implications for weak lensing

Author: Bonnett, C, Troxel, MA, Hartley, W, Amara, A, Leistedt, B, Becker, MR, Bernstein, GM, Bridle, SL, Bruderer, C, Busha, MT, Carrasco Kind, M, Childress, MJ, Castander, FJ, Chang, C, Crocce, M, Davis, TM, Eifler, TF, Frieman, J, Gangkofner, C, Gaztanaga, E, Glazebrook, K, Gruen, D, Kacprzak, T, King, A, Kwan, J, Lahav, O, Lewis, G, Lidman, C, Lin, H, MacCrann, N, Miquel, R, O'Neill, CR, Palmese, A, Peiris, HV, Refregier, A, Rozo, E, Rykoff, ES, Sadeh, I, Sánchez, C, Sheldon, E, Uddin, S, Wechsler, RH, Zuntz, J, Abbott, T, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Bauer, AH, Benoit-Lévy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Carnero Rosell, A, Carretero, J, Cunha, CE, D'Andrea, CB, Da Costa, LN, Depoy, DL, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Fausti Neto, A, Fernandez, E, Flaugher, B, Fosalba, P, Gerdes, DW, Gruendl, RA, Honscheid, K, Jain, B, James, DJ, Jarvis, M, Kim, AG, Kuehn, K, Kuropatkin, N, Li, TS, Lima, M, Maia, MAG, March, M, Marshall, JL, Martini, P, Melchior, P, Miller, CJ, Neilsen, E, Nichol, RC, Nord, B, Ogando, R, Plazas, AA, Reil, K, Romer, AK, Roodman, A, Sako, M, Sanchez, E, Santiago, B, Smith, RC, Soares-Santos, M, and Sobreira, F
Subjects: astro-ph.CO
Abstract: We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model- or machine learning-based photometric redshift methods - annz2, bpz calibrated against BCC-Ufig simulations, skynet, and tpz - are analyzed. For training, calibration, and testing of these methods, we construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evaluated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-z's. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72±0.01 over the range 0.3
Published: 2016

7. Cosmology from cosmic shear with Dark Energy Survey Science Verification data

Author: Abbott, T, Abdalla, FB, Allam, S, Amara, A, Annis, J, Armstrong, R, Bacon, D, Banerji, M, Bauer, AH, Baxter, E, Becker, MR, Benoit-Lévy, A, Bernstein, RA, Bernstein, GM, Bertin, E, Blazek, J, Bonnett, C, Bridle, SL, Brooks, D, Bruderer, C, Buckley-Geer, E, Burke, DL, Busha, MT, Capozzi, D, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Chang, C, Clampitt, J, Crocce, M, Cunha, CE, D'Andrea, CB, Da Costa, LN, Das, R, Depoy, DL, Desai, S, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Efstathiou, G, Eifler, TF, Erickson, B, Estrada, J, Evrard, AE, Fausti Neto, A, Fernandez, E, Finley, DA, Flaugher, B, Fosalba, P, Friedrich, O, Frieman, J, Gangkofner, C, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, Hartley, W, Hirsch, M, Honscheid, K, Huff, EM, Jain, B, James, DJ, Jarvis, M, Kacprzak, T, Kent, S, Kirk, D, Krause, E, Kravtsov, A, Kuehn, K, Kuropatkin, N, Kwan, J, Lahav, O, Leistedt, B, Li, TS, Lima, M, Lin, H, MacCrann, N, March, M, Marshall, JL, Martini, P, McMahon, RG, Melchior, P, Miller, CJ, Miquel, R, Mohr, JJ, Neilsen, E, Nichol, RC, Nicola, A, Nord, B, Ogando, R, Palmese, A, Peiris, HV, Plazas, AA, Refregier, A, and Roe, N
Subjects: astro-ph.CO
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 σ8(Ωm/0.3)0.5=0.81±0.06 (68% confidence), after marginalizing 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 marginalizing 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 data sets. Our uncertainties are ∼30% larger than those from CFHTLenS when we carry out a comparable analysis of the two data sets, 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 σ8(Ωm/0.3)0.5 is present regardless of the value of w.
Published: 2016

8. Discovery of two gravitationally lensed quasars in the Dark Energy Survey

Author: Agnello, A, Treu, T, Ostrovski, F, Schechter, PL, Buckley-Geer, EJ, Lin, H, Auger, MW, Courbin, F, Fassnacht, CD, Frieman, J, Kuropatkin, N, Marshall, PJ, McMahon, RG, Meylan, G, More, A, Suyu, SH, Rusu, CE, Finley, D, Abbott, T, Abdalla, FB, Allam, S, Annis, J, Banerji, M, Benoit-Levy, A, Bertin, E, Brooks, D, Burke, DL, Carnero Rosell, A, Kind, M Carrasco, Carretero, J, Cunha, CE, D'Andrea, CB, da Costa, LN, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Eifler, TF, Estrada, J, Fausti Neto, A, Flaugher, B, Fosalba, P, Gerdes, DW, Gruen, D, Gutierrez, G, Honscheid, K, James, DJ, Kuehn, K, Lahav, O, Lima, M, Maia, MAG, March, M, Marshall, JL, Martini, P, Melchior, P, Miller, CJ, Miquel, R, Nichol, RC, Ogando, R, Plazas, AA, Reil, K, Romer, AK, Roodman, A, Sako, M, Sanchez, E, Santiago, B, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Tucker, D, Walker, AR, Wechsler, RH, and Zhang, Y
Subjects: gravitational lensing: strong, methods: observational, methods: statistical, quasars: emission lines, astro-ph.GA, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract: We present spectroscopic confirmation of two new lensed quasars via dataobtained at the 6.5m Magellan/Baade Telescope. The lens candidates have beenselected from the Dark Energy Survey (DES) and WISE based on their multi-bandphotometry and extended morphology in DES images. Images of DES J0115-5244 showtwo blue point sources at either side of a red galaxy. Our long-slit dataconfirm that both point sources are images of the same quasar at $z_{s}=1.64.$The Einstein Radius estimated from the DES images is $0.51$". DES J2200+0110 isin the area of overlap between DES and the Sloan Digital Sky Survey (SDSS). Twoblue components are visible in the DES and SDSS images. The SDSS fiber spectrumshows a quasar component at $z_{s}=2.38$ and absorption compatible with Mg IIand Fe II at $z_{l}=0.799$, which we tentatively associate with the foregroundlens galaxy. The long-slit Magellan spectra show that the blue components areresolved images of the same quasar. The Einstein Radius is $0.68$"corresponding to an enclosed mass of $1.6\times10^{11}\,M_{\odot}.$ Three othercandidates were observed and rejected, two being low-redshift pairs ofstarburst galaxies, and one being a quasar behind a blue star. These firstconfirmation results provide an important empirical validation of thedata-mining and model-based selection that is being applied to the entire DESdataset.
Published: 2015

9. AUTOMATED TRANSIENT IDENTIFICATION IN THE DARK ENERGY SURVEY (vol 150, 82, 2015)

Author: Goldstein, DA, D'Andrea, CB, Fischer, JA, Foley, RJ, Gupta, RR, Kessler, R, Kim, AG, Nichol, RC, Nugent, PE, Papadopoulos, A, Sako, M, Smith, M, Sullivan, M, Thomas, RC, Wester, W, Wolf, RC, Abdalla, FB, Banerji, M, Benoit-Levy, A, Bertin, E, Brooks, D, Carnero Rosell, A, Castander, FJ, da Costa, LN, Covarrubias, R, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Fausti Neto, A, Finley, DA, Flaugher, B, Fosalba, P, Frieman, J, Gerdes, D, Gruen, D, Gruendl, RA, James, D, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Maia, MAG, Makler, M, March, M, Marshall, JL, Martini, P, Merritt, KW, Miquel, R, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, and Walker, AR
Subjects: Astronomy & Astrophysics, Astronomical and Space Sciences
Published: 2015

10. Sasquatch: Rubin Observatory metrics and telemetry service

Author: Ibsen, Jorge, Chiozzi, Gianluca, Fausti Neto, Angelo, Economou, Frossie, Reuter, Michael A., Sick, Jonathan, Allbery, Russ, and Thornton, Adam J.
Published: 2024
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11. DES science portal: Creating science-ready catalogs

Author: Fausti Neto, A., da Costa, L.N., Carnero, A., Gschwend, J., Ogando, R.L.C., Sobreira, F., Maia, M.A.G., Santiago, B.X., Rosenfeld, R., Singulani, C., Adean, C., Nunes, L.D.P., Campisano, R., Brito, R., Soares, G., Vila-Verde, G.C., Abbott, T.M.C., Abdalla, F.B., Allam, S., Benoit-Lévy, A., Brooks, D., Buckley-Geer, E., Capozzi, D., Carrasco Kind, M., Carretero, J., D’Andrea, C.B., Desai, S., Doel, P., Drlica-Wagner, A., Evrard, A.E., Fosalba, P., García-Bellido, J., Gerdes, D.W., Gruendl, R.A., Gutierrez, G., Honscheid, K., James, D.J., Jeltema, T.E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J.L., Melchior, P., Menanteau, F., Plazas, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Suchyta, E., Swanson, M.E.C., Tarle, G., and Walker, A.R.
Published: 2018
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12. DES science portal: Creating science-ready catalogs.

Author: Angelo Fausti Neto, Luiz Nicolaci da Costa, Aurelio Carnero Rosell, Julia Gschwend, R. L. C. Ogando, Flavia Sobreira, Marcio A. G. Maia, Basillio X. Santiago, Rogério Rosenfeld, C. Singulani, C. Adean, L. D. P. Nunes, Riccardo Campisano, R. Brito, G. Soares, G. C. Vila-Verde, Timothy M. C. Abbott, Filipe B. Abdalla, Sahar Allam, Aurélien Benoit-Lévy, David D. Brooks, Elizabeth Buckley-Geer, Diego Capozzi, Matias Carrasco Kind, Jorge Carretero, Chris D'Andrea, Shantanu Desai, Peter Doel, Alex Drlica-Wagner, August E. Evrard, Pablo Fosalba, Juan García-Bellido, David W. Gerdes, Robert A. Gruendl, Gaston R. Gutiérrez, Klaus Honscheid, David J. James, Tesla E. Jeltema, Kyler W. Kuehn, Steve E. E. Kuhlmann, Nikolay Kuropatkin, Ofer Lahav, Marcos Lima, Jennifer L. Marshall, Peter Melchior, Felipe Menanteau, Andreas Alejandro Plazas, Eusebio Sánchez, Victor E. Scarpine, Rafe H. Schindler, Michael S. Schubnell, Ignacio Sevilla-Noarbe, Mathew C. Smith, Robert C. Smith, Eric Suchyta, Mollye E. C. Swanson, Gregory G. Tarlé, and Alistair R. Walker
Published: 2018
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13. DES science portal: Computing photometric redshifts.

Author: Julia Gschwend, A. Carnero Rossel, Ricardo Ogando, Angelo Fausti Neto, Marcio A. G. Maia, Luiz Nicolaci da Costa, Marcos Lima, Paulo S. S. Pellegrini, Riccardo Campisano, C. Singulani, C. Adean, Christophe O. Benoist, Michel Aguena, Matias Carrasco Kind, Tamara M. Davis, J. DeVicente, William G. Hartley, Ben Hoyle, Antonella Palmese, Iftach H. Sadeh, Timothy M. C. Abbott, Filipe B. Abdalla, Sahar Allam, James Annis, Jacobo Asorey, David D. Brooks, Josh Calcino, Daniela Carollo, Francisco J. Castander, Chris D'Andrea, Shantanu Desai, August E. Evrard, Pablo Fosalba, Joshua A. Frieman, Juan García-Bellido, Karl Glazebrook, David W. Gerdes, Robert A. Gruendl, Gaston R. Gutiérrez, Samuel R. Hinton, Devon L. Hollowood, Klaus Honscheid, Janie K. Hoormann, David J. James, Kyler W. Kuehn, Nikolay Kuropatkin, Ofer Lahav, Geraint F. Lewis, Christopher E. Lidman, Huan Lin, Edward MacAulay, Jennifer L. Marshall, Peter Melchior, Ramon Miquel, Anais Möller, Andreas Alejandro Plazas, Eusebio Sánchez, Basillio X. Santiago, Victor E. Scarpine, Rafe H. Schindler, Ignacio Sevilla-Noarbe, Mathew C. Smith, Natalia E. Sommer, Eric Suchyta, Mollye E. C. Swanson, Gregory G. Tarlé, Brad E. Tucker, Douglas L. Tucker, Syed Ashraf Uddin, and Alistair R. Walker
Published: 2018
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14. Rubin Observatory Commissioning Camera: summit integration

Author: Brian Stalder, Kevin Reil, Christian Aguilar, Claudio Araya, Anthony Borstad, Boyd Bowdish, Myung Cho, Stephen Cisneros, Chuck Claver, Julio Constanzo, Giovanni Corvetto, Holger Drass, Frossie Economou, Erik Dennihy, Alan Eisner, Juan Fabrega, Angelo Fausti Neto, Merlin Fisher-Levine, Ivan Gonzalez, Ronald Harris, Diane Hascall, Justine Haupt, Josh Hoblitt, James Howard, Mike Huffer, Tim Jenness, David Jiménez Mejías, Brian Johnson, Tony Johnson, K. Simon Krughoff, Craig Lage, Travis Lange, Ming Liang, Juan Lopez, Margaux Lopez, Robert Lupton, Guido Maulen, Felipe Menanteau, Neill Mills, Glenn Morris, Freddy Munoz, Homer Neal, Douglas R. Neill, Scott Newbry, Andrei Nomerotski, Dmitry Onoprienko, Ian Ordenes, Juan Orellana, Shawn Osier, HyeYun Park, Stephen Pietrowicz, Andrés Alejandro Plazas Malagón, Gary Poczulp, Brian Qiu, Bruno Quint, Heinrich Reinking, Michael Reuter, Tiago Ribeiro, Rodrigo Rojas, Sandra Romero, Rafe Schindler, Bill Schoening, Jacques Sebag, Alysha Shugart, Cristian Silva, Ioana Sotuela, Anthony Tache, Diego Tapia, John G. Thayer, Sandrine Thomas, Roberto Tighe, Tei-Wei Tsai, Max Turri, Anthony Tyson, Luis Vergara, Christopher Walter, Oliver Wiecha, and Van Xiong
Published: 2022

15. Rubin Observatory Commissioning Camera: summit integration

Author: Stalder, Brian, primary, Reil, Kevin, additional, Aguilar, Christian, additional, Araya, Claudio, additional, Borstad, Anthony, additional, Bowdish, Boyd, additional, Cho, Myung, additional, Cisneros, Stephen, additional, Claver, Chuck, additional, Constanzo, Julio, additional, Corvetto, Giovanni, additional, Drass, Holger, additional, Economou, Frossie, additional, Dennihy, Erik, additional, Eisner, Alan, additional, Fabrega, Juan, additional, Fausti Neto, Angelo, additional, Fisher-Levine, Merlin, additional, Gonzalez, Ivan, additional, Harris, Ronald, additional, Hascall, Diane, additional, Haupt, Justine, additional, Hoblitt, Josh, additional, Howard, James, additional, Huffer, Mike, additional, Jenness, Tim, additional, Jiménez Mejías, David, additional, Johnson, Brian, additional, Johnson, Tony, additional, Krughoff, K. Simon, additional, Lage, Craig, additional, Lange, Travis, additional, Liang, Ming, additional, Lopez, Juan, additional, Lopez, Margaux, additional, Lupton, Robert, additional, Maulen, Guido, additional, Menanteau, Felipe, additional, Mills, Neill, additional, Morris, Glenn, additional, Munoz, Freddy, additional, Neal, Homer, additional, Neill, Douglas R., additional, Newbry, Scott, additional, Nomerotski, Andrei, additional, Onoprienko, Dmitry, additional, Ordenes, Ian, additional, Orellana, Juan, additional, Osier, Shawn, additional, Park, HyeYun, additional, Pietrowicz, Stephen, additional, Plazas Malagón, Andrés Alejandro, additional, Poczulp, Gary, additional, Qiu, Brian, additional, Quint, Bruno, additional, Reinking, Heinrich, additional, Reuter, Michael, additional, Ribeiro, Tiago, additional, Rojas, Rodrigo, additional, Romero, Sandra, additional, Schindler, Rafe, additional, Schoening, Bill, additional, Sebag, Jacques, additional, Shugart, Alysha, additional, Silva, Cristian, additional, Sotuela, Ioana, additional, Tache, Anthony, additional, Tapia, Diego, additional, Thayer, John G., additional, Thomas, Sandrine, additional, Tighe, Roberto, additional, Tsai, Tei-Wei, additional, Turri, Max, additional, Tyson, Anthony, additional, Vergara, Luis, additional, Walter, Christopher, additional, Wiecha, Oliver, additional, and Xiong, Van, additional
Published: 2022
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16. Cosmic shear measurements with Dark Energy Survey Science Verification data

Author: M. R. Becker, M. A. Troxel, N. MacCrann, E. Krause, T. F. Eifler, O. Friedrich, A. Nicola, A. Refregier, A. Amara, D. Bacon, G. M. Bernstein, C. Bonnett, S. L. Bridle, M. T. Busha, C. Chang, S. Dodelson, B. Erickson, A. E. Evrard, J. Frieman, E. Gaztanaga, D. Gruen, W. Hartley, B. Jain, M. Jarvis, T. Kacprzak, D. Kirk, A. Kravtsov, B. Leistedt, H. V. Peiris, E. S. Rykoff, C. Sabiu, C. Sánchez, H. Seo, E. Sheldon, R. H. Wechsler, J. Zuntz, T. Abbott, F. B. Abdalla, S. Allam, R. Armstrong, M. Banerji, A. H. Bauer, A. Benoit-Lévy, E. Bertin, D. Brooks, E. Buckley-Geer, D. L. Burke, D. Capozzi, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, M. Crocce, C. E. Cunha, C. B. D’Andrea, L. N. da Costa, D. L. DePoy, S. Desai, H. T. Diehl, J. P. Dietrich, P. Doel, A. Fausti Neto, E. Fernandez, D. A. Finley, B. Flaugher, P. Fosalba, D. W. Gerdes, R. A. Gruendl, G. Gutierrez, K. Honscheid, D. J. James, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, M. Lima, M. A. G. Maia, M. March, P. Martini, P. Melchior, C. J. Miller, R. Miquel, J. J. Mohr, R. C. Nichol, B. Nord, R. Ogando, A. A. Plazas, K. Reil, A. K. Romer, A. Roodman, M. Sako, E. Sanchez, V. Scarpine, M. Schubnell, I. Sevilla-Noarbe, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, J. Thaler, D. Thomas, V. Vikram, and A. R. Walker
Published: 2016
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17. Cosmology from cosmic shear with Dark Energy Survey Science Verification data

Author: T. Abbott, F. B. Abdalla, S. Allam, A. Amara, J. Annis, R. Armstrong, D. Bacon, M. Banerji, A. H. Bauer, E. Baxter, M. R. Becker, A. Benoit-Lévy, R. A. Bernstein, G. M. Bernstein, E. Bertin, J. Blazek, C. Bonnett, S. L. Bridle, D. Brooks, C. Bruderer, E. Buckley-Geer, D. L. Burke, M. T. Busha, D. Capozzi, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Chang, J. Clampitt, M. Crocce, C. E. Cunha, C. B. D’Andrea, L. N. da Costa, R. Das, D. L. DePoy, S. Desai, H. T. Diehl, J. P. Dietrich, S. Dodelson, P. Doel, A. Drlica-Wagner, G. Efstathiou, T. F. Eifler, B. Erickson, J. Estrada, A. E. Evrard, A. Fausti Neto, E. Fernandez, D. A. Finley, B. Flaugher, P. Fosalba, O. Friedrich, J. Frieman, C. Gangkofner, J. Garcia-Bellido, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, G. Gutierrez, W. Hartley, M. Hirsch, K. Honscheid, E. M. Huff, B. Jain, D. J. James, M. Jarvis, T. Kacprzak, S. Kent, D. Kirk, E. Krause, A. Kravtsov, K. Kuehn, N. Kuropatkin, J. Kwan, O. Lahav, B. Leistedt, T. S. Li, M. Lima, H. Lin, N. MacCrann, M. March, J. L. Marshall, P. Martini, R. G. McMahon, P. Melchior, C. J. Miller, R. Miquel, J. J. Mohr, E. Neilsen, R. C. Nichol, A. Nicola, B. Nord, R. Ogando, A. Palmese, H. V. Peiris, A. A. Plazas, A. Refregier, N. Roe, A. K. Romer, A. Roodman, B. Rowe, E. S. Rykoff, C. Sabiu, I. Sadeh, M. Sako, S. Samuroff, E. Sanchez, C. Sánchez, H. Seo, I. Sevilla-Noarbe, E. Sheldon, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, J. Thaler, D. Thomas, M. A. Troxel, V. Vikram, A. R. Walker, R. H. Wechsler, J. Weller, Y. Zhang, and J. Zuntz
Published: 2016
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18. Rubin Observatory Commissioning Camera: summit integration

Author: Evans, Christopher J., Bryant, Julia J., Motohara, Kentaro, Stalder, Brian, Reil, Kevin, Aguilar, Christian, Araya, Claudio, Borstad, Anthony, Bowdish, Boyd, Cho, Myung, Cisneros, Stephen, Claver, Chuck, Constanzo, Julio, Corvetto, Giovanni, Drass, Holger, Economou, Frossie, Dennihy, Erik, Eisner, Alan, Fabrega, Juan, Fausti Neto, Angelo, Fisher-Levine, Merlin, Gonzalez, Ivan, Harris, Ronald, Hascall, Diane, Haupt, Justine, Hoblitt, Josh, Howard, James, Huffer, Mike, Jenness, Tim, Jiménez Mejías, David, Johnson, Brian, Johnson, Tony, Krughoff, K. Simon, Lage, Craig, Lange, Travis, Liang, Ming, Lopez, Juan, Lopez, Margaux, Lupton, Robert, Maulen, Guido, Menanteau, Felipe, Mills, Neill, Morris, Glenn R., Munoz, Freddy, Neal, Homer, Neill, Douglas R., Newbry, Scott, Nomerotski, Andrei, Onoprienko, Dmitry, Ordenes, Ian, Orellana, Juan, Osier, Shawn, Park, HyeYun, Pietrowicz, Steve, Plazas, Andres, Poczulp, Gary, Qiu, Brian, Quint, Bruno, Reinking, Heinrich, Reuter, Michael, Ribeiro, Tiago, Rojas, Rodrigo, Romero, Sandra, Schindler, Rafe, Schoening, Bill, Sebag, Jacques, Shugart, Alysha, Silva, Cristian, Sotuela, Ioana, Tache, Anthony, Tapia, Diego, Thayer, John G., Thomas, Sandrine, Tighe, Roberto, Tsai, Tei-Wei, Turri, Max, Tyson, Tony, Vergara, Luis, Walter, Christopher, Wiecha, Oliver, and Xiong, Van
Published: 2022
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19. The Dark Energy Survey Data Release 1

Author: M. W. G. Johnson, M. Baumer, Tesla E. Jeltema, Eric H. Neilsen, Peter Nugent, Martin Crocce, S. Hamilton, M. Smith, Antonella Palmese, Nora Shipp, Eli S. Rykoff, F. Nogueira, L. Baruah, Daniel Gruen, Daniel Scolnic, Brian Nord, M. A. G. Maia, Brian Yanny, Matthias Klein, J. Song, R. R. Gupta, Yanxi Zhang, Arya Farahi, J. Carretero, M. March, Basilio X. Santiago, Tamara M. Davis, Shantanu Desai, Gary S. Da Costa, Jochen Weller, T. F. Eifler, Daniel A. Goldstein, J. M. Hislop, Joseph J. Mohr, R. C. Thomas, Erin Sheldon, David Brooks, M. E. C. Swanson, A. Porredon, A. Carnero Rosell, A. Saro, D. W. Gerdes, Xi Chen, Attila Kovács, Eric Morganson, R. C. Wolf, J. P. Dietrich, A. Kremin, T. M. C. Abbott, Richard G. McMahon, Jeremy Mould, J. D. Maloney, Jacobo Asorey, A. Benoit-Lévy, Hiranya V. Peiris, Ofer Lahav, Vinu Vikram, J. Lasker, E. J. Sanchez, B. Flaugher, S. Juneau, Risa H. Wechsler, Ricardo L. C. Ogando, Alistair R. Walker, A. A. Plazas, Ryan J. Foley, M. Carrasco Kind, W. C. Wester, Jennifer L. Marshall, D. L. Burke, Adam Amara, A. Scott, M.L. Sánchez, Jonathan Blazek, C. B. D'Andrea, Marcelle Soares-Santos, R. C. Smith, S. E. Kuhlmann, Ashley J. Ross, Robert C. Nichol, Ben Hoyle, G. Daues, M. Gower, C. J. Miller, M. D. Johnson, Wayne A. Barkhouse, Samuel Hinton, Felipe Menanteau, Kevin Reil, L. Nunes, F. Paz-Chinchón, David J. James, Tenglin Li, Scott Dodelson, Santiago Avila, Ann Elliott, Chihway Chang, T. Kacprzak, G. Tarle, Knut Olsen, R. Das, Ramon Miquel, Lyndsay Old, Juan Garcia-Bellido, E. Bertin, A. Roodman, Tommaso Giannantonio, Carlos E. Cunha, J. Poh, Pablo Fosalba, Enrique Gaztanaga, G. Gutierrez, J. DeRose, J. J. Thaler, Enrique Fernández, Will J. Percival, S. Allam, Paul M. Ricker, A. Pujol, Robert A. Gruendl, V. Scarpine, Andrew B. Pace, R. P. Rollins, K. Honscheid, Timothy A. McKay, Darren L. DePoy, G. Khullar, R. T. Li, Joe Zuntz, Alex Drlica-Wagner, R. Nikutta, Francisco J. Castander, C. Pond, Douglas L. Tucker, Don Petravick, W. G. Hartley, A. K. Vivas, R. Cawthon, Riccardo Campisano, D. A. Finley, D. Brout, Karl Glazebrook, Dragan Huterer, Peter Melchior, Elisabeth Krause, Mark Sullivan, Kyler Kuehn, V. C. Busti, P. Rooney, C. J. Conselice, Huan Lin, Marc Manera, J. Annis, Sebastian Bocquet, A. M. G. Koziol, M. L. Silveira, M. Fitzpatrick, Andrew R. Liddle, Alfredo Zenteno, O. Ballester, Steve Kent, Daniel Thomas, E. Buckley-Geer, Michael Troxel, A. K. Romer, Paul Martini, A. Fausti Neto, Keith Bechtol, C. Davis, J. Gschwend, Gary Bernstein, Hao-Yi Wu, Peter Doel, H. T. Diehl, J. De Vicente, J. P. Marriner, M. S. S. Gill, E. Suchyta, Niall MacCrann, August E. Evrard, Alexandre Refregier, Douglas N. Friedel, Albert Stebbins, M. Banerji, Joshua A. Frieman, I. Sevilla-Noarbe, J. A. Smith, T. McClintock, N. Kuropatkin, L. N. da Costa, Laia Cardiel-Sas, M. Sako, D. L. Hollowood, S. Serrano, David L. Nidever, Marcos Lima, Richard G. Kron, P. Lopez-Reyes, Filipe B. Abdalla, Bhuvnesh Jain, Matthew R. Becker, Flavia Sobreira, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), DES, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), NOAO Data Lab, Abbott, T. M. C., Abdalla, F. B., Allam, S., Amara, A., Annis, J., Asorey, J., Avila, S., Ballester, O., Banerji, M., Barkhouse, W., Baruah, L., Baumer, M., Bechtol, K., Becker, M. R., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Blazek, J., Bocquet, S., Brooks, D., Brout, Buckley-Geer, E., Burke, D. L., Busti, V., Campisano, R., Cardiel-Sas, L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, X., Conselice, C., Costa, G., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., Daues, G., 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., Evrard, A. E., Farahi, A., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fosalba, P., Friedel, D. N., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gower, M., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Hislop, J. M., Hollowood, D., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kacprzak, T., Kent, S., Khullar, G., Klein, M., Kovacs, A., Koziol, A. M. G., Krause, E., Kremin, A., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lasker, J., Li, T. S., Li, R. T., Liddle, A. R., Lima, M., Lin, H., López-Reyes, P., Maccrann, N., Maia, M. A. G., Maloney, J. D., Manera, M., March, M., Marriner, J., Marshall, J. L., Martini, P., Mcclintock, T., Mckay, T., Mcmahon, R. G., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morganson, E., Mould, J., Neilsen, E., Nichol, R. C., Nogueira, F., Nord, B., Nugent, P., Nunes, L., Ogando, R. L. C., Old, L., Pace, A. B., Palmese, A., Paz-Chinchón, F., Peiris, H. V., Percival, W. J., Petravick, D., Plazas, A. A., Poh, J., Pond, C., Porredon, A., Pujol, A., Refregier, A., Reil, K., Ricker, P. M., Rollins, R. P., Romer, A. K., Roodman, A., Rooney, P., Ross, A. J., Rykoff, E. S., Sako, M., Sanchez, M. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shipp, N., Silveira, M. L., Smith, M., Smith, R. C., Smith, J. A., Soares-Santos, M., Sobreira, F., Song, J., Stebbins, A., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Vivas, A. K., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Wu, H., Yanny, B., Zenteno, A., Zhang, Y., Zuntz, J., Des, Collaboration, Juneau, S., Fitzpatrick, M., Nikutta, R., Nidever, D., Olsen, K., Scott, A., and NOAO Data, Lab
Subjects: Astronomical Objects, catalog, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], techniques: image processing, Astrophysics, astronomical databases: miscellaneous, 01 natural sciences, law.invention, photometric [techniques], techniques: photometric, law, Observatory, Astrophysics - Cosmology and Nongalactic Astrophysic, 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics, image processing [techniques], observations [cosmology], sky survey, Astrophysics - Solar and Stellar Astrophysics, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, sextractor, Data release, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.SR, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, astro-ph.GA, FOS: Physical sciences, Astronomy & Astrophysics, miscellaneou [astronomical databases], Telescope, surveys, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, survey, Astronomical And Space Sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Physical Chemistry (Incl. Structural), 010308 nuclear & particles physics, Organic Chemistry, representations, Astronomy and Astrophysics, miscellaneous [astronomical databases], angular masks, Astrophysics - Astrophysics of Galaxies, Galaxy, Data set, catalogs, cosmology: observations, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: We describe the first public data release of the Dark Energy Survey, DES DR1, consisting of reduced single epoch images, coadded images, coadded source catalogs, and associated products and services assembled over the first three years of DES science operations. DES DR1 is based on optical/near-infrared imaging from 345 distinct nights (August 2013 to February 2016) by the Dark Energy Camera mounted on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. We release data from the DES wide-area survey covering ~5,000 sq. deg. of the southern Galactic cap in five broad photometric bands, grizY. DES DR1 has a median delivered point-spread function of g = 1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.90 arcsec FWHM, a photometric precision of < 1% in all bands, and an astrometric precision of 151 mas. The median coadded catalog depth for a 1.95" diameter aperture at S/N = 10 is g = 24.33, r = 24.08, i = 23.44, z = 22.69, and Y = 21.44 mag. DES DR1 includes nearly 400M distinct astronomical objects detected in ~10,000 coadd tiles of size 0.534 sq. deg. produced from ~39,000 individual exposures. Benchmark galaxy and stellar samples contain ~310M and ~ 80M objects, respectively, following a basic object quality selection. These data are accessible through a range of interfaces, including query web clients, image cutout servers, jupyter notebooks, and an interactive coadd image visualization tool. DES DR1 constitutes the largest photometric data set to date at the achieved depth and photometric precision., 30 pages, 20 Figures. Release page found at this url https://des.ncsa.illinois.edu/releases/dr1
Published: 2018

20. LSST: from Science Drivers to Reference Design and Anticipated Data Products

Author: Željko Ivezić, Steven M. Kahn, J. Anthony Tyson, Bob Abel, Emily Acosta, Robyn Allsman, David Alonso, Yusra AlSayyad, Scott F. Anderson, John Andrew, James Roger P. Angel, George Z. Angeli, Reza Ansari, Pierre Antilogus, Constanza Araujo, Robert Armstrong, Kirk T. Arndt, Pierre Astier, Éric Aubourg, Nicole Auza, Tim S. Axelrod, Deborah J. Bard, Jeff D. Barr, Aurelian Barrau, James G. Bartlett, Amanda E. Bauer, Brian J. Bauman, Sylvain Baumont, Ellen Bechtol, Keith Bechtol, Andrew C. Becker, Jacek Becla, Cristina Beldica, Steve Bellavia, Federica B. Bianco, Rahul Biswas, Guillaume Blanc, Jonathan Blazek, Roger D. Blandford, Josh S. Bloom, Joanne Bogart, Tim W. Bond, Michael T. Booth, Anders W. Borgland, Kirk Borne, James F. Bosch, Dominique Boutigny, Craig A. Brackett, Andrew Bradshaw, William Nielsen Brandt, Michael E. Brown, James S. Bullock, Patricia Burchat, David L. Burke, Gianpietro Cagnoli, Daniel Calabrese, Shawn Callahan, Alice L. Callen, Jeffrey L. Carlin, Erin L. Carlson, Srinivasan Chandrasekharan, Glenaver Charles-Emerson, Steve Chesley, Elliott C. Cheu, Hsin-Fang Chiang, James Chiang, Carol Chirino, Derek Chow, David R. Ciardi, Charles F. Claver, Johann Cohen-Tanugi, Joseph J. Cockrum, Rebecca Coles, Andrew J. Connolly, Kem H. Cook, Asantha Cooray, Kevin R. Covey, Chris Cribbs, Wei Cui, Roc Cutri, Philip N. Daly, Scott F. Daniel, Felipe Daruich, Guillaume Daubard, Greg Daues, William Dawson, Francisco Delgado, Alfred Dellapenna, Robert de Peyster, Miguel de Val-Borro, Seth W. Digel, Peter Doherty, Richard Dubois, Gregory P. Dubois-Felsmann, Josef Durech, Frossie Economou, Tim Eifler, Michael Eracleous, Benjamin L. Emmons, Angelo Fausti Neto, Henry Ferguson, Enrique Figueroa, Merlin Fisher-Levine, Warren Focke, Michael D. Foss, James Frank, Michael D. Freemon, Emmanuel Gangler, Eric Gawiser, John C. Geary, Perry Gee, Marla Geha, Charles J. B. Gessner, Robert R. Gibson, D. Kirk Gilmore, Thomas Glanzman, William Glick, Tatiana Goldina, Daniel A. Goldstein, Iain Goodenow, Melissa L. Graham, William J. Gressler, Philippe Gris, Leanne P. Guy, Augustin Guyonnet, Gunther Haller, Ron Harris, Patrick A. Hascall, Justine Haupt, Fabio Hernandez, Sven Herrmann, Edward Hileman, Joshua Hoblitt, John A. Hodgson, Craig Hogan, James D. Howard, Dajun Huang, Michael E. Huffer, Patrick Ingraham, Walter R. Innes, Suzanne H. Jacoby, Bhuvnesh Jain, Fabrice Jammes, James Jee, Tim Jenness, Garrett Jernigan, Darko Jevremović, Kenneth Johns, Anthony S. Johnson, Margaret W. G. Johnson, R. Lynne Jones, Claire Juramy-Gilles, Mario Jurić, Jason S. Kalirai, Nitya J. Kallivayalil, Bryce Kalmbach, Jeffrey P. Kantor, Pierre Karst, Mansi M. Kasliwal, Heather Kelly, Richard Kessler, Veronica Kinnison, David Kirkby, Lloyd Knox, Ivan V. Kotov, Victor L. Krabbendam, K. Simon Krughoff, Petr Kubánek, John Kuczewski, Shri Kulkarni, John Ku, Nadine R. Kurita, Craig S. Lage, Ron Lambert, Travis Lange, J. Brian Langton, Laurent Le Guillou, Deborah Levine, Ming Liang, Kian-Tat Lim, Chris J. Lintott, Kevin E. Long, Margaux Lopez, Paul J. Lotz, Robert H. Lupton, Nate B. Lust, Lauren A. MacArthur, Ashish Mahabal, Rachel Mandelbaum, Thomas W. Markiewicz, Darren S. Marsh, Philip J. Marshall, Stuart Marshall, Morgan May, Robert McKercher, Michelle McQueen, Joshua Meyers, Myriam Migliore, Michelle Miller, David J. Mills, Connor Miraval, Joachim Moeyens, Fred E. Moolekamp, David G. Monet, Marc Moniez, Serge Monkewitz, Christopher Montgomery, Christopher B. Morrison, Fritz Mueller, Gary P. Muller, Freddy Muñoz Arancibia, Douglas R. Neill, Scott P. Newbry, Jean-Yves Nief, Andrei Nomerotski, Martin Nordby, Paul O’Connor, John Oliver, Scot S. Olivier, Knut Olsen, William O’Mullane, Sandra Ortiz, Shawn Osier, Russell E. Owen, Reynald Pain, Paul E. Palecek, John K. Parejko, James B. Parsons, Nathan M. Pease, J. Matt Peterson, John R. Peterson, Donald L. Petravick, M. E. Libby Petrick, Cathy E. Petry, Francesco Pierfederici, Stephen Pietrowicz, Rob Pike, Philip A. Pinto, Raymond Plante, Stephen Plate, Joel P. Plutchak, Paul A. Price, Michael Prouza, Veljko Radeka, Jayadev Rajagopal, Andrew P. Rasmussen, Nicolas Regnault, Kevin A. Reil, David J. Reiss, Michael A. Reuter, Stephen T. Ridgway, Vincent J. Riot, Steve Ritz, Sean Robinson, William Roby, Aaron Roodman, Wayne Rosing, Cecille Roucelle, Matthew R. Rumore, Stefano Russo, Abhijit Saha, Benoit Sassolas, Terry L. Schalk, Pim Schellart, Rafe H. Schindler, Samuel Schmidt, Donald P. Schneider, Michael D. Schneider, William Schoening, German Schumacher, Megan E. Schwamb, Jacques Sebag, Brian Selvy, Glenn H. Sembroski, Lynn G. Seppala, Andrew Serio, Eduardo Serrano, Richard A. Shaw, Ian Shipsey, Jonathan Sick, Nicole Silvestri, Colin T. Slater, J. Allyn Smith, R. Chris Smith, Shahram Sobhani, Christine Soldahl, Lisa Storrie-Lombardi, Edward Stover, Michael A. Strauss, Rachel A. Street, Christopher W. Stubbs, Ian S. Sullivan, Donald Sweeney, John D. Swinbank, Alexander Szalay, Peter Takacs, Stephen A. Tether, Jon J. Thaler, John Gregg Thayer, Sandrine Thomas, Adam J. Thornton, Vaikunth Thukral, Jeffrey Tice, David E. Trilling, Max Turri, Richard Van Berg, Daniel Vanden Berk, Kurt Vetter, Francoise Virieux, Tomislav Vucina, William Wahl, Lucianne Walkowicz, Brian Walsh, Christopher W. Walter, Daniel L. Wang, Shin-Yawn Wang, Michael Warner, Oliver Wiecha, Beth Willman, Scott E. Winters, David Wittman, Sidney C. Wolff, W. Michael Wood-Vasey, Xiuqin Wu, Bo Xin, Peter Yoachim, Hu Zhan, Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), LSST, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, observational [methods], Field of view, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, law, size distribution, sagittarius dwarf galaxy, 010303 astronomy & astrophysics, stars: general, media_common, Physics, Reference design, general [stars], gamma-ray bursts, Astrophysics (astro-ph), observations [cosmology], proper motion stars, ia supernovae, astrometry, methods: observational, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Milky Way, media_common.quotation_subject, Dark matter, FOS: Physical sciences, Large Synoptic Survey Telescope, Astronomy & Astrophysics, milky-way tomography, Primary mirror, Telescope, surveys, astro-ph, 0103 physical sciences, Galaxy: general, general [Galaxy], 0105 earth and related environmental sciences, dark-energy constraints, Organic Chemistry, Astronomy and Astrophysics, Space and Planetary Science, Sky, tidal disruption events, cosmology: observations, digital sky survey, lensing power spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: (Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. LSST will be a wide-field ground-based system sited at Cerro Pach\'{o}n in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg$^2$ field of view, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$\sigma$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $\delta, Comment: 57 pages, 32 color figures, version with high-resolution figures available from https://www.lsst.org/overview
Published: 2019

21. Dark Energy Survey Year 1 Results: The Impact of Galaxy Neighbours on Weak Lensing Cosmology with im3shape

Author: S Samuroff, S L Bridle, J Zuntz, M A Troxel, D Gruen, R P Rollins, G M Bernstein, T F Eifler, E M Huff, T Kacprzak, E Krause, N MacCrann, F B Abdalla, S Allam, J Annis, K Bechtol, A Benoit-Lévy, E Bertin, D Brooks, E Buckley-Geer, A Carnero Rosell, M Carrasco Kind, J Carretero, M Crocce, C B D'Andrea, L N da Costa, C Davis, S Desai, P Doel, A Fausti Neto, B Flaugher, P Fosalba, J Frieman, J García-Bellido, D W Gerdes, R A Gruendl, J Gschwend, G Gutierrez, K Honscheid, D J James, M Jarvis, T Jeltema, D Kirk, K Kuehn, S Kuhlmann, T S Li, M Lima, M A G Maia, M March, J L Marshall, P Martini, P Melchior, F Menanteau, R Miquel, B Nord, R L C Ogando, A A Plazas, A Roodman, E Sanchez, V Scarpine, R Schindler, M Schubnell, I Sevilla-Noarbe, E Sheldon, M Smith, M Soares-Santos, F Sobreira, E Suchyta, G Tarle, D Thomas, D L Tucker, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Point spread function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmological parameters, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, gravitational lensing: weak, statistics [Galaxies], 0103 physical sciences, cosmological parameters, observations [Cosmology], 010303 astronomy & astrophysics, Weak gravitational lensing, galaxies: statistics, Physics, Number density, 010308 nuclear & particles physics, Multiplicative function, Astronomy and Astrophysics, Galaxy, Amplitude, Space and Planetary Science, cosmology: observations, Dark energy, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 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: 2018

22. Dark Energy Survey Year 1 results: curved-sky weak lensing mass map

Author: Peter Doel, H. T. Diehl, David Bacon, Niall MacCrann, C. Davis, J. Gschwend, C. B. D'Andrea, S. E. Kuhlmann, Gary Bernstein, David J. James, Daniel B. Thomas, S. Samuroff, J. Prat, Pablo Fosalba, Tesla E. Jeltema, E. Suchyta, Elisabeth Krause, K. Honscheid, T. Kacprzak, G. Gutierrez, Alex Drlica-Wagner, C. Bonnett, A. Benoit-Lévy, M. A. G. Maia, Michael Troxel, R. Cawthon, R. P. Rollins, A. A. Plazas, Daniel Gruen, E. M. Huff, Vinu Vikram, Shantanu Desai, J. Annis, Felipe Menanteau, E. Buckley-Geer, R. C. Smith, Douglas L. Tucker, Kyler Kuehn, M. D. Johnson, J. De Vicente, J. Carretero, Eli S. Rykoff, A. Alarcon, Eric H. Neilsen, I. Sevilla-Noarbe, Martin Crocce, Matt J. Jarvis, Ramon Miquel, Matthew Smith, Jack Elvin-Poole, Donnacha Kirk, B. Flaugher, A. Pujol, T. S. Li, C. Sánchez, Alistair R. Walker, J. P. Dietrich, Huan Lin, Eric J. Baxter, M. T. Busha, P. Vielzeuf, M. W. G. Johnson, A. Carnero Rosell, Don Petravick, Marcelle Soares-Santos, M. Gatti, Yanxi Zhang, Erin Sheldon, W. G. Hartley, T. N. Varga, David Brooks, W. C. Wester, Steve Kent, L. N. da Costa, Peter Melchior, Juan Garcia-Bellido, Attila Kovács, V. Scarpine, A. K. Romer, Eduardo Rozo, A. Roodman, D. L. Burke, Tommaso Giannantonio, Matthew R. Becker, Flavia Sobreira, Paul Martini, S. Allam, Robert A. Gruendl, Ricardo L. C. Ogando, Joshua A. Frieman, J. DeRose, A. Fausti Neto, Ben Hoyle, G. Tarle, Enrique Fernández, Marcos Lima, M. Sako, Markus Michael Rau, Keith Bechtol, M. March, Risa H. Wechsler, E. Bertin, Chihway Chang, Carlos E. Cunha, F. J. Castander, Enrique Gaztanaga, T. M. C. Abbott, Joseph J. Mohr, E. J. Sanchez, Juan Estrada, Joe Zuntz, B. Mawdsley, Michael Schubnell, M. Carrasco Kind, Robert C. Nichol, Filipe B. Abdalla, Bhuvnesh Jain, Ofer Lahav, Boris Leistedt, Niall Jeffrey, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, gravitational lensing: weak, surveys, 0103 physical sciences, media_common.cataloged_instance, European union, Astronomy observatory, 010303 astronomy & astrophysics, STFC, media_common, QB, Physics, 010308 nuclear & particles physics, European research, Astronomy, RCUK, Astronomy and Astrophysics, Space and Planetary Science, Research council, Fundamental physics, astro-ph.CO, Christian ministry, National laboratory, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We construct the largest curved-sky galaxy weak lensing mass map to date from the DES first-year (DES Y1) data. The map, about 10 times larger than previous work, is constructed over a contiguous $\approx1,500 $deg$^2$, covering a comoving volume of $\approx10 $Gpc$^3$. The effects of masking, sampling, and noise are tested using simulations. We generate weak lensing maps from two DES Y1 shear catalogs, Metacalibration and Im3shape, with sources at redshift $0.2, Comment: 25 pages, 19 figures, 1 table; revision with changes implemented according to journal referee
Published: 2018
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23. DES Science Portal: Computing Photometric Redshifts

Author: Paulo S. Pellegrini, J. Calcino, David J. James, E. Suchyta, August E. Evrard, Pablo Fosalba, Antonella Palmese, G. Tarle, C. Adean, Filipe B. Abdalla, Geraint F. Lewis, Tamara M. Davis, Karl Glazebrook, Douglas L. Tucker, C. Lidman, Kyler Kuehn, Marcos Lima, J. Asorey, David J. Brooks, C. Singulani, Daniela Carollo, I. Sevilla-Noarbe, J. Annis, M. Carrasco Kind, A. C. Rossel, C. B. D'Andrea, N. Kuropatkin, M. E. C. Swanson, Francisco J. Castander, L. N. da Costa, Jennifer L. Marshall, Brad E. Tucker, Flavia Sobreira, T. M. C. Abbott, Peter Melchior, D. L. Hollowood, Michel Aguena, M. Smith, V. Scarpine, A. A. Plazas, E. J. Sanchez, M. A. G. Maia, Basilio X. Santiago, Alistair R. Walker, Ricardo L. C. Ogando, I. Sadeh, S. Allam, Robert A. Gruendl, Ben Hoyle, D. W. Gerdes, Joshua A. Frieman, C. Benoist, Riccardo Campisano, Angelo Fausti Neto, J. De Vicente, S. A. Uddin, Huan Lin, K. Honscheid, Ofer Lahav, W. G. Hartley, R. H. Schindler, J. K. Hoormann, Edward Macaulay, Samuel Hinton, G. Gutierrez, N. E. Sommer, Sachin N. Desai, J. Gschwend, Ramon Miquel, Anais Möller, Juan Garcia-Bellido, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Data interface, photometry, Computer science, FOS: Physical sciences, Context (language use), computer.software_genre, 01 natural sciences, Astronomical data bases: surveys, Scientific analysis, Galaxies: distances and redshifts, surveys, Methods: data analysis, 0103 physical sciences, distances and redshifts, statistics [Galaxies], Astronomical databases: catalogs, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], data analysis [Methods], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, STFC, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, DES, Redshift, Computer Science Applications, Workflow, Space and Planetary Science, statistics, Astrophysics of Galaxies (astro-ph.GA), ddc:520, Data mining, catalogs, surveys [Astronomical databases], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], computer
Abstract: Astronomy and computing 25, 58-80 (2018). doi:10.1016/j.ascom.2018.08.008, A significant challenge facing photometric surveys for cosmological purposes is the need to produce reliable redshift estimates. The estimation of photometric redshifts (photo-s) has been consolidated as the standard strategy to bypass the high production costs and incompleteness of spectroscopic redshift samples. Training-based photo- methods require the preparation of a high-quality list of spectroscopic redshifts, which needs to be constantly updated. The photo- training, validation, and estimation must be performed in a consistent and reproducible way in order to accomplish the scientific requirements. To meet this purpose, we developed an integrated web-based data interface that not only provides the framework to carry out the above steps in a systematic way, enabling the ease testing and comparison of different algorithms, but also addresses the processing requirements by parallelizing the calculation in a transparent way for the user. This framework called the Science Portal (hereafter Portal) was developed in the context the Dark Energy Survey (DES) to facilitate scientific analysis. In this paper, we show how the Portal can provide a reliable environment to access vast datasets, provide validation algorithms and metrics, even in the case of multiple photo-s methods. It is possible to maintain the provenance between the steps of a chain of workflows while ensuring reproducibility of the results. We illustrate how the Portal can be used to provide photo- estimates using the DES first year (Y1A1) data. While the DES collaboration is still developing techniques to obtain more precise photo-s, having a structured framework like the one presented here is critical for the systematic vetting of DES algorithmic improvements and the consistent production of photo-zs in future DES releases., Published by Elsevier, Amsterdam [u.a.]
Published: 2018

24. Discovery of two gravitationally lensed quasars in the Dark Energy Survey

Author: Tim Eifler, A. Roodman, David J. James, Pablo Fosalba, Anupreeta More, Adriano Agnello, E. Bertin, I. Sevilla-Noarbe, Peter Melchior, J. Annis, A. Carnero Rosell, Philip J. Marshall, A. K. Romer, J. J. Thaler, Yanming Zhang, L. N. da Costa, Paul Martini, A. Fausti Neto, Ramon Miquel, Sherry H. Suyu, F. Ostrovski, M. Carrasco Kind, Matthew W. Auger, Flavia Sobreira, Robert C. Nichol, G. Meylan, Christopher D. Fassnacht, Shantanu Desai, A. A. Plazas, Frederic Courbin, David Brooks, M. E. C. Swanson, Gregory Tarle, Jennifer L. Marshall, M. March, Basilio X. Santiago, A. Benoit-Lévy, M. Banerji, K. Honscheid, Cristian E. Rusu, Juan Estrada, Ofer Lahav, B. Flaugher, C. B. D'Andrea, Risa H. Wechsler, Christopher J. Miller, Robert Connon Smith, Michael Schubnell, Nikolay Kuropatkin, Peter Doel, Kevin Reil, V. Scarpine, E. Buckley-Geer, Tommaso Treu, H. T. Diehl, F. B. Abdalla, G. Gutierrez, Alistair R. Walker, Marcelle Soares-Santos, Douglas L. Tucker, Kyler Kuehn, J. Carretero, J. P. Dietrich, Richard G. McMahon, Josh Frieman, D. A. Finley, Huan Lin, E. Suchyta, M. Sako, Marcio A. G. Maia, Paul L. Schechter, Daniel Gruen, Ricardo L. C. Ogando, Marcos Lima, D. L. Burke, D. W. Gerdes, S. Allam, T. M. C. Abbott, E. J. Sanchez, Carlos E. Cunha, Massachusetts Institute of Technology. Department of Physics, and Schechter, Paul L
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, astro-ph.GA, media_common.quotation_subject, statistical [methods], observational [methods], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Einstein radius, Photometry (optics), symbols.namesake, emission lines [quasars], Astrophysics::Solar and Stellar Astrophysics, STFC, Astrophysics::Galaxy Astrophysics, QB, media_common, Physics, methods: statistical, biology, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, gravitational lensing: strong, Astronomy, Astronomy and Astrophysics, Quasar, biology.organism_classification, Astrophysics - Astrophysics of Galaxies, Galaxy, quasars: emission lines, Einstein Cross, Galaxias, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), strong [gravitational lensing], astro-ph.CO, symbols, methods: observational, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present spectroscopic confirmation of two new lensed quasars via data obtained at the 6.5m Magellan/Baade Telescope. The lens candidates have been selected from the Dark Energy Survey (DES) and WISE based on their multi-band photometry and extended morphology in DES images. Images of DES J0115-5244 show two blue point sources at either side of a red galaxy. Our long-slit data confirm that both point sources are images of the same quasar at $z_{s}=1.64.$ The Einstein Radius estimated from the DES images is $0.51$". DES J2200+0110 is in the area of overlap between DES and the Sloan Digital Sky Survey (SDSS). Two blue components are visible in the DES and SDSS images. The SDSS fiber spectrum shows a quasar component at $z_{s}=2.38$ and absorption compatible with Mg II and Fe II at $z_{l}=0.799$, which we tentatively associate with the foreground lens galaxy. The long-slit Magellan spectra show that the blue components are resolved images of the same quasar. The Einstein Radius is $0.68$" corresponding to an enclosed mass of $1.6\times10^{11}\,M_{\odot}.$ Three other candidates were observed and rejected, two being low-redshift pairs of starburst galaxies, and one being a quasar behind a blue star. These first confirmation results provide an important empirical validation of the data-mining and model-based selection that is being applied to the entire DES dataset., 7 pages, 1 figure, 2 tables, MNRAS subm. This paper includes data gathered with the 6.5m Baade Telescopes located at Las Campanas Observatory, Chile. This paper has gone through internal review by the DES collaboration, FERMILAB-PUB-15-341-AE
Published: 2015

25. Galaxy Populations in Massive Galaxy Clusters to z=1.1: Color Distribution, Concentration, Halo Occupation Number and Red Sequence Fraction

Author: Alistair R. Walker, Marcelle Soares-Santos, J. Carretero, A. Fausti-Neto, A. Benoit-Lévy, Ofer Lahav, Peter Doel, Joseph J. Mohr, J. P. Dietrich, A. Saro, Shantanu Desai, R. L. C. Ogando, A. Carnero, G. Tarle, H. T. Diehl, Eduardo Rozo, C. Hennig, G. Gutierrez, Ramon Miquel, A. Zenteno, Nikhel Gupta, Jennifer L. Marshall, Brian Nord, R. C. Smith, I-Non Chiu, Sebastian Bocquet, V. Strazzullo, Eric H. Neilsen, K. Honscheid, B. Stalder, T. M. C. Abbott, Daniel Thomas, Daniel Gruen, M. Carrasco Kind, Michael McDonald, Yanxi Zhang, Tim Eifler, Vinu Vikram, David J. Brooks, S. A. Stanford, E. J. Sanchez, R. Capasso, Michael Schubnell, M. E. C. Swanson, David J. James, R. A. Bernstein, C. B. D'Andrea, Pablo Fosalba, Christian L. Reichardt, L. N. daCosta, Julie Hlavacek-Larrondo, Anthony H. Gonzalez, A. A. Plazas, E. Suchyta, August E. Evrard, E. Bertin, C. Gangkofner, F. B. Abdalla, Matthew B. Bayliss, Eli S. Rykoff, Diego Capozzi, A. K. Romer, Peter Melchior, Paul Martini, Flavia Sobreira, C. J. Miller, M. March, Basilio X. Santiago, Kyler Kuehn, I. Sevilla-Noarbe, N. Kuropatkin, Joshua A. Frieman, Robert A. Gruendl, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Hennig, C., Mohr, J. J., Zenteno, A., Desai, S., Dietrich, J. P., Bocquet, S., Strazzullo, V., Saro, A., Abbott, T. M. C., Abdalla, F. B., Bayliss, M., Benoit-Levy, A., Bernstein, R. A., Bertin, E., Brooks, D., Capasso, R., Capozzi, D., Carnero, A., Carrasco Kind, M., Carretero, J., Chiu, I., D'Andrea, C. B., Dacosta, L. N., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Fausti-Neto, A., Fosalba, P., Frieman, J., Gangkofner, C., Gonzalez, A., Gruen, D., Gruendl, R. A., Gupta, N., Gutierrez, G., Honscheid, K., Hlavacek-Larrondo, J., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., March, M., Marshall, J. L., Martini, P., Mcdonald, M., Melchior, P., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R., Plazas, A. A., Reichardt, C., Romer, A. K., Rozo, E., Rykoff, E. S., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Stalder, B., Stanford, S. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Walker, A. R., Zhang, Y., MIT Kavli Institute for Astrophysics and Space Research, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: galaxies: clusters: individual, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Virial theorem, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, clusters: general [galaxies], galaxies: formation, education, 010303 astronomy & astrophysics, evolution [galaxies], STFC, Galaxy cluster, luminosity function [galaxies], QB, Luminosity function (astronomy), Physics, education.field_of_study, clusters: individual [galaxies], 010308 nuclear & particles physics, RCUK, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies: luminosity function, South Pole Telescope, Space and Planetary Science, mass function, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), Baryon acoustic oscillations, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the galaxy populations in 74 Sunyaev Zeldovich Effect (SZE) selected clusters from the South Pole Telescope (SPT) survey that have been imaged in the science verification phase of the Dark Energy Survey (DES). The sample extends up to $z\sim 1.1$ with $4 \times 10^{14} M_{\odot}\le M_{200}\le 3\times 10^{15} M_{\odot}$. Using the band containing the 4000~\AA\ break and its redward neighbor, we study the color-magnitude distributions of cluster galaxies to $\sim m_*+2$, finding: (1) the intrinsic rest frame $g-r$ color width of the red sequence (RS) population is $\sim$0.03 out to $z\sim0.85$ with a preference for an increase to $\sim0.07$ at $z=1$ and (2) the prominence of the RS declines beyond $z\sim0.6$. The spatial distribution of cluster galaxies is well described by the NFW profile out to $4R_{200}$ with a concentration of $c_{\mathrm{g}} = 3.59^{+0.20}_{-0.18}$, $5.37^{+0.27}_{-0.24}$ and $1.38^{+0.21}_{-0.19}$ for the full, the RS and the blue non-RS populations, respectively, but with $\sim40$\% to 55\% cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region $N_{200}$ exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The red sequence (RS) fraction within $R_{200}$ is $(68\pm3)$\% at $z=0.46$, varies from $\sim$55\% at $z=1$ to $\sim$80\% at $z=0.1$, and exhibits intrinsic variation among clusters of $\sim14$\%. We discuss a model that suggests the observed redshift trend in RS fraction favors a transformation timescale for infalling field galaxies to become RS galaxies of 2 to 3~Gyr., Comment: 22 pages, 14 figures, submitted to MNRAS
Published: 2016

26. A Measurement of CMB Cluster Lensing with SPT and DES Year 1 Data

Author: I. Sevilla-Noarbe, N. Kuropatkin, J. T. Sayre, L. N. da Costa, Joshua A. Frieman, Z. Hou, Elizabeth George, N. W. Halverson, Gilbert Holder, J. Carretero, C. B. D'Andrea, S. E. Kuhlmann, W. B. Everett, E. Suchyta, Jeff McMahon, Peter Doel, Ofer Lahav, C. J. Miller, Jennifer L. Marshall, A. A. Plazas, K. Honscheid, A. K. Romer, K. Aylor, Alistair R. Walker, Paul Martini, J. P. Dietrich, Stephen Padin, K. K. Schaffer, Marcelle Soares-Santos, B. Flaugher, Tenglin Li, Scott Dodelson, Eli S. Rykoff, A. Fausti Neto, John E. Carlstrom, R. H. Schindler, A. Benoit-Lévy, T. Natoli, Chihway Chang, Carlos E. Cunha, A. T. Crites, D. Luong-Van, J. D. Hrubes, K. T. Story, H-M. Cho, T. de Haan, Joaquin Vieira, S. S. Meyer, L. M. Mocanu, Alex Drlica-Wagner, G. Tarle, V. Scarpine, Shantanu Desai, Eric J. Baxter, Adrian T. Lee, Elisabeth Krause, Lloyd Knox, Daniel Gruen, R. C. Smith, E. Bertin, Brian Nord, A. Carnero Rosell, Juan Garcia-Bellido, Matt Dobbs, Joe Zuntz, S. Patil, A. Roodman, J. Annis, Ricardo L. C. Ogando, W. G. Hartley, Tommaso Giannantonio, Daniel P. Marrone, Mathew Smith, Eduardo Rozo, C. Davis, T. M. Crawford, G. Gutierrez, J. Gschwend, Michael Troxel, Lindsey Bleem, Matt J. Jarvis, Daniel Thomas, E. Buckley-Geer, Yanxi Zhang, David J. James, A. Manzotti, David Rapetti, Z. K. Staniszewski, Felipe Menanteau, Y. Omori, Enrique Gaztanaga, Pablo Fosalba, T. M. C. Abbott, Peter Melchior, K. Vanderlinde, Kyler Kuehn, E. J. Sanchez, Martin Crocce, R. Williamson, Antony A. Stark, Bhuvnesh Jain, M. Carrasco Kind, J. E. Ruhl, W. L. Holzapfel, Flavia Sobreira, Ramon Miquel, Srinivasan Raghunathan, M. March, M. Sako, Erik Shirokoff, Joseph J. Mohr, Tesla E. Jeltema, Marcos Lima, Juan Estrada, Bradford Benson, E. M. Leitch, D. L. Burke, C. Pryke, Michael Schubnell, N. L. Harrington, Robert A. Gruendl, Christian L. Reichardt, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, SPT, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gravitational lensing: weak, weak [gravitational lensing], 0103 physical sciences, Cluster (physics), cosmic back ground radiation, clusters: general [galaxies], 010303 astronomy & astrophysics, Galaxy cluster, STFC, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, RCUK, Astronomy and Astrophysics, Redshift, Galaxy, South Pole Telescope, Space and Planetary Science, galaxies: clusters: general, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Clusters of galaxies gravitationally lens the cosmic microwave background (CMB) radiation, resulting in a distinct imprint in the CMB on arcminute scales. Measurement of this effect offers a promising way to constrain the masses of galaxy clusters, particularly those at high redshift. We use CMB maps from the South Pole Telescope Sunyaev-Zel'dovich (SZ) survey to measure the CMB lensing signal around galaxy clusters identified in optical imaging from first year observations of the Dark Energy Survey. The cluster catalog used in this analysis contains 3697 members with mean redshift of $\bar{z} = 0.45$. We detect lensing of the CMB by the galaxy clusters at $8.1\sigma$ significance. Using the measured lensing signal, we constrain the amplitude of the relation between cluster mass and optical richness to roughly $17\%$ precision, finding good agreement with recent constraints obtained with galaxy lensing. The error budget is dominated by statistical noise but includes significant contributions from systematic biases due to the thermal SZ effect and cluster miscentering., Comment: 16 pages, 5 figures; replaced to match version accepted by MNRAS
Published: 2017

27. The DES Bright Arcs Survey: Hundreds of Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey Science Verification and Year 1 Observations

Author: Joshua A. Frieman, M. E. C. Swanson, L. N. da Costa, C. B. D'Andrea, S. E. Kuhlmann, E. Suchyta, August E. Evrard, Michael Schubnell, A. Benoit-Lévy, Kevin Reil, M. Smith, Ramon Miquel, Anupreeta More, Jennifer L. Marshall, Shantanu Desai, David J. Brooks, Alistair R. Walker, Daniel Gruen, Peter Nugent, Marcelle Soares-Santos, M. Sako, Thomas E. Collett, B. Flaugher, B. Welch, D. L. Tucker, Rafe Schindler, J. P. Dietrich, F. B. Abdalla, Erin Sheldon, S. Gaitsch, Juan Garcia-Bellido, Brian Nord, Nikolay Kuropatkin, Flavia Sobreira, Hallie Gaitsch, D. W. Gerdes, E. J. Sanchez, David J. James, D. A. Finley, J. Nightingale, Daniel Thomas, Kyler Kuehn, H. T. Diehl, E. Buckley-Geer, Tenglin Li, Yanxi Zhang, Carlos E. Cunha, J. Carretero, Alex Drlica-Wagner, A. K. Romer, M. S. S. Gill, Daniel A. Goldstein, A. Pellico, A. Fausti Neto, J. Gschwend, Marcos Lima, C. Furlanetto, Basilio X. Santiago, Ricardo L. C. Ogando, M. Carrasco Kind, E. Bertin, Robert C. Nichol, A. A. Plazas, K. A. Lindgren, D. L. Burke, A. Carnero Rosell, J. Annis, S. Allam, Robert A. Gruendl, Huan Lin, G. Gutierrez, Felipe Menanteau, C. Odden, Gregory Tarle, V. Scarpine, I. Sevilla-Noarbe, Ofer Lahav, Marcio A. G. Maia, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Strong gravitational lensing, AST-1138766, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, law.invention, Particle and Plasma Physics, law, galaxies: high-redshift, 0103 physical sciences, Nuclear, 010303 astronomy & astrophysics, Galaxy cluster, STFC, ComputingMilieux_MISCELLANEOUS, QB, Physics, 010308 nuclear & particles physics, Astronomy, Molecular, RCUK, gravitational lensing: strong, Astronomy and Astrophysics, Galaxy, Lens (optics), Gravitational lens, Space and Planetary Science, Limiting magnitude, strong [gravitational lensing], Magnitude (astronomy), Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, high-redshift [galaxies], Physical Chemistry (incl. Structural)
Abstract: We report the results of searches for strong gravitational lens systems in the Dark Energy Survey (DES) Science Verification and Year 1 observations. The Science Verification data span approximately 250 sq. deg. with a median i-band limiting magnitude for extended objects (10 sigma) of 23.0. The Year 1 data span approximately 2000 sq. deg. and have an i-band limiting magnitude for extended objects (10 sigma) of 22.9. As these data sets are both wide and deep, they are particularly useful for identifying strong gravitational lens candidates. Potential strong gravitational lens candidate systems were initially identified based on a color and magnitude selection in the DES object catalogs or because the system is at the location of a previously identified galaxy cluster. Cutout images of potential candidates were then visually scanned using an object viewer and numerically ranked according to whether or not we judged them to be likely strong gravitational lens systems. Having scanned nearly 400,000 cutouts, we present 374 candidate strong lens systems, of which 348 are identified for the first time. We provide the R.A. and decl., the magnitudes and photometric properties of the lens and source objects, and the distance (radius) of the source(s) from the lens center for each system.
Published: 2017

28. The Dark Energy Survey view of the Sagittarius stream : discovery of two faint stellar system candidates

Author: Daniel Gruen, D. W. Gerdes, Alistair R. Walker, Marcelle Soares-Santos, M. A. G. Maia, Peter Doel, H. T. Diehl, Ramon Miquel, Keith Bechtol, Gregory Tarle, D. L. Burke, Daniel Thomas, Emmanuel Bertin, L. Whiteway, E. J. Sanchez, E. Luque, V. Scarpine, A. Benoit-Lévy, G. Gutierrez, A. Carnero Rosell, James Annis, A. K. Vivas, Alex Drlica-Wagner, Gary Bernstein, Eduardo Balbinot, S. Allam, Robert A. Gruendl, Eric Morganson, A. K. Romer, Tenglin Li, Anna B. A. Queiroz, Scott Dodelson, M. S. Schubnell, D. A. Finley, Alex G. Kim, I. Sevilla-Noarbe, J. Carretero, Paul Martini, David J. James, A. Fausti Neto, Daniel A. Goldstein, T. D. Abbott, Pablo Fosalba, Jennifer L. Marshall, Carlos Cunha, Flavia Sobreira, F. B. Abdalla, Brian Yanny, Shantanu Desai, Kyler Kuehn, L. N. da Costa, M. Carrasco Kind, David Brooks, M. E. C. Swanson, Basilio X. Santiago, Robert Connon Smith, Brian Nord, A. A. Plazas, E. Suchyta, Adriano Pieres, Ofer Lahav, Ricardo L. C. Ogando, B. Flaugher, C. B. D'Andrea, Nikolay Kuropatkin, A. E. Evrard, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Orbital plane, astro-ph.SR, dwarf [galaxies], [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Metallicity, astro-ph.GA, FOS: Physical sciences, Sagittarius Stream, Astrophysics, Astronomy & Astrophysics, Metalicidade, 01 natural sciences, globular clusters: general, Luminosity, Affordable and Clean Energy, 0103 physical sciences, Aglomerados globulares, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), STFC, general [globular clusters], QB, Dwarf galaxy, Physics, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Radius, galaxies: dwarf, Astrophysics - Astrophysics of Galaxies, Galáxias ativas, Galaxies dwarf, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Globular clusters general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Sagittarius, Astronomical and Space Sciences
Abstract: We report the discovery of two new candidate stellar systems in the constellation of Cetus using the data from the first two years of the Dark Energy Survey (DES). The objects, DES J0111-1341 and DES J0225+0304, are located at a heliocentric distance of ~ 25 kpc and appear to have old and metal-poor populations. Their distances to the Sagittarius orbital plane, ~ 1.73 kpc (DES J0111-1341) and ~ 0.50 kpc (DES J0225+0304), indicate that they are possibly associated with the Sagittarius dwarf stream. The half-light radius (r_h ~ 4.55 pc) and luminosity (M_V ~ +0.3) of DES J0111-1341 are consistent with it being an ultrafaint stellar cluster, while the half-light radius (r_h ~ 18.55 pc) and luminosity (M_V ~ -1.1) of DES J0225+0304 place it in an ambiguous region of size-luminosity space between stellar clusters and dwarf galaxies. Determinations of the characteristic parameters of the Sagittarius stream, metallicity spread (-2.18 < [Fe/H] < -0.95) and distance gradient (23 kpc < D_sun < 29 kpc), within the DES footprint in the Southern hemisphere, using the same DES data, also indicate a possible association between these systems. If these objects are confirmed through spectroscopic follow-up to be gravitationally bound systems and to share a Galactic trajectory with the Sagittarius stream, DES J0111-1341 and DES J0225+0304 would be the first ultrafaint stellar systems associated with the Sagittarius stream. Furthermore, DES J0225+0304 would also be the first confirmed case of an ultrafaint satellite of a satellite., 13 pages, 9 figures, 1 table
Published: 2017

29. An $r$-process enhanced star in the dwarf galaxy Tucana III

Author: Kyler Kuehn, L. N. da Costa, A. A. Plazas, Darren L. DePoy, A. Benoit-Lévy, Robert A. Gruendl, Ofer Lahav, G. Gutierrez, Shantanu Desai, E. Suchyta, B. Flaugher, R. A. Bernstein, Robert Connon Smith, V. Scarpine, J. Gschwend, Sahar S. Allam, E. Buckley-Geer, J. Carretero, David Brooks, M. E. C. Swanson, J. D. Simon, D. Q. Nagasawa, A. Carnero Rosell, David James, Alistair R. Walker, Marcelle Soares-Santos, E. J. Sanchez, James Annis, Daniel Gruen, Tenglin Li, G. Tarle, M. Carrasco Kind, Elisabeth Krause, D. W. Gerdes, Joshua A. Frieman, Tim Eifler, Daniela Carollo, Ramon Miquel, Carlos Cunha, Juan Garcia-Bellido, Flavia Sobreira, Basilio X. Santiago, Terese T. Hansen, Enrique Gaztanaga, Keith Bechtol, N. P. Kuropatkin, A. K. Romer, A. Fausti Neto, Alex Drlica-Wagner, Jennifer L. Marshall, F. B. Abdalla, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Milky Way, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), 01 natural sciences, Abundance (ecology), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Dwarf galaxy, QB, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), r-process, Halo, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Chemically peculiar stars in dwarf galaxies provide a window for exploring the birth environment of stars with varying chemical enrichment. We present a chemical abundance analysis of the brightest star in the newly discovered ultra-faint dwarf galaxy candidate Tucana III. Because it is particularly bright for a star in an ultra-faint Milky Way satellite, we are able to measure the abundance of 28 elements, including 13 neutron-capture species. This star, DES J235532.66$-$593114.9 (DES J235532), shows a mild enhancement in neutron-capture elements associated with the $r$-process and can be classified as an $r$-I star. DES J235532 is the first $r$-I star to be discovered in an ultra-faint satellite, and Tuc III is the second extremely low-luminosity system found to contain $r$-process enriched material, after Reticulum II. Comparison of the abundance pattern of DES J235532 with $r$-I and $r$-II stars found in other dwarf galaxies and in the Milky Way halo suggests a common astrophysical origin for the neutron-capture elements seen in all $r$-process enhanced stars. We explore both internal and external scenarios for the $r$-process enrichment of Tuc III and show that with abundance patterns for additional stars it should be possible to distinguish between them., 12 pages, 5 figures. Accepted for publication in ApJ
Published: 2017

30. Photometric redshifts and clustering of emission line galaxies selected jointly by DES and eBOSS

Author: Jouvel, Stéphanie, Delubac, Timothée, Comparat, Johan, Camacho Chavez, Hugo Orlando, Carnero Rosell, Aurelio, Abdalla, Filipe B., Kneib, J.P., Merson, Alexander I., Lima, Marcos Vinicius Borges Teixeira, Sobreira, Flávia, Costa, Luiz N. da, Prada, F., Zhu, Guangtun, Benoit-Lévy, Aurélien, Macorra, Axel de la, Kuropatkin, Nikolay P., Lin, H., Abbott, Timothy M. C., Allam, Sahar S., Banerji, M., Bertin, Emmanuel, Brooks, D., Capozzi, Diego, Carrasco Kind, Matías, Carretero Palacios, Jorge, Castander Serentill, Francisco Javier, Cunha, Carlos Eduardo, Desai, S., Doel, Peter, Eifler, Tim, Estrada, Juan, Fausti Neto, Angelo, Flaugher, Brenna, Fosalba Vela, Pablo, Frieman, Joshua A., Gaztañaga, Enrique, Gerdes, David W., Gruen, Daniel, Gruendl, Robert A., Gutierrez, Gaston R., Honscheid, K., James, David J., Kuehn, Kyler, Lahav, Ofer, Li, T. S., Maia, Marcio Antonio Geimba, March, Marisa Cristina, Marshall, Jennifer L., Miquel, Ramon, Ogando, Ricardo L.C., Percival, Will J., Plazas Malagón, Andrés Alejandro, Reil, Kevin, Romer, Anita K., Roodman, Aaron, Rykoff, Eli, Sako, Masao, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Scarpine, Victor Emanuel, Sevilla Noarbe, Ignacio, Soares-Santos, Marcelle, Suchyta, Eric, Tarle, Gregory, Thaler, Jon J., Thomas, D., Walker, Alistair, Zhang, Yuanyuan, and Brownstein, Joel R.
Subjects: Mapeamentos astronômicos, Fotometria astronômica, Deslocamento para o vermelho, Surveys, Espectroscopia, observations [Cosmology]
Abstract: We present the results of the first observations of the emission line galaxies (ELG) of the extended Baryon Oscillation Spectroscopic Survey. From the total 9000 targets, 4600 have been selected from the Dark Energy Survey (DES). In this subsample, the total success rate for redshifts between 0.6 and 1.2 is 71 and 68 per cent for a bright and a faint samples, respectively, including redshifts measured from a single strong emission line. The mean redshift is 0.80 for the bright and 0.87 for the faint sample, while the percentage of unknown redshifts is 15 and 13 per cent, respectively. In both cases, the star contamination is lower than 2 per cent. We evaluate how well the ELG redshifts are measured using the target selection photometry and validating with the spectroscopic redshifts measured by eBOSS. We explore different techniques to reduce the photometric redshift outliers fraction with a comparison between the template fitting, the neural networks and the random forest methods. Finally, we study the clustering properties of the DES SVA1 ELG samples. We select only the most secure spectroscopic redshift in the redshift range 0.6 < z < 1.2, leading to a mean redshift for the bright and faint sample of 0.85 and 0.90, respectively. We measure the projected angular correlation function and obtain a galaxy bias averaging on scales from 1 to 10 Mpc h−1 of 1.58 ± 0.10 for the bright sample and 1.65 ± 0.12 for the faint sample. These values are representative of a galaxy population with MB − log(h) < −20.5, in agreement with what we measure by fitting galaxy templates to the photometric data.
Published: 2017

31. Deep SOAR follow-up photometry of two Milky Way outer-halo companions discovered with Dark Energy Survey

Author: V. Scarpine, G. Tarle, Tim Eifler, J. Carretero, Peter Doel, Flavia Sobreira, Alistair R. Walker, Alex Drlica-Wagner, Daniel Gruen, Filipe B. Abdalla, M. dal Ponte, Marcelle Soares-Santos, A. Benoit-Lévy, A. Fausti Neto, Andrew B. Pace, M. A. G. Maia, D. W. Gerdes, E. J. Sanchez, S. Allam, Robert A. Gruendl, Jennifer L. Marshall, David J. Brooks, M. Carrasco Kind, Robert C. Nichol, A. Carnero Rosell, Martin Crocce, Daniel Thomas, C. Davis, Adriano Pieres, Richard G. Kron, Keith Bechtol, K. Honscheid, Basilio X. Santiago, Ramon Miquel, E. Suchyta, Eduardo Balbinot, B. Flaugher, E. Luque, Nikolay Kuropatkin, E. Bertin, J. Annis, A. A. Plazas, Anna B. A. Queiroz, G. Gutierrez, David J. James, R. H. Schindler, Juan Garcia-Bellido, I. Sevilla-Noarbe, Mathew Smith, L. N. da Costa, Kyler Kuehn, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Stellar mass, Metallicity, Milky Way, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, globular clusters: general, Luminosity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Stellar density, STFC, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, Astronomy, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Galaxy: halo, Star cluster, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We report the discovery of a new star cluster, DES 3, in the constellation of Indus, and deeper observations of the previously identified satellite DES J0222.7$-$5217 (Eridanus III). DES 3 was detected as a stellar overdensity in first-year Dark Energy Survey data, and confirmed with deeper photometry from the 4.1 metre Southern Astrophysical Research (SOAR) telescope. The new system was detected with a relatively high significance and appears in the DES images as a compact concentration of faint blue point sources. We determine that DES 3 is located at a heliocentric distance of $\sim 76\,\mathrm{kpc}$ and it is dominated by an old ($\simeq 9.8\,\mathrm{Gyr}$) and metal-poor ($\mathrm{[Fe/H]}\simeq -1.88$) population. While the age and metallicity values of DES 3 are similar to globular clusters, its half-light radius ($r_\mathrm{h}\sim 6.5\,\mathrm{pc}$) and luminosity ($M_V \sim -1.9$) are more indicative of faint star clusters. Based on the apparent angular size, DES 3, with a value of $r_\mathrm{h}\sim 0.\!^{\prime}3$, is among the smallest faint star clusters known to date. Furthermore, using deeper imaging of DES J0222.7$-$5217 taken with the SOAR telescope, we update structural parameters and perform the first isochrone modeling. Our analysis yields the first age ($\simeq 12.6\,\mathrm{Gyr}$) and metallicity ($\mathrm{[Fe/H]}\simeq -2.01$) estimates for this object. The half-light radius ($r_\mathrm{h}\sim 10.5\,\mathrm{pc}$) and luminosity ($M_V\sim -2.7$) of DES J0222.7$-$5217 suggest that it is likely a faint star cluster. The discovery of DES 3 indicates that the census of stellar systems in the Milky Way is still far from complete, and demonstrates the power of modern wide-field imaging surveys to improve our knowledge of the Galaxy's satellite population., Comment: 11 pages, 9 figures, 3 tables
Published: 2017
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32. A stellar overdensity associated with the Small Magellanic Cloud

Author: G. Gutierrez, Nicolas F. Martin, A. Benoit-Lévy, B. Flaugher, E. Luque, K. Honscheid, Nikolay Kuropatkin, Peter Doel, W. C. Wester, Noelia E. D. Noël, J. Carretero, H. T. Diehl, M. Carrasco Kind, G. Tarle, Jennifer L. Marshall, David J. James, Daniel Gruen, A. K. Romer, R. P. van der Marel, Guy S. Stringfellow, Felipe Menanteau, Ramon Miquel, T. M. C. Abbott, Gurtina Besla, M. Sako, A. Fausti Neto, Pablo Fosalba, J. Gschwend, E. J. Sanchez, C. B. D'Andrea, Douglas L. Tucker, S. Allam, Robert A. Gruendl, Kyler Kuehn, Flavia Sobreira, David Martinez-Delgado, Alex Drlica-Wagner, Keith Bechtol, Eduardo Balbinot, F. B. Abdalla, William G. Hartley, Tenglin Li, Ricardo L. C. Ogando, Carme Gallart, A. Carnero Rosell, Basilio X. Santiago, D. L. Nidever, Adriano Pieres, Carlos E. Cunha, J. Annis, M. E. C. Swanson, Shantanu Desai, R. C. Smith, Juan Garcia-Bellido, M. R. L. Cioni, E. Suchyta, A. A. Plazas, Vasily Belokurov, M. A. G. Maia, Michael Schubnell, I. Sevilla-Noarbe, L. N. da Costa, Blair C. Conn, K. A. G. Olsen, V. Scarpine, Alistair R. Walker, Marcelle Soares-Santos, S. R. Majewski, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Observatoire astronomique de Strasbourg ( ObAS ), Université de Strasbourg ( UNISTRA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Higher education, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Library science, interactions [Galaxies], 01 natural sciences, 0103 physical sciences, Magellanic Clouds, galaxies: interactions, Formacao de estrelas, 010303 astronomy & astrophysics, QB, Mapeamentos astronômicos, Physics, 010308 nuclear & particles physics, business.industry, European research, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Fundamental physics, Christian ministry, Small Magellanic Cloud, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Pequena Nuvem de Magalhães
Abstract: We report the discovery of a stellar over-density 8$^{\circ}$ north of the center of the Small Magellanic Cloud (Small Magellanic Cloud Northern Over-Density; SMCNOD) using data from the first two years of the Dark Energy Survey (DES) and the first year of the MAGellanic SatelLITEs Survey (MagLiteS). The SMCNOD is indistinguishable in age, metallicity and distance from the nearby SMC stars, being primarly composed of intermediate-age stars (6 Gyr, Z=0.001), with a small fraction of young stars (1 Gyr, Z=0.01). The SMCNOD has an elongated shape with an ellipticity of 0.6 and a size of $\sim$ 6x2 deg. It has an absolute magnitude of $M_V \cong$ -7.7, $r_h = 2.1$ kpc, and $\mu_V(r, Comment: 14 pages, 10 color figures
Published: 2017

33. Galaxy–galaxy lensing in the Dark Energy Survey Science Verification data

Author: Michael Schubnell, David Brooks, M. E. C. Swanson, I. Sevilla-Noarbe, B. Flaugher, E. Sheldon, N. Kuropatkin, J. P. Dietrich, Ashley J. Ross, Daniel Gruen, Robert Armstrong, L. N. da Costa, R. C. Smith, Peter Doel, Joseph J. Mohr, Peter Melchior, Matthew R. Becker, M. Carrasco Kind, Jennifer L. Marshall, Robert C. Nichol, H. T. Diehl, A. K. Romer, Flavia Sobreira, Shantanu Desai, Daniel Thomas, Juan Estrada, Gregory Tarle, Eduardo Rozo, D. L. Burke, Y. Fang, E. Suchyta, A. Fausti Neto, Niall MacCrann, F. B. Abdalla, M. March, C. B. D'Andrea, August E. Evrard, C. Bonnett, J. Prat, Brian Nord, Eli S. Rykoff, Alistair R. Walker, Marcelle Soares-Santos, Gary Bernstein, Enrique Gaztanaga, David J. James, Pablo Fosalba, Joseph Clampitt, Marcos Lima, Bhuvnesh Jain, E. Bertin, M. Jarvis, Robert A. Gruendl, Youngsoo Park, A. Carnero Rosell, Ofer Lahav, J. Kwan, A. A. Plazas, K. Honscheid, Vinu Vikram, V. Scarpine, Joshua A. Frieman, Michael Troxel, Kyler Kuehn, A. Benoit-Lévy, Elisabeth Krause, Martin Crocce, Ramon Miquel, C. Sánchez, P. Martini, Risa H. Wechsler, T. M. C. Abbott, E. J. Sanchez, Joe Zuntz, Jonathan Blazek, Carlos E. Cunha, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: Physics, 010308 nuclear & particles physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Strong gravitational lensing, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift survey, 01 natural sciences, Halo occupation distribution, Redshift, galaxies: haloes, Gravitational lens, gravitational lensing: weak, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, QB, Photometric redshift
Abstract: International audience; We present galaxy–galaxy lensing results from 139 deg^2 of Dark Energy Survey (DES) Science Verification (SV) data. Our lens sample consists of red galaxies, known as redMaGiC, which are specifically selected to have a low photometric redshift error and outlier rate. The lensing measurement has a total signal-to-noise ratio of 29 over scales 0.09 < R < 15 Mpc h^−1, including all lenses over a wide redshift range 0.2 < z < 0.8. Dividing the lenses into three redshift bins for this constant moving number density sample, we find no evidence for evolution in the halo mass with redshift. We obtain consistent results for the lensing measurement with two independent shear pipelines, ngmix and im3shape. We perform a number of null tests on the shear and photometric redshift catalogues and quantify resulting systematic uncertainties. Covariances from jackknife subsamples of the data are validated with a suite of 50 mock surveys. The result and systematic checks in this work provide a critical input for future cosmological and galaxy evolution studies with the DES data and redMaGiC galaxy samples. We fit a halo occupation distribution (HOD) model, and demonstrate that our data constrain the mean halo mass of the lens galaxies, despite strong degeneracies between individual HOD parameters.
Published: 2017

34. Galaxy populations in massive galaxy clusters to z = 1.1 : colour distribution, concentration, halo occupation number and red sequence fraction

Author: Hennig, C., Mohr, Joseph J., Zenteno, Alfredo, Desai, S., Dietrich, Jörg P., Bocquet, Sebastian, Strazzullo, Veronica, Saro, Alexandro, Abbott, Timothy M. C., Abdalla, Filipe B., Bayliss, Matthew B., Benoit-Lévy, Aurélien, Bernstein, Gary M., Bertin, Emmanuel, Brooks, D., Capasso, Raffaella, Capozzi, Diego, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Chiu, I. Non Tim, D'Andrea, Christopher B., Costa, Luiz N. da, Diehl, H. Thomas, Doel, Peter, Eifler, Tim, Evrard, August E., Fausti Neto, Angelo, Fosalba Vela, Pablo, Frieman, Joshua A., Gangkofner, C., Gonzalez, Anthony, Gruen, Daniel, Gruendl, Robert A., Gupta, Nayantara, Gutierrez, Gaston R., Honscheid, K., Hlavacek-Larrondo, Julie, James, David J., Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, March, Marisa Cristina, Marshall, Jennifer L., Martini, Paul, McDonald, Michael Kenneth, Melchior, Peter M., Miller, Christopher J., Miquel, Ramon, Neilsen, Eric H., Nord, Brian Dennis, Ogando, Ricardo L.C., Plazas Malagón, Andrés Alejandro, Reichardt, Christian L., Romer, Anita K., Rozo, Eduardo, Rykoff, Eli, Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Schubnell, Michael, Sevilla Noarbe, Ignacio, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Stalder, Brian, Stanford, Spencer Adam, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Thomas, D., Vikram, Vinu, Walker, Alistair, and Zhang, Yuanyuan
Subjects: Galáxias ativas, Galaxies formation, Populacoes estelares, Galaxies evolution, Galaxies clusters individual, Galaxies mass function, Galaxies luminosity function, Aglomerados globulares, Galaxies clusters general
Abstract: We study the galaxy populations in 74 Sunyaev–Zeldovich effect selected clusters from the South Pole Telescope survey, which have been imaged in the science verification phase of the Dark Energy Survey. The sample extends up to z ∼ 1.1 with 4 × 1014M ≤ M200 ≤ 3 × 1015M . Using the band containing the 4000 Å break and its redward neighbour, we study the colour–magnitude distributions of cluster galaxies to ∼m∗ + 2, finding that: (1)The intrinsic rest frame g − r colour width of the red sequence (RS) population is ∼0.03 out to z ∼ 0.85 with a preference for an increase to ∼0.07 at z = 1, and (2) the prominence of the RS declines beyond z ∼ 0.6. The spatial distribution of cluster galaxies is well described by the NFW profile out to 4R200 with a concentration of cg = 3.59+0.20 −0.18, 5.37+0.27 −0.24 and 1.38+0.21 −0.19 for the full, the RS and the blue non-RS populations, respectively, but with ∼40 per cent to 55 per cent cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region N200 exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The RS fraction within R200 is (68 ± 3) per cent at z = 0.46, varies from ∼55 per cent at z = 1 to ∼80 per cent at z = 0.1 and exhibits intrinsic variation among clusters of ∼14 per cent. We discuss a model that suggests that the observed redshift trend in RS fraction favours a transformation time-scale for infalling field galaxies to become RS galaxies of 2–3 Gyr.
Published: 2017

35. An r -process enhanced star in the dwarf galaxy Tucana III

Author: Hansen, Terese T., Simon, Josh D., Marshall, Jennifer L., Li, T. S., Carollo, Daniela, DePoy, Darren L., Nagasawa, Daniel Q., Bernstein, Rebecca A., Drlica-Wagner, Alex, Abdalla, Filipe B., Allam, Sahar S., Annis, James T., Bechtol, Keith, Benoit-Lévy, Aurélien, Brooks, D., Buckley-Geer, Elizabeth, Carnero Rosell, Aurelio, Carrasco Kind, Matías, Carretero Palacios, Jorge, Cunha, Carlos Eduardo, Costa, Luiz N. da, Desai, S., Eifler, Tim, Fausti Neto, Angelo, Flaugher, Brenna, Frieman, Joshua A., García-Bellido, Juan, Gaztañaga, Enrique, Gerdes, David W., Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia de Figueiredo, Gutierrez, Gaston R., James, David J., Krause, Elisabeth, Kuehn, Kyler, Kuropatkin, Nikolay P., Lahav, Ofer, Miquel, Ramon, Plazas Malagón, Andrés Alejandro, Romer, Anita K., Sanchez-Alvaro, Eusebio, Santiago, Basilio Xavier, Scarpine, Victor Emanuel, Smith, Robert Christopher, Soares-Santos, Marcelle, Sobreira, Flávia, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Walker, Alistair, and DES Collaboration
Subjects: dwarf [Galaxies], Readable tables, Nucleosíntese, Captura radioativa de nêutrons, abundances [Stars], abundances [galaxies], Metalicidade, Composicao estelar, machine [Supporting material], chemically peculiar [Stars]
Abstract: Chemically peculiar stars in dwarf galaxies provide a window for exploring the birth environment of stars with varying chemical enrichment. We present a chemical abundance analysis of the brightest star in the newly discovered ultra-faint dwarf galaxy candidate Tucana III. Because it is particularly bright for a star in an ultra-faint Milky Way (MW) satellite, we are able to measure the abundance of 28 elements, including 13 neutron-capture species. This star, DES J235532.66−593114.9 (DES J235532), shows a mild enhancement in neutron-capture elements associated with the r-process and can be classified as an r-I star. DES J235532 is the first r-I star to be discovered in an ultra-faint satellite, and Tuc III is the second extremely low-luminosity system found to contain rprocess enriched material, after Reticulum II. Comparison of the abundance pattern of DES J235532 with r-I and r-II stars found in other dwarf galaxies and in the MW halo suggests a common astrophysical origin for the neutron-capture elements seen in all r-process enhanced stars. We explore both internal and external scenarios for the r-process enrichment of Tuc III and show that with abundance patterns for additional stars, it should be possible to distinguish between them.
Published: 2017

36. Cosmic Voids and Void Lensing in the Dark Energy Survey Science Verification Data

Author: C. B. D'Andrea, A. A. Plazas, P. Vielzeuf, A. Benoit-Lévy, Jennifer L. Marshall, W. G. Hartley, F. B. Abdalla, Martin Crocce, Peter Doel, M. Carrasco Kind, M. Jarvis, G. Gutierrez, H. T. Diehl, K. Honscheid, Jochen Weller, R. C. Smith, Erin Sheldon, David Brooks, Enrique Gaztanaga, Michael Schubnell, Dragan Huterer, T. M. C. Abbott, J. Carretero, Eli S. Rykoff, E. J. Sanchez, Peter Melchior, J. P. Dietrich, Risa H. Wechsler, Adam Amara, Kevin Reil, Joseph DeRose, A. Carnero Rosell, David J. James, Attila Kovács, J. Annis, Kyler Kuehn, M. A. G. Maia, Nico Hamaus, Gary Bernstein, Pablo Fosalba, Ofer Lahav, Carlos E. Cunha, B. Flaugher, Juan Garcia-Bellido, Joe Zuntz, Bhuvnesh Jain, Eduardo Rozo, Flavia Sobreira, Shantanu Desai, Gregory Tarle, Robert A. Gruendl, E. Bertin, R. A. Bernstein, Joshua A. Frieman, E. Suchyta, August E. Evrard, C. Bonnett, Elisabeth Krause, I. Sevilla-Noarbe, L. N. da Costa, Ramon Miquel, C. Sánchez, Seshadri Nadathur, A. K. Romer, A. Fausti Neto, Joseph Clampitt, Marcos Lima, Alistair R. Walker, Marcelle Soares-Santos, Daniel Thomas, E. Buckley-Geer, Daniel Gruen, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Barcelona Inst Sci & Technol, Univ Penn, Ctr Invest Energet Medioambientales & Tecnol CIEM, Univ Portsmouth, Stanford Univ, SLAC Natl Accelerator Lab, Univ Munich, Univ Michigan, ETH, UCL, Inst Catalana Rec & Estudis Avancats, Univ Arizona, Brookhaven Natl Lab, Univ Manchester, Natl Opt Astron Observ, Rhodes Univ, Fermilab Natl Accelerator Lab, CNRS, UPMC Univ Paris 06, Carnegie Observ, Lab Interinst Astron LIneA, Observ Nacl, Univ Illinois, Natl Ctr Supercomp Applicat, CSIC, Univ Southampton, Excellence Cluster Univ, Univ Chicago, Ohio State Univ, Australian Astron Observ, Universidade de São Paulo (USP), Texas A&M Univ, Princeton Univ, CALTECH, Univ Sussex, Universidade Estadual Paulista (Unesp), Oak Ridge Natl Lab, and Max Planck Inst Extraterr Phys
Subjects: Cosmology and Gravitation, Void (astronomy), Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gravitational lensing: weak, weak [gravitational lensing], 0103 physical sciences, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, QB, weak, Cosmology: observations, Large-scale structure of Universe [Gravitational lensing], Physics, 010308 nuclear & particles physics, RCUK, Astronomy, Astronomy and Astrophysics, Radius, observations [cosmology], Galaxy, Redshift, Space and Planetary Science, cosmology: observations, astro-ph.CO, Dark energy, large-scale structure of Universe, Giant Void, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: osmic voids are usually identified in spectroscopic galaxy surveys, where 3D information about the large-scale structure of the Universe is available. Although an increasing amount of photometric data is being produced, its potential for void studies is limited since photometric redshifts induce line-of-sight position errors of ≥50 Mpc h−1 which can render many voids undetectable. We present a new void finder designed for photometric surveys, validate it using simulations, and apply it to the high-quality photo-z redMaGiC galaxy sample of the DES Science Verification data. The algorithm works by projecting galaxies into 2D slices and finding voids in the smoothed 2D galaxy density field of the slice. Fixing the line-of-sight size of the slices to be at least twice the photo-z scatter, the number of voids found in simulated spectroscopic and photometric galaxy catalogues is within 20 per cent for all transverse void sizes, and indistinguishable for the largest voids (Rv ≥ 70 Mpc h−1). The positions, radii, and projected galaxy profiles of photometric voids also accurately match the spectroscopic void sample. Applying the algorithm to the DES-SV data in the redshift range 0.2 < z < 0.8, we identify 87 voids with comoving radii spanning the range 18–120 Mpc h−1, and carry out a stacked weak lensing measurement. With a significance of 4.4σ, the lensing measurement confirms that the voids are truly underdense in the matter field and hence not a product of Poisson noise, tracer density effects or systematics in the data. It also demonstrates, for the first time in real data, the viability of void lensing studies in photometric surveys., Monthly Notices of the Royal Astronomical Society, 465 (1), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711
Published: 2017

37. Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters

Author: Ricardo L. C. Ogando, Martin Crocce, A. Roodman, David J. Brooks, Robert Armstrong, A. A. Plazas, Joseph J. Mohr, Jochen Weller, Mark Brodwin, Diego Capozzi, W. L. Holzapfel, M. A. G. Maia, J. J. Thaler, E. Bertin, C. Gangkofner, A. Saro, David J. James, T. M. C. Abbott, Ofer Lahav, M. Carrasco Kind, E. Fernandez, R. Covarrubias, Robert Connon Smith, Darren L. DePoy, Alistair R. Walker, Pablo Fosalba, Marcelle Soares-Santos, R. Capasso, V. Strazzullo, E. J. Sanchez, Michael McDonald, B. Stalder, Gary Bernstein, Risa H. Wechsler, V. Upadhyay, Enrique Gaztanaga, Vinu Vikram, Huan Lin, Lindsey Bleem, T. M. Crawford, John E. Carlstrom, Peter Melchior, Tianjun Li, Shantanu Desai, Sebastian Bocquet, Brian Nord, Bhuvnesh Jain, Peter Doel, J. P. Dietrich, A. von der Linden, Bradford Benson, Daniel Thomas, M. E. C. Swanson, I. Sevilla, E. Buckley-Geer, Michael Schubnell, F. B. Abdalla, Scott Dodelson, A. Benoit-Lévy, Carlos E. Cunha, T. de Haan, H. T. Diehl, Jennifer L. Marshall, Christian L. Reichardt, D. L. Burke, Tim Eifler, Antony A. Stark, A. H. Bauer, S. Allam, Robert A. Gruendl, Alfredo Zenteno, Flavia Sobreira, I-Non Chiu, C. Hennig, B. Flaugher, C. B. D'Andrea, M. March, Ramon Miquel, Eduardo Rozo, K. E. Ziegler, A. K. Romer, Paul Martini, W. C. Wester, A. Fausti Neto, K. Honscheid, Christopher J. Miller, Matthew B. Bayliss, Eli S. Rykoff, N. Kuropatkin, L. N. da Costa, M. Banerji, Joshua A. Frieman, A. Carnero Rosell, M. Sako, Douglas L. Tucker, Kyler Kuehn, Gregory Tarle, Nikhel Gupta, E. Suchyta, August E. Evrard, Daniel Gruen, D. W. Gerdes, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, McDonald, Michael A., Saro, A., Bocquet, S., Rozo, E., Benson, B. A., Mohr, J., Rykoff, E. S., Soares-Santos, M., Bleem, L., Dodelson, S., Melchior, P., Sobreira, F., Upadhyay, V., Weller, J., Abbott, T., Abdalla, F. B., Allam, S., Armstrong, R., Banerji, M., Bauer, A. H., Bayliss, M., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Brodwin, M., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Capasso, R., Capozzi, D., Carnero Rosell, A., Carrasco Kind, M., Chiu, I., Covarrubias, R., Crawford, T. M., Crocce, M., D'Andrea, C. B., da Costa, L. N., Depoy, D. L., Desai, S., de Haan, T., Diehl, H. T., Dietrich, J. P., Doel, P., Cunha, C. E, Eifler, T. F., Evrard, A. E., Fausti Neto, A., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Gangkofner, C., Gaztanaga, E., Gerdes, D., Gruen, D., Gruendl, R. A., Gupta, N., Hennig, C., Holzapfel, W. L., Honscheid, K., Jain, B., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, Paul, Mcdonald, M., Miller, C. J., Miquel, R., Nord, B., Ogando, R., Plazas, A. A., Reichardt, C. L., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Schubnell, M., Sevilla, I., Smith, R. C., Stalder, B., Stark, A. A., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Tucker, D., Vikram, V., von der Linden, A., Walker, A. R., Wechsler, R. H., Wester, W., Zenteno, A., and Ziegler, K. E.
Subjects: statistics [galaxies], Large-scale structure of Universe, Galaxies: abundances, Astrophysics, abundance [Galaxies], miscellaneous [cosmology], Lambda, Catalogue, 01 natural sciences, haloe [Galaxies], clusters: general [galaxies], 010303 astronomy & astrophysics, catalogues, QB, Physics, education.field_of_study, Sigma, haloes [galaxies], South Pole Telescope, astro-ph.CO, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Galaxies: statistics, Cosmology: miscellaneous, Population, FOS: Physical sciences, Methods: data analysis, abundances [galaxies], 0103 physical sciences, data analysis [methods], Cluster (physics), miscellaneou [Cosmology], Galaxies: haloes, education, STFC, Galaxy cluster, Catalogues, Galaxies: clusters: general, Astronomy and Astrophysics, Space and Planetary Science, statistic [Galaxies], 010308 nuclear & particles physics, RCUK, Astronomy, Astronomy and Astrophysic, Redshift, data analysi [Methods], Dark energy
Abstract: We cross-match galaxy cluster candidates selected via their Sunyaev–Zel'dovich effect (SZE) signatures in 129.1 deg[superscript 2] of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey science verification data. We identify 25 clusters between 0.1 ≲ z ≲ 0.8 in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness λ-mass relation with the following function 〈ln λ|M500〉 ∝ Bλln M500 + Cλln E(z) and use SPT-SZ cluster masses and RM richnesses λ to constrain the parameters. We find Bλ=1.14[superscript +0.21][subscript −0.18 and Cλ=0.73[superscript +0.77][subscript −0.75]. The associated scatter in mass at fixed richness is σlnM|λ=0.18[superscript +0.08][subscript −0.05] at a characteristic richness λ = 70. We demonstrate that our model provides an adequate description of the matched sample, showing that the fraction of SPT-SZ-selected clusters with RM counterparts is consistent with expectations and that the fraction of RM-selected clusters with SPT-SZ counterparts is in mild tension with expectation. We model the optical-SZE cluster positional offset distribution with the sum of two Gaussians, showing that it is consistent with a dominant, centrally peaked population and a subdominant population characterized by larger offsets. We also cross-match the RM catalogue with SPT-SZ candidates below the official catalogue threshold significance ξ = 4.5, using the RM catalogue to provide optical confirmation and redshifts for 15 additional clusters with ξ ∈ [4, 4.5]., Kavli Foundation, Gordon and Betty Moore Foundation (Grant GBMF 947)
Published: 2015

38. Search for gamma-ray emission from des dwarf spheroidal galaxy candidates with Fermi-LAT data

Author: Drlica-Wagner, Albert, Bechtol, Wood, Strigari, nchez-Conde, Baldini, Essig, Cohen-Tanugi, Anderson, Bellazzini, Bloom, E. D., Caputo, Cecchi, Charles, Chiang, de Angelis, Funk, Fusco, Gargano, Giglietto, Giordano, Guiriec, Gustafsson, Kuss, Loparco, Lubrano, Mirabal, Mizuno, Morselli, Ohsugi, Orlando E, Persic, Rainò, Sehgal, Spada, Suson, D. J., Zaharijas, Zimmer, Fermi-LAT Collaboration, Abbott, Allam, Balbinot, Bauer, A. H., Benoit-Lé, Bernstein, R. A., G. M., Bertin, Brooks, Buckley-Geer, Burke, D. L., Carnero Rosell, Castander, F. J., Covarrubias, D'Andrea, C. B., da Costa, L. N., DePoy, Desai, Diehl, H. T., Cunha, C. E., Eifler, T. F., Estrada, Evrard, A. E., Fausti Neto, Fernandez, Finley, D. A., Flaugher, Frieman, Gaztanaga, Gerdes, Gruen, Gruendl, Gutierrez, Honscheid, Jain, James, Jeltema, Kent, Kron, Kuehn, Kuropatkin, Lahav, T. S., Luque, Maia, M. A. G., Makler, March, Marshall, Martini, Merritt, K. W., Miller, Miquel, Mohr, Neilsen, Nord, Ogando, Peoples, Petravick, Pieres, Plazas, A. A., Queiroz, Romer, A. K., Roodman, Rykoff, E. S., Sako, Sanchez, Santiago, Scarpine, Schubnell, Sevilla, Smith, R. C., Soares-Santos, Sobreira, Suchyta, Swanson, M. E. C., Tarle, Thaler, Thomas, Tucker, Walker, A. R., Wechsler, R. H., Wester, Williams, Yanny, Zuntz, The DES Collaboration, Drlica-Wagner, Albert, Bechtol, Wood, Strigari, Sá, nchez-Conde, Baldini, Essig, Cohen-Tanugi, Anderson, Bellazzini, Bloom, E., D., Caputo, Cecchi, Charles, Chiang, De, Angeli, Funk, Fusco, Gargano, Giglietto, Giordano, Guiriec, Gustafsson, Kuss, Loparco, Lubrano, Mirabal, Mizuno, Morselli, Ohsugi, Orlando, E, Persic, Rainò, Sehgal, Spada, Suson, D., J., Zaharijas, Zimmer, Fermi-LAT, Collaboration, Abbott, Allam, Balbinot, Bauer, A., H., Benoit-Lé, Vy, Bernstein, R., A., G., M., Bertin, Brooks, Buckley-Geer, Burke, D., L., Carnero, Rosell, Castander, F., J., Covarrubias, D'Andrea, C., B., Da, Costa, L., N., Depoy, Desai, Diehl, H., T., Cunha, C., E., Eifler, T., F., Estrada, Evrard, A., E., Fausti, Neto, Fernandez, Finley, D., A., Flaugher, Frieman, Gaztanaga, Gerdes, Gruen, Gruendl, Gutierrez, Honscheid, Jain, James, Jeltema, Kent, Kron, Kuehn, Kuropatkin, Lahav, Li, T., S., Luque, Maia, M. A., G., Makler, March, Marshall, Martini, Merritt, K., W., Miller, Miquel, Mohr, Neilsen, Nord, Ogando, Peoples, Petravick, Pieres, Plazas, A., A., Queiroz, Romer, A., K., Roodman, Rykoff, E., S., Sako, Sanchez, Santiago, Scarpine, Schubnell, Sevilla, Smith, R., C., Soares-Santos, Sobreira, Suchyta, Swanson, M. E., C., Tarle, Thaler, Thomas, Tucker, Walker, A., R., Wechsler, R., H., Wester, Williams, Yanny, Zuntz, The DES, Collaboration, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, DES, and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)
Subjects: dwarf [galaxies], Astrophysics, thermal, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Satellite galaxy, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], dark energy, white dwarf, QB, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, galaxies: dwarf, dark matter, gamma rays: galaxies, Local Group, Space and Planetary Science, Astronomy and Astrophysics, gamma ray: emission, Astrophysics - High Energy Astrophysical Phenomena, Cosmology and Gravitation, Milky Way, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, GLAST, cross section: annihilation, dark matter: halo, galaxie [gamma rays], STFC, Astrophysics::Galaxy Astrophysics, hep-ex, RCUK, dark matter: annihilation, Astrophysics - Astrophysics of Galaxies, Dwarf spheroidal galaxy, Dark matter halo, Astrophysics of Galaxies (astro-ph.GA), Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract: Due to their proximity, high dark-matter content, and apparent absence of non-thermal processes, Milky Way dwarf spheroidal satellite galaxies (dSphs) are excellent targets for the indirect detection of dark matter. Recently, eight new dSph candidates were discovered using the first year of data from the Dark Energy Survey (DES). We searched for gamma-ray emission coincident with the positions of these new objects in six years of Fermi Large Area Telescope data. We found no significant excesses of gamma-ray emission. Under the assumption that the DES candidates are dSphs with dark matter halo properties similar to the known dSphs, we computed individual and combined limits on the velocity-averaged dark matter annihilation cross section for these new targets. If the estimated dark-matter content of these dSph candidates is confirmed, they will constrain the annihilation cross section to lie below the thermal relic cross section for dark matter particles with masses < 20 GeV annihilating via the b-bbar or tau+tau- channels., 9 pages, 4 figures, 1 table. Updated to published version. Readers may be interested in the related work by Ackermann et al. arXiv:1503.02641 (The Fermi-LAT Collaboration), Bechtol, Drlica-Wagner, et al. arXiv:1503.02584 (The DES Collaboration), and Koposov, Belokurov, Torrealba, & Evans arXiv:1503.02079
Published: 2015

39. Dark energy survey operations: years 4 and 5

Author: Gruendl, Robert A., primary, Tucker, Douglas L., primary, Bocquet, Sebastian, primary, Ferte, Agnes, primary, Friswell, Indiarose, primary, Furnell, Kate E., primary, Khullar, Gourav, primary, Kron, Richard, primary, Kuropatkin, Nikolay, primary, Lasker, James, primary, Manera, Marc, primary, March, Marisa, primary, Medford, Michael, primary, Menanteau, Felipe, primary, Mohammed, Irshad, primary, Monroy, Martin, primary, Moraes, Bruno, primary, Morganson, Eric, primary, Muir, Jessica, primary, Murphy, Martin, primary, Nord, Brian, primary, Pace, Anthony, primary, Palmese, Antonella, primary, Park, Youngsoo, primary, Paz-Chinchon, Francisko, primary, Pereira, Maria E., primary, Petravick, Donald, primary, Plazas, Andres, primary, Poh, Jason, primary, Prochaska, Travis, primary, Sako, Masao, primary, Sauseda, Marcus, primary, Scolnic, Daniel, primary, Secco, Lucas, primary, Sevilla-Noarbe, Ignacio, primary, Shipp, Nora, primary, Smith, John A., primary, Soergel, Bjeorn, primary, Stebbins, Albert, primary, Story, Kyle, primary, Stringer, Katelyn, primary, Tarsitano, Ferderica, primary, Thomas, Benjamin, primary, Vivas, Kathy, primary, Wang, Mei-yu, primary, Weaverdyck, Curtis, primary, Weaverdyck, Noah, primary, wester, William, primary, Wethers, Clare, primary, Wilkenson, Reece, primary, Wu, Hao-Yi, primary, Yanny, Brian, primary, Zenteno, Alfredo, primary, Zhang, Yuanyuan, primary, Diehl, H. Thomas, primary, Neilsen, Eric, primary, Marshall, Jennifer L., primary, DePoy, Darren L., primary, Romer, A. Kathy, primary, Abbott, Timothy M., primary, Soares-Santos, Marcelle, primary, Allam, Sahar, primary, Walker, Alistair R., primary, Kent, Stephen M., primary, Honscheid, Klaus, primary, Roodman, Aaron, primary, Lathrop, Andrew G., primary, Reil, Kevin, primary, Li, Ting S., primary, Elliott, Anne E., primary, Alvarez, Otto, primary, Annis, James, primary, Balbinot, Eduardo, primary, Bhargava, Sunayana, primary, Bechtol, Keith, primary, Bernstein, Gary, primary, Bhatawdekar, Rachana, primary, Brout, Dillon, primary, Capasso, Raffaella, primary, Cawthon, Ross, primary, Chang, Chihway, primary, Cook, Erika, primary, Conselice, Chris, primary, Cruz, Jamie, primary, D'Andrea, Chris, primary, da Costa, Luiz, primary, Das, Rutuparna, primary, Drlica-Wagner, Alex, primary, Everett, Spencer W., primary, Frieman, Josh, primary, Fausti-Neto, Angelo, primary, Gelman, Landon P., primary, Gerdes, David W., primary, Gill, Mandeep S., primary, Goldstein, Daniel A., primary, Gruen, Daniel, primary, Gulledge, Deborah J., primary, Hamilton, Stephanie, primary, Hollowood, Devon, primary, James, David J., primary, Johnson, Michael D., primary, Johnson, Margaret W., primary, Kessler, Richard S., primary, Kovacs, Eve, primary, and Kremin, Anthony, primary
Published: 2018
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40. Deep SOAR follow-up photometry of two Milky Way outer-halo companions discovered with Dark Energy Survey

Author: Luque, E, primary, Santiago, B, additional, Pieres, A, additional, Marshall, J L, additional, Pace, A B, additional, Kron, R, additional, Drlica-Wagner, A, additional, Queiroz, A, additional, Balbinot, E, additional, dal Ponte, M, additional, Fausti Neto, A, additional, da Costa, L N, additional, Maia, M A G, additional, Walker, A R, additional, Abdalla, F B, additional, Allam, S, additional, Annis, J, additional, Bechtol, K, additional, Benoit-Lévy, A, additional, Bertin, E, additional, Brooks, D, additional, Carnero Rosell, A, additional, Carrasco Kind, M, additional, Carretero, J, additional, Crocce, M, additional, Davis, C, additional, Doel, P, additional, Eifler, T F, additional, Flaugher, B, additional, García-Bellido, J, additional, Gerdes, D W, additional, Gruen, D, additional, Gruendl, R A, additional, Gutierrez, G, additional, Honscheid, K, additional, James, D J, additional, Kuehn, K, additional, Kuropatkin, N, additional, Miquel, R, additional, Nichol, R C, additional, Plazas, A A, additional, Sanchez, E, additional, Scarpine, V, additional, Schindler, R, additional, Sevilla-Noarbe, I, additional, Smith, M, additional, Soares-Santos, M, additional, Sobreira, F, additional, Suchyta, E, additional, Tarle, G, additional, and Thomas, D, additional
Published: 2018
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41. Dark Energy Survey Year 1 results: the impact of galaxy neighbours on weak lensing cosmology with im3shape

Author: Samuroff, S, primary, Bridle, S L, additional, Zuntz, J, additional, Troxel, M A, additional, Gruen, D, additional, Rollins, R P, additional, Bernstein, G M, additional, Eifler, T F, additional, Huff, E M, additional, Kacprzak, T, additional, Krause, E, additional, MacCrann, N, additional, Abdalla, F B, additional, Allam, S, additional, Annis, J, additional, Bechtol, K, additional, Benoit-Lévy, A, additional, Bertin, E, additional, Brooks, D, additional, Buckley-Geer, E, additional, Carnero Rosell, A, additional, Carrasco Kind, M, additional, Carretero, J, additional, Crocce, M, additional, D'Andrea, C B, additional, da Costa, L N, additional, Davis, C, additional, Desai, S, additional, Doel, P, additional, Fausti Neto, A, additional, Flaugher, B, additional, Fosalba, P, additional, Frieman, J, additional, García-Bellido, J, additional, Gerdes, D W, additional, Gruendl, R A, additional, Gschwend, J, additional, Gutierrez, G, additional, Honscheid, K, additional, James, D J, additional, Jarvis, M, additional, Jeltema, T, additional, Kirk, D, additional, Kuehn, K, additional, Kuhlmann, S, additional, Li, T S, additional, Lima, M, additional, Maia, M A G, additional, March, M, additional, Marshall, J L, additional, Martini, P, additional, Melchior, P, additional, Menanteau, F, additional, Miquel, R, additional, Nord, B, additional, Ogando, R L C, additional, Plazas, A A, additional, Roodman, A, additional, Sanchez, E, additional, Scarpine, V, additional, Schindler, R, additional, Schubnell, M, additional, Sevilla-Noarbe, I, additional, Sheldon, E, additional, Smith, M, additional, Soares-Santos, M, additional, Sobreira, F, additional, Suchyta, E, additional, Tarle, G, additional, Thomas, D, additional, and Tucker, D L, additional
Published: 2017
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42. SEARCHING FOR DARK MATTER ANNIHILATION IN RECENTLY DISCOVERED MILKY WAY SATELLITES WITH FERMI-LAT

Author: Albert, A., Anderson, Brandon, Bechtol, K., Drlica-Wagner, A., Meyer, Manuel, Sánchez-Conde, Miguel, Strigari, L., Wood, M., Abbott, T. M. C., Abdalla, F. B., Benoit-Levy, A., Bernstein, G. M., Bernstein, R. A., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., 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., Fausti Neto, A., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Honscheid, K., James, D. J., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Rykoff, E. S., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., Walker, A. R., Wechsler, R. H., Albert, A., Anderson, Brandon, Bechtol, K., Drlica-Wagner, A., Meyer, Manuel, Sánchez-Conde, Miguel, Strigari, L., Wood, M., Abbott, T. M. C., Abdalla, F. B., Benoit-Levy, A., Bernstein, G. M., Bernstein, R. A., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., 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., Fausti Neto, A., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Honscheid, K., James, D. J., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Rykoff, E. S., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., Walker, A. R., and Wechsler, R. H.
Abstract: We search for excess gamma-ray emission coincident with the positions of confirmed and candidate Milky Way satellite galaxies using six years of data from the Fermi Large Area Telescope (LAT). Our sample of 45 stellar systems includes 28 kinematically confirmed dark-matter-dominated dwarf spheroidal galaxies (dSphs) and 17 recently discovered systems that have photometric characteristics consistent with the population of known dSphs. For each of these targets, the relative predicted gamma-ray flux due to dark matter annihilation is taken from kinematic analysis if available, and estimated from a distance-based scaling relation otherwise, assuming that the stellar systems are DM-dominated dSphs. LAT data coincident with four of the newly discovered targets show a slight preference (each similar to 2 sigma local) for gamma-ray emission in excess of the background. However, the ensemble of derived gamma-ray flux upper limits for individual targets is consistent with the expectation from analyzing random blank-sky regions, and a combined analysis of the population of stellar systems yields no globally significant excess (global significance < 1 sigma). Our analysis has increased sensitivity compared to the analysis of 15 confirmed dSphs by Ackermann et al. The observed constraints on the DM annihilation cross section are statistically consistent with the background expectation, improving by a factor of similar to 2 for large DM masses (m(DM, b<(b)over bar>) greater than or similar to 1 TeV and m(DM, tau+tau-) greater than or similar to 70 GeV) and weakening by a factor of similar to 1.5 at lower masses relative to previously observed limits.
Published: 2017
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43. Optical-SZE scaling relations for DES optically selected clusters within the SPT-SZ Survey

Author: Saro, A, Bocquet, S, Mohr, J, Rozo, E, Benson, BA, Dodelson, S, Rykoff, ES, Bleem, L, Abbott, TMC, Abdalla, FB, Allen, S, Annis, J, Benoit-Levy, A, Brooks, D, Burke, DL, Capasso, R, Carnero Rosell, A, Kind, MC, Carretero, J, Chiu, I, Crawford, TM, Cunha, CE, D'Andrea, CB, da Costa, LN, Desai, S, Dietrich, JP, Evrard, AE, Fausti Neto, A, Flaugher, B, Fosalba, P, Frieman, J, Gangkofner, C, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Grandis, S, Gruen, D, Gruend, RA, Gupta, N, Gutierrez, G, Holzapfel, WL, James, DJ, Kuehn, K, Kuropatkin, N, Lima, M, Marshall, JL, McDonald, M, Melchior, P, Menanteau, F, Miquel, R, Ogando, R, Plazas, AA, Rapetti, D, Reichardt, CL, Reil, K, Romer, AK, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Soergel, B, Strazzullo, V, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vikram, V, Walker, AR, Zenteno, A, Saro, A, Bocquet, S, Mohr, J, Rozo, E, Benson, BA, Dodelson, S, Rykoff, ES, Bleem, L, Abbott, TMC, Abdalla, FB, Allen, S, Annis, J, Benoit-Levy, A, Brooks, D, Burke, DL, Capasso, R, Carnero Rosell, A, Kind, MC, Carretero, J, Chiu, I, Crawford, TM, Cunha, CE, D'Andrea, CB, da Costa, LN, Desai, S, Dietrich, JP, Evrard, AE, Fausti Neto, A, Flaugher, B, Fosalba, P, Frieman, J, Gangkofner, C, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Grandis, S, Gruen, D, Gruend, RA, Gupta, N, Gutierrez, G, Holzapfel, WL, James, DJ, Kuehn, K, Kuropatkin, N, Lima, M, Marshall, JL, McDonald, M, Melchior, P, Menanteau, F, Miquel, R, Ogando, R, Plazas, AA, Rapetti, D, Reichardt, CL, Reil, K, Romer, AK, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Soergel, B, Strazzullo, V, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vikram, V, Walker, AR, and Zenteno, A
Published: 2017

44. Galaxy populations in massive galaxy clusters to z=1.1: colour distribution, concentration, halo occupation number and red sequence fraction

Author: Hennig, C, Mohr, JJ, Zenteno, A, Desai, S, Dietrich, JP, Bocquet, S, Strazzullo, V, Saro, A, Abbott, TMC, Abdalla, FB, Bayliss, M, Benoit-Levy, A, Bernstein, RA, Bertin, E, Brooks, D, Capasso, R, Capozzi, D, Carnero, A, Kind, MC, Carretero, J, Chiu, I, D'Andrea, CB, daCosta, LN, Diehl, HT, Doel, P, Eifler, TF, Evrard, AE, Fausti-Neto, A, Fosalba, P, Frieman, J, Gangkofner, C, Gonzalez, A, Gruen, D, Gruendl, RA, Gupta, N, Gutierrez, G, Honscheid, K, Hlavacek-Larrondo, J, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, March, M, Marshall, JL, Martini, P, McDonald, M, Melchior, P, Miller, CJ, Miquel, R, Neilsen, E, Nord, B, Ogando, R, Plazas, AA, Reichardt, C, Romer, AK, Rozo, E, Rykoff, ES, Sanchez, E, Santiago, B, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Stalder, B, Stanford, SA, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vikram, V, Walker, AR, Zhang, Y, Hennig, C, Mohr, JJ, Zenteno, A, Desai, S, Dietrich, JP, Bocquet, S, Strazzullo, V, Saro, A, Abbott, TMC, Abdalla, FB, Bayliss, M, Benoit-Levy, A, Bernstein, RA, Bertin, E, Brooks, D, Capasso, R, Capozzi, D, Carnero, A, Kind, MC, Carretero, J, Chiu, I, D'Andrea, CB, daCosta, LN, Diehl, HT, Doel, P, Eifler, TF, Evrard, AE, Fausti-Neto, A, Fosalba, P, Frieman, J, Gangkofner, C, Gonzalez, A, Gruen, D, Gruendl, RA, Gupta, N, Gutierrez, G, Honscheid, K, Hlavacek-Larrondo, J, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, March, M, Marshall, JL, Martini, P, McDonald, M, Melchior, P, Miller, CJ, Miquel, R, Neilsen, E, Nord, B, Ogando, R, Plazas, AA, Reichardt, C, Romer, AK, Rozo, E, Rykoff, ES, Sanchez, E, Santiago, B, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Stalder, B, Stanford, SA, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Vikram, V, Walker, AR, and Zhang, Y
Abstract: We study the galaxy populations in 74 Sunyaev–Zeldovich effect selected clusters from the South Pole Telescope survey, which have been imaged in the science verification phase of the Dark Energy Survey. The sample extends up to z ∼ 1.1 with 4 × 1014 M⊙ ≤ M200 ≤ 3 × 1015M⊙. Using the band containing the 4000 Å break and its redward neighbour, we study the colour–magnitude distributions of cluster galaxies to ∼m* + 2, finding that: (1)The intrinsic rest frame g − r colour width of the red sequence (RS) population is ∼0.03 out to z ∼ 0.85 with a preference for an increase to ∼0.07 at z = 1, and (2) the prominence of the RS declines beyond z ∼ 0.6. The spatial distribution of cluster galaxies is well described by the NFW profile out to 4R200 with a concentration of cg=3.59+0.20−0.18⁠, 5.37+0.27−0.24 and 1.38+0.21−0.19 for the full, the RS and the blue non-RS populations, respectively, but with ∼40 per cent to 55 per cent cluster to cluster variation and no statistically significant redshift or mass trends. The number of galaxies within the virial region N200 exhibits a mass trend indicating that the number of galaxies per unit total mass is lower in the most massive clusters, and shows no significant redshift trend. The RS fraction within R200 is (68 ± 3) per cent at z = 0.46, varies from ∼55 per cent at z = 1 to ∼80 per cent at z = 0.1 and exhibits intrinsic variation among clusters of ∼14 per cent. We discuss a model that suggests that the observed redshift trend in RS fraction favours a transformation time-scale for infalling field galaxies to become RS galaxies of 2–3 Gyr.
Published: 2017

45. Mapping and Simulating Systematics due to Spatially Varying Observing Conditions in DES Science Verification Data

Author: Antonella Palmese, Carlos Solans Sanchez, J. L. Marshall, William Wester, Kyler Kuehn, Martin Crocce, Eli S. Rykoff, D. L. Burke, Boris Leistedt, Jon J Thaler, David J. James, Michael T. Busha, J. Carretero, Yanming Zhang, V. Vikram, Ofer Lahav, David Brooks, Matthew R. Becker, Flavia Sobreira, Robert A. Gruendl, B. Flaugher, C. B. D'Andrea, M. E. C. Swanson, Pablo Fosalba, Carlos Cunha, Stephen M. Kent, C. L. Chang, E. M. Huff, A. Carnero Rosell, A. Roodman, Brian Nord, Claudio Bruderer, V. Scarpine, Daniel Thomas, E. Buckley-Geer, Emmanuel Bertin, A. Benoit-Lévy, Marcos Lima, E. J. Sanchez, Joshua A. Frieman, Ashley J. Ross, Peter Melchior, Ramon Miquel, R. C. Smith, Enrique Gaztanaga, Eduardo Rozo, I. Sadeh, I. Sevilla-Noarbe, Will J. Percival, M. March, Basilio X. Santiago, C. Bonnett, Alistair R. Walker, G. Gutierrez, Shantanu Desai, R. A. Bernstein, Joe Zuntz, M. Banerji, Darren L. DePoy, Marcelle Soares-Santos, Gregory Tarle, F. B. Abdalla, F. Elsner, A. K. Romer, Sahar S. Allam, E. Suchyta, August E. Evrard, Risa H. Wechsler, Ricardo L. C. Ogando, Paul Martini, M. Jarvis, L. N. da Costa, M. A. G. Maia, Alexandre Refregier, K. Honscheid, Adam Amara, A. Fausti Neto, Christopher J. Miller, Tim Eifler, Kevin Reil, Tenglin Li, Sarah Bridle, M. Carrasco Kind, Robert C. Nichol, N. P. Kuropatkin, Daniel Gruen, Hiranya V. Peiris, A. A. Plazas, Diego Capozzi, D. W. Gerdes, Peter Doel, H. T. Diehl, A. H. Bauer, Gary Bernstein, and M. S. Schubnell
Subjects: Cosmology and Gravitation, statistics [galaxies], Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Large Synoptic Survey Telescope, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Deslocamento para o vermelho, galaxy surveys, Cluster analysis, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, QB, media_common, Aglomerados de galaxias, Mapeamentos astronômicos, Physics, large-scale structure of universe, spatial systematics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, precision cosmology, RCUK, Astronomy and Astrophysics, Redshift, Galaxy, observations [cosmology], Fotometria astronômica, Null (SQL), Space and Planetary Science, Sky, astro-ph.CO, Dark energy, distances and redshifts [galaxies], image simulations, 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., 13 pages, 12 figures
Published: 2016

46. Joint analysis of galaxy-galaxy lensing and galaxy clustering: Methodology and forecasts for Dark Energy Survey

Author: Park, Y., Krause, E., Dodelson, S., Jain, B., Amara, A., Becker, M. R., Bridle, S. L., Clampitt, J., Crocce, M., Fosalba, P., Gaztanaga, E., Honscheid, K., Rozo, E., Sobreira, F., Sanchez, C., Wechsler, R. H., Abbott, T., Abdalla, F. B., Allam, S., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Da Costa, L. N., Depoy, D. L., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., James, D. J., Kent, S., Kuehn, K., Kuropatkin, N., Marcos Lima, Maia, M. A. G., Marshall, J. L., Melchior, P., Miller, C. J., Miquel, R., Nichol, R. C., Ogando, R., Plazas, A. A., Roe, N., Romer, A. K., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Vikram, V., Walker, A. R., Weller, J., and Zuntz, J.
Subjects: Quantum Physics, Particle and Plasma Physics, Molecular, Nuclear, Astrophysics::Cosmology and Extragalactic Astrophysics, Atomic, Nuclear & Particles Physics, Astronomical and Space Sciences, Astrophysics::Galaxy Astrophysics
Abstract: The joint analysis of galaxy-galaxy lensing and galaxy clustering is a promising method for inferring the growth function of large-scale structure. Anticipating a near future application of this analysis to Dark Energy Survey (DES) measurements of galaxy positions and shapes, we develop a practical approach to modeling the assumptions and systematic effects affecting the joint analysis of small-scale galaxy-galaxy lensing and large-scale galaxy clustering. Introducing parameters that characterize the halo occupation distribution (HOD), photometric redshift uncertainties, and shear measurement errors, we study how external priors on different subsets of these parameters affect our growth constraints. Degeneracies within the HOD model, as well as between the HOD and the growth function, are identified as the dominant source of complication, with other systematic effects being subdominant. The impact of HOD parameters and their degeneracies necessitate the detailed joint modeling of the galaxy sample that we employ. We conclude that DES data will provide powerful constraints on the evolution of structure growth in the Universe, conservatively/optimistically constraining the growth function to 7.9%/4.8% with its first-year data that cover over 1000 square degrees, and to 3.9%/2.3% with its full five-year data that will survey 5000 square degrees, including both statistical and systematic uncertainties.
Published: 2016

47. Joint analysis of galaxy-galaxy lensing and galaxy clustering: methodology and forecasts for dark energy survey

Author: K. Honscheid, Christopher J. Miller, E. S. Rykoff, Natalie A. Roe, Jennifer L. Marshall, D. A. Finley, Shantanu Desai, Carles Sanchez, Enrique Gaztanaga, J. Carretero, A. Benoit-Lévy, E. Bertin, A. Carnero Rosell, Vinu Vikram, E. Buckley-Geer, F. B. Abdalla, Tim Eifler, Daniel Gruen, J. Zuntz, Elisabeth Krause, V. Scarpine, G. Gutierrez, M. Carrasco Kind, Ricardo L. C. Ogando, P. Fosalba, Alistair R. Walker, Matthew R. Becker, Flavia Sobreira, M. Schubnell, Robert C. Nichol, J. J. Thaler, Youngsoo Park, Sarah Bridle, Scott Dodelson, D. L. Burke, Marcelle Soares-Santos, D. W. Gerdes, Martin Crocce, Ramon Miquel, Jochen Weller, Francisco J. Castander, T. M. C. Abbott, David Brooks, M. E. C. Swanson, E. Fernandez, A. A. Plazas, E. J. Sanchez, Adam Amara, S. Allam, Robert A. Gruendl, Gregory Tarle, David J. James, Peter Doel, E. Suchyta, B. Flaugher, Darren L. DePoy, Steve Kent, Risa H. Wechsler, Eduardo Rozo, Nikolay Kuropatkin, A. K. Romer, Bhuvnesh Jain, A. Fausti Neto, I. Sevilla-Noarbe, J. P. Dietrich, L. N. da Costa, Kyler Kuehn, Joseph Clampitt, Marcos Lima, Peter Melchior, and M. A. G. Maia
Subjects: Physics, Observational error, 010308 nuclear & particles physics, AST-1138766, RCUK, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo occupation distribution, Cosmology, Galaxy, 0103 physical sciences, Dark energy, astro-ph.CO, Cluster analysis, dark energy, 010303 astronomy & astrophysics, cosmology, uploaded-in-3-months-elsewhere, Weak gravitational lensing, STFC, Astrophysics::Galaxy Astrophysics, Photometric redshift, QB
Abstract: The joint analysis of galaxy-galaxy lensing and galaxy clustering is a promising method for inferring the growth function of large scale structure. This analysis will be carried out on data from the Dark Energy Survey (DES), with its measurements of both the distribution of galaxies and the tangential shears of background galaxies induced by these foreground lenses. We develop a practical approach to modeling the assumptions and systematic effects affecting small scale lensing, which provides halo masses, and large scale galaxy clustering. Introducing parameters that characterize the halo occupation distribution (HOD), photometric redshift uncertainties, and shear measurement errors, we study how external priors on different subsets of these parameters affect our growth constraints. Degeneracies within the HOD model, as well as between the HOD and the growth function, are identified as the dominant source of complication, with other systematic effects sub-dominant. The impact of HOD parameters and their degeneracies necessitate the detailed joint modeling of the galaxy sample that we employ. We conclude that DES data will provide powerful constraints on the evolution of structure growth in the universe, conservatively/optimistically constraining the growth function to 7.9%/4.8% with its first-year data that covered over 1000 square degrees, and to 3.9%/2.3% with its full five-year data that will survey 5000 square degrees, including both statistical and systematic uncertainties.
Published: 2016

48. redMaGiC: selecting luminous red galaxies from the DES Science Verification data

Author: Alistair R. Walker, Marcelle Soares-Santos, Flavia Sobreira, Peter Doel, Martin Crocce, Ricardo L. C. Ogando, H. T. Diehl, Enrique Gaztanaga, Vinu Vikram, Eli S. Rykoff, M. March, Basilio X. Santiago, M. Carrasco Kind, Robert C. Nichol, M. Jarvis, Ben Hoyle, J. J. Thaler, A. H. Bauer, T. M. C. Abbott, Hiranya V. Peiris, D. L. Burke, E. Bertin, C. Davis, E. J. Sanchez, C. Bonnett, Shantanu Desai, I. Sevilla-Noarbe, A. Benoit-Lévy, Syed Uddin, Daniela Carollo, A. A. Plazas, Gary Bernstein, Brian Nord, Marcio A. G. Maia, Diego Capozzi, Peter Melchior, Carlos E. Cunha, Robert A. Gruendl, David Brooks, M. E. C. Swanson, P. Fosalba, C. Lidman, Ofer Lahav, Alexandra Abate, Darren L. DePoy, A. Carnero Rosell, L. N. da Costa, Eduardo Rozo, David J. James, Kyler Kuehn, Ramon Miquel, Daniel Thomas, E. Buckley-Geer, Tim Eifler, Karl Glazebrook, W. C. Wester, Manda Banerji, Risa H. Wechsler, R. C. Smith, J. Carretero, K. Honscheid, Tamara M. Davis, A. K. Romer, Paul Martini, B. Flaugher, C. B. D'Andrea, A. Fausti Neto, J. P. Dietrich, Nikolay Kuropatkin, A. Roodman, M. J. Childress, Joshua A. Frieman, C. R. O'Neill, E. Suchyta, August E. Evrard, Joseph J. Mohr, Michael Schubnell, M. Sako, A. G. Kim, Marcos Lima, Boris Leistedt, Francisco J. Castander, Y. Zhang, F. B. Abdalla, Daniel Gruen, D. W. Gerdes, and C. J. Miller
Subjects: Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gaussian, media_common.quotation_subject, astro-ph.GA, statistical [methods], Extrapolation, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, photometric [techniques], symbols.namesake, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), STFC, Astrophysics::Galaxy Astrophysics, Photometric redshift, media_common, QB, Physics, 010308 nuclear & particles physics, Sigma, Astronomy, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Outlier, symbols, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, general [galaxies], astro-ph.IM
Abstract: We introduce redMaGiC, an automated algorithm for selecting Luminous Red Galaxies (LRGs). The algorithm was specifically developed to minimize photometric redshift uncertainties in photometric large-scale structure studies. redMaGiC achieves this by self-training the color-cuts necessary to produce a luminosity-thresholded LRG sample of constant comoving density. We demonstrate that redMaGiC photozs are very nearly as accurate as the best machine-learning based methods, yet they require minimal spectroscopic training, do not suffer from extrapolation biases, and are very nearly Gaussian. We apply our algorithm to Dark Energy Survey (DES) Science Verification (SV) data to produce a redMaGiC catalog sampling the redshift range $z\in[0.2,0.8]$. Our fiducial sample has a comoving space density of $10^{-3}\ (h^{-1} Mpc)^{-3}$, and a median photoz bias ($z_{spec}-z_{photo}$) and scatter $(\sigma_z/(1+z))$ of 0.005 and 0.017 respectively. The corresponding $5\sigma$ outlier fraction is 1.4%. We also test our algorithm with Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8) and Stripe 82 data, and discuss how spectroscopic training can be used to control photoz biases at the 0.1% level., Comment: comments welcome
Published: 2016

49. A DECAM SEARCH FOR AN OPTICAL COUNTERPART TO THE LIGO GRAVITATIONAL-WAVE EVENT GW151226

Author: Wen-fai Fong, Brian Yanny, Shantanu Desai, John Marriner, A. K. Romer, D. L. Burke, R. C. Thomas, A. A. Plazas, A. Fausti Neto, Armin Rest, A. Carnero Rosell, D. L. Tucker, Eliot Quataert, Richard Kessler, William Wester, Kyler Kuehn, V. A. Villar, E. Suchyta, August E. Evrard, Philip S. Cowperthwaite, A. Benoit-Lévy, Keith Bechtol, K. Honscheid, Kevin Reil, M. Carrasco Kind, Robert C. Nichol, Peter K. G. Williams, Daniel Scolnic, G. Strampelli, Eric H. Neilsen, Marcos Lima, D. J. Brout, V. Scarpine, Felipe Menanteau, Edo Berger, Alex Drlica-Wagner, Derek B. Fox, Brian Nord, Gregory Tarle, Daniel Kasen, Raffaella Margutti, G. Gutierrez, Masao Sako, R. C. Smith, Carlos Cunha, I. Sevilla-Noarbe, Huan Lin, Juan Garcia-Bellido, Ryan Chornock, Ben Farr, David J. James, Ramon Miquel, Brian D. Metzger, Pablo Fosalba, Robert Armstrong, L. N. da Costa, Duncan A. Brown, Alistair R. Walker, S. Allam, Robert A. Gruendl, Hsin-Yu Chen, Maria R. Drout, Marcelle Soares-Santos, J. Annis, Zoheyr Doctor, Flavia Sobreira, Thomas Matheson, M. W. G. Johnson, Jennifer L. Marshall, S. B. Cenko, F. B. Abdalla, Elisabeth Krause, Joseph J. Mohr, Joshua A. Frieman, Tommaso Giannantonio, H. T. Diehl, M. S. S. Gill, Daniel Thomas, E. Buckley-Geer, David Brooks, Francisco J. Castander, E. Bertin, Marcio A. G. Maia, Michael D. Johnson, Ken Herner, Nathan Smith, Daniel Gruen, D. A. Finley, J. Carretero, D. W. Gerdes, Daniel A. Goldstein, J. P. Dietrich, Jochen Weller, T. M. C. Abbott, R. J. Foley, E. J. Sanchez, C. B. D'Andrea, Nikolay Kuropatkin, Daniel E. Holz, Ricardo L. C. Ogando, UAM. Departamento de Física Teórica, Harvard Smithsonian Ctr Astrophys, Fermilab Natl Accelerator Lab, Univ Penn, Syracuse Univ, NASA, Univ Maryland, Univ Chicago, Ohio Univ, Univ Calif Santa Cruz, Univ Illinois, Univ Arizona, Penn State Univ, Univ Autonoma Madrid, Stanford Univ, SLAC Natl Accelerator Lab, Natl Ctr Supercomputing Applicat, Univ Calif Berkeley, Lawrence Berkeley Natl Lab, NYU, Natl Opt Astron Observ, Columbia Univ, Space Telescope Sci Inst, Universidade Estadual Paulista (Unesp), Lab Interinst E Astron LIneA, UCL, Rhodes Univ, Princeton Univ, Univ Wisconsin, CNRS, Univ Paris 06, Observ Nacl, IEEC CSIC, Barcelona Inst Sci & Technol, Univ Portsmouth, Univ Southampton, Univ Munich, Excellence Cluster Universe, Univ Michigan, Univ Cambridge, Ohio State Univ, Australian Astron Observ, Universidade de São Paulo (USP), Texas A&M Univ, Inst Catalana Recerca & Estudis Avancats, Max Planck Inst Extraterr Phys, CALTECH, Univ Sussex, and Ctr Invest Energet Medioambientales & Tecnol CIEM
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), close [binaries], FOS: Physical sciences, Astrophysics, Surveys, Kilonova, Astronomy & Astrophysics, 01 natural sciences, Gravitational waves, neutron [stars], surveys, Stars: Neutron, 0103 physical sciences, GW151226, 010303 astronomy & astrophysics, STFC, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, 010308 nuclear & particles physics, Gravitational wave, Detector, Física, RCUK, Astronomy and Astrophysics, Galaxy, LIGO, Binaries: Close, Supernova, gravitational waves, 13. Climate action, Space and Planetary Science, Dark energy, astro-ph.CO, Catalogs, Astrophysics - High Energy Astrophysical Phenomena, catalogs, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Astrophysical Journal Letters 826.2 (2016): L29 reproduced by permission of the AAS, We report the results of a Dark Energy Camera optical follow-up of the gravitational-wave (GW) event GW151226, discovered by the Advanced Laser Interferometer Gravitational-wave Observatory detectors. Our observations cover 28.8 deg2 of the localization region in the i and z bands (containing 3% of the BAYESTAR localization probability), starting 10 hr after the event was announced and spanning four epochs at 2-24 days after the GW detection. We achieve 5σ point-source limiting magnitudes of i ≈ 21.7 and z ≈ 21.5, with a scatter of 0.4 mag, in our difference images. Given the two-day delay, we search this area for a rapidly declining optical counterpart with ≥ 3σ significance steady decline between the first and final observations. We recover four sources that pass our selection criteria, of which three are cataloged active galactic nuclei. The fourth source is offset by 5.8 arcsec from the center of a galaxy at a distance of 187 Mpc, exhibits a rapid decline by 0.5 mag over 4 days, and has a red color of i - z ≈ 0.3 mag. These properties could satisfy a set of cuts designed to identify kilonovae. However, this source was detected several times, starting 94 days prior to GW151226, in the Pan-STARRS Survey for Transients (dubbed as PS15cdi) and is therefore unrelated to the GW event. Given its long-term behavior, PS15cdi is likely a Type IIP supernova that transitioned out of its plateau phase during our observations, mimicking a kilonova-like behavior. We comment on the implications of this detection for contamination in future optical follow-up observations, P.S.C. is grateful for support provided by the NSF through the Graduate Research Fellowship Program, grant DGE1144152. R. J.F. gratefully acknowledges support from NSF grant AST– 1518052 and the Alfred P. Sloan Foundation. D.E.H. was supported by NSF CAREER grant PHY-1151836. He also acknowledges support from the Kavli Institute for Cosmological Physics at the University of Chicago through NSF grant PHY- 1125897 as well as an endowment from the Kavli Foundation. The DES Data Management System is supported by the NSF under grant number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the ERC under the EU’s 7th Framework Programme including grants ERC 240672, 291329,and 306478
Published: 2016

50. Cosmic shear measurements with Dark Energy Survey Science Verification data

Author: A. Roodman, A. K. Romer, Darren L. DePoy, A. Fausti Neto, M. Sako, Marcos Lima, Andrina Nicola, D. L. Burke, J. Carretero, T. Kacprzak, E. Suchyta, August E. Evrard, Andrey V. Kravtsov, Francisco J. Castander, G. Gutierrez, Alexandre Refregier, Matthew R. Becker, Flavia Sobreira, Cristiano G. Sabiu, S. Allam, Robert A. Gruendl, Joseph J. Mohr, J. P. Dietrich, A. A. Plazas, Gary Bernstein, Vinu Vikram, Diego Capozzi, A. Benoit-Lévy, M. T. Busha, David Brooks, M. E. C. Swanson, M. Carrasco Kind, Ofer Lahav, Eli S. Rykoff, David J. James, Michael Schubnell, Robert C. Nichol, William G. Hartley, Risa H. Wechsler, Matt J. Jarvis, Peter Doel, T. M. C. Abbott, Tim Eifler, Pablo Fosalba, V. Scarpine, Kevin Reil, Hiranya V. Peiris, Carles Sanchez, M. March, Enrique Gaztanaga, Oliver Friedrich, H. T. Diehl, Peter Melchior, E. J. Sanchez, R. C. Smith, David Bacon, Joe Zuntz, Daniel Gruen, Boris Leistedt, Robert Armstrong, A. H. Bauer, Niall MacCrann, B. Flaugher, C. B. D'Andrea, E. Sheldon, Brandon M. S. Erickson, E. Bertin, Ramon Miquel, Daniel Thomas, E. Buckley-Geer, Martin Crocce, Adam Amara, A. Carnero Rosell, C. Bonnett, Shantanu Desai, D. A. Finley, P. Martini, D. W. Gerdes, Bhuvnesh Jain, J. J. Thaler, Sarah Bridle, Scott Dodelson, Elisabeth Krause, Chihway Chang, Carlos E. Cunha, F. B. Abdalla, Donnacha Kirk, E. Fernandez, Alistair R. Walker, K. Honscheid, Marcelle Soares-Santos, C. J. Miller, Hee-Jong Seo, Ricardo L. C. Ogando, Brian Nord, Gregory Tarle, M. A. G. Maia, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, M. Banerji, Joshua A. Frieman, Kyler Kuehn, Michael Troxel, and Tianjun Li
Subjects: IMPACT, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Physics, Particles & Fields, 0103 physical sciences, Sample variance, Statistical physics, COVARIANCE, NOISE BIAS, 010303 astronomy & astrophysics, Weak gravitational lensing, QB, Physics, Science & Technology, COSMIC cancer database, 010308 nuclear & particles physics, Covariance matrix, WEAK LENSING SURVEYS, GALAXY SHAPE MEASUREMENT, STATISTICS, SIMULATIONS, Galaxy, POLARIZATION POWER SPECTRA, MODEL, Physical Sciences, astro-ph.CO, Dark energy, Halo, MATTER, Jackknife resampling
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 9.7 sigma . Cosmological constraints from the measurements in this work are presented in a companion paper [DES et al., Phys. Rev. D 94, 022001 (2016).].
Published: 2016

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178 results on '"Fausti Neto, A"'

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