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301. Cosmological Constraints from Multiple Probes in the Dark Energy Survey

Author

Abbott, TMC, Alarcon, A, Allam, S, Andersen, P, Andrade-Oliveira, F, Annis, J, Asorey, J, Avila, S, Bacon, D, Banik, N, Bassett, BA, Baxter, E, Bechtol, K, Becker, MR, Bernstein, GM, Bertin, E, Blazek, J, Bridle, SL, Brooks, D, Brout, D, Burke, DL, Calcino, J, Camacho, H, Campos, A, Rosell, A Carnero, Carollo, D, Kind, M Carrasco, Carretero, J, Castander, FJ, Cawthon, R, Challis, P, Chan, KC, Chang, C, Childress, M, Crocce, M, Cunha, CE, D’Andrea, CB, da Costa, LN, Davis, C, Davis, TM, De Vicente, J, DePoy, DL, DeRose, J, Desai, S, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Eifler, TF, Elvin-Poole, J, Estrada, J, Evrard, AE, Fernandez, E, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, Galbany, L, García-Bellido, J, Gatti, M, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Glazebrook, K, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hinton, SR, Hollowood, DL, Honscheid, K, Hoormann, JK, Hoyle, B, Huterer, D, Jain, B, James, DJ, Jarvis, M, Jeltema, T, Kasai, E, Kent, S, Kessler, R, Kim, AG, Kokron, N, Krause, E, Kron, R, Kuehn, K, Kuropatkin, N, Lahav, O, Lasker, J, Lemos, P, Lewis, GF, Li, TS, Lidman, C, Lima, M, Lin, H, Macaulay, E, and MacCrann, N

Subjects
Particle and High Energy Physics, Physical Sciences, Affordable and Clean Energy, DES Collaboration, astro-ph.CO, Mathematical Sciences, Engineering, General Physics, Mathematical sciences, Physical sciences
Abstract

The combination of multiple observational probes has long been advocated as a powerful technique to constrain cosmological parameters, in particular dark energy. The Dark Energy Survey has measured 207 spectroscopically confirmed type Ia supernova light curves, the baryon acoustic oscillation feature, weak gravitational lensing, and galaxy clustering. Here we present combined results from these probes, deriving constraints on the equation of state, w, of dark energy and its energy density in the Universe. Independently of other experiments, such as those that measure the cosmic microwave background, the probes from this single photometric survey rule out a Universe with no dark energy, finding w=-0.80_{-0.11}^{+0.09}. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of Ω_{b}=0.069_{-0.012}^{+0.009} that is independent of early Universe measurements. These results demonstrate the potential power of large multiprobe photometric surveys and pave the way for order of magnitude advances in our constraints on properties of dark energy and cosmology over the next decade.

Published
2019

302. Steve: A Hierarchical Bayesian Model for Supernova Cosmology

Author

Hinton, SR, Davis, TM, Kim, AG, Brout, D, D’Andrea, CB, Kessler, R, Lasker, J, Lidman, C, Macaulay, E, Möller, A, Sako, M, Scolnic, D, Smith, M, Wolf, RC, Childress, M, Morganson, E, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cunha, CE, da Costa, LN, Davis, C, De Vicente, J, DePoy, DL, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Marshall, JL, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Sobreira, F, Suchyta, E, Tarle, G, Thomas, D, Vikram, V, and Zhang, Y

Subjects
Nuclear and Plasma Physics, Physical Sciences, Affordable and Clean Energy, dark energy, methods: data analysis, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present a new Bayesian hierarchical model (BHM) named Steve for performing Type Ia supernova (SN Ia) cosmology fits. This advances previous works by including an improved treatment of Malmquist bias, accounting for additional sources of systematic uncertainty, and increasing numerical efficiency. Given light-curve fit parameters, redshifts, and host-galaxy masses, we fit Steve simultaneously for parameters describing cosmology, SN Ia populations, and systematic uncertainties. Selection effects are characterized using Monte Carlo simulations. We demonstrate its implementation by fitting realizations of SN Ia data sets where the SN Ia model closely follows that used in Steve. Next, we validate on more realistic SNANA simulations of SN Ia samples from the Dark Energy Survey and low-redshift surveys (DES Collaboration et al. 2018). These simulated data sets contain more than 60,000 SNe Ia, which we use to evaluate biases in the recovery of cosmological parameters, specifically the equation of state of dark energy, w. This is the most rigorous test of a BHM method applied to SN Ia cosmology fitting and reveals small w biases that depend on the simulated SN Ia properties, in particular the intrinsic SN Ia scatter model. This w bias is less than 0.03 on average, less than half the statistical uncertainty on w. These simulation test results are a concern for BHM cosmology fitting applications on large upcoming surveys; therefore, future development will focus on minimizing the sensitivity of Steve to the SN Ia intrinsic scatter model.

Published
2019

303. First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary–Black-hole Merger GW170814

Author

Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, DE, Lin, H, Pereira, MES, Garcia, A, Herner, K, Kessler, R, Peiris, HV, Sako, M, Allam, S, Brout, D, Rosell, A Carnero, Chen, HY, Conselice, C, deRose, J, deVicente, J, Diehl, HT, Gill, MSS, Gschwend, J, Sevilla-Noarbe, I, Tucker, DL, Wechsler, R, Berger, E, Cowperthwaite, PS, Metzger, BD, Williams, PKG, Abbott, TMC, Abdalla, FB, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Kind, M Carrasco, Carretero, J, Castander, FJ, Crocce, M, Cunha, CE, D’Andrea, CB, da Costa, LN, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, TF, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, Hollowood, DL, Hoyle, B, James, DJ, Jeltema, T, Kuehn, K, Kuropatkin, N, Li, TS, Lima, M, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Neilsen, E, Ogando, RLC, Plazas, AA, Romer, AK, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, RC, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, RC, Walker, AR, Wester, W, Zuntz, J, Abbott, BP, Abbott, R, Abbott, TD, Abraham, S, Acernese, F, and Ackley, K

Subjects
Astronomical Sciences, Physical Sciences, catalogs, cosmology: observations, gravitational waves, surveys, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Space sciences
Abstract

We present a multi-messenger measurement of the Hubble constant H 0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO)/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black hole merger. Our analysis results in , which is consistent with both SN Ia and cosmic microwave background measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20, 140] km s-1 Mpc-1, and it depends on the assumed prior range. If we take a broader prior of [10, 220] km s-1 Mpc-1, we find (57% of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on H 0.

Published
2019

304. First cosmology results using Type Ia supernova from the Dark Energy Survey: simulations to correct supernova distance biases

Author

Kessler, R, Brout, D, D’Andrea, CB, Davis, TM, Hinton, SR, Kim, AG, Lasker, J, Lidman, C, Macaulay, E, Möller, A, Sako, M, Scolnic, D, Smith, M, Sullivan, M, Zhang, B, Andersen, P, Asorey, J, Avelino, A, Calcino, J, Carollo, D, Challis, P, Childress, M, Clocchiatti, A, Crawford, S, Filippenko, AV, Foley, RJ, Glazebrook, K, Hoormann, JK, Kasai, E, Kirshner, RP, Lewis, GF, Mandel, KS, March, M, Morganson, E, Muthukrishna, D, Nugent, P, Pan, Y-C, Sommer, NE, Swann, E, Thomas, RC, Tucker, BE, Uddin, SA, Abbott, TMC, Allam, S, Annis, J, Avila, S, Banerji, M, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Crocce, M, da Costa, LN, Davis, C, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Johnson, MWG, Johnson, MD, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Marshall, JL, Martini, P, Menanteau, F, Miller, CJ, Miquel, R, Nord, B, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, and Soares-Santos, M

Subjects
Space Sciences, Physical Sciences, Affordable and Clean Energy, techniques, cosmology, supernovae, (cosmology:) dark energy, astro-ph.CO, astro-ph.IM, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We describe catalogue-level simulations of Type Ia supernova (SN Ia) light curves in the Dark Energy Survey Supernova Program (DES-SN) and in low-redshift samples from the Center for Astrophysics (CfA) and the Carnegie Supernova Project (CSP). These simulations are used to model biases from selection effects and light-curve analysis and to determine bias corrections for SN Ia distance moduli that are used to measure cosmological parameters. To generate realistic light curves, the simulation uses a detailed SN Ia model, incorporates information from observations (point spread function, sky noise, zero-point), and uses summary information (e.g. detection efficiency versus signal-to-noise ratio) based on 10 000 fake SN light curves whose fluxes were overlaid on images and processed with our analysis pipelines. The quality of the simulation is illustrated by predicting distributions observed in the data. Averaging within redshift bins, we find distance modulus biases up to 0.05 mag over the redshift ranges of the low-z and DES-SN samples. For individual events, particularly those with extreme red or blue colour, distance biases can reach 0.4 mag. Therefore, accurately determining bias corrections is critical for precision measurements of cosmological parameters. Files used to make these corrections are available at https://des.ncsa.illinois.edu/releases/sn.

Published
2019

305. Finding high-redshift strong lenses in DES using convolutional neural networks

Author

Jacobs, C, Collett, T, Glazebrook, K, McCarthy, C, Qin, AK, Abbott, TMC, Abdalla, FB, Annis, J, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, da Costa, LN, Davis, C, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, Hoyle, B, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Lin, H, Maia, MAG, Martini, P, Miller, CJ, Miquel, R, Nord, B, Plazas, AA, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Vikram, V, Walker, AR, Zhang, Y, Zuntz, J, and Collaboration, DES

Subjects
Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, gravitational lensing: strong, methods: statistical, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We search Dark Energy Survey (DES) Year 3 imaging data for galaxy-galaxy strong gravitational lenses using convolutional neural networks. We generate 250 000 simulated lenses at redshifts > 0.8 from which we create a data set for training the neural networks with realistic seeing, sky and shot noise. Using the simulations as a guide, we build a catalogue of 1.1 million DES sources with 1.8 < g − i < 5, 0.6 < g − r < 3, r mag > 19, g mag > 20, and i mag > 18.2. We train two ensembles of neural networks on training sets consisting of simulated lenses, simulated non-lenses, and real sources. We use the neural networks to score images of each of the sources in our catalogue with a value from 0 to 1, and select those with scores greater than a chosen threshold for visual inspection, resulting in a candidate set of 7301 galaxies. During visual inspection, we rate 84 as 'probably' or 'definitely' lenses. Four of these are previously known lenses or lens candidates. We inspect a further 9428 candidates with a different score threshold, and identify four new candidates. We present 84 new strong lens candidates, selected after a few hours of visual inspection by astronomers. This catalogue contains a comparable number of high-redshift lenses to that predicted by simulations. Based on simulations, we estimate our sample to contain most discoverable lenses in this imaging and at this redshift range.

Published
2019

306. First Cosmology Results Using SNe Ia from the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation

Author

Brout, D, Scolnic, D, Kessler, R, D’Andrea, CB, Davis, TM, Gupta, RR, Hinton, SR, Kim, AG, Lasker, J, Lidman, C, Macaulay, E, Möller, A, Nichol, RC, Sako, M, Smith, M, Sullivan, M, Zhang, B, Andersen, P, Asorey, J, Avelino, A, Bassett, BA, Brown, P, Calcino, J, Carollo, D, Challis, P, Childress, M, Clocchiatti, A, Filippenko, AV, Foley, RJ, Galbany, L, Glazebrook, K, Hoormann, JK, Kasai, E, Kirshner, RP, Kuehn, K, Kuhlmann, S, Lewis, GF, Mandel, KS, March, M, Miranda, V, Morganson, E, Muthukrishna, D, Nugent, P, Palmese, A, Pan, Y-C, Sharp, R, Sommer, NE, Swann, E, Thomas, RC, Tucker, BE, Uddin, SA, Wester, W, Abbott, TMC, Allam, S, Annis, J, Avila, S, Bechtol, K, Bernstein, GM, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Cunha, CE, da Costa, LN, Davis, C, De Vicente, J, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Drlica-Wagner, A, Eifler, TF, Estrada, J, Fernandez, E, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gruen, D, Gruendl, RA, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, Hoyle, B, James, DJ, Jarvis, M, Jeltema, T, Krause, E, Lahav, O, Li, TS, Lima, M, Maia, MAG, Marriner, J, Marshall, JL, Martini, P, and Menanteau, F

Subjects
Particle and High Energy Physics, Physical Sciences, Affordable and Clean Energy, cosmological parameters, dark energy, supernovae: general, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017 < z < 0.849. We combine the DES-SN sample with an external sample of 122 low-redshift (z < 0.1) SNe Ia, resulting in a "DES-SN3YR" sample of 329 SNe Ia. Our cosmological analyses are blinded: after combining our DES-SN3YR distances with constraints from the Cosmic Microwave Background, our uncertainties in the measurement of the dark energy equation-of-state parameter, w, are 0.042 (stat) and 0.059 (stat+syst) at 68% confidence. We provide a detailed systematic uncertainty budget, which has nearly equal contributions from photometric calibration, astrophysical bias corrections, and instrumental bias corrections. We also include several new sources of systematic uncertainty. While our sample is less than one-third the size of the Pantheon sample, our constraints on w are only larger by 1.4×, showing the impact of the DES-SN Ia light-curve quality. We find that the traditional stretch and color standardization parameters of the DES-SNe Ia are in agreement with earlier SN Ia samples such as Pan-STARRS1 and the Supernova Legacy Survey. However, we find smaller intrinsic scatter about the Hubble diagram (0.077 mag). Interestingly, we find no evidence for a Hubble residual step (0.007 ± 0.018 mag) as a function of host-galaxy mass for the DES subset, in 2.4σ tension with previous measurements. We also present novel validation methods of our sample using simulated SNe Ia inserted in DECam images and using large catalog-level simulations to test for biases in our analysis pipelines.

Published
2019

307. First Cosmology Results Using Type Ia Supernovae from the Dark Energy Survey: Photometric Pipeline and Light-curve Data Release

Author

Brout, D, Sako, M, Scolnic, D, Kessler, R, D’Andrea, CB, Davis, TM, Hinton, SR, Kim, AG, Lasker, J, Macaulay, E, Möller, A, Nichol, RC, Smith, M, Sullivan, M, Wolf, RC, Allam, S, Bassett, BA, Brown, P, Castander, FJ, Childress, M, Foley, RJ, Galbany, L, Herner, K, Kasai, E, March, M, Morganson, E, Nugent, P, Pan, Y-C, Thomas, RC, Tucker, BE, Wester, W, Abbott, TMC, Annis, J, Avila, S, Bertin, E, Brooks, D, Burke, DL, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Crocce, M, Cunha, CE, da Costa, LN, Davis, C, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Marshall, JL, Martini, P, Miquel, R, Nord, B, Plazas, AA, Roodman, A, Rykoff, ES, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Tucker, DL, Walker, AR, Yanny, B, and Zhang, Y

Subjects
Space Sciences, Physical Sciences, Affordable and Clean Energy, cosmology: observations, supernovae: general, techniques: photometric, astro-ph.IM, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present griz light curves of 251 SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program's (DES-SN) spectroscopically classified sample. The photometric pipeline described in this paper produces the calibrated fluxes and associated uncertainties used in the cosmological parameter analysis by employing a scene modeling approach that simultaneously models a variable transient flux and temporally constant host galaxy. We inject artificial point sources onto DECam images to test the accuracy of our photometric method. Upon comparison of input and measured artificial supernova fluxes, we find that flux biases peak at 3 mmag. We require corrections to our photometric uncertainties as a function of host galaxy surface brightness at the transient location, similar to that seen by the DES Difference Imaging Pipeline used to discover transients. The public release of the light curves can be found at https://des.ncsa.illinois.edu/releases/sn.

Published
2019

308. Mass Calibration of Optically Selected DES Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data

Author

Raghunathan, S, Patil, S, Baxter, E, Benson, BA, Bleem, LE, Chou, TL, Crawford, TM, Holder, GP, McClintock, T, Reichardt, CL, Rozo, E, Varga, TN, Abbott, TMC, Ade, PAR, Allam, S, Anderson, AJ, Annis, J, Austermann, JE, Avila, S, Beall, JA, Bechtol, K, Bender, AN, Bernstein, G, Bertin, E, Bianchini, F, Brooks, D, Burke, DL, Carlstrom, JE, Carretero, J, Chang, CL, Chiang, HC, Cho, H-M, Citron, R, Crites, AT, Cunha, CE, da Costa, LN, Davis, C, Desai, S, Diehl, HT, Dietrich, JP, Dobbs, MA, Doel, P, Eifler, TF, Everett, W, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gallicchio, J, García-Bellido, J, Gaztanaga, E, George, EM, Gilbert, A, Gruen, D, Gruendl, RA, Gschwend, J, Gupta, N, Gutierrez, G, de Haan, T, Halverson, NW, Harrington, N, Hartley, WG, Henning, JW, Hilton, GC, Hollowood, DL, Holzapfel, WL, Honscheid, K, Hou, Z, Hoyle, B, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, James, DJ, Jeltema, T, Kim, AG, Kind, M Carrasco, Knox, L, Kovacs, A, Kuehn, K, Kuropatkin, N, Lee, AT, Li, TS, Lima, M, Maia, MAG, Marshall, JL, McMahon, JJ, Melchior, P, Menanteau, F, Meyer, SS, Miller, CJ, Miquel, R, Mocanu, L, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, and Plazas, AA

Subjects
Nuclear and Plasma Physics, Physical Sciences, cosmic background radiation, galaxies: clusters: general, gravitational lensing: weak, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We use cosmic microwave background (CMB) temperature maps from the 500 deg 2 SPTpol survey to measure the stacked lensing convergence of galaxy clusters from the Dark Energy Survey (DES) Year-3 redMaPPer (RM) cluster catalog. The lensing signal is extracted through a modified quadratic estimator designed to be unbiased by the thermal Sunyaev-Zel'dovich (tSZ) effect. The modified estimator uses a tSZ-free map, constructed from the SPTpol 95 and 150 GHz data sets, to estimate the background CMB gradient. For lensing reconstruction, we employ two versions of the RM catalog: a flux-limited sample containing 4003 clusters and a volume-limited sample with 1741 clusters. We detect lensing at a significance of 8.7σ(6.7σ) with the flux (volume)-limited sample. By modeling the reconstructed convergence using the Navarro-Frenk-White profile, we find the average lensing masses to be M 200m = (1.62 -0.25+0.32 [stat] ± 0.04 [sys.]) and (1.28 -0.18+0.14 [stat] ± 0.03[sys.])× 10 14 M ⊙ for the volume- and flux-limited samples, respectively. The systematic error budget is much smaller than the statistical uncertainty and is dominated by the uncertainties in the RM cluster centroids. We use the volume-limited sample to calibrate the normalization of the mass-richness scaling relation, and find a result consistent with the galaxy weak-lensing measurements from DES.

Published
2019

309. First Cosmology Results using Type Ia Supernovae from the Dark Energy Survey: Constraints on Cosmological Parameters

Author

Abbott, TMC, Allam, S, Andersen, P, Angus, C, Asorey, J, Avelino, A, Avila, S, Bassett, BA, Bechtol, K, Bernstein, GM, Bertin, E, Brooks, D, Brout, D, Brown, P, Burke, DL, Calcino, J, Rosell, A Carnero, Carollo, D, Kind, M Carrasco, Carretero, J, Casas, R, Castander, FJ, Cawthon, R, Challis, P, Childress, M, Clocchiatti, A, Cunha, CE, D’Andrea, CB, da Costa, LN, Davis, C, Davis, TM, De Vicente, J, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Drlica-Wagner, A, Eifler, TF, Evrard, AE, Fernandez, E, Filippenko, AV, Finley, DA, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, Galbany, L, García-Bellido, J, Gaztanaga, E, Giannantonio, T, Glazebrook, K, Goldstein, DA, González-Gaitán, S, Gruen, D, Gruendl, RA, Gschwend, J, Gupta, RR, Gutierrez, G, Hartley, WG, Hinton, SR, Hollowood, DL, Honscheid, K, Hoormann, JK, Hoyle, B, James, DJ, Jeltema, T, Johnson, MWG, Johnson, MD, Kasai, E, Kent, S, Kessler, R, Kim, AG, Kirshner, RP, Kovacs, E, Krause, E, Kron, R, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lahav, O, Lasker, J, Lewis, GF, Li, TS, Lidman, C, Lima, M, Lin, H, Macaulay, E, Maia, MAG, Mandel, KS, March, M, Marriner, J, Marshall, JL, Martini, P, Menanteau, F, Miller, CJ, Miquel, R, Miranda, V, Mohr, JJ, Morganson, E, and Muthukrishna, D

Subjects
Particle and High Energy Physics, Physical Sciences, Affordable and Clean Energy, dark energy, dark matter, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Space sciences
Abstract

We present the first cosmological parameter constraints using measurements of type Ia supernovae (SNe Ia) from the Dark Energy Survey Supernova Program (DES-SN). The analysis uses a subsample of 207 spectroscopically confirmed SNe Ia from the first three years of DES-SN, combined with a low-redshift sample of 122 SNe from the literature. Our "DES-SN3YR" result from these 329 SNe Ia is based on a series of companion analyses and improvements covering SN Ia discovery, spectroscopic selection, photometry, calibration, distance bias corrections, and evaluation of systematic uncertainties. For a flat ΛCDM model we find a matter density Ω m = 0.331 ± 0.038. For a flat wCDM model, and combining our SN Ia constraints with those from the cosmic microwave background (CMB), we find a dark energy equation of state w = -0.978 ± 0.059, and ω m = 0.321 ± 0.018. For a flat w 0 w a CDM model, and combining probes from SN Ia, CMB and baryon acoustic oscillations, we find w0 = -0.885 ± 0.114 and w a = -0.387 ± 0.430. These results are in agreement with a cosmological constant and with previous constraints using SNe Ia (Pantheon, JLA).

Published
2019

311. Dark Energy Survey Year 1 Results: Calibration of redMaGiC Redshift Distributions in DES and SDSS from Cross-Correlations

Author

Cawthon, R., Davis, C., Gatti, M., Vielzeuf, P., Elvin-Poole, J., Rozo, E., Frieman, J., Rykoff, E. S., Alarcon, A., Bernstein, G. M., Bonnett, C., Rosell, A. Carnero, Castander, F. J., Chang, C., da Costa, L. N., De Vicente, J., DeRose, J., Drlica-Wagner, A., Gaztanaga, E., Giannantonio, T., Gruen, D., Gschwend, J., Hartley, W. G., Hoyle, B., Lin, H., Maia, M. A. G., Miquel, R., Ogando, R. L. C., Rau, M. M., Roodman, A., Ross, A. J., Sevilla-Noarbe, I., Troxel, M. A., Wechsler, R. H., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Banerji, M., Bechtol, K., Bernstein, R. A., Bertin, E., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Hollowood, D., Honscheid, K., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sheldon, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., and Walker, A. R.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present calibrations of the redshift distributions of redMaGiC galaxies in the Dark Energy Survey Year 1 (DES Y1) and Sloan Digital Sky Survey (SDSS) DR8 data. These results determine the priors of the redshift distribution of redMaGiC galaxies, which were used for galaxy clustering measurements and as lenses for galaxy-galaxy lensing measurements in DES Y1 cosmological analyses. We empirically determine the bias in redMaGiC photometric redshift estimates using angular cross-correlations with Baryon Oscillation Spectroscopic Survey (BOSS) galaxies. For DES, we calibrate a single parameter redshift bias in three photometric redshift bins: $z \in[0.15,0.3]$, [0.3,0.45], and [0.45,0.6]. Our best fit results in each bin give photometric redshift biases of $|\Delta z|<0.01$. To further test the redMaGiC algorithm, we apply our calibration procedure to SDSS redMaGiC galaxies, where the statistical precision of the cross-correlation measurement is much higher due to a greater overlap with BOSS galaxies. For SDSS, we also find best fit results of $|\Delta z|<0.01$. We compare our results to other analyses of redMaGiC photometric redshifts., Comment: 18 pages, 12 figures. Minor changes to text to match version accepted by MNRAS

Published
2017
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312. Dark Energy Survey Year 1 Results: galaxy mock catalogues for BAO

Author

Avila, S., Crocce, M., Ross, A. J., García-Bellido, J., Percival, W. J., Camacho, N. Banik H., Kokron, N., Chan, K. C., Andrade-Oliveira, F., Gomes, R., Gomes, D., Lima, M., Rosenfeld, R., Salvador, A. I., Friedrich, O., Abdalla, F. B., Annis, J., Benoit-Lévy, A., Bertin, E., Brooks, D., Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., Doel, P., Fosalba, P., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hollowood, D., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Miquel, R., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyt, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Walker, A. R.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Mock catalogues are a crucial tool in the analysis of galaxy surveys data, both for the accurate computation of covariance matrices, and for the optimisation of analysis methodology and validation of data sets. In this paper, we present a set of 1800 galaxy mock catalogues designed to match the Dark Energy Survey Year-1 BAO sample (Crocce et al. 2017) in abundance, observational volume, redshift distribution and uncertainty, and redshift dependent clustering. The simulated samples were built upon HALOGEN (Avila et al. 2015) halo catalogues, based on a $2LPT$ density field with an exponential bias. For each of them, a lightcone is constructed by the superposition of snapshots in the redshift range $0.45

Published
2017
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313. Dark Energy Survey Year 1 Results: Galaxy Sample for BAO Measurement

Author

Crocce, M., Ross, A. J., Sevilla-Noarbe, I., Gaztanaga, E., Elvin-Poole, J., Avila, S., Alarcon, A., Chan, K. C., Banik, N., Carretero, J., Sanchez, E., Hartley, W. G., Sanchez, C., Giannantonio, T., Rosenfeld, R., Salvador, A. I., Garcia-Fernandez, M., Garcia-Bellido, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Levy, A., Bernstein, G. M., Bernstein, R. A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Cawthon, R., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Fosalba, P., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D., Honscheid, K., Jain, B., James, D. J., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Nichol, R. C., Percival, W. J., Plazas, A. A., Sako, M., Scarpine, V., Schindler, R., Scolnic, D., Sheldon, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Yanny, B., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We define and characterise a sample of 1.3 million galaxies extracted from the first year of Dark Energy Survey data, optimised to measure Baryon Acoustic Oscillations in the presence of significant redshift uncertainties. The sample is dominated by luminous red galaxies located at redshifts $z \gtrsim 0.6$. We define the exact selection using color and magnitude cuts that balance the need of high number densities and small photometric redshift uncertainties, using the corresponding forecasted BAO distance error as a figure-of-merit in the process. The typical photo-$z$ uncertainty varies from $2.3\%$ to $3.6\%$ (in units of 1+$z$) from $z=0.6$ to $1$, with number densities from $200$ to $130$ galaxies per deg$^2$ in tomographic bins of width $\Delta z = 0.1$. Next we summarise the validation of the photometric redshift estimation. We characterise and mitigate observational systematics including stellar contamination, and show that the clustering on large scales is robust in front of those contaminants. We show that the clustering signal in the auto-correlations and cross-correlations is generally consistent with theoretical models, which serves as an additional test of the redshift distributions., Comment: 15 pages, 12 figures. Added discussion on photo-z validation and other tests added based on referee's comments. Matches published version in MNRAS

Published
2017
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314. Dark Energy Survey Year 1 Results: Measurement of the Baryon Acoustic Oscillation scale in the distribution of galaxies to redshift 1

Author

The Dark Energy Survey Collaboration, Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Allam, S., Andrade-Oliveira, F., Annis, J., Avila, S., Banerji, M., Banik, N., Bechtol, K., Bernstein, G. M., Bernstein, R. A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Camacho, H., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chan, K. C., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., De Vicente, J., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Estrada, J., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D., Honscheid, K., Hoyle, B., Jain, B., James, D. J., Jeltema, T., Johnson, M. D., Kent, S., Kokron, N., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lacasa, F., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Manera, M., Marriner, J., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Percival, W. J., Plazas, A. A., Porredon, A., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rozo, E., Rykoff, E. S., Sako, M., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Yanny, B., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present angular diameter distance measurements obtained by locating the BAO scale in the distribution of galaxies selected from the first year of Dark Energy Survey data. We consider a sample of over 1.3 million galaxies distributed over a footprint of 1318 deg$^2$ with $0.6 < z_{\rm photo} < 1$ and a typical redshift uncertainty of $0.03(1+z)$. This sample was selected, as fully described in a companion paper, using a color/magnitude selection that optimizes trade-offs between number density and redshift uncertainty. We investigate the BAO signal in the projected clustering using three conventions, the angular separation, the co-moving transverse separation, and spherical harmonics. Further, we compare results obtained from template based and machine learning photometric redshift determinations. We use 1800 simulations that approximate our sample in order to produce covariance matrices and allow us to validate our distance scale measurement methodology. We measure the angular diameter distance, $D_A$, at the effective redshift of our sample divided by the true physical scale of the BAO feature, $r_{\rm d}$. We obtain close to a 4 per cent distance measurement of $D_A(z_{\rm eff}=0.81)/r_{\rm d} = 10.75\pm 0.43 $. These results are consistent with the flat $\Lambda$CDM concordance cosmological model supported by numerous other recent experimental results. All data products are publicly available here: https://des.ncsa.illinois.edu/releases/y1a1/bao, Comment: accepted by MNRAS; main results unchanged, some restructuring, clarifications, and robustness tests added based on referee's comments; all data products are publicly available here: https://des.ncsa.illinois.edu/releases/y1a1/bao

Published
2017
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315. Studying the Ultraviolet Spectrum of the First Spectroscopically Confirmed Supernova at redshift two

Author

Smith, M., Sullivan, M., Nichol, R. C., Galbany, L., D'Andrea, C. B., Inserra, C., Lidman, C., Rest, A., Schirmer, M., Filippenko, A. V., Zheng, W., Cenko, S. Bradley, Angus, C. R., Brown, P. J., Davis, T. M., Finley, D. A., Gonzalez-Gaitan, S., Gutierrez, C. P., Kessler, R., Kuhlmann, S., Marriner, J., Moller, A., Nugent, P. E., Prajs, S., Thomas, R., Wolf, R., Zenteno, A., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Levy, A., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Johnson, M. W. G., Kuehn, K., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miguel, R., Ogando, R. L. C., Petravick, D., Plazas, A. A., Romer, A. K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Walker, A. R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present observations of DES16C2nm, the first spectroscopically confirmed hydrogen-free superluminous supernova (SLSN-I) at redshift z~2. DES16C2nm was discovered by the Dark Energy Survey (DES) Supernova Program, with follow-up photometric data from the Hubble Space Telescope, Gemini, and the European Southern Observatory Very Large Telescope supplementing the DES data. Spectroscopic observations confirm DES16C2nm to be at z=1.998, and spectroscopically similar to Gaia16apd (a SLSN-I at z=0.102), with a peak absolute magnitude of U=-22.26$\pm$0.06. The high redshift of DES16C2nm provides a unique opportunity to study the ultraviolet (UV) properties of SLSNe-I. Combining DES16C2nm with ten similar events from the literature, we show that there exists a homogeneous class of SLSNe-I in the UV (~2500A), with peak luminosities in the (rest-frame) U band, and increasing absorption to shorter wavelengths. There is no evidence that the mean photometric and spectroscopic properties of SLSNe-I differ between low (z<1) and high redshift (z>1), but there is clear evidence of diversity in the spectrum at <2000A, possibly caused by the variations in temperature between events. No significant correlations are observed between spectral line velocities and photometric luminosity. Using these data, we estimate that SLSNe-I can be discovered to z=3.8 by DES. While SLSNe-I are typically identified from their blue observed colors at low redshift (z<1), we highlight that at z>2 these events appear optically red, peaking in the observer-frame z-band. Such characteristics are critical to identify these objects with future facilities such as the Large Synoptic Survey Telescope, Euclid, and the Wide-Field Infrared Survey Telescope, which should detect such SLSNe-I to z=3.5, 3.7, and 6.6, respectively., Comment: Accepted for publication in ApJ

Published
2017
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316. Quasar Accretion Disk Sizes From Continuum Reverberation Mapping From the Dark Energy Survey

Author

Mudd, D., Martini, P., Zu, Y., Kochanek, C., Peterson, B., Kessler, R., Davis, T. M., Hoorman, J., King, A., Lidman, C., Sommer, N., Tucker, B. E., Asorey, J., Hinton, S., Glazebrook, K., Kuehn, K., Lewis, G., MaCaulay, E., Moller, A., O'Neill, C., Zhang, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Banerji, M., Benoit-Levy, A., Bertin, E., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Doel, P., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., James, D. J., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., McMahon, R. G., Menanteau, F., Miquel, R., Plazas, A. A., Romer, A. K., Sanchez, E., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., and Collaboration, The DES

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present accretion disk size measurements for 15 luminous quasars at $0.7 \leq z \leq 1.9$ derived from $griz$ light curves from the Dark Energy Survey. We measure the disk sizes with continuum reverberation mapping using two methods, both of which are derived from the expectation that accretion disks have a radial temperature gradient and the continuum emission at a given radius is well-described by a single blackbody. In the first method we measure the relative lags between the multiband light curves, which provides the relative time lag between shorter and longer wavelength variations. From this, we are only able to constrain upper limits on disk sizes, as many are consistent with no lag the 2$\sigma$ level. The second method fits the model parameters for the canonical thin disk directly rather than solving for the individual time lags between the light curves. Our measurements demonstrate good agreement with the sizes predicted by this model for accretion rates between 0.3-1 times the Eddington rate. Given our large uncertainties, our measurements are also consistent with disk size measurements from gravitational microlensing studies of strongly lensed quasars, as well as other photometric reverberation mapping results, that find disk sizes that are a factor of a few ($\sim$3) larger than predictions., Comment: Accepted by ApJ, comments still welcome!

Published
2017
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317. Dark Energy Survey Year 1 Results: A Precise H0 Measurement from DES Y1, BAO, and D/H Data

Author

DES Collaboration, Abbott, T. M. C., Abdalla, F. B., Annis, J., Bechtol, K., Benson, B. A., Bernstein, R. A., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Crawford, T. M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Evrard, A. E., Fernandez, E., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Henning, J. W., Honscheid, K., Hoyle, B., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. D., Johnson, M. W. G., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Liddle, A. R., Lima, M., Lin, H., Maia, M. A. G., Manzotti, A., March, M., Marshall, J. L., Miquel, R., Mohr, J. J., Natoli, T., Nugent, P., Ogando, R. L. C., Park, Y., Plazas, A. A., Reichardt, C. L., Reil, K., Roodman, A., Ross, A. J., Rozo, E., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Troxel, M. A., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wu, W. L. K., and Zuntz, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We combine Dark Energy Survey Year 1 clustering and weak lensing data with Baryon Acoustic Oscillations (BAO) and Big Bang Nucleosynthesis (BBN) experiments to constrain the Hubble constant. Assuming a flat $\Lambda$CDM model with minimal neutrino mass ($\sum m_\nu = 0.06$ eV) we find $H_0=67.2^{+1.2}_{-1.0}$ km/s/Mpc (68% CL). This result is completely independent of Hubble constant measurements based on the distance ladder, Cosmic Microwave Background (CMB) anisotropies (both temperature and polarization), and strong lensing constraints. There are now five data sets that: a) have no shared observational systematics; and b) each constrain the Hubble constant with a few percent level precision. We compare these five independent measurements, and find that, as a set, the differences between them are significant at the $2.1\sigma$ level ($\chi^2/dof=20.1/11$, probability to exceed=4%). This difference is low enough that we consider the data sets statistically consistent with each other. The best fit Hubble constant obtained by combining all five data sets is $H_0 = 69.1^{+0.4}_{-0.6}$ km/s/Mpc., Comment: 11 pages, 2 figures

Published
2017
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318. Evidence for Dynamically Driven Formation of the GW170817 Neutron Star Binary in NGC 4993

Author

Palmese, A., Hartley, W., Tarsitano, F., Conselice, C., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H. T., Fruchter, A., Garcia-Bellido, J., Herner, K., Levan, A. J., Li, T. S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T. M. C., Abdalla, F. B., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., McMahon, R. G., Menanteau, F., Miller, C. J., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Reil, K., Romer, A. K., Sanchez, E., Schindler, R., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Walker, A. R., Weller, J., Zhang, Y., and Zuntz, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present a study of NGC 4993, the host galaxy of the GW170817 gravitational wave event, the GRB170817A short gamma-ray burst (sGRB) and the AT2017gfo kilonova. We use Dark Energy Camera imaging, AAT spectra and publicly available data, relating our findings to binary neutron star (BNS) formation scenarios and merger delay timescales. NGC4993 is a nearby (40 Mpc) early-type galaxy, with $i$-band S\'ersic index $n=4.0$ and low asymmetry ($A=0.04\pm 0.01$). These properties are unusual for sGRB hosts. However, NGC4993 presents shell-like structures and dust lanes indicative of a recent galaxy merger, with the optical transient located close to a shell. We constrain the star formation history (SFH) of the galaxy assuming that the galaxy merger produced a star formation burst, but find little to no on-going star formation in either spatially-resolved broadband SED or spectral fitting. We use the best-fit SFH to estimate the BNS merger rate in this type of galaxy, as $R_{NSM}^{gal}= 5.7^{+0.57}_{-3.3} \times 10^{-6} {\rm yr}^{-1}$. If star formation is the only considered BNS formation scenario, the expected number of BNS mergers from early-type galaxies detectable with LIGO during its first two observing seasons is $0.038^{+0.004}_{-0.022}$, as opposed to $\sim 0.5$ from all galaxy types. Hypothesizing that the binary system formed due to dynamical interactions during the galaxy merger, the subsequent time elapsed can constrain the delay time of the BNS coalescence. By using velocity dispersion estimates and the position of the shells, we find that the galaxy merger occurred $t_{\rm mer}\lesssim 200~{\rm Myr}$ prior to the BNS coalescence., Comment: 9 pages, 4 figures, 1 table. Edited to match the ApJL version

Published
2017
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319. The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles

Author

Chang, C., Baxter, E., Jain, B., Sánchez, C., Adhikari, S., Varga, T. N., Fang, Y., Rozo, E., Rykoff, E. S., Kravtsov, A., Gruen, D., Huff, E. M., Jarvis, M., Kim, A. G., Prat, J., MacCrann, N., McClintock, T., Palmese, A., Rapetti, D., Rollins, R. P., Samuroff, S., Sheldon, E., Troxel, M. A., Wechsler, R. H., Zhang, Y., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bernstein, G. M., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., D'Andrea, C. B., da, L. N., Davis, C., Desai, S., Diehl, H. T., Dietrich, J. P., Drlica-Wagner, A., Eifler, T. F., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Lahav, O., Lima, M., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Nord, B., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Weller, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The cluster-centric radius at which this process occurs, r_sp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near r_sp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first year Dark Energy Survey (DES) data. For a cluster sample with mean M_200m mass ~2.5 x 10^14 M_sun, we find strong evidence of a splashback-like steepening of the galaxy density profile and measure r_sp=1.13 +/- 0.07 Mpc/h, consistent with earlier SDSS measurements of More et al. (2016) and Baxter et al. (2017). Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure r_sp=1.34 +/- 0.21 Mpc/h from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that consistent with LCDM simulations, r_sp scales with R_200m and does not evolve with redshift over the redshift range of 0.3--0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of r_sp. We discuss progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples., Comment: 25 pages, 15 figures; update to journal accepted version

Published
2017
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320. A gravitational-wave standard siren measurement of the Hubble constant

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. 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X., Ramirez-Ruiz, E., Rest, A., Rojas-Bravo, C., Shappee, B. J., Siebert, M. R., Simon, J. D., Ulloa, N., Annis, J., Soares-Santos, M., Brout, D., Scolnic, D., Diehl, H. T., Frieman, J., Berger, E., Alexander, K. D., Allam, S., Balbinot, E., Blanchard, P., Butler, R. E., Chornock, R., Cook, E. R., Cowperthwaite, P., Drlica-Wagner, A., Durret, F., Eftekhari, T., Finley, D. A., Fong, W., Fryer, C. L., García-Bellido, J., Gill, M. S . S., Gruendl, R. A., Hartley, W., Herner, K., Huterer, D., Kessler, R., Li, T. S., Lin, H., Lopes, P. A. A., Lourenço, A. C. C., Margutti, R., Marriner, J., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muñoz, R. R., Muir, J., Nicholl, M., Nugent, P., Palmese, A., Paz-Chinchón, F., Quataert, E., Sako, M., Sauseda, M., Schlegel, D. J., Secco, L. F., Smith, N., Sobreira, F., Stebbins, A., Villar, V. A., Vivas, A. K., Wester, W., Williams, P. K. G., Yanny, B., Zenteno, A., Abbott, T. M. C., Abdalla, F. B., Bechtol, K., Benoit-Lévy, A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Estrada, J., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gutierrez, G., Hartley, W. G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Zhang, Y., Haislip, J. B., Kouprianov, V. V., Reichart, D. E., Tartaglia, L., Sand, D. J., Valenti, S., Yang, S., Arcavi, Iair, Hosseinzadeh, Griffin, Howell, D. Andrew, McCully, Curtis, Poznanski, Dovi, Vasylyev, Sergiy, Tanvir, N. R., Levan, A. J., Hjorth, J., Cano, Z., Copperwheat, C., de Ugarte-Postigo, A., Evans, P. A., Fynbo, J. P. U., González-Fernández, C., Greiner, J., Irwin, M., Lyman, J., Mandel, I., McMahon, R., Milvang-Jensen, B., O'Brien, P., Osborne, J. P., Perley, D. A., Pian, E., Palazzi, E., Rol, E., Rosetti, S., Rosswog, S., Rowlinson, A., Schulze, S., Steeghs, D. T. H., Thöne, C. C., Ulaczyk, K., Watson, D., Wiersema, K., Lipunov, V. M., Gorbovskoy, E., Kornilov, V. G., Tyurina, N ., Balanutsa, P., Vlasenko, D., Gorbunov, I., Podesta, R., Levato, H., Saffe, C., Buckley, D. A. H., Budnev, N. M., Gress, O., Yurkov, V., Rebolo, R., and Serra-Ricart, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The detection of GW170817 in both gravitational waves and electromagnetic waves heralds the age of gravitational-wave multi-messenger astronomy. On 17 August 2017 the Advanced LIGO and Virgo detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than 2 seconds after the merger, a gamma-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO-Virgo-derived location of the gravitational-wave source. This sky region was subsequently observed by optical astronomy facilities, resulting in the identification of an optical transient signal within $\sim 10$ arcsec of the galaxy NGC 4993. These multi-messenger observations allow us to use GW170817 as a standard siren, the gravitational-wave analog of an astronomical standard candle, to measure the Hubble constant. This quantity, which represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Our measurement combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using electromagnetic data. This approach does not require any form of cosmic "distance ladder;" the gravitational wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be $70.0^{+12.0}_{-8.0} \, \mathrm{km} \, \mathrm{s}^{-1} \, \mathrm{Mpc}^{-1}$ (maximum a posteriori and 68% credible interval). This is consistent with existing measurements, while being completely independent of them. Additional standard-siren measurements from future gravitational-wave sources will provide precision constraints of this important cosmological parameter., Comment: 26 pages, 5 figures, Nature in press. For more information see https://dcc.ligo.org/LIGO-P1700296/public

Published
2017
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321. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. II. UV, Optical, and Near-IR Light Curves and Comparison to Kilonova Models

Author

Cowperthwaite, P. S., Berger, E., Villar, V. A., Metzger, B. D., Nicholl, M., Chornock, R., Blanchard, P. K., Fong, W., Margutti, R., Soares-Santos, M., Alexander, K. D., Allam, S., Annis, J., Brout, D., Brown, D. A., Butler, R. E., Chen, H. -Y., Diehl, H. T., Doctor, Z., Drout, M. R., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Frieman, J. A., Fryer, C. L., García-Bellido, J., Gill, M. S. S., Guillochon, J., Herner, K., Holz, D. E., Kasen, D., Kessler, R., Marriner, J., Matheson, T., Neilsen, Jr., E. H., Quataert, E., Palmese, A., Rest, A., Sako, M., Scolnic, D. M., Smith, N., Tucker, D. L., Williams, P. K. G., Balbinot, E., Carlin, J. L., Cook, E. R., Durret, F., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Marshall, J. L., Medina, G. E., Muir, J., Muñoz, R. R., Sauseda, M., Schlegel, D. J., Secco, L. F., Vivas, A. K., Wester, W., Zenteno, A., Zhang, Y., Abbott, T. M. C., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Martini, P., McMahon, R. G., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Ogando, R. L. C., Plazas, A. A., Roe, N., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Yanny, B., and Zuntz, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present UV, optical, and NIR photometry of the first electromagnetic counterpart to a gravitational wave source from Advanced LIGO/Virgo, the binary neutron star merger GW170817. Our data set extends from the discovery of the optical counterpart at $0.47$ days to $18.5$ days post-merger, and includes observations with the Dark Energy Camera (DECam), Gemini-South/FLAMINGOS-2 (GS/F2), and the {\it Hubble Space Telescope} ({\it HST}). The spectral energy distribution (SED) inferred from this photometry at $0.6$ days is well described by a blackbody model with $T\approx 8300$ K, a radius of $R\approx 4.5\times 10^{14}$ cm (corresponding to an expansion velocity of $v\approx 0.3c$), and a bolometric luminosity of $L_{\rm bol}\approx 5\times10^{41}$ erg s$^{-1}$. At $1.5$ days we find a multi-component SED across the optical and NIR, and subsequently we observe rapid fading in the UV and blue optical bands and significant reddening of the optical/NIR colors. Modeling the entire data set we find that models with heating from radioactive decay of $^{56}$Ni, or those with only a single component of opacity from $r$-process elements, fail to capture the rapid optical decline and red optical/NIR colors. Instead, models with two components consistent with lanthanide-poor and lanthanide-rich ejecta provide a good fit to the data, the resulting "blue" component has $M_\mathrm{ej}^\mathrm{blue}\approx 0.01$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{blue}\approx 0.3$c, and the "red" component has $M_\mathrm{ej}^\mathrm{red}\approx 0.04$ M$_\odot$ and $v_\mathrm{ej}^\mathrm{red}\approx 0.1$c. These ejecta masses are broadly consistent with the estimated $r$-process production rate required to explain the Milky Way $r$-process abundances, providing the first evidence that BNS mergers can be a dominant site of $r$-process enrichment., Comment: 13 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC

Published
2017
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322. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Dark Energy Camera Discovery of the Optical Counterpart

Author

Soares-Santos, M., Holz, D. E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H., Kessler, R., Sako, M., Allam, S., Tucker, D. L., Butler, R. E., Palmese, A., Doctor, Z., Diehl, H. T., Frieman, J., Yanny, B., Lin, H., Scolnic, D., Cowperthwaite, P., Neilsen, E., Marriner, J., Kuropatkin, N., Hartley, W. G., Paz-Chinchón, F., Alexander, K. D., Balbinot, E., Blanchard, P., Brown, D. A., Carlin, J. L., Conselice, C., Cook, E. R., Drlica-Wagner, A., Drout, M. R., Durret, F., Eftekhari, T., Farr, B., Finley, D. A., Foley, R. J., Fong, W., Fryer, C. L., García-Bellido, J., Gill, M. S . S., Gruendl, R. A., Hanna, C., Kasen, D., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Margutti, R., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muñoz, R. R., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D. J., Secco, L. F., Sobreira, F., Stebbins, A., Villar, V. A., Walker, A. R., Wester, W., Williams, P. K. G., Zenteno, A., Zhang, Y., Abbott, T. M. C., Abdalla, F. B., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M. A. G., March, M., McMahon, R. G., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Wechsler, R. H., and Weller, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the Dark Energy Camera (DECam) discovery of the optical counterpart of the first binary neutron star merger detected through gravitational wave emission, GW170817. Our observations commenced 10.5 hours post-merger, as soon as the localization region became accessible from Chile. We imaged 70 deg$^2$ in the $i$ and $z$ bands, covering 93\% of the initial integrated localization probability, to a depth necessary to identify likely optical counterparts (e.g., a kilonova). At 11.4 hours post-merger we detected a bright optical transient located $10.6''$ from the nucleus of NGC\,4993 at redshift $z=0.0098$, consistent (for $H_0 = 70$\, km s$^{-1}$ Mpc$^{-1}$) with the distance of $40 \pm 8$\, Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes $i\approx 17.30$ and $z\approx 17.45$, and thus an absolute magnitude of $M_i = -15.7$, in the luminosity range expected for a kilonova. We identified 1,500 potential transient candidates. Applying simple selection criteria aimed at rejecting background events such as supernovae, we find the transient associated with NGC\,4993 as the only remaining plausible counterpart, and reject chance coincidence at the 99.5\% confidence level. We therefore conclude that the optical counterpart we have identified near NGC\,4993 is associated with GW170817. This discovery ushers in the era of multi-messenger astronomy with gravitational waves, and demonstrates the power of DECam to identify the optical counterparts of gravitational-wave sources., Comment: 9 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC

Published
2017
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323. How Many Kilonovae Can Be Found in Past, Present, and Future Survey Datasets?

Author

Scolnic, D., Kessler, R., Brout, D., Cowperthwaite, P. S., Soares-Santos, M., Annis, J., Herner, K., Chen, H. -Y., Sako, M., Doctor, Z., Butler, R. E., Palmese, A., Diehl, H. T., Frieman, J., Holz, D. E., Berger, E., Chornock, R., Villar, V. A., Nicholl, M., Biswas, R., Hounsell, R., Foley, R. J., Metzger, J., Rest, A., García-Bellido, J., Möller, A., Nugent, P., Abbott, T. M. C., Abdalla, F. B., Allam, S., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Doel, P., Drlica-Wagner, A., Eifler, T. F., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., James, D. J., Johnson, M. W. G., Johnson, M. D., Krause, E., Kuehn, K., Kuhlmann, S., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Neilsen, E., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, R. C., Tucker, D. L., Walker, A. R., and Collaboration, DES

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The discovery of a kilonova (KN) associated with the Advanced LIGO (aLIGO)/Virgo event GW170817 opens up new avenues of multi-messenger astrophysics. Here, using realistic simulations, we provide estimates of the number of KNe that could be found in data from past, present and future surveys without a gravitational-wave trigger. For the simulation, we construct a spectral time-series model based on the DES-GW multi-band light-curve from the single known KN event, and we use an average of BNS rates from past studies of $10^3 \rm{Gpc}^{-3}/\rm{year}$, consistent with the $1$ event found so far. Examining past and current datasets from transient surveys, the number of KNe we expect to find for ASAS-SN, SDSS, PS1, SNLS, DES, and SMT is between 0 and $0.3$. We predict the number of detections per future survey to be: 8.3 from ATLAS, 10.6 from ZTF, 5.5/69 from LSST (the Deep Drilling / Wide Fast Deep), and 16.0 from WFIRST. The maximum redshift of KNe discovered for each survey is z = 0.8 for WFIRST, z = 0.25 for LSST and z = 0.04 for ZTF and ATLAS. For the LSST survey, we also provide contamination estimates from Type Ia and Core-collapse supernovae: after light-curve and template-matching requirements, we estimate a background of just 2 events. More broadly, we stress that future transient surveys should consider how to optimize their search strategies to improve their detection efficiency, and to consider similar analyses for GW follow-up programs., Comment: Submitted to ApJL

Published
2017
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324. Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey Data II: Hierarchical Bayesian Modeling of the Red-Sequence Galaxy Luminosity Function

Author

Zhang, Y., Miller, C. J., Rooney, P., Bermeo, A., Romer, A. K., cervantes, C. Vergara, Rykoff, E. S., Hennig, C., Das, R., Mckay, T., Song, J., Wilcox, H., Bacon, D., Bridle, S. L., Collins, C., Conselice, C., Hilton, M., Hoyle, B., Kay, S., Liddle, A. R., Mann, R. G., Mehrtens, N., Mayers, J., Nichol, R. C., Sahlen, M., Stott, J., Viana, P. T. P., Wechsler, R. H., Abbott, T., Abdalla, F. B., Allam, S., Benoit-levy, A., Brooks, D., Buckley-geer, E., Burke, D. L., rosell, A. Carnero, kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., Dandrea, C. B., Da costa, L. N., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Flaugher, B., Fosalba, P., Garcia-bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Schubnell, M., Sevilla-noarbe, I., Smith, M., Soares-santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Walker, A. R.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Using $\sim 100$ X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the luminosity function simultaneously in redshift ($0.1

Published
2017

325. Density split statistics: joint model of counts and lensing in cells

Author

Friedrich, O., Gruen, D., DeRose, J., Kirk, D., Krause, E., McClintock, T., Rykoff, E. S., Seitz, S., Wechsler, R. H., Bernstein, G. M., Blazek, J., Chang, C., Hilbert, S., Jain, B., Kovacs, A., Lahav, O., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Levy, A., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Diehl, H. T., Dietrich, J. P., Drlica-Wagner, A., Eifler, T. F., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jarvis, M., Kuehn, K., Kuropatkin, N., Lima, M., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Nord, B., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Vikram, V., and Weller, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present density split statistics, a framework that studies lensing and counts-in-cells as a function of foreground galaxy density, thereby providing a large-scale measurement of both 2-point and 3-point statistics. Our method extends our earlier work on trough lensing and is summarized as follows: given a foreground (low redshift) population of galaxies, we divide the sky into subareas of equal size but distinct galaxy density. We then measure lensing around uniformly spaced points separately in each of these subareas, as well as counts-in-cells statistics (CiC). The lensing signals trace the matter density contrast around regions of fixed galaxy density. Through the CiC measurements this can be related to the density profile around regions of fixed matter density. Together, these measurements constitute a powerful probe of cosmology, the skewness of the density field and the connection of galaxies and matter. In this paper we show how to model both the density split lensing signal and CiC from basic ingredients: a non-linear power spectrum, clustering hierarchy coefficients from perturbation theory and a parametric model for galaxy bias and shot-noise. Using N-body simulations, we demonstrate that this model is sufficiently accurate for a cosmological analysis on year 1 data from the Dark Energy Survey., Comment: 21 pages + appendix, accepted for publication in PRD

Published
2017
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326. Density split statistics: Cosmological constraints from counts and lensing in cells in DES Y1 and SDSS data

Author

Gruen, D., Friedrich, O., Krause, E., DeRose, J., Cawthon, R., Davis, C., Elvin-Poole, J., Rykoff, E. S., Wechsler, R. H., Alarcon, A., Bernstein, G. M., Blazek, J., Chang, C., Clampitt, J., Crocce, M., De Vicente, J., Gatti, M., Gill, M. S. S., Hartley, W. G., Hilbert, S., Hoyle, B., Jain, B., Jarvis, M., Lahav, O., MacCrann, N., McClintock, T., Prat, J., Rollins, R. P., Ross, A. J., Rozo, E., Samuroff, S., Sánchez, C., Sheldon, E., Troxel, M. A., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Walker, A. R., Weller, J., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We derive cosmological constraints from the probability distribution function (PDF) of evolved large-scale matter density fluctuations. We do this by splitting lines of sight by density based on their count of tracer galaxies, and by measuring both gravitational shear around and counts-in-cells in overdense and underdense lines of sight, in Dark Energy Survey (DES) First Year and Sloan Digital Sky Survey (SDSS) data. Our analysis uses a perturbation theory model (see companion paper Friedrich at al.) and is validated using N-body simulation realizations and log-normal mocks. It allows us to constrain cosmology, bias and stochasticity of galaxies w.r.t. matter density and, in addition, the skewness of the matter density field. From a Bayesian model comparison, we find that the data weakly prefer a connection of galaxies and matter that is stochastic beyond Poisson fluctuations on <=20 arcmin angular smoothing scale. The two stochasticity models we fit yield DES constraints on the matter density $\Omega_m=0.26^{+0.04}_{-0.03}$ and $\Omega_m=0.28^{+0.05}_{-0.04}$ that are consistent with each other. These values also agree with the DES analysis of galaxy and shear two-point functions (3x2pt) that only uses second moments of the PDF. Constraints on $\sigma_8$ are model dependent ($\sigma_8=0.97^{+0.07}_{-0.06}$ and $0.80^{+0.06}_{-0.07}$ for the two stochasticity models), but consistent with each other and with the 3x2pt results if stochasticity is at the low end of the posterior range. As an additional test of gravity, counts and lensing in cells allow to compare the skewness $S_3$ of the matter density PDF to its LCDM prediction. We find no evidence of excess skewness in any model or data set, with better than 25 per cent relative precision in the skewness estimate from DES alone., Comment: 33 pages, 22 figures; matches published version

Published
2017
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327. Dark Energy Survey Year 1 Results: Cross-Correlation Redshifts in the DES -- Calibration of the Weak Lensing Source Redshift Distributions

Author

Davis, C., Gatti, M., Vielzeuf, P., Cawthon, R., Rozo, E., Alarcon, A., Bernstein, G. M., Bonnett, C., Rosell, A. Carnero, Castander, F. J., Chang, C., da Costa, L. N., Davis, T. M., De Vicente, J., DeRose, J., Drlica-Wagner, A., Elvin-Poole, J., Gaztanaga, E., Gruen, D., Gschwend, J., Hartley, W. G., Hoyle, B., Lin, H., Maia, M. A. G., Miquel, R., Ogando, R. L. C., Rau, M. M., Roodman, A., Rykoff, E. S., Sevilla-Noarbe, I., Troxel, M. A., Wechsler, R. H., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Brooks, D., Buckley-Geer, E., Burke, D. L., Kind, M. Carrasco, Carretero, J., Crocce, M., Cunha, C. E., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., March, M., Marshall, J. L., Menanteau, F., Nichol, R. C., Nord, B., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., and Zuntz, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the calibration of the Dark Energy Survey Year 1 (DES Y1) weak lensing source galaxy redshift distributions from clustering measurements. By cross-correlating the positions of source galaxies with luminous red galaxies selected by the redMaGiC algorithm we measure the redshift distributions of the source galaxies as placed into different tomographic bins. These measurements constrain any such shifts to an accuracy of $\sim0.02$ and can be computed even when the clustering measurements do not span the full redshift range. The highest-redshift source bin is not constrained by the clustering measurements because of the minimal redshift overlap with the redMaGiC galaxies. We compare our constraints with those obtained from $\texttt{COSMOS}$ 30-band photometry and find that our two very different methods produce consistent constraints., Comment: 13 pages, 7 figures. Submitting to MNRAS. Feedback welcome!

Published
2017

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

Author

Luque, E., Santiago, B., Pieres, A., Marshall, J. L., Pace, A. B., Kron, R., Drlica-Wagner, A., Queiroz, A., Balbinot, E., Ponte, M. dal, Neto, A. Fausti, da Costa, L. N., Maia, M. A. G., Walker, A. R., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Crocce, M., Davis, C., Doel, P., Eifler, T. F., Flaugher, B., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Miquel, R., Nichol, R. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., and Thomas, D.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
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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329. Dark Energy Survey Year 1 Results: Cross-Correlation Redshifts - Methods and Systematics Characterization

Author

Gatti, M., Vielzeuf, P., Davis, C., Cawthon, R., Rau, M. M., DeRose, J., De Vicente, J., Alarcon, A., Rozo, E., Gaztanaga, E., Hoyle, B., Miquel, R., Bernstein, G. M., Bonnett, C., Rosell, A. Carnero, Castander, F. J., Chang, C., da Costa, L. N., Gruen, D., Gschwend, J., Hartley, W. G., Lin, H., MacCrann, N., Maia, M. A. G., Ogando, R. L. C., Roodman, A., Sevilla-Noarbe, I., Troxel, M. A., Wechsler, R. H., Asorey, J., Davis, T. M., Glazebrook, K., Hinton, S. R., Lewis, G., Lidman, C., Macaulay, E., Möller, A., O'Neill, C. R., Sommer, N. E., Uddin, S. A., Yuan, F., Zhang, B., Abbott, T. M. C., Allam, S., Annis, J., Bechtol, K., Brooks, D., Burke, D. L., Carollo, D., Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., DePoy, D. L., Desai, S., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Goldstein, D. A., Gruendl, R. A., Gutierrez, G., Honscheid, K., Hoormann, J. K., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Li, T. S., Lima, M., Marshall, J. L., Melchior, P., Menanteau, F., Nichol, R. C., Nord, B., Plazas, A. A., Reil, K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sheldon, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Wester, W., and Wolf, R. C.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use numerical simulations to characterize the performance of a clustering-based method to calibrate photometric redshift biases. In particular, we cross-correlate the weak lensing (WL) source galaxies from the Dark Energy Survey Year 1 (DES Y1) sample with redMaGiC galaxies (luminous red galaxies with secure photometric redshifts) to estimate the redshift distribution of the former sample. The recovered redshift distributions are used to calibrate the photometric redshift bias of standard photo-$z$ methods applied to the same source galaxy sample. We apply the method to three photo-$z$ codes run in our simulated data: Bayesian Photometric Redshift (BPZ), Directional Neighborhood Fitting (DNF), and Random Forest-based photo-$z$ (RF). We characterize the systematic uncertainties of our calibration procedure, and find that these systematic uncertainties dominate our error budget. The dominant systematics are due to our assumption of unevolving bias and clustering across each redshift bin, and to differences between the shapes of the redshift distributions derived by clustering vs photo-$z$'s. The systematic uncertainty in the mean redshift bias of the source galaxy sample is $\Delta z \lesssim 0.02$, though the precise value depends on the redshift bin under consideration. We discuss possible ways to mitigate the impact of our dominant systematics in future analyses., Comment: submitted to MNRAS

Published
2017
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330. OzDES multifibre spectroscopy for the Dark Energy Survey: Three year results and first data release

Author

Childress, M. J., Lidman, C., Davis, T. M., Tucker, B. E., Asorey, J., Yuan, F., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Banerji, M., Benoit-Levy, A., Bernard, S. R., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., da Costa, L. N., D'Andrea, C. B., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Foley, R. J., Fosalba, P., Frieman, J., Garcia-Bellido, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hinton, S. R., Hoormann, J. K., James, D. J., Kessler, R., Kim, A. G., King, A. L., Kovacs, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lagattuta, D. J., Lewis, G. F., Li, T. S., Lima, M., Lin, H., Macaulay, E., Maia, M. A. G., Marriner, J., March, M., Marshall, J. L., Martini, P., McMahon, R. G., Menanteau, F., Miquel, R., Moller, A., Morganson, E., Mould, J., Mudd, D., Muthukrishna, D., Nichol, R. C., Nord, B., Ogando, R. L. C., Ostrovski, F., Parkinson, D., Plazas, A. A., Reed, S. L., Reil, K., Romer, A. K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Seymour, N., Sharp, R., Smith, M., Soares-Santos, M., Sobreira, F., Sommer, N. E., Spinka, H., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Uddin, S. A., Walker, A. R., Wester, W., and Zhang, B. R.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present results for the first three years of OzDES, a six-year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multi-year baseline, and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17,000 objects, including the redshifts of 2,566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise, magnitude, and exposure time, finding that our redshift success rate increases significantly at a signal-to-noise of 2 to 3 per 1-Angstrom bin. We also find that the change in signal-to-noise with exposure time closely matches the Poisson limit for stacked exposures as long as 10 hours. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as the 4m Multi-Object Spectroscopic Telescope (4MOST), the Subaru Prime Focus Spectrograph (PFS), and the Maunakea Spectroscopic Explorer (MSE). This work marks the first OzDES data release, comprising 14,693 redshifts. OzDES is on target to obtain over a yield of approximately 5,700 supernova host-galaxy redshifts., Comment: Accepted for publication in MNRAS. Redshift data release is available at http://www.mso.anu.edu.au/ozdes/DR1

Published
2017
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331. Chemical Abundance Analysis of Three $\alpha$-Poor, Metal-Poor Stars in the Ultra-Faint Dwarf Galaxy Horologium I

Author

Nagasawa, D. Q., Marshall, J. L., Simon, J. D., Hansen, T. T., Li, T. S., Bernstein, R. A., Balbinot, E., Drlica-Wagner, A., Pace, A. B., Strigari, L. E., Pellegrino, C. M., DePoy, D. L., Suntzeff, N. B., Bechtol, K., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Benoit-Lévy, A., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Doel, P., Eifler, T. F., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., March, M., Miquel, R., Nord, B., Roodman, A., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., Wechsler, R. H., Wolf, R. C., and Yanny, B.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present chemical abundance measurements of three stars in the ultra-faint dwarf galaxy Horologium I, a Milky Way satellite discovered by the Dark Energy Survey. Using high resolution spectroscopic observations we measure the metallicity of the three stars as well as abundance ratios of several $\alpha$-elements, iron-peak elements, and neutron-capture elements. The abundance pattern is relatively consistent among all three stars, which have a low average metallicity of [Fe/H] $\sim -2.6$ and are not $\alpha$-enhanced ([$\alpha$/Fe] $\sim 0.0$). This result is unexpected when compared to other low-metallicity stars in the Galactic halo and other ultra-faint dwarfs and hints at an entirely different mechanism for the enrichment of Hor I compared to other satellites. We discuss possible scenarios that could lead to this observed nucleosynthetic signature including extended star formation, a Population III supernova, and a possible association with the Large Magellanic Cloud.

Published
2017
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332. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cosmic Shear

Author

Troxel, M. A., MacCrann, N., Zuntz, J., Eifler, T. F., Krause, E., Dodelson, S., Gruen, D., Blazek, J., Friedrich, O., Samuroff, S., Prat, J., Secco, L. F., Davis, C., Ferté, A., DeRose, J., Alarcon, A., Amara, A., Baxter, E., Becker, M. R., Bernstein, G. M., Bridle, S. L., Cawthon, R., Chang, C., Choi, A., De Vicente, J., Drlica-Wagner, A., Elvin-Poole, J., Frieman, J., Gatti, M., Hartley, W. G., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Kacprzak, T., Kirk, D., Kokron, N., Krawiec, C., Lahav, O., Liddle, A. R., Peacock, J., Rau, M. M., Refregier, A., Rollins, R. P., Rozo, E., Rykoff, E. S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Stebbins, A., Varga, T. N., Vielzeuf, P., Wang, M., Wechsler, R. H., Yanny, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Fernandez, E., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gschwend, J., Gutierrez, G., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Nord, B., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use 26 million galaxies from the Dark Energy Survey (DES) Year 1 shape catalogs over 1321 deg$^2$ of the sky to produce the most significant measurement of cosmic shear in a galaxy survey to date. We constrain cosmological parameters in both the flat $\Lambda$CDM and $w$CDM models, while also varying the neutrino mass density. These results are shown to be robust using two independent shape catalogs, two independent \photoz\ calibration methods, and two independent analysis pipelines in a blind analysis. We find a 3.5\% fractional uncertainty on $\sigma_8(\Omega_m/0.3)^{0.5} = 0.782^{+0.027}_{-0.027}$ at 68\% CL, which is a factor of 2.5 improvement over the fractional constraining power of our DES Science Verification results. In $w$CDM, we find a 4.8\% fractional uncertainty on $\sigma_8(\Omega_m/0.3)^{0.5} = 0.777^{+0.036}_{-0.038}$ and a dark energy equation-of-state $w=-0.95^{+0.33}_{-0.39}$. We find results that are consistent with previous cosmic shear constraints in $\sigma_8$ -- $\Omega_m$, and see no evidence for disagreement of our weak lensing data with data from the CMB. Finally, we find no evidence preferring a $w$CDM model allowing $w\ne -1$. We expect further significant improvements with subsequent years of DES data, which will more than triple the sky coverage of our shape catalogs and double the effective integrated exposure time per galaxy., Comment: 32 pages, 19 figures; matches PRD referee response version

Published
2017
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333. Dark Energy Survey Year 1 Results: Galaxy clustering for combined probes

Author

Elvin-Poole, J., Crocce, M., Ross, A. J., Giannantonio, T., Rozo, E., Rykoff, E. S., Avila, S., Banik, N., Blazek, J., Bridle, S. L., Cawthon, R., Drlica-Wagner, A., Friedrich, O., Kokron, N., Krause, E., MacCrann, N., Prat, J., Sanchez, C., Secco, L. F., Sevilla-Noarbe, I., Troxel, M. A., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Asorey, J., Bechtol, K., Becker, M. R., Benoit-Levy, A., Bernstein, G. M., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., DAndrea, C. B., da Costa, L. N., Davis, T. M., Davis, C., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Eifler, T. F., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoormann, J. K., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., King, A., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lewis, G., Li, T. S., Lidman, C., Lima, M., Lin, H., Macaulay, E., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moller, A., Nichol, R. C., Nord, B., ONeill, C. R., Percival, W. J., Petravick, D., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sheldon, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Uddin, S. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Yuan, F., Zhang, B., and Zuntz, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We measure the clustering of DES Year 1 galaxies that are intended to be combined with weak lensing samples in order to produce precise cosmological constraints from the joint analysis of large-scale structure and lensing correlations. Two-point correlation functions are measured for a sample of $6.6 \times 10^{5}$ luminous red galaxies selected using the \textsc{redMaGiC} algorithm over an area of $1321$ square degrees, in the redshift range $0.15 < z < 0.9$, split into five tomographic redshift bins. The sample has a mean redshift uncertainty of $\sigma_{z}/(1+z) = 0.017$. We quantify and correct spurious correlations induced by spatially variable survey properties, testing their impact on the clustering measurements and covariance. We demonstrate the sample's robustness by testing for stellar contamination, for potential biases that could arise from the systematic correction, and for the consistency between the two-point auto- and cross-correlation functions. We show that the corrections we apply have a significant impact on the resultant measurement of cosmological parameters, but that the results are robust against arbitrary choices in the correction method. We find the linear galaxy bias in each redshift bin in a fiducial cosmology to be $b(z$=$0.24)=1.40 \pm 0.08$, $b(z$=$0.38)=1.61 \pm 0.05$, $b(z$=$0.53)=1.60 \pm 0.04$ for galaxies with luminosities $L/L_*>$$0.5$, $b(z$=$0.68)=1.93 \pm 0.05$ for $L/L_*>$$1$ and $b(z$=$0.83)=1.99 \pm 0.07$ for $L/L_*$$>1.5$, broadly consistent with expectations for the redshift and luminosity dependence of the bias of red galaxies. We show these measurements to be consistent with the linear bias obtained from tangential shear measurements., Comment: 20 pages, 13 figures. Version accepted by PRD, minor changes to text, covariance matrix updated, conclusions unchanged

Published
2017
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334. Dark Energy Survey Year 1 Results: Curved-Sky Weak Lensing Mass Map

Author

Chang, C., Pujol, A., Mawdsley, B., Bacon, D., Elvin-Poole, J., Melchior, P., Kovács, A., Jain, B., Leistedt, B., Giannantonio, T., Alarcon, A., Baxter, E., Bechtol, K., Becker, M. R., Benoit-Lévy, A., Bernstein, G. M., Bonnett, C., Busha, M. T., Rosell, A. Carnero, Castander, F. J., Cawthon, R., da Costa, L. N., Davis, C., De Vicente, J., DeRose, J., Drlica-Wagner, A., Fosalba, P., Gatti, M., Gaztanaga, E., Gruen, D., Gschwend, J., Hartley, W. G., Hoyle, B., Huff, E. M., Jarvis, M., Jeffrey, N., Kacprzak, T., Lin, H., MacCrann, N., Maia, M. A. G., Ogando, R. L. C., Prat, J., Rau, M. M., Rollins, R. P., Roodman, A., Rozo, E., Rykoff, E. S., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Troxel, M. A., Varga, T. N., Vielzeuf, P., Vikram, V., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Kind, M. Carrasco, Carretero, J., Crocce, M., Cunha, C. E., D'Andrea, C. B., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Neto, A. Fausti, Fernandez, E., Flaugher, B., Frieman, J., García-Bellido, J., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Krause, E., Kuehn, K., Kuhlmann, S., Lahav, O., Li, T. S., Lima, M., March, M., Martini, P., Menanteau, F., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Petravick, D., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., Wester, W., and Zhang, Y.

Subjects
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

Published
2017
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335. Dark Energy Survey Year 1 Results: Redshift distributions of the weak lensing source galaxies

Author

Hoyle, B., Gruen, D., Bernstein, G. M., Rau, M. M., De Vicente, J., Hartley, W. G., Gaztanaga, E., DeRose, J., Troxel, M. A., Davis, C., Alarcon, A., MacCrann, N., Prat, J., Sánchez, C., Sheldon, E., Wechsler, R. H., Asorey, J., Becker, M. R., Bonnett, C., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Castander, F. J., Cawthon, R., Chang, C., Childress, M., Davis, T. M., Drlica-Wagner, A., Gatti, M., Glazebrook, K., Gschwend, J., Hinton, S. R., Hoormann, J. K., Kim, A. G., King, A., Kuehn, K., Lewis, G., Lidman, C., Lin, H., Macaulay, E., Maia, M. A. G., Martini, P., Mudd, D., Möller, A., Nichol, R. C., Ogando, R. L. C., Rollins, R. P., Roodman, A., Ross, A. J., Rozo, E., Rykoff, E. S., Samuroff, S., Sevilla-Noarbe, I., Sharp, R., Sommer, N. E., Tucker, B. E., Uddin, S. A., Varga, T. N., Vielzeuf, P., Yuan, F., Zhang, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Busha, M. T., Capozzi, D., Carretero, J., Crocce, M., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kirk, D., Krause, E., Kuhlmann, S., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Nord, B., O'Neill, C. R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Wester, W., Wolf, R. C., Yanny, B., and Zuntz, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the derivation and validation of redshift distribution estimates and their uncertainties for the galaxies used as weak lensing sources in the Dark Energy Survey (DES) Year 1 cosmological analyses. The Bayesian Photometric Redshift (BPZ) code is used to assign galaxies to four redshift bins between z=0.2 and 1.3, and to produce initial estimates of the lensing-weighted redshift distributions $n^i_{PZ}(z)$ for bin i. Accurate determination of cosmological parameters depends critically on knowledge of $n^i$ but is insensitive to bin assignments or redshift errors for individual galaxies. The cosmological analyses allow for shifts $n^i(z)=n^i_{PZ}(z-\Delta z^i)$ to correct the mean redshift of $n^i(z)$ for biases in $n^i_{\rm PZ}$. The $\Delta z^i$ are constrained by comparison of independently estimated 30-band photometric redshifts of galaxies in the COSMOS field to BPZ estimates made from the DES griz fluxes, for a sample matched in fluxes, pre-seeing size, and lensing weight to the DES weak-lensing sources. In companion papers, the $\Delta z^i$ are further constrained by the angular clustering of the source galaxies around red galaxies with secure photometric redshifts at 0.15

Published
2017
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336. Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

Author

DES Collaboration, Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Aleksić, J., Allam, S., Allen, S., Amara, A., Annis, J., Asorey, J., Avila, S., Bacon, D., Balbinot, E., Banerji, M., Banik, N., Barkhouse, W., Baumer, M., Baxter, E., Bechtol, K., Becker, M. R., Benoit-Lévy, A., Benson, B. A., Bernstein, G. M., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Buckley-Geer, E., Burke, D. L., Busha, M. T., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, N., Childress, M., Choi, A., Conselice, C., Crittenden, R., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., Davis, T. M., Davis, C., De Vicente, J., DePoy, D. L., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elliott, A. E., Elsner, F., Elvin-Poole, J., Estrada, J., Evrard, A. E., Fang, Y., Fernandez, E., Ferté, A., Finley, D. A., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., García-Bellido, J., Garcia-Fernandez, M., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. D., Johnson, M. W. G., Kacprzak, T., Kent, S., Kim, A. G., King, A., Kirk, D., Kokron, N., Kovacs, A., Krause, E., Krawiec, C., Kremin, A., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lacasa, F., Lahav, O., Li, T. S., Liddle, A. R., Lidman, C., Lima, M., Lin, H., MacCrann, N., Maia, M. A. G., Makler, M., Manera, M., March, M., Marshall, J. L., Martini, P., McMahon, R. G., Melchior, P., Menanteau, F., Miquel, R., Miranda, V., Mudd, D., Muir, J., Möller, A., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R. L. C., Palmese, A., Peacock, J., Peiris, H. V., Peoples, J., Percival, W. J., Petravick, D., Plazas, A. A., Porredon, A., Prat, J., Pujol, A., Rau, M. M., Refregier, A., Ricker, P. M., Roe, N., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rozo, E., Rykoff, E. S., Sako, M., Salvador, A. I., Samuroff, S., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Smith, M., Smith, J., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Tucker, B. E., Uddin, S. A., Varga, T. N., Vielzeuf, P., Vikram, V., Vivas, A. K., Walker, A. R., Wang, M., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Yanny, B., Yuan, F., Zenteno, A., Zhang, B., Zhang, Y., and Zuntz, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present cosmological results from a combined analysis of galaxy clustering and weak gravitational lensing, using 1321 deg$^2$ of $griz$ imaging data from the first year of the Dark Energy Survey (DES Y1). We combine three two-point functions: (i) the cosmic shear correlation function of 26 million source galaxies in four redshift bins, (ii) the galaxy angular autocorrelation function of 650,000 luminous red galaxies in five redshift bins, and (iii) the galaxy-shear cross-correlation of luminous red galaxy positions and source galaxy shears. To demonstrate the robustness of these results, we use independent pairs of galaxy shape, photometric redshift estimation and validation, and likelihood analysis pipelines. To prevent confirmation bias, the bulk of the analysis was carried out while blind to the true results; we describe an extensive suite of systematics checks performed and passed during this blinded phase. The data are modeled in flat $\Lambda$CDM and $w$CDM cosmologies, marginalizing over 20 nuisance parameters, varying 6 (for $\Lambda$CDM) or 7 (for $w$CDM) cosmological parameters including the neutrino mass density and including the 457 $\times$ 457 element analytic covariance matrix. We find consistent cosmological results from these three two-point functions, and from their combination obtain $S_8 \equiv \sigma_8 (\Omega_m/0.3)^{0.5} = 0.783^{+0.021}_{-0.025}$ and $\Omega_m = 0.264^{+0.032}_{-0.019}$ for $\Lambda$CDM for $w$CDM, we find $S_8 = 0.794^{+0.029}_{-0.027}$, $\Omega_m = 0.279^{+0.043}_{-0.022}$, and $w=-0.80^{+0.20}_{-0.22}$ at 68% CL. The precision of these DES Y1 results rivals that from the Planck cosmic microwave background measurements, allowing a comparison of structure in the very early and late Universe on equal terms. Although the DES Y1 best-fit values for $S_8$ and $\Omega_m$ are lower than the central values from Planck ..., Comment: Matches published version. Results essentially unchanged, except updated covariance matrix leads to improved chi^2 (colored text removed)

Published
2017
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337. Dark Energy Survey Year 1 Results: The Impact of Galaxy Neighbours on Weak Lensing Cosmology with im3shape

Author

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

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use a suite of simulated images based on Year 1 of the Dark Energy Survey to explore the impact of galaxy neighbours on shape measurement and shear cosmology. The hoopoe image simulations include realistic blending, galaxy positions, and spatial variations in depth and PSF properties. Using the im3shape maximum-likelihood shape measurement code, we identify four mechanisms by which neighbours can have a non-negligible influence on shear estimation. These effects, if ignored, would contribute a net multiplicative bias of $m \sim 0.03 - 0.09$ in the DES Y1 im3shape catalogue, though the precise impact will be dependent on both the measurement code and the selection cuts applied. This can be reduced to percentage level or less by removing objects with close neighbours, at a cost to the effective number density of galaxies $n_\mathrm{eff}$ of 30%. We use the cosmological inference pipeline of DES Y1 to explore the cosmological implications of neighbour bias and show that omitting blending from the calibration simulation for DES Y1 would bias the inferred clustering amplitude $S_8\equiv \sigma_8 (\Omega _\mathrm{m} /0.3)^{0.5}$ by $2 \sigma$ towards low values. Finally, we use the hoopoe simulations to test the effect of neighbour-induced spatial correlations in the multiplicative bias. We find the impact on the recovered $S_8$ of ignoring such correlations to be subdominant to statistical error at the current level of precision., Comment: 20 pages, submitted to MNRAS

Published
2017
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338. Dark Energy Survey Year 1 Results: Galaxy-Galaxy Lensing

Author

Prat, J., Sánchez, C., Fang, Y., Gruen, D., Elvin-Poole, J., Kokron, N., Secco, L. F., Jain, B., Miquel, R., MacCrann, N., Troxel, M. A., Alarcon, A., Bacon, D., Bernstein, G. M., Blazek, J., Cawthon, R., Chang, C., Crocce, M., Davis, C., De Vicente, J., Dietrich, J. P., Drlica-Wagner, A., Friedrich, O., Gatti, M., Hartley, W. G., Hoyle, B., Huff, E. M., Jarvis, M., Rau, M. M., Rollins, R. P., Ross, A. J., Rozo, E., Rykoff, E. S., Samuroff, S., Sheldon, E., Varga, T. N., Vielzeuf, P., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dodelson, S., Eifler, T. F., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kirk, D., Krause, E., Kuehn, K., Kuhlmann, S., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Mohr, J. J., Nichol, R. C., Nord, B., Plazas, A. A., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Yanny, B., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present galaxy-galaxy lensing measurements from 1321 sq. deg. of the Dark Energy Survey (DES) Year 1 (Y1) data. The lens sample consists of a selection of 660,000 red galaxies with high-precision photometric redshifts, known as redMaGiC, split into five tomographic bins in the redshift range $0.15 < z < 0.9$. We use two different source samples, obtained from the Metacalibration (26 million galaxies) and Im3shape (18 million galaxies) shear estimation codes, which are split into four photometric redshift bins in the range $0.2 < z < 1.3$. We perform extensive testing of potential systematic effects that can bias the galaxy-galaxy lensing signal, including those from shear estimation, photometric redshifts, and observational properties. Covariances are obtained from jackknife subsamples of the data and validated with a suite of log-normal simulations. We use the shear-ratio geometric test to obtain independent constraints on the mean of the source redshift distributions, providing validation of those obtained from other photo-$z$ studies with the same data. We find consistency between the galaxy bias estimates obtained from our galaxy-galaxy lensing measurements and from galaxy clustering, therefore showing the galaxy-matter cross-correlation coefficient $r$ to be consistent with one, measured over the scales used for the cosmological analysis. The results in this work present one of the three two-point correlation functions, along with galaxy clustering and cosmic shear, used in the DES cosmological analysis of Y1 data, and hence the methodology and the systematics tests presented here provide a critical input for that study as well as for future cosmological analyses in DES and other photometric galaxy surveys., Comment: 26 pages, 19 figures. Matches the version accepted by PRD

Published
2017
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339. Dark Energy Survey Year 1 Results: Weak Lensing Shape Catalogues

Author

Zuntz, J., Sheldon, E., Samuroff, S., Troxel, M. A., Jarvis, M., MacCrann, N., Gruen, D., Prat, J., Sánchez, C., Choi, A., Bridle, S. L., Bernstein, G. M., Dodelson, S., Drlica-Wagner, A., Fang, Y., Gruendl, R. A., Hoyle, B., Huff, E. M., Jain, B., Kirk, D., Kacprzak, T., Krawiec, C., Plazas, A. A., Rollins, R. P., Rykoff, E. S., Sevilla-Noarbe, I., Soergel, B., Varga, T. N., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Evrard, A. E., Neto, A. Fausti, Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., March, M., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Ogando, R. L. C., Roe, N., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., and Zhang, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present two galaxy shape catalogues from the Dark Energy Survey Year 1 data set, covering 1500 square degrees with a median redshift of $0.59$. The catalogues cover two main fields: Stripe 82, and an area overlapping the South Pole Telescope survey region. We describe our data analysis process and in particular our shape measurement using two independent shear measurement pipelines, METACALIBRATION and IM3SHAPE. The METACALIBRATION catalogue uses a Gaussian model with an innovative internal calibration scheme, and was applied to $riz$-bands, yielding 34.8M objects. The IM3SHAPE catalogue uses a maximum-likelihood bulge/disc model calibrated using simulations, and was applied to $r$-band data, yielding 21.9M objects. Both catalogues pass a suite of null tests that demonstrate their fitness for use in weak lensing science. We estimate the 1$\sigma$ uncertainties in multiplicative shear calibration to be $0.013$ and $0.025$ for the METACALIBRATION and IM3SHAPE catalogues, respectively., Comment: 36 Pages, 29 figures. This version accepted for publication in MNRAS

Published
2017
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340. Dark Energy Survey Year 1 Results: Photometric Data Set for Cosmology

Author

Drlica-Wagner, A., Sevilla-Noarbe, I., Rykoff, E. S., Gruendl, R. A., Yanny, B., Tucker, D. L., Hoyle, B., Rosell, A. Carnero, Bernstein, G. M., Bechtol, K., Becker, M. R., Benoit-Levy, A., Bertin, E., Kind, M. Carrasco, Davis, C., de Vicente, J., Diehl, H. T., Gruen, D., Hartley, W. G., Leistedt, B., Li, T. S., Marshall, J. L., Neilsen, E., Rau, M. M., Sheldon, E., Smith, J., Troxel, M. A., Wyatt, S., Zhang, Y., Abbott, T. M. C., Abdalla, F. B., Allam, S., Banerji, M., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., DePoy, D. L., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Neto, A. Fausti, Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Martini, P., McMahon, R. G., Melchior, P., Menanteau, F., Miquel, R., Nichol, R. C., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Vikram, V., Walker, A. R., Wechsler, R. H., and Zuntz, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the creation, content, and validation of the Dark Energy Survey (DES) internal year-one cosmology data set, Y1A1 GOLD, in support of upcoming cosmological analyses. The Y1A1 GOLD data set is assembled from multiple epochs of DES imaging and consists of calibrated photometric zeropoints, object catalogs, and ancillary data products - e.g., maps of survey depth and observing conditions, star-galaxy classification, and photometric redshift estimates - that are necessary for accurate cosmological analyses. The Y1A1 GOLD wide-area object catalog consists of ~137 million objects detected in coadded images covering ~1800 deg$^2$ in the DES grizY filters. The 10{\sigma} limiting magnitude for galaxies is g = 23.4, r = 23.2, i = 22.5, z = 21.8, and Y = 20.1. Photometric calibration of Y1A1 GOLD was performed by combining nightly zeropoint solutions with stellar-locus regression, and the absolute calibration accuracy is better than 2% over the survey area. DES Y1A1 GOLD is the largest photometric data set at the achieved depth to date, enabling precise measurements of cosmic acceleration at z $\lesssim$ 1., Comment: 43 pages, 28 figures, 8 tables; updated to match published version

Published
2017
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341. A Measurement of CMB Cluster Lensing with SPT and DES Year 1 Data

Author

Baxter, E. J., Raghunathan, S., Crawford, T. M., Fosalba, P., Hou, Z., Holder, G. P., Omori, Y., Patil, S., Rozo, E., Abbott, T. M. C., Annis, J., Aylor, K., Benoit-Lévy, A., Benson, B. A., Bertin, E., Bleem, L., Buckley-Geer, E., Burke, D. L., Carlstrom, J., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C. L., Cho, H-M., Crites, A. T., Crocce, M., Cunha, C. E., da Costa, L. N., D'Andrea, C. B., Davis, C., de Haan, T., Desai, S., Dobbs, M. A., Dodelson, S., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Estrada, J., Everett, W. B., Neto, A. Fausti, Flaugher, B., Frieman, J., García-Bellido, J., George, E. M., Gaztanaga, E., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Knox, L., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lee, A. T., Leitch, E. M., Li, T. S., Lima, M., Luong-Van, D., Manzotti, A., March, M., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miller, C. J., Miquel, R., Mocanu, L. M., Mohr, J. J., Natoli, T., Nord, B., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Rapetti, D., Reichardt, C. L., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E., Sako, M., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R. C., Soares-Santos, M., Staniszewski, F. Z., Stark, A., Story, K., Suchyta, E., Tarle, G., Thomas, D., Troxel, M. A., Vanderlinde, K., Vieira, J. D., Walker, A. R., Williamson, R., Zhang, Y., and Zuntz, J.

Subjects
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
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342. Evolution of Galaxy Luminosity and Stellar-Mass Functions since $z=1$ with the Dark Energy Survey Science Verification Data

Author

Capozzi, D., Etherington, J., Thomas, D., Maraston, C., Rykoff, E. S., Sevilla-Noarbe, I., Bechtol, K., Kind, M. Carrasco, Drlica-Wagner, A., Pforr, J., Gschwend, J., Rosell, A. Carnero, Pellegrini, P., Maia, M. A. G., da Costa, L. N., Benoit-Lévy, A., Swanson, M. E. C., Wechsler, R. H., Banerji, M., Papovich, C., Morice-Atkinson, X., Abdalla, F., Brooks, D., Carretero, J., Cunha, C., D'Andrea, C., Desai, S., Diehl, T. H., Evrards, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., James, D., Jeltema, T., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Nord, B., Ogando, R. L. C., Malagòn, A. A. Plazas, Romer, A. K., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., and Tarle, G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present the first study of the evolution of the galaxy luminosity and stellar-mass functions (GLF and GSMF) carried out by the Dark Energy Survey (DES). We describe the COMMODORE galaxy catalogue selected from Science Verification images. This catalogue is made of $\sim 4\times 10^{6}$ galaxies at $0

Published
2017

343. Cross-Correlation Redshift Calibration Without Spectroscopic Calibration Samples in DES Science Verification Data

Author

Davis, C., Rozo, E., Roodman, A., Alarcon, A., Cawthon, R., Gatti, M., Lin, H., Miquel, R., Rykoff, E. S., Troxel, M. A., Vielzeuf, P., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Neto, A. Fausti, Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., March, M., Marshall, J. L., Martini, P., Melchior, P., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Walker, A. R., and Wechsler, R. H.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Galaxy cross-correlations with high-fidelity redshift samples hold the potential to precisely calibrate systematic photometric redshift uncertainties arising from the unavailability of complete and representative training and validation samples of galaxies. However, application of this technique in the Dark Energy Survey (DES) is hampered by the relatively low number density, small area, and modest redshift overlap between photometric and spectroscopic samples. We propose instead using photometric catalogs with reliable photometric redshifts for photo-z calibration via cross-correlations. We verify the viability of our proposal using redMaPPer clusters from the Sloan Digital Sky Survey (SDSS) to successfully recover the redshift distribution of SDSS spectroscopic galaxies. We demonstrate how to combine photo-z with cross-correlation data to calibrate photometric redshift biases while marginalizing over possible clustering bias evolution in either the calibration or unknown photometric samples. We apply our method to DES Science Verification (DES SV) data in order to constrain the photometric redshift distribution of a galaxy sample selected for weak lensing studies, constraining the mean of the tomographic redshift distributions to a statistical uncertainty of $\Delta z \sim \pm 0.01$. We forecast that our proposal can in principle control photometric redshift uncertainties in DES weak lensing experiments at a level near the intrinsic statistical noise of the experiment over the range of redshifts where redMaPPer clusters are available. Our results provide strong motivation to launch a program to fully characterize the systematic errors from bias evolution and photo-z shapes in our calibration procedure., Comment: 12 pages, 5 figures. Submitted to MNRAS. Comments welcome!

Published
2017
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344. DES15E2mlf: A Spectroscopically Confirmed Superluminous Supernova that Exploded 3.5 Gyr After the Big Bang

Author

Pan, Y. -C., Foley, R. J., Smith, M., Galbany, L., D'Andrea, C. B., Gonzalez-Gaitan, S., Jarvis, M. J., Kessler, R., Kovacs, E., Lidman, C., Nichol, R. C., Papadopoulos, A., Sako, M., Sullivan, M., Abbott, T. M. C., Abdalla, F. B., Annis, J., Bechtol, K., Benoit-Levy, A., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., da Costa, L. N., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Finley, D. A., Flaugher, B., Frieman, J., Garcia-Bellido, J., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., James, D. J., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Miquel, R., Nugent, P., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Thomas, R. C., and Walker, A. R.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the Dark Energy Survey (DES) discovery of DES15E2mlf, the most distant superluminous supernova (SLSN) spectroscopically confirmed to date. The light curves and Gemini spectroscopy of DES15E2mlf indicate that it is a Type I superluminous supernova (SLSN-I) at z = 1.861 (a lookback time of ~10 Gyr) and peaking at M_AB = -22.3 +/- 0.1 mag. Given the high redshift, our data probe the rest-frame ultraviolet (1400-3500 A) properties of the SN, finding velocity of the C III feature changes by ~5600 km/s over 14 days around maximum light. We find the host galaxy of DES15E2mlf has a stellar mass of 3.5^+3.6_-2.4 x 10^9 M_sun, which is more massive than the typical SLSN-I host galaxy., Comment: MNRAS in press

Published
2017
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345. Dark Energy Survey Year 1 Results: Multi-Probe Methodology and Simulated Likelihood Analyses

Author

Krause, E., Eifler, T. F., Zuntz, J., Friedrich, O., Troxel, M. A., Dodelson, S., Blazek, J., Secco, L. F., MacCrann, N., Baxter, E., Chang, C., Chen, N., Crocce, M., DeRose, J., Ferte, A., Kokron, N., Lacasa, F., Miranda, V., Omori, Y., Porredon, A., Rosenfeld, R., Samuroff, S., Wang, M., Wechsler, R. H., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bechtol, K., Benoit-Levy, A., Bernstein, G. M., Brooks, D., Burke, D. L., Capozzi, D., Kind, M. Carrasco, Carretero, J., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Nichol, R. C., Plazas, A. A., Romer, A. K., Rykoff, E. S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the methodology for and detail the implementation of the Dark Energy Survey (DES) 3x2pt DES Year 1 (Y1) analysis, which combines configuration-space two-point statistics from three different cosmological probes: cosmic shear, galaxy-galaxy lensing, and galaxy clustering, using data from the first year of DES observations. We have developed two independent modeling pipelines and describe the code validation process. We derive expressions for analytical real-space multi-probe covariances, and describe their validation with numerical simulations. We stress-test the inference pipelines in simulated likelihood analyses that vary 6-7 cosmology parameters plus 20 nuisance parameters and precisely resemble the analysis to be presented in the DES 3x2pt analysis paper, using a variety of simulated input data vectors with varying assumptions. We find that any disagreement between pipelines leads to changes in assigned likelihood $\Delta \chi^2 \le 0.045$ with respect to the statistical error of the DES Y1 data vector. We also find that angular binning and survey mask do not impact our analytic covariance at a significant level. We determine lower bounds on scales used for analysis of galaxy clustering (8 Mpc$~h^{-1}$) and galaxy-galaxy lensing (12 Mpc$~h^{-1}$) such that the impact of modeling uncertainties in the non-linear regime is well below statistical errors, and show that our analysis choices are robust against a variety of systematics. These tests demonstrate that we have a robust analysis pipeline that yields unbiased cosmological parameter inferences for the flagship 3x2pt DES Y1 analysis. We emphasize that the level of independent code development and subsequent code comparison as demonstrated in this paper is necessary to produce credible constraints from increasingly complex multi-probe analyses of current data.

Published
2017

346. COSMOGRAIL XVI: Time delays for the quadruply imaged quasar DES J0408-5354 with high-cadence photometric monitoring

Author

Courbin, F., Bonvin, V., Buckley-Geer, E., Fassnacht, C. D., Frieman, J., Lin, H., Marshall, P. J., Suyu, S. H., Treu, T., Anguita, T., Motta, V., Meylan, G., Paic, E., Tewes, M., Agnello, A., Chao, D. C. -Y., Chijani, M., Gilman, D., Rojas, K., Williams, P., Hempel, A., Kim, S., Lachaume, R., Rabus, M., Abbott, T. M. C., Allam, S., Annis, J., Banerji, M., Bechtol, K., Benoit-Lévy, A., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., D'Andrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., McMahon, R. G., Menanteau, F., Miquel, R., Nord, B., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Tucker, D. L., Walker, A. R., and Wester, W.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present time-delay measurements for the new quadruply imaged quasar DES J0408-5354, the first quadruply imaged quasar found in the Dark Energy Survey (DES). Our result is made possible by implementing a new observational strategy using almost daily observations with the MPIA 2.2m telescope at La Silla observatory and deep exposures reaching a signal-to-noise ratio of about 1000 per quasar image. This data quality allows us to catch small photometric variations (a few mmag rms) of the quasar, acting on temporal scales much shorter than microlensing, hence making the time delay measurement very robust against microlensing. In only 7 months we measure very accurately one of the time delays in DES J0408-5354: Dt(AB) = -112.1 +- 2.1 days (1.8%) using only the MPIA 2.2m data. In combination with data taken with the 1.2m Euler Swiss telescope, we also measure two delays involving the D component of the system Dt(AD) = -155.5 +- 12.8 days (8.2%) and Dt(BD) = -42.4 +- 17.6 days (41%), where all the error bars include systematics. Turning these time delays into cosmological constraints will require deep HST imaging or ground-based Adaptive Optics (AO), and information on the velocity field of the lensing galaxy., Comment: 9 pages, 5 figures, accepted for publication in Astronomy & Astrophysics

Published
2017
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347. Extreme variability quasars from the Sloan Digital Sky Survey and the Dark Energy Survey

Author

Rumbaugh, Nick, Shen, Yue, Morganson, Eric, Liu, Xin, Banerji, Manda, McMahon, Richard G., Abdalla, Filipe, Benoit-Levy, Aurelien, Bertin, Emmanuel, Brooks, David, Buckley-Geer, Elizabeth, Capozzi, Diego, Rosell, Aurelio Carnero, Kind, M. Carrasco, Carretero, Jorge, Cunha, Carlos, D'Andrea, Chris, da Costa, Luiz, DePoy, Darren, Desai, Shantanu, Doel, Peter, Frieman, Joshua, Garcia-Bellido, Juan, Gruen, Daniel, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Honscheid, Klaus, James, David, Kuehn, Kyler, Kuhlmann, Steve, Kuropatkin, Nikolay, Lima, Marcos, Maia, Marcio, Marshall, Jennifer, Martini, Paul, Menanteau, Felipe, Malagon, Andres Plazas, Reil, Kevin, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schindler, Rafe, Schubnell, Michael, Sheldon, Erin, Smith, Mathew, Soares-Santos, Marcelle, Sobreira, Flavia, Suchyta, Eric, Swanson, Molly, Walker, Alistair, and Wester, William

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform a systematic search for long-term extreme variability quasars (EVQs) in the overlapping Sloan Digital Sky Survey (SDSS) and 3-Year Dark Energy Survey (DES) imaging, which provide light curves spanning more than 15 years. We identified ~1000 EVQs with a maximum g band magnitude change of more than 1 mag over this period, about 10% of all quasars searched. The EVQs have L_bol~10^45-10^47 erg/s and L/L_Edd~0.01-1. Accounting for selection effects, we estimate an intrinsic EVQ fraction of ~30-50% among all g<~22 quasars over a baseline of ~15 years. These EVQs are good candidates for so-called "changing-look quasars", where a spectral transition between the two types of quasars (broad-line and narrow-line) is observed between the dim and bright states. We performed detailed multi-wavelength, spectral and variability analyses for the EVQs and compared to their parent quasar sample. We found that EVQs are distinct from a control sample of quasars matched in redshift and optical luminosity: (1) their UV broad emission lines have larger equivalent widths; (2) their Eddington ratios are systematically lower; and (3) they are more variable on all timescales. The intrinsic difference in quasar properties for EVQs suggest that internal processes associated with accretion are the main driver for the observed extreme long-term variability. However, despite their different properties, EVQs seem to be in the tail of a continuous distribution of quasar properties, rather than standing out as a distinct population. We speculate that EVQs are normal quasars accreting at relatively low accretion rates, where the accretion flow is more likely to experience instabilities that drive the factor of few changes in flux on multi-year timescales., Comment: submitted to ApJ; comments welcome

Published
2017
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348. A Multi-component Matched Filter Cluster Confirmation Tool for eROSITA: Initial Application to the RASS and DES-SV Datasets

Author

Klein, M., Mohr, J. J., Desai, S., Israel, H., Allam, S., Benoit-Lévy, A., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Cunha, C. E., da Costa, L. N., Dietrich, J. P., Eifler, T. F., Evrard, A. E., Frieman, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., March, M., Melchior, P., Menanteau, F., Miquel, R., Plazas, A. A., Reil, K., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Collaboration, the DES

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe a multi-component matched filter cluster confirmation tool (MCMF) designed for the study of large X-ray source catalogs produced by the upcoming X-ray all-sky survey mission eROSITA. We apply the method to confirm a sample of 88 clusters with redshifts $0.05

Published
2017
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349. Forward Global Photometric Calibration of the Dark Energy Survey

Author

Burke, D., Rykoff, E. S., Allam, S., Annis, J., Bechtol, K., Bernstein, G. M., Drlica-Wagner, A., Finley, D. A., Gruendl, R. A., James, D. J., Kent, S., Kessler, R., Kuhlmann, S., Lasker, J., Li, T. S., Scolnic, D., Smith, J. Allyn, Tucker, D. L., Wester, W., Yanny, B., Abbot, T. M. C., Abdalla, F. B., Benoit-Levy, A., Bertin, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Doel, P., Estrada, J., Garcia-Bellido, J., Gruen, D., Gutierrez, G., Honscheid, K., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Plazas, A. A., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., and Walker, A. R.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Many scientific goals for the Dark Energy Survey (DES) require calibration of optical/NIR broadband $b = grizY$ photometry that is stable in time and uniform over the celestial sky to one percent or better. It is also necessary to limit to similar accuracy systematic uncertainty in the calibrated broadband magnitudes due to uncertainty in the spectrum of the source. Here we present a "Forward Global Calibration Method (FGCM)" for photometric calibration of the DES, and we present results of its application to the first three years of the survey (Y3A1). The FGCM combines data taken with auxiliary instrumentation at the observatory with data from the broad-band survey imaging itself and models of the instrument and atmosphere to estimate the spatial- and time-dependence of the passbands of individual DES survey exposures. "Standard" passbands are chosen that are typical of the passbands encountered during the survey. The passband of any individual observation is combined with an estimate of the source spectral shape to yield a magnitude $m_b^{\mathrm{std}}$ in the standard system. This "chromatic correction" to the standard system is necessary to achieve sub-percent calibrations. The FGCM achieves reproducible and stable photometric calibration of standard magnitudes $m_b^{\mathrm{std}}$ of stellar sources over the multi-year Y3A1 data sample with residual random calibration errors of $\sigma=5-6\,\mathrm{mmag}$ per exposure. The accuracy of the calibration is uniform across the $5000\,\mathrm{deg}^2$ DES footprint to within $\sigma=7\,\mathrm{mmag}$. The systematic uncertainties of magnitudes in the standard system due to the spectra of sources are less than $5\,\mathrm{mmag}$ for main sequence stars with $0.5

Published
2017
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350. Astrometric calibration and performance of the Dark Energy Camera

Author

Bernstein, G. M., Armstrong, R., Plazas, A. A., Walker, A. R., Abbott, T. M. C., Allam, S., Bechtol, K., Benoit-Lévy, A., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Eifler, T. F., Fernandez, E., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kent, S., Krause, E., Kuehn, K., Kuropatkin, N., Li, T. S., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Reil, K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., and Tarle, G.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We characterize the ability of the Dark Energy Camera (DECam) to perform relative astrometry across its 500~Mpix, 3 deg^2 science field of view, and across 4 years of operation. This is done using internal comparisons of ~4x10^7 measurements of high-S/N stellar images obtained in repeat visits to fields of moderate stellar density, with the telescope dithered to move the sources around the array. An empirical astrometric model includes terms for: optical distortions; stray electric fields in the CCD detectors; chromatic terms in the instrumental and atmospheric optics; shifts in CCD relative positions of up to ~10 um when the DECam temperature cycles; and low-order distortions to each exposure from changes in atmospheric refraction and telescope alignment. Errors in this astrometric model are dominated by stochastic variations with typical amplitudes of 10-30 mas (in a 30 s exposure) and 5-10 arcmin coherence length, plausibly attributed to Kolmogorov-spectrum atmospheric turbulence. The size of these atmospheric distortions is not closely related to the seeing. Given an astrometric reference catalog at density ~0.7 arcmin^{-2}, e.g. from Gaia, the typical atmospheric distortions can be interpolated to 7 mas RMS accuracy (for 30 s exposures) with 1 arcmin coherence length for residual errors. Remaining detectable error contributors are 2-4 mas RMS from unmodelled stray electric fields in the devices, and another 2-4 mas RMS from focal plane shifts between camera thermal cycles. Thus the astrometric solution for a single DECam exposure is accurate to 3-6 mas (0.02 pixels, or 300 nm) on the focal plane, plus the stochastic atmospheric distortion., Comment: Submitted to PASP

Published
2017
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