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275 results on '"Van Waerbeke, Ludovic"'

253. CFHTLenS: cosmological constraints from a combination of cosmic shear two-point and three-point correlations.

Author

Fu, Liping, Kilbinger, Martin, Erben, Thomas, Heymans, Catherine, Hildebrandt, Hendrik, Hoekstra, Henk, Kitching, Thomas D., Mellier, Yannick, Miller, Lance, Semboloni, Elisabetta, Simon, Patrick, Van Waerbeke, Ludovic, Coupon, Jean, Harnois-Déraps, Joachim, Hudson, Michael J., Kuijken, Konrad, Rowe, Barnaby, Schrabback, Tim, Vafaei, Sanaz, and Velander, Malin

Subjects
METAPHYSICAL cosmology, ANISOTROPY, COSMIC background radiation, ASTROPHYSICS, OPTICAL apertures
Abstract

Higher order, non-Gaussian aspects of the large-scale structure carry valuable information on structure formation and cosmology, which is complementary to second-order statistics. In this work, we measure second- and third-order weak-lensing aperture-mass moments from the Canada–France–Hawaii Lensing Survey (CFHTLenS) and combine those with cosmic microwave background (CMB) anisotropy probes. The third moment is measured with a significance of 2σ. The combined constraint on Σ8 = σ8(Ωm/0.27)α is improved by 10 per cent, in comparison to the second-order only, and the allowed ranges for Ωm and σ8 are substantially reduced. Including general triangles of the lensing bispectrum yields tighter constraints compared to probing mainly equilateral triangles. Second- and third-order CFHTLenS lensing measurements improve Planck CMB constraints on Ωm and σ8 by 26 per cent for flat Λ cold dark matter. For a model with free curvature, the joint CFHTLenS–Planck result is Ωm = 0.28 ± 0.02 (68 per cent confidence), which is an improvement of 43 per cent compared to Planck alone. We test how our results are potentially subject to three astrophysical sources of contamination: source-lens clustering, the intrinsic alignment of galaxy shapes, and baryonic effects. We explore future limitations of the cosmological use of third-order weak lensing, such as the non-linear model and the Gaussianity of the likelihood function. [ABSTRACT FROM AUTHOR]

Published
2014

255. CFHTLenS: testing the laws of gravity with tomographic weak lensing and redshift-space distortions.

Author

Simpson, Fergus, Heymans, Catherine, Parkinson, David, Blake, Chris, Kilbinger, Martin, Benjamin, Jonathan, Erben, Thomas, Hildebrandt, Hendrik, Hoekstra, Henk, Kitching, Thomas D., Mellier, Yannick, Miller, Lance, Van Waerbeke, Ludovic, Coupon, Jean, Fu, Liping, Harnois-Déraps, Joachim, Hudson, Michael J., Kuijken, Koenraad, Rowe, Barnaby, and Schrabback, Tim

Subjects
GRAVITATIONAL lenses, TOMOGRAPHY, DARK energy, REDSHIFT, GENERAL relativity (Physics), TELESCOPES, ASTRONOMICAL observations
Abstract

Dark energy may be the first sign of new fundamental physics in the Universe, taking either a physical form or revealing a correction to Einsteinian gravity. Weak gravitational lensing and galaxy peculiar velocities provide complementary probes of general relativity, and in combination allow us to test modified theories of gravity in a unique way. We perform such an analysis by combining measurements of cosmic shear tomography from the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS) with the growth of structure from the WiggleZ Dark Energy Survey and the Six-degree-Field Galaxy Survey, producing the strongest existing joint constraints on the metric potentials that describe general theories of gravity. For scale-independent modifications to the metric potentials which evolve linearly with the effective dark energy density, we find present-day cosmological deviations in the Newtonian potential and curvature potential from the prediction of general relativity to be ΔΨ/Ψ = 0.05 ± 0.25 and ΔΦ/Φ = −0.05 ± 0.3, respectively (68 per cent confidence limits). [ABSTRACT FROM PUBLISHER]

Published
2013
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256. From weak lensing to non-Gaussianity via Minkowski functionals.

Author

Munshi, Dipak, van Waerbeke, Ludovic, Smidt, Joseph, and Coles, Peter

Subjects
*GENERALIZED spaces, *FUNCTIONAL analysis, *STOCHASTIC convergence, *GRAVITATIONAL lenses, *ESTIMATES, *DARK matter, *HALOS (Meteorology), *COMPUTER simulation, *METAPHYSICAL cosmology, UNIVERSE
Abstract

ABSTRACT We present a new harmonic-domain-based approach for extracting morphological information, in the form of Minkowski functionals (MFs), from weak-lensing convergence maps. Using a perturbative expansion of the MFs, which is expected to be valid for the range of angular scales probed by most current weak-lensing surveys, we show that the study of three generalized skewness parameters is equivalent to the study of the three MFs defined in 2D. We then extend these skewness parameters to three associated skew spectra which carry more information about the convergence bispectrum than their one-point counterparts. We discuss various issues such as noise and incomplete sky coverage in the context of estimation of these skew spectra from realistic data. Our technique provides an alternative to the pixel-space approaches typically used in the estimation of MFs, and it can be particularly useful in the presence of masks with non-trivial topology. Analytical modelling of weak-lensing statistics relies on an accurate modelling of the statistics of the underlying density distribution. We apply three different formalisms to model the underlying dark matter bispectrum: the hierarchical ansatz, halo model and a fitting function based on numerical simulations; MFs resulting from each of these formalisms are computed and compared. We investigate the extent to which late-time gravity-induced non-Gaussianity (to which weak lensing is primarily sensitive) can be separated from primordial non-Gaussianity and how this separation depends on source redshift and angular scale. [ABSTRACT FROM AUTHOR]

Published
2012
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257. Weak lensing from space: first cosmological constraints from three-point shear statistics.

Author

Semboloni, Elisabetta, Schrabback, Tim, van Waerbeke, Ludovic, Vafaei, Sanaz, Hartlap, Jan, and Hilbert, Stefan

Subjects
GRAVITATIONAL lenses, CONSTRAINTS (Physics), SHEAR (Mechanics), COSMIC background radiation, SIMULATION methods & models, DARK matter
Abstract

We use weak lensing data from the Hubble Space Telescope COSMOS survey to measure the second- and third-order moments of the cosmic shear field, estimated from about 450 000 galaxies with average redshift . We measure two- and three-point shear statistics using a tree-code, dividing the signal in E, B and mixed components. We present a detection of the third-order moment of the aperture mass statistic and verify that the measurement is robust against systematic errors caused by point spread function (PSF) residuals and by the intrinsic alignments between galaxies. The amplitude of the measured three-point cosmic shear signal is in very good agreement with the predictions for a 7-yr Wilkinson Microwave Anisotropy Probe ( WMAP7) best-fitting model, whereas the amplitudes of potential systematics are consistent with zero. We make use of three sets of large Lambda cold dark matter () simulations to test the accuracy of the cosmological predictions and to estimate the influence of the cosmology-dependent covariance. We perform a likelihood analysis using the measurement of and find that the degeneracy direction is well fitted by the relation: which is in good agreement with the best-fitting relation obtained by using the measurement of : . We present the first measurement of the more generalized three-point shear statistic and find a very good agreement with the WMAP7 best-fitting cosmology. The cosmological interpretation of gives . Furthermore, the combined likelihood analysis of and improves the accuracy of the cosmological constraints to , showing the high potential of this combination of measurements to infer cosmological constraints. [ABSTRACT FROM AUTHOR]

Published
2011
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258. Large-scale structure and dynamics of the most X-ray luminous galaxy cluster known – RX J1347−1145.

Author

Ting Lu, Gilbank, David G., Balogh, Michael L., Milkeraitis, Martha, Hoekstra, Henk, Van Waerbeke, Ludovic, Wake, David A., Edge, Alastair C., and Bower, Richard G.

Subjects
GALAXY clusters, X-rays, ASTRONOMICAL instruments, SPECTRUM analysis instruments, ASTRONOMY
Abstract

We present photometric, spectroscopic and weak lensing analysis of the large-scale structure and dynamics of the most X-ray luminous galaxy cluster known, RX , at . We spectroscopically confirmed 47 new members with Low Dispersion Survey Spectrograph 3 (LDSS3) on the Magellan telescope. Together with previously known members, we measure a new velocity dispersion of . The mass inferred from our velocity dispersion is , with , under the assumption of a singular isothermal sphere. We also present a weak lensing analysis using deep Canada–France–Hawaii Telescope (CFHT) data on this cluster, and find a deprojected mass of within r200, in excellent agreement with our dynamical estimate. Thus, our new dynamical mass estimate is consistent with that from weak lensing and X-ray studies in the literature, resolving a previously claimed discrepancy. We photometrically detect and spectroscopically confirm another massive cluster with and south-west of RX , which we refer to as . Our spectroscopic survey reveals a possible excess of galaxies in velocity space in the region between RX and ; comparing with simulations, this excess appears consistent with that expected from a large filamentary structure traced by galaxies connecting these two clusters. [ABSTRACT FROM AUTHOR]

Published
2010
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259. Cosmological constraints from the 100-deg2 weak-lensing survey.

Author

Benjamin, Jonathan, Heymans, Catherine, Semboloni, Elisabetta, van Waerbeke, Ludovic, Hoekstra, Henk, Erben, Thomas, Gladders, Michael D., Hetterscheidt, Marco, Mellier, Yannick, and Yee, H. K. C.

Subjects
REDSHIFT, COSMOLOGICAL constant, SPECTRUM analysis, GALAXIES, POWER (Mechanics), SURVEYS
Abstract

We present a cosmic shear analysis of the 100-deg2 weak-lensing survey, combining data from the CFHTLS-Wide, RCS, VIRMOS-DESCART and GaBoDS surveys. Spanning ∼100 deg2, with a median source redshift , this combined survey allows us to place tight joint constraints on the matter density parameter Ωm, and the amplitude of the matter power spectrum σ8, finding . Tables of the measured shear correlation function and the calculated covariance matrix for each survey are included as supplementary material to the online version of this article. The accuracy of our results is a marked improvement on previous work owing to three important differences in our analysis; we correctly account for sample variance errors by including a non-Gaussian contribution estimated from numerical simulations; we correct the measured shear for a calibration bias as estimated from simulated data; we model the redshift distribution, , of each survey from the largest deep photometric redshift catalogue currently available from the CFHTLS-Deep. This catalogue is randomly sampled to reproduce the magnitude distribution of each survey with the resulting survey-dependent parametrized using two different models. While our results are consistent for the models tested, we find that our cosmological parameter constraints depend weakly (at the 5 per cent level) on the inclusion or exclusion of galaxies with low-confidence photometric redshift estimates . These high-redshift galaxies are relatively few in number but contribute a significant weak-lensing signal. It will therefore be important for future weak-lensing surveys to obtain near-infrared data to reliably determine the number of high-redshift galaxies in cosmic shear analyses. [ABSTRACT FROM AUTHOR]

Published
2007
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260. lemomaf: Lensed Mock Map Facility.

Author

Forero-Romero, Jaime E., Blaizot, Jérémy, Devriendt, Julien, Van Waerbeke, Ludovic, and Guiderdoni, Bruno

Subjects
GRAVITATIONAL lenses, LARGE scale structure (Astronomy), WAVELENGTHS, REDSHIFT, GALAXY formation, DENSITY functionals
Abstract

We present the Lensed Mock Map Facility (lemomaf), a tool designed to perform mock weak-lensing measurements on numerically simulated chunks of the Universe. Coupling N-body simulations to a semi-analytical model of galaxy formation,lemomaf can create realistic lensed images and mock catalogues of galaxies, at wavelengths ranging from the ultraviolet to the submillimetre. To demonstrate the power of such a tool, we compute predictions of the source–lens clustering (SLC) effect on the convergence statistics, and quantify the impact of weak lensing on galaxy counts in two different filters. We find that the SLC effect skews the probability density function of the convergence towards low values, with an intensity which strongly depends on the redshift distribution of galaxies. On the other hand, the degree of enhancement or depletion in galaxy counts due to weak lensing is independent of the SLC effect. We discuss the impact on the two-point shear statistics to be measured by future missions like SNAP and LSST. The SLC effect would bias the estimation of σ8 from two-point statistics up to 5 per cent for a narrow redshift distribution of mean , and up to 2 per cent in small angular scales for a redshift distribution of mean . We conclude that accurate photometric redshifts for individual galaxies are necessary in order to quantify and isolate the SLC effect. [ABSTRACT FROM AUTHOR]

Published
2007
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261. Cosmic variance of weak lensing surveys in the non-Gaussian regime.

Author

Semboloni, Elisabetta, Van Waerbeke, Ludovic, Heymans, Catherine, Hamana, Takashi, Colombi, Stephane, White, Martin, and Mellier, Yannick

Subjects
*GRAVITATIONAL lenses, *MICROLENSING (Astrophysics), *SURVEYS, *REDSHIFT, *CALIBRATION
Abstract

The results from weak gravitational lensing analyses are subject to a cosmic variance error term that has previously been estimated assuming Gaussian statistics. In this Letter we address the issue of estimating cosmic variance errors for weak lensing surveys in the non-Gaussian regime. Using standard cold dark matter model ray-tracing simulations characterized by and for different survey redshifts , we determine the variance of the two-point shear correlation function measured across 64 independent lines of sight. We compare the measured variance to the variance expected from a random Gaussian field and derive a redshift-dependent non-Gaussian calibration relation. We find that the ratio between the non-Gaussian and Gaussian variance at 1 arcmin can be as high as ∼30 for a survey with source redshift and ∼10 for . The transition scale above which the ratio is consistent with unity is found to be arcmin for and arcmin for . We provide fitting formulae to our results permitting the estimation of non-Gaussian cosmic variance errors, and discuss the impact on current and future surveys. A more extensive set of simulations will, however, be required to investigate the dependence of our results on cosmology, specifically on the amplitude of clustering. [ABSTRACT FROM AUTHOR]

Published
2007
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262. Results of the GREAT08 Challenge: an image analysis competition for cosmological lensing

Author

Bridle, Sarah, Balan, Sreekumar T., Bethge, Matthias, Gentile, Marc, Harmeling, Stefan, Heymans, Catherine, Hirsch, Michael, Hosseini, Reshad, Jarvis, Mike, Kirk, Donnacha, Kitching, Thomas, Kuijken, Konrad, Lewis, Antony, Paulin-Henriksson, Stephane, Schoelkopf, Bernhard, Velander, Malin, Voigt, Lisa, Witherick, Dugan, Amara, Adam, Bernstein, Gary, Courbin, Frederic, Gill, Mandeep, Heavens, Alan, Mandelbaum, Rachel, Massey, Richard, Moghaddam, Baback, Rassat, Anais, Refregier, Alexandre, Rhodes, Jason, Schrabback, Tim, Shawe-Taylor, John, Shmakova, Marina, Van Waerbeke, Ludovic, and Wittman, David

Subjects
statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, techniques: image processing, gravitational lensing: weak, Large-scale structure of Universe, Intrinsic Alignments, Galaxy Shape Measurement, image processing [Techniques], Weak, data analysis [Methods], observations [Cosmology], Tomography, methods: statistical, Power Spectra, Requirements, Redshift, methods: data analysis, Dark Energy, weak, Methods: data analysis, Methods: statistical, Techniques: image processing, Cosmology: observations, Large-scale structure of universe [Gravitational lensing], cosmology: observations, Calibration, Cosmic Shear, large-scale structure of Universe, weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Monthly Notices of the Royal Astronomical Society, 405 (3), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

263. CFHTLenS: a weak lensing shear analysis of the 3D-Matched-Filter galaxy clusters

Author

Ford, Jes, Van Waerbeke, Ludovic, Milkeraitis, Martha, Laigle, Clotilde, Hildebrandt, Hendrik, Erben, Thomas, Heymans, Catherine, Hoekstra, Henk, Kitching, Thomas, Mellier, Yannick, Miller, Lance, Choi, Ami, Coupon, Jean, Fu, Liping, Hudson, Michael J., Kuijken, Konrad, Robertson, Naomi, Rowe, Barnaby, Schrabback, Tim, Velander, Malin, Ford, Jes, Van Waerbeke, Ludovic, Milkeraitis, Martha, Laigle, Clotilde, Hildebrandt, Hendrik, Erben, Thomas, Heymans, Catherine, Hoekstra, Henk, Kitching, Thomas, Mellier, Yannick, Miller, Lance, Choi, Ami, Coupon, Jean, Fu, Liping, Hudson, Michael J., Kuijken, Konrad, Robertson, Naomi, Rowe, Barnaby, Schrabback, Tim, and Velander, Malin

Abstract

We present the cluster mass-richness scaling relation calibrated by a weak lensing analysis of ≳ 18000 galaxy cluster candidates in the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). Detected using the 3D-Matched-Filter (MF) cluster-finder of Milkeraitis etal., these cluster candidates span a wide range of masses, from the small group scale up to∼1015 M⊙, and redshifts 0.2≲z≲0.9. The total significance of the stacked shear measurement amounts to 54σ. We compare cluster masses determined using weak lensing shear and magnification, finding the measurements in individual richness bins to yield 1σ compatibility, but with magnification estimates biased low. This first direct mass comparison yields important insights for improving the systematics handling of future lensing magnification work. In addition, we confirm analyses that suggest cluster miscentring has an important effect on the observed 3D-MF halo profiles, and we quantify this by fitting for projected cluster centroid offsets, which are typically∼0.4arcmin. We bin the cluster candidates as a function of redshift, finding similar cluster masses and richness across the full range up to z∼0.9. We measure the 3D-MF mass-richness scaling relation M200=M0(N200/20)β. We find a normalization $M_0 \sim (2.7^{+0.5}_{-0.4}) \times 10^{13} \,\mathrm{M}_{{\odot }}$, and a logarithmic slope of β∼1.4±0.1, both of which are in 1σ agreement with results from the magnification analysis. We find no evidence for a redshift dependence of the normalization. The CFHTLenS 3D-MF cluster catalogue is now available at cfhtlens.org

264. Cosmological constraints from weak lensing peak statistics with Canada-France-Hawaii Telescope Stripe 82 Survey

Author

Liu, Xiangkun, Pan, Chuzhong, Li, Ran, Shan, Huanyuan, Wang, Qiao, Fu, Liping, Fan, Zuhui, Kneib, Jean-Paul, Leauthaud, Alexie, Van Waerbeke, Ludovic, Makler, Martin, Moraes, Bruno, Erben, Thomas, Charbonnier, Aldée, Liu, Xiangkun, Pan, Chuzhong, Li, Ran, Shan, Huanyuan, Wang, Qiao, Fu, Liping, Fan, Zuhui, Kneib, Jean-Paul, Leauthaud, Alexie, Van Waerbeke, Ludovic, Makler, Martin, Moraes, Bruno, Erben, Thomas, and Charbonnier, Aldée

Abstract

We derived constraints on cosmological parameters using weak lensing peak statistics measured on the ∼ 130 deg2 of the Canada-France-Hawaii Telescope Stripe 82 Survey. This analysis demonstrates the feasibility of using peak statistics in cosmological studies. For our measurements, we considered peaks with signal-to-noise ratio in the range of ν = [3, 6]. For a flat Λ cold dark matter model with only (Ωm, σ8) as free parameters, we constrained the parameters of the following relation Σ8 = σ8(Ωm/0.27)α to be Σ8 = 0.82 ± 0.03 and α = 0.43 ± 0.02. The α value found is considerably smaller than the one measured in two-point and three-point cosmic shear correlation analyses, showing a significant complement of peak statistics to standard weak lensing cosmological studies. The derived constraints on (Ωm, σ8) are fully consistent with the ones from either WMAP9 or Planck. From the weak lensing peak abundances alone, we obtained marginalized mean values of $\Omega _{\rm m}=0.38^{+0.27}_{-0.24}$ and σ8 = 0.81 ± 0.26. Finally, we also explored the potential of using weak lensing peak statistics to constrain the mass-concentration relation of dark matter haloes simultaneously with cosmological parameters

265. The dark matter environment of the Abell 901/902 supercluster: a weak lensing analysis of the HST STAGES survey

Author

Heymans, Catherine, Gray, Meghan E., Peng, Chien Y., Van Waerbeke, Ludovic, Bell, Eric F., Wolf, Christian, Bacon, David, Balogh, Michael, Barazza, Fabio D., Barden, Marco, Böhm, Asmus, Caldwell, John A. R., Häußler, Boris, Jahnke, Knud, Jogee, Shardha, Van Kampen, Eelco, Lane, Kyle, McIntosh, Daniel H., Meisenheimer, Klaus, Mellier, Yannick, Sánchez, Sebastian F., Taylor, Andy N., Wisotzki, Lutz, Zheng, Xianzhong, Heymans, Catherine, Gray, Meghan E., Peng, Chien Y., Van Waerbeke, Ludovic, Bell, Eric F., Wolf, Christian, Bacon, David, Balogh, Michael, Barazza, Fabio D., Barden, Marco, Böhm, Asmus, Caldwell, John A. R., Häußler, Boris, Jahnke, Knud, Jogee, Shardha, Van Kampen, Eelco, Lane, Kyle, McIntosh, Daniel H., Meisenheimer, Klaus, Mellier, Yannick, Sánchez, Sebastian F., Taylor, Andy N., Wisotzki, Lutz, and Zheng, Xianzhong

Abstract

We present a high-resolution dark matter reconstruction of the z= 0.165 Abell 901/902 supercluster from a weak lensing analysis of the Hubble Space Telescope STAGES survey. We detect the four main structures of the supercluster at high significance, resolving substructure within and between the clusters. We find that the distribution of dark matter is well traced by the cluster galaxies, with the brightest cluster galaxies marking out the strongest peaks in the dark matter distribution. We also find a significant extension of the dark matter distribution of Abell 901a in the direction of an infalling X-ray group Abell 901α. We present mass, mass-to-light and mass-to-stellar mass ratio measurements of the structures and substructures that we detect. We find no evidence for variation of the mass-to-light and mass-to-stellar mass ratio between the different clusters. We compare our space-based lensing analysis with an earlier ground-based lensing analysis of the supercluster to demonstrate the importance of space-based imaging for future weak lensing dark matter ‘observations'

266. Large-scale structure and dynamics of the most X-ray luminous galaxy cluster known - RX J1347−1145

Author

Lu, Ting, Gilbank, David G., Balogh, Michael L., Milkeraitis, Martha, Hoekstra, Henk, Van Waerbeke, Ludovic, Wake, David A., Edge, Alastair C., Bower, Richard G., Lu, Ting, Gilbank, David G., Balogh, Michael L., Milkeraitis, Martha, Hoekstra, Henk, Van Waerbeke, Ludovic, Wake, David A., Edge, Alastair C., and Bower, Richard G.

Abstract

We present photometric, spectroscopic and weak lensing analysis of the large-scale structure and dynamics of the most X-ray luminous galaxy cluster known, RXJ1347−1145, at z=0.451. We spectroscopically confirmed 47 new members with Low Dispersion Survey Spectrograph 3 (LDSS3) on the Magellan telescope. Together with previously known members, we measure a new velocity dispersion of 1163 ± 97 km s−1. The mass inferred from our velocity dispersion is M200 = 1.16+0.32−0.27 × 1015M⊙ with r200 = 1.85 Mpc, under the assumption of a singular isothermal sphere. We also present a weak lensing analysis using deep Canada–France–Hawaii Telescope (CFHT) data on this cluster, and find a deprojected mass of 1.47+0.46−0.43 × 1015M⊙ within r200, in excellent agreement with our dynamical estimate. Thus, our new dynamical mass estimate is consistent with that from weak lensing and X-ray studies in the literature, resolving a previously claimed discrepancy. We photometrically detect and spectroscopically confirm another massive cluster with σ = 780 ± 100 km s−1 and M200 = 3.4+1.4−1.1 × 1014M⊙ ~ 7 Mpc south-west of RX J1347−1145, which we refer to as RXJ1347−SW. Our spectroscopic survey reveals a possible excess of galaxies in velocity space in the region between RX J1347−1145 and RXJ1347−SW; comparing with simulations, this excess appears consistent with that expected from a large filamentary structure traced by galaxies connecting these two clusters.

267. The Herschel-SPIRE Legacy Survey (HSLS): the scientific goals of a shallow and wide submillimeter imaging survey with SPIRE

Author

Cooray, Asantha, Eales, Steve, Chapman, Scott, Clements, David L., Dore, Olivier, Farrah, Duncan, Jarvis, Matt J., Kaplinghat, Manoj, Negrello, Mattia, Melchiorri, Alessandro, Peiris, Hiranya, Pope, Alexandra, Santos, Mario G., Serjeant, Stephen, Thompson, Mark, White, Glenn, Amblard, Alexandre, Banerji, Manda, Corasaniti, Pier-Stefano, Das, Sudeep, de Bernardis, Francesco, de Zotti, Gianfranco, Giannantonio, Tommaso, Gonzalez-Nuevo Gonzalez, Joaquin, Khostovan, Ali Ahmad, Mitchell-Wynne, Ketron, Serra, Paolo, Song, Yong-Seon, Vieira, Joaquin, Wang, Lingyu, Zemcov, Michael, Abdalla, Filipe, Afonso, Jose, Aghanim, Nabila, Andreani, Paola, Aretxaga, Itziar, Auld, Robbie, Baes, Maarten, Baker, Andrew, Barkats, Denis, Belen Barreiro, R., Bartolo, Nicola, Barton, Elizabeth, Barway, Sudhanshu, Stefano Battistelli, Elia, Baugh, Carlton, Beelen, Alexander, Benabed, Karim, Blain, Andrew, Bland-Hawthorn, Joss, Bock, James~J., Bond, J. Richard, Borrill, Julian, Borys, Colin, Boselli, Alessandro, Bouchet, Francois R., Bridge, Carrie, Brighenti, Fabrizio, Buat, Veronique, Buote, David, Burgarella, Denis, Bussmann, Robert, Calabrese, Erminia, Cantalupo, Christopher, Carlberg, Raymond, Sofia Carvalho, Carla, Casey, Caitlin, Cava, Antonio, Cepa, Jordi, Chapin, Edward, Chary, Ranga Ram, Chen, Xuelei, Colafrancesco, Sergio, Cole, Shaun, Coles, Peter, Conley, Alexander, Conversi, Luca, Cooke, Jeff, Crawford, Steven, Cress, Catherine, da Cunha, Elisabete, Dalton, Gavin, Danese, Luigi, Dannerbauer, Helmut, Davies, Jonathan, de Bernardis, Paolo, de Putter, Roland, Devlin, Mark, Diego, Jose M., Dole, Herve, Douspis, Marian, Dunkley, Joanna, Dunlop, James, Dunne, Loretta, Dunner, Rolando, Dye, Simon, Efstathiou, George, Egami, Eiichi, Fang, Taotao, Ferrero, Patrizia, Franceschini, Alberto, Frazer, Christopher C., Frayer, David, Frenk, Carlos, Ganga, Ken, Gavazzi, Raphael, Glenn, Jason, Gong, Yan, Gonzalez-Solares, Eduardo, Griffin, Matt, Guo, Qi, Gurwell, Mark, Hajian, Amir, Halpern, Mark, Hanson, Duncan, Hardcastle, Martin, Hatziminaoglou, Evanthia, Heavens, Alan, Heinis, Sebastien, Herranz, Diego, Hilton, Matt, Ho, Shirley, Holwerda, Benne W., Hopwood, Rosalind, Horner, Jonathan, Huffenberger, Kevin, Hughes, David H., Hughes, John P., Ibar, Edo, Ivison, Rob, Jackson, Neal, Jaffe, Andrew, Jenness, Timothy, Joncas, Gilles, Joudaki, Shahab, Kaviraj, Sugata, Kim, Sam, King, Lindsay, Kisner, Theodore, Knapen, Johan, Kniazev, Alexei, Komatsu, Eiichiro, Koopmans, Leon, Kuo, Chao-Lin, Lacey, Cedric, Lahav, Ofer, Lasenby, Anthony N., Lawrence, Andy, Lee, Myung Gyoon, Leeuw, Lerothodi L., Levenson, Louis R., Lewis, Geraint, Loaring, Nicola, Lopez-Caniego, Marcos, Maddox, Steve, Marriage, Tobias, Marsden, Gaelen, Martinez-Gonzalez, Enrique, Masi, Silvia, Matarrese, Sabino, Mathews, William G., Matsuura, Shuji, McMahon, Richard, Mellier, Yannick, Menanteau, Felipe, Michalowski, Michal~J., Millea, Marius, Mobasher, Bahram, Mohanty, Subhanjoy, Montier, Ludovic, Moodley, Kavilan, Moriarty-Schieven, Gerald H., Mortier, Angela, Munshi, Dipak, Murphy, Eric, Nandra, Kirpal, Natoli, Paolo, Nguyen, Hien, Oliver, Seb, Omont, Alain, Page, Lyman, Page, Mathew, Paladini, Roberta, Pandolfi, Stefania, Pascale, Enzo, Patanchon, Guillaume, Peacock, John, Pearson, Chris, Perez-Fournon, Ismael, Perez-Gonz, Pablo G., Piacentini, Francesco, Pierpaoli, Elena, Pohlen, Michael, Pointecouteau, Etienne, Polenta, Gianluca, Rawlings, Jason, Reese, Erik~D., Rigby, Emma, Rodighiero, Giulia, Romero-Colmenero, Encarni, Roseboom, Isaac, Rowan-Robinson, Michael, Sanchez-Portal, Miguel, Schmidt, Fabian, Schneider, Michael, Schulz, Bernhard, Scott, Douglas, Sedgwick, Chris, Sehgal, Neelima, Seymour, Nick, Sherwin, Blake~D., Short, Jo, Shupe, David, Sievers, Jonathan, Skibba, Ramin, Smidt, Joseph, Smith, Anthony, Smith, Daniel J. B., Smith, Matthew W. L., Spergel, David, Staggs, Suzanne, Stevens, Jason, Switzer, Eric, Takagi, Toshinobu, Takeuchi, Tsutomu, Temi, Pasquale, Trichas, Markos, Trigilio, Corrado, Tugwell, Katherine, Umana, Grazia, Vacca, William, Vaccari, Mattia, Vaisanen, Petri, Valtchanov, Ivan, van der Heyden, Kurt, van der Werf, Paul P., van Kampen, Eelco, van Waerbeke, Ludovic, Vegetti, Simona, Veneziani, Marcella, Verde, Licia, Verma, Aprajita, Vielva, Patricio, Viero, Marco P., Vila Vilaro, Baltasar, Wardlow, Julie, Wilson, Grant, Wright, Edward L., Xu, C. Kevin, Yun, Min S., Cooray, Asantha, Eales, Steve, Chapman, Scott, Clements, David L., Dore, Olivier, Farrah, Duncan, Jarvis, Matt J., Kaplinghat, Manoj, Negrello, Mattia, Melchiorri, Alessandro, Peiris, Hiranya, Pope, Alexandra, Santos, Mario G., Serjeant, Stephen, Thompson, Mark, White, Glenn, Amblard, Alexandre, Banerji, Manda, Corasaniti, Pier-Stefano, Das, Sudeep, de Bernardis, Francesco, de Zotti, Gianfranco, Giannantonio, Tommaso, Gonzalez-Nuevo Gonzalez, Joaquin, Khostovan, Ali Ahmad, Mitchell-Wynne, Ketron, Serra, Paolo, Song, Yong-Seon, Vieira, Joaquin, Wang, Lingyu, Zemcov, Michael, Abdalla, Filipe, Afonso, Jose, Aghanim, Nabila, Andreani, Paola, Aretxaga, Itziar, Auld, Robbie, Baes, Maarten, Baker, Andrew, Barkats, Denis, Belen Barreiro, R., Bartolo, Nicola, Barton, Elizabeth, Barway, Sudhanshu, Stefano Battistelli, Elia, Baugh, Carlton, Beelen, Alexander, Benabed, Karim, Blain, Andrew, Bland-Hawthorn, Joss, Bock, James~J., Bond, J. Richard, Borrill, Julian, Borys, Colin, Boselli, Alessandro, Bouchet, Francois R., Bridge, Carrie, Brighenti, Fabrizio, Buat, Veronique, Buote, David, Burgarella, Denis, Bussmann, Robert, Calabrese, Erminia, Cantalupo, Christopher, Carlberg, Raymond, Sofia Carvalho, Carla, Casey, Caitlin, Cava, Antonio, Cepa, Jordi, Chapin, Edward, Chary, Ranga Ram, Chen, Xuelei, Colafrancesco, Sergio, Cole, Shaun, Coles, Peter, Conley, Alexander, Conversi, Luca, Cooke, Jeff, Crawford, Steven, Cress, Catherine, da Cunha, Elisabete, Dalton, Gavin, Danese, Luigi, Dannerbauer, Helmut, Davies, Jonathan, de Bernardis, Paolo, de Putter, Roland, Devlin, Mark, Diego, Jose M., Dole, Herve, Douspis, Marian, Dunkley, Joanna, Dunlop, James, Dunne, Loretta, Dunner, Rolando, Dye, Simon, Efstathiou, George, Egami, Eiichi, Fang, Taotao, Ferrero, Patrizia, Franceschini, Alberto, Frazer, Christopher C., Frayer, David, Frenk, Carlos, Ganga, Ken, Gavazzi, Raphael, Glenn, Jason, Gong, Yan, Gonzalez-Solares, Eduardo, Griffin, Matt, Guo, Qi, Gurwell, Mark, Hajian, Amir, Halpern, Mark, Hanson, Duncan, Hardcastle, Martin, Hatziminaoglou, Evanthia, Heavens, Alan, Heinis, Sebastien, Herranz, Diego, Hilton, Matt, Ho, Shirley, Holwerda, Benne W., Hopwood, Rosalind, Horner, Jonathan, Huffenberger, Kevin, Hughes, David H., Hughes, John P., Ibar, Edo, Ivison, Rob, Jackson, Neal, Jaffe, Andrew, Jenness, Timothy, Joncas, Gilles, Joudaki, Shahab, Kaviraj, Sugata, Kim, Sam, King, Lindsay, Kisner, Theodore, Knapen, Johan, Kniazev, Alexei, Komatsu, Eiichiro, Koopmans, Leon, Kuo, Chao-Lin, Lacey, Cedric, Lahav, Ofer, Lasenby, Anthony N., Lawrence, Andy, Lee, Myung Gyoon, Leeuw, Lerothodi L., Levenson, Louis R., Lewis, Geraint, Loaring, Nicola, Lopez-Caniego, Marcos, Maddox, Steve, Marriage, Tobias, Marsden, Gaelen, Martinez-Gonzalez, Enrique, Masi, Silvia, Matarrese, Sabino, Mathews, William G., Matsuura, Shuji, McMahon, Richard, Mellier, Yannick, Menanteau, Felipe, Michalowski, Michal~J., Millea, Marius, Mobasher, Bahram, Mohanty, Subhanjoy, Montier, Ludovic, Moodley, Kavilan, Moriarty-Schieven, Gerald H., Mortier, Angela, Munshi, Dipak, Murphy, Eric, Nandra, Kirpal, Natoli, Paolo, Nguyen, Hien, Oliver, Seb, Omont, Alain, Page, Lyman, Page, Mathew, Paladini, Roberta, Pandolfi, Stefania, Pascale, Enzo, Patanchon, Guillaume, Peacock, John, Pearson, Chris, Perez-Fournon, Ismael, Perez-Gonz, Pablo G., Piacentini, Francesco, Pierpaoli, Elena, Pohlen, Michael, Pointecouteau, Etienne, Polenta, Gianluca, Rawlings, Jason, Reese, Erik~D., Rigby, Emma, Rodighiero, Giulia, Romero-Colmenero, Encarni, Roseboom, Isaac, Rowan-Robinson, Michael, Sanchez-Portal, Miguel, Schmidt, Fabian, Schneider, Michael, Schulz, Bernhard, Scott, Douglas, Sedgwick, Chris, Sehgal, Neelima, Seymour, Nick, Sherwin, Blake~D., Short, Jo, Shupe, David, Sievers, Jonathan, Skibba, Ramin, Smidt, Joseph, Smith, Anthony, Smith, Daniel J. B., Smith, Matthew W. L., Spergel, David, Staggs, Suzanne, Stevens, Jason, Switzer, Eric, Takagi, Toshinobu, Takeuchi, Tsutomu, Temi, Pasquale, Trichas, Markos, Trigilio, Corrado, Tugwell, Katherine, Umana, Grazia, Vacca, William, Vaccari, Mattia, Vaisanen, Petri, Valtchanov, Ivan, van der Heyden, Kurt, van der Werf, Paul P., van Kampen, Eelco, van Waerbeke, Ludovic, Vegetti, Simona, Veneziani, Marcella, Verde, Licia, Verma, Aprajita, Vielva, Patricio, Viero, Marco P., Vila Vilaro, Baltasar, Wardlow, Julie, Wilson, Grant, Wright, Edward L., Xu, C. Kevin, and Yun, Min S.

Abstract

A large sub-mm survey with Herschel will enable many exciting science opportunities, especially in an era of wide-field optical and radio surveys and high resolution cosmic microwave background experiments. The Herschel-SPIRE Legacy Survey (HSLS), will lead to imaging data over 4000 sq. degrees at 250, 350, and 500 micron. Major Goals of HSLS are: (a) produce a catalog of 2.5 to 3 million galaxies down to 26, 27 and 33 mJy (50% completeness; 5 sigma confusion noise) at 250, 350 and 500 micron, respectively, in the southern hemisphere (3000 sq. degrees) and in an equatorial strip (1000 sq. degrees), areas which have extensive multi-wavelength coverage and are easily accessible from ALMA. Two thirds of the of the sources are expected to be at z > 1, one third at z > 2 and about a 1000 at z > 5. (b) Remove point source confusion in secondary anisotropy studies with Planck and ground-based CMB data. (c) Find at least 1200 strongly lensed bright sub-mm sources leading to a 2% test of general relativity. (d) Identify 200 proto-cluster regions at z of 2 and perform an unbiased study of the environmental dependence of star formation. (e) Perform an unbiased survey for star formation and dust at high Galactic latitude and make a census of debris disks and dust around AGB stars and white dwarfs.

268. Results of the GREAT08 Challenge: an image analysis competition for cosmological lensing

Author

Bridle, Sarah, Balan, Sreekumar T., Bethge, Matthias, Gentile, Marc, Harmeling, Stefan, Heymans, Catherine, Hirsch, Michael, Hosseini, Reshad, Jarvis, Mike, Kirk, Donnacha, Kitching, Thomas, Kuijken, Konrad, Lewis, Antony, Paulin-Henriksson, Stephane, Schölkopf, Bernhard, Velander, Malin, Voigt, Lisa, Witherick, Dugan, Amara, Adam, Bernstein, Gary, Courbin, Frédéric, Gill, Mandeep, Heavens, Alan, Mandelbaum, Rachel, Massey, Richard, Moghaddam, Baback, Rassat, Anais, Réfrégier, Alexandre, Rhodes, Jason, Schrabback, Tim, Shawe-Taylor, John, Shmakova, Marina, van Waerbeke, Ludovic, Wittman, David, Bridle, Sarah, Balan, Sreekumar T., Bethge, Matthias, Gentile, Marc, Harmeling, Stefan, Heymans, Catherine, Hirsch, Michael, Hosseini, Reshad, Jarvis, Mike, Kirk, Donnacha, Kitching, Thomas, Kuijken, Konrad, Lewis, Antony, Paulin-Henriksson, Stephane, Schölkopf, Bernhard, Velander, Malin, Voigt, Lisa, Witherick, Dugan, Amara, Adam, Bernstein, Gary, Courbin, Frédéric, Gill, Mandeep, Heavens, Alan, Mandelbaum, Rachel, Massey, Richard, Moghaddam, Baback, Rassat, Anais, Réfrégier, Alexandre, Rhodes, Jason, Schrabback, Tim, Shawe-Taylor, John, Shmakova, Marina, van Waerbeke, Ludovic, and Wittman, David

Abstract

We present the results of the Gravitational LEnsing Accuracy Testing 2008 (GREAT08) Challenge, a blind analysis challenge to infer weak gravitational lensing shear distortions from images. The primary goal was to stimulate new ideas by presenting the problem to researchers outside the shear measurement community. Six GREAT08 Team methods were presented at the launch of the Challenge and five additional groups submitted results during the 6-month competition. Participants analyzed 30 million simulated galaxies with a range in signal-to-noise ratio, point spread function ellipticity, galaxy size and galaxy type. The large quantity of simulations allowed shear measurement methods to be assessed at a level of accuracy suitable for currently planned future cosmic shear observations for the first time. Different methods perform well in different parts of simulation parameter space and come close to the target level of accuracy in several of these. A number of fresh ideas have emerged as a result of the Challenge including a re-examination of the process of combining information from different galaxies, which reduces the dependence on realistic galaxy modelling. The image simulations will become increasingly sophisticated in future GREAT Challenges, meanwhile the GREAT08 simulations remain as a benchmark for additional developments in shear measurement algorithms

269. CFHTLenS: co-evolution of galaxies and their dark matter haloes

Author

Hudson, Michael J., Gillis, Bryan R., Coupon, Jean, Hildebrandt, Hendrik, Erben, Thomas, Heymans, Catherine, Hoekstra, Henk, Kitching, Thomas D., Mellier, Yannick, Miller, Lance, Van Waerbeke, Ludovic, Bonnett, Christopher, Fu, Liping, Kuijken, Konrad, Rowe, Barnaby, Schrabback, Tim, Semboloni, Elisabetta, van Uitert, Edo, Velander, Malin, Hudson, Michael J., Gillis, Bryan R., Coupon, Jean, Hildebrandt, Hendrik, Erben, Thomas, Heymans, Catherine, Hoekstra, Henk, Kitching, Thomas D., Mellier, Yannick, Miller, Lance, Van Waerbeke, Ludovic, Bonnett, Christopher, Fu, Liping, Kuijken, Konrad, Rowe, Barnaby, Schrabback, Tim, Semboloni, Elisabetta, van Uitert, Edo, and Velander, Malin

Abstract

Galaxy-galaxy weak lensing is a direct probe of the mean matter distribution around galaxies. The depth and sky coverage of the Canada-France-Hawaii Telescope Legacy Survey yield statistically significant galaxy halo mass measurements over a much wider range of stellar masses (108.75 to 1011.3 M⊙) and redshifts (0.2

270. CFHTLenS: weak lensing constraints on the ellipticity of galaxy-scale matter haloes and the galaxy-halo misalignment

Author

Schrabback, Tim, Hilbert, Stefan, Hoekstra, Henk, Simon, Patrick, van Uitert, Edo, Erben, Thomas, Heymans, Catherine, Hildebrandt, Hendrik, Kitching, Thomas D., Mellier, Yannick, Miller, Lance, Van Waerbeke, Ludovic, Bett, Philip, Coupon, Jean, Fu, Liping, Hudson, Michael J., Joachimi, Benjamin, Kilbinger, Martin, Kuijken, Konrad, Schrabback, Tim, Hilbert, Stefan, Hoekstra, Henk, Simon, Patrick, van Uitert, Edo, Erben, Thomas, Heymans, Catherine, Hildebrandt, Hendrik, Kitching, Thomas D., Mellier, Yannick, Miller, Lance, Van Waerbeke, Ludovic, Bett, Philip, Coupon, Jean, Fu, Liping, Hudson, Michael J., Joachimi, Benjamin, Kilbinger, Martin, and Kuijken, Konrad

Abstract

We present weak lensing constraints on the ellipticity of galaxy-scale matter haloes and the galaxy-halo misalignment. Using data from the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS), we measure the weighted-average ratio of the aligned projected ellipticity components of galaxy matter haloes and their embedded galaxies, fh, split by galaxy type. We then compare our observations to measurements taken from the Millennium Simulation, assuming different models of galaxy-halo misalignment. Using the Millennium Simulation, we verify that the statistical estimator used removes contamination from cosmic shear. We also detect an additional signal in the simulation, which we interpret as the impact of intrinsic shape-shear alignments between the lenses and their large-scale structure environment. These alignments are likely to have caused some of the previous observational constraints on fh to be biased high. From CFHTLenS, we find fh=−0.04±0.25 for early-type galaxies, which is consistent with current models for the galaxy-halo misalignment predicting fh ≃ 0.20. For late-type galaxies we measure $f_\mathrm{h}=0.69_{-0.36}^{+0.37}$ from CFHTLenS. This can be compared to the simulated results which yield fh ≃ 0.02 for misaligned late-type models

271. The Herschel-SPIRE Legacy Survey (HSLS): the scientific goals of a shallow and wide submillimeter imaging survey with SPIRE

Author

Cooray, Asantha, Eales, Steve, Chapman, Scott, Clements, David L., Dore, Olivier, Farrah, Duncan, Jarvis, Matt J., Kaplinghat, Manoj, Negrello, Mattia, Melchiorri, Alessandro, Peiris, Hiranya, Pope, Alexandra, Santos, Mario G., Serjeant, Stephen, Thompson, Mark, White, Glenn, Amblard, Alexandre, Banerji, Manda, Corasaniti, Pier-Stefano, Das, Sudeep, de Bernardis, Francesco, de Zotti, Gianfranco, Giannantonio, Tommaso, Gonzalez-Nuevo Gonzalez, Joaquin, Khostovan, Ali Ahmad, Mitchell-Wynne, Ketron, Serra, Paolo, Song, Yong-Seon, Vieira, Joaquin, Wang, Lingyu, Zemcov, Michael, Abdalla, Filipe, Afonso, Jose, Aghanim, Nabila, Andreani, Paola, Aretxaga, Itziar, Auld, Robbie, Baes, Maarten, Baker, Andrew, Barkats, Denis, Belen Barreiro, R., Bartolo, Nicola, Barton, Elizabeth, Barway, Sudhanshu, Stefano Battistelli, Elia, Baugh, Carlton, Beelen, Alexander, Benabed, Karim, Blain, Andrew, Bland-Hawthorn, Joss, Bock, James~J., Bond, J. Richard, Borrill, Julian, Borys, Colin, Boselli, Alessandro, Bouchet, Francois R., Bridge, Carrie, Brighenti, Fabrizio, Buat, Veronique, Buote, David, Burgarella, Denis, Bussmann, Robert, Calabrese, Erminia, Cantalupo, Christopher, Carlberg, Raymond, Sofia Carvalho, Carla, Casey, Caitlin, Cava, Antonio, Cepa, Jordi, Chapin, Edward, Chary, Ranga Ram, Chen, Xuelei, Colafrancesco, Sergio, Cole, Shaun, Coles, Peter, Conley, Alexander, Conversi, Luca, Cooke, Jeff, Crawford, Steven, Cress, Catherine, da Cunha, Elisabete, Dalton, Gavin, Danese, Luigi, Dannerbauer, Helmut, Davies, Jonathan, de Bernardis, Paolo, de Putter, Roland, Devlin, Mark, Diego, Jose M., Dole, Herve, Douspis, Marian, Dunkley, Joanna, Dunlop, James, Dunne, Loretta, Dunner, Rolando, Dye, Simon, Efstathiou, George, Egami, Eiichi, Fang, Taotao, Ferrero, Patrizia, Franceschini, Alberto, Frazer, Christopher C., Frayer, David, Frenk, Carlos, Ganga, Ken, Gavazzi, Raphael, Glenn, Jason, Gong, Yan, Gonzalez-Solares, Eduardo, Griffin, Matt, Guo, Qi, Gurwell, Mark, Hajian, Amir, Halpern, Mark, Hanson, Duncan, Hardcastle, Martin, Hatziminaoglou, Evanthia, Heavens, Alan, Heinis, Sebastien, Herranz, Diego, Hilton, Matt, Ho, Shirley, Holwerda, Benne W., Hopwood, Rosalind, Horner, Jonathan, Huffenberger, Kevin, Hughes, David H., Hughes, John P., Ibar, Edo, Ivison, Rob, Jackson, Neal, Jaffe, Andrew, Jenness, Timothy, Joncas, Gilles, Joudaki, Shahab, Kaviraj, Sugata, Kim, Sam, King, Lindsay, Kisner, Theodore, Knapen, Johan, Kniazev, Alexei, Komatsu, Eiichiro, Koopmans, Leon, Kuo, Chao-Lin, Lacey, Cedric, Lahav, Ofer, Lasenby, Anthony N., Lawrence, Andy, Lee, Myung Gyoon, Leeuw, Lerothodi L., Levenson, Louis R., Lewis, Geraint, Loaring, Nicola, Lopez-Caniego, Marcos, Maddox, Steve, Marriage, Tobias, Marsden, Gaelen, Martinez-Gonzalez, Enrique, Masi, Silvia, Matarrese, Sabino, Mathews, William G., Matsuura, Shuji, McMahon, Richard, Mellier, Yannick, Menanteau, Felipe, Michalowski, Michal~J., Millea, Marius, Mobasher, Bahram, Mohanty, Subhanjoy, Montier, Ludovic, Moodley, Kavilan, Moriarty-Schieven, Gerald H., Mortier, Angela, Munshi, Dipak, Murphy, Eric, Nandra, Kirpal, Natoli, Paolo, Nguyen, Hien, Oliver, Seb, Omont, Alain, Page, Lyman, Page, Mathew, Paladini, Roberta, Pandolfi, Stefania, Pascale, Enzo, Patanchon, Guillaume, Peacock, John, Pearson, Chris, Perez-Fournon, Ismael, Perez-Gonz, Pablo G., Piacentini, Francesco, Pierpaoli, Elena, Pohlen, Michael, Pointecouteau, Etienne, Polenta, Gianluca, Rawlings, Jason, Reese, Erik~D., Rigby, Emma, Rodighiero, Giulia, Romero-Colmenero, Encarni, Roseboom, Isaac, Rowan-Robinson, Michael, Sanchez-Portal, Miguel, Schmidt, Fabian, Schneider, Michael, Schulz, Bernhard, Scott, Douglas, Sedgwick, Chris, Sehgal, Neelima, Seymour, Nick, Sherwin, Blake~D., Short, Jo, Shupe, David, Sievers, Jonathan, Skibba, Ramin, Smidt, Joseph, Smith, Anthony, Smith, Daniel J. B., Smith, Matthew W. L., Spergel, David, Staggs, Suzanne, Stevens, Jason, Switzer, Eric, Takagi, Toshinobu, Takeuchi, Tsutomu, Temi, Pasquale, Trichas, Markos, Trigilio, Corrado, Tugwell, Katherine, Umana, Grazia, Vacca, William, Vaccari, Mattia, Vaisanen, Petri, Valtchanov, Ivan, van der Heyden, Kurt, van der Werf, Paul P., van Kampen, Eelco, van Waerbeke, Ludovic, Vegetti, Simona, Veneziani, Marcella, Verde, Licia, Verma, Aprajita, Vielva, Patricio, Viero, Marco P., Vila Vilaro, Baltasar, Wardlow, Julie, Wilson, Grant, Wright, Edward L., Xu, C. Kevin, Yun, Min S., Cooray, Asantha, Eales, Steve, Chapman, Scott, Clements, David L., Dore, Olivier, Farrah, Duncan, Jarvis, Matt J., Kaplinghat, Manoj, Negrello, Mattia, Melchiorri, Alessandro, Peiris, Hiranya, Pope, Alexandra, Santos, Mario G., Serjeant, Stephen, Thompson, Mark, White, Glenn, Amblard, Alexandre, Banerji, Manda, Corasaniti, Pier-Stefano, Das, Sudeep, de Bernardis, Francesco, de Zotti, Gianfranco, Giannantonio, Tommaso, Gonzalez-Nuevo Gonzalez, Joaquin, Khostovan, Ali Ahmad, Mitchell-Wynne, Ketron, Serra, Paolo, Song, Yong-Seon, Vieira, Joaquin, Wang, Lingyu, Zemcov, Michael, Abdalla, Filipe, Afonso, Jose, Aghanim, Nabila, Andreani, Paola, Aretxaga, Itziar, Auld, Robbie, Baes, Maarten, Baker, Andrew, Barkats, Denis, Belen Barreiro, R., Bartolo, Nicola, Barton, Elizabeth, Barway, Sudhanshu, Stefano Battistelli, Elia, Baugh, Carlton, Beelen, Alexander, Benabed, Karim, Blain, Andrew, Bland-Hawthorn, Joss, Bock, James~J., Bond, J. Richard, Borrill, Julian, Borys, Colin, Boselli, Alessandro, Bouchet, Francois R., Bridge, Carrie, Brighenti, Fabrizio, Buat, Veronique, Buote, David, Burgarella, Denis, Bussmann, Robert, Calabrese, Erminia, Cantalupo, Christopher, Carlberg, Raymond, Sofia Carvalho, Carla, Casey, Caitlin, Cava, Antonio, Cepa, Jordi, Chapin, Edward, Chary, Ranga Ram, Chen, Xuelei, Colafrancesco, Sergio, Cole, Shaun, Coles, Peter, Conley, Alexander, Conversi, Luca, Cooke, Jeff, Crawford, Steven, Cress, Catherine, da Cunha, Elisabete, Dalton, Gavin, Danese, Luigi, Dannerbauer, Helmut, Davies, Jonathan, de Bernardis, Paolo, de Putter, Roland, Devlin, Mark, Diego, Jose M., Dole, Herve, Douspis, Marian, Dunkley, Joanna, Dunlop, James, Dunne, Loretta, Dunner, Rolando, Dye, Simon, Efstathiou, George, Egami, Eiichi, Fang, Taotao, Ferrero, Patrizia, Franceschini, Alberto, Frazer, Christopher C., Frayer, David, Frenk, Carlos, Ganga, Ken, Gavazzi, Raphael, Glenn, Jason, Gong, Yan, Gonzalez-Solares, Eduardo, Griffin, Matt, Guo, Qi, Gurwell, Mark, Hajian, Amir, Halpern, Mark, Hanson, Duncan, Hardcastle, Martin, Hatziminaoglou, Evanthia, Heavens, Alan, Heinis, Sebastien, Herranz, Diego, Hilton, Matt, Ho, Shirley, Holwerda, Benne W., Hopwood, Rosalind, Horner, Jonathan, Huffenberger, Kevin, Hughes, David H., Hughes, John P., Ibar, Edo, Ivison, Rob, Jackson, Neal, Jaffe, Andrew, Jenness, Timothy, Joncas, Gilles, Joudaki, Shahab, Kaviraj, Sugata, Kim, Sam, King, Lindsay, Kisner, Theodore, Knapen, Johan, Kniazev, Alexei, Komatsu, Eiichiro, Koopmans, Leon, Kuo, Chao-Lin, Lacey, Cedric, Lahav, Ofer, Lasenby, Anthony N., Lawrence, Andy, Lee, Myung Gyoon, Leeuw, Lerothodi L., Levenson, Louis R., Lewis, Geraint, Loaring, Nicola, Lopez-Caniego, Marcos, Maddox, Steve, Marriage, Tobias, Marsden, Gaelen, Martinez-Gonzalez, Enrique, Masi, Silvia, Matarrese, Sabino, Mathews, William G., Matsuura, Shuji, McMahon, Richard, Mellier, Yannick, Menanteau, Felipe, Michalowski, Michal~J., Millea, Marius, Mobasher, Bahram, Mohanty, Subhanjoy, Montier, Ludovic, Moodley, Kavilan, Moriarty-Schieven, Gerald H., Mortier, Angela, Munshi, Dipak, Murphy, Eric, Nandra, Kirpal, Natoli, Paolo, Nguyen, Hien, Oliver, Seb, Omont, Alain, Page, Lyman, Page, Mathew, Paladini, Roberta, Pandolfi, Stefania, Pascale, Enzo, Patanchon, Guillaume, Peacock, John, Pearson, Chris, Perez-Fournon, Ismael, Perez-Gonz, Pablo G., Piacentini, Francesco, Pierpaoli, Elena, Pohlen, Michael, Pointecouteau, Etienne, Polenta, Gianluca, Rawlings, Jason, Reese, Erik~D., Rigby, Emma, Rodighiero, Giulia, Romero-Colmenero, Encarni, Roseboom, Isaac, Rowan-Robinson, Michael, Sanchez-Portal, Miguel, Schmidt, Fabian, Schneider, Michael, Schulz, Bernhard, Scott, Douglas, Sedgwick, Chris, Sehgal, Neelima, Seymour, Nick, Sherwin, Blake~D., Short, Jo, Shupe, David, Sievers, Jonathan, Skibba, Ramin, Smidt, Joseph, Smith, Anthony, Smith, Daniel J. B., Smith, Matthew W. L., Spergel, David, Staggs, Suzanne, Stevens, Jason, Switzer, Eric, Takagi, Toshinobu, Takeuchi, Tsutomu, Temi, Pasquale, Trichas, Markos, Trigilio, Corrado, Tugwell, Katherine, Umana, Grazia, Vacca, William, Vaccari, Mattia, Vaisanen, Petri, Valtchanov, Ivan, van der Heyden, Kurt, van der Werf, Paul P., van Kampen, Eelco, van Waerbeke, Ludovic, Vegetti, Simona, Veneziani, Marcella, Verde, Licia, Verma, Aprajita, Vielva, Patricio, Viero, Marco P., Vila Vilaro, Baltasar, Wardlow, Julie, Wilson, Grant, Wright, Edward L., Xu, C. Kevin, and Yun, Min S.

Abstract

A large sub-mm survey with Herschel will enable many exciting science opportunities, especially in an era of wide-field optical and radio surveys and high resolution cosmic microwave background experiments. The Herschel-SPIRE Legacy Survey (HSLS), will lead to imaging data over 4000 sq. degrees at 250, 350, and 500 micron. Major Goals of HSLS are: (a) produce a catalog of 2.5 to 3 million galaxies down to 26, 27 and 33 mJy (50% completeness; 5 sigma confusion noise) at 250, 350 and 500 micron, respectively, in the southern hemisphere (3000 sq. degrees) and in an equatorial strip (1000 sq. degrees), areas which have extensive multi-wavelength coverage and are easily accessible from ALMA. Two thirds of the of the sources are expected to be at z > 1, one third at z > 2 and about a 1000 at z > 5. (b) Remove point source confusion in secondary anisotropy studies with Planck and ground-based CMB data. (c) Find at least 1200 strongly lensed bright sub-mm sources leading to a 2% test of general relativity. (d) Identify 200 proto-cluster regions at z of 2 and perform an unbiased study of the environmental dependence of star formation. (e) Perform an unbiased survey for star formation and dust at high Galactic latitude and make a census of debris disks and dust around AGB stars and white dwarfs.

273. Proposed network to detect axion quark nugget dark matter.

Author

Xunyu Liang, Peshkov, Egor, Van Waerbeke, Ludovic, and Zhitnitsky, Ariel

Subjects
*DARK matter, *X-rays, *AXIONS, *QUARKS, *QUANTUM chromodynamics
Abstract

A network of synchronized detectors can increase the likelihood of discovering the QCD axion within the axion quark nugget (AQN) dark matter model. A similar network can also discriminate the x rays emitted by the AQNs from the background signal. These networks can provide information on the directionality of the dark matter flux (if any), as well as its velocity distribution, and can therefore test the Standard Halo Model. We show that the optimal configuration to detect AQN-induced axions is a triangular network of stations 100 km apart. For x rays, the optimal network is an array of tetrahedral units. [ABSTRACT FROM AUTHOR]

Published
2021
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274. Impulsive radio events in quiet solar corona and axion quark nugget dark matter.

Author

Shuailiang Ge, Siddiqui, Md Shahriar Rahim, Van Waerbeke, Ludovic, and Zhitnitsky, Ariel

Subjects
*DARK matter, *AXIONS, *SOLAR radio bursts, *QUARKS, *RADIOS, *SOLAR flares, *SOLAR corona
Abstract

The Murchison Widefield Array (MWA) recorded impulsive radio events in the quiet solar corona at frequencies 98, 120, 132, and 160 MHz [S. Mondal, D. Oberoi, and A. Mohan, Astrophys. J. 895, L39 (2020)]. We propose that these radio events are the direct manifestation of dark matter annihilation events within the axion quark nugget (AQN) framework. It has been argued [A. Zhitnitsky, J. Cosmol. Astropart. Phys. 10 (2017) 050; N. Raza, L. vanWaerbeke, and A. Zhitnitsky, Phys. Rev. D 98, 103527 (2018)] that the AQN-annihilation events in the quiet solar corona can be identified with the nanoflares conjectured by Parker [Astrophys. J. 264, 642 (1983)]. We further support this claim by demonstrating that observed impulsive radio events [S. Mondal, D. Oberoi, and A. Mohan, Astrophys. J. 895, L39 (2020)], including their rate of appearance, their temporal and spatial distributions, and their energetics, are matching the generic consequences of AQN annihilations in the quiet corona. We propose to test this idea by analyzing the correlated clustering of impulsive radio events in different frequency bands. These correlations are expressed in terms of the time delays between radio events in different frequency bands measured in seconds. We also make generic predictions for low (80 and 89 MHz) and high (179, 196, 217, and 240 MHz) frequency bands, that have been recorded, but not published, by Mondal et al. [Astrophys. J. 895, L392020]. We finally suggest to test our proposal by studying possible cross-correlation between MWA radio signals and Solar Orbiter recording of extreme UV photons (aka "campfires"). [ABSTRACT FROM AUTHOR]

Published
2020
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275. Axion quark nugget dark matter: Time modulations and amplifications.

Author

Xunyu Liang, Mead, Alexander, Siddiqui, Md Shahriar Rahim, Van Waerbeke, Ludovic, and Zhitnitsky, Ariel

Subjects
*DARK matter, *AXIONS, *SURFACE of the earth, *QUARKS
Abstract

We study the new mechanism of the axion production suggested recently in [H. Fischer, X. Liang, Y. Semertzidis, A. Zhitnitsky, and K. Zioutas, Phys. Rev. D 98, 043013 (2018), K. Lawson, X. Liang, A. Mead, M. S. R. Siddiqui, L. Van Waerbeke, and A. Zhitnitsky, Phys. Rev. D 100, 043531 (2019)]. This mechanism is based on the so-called axion quark nugget (AQN) dark matter model, which was originally invented to explain the similarity of the dark and visible cosmological matter densities. We perform numerical simulations to evaluate the axion flux on the Earth's surface. We examine annual and daily modulations, which have been studied previously and are known to occur for any type of dark matter. We also discuss a novel type of short time enhancements which are unique to the AQN model: the statistical fluctuations and burstlike amplification, both of which can drastically amplify the axion signal, up to a factor ∼10²-10³ for a very short period of time. The present work studies the AQN-induced axions within the mass window 10-6 eV≲ma≲10-3 eV with typical velocities ⟨va⟩∼0.6c. We also comment on the broadband detection strategy to search for such relativistic axions by studying the daily and annual time modulations as well as random burstlike amplifications. [ABSTRACT FROM AUTHOR]

Published
2020
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