Publications
367 results found
Ade PAR, Aghanim N, Arnaud M, et al., 2011, <i>Planck</i> early results. XVII. Origin of the submillimetre excess dust emission in the Magellanic Clouds, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 123
Aatrokoski J, Ade PAR, Aghanim N, et al., 2011, <i>Planck</i> early results. XV. Spectral energy distributions and radio continuum spectra of northern extragalactic radio sources, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 95
Ade PAR, Aghanim N, Angelakis E, et al., 2011, <i>Planck</i> early results. XIV. ERCSC validation and extreme radio sources, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 57
Ade PAR, Aghanim N, Arnaud M, et al., 2011, <i>Planck</i> early results. VIII. The all-sky early Sunyaev-Zeldovich cluster sample, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 316
Abergel A, Ade PAR, Aghanim N, et al., 2011, <i>Planck</i> early results. XXV. Thermal dust in nearby molecular clouds, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 158
Abergel A, Ade PAR, Aghanim N, et al., 2011, <i>Planck</i> early results. XXIV. Dust in the diffuse interstellar medium and the Galactic halo, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 140
Ade PAR, Aghanim N, Arnaud M, et al., 2011, <i>Planck</i> early results. XVIII. The power spectrum of cosmic infrared background anisotropies, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 74
Ade PAR, Aghanim N, Arnaud M, et al., 2011, <i>Planck</i> early results. XIX. All-sky temperature and dust optical depth from <i>Planck</i> and IRAS. Constraints on the "dark gas" in our Galaxy, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 268
Ade PAR, Aghanim N, Arnaud M, et al., 2011, <i>Planck</i> early results. XXIII. The first all-sky survey of Galactic cold clumps, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 72
Aghanim N, Arnaud M, Ashdown M, et al., 2011, <i>Planck</i> early results. XXVI. Detection with <i>Planck</i> and confirmation by <i>XMM</i>-<i>Newton</i> of PLCK G266.6-27.3, an exceptionally X-ray luminous and massive galaxy cluster at <i>z</i> ∼ 1, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 69
Abergel A, Ade PAR, Aghanim N, et al., 2011, <i>Planck</i> early results. XXI. Properties of the interstellar medium in the Galactic plane, ASTRONOMY & ASTROPHYSICS, Vol: 536, ISSN: 0004-6361
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- Citations: 54
Watson LJ, Mortlock DJ, Jaffe AH, 2011, A Bayesian analysis of the 27 highest energy cosmic rays detected by the Pierre Auger Observatory, Monthly Notices of the Royal Astronomical Society, Vol: 418, Pages: 206-213, ISSN: 0035-8711
It is possible that ultrahigh energy cosmic rays (UHECRs) are generated by active galactic nuclei (AGNs), but there is currently no conclusive evidence for this hypothesis. Several reports of correlations between the arrival directions of UHECRs and the positions of nearby AGNs have been made, the strongest detection coming from a sample of 27 UHECRs detected by the Pierre Auger Observatory (PAO). However, the PAO results were based on a statistical methodology that not only ignored some relevant information (most obviously the UHECR arrival energies, but also some of the information in the arrival directions), but also involved some problematic fine-tuning of the correlation parameters. Here we present a fully Bayesian analysis of the PAO data (collected before 2007 September), which makes use of more of the available information, and find that a fraction FAGN= 0.15+0.10−0.07 of the UHECRs originate from known AGNs in the Veron-Cetty and Veron (VCV) catalogue. The hypothesis that all the UHECRs come from VCV AGNs is ruled out, although there remains a small possibility that the PAO–AGN correlation is coincidental (FAGN= 0.15 is 200 times as probable as FAGN= 0.00).
Bowyer J, Jaffe AH, 2011, Improved method for detecting local discontinuities in CMB data by finite differencing, Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol: 83, ISSN: 1550-2368
An unexpected distribution of temperatures in the CMB could be a sign of new physics. In particular, the existence of cosmic defects could be indicated by temperature discontinuities via the Kaiser-Stebbins effect. In this paper, we show how performing finite differences on a CMB map, with the noise regularized in harmonic space, may expose such discontinuities, and we report the results of this process on the 7-year Wilkinson Microwave Anisotropy Probe data.
Keating B, Moyerman S, Boettger D, et al., 2011, Ultra high energy cosmology with POLARBEAR
Observations of the temperature anisotropy of the Cosmic Microwave Background (CMB) lend support to an inflationary origin of the universe, yet no direct evidence verifying inflation exists. Many current experiments are focussing on the CMB's polarization anisotropy, specifically its curl component (called “B-mode” polarization), which remains undetected. The inflationary paradigm predicts the existence of a primordial gravitational wave background that imprints a unique B-mode signature on the CMB's polarization at large angular scales. The CMB B-mode signal also encodes gravitational lensing information at smaller angular scales, bearing the imprint of cosmological large scale structures (LSS) which in turn may elucidate the properties of cosmological neutrinos. The quest for detection of these signals; each of which is orders of magnitude smaller than the CMB temperature anisotropy signal, has motivated the development of background-limited detectors with precise control of systematic effects. The POLARBEAR experiment is designed to perform a deep search for the signature of gravitational waves from inflation and to characterize lensing of the CMB by LSS. POLARBEAR is a 3.5 meter ground-based telescope with 3.8 arcminute angular resolution at 150 GHz. At the heart of the POLARBEAR receiver is an array featuring 1274 antenna-coupled superconducting transition edge sensor (TES) bolometers cooled to 0.25 Kelvin. POLARBEAR is designed to reach a tensor-to-scalar ratio of 0.025 after two years of observation - more than an order of magnitude improvement over the current best results, which would test physics at energies near the GUT scale. POLARBEAR had an engineering run in the Inyo Mountains of Eastern California in 2010 and will begin observations in the Atacama Desert in Chile in 2011.
Keating B, Moyerman S, Boettger D, et al., 2011, Ultra high energy cosmology with POLARBEAR, Proceedings of the 2011 Meeting of the Division of Particles and Fields of the American Physical Society, DPF 2011
© Proceedings of the 2011 Meeting of the Division of Particles and Fields of the American Physical Society, DPF 2011. All rights reserved. Observations of the temperature anisotropy of the Cosmic Microwave Background (CMB) lend support to an inflationary origin of the universe, yet no direct evidence verifying inflation exists. Many current experiments are focussing on the CMB's polarization anisotropy, specifically its curl component (called “B-mode” polarization), which remains undetected. The inflationary paradigm predicts the existence of a primordial gravitational wave background that imprints a unique B-mode signature on the CMB's polarization at large angular scales. The CMB B-mode signal also encodes gravitational lensing information at smaller angular scales, bearing the imprint of cosmological large scale structures (LSS) which in turn may elucidate the properties of cosmological neutrinos. The quest for detection of these signals; each of which is orders of magnitude smaller than the CMB temperature anisotropy signal, has motivated the development of background-limited detectors with precise control of systematic effects. The POLARBEAR experiment is designed to perform a deep search for the signature of gravitational waves from inflation and to characterize lensing of the CMB by LSS. POLARBEAR is a 3.5 meter ground-based telescope with 3.8 arcminute angular resolution at 150 GHz. At the heart of the POLARBEAR receiver is an array featuring 1274 antenna-coupled superconducting transition edge sensor (TES) bolometers cooled to 0.25 Kelvin. POLARBEAR is designed to reach a tensor-to-scalar ratio of 0.025 after two years of observation - more than an order of magnitude improvement over the current best results, which would test physics at energies near the GUT scale. POLARBEAR had an engineering run in the Inyo Mountains of Eastern California in 2010 and will begin observations in the Atacama Desert in Chile in 2011.
Klein J, Aboobaker A, Ade P, et al., 2011, A Cryogenic Half-Wave Plate Polarimeter Using a Superconducting Magnetic Bearing, Conference on Cryogenic Optical Systems and Instruments XIII, Publisher: SPIE-INT SOC OPTICAL ENGINEERING, ISSN: 0277-786X
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- Citations: 13
Keskitalo R, Ashdown MAJ, Cabella P, et al., 2010, Residual noise covariance for <i>Planck</i> low-resolution data analysis, ASTRONOMY & ASTROPHYSICS, Vol: 522, ISSN: 0004-6361
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- Citations: 9
Tauber JA, Norgaard-Nielsen HU, Ade PAR, et al., 2010, <i>Planck</i> pre-launch status: The optical system, ASTRONOMY & ASTROPHYSICS, Vol: 520, ISSN: 0004-6361
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- Citations: 66
Tauber JA, Mandolesi N, Puget J-L, et al., 2010, <i>Planck</i> pre-launch status: The <i>Planck</i> mission, ASTRONOMY & ASTROPHYSICS, Vol: 520, ISSN: 0004-6361
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- Citations: 276
Aubin F, Aboobaker AM, Ade P, et al., 2010, First implementation of TES bolometer arrays with SQUID-based multiplexed readout on a balloon-borne platform, ISSN: 0277-786X
EBEX (the E and B EXperiment) is a balloon-borne telescope designed to measure the polarisation of the cosmic microwave background radiation. During a two week long duration science flight over Antarctica, EBEX will operate 768, 384 and 280 spider-web transition edge sensor (TES) bolometers at 150, 250 and 410 GHz, respectively. The 10-hour EBEX engineering flight in June 2009 over New Mexico and Arizona provided the first usage of both a large array of TES bolometers and a Superconducting QUantum Interference Device (SQUID) based multiplexed readout in a space-like environment. This successful demonstration increases the technology readiness level of these bolometers and the associated readout system for future space missions. A total of 82, 49 and 82 TES detectors were operated during the engineering flight at 150, 250 and 410 GHz. The sensors were read out with a new SQUID-based digital frequency domain multiplexed readout system that was designed to meet the low power consumption and robust autonomous operation requirements presented by a balloon experiment. Here we describe the system and the remote, automated tuning of the bolometers and SQUIDs. We compare results from tuning at float to ground, and discuss bolometer performance during flight. © 2010 SPIE.
Cantalupo CM, Borrill JD, Jaffe AH, et al., 2010, MADmap: A MASSIVELY PARALLEL MAXIMUM LIKELIHOOD COSMIC MICROWAVE BACKGROUND MAP-MAKER, ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Vol: 187, Pages: 212-227, ISSN: 0067-0049
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- Citations: 67
Juszkiewicz R, Feldman HA, Fry JN, et al., 2010, Weakly nonlinear dynamics and the sigma(8) parameter, Journal of Cosmology and Astroparticle Physics, Vol: 2010, ISSN: 1475-7516
The amplitude of cosmological density fluctuations, σ8, has been studied and estimated by analysing many cosmological observations. The values of the estimates vary considerably between the various probes. However, different estimators probe the value of σ8 in different cosmological scales and do not take into account the nonlinear evolution of the parameter at late times. We show that estimates of the amplitude of cosmological density fluctuations derived from cosmic flows are systematically higher than those inferred at early epochs from the CMB because of nonlinear evolution at later times. We discuss the past and future evolution of linear and nonlinear perturbations, derive corrections to the value of σ8 and compare amplitudes after accounting for these differences.
Paykari P, Jaffe AH, 2010, Optimal binning of the primordial power spectrum, Astrophysical Journal, Vol: 711, Pages: 1-12, ISSN: 0004-637X
The primordial power spectrum describes the initial perturbations in the universe, which eventually grew into the large-scale structure we observe today, and thereby provides an indirect probe of inflation or other structure-formation mechanisms. In this paper, we will investigate the best scales the primordial power spectrum can be probed with in accordance with the knowledge about other cosmological parameters such as Ωb, Ωc, ΩΛ, h, and τ. The aim is to find the most informative way of measuring the primordial power spectrum at different length scales, using different types of surveys and the information they provide for the desired cosmological parameters. We will find the optimal binning of the primordial power spectrum for this purpose by making use of the Fisher matrix formalism. To investigate the correlations between the cosmological parameters, mentioned above, and a set of primordial power spectrum bins, we make use of principal component analysis and the Hermitian square root of the Fisher matrix. The surveys used in this project are Planck and the Sloan Digital Sky Survey (Bright Red Galaxy), but the formalism can easily be extended to any windowed measurements of the perturbation spectrum. © 2010. The American Astronomical Society. All rights reserved.
Reichborn-Kjennerud B, Aboobaker AM, Ade P, et al., 2010, EBEX: A balloon-borne CMB polarization experiment, MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY V, Vol: 7741, ISSN: 0277-786X
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- Citations: 53
Milligan M, Ade P, Aubin F, et al., 2010, Software systems for operation, control, and monitoring of the EBEX instrument, SOFTWARE AND CYBERINFRASTRUCTURE FOR ASTRONOMY, Vol: 7740, ISSN: 0277-786X
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- Citations: 2
Arnold K, Ade PAR, Anthony AE, et al., 2010, The POLARBEAR CMB Polarization Experiment, Conference on Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V, Publisher: SPIE-INT SOC OPTICAL ENGINEERING, ISSN: 0277-786X
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- Citations: 23
Colombi S, Jaffe A, Novikov D, et al., 2009, Accurate estimators of power spectra in N-body simulations, Monthly Notices of the Royal Astronomical Society, Vol: 393, Pages: 511-526, ISSN: 1365-2966
Jaffe A, 2009, Not wrapped up yet, Physics World, Vol: 22, Pages: 36-37, ISSN: 0953-8585
Jaffe AH, 2009, Bayesian analysis of cosmic microwave background data, Bayesian Methods in Cosmology, Pages: 229-244, ISBN: 9780521887946
Introduction Surveying the Universe is the ultimate remote sensing problem. Inferring the intrinsic properties of the galaxy population, via analysis of survey-generated catalogues, is a major challenge for twenty-first century cosmology, but this challenge must be met without any prospect of measuring these properties in situ. Thus, for example, our knowledge of the intrinsic luminosity and spatial distribution of galaxies is filtered by imperfect distance information and by observational selection effects, issues which have come to be known generically in the literature as 'Malmquist bias'. Figure 11.1 shows schematically how such effects may distort our inferences about the underlying population since, in general, these must be derived from a noisy, sparse and truncated sample of galaxies. There is a long (and mostly honourable!) tradition in the astronomical literature of attempts to cast such remote surveying problems within a rigorous statistical framework. Indeed, it is interesting to note that seminal examples from the early twentieth century (Eddington 1913, 1940; Malmquist 1920, 1922) display, at least with hindsight, hints of a Bayesian formulation long before the recent renaissance of Bayesian methods in astronomy. Unfortunately, space does not permit us to review in detail that early literature, nor many of the more recent papers which evolved from it. A more thorough discussion of the literature on statistical analysis of survey data can be found in, e.g., Hendry and Simmons (1995), Strauss and Willick (1995), Teerikorpi (1997) and Loredo (2007).
Hobson MP, Jaffe AH, Liddle AR, et al., 2009, Bayesian methods in cosmology, ISBN: 9780521887946
In recent years cosmologists have advanced from largely qualitative models of the Universe to precision modelling using Bayesian methods, in order to determine the properties of the Universe to high accuracy. This timely book is the only comprehensive introduction to the use of Bayesian methods in cosmological studies, and is an essential reference for graduate students and researchers in cosmology, astrophysics and applied statistics. The first part of the book focuses on methodology, setting the basic foundations and giving a detailed description of techniques. It covers topics including the estimation of parameters, Bayesian model comparison, and separation of signals. The second part explores a diverse range of applications, from the detection of astronomical sources (including through gravitational waves), to cosmic microwave background analysis and the quantification and classification of galaxy properties. Contributions from 24 highly regarded cosmologists and statisticians make this an authoritative guide to the subject.
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- Citations: 43
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