Dominique Sluse
University of Liège
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Featured researches published by Dominique Sluse.
Monthly Notices of the Royal Astronomical Society | 2017
V. Bonvin; F. Courbin; Sherry H. Suyu; Phil Marshall; Cristian E. Rusu; Dominique Sluse; M. Tewes; Kenneth C. Wong; Thomas E. Collett; C. D. Fassnacht; Tommaso Treu; Matthew W. Auger; Stefan Hilbert; Léon V. E. Koopmans; G. Meylan; N. Rumbaugh; Alessandro Sonnenfeld; C. Spiniello
We present a new measurement of the Hubble Constant H-0 and other cosmological parameters based on the joint analysis of three multiply imaged quasar systems with measured gravitational time delays. First, we measure the time delay of HE 0435-1223 from 13-yr light curves obtained as part of the COSMOGRAIL project. Companion papers detail the modelling of the main deflectors and line-of-sight effects, and how these data are combined to determine the time-delay distance of HE 0435-1223. Crucially, the measurements are carried out blindly with respect to cosmological parameters in order to avoid confirmation bias. We then combine the time-delay distance of HE 0435-1223 with previous measurements from systems B1608+656 and RXJ1131-1231 to create a Time Delay Strong Lensing probe (IDSL). In flat A cold dark matter (ACDM) with free matter and energy density, we find H-0 = 71.9(-3.0)(+2.4) km s(-1) Mpc(-1) and Omega(Lambda) = 0.62(-0.35)(+0.24) This measurement is completely independent of, and in agreement with, the local distance ladder measurements of H-0. We explore more general cosmological models combining TDSL with other probes, illustrating its power to break degeneracies inherent to other methods. The joint constraints from IDSL and Planck are H-0 = 69.2(-2.2)(+1.4) km s(-1) Mpc(-1), Omega(Lambda) = 0.70(-0.01)(+0.01) and Omega(k) = 0.003(-0.006)(+0.004) in open ACDM and H-0 = 79.0(-4.2)(+4.4) km s(-1) Mpc(-1), Omega(de) = 0.77(-0.03)(+0.02) and w = -1.38(-0.16)(+0.14) in flat wCDM. In combination with Planck and baryon acoustic oscillation data, when relaxing the constraints on the numbers of relativistic species we find N-eff = 3.34(-0.21)(+0.21) in N-eff Lambda CDM and when relaxing the total mass of neutrinos we find Sigma rn(nu) <= 0.182 eV in m(nu) Lambda CDM. Finally, in an open wCDM in combination with Planck and cosmic microwave background lensing, we find H-0 = 77.9(-4.2)(+5.0) km s(-1) Mpc(-1), Omega(de) = 0.77(-0.03)(+0.03), Omega(k) = -0.003(-0.004)(+0.004) and w = -1.37(-0.23)(+0.18).
Astronomy and Astrophysics | 2005
Damien Hutsemekers; R. Cabanac; H. Lamy; Dominique Sluse
Based on a new sample of 355 quasars with significant optical polarization and using complementary statistical methods, we confirm that quasar polarization vectors are not randomly oriented over the sky with a probability often in excess of 99.9%. The polarization vectors appear coherently oriented or aligned over huge (~1 Gpc) regions of the sky located at both low (
Astronomy and Astrophysics | 2013
M. Tewes; F. Courbin; G. Meylan; Christopher S. Kochanek; Eva Eulaers; N. Cantale; A. M. Mosquera; Pierre Magain; H. Van Winckel; Dominique Sluse; G. Cataldi; D. Voros; Simon Dye
z \sim 0.5
Astronomy and Astrophysics | 2011
F. Courbin; Virginie Chantry; Y. Revaz; Dominique Sluse; C. Faure; M. Tewes; Eva Eulaers; Mina Koleva; I. Asfandiyarov; S. Dye; Pierre Magain; H. Van Winckel; Jonathan A. Coles; Prasenjit Saha; M. Ibrahimov; G. Meylan
) and high (
Astronomy and Astrophysics | 2013
Peter Schneider; Dominique Sluse
z \sim 1.5
Astronomy and Astrophysics | 2012
Dominique Sluse; Damien Hutsemekers; F. Courbin; G. Meylan; Joachim Wambsganss
) redshifts and characterized by different preferred directions of the quasar polarization. In fact, there seems to exist a regular alternance along the line of sight of regions of randomly and aligned polarization vectors with a typical comoving length scale of 1.5 Gpc. Furthermore, the mean polarization angle
Astronomy and Astrophysics | 2011
Dominique Sluse; R. W. Schmidt; F. Courbin; Damien Hutsemekers; G. Meylan; A. Eigenbrod; T. Anguita; Eric Agol; Joachim Wambsganss
\bar{\theta}
Monthly Notices of the Royal Astronomical Society | 2017
Sherry H. Suyu; V. Bonvin; F. Courbin; C. D. Fassnacht; Cristian E. Rusu; Dominique Sluse; Tommaso Treu; Kenneth C. Wong; Matthew W. Auger; Xuheng Ding; Stefan Hilbert; Philip J. Marshall; N. Rumbaugh; Alessandro Sonnenfeld; M. Tewes; O. Tihhonova; A. Agnello; R. D. Blandford; Geoff C. F. Chen; Thomas E. Collett; Léon V. E. Koopmans; Kai Liao; G. Meylan; C. Spiniello
appears to rotate with redshift at the rate of ~30° per Gpc. The symmetry of the the
Monthly Notices of the Royal Astronomical Society | 2015
D. Xu; Dominique Sluse; Liang Gao; Jie Wang; Carlos S. Frenk; Shude Mao; Peter Schneider; Volker Springel
\bar{\theta} -z
Astronomy and Astrophysics | 2007
Dominique Sluse; Jean-François Claeskens; Damien Hutsemekers; Jean Surdej
relation is mirror-like, the mean polarization angle rotating clockwise with increasing redshift in North Galactic hemisphere and counter-clockwise in the South Galactic one. These characteristics make the alignment effect difficult to explain in terms of local mechanisms, namely a contamination by interstellar polarization in our Galaxy. While interpretations like a global rotation of the Universe can potentially explain the effect, the properties we observe qualitatively correspond to the dichroism and birefringence predicted by photon-pseudoscalar oscillation within a magnetic field. Interestingly, the alignment effect seems to be prominent along an axis not far from preferred directions tentatively identified in the Cosmic Microwave Background maps. Although many questions and more particularly the interpretation of the effect remain open, alignments of quasar polarization vectors appear as a promising new way to probe the Universe and its dark components at extremely large scales.