000128122 001__ 128122
000128122 005__ 20190509132211.0
000128122 0247_ $$2doi$$a10.5075/epfl-thesis-4235
000128122 02470 $$2urn$$aurn:nbn:ch:bel-epfl-thesis4235-6
000128122 02471 $$2nebis$$a5666236
000128122 037__ $$aTHESIS
000128122 041__ $$aeng
000128122 088__ $$a4235
000128122 245__ $$aAstrophysical applications of gravitationally lensed quasars$$bfrom dark matter halos to the structure of quasar accretion disks
000128122 269__ $$a2008
000128122 260__ $$aLausanne$$bEPFL$$c2008
000128122 300__ $$a228
000128122 336__ $$aTheses
000128122 500__ $$aPrix "Mention EPFL Press 2010" Presses Polytechniques et Universitaires Romandes
000128122 520__ $$aGravitational lensing describes how light is deflected as it passes in the vicinity of a mass distribution. The amplitude of the deflection is proportional to the mass of the deflector, called "gravitational lens", and is generally weak, even for large masses. The faintness of this phenomenon explains why gravitational lensing remained essentially unobserved until the late 1970s (only gravitational lensing by the Sun has been observed during the solar eclipse of 1919). Before that time, gravitational lensing was considered merely as a theoretical curiosity. However, the situation dramatically changed with the discovery of the first extragalactic gravitational lens in 1979. Since then, together with the technological progress of astronomical instruments, gravitational lensing has turned from a curiosity into a powerful tool to address important astrophysical and cosmological questions. The present thesis focuses on applications related to gravitationally lensed quasars. Quasars are active galactic nuclei, where matter is heated up as it spirals down onto the central supermassive black hole. When a galaxy is located on the line of sight to a distant quasar, it acts as a gravitational lens and produces multiple images of this background source. The light of the quasar follows different paths for each of its images. Thus, variations of the intrinsic quasar luminosity are observed at different times in each image. The time delays between the images can be used to determine the Hubble constant H0, because they are inversely proportional to H0. This constant describes the current expansion rate of the Universe, and is one of the fundamental parameters of cosmological models. Many efforts have been spent over the years to determine H0, but its value is still poorly constrained. Gravitational lensing has the potential to noticeably decrease the uncertainty of H0. In practice, this requires regular and long-term monitoring of lensed quasars. We have run a series of numerical simulations to both optimize the available telescope time, and measure the time delays with an accuracy of a few percent. The results of these simulations are presented in the form of compact plots to be used to optimize the observational strategy of present and future monitoring programs. Once the time delays are measured, one can infer estimates of H0, provided several other observational constraints are available. A key element to accurately convert time delays into H0 is the redshift of the lensing galaxy. These redshift measurements are difficult because lensing galaxies are generally hidden in the glare of the much brighter quasar images. As a consequence, lens redshifts are often poorly constrained or even completely unknown. We have acquired spectroscopic data of sixteen lensing galaxies with the Very Large Telescope located in Chile. In combination with a powerful deconvolution algorithm, we determine the redshift of these sixteen lensing galaxies, which represents about 25% of all currently known quasar lensing galaxies. These results are useful for both H0 determinations and statistical studies of gravitational lenses, which can be used to provide new constraints on cosmological parameters. While the first part of this thesis focuses on the acquisition of observational constraints for the lens models, the main part consists in using the phenomenon of microlensing to determine the energy profile (or spatial structure) of quasar accretion disks. Microlensing is produced by the stars located in the lensing galaxy. These stars act as secondary lenses, and are called microlenses. Since the stars are moving in the galaxy, they induce flux and color variations in the images of the lensed quasar. These effects can be used as a natural telescope to probe the still mysterious inner structures of quasars with a spatial resolution about ten thousand times better than the capacities of current astronomical instruments, including the Very Large Telescope Interferometer. We present a three-year long spectrophotometric monitoring of the lensed quasar QSO 2237+0305, also known as the Einstein Cross, conducted at the Very Large Telescope. This monitoring reveals significant microlensing-induced variations in the spectra of the quasar images. In a subsequent analysis, we find that the source responsible for the optical and ultraviolet continuum has an energy profile well reproduced by a power-law R α λζ with ζ = 1.2 ± 0.3, where R is the size of the source emitting at wavelength λ. This agrees with the predictions of the standard thin accretion disk model and is, so far, the most accurate determination of a quasar energy profile. As a complement to our microlensing study, we have obtained high spectral and spatial resolution observations of the lensing galaxy of QSO 2237+0305. Our spectroscopic data are acquired with the SINFONI, FLAMES, and FORS2 spectrographs of the Very Large Telescope. We describe the reduction of these data, and provide the currently best and most complete determination of the kinematics of a gravitational lens. The comparison of our data with previously published dynamical models suggests that those may have overestimated the mass of the galaxy bulge. Thus, new and more sophisticated models are required. These models, combined with gravitational lensing, will provide two independent constraints on the mass distribution. This will allow to better determine the quantity and distribution of dark matter in this lensing galaxy, and especially in its extended halo.
000128122 586__ $$aEPFL, 2010
000128122 6531_ $$aaccretion disk
000128122 6531_ $$aastrophysics
000128122 6531_ $$acosmological parameters
000128122 6531_ $$acosmology
000128122 6531_ $$adark matter
000128122 6531_ $$adeconvolution
000128122 6531_ $$aEinstein Cross
000128122 6531_ $$agravitational lensing
000128122 6531_ $$aHubble constant
000128122 6531_ $$amicrolensing
000128122 6531_ $$aQSO 2237+0305
000128122 6531_ $$aquasar
000128122 6531_ $$aredshift
000128122 6531_ $$aspectroscopy
000128122 6531_ $$atime delay
000128122 6531_ $$aastrophysique
000128122 6531_ $$aconstante de Hubble
000128122 6531_ $$acosmologie
000128122 6531_ $$aCroix d'Einstein
000128122 6531_ $$adécalage vers le rouge (redshift)
000128122 6531_ $$adéconvolution
000128122 6531_ $$adisque d'accrétion
000128122 6531_ $$alentille gravitationnelle
000128122 6531_ $$amatière sombre
000128122 6531_ $$amicrolentille
000128122 6531_ $$aparamètres cosmologiques
000128122 6531_ $$aQSO 2237+0305
000128122 6531_ $$aquasar
000128122 6531_ $$aretard temporel
000128122 6531_ $$aspectroscopie
000128122 700__ $$0245113$$aEigenbrod, Alexander$$g162230
000128122 720_2 $$0244706$$aMeylan, Georges$$edir.$$g158695
000128122 720_2 $$0245072$$aCourbin, Frédéric$$edir.$$g166196
000128122 8564_ $$uhttp://commission-recherche.epfl.ch/op/edit/page-42230.html$$zAward
000128122 8564_ $$s42185407$$uhttps://infoscience.epfl.ch/record/128122/files/EPFL_TH4235.pdf$$yTexte intégral / Full text$$zTexte intégral / Full text
000128122 909C0 $$0252365$$pLASTRO$$xU10933
000128122 909CO $$ooai:infoscience.tind.io:128122$$pDOI$$pGLOBAL_SET$$pSB$$pthesis$$pthesis-bn2018$$qDOI2
000128122 918__ $$aSB$$cIPEP$$dEDPY
000128122 919__ $$aLASTRO
000128122 920__ $$b2008
000128122 970__ $$a4235/THESES
000128122 973__ $$aEPFL$$sPUBLISHED
000128122 980__ $$aTHESIS