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I address the problem of finding a background model for the estimation of resistivities in the earth from controlled-source electromagnetic (CSEM) data by using seismic data and well logs as constraints. Estimation of resistivities is normally done by trial-and-error, in a process called “inversion”, by finding a model of the earth whose responses match the data to within an acceptable error; what comes out of the inversion is what is put into the model by the geophysicist: it does not come out of the data directly. The premise underlying this thesis is that an earth model can be found that satisfies not only the CSEM data but also the seismic data and any well logs. I present a methodology to determine background resistivities from seismic velocities using rock physics, structural constraints, and depth trends. The physical parameters of the seismic wave equation are different from those in the electromagnetic diffusion equation, so there is no direct link between the governing equations. I therefore use a Bayesian framework to incorporate not only the errors in the data and our limited knowledge of the rock parameters, but also the uncertainty of our chosen and calibrated velocity-to-resistivity transform. To test the methodology I use a well log from the North Sea Harding South oil and gas field to calibrate the transform, and apply it to seismic velocities of the nearby Harding Central oil and gas field. I also use short-offset CSEM inversions to estimate the electric anisotropy and to improve the shallow part of the resistivity model, where there is no well control. Three-dimensional modelling of this resistivity model predicts the acquired CSEM data within the estimated uncertainty. This methodology makes it possible to estimate background resistivities from seismic velocities, well logs, and other available geophysical and geological data. Subsequent CSEM surveys can then focus on finding resistive anomalies relative to this background model; these are, potentially, hydrocarbon-bearing formations.

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Insufficient instrument thermomechanical stability is one of the many roadblocks for achieving 10 cm s(-1) Doppler radial velocity precision, the precision needed to detect Earth-twins orbiting solar-type stars. Highly temperature and pressure stabilized spectrographs allow us to better calibrate out instrumental drifts, thereby helping in distinguishing instrumental noise from astrophysical stellar signals. We present the design and performance of the Environmental Control System (ECS) for the Habitable-zone Planet Finder (HPF), a high-resolution (R = 50,000) fiber-fed near-infrared (NIR) spectrograph for the 10 m Hobby-Eberly Telescope at McDonald Observatory. HPF will operate at 180 K, driven by the choice of an H2RG NIR detector array with a 1.7 mu m cutoff. This ECS has demonstrated 0.6 mK rms stability over 15 days at both 180 and 300 K, and maintained high-quality vacuum (< 10 (7) Torr) over months, during long-term stability tests conducted without a planned passive thermal enclosure surrounding the vacuum chamber. This control scheme is versatile and can be applied as a blueprint to stabilize future NIR and optical high-precision Doppler instruments over a wide temperature range from similar to 77 K to elevated room temperatures. A similar ECS is being implemented to stabilize NEID, the NASA/NSF NN-EXPLORE spectrograph for the 3.5 m WIYN telescope at Kitt Peak, operating at 300 K. A [full SolidWorks 3D-CAD model] and a comprehensive parts list of the HPF ECS are included with this manuscript to facilitate the adaptation of this versatile environmental control scheme in the broader astronomical community.

Peculiar velocities are possibly the most powerful probes of very large-scale mass density fluctuations in the nearby Universe. When coupled with a density field they also can constrain the growth factor of the universe by measuring the proportionality constant between observed velocities and linear theory predicted velocities. In this thesis, I measure a bulk flow of SN within 20,000 km s^1 of 197 +/- 56 km s^1 in direction l = 295 deg +/- 16deg, b = 11deg +/- 14deg , which is consistent with predictions of ΛCDM for large scale mass density fluctuations. Using the IRAS Point Source Catalog Redshift survey (PSCz) galaxy density field and the SNe peculiar velocities I calculated Ω^55_m σ8 to be 0.40 +/- 0.07 which is in excellent agreement with the results of WMAP7: Ω^55_m σ8 = 0.39 +/-0.04. By combining my measured value of with results from other studies, I measure the growth factor γ to be = 0.621 +/- 0.08 which is consistent with Λ CDM's prediction of 0.55. I conclude by exploring some of the systematic errors that could have affected my measurements of β. I find that when β is measured using a reconstruction method the result can be underestimated by between 7 and 15 %.

No description available.

Peculiar velocities are possibly the most powerful probes of very large-scale mass density fluctuations in the nearby Universe. When coupled with a density field they also can constrain the growth factor of the universe by measuring the proportionality constant between observed velocities and linear theory predicted velocities. In this thesis, I measure a bulk flow of SN within 20,000 km s^1 of 197 +/- 56 km s^1 in direction l = 295 deg +/- 16deg, b = 11deg +/- 14deg , which is consistent with predictions of ΛCDM for large scale mass density fluctuations. Using the IRAS Point Source Catalog Redshift survey (PSCz) galaxy density field and the SNe peculiar velocities I calculated Ω^55_m σ8 to be 0.40 +/- 0.07 which is in excellent agreement with the results of WMAP7: Ω^55_m σ8 = 0.39 +/-0.04. By combining my measured value of with results from other studies, I measure the growth factor γ to be = 0.621 +/- 0.08 which is consistent with Λ CDM's prediction of 0.55. I conclude by exploring some of the systematic errors that could have affected my measurements of β. I find that when β is measured using a reconstruction method the result can be underestimated by between 7 and 15 %.

Evaluation of the effect of particle cementation on the stiffness of uniform sand was carried out by measuring compression wave velocities (VP) and shear wave velocities (VS) on both clean and artificially cemented specimens. Piezoelectric transducers (PT) were used to perform the majority of the measurements. Shear wave velocity (VS), shear moduli (G) and material damping ratio (D) of clean and artificially cemented specimens were also determined using resonant column (RC) testing. Linear (shearing strains ≤ 0.001%) and nonlinear (shearing strains > 0.001%) behavior of the specimens were evaluated in the resonant column tests. The sand selected for this investigation is commonly known as Hickory sand, from the Hickory formation, western Llano uplift, Texas. This material was selected for its grain geometry and gradation; it consists of uniformly graded sand with rounded particles. The sand specimens were artificially cemented with a solution of hydrated sodium silicate and water. Sodium silicate is an alkaline compound obtained from the reaction of sodium hydroxide and silica. All artificially cemented specimens and uncemented hickory sand specimens were formed by pluviation through air. The microstructure of the specimens was visually assessed with images obtained from both optical and scanning electron (SEM) microscopes. These images confirmed that the procedure used to form artificially cemented specimens provides cementation around the contacts while some grain-to-grain contact appears to be preserved. Seismic and drained strength measurements on Hickory sand specimens were obtained from different cement concentrations and compared with results from clean sand specimens. Among the findings of this investigation are: (1) the procedure to artificially cement sand specimens in the laboratory was successful, (2) the slopes (nP and nS) obtained from the relationships between compression and shear wave velocities with effective isotropic confining pressure in log-log scale decrease as the cement content increases, and (3) as increasing amounts of cement are added to the sand particles, the nonlinearity of the specimens increases up to certain amount of cement, after which the nonlinearity of the specimen decreases and tends towards rock-like behavior. / text

We study the motion of giant stars in the Solar neighbourhood and what they tell us about the dynamics of the Galaxy: we thus contribute to the huge project of understanding the structure and evolution of the Galaxy as a whole. We present a kinematic analysis of 5952 K and 739 M giant stars which includes for the first time radial velocity data from an important survey performed with the CORAVEL spectrovelocimeter at the Observatoire de Haute Provence. Parallaxes from the Hipparcos catalogue and proper motions from the Tycho-2 catalogue are also used. A maximum-likelihood method, based on a bayesian approach, is applied to the data, in order to make full use of all the available stars, and to derive the kinematic properties of the subgroups forming a rich small-scale structure in velocity space. Isochrones in the Hertzsprung-Russell diagram reveal a very wide range of ages for stars belonging to these subgroups, which are thus most probably related to the dynamical perturbation by transient spiral waves rather than to cluster remnants. A possible explanation for the presence of young group/clusters in the same area of velocity space is that they have been put there by the spiral wave associated with their formation, while the kinematics of the older stars of our sample has also been disturbed by the same wave. The emerging picture is thus one of "dynamical streams" pervading the Solar neighbourhood and travelling in the Galaxy with a similar spatial velocity. The term "dynamical stream" is more appropriate than the traditional term "supercluster" since it involves stars of different ages, not born at the same place nor at the same time. We then discuss, in the light of our results, the validity of older evaluations of the Solar motion in the Galaxy. We finally argue that dynamical modeling is essential for a better understanding of the physics hiding behind the observed kinematics. An accurate axisymmetric model of the Galaxy is a necessary starting point in order to understand the true effects of non-axisymmetric perturbations such as spiral waves. To establish such a model, we develop new galactic potentials that fit some fundamental parameters of the Milky Way. We also develop new component distribution functions that depend on three analytic integrals of the motion and that can represent realistic stellar disks.