Mainz, Univ., Diss., 2002. / Computerdatei im Fernzugriff.

Mainz, Univ., Diss., 2002. / Computerdatei im Fernzugriff.

Mainz, University, Diss., 2002.

Thesis (M.S.)--Brigham Young University. Dept. of Geological Sciences, 2008. / Includes bibliographical references (p. 40-45).

University, Diss., 2002--Mainz.

Universiẗat, Diss., 2005--Heidelberg.

Cumulate xenoliths erupted with alkalic hawaiite lavas from a postshield cinder cone on Mauna Kea, Hawaii include a variety of mafic and ultramafic rock types. Previous studies of major and trace element compositions of minerals in the xenoliths are interpreted to show transitional to alkalic magma parentages from the postshield stage, although any orthopyroxene-bearing xenoliths are considered to have tholeiitic parents. Major element compositions minerals were analyzed using the electron microprobe and trace element compositions of clinopyroxene grains were analyzed by laser ablation inductively coupled plasma mass spectrometry. In this study, major element compositions of clinopyroxene, olivine and plagioclase grains and trace element compositions in clinopyroxene grains in xenoliths lacking orthopyroxene indicate a transitional magma parentage consistant with postshield magmas. Trace element compositions of possible parent magmas of the xenoliths were calculated from clinopyroxene compositions using partition coefficients for basaltic liquids from Hauri et al. (1994). Liquids calculated from the clinopyroxene in the xenoliths were compared to Mauna Kea shield lavas and to the postshield Hamakua and Laupahoehoe units. Chondrite-normalized rare earth element (REE) patterns of liquids calculated from both orthopyroxene-bearing xenoliths and those without orthopyroxene were similar REE patterns of both Mauna Kea postshield tholeitic and alkalic lavas. Liquids from a wehrlite and an olivine gabbronorite have REE patterns similar to tholeiitic shield basalts. To better distinguish the transitional xenolith sources as one of Mauna Kea's two postshield substages, the older, basaltic Hamakua unit or the younger hawaiitic Laupahoehoe unit, variation diagrams compared calculated liquid compositions to Mauna Kea lavas from the shield and postshield stages. Calculated liquid trace element concentrations are similar to those of Hamakua lavas.

The performance of astronomical interferometer arrays operating at (sub) millimeter wave-lengths is seriously compromised by rapid variations of atmospheric water vapour content that distort the phase coherence of incoming celestial signals. Unless corrected, these phase distortions, which vary rapidly with time and from antenna to antenna, seriously compromise the sensitivity and image quality of these arrays. Building on the success of a prototype infrared radiometer for millimeter astronomy (IRMA I), which was ued to measure atmospheric water vapour column abundance, this thesis presents results from a second generation radiometer (IRMA II) operating at the James Clerk Maxwell Telescope (JCMT) on Mauna Kea, Hawaii from December, 2000 to March, 2001. These results include comparisons with other measures of water vapour abundance available on the summit of Mauna Kea and a comparison with a theorteical curve-of-growth calculated from a new radiative transfer model, ULTRAM, developed specifically for the purpose. Plans for a third generation radiometer (IRMA III) are also be discussed. / xii, 143 leaves : ill. ; 28 cm.

Fourier transform spectroscopy (FTS) is one of the premier ways to collect source information through emitted radiation. It is so named because the principal measurement technique involves the analysis of spectra determined from the Fourier transform of a time-domain interference pattern. Given options in the field, many space- and ground-based instruments have selected Fourier transform spectrometers for their measurements. The Herschel Space Observatory, launched on May 14, 2009, has three on-board instruments. One, SPIRE, comprises a FTS paired with bolometer detector arrays. SCUBA-2 (Submillimetre Common User Bolometer Array) and FTS-2 have recently been commissioned and will be mounted within the collecting dish of the James Clerk Maxwell Telescope by Fall, 2010. The use of FTS in these two observatories will be examined. While work towards each project is independently useful, the thesis is bound by the commonality between the two, as each seeks similar answers from vastly different viewpoints. / xvii, 123 leaves : ill. (some col.) ; 29 cm

L’arrivée du spectromètre imageur à transformée de Fourier SITELLE au télescope Canada-France-Hawaï souligne la nécessité d’un calculateur de temps d’exposition permettant aux utilisateurs de l’instrument de planifier leurs observations et leurs demandes de temps de télescope. Une grande partie de mon projet est ainsi le développement d’un code de simulation capable de reproduire les résultats de SITELLE et de son prédecesseur SpIOMM, installé à l’Observatoire du Mont-Mégantic. La précision des simulations est confirmée par une comparaison avec des données SpIOMM et les premières observations de SITELLE. La seconde partie de mon projet consiste en une analyse spectrale de données observationelles. Prenant avantage du grand champ de vue de SpIOMM, les caractéristiques du gaz ionisé (vitesse radiale et intensité) sont étudiées pour l’ensemble de la paire de galaxies en interaction Arp 72. La courbe de rotation dans le visible ainsi que le gradient de métallicité de NGC 5996, la galaxie principale d’Arp 72, sont obtenues ici pour la première fois. La galaxie spirale NGC 7320 est également étudiée à partir d’observations faites à la fois avec SpIOMM et SITELLE. / The arrival of the Fourier-transform imaging spectrometer SITELLE at the Canada-France-Hawaii telescope highlights the importance of having an exposure time calculator allowing the instrument’s users to plan ahead their observing proposals. A large part of my project is the development of a simulator able to reproduce the results obtained with SITELLE and its predecessor SpIOMM. The accuracy of the simulations is confirmed through comparison with SpIOMM data and SITELLE’s first observations. The second part of my project is the spectral analysis of observational data. SpIOMM’s large field of view allows us to study the properties (radial velocities and line intensities) of the ionized gas through the entirety of Arp 72, a pair of interacting galaxies. For the first time, the rotation curve in the optical and the metallicity gradient are obtained for NGC 5996, the main galaxy in Arp 72. Both SpIOMM and SITELLE results are also shown for the dwarf spiral galaxy NGC 7320.