REMAKING THE ICONIC LULU: TRANSFORMATIONS OF CHARACTER, CONTEXT, AND MUSIC

Using Alban Berg’s opera Lulu as a case study, this dissertation explores the fluid nature of cultural artifacts as they are reborn within new socio-cultural contexts. By examining several Lulu productions, this inquiry seeks to understand the changes of meaning that have occurred through the transformation of canonic works in the twentieth- and twenty-first centuries. Central to this project is the shifting nature of the character of Lulu, not only in Berg’s opera, but also in various artistic genres that preceded and affected his own conceptions, as well as her appearances in selected productions. This study contrasts modern Lulu productions with the composer’s intentions for the opera, using Berg’s operatic text as a basis for comparison. These assessments will be made through a semiotic analysis of various staging elements, musical and textual analysis of archival materials, and consideration of past Lulu scholarship. Relevant features of the political, cultural, and social climate of each production are also be investigated. Two Werktreue productions are examined: the Austrian première of Lulu at the Theatre an der Wien (1962) and the Metropolitan Opera staging by John Dexter (1977). Several Regietheater productions are also studied, including the three-act 1979 première at the Paris Opera—complete with Friedrich Cerha’s third act—as well as stagings at the Glyndebourne Festival, Opernhaus Zürich, the Royal Opera House, the Theater Basel, and the Gran Teatre del Liceu. Although much scholarship has been written on Lulu, directors have implemented some of the most radical changes to the opera. Building on Lydia Goehr’s definition of the work-concept in The Imaginary Museum of Historical Works, this project examines the role of these radically altered stagings as challenges to the work-concept of Lulu. In order to assess the portrayal of Lulu in the above-listed productions, this dissertation investigates the origins of her character, tracing the genesis of Lulu and the numerous artists who molded her, including Félicien Champsaur, Frank Wedekind, Leopold Jessner, and G. W. Pabst. Finally, this dissertation considers a work that goes beyond modifications of orchestration, setting, and staging in Regietheater productions. Olga Neuwirth’s opera, American Lulu, represents the ultimate authorial challenge, functioning as both an adaptation of Berg’s text and as a newly composed work. This inquiry explores the transformed mise en scène and re-imagined characters of American Lulu, investigating Neuwirth’s politicized changes and the effect that these alterations have on the story of Lulu. In addition to analyzing her score and libretto, this study examines the performance and depiction of race and sexuality in two American Lulu productions, at the Komische Oper Berlin and the Young Vic in London. Several Lulu performances discussed in this study explore an area which, even as recently as the publication of Roger Parker’s Remaking the Song, was called “untouched”: the alteration of the operatic text itself. Whether these updated works and radical stagings are considered a passing trend or true innovations, the effect of staging on operagoers is undeniable. Like the shifting interpretations of the iconic character herself, the complex history of Lulu reflects the development of canonic works over time, as they are altered, transformed, and reborn in new environments

Problems, Puzzles, and Paradoxes for a Moral Psychology of Fiction

The goal of my dissertation is to provide a comprehensive account of our psychological engagements with fiction. While many aestheticians have written on issues concerning art and ethics, only a few have addressed the ways in which works of fiction offer problems for general accounts of morality, let alone how we go about making moral judgments about fictions in the first place. My dissertation fills that gap. I argue that the first challenge in explaining our interactions with fiction arises from functional and inferential arguments that entail that our mental states about fictional entities are non-genuine. This means that our mental states during our engagements with fiction are different in kind from typical beliefs, emotions, desires, etc. that we have in real-life contexts. I call this position the Distinct Attitude View (DAV). In its place, I propose a common-sense, standard attitude view (SAV): the idea that our psychological interactions with non-real entities can be explained in terms of the intentional content of those states as opposed to a distinct type of mental state. In expanding the SAV, I develop several independent accounts of social cognition, emotions, and moral judgments. I also show how the SAV can dissolve standard problems in the philosophy and psychology of aesthetic experience: the paradox of fiction, the problem of imaginative existence, and the sympathy for the devil phenomenon, amongst others

The Nature of Fictional Characters

This paper explores the ramifications of a central question concerning our everyday experience with film and other art forms: how it is possible to recognize a character in a sequel or related artwork as the exact same character as that found in the original or previous artwork. My main goal is to determine necessary and sufficient identity conditions for fictional film characters which may adequately account for our everyday discussion of these characters. After addressing several intuitions which any theory of fictional characters must address, I propose that film and other characters should be best understood as “abstract artifacts” following the Amie Thomasson’s artifactual theory of fictional characters. I then propose Thomasson’s theory as the best way to explain fictional characters and apply her theory to film characters, before addressing two interesting and problematic examples of film characters

Java operating systems: design and implementation

Journal ArticleLanguage-based extensible systems such as Java use type safety to provide memory safety in a single address space. Memory safety alone, however, is not sufficient to protect different applications from each other. such systems must support a process model that enables the control and management of computational resources. In particular, language-based extensible systems must support resource control mechanisms analogous to those in standard operating-systems. They must support the separation of processes and limit their use of resources, but still support safe and efficient interprocess communication

Ionization Sources and Physical Conditions in the Diffuse Ionized Gas Halos of Four Edge-On Galaxies

Deep long-slit spectra of the diffuse ionized gas halos of the edge-on spiral galaxies NGC 4302 and UGC 10288 are presented. These data, along with previously presented data for NGC 5775 and NGC 891, are used to address the issue of how DIG halos are energized. Composite photo-ionization/shock models are generally better at explaining runs of line ratios in these galaxies than photo-ionization models alone. Models of line ratios in NGC 5775 require a greater contribution from shocks for filamentary regions than for non-filamentary regions to explain the run of [OIII]/Halpha. In either case, the [SII]/[NII] ratio is not well fit by the models. Composite models for UGC 10288 are successful at reproducing the run of [SII]/[NII] for all but the the highest values of [NII]/Halpha; however, the run of [OIII]/Halpha vs. [NII]/Halpha does not show any discernible trend, making it difficult to determine whether or not shocks make a contribution. We also examine whether the data can be explained simply by an increase in temperature with z in a pure photo-ionization model. Runs of [SII]/Halpha, [NII]/Halpha, and [SII]/[NII] in each of the four galaxies are consistent with such an increase. However, the runs of [OIII]/Halpha vs. z in NGC 5775 and UGC 10288 require unusually high ionization fractions of O^{++} that can not be explained without invoking a secondary ionization source or at the very least a much higher temperature for the [OIII]-emitting component than for the [SII]- and [NII]-emitting component. An increase in temperature with z is generally more successful at explaining the [OIII]/Halpha run in NGC 891.Comment: 42 pages in aaspp4.sty format. This includes the 19 figures. Reference added. Accepted for publication in Ap

Constraining the extra heating of the Diffuse Ionized Gas in the Milky Way

The detailed observations of the diffuse ionized gas through the emission lines H$\alpha$, [NII], and [SII] in the Perseus Arm of our Galaxy by the Wisconsin H$\alpha$ Mapper (WHAM)--survey challenge photoionization models. They have to explain the observed rise in the line ratios [NII]/H$\alpha$ and [SII]/H$\alpha$. The models described here consider for the first time the detailed observational geometry toward the Perseus Arm. The models address the vertical variation of the line ratios up to height of 2 kpc above the midplane. The rising trends of the line ratios are matched. The increase in the line ratios is reflected in a rise of the temperature of the gas layer. This is due to the progressive hardening of the radiation going through the gas. However an extra heating above photoionization is needed to explain the absolute values. Two different extra heating rates are investigated which are proportional to $n^0$ and $n^1$. The models show that a combination of both are best to explain the data, where the extra heating independent of density is dominant for z $>$ 0.8 kpc.Comment: accepted for publication in Ap

Emission Line Ratios and Variations in Temperature and Ionization State in the Diffuse Ionized Gas of Five Edge-on Galaxies

We present spectroscopic observations of ionized gas in the disk-halo regions of five edge-on galaxies, covering a wavelength range from [OII] 3727A to [SII] 6716.4A. The inclusion of the [OII] emission provides additional constraints on the properties of the diffuse ionized gas (DIG), in particular, the origin of the observed spatial variations in the line intensity ratios. We have derived electron temperatures, ionization fractions and abundances along the slit. Our data include both slit positions parallel and perpendicular to the galactic disks. This allowed us to examine variations in the line intensity ratios with height above the midplane as well as distance from the galactic centers. The observed increase in the [OII]/Halpha line ratio towards the halo seems to require an increase in electron temperature caused by a non-ionizing heating mechanism. We conclude that gradients in the electron temperature can play a significant role in the observed variations in the optical emission line ratios from extraplanar DIG.Comment: accepted for publication in ApJ, 43 pages including 26 figure

High Latitude HI in NGC 2613: Buoyant Disk-Halo Outflow

We combine new VLA D array HI data of NGC 2613 with previous high resolution data to show new disk-halo features in this galaxy. The global HI distribution is modeled in detail using a technique which can disentangle the effects of inclination from scale height and can also solve for the average volume density distribution in and perpendicular to the disk. The model shows that the galaxy's inclination is on the low end of the range given by Chaves & Irwin (2001) and that the HI disk is thin (z_e = 188 pc), showing no evidence for halo. Numerous discrete disk-halo features are observed, however, achieving z heights up to 28 kpc from mid-plane. One prominent feature in particular, of mass, 8X10^7 Msun and height, 22 kpc, is seen on the advancing side of the galaxy at a projected galactocentric radius of 15.5 kpc. If this feature achieves such high latitudes because of events in the disk alone, then input energies of order ~ 10^{56} ergs are required. We have instead investigated the feasibility of such a large feature being produced via buoyancy (with drag) within a hot, pre-existing X-ray corona. Reasonable plume densities, temperatures, stall height (~ 11 kpc), outflow velocities and ages can indeed be achieved in this way. The advantage of this scenario is that the input energy need only be sufficient to produce blow-out, a condition which requires a reduction of three orders of magnitude in energy. If this is correct, there should be an observable X-ray halo around NGC 2613.Comment: 32 pages 7 gif figures, accepted by Ap

Infrared Spectroscopy of the Diffuse Ionized Halo of NGC 891

We present infrared spectroscopy from the Spitzer Space Telescope at one disk position and two positions at a height of 1 kpc from the disk in the edge-on spiral NGC 891, with the primary goal of studying halo ionization. Our main result is that the [Ne III]/[Ne II] ratio, which provides a measure of the hardness of the ionizing spectrum free from the major problems plaguing optical line ratios, is enhanced in the extraplanar pointings relative to the disk pointing. Using a 2D Monte Carlo-based photo-ionization code which accounts for the effects of radiation field hardening, we find that this trend cannot be reproduced by any plausible photo-ionization model, and that a secondary source of ionization must therefore operate in gaseous halos. We also present the first spectroscopic detections of extraplanar PAH features in an external normal galaxy. If they are in an exponential layer, very rough emission scale-heights of 330-530 pc are implied for the various features. Extinction may be non-negligible in the midplane and reduce these scale-heights significantly. There is little significant variation in the relative emission from the various features between disk and extraplanar environment. Only the 17.4 micron feature is significantly enhanced in the extraplanar gas compared to the other features, possibly indicating a preference for larger PAHs in the halo.Comment: 35 pages in ApJ preprint format, 8 figures, accepted for publication in ApJ. Minor change to Introduction to give appropriate credit to earlier, related wor

Imaging Fabry-Perot Spectroscopy of NGC 5775: Kinematics of the Diffuse Ionized Gas Halo

We present imaging Fabry-Perot observations of Halpha emission in the nearly edge-on spiral galaxy NGC 5775. We have derived a rotation curve and a radial density profile along the major axis by examining position-velocity (PV) diagrams from the Fabry-Perot data cube as well as a CO 2-1 data cube from the literature. PV diagrams constructed parallel to the major axis are used to examine changes in azimuthal velocity as a function of height above the midplane. The results of this analysis reveal the presence of a vertical gradient in azimuthal velocity. The magnitude of this gradient is approximately 1 km/s/arcsec, or about 8 km/s/kpc, though a higher value of the gradient may be appropriate in localized regions of the halo. The evidence for an azimuthal velocity gradient is much stronger for the approaching half of the galaxy, although earlier slit spectra are consistent with a gradient on both sides. There is evidence for an outward radial redistribution of gas in the halo. The form of the rotation curve may also change with height, but this is not certain. We compare these results with those of an entirely ballistic model of a disk-halo flow. The model predicts a vertical gradient in azimuthal velocity which is shallower than the observed gradient, indicating that an additional mechanism is required to further slow the rotation speeds in the halo.Comment: 18 pages, 18 figures. Uses emulateapj.cls. Accepted for publication in Ap