\u27No Home Here\u27: Female Space and the Modernist Aesthetic in Nella Larsen\u27s Quicksand and Sylvia Plath\u27s The Bell Jar

In her 1929 essay A Room of One\u27s Own, Virginia Woolf famously asserts that a woman must have money and a room of her own if she is to write fiction (4). This concept places an immediate importance on the role of the Modernist female subject as an artist and as an architect, constructing the places and spaces that she exists within. With Woolf\u27s argument as its point of departure, this thesis investigates the theme of female space in two Modernist texts: Nella Larsen\u27s Quicksand (1928) and Sylvia Plath\u27s The Bell Jar (1963). The respective protagonists of Quicksand and The Bell Jar, Helga Crane and Esther Greenwood, each undertake journeys to obtain spaces that are purely their own. However, this thesis positions each space that Helga and Esther occupy as both male-constructed and male-dominated in order to address the inherent gendering of space and its impact on the development of feminine identities. This thesis focuses specifically on the roles of the mother, the muse, and the female mentor, tracking the spaces in which Helga and Esther begin to adhere to these roles. Expanding on Lauren Berlant\u27s theory of cruel optimism, this thesis will use the term cruel femininity to support its intervening claim that the respective relationships that Helga and Esther each have with their own feminine identities begin to turn cruel as they internalize the male-dominated spatial structures surrounding them. Overall, this thesis argues that there is no space in existence where Helga and Esther can realize their full potential as human beings, as long as the spatial structures within their communities continue to be controlled by hegemonic, patriarchal beliefs

Extending Traditional Static Analysis Techniques to Support Development, Testing and Maintenance of Component-Based Solutions

Traditional static code analysis encompasses a mature set of techniques for helping understand and optimize programs, such as dead code elimination, program slicing, and partial evaluation (code specialization). It is well understood that compared to other program analysis techniques (e.g., dynamic analysis), static analysis techniques do a reasonable job for the cost associated with implementing them. Industry and government are moving away from more ‘traditional’ development approaches towards component-based approaches as ‘the norm.’ Component-based applications most often comprise a collection of distributed object-oriented components such as forms, code snippets, reports, modules, databases, objects, containers, and the like. These components are glued together by code typically written in a visual language. Some industrial experience shows that component-based development and the subsequent use of visual development environments, while reducing an application\u27s total development time, actually increase certain maintenance problems. This provides a motivation for using automated analysis techniques on such systems. The results of this research show that traditional static analysis techniques may not be sufficient for analyzing component-based systems. We examine closely the characteristics of a component-based system and document many of the issues that we feel make the development, analysis, testing and maintenance of such systems more difficult. By analyzing additional summary information for the components as well as any available source code for an application, we show ways in which traditional static analysis techniques may be augmented, thereby increasing the accuracy of static analysis results and ultimately making the maintenance of component-based systems a manageable task. We develop a technique to use semantic information about component properties obtained from type library and interface definition language files, and demonstrate this technique by extending a traditional unreachable code algorithm. To support more complex analysis, we then develop a technique for component developers to provide summary information about a component. This information can be integrated with several traditional static analysis techniques to analyze component-based systems more precisely. We then demonstrate the effectiveness of these techniques on several real Department of Defense (DoD) COTS component-based systems

Ca II and Na I Quasar Absorption-Line Systems in an Emission-Selected Sample of SDSS DR7 Galaxy/Quasar Projections: I. Sample Selection

The aim of this project is to identify low-redshift host galaxies of quasar absorption-line systems by selecting galaxies which are seen in projection onto quasar sightlines. To this end, we use the Seventh Data Release of the Sloan Digital Sky Survey (SDSS-DR7) to construct a parent sample of 97489 galaxy/quasar projections at impact parameters of up to 100 kpc to the foreground galaxy. We then search the quasar spectra for absorption line systems of Ca II and Na I within +- 500 km/s of the galaxy's velocity. This yields 92 Ca II and 16 Na I absorption systems. We find that most of the Ca II and Na I systems are sightlines through the Galactic disk, through High Velocity Cloud complexes in our halo, or Virgo cluster sightlines. Placing constraints on the absorption line rest equivalent width significance (>=3.0 sigma), the Local Standard of Rest velocity along the sightline (>= 345 km/s), and the ratio of the impact parameter to the galaxy optical radius (<=5.0), we identify 4 absorption line systems that are associated with low-redshift galaxies at high confidence, consisting of two Ca II systems (one of which also shows Na I), and two Na I systems. These 4 systems arise in blue, L_r^* galaxies. Tables of the 108 absorption systems are provided to facilitate future follow up.Comment: 13 pages, 11 figures, 6 tables; online data included in electronic version as 1 FITS table and 2 machine readable tables; to be published in The Astronomical Journa

Host Galaxy Properties of CaII and NaI Quasar Absorption-Line Systems

Many questions remain within the areas of galaxy formation and evolution. Understanding the origin of gas in galaxy environments, whether as tidal debris, infalling High Velocity Clouds, galaxy outflows, or as gaseous material residing in galaxy disks, is an important step in answering those questions. Quasar absorption-lines can often be used to probe the environments of intervening galaxies. Traditionally, quasar absorption-lines are studied independently of the host galaxy but this method denies us the exploration of the connection between galaxy and environment. Instead, one can select pairs of known galaxies and quasars. This gives much more information regarding the host galaxy and allows us to better connect galaxy properties with associated absorbers. We use the seventh data release of the Sloan Digital Sky Survey to generate a sample of spectroscopic galaxy-quasar pairs. We cross-correlated a sample of 105,000 quasars and ~800,000 galaxies to produce ~98,000 galaxy-quasar pairs, with the quasar projected within 100 kpc of the galaxy. Adopting an automated line-finding algorithm and using the galaxy redshift as a prior, we search through all quasar spectra and identify CaII and NaI absorption due to the intervening galaxy. This procedure produced 1745 Ca~II absorbers and 4500 NaI absorbers detected at or above 2-sigma. Stacking analysis of a subset of absorbers at z>0.01, with significances at or above 3-sigma, showed strong CaII and NaI features around external galaxies. Using the same subset of absorbers at z>0.01, we looked for correlations between absorber and galaxy properties and examined differences in galaxy properties between the absorbers and non-absorbers. We found no correlations with absorber strength or differences between many galaxy properties at the 3-sigma level. The lack of correlations and differences between absorbers and non-absorbers suggest a ubiquitous nature for CaII and NaI around all types of galaxies, with the absorbers showing no geometric preference within galaxy halos. This suggests a possible origin as leftover debris from past mergers that has been redistributed within the halo over time. The main results are presented in Chapters 3 and 4, with complimentary work presented in Chapter 5

HI Observations of the Ca II absorbing galaxies Mrk 1456 and SDSS J211701.26-002633.7

In an effort to study Damped Lyman Alpha galaxies at low redshift, we have been using the Sloan Digital Sky Survey to identify galaxies projected onto QSO sightlines and to characterize their optical properties. For low redshift galaxies, the HI 21cm emission line can be used as an alternate tool for identifying possible DLA galaxies, since HI emitting galaxies typically exhibit HI columns that are larger than the classical DLA limit. Here we report on follow-up HI 21 cm emission line observations of two DLA candidates that are both low-redshift spiral galaxies, Mrk 1456 and SDSS J211701.26-002633.7. The observations were made using the Green Bank and Arecibo Telescopes, respectively. Analysis of their HI properties reveal the galaxies to be about one and two M_HI* galaxies, respectively, and to have average HI mass, gas-richness, and gas mass fraction for their morphological types. We consider Mrk 1456 and SDSS J211701.26-002633.7 to be candidate DLA systems based upon the strength of the CaII absorption lines they cause in their QSO's spectra, and impact parameters to the QSO that are smaller than the stellar disk. Compared to the small numbers of other HI-detected DLA and candidate DLA galaxies, Mrk 1456 and SDSS J211701.26-002633.7 have high HI masses. When compared with the expected properties of low-z DLAs from an HI-detected sample of galaxies, Mrk 1456 and SDSS J211701.26-002633.7 fall within the ranges for impact parameter and B-band absolute magnitude; and the HI mass distribution for the HI-detected DLAs agrees with that of the expected HI mass distribution for low-z DLAs. Our observations support galaxy-evolution models in which high mass galaxies make up an increasing contribution to the DLA cross-section at lower redshifts. [abridged]Comment: 12 pages, 5 figures, 5 tables; to be published in The Astronomical Journa

Precious Metals in SDSS Quasar Spectra I: Tracking the Evolution of Strong, 1.5 < z < 4.5 CIV Absorbers with Thousands of Systems

We have vastly increased the CIV statistics at intermediate redshift by surveying the thousands of quasars in the Sloan Digital Sky Survey Data-Release 7. We visually verified over 16,000 CIV systems with 1.46 < z < 4.55---a sample size that renders Poisson error negligible. Detailed Monte Carlo simulations show we are approximately 50% complete down to rest equivalent widths W_r ~ 0.6 \AA. We analyzed the sample as a whole and in ten small redshift bins with approximately 1500 doublets each. The equivalent width frequency distributions f(W_r) were well modeled by an exponential, with little evolution in shape. In contrast with previous studies that modeled the frequency distribution as a single power law, the fitted exponential gives a finite mass density for the CIV ions. The co-moving line density dN_CIV/dX evolved smoothly with redshift, increasing by a factor of 2.37+/-0.09 from z = 4.55 to 1.96, then plateauing at dN_CIV/dX ~ 0.34 for z = 1.96 to 1.46. Comparing our SDSS sample with z < 1 (ultraviolet) and z > 5 (infrared) surveys, we see an approximately 10-fold increase in dN_CIV/dX over z ~ 6 --> 0, for W_r >= 0.6 \AA. This suggests a monotonic and significant increase in the enrichment of gas outside galaxies over the 12 Gyr lifetime of the universe.Comment: 17 pages (emulateapj), 13 figures, 4 tables; accepted to ApJ and in press; also see http://igmabsorbers.inf

P-MaNGA : full spectral fitting and stellar population maps from prototype observations

MC acknowledges support from a Royal Society University Research Fellowship.MaNGA (Mapping Nearby Galaxies at Apache Point Observatory) is a 6-yearSDSS-IV survey that will obtain resolved spectroscopy from 3600 Å to10300 Å for a representative sample of over 10,000 nearby galaxies.In this paper, we derive spatially resolved stellar population properties and radial gradients by performing full spectral fitting of observed galaxy spectra from P-MaNGA, a prototype of the MaNGA instrument. These data include spectra for eighteen galaxies, covering a large range of morphological type. We derive age, metallicity, dust and stellar mass maps, and their radial gradients, using high spectral-resolution stellar population models, and assess the impact of varying the stellar library input to the models. We introduce a method to determine dust extinction which is able to give smooth stellar mass maps even in cases of high and spatially non-uniform dust attenuation.With the spectral fitting we produce detailed maps of stellar population properties which allow us to identify galactic features among this diverse sample such as spiral structure, smooth radial profiles with little azimuthal structure in spheroidal galaxies, and spatially distinct galaxy sub-components. In agreement with the literature, we find the gradients for galaxies identified as early-type to be on average flat in age, and negative (- 0.15 dex / Re ) in metallicity,whereas the gradients for late-type galaxies are on average negative in age (- 0.39 dex / Re ) and flat in metallicity. We demonstrate howdifferent levels of data quality change the precision with which radialgradients can be measured. We show how this analysis, extended to thelarge numbers of MaNGA galaxies, will have the potential to shed lighton galaxy structure and evolution.PostprintPeer reviewe