THE GEMINI NICI PLANET-FINDING CAMPAIGN: DISCOVERY OF A SUBSTELLAR L DWARF COMPANION TO THE NEARBY YOUNG M DWARF CD-35 2722

We present the discovery of a wide (67 AU) substellar companion to the nearby (21 pc) young solar-metallicity M1 dwarf CD-35 2722, a member of the approximate to 100 Myr AB Doradus association. Two epochs of astrometry from the NICI Planet-Finding Campaign confirm that CD-35 2722 B is physically associated with the primary star. Near-IR spectra indicate a spectral type of L4 +/- 1 with a moderately low surface gravity, making it one of the coolest young companions found to date. The absorption lines and near-IR continuum shape of CD-35 2722 B agree especially well the dusty field L4.5 dwarf 2MASS J22244381-0158521, while the near-IR colors and absolute magnitudes match those of the 5 Myr old L4 planetary-mass companion, 1RXS J160929.1-210524 b. Overall, CD-35 2722 B appears to be an intermediate-age benchmark for L dwarfs, with a less peaked H-band continuum than the youngest objects and near-IR absorption lines comparable to field objects. We fit Ames-Dusty model atmospheres to the near-IR spectra and find T(eff) = 1700-1900 K and log(g) = 4.5 +/- 0.5. The spectra also show that the radial velocities of components A and B agree to within +/- 10 km s(-1), further confirming their physical association. Using the age and bolometric luminosity of CD-35 2722 B, we derive a mass of 31 +/- 8 M(Jup) from the Lyon/Dusty evolutionary models. Altogether, young late-M to mid-L type companions appear to be overluminous for their near-IR spectral type compared with field objects, in contrast to the underluminosity of young late-L and early-T dwarfs.

Metallicities for six nearby open clusters from high-resolution spectra of giant stars [Fe/H] values for a planet search sample

We present a study of the stellar parameters and iron abundances of 18 giant stars in six open clusters. The analysis was based on high-resolution and high-S/N spectra obtained with the UVES spectrograph (VLT-UT2). The results complement our previous study where 13 clusters were already analyzed. The total sample of 18 clusters is part of a program to search for planets around giant stars. The results show that the 18 clusters cover a metallicity range between -0.23 and +0.23 dex. Together with the derivation of the stellar masses, these metallicities will allow the metallicity and mass effects to be disentangled when analyzing the frequency of planets as a function of these stellar parameters.

THE GEMINI NICI PLANET-FINDING CAMPAIGN: DISCOVERY OF A MULTIPLE SYSTEM ORBITING THE YOUNG A STAR HD 1160

We report the discovery of two low-mass companions to the young A0V star HD 1160 at projected separations of 81 +/- 5 AU (HD 1160 B) and 533 +/- 25 AU (HD 1160 C) by the Gemini NICI Planet-Finding Campaign. Very Large Telescope images of the system taken over a decade for the purpose of using HD 1160 A as a photometric calibrator confirm that both companions are physically associated. By comparing the system to members of young moving groups and open clusters with well-established ages, we estimate an age of 50(-40)(+50) Myr for HD 1160 ABC. While the UVW motion of the system does not match any known moving group, the small magnitude of the space velocity is consistent with youth. Near-IR spectroscopy shows HD 1160 C to be an M3.5 +/- 0.5 star with an estimated mass of 0.22(-0.04)(+0.03) M-circle dot, while NIR photometry of HD 1160 B suggests a brown dwarf with a mass of 33(-9)(+12) M-Jup. The very small mass ratio (0.014) between the A and B components of the system is rare for A star binaries, and would represent a planetary-mass companion were HD 1160 A to be slightly less massive than the Sun.

The SOPHIE search for northern extrasolar planets: X. Detection and characterization of giant planets by the dozen

We present new radial velocity measurements of eight stars that were secured with the spectrograph SOPHIE at the 193 cm telescope of the Haute-Provence Observatory. The measurements allow detecting and characterizing new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes of between 6.7 and 9.6; the planets have minimum masses Mp sin i of between 0.4 to 3.8 MJup and orbitalperiods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD 143105, HIP 109600, HD 35759, HIP 109384, HD 220842, and HD 12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP 65407, allows the discovery of two giant planets that orbit just outside the 12:5 resonance in weak mutual interaction. The last star, HD 141399, was already known to host a four-planet system; our additional data and analyses allow new constraints to be set on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planet systems. HD 143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted even though this is not a transiting system. The giant planets HIP 109600b, HIP 109384b, and HD 141399c are located in the habitable zone of their host star.

Two roads to planet detection

One of the most exciting discoveries in astrophysics of the last last decade is of the sheer diversity of planetary systems. These include "hot Jupiters", giant planets so close to their host stars that they orbit once every few days; "Super-Earths", planets with sizes intermediate to those of Earth and Neptune, of which no analogs exist in our own solar system; multi-planet systems with planets smaller than Mars to larger than Jupiter; planets orbiting binary stars; free-floating planets flying through the emptiness of space without any star; even planets orbiting pulsars. Despite these remarkable discoveries, the field is still young, and there are many areas about which precious little is known. In particular, we don't know the planets orbiting Sun-like stars nearest to our own solar system, and we know very little about the compositions of extrasolar planets. This thesis provides developments in those directions, through two instrumentation projects.

The first chapter of this thesis concerns detecting planets in the Solar neighborhood using precision stellar radial velocities, also known as the Doppler technique. We present an analysis determining the most efficient way to detect planets considering factors such as spectral type, wavelengths of observation, spectrograph resolution, observing time, and instrumental sensitivity. We show that G and K dwarfs observed at 400-600 nm are the best targets for surveys complete down to a given planet mass and out to a specified orbital period. Overall we find that M dwarfs observed at 700-800 nm are the best targets for habitable-zone planets, particularly when including the effects of systematic noise floors caused by instrumental imperfections. Somewhat surprisingly, we demonstrate that a modestly sized observatory, with a dedicated observing program, is up to the task of discovering such planets.

We present just such an observatory in the second chapter, called the "MINiature Exoplanet Radial Velocity Array," or MINERVA. We describe the design, which uses a novel multi-aperture approach to increase stability and performance through lower system etendue, as well as keeping costs and time to deployment down. We present calculations of the expected planet yield, and data showing the system performance from our testing and development of the system at Caltech's campus. We also present the motivation, design, and performance of a fiber coupling system for the array, critical for efficiently and reliably bringing light from the telescopes to the spectrograph. We finish by presenting the current status of MINERVA, operational at Mt. Hopkins observatory in Arizona.

The second part of this thesis concerns a very different method of planet detection, direct imaging, which involves discovery and characterization of planets by collecting and analyzing their light. Directly analyzing planetary light is the most promising way to study their atmospheres, formation histories, and compositions. Direct imaging is extremely challenging, as it requires a high performance adaptive optics system to unblur the point-spread function of the parent star through the atmosphere, a coronagraph to suppress stellar diffraction, and image post-processing to remove non-common path "speckle" aberrations that can overwhelm any planetary companions.

To this end, we present the "Stellar Double Coronagraph," or SDC, a flexible coronagraphic platform for use with the 200" Hale telescope. It has two focal and pupil planes, allowing for a number of different observing modes, including multiple vortex phase masks in series for improved contrast and inner working angle behind the obscured aperture of the telescope. We present the motivation, design, performance, and data reduction pipeline of the instrument. In the following chapter, we present some early science results, including the first image of a companion to the star delta Andromeda, which had been previously hypothesized but never seen.

A further chapter presents a wavefront control code developed for the instrument, using the technique of "speckle nulling," which can remove optical aberrations from the system using the deformable mirror of the adaptive optics system. This code allows for improved contrast and inner working angles, and was written in a modular style so as to be portable to other high contrast imaging platforms. We present its performance on optical, near-infrared, and thermal infrared instruments on the Palomar and Keck telescopes, showing how it can improve contrasts by a factor of a few in less than ten iterations.

One of the large challenges in direct imaging is sensing and correcting the electric field in the focal plane to remove scattered light that can be much brighter than any planets. In the last chapter, we present a new method of focal-plane wavefront sensing, combining a coronagraph with a simple phase-shifting interferometer. We present its design and implementation on the Stellar Double Coronagraph, demonstrating its ability to create regions of high contrast by measuring and correcting for optical aberrations in the focal plane. Finally, we derive how it is possible to use the same hardware to distinguish companions from speckle errors using the principles of optical coherence. We present results observing the brown dwarf HD 49197b, demonstrating the ability to detect it despite it being buried in the speckle noise floor. We believe this is the first detection of a substellar companion using the coherence properties of light.

Discovery of a low-mass brown dwarf companion of the young nearby star G196-3.

A substellar-mass object in orbit at about 300 astronomical units from the young low-mass star G 196-3 was detected by direct imaging. Optical and infrared photometry and low- and intermediate-resolution spectroscopy of the faint companion, hereafter referred to as G 196-3B, confirm its cool atmosphere ?15 Jupiter masses. The separation and allow its mass to be estimated at 25?10 between the objects and their mass ratio suggest the fragmentation of a collapsing cloud as the most likely origin for G 196-3B, but alternatively it could have originated from a protoplanetary disc that has been dissipated. Whatever the formation process was, the young age of the primary star (about 100 million years) demonstrates that substellar companions can form on short time scales.

Encyclopedia contributions: entries C-G in Oxford Companion to Australian Gardens

Caulfield, Harold William; p.131 Cowan, Alexander; p.164 Cowley, Ebenezer; p.164 East Talgai Station; p.193 Eaves, S.H.; p.193-194 Edgar, J.S.; p.196 Everist, Selwyn; p.206 Experimental Farms and Gardens; pp.207-208 Government Houses - Queensland; pp.267-268

Encyclopedia contributions: Entries H-M in Oxford Companion to Australian Gardens

The Oxford Companion to Australian Gardens is the first comprehensive reference book to cover all aspects of Australian gardens, and the history of gardening and garden design in Australia. The book is comprised of over 400 thematic, bibliographic and place based entries, and is extensively illustrated and cross referenced to ensure ease of use and thorough coverage of the field. The Companion contributes to the understanding of gardens and gardening by including entries on designed landscapes, agriculture, architecture, art, botany, ecology, forestry, horticulture, landscape architecture, town planning and viticulture and will become the standard reference on the subject. Herbert,

Encyclopedia contributions: entries N-R in Oxford Companion to Australian

New Farm Park; p.436 Oakman, H.O. (with Jan Seto); p.449 Paranella, Jose; p.463 Perrott family; p.469 Pink, James; p.475 Queensland; pp.495-497 The Queenslander; pp.497-498 The Queensland Horticulturist; p.498 Rawson, Mina; p.502 Rockhampton Botanic Gardens; p.572

Oxford Companion to Australian Gardens [contributions: entries S-V]

Shelton, Edward Mason; p.548 Sherwood Arboretum; p.550 Soutter, William; pp.563-564 Styles or gardens and designed landscapes; pp.575-576 Summer-house; pp.579-580 Trapnell, Walter George; p.602 Tropical Gardens; pp.604-605 Wickham Park; p.642 Wijaya, Made; p.642 Williams, George; p.644 Williams, Keith A.W.; p.644 Verandah Garadening; p.614

The Ashgate Research Companion to Queer Theory edited by Giffney and O'Rourke [Review]

The Ashgate Research Companion to Queer Theory is a solid collection providing an overview of the past, present and future applications of queer theory. The Companion confidently lives up to its name as a research companion offering useful theories and methodologies for the reader to utilise queer theory in their own work.

Encyclopedia contributions : entries S-Z in Oxford Companion to Australian Gardens

Shelton, E.M. (p.548); Sherwood Arboretum (p.550); Soutter, William (pp.563-4); Styles (pp.575-6); Summer-House (579-580); Trapnell, W.G. (p.602); Tropical Gardens (pp.604-5);Verandah Gardening (p.614); Wickham Park (p.642); Wijaya, Made (p.642); Williams, George (p.644); Williams Keith A (p.644).

Keeping House : a novel and novel companion

The creative work of this study is a novel-length work of literary fiction called Keeping House (published as Grace's Table, by University of Queensland Press, April 2014). Grace has not had twelve people at her table for a long time. Hers isn't the kind of family who share regular Sunday meals. As Grace prepares the feast, she reflects on her life, her marriage and her friendships. When the three generations of her family come together, simmering tensions from the past threaten to boil over. The one thing that no one can talk about is the one thing that no one can forget. Grace's Table is a moving and often funny novel using food as a language to explore the power of memory and the family rituals that define us. The exegetical component of this study does not adhere to traditional research pedagogies. Instead, it follows the model of what the literature describes as fictocriticism. It is the intention that the exegesis be read as a hybrid genre; one that combines creative practice and theory and blurs the boundaries between philosophy and fiction. In offering itself as an alternative to the exegetical canon it provides a model for the multiplicity of knowledge production suited to the discipline of practice-led research. The exegesis mirrors structural elements of the creative work by inviting twelve guests into the domestic space of the novel to share a meal. The guests, chosen for their diverse thinking, enable examination of the various agents of power involved in the delivery of food. Their ideas cross genders, ages and time periods; their motivations and opinions often collide. Some are more concerned with the spatial politics of where food is consumed, others with its actual preparation and consumption. Each, however, provides a series of creative reflective conversations throughout the meal which help to answer the research question: How can disempowered women take authority within their domestic space? Michel de Certeau must defend his "operational tactics" or "art of the weak" 1 as a means by which women can subvert the colonisation of their domestic space against Michel Foucault's ideas about the functions of a "disciplinary apparatus". 2 Erving Goffman argues that the success of de Certeau's "tactics" depends upon his theories of "performance" and "masquerade" 3; a claim de Certeau refutes. Doreen Massey and the author combine forces in arguing for space, time and politics to be seen as interconnected, non-static and often contested. The author calls for identity, or sense of self, to be considered a further dimension which impacts on the function of spatial models. Yu-Fi Tuan speaks of the intimacy of kitchens; Gaston Bachelard the power of daydreams; and Jean Anthelme Brillat-Savarin gives the reader a taste of the nourishing arts. Roland Barthes forces the author to reconsider her function as a writer and her understanding of the reader's relationship with a text. Fictional characters from two texts have a place at the table – Marian from The Edible Woman by Margaret Atwood 4 and Lilian from Lilian's Story by Kate Grenville. 5 Each explores how they successfully subverted expectations of their gender. The author interprets and applies elements of the conversations to support Grace's tactics in the novel as well as those related to her own creative research practice. Grace serves her guests, reflecting on what is said and how it relates to her story. Over coffee, the two come together to examine what each has learned.

A Companion to New Media Dynamics

A Companion to New Media Dynamics presents a state-of-the-art collection of multidisciplinary readings that examine the origins, evolution, and cultural underpinnings of the media of the digital age in terms of dynamic change Presents a state-of-the-art collection of original readings relating to new media in terms of dynamic change. - Features interdisciplinary contributions encompassing the sciences, social sciences, humanities and creative arts - Addresses a wide range of issues from the ownership and regulation of new media to their form and cultural uses - Provides readers with a glimpse of new media dynamics at three levels of scale: the ‘macro’ or system level; the ‘meso’ or institutional level; and ‘micro’ or agency level