The redshifts and emission-line strengths for XXXX Galaxies in 29 fields of the WFC3 Infrared Spectroscopic Parallels (WISP) Survey are presented.

ABSTRACT Resonance Cones were observed in a plasma affected by a steady state magnetic field and their angular distribution was measured over a set of electric radio frequencies from the time varying oscillation of a short antenna. The angles were compared to the theoretical values under the cold electron approximation and found to match within a few degrees. Resonance cones at smaller angles were also observed, as predicted by theory for warm electron temperatures where $}{T_{e}}\ll1$[3].

Using an antenna to generate whistler waves in a plasma using a helium source and a magnetic field probe to measure perturbations in the magnetic field, a biased disc was placed behind the wave generator to create ducting. Ducted waves were seen to propagate towards density minimum when in a region of high magnetic field, and then along a density maximum when in a region of lower magnetic field. A simulation was created using theory, which was found not to agree with measured results.

LECTURES AND NOTES week 8 notes review Taylors Theorem says if f is analytic on {z : |z − z₀|<r} and continuous on the domain that includes the boundary, then $f(z)=^{\infty}f^{(n)}(z_0){n!}$ and this series converges absolutely. Cauchys inequality says that if is analytic in {z ∈ 𝕔 : |z − z₀|<r} and |f(z)| ≤ c in the disk then the function converges absolutely. Isolated Singularities A function which is analytic on the punctured disk {z ∈ 𝕔 : 0 < |z − z₀|<r} has an isolated singularity at z₀.There are three examples of isolated singularities. 1. removable singularity: where f(z) is bounded for some r > 0 on {0 < |z − z₀|<r}, remains bounded as z → z₀ 2. poles: where limz → z₀|f(z)| = ∞ 3. essential singularity: when 1 or 2 dont apply lemma: if f has a removable singularity at z₀ then the limz → z₀f(z) exists and extends f to an analytic function at z₀.

INTRODUCTION Radio emission from the ionosphere can produce a whistling sound in the audio frequency that can be heard[1]. The whistling sounds are described as groups of descending tones which are called the whistler mode. When lightning hits the southern hemisphere it produces a range of radio waves, some of which can travel along the earths magnetic field lines from the southern hemisphere to the northern hemisphere[1].These waves are called extraordinary waves .The extraordinary waves emit two solutions to the wave equation named L and R waves.The L and R refer to left and right hand circularly polarized. The waves that describe the whistling sound are R waves and they will be detected in the north and the different frequencies of these waves will travel at different speeds. For $\omega<}{2}$ the phase and group velocities increase with frequency, where $={m}$ is the electron cyclotron frequency[1]. Due to this, the lower frequencies will arrive at the northern hemisphere later than the higher frequencies will, causing the descending tone in the whistler mode. These R waves waves that travel along the magnetic field lines are called whistler waves and these waves can only propagate for $\omega<{2}$. This lab seeks out to measure the dispersion relation of the whistler waves and to find the wave patterns theoretically and experimentally in the inductively coupled plasma device using Appletons equation.

ABSTRACT: The time delays between point-like images in gravitational lens systems can be used to measure cosmological parameters as well as probe the dark matter (sub-)structure within the lens galaxy. The number of lenses with measuring time delays is growing rapidly due to dedicated efforts. In the near future, the upcoming _Large Synoptic Survey Telescope_ (LSST), will monitor ∼10³ lens systems consisting of a foreground elliptical galaxy producing multiple images of a background quasar. In an effort to assess the present capabilities of the community to accurately measure the time delays in strong gravitational lens systems, and to provide input to dedicated monitoring campaigns and future LSST cosmology feasibility studies, we pose a “Time Delay Challenge” (TDC). The challenge is organized as a set of “ladders,” each containing a group of simulated datasets to be analyzed blindly by participating independent analysis teams. Each rung on a ladder consists of a set of realistic mock observed lensed quasar light curves, with the rungs’ datasets increasing in complexity and realism to incorporate a variety of anticipated physical and experimental effects. The initial challenge described here has two ladders, TDC0 and TDC1. TDC0 has a small number of datasets, and is designed to be used as a practice set by the participating teams as they set up their analysis pipelines. The non mondatory deadline for completion of TDC0 will be December 1 2013. The teams that perform sufficiently well on TDC0 will then be able to participate in the much more demanding TDC1. TDC1 will consists of 10³ lightcurves, a sample designed to provide the statistical power to make meaningful statements about the sub-percent accuracy that will be required to provide competitive Dark Energy constraints in the LSST era. In this paper we describe the simulated datasets in general terms, lay out the structure of the challenge and define a minimal set of metrics that will be used to quantify the goodness-of-fit, efficiency, precision, and accuracy of the algorithms. The results for TDC1 from the participating teams will be presented in a companion paper to be submitted after the closing of TDC1, with all TDC1 participants as co-authors.

Overview This open document is being used to describe and record the events at the Radcliffe Exploratory Seminar on Data Curation and Analysis, to be held at the Radcliffe Institute for Advanced Study, May 9-10 2013. This Google Drive Directory should be used to deposit all files contributed by participants before and during the meeting. (Click "Open in Drive" on your browser to make a new folder, e.g. with your name as its name.) This Google Doc is used for collaborative real-time note-taking. ABSTRACT: Rapid advances in technology have allowed us to collect vast amounts of data in myriad fields and forms, but our ability to manage and analyze these data has not kept pace. As a result, the amount of data collected far exceeds what can be analyzed and, often, what can be archived. These issues only become more pressing as data collection accelerates. Astronomers and astrophysicists, for example, collect terabytes of data per night; the phrase “drowning in a data tsunami” is increasingly used to describe this situation. The issues of what to keep and what to distribute are surprisingly complex, even when we put aside technological issues such as long-term storage and retrieval. A central challenge is the fundamental conflict between reducing the size of data and preserving information for future scientific inquires and statistical analyses. Complicating matters further, the parties/teams involved in the entire data collection, curation, and analysis process often have only limited communication with each other owing to the sequential nature of this process. This seminar brings together a core group of leading experts and emerging scholars in information and natural sciences to discuss, debate, and design principles and strategies to address this grand challenge, which increasingly affects almost every aspect of science and society. GOAL: By gathering experts from information and natural sciences, we aim to start building a set of principles and methods that will allow us to understand such problems and to provide better preprocessing, analyses, and data preservation, especially in the context of the natural sciences. The ultimate goals of this research include providing methods for assessing the validity of such collaborative analyses, guidance on statistically-principled preprocessing, and a rich new theory of statistical learning and inference with multiple parties. We believe that this collaboration will simultaneously sow the seeds for innovative mathematical theory and shed light on directly usable guidelines for the construction and curation of scientific databases.