Wednesday. Still way behind on astro-ph. Rock climbing last night was fun, with Karina and Peter. Talked to Gary over e-mail about ReMatch not quite working with SWARP. I should talk to Jon too, about the cluster project.
1201.0002
New air fluorescence detectors employed in the telescope array experiment
Tokuno et al
Telescope Array experiment (TA) in Utah, USA: observe UHE CR: a surface detector (SD) array and 3 fluorescence detector (FD) stations. The FD stations, installed surrounding the SD array, measure the air fluorescence light emitted from extensive air showers (EASs) for precise determination of energies and species. One of the FD stations were relocated from the High Resolution Fly's Eye experiment. The other two are new, designed for the TA experiment. The FD consists of a primary mirror and camera equipped with photomultiplier tubes. To obtain the EAS parameters with high accuracies, understanding the FD optical characteristics is necessary. Results of the monitored mirror reflectance during the observation time are described.
1201.0016
Inferences on the distribution of LyA emission of z~7 and z~8 galaxies
Treu, Trenti, Stiavelli, Auger, Bradley
Spectro confirmation of galaxies at z>7 are difficult due to drop in LyA intensity, compared to samples at z~6. This is probably a cosmic reionization signal, but the dataset is small, heteregenous, and often incomplete. Use Bayesian framework to interpret this evidence. Two simple phenomenological models: a smooth one, and a patchy one. Challenging but feasible to constrain the distribution of LyA emitters at z~8 and distinguish between models.
1201.0072
Acoustic detection of astrophysical neutrinos in South Pole ice
Vandenbroucke
HE particles interact in dense media to produce a particle shower, most of the shower energy is deposited in the medium as heat, causing it to expand locally and emit a shock wave with a medium dependent peak frequency (~10kHz). South Pole Ice is suited. Detect cosmogenic neutrinos (GZK) with multiple methods (optical/radio/acoustic extention of the IceCube array). SPATS (South Pole acoustic test setup) measures the attenuation length, sound speed profile, noise floor, and transient noise sources in situ at the South Pole. Sound speed in ice between 200m and 500m: 3878 pm 12 m/s for pressure waves, and 1975.8 pm 8 m/s for shear waves. Acoustic amplitude attenuation length 316 pm 105 m. BG noise floor Gaussian and stable on 1s to 2yr time scale. Detected transient events over 1 yr.
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