Matched filtering with interferometric 21 cm experiments

Global 21 cm signal experiments : A designer ’ s guide

Foreground Contamination in Interferometric Measurements of the Redshifted 21 Cm Power Spectrum

Subtraction of astrophysical foreground contamination from “dirty” sky maps produced by simulated measurements of the Murchison Widefield Array (MWA) has been performed by fitting a 2-order polynomial along the spectral dimension of each pixel in the data cubes. The simulations include the effects of the frequency-dependent primary antenna beams and synthesized array beams and recover the one-d...

How well can we measure and understand foregrounds with 21 cm experiments?

Before it becomes a sensitive probe of the Epoch of Reionization, the Dark Ages, and fundamental physics, 21 cm tomography must successfully contend with the issue of foreground contamination. Broadband foreground sources are expected to be roughly four orders of magnitude larger than any cosmological signals, so precise foreground models will be necessary. Such foreground models often contain ...

Sub-10 cm Interferometric Accelerometer With Nano-g Resolution

A high-resolution accelerometer with a bulk-micromachined silicon proof mass and an interferometric position sensor was developed for measuring vibratory accelerations. The interferometer consists of interdigitated fingers that are alternately attached to the proof mass and support substrate. Illuminating the fingers with coherent light generates a series of diffracted beams. The intensity of a...

Double-rotated Matched Filtering

Using the concept of steerable filters, it is possible to represent the rotation of a known template – and thus arbitrary orientations of lines or edges – as a linear combination of a fixed number of base filters, thus allowing a computationally efficient detection of 1D structures. In spite of their usefulness in many image processing areas, such structures exhibit one important drawback: Due ...