Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21841006b&link_type=abstract
American Astronomical Society, AAS Meeting #218, #410.06; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
The 21cm Hydrogen spin flip transition has great potential to constrain the standard model of cosmology. A standard galaxy survey requires high resolution and sensitivity to identify individual galaxies. Instead using 21-cm emission, a low-resolution intensity mapping technique that resolves only large-scale linear cosmic structure will be much more efficient.
At the frequencies 500-1000MHz redshifted 21cm emission can be used to study dark energy. At these frequencies, neither a standard phased array nor single dish is optimal. The Pittsburgh Cylindrical Prototype Telescope (PCPT) is a hybrid of these designs, close spaced parabolic cylinders. A cylinder views a strip of the sky, broken into as many beams as there are feeds along the focal line. This hybrid allows for much higher survey speed than a single dish, and a much larger collecting area than a traditional synthesis array.
The PCPT is comprised of two 10m by 25m cylinders, centers spaced 25m apart. The telescope is a fixed drift-scan design. The cylinders are oriented N-S, such that the entire sky is swept through its 2o by 90o primary beam every day. Each feed line has 16 dipoles for each polarization spaced by 0.7λ, giving a 2o by 5o resolution after digital beam-forming. The dipoles directly feed a room temperature low noise amplifier made on the same circuit board. These LNA's have a measured noise temperature of 20K. Since the radio environment of Pittsburgh is full of strong terrestrial sources, a filter was added in front of the LNA, which raised the system temperature to about 100 Kelvin. We present continuum maps as well as 21cm maps of the galaxy made with the PCPT.
Bandura Kevin
Cylindrical Radio Telescope Team
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