There are few data available with which to constrain the thermal history of the intergalactic medium (IGM) following global recombination. Thus far, most constraints flow from analyses of the Cosmic Microwave Background and optical spectroscopy along a few lines of sight. However, direct study of the IGM in emission or absorption against the CMB via the 1S hyperfine transition of Hydrogen would enable broad characterization thermal history and source populations. New generations of radio arrays are in development to measure this line signature. Bright foreground emission and the complexity of instrument calibration models are significant hurdles. How to optimize these is uncertain, resulting in a diversity in approaches. We discuss recent limits on line brightness, array efforts including the new Large Aperture Experiment to Detect the Dark Ages (LEDA), and the next generation Hydrogen Reionization Array (HERA) concept.
[1]
James Aguirre,et al.
A SENSITIVITY AND ARRAY-CONFIGURATION STUDY FOR MEASURING THE POWER SPECTRUM OF 21 cm EMISSION FROM REIONIZATION
,
2011,
1103.2135.
[2]
M. Lueker,et al.
COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF REIONIZATION FROM THE SOUTH POLE TELESCOPE
,
2011,
1111.6386.
[3]
Abraham Loeb,et al.
21 cm cosmology in the 21st century
,
2011,
Reports on progress in physics. Physical Society.
[4]
Michael A. Clark,et al.
Accelerating radio astronomy cross-correlation with graphics processing units
,
2011,
Int. J. High Perform. Comput. Appl..
[5]
Max Tegmark,et al.
Astrophysics from the Highly-Redshifted 21 cm Line
,
2009,
0902.3011.