Cosmic Microwave Background Observables and Their Cosmological Implications

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The First Cosmic Structures and Their Effects (2004, background): “…eXperiment IMaging Array), DASI4 (Degree Angular Scale Interferometer) and, more recently, WMAP5 (Wilkinson Microwave Anisotropy Probe) which provided the power spectrum of temperature anisotropies on a wide range of angular scales (Hu et al. 2001; Sievers et al. 2003; Spergel et al. 2003).”
The Void Phenomenon (2001, unknown): “The CDM model is maturing, most dramatically in its success in relating the power spectrum of the thermal background radiation temperature to observationally acceptable cosmological parameters (e.g., Hu et al. 2001).”
The Atacama Cosmology Telescope: cosmological parameters from three seasons of data (2013, unknown): “Extra relativistic energy density damps the small-scale CMB power – see Hou et al. (2013) for a concise recent review, and the discussions in Hu & Dodelson (2002); Hu et al. (2001); Bashinsky & Seljak (2004); Tegmark (2005); Lesgourgues & Pastor (2006); Hannestad (2010).”
Constraints on the Equation of State of Dark Energy and the Hubble Constant from Stellar Ages and the Cosmic Microwave Background (2003, background): “Method If the universe is assumed to be flat, the position of the first acoustic peak (l1 in the standard spherical harmonics notation) depends primarily on the age of the universe and on the effective value7 of w (Caldwell et al. 1998; Hu et al. 2001; Knox, Christensen, & Skordis 2001).”