Redshifting rings of power

By Wayne Hu, Zoltán Haiman. 2003

170 citations recorded by the source corpus.

The cosmic microwave background (CMB) has provided a precise template for features in the linear power spectrum: the matter-radiation turnover, sound horizon drop, and acoustic oscillations. In a two-dimensional power spectrum in redshift and angular space, the features appear as distorted rings, and yield simultaneous, purely geometric, measures of the Hubble parameter $H(z)$ and angular diameter distance ${D}_{A}(z)$ via an absolute version of the Alcock-Paczynski test. Employing a simple Fisher matrix tool, we explore how future surveys can exploit these rings of power for dark energy studies. High-z CMB determinations of H and ${D}_{A}$ are best complemented at moderate to low redshift $(z\ensuremath{\lesssim}0.5)$ with a population of objects that are at least as abundant as clusters of galaxies. We find that a sample similar to that of the ongoing SDSS luminous red galaxy survey can achieve statistical errors at the $\ensuremath{\sim}5%$ level for ${D}_{A}(z)$ and $H(z)$ in several redshift bins. This, in turn, implies errors of $\ensuremath{\sigma}(w)=0.03--0.05$ for a constant dark energy equation of state in a flat universe. Deep galaxy cluster surveys such as the planned South Pole Telescope survey can extend this test out to $z\ensuremath{\sim}1$ or as far as redshift follow-up is available. We find that the expected constraints are at the $\ensuremath{\sigma}(w)=0.04--0.08$ level, comparable to those of galaxies and complementary in redshift coverage.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/49c449f47e219db06533c81b50650d76b4f18860

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Citations in the corpus

On the Robustness of the Acoustic Scale in the Low-Redshift Clustering of Matter (2006, background): “…and expansion history of the Universe (Eisenstein, Hu, & Tegmark 1998; Cooray, Hu, Huterer & Joffre 2001; Eisenstein 2003; Blake & Glazebrook 2003; Hu & Haiman 2003; Seo & Eisenstein 2003; Linder 2003; Matsubara 2004; Amendola et al. 2005; Blake & Bridle 2005; Glazebrook & Blake 2005; Dolney,…”
The WiggleZ Dark Energy Survey: testing the cosmological model with baryon acoustic oscillations at z= 0.6 (2011, background): “…of BAOs provide a standard cosmological ruler that can map out the cosmic expansion history and provide precise and robust constraints on the nature of the “dark energy” that is apparently dominating the current cosmic dynamics (Blake & Glazebrook 2003; Hu & Haiman 2003; Seo & Eisenstein 2003).”
The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations (2011, background): “…of baryon acoustic oscillations (BAOs) in the large-scale clustering pattern of galaxies, and their application as a cosmological standard ruler (Eisenstein, Hu & Tegmark 1998, Cooray et al. 2001, Eisenstein 2003, Blake & Glazebrook 2003, Seo & Eisenstein 2003, Linder 2003, Hu & Haiman 2003).”
A 2 per cent distance to $z$=0.35 by reconstructing baryon acoustic oscillations - I. Methods and application to the Sloan Digital Sky Survey (2012, background): “…cent distance to z = 0.35 2133 the angular diameter distance (with the ruler aligned perpendicular to the line of sight) and the Hubble parameter (with the ruler parallel to the line of sight) as a function of redshift (Blake & Glazebrook 2003; Hu & Haiman 2003; Linder 2003; Seo & Eisenstein 2003).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring DA and H at z = 0.57 from the baryon acoustic peak in the data release 9 spectroscopic galaxy sample (2013, background): “By repeating this at a variety of redshifts, one can map out the cosmic expansion history and constrain the properties of dark energy (Eisenstein 2002; Blake & Glazebrook 2003; Hu & Haiman 2003; Linder 2003; Seo & Eisenstein 2003).”
Probing Dark Energy with Baryonic Acoustic Oscillations from Future Large Galaxy Redshift Surveys (2003, methodology): “Contemporaneously with this paper, Hu & Haiman (2003) used a Fisher matrix technique similar to ours to study the performance of a mid-redshift cluster survey.”
The detectability of baryonic acoustic oscillations in future galaxy surveys. (2007, background): “Early theoretical work in this area used linear perturbation theory (Blake & Glazebrook 2003; Hu & Haiman 2003; Glazebrook & Blake 2005).”
Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, background): “…as a standard ruler which can be used to measure the distance–redshift relation, and hence constrain the dark energy equation of state (Blake & Glazebrook 2003; Hu & Haiman 2003; Linder 2003; Seo & Eisenstein 2003; Wang 2006; Guzik, Bernstein & Smith 2007; Seo & Eisenstein 2007; Seo et al. 2008).”
Measuring DA and H at z = 0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations (2012, background): “…today, which makes it an ideal standard ruler (Eisenstein & Hu 1998; Eisenstein, Hu & Tegmark 1998; Blake & Glazebrook 2003; Eisenstein 2003; Hu & Haiman 2003; Linder 2003; Seo & Eisenstein 2003; Matsubara 2004; Abdalla & Rawlings 2005; Amendola, Quercellini & Giallongo 2005; Angulo et al.…”
Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph (2012, methodology): “In particular, the CMBinferred BAO scale of 150 Mpc gives a powerful standard ruler for this geometrical test (Eisenstein et al. 2005; Percival et al. 2007; Blake et al. 2011; Hu & Haiman 2003; Seo & Eisenstein 2003).”
Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies (2005, background): “The last application can provide precise and robust constraints (Blake & Glazebrook 2003; Hu & Haiman 2003; Linder 2003; Seo & Eisenstein 2003; Amendola et al. 2004; Dolney, Jain, & Takada 2004; Matsubara 2004) on the acceleration of the expansion rate of the universe (Riess et al. 1998; Perlmutter…”
Baryonic Acoustic Oscillations in Simulated Galaxy Redshift Surveys (2005, background): “See Blake & Glazebrook (2003), Linder (2003), Hu & Haiman (2003), Amendola et al. (2005), Cooray (2004), Dolney et al. (2004), and Matsubara (2004) for similar studies.”