The Kinetic Sunyaev-Zel’dovich Effect from Reionization

By M. McQuinn, S. Furlanetto, L. Hernquist, Oliver Zahn, M. Zaldarriaga. 2005

142 citations recorded by the source corpus.

During the epoch of reionization, local variations in the ionized fraction (patchiness) imprint arcminute-scale temperature anisotropies in the CMB through the kinetic Sunyaev-Zel'dovich (kSZ) effect. We employ an improved version of an analytic model of reionization devised by Furlanetto and coworkers to calculate the kSZ anisotropy from patchy reionization. This model uses extended Press-Schechter theory to determine the distribution and evolution of H II bubbles and produces qualitatively similar reionization histories to those seen in recent numerical simulations. We find that the angular power spectrum of the kSZ anisotropies depends strongly on the size distribution of the H II bubbles and on the duration of reionization. In addition, we show that upcoming measurements of the kSZ effect should be able to distinguish between several popular reionization scenarios. In particular, the amplitude of the patchy power spectrum for reionization scenarios in which the IGM is significantly ionized by Population III stars (or by miniquasars/decaying particles) can be larger (or smaller) by over a factor of 3 than the amplitude in more traditional reionization histories (with temperature anisotropies that range between 0.5 and 3 μK at l = 5000). We highlight the differences in the kSZ signal between many possible reionization morphologies and discuss the constraints that future observations of the kSZ will place on this epoch.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

The Evolution of the Intergalactic Medium (2015, background): “…derives from structures after reionization, but the prediction of reionization calculations is that there should be a significant fraction that owes to reionization (Gruzinov & Hu 1998; Knox, Scoccimarro & Dodelson 1998; Santos et al. 2003; Zahn et al. 2005; McQuinn et al. 2005; Iliev et al. 2007).”
The evolution of CMB spectral distortions in the early Universe (2011, background): “Also, the effect of unresolved SZ clusters (Markevitch et al. 1991), the kinetic SZ effect from reionization (e.g., see McQuinn et al. 2005, and references therein), and the integrated signals from dusty galaxies (e.g., see Righi et al. 2008; Viero et al. 2009; Vieira t al.”
Studying reionization with Lyα emitters (2007, background): “In addition, a sizable fraction of arc-minute-scale CMB anisotropies are imprinted during patchy reionization (Santos et al. 2003; Zahn et al. 2005; McQuinn et al. 2005), and the Atacama Cosmology Telescope and the South Pole Telescope are starting to observe these anisotropies.1 These observations…”
CMB at 2 × 2 order: the dissipation of primordial acoustic waves and the observable part of the associated energy release (2012, background): “…the effect of unresolved SZ clusters (Markevitch et al. 1991), thethermal SZ effect and the second order Doppler effect from reionization (e.g., see McQuinn et al. 2005, and references therein), and the integrated signals from dusty galaxies (e.g., see Righiet al. 2008; Viero et al. 2009; Vieira…”
The Atacama Cosmology Telescope: likelihood for small-scale CMB data (2013, background): “, [27, 33, 45], as well as from the motion of galaxy clusters at later times.”
Cosmological Parameter Estimation Using 21 cm Radiation from the Epoch of Reionization (2005, methodology): “McQuinn et al. (2005) showed that it is not necessary to consider bubble substructure in this analytic model when constructing Px ; only the size of a bubble and the average density within a bubble are important.”
Simulations and Analytic Calculations of Bubble Growth during Hydrogen Reionization (2006, methodology): “On large scales, linear infall boosts the spherically averaged 21 cm redshift power spectrum relative to its real space analogue, analogous to the ‘Kaiser effect’ in galaxy surveys (Kaiser 1987; Bharadwaj & Ali 2004; McQuinn et al. 2005; Barkana & Loeb 2005).”
PRISM (Polarized Radiation Imaging and Spectroscopy Mission): an extended white paper (2013, background): “Z effect also generates non-Gaussian anisotropy on the sky, with contributions from the epoch of reionization because of variations in the ionization fraction related to the patchiness of the process [137]. At ‘ ’1000 2000 the CMB power spectrum has a substantial contribution due to this signal. PRI”
COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF REIONIZATION FROM THE SOUTH POLE TELESCOPE (2011, background): “(7) Hence, we can define a barrier δx(r, z) which fluctuations have to cross for their baryonic content to become ion- 2 The reason we do not use purely analytic models is that they have difficulties describing the partial overlap stage of merging ionized regions (e.g., McQuinn et al. 2005b).”
PROBING THE INFLATON: SMALL-SCALE POWER SPECTRUM CONSTRAINTS FROM MEASUREMENTS OF THE COSMIC MICROWAVE BACKGROUND ENERGY SPECTRUM (2012, background): “…& Zeldovich 1972; Cen & Ostriker 1999; Miniati et al. 2000);unresolved SZ clusters(Markevitch et al. 1991); the thermal SZ effect and second order Doppler effect from reionization(McQuinn et al. 2005)) can cause an averagey-distortion that is expected to be orders of magnitude larger in amplitude.”
Taxing the rich: Recombinations and bubble growth during reionization (2005, result): “…hexagons show the fraction of the ionized volume in bubbles with R = Rmax for the model with recombinations. bubbles as lie in large bubbles for the pure FZH04 model.3 With our linear barrier, the difference is slightly larger [compare our equation (18) with equation (11) of McQuinn et al. (2005)].”
Early Cosmological H II/He III Regions and Their Impact on Second-Generation Star Formation (2006, background): “The shape and extent of the early H ii regions determine the global topology of the distribution of neutral and ionized gas at different epochs (e.g.,McQuinn et al. 2005, 2007; Zahn et al. 2005, 2007), which can be probed by future ground-based radio observations; turned around, the observations…”
The physics of the intergalactic medium (2007, background): “Polarization anisotropy measure- ments on arcminute scales by the Planck satellite,23 to be launched in 2008, may reveal the expected patchiness of reionization, which may be used to discriminate between competing reionization scenarios (McQuinn et al., 2005; Santos et al., 2003; Zahn et al., 2005).”
SIMULATIONS OF THE MICROWAVE SKY (2009, unknown): “1000 (e.g. Santos et al. 2003; McQuinn et al. 2005; Zahn et al. 2005).”
The morphology of H ii regions during reionization (2006, background): “The size distribution of H II regions during reionization affects the spectrum of these anisotropies (McQuinn et al. 2005; Zahn et al. 2005; Iliev et al. 2006b).”
Reionization and the Cosmic Dawn with the Square Kilometre Array (2012, methodology): “More detailed modeling of the effect of patchy reionization were subsequently performed using numerical simulations (Salvaterra et al. 2005; Iliev et al. 2007) and semi-analytical models (McQuinn et al. 2005; Zahn et al. 2005; Mesinger et al. 2012).”