Precision epoch of reionization studies with next-generation CMB experiments

Calabrese, E.; Hložek, Renée; Battaglia, Nick; Bond, J. R.; Bernardis, Francesco De; Devlin, Mark J.; Hajian, Amir; Henderson, S.; Hil, J. Colin; Kosowsky, Arthur; Louis, Thibaut; McMahon, Jeff; Moodley, Kavilan; Newburgh, Laura; Niemack, Michael D.; Page, Lyman A.; Partridge, B.; Sehgal, Neelima; Sievers, Jonathan; Spergel, David N.; Staggs, Suzanne T.; Switzer, Eric R.; Trac, Hy; Wollack, Edward J.

doi:10.1088/1475-7516/2014/08/010

Cited by 107 publications

(107 citation statements)

References 92 publications

(133 reference statements)

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“…Above this mass scale the ψDM galaxy number density should be close to CDM, and therefore consistent with the observational constraint [55,56]. Larger ψDM simulations with the addition of baryons will be invaluable for supporting these arguments and testing with the forthcoming observations such as JWST [57] and AdvACT [58].…”

supporting

confidence: 66%

Understanding the Core-Halo Relation of Quantum Wave Dark Matter from 3D Simulations

Schive¹,

Liao²,

Woo³

et al. 2014

Phys. Rev. Lett.

467

593

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We examine the nonlinear structure of gravitationally collapsed objects that form in our simulations of wavelike cold dark matter (ψDM), described by the Schrödinger-Poisson (SP) equation with a particle mass ∼ 10 −22 eV. A distinct gravitationally self-bound solitonic core is found at the center of every halo, with a profile quite different from cores modeled in the warm or self-interacting dark matter scenarios. Furthermore, we show that each solitonic core is surrounded by an extended halo composed of large fluctuating dark matter granules which modulate the halo density on a scale comparable to the diameter of the solitonic core. The scaling symmetry of the SP equation and the uncertainty principle tightly relate the core mass to the halo specific energy, which, in the context of cosmological structure formation, leads to a simple scaling between core mass (Mc) and haloh , where a is the cosmic scale factor. We verify this scaling relation by (i) examining the internal structure of a statistical sample of virialized halos that form in our 3D cosmological simulations, and by (ii) merging multiple solitons to create individual virialized objects. Sufficient simulation resolution is achieved by adaptive mesh refinement and graphic processing units acceleration. From this scaling relation, present dwarf satellite galaxies are predicted to have kpc sized cores and a minimum mass of ∼ 10 8 M⊙, capable of solving the small-scale controversies in the cold dark matter model. Moreover, galaxies of 2 × 10 12 M⊙ at z = 8 should have massive solitonic cores of ∼ 2 × 10 9 M⊙ within ∼ 60 pc. Such cores can provide a favorable local environment for funneling the gas that leads to the prompt formation of early stellar spheroids and quasars.PACS numbers: 03.75. Lm, 95.35.+d, 98.56.Wm, 98.62.Gq Accumulating evidences suggest that the Universe contains ∼ 26% dark matter [1] which interacts primarily through self-gravity. Dark matter comprising very light bosons with a mass m ψ ∼ 10 −22 eV has been recognized as a viable means of suppressing low mass galaxies and providing cored profiles in dark matter dominated galaxies [2,3]. Interestingly, this boson mass scale can naturally arise in a non-QCD axion model [4], lending support for the very light boson. The relative deficiency of the observed number of low-mass galaxies is a major problem for standard cold dark matter (CDM) [5][6][7], for which a steeply rising mass function is predicted [8]. Furthermore, the dwarf spheroidal galaxies [9-20] and low surface brightness galaxies [21,22] are generally inferred to have large flat cores of dark matter, at odds with the singular cores required by standard CDM [23,24]. Complicated baryonic physics such as supernova feedback is required to solve both issues in the CDM paradigm [25][26][27][28][29][30][31][32][33][34].Extremely light bosonic dark matter can be assumed to be non-thermally generated and described by a single coherent wave function [2,[35][36][37][38], which we term ψDM. Here solutions to both the missing-satellite and ...

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supporting

confidence: 66%

Understanding the Core-Halo Relation of Quantum Wave Dark Matter from 3D Simulations

Schive¹,

Liao²,

Woo³

et al. 2014

Phys. Rev. Lett.

467

593

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“…Potential improvements in the covariance could include taking advantage of multi-frequency information available in upcoming surveys (e.g., Benson et al 2014;Calabrese et al 2014) to improve the kSZ signal extraction and reduce the measurement error. Larger LRG catalogs could also be used, such as in the first kSZ detection; however, this increases uncertainty in the minimum mass of the cluster sample.…”

Section: Discussionmentioning

confidence: 99%

“…We forecast cosmological constraints for three different combinations of surveys: (1) a current (Stage II) CMB survey, such as ACTPol (Niemack et al 2010), combined with a galaxy sample that includes spectroscopic redshifts, such as SDSS BOSS (Comparat et al 2013), (2) a near-term (Stage III) survey, such as Advanced ACTPol (Calabrese et al 2014), also combined with SDSS BOSS, and (3) a longer-term (Stage IV) survey, such as CMB-S4 (Abazajian et al 2013), combined with a next generation spectroscopic survey, such as DESI (Levi et al 2013). …”

Section: Cosmological Modelmentioning

confidence: 99%

“…We assume a BOSS-like spectroscopic survey for Stages II and III and a DESI-like Stage IV survey with redshift ranges that are determined by the redshift coverage of the LRG sample and assume joint photometric survey data. We assume Stages II and III have access to the same or comparable LRG surveys so retain the same limiting mass, but do slightly increase CMB overlap with these data due to the larger survey area planned for Advanced ACTPol (Calabrese et al 2014). For Stage IV we assume a deeper LRG survey that provides lower minimum mass, higher z, and larger overlap.…”

Section: Cosmological Modelmentioning

confidence: 99%

“…This approach minimizes contributions from the CMB, thermal SZ, and foregrounds, which can be treated as approximately constant on these scales, and by averaging over many clusters pairs any effects independent of the separation will cancel. CMB surveys such as ACTPol (Niemack et al 2010), SPTPol (Austermann et al 2012), Advanced ACTPol (Calabrese et al 2014), SPT-3 G (Benson et al 2014), and a next-generation, so-called Stage IV CMB survey (Abazajian et al 2013) in combination with overlapping galaxy surveys, such as those described above, can improve upon this detection and enable the use of mean pairwise velocities as a cosmological probe.…”

Section: Introductionmentioning

confidence: 99%

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Constraints on Gravity and Dark Energy From the Pairwise Kinematic Sunyaev–zel’dovich Effect

Mueller

Bernardis

Bean

et al. 2015

ApJ

Self Cite

124

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We calculate the constraints on dark energy and cosmic modifications to gravity achievable with upcoming cosmic microwave background (CMB) surveys sensitive to the Sunyaev-Zel'dovich (SZ) effects. The analysis focuses on using the mean pairwise velocity of clusters as observed through the kinematic SZ effect (kSZ), an approach based on the same methods used for the first detection of the kSZ effect, and includes a detailed derivation and discussion of this statistic's covariance under a variety of different survey assumptions. The potential of current, Stage II, and upcoming, Stages III and IV, CMB observations are considered, in combination with contemporaneous spectroscopic and photometric galaxy observations. A detailed assessment is made of the sensitivity to the assumed statistical and systematic uncertainties in the optical depth determination, the magnitude and uncertainty in the minimum detectable mass, and the importance of pairwise velocity correlations at small separations, where nonlinear effects can start to arise. In combination with Stage III constraints on the expansion history, such as those projected by the Dark Energy Task Force, we forecast 5% and 3% for fractional errors on the growth factor, γ, for Stage III and IV surveys, respectively, and 2% constraints on the growth rate, f g , for a Stage IV survey for < < z 0.2 0.6. The results suggest that kSZ measurements of cluster peculiar velocities, obtained from crosscorrelation with upcoming spectroscopic galaxy surveys, could provide robust tests of dark energy and theories of gravity on cosmic scales.

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Observing the Epoch of Reionization with the Cosmic Microwave Background

Reichardt

2016

Understanding the Epoch of Cosmic Reionization

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We review the observable consequences of the epoch of reionization (EoR) on the cosmic microwave background (CMB), and the resulting constraints on the EoR. We discuss how Thomson scattering with the free electrons produced during EoR equates to an optical depth for CMB photons. The optical depth measurements from the WMAP and Planck satellites, using large-scale CMB polarization power spectra, is one of the few current constraints on the timing of cosmic reionization. We also present forecasts for the precision with which the optical depth will be measured by future satellite missions. Second, we consider the kinematic Sunyaev-Zel'dovich (kSZ) effect, and how the kSZ power spectrum depends on the duration of reionization. We review current measurements of the kSZ power and forecasts for future experiments. Finally, we mention proposals to look for spectral distortions in the CMB that are related to the electron temperature at EoR, and ideas to map the variations in the optical depth across the sky.Comment: Book chapter in "Understanding the Epoch of Cosmic Reionization: Challenges and Progress", Springer International Publishing, Ed. Andrei Mesinger, ISBN 978-3-319-21956-

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Precision epoch of reionization studies with next-generation CMB experiments

Cited by 107 publications

References 92 publications

Understanding the Core-Halo Relation of Quantum Wave Dark Matter from 3D Simulations

Understanding the Core-Halo Relation of Quantum Wave Dark Matter from 3D Simulations

Constraints on Gravity and Dark Energy From the Pairwise Kinematic Sunyaev–zel’dovich Effect

Observing the Epoch of Reionization with the Cosmic Microwave Background

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