Redshift Dependence of the Cosmic Microwave Background Temperature From Sunyaev-Zeldovich Measurements

Luzzi, G.; Shimon, Meir; Lamagna, L.; Rephaeli, Yoel; Petris, M. De; Conte, A.; Gregori, S. De; Battistelli, E. S.

doi:10.1088/0004-637x/705/2/1122

Cited by 91 publications

(151 citation statements)

References 34 publications

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“…Our measurements based on the rotational excitation of CO molecules are represented by red filled circles at 1.7 < z < 2.7. Other measurements at z > 0 are based (i) on the S-Z effect (blue triangles at z < 0.6, Luzzi et al 2009) and (ii) on the analysis of the fine structure of atomic carbon (green open squares: z = 1.8, Cui et al 2005; z = 2.0, Ge et al 1997; z = 2.3, Srianand et al 2000; z = 3.0, Molaro et al 2002). Upper limits come from the analysis of atomic carbon (from the literature and our UVES sample, see Srianand et al 2008) and from the analysis of molecular absorption lines in the lensing galaxy of PKS 1830-211 (open circle at z = 0.9, Wiklind & Combes 1996).…”

Section: Resultsmentioning

confidence: 99%

“…The first one relies on the measurement of a small change in the spectral intensity of the CMB towards clusters of galaxies owing to inverse Compton scattering of photons by the hot intra-cluster gas: the so-called Sunyaev-Zel'dovich (S-Z) effect (Fabbri et al 1978;Rephaeli 1980). Although this technique permits precise measurements (ΔT ∼ 0.3 K; Battistelli et al 2002;Luzzi et al 2009), the method is essentially limited to z < 0.6 because of the scarcity of known clusters at higher redshifts. The other technique uses the excitation of interstellar atomic or molecular species that have transition energies in the sub-millimetre range and can be excited by CMB photons.…”

Section: Introductionmentioning

confidence: 99%

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The evolution of the cosmic microwave background temperature

Noterdaeme

Petitjean

Srianand

et al. 2011

A&A

169

164

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A milestone of modern cosmology was the prediction and serendipitous discovery of the cosmic microwave background (CMB), the radiation leftover after decoupling from matter in the early evolutionary stages of the Universe. A prediction of the standard hot Big-Bang model is the linear increase with redshift of the black-body temperature of the CMB (T CMB ). This radiation excites the rotational levels of some interstellar molecules, including carbon monoxide (CO), which can serve as cosmic thermometers. Using three new and two previously reported CO absorption-line systems detected in quasar spectra during a systematic survey carried out using VLT/UVES, we constrain the evolution of T CMB to z ∼ 3. Combining our precise measurements with previous constraints, we obtain T CMB (z) = (2.725 ± 0.002) × (1 + z) 1−β K with β = −0.007 ± 0.027, a more than two-fold improvement in precision. The measurements are consistent with the standard (i.e. adiabatic, β = 0) Big-Bang model and provide a strong constraint on the effective equation of state of decaying dark energy (i.e. w eff = −0.996 ± 0.025).

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The evolution of the cosmic microwave background temperature

Noterdaeme

Petitjean

Srianand

et al. 2011

A&A

169

164

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“…Let us consider the bound on β coming from T CMB (z) constraints, at redshifts in the range z = 0.023 − 0.546, from multi-frequency measurements of the SZ effect towards the 13 clusters of Ref [5]. By fitting the T CMB (z) data points and relaxing the condition of a positive prior on β, that is allowing for photon dimming/absorption (corresponding to β < 0) as well as photon creation (β > 0), we get β = 0.065 ± 0.080.…”

Section: Constraints From the Sz Effect Towards Clustersmentioning

confidence: 99%

Constraints on the CMB temperature-redshift dependence from SZ and distance measurements

Avgoustidis

Luzzi

Martins

et al. 2012

J. Cosmol. Astropart. Phys.

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Abstract. The relation between redshift and the CMB temperature, T CMB (z) = T 0 (1 + z) is a key prediction of standard cosmology, but is violated in many nonstandard models. Constraining possible deviations to this law is an effective way to test the ΛCDM paradigm and search for hints of new physics. We present state-ofthe-art constraints, using both direct and indirect measurements. In particular, we point out that in models where photons can be created or destroyed, not only does the temperature-redshift relation change, but so does the distance duality relation, and these departures from the standard behaviour are related, providing us with an opportunity to improve constraints. We show that current datasets limit possible deviations of the form T CMB (z) = T 0 (1 + z) 1−β to be β = 0.004 ± 0.016 up to a redshift z ∼ 3. We also discuss how, with the next generation of space and ground-based experiments, these constraints can be improved by more than one order of magnitude.

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“…The first one relies on the measurement of a small change in the spectral intensity of the CMB towards clusters of galaxies owing to inverse Compton scattering of photons by the hot intra-cluster gas: the so-called Sunyaev-Zeldovich (S-Z) effect. Although this technique per-mits precise measurements ∆T ∼ 0.3 K (Luzzi et al 2009;Hurier et al 2014), the method is essentially limited to z < 1 because of the scarcity of known clusters at higher redshifts. The other technique uses the excitation of interstellar atomic or molecular species that have transition energies in the sub-millimetre range and can be excited by CMB photons.…”

Section: Measuring the Temperature Of The Cosmic Microwave Backgroundmentioning

confidence: 99%

GRBs and Fundamental Physics

Petitjean

Wang

et al. 2016

Space Sci Rev

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Gamma-ray bursts (GRBs) are short and intense flashes at the cosmological distances, which are the most luminous explosions in the Universe. The high luminosities of GRBs make them detectable out to the edge of the visible universe. So, they are unique tools to probe the properties of high-redshift universe: including the cosmic expansion and dark energy, star formation rate, the reionization epoch and the metal evolution of the Universe. First, they can be used to constrain the history of cosmic acceleration and the evolution of dark energy in a redshift range hardly achievable by other cosmological probes. Second, long GRBs are believed to be formed by collapse of massive stars. So they can be used to derive the high-redshift star formation rate, which can not be probed by current observations. Moreover, the use of GRBs as cosmological tools could unveil the reionization history and metal evolution of the Universe, the intergalactic medium (IGM) properties and the nature of first stars in the early universe. But beyond that, the GRB high-energy photons can be applied to constrain Lorentz invariance violation (LIV) and to test Einstein's Equivalence Principle (EEP). In this paper, we review the progress on the GRB cosmology and fundamental physics probed by GRBs.

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Redshift Dependence of the Cosmic Microwave Background Temperature From Sunyaev-Zeldovich Measurements

Cited by 91 publications

References 34 publications

The evolution of the cosmic microwave background temperature

The evolution of the cosmic microwave background temperature

Constraints on the CMB temperature-redshift dependence from SZ and distance measurements

GRBs and Fundamental Physics

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