What can we learn on the thermal history of the Universe from future cosmic microwave background spectrum measurements at long wavelengths

Abstract

We analyse the implications of future observations of the cosmic microwave background (CMB) absolute temperature at centimetre and decimetre wavelengths, where both ground, balloon and space experiments are currently under way to complement the accurate COBE/FIRAS data available at λ 1 cm.Our analysis shows that forthcoming ground and balloon measurements will allow a better understanding of free-free distortions but will not be able to significantly improve the constraints already provided by the FIRAS data on the possible energy exchanges in the primeval plasma. The same holds even for observations with sensitivities up to ∼10 times better than those of forthcoming experiments.Thus, we have studied the impact of very high-quality data, such as those, in principle, achievable with a space experiment such as the Diffuse Microwave Emission Survey (DIMES) planned to measure the CMB absolute temperature at 0.5 λ ∼ 15 cm with a sensitivity of ∼0.1 mK, close to that of FIRAS. We have demonstrated that such high-quality data would improve by a factor of ∼50 the FIRAS results on the fractional energy exchanges, / i , associated with dissipation processes possibly occurred in a wide range of cosmic epochs, at intermediate and high redshifts (y h 1), and that the energy dissipation epoch could also be significantly constrained. By jointly considering two dissipation processes occurring at different epochs, we demonstrated that the sensitivity and frequency coverage of a DIMESlike experiment would allow one to accurately recover the epoch and the amount of energy possibly injected into the radiation field at early and intermediate epochs even in the presence of a possible late distortion, while the constraints on the energy possibly dissipated at late epochs can be improved by a factor of 2. In addition, such measurements can provide an independent and very accurate cross-check of FIRAS calibration.Finally, a DIMES-like experiment will be able to provide indicative independent estimates of the baryon density: the product b H 2 0 can be recovered within a factor of ∼2-5 even in the case of (very small) early distortions with / i ∼ (5-2) × 10 −6 . On the other hand, for b (H 0 /50) 2 0.2, an independent baryon density determination with an accuracy at ∼ per cent level, comparable to that achievable with CMB anisotropy experiments, would require an accuracy of ∼1 mK or better in the measurement of possible early distortions but up to a wavelength from ∼ few × dm to ∼7 dm, according to the baryon density value.

TRIS. II. Search for CMB Spectral Distortions at 0.60, 0.82, and 2.5 GHz

“…29 No. 1, 2008Burigana & Salvaterra 2003 2 ) À2 = 3 . The limit set by COBE FIRAS on the chemical potential (jj < 9 ; 10 À5 ) implies a spectral distortion ÁT BE P 17 mK (95% CL), so the current measurements at low frequency, including TRIS, are not yet accurate enough to detect BE min and constrain further b .…”

Spectral distortion of the CMB by the cumulative CO emission from galaxies throughout cosmic history

“…However, the standard model of cosmology predicts tiny deviations from the Planckian spectrum due to cosmological processes which heat, cool, scatter, and create CMB photons throughout the history of the Universe Sunyaev & Zeldovich 1970;Illarionov & Sunyaev 1975a,b;Danese & de Zotti 1982;Burigana, Danese, & de Zotti 1991;Hu & Silk 1993;Burigana & Salvaterra 2003;Sunyaev & Khatri 2013). While at redshifts z 2×10 6 , the thermalization process (mediated by the combined action of double Compton emission, Bremsstrahlung and Compton scattering) is rapid enough to efficiently erase any distortion to unobservable levels, at lower redshifts, the CMB spectrum becomes vulnerable and spectral distortions that form are "locked in" and can thus be theoretically observed today Chluba 2014;Chluba, Hamann, & Patil 2015).…”

On the effect of cyclotron emission on the spectral distortions of the cosmic microwave background

“…Consequently, the constraints on the energy dissipations at various cosmic times set by the currently available data (Salvaterra and Burigana, 2002) and expected by future experiments (Kogut, 1996, Fixsen and Mather, 2002, Burigana and Salvaterra, 2003, Burigana et al, 2004 can be derived, under quite general assumptions, by considering only Compton scattering, bremsstrahlung, and double Compton, other than, obviously, the considered dissipation process(es).…”