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V. Fish, W. Alef, J. Anderson, K. Asada, A. Baudry, et al. , (2013), arXiv:1309.3519 [astro-ph.IM]
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F. Pepe, S. Cristiani, R. Rebolo, N. C. Santos, H. Dekker, D. Mégevand, F. M. Zerbi, A. Cabral, P. Molaro, P. Di Marcantonio, M. Abreu, M. Affolter, M. Aliverti, C. Allende Prieto, M. Amate, G. Avila, V. Baldini, P. Bristow, C. Broeg, R. Cirami, J. Coelho, P. Conconi, I. Coretti, G. Cupani, V. D’Odorico, V. De Caprio, B. Delabre, R. Dorn, P. Figueira, A. Fragoso, S. Galeotta, L. Genolet, R. Gomes, J. I. González Hernández, I. Hughes, O. Iwert, F. Kerber, M. Landoni, J.-L. Lizon, C. Lovis, C. Maire, M. Mannetta, C. Martins, M. A. Monteiro, A. Oliveira, E. Poretti, J. L. Rasilla, M. Riva, S. Santana Tschudi, P. Santos, D. Sosnowska, S. Sousa, P. Spanò, F. Tenegi, G. Toso, E. Vanzella, M. Viel, and M. R. Zapatero Osorio, The Messenger 153
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2015

Sub-percent constraints on cosmological temperature evolution

Avgoustidis, A., Génova-Santos, R. T., Luzzi, G. et al.

Understand

The redshift dependence of the cosmic microwave background temperature is one of the key cosmological observables.

In the standard cosmological model one has $T(z)=T_0(1+z)$, where $T_0$ is the present-day temperature.
Deviations from this behavior would imply the presence of new physics.
Here we discuss how the combination of all currently available direct and indirect measurements of $T(z)$ constrains the common phenomenological parametrization $T(z)=T_0(1+z)^{1-\beta}$, and obtain the first sub-percent constraint on the $\beta$ parameter, specifically $\beta=(7.6\pm8.0)\times10^{-3}$ at the $68.3\%$ confidence level.

Built on

J. M. H. Etherington, Phil. Mag. 15
1933
Earlier work this paper cites.
D. J. Fixsen, Ap. J. 707
Original
1955
Earlier work this paper cites.
J. N. Bahcall and R. A. Wolf, Ap. J. 152
1968
Earlier work this paper cites.
R. A. Sunyaev and Y. B. Zeldovich, Astrophys. & Sp. Sci. 7
1970
Earlier work this paper cites.
R. Fabbri, F. Melchiorri, and V. Natale, Astrophys. & Sp. Sci. 59
1978
Earlier work this paper cites.
Y. Rephaeli, Ap. J. 241
1980
Earlier work this paper cites.
A. G. Riess et al. (Supernova Search Team), Astron.J. 116
1998
Earlier work this paper cites.
S. Perlmutter, G. Aldering, G. Goldhaber, R. A. Knop, P. Nugent, P. G. Castro, S. Deustua, S. Fabbro, A. Goobar, D. E. Groom, I. M. Hook, A. G. Kim, M. Y. Kim, J. C. Lee, N. J. Nunes, R. Pain, C. R. Pennypacker, R. Quimby, C. Lidman, R. S. Ellis, M. Irwin, R. G. McMahon, P. Ruiz-Lapuente, N. Walton, B. Schaefer, B. J. Boyle, A. V. Filippenko, T. Matheson, A. S. Fruchter, N. Panagia, H. J. M. Newberg, W. J. Couch, and T. S. C. Project, Ap. J. 517
1999
Earlier work this paper cites.
G. D’Agostini, ArXiv High Energy Physics - Experiment e-prints (1999), hep-ex/9910036
1999
Earlier work this paper cites.
A. N. Aguirre, Astrophys.J. 512
1999
Earlier work this paper cites.
J. A. S. Lima, A. I. Silva, and S. M. Viegas, M.N.R.A.S. 312
2000
Earlier work this paper cites.
R. Srianand, P. Petitjean, and C. Ledoux, Nature 408
2000
Earlier work this paper cites.
J. Ge, J. Bechtold, and V. P. Kulkarni, Ap. J. Lett. 547
2001
Earlier work this paper cites.
E. S. Battistelli, M. De Petris, L. Lamagna, F. Melchiorri, E. Palladino, G. Savini, A. Cooray, A. Melchiorri, Y. Rephaeli, and M. Shimon, Ap. J. Lett. 580
2002
Earlier work this paper cites.
P. Molaro, S. A. Levshakov, M. Dessauges-Zavadsky, and S. D’Odorico, A. & A. 381
2002
Earlier work this paper cites.
G. Dvali and M. Zaldarriaga, Phys.Rev.Lett. 88
2002
Earlier work this paper cites.
R. Jimenez, L. Verde, T. Treu, and D. Stern, Astrophys.J. 593
2003
Earlier work this paper cites.
B. A. Bassett and M. Kunz, Phys.Rev. D69
2004
Earlier work this paper cites.
J. Cui, J. Bechtold, J. Ge, and D. M. Meyer, Ap. J. 633
2005
Earlier work this paper cites.