Constraining quantum collapse inflationary models with current data: The semiclassical approach

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The hypothesis of the self-induced collapse of the inflaton wave function was introduced as a candidate for the physical process responsible for the emergence of inhomogeneity and anisotropy at all scales. In particular, we consider different proposal for the precise form of the dynamics of the infl...

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Autor principal: Piccirilli, M.P
Otros Autores: León, G., Landau, S.J, Benetti, M., Sudarsky, D.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: World Scientific Publishing Co. Pte Ltd 2019
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Piccirilli, M.P. 
245 1 0 |a Constraining quantum collapse inflationary models with current data: The semiclassical approach 
260 |b World Scientific Publishing Co. Pte Ltd  |c 2019 
506 |2 openaire  |e Política editorial 
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520 3 |a The hypothesis of the self-induced collapse of the inflaton wave function was introduced as a candidate for the physical process responsible for the emergence of inhomogeneity and anisotropy at all scales. In particular, we consider different proposal for the precise form of the dynamics of the inflaton wave function: (i) the GRW-type collapse schemes proposals based on spontaneous individual collapses which generate nonvanishing expectation values of various physical quantities taken as ansatz modifications of the standard inflationary scenario; (ii) the proposal based on a Continuous Spontaneous Localization (CSL) type modification of the Schrödinger evolution of the inflaton wave function, based on a natural choice of collapse operator. We perform a systematic analysis within the semi-classical gravity approximation, of the standing of those models considering a full quasi-de Sitter expansion scenario. We note that the predictions for the Cosmic Microwave Background (CMB) temperature and polarization spectrum differ slightly from those of the standard cosmological model. We also analyze these proposals with a Bayesian model comparison using recent CMB and Baryonic Acoustic Oscillations (BAO) data. Our results show a moderate preference of the joint CMB and BAO data for one of the studied collapse schemes model over the ACDM one, while there is no preference when only CMB data are considered. Additionally, analysis using CMB data provide the same Bayesian evidence for both the CSL and Standard Models, i.e. the data have no preference between the simplicity of the LCDM model and the complexity of the collapse scenario. © 2019 World Scientific Publishing Company.  |l eng 
536 |a Detalles de la financiación: National Science and Technology Development Agency 
536 |a Detalles de la financiación: Universidad Nacional de La Plata 
536 |a Detalles de la financiación: Consejo Nacional de Ciencia y Tecnología, 101712 
536 |a Detalles de la financiación: Instituto Nazionale di Fisica Nucleare, PIP 11220120100504 CONICET 
536 |a Detalles de la financiación: Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro 
536 |a Detalles de la financiación: Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro 
536 |a Detalles de la financiación: IG 100316 
536 |a Detalles de la financiación: Agencia Nacional de Promoción Científica y Tecnológica, PICT-2016-0081, G140 
536 |a Detalles de la financiación: The authors acknowledge the use of the supercluster Mitzli at UNAM for the statistical analyses and thank the people of DGSCA-UNAM for computational and technical support. MB acknowledges financial support from the Funda¸cão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ – fellowship Nota 10), and is also supported by INFN, Naples section, QGSKY project. MPP, GL and SL are supported by PIP 11220120100504 CONICET and by the National Agency for the Promotion of Science and Technology (ANPCYT) of Argentina grant PICT-2016-0081; and by grant G140 from UNLP. DS acknowledges partial financial support from DGAPA-UNAM project IG 100316 and by CONACYT project 101712, the FAE-Network of CONACYT, as well as the sabbatical fellowships from CO-MEX-US (Fullbright–Garcia Robles) and from DGAPA-UNAM (Paspa). The authors acknowledge the use of CosmoMC71 and Multinest code.72–74 
593 |a Grupo de Astrofísica, Relatividad y Cosmología, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de la Plata, Paseo del Bosque S/N 1900 La Plata, Pcia de Buenos Aires, Argentina 
593 |a Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires and IFIBA, CONICET, Ciudad Universitaria - PabI, Buenos Aires, 1428, Argentina 
593 |a Observatório Nacional, Rua General José Cristino 77, Rio de Janeiro, 20921-400, RJ, Brazil 
593 |a University of Naples Federico II, Physics Department Ettore Pancini, Monte sant'Angelo Campus, Via Cinthia 21, Naples, I-80126, Italy 
593 |a Istituto Nazionale di Fisica Nucleare (INFN), Sez. Napoli, Monte sant'Angelo Campus, Via Cinthia 9, Naples, I-80126, Italy 
593 |a Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, A.P. 70-543, México D.F., 04510, Mexico 
690 1 0 |a COSMOLOGICAL PARAMETERS FROM CMB 
690 1 0 |a INFLATION 
690 1 0 |a PHYSICS OF THE EARLY UNIVERSE 
700 1 |a León, G. 
700 1 |a Landau, S.J. 
700 1 |a Benetti, M. 
700 1 |a Sudarsky, D. 
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