Constraining nonstandard recombination: A worked example

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We fit the BOOMERANG, MAXIMA and COBE-DMR measurements of the cosmic microwave background anisotropy in spatially flat cosmological models where departures from standard recombination of the primeval plasma are parametrized through a change in the fine structure constant a compared to its present va...

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Autor principal: Landau, S.J
Otros Autores: Harari, Diego Darío, Zaldarriaga, M.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2001
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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024 7 |2 scopus  |a 2-s2.0-0034884072 
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100 1 |a Landau, S.J. 
245 1 0 |a Constraining nonstandard recombination: A worked example 
260 |c 2001 
270 1 0 |m Landau, S.J.; Facultad de Ciencias Astronômicas y Geoffsicas, U.N.L.P., Paseo del Basque S/N, 1900 La Plata, Argentina; email: slandau@natura.fcaglp.unlp.edu.ar 
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506 |2 openaire  |e Política editorial 
520 3 |a We fit the BOOMERANG, MAXIMA and COBE-DMR measurements of the cosmic microwave background anisotropy in spatially flat cosmological models where departures from standard recombination of the primeval plasma are parametrized through a change in the fine structure constant a compared to its present value. In addition to α we vary the baryon and dark matter densities, the spectral index of scalar fluctuations, and the Hubble constant. Within the class of models considered, the lack of a prominent second acoustic peak in the measured spectrum can be accommodated either by a relatively large baryon density, by a tilt towards the red in the spectrum of density fluctuations, or by a delay in the time at which neutral hydrogen formed. The ratio between the second and first peak decreases by around 25% either if the baryon density Ω b h 2 is increased or the spectral index n decreased by a comparable amount, or if neutral hydrogen formed at a redshift z* about 15% smaller than its standard value. We find that the present data are best fitted by a delay in recombination, with a lower baryon density than the best fit if recombination is standard. Our best fit model has z* = 900, Ω b h 2 = 0.024, Ω b h 2 =O.I4, //0=49 and =1.02. Compatible with present data at 95% confidence level 780<z*; 1150, 0.018<Ω b h 2 <0.036, 0.07<Ω b h 2 <0.3 and 0.9<< 1.2. ©2001 The American Physical Society.  |l eng 
593 |a Facultad de Ciencias Astronômicas y Geoffsicas, U.N.L.P., Paseo del Basque S/N, 1900 La Plata, Argentina 
593 |a Departamento de fi'Sica, FCEyN, Ciudad Universitaria, Pabell'on 1, 1428 Buenos Aires, Argentina 
593 |a Institute for Advanced Study, Princeton, NJ 08540, United States 
690 1 0 |a HYDROGEN 
690 1 0 |a ACOUSTICS 
690 1 0 |a ANISOTROPY 
690 1 0 |a ARTICLE 
690 1 0 |a COSMOS 
690 1 0 |a DENSITY 
690 1 0 |a MATHEMATICAL MODEL 
690 1 0 |a MICROWAVE RADIATION 
690 1 0 |a MOLECULAR INTERACTION 
700 1 |a Harari, Diego Darío 
700 1 |a Zaldarriaga, M. 
773 0 |d 2001  |g v. 63  |k n. 8  |x 05562821  |w (AR-BaUEN)CENRE-394  |t Physical Review D 
856 4 1 |u https://www.scopus.com/inward/record.uri?eid=2-s2.0-0034884072&doi=10.1103%2fPhysRevD.63.083505&partnerID=40&md5=46ce7aa0568973cb30703d82cd8b8280  |y Registro en Scopus 
856 4 0 |u https://doi.org/10.1103/PhysRevD.63.083505  |y DOI 
856 4 0 |u https://hdl.handle.net/20.500.12110/paper_05562821_v63_n8_p_Landau  |y Handle 
856 4 0 |u https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_05562821_v63_n8_p_Landau  |y Registro en la Biblioteca Digital 
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