Oscilaciones acústicas y el espectro de potencias
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Universidad Industrial de Santander
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En el paradigma actual de la cosmología, el modelo que goza de mayor aceptación, dadas las pruebas observacionales, es conocido como ΛCDM (Cosmic Microwave Background). Este modelo está dominado principalmente por dos constituyentes acerca de los cuales la física sabe muy poco: la energía oscura, con un 70 %, es la principal componente y la causante de la expansión acelerada del Universo, mientras que la materia oscura, con un 25 % aproximadamente, es la componente principal de las estructuras auto-gravitantes. En mucho menos proporción se tiene la componente bariónica, la principal constituyente de las estrellas y por ende de la parte luminosa de las galaxias. Otras especies con menor proporción son las constituyentes relativistas, entre las cuales se tienen los neutrinos y fotones. Después del periodo de expansión acelerada del universo, denominado periodo inflacionario, debido a las altas temperaturas el plasma primordial constituido de especies relativistas fue el componente dominante en el Universo. En ese plasma la materia bariónica se encuentra ionizada y se acopla a la radiación vía dispersión de Compton. Tal plasma caliente desarrolla inestabilidades mediante la manifiestas en ondas de sonido y rarefacciones. Estas perturbaciones son soportadas hasta cuando el Universo en su expansión se ha enfriado lo suficiente para formar materia neutra. Después de esta recombinación, la radiación se desacopla formando el mar de fotones de CMB. Junto con perturbaciones métricas que aparecen por inflación en el potencial de la materia oscura, las oscilaciones del plasma quedaron impresas tanto en la temperatura de CMB como en el espectro de potencias de materia. Aquí se muestra cómo el lensamiento débil puede ser usado para estudiar estas oscilaciones.
In the current paradigm of cosmology, the ΛCDM model enjoys greater acceptance given the observational evidence. This model is domi-nated mainly by two components of which physics knows very little about them. The dark energy, with a 70% is the main component and caused the rapid universe expansion, while the dark matter, with a 25%, is the major component of the self-gravitantes structures. In less proportion then exists the baryonic component which is the main constituent of stars and there-fore part of the luminous galaxies. Other species in lower proportion are the relativists neutrinos and photons. After the period of rapid expansion, called inflation, the high temperature relativistic plasma was the dominant component in the Universe. This baryonic plasma matter is ionized and is coupled to radiation dispersal via Compton. This hot plasma develops instabilities and trigger sound waves and rarefaction. These disruptions are supported until the universe in its expansion has cooled enough to form a neutral field. After these recombination, radiation was undocked forming the sea of photons of CMB. Along with disturbances metric placed on the potential for inflation of dark matter, plasma oscillations were printed both in the temperature of CMB as in the power spectrum of matter. Here it is shown how Weak Lensing can be used to study these oscillations.
In the current paradigm of cosmology, the ΛCDM model enjoys greater acceptance given the observational evidence. This model is domi-nated mainly by two components of which physics knows very little about them. The dark energy, with a 70% is the main component and caused the rapid universe expansion, while the dark matter, with a 25%, is the major component of the self-gravitantes structures. In less proportion then exists the baryonic component which is the main constituent of stars and there-fore part of the luminous galaxies. Other species in lower proportion are the relativists neutrinos and photons. After the period of rapid expansion, called inflation, the high temperature relativistic plasma was the dominant component in the Universe. This baryonic plasma matter is ionized and is coupled to radiation dispersal via Compton. This hot plasma develops instabilities and trigger sound waves and rarefaction. These disruptions are supported until the universe in its expansion has cooled enough to form a neutral field. After these recombination, radiation was undocked forming the sea of photons of CMB. Along with disturbances metric placed on the potential for inflation of dark matter, plasma oscillations were printed both in the temperature of CMB as in the power spectrum of matter. Here it is shown how Weak Lensing can be used to study these oscillations.
Keywords
cosmology, acoustic oscillations, power-spectrum, weak lensing, Boltzmann equation, cosmología, oscilaciones acústicas, espectro de potencias, lensamiento débil, ecuación de Boltzmann