{"id":{"repo_id":"uiuc","oai_identifier":"oai:www.ideals.illinois.edu:2142/34779"},"canonical_url":"https://search.dev.ndltd.org/etd/uiuc/oai:www.ideals.illinois.edu:2142/34779","repository":{"repo_id":"uiuc","name":"University of Illinois - Urbana-Champaign","base_url":"https://www.ideals.illinois.edu/oai-pmh"},"display":{"title":"The cosmic microwave background: gaussianity and polarization","abstract":"The Cosmic Microwave Background (CMB) is a window to the earliest parts of the universe that we can still directly see. As such, it provides excellent data for testing the currently accepted model of cosmology: an expanding Friedmann-Robertson-Walker spacetime that is statistically described by about six parameters. This dissertation presents three tools for probing that standard model of cosmology and tests them on real CMB data. The first tool checks the peaks and valleys in the CMB to make sure they statistically match those expected from a Gaussian random field, as predicted by our standard model. To do this, we analyze the one- and two-point correlation functions and compare those to simulated Gaussian skies with the same power spectrum and noise. We find some discrepancies in the WMAP data, and we can interpret these as either a detection of non-Gaussianity, or some foreground or other overlooked detail in our model of the experiment. The second tool provides a statistically sound and relatively rapid technique for estimating the polarized power spectrum of the CMB. This is the Gibbs sampler, applied to power spectra; it samples the power spectra according to either the likelihood, or Bayesian posterior probability, as desired. These samples accurately reflect the error bars on the power spectra, and a correct understanding of the error bars is essential to assuring that our standard model properly predicts the power spectra. We demonstrate this tool on the COBE data, polarized simulations, and the polarized 3-year WMAP data. The third tool we present is a method of visualizing the CMB, which is useful for displaying polarized fields in an easily understood fashion. While this does not directly test the standard model, it does provide a way to more clearly understand our data and look for possible unwanted artifacts, such as polarized Iii foregrounds. As a way to detect contaminants in the CMB data, it will be very useful when trying to test the standard model of cosmology.","abstract_html":"The Cosmic Microwave Background (CMB) is a window to the earliest parts of the universe that we can still directly see. As such, it provides excellent data for testing the currently accepted model of cosmology: an expanding Friedmann-Robertson-Walker spacetime that is statistically described by about six parameters. This dissertation presents three tools for probing that standard model of cosmology and tests them on real CMB data. The first tool checks the peaks and valleys in the CMB to make sure they statistically match those expected from a Gaussian random field, as predicted by our standard model. To do this, we analyze the one- and two-point correlation functions and compare those to simulated Gaussian skies with the same power spectrum and noise. We find some discrepancies in the WMAP data, and we can interpret these as either a detection of non-Gaussianity, or some foreground or other overlooked detail in our model of the experiment. The second tool provides a statistically sound and relatively rapid technique for estimating the polarized power spectrum of the CMB. This is the Gibbs sampler, applied to power spectra; it samples the power spectra according to either the likelihood, or Bayesian posterior probability, as desired. These samples accurately reflect the error bars on the power spectra, and a correct understanding of the error bars is essential to assuring that our standard model properly predicts the power spectra. We demonstrate this tool on the COBE data, polarized simulations, and the polarized 3-year WMAP data. The third tool we present is a method of visualizing the CMB, which is useful for displaying polarized fields in an easily understood fashion. While this does not directly test the standard model, it does provide a way to more clearly understand our data and look for possible unwanted artifacts, such as polarized Iii foregrounds. As a way to detect contaminants in the CMB data, it will be very useful when trying to test the standard model of cosmology.","abstract_has_math":false,"creators":["Larson, David Leonard"],"institution":null,"degree_name":"Ph.D.","degree_level":"Dissertation","degree_discipline":"Physics","degree_department":null,"school":null,"contributors":["Wandelt, Benjamin D."],"advisors":[],"committee_chairs":[],"committee_members":[],"year":2012,"date_issued":"2012-10-23T19:35:54Z","date_published":"2012-10-23T19:35:54Z","updated_at":"2026-07-22T22:25:31Z","subjects":["Cosmic Microwave Background (CMB)","Mathematical Properties","Non-Gaussianity","Gibbs Sampling"],"languages":["en"],"rights":["©2006 David Leonard Larson"],"rights_urls":[],"identifier_entries":[{"key":"dc:identifier","label":"Identifier","values":["5640700"],"render_values":[{"text":"5640700","href":null,"code":true}]}]},"links":{"outbound_url":"http://hdl.handle.net/2142/34779","outbound_label":"Handle","outbound_source":"dc:identifier"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor","label":"Contributor","values":["Wandelt, Benjamin D."]},{"key":"dc:creator","label":"Author","values":["Larson, David Leonard"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date","label":"Dc Date","values":["2012-10-23T19:35:54Z","10000-01-01","2006-10"]},{"key":"dc:type","label":"Dc Type","values":["Dissertation / Thesis","text"]},{"key":"thesis:degree_discipline","label":"Discipline","values":["Physics"]},{"key":"thesis:degree_level","label":"Degree Level","values":["Dissertation"]},{"key":"thesis:degree_name","label":"Degree Name","values":["Ph.D."]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["Cosmic Microwave Background (CMB)","Mathematical Properties","Non-Gaussianity","Gibbs Sampling"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language","label":"Dc Language","values":["en"]},{"key":"dc:rights","label":"Dc Rights","values":["©2006 David Leonard Larson"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier","label":"Identifier","values":["5640700","http://hdl.handle.net/2142/34779"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description","label":"Description","values":["The Cosmic Microwave Background (CMB) is a window to the earliest parts of the universe that we can still directly see. As such, it provides excellent data for testing the currently accepted model of cosmology: an expanding Friedmann-Robertson-Walker spacetime that is statistically described by about six parameters. This dissertation presents three tools for probing that standard model of cosmology and tests them on real CMB data. The first tool checks the peaks and valleys in the CMB to make sure they statistically match those expected from a Gaussian random field, as predicted by our standard model. To do this, we analyze the one- and two-point correlation functions and compare those to simulated Gaussian skies with the same power spectrum and noise. We find some discrepancies in the WMAP data, and we can interpret these as either a detection of non-Gaussianity, or some foreground or other overlooked detail in our model of the experiment. The second tool provides a statistically sound and relatively rapid technique for estimating the polarized power spectrum of the CMB. This is the Gibbs sampler, applied to power spectra; it samples the power spectra according to either the likelihood, or Bayesian posterior probability, as desired. These samples accurately reflect the error bars on the power spectra, and a correct understanding of the error bars is essential to assuring that our standard model properly predicts the power spectra. We demonstrate this tool on the COBE data, polarized simulations, and the polarized 3-year WMAP data. The third tool we present is a method of visualizing the CMB, which is useful for displaying polarized fields in an easily understood fashion. While this does not directly test the standard model, it does provide a way to more clearly understand our data and look for possible unwanted artifacts, such as polarized Iii foregrounds. As a way to detect contaminants in the CMB data, it will be very useful when trying to test the standard model of cosmology.","Submitted by Meng Tao (mengtao2@illinois.edu) on 2012-10-23T19:35:54Z No. of bitstreams: 1 Larson_David.pdf: 8526588 bytes, checksum: eeb05c698a2f3ea421358740ceb755f4 (MD5)","Made available in DSpace on 2012-10-23T19:35:54Z (GMT). No. of bitstreams: 1 Larson_David.pdf: 8526588 bytes, checksum: eeb05c698a2f3ea421358740ceb755f4 (MD5) Previous issue date: 2006-10","Item marked as restricted to the 'UIUC Users [automated]' Group (id=2) by Meng Tao (mengtao2@illinois.edu) on 2012-10-23T19:35:54Z Item is restricted indefinitely.","Restriction data tranferred 2014-07-01T11:11:11-05:00 Original Data Group with Access UIUC Users [automated] Release Date: none Reason: Post 1923. No authorization form.","Post 1923. No authorization form.","U of I Only"]},{"key":"dc:title","label":"Title","values":["The cosmic microwave background: gaussianity and polarization"]}]}],"canonical_facts":{"dc:contributor":["Wandelt, Benjamin D."],"dc:creator":["Larson, David Leonard"],"dc:date":["2012-10-23T19:35:54Z","10000-01-01","2006-10"],"dc:description":["The Cosmic Microwave Background (CMB) is a window to the earliest parts of the universe that we can still directly see. As such, it provides excellent data for testing the currently accepted model of cosmology: an expanding Friedmann-Robertson-Walker spacetime that is statistically described by about six parameters. This dissertation presents three tools for probing that standard model of cosmology and tests them on real CMB data. The first tool checks the peaks and valleys in the CMB to make sure they statistically match those expected from a Gaussian random field, as predicted by our standard model. To do this, we analyze the one- and two-point correlation functions and compare those to simulated Gaussian skies with the same power spectrum and noise. We find some discrepancies in the WMAP data, and we can interpret these as either a detection of non-Gaussianity, or some foreground or other overlooked detail in our model of the experiment. The second tool provides a statistically sound and relatively rapid technique for estimating the polarized power spectrum of the CMB. This is the Gibbs sampler, applied to power spectra; it samples the power spectra according to either the likelihood, or Bayesian posterior probability, as desired. These samples accurately reflect the error bars on the power spectra, and a correct understanding of the error bars is essential to assuring that our standard model properly predicts the power spectra. We demonstrate this tool on the COBE data, polarized simulations, and the polarized 3-year WMAP data. The third tool we present is a method of visualizing the CMB, which is useful for displaying polarized fields in an easily understood fashion. While this does not directly test the standard model, it does provide a way to more clearly understand our data and look for possible unwanted artifacts, such as polarized Iii foregrounds. As a way to detect contaminants in the CMB data, it will be very useful when trying to test the standard model of cosmology.","Submitted by Meng Tao (mengtao2@illinois.edu) on 2012-10-23T19:35:54Z No. of bitstreams: 1 Larson_David.pdf: 8526588 bytes, checksum: eeb05c698a2f3ea421358740ceb755f4 (MD5)","Made available in DSpace on 2012-10-23T19:35:54Z (GMT). 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