Towards a cosmological neutrino mass detection
Future cosmological measurements should enable the sum of neutrino masses to be determined indirectly through their effects on the expansion rate of the Universe and the clustering of matter. We consider prospects for the gravitationally lensed cosmic microwave background (CMB) anisotropies and bary...
| Main Authors: | , , , , |
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| Format: | Journal article |
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American Physical Society
2015
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| _version_ | 1826299012450353152 |
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| author | Allison, R Caucal, P Calabrese, E Dunkley, J Louis, T |
| author_facet | Allison, R Caucal, P Calabrese, E Dunkley, J Louis, T |
| author_sort | Allison, R |
| collection | OXFORD |
| description | Future cosmological measurements should enable the sum of neutrino masses to be determined indirectly through their effects on the expansion rate of the Universe and the clustering of matter. We consider prospects for the gravitationally lensed cosmic microwave background (CMB) anisotropies and baryon acoustic oscillations (BAOs) in the galaxy distribution, examining how the projected uncertainty of ≈15 meV on the neutrino mass sum (a 4σ detection of the minimal mass) might be reached over the next decade. The current 1σ uncertainty of ≈103 meV (Planck-2015 þ BAO-15) will be improved by upcoming “Stage-3” (S3) CMB experiments (S3 þ BAO-15∶ 44 meV), then upcoming BAO measurements (S3 þ DESI∶ 22 meV), and planned next-generation “Stage 4” (S4) CMB experiments (S4 þ DESI∶ 15–19 meV, depending on angular range). An improved optical depth measurement is important: the projected neutrino mass uncertainty increases to 26 meV if S4 is limited to l > 20 and combined with current large-scale polarization data. Looking beyond ΛCDM, including curvature uncertainty increases the forecast mass error by ≈50% for S4 þ DESI, and more than doubles the error with a two-parameter dark-energy equation of state. Complementary low-redshift probes including galaxy lensing will play a role in distinguishing between massive neutrinos and a departure from a w ¼ −1, flat geometry. |
| first_indexed | 2024-03-07T04:55:26Z |
| format | Journal article |
| id | oxford-uuid:d67280ea-ea28-4db3-80f0-3f44c3859670 |
| institution | University of Oxford |
| last_indexed | 2024-03-07T04:55:26Z |
| publishDate | 2015 |
| publisher | American Physical Society |
| record_format | dspace |
| spelling | oxford-uuid:d67280ea-ea28-4db3-80f0-3f44c38596702022-03-27T08:33:35ZTowards a cosmological neutrino mass detectionJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:d67280ea-ea28-4db3-80f0-3f44c3859670Symplectic Elements at OxfordAmerican Physical Society2015Allison, RCaucal, PCalabrese, EDunkley, JLouis, TFuture cosmological measurements should enable the sum of neutrino masses to be determined indirectly through their effects on the expansion rate of the Universe and the clustering of matter. We consider prospects for the gravitationally lensed cosmic microwave background (CMB) anisotropies and baryon acoustic oscillations (BAOs) in the galaxy distribution, examining how the projected uncertainty of ≈15 meV on the neutrino mass sum (a 4σ detection of the minimal mass) might be reached over the next decade. The current 1σ uncertainty of ≈103 meV (Planck-2015 þ BAO-15) will be improved by upcoming “Stage-3” (S3) CMB experiments (S3 þ BAO-15∶ 44 meV), then upcoming BAO measurements (S3 þ DESI∶ 22 meV), and planned next-generation “Stage 4” (S4) CMB experiments (S4 þ DESI∶ 15–19 meV, depending on angular range). An improved optical depth measurement is important: the projected neutrino mass uncertainty increases to 26 meV if S4 is limited to l > 20 and combined with current large-scale polarization data. Looking beyond ΛCDM, including curvature uncertainty increases the forecast mass error by ≈50% for S4 þ DESI, and more than doubles the error with a two-parameter dark-energy equation of state. Complementary low-redshift probes including galaxy lensing will play a role in distinguishing between massive neutrinos and a departure from a w ¼ −1, flat geometry. |
| spellingShingle | Allison, R Caucal, P Calabrese, E Dunkley, J Louis, T Towards a cosmological neutrino mass detection |
| title | Towards a cosmological neutrino mass detection |
| title_full | Towards a cosmological neutrino mass detection |
| title_fullStr | Towards a cosmological neutrino mass detection |
| title_full_unstemmed | Towards a cosmological neutrino mass detection |
| title_short | Towards a cosmological neutrino mass detection |
| title_sort | towards a cosmological neutrino mass detection |
| work_keys_str_mv | AT allisonr towardsacosmologicalneutrinomassdetection AT caucalp towardsacosmologicalneutrinomassdetection AT calabresee towardsacosmologicalneutrinomassdetection AT dunkleyj towardsacosmologicalneutrinomassdetection AT louist towardsacosmologicalneutrinomassdetection |