Observable primordial vector modes
| dc.creator | Lewis, Antony | |
| dc.date | 2004-03-24 | |
| dc.date | 2004-06-04 | |
| dc.date.accessioned | 2026-07-07T02:12:44Z | |
| dc.date.available | 2026-07-07T02:12:44Z | |
| dc.description | Primordial vector modes describe vortical fluid perturbations in the early universe. A regular solution exists with constant non-zero radiation vorticities on super-horizon scales. Baryons are tightly coupled to the photons, and the baryon velocity only decays by an order unity factor by recombination, leading to an observable CMB anisotropy signature via the Doppler effect. There is also a large B-mode CMB polarization signal, with significant power on scales larger than l~2000. This B-mode signature is distinct from that expected from tensor modes or gravitational lensing, and makes a primordial vector to scalar mode power ratio ~10^(-6) detectable. Future observations aimed at detecting large scale B-modes from gravitational waves will also be sensitive to regular vector modes at around this level. | |
| dc.description | Changes and corrections to match PRD accepted version. Additional material at http://cosmologist.info/notes/vectors/ | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0403583 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0403583 | |
| dc.identifier | Phys.Rev. D70 (2004) 043518 | |
| dc.identifier | doi:10.1103/PhysRevD.70.043518 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/7558 | |
| dc.subject | Astrophysics | |
| dc.subject | High Energy Physics - Phenomenology | |
| dc.title | Observable primordial vector modes | |
| dc.type | text |