关于通货膨胀，WMAP和SDSS到底说明了什么？
What do WMAP and SDSS really tell about inflation?
摘要：
我们从WMAP的3年数据中结合Sloan亮红星系巡天得到了哈勃函数H（phi）和暴胀势V（phi）的新约束（SDSS-LRG），使用一种新的方法，该方法似乎比最近的大多数文献更通用，保守和模型无关，因为它既不依赖于慢滚近似，也不依赖于超出可观测e-折叠范围的势能的任何外推方案，也不依赖于关于暴胀子速度的初始条件的附加假设。最后一个特征代表了这项工作的主要改进，并且通过在V（phi）之前重建H（phi）而成为可能。我们的结果仅依赖于这样的假设，即在对应于~ 10个e-折叠的可观测范围内，暴胀没有中断，并且函数H（phi）足够光滑，可以在一阶、二阶或三阶进行泰勒展开。我们的结论是，由数据所允许的各种潜力仍然很大。然而，很明显，前两个慢滚参数确实很小，而超过它们的慢滚扩展的有效性还没有建立。
英文摘要：
We derive new constraints on the Hubble function H(phi) and subsequently on the inflationary potential V(phi) from WMAP 3-year data combined with the Sloan Luminous Red Galaxy survey (SDSS-LRG), using a new methodology which appears to be more generic, conservative and model-independent than in most of the recent literature, since it depends neither on the slow-roll approximation, nor on any extrapolation scheme for the potential beyond the observable e-fold range, nor on additional assumptions about initial conditions for the inflaton velocity. This last feature represents the main improvement of this work, and is made possible by the reconstruction of H(phi) prior to V(phi). Our results only rely on the assumption that within the observable range, corresponding to ~ 10 e-folds, inflation is not interrupted and the function H(phi) is smooth enough for being Taylor-expanded at order one, two or three. We conclude that the variety of potentials allowed by the data is still large. However, it is clear that the first two slow-roll parameters are really small while the validity of the slow-roll expansion beyond them is not established.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
