Planck 2018 结果。V. CMB 功率谱与似然函数
宇宙学与河外天体物理
2020-09-16 v2
摘要
本文描述了 2018 年 Planck CMB 似然函数，采用与 2015 年类似的混合方法，在低和多极矩与高多极矩处采用不同近似，并实现了若干方法与分析上的改进。借助更真实的模拟，以及对系统误差更好的修正和建模，我们现在可以充分利用高频仪器（High Frequency Instrument）的偏振数据。低多极矩 100×143 GHz EE 交叉谱将再电离光学深度参数 的限制提高到优于 15%（与其他低和多 似然函数联合时）。我们还基于低频仪器（Low Frequency Instrument）数据更新了 2015 年基线低 联合 TEB 似然函数，其给出的 限制较弱。在高多极矩处，更好的温度到偏振泄漏模型以及偏振通道有效定标（偏振效率或 PE）的修正使我们能够充分利用偏振谱，与仅用 TT 的限制相比，CDM 参数的限制改善了 20% 至 30%。对偏振建模的检验显示出良好的一致性，但存在一些残余的建模不确定性，其中 PE 建模的精度是主要限制。利用我们的各种检验、模拟以及不同高 实现之间的比较，我们估计结果的一致性优于 0.5 水平。先前已存在的微小异常（如 <800 与 >800 参数之间的差异，或对 峰值更多平滑的偏好）被证明由 TT 功率谱驱动，并且不因加入偏振而有显著改变。总体而言，Planck 遗留 CMB 似然函数为约束宇宙学模型提供了稳健工具，并可作为未来 CMB 观测的参考。（节略）
引用
@article{arxiv.1907.12875,
title = {Planck 2018 results. V. CMB power spectra and likelihoods},
author = {Planck Collaboration and N. Aghanim and Y. Akrami and M. Ashdown and J. Aumont and C. Baccigalupi and M. Ballardini and A. J. Banday and R. B. Barreiro and N. Bartolo and S. Basak and K. Benabed and J. -P. Bernard and M. Bersanelli and P. Bielewicz and J. J. Bock and J. R. Bond and J. Borrill and F. R. Bouchet and F. Boulanger and M. Bucher and C. Burigana and R. C. Butler and E. Calabrese and J. -F. Cardoso and J. Carron and B. Casaponsa and A. Challinor and H. C. Chiang and L. P. L. Colombo and C. Combet and B. P. Crill and F. Cuttaia and P. de Bernardis and A. de Rosa and G. de Zotti and J. Delabrouille and J. -M. Delouis and E. Di Valentino and J. M. Diego and O. Doré and M. Douspis and A. Ducout and X. Dupac and S. Dusini and G. Efstathiou and F. Elsner and T. A. Enßlin and H. K. Eriksen and Y. Fantaye and R. Fernandez-Cobos and F. Finelli and M. Frailis and A. A. Fraisse and E. Franceschi and A. Frolov and S. Galeotta and S. Galli and K. Ganga and R. T. Génova-Santos and M. Gerbino and T. Ghosh and Y. Giraud-Héraud and J. González-Nuevo and K. M. Górski and S. Gratton and A. Gruppuso and J. E. Gudmundsson and J. Hamann and W. Handley and F. K. Hansen and D. Herranz and E. Hivon and Z. Huang and A. H. Jaffe and W. C. Jones and E. Keihänen and R. Keskitalo and K. Kiiveri and J. Kim and T. S. Kisner and N. Krachmalnicoff and M. Kunz and H. Kurki-Suonio and G. Lagache and J. -M. Lamarre and A. Lasenby and M. Lattanzi and C. R. Lawrence and M. Le Jeune and F. Levrier and A. Lewis and M. Liguori and P. B. Lilje and M. Lilley and V. Lindholm and M. López-Caniego and P. M. Lubin and Y. -Z. Ma and J. F. Macías-Pérez and G. Maggio and D. Maino and N. Mandolesi and A. Mangilli and A. Marcos-Caballero and M. Maris and P. G. Martin and E. Martínez-González and S. Matarrese and N. Mauri and J. D. McEwen and P. R. Meinhold and A. Melchiorri and A. Mennella and M. Migliaccio and M. Millea and M. -A. Miville-Deschênes and D. Molinari and A. Moneti and L. Montier and G. Morgante and A. Moss and P. Natoli and H. U. Nørgaard-Nielsen and L. Pagano and D. Paoletti and B. Partridge and G. Patanchon and H. V. Peiris and F. Perrotta and V. Pettorino and F. Piacentini and G. Polenta and J. -L. Puget and J. P. Rachen and M. Reinecke and M. Remazeilles and A. Renzi and G. Rocha and C. Rosset and G. Roudier and J. A. Rubiño-Martín and B. Ruiz-Granados and L. Salvati and M. Sandri and M. Savelainen and D. Scott and E. P. S. Shellard and C. Sirignano and G. Sirri and L. D. Spencer and R. Sunyaev and A. -S. Suur-Uski and J. A. Tauber and D. Tavagnacco and M. Tenti and L. Toffolatti and M. Tomasi and T. Trombetti and J. Valiviita and B. Van Tent and P. Vielva and F. Villa and N. Vittorio and B. D. Wandelt and I. K. Wehus and A. Zacchei and A. Zonca},
journal= {arXiv preprint arXiv:1907.12875},
year = {2020}
}
备注
Revised to match version published in Astronomy & Astrophysics