论文标题

QUBIC I:概述和科学图

QUBIC I: Overview and ScienceProgram

论文作者

Hamilton, J. -Ch., Mousset, L., Battistelli, E. S., Bigot-Sazy, M. -A., Chanial, P., Charlassier, R., D'Alessandro, G., de Bernardis, P., De Petris, M., Lerena, M. M. Gamboa, Grandsire, L., Lau, S., Marnieros, S., Masi, S., Mennella, A., O'Sullivan, C., Piat, M., Riccardi, G., Scóccola, C., Stolpovskiy, M., Tartari, A., Torchinsky, S. A., Voisin, F., Zannoni, M., Ade, P., Alberro, J. G., Almela, A., Amico, G., Arnaldi, L. H., Auguste, D., Aumont, J., Azzoni, S., Banfi, S., Bélier, B., Baù, A., Bennett, D., Bergé, L., Bernard, J. -Ph., Bersanelli, M., Bonaparte, J., Bonis, J., Bunn, E., Burke, D., Buzi, D., Cavaliere, F., Chapron, C., Cerutti, A. C. Cobos, Columbro, F., Coppolecchia, A., De Gasperis, G., De Leo, M., Dheilly, S., Duca, C., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Ferreyro, L. P., Fracchia, D., Franceschet, C., Ganga, K. M., García, B., Redondo, M. E. García, Gaspard, M., Gayer, D., Gervasi, M., Giard, M., Gilles, V., Giraud-Heraud, Y., Berisso, M. Gómez, González, M., Gradziel, M., Hampel, M. R., Harari, D., Henrot-Versillé, S., Incardona, F., Jules, E., Kaplan, J., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Maffei, B., Marty, W., Mattei, A., May, A., McCulloch, M., Mele, L., Melo, D., Montier, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Nati, F., Olivieri, E., Oriol, C., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perciballi, M., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Platino, M., Polenta, G., Prêle, D., Puddu, R., Rambaud, D., Ringegni, P., Romero, G. E., Rasztocky, E., Salum, J. M., Schillaci, A., Scully, S., Spinelli, S., Stankowiak, G., Supanitsky, A. D., Thermeau, J. -P., Timbie, P., Tomasi, M., Tucker, C., Tucker, G., Viganò, D., Vittorio, N., Wicek, F., Wright, M., Zullo, A.

论文摘要

Q $ \&$ U的射流干涉仪用于宇宙学(Qubic)是一种新型的偏振计,用于测量宇宙微波背景(CMB)的B模式极化,这是观察宇宙学的主要挑战之一。该信号有望达到数十万个NK的顺序,容易产生仪器系统效应,并受到各种天体物理前景污染,这些前景只能通过多核电观测来控制。 Qubic旨在通过一种新的方法来解决这些观察性问题,该方法将干涉仪的优势在控制仪器系统效应的方面与横梁探测器的宽带宽带敏感性有关。 Qubic合成光束具有频率依赖性的形状,可以在仪器的两个物理带(150和220 GHz)内生成CMB极化图的地图。这些功能使Qubic与其他乐器互补,并特别适合表征和消除银河前景污染。在本文中,我们首先概述了Qubic仪器设计,校准运动的主要结果,并介绍了Qubic的科学计划,不仅包括测量原始B模型,还包括对银河前景的测量。我们对典型的观察和测量进行了预测:在天空上整合了三年的整合,并假设我们在阿根廷的网站上可以完美的前景清除以及稳定的大气条件,我们的模拟表明,我们可以实现对有效的张量表与量表比率的统计敏感性(包括原始和前景B-Modes)(包括原始的B-Modes)$队标= 0.0015 $。

The Q $\&$ U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) $σ(r)=0.015$.

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