标题： QUBIC I：概述和科学计划 显示英文标题

标题： QUBIC I: Overview and ScienceProgram

摘要： QUBIC（宇宙学用Q $\&$ U光度干涉仪）是一种新型的偏振计，专为测量宇宙微波背景（CMB）的B模式偏振而优化，这是观测宇宙学的主要挑战之一。 信号预计在几十分之一纳开尔文量级，容易受到仪器系统效应的影响，并且被各种天体物理前景污染，这些只能通过多色观测来控制。 QUBIC设计采用一种新方法，结合了干涉测量在控制仪器系统效应方面的优势以及光度探测器在宽频带、背景受限灵敏度方面的优势，以解决这些观测问题。 QUBIC合成光束的形状随频率变化，使其能够在仪器的两个物理波段（150和220 GHz）内产生多个子波段的CMB偏振图。 这些特性使QUBIC与其他仪器互补，并特别适合表征和去除银河系前景污染。 在本文中，作为八篇系列文章的第一篇，我们概述了QUBIC仪器设计、校准活动的主要结果，并介绍了QUBIC的科学计划，包括不仅测量原初B模式，还包括测量银河系前景。 我们给出了典型观测和测量的预测：在阿根廷站点假设完美的前景去除以及稳定的天气条件下，经过三年的天空积分，我们的模拟表明，我们可以实现对有效张量-标量比（包括原初和前景B模式）的统计灵敏度 $\sigma(r)=0.015$。 显示英文摘要

摘要： 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) $\sigma(r)=0.015$.