Bolometric Interferometry is a technology currently under development that will be first dedicated to the detection of B-mode polarization fluctuations in the Cosmic Microwave Background. A bolometric interferometer will have to take advantage of the wide spectral detection band of its bolometers in order to be competitive with imaging experiments. A crucial concern is that interferometers are presumed to be importantly affected by a spoiling effect known as bandwidth smearing. In this paper, we investigate how the bandwidth modifies the work principle of a bolometric interferometer and how it affects its sensitivity to the CMB angular power spectra. We obtain analytical expressions for the broadband visibilities measured by broadband heterodyne and bolometric interferometers. We investigate how the visibilities must be reconstructed in a broadband bolometric interferometer and show that this critically depends on hardware properties of the modulation phase shifters. Using an angular power spectrum estimator accounting for the bandwidth, we finally calculate the sensitivity of a broadband bolometric interferometer. A numerical simulation has been performed and confirms the analytical results. We conclude (i) that broadband bolometric interferometers allow broadband visibilities to be reconstructed whatever the kind of phase shifters used and (ii) that for dedicated B-mode bolometric interferometers, the sensitivity loss due to bandwidth smearing is quite acceptable, even for wideband instruments (a factor 2 loss for a typical 20% bandwidth experiment).
Options for Compression of radio interferometry data: lossy compression of visibilities and lossless compression of uv-visibility grids for the MHONGOOSE survey
International Centre for Radio Astronomy Research (ICRAR), University of Western Australia（西澳大利亚大学国际射电天文研究中心）；Australia Telescope National Facility, CSIRO Space & Astronomy（CSIRO空间与天文局澳大利亚望远镜国家设施）；Netherlands Institute for Radio Astronomy (ASTRON)（荷兰射电天文研究所）；Dept. of Astronomy, Univ. of Cape Town（开普敦大学天文学系）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Australian SKA Regional Centre (AusSRC), University of Western Australia（西澳大利亚大学澳大利亚SKA区域中心）
Asgard/NOTT: L-band nulling interferometry at the VLTI -- III. The mid-infrared integrated optics beam combiner for NOTT
I. Physikalisches Institut der Universität zu Köln（科隆大学第一物理研究所）；Department of Physics & Astronomy, University of California, Los Angeles（加州大学洛杉矶分校物理与天文学系）；Institute of Astronomy, KU Leuven（鲁汶大学天体物理研究所）
QUBIC: using NbSi TESs with a bolometric interferometer to characterize the polarisation of the CMB
QUBIC（Q \& U Bolometric Interferometer for Cosmology）是一个国际地面实验，专门用于测量宇宙微波背景（CMB）的偏振起伏。它是基于测热干涉测量，一个原始的检测技术相结合的免疫系统的影响与低温非相干探测器的灵敏度的干涉仪。QUBIC将部署在阿根廷萨尔塔省San Antonio de los Cobres附近的Alto Chorrillos山区。QUBIC检测链由2048个冷却至350 mK的NbSi跃迁边缘传感器（TES）组成。电压偏置的TES通过基于1 K超导量子干涉器件（SQUID）和60 K新型SiGe专用集成电路（ASIC）的时域多路复用读取，从而实现前所未有的复用（MUX）因子128。QUBIC实验目前正在实验室中进行表征，在升级到完整仪器之前，减少了探测器的数量。我将介绍这个表征阶段的最后结果，重点是探测器和读出系统。
Achieving efficient broadband spatial filtering for LIFE: status and plan
ETH Zürich（苏黎世联邦理工学院）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Sydney Institute for Astronomy, School of Physics, University of Sydney（悉尼大学物理学院天体物理研究所）；Research School of Astronomy & Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）
