| Issue |
EPJ Web Conf.
Volume 293, 2024
mm Universe 2023 - Observing the Universe at mm Wavelengths
|
|
|---|---|---|
| Article Number | 00029 | |
| Number of page(s) | 6 | |
| DOI | https://doi.org/10.1051/epjconf/202429300029 | |
| Published online | 28 March 2024 | |
https://doi.org/10.1051/epjconf/202429300029
The advantage of Bolometric Interferometry for controlling Galactic foreground contamination in CMB primordial B-modes measurements
1 Università degli studi di Milano, Italy
2 INFN sezione di Milano, Milano, Italy
3 Université Paris Cité, CNRS, Astroparticule et Cosmologie, Paris, France
4 Université PSL, Observatoire de Paris, AstroParticule et Cosmologie, Paris, France
5 Waterloo Centre for Astrophysics, University of Waterloo, Waterloo, Canada
6 Department of Physics and Astronomy, University of Waterloo, Waterloo, Canada
7 Università di Roma - La Sapienza, Italy
8 Università di Milano – Bicocca, Italy
9 Instituto Argentino de Radioastronomía, Buenos Aires, Argentina
10 Consejo Nacional de Investigaciones Científicas y Técnicas, Ciudad de Buenos Aires, Argentina
11 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina
* e-mail: elenia.manzan@unimi.it
Published online: 28 March 2024
In the quest for the faint primordial B-mode polarization of the Cosmic Microwave Background, three are the key requirements for any present or future experiment: an utmost sensitivity, excellent control over instrumental systematic effects and over Galactic foreground contamination.
Bolometric Interferometry (BI) is a novel technique that matches them all by combining the sensitivity of bolometric detectors, the control of instrumental systematics from interferometry and a software-based, tunable, in-band spectral resolution due to its ability to perform band-splitting during data analysis (spectral imaging).
In this paper, we investigate how the spectral imaging capability of BI can help in detecting residual contamination in case an over-simplified model of foreground emission is assumed in the analysis. To mimic this situation, we focus on the next generation of ground-based CMB experiment, CMB-S4, and compare its anticipated sensitivities, frequency and sky coverage with a hypothetical version of the same experiment based on BI, CMB-S4/BI, assuming that lineof-sight (LOS) frequency decorrelation is present in dust emission but is not accounted for during component separation.
We show results from a Monte-Carlo analysis based on a parametric component separation method (FGBuster), highlighting how BI has the potential to diagnose the presence of foreground residuals in estimates of the tensor-to-scalar ratio r in the case of unaccounted Galactic dust LOS frequency decorrelation.
© The Authors, published by EDP Sciences, 2024
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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