The Einstein polarization interferometer for cosmology (EPIC) and the millimeter-wave bolometric interferometer (MBI)

Timbie, Peter; Tucker, Gregory S.; Ali, Shehzad; Bierman, E. M.; Bunn, Emory F.; Calderón, Carolina; Gault, A.; Hyland, P.; Keating, Brian; Kim, J.; Korotkov, Andrei; Malu, Siddharth; Mauskopf, Philip Daniel; Murphy, John A.; O'Sullivan, Créidhe M.; Piccirillo, L.; Wandelt, B. D.

doi:10.1016/j.newar.2006.09.031

Cited by 25 publications

(20 citation statements)

References 28 publications

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“…The realization of a beam combiner is an issue in itself that will not be assessed in the present article. As an example, this can be achieved using a Butler combiner (Butler 1961, Dall'Omo 2003 or with a quasi-optical Fizeau combiner such as the one used for the MBI instrument (Timbie et al 2006). All of these devices are such that the 2N h input channels result after passing through the beam combiner in N out output channels that are linear combinations of the input ones.…”

Section: Beam Combinermentioning

confidence: 99%

“…As was said before there are two main designs for the beam combiner: Butler combiner (Dall'Omo 2003) or quasi optical combiner (Timbie et al 2006). Without going into details, let us say that identical phase shifts for equivalent baselines are naturally obtained for the quasi optical combiner, and are achieved through an adequate wiring for the Butler combiner.…”

Section: C) Beam Combiner Phase Differencementioning

confidence: 99%

“…A new concept of an instrument called a "bolometric interferometer" is currently under developement (MBI Timbie et al 2006, BRAIN Polenta et al 2003Charlassier et al 2008). In such an instrument, the interference fringes are "imaged" using bolometers.…”

Section: Introductionmentioning

confidence: 99%

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An efficient phase-shifting scheme for bolometric additive interferometry

Charlassier¹,

Hamilton²,

Bréelle³

et al. 2009

A&A

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Context. Most upcoming CMB polarization experiments will use direct imaging to search for primordial gravitational waves through the B-modes. Bolometric interferometry is an appealing alternative to direct imaging that combines the advantages of interferometry in terms of systematic effects handling and those of bolometric detectors in terms of sensitivity. Aims. We calculate the signal from a bolometric interferometer in order to investigate its sensitivity to the Stokes parameters paying particular attention to the choice of the phase shifting scheme applied to the input channels in order to modulate the signal. Methods. The signal is expressed as a linear combination of the Stokes parameter visibilities whose coefficients are functions of the phase shifts. Results. We show that the signal to noise ratio on the reconstructed visibilities can be maximized provided the fact that the phase shifting scheme is chosen in a particular way called "coherent summation of equivalent baselines". As a result, a bolometric interferometer is competitive with an imager having the same number of horns, but only if the coherent summation of equivalent baselines is performed. We confirm our calculations using a Monte-Carlo simulation. We also discuss the impact of the uncertainties on the relative calibration between bolometers and propose a way to avoid this systematic effect.

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Section: Beam Combinermentioning

confidence: 99%

Section: C) Beam Combiner Phase Differencementioning

confidence: 99%

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An efficient phase-shifting scheme for bolometric additive interferometry

Charlassier¹,

Hamilton²,

Bréelle³

et al. 2009

A&A

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show abstract

“…This was first detected by the Degree Angular Scale Interferometer (DASI) experiment [2] in 2002. Accurate measurements of this polarization are expected to lead to tighter constraints on cosmological parameters describing the density, composition and expansion rate of the universe and the latest generation of experiments, such as QUaD [3], PLANK [4] and MBI [5], are only now approaching the sensitivity needed to carry out these measurements. CMB polarization is generally decomposed into two coordinate-independent components, called E-and B-modes.…”

Section: Polarization and The Cosmic Microwave Backgroundmentioning

confidence: 99%

Modeling the quasi-optical performance of CMB astronomical interferometers

Curran¹,

Grądziel

O'Sullivan

et al. 2008

SPIE Proceedings

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The Millimeter-Wave Bolometric Interferometer (MBI) is a ground-based instrument designed to measure the polarization anisotropies of the Cosmic Microwave Background (CMB) and contains a number of quasi-optical components, including a complex back-to-back system of corrugated feed-horn antennas. In this paper we use MBI as an example to demonstrate the existing modeling techniques and as a focus to develop extended modeling capabilities. The software we use to model this system targets the millimeter and sub-millimeter region of the electromagnetic spectrum and has been extended to efficiently model the performance of back-to-back corrugated horns embedded in larger optical systems. This allows the calculation of the coupling of radiation from the sky to the detector array through a back-to-back horn feed system.

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“…Because the B-mode signal is expected to be very faint, control of systematic errors is of paramount importance. An argument can be made (Timbie et al 2006, Bunn 2007 that interferometers provide better control of systematics than imaging telescopes. This is one of the reasons that, for instance, the QUBIC collaboration (Ghribi et al 2013) is constructing an instrument based on the novel approach of bolometric interferometry.…”

mentioning

confidence: 99%

Simulation of the analysis of interferometric microwave background polarization data

Bunn¹,

Karakci

Sutter

et al. 2014

Proc. IAU

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We present results from an end-to-end simulation pipeline of interferometric observations of cosmic microwave background polarization. We use both maximum-likelihood and Gibbs sampling techniques to estimate the power spectrum. In addition, we use Gibbs sampling for image reconstruction from interferometric visibilities. The results indicate the level to which various systematic errors (e.g., pointing errors, gain errors, beam shape errors, cross polarization) must be controlled in order to successfully detect and characterize primordial B modes and achieve other scientific goals. In addition, we show that Gibbs sampling is an effective method of image reconstruction for interferometric data in other astrophysical contexts.

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The Einstein polarization interferometer for cosmology (EPIC) and the millimeter-wave bolometric interferometer (MBI)

Cited by 25 publications

References 28 publications

An efficient phase-shifting scheme for bolometric additive interferometry

An efficient phase-shifting scheme for bolometric additive interferometry

Modeling the quasi-optical performance of CMB astronomical interferometers

Simulation of the analysis of interferometric microwave background polarization data

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