SPIDER: a balloon-borne CMB polarimeter for large angular scales

Filippini, J. P.; Ade, Peter A. R.; Amiri, M.; Benton, S. J.; Bihary, R.; Bock, J. J.; Bond, J. R.; Bonetti, J. A.; Bryan, Sean; Burger, B.; Chiang, H. C.; Contaldi, C. R.; Crill, B. P.; Doré, O.; Farhang, M.; Fissel, Laura M.; Gandilo, N. N.; Golwala, S. R.; Gudmundsson, J. E.; Halpern, M.; Hasselfield, Matthew; Hilton, G. C.; Holmes, W. A.; Hristov, V. V.; Irwin, K. D.; Jones, W. C.; Kuo, C. L.; MacTavish, C. J.; Mason, P.; Montroy, T. E.; Morford, T. A.; Netterfield, C. B.; O'Dea, D.; Rahlin, A.; Reintsema, C. D.; Ruhl, J. E.; Runyan, M. C.; Schenker, Matthew A.; Shariff, J. A.; Soler, J. D.; Trangsrud, A.; Tucker, C.; Tucker, R. S.; Turner, Anthony

doi:10.1117/12.857720

Cited by 63 publications

(38 citation statements)

References 39 publications

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“…An all-sky cosmic variance-limited measurement to much smaller scales is feasible with current technology and several experimental designs have been proposed [330,332,333]. Although none of the former have been selected for funding to date, ground based and sub-orbital CMB polarisation measurements (which either by themselves [334] or taken in combination [335][336][337][338][339][340][341][342][343][344][345][346][347][348], promise almost full sky coverage) remain one of the most promising future avenues for the detection of features, especially on the largest scales.…”

Section: Cmb Polarisation Anisotropiesmentioning

confidence: 99%

Features and new physical scales in primordial observables: Theory and observation

Chluba

Hamann

Patil

2015

Int. J. Mod. Phys. D

212

233

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June 22, 20152 All cosmological observations to date are consistent with adiabatic, Gaussian and nearly scale invariant initial conditions. These findings provide strong evidence for a particular symmetry breaking pattern in the very early universe (with a close to vanishing order parameter, ), widely accepted as conforming to the predictions of the simplest realizations of the inflationary paradigm. However, given that our observations are only privy to perturbations, in inferring something about the background that gave rise to them, it should be clear that many different underlying constructions project onto the same set of cosmological observables. Features in the primordial correlation functions, if present, would offer a unique and discriminating window onto the parent theory in which the mechanism that generated the initial conditions is embedded. In certain contexts, simple linear response theory allows us to infer new characteristic scales from the presence of features that can break the aforementioned degeneracies among different background models, and in some cases can even offer a limited spectroscopy of the heavier degrees of freedom that couple to the inflaton. In this review, we offer a pedagogical survey of the diverse, theoretically well grounded mechanisms which can imprint features into primordial correlation functions in addition to reviewing the techniques one can employ to probe observations. These observations include cosmic microwave background anisotropies and spectral distortions as well as the matter two and three point functions as inferred from large-scale structure and potentially, 21 cm surveys.

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Section: Cmb Polarisation Anisotropiesmentioning

confidence: 99%

Features and new physical scales in primordial observables: Theory and observation

Chluba

Hamann

Patil

2015

Int. J. Mod. Phys. D

212

233

View full text Add to dashboard Cite

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“…1). No other large-area higher-sensitivity observations are underway or planned in this wavelength range, with this resolution, and with a survey optimized to complement ground-based CMB observatories [9,10,11]. Ground-based observations are underway or planned at 220 GHz, where the dust is several times brighter than at 150 GHz and can be used as a foreground monitor, including by the Keck Array [12], Advanced ACTPol [13], Simons Array [14], and SPT-3G [15] projects (Fig.…”

Section: Cmb B-mode Polarization and Foregroundsmentioning

confidence: 99%

BFORE: The B-mode Foreground Experiment

et al. 2015

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The B-mode Foreground Experiment (BFORE) is a proposed NASA balloon project designed to make optimal use of the sub-orbital platform by concentrating on three dust foreground bands (270, 350, and 600 GHz) that complement ground-based cosmic microwave background (CMB) programs. BFORE will survey ∼1/4 of the sky with 1.7 -3.7 arcminute resolution, enabling precise characterization of the Galactic dust that now limits constraints on inflation from CMB B-mode polarization measurements. In addition, BFORE's combination of frequency coverage, large survey area, and angular resolution enables science far beyond the critical goal of measuring foregrounds. BFORE will constrain the velocities of thousands of galaxy clusters, provide a new window on the cosmic infrared background, and probe magnetic fields in the interstellar medium. We review the BFORE science case, timeline, and instrument design, which is based on a compact off-axis telescope coupled to >10,000 superconducting detectors.

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“…A number of suborbital missions are targeting the B-mode spectrum at the recombination peak, 5,6 but…”

Section: +007mentioning

confidence: 99%

The Primordial Inflation Polarization Explorer (PIPER)

et al. 2016

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The Primordial Inflation Polarization Explorer (Piper) is a balloon-borne cosmic microwave background (CMB) polarimeter designed to search for evidence of inflation by measuring the large-angular scale CMB polarization signal. Bicep2 recently reported a detection of B-mode power corresponding to the tensor-to-scalar ratio r = 0.2 on ∼ 2 degree scales. If the Bicep2 signal is caused by inflationary gravitational waves (IGWs), then there should be a corresponding increase in B-mode power on angular scales larger than 18 degrees. Piper is currently the only suborbital instrument capable of fully testing and extending the Bicep2 results by measuring the B-mode power spectrum on angular scales θ =∼ 0.6• to 90• , covering both the reionization bump and recombination peak, with sensitivity to measure the tensor-to-scalar ratio down to r = 0.007, and four frequency bands to distinguish foregrounds. Piper will accomplish this by mapping 85% of the sky in four frequency bands (200, 270, 350, 600 GHz) over a series of 8 conventional balloon flights from the northern and southern hemispheres. The instrument has background-limited sensitivity provided by fully cryogenic (1.5 K) optics focusing the sky signal onto four 32×40-pixel arrays of time-domain multiplexed Transition-Edge Sensor (TES) bolometers held at 140 mK. Polarization sensitivity and systematic control are provided by front-end Variabledelay Polarization Modulators (VPMs), which rapidly modulate only the polarized sky signal at 3 Hz and allow Piper to instantaneously measure the full Stokes vector (I, Q, U, V ) for each pointing. We describe the Piper instrument and progress towards its first flight. Keywords: polarimeter, cosmic microwave background, bolometerSend correspondence to Justin Lazear: jlazear@pha.jhu.edu Copyright 2014 Society of Photo Optical Instrumentation Engineers. One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited.arXiv:1407.2584v1 [astro-ph.IM] 9 Jul 2014 Figure 1. The CMB anisotropy polarization map may be decomposed into curl-free even-parity E-modes and divergencefree odd-parity B-modes. Primordial B-modes are only created by tensor perturbations (inflationary gravitational waves).

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SPIDER: a balloon-borne CMB polarimeter for large angular scales

Cited by 63 publications

References 39 publications

Features and new physical scales in primordial observables: Theory and observation

Features and new physical scales in primordial observables: Theory and observation

BFORE: The B-mode Foreground Experiment

The Primordial Inflation Polarization Explorer (PIPER)

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