Optical design of PICO: a concept for a space mission to probe inflation and cosmic origins

Young, Karl; Alvarez, Marcelo A.; Battaglia, Nicholas; Bock, J. J.; Borrill, J.; Chuss, David T.; Crill, B. P.; Delabrouille, J.; Devlin, Mark J.; Fissel, Laura M.; Flauger, Raphael; Green, Daniel; Górski, K. M.; Hanany, Shaul; Hills, R. E.; Hubmayr, Johannes; Johnson, Bradley R.; Jones, W. C.; Knox, L.; Kogut, A.; Lawrence, Charles; Matsumura, Tomotake; McGuire, J. E.; McMahon, Jeff; O’Brient, R.; Pryke, C.; Sutin, Brian M.; Tan, Xin Zhi; Trangsrud, A.; Wen, Qi; Zotti, G. de

doi:10.1117/12.2309421

Cited by 17 publications

(17 citation statements)

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“…Both satellites would map hundreds of square degrees, with ∼10 ′′ , at 100 and 250 µm, respectively. A satellite targeting the entire sky, the Probe for Inflation and Cosmic Origins (PICO), has also been proposed (Sutin et al, 2018;Young et al, 2018). PICO would provide coverage in 10 frequency bands between 375 µm to 2 mm, with a best resolution of 1.1 ′ .…”

Section: Future Polarimetersmentioning

confidence: 99%

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Pattle

Fissel

2019

Front. Astron. Space Sci.

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Observations of star-forming regions by the current and upcoming generation of submillimeter polarimeters will shed new light on the evolution of magnetic fields over the cloud-to-core size scales involved in the early stages of the star formation process. Recent wide-area and high-sensitivity polarization observations have drawn attention to the challenges of modeling magnetic field structure of star forming regions, due to variations in dust polarization properties in the interstellar medium. However, these observations also for the first time provide sufficient information to begin to break the degeneracy between polarization efficiency variations and depolarization due to magnetic field sub-beam structure, and thus to accurately infer magnetic field properties in the star-forming interstellar medium. In this article we discuss submillimeter and far-infrared polarization observations of star-forming regions made with single-dish instruments. We summarize past, present and forthcoming single-dish instrumentation, and discuss techniques which have been developed or proposed to interpret polarization observations, both in order to infer the morphology and strength of the magnetic field, and in order to determine the environments in which dust polarization observations reliably trace the magnetic field. We review recent polarimetric observations of molecular clouds, filaments, and starless and protostellar cores, and discuss how the application of the full range of modern analysis techniques to recent observations will advance our understanding of the role played by the magnetic field in the early stages of star formation.

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Section: Future Polarimetersmentioning

confidence: 99%

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Pattle

Fissel

2019

Front. Astron. Space Sci.

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“…The bias in the value of r found from our simulations are less than 0.5-σ for the CMB missions such as Simons Observatory (Aguirre et al 2018) and LiteBIRD (Matsumura et al 2013) and hence are not going to contaminate the value of primordial gravitational wave signal severely. However, for the proposed CMB experiments with σ(r) 5 × 10 −4 such as CMB-S4 (Abazajian et al 2016), CMB-Bharat 7 and PICO (Young et al 2018;Hanany et al 2019), the bias in the value of r can be greater than 1-σ as shown in Figure 5. The amount of bias varies with the model of reionization and may be difficult to estimate this bias robustly from CMB polarization data alone.…”

Section: Resultsmentioning

confidence: 98%

“…A possible source of secondary anisotropy is the B-mode polarization arising from the patchy electron distribution during reionization. This can potentially contaminate the recombination bump of the B-mode polarization leading to a bias in the inferred value of r. Hence an accurate and reliable computation of the signal arising from reionization is crucial for the upcoming experiments that aim to detect the primordial B-modes (Matsumura et al 2013;Aguirre et al 2018;Abazajian et al 2016;Young et al 2018). As per the current understanding, reionization is an inhomogeneous and complex process (Mesinger & Furlanetto 2007;Zahn et al 2007;Choudhury et al 2009;Mitra et al 2018) which depends on various astrophysical processes related to early galaxy formation.…”

Section: Introductionmentioning

confidence: 99%

“…By using the power spectrum of the electron density from the semi-numerical and analytical method, we estimate the CMB B-mode polarization power spectrum due to patchy reionization for different reionization scenarios. We then estimate the implication of the patchy reionization on the value of r, which are accessible from the upcoming and proposed CMB experiments such as LiteBIRD (Matsumura et al 2013), Simons Observatory (SO) (Aguirre et al 2018), CMB Stage-4 (CMB-S4) (Abazajian et al 2016), CMB-Bharat 2 and Probe of Inflation and Cosmic Origins (PICO) (Young et al 2018;Hanany et al 2019). Our analysis indicates that in order to make an unambiguous detection of r 10 −3 , we need to remove the patchy reionization signal (de-tau) along with the lensing (de-lensing) for proposed CMB experiments such as CMB-S4, CMB-Bharat and PICO.…”

Section: Introductionmentioning

confidence: 99%

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Is patchy reionization an obstacle in detecting the primordial gravitational wave signal?

Mukherjee

Paul

Choudhury

2019

Monthly Notices of the Royal Astronomical Society

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The large-scale CMB B-mode polarization is the direct probe to the low frequency primordial gravitational wave signal. However, unambiguous measurement of this signal requires a precise understanding of the possible contamination. One such potential contamination arises from the patchiness in the spatial distribution of free electrons during the epoch of reionization. We estimate the B-mode power spectrum due to patchy reionization using a combination of photon-conserving semi-numerical simulation and analytical calculation, and compare its amplitude with the primordial B-mode signal. For a reionization history which is in agreement with several latest observations, we find that a stronger secondary B-mode polarization signal is produced when the reionization is driven by the sources in massive halos and its amplitude can be comparable to the recombination bump for tensor to scalar ratio (r) 5 × 10 −4 . If contamination from patchy reionization is neglected in the analysis of B-mode polarization data, then for the models of reionization considered in this analysis, we find a maximum bias of about 30% in the value of r = 10 −3 when spatial modes between ∈ [50, 200] are used with a delensing efficiency of 50%. The inferred bias from patchy reionization is not a severe issue for the upcoming ground-based CMB experiment Simons Observatory, but can be a potential source of confusion for proposed CMB experiments which target to detect the value of r < 10 −3 . However, this obstacle can be removed by utilizing the difference in the shape of the power spectrum from the primordial signal. 1 This value changes by about 1-σ with change in the reionization model (Planck Collaboration et al. 2018).

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“…A future data-driven model of the galactic magnetic field in future will allow making more precise statements. Future experiments such as Simons Observatory [61], Simons Array [62], Adv-ACT [63], SPT-3G [62] and proposed missions like CMB-S4 [64], LiteBIRD [65], CMB-Bharat, PIXIE [66] and PICO [67] will improve these constraints significantly. Future CMB experiments having more frequency channels will play a crutial role in removing the contamination from CMB fluctuations and the galactic foregrounds.…”

Section: Resultsmentioning

confidence: 99%

Constraints on non-resonant photon-axion conversion from the Planck satellite data

Mukherjee

Khatri

Wandelt

2019

J. Cosmol. Astropart. Phys.

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The non-resonant conversion of Cosmic Microwave Background (CMB) photons into scalar as well as light pseudoscalar particles such as axion-like particles (ALPs) in the presence of turbulent magnetic fields can cause a unique, spatially fluctuating spectral distortion in the CMB. We use the publicly available Planck temperature maps for the frequency channels (70-545 GHz) to obtain the first ALP distortion map using 45% clean part of the sky. The 95 th percentile upper limit on the RMS fluctuation of ALP distortions from the cleanest part of the CMB sky at 15 arcmin angular resolution is 18.5 × 10 −6 . The RMS fluctuation in the distortion map is also consistent with different combinations of frequency channels and sky-fractions.

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Optical design of PICO: a concept for a space mission to probe inflation and cosmic origins

Cited by 17 publications

References 17 publications

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Is patchy reionization an obstacle in detecting the primordial gravitational wave signal?

Constraints on non-resonant photon-axion conversion from the Planck satellite data

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