Microwave Spectro-Polarimetry of Matter and Radiation across Space and Time

Delabrouille, J.; Abitbol, Maximilian H.; Aghanim, N.; Ali-Haı̈moud, Yacine; Alonso, David; Alvarez, Marcelo A.; Banday, A. J.; Bartlett, J. G.; Baselmans, J. J. A.; Basu, Kaustuv; Battaglia, Nicholas; Climent, José Ramón Bermejo; Bernal, José; Béthermin, M.; Bolliet, Boris; Bonato, Matteo; Bouchet, F. R.; Breysse, Patrick C.; Burigana, C.; Cai, Zhen-Yi; Chluba, Jens; Churazov, E.; Dannerbauer, H.; Bernardis, P. de; Zotti, G. de; Valentino, Eleonora Di; Dimastrogiovanni, Emanuela; Endo, Akira; Erler, Jens; Ferraro, Simone; Finelli⋆, F.; Fixsen, D. J.; Hanany, Shaul; Hart, Luke; Hernandez-Monteagudo, Carlos; Colin, Hill, J.; Hotinli, Selim C.; Karatsu, K.; Karkare, K. S.; Keating, Garrett K.; Khabibullin, Ildar; Kogut, A.; Kohri, Kazunori; Kovetz, Ely D.; Lagache, G.; Lesgourgues, Julien; Madhavacheril, Mathew S.; Maffei, B.; Mandolesi, N.; Martins, C. J. A. P.; Masi, S.; Mather, John C.; Melin, Jean-Baptiste; Dizgah, Azadeh Moradinezhad; Mroczkowski, Tony; Mukherjee, Suvodip; Nagai, Daisuke; Negrello, M.; Palanque-Delabrouille, N.; Paoletti, D.; Patil, Subodh P.; Raghunathan, S.; Ravenni, Andrea; Remazeilles, M.; Revéret, V.; Rodriguez, L.; Rotti, Aditya; Rubino, Martin, Jose-Alberto; Sayers, Jack; Scott, Douglas; Silk, Joseph; Silva, Marta; Souradeep, T.; Sugiyama, Naonori S.; Sunyaev, R.; Switzer, Eric R.; Tartari, A.; Trombetti, T.; Zubeldia, Íñigo

doi:10.48550/arxiv.1909.01591

Cited by 32 publications

(47 citation statements)

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“…As an example of a more futuristic survey, capable of measuring BAO at percent-level precision, given the challenges of ground-based measurements of [CII] due to limited atmospheric transmission at the relevant frequencies, we consider a space-based mission with a similar specification to the design proposed in Refs. [15,36], with 64 spectrometers with spectral resolution of R = 300 and background-limited performance and an actively cooled aperture, with a survey covering f sky = 0.25 in a total of 18000 hours. We refer the reader to Refs.…”

Section: Baryon Acoustic Oscillationsmentioning

confidence: 99%

“…We refer the reader to Refs. [26,36] for details of instrument specifications and noise calculation.…”

Section: Baryon Acoustic Oscillationsmentioning

confidence: 99%

“…Looking ahead, in addition to several 21-cm surveys, a wide range of ground-and space-based experiments (e.g., COMAP [10], TIME [31], CONCERTO [32], CCAT-prime [33] EXCLAIM [34], SPHEREx [3] and CDIM [35]) will provide higher-fidelity detection of line intensity fluctuations at different redshifts from several emission lines 1 . Success of these surveys will pave the way for next generation wide-field LIM surveys (e.g., [36,37]), capable of providing precision cosmological constraints.…”

Section: Introductionmentioning

confidence: 99%

“…The dotted lines are the theoretical predictions using linear theory, while the dashed lines are the nonlinear model. The vertical lines are the expected error bars for the BAO measurement in [CII] intensity maps at z = 1 (bottom curve) and z = 4.5 (top curve) from space-mission as proposed in EASA Voyage 2050 Microwave Spectro-Polarimetry white paper[36]. The curves at different redshifts are shifted w.r.t.…”

mentioning

confidence: 99%

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Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

Dizgah,

Nikakhtar,

Keating

et al. 2021

Preprint

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Line intensity mapping (LIM) is an emerging technique with a unique potential to probe a wide range of scales and redshifts. Realizing the full potential of LIM, however, relies on accurate modeling of the signal. We introduce an extended halo model for the power spectrum of intensity fluctuations of CO rotational lines and [CII] fine transition line in real space, modeling nonlinearities in matter fluctuations and biasing relation between the line intensity fluctuations and the underlying dark matter distribution. We also compute the stochastic contributions beyond the Poisson approximation using the halo model framework. To establish the accuracy of the model, we create the first cosmological-scale simulations of CO and [CII] intensity maps, MithraLIMSims, at redshifts 0.5 ≤ z ≤ 6, using halo catalogs from Hidden-Valley simulations, and painting halos according to mass-redshift-luminosity relations for each line. We show that at z = 1 on scales k max 0.8 Mpc −1 h, the model predictions of clustering power (with only two free parameters) are in agreement with the measured power spectrum at better than 5%. At higher redshift of z = 4.5, this remarkable agreement extends to smaller scale of k max 2 Mpc −1 h. Furthermore, we show that on large scales, the stochastic contributions to CO and CII power spectra are non-Poissonian, with amplitudes reproduced reasonably well by the halo model prescription. Lastly, we assess the performance of the theoretical model of the baryon acoustic oscillations (BAO) and show that hypothetical LIM surveys probing CO lines at z = 1, that can be deployed within this decade, will be able to make a high significance measurement of the BAO. On a longer time scale, a space-based mission probing [CII] line can uniquely measure the BAO on a wide range of redshifts at an unprecedented precision.

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Section: Baryon Acoustic Oscillationsmentioning

confidence: 99%

“…We refer the reader to Refs. [26,36] for details of instrument specifications and noise calculation.…”

Section: Baryon Acoustic Oscillationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

Dizgah,

Nikakhtar,

Keating

et al. 2021

Preprint

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“…Among the experiments that are currently ongoing or in preparation, ground based experiments are expected to be limited by their restricted frequency and sky coverage, while the LiteBIRD (Hazumi et al 2019) space mission, owing to its limited angular resolution (∼30 ), will be limited by confusion between primordial and lensing polarization Bmodes. To overcome these limitations, other experiments have been proposed, such as COrE (The COrE Collaboration et al 2011;Delabrouille et al 2018), PRISM (André et al 2014), PICO (Hanany et al 2019), and more recently an ambitious spectro-polarimetric survey of the microwave sky (Delabrouille et al 2019). Exploring Cosmic History and Origin (ECHO) 1 is the latest addition to this list with similar objectives.…”

Section: Introductionmentioning

confidence: 99%

$B$-mode forecast of CMB-Bh$\overline{a}$rat

Adak,

Sen,

Basak

et al. 2021

Preprint

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Exploring Cosmic History and Origins (ECHO), popularly known as 'CMB-Bharat', is a space mission that has been proposed to the Indian Space Research Organisation (ISRO) for the scientific exploitation of the Cosmic Microwave Background (CMB) at the next level of precision and accuracy. The quest for the CMB polarization B-mode signals, generated by inflationary gravitational waves in the very early universe, is one of the key scientific goals of its experimental design. This work studies the potential of the proposed ECHO instrumental configuration to detect the target tensor-to-scalar ratio r ∼ 10 −3 at 3σ significance level, which covers the predictions of a large class of inflationary models. We investigate the performance of two different component separation pipelines, NILC and Commander, for the measurement of r in presence of different physically motivated models of astrophysical foregrounds. For a simplistic foreground model (only polarized dust and synchrotron), both component separation pipelines can achieve the desired sensitivity of ECHO, i.e. σ(r = 0) ∼ (0.4 − 0.7) × 10 −3 . NILC performs better than Commander in terms of bias on recovered r for complex spectral models (power-law and curved power-law) of the synchrotron emission and complex dust models (dust decorrelation). Assuming 84% delensing, we can achieve an improvement of σ(r = 0) by approximately 50% as compared to the results obtained for the same configuration without any lensing correction.

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Testing the analytical blind separation method in simulated CMB polarization maps

Santos

Yao

et al. 2021

A&A

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Context. Multi-frequency observations are needed to separate the cosmic microwave background (CMB) from foreground emission and accurately extract cosmological information from the data. The analytical blind separation (ABS) method is dedicated to extracting the CMB power spectrum from multi-frequency observations in the presence of contamination from astrophysical foreground emission and instrumental noise. Aims. In this study, we apply the ABS method to simulated sky maps as could be observed with a future space-borne survey in order to test its capability of determining the CMB polarization E- and B-mode power spectra. Methods. We present the ABS method performance on simulations for both a full-sky analysis and for an analysis concentrating on sky regions less impacted by Galactic foreground emission. Results. We discuss the origin and minimization of biases in the estimated CMB polarization angular power spectra. We find that the ABS method performs quite well for the analysis of full-sky observations at intermediate and small angular scales, in spite of strong foreground contamination. On the largest scales, extra work is still required to reduce biases of various origins and the impact of confusion between CMB E and B polarization for partial sky analyses.

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Microwave Spectro-Polarimetry of Matter and Radiation across Space and Time

Cited by 32 publications

References 0 publications

Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

Precision Tests of CO and [CII] Power Spectra Models against Simulated Intensity Maps

$B$-mode forecast of CMB-Bh$\overline{a}$rat

Testing the analytical blind separation method in simulated CMB polarization maps

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