ALMA Band 3 polarimetric follow-up of a complete sample of faint PACO sources

Galluzzi, V.; Puglisi, Giuseppe; Burkutean, S.; Liuzzo, E.; Bonato, M.; Massardi, M.; Paladino, R.; Gregorini, L.; Ricci, R.; Trombetti, T.; Toffolatti, L.; Burigana, C.; Bonaldi, A.; Bonavera, L.; Casasola, V.; Zotti, G. de; Ekers, R. D.; Alighieri, S. di Serego; López‐Caniego, M.; Tucci, M.

doi:10.1093/mnras/stz1930

Cited by 10 publications

(17 citation statements)

References 44 publications

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“…Their findings show that the distribution of the observed Π fractions is, again, well fitted by a log-normal distribution, thus confirming previous outcomes at lower frequencies (Massardi et al 2013;Galluzzi et al 2018) and also the predictions of Tucci & Toffolatti (2012). The analysis of Galluzzi et al (2019) also confirms the absence of any statistically significant trend of polarisation properties of ERS with the frequency or the flux density.…”

Section: Introductionsupporting

confidence: 79%

“…However, no previous knowledge about P 0 is assumed in these papers and this information, if available, could be very useful after being incorporated in a Bayesian scheme. Recently, relevant data about the distribution of the polarisation fraction at different frequencies, Π = P 0 /S 0 , with S 0 being the source flux density, have been presented (Massardi et al 2013;Galluzzi et al 2017Galluzzi et al , 2019. According to these authors, this distribution can be represented by a log-normal probability density function (pdf)…”

Section: Methodsmentioning

confidence: 99%

“…However, the knowledge of the total and polarisation fraction of ERS is rapidly improving at high radio frequencies thanks to large samples of sources mainly observed by the Australia Telescope Compact Array (ATCA) and by the Very Large Array (VLA) (Sadler et al 2006;López-Caniego et al 2009;Massardi et al 2008Massardi et al , 2011Massardi et al , 2013Murphy et al 2010;Jackson et al 2010;Galluzzi et al 2017Galluzzi et al , 2018. More recently, and thanks to the very high sensitivity of the new detectors of the Atacama Large Millimetre Array (ALMA), Galluzzi et al (2019) could extend the analysis of polarisation properties of ERS performed by Galluzzi et al (2018) up to 97.5 GHz, by polarimetric observations of a complete sample of 32 extragalactic radio sources. Their findings show that the distribution of the observed Π fractions is, again, well fitted by a log-normal distribution, thus confirming previous outcomes at lower frequencies (Massardi et al 2013;Galluzzi et al 2018) and also the predictions of Tucci & Toffolatti (2012).…”

Section: Introductionmentioning

confidence: 99%

“…It is convenient to use the Stokes' parameters S, Q, U, and V (S for total intensity 1 in terms of flux density, see, e.g. Galluzzi et al (2019), Q and U for linear polarisation, and V for circular polarisation), but other representations are also possible. The Stokes' V parameter is not usually considered since Thomson scattering does not induce circular polarisation in the CMB.…”

Section: Introductionmentioning

confidence: 99%

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A Bayesian method for point source polarisation estimation

Herranz

Argüeso

Toffolatti

et al. 2021

A&A

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The estimation of the polarisation P of extragalactic compact sources in cosmic microwave background (CMB) images is a very important task in order to clean these images for cosmological purposes -for example, to constrain the tensor-to-scalar ratio of primordial fluctuations during inflation-and also to obtain relevant astrophysical information about the compact sources themselves in a frequency range, ν ∼ 10-200 GHz, where observations have only very recently started to become available. In this paper, we propose a Bayesian maximum a posteriori (MAP) approach estimation scheme which incorporates prior information about the distribution of the polarisation fraction of extragalactic compact sources between 1 and 100 GHz. We apply this Bayesian scheme to white noise simulations and to more realistic simulations that include CMB intensity, Galactic foregrounds, and instrumental noise with the characteristics of the QUIJOTE (Q U I JOint TEnerife) experiment wide survey at 11 GHz. Using these simulations, we also compare our Bayesian method with the frequentist filtered fusion method that has been already used in the Wilkinson Microwave Anisotropy Probe (WMAP) data and in the Planck mission. We find that the Bayesian method allows us to decrease the threshold for a feasible estimation of P to levels below ∼ 100 mJy (as compared to ∼ 500 mJy which was the equivalent threshold for the frequentist filtered fusion). We compare the bias introduced by the Bayesian method and find it to be small in absolute terms. Finally, we test the robustness of the Bayesian estimator against uncertainties in the prior and in the flux density of the sources. We find that the Bayesian estimator is robust against moderate changes in the parameters of the prior and almost insensitive to realistic errors in the estimated photometry of the sources.

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Section: Introductionsupporting

confidence: 79%

Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A Bayesian method for point source polarisation estimation

Herranz

Argüeso

Toffolatti

et al. 2021

A&A

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“…Only a few tens of sources (all radio) were detected by Planck in the 'extragalactic zone' [11]. Galluzzi et al [124] carried out ALMA high sensitivity polarimetric observations at 97.5 GHz of a complete sample of 32 compact extragalactic radio sources brighter than 200 mJy at 20 GHz; a detection rate of 97% was achieved.…”

Section: Detecting Sources In Polarizationmentioning

confidence: 99%

Extragalactic Astrophysics With Next-Generation CMB Experiments

Zotti

Bonato

Negrello

et al. 2019

Front. Astron. Space Sci.

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Planck, SPT and ACT surveys have clearly demonstrated that Cosmic Microwave Background (CMB) experiments, while optimised for cosmological measurements, have made important contributions to the field of extragalactic astrophysics in the last decade. Future CMB experiments have the potential to make even greater contributions. One example is the detection of highz galaxies with extreme gravitational amplifications. The combination of flux boosting and of stretching of the images has allowed the investigation of the structure of galaxies at z 3 with the astounding spatial resolution of about 60 pc. Another example is the detection of proto-clusters of dusty galaxies at high z when they may not yet possess the hot intergalactic medium allowing their detection in X-rays or via the Sunyaev-Zeldovich effect. Next generation CMB experiments, like PICO, CORE, CMB-Bharat from space and Simons Observatory and CMB-S4 from the ground, will discover several thousands of strongly lensed galaxies out to z ∼ 6 or more and of 1 arXiv:1907.05323v1 [astro-ph.GA] 11 Jul 2019 De Zotti et al. Running Title Figure 1. Effect of angular resolution on the confusion limit. The filled blue circles show the differential counts of sources on SPT maps degraded to the PICO resolution at 150 GHz (FWHM = 6.2 ; left panel) and 220 GHz (FWHM = 3.6 ; right panel) compared with the SPT counts of Mocanu et al. [5, orange stars]. The vertical dot-dashed lines correspond, from left to right, to the 90% completeness limits at the full SPT resolution, at the PICO resolution and at the Planck resolution.galaxy proto-clusters caught in the phase when their member galaxies where forming the bulk of their stars. They will also detect tens of thousands of local dusty galaxies and thousands of radio sources at least up to z 5. Moreover they will measure the polarized emission of thousands of radio sources and of dusty galaxies at mm/sub-mm wavelengths.

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Impact of polarised extragalactic sources on the measurement of CMBB-mode anisotropies

Lagache

Béthermin

Montier

et al. 2020

A&A

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One of the main goals of cosmology is to search for the imprint of primordial gravitational waves in the polarisation filed of the cosmic microwave background to probe inflation theories. One of the obstacles in detecting the primordial signal is that the cosmic microwave background B-mode polarisation must be extracted from among astrophysical contaminations. Most efforts have focus on limiting Galactic foreground residuals, but extragalactic foregrounds cannot be ignored at the large scale (ℓ ≲ 150), where the primordial B-modes are the brightest. We present a complete analysis of extragalactic foreground contamination that is due to polarised emission of radio and dusty star-forming galaxies. We update or use current models that are validated using the most recent measurements of source number counts, shot noise, and cosmic infrared background power spectra. We predict the flux limit (confusion noise) for future cosmic microwave background (CMB) space-based or balloon-borne experiments (IDS, PIPER, SPIDER, LiteBIRD, and PICO), as well as ground-based experiments (C-BASS, NEXT-BASS, QUIJOTE, AdvACTPOL, BICEP3+Keck, BICEPArray, CLASS, Simons Observatory, SPT3G, and S4). The telescope aperture size (and frequency) is the main characteristic that affects the level of confusion noise. Using the flux limits and assuming mean polarisation fractions independent of flux and frequency for radio and dusty galaxies, we computed the B-mode power spectra of the three extragalactic foregrounds (radio source shot noise, dusty galaxy shot noise, and clustering). We discuss their relative levels and compare their amplitudes to that of the primordial tensor modes parametrised by the tensor-to-scalar ratio r. At the reionisation bump (ℓ = 5), contamination by extragalactic foregrounds is negligible. While the contamination is much lower than the targeted sensitivity on r for large-aperture telescopes at the recombination peak (ℓ = 80), it is at a comparable level for some of the medium- (∼1.5 m) and small-aperture telescope (≤0.6 m) experiments. For example, the contamination is at the level of the 68% confidence level uncertainty on the primordial r for the LiteBIRD and PICO space-based experiments. These results were obtained in the absence of multi-frequency component separation (i.e. considering each frequency independently). We stress that extragalactic foreground contaminations have to be included in the input sky models of component separation methods dedicated to the recovery of the CMB primordial B-mode power spectrum. Finally, we also provide some useful unit conversion factors and give some predictions for the SPICA B-BOP experiment, which is dedicated to Galactic and extragalactic polarisation studies. We show that SPICA B-BOP will be limited at 200 and 350 μm by confusion from extragalactic sources for long integrations in polarisation, but very short integrations in intensity.

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ALMA Band 3 polarimetric follow-up of a complete sample of faint PACO sources

Cited by 10 publications

References 44 publications

A Bayesian method for point source polarisation estimation

A Bayesian method for point source polarisation estimation

Extragalactic Astrophysics With Next-Generation CMB Experiments

Impact of polarised extragalactic sources on the measurement of CMBB-mode anisotropies

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