Local analyses of<i>Planck</i>maps with Minkowski functionals

Novaes, Camila P.; Bernui, Armando; Marques, Gabriela A.; Ferreira, Ivan Soares

doi:10.1093/mnras/stw1427

Cited by 25 publications

(24 citation statements)

References 49 publications

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“…The marginalized constraint on neutrino mass from three MFs combined improves that from the power spectrum alone by a factor of 4.82. Comparing the constraining power from the three MFs, we find that V 2 V 1 > V 0 , similar to findings in previous work [20,28,54]. This is because both perimeter (V 1 ) and genus (V 2 ) are sensitive to not only the overall distribution of under/over-density, as probed by area (V 0 ), but also their spatial information.…”

Section: Joint Constraintssupporting

confidence: 88%

Constraining neutrino mass with weak lensing Minkowski Functionals

Marques

Bernui

Novaes

et al. 2019

J. Cosmol. Astropart. Phys.

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The presence of massive neutrinos affects structure formation, leaving imprints on large-scale structure observables such as the weak lensing field. The common lensing analyses with two-point statistics are insensitive to the large amount of non-Gaussian information in the density field. We investigate non-Gaussian tools, in particular the Minkowski Functionals (MFs)-morphological descriptors including area, perimeter, and genus-in an attempt to recover the higher-order information. We use convergence maps from the Cosmological Massive Neutrino Simulations (MassiveNus) and assume galaxy noise, density, and redshift distribution for an LSST-like survey. We show that MFs are sensitive to the neutrino mass sum, and the sensitivity is redshift dependent and is non-Gaussian. We find that redshift tomography significantly improves the constraints on neutrino mass for MFs, compared to the improvements for the power spectrum. We attribute this to the stronger redshift dependence of neutrino effects on small scales. We then build an emulator to model the power spectrum and MFs, and study the constraints on [M ν , Ω m , A s ] from the power spectrum, MFs, and their combination. We show that MFs significantly outperform the power spectrum in constraining neutrino mass, by more than a factor of four. However, a thorough study of the impact from systematics such as baryon physics and galaxy shape and redshift biases will be important to realize the full potential of MFs.

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Section: Joint Constraintssupporting

confidence: 88%

Constraining neutrino mass with weak lensing Minkowski Functionals

Marques

Bernui

Novaes

et al. 2019

J. Cosmol. Astropart. Phys.

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“…The statistical isotropy of the universe is being tested for many extragalactic objects like Radio sources (Blake & Wall 2002;Ghosh et al 2016), Gamma-ray bursts (Bernui et al 2008a;Tarnopolski 2017;Řípa & Shafiello 2018), galaxy clusters (Bengaly et al 2017a), and galaxy datasets like the WISE (Yoon et al 2014;Bengaly et al 2017b;Novaes et al 2018) and the SDSS catalogues (Sarkar et al 2019), where all these analyses show a good concordance with the isotropy of the universe. The Planck Convergence and Cosmic Microwave Background temperature fluctuations maps have been examined and are also consistent with statistical isotropy at small angular scales (Ade et al 2016;Novaes et al 2016;Marques et al 2018), although some controversy remains at large angles (Bernui 2008b;Gruppuso et al 2013; Polase-mail: felipeavila@on.br tri, Gruppuso & Natoli 2015;Schwarz et al 2016;Aluri, Ralston & Weltman 2017;Rath et al 2017;Bernui et al 2018).…”

Section: Introductionmentioning

confidence: 87%

The angular scale of homogeneity in the local Universe with the SDSS blue galaxies

Avila

Novaes

Bernui

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We probe the angular scale of homogeneity in the local Universe using blue galaxies from the SDSS survey as a cosmological tracer. Through the scaled counts in spherical caps, N (< θ), and the fractal correlation dimension, D 2 (θ), we find an angular scale of transition to homogeneity for this sample of θ H = 22.19 • ±1.02 • . A comparison of this measurement with another obtained using a different cosmic tracer at a similar redshift range (z < 0.06), namely, the HI extragalactic sources from the ALFALFA catalogue, confirms that both results are in excellent agreement (taking into account the corresponding bias correction). We also perform tests to asses the robustness of our results. For instance, we test if the size of the surveyed area is large enough to identify the transition scale we search for, and also we investigate a reduced sample of blue galaxies, obtaining in both cases a similar angular scale for the transition to homogeneity. Our results, besides confirming the existence of an angular scale of transition to homogeneity in different cosmic tracers present in the local Universe, show that the observed angular scale θ H agrees well with what is expected in the ΛCDM scenario. Although we can not prove spatial homogeneity within the approach followed, our results provide one more evidence of it, strengthening the validity of the Cosmological Principle.

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“…Besides, the projected isotropy of the Planck convergence map [19] and of the WISE galaxy map [20][21][22][23] have been also investigated without indications of a possible CP violation. The cosmic microwave background (CMB) radiation is also consistent with statistical isotropy at small angular scales [24][25][26], although some controversy exists at the largest scales [27][28][29][30][31][32][33][34][35].…”

Section: Introductionmentioning

confidence: 99%