SearcharxivSearch

arXiv · 1707.02259

Exploring cosmic origins with CORE: gravitational lensing of the CMB

Anthony Challinor·Rupert Allison·Julien Carron·Josquin Errard·Stephen Feeney·Thomas Kitching·Julien Lesgourgues·Antony Lewis·Íñigo Zubeldía·Ana Achucarro·Peter Ade·Mark Ashdown·Mario Ballardini·A. J. Banday·Ranajoy Banerji·James Bartlett·Nicola Bartolo·Soumen Basak·Daniel Baumann·Marco Bersanelli·Anna Bonaldi·Matteo Bonato·Julian Borrill·François Bouchet·François Boulanger·Thejs Brinckmann·Martin Bucher·Carlo Burigana·Alessandro Buzzelli·Zhen-Yi Cai·Martino Calvo·Carla-Sofia Carvalho·Gabriella Castellano·Jens Chluba·Sebastien Clesse·Ivan Colantoni·Alessandro Coppolecchia·Martin Crook·Giuseppe d'Alessandro·Paolo de Bernardis·Giancarlo de Gasperis·Gianfranco De Zotti·Jacques Delabrouille·Eleonora Di Valentino·Jose-Maria Diego·Raul Fernandez-Cobos·Simone Ferraro·Fabio Finelli·Francesco Forastieri·Silvia Galli·Ricardo Genova-Santos·Martina Gerbino·Joaquin González-Nuevo·Sebastian Grandis·Joshua Greenslade·Steffen Hagstotz·Shaul Hanany·Will Handley·Carlos Hernandez-Monteagudo·Carlos Hervías-Caimapo·Matthew Hills·Eric Hivon·Kimmo Kiiveri·Ted Kisner·Martin Kunz·Hannu Kurki-Suonio·Luca Lamagna·Anthony Lasenby·Massimiliano Lattanzi·Michele Liguori·Valtteri Lindholm·Marcos López-Caniego·Gemma Luzzi·Bruno Maffei·Enrique Martinez-González·C. J. A. P. Martins·Silvia Masi·Darragh McCarthy·Alessandro Melchiorri·Jean-Baptiste Melin·Diego Molinari·Alessandro Monfardini·Paolo Natoli·Mattia Negrello·Alessio Notari·Alessandro Paiella·Daniela Paoletti·Guillaume Patanchon·Michel Piat·Giampaolo Pisano·Linda Polastri·Gianluca Polenta·Agnieszka Pollo·Vivian Poulin·Miguel Quartin·Mathieu Remazeilles·Matthieu Roman·Jose-Alberto Rubino-Martin·Laura Salvati·Andrea Tartari

Abstract

Lensing of the CMB is now a well-developed probe of large-scale clustering over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission can produce a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that it will enable. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous BAO measurements, three times smaller than the minimum total mass allowed by neutrino oscillations. In the search for B-mode polarization from primordial gravitational waves with CORE, lens-induced B-modes will dominate over instrument noise, limiting constraints on the gravitational wave power spectrum amplitude. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60%. This improves to 70% by combining lensing and CIB measurements from CORE, reducing the error on the gravitational wave amplitude by 2.5 compared to no delensing (in the null hypothesis). Lensing measurements from CORE will allow calibration of the halo masses of the 40000 galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. CORE can accurately remove Galactic emission from CMB maps with its 19 frequency channels. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE. [abridged]

Explore related subjects

Keep this discovery

BibTeXRIS

Anthony Challinor, Rupert Allison, Julien Carron, Josquin Errard, Stephen Feeney, Thomas Kitching, Julien Lesgourgues, Antony Lewis, Íñigo Zubeldía, Ana Achucarro, Peter Ade, Mark Ashdown, Mario Ballardini, A. J. Banday, Ranajoy Banerji, James Bartlett, Nicola Bartolo, Soumen Basak, Daniel Baumann, Marco Bersanelli, Anna Bonaldi, Matteo Bonato, Julian Borrill, François Bouchet, François Boulanger, Thejs Brinckmann, Martin Bucher, Carlo Burigana, Alessandro Buzzelli, Zhen-Yi Cai, Martino Calvo, Carla-Sofia Carvalho, Gabriella Castellano, Jens Chluba, Sebastien Clesse, Ivan Colantoni, Alessandro Coppolecchia, Martin Crook, Giuseppe d'Alessandro, Paolo de Bernardis, Giancarlo de Gasperis, Gianfranco De Zotti, Jacques Delabrouille, Eleonora Di Valentino, Jose-Maria Diego, Raul Fernandez-Cobos, Simone Ferraro, Fabio Finelli, Francesco Forastieri, Silvia Galli, Ricardo Genova-Santos, Martina Gerbino, Joaquin González-Nuevo, Sebastian Grandis, Joshua Greenslade, Steffen Hagstotz, Shaul Hanany, Will Handley, Carlos Hernandez-Monteagudo, Carlos Hervías-Caimapo, Matthew Hills, Eric Hivon, Kimmo Kiiveri, Ted Kisner, Martin Kunz, Hannu Kurki-Suonio, Luca Lamagna, Anthony Lasenby, Massimiliano Lattanzi, Michele Liguori, Valtteri Lindholm, Marcos López-Caniego, Gemma Luzzi, Bruno Maffei, Enrique Martinez-González, C. J. A. P. Martins, Silvia Masi, Darragh McCarthy, Alessandro Melchiorri, Jean-Baptiste Melin, Diego Molinari, Alessandro Monfardini, Paolo Natoli, Mattia Negrello, Alessio Notari, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Michel Piat, Giampaolo Pisano, Linda Polastri, Gianluca Polenta, Agnieszka Pollo, Vivian Poulin, Miguel Quartin, Mathieu Remazeilles, Matthieu Roman, Jose-Alberto Rubino-Martin, Laura Salvati, Andrea Tartari. 2017-07-07. Exploring cosmic origins with CORE: gravitational lensing of the CMB. https://doi.org/10.1088/1475-7516/2018/04/018

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Constraining spinning primordial black holes with interstellar dust heating

Primordial black holes (PBHs) are a well-motivated dark matter candidate, and their cosmic abundance is constrained by a variety of observational probes. PBHs in the mass range $10^{15}\,\text{g}\,{-}\,10^{17}\,\text{g}$ are evaporating today via Hawking radiation, a process that can heat interstellar dust and modify its thermal emission. Recent studies have used this effect to place constraints on the abundance of non-spinning PBHs. We extend this approach by investigating the influence of PBH spin on dust-heating constraints. Furthermore, we account for secondary photons that originate not only from the decay of gauge bosons but also from the decay of hadrons produced via the fragmentation of primary quarks and gluons emitted through Hawking radiation. By comparing the dust heating rate induced by spinning PBHs with the maximum cooling rate of dust, considering both silicate and graphite grains, we derive new upper limits on the fraction of dark matter in the form of PBHs, $f_{\rm PBH}$. Our results show that the constraints depend on both PBH mass and spin. Smaller PBHs with higher spin yield stronger limits. For example, in the cases we investigated, the strongest constraint is $f_{\rm PBH} \sim 1.5 \times 10^{-4}$ for $M_{\rm PBH} = 10^{15}{\rm g}$ and spin parameter $a_{*} = 0.9999$. Although these limits are less stringent than existing constraints in the same mass range, they provide a distinct and complementary approach to constraining the abundance of PBHs.

astro-ph.CO

Two-parameter continuous deformation of Starobinsky inflation as a bridge between Planck and ACT DESI data with $N_\star\in(50,60)$

We present a family of plateau-type inflationary potentials, eq.~\eqref{Vgeneral}, and analyze a two-parameter $\alpha\beta$-Starobinsky specialization that interpolates continuously between a \emph{maximal} plateau ($V\!\to\!V_0$) and a \emph{submaximal} plateau ($V\!\to\!V_\infty 0$ with $x_\star\gg 1/\beta$ the slow-roll scaling laws change to $n_s\simeq 1-\frac{4}{3N_\star},\, r\simeq\mathcal{C}(\alpha,\beta)\,N_\star^{-4/3},$ with an explicit coefficient $\mathcal{C}(\alpha,\beta)$ set by the plateau truncation. This deformation lifts $n_s$ at fixed $N_\star$ while further suppressing $r$, reconciling the Planck~2018 constraint $n_s=0.9649\pm0.0042$ (68\% CL) and BICEP/Keck18 data $r_{0.05}<0.036$ (95\% CL), with the higher central values $n_s\sim0.97$--$0.98$ preferred by ACT+DESI~DR2 (BAO), within the theoretically motivated interval $N_\star\in(50,60)$ and without exotic reheating. We provide an exact identity for $V/V'$ enabling analytic control of $N_\star$, a practical crossover criterion $\beta\,x_\star\ll1$ vs.\ $\gg1$, and a transparent mapping between $(\alpha,\beta)$ and the observables $(n_s,r,N_\star)$. These yield sharp, testable signatures, particularly the softened $N_\star$-scaling of $r$, that distinguish a maximal from a submaximal plateau with upcoming CMB and LSS data.

astro-ph.CO

A Tale of Two Gauges: Effective Field Theory for Relativistic Behavior of Cosmological Axions

In this work, we present a formalism to model the relativistic behavior of axions. The relativistic behavior of axions is surprisingly difficult to model precisely, as it involves oscillations on timescales much shorter than the Hubble timescale. To overcome this challenge, one typically resorts to some form of effective treatment, focusing only on the time-averaged description of the exact oscillations. Salehian, Namjoo & Kaiser provide a systematic framework for such treatment, based on the effective field theory formalism. While the aforementioned study was formulated for axion perturbations in the Newtonian gauge with no anisotropic stress, we extend the formalism to the synchronous gauge that is more conventionally used for numerical implementation in a realistic cosmological setting. Unlike their work, however, we propose a fluid interpretation in which the axion field can be identified as a perfect fluid at all times, both in the exact and effective regimes. Moreover, we present the effective field theory for the Newtonian gauge with non-zero anisotropic stress, making the original formulation more general and useful for scenarios where the matter content of the universe is multi-component. These results lay the theoretical foundation for a companion paper where we discuss how the axion field should be incorporated alongside other species in common cosmological Boltzmann solvers.

astro-ph.CO