Issue 
A&A
Volume 596, December 2016



Article Number  A102  
Number of page(s)  19  
Section  Cosmology (including clusters of galaxies)  
DOI  https://doi.org/10.1051/00046361/201527932  
Published online  12 December 2016 
Planck intermediate results
XLI. A map of lensinginduced Bmodes
^{1} APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10 rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
^{2} Aalto University Metsähovi Radio Observatory and Dept of Radio Science and Engineering, PO Box 13000, 00076 Aalto, Finland
^{3} African Institute for Mathematical Sciences, 6–8 Melrose Road, Muizenberg, 00040 Cape Town, South Africa
^{4} Agenzia Spaziale Italiana Science Data Center, via del Politecnico snc, 00133 Roma, Italy
^{5} Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
^{6} Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, UK
^{7} Astrophysics & Cosmology Research Unit, School of Mathematics, Statistics & Computer Science, University of KwaZuluNatal, Westville Campus, Private Bag X54001, 4000 Durban, South Africa
^{8} CGEE, SCS Qd 9, Lote C, Torre C, 4° andar, Ed. Parque Cidade Corporate, CEP 70308200 Brasília, DF, Brazil
^{9} CITA, University of Toronto, 60 St. George St., Toronto, ON M5S 3H8, Canada
^{10} CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
^{11} CRANN, Trinity College, Dublin, Ireland
^{12} California Institute of Technology, Pasadena, California, CA 911098 USA
^{13} Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan, 1, planta 2, 44001 Teruel, Spain
^{14} Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California, USA
^{15} DSM/Irfu/SPP, CEASaclay, 91191 GifsurYvette Cedex, France
^{16} DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark
^{17} Département de Physique Théorique, Université de Genève, 24 Quai E. Ansermet, 1211 Genève 4, Switzerland
^{18} Departamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain
^{19} Departamento de Física, Universidad de Oviedo, Avda. Calvo Sotelo s/n, 33007 Oviedo, Spain
^{20} Department of Astronomy and Astrophysics, University of Toronto, 50 Saint George Street, Toronto, Ontario, Canada
^{21} Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
^{22} Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada
^{23} Department of Physics and Astronomy, Dana and David Dornsife College of Letter, Arts and Sciences, University of Southern California, Los Angeles, CA 90089, USA
^{24} Department of Physics and Astronomy, University College London, London WC1E 6BT, UK
^{25} Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, 00560 Helsinki, Finland
^{26} Department of Physics, Princeton University, Princeton, New Jersey, NJ 08544, USA
^{27} Department of Physics, University of California, One Shields Avenue, Davis, California, CA 93106, USA
^{28} Department of Physics, University of California, Santa Barbara, CA 93106 California, USA
^{29} Department of Physics, University ofIllinois at UrbanaChampaign, 1110 West Green Street, Urbana, IL 61801 Illinois, USA
^{30} Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131 Padova, Italy
^{31} Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, via Saragat 1, 44122 Ferrara, Italy
^{32} Dipartimento di Fisica, Università La Sapienza, P. le A. Moro 2, 00133 Roma, Italy
^{33} Dipartimento di Fisica, Università degli Studi di Milano, via Celoria 16, 20133 Milano, Italy
^{34} Dipartimento di Matematica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, 00133 Roma, Italy
^{35} Discovery Center, Niels Bohr Institute, Blegdamsvej 17, 1165 Copenhagen, Denmark
^{36} Discovery Center, Niels Bohr Institute, Copenhagen University, Blegdamsvej 17, 1165 Copenhagen, Denmark
^{37} European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, 28691 Villanueva de la Cañada, Madrid, Spain
^{38} European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
^{39} Facoltà di Ingegneria, Università degli Studi eCampus, via Isimbardi 10, 22060 Novedrate (CO), Italy
^{40} Gran Sasso Science Institute, INFN, viale F. Crispi 7, 67100 L’ Aquila, Italy
^{41} HGSFP and University of Heidelberg, Theoretical Physics Department, Philosophenweg 16, 69120 Heidelberg, Germany
^{42} Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland
^{43} INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35131 Padova, Italy
^{44} INAF–Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy
^{45} INAF–Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy
^{46} INAF/IASF Bologna, via Gobetti 101, 40126 Bologna, Italy
^{47} INAF/IASF Milano, via E. Bassini 15, 20133 Milano, Italy
^{48} INFN, Sezione di Bologna, via Irnerio 46, 40126 Bologna, Italy
^{49} INFN, Sezione di Roma 1, Università di Roma Sapienza, Piazzale Aldo Moro 2, 00185 Roma, Italy
^{50} INFN, Sezione di Roma 2, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, 00133 Roma, Italy
^{51} IUCAA, Post Bag 4, Ganeshkhind, Pune University Campus, 411 007 Pune, India
^{52} Imperial College London, Astrophysics group, Blackett Laboratory, Prince Consort Road, London, SW7 2AZ, UK
^{53} Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
^{54} Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université ParisSud 11, Bâtiment 121, 91898 Orsay, France
^{55} Institut d’Astrophysique de Paris, CNRS (UMR7095), 98bis Boulevard Arago, 75014 Paris, France
^{56} Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
^{57} Institute of Theoretical Astrophysics, University of Oslo, Blindern, 0371 Oslo, Norway
^{58} Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, La Laguna, 38205 Tenerife, Spain
^{59} Instituto de Física de Cantabria (CSICUniversidad de Cantabria), Avda. de los Castros s/n, 39005 Santander, Spain
^{60} Istituto Nazionale di Fisica Nucleare, Sezione di Padova, via Marzolo 8, 35131 Padova, Italy
^{61} Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
^{62} Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, UK
^{63} Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
^{64} Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
^{65} Kazan Federal University, 18 Kremlyovskaya St., 420008 Kazan, Russia
^{66} LAL, Université ParisSud, CNRS/IN2P3, 91898 Orsay, France
^{67} LERMA, CNRS, Observatoire de Paris, 61 Avenue de l’Observatoire, 75000 Paris, France
^{68} Laboratoire AIM, IRFU/Service d’Astrophysique – CEA/DSM – CNRS – Université Paris Diderot, Bât. 709, CEASaclay, 91191 GifsurYvette Cedex, France
^{69} Laboratoire Traitement et Communication de l’Information, CNRS (UMR 5141) and Télécom ParisTech, 46 rue Barrault 75634 Paris Cedex 13, France
^{70} Laboratoire de Physique Subatomique et Cosmologie, Université GrenobleAlpes, CNRS/IN2P3, 53 rue des Martyrs, 38026 Grenoble Cedex, France
^{71} Laboratoire de Physique Théorique, Université ParisSud 11 & CNRS, Bâtiment 210, 91405 Orsay, France
^{72} Lawrence Berkeley National Laboratory, Berkeley, California CA 94720, USA
^{73} Lebedev Physical Institute of the Russian Academy of Sciences, Astro Space Centre, 84/32 Profsoyuznaya st., 117997 Moscow, GSP7, Russia
^{74} MaxPlanckInstitut für Astrophysik, KarlSchwarzschildStr. 1, 85741 Garching, Germany
^{75} National University of Ireland, Department of Experimental Physics, Maynooth, Co. Kildare, Ireland
^{76} Nicolaus Copernicus Astronomical Center, Bartycka 18, 00716 Warsaw, Poland
^{77} Niels Bohr Institute, Blegdamsvej 17, 1165 Copenhagen, Denmark
^{78} Niels Bohr Institute, Copenhagen University, Blegdamsvej 17, 1165 Copenhagen, Denmark
^{79} Nordita (Nordic Institute for Theoretical Physics), Roslagstullsbacken 23, 106 91 Stockholm, Sweden
^{80} Optical Science Laboratory, University College London, Gower Street, London, UK
^{81} SISSA, Astrophysics Sector, via Bonomea 265, 34136 Trieste, Italy
^{82} School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, UK
^{83} School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD, UK
^{84} Sorbonne UniversitéUPMC, UMR7095, Institut d’Astrophysique de Paris, 98bis Boulevard Arago, 75014 Paris, France
^{85} Space Research Institute (IKI), Russian Academy of Sciences, Profsoyuznaya Str, 84/32, 117997 Moscow, Russia
^{86} Space Sciences Laboratory, University of California, Berkeley, CA 94720 California, USA
^{87} Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Zelenchukskiy region, 369167 KarachaiCherkessian Republic, Russia
^{88} SubDepartment of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
^{89} The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, 106 91 Stockholm, Sweden
^{90} UPMC Univ Paris 06, UMR7095, 98bis Boulevard Arago, 75014 Paris, France
^{91} Université de Toulouse, UPSOMP, IRAP, 31028 Toulouse Cedex 4, France
^{92} University of Granada, Departamento de Física Teórica y del Cosmos, Facultad de Ciencias, 18071 Granada, Spain
^{93} University of Granada, Instituto Carlos I de Física Teórica y Computacional, 18071 Granada, Spain
^{94} Warsaw University Observatory, Aleje Ujazdowskie 4, 00478 Warszawa, Poland
^{⋆}
Corresponding author: L. Perotto, email: laurence.perotto@lpsc.in2p3.fr
Received: 9 December 2015
Accepted: 7 September 2016
The secondary cosmic microwave background (CMB) Bmodes stem from the postdecoupling distortion of the polarization Emodes due to the gravitational lensing effect of largescale structures. These lensinginduced Bmodes constitute both a valuable probe of the dark matter distribution and an important contaminant for the extraction of the primary CMB Bmodes from inflation. Planck provides accurate nearly allsky measurements of both the polarization Emodes and the integrated mass distribution via the reconstruction of the CMB lensing potential. By combining these two data products, we have produced an allsky template map of the lensinginduced Bmodes using a realspace algorithm that minimizes the impact of sky masks. The crosscorrelation of this template with an observed (primordial and secondary) Bmode map can be used to measure the lensing Bmode power spectrum at multipoles up to 2000. In particular, when crosscorrelating with the Bmode contribution directly derived from the Planck polarization maps, we obtain lensinginduced Bmode power spectrum measurement at a significance level of 12σ, which agrees with the theoretical expectation derived from the Planck bestfit Λ cold dark matter model. This unique nearly allsky secondary Bmode template, which includes the lensinginduced information from intermediate to small (10 ≲ ℓ ≲ 1000) angular scales, is delivered as part of the Planck 2015 public data release. It will be particularly useful for experiments searching for primordial Bmodes, such as BICEP2/Keck Array or LiteBIRD, since it will enable an estimate to be made of the lensinginduced contribution to the measured total CMB Bmodes.
Key words: cosmology: observations / cosmic background radiation / polarization / gravitational lensing: weak
© ESO, 2016
1. Introduction
Cosmic microwave background (CMB) polarization anisotropies can be decomposed into curlfree Emodes and gradientfree Bmodes. In contrast to primordial Emodes, primordial Bmodes are sourced only by tensor perturbations (Polnarev 1985; Spergel & Zaldarriaga 1997; Kamionkowski et al. 1997; Seljak & Zaldarriaga 1997) that can be formed in the predecoupling Universe due to an early inflationary phase (Grishchuk 1975; Starobinsky 1979, 1982). Thus, primordial Bmodes of the CMB polarization are a direct probe of cosmological inflation (see Guth 1981; Linde 1982, for details on inflationary theory). The measurement of the primordial Bmode power spectrum, which peaks at degree angular scales, is the main target of a plethora of groundbased experiments and satellite proposals. There was great excitement in early 2014 when Bmodes at the relevant angular scales detected by the BICEP2 experiment were interpreted as evidence of inflationary gravitational waves (Ade et al. 2014a). Investigating the polarized dust emission in the BICEP2 observation field using the 353GHz data, Planck^{1} revealed a higher dust contamination level than expected from prePlanck foreground models (Planck Collaboration Int. XXX 2016). In BICEP2/Keck Array and Planck Collaborations (2015), a joint analysis of the BICEP2/Keck Array data at 100 and 150 GHz and the fullmission Planck data (particularly the 353GHz polarized data) has been conducted. This provides the stateoftheart constraints on the tensortoscalar ratio, r, which is currently consistent with no detection of a primordial Bmode signal. When combined with the limit derived from the temperature data (as discussed in Planck Collaboration XVI 2014 and Planck Collaboration XIII 2016), the current 95% upper limit is r< 0.08, which already rules out some of the simplest inflationary potentials (Planck Collaboration XX 2016). We stand at the threshold of a particularly exciting epoch that is marked by several ongoing or nearfuture groundbased experimental efforts, based on technology that is sensitive and mature enough to probe the primordial Bmodes to theoretically interesting levels.
In addition to the primordial contribution, a secondary contribution is expected from the postdecoupling distortion of the CMB polarization due to the effect of gravitational lensing (see Lewis & Challinor 2006, for a review of CMB lensing). In particular, the lensing of the primordial CMB polarization Emodes leads to an additional Bmode contribution. The secondary Bmode contribution to the ${\mathit{C}}_{\mathit{\ell}}^{\mathit{BB}}$ power spectrum dominates over the primary one at ℓ ≳ 150, even for large values of the tensortoscalar ratio, (r ~ 1). Thus, it must be corrected for, in order to measure the imprint of primordial tensor modes. This correction is generally referred to as “delensing”.
The secondary Bmode power spectrum can be estimated by crosscorrelating the total observed Bmode map with a template constructed by combining a tracer of the gravitational potential and an estimate of the primordial Emodes. Using such a crosscorrelation approach, the SPTpol team (Hanson et al. 2013) reported the first estimate of the lensing Bmode power spectrum, consisting of a roughly ≲8σ measurement in the multipole range 300 <ℓ < 2750 using HerschelSPIRE data as the mass tracer.The POLARBEAR collaboration detected the lensing Bmodes using CMB polarization data by fitting an amplitude relative to the theoretical expectations to their CMB polarization trispectrum measurements, and reported a 4.2σ rejection of the nullhypothesis (Ade et al. 2014b). Similarly, the ACTPol team reported 3.2σ evidence of the lensing Bmode signal within its first season data, using the correlation of the lensing potential estimate and the cosmic infrared background fluctuations measured by Planck (van Engelen et al. 2015).Finally, using the full mission temperature and polarization data, Planck obtained a templatebased crosscorrelation measurement of the lensing Bmode power spectrum that covers the multipole range 100 < ℓ < 2000, at a significance level of approximately 10σ, as described in Planck Collaboration XV (2016).
Secondary Bmodes dominate any potential primordial Bmodes at high multipoles, thus the highℓBB power spectrum of the observed polarization maps can also be used to make a lensinginduced Bmode measurement.The POLARBEAR collaboration reported the first BB measurement (at around 2σ) of the Bmode power spectrum in the multipole range 500 < ℓ < 2100 (The Polarbear Collaboration 2014). The SPTpol experiment also made a BB estimate of the lensing Bmodes in the range 300 < ℓ < 2300, representing a >4σ detection Keisler et al. (2015). Moreover, a nonzero lensing Bmode signal has been found in the BICEP2/Keck Array data with around 7σ significance, by fitting a freelyfloating CMB lensing amplitude in the joint analysis with Planck data (BICEP2/Keck Array and Planck Collaborations 2015).
For current or future experiments targeting the detection of primordial Bmodes, a precise estimation of the secondary CMB Bmodes at large and intermediate angular scales is required in order to separate the secondary contributions from potential primordial Bmodes.On the one hand, large angular scale experiments lack the highresolution Emode measurements that are required to measure the lensinginduced Bmode signal. On the other hand, for highresolution experiments, partial sky coverage limits their ability to extract the Bmode power spectrum and to reconstruct the lensing potential at large angular scales.Thus, such experiments would benefit from a preestimated secondary Bmode template, covering angular scales from a few degrees down to subdegree scales and matching their sky coverage.
We present an allsky secondary Bmode template spanning from intermediate to large angular scales, synthesized using the full mission Planck data. In Planck Collaboration XV (2016), the lensing Bmode estimate was bandlimited to ℓ> 100, in order to conservatively alleviate any lowℓ systematic effects. In contrast, here the focus is on improving the reliability at intermediate angular scales (10 <ℓ< 200). We also extend the lensing Bmode results of Planck Collaboration XV (2016) by producing a lensing Bmode map, by performing extensive characterization and robustness tests of this template map and by discussing its utility for Bmode oriented experiments. This Bmode map is delivered as part of the Planck 2015 data release.
The outline of this paper is as follows. Section 2 describes the data and simulations that we use. We detail the methodology for the template synthesis in Sect. 3, and describe the construction of the mask in Sect. 4. The lensing Bmode template reconstruction method is validated using simulations in Sect. 5. We present the template we have obtained from Planck foregroundcleaned data in Sect. 6, and assess its robustness against foreground contamination and the choice of the data to crosscorrelate with in Sect. 7. Section 8 addresses the implications of the template for external experiments targeting primordial Bmode searches. We summarize and conclude in Sect. 9.
2. Data and simulations
Planck sky maps:we have used foregroundcleaned CMB temperature and polarization maps derived from the Planck satellite full mission frequency channel maps from 30 to 857 GHz in temperature and 30 to 353 GHz in polarization (Planck Collaboration I 2016; Planck Collaboration II 2016; Planck Collaboration III 2016; Planck Collaboration IV 2016; Planck Collaboration V 2016; Planck Collaboration VI 2016; Planck Collaboration VII 2016; Planck Collaboration VIII 2016). Our main results are based on Stokes I, Q, and U maps constructed using the SMICA componentseparation algorithm (Delabrouille et al. 2003) in temperature and polarization simultaneously (Planck Collaboration IX 2016). The maps are at 5′ resolution in N_{side} = 2048HEALPix pixelization (Górski et al. 2005)^{2}. For the sake of assessing the robustness of our results, we have also utilized foregroundcleaned maps that are produced using the other Planck componentseparation methods, namely Commander, NILC, and SEVEM (Planck Collaboration XII 2014; Planck Collaboration IX 2016; Planck Collaboration X 2016).The current publicly available Planck HFI polarization maps, which are part of the Planck 2015 data release, are highpass filtered at ℓ ≲ 30 because of residual systematic effects on angular scales greater than 10° (Planck Collaboration VII 2016; Planck Collaboration VIII 2016). However, we have used polarization maps covering all angular scale for our analysis, since the results have proved not to be sensitive to CMB Emode polarization at large angular scales^{3}.
Full Focal Plane simulations:for methodological validation and for the bias correction of the lensing potential at the map level (known as the “meanfield” correction), we have relied on the eighth Planck Full Focal Plane (FFP8 hereafter) suite of simulations, as described in Planck Collaboration XII (2016). Specifically, we have used FFP8 MonteCarlo realizations of the Stokes I, Q, and U outputs of the SMICA componentseparation method. These have been obtained by processing through the SMICA algorithm the simulated beamconvolved CMB and noise realizations of the nine Planck frequency channels, as described in Planck Collaboration IX (2016). As a result, both the noise realizations and the beam transfer function are representative of those of the SMICA foregroundcleaned maps. Finally, the calibration of the Planck 2015 data has been taken into account by rescaling the CMB realizations as in Planck Collaboration XV (2016).
Fiducial cosmology:for normalizing the lensing potential map estimate and computing the filter and transfer functions of the Bmode template, we have used fiducial power spectra derived from the 2015 Planck base ΛCDM cosmological parameters that have been determined from the combination of the 2015 temperature and “lowP” likelihoods, as described in Planck Collaboration XIII (2016).
3. Bmode map reconstruction
3.1. Formalism
The secondary Bmodes of CMB polarization arise from a leakage of a fraction of the Emodes into Bmodes due to the polarization remapping induced by the CMB lensing effect. In terms of the polarization spintwo components _{± 2}P ≡ Q ± iU, and at first order in the lensing potential φ, the lensinginduced contribution reads ${\mathrm{\pm}\mathrm{2}}_{}{\mathit{P}}^{\mathrm{lens}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{=}{\mathrm{\nabla}}_{\mathrm{\pm}\mathrm{2}}{\mathit{P}}^{\mathrm{prim}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{\xb7}\mathrm{\nabla}\mathit{\phi}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathit{,}$(1)where ${}_{\mathrm{\pm}\mathrm{2}}\mathit{P}^{\mathrm{prim}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}$ are the polarization fields that would be observed in the absence of the lensing effect (Zaldarriaga & Seljak 1998; Lewis & Challinor 2006). Rewriting the secondary polarization fields in terms of the rotationally invariant E and Bmode fields, so that ${\mathrm{\pm}\mathrm{2}}_{}{\mathit{P}}^{\mathrm{lens}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{=}\mathrm{\nabla}\left[\sum _{{\mathit{\ell}}^{\mathrm{\prime}}{\mathit{m}}^{\mathrm{\prime}}}\mathrm{(}{\mathit{E}}_{{\mathit{\ell}}^{\mathrm{\prime}}{\mathit{m}}^{\mathrm{\prime}}}^{\mathrm{prim}}\mathrm{\pm}\mathrm{i}{{\mathit{B}}_{{\mathit{\ell}}^{\mathrm{\prime}}{\mathit{m}}^{\mathrm{\prime}}}^{\mathrm{prim}}}^{\mathrm{)}}{\mathrm{\pm}\mathrm{2}}_{}{\mathit{Y}}_{{\mathit{\ell}}^{\mathrm{\prime}}{\mathit{m}}^{\mathrm{\prime}}}\right]\mathrm{\xb7}\mathrm{\nabla}\mathit{\phi}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathit{,}$(2)and considering their spintwo sphericalharmonic coefficients ${\mathrm{\pm}\mathrm{2}}_{}{\mathit{P}}_{\mathit{\ell m}}^{\mathrm{lens}}\mathrm{=}\mathrm{\int}\mathrm{d}\stackrel{\u02c6}{{n}\hspace{0.17em}}{\hspace{0.17em}}_{\mathrm{\pm}\mathrm{2}}{\mathit{P}}^{\mathrm{lens}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}{\hspace{0.17em}}_{\mathrm{\pm}\mathrm{2}}{\mathit{Y}}_{\mathit{\ell m}}^{\mathrm{\ast}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathit{,}$(3)one finds that the gradientfree Bmode polarization receives a secondary contribution that depends on the primordial Bmodes and the unlensed curlfree Emodes, of the form ${\mathit{B}}_{\mathit{\ell m}}^{\mathrm{lens}}\mathrm{=}\frac{\mathrm{1}}{\mathrm{2}\mathrm{i}}{\mathrm{(}}_{\mathrm{+}\mathrm{2}}{\mathit{P}}_{\mathit{\ell m}}^{\mathrm{lens}}{\mathrm{}}_{2}{{\mathit{P}}_{\mathit{\ell m}}^{\mathrm{lens}}}^{\mathrm{)}}\mathit{.}$(4)
3.2. Algorithm
First, we state the assumptions on which our algorithm is based. Since the Emode amplitude is at least an order of magnitude greater than the primordial Bmode amplitude, the ${\mathit{B}}_{\mathit{\ell m}}^{\mathrm{lens}}$ contribution that comes from the Emode remapping largely dominates over the one from the lensing perturbation of the primordial Bmodes. From now on, the latter can safely be neglected, consistent with the assumptions in Planck Collaboration XV (2016). We replace the primordial Emodes that appear in Eq. (2) with the total Emodes, E = E^{prim} + δE. This amounts to neglecting the secondorder contribution to B^{lens} due to δE, that is to say the lensing perturbation of the Emodes themselves.
We then consider pure E polarization fields: ${\mathrm{\pm}\mathrm{2}}_{}{\mathit{P}}^{\mathit{E}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{\equiv}{\mathit{Q}}^{\mathit{E}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{+}\mathit{i}{\mathit{U}}^{\mathit{E}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{\equiv}\sum _{\mathit{\ell m}}{\mathit{E}}_{\mathit{\ell m}}{\hspace{0.17em}}_{\mathrm{\pm}\mathrm{2}}{\mathit{Y}}_{\mathit{\ell m}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathit{,}$(5)which define pureE Stokes parameters Q^{E}, U^{E}.
Implementing the above assumptions into Eq. (3) and using the definition given in Eq. (5), we build a secondary polarization estimator that has the generic form ${\mathrm{\pm}\mathrm{2}}_{}\mathit{P\u0302}\begin{array}{c}\mathrm{lens}\\ \mathit{\ell m}\end{array}\mathrm{=}{\mathrm{\mathcal{B}}}_{\mathit{\ell}}^{1}\mathrm{\int}\mathrm{d}\stackrel{\u02c6}{{n}\hspace{0.17em}}\hspace{0.17em}\hspace{0.17em}{\mathrm{\nabla}}_{\mathrm{\pm}\mathrm{2}}\begin{array}{c}\mathrm{\U0010ff66}\\ {\mathit{P}}^{\mathit{E}}\end{array}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{\xb7}\mathrm{\nabla}\begin{array}{c}\mathrm{\U0010ff65}\\ \mathit{\phi}\end{array}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\hspace{0.17em}{\hspace{0.17em}}_{\mathrm{\pm}\mathrm{2}}{\mathit{Y}}_{\mathit{\ell m}}^{\mathrm{\ast}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathit{,}$(6)where ${}_{\mathrm{\pm}\mathrm{2}}\begin{array}{c}{}_{\mathrm{\U0010ff66}}\\ {\mathit{P}}^{\mathit{E}}\end{array}$ and $\begin{array}{c}{\mathrm{\U0010ff65}}^{}\\ \mathit{\phi}\end{array}$ are the filtered versions of the pureE polarization and lensing potential fields, respectively, whereas ℬ_{ℓ} is a transfer function ensuring that the estimator is unbiased. These quantities are defined below in Sect. 3.4. We finally define secondary CMB Bmode template Stokes maps $\mathrm{\left(}{\mathit{Q}}^{\mathrm{lens}}\mathrm{\right(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\left)}\mathit{,}{\mathit{U}}^{\mathrm{lens}}\mathrm{\right(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\left)}\mathrm{\right)}$ by preserving the Bmode contribution in Eq. (6) and transforming back to real space.
In summary, we reconstruct the allsky Bmode template using a dedicated pipeline that consists of:

(i)
estimation of the deflection field using the filteredreconstructed gravitational potential,$\mathrm{\nabla}\begin{array}{c}{}^{\mathrm{\U0010ff65}}\\ \mathit{\phi}\end{array}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}$;

(ii)
computation of the gradient of the filtered pure Emode input maps, ${\mathrm{\nabla}}_{\mathrm{\pm}\mathrm{2}}\begin{array}{c}{}_{\mathrm{\U0010ff66}}\\ {\mathit{P}}^{\mathit{E}}\end{array}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}$;

(iii)
calculation of the analytical transfer function;

(iv)
construction of the polarization template using Eq. (6);

(v)
formation of a secondary Bmode template using Eq. (4).
These steps are further detailed in the rest of this section.
3.3. Allsky lensing potential reconstruction
The paths of CMB photons are weakly deflected by the matter encountered along the way from the lastscattering surface. As a result, the primary CMB observables are remapped according to the gradient of the gravitational potential φ integrated along the lineofsight (Blanchard & Schneider 1987). This induces higherorder correlations within the CMB observables; namely, a nonvanishing connected part of the fourpoint correlation function, or equivalently in the spherical harmonic domain, a trispectrum, in the CMB maps. These can be used, in turn, to reconstruct the intervening mass distribution (Bernardeau 1997; Zaldarriaga & Seljak 1999). Specifically, to first order in φ, the lensing induces a correlation between the observed (lensed) CMB maps and the gradient of the primary (unlensed) maps. Building upon this property, quadratic estimators have been proposed to extract a lensing potential estimate from the observed map (Hu 2001b,a; Hu & Okamoto 2002; Okamoto & Hu 2003). We have reconstructed the lensing potential over a large portion of the sky using the allsky quadratic estimator described in Okamoto & Hu (2003), which has been modified to deal with cut skies.
3.3.1. Inpainting of the temperature map
In Planck Collaboration XV (2016), foregroundcontaminated regions have been masked out at the stage of the inversevariance filtering of the input CMB maps, by allocating infinite variance to masked pixels. The reconstructed φ is thus nullvalued in the pixels inside the analysis mask. For the sake of synthesizing Stokes maps $\mathrm{\left(}{\mathit{Q}}^{\mathrm{lens}}\mathrm{\right(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\left)}\mathit{,}{\mathit{U}}^{\mathrm{lens}}\mathrm{\right(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\left)}\mathrm{\right)}$, as described in Sect. 3.2, using such a masked φ estimate would induce prohibitive amounts of mode mixing. Thus, we have used the METIS method, in which the masked CMB maps are restored to a complete sky coverage, before their ingestion into the quadratic estimator, by means of an inpainting procedure based on the “sparsity” concept (Abrial et al. 2007). More details are given in Perotto et al. (2010), where this method has been first described and in Planck Collaboration XVII (2014), where it has been used to perform consistency tests. As a result of this procedure, the METIS method provides a φ estimate that is effectively inpainted to cover the full sky. To illustrate this property, Fig. 1 shows a Wienerfiltered version of the φ estimate reconstructed from the SMICA temperature map using the baseline “L80” lensing mask that we describe below in Sect. 4.
As well as offering the advantage of mitigating the bias that the mask induces in the φ map, which is discussed in Sect. 3.3.2, this allows us to construct the secondary polarization template map using Eq. (6), alleviating the need for further processing steps to deal with partial sky coverage.
Fig. 1 Wienerfiltered lensing potential estimated from the SMICA foregroundcleaned temperature map using the f_{sky} ≃ 80% lensing mask. The lensing potential estimate, which is shown in Galactic coordinates, is effectively inpainted using a lensing extraction method that relies on an inpainting of the input temperature map, as discussed in Sect. 3.3.1. 
3.3.2. Meanfield debiasing
The quadratic estimator is based on the fact that, for a fixed lens distribution, the lensing breaks the statistical isotropy of the CMB maps; specifically, it introduces offdiagonal terms of the CMB covariance (Hu & Okamoto 2002). Therefore this is also sensitive to any other source of statistical anisotropies in the maps. For Planck data, the bias induced at the φ map level by any known sources of statistical anisotropies, which is referred to as the “meanfield bias”, is dominated by the effects of masking (Planck Collaboration XVII 2014). The meanfield bias can be estimated from MonteCarlo (MC) simulations that include all the instrumental and observational effects that can lead to a sizeable meanfield (e.g. the mask, the spatial inhomogeneity in the noise, which yields the first subdominant mean field, and the beam asymmetry), by averaging the φ estimates obtained on MC realizations. We have used a set of 100 FFP8 realizations to obtain an estimate $\mathrm{\u27e8}\mathit{\phi \u0305}{}_{\mathrm{LM}}\mathrm{\u27e9}_{\mathrm{MC}}$ of the meanfield modes^{4} for the nonnormalized φ modes, labelled . This meanfield estimate has then been subtracted from to obtain the unbiased estimate of φ in the spherical harmonic domain, given by $\mathit{\phi \u0302}\mathrm{LM}\mathrm{=}{\mathrm{\mathcal{A}}}_{\mathrm{L}}\left(\mathit{\phi \u0305}\mathrm{LM}\mathrm{}\mathrm{\u27e8}\mathit{\phi \u0305}\mathrm{LM}{\mathrm{\u27e9}}_{\mathrm{MC}}\right)\mathit{,}$(7)where is the normalization function, which ensures that the estimator is unbiased. This is related to the normalization ${\mathit{A}}_{\mathrm{L}}^{\mathit{\alpha}}$ given in Okamoto & Hu (2003)^{5}, via ${\mathrm{\mathcal{A}}}_{\mathrm{L}}\mathrm{=}\mathrm{\left[}\mathit{L}\mathrm{\right(}\mathit{L}\mathrm{+}\mathrm{1}\mathrm{)}{\mathrm{]}}^{1}{\mathit{A}}_{\mathrm{L}}^{\mathit{\alpha}}$, and has been analytically calculated using the fiducial cosmology described in Sect. 2. To handle the slight difference between FFP8 input cosmology and the fiducial cosmology considered here, the meanfield $\mathrm{\u27e8}\mathit{\phi \u0305}{}_{\mathrm{LM}}\mathrm{\u27e9}_{\mathrm{MC}}$ has been multiplied by the ratio of the normalization functions derived from the input FFP8 and fiducial cosmological models.
3.3.3. Mass tracer choice
In addition to the lensing potential quadratic estimate, other tracers of the underlying lensing potential could be used to form a lensinginduced Bmode template. The cosmic infrared background (CIB) emission is of particular interest for this purpose since, in contrast to most of the largescale structure tracers, which probe only a limited range of redshifts; its redshift distribution has a broad overlap with the lensing potential kernel (Song et al. 2003). Using the bestfit halobased model of Planck Collaboration XVIII (2011), Planck Collaboration XVIII (2014) have reported a roughly 80% correlation of the CIB fluctuations measured by Planck with the lensing potential, in agreement with the model expectations. For the sake of the lensing Bmode measurement, however, the uncertainties in the CIB modelling will have a large impact on the signal estimate, unless the CIB model parameters are marginalized within a joint analysis including lensing cross and autopower spectrum measurements of the CIB (Sherwin & Schmittfull 2015). Moreover, the foreground residuals are another concern for any lensing Bmode template synthesized from the CIB, as also discussed in Sherwin & Schmittfull (2015). The CIB signal is the most precisely measured at high frequencies, where the Galactic dust emission is also important. Any Galactic dust residuals in the CIB template map could be correlated either with the polarized dust residuals or with the intensitytopolarization leakage of the dust emission in the CMB E and Bmode maps.
Similarly, lensing potential estimates can also be extracted by means of a quadratic estimator on the Planck polarization maps. This, combined with the temperaturebased φ estimate, reduces the power spectrum of the φ reconstruction noise by roughly 25%. However, for measuring the lensing Bmode power spectrum using a templatebased approach, resorting to a polarizationbased φ estimate would require us to correct for a nonnegligible Gaussian bias (Planck Collaboration XV 2016; Namikawa & Nagata 2014).
Here we have chosen to employ only the lensing potential estimate to produce a lensing Bmode template that is modelindependent and more robust to foreground residuals; and to use the temperature data only for estimating the lensing potential, which ensures desirable properties for our template, as discussed in Sect. 5. Relying on the independent analysis presented in Planck Collaboration XV (2016), we show in Sect. 7.4 that these choices induce at worst a marginal increase in the statistical uncertainties of the lensing Bmode measurements.
3.4. Lensinginduced polarization fields
Using the lensing potential estimate discussed above and the observed Emode map, we have reconstructed the template of the secondary polarization field as in Eq. (6). To reduce uncertainties, we have used filtered versions of those maps that are defined as $\begin{array}{c}\mathrm{\U0010ff65}\\ \mathit{\phi}\end{array}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{=}\mathrm{\int}\mathrm{d}\stackrel{\u02c6}{{n}\hspace{0.17em}}\hspace{0.17em}\hspace{0.17em}{\mathit{f}}_{\mathrm{L}}^{\mathit{\phi}}\hspace{0.17em}\mathit{\phi \u0302}\mathrm{LM}\hspace{0.17em}{\mathit{Y}}_{\mathrm{LM}}^{\mathrm{\ast}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathit{,}$(8)and ${\mathrm{\pm}\mathrm{2}}_{}\begin{array}{c}\mathrm{\U0010ff66}\\ {\mathit{P}}^{\mathit{E}}\end{array}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathrm{=}\mathrm{\int}\mathrm{d}\stackrel{\u02c6}{{n}\hspace{0.17em}}\hspace{0.17em}\hspace{0.17em}{\mathit{f}}_{\mathit{\ell}}^{\mathit{E}}\hspace{0.17em}{\mathit{E}}_{\mathit{\ell m}}\hspace{0.17em}{\hspace{0.17em}}_{\mathrm{\pm}\mathrm{2}}{\mathit{Y}}_{\mathit{\ell m}}^{\mathrm{\ast}}\mathrm{\left(}\stackrel{\u02c6}{{n}\hspace{0.17em}}\mathrm{\right)}\mathit{.}$(9)The filter functions for φ and E, ${\mathit{f}}_{\mathrm{L}}^{\mathit{\phi}}$ and ${\mathit{f}}_{\mathit{\ell}}^{\mathit{E}}$, are Wiener filters, based on the optimality arguments developed in Smith et al. (2009a). In Planck Collaboration XV (2016), the φ estimates at L< 8 have been discarded because of instability to the choice of the method used to correct the meanfield. Consistently, we have filtered the φ estimate to L ≤ 10 in order to conservatively avoid any meanfield related issues. We have used a tapering filter, labelled f_{10}, that smoothly goes from zero at L = 5 to unity at L = 15 by means of a powerofcosine function centred in L = 10. Using this filter, we still preserve 99% of the available information for measuring the crosscorrelation Bmode power spectrum. The filtered pureE polarization fields ${}_{\mathrm{\pm}\mathrm{2}}\begin{array}{c}{}_{\mathrm{\U0010ff66}}\\ {\mathit{P}}^{\mathit{E}}\end{array}$ have been directly obtained from the fullsky observed Q and U maps by transforming into the spinweighted spherical harmonic basis, filtering the Emodes, and reforming Stokes parameter fields with a null Bmode component. No deconvolution of the beam has been performed at this stage, which yields further filtering of the Emodes at high multipoles. Our filtering functions are defined by $\begin{array}{ccc}{\mathit{f}}_{\mathrm{L}}^{\mathit{\phi}}& \mathrm{=}& \frac{{\mathit{f}}_{\mathrm{10}}{\mathit{C}}_{\mathrm{L}}^{\mathit{\phi ,}\mathrm{fid}}}{{\mathit{C}}_{\mathrm{L}}^{\mathit{\phi ,}\mathrm{fid}}\mathrm{+}{\mathit{N}}_{\mathrm{L}}^{\mathit{\phi}}}\mathit{,}\\ {\mathit{f}}_{\mathit{\ell}}^{\mathit{E}}& \mathrm{=}& \end{array}$(10)where ${\mathit{C}}_{\mathrm{L}}^{\mathit{\phi}}$ and ${\mathit{C}}_{\mathit{\ell}}^{\mathit{E}}$ are the fiducial φ and Emode power spectra; ${\mathit{N}}_{\mathrm{L}}^{\mathit{\phi}}$ is the φ reconstruction noise power spectrum calculated following Okamoto & Hu (2003); and ${\mathit{N}}_{\mathrm{L}}^{\mathit{E}}$ is the pixel and beamdeconvolved power spectrum of the Emode noise.
These steps have been performed using the fast spinweighted spherical harmonic transform capability of the HEALPix library to generate Q^{E} and U^{E} and compute their derivatives. Thanks to this simple implementation, a Bmode template map at a resolution of 5′ can be reconstructed from the φ estimate and the observed Q and U maps in a reasonable amount of computing time, which enables the use of MonteCarlo simulations. For example, the computing time is about two minutes using eight cores of the Linux AMD64 machines of the Institut National de Physique Nucléaire et de Physique des Particules (IN2P3) Computing Center^{6}.
Using a harmonic approach, as in Hu (2000), we compute the transfer function that appears in Eq. (6) by imposing the condition that the secondary Bmode template satisfies $\mathrm{\u27e8}{\mathit{B}}_{\mathit{\ell m}}^{\mathrm{\ast}}\mathit{B\u0302}\begin{array}{c}\mathrm{lens}\\ {\mathit{\ell}}^{\mathrm{\prime}}{\mathit{m}}^{\mathrm{\prime}}\end{array}\mathrm{\u27e9}\mathrm{=}{\mathit{\delta}}_{\mathit{\ell}{\mathit{\ell}}^{\mathrm{\prime}}}{\mathit{\delta}}_{\mathit{m}{\mathit{m}}^{\mathrm{\prime}}}\hspace{0.17em}{\mathit{C}}_{\mathit{\ell}}^{\mathit{B,}\mathrm{fid}}\mathit{,}$(11)where ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B,}\mathrm{fid}}$ is the fiducial lensinginduced Bmode power spectrum (r = 0).
In terms of the fiducial power spectra ${\mathit{C}}_{\mathit{\ell}}^{\mathit{X,}\mathrm{fid}}$, X = { E,B,φ }, we obtain a transfer function ${\mathrm{\mathcal{B}}}_{\mathit{\ell}}\mathrm{=}\frac{\mathrm{1}}{{\mathit{C}}_{\mathit{\ell}}^{\mathit{B,}\mathrm{fid}}}\sum _{\mathrm{L}{\mathit{\ell}}^{\mathrm{\prime}}}{\mathit{f}}_{\mathrm{L}}^{\mathit{\phi}}{\mathit{C}}_{\mathrm{L}}^{\mathit{\phi ,}\mathrm{fid}}\hspace{0.17em}{\mathit{f}}_{{\mathit{\ell}}^{\mathrm{\prime}}}^{\mathit{E}}{\mathit{B}}_{{\mathit{\ell}}^{\mathrm{\prime}}}{\mathit{C}}_{{\mathit{\ell}}^{\mathrm{\prime}}}^{\mathit{E,}\mathrm{fid}}{\hspace{0.17em}}_{\mathrm{2}}{\mathit{F}}_{\mathit{\ell}\mathrm{L}{\mathit{\ell}}^{\mathrm{\prime}}}\mathit{,}$(12)where B_{ℓ′} is the beam function of the polarization maps, and _{2}F_{ℓLℓ′} is a geometrical term defined in Hu (2000).
3.5. Bmode template synthesis
Our secondary Bmode template is obtained as in Eq. (4) that is $\mathit{B\u0302}\begin{array}{c}\mathrm{lens}\\ \mathit{\ell m}\end{array}\mathrm{=}\frac{\mathrm{1}}{\mathrm{2}\mathrm{i}}{\mathrm{(}}_{\mathrm{+}\mathrm{2}}\mathit{P\u0302}\begin{array}{c}\mathrm{lens}\\ \mathit{\ell m}\end{array}{\mathrm{}}_{2}\mathit{P\u0302}{\begin{array}{c}\mathrm{lens}\\ \mathit{\ell m}\end{array}}^{\mathrm{)}}\mathit{.}$(13)This is computed from ${}_{\mathrm{\pm}\mathrm{2}}\mathit{P\u0302}\begin{array}{c}\mathrm{lens}\\ \mathit{\ell m}\end{array}$, the spinweighted spherical harmonic transforms of our realspace secondary polarization estimates ${}^{\mathrm{(}}\mathit{Q}^{\mathrm{lens}}\mathrm{\pm}\mathrm{i}{\mathit{U}}^{\mathrm{lens}}{\mathrm{)}}^{}$ that are corrected for the transfer function given in Eq. (12).
3.6. Crosscorrelation power spectrum of the template
We form the crosscorrelation power spectrum between the template Bmodes given in Eq. (13) and the observed Bmodes, ${\mathit{B}}_{\mathit{\ell m}}^{\mathrm{obs}}$, using $\mathit{C\u0302}\begin{array}{c}\mathit{B}{\mathit{B}}^{\mathrm{lens}}\\ \mathit{\ell}\end{array}\mathrm{=}\frac{\mathrm{1}}{{\mathit{f}}_{\mathrm{sky}}^{\mathrm{eff}}\mathrm{(}\mathrm{2}\mathit{\ell}\mathrm{+}\mathrm{1}\mathrm{)}}\sum _{\mathit{m}\mathrm{=}\mathrm{}\mathit{\ell}}^{\mathit{\ell}}{\mathit{B}}_{\mathit{\ell m}}^{\mathrm{obs}\hspace{0.17em}\mathrm{\ast}}\stackrel{}{{{\mathit{B}}_{\mathit{\ell m}}^{\mathrm{lens}}}_{\mathrm{\u02dc}}}\mathit{,}$(14)where the asterisk denotes complex conjugation; and $\stackrel{}{{{\mathit{B}}_{\mathit{\ell m}}^{\mathrm{lens}}}_{\mathrm{\u02dc}}}$ is a shorthand notation for the template Bmode harmonic coefficients obtained as in Eq. (12), but using an apodized and masked version of the realspace secondary polarization estimates ${}^{\mathrm{(}}\mathit{Q}^{\mathrm{lens}}\mathrm{\pm}\mathrm{i}{\mathit{U}}^{\mathrm{lens}}{\mathrm{)}}^{}$. This apodized mask, the construction of which is described in Sect. 4, leaves an effective available sky fraction ${\mathit{f}}_{\mathrm{sky}}^{\mathrm{eff}}$ for analysis. The BB^{lens} crosscorrelation power spectrum represents an estimate of the lensing Bmode power spectrum. Moreover, this does not require any noise term subtraction, as we verify in Sect. 5.
The BB^{lens} power spectrum variance is estimated to a good approximation using ${\mathit{\sigma}}^{\mathrm{2}}\left(\mathit{C\u0302}\begin{array}{c}\mathit{B}{\mathit{B}}^{\mathrm{lens}}\\ \mathit{\ell}\end{array}\right)\hspace{0.17em}\mathrm{=}\hspace{0.17em}\frac{\mathrm{1}}{{\mathit{f}}_{\mathrm{sky}}^{\mathrm{eff}}\mathrm{(}\mathrm{2}\mathit{\ell}\mathrm{+}\mathrm{1}\mathrm{)}}\left[\mathrm{(}{\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}{\mathrm{)}}^{\mathrm{2}}\mathrm{+}\mathrm{(}\mathit{C\u0302}\begin{array}{c}{\mathit{B}}^{\mathrm{obs}}\\ \mathit{\ell}\end{array}\mathrm{\left)}\mathrm{\right(}\mathit{C\u0302}\begin{array}{c}{\mathit{B}}^{\mathrm{lens}}\\ \mathit{\ell}\end{array}\mathrm{)}\right]\mathit{,}$(15)where $\mathit{C\u0302}\begin{array}{c}{\mathit{B}}^{\mathrm{obs}}\\ \mathit{\ell}\end{array}$ is the autocorrelation power spectrum of the observed Bmodes and $\mathit{C\u0302}\begin{array}{c}{\mathit{B}}^{\mathrm{lens}}\\ \mathit{\ell}\end{array}$ the one of the template. Equation (15) consists of a Gaussian variance prescription (see e.g. Knox 1995), which is not expected to rigorously apply to the lensing Bmode power spectrum estimate, because of its “substructure” (since it is based on the sum of the TTEB trispectrum of the observed CMB signal). However, for a template map constructed on the Planck polarization maps, given the polarization noise level, the higherorder terms that enter the variance are subdominant, as is further discussed and tested in Sect. 5.
4. Construction of the Bmode mask
In this section, we detail the methodology for constructing the template mask. This has involved first preparing a series of foreground masks targeted at specific foreground emission in temperature. These foreground masks have been then combined to construct an analysis mask for the lensing potential reconstruction. Finally, the lensing analysis mask has been modified to define a mask for the template map. These three steps are detailed in Sects. 4.1–4.3 below.
4.1. Foreground masks
Galactic mask
We have masked the regions of the sky that are strongly contaminated by the diffuse Galactic emission, the carbonmonoxide (CO) transition line emission and the extended nearby galaxy emission. This Galactic mask has been produced following the method described in Planck Collaboration XVI (2014). It includes the diffuse Galactic mask described in Planck Collaboration XII (2014), which is produced by thresholding a combination of CMBcorrected temperature maps at 30 and 353 GHz until a desired sky fraction is preserved. For our baseline analysis, we have used a diffuse Galactic mask that retains about 80% of the sky. This diffuse Galactic mask discards mainly low latitude regions. To mask the CO lines contamination at intermediate latitudes, we have used the CO mask described in Appendix A of Planck Collaboration XI (2016), which has been obtained by thresholding a smoothed version of the Type 3 CO map (Planck Collaboration XIII 2014) at 1 K_{RJ} km s^{1}. Furthermore, we have removed the emission from the most extended nearby galaxies, including the two Magellanic clouds (LMC, SMC) and M 31, by cutting a radius that covers each galaxy in the 857GHz map, as described in Planck Collaboration XI (2016). Our Galactic mask, which is the merge of the diffuse Galactic, COline, and extended nearby galaxy masks, consists of large cuts that extend over more than two degrees on the sky, and preserves 79% of the sky.
Extragalactic object masks
We have masked the infrared (IR) and radio point sources that have been detected in the temperature maps in frequency channels from 70 to 353 GHz using the Planck compact object catalogues, as well as the sky areas contaminated by the SunyaevZeldovich (SZ) emission using both Planck SZ cluster catalogues and Compton parameter maps. We started with the individual masks targeted at 100, 143, and 217 GHz that have been used in Planck Collaboration XVII (2014). These masks have been produced using the Planck Early Release Compact Source Catalogue (ERSC; Planck Collaboration VII 2011), the Planck Catalogue of Compact Sources (PCCS; Planck Collaboration XXVIII 2014), and the Planck catalogue of SunyaevZeldovich sources (PSZ; Planck Collaboration XXIX 2014). These have been merged with the conservative pointsource masks produced using the 2015 catalogue (PCCS2; Planck Collaboration XXVI 2016), which are presented in Planck Collaboration XI (2016). The SZ emission hav been further removed using the template Compton parameter y map for the detected galaxy clusters of the 2015 SZ catalogue (PSZ2; Planck Collaboration XXVII 2016) that is described in Planck Collaboration XXII (2016). Individual SZ masks have been constructed for 100, 143, and 217 GHz separately, by converting the template ymap into CMB temperature using the corresponding conversion factors listed in Planck Collaboration XXII (2016), and thresholding at 10 μK. Finally, we have masked several small nearby galaxies including M 33, M 81, M 82, M 101, and CenA, as described in Planck Collaboration XI (2016).
We have combined these individual masks to produce two extragalactic object masks that differ in the maximum cut radius. First, the “extended object mask” is made of holes the largest angular size of which ranges from two degrees to 30′. This includes the extended SZ clusters and the small nearby galaxies. Second, the “compact object mask” is a collection of small holes of cut radius smaller than 30′, and comprises the detected radio and IR point sources and the pointlike SZ clusters. The latter represents a conservative point source mask that includes all the point sources detected above S/N = 5 in the 100, 143, and 217GHz maps, as well as the point sources detected above S/N = 10 in the adjacent frequencies (including 70 and 353 GHz). This has been used in Sect. 7.2 to test the robustness of our results againts point source residuals in the SMICA map.
4.2. Lensing analysis mask
For the lensing potential reconstruction, we have prepared a composite mask targeted at the SMICA temperature map. This map comes along with a “confidence” mask that defines the sky areas where the CMB solution is trusted. The SMICA confidence mask, a thorough description of which is given in Planck Collaboration IX (2016), has been produced by thresholding the CMB power map that is obtained in squaring a bandpass filtered and smoothed version of the SMICA map. Our lensing mask combines the Galactic, extended, and compact object masks after some changes driven by the SMICA confidence mask. Namely, the LMC and three molecular clouds at medium latitudes have been masked more conservatively in the SMICA mask than in our initial Galactic mask. We have enlarged the latter accordingly. In the compact object mask, IR and radio source holes that are not also present in the SMICA confidence mask have been discarded. They mainly corresponds to point sources detected in the 353GHz map, and are strongly weighted down in the SMICA CMB map. The modified compact object mask removes 0.6% of the sky in addition to the 21.4% Galactic and the 0.4% extended object cuts. The baseline lensing mask, which consists of the combination of these three masks, retains 77.6% of the sky and is labelled L80.
In Sect. 7.2, however, we test the stability of our results against source contamination by using a mask accounting for more pointlike and extended sources. This has been constructed as the union of the Galactic, extended, and compact objects and SMICA confidence masks. This mask, in which the cut sky fraction due to point sources is as large as 1.5%, preserves 76% of the sky for analysis and is named L80s.
4.3. Template analysis mask
4.3.1. Methodology for constructing the mask
Given the lensing mask, the construction of the template mask is a tradeoff between preserving a large sky fraction for analysis and alleviating the bias induced by the lensing reconstruction on an incomplete sky. Inpainting the masked temperature map from which the lensing potential is extracted, as described in Sect. 3.3, strongly suppresses this effect. The pointlike holes induce negligible bias in the lensing potential reconstruction provided they are treated by inpainting beforehand (BenoitLévy et al. 2013). Therefore, the compact object mask does not need to be propagated to the template map, as it is verified using MonteCarlo simulations in Sect. 5. However, larger sky cuts performed by the lensing mask (e.g., those arising from the Galactic and extended object masks) have to be applied to the Bmode template. Furthermore, some artefacts may be seen near the mask boundaries, which we refer to as the mask leakage, and which arises from the convolution of the signal with the mask sidelobes when transforming in spherical harmonic space (Plaszczynski et al. 2012). From these considerations, we have tailored a method of constructing the mask template using MonteCarlo simulations: starting with the combination of the Galactic and the extended object masks, we progressively enlarged the mask beyond the boundaries, until we observed a negligible residual bias in the crosscorrelation power spectrum of the template. This has been obtained by extending the Galactic mask 3° beyond the boundaries and the extended compact object mask 30′ beyond. In Sect. 5, we check that using a template mask that are constructed in this fashion allows no significant impact in the BB^{lens} lensing Bmode power spectrum.
4.3.2. The baseline and test template masks
The baseline mask of the lensing Bmode template map has been constructed from the lensing analysis L80 mask using the method described above. Specifically, the Galactic mask has been enlarged 3° beyond the boundaries, removing 30% of the sky, and the extended object mask has been also slightly widened by 30′ beyond the boundaries, removing an additional 1.2% of the sky. The baseline template mask preserves a sky fraction of 69% and is named B70.
In Sect. 7.2, however, we check that consistent results are obtained using either the Galactic mask as it is, without enlargement, or a more conservative Galactic mask that removes 40% of the sky. The most aggressive template mask, labelled B80, leaves 77% of the sky for the analysis, and the most conservative one, named B60, leaves 58%. We also test against extragalactic contamination through using the lensing L80s mask for the lensing potential reconstruction and the corresponding template mask constructed using the method described in Sect. 4.3.1 and labelled B70s. In addition to these masks that are targeted at the temperature map, in Sect. 7.2, we also use a mask tailored for polarization in order to test against polarized foreground contamination. For this purpose, the B70 mask has been combined with the SMICA confidence mask for polarization, a detailed description of which is given in Planck Collaboration IX (2016). The latter removes regions of the sky where the polarization power (which is computed by squaring a lowpass filtersmoothed version of the SMICA polarization map) exceeds 5 μK^{2}. The combined B70 and SMICA confidence mask for polarization is labelled B70p and retains 68% of the sky.
When computing the lensing Bmode power spectrum, we have employed apodized versions of the masks, using a cosine taper of 2° width for the Galactic mask and 30′ width for the extended object mask. As a consequence, effective sky fractions available for the power spectrum are 5–10% lower than the sky fraction of the template analysis masks. A list of the template masks discussed here is given in Table 1, together with the corresponding sky fraction, both with and without apodization.
Template analysis masks.
5. Validation on simulations
We now validate the pipeline described in Sect. 3and test the impact of masking as described in Sect. 4.3 using a MonteCarlo (MC) approach. We analyse our template by forming the BB^{lens} power spectrum given in Eq. (14), which has two objectives:

(i)
to assess that the template encloses the expected lensing Bmodeinformation, thus validating the assumptions on which thesynthesis method relies;

(ii)
to demonstrate its utility for measuring the secondary Bmode power spectrum.
We use two independent sets of 100 SMICAI, Q, and U simulations, part of the FFP8 MC simulation set described in Sect. 2.
5.1. Fullrange power spectrum estimate
We have applied the pipeline described above to the SMICA temperature and Stokes parameter simulations to obtain a set of 100 estimates. For the lensing reconstruction on the temperature simulations, we have used the baseline L80 lensing mask, and employed the second simulation set for the meanfield bias correction. Then, lensing Bmode power spectrum estimates have been formed by crosscorrelating and the input Bmodes as in Eq. (14), and using the apodized version of the B70 mask. We have estimated the lensing Bmode BB^{lens} bandpowers by multiplying Eq. (14) by ℓ(ℓ + 1)/2π and averaging the multipoles over bins of width Δℓ ≥ 100 to further reduce the pseudoC_{ℓ} multipole mixing.
Figure 2 shows the averaged BB^{lens} bandpowers obtained using the apodized B70 mask. The error bars have been estimated using the standard deviation of 100 estimates of the BB^{lens} bandpowers with the apodized B70 mask. The averaged BB^{lens} bandpower residuals, i.e. $\mathrm{\Delta}{\mathit{C}}_{\mathit{b}}^{\mathit{BB}\mathrm{lens}}\mathrm{=}{\sum}_{\mathit{\ell}\mathrm{\in}\mathit{b}}{\mathit{C}}_{\mathit{\ell}}^{\mathit{BB}\mathrm{lens}}\mathrm{}{\mathit{C}}_{\mathit{\ell}}^{\mathit{BB,}\mathrm{fid}}$, are plotted in the lower panel of Fig. 2; this shows a negligible residual bias of ≲ 0.1σ up to multipoles of 2000. Relative to the input lensing Bmode bandpower, this corresponds to less than a percent. To isolate the impact of the inpainting, we have also extracted the lensing Bmodes using the lensing potential reconstructed from the fullsky temperature map, that is without using any mask. For comparison, the bandpower residuals are also plotted for fullsky case in Fig. 2.
Fig. 2 Lensing Bmode power spectrum obtained by crosscorrelating the B^{lens} templates with the corresponding fiducial Bmode simulations (top), and residuals with respect to the model (bottom). Top: averaged BB^{lens} bandpowers using the apodized B70 template mask, with multipole bins of Δℓ ≥ 100 (blue points). The error bars are the standard deviation on the mean of the bandpower estimate set. The dark blue curve is the fiducial Bmode power spectrum of our simulations, which assumes r = 0. Bottom: BB^{lens} bandpower residual with respect to the fiducial model, given in units of the 1σ error of a single realization. For comparison, we also show the bandpower residuals obtained without masking, as discussed in Sect. 5.1 (red points). Dashed lines show the ± 1σ range of 100 realizations, indicating the precision level to which we are able to test against bias. 
We have further tested that the BB^{lens} bandpowers constitute an unbiased estimate of the fiducial lensing Bmodes by fitting an amplitude with respect to the fiducial model. The averaged amplitude A_{Blens} obtained on 100 estimates of the BB^{lens} bandpowers using the B70 mask is 0.989 ± 0.008, where the error has been evaluated using the standard deviation of the A_{Blens} estimates normalized by the square root of the number of realizations. We therefore conclude that our pipeline provides us with an unbiased estimate of A_{Blens}.
It is worth noting that the choice of extracting the lensing potential from the temperatureonly data ensures the absence of Gaussian ${\mathit{N}}_{\mathrm{L}}^{\mathrm{\left(}\mathrm{0}\mathrm{\right)}}$like bias, which must be corrected for in the case of a lensing extraction using Bmode information. It also gives a strong suppression of any higherorder bias terms.
5.2. Statistical error budget
First, we have quantified the statistical error associated with our lensing Bmode bandpower measure via simulations by computing the standard deviation of our MC bandpower estimates. Then, these MC error bars have been compared to semianalytical errors evaluated in taking the square root of the Gaussian variance given in Eq. (15). The autocorrelation Bmode power spectrum of the SMICA simulation has been modelled using ${\mathit{C}}_{\mathit{\ell}}^{{\mathit{B}}^{\mathrm{obs}}}\mathrm{=}{\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}\mathrm{+}{\mathit{B}}_{\mathit{\ell}}^{2}{\mathit{N}}_{\mathit{\ell}}^{\mathit{B}}$, where ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ and ${\mathit{N}}_{\mathit{\ell}}^{\mathit{B}}$ are the MC input signal and noise power spectra and B_{ℓ} is the beam function. For the autocorrelation power spectrum of the template, we have used the averaged estimate on our MC set. Furthermore, we have used the Δℓ ≥ 100 binning function to average the variance over multipoles. We note that these large multipole bins contribute to drive our bandpower estimates close to a normal distribution by virtue of the centrallimit theorem, which in turn, brings the Gaussian variance of Eq. (15) closer to the true variance.
In Fig. 3, we plot the MC error bars and the semianalytical ones. For comparison purposes, we also show the errors one would have obtained from a BB power spectrum measurement by computing the autopower spectrum of the fiducial Bmode map.
Fig. 3 Error budget. We compare the MC derived uncertainties σ_{MC} associated with the BB^{lens} measurements to the semianalytical errors σ_{G} obtained using Eq. (15). Top: averaged BB^{lens} bandpowers using either σ_{MC} (blue) or σ_{G} (red) as error estimates. For illustration, we also show the expected sensitivity of the PlanckSMICA CMB polarization map to the BB bandpowers (grey boxes), whose uncertainties are a factor of four larger than those of the BB^{lens} bandpowers using the lensing Bmode template. Bottom: relative difference of σ_{G} with respect to σ_{MC}. Dashed lines show a 15% difference. 
The uncertainties in our BB^{lens} bandpowers are well approximated by the semianalytical errors at all multipoles. In the lower panel of Fig. 3 we plot the relative difference between the semianalytical errors using Eq. (15) and the error estimates obtained by simulations. Using Eq. (15) leads to a 16% underestimate of the error in the first multipole bin and less than 10% underestimation at higher multipoles. These results validate the use of Eq. (15) to evaluate the templatebased Bmode power spectrum uncertainties. We also find that the uncertainties of the BB^{lens} power spectrum using the template map are approximately four times lower than those of a total Bmode BB measurement coming directly from the Bmode map.
Gathering the results of our MC analysis, we observe that, when used in crosscorrelation with the Bmode map, the lensing Bmode template we compute provides a lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ measurement, which: (i) does not rely on any bias subtraction; (ii) has nearly optimal uncertainty; and (iii) has four times lower uncertainty than the BB measurement on the fiducial Bmode map.
6. Planckderived secondary Bmode template
6.1. Template synthesis
We have produced the template map of the lensing Bmodes by applying the pipeline described in Sect. 3 to the foregroundcleaned temperature and polarization maps obtained using the SMICA componentseparation method, as described in Sect. 2. We have first obtained the and Û^{lens} templates defined in Sect. 3.2, filtered versions of which are plotted in Fig. 4. Specifically, the maps have been smoothed using a Gaussian beam of 1°FWHM to highlight any lowℓ systematic effects, such as those due to intensitytopolarization leakage. This first inspection indicates that these templates are not affected by any obvious lowℓ systematic effects. More rigorous tests, however, are performed in Sect. 7.3 using intensitytopolarization leakage corrected maps.
Fig. 4 SMICA lensinginduced Q and U templates that have been convolved with a Gaussian beam of 60′FWHM to highlight the large angular scales (corresponding to multipoles below 200). No spurious patterns are observed at large angular scales. 
Then we have used the SMICA and Û^{lens} templates to make our secondary Bmode template, as described in Sect. 3.5. For illustration purposes, we have produced a Bmode template map by inverting $\mathit{B\u0302}\begin{array}{c}\mathrm{lens}\\ \mathit{\ell m}\end{array}$ back to pixelspace through an inverse spherical harmonic transform. Although our Bmode template contains information in the multipole range 10 <ℓ< 2000, Fig. 5 shows two filtered versions of the Bmode map to highlight different ranges of angular scale. The highresolution map (which is simply slightly smoothed using a Gaussian beam of 10 ′FWHM) should show any important foreground contamination at small angular scales, whereas the lowresolution one (which is smoothed using a 1° Gaussian beam and downgraded to N_{side} = 256HEALPix resolution) should reveal any large angular scale systematic effects. No evident systematic effects are observed in the maps plotted in Fig. 5. In Sect. 7, we further assess the template robustness against various systematic effects by means of a series of tests at the power spectrum level.
Fig. 5 Planckderived Bmode template map computed using the SMICA foregroundcleaned CMB maps. For illustration, the map has been convolved with a Gaussian beam of 10′ (upper panel) and 60′ (lower panel) FWHM. The grey area represents the L80 mask, which was used at the lensing potential reconstruction stage. No obvious foreground residuals are seen in the highresolution map, nor any obvious systematic effects in the lowresolution one. 
6.2. Variance contributions
In this section, we describe and quantify the various contributions that enter the template map variance. In particular, ranking the sources of variance helps us in quantifying the template variance dependence in the choice of the lensing potential estimates discussed in Sect. 3.3. This also anticipates the discussion that we develop in Sect. 8 on the utility of the Planck template for other experiments that are attempting to measure the lensing Bmodes, compared to the use of a template that combines the Planck lens reconstruction and the experiment’s Emode measurement.
Using the autopower spectrum estimate $\mathit{C\u0302}\begin{array}{c}{\mathit{B}}^{\mathrm{lens}}\\ \mathit{\ell}\end{array}$ computed on the apodized masked template, the template variance is ${\mathit{\sigma}}^{\mathrm{2}}\mathrm{\left(}{\mathit{B}}^{\mathrm{lens}}\mathrm{\right)}\hspace{0.17em}\mathrm{=}\hspace{0.17em}\frac{\mathrm{1}}{{\mathit{f}}_{\mathrm{sky}}^{\mathrm{eff}}\mathrm{(}\mathrm{2}\mathit{\ell}\mathrm{+}\mathrm{1}\mathrm{)}}\mathit{C\u0302}\begin{array}{c}{\mathit{B}}^{\mathrm{lens}}\\ \mathit{\ell}\end{array}\mathit{,}$(16)where ${\mathit{f}}_{\mathrm{sky}}^{\mathrm{eff}}$ is the effective sky fraction that is preserved by the apodized B70 mask. This receives three main contributions: cosmic variance of both the CMB Emodes and the lenses; instrumental noise; and lens reconstruction noise. For the sake of completeness, other subdominant contributions could include foreground residuals, higherorder terms and secondary contractions of the CMB trispectrum (such as the socalled N^{(1)} bias of the lens reconstruction). Within this model, ${\mathit{C}}_{\mathit{\ell}}^{{\mathit{B}}^{\mathrm{lens}}}$ can be analytically calculated using ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B\u0302}\mathrm{lens}}\mathrm{=}{\mathrm{\mathcal{B}}}_{\mathit{\ell}}^{2}\hspace{0.17em}\sum _{\mathrm{L}{\mathit{\ell}}^{\mathrm{\prime}}}\mathrm{\left(}{\mathit{f}}_{\mathrm{L}}^{\mathit{\phi}}{\mathrm{)}}^{\mathrm{2}}\mathrm{\right(}{\mathit{C}}_{\mathrm{L}}^{\mathit{\phi ,}\mathrm{fid}}\mathrm{+}{\mathit{N}}_{\mathrm{L}}^{\mathit{\phi}}\mathrm{)}\hspace{0.17em}\mathrm{(}{\mathit{f}}_{{\mathit{\ell}}^{\mathrm{\prime}}}^{\mathit{E}}{\mathit{B}}_{{\mathit{\ell}}^{\mathrm{\prime}}}{\mathrm{)}}^{\mathrm{2}}\mathrm{(}{\mathit{C}}_{{\mathit{\ell}}^{\mathrm{\prime}}}^{\mathit{E,}\mathrm{fid}}\mathrm{+}{\mathit{N}}_{{\mathit{\ell}}^{\mathrm{\prime}}}^{\mathit{E}}\mathrm{)}{\hspace{0.17em}}_{\mathrm{2}}{\mathit{F}}_{\mathit{\ell L}{\mathit{\ell}}^{\mathrm{\prime}}}\mathit{,}$(17)where the notation is the same as in Eqs. (10) and (12). Although the variance is evaluated using the template power spectrum estimate, Eq. (17) provides us with a useful tool for isolating the relative contributions to the total variance of the template. It can be decomposed into four terms: the “cosmic variance” contribution, which arises from the product of the φ and E power spectra; the “pure noise” contribution, which involves the product of both noise spectra; and two crossterms, namely the “φnoise primed” contribution ${\mathit{N}}_{\mathrm{L}}^{\mathit{\phi}}{\mathit{C}}_{\mathit{\ell}}^{\mathit{E}}$ and the “Enoise primed” contribution ${\mathit{C}}_{\mathrm{L}}^{\mathit{\phi}}{\mathit{N}}_{\mathit{\ell}}^{\mathit{E}}$. In Fig. 6, we plot the different contributions to the total variance of the template.
Fig. 6 Template map variance budget. The total variance of the template, plotted in dark blue, is split into the contribution of the lens reconstruction noise (orange) and Emode noise (green) crossterms; and the pure noise (yellow) and cosmic variance (light blue) terms defined in Sect. 6.2. 
The template variance is dominated by the φnoise primed crossterm, which contributes an amount of about 60% to the total variance. To further quantify the template variance dependence on the φ estimate, we have rescaled ${\mathit{N}}_{\mathrm{L}}^{\mathit{\phi}}$ by a factor of 0.75 in Eq. (17), which represents a simple way to emulate the precision gain that could be obtained by including the polarizationbased φ reconstruction and a more precise φ estimate at high multipoles (e.g. using the CIB as a mass tracer). This has resulted in a 20% reduction of the template variance. This, in turn, has been propagated to the variance of the BB^{lens} measurement using Eq. (15), and has induced a 12% improvement of the signal detection significance, in agreement with the independent analysis reported in Planck Collaboration XV (2016) and discussed in Sect. 7.4.
The Emode noise power spectrum, which contributes mainly through the pure noise term, provides less than 35% of the variance up to ℓ = 800. As a consequence, very little leverage is left for other experiments to improve on the template uncertainties by producing a new template that combines each experiment’s Emode measurement with the Planck lensing potential reconstruction. In Sect. 8, we see that the Planck template offers other experiments a useful tool for measuring the lensing Bmodes.
7. Robustness tests of our template
We now perform a series of consistency tests to characterize the Bmode template described in Sect. 6, with a view to using it for measuring the lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ in crosscorrelation with observed polarization maps. In Sect. 7.2, we assess the template robustness against foreground residuals, first in varying the morphology and level of conservatism of the mask, and then in using foregroundcleaned CMB maps obtained with four independent componentseparation algorithms. In Sect. 7.3, we use the Planck polarization maps in individual frequency channels to assess the stability of the lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ estimates with respect to the observed map to which our template is correlated. In Sect. 7.4, we discuss the consistency of the baseline lensing Bmode power spectrum presented here with the independent determination in Planck Collaboration XV (2016), which used various mass tracers. Finally, in Sect. 7.5, the Planck lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ measurements obtained using the Bmode template is compared to external measurements.
7.1. Template tests using Bmode bandpower estimates
With the aim of testing the Bmode template, we have followed the templatebased crosscorrelation power spectrum approach that we developed to validate our pipeline via simulations, as described in Sect. 5.1. The tests that have been performed there also allow for an endtoend assessment of the entire pipeline, whose main specifications are recalled below. Using FPP8 MC simulations for the SMICA method, together with the B70 template mask, we found that: (i) unbiased lensing Bmode bandpower estimates are obtained by crosscorrelating the Bmode template estimate with the input Bmode map; and (ii) the semianalytical Gaussian variance given in Eq. (15) provides a good approximation for the uncertainties. To test the consistency of the bandpower estimates with theoretical expectations, we fitted an amplitude with respect to the fiducial ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ bandpowers, and found an average value of 0.989 ± 0.008, which indicates that the lensing Bmode signal is accurately retrieved.
Here, we have used the Bmode template presented in Sect. 6 in crosscorrelation with the SMICA foregroundcleaned polarization maps, and have applied the B70 template mask to obtain a baseline lensing Bmode bandpower estimate, which is compared below to various other estimates. We further check the consistency between the baseline and alternative estimates by comparing the measured amplitude difference to the expected variance of the difference in MonteCarlo simulations.
7.2. Robustness against foreground residuals
The robustness of the baseline measurements against the impact of foregrounds is assessed by comparison with alternative estimates that have different residuals. A first sequence of alternative estimates have been obtained by employing masks of various levels of conservatism with respect to the Galactic and extragalactic foregrounds in temperature and polarization. These are detailed in Sects. 7.2.1 to 7.2.3. The corresponding fitted A_{Blens} amplitudes and differences from the B70 estimate are listed in Table 2. Secondly, we consider measurements obtained with foregroundcleaned maps using different componentseparation methods and give the resulting amplitudes in Sect. 7.2.3.
7.2.1. Galactic contamination tests
We test for residual foreground contamination around the Galactic plane by comparing the B70 lensing Bmode estimate to estimates using the more conservative B60 mask and the more aggressive B80 mask, discussed in Sect. 4. We recall that B80 includes a Galactic mask that preserves 80% of the sky; this Galactic mask has been extended by 3° beyond its boundaries for constructing B70, while B60 includes a larger diffuse Galactic mask that retains about 60% of the sky. We have employed the apodized version of the masks using cosine tapers, as described in Sect. 4. For B80, however, we have used slightly larger apodization widths, namely 3° for the Galactic mask (instead of 2°) and 1° for the extended compact object mask (instead of 30′).
The lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ bandpower estimates using the B60, B70, and B80 masks are shown in Fig. 7, and the fitted amplitudes are listed in Table 2. Both the B60 and B80 estimates are consistent with the B70 estimate. In particular, the agreement between the B60 and B70 lensing Bmode estimates indicates that any impact of Galactic foreground residuals lies well below the uncertainties. The consistency between the B70 and B80 estimates further indicates that: (i) an 80% Galactic cut suffices to avoid any Galactic foreground residuals in the SMICA map; and (ii) any leakage near the border of the mask (treated by inpainting) has negligible impact.
Bandpower amplitudes for various analysis masks, which are listed in the first column.
7.2.2. Extragalactic object contamination tests
For extracting the lensing potential φ map estimate that is used for the Bmode template synthesis, we have employed the L80 lensing mask described in Sect. 4.2. This cuts out any point sources included in the intersection of the conservative compact object mask described in Sect. 4.1 and the SMICA confidence mask. Here we test the stability of the Bmode estimate through the use of a more conservative point source mask that involves the union of these two masks. Namelly, we have produced an alternative estimate that relies on a φ reconstruction using the L80s lensing mask, which includes the union of the compact object and the SMICA masks (see Sect. 4.2). In L80s, the sky area that is removed due to the expected point source contamination is increased by a factor of 2.3 compared to the L80 case. The extended object mask is also slightly enlarged by 25% due to areas of radius between 30′ and 120′ located at intermediate Galactic latitudes that are present in the SMICA confidence mask. The Bmode bandpowers have then been estimated using the corresponding B70s mask for the template (which removes 1% more sky fraction than the baseline B70 mask, including about a hundred additional extragalactic objects). The B70s bandpower estimate, which is plotted in Fig. 7, is consistent with the baseline B70 estimate within uncertainties. The fitted amplitude difference from the B70 estimate, which is given in Table 2, is well within the expected difference estimated from simulations. This validates the choices we made to include the expected point sources to our baseline mask, and indicates that our analysis is free from any sizeable bias due to extragalactic objects.
7.2.3. Polarized foreground emission tests
We test for the impact of polarized foreground residuals by comparing the B70 estimate to an estimate using the B70p mask targeted at the SMICA polarization maps, as discussed in Sect. 4.3. The B70p mask discards a sky fraction 2.5% larger than B70, mainly because of extended areas at medium latitude that may be contaminated by polarized foreground residuals. The lensing Bmode bandpower estimates using the B70 and B70p masks are plotted in Fig. 7 and the corresponding amplitude fits are given in Table 2. The B70p estimate well agrees with the B70 estimate. We therefore expect no significant bias related to polarized foreground residuals.
Fig. 7 Crosscorrelation of our Bmode template with the SMICA polarization map using masks of different levels of conservatism. The data points show the lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ bandpowers estimated using masks that preserve a sky fraction of about 60% (labelled B60), 70% (“B70”), and 80% (“B80”), and that are targeted to the foreground emission in temperature (see Sect. 7.2.1); as well as using the 68% “B70s” mask, which allows for a more conservative masking of the extragalactic objects (see Sect. 7.2.2), and the 68% polarizationtargeted “B70p” mask (see Sect. 7.2.3). The residuals with respect to the model in units of the 1σ bandpower uncertainties are shown in the lower panel. The good agreement of all cases within errorbars provides a robustness test against foregrounds, as discussed in Sect. 7.2. 
From the tests performed so far, the results of which are gathered in Table 2, we have found all the bandpower estimates, from the most conservative f_{sky} = 0.58 to the most optimistic f_{sky} = 0.77 analysis and whatever the morphology of the mask, in good agreement with the baseline estimate. This provides an indication that (i) the Bmode template is robust against any foreground contamination or any impact of the skycut; and (ii) it allows us to obtain reliable lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ measurements for up to 70% of the sky.
We further test our template robustness against foreground residuals by comparing results using the four Planck componentseparation methods, as described in Planck Collaboration IX (2016). We have focused on the polarized foreground residuals; we have used different foregroundcleaned Stokes parameter maps, but the same temperature map: specifically, the lensing Bmode templates have been synthesized from the foregroundcleaned Stokes Q and U maps using different codes and a fixed lensing potential extraction obtained from the SMICA temperature map. For this specific test, we have produced a common mask that combines the B80 mask and the union of the confidence masks provided by each of the componentseparation methods described in Planck Collaboration IX (2016). The common mask retains a sky fraction of 75% for analysis, and its apodized version preserves an effective sky fraction of 62%. Figure 8 shows the resulting lensing Bmode power spectra, obtained through crosscorrelation of the lensing Bmode templates with the input Stokes Q and U maps from the corresponding componentseparation method.
Fig. 8 Consistency of our results using the four Planck componentseparation algorithms. The data points shown in the upper panel represent the lensing Bmode bandpower measurements obtained by crosscorrelating the lensing Bmode template estimates using the Commander (red), NILC (orange), SEVEM (forest green), and SMICA (blue) cleaned polarization map with the corresponding Bmode map. The residuals with respect to the model in units of the 1σ bandpower uncertainties are shown in the lower panel. The consistency of the four estimates strongly indicates the robustness of our baseline template against polarized foreground residuals, as discussed in Sect. 7.2.3. 
The four Stokes Q and U foregroundcleaned solutions lead to consistent lensing Bmode power spectrum measurements (within 1σ) over the entire multipole range probed. We measure fits to the amplitude with respect to the fiducial model of: $\begin{array}{ccc}{\mathit{A}}_{\mathit{B}\mathrm{lens}}& \mathrm{=}& \mathrm{1.01}\mathrm{\pm}\mathrm{0.11}\u2001\mathrm{\left(}\mathrm{Commander}\mathrm{\right)}\mathrm{;}\\ {\mathit{A}}_{\mathit{B}\mathrm{lens}}& \mathrm{=}& \mathrm{0.97}\mathrm{\pm}\mathrm{0.09}\u2001\mathrm{\left(}\mathrm{NILC}\mathrm{\right)}\mathrm{;}\\ {\mathit{A}}_{\mathit{B}\mathrm{lens}}& \mathrm{=}& \mathrm{1.00}\mathrm{\pm}\mathrm{0.10}\u2001\mathrm{\left(}\mathrm{SEVEM}\mathrm{\right)}\mathrm{;}\\ {\mathit{A}}_{\mathit{B}\mathrm{lens}}& \mathrm{=}& \mathrm{0.97}\mathrm{\pm}\mathrm{0.08}\u2001\mathrm{\left(}\mathrm{SMICA}\mathrm{\right)}\mathit{.}\end{array}$These correspond to 9.5σ, 11.3σ, 9.7σ, and 11.8σ detections of the lensing Bmodes, respectively. The consistency of the lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ measurements based on four CMB solutions with different foreground residuals indicates the immunity of our baseline lensing Bmode template to polarized foreground emission.
7.3. Stability with respect to the observed polarization
So far, we have considered the crosscorrelation of the Bmode template synthesized from the Stokes I, Q, and U foregroundcleaned maps, with the same Q, U maps. We now test the crosscorrelation of our baseline template with other CMB foregroundcleaned polarization maps. In particular, we have used foreground and intensitytopolarization leakagecorrected Planck channel maps at 100, 143, and 217 GHz, which also serve to test the robustness of our template against lowℓ systematic effects. These single channel maps rely on the prelaunch groundbased measurements of the detector bandpasses to correct for the intensitytopolarization leakage due to bandpass mismatch between the detectors within a frequency channel, as described in Planck Collaboration VIII (2016). The polarized emission of the Galactic dust has been corrected for by using the 353GHz map as a dust template.
In Fig. 9, we compare the baseline BB^{lens} bandpowers from the B70 SMICA analysis to the bandpowers obtained by correlating our SMICABmode template with the Bmode maps at 100, 143, and 217 GHz built out of the corresponding single channel foregroundcleaned polarization maps and using the same B70 mask. The bandpower estimates are in good agreement with each other within uncertainties, indicating the robustness of our template against polarization systematic effects (that mainly affect the low multipoles).
Fig. 9 Stability to the change in the observed polarization map. Data points shown in the upper panel are the BB^{lens} bandpowers obtained from the crosscorrelation of our SMICABmode template with the SMICA polarization map (red), and with single frequency polarization maps at 100 GHz (yellow), 143 GHz (green), and 217 GHz (blue), which were corrected for foreground and intensitytopolarization leakage. Residuals with respect to the model in units of the 1σ bandpower uncertainties are shown in the lower panel. 
We find that our lensing Bmode template provides stable measurements of the CMB lensing Bmodes independent of the choice of the polarization maps with which it is correlated.
7.4. Consistency with previous Planck results
First of all, we have checked that the baseline lensing Bmode power spectrum presented here is consistent with the independent determination of Planck Collaboration XV (2016) over the 100 < ℓ < 2000 multipole range, which provides us with further validation of our methodology choices^{7}.
In Planck Collaboration XV (2016), lensinginduced Bmode power spectrum measurements have been obtained using various mass tracers: lensing potential reconstructions using either both temperature and polarization data or temperature data only; and CIB fluctuations measured by Planck in the 545GHz channel. The latter have relied on a model of the CIB emission for calculating its crosscorrelation with the lensing potential. All cases have been consistent with theoretical expectations and in good agreement with each other, which validates the stability of the measurement with respect to the mass tracer choice. The additional information brought by the polarizationbased φ estimates yields a 10% improvement of the lensing Bmode detection significance compared to the case using the temperaturebased φ estimate, whereas the use of the CIB fluctuations as a mass tracer lowers the detection significance by roughly the same amount. Thus, including the polarization information for reconstructing φ or using the CIB as a mass tracer would not have substantially improved the uncertainties of the Bmode template that we have produced.
7.5. Consistency with external results
Our BB^{lens} bandpower estimates are a measurement of the lensing Bmode power spectrum that we now compare to measurements reported by other experiments.
As stated in Sect. 1, the available Bmode measurements come in two flavours: the BB power spectrum of the observed polarization maps measures the total Bmode signal; whereas the BB^{lens} power spectrum between a template and the observed polarization maps probes the secondary contribution only.
In Fig. 10, we gather the composite ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ measurements obtained by BICEP2/Keck Array, POLARBEAR, SPTpol, and the Planck mission, which represents the landscape of current CMB Bmode bandpower estimates. The BB power spectrum measurements of BICEP2/Keck Array^{8}, POLARBEAR (The Polarbear Collaboration 2014) and SPTpol (Keisler et al. 2015) are collected by the brace labelled BB in Fig. 10. For BICEP2/Keck Array, we plot the Bmode bandpowers in the multipole range 20 <ℓ< 335, obtained from the combination of the BICEP2 and Keck Array maps reported in BICEP2 and Keck Array Collaborations (2015a) and corrected for polarized dust emission using Planck data, as described in BICEP2/Keck Array and Planck Collaborations (2015, which is referred to as BKP hereafter). The BB^{lens} measurements of SPTpol (Hanson et al. 2013) and Planck (this analysis) are gathered by the brace labelled BB^{lens}.For PlanckBB^{lens} bandpowers, we select the B70 analysis whose robustness has been assessed in Sect. 7.2. The 4.2σ lensing Bmode detection reported by the POLARBEAR team (Ade et al. 2014b) and the 3.2σ detection obtained by ACTpol (van Engelen et al. 2015) are not shown in Fig. 10 for clarity.
Fig. 10 Consistency with external Bmode power spectrum measurements on the full multipole range (top) and at ℓ< 350 (bottom). We compare our baseline BB^{lens} estimate (red points) to the SPTpol templatebased results (green points; Hanson et al. 2013); and to the BB power spectrum measurements from BICEP2/Keck Array (blue boxes; BICEP2 and Keck Array Collaborations 2015a), POLARBEAR (light blue boxes; The Polarbear Collaboration 2014), and SPTpol (yellow boxes; Keisler et al. 2015), as discussed in Sect. 7.5. The black line shows the theoretical lensing Bmode power spectrum for the base ΛCDM bestfit Planck model (with r = 0). 
Our Planckderived BB^{lens} bandpowers are in good agreement with other Bmode measurements, using both the BB or the BB^{lens} power spectrum methods. Planck provides the most precise measurement of the lensinginduced Bmode power spectrum to date (as assessed in Planck Collaboration XV 2016). Covering a wide multipole range 10 <ℓ< 2000, our bandpowers consists of lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ measurements at a significance level as high as 12σ. It is also worth focusing on the lowℓ range. The ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ measurements are expanded at ℓ > 350 in the lower panel of Fig. 10, which illustrates the lensing Bmode template utility for the primordialtosecondary Bmode discrimination. Using Planck data alone, which combines wide sky coverage, necessary to probe low multipoles, and a good angular resolution, needed for the lensing potential extraction, the lensing Bmode template enables us to extend the measure of the lensinginduced ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ into the low multipole range.
8. Implications for current and future Bmode experiments
Here, we address the implications of the template for experiments targeting primordial Bmodes. A full joint analysis using external data is beyond the scope of this paper. However, as examples we discuss two different aspects. First, we address to what extent the template can help experiments in measuring the lensing Bmode power spectrum, in particular over the largest accessible angular scales. Secondly, we forecast the improvement of the lensing amplitude measurement when using the Planck lensing Bmode template, and we discuss whether this improvement can translate into a better sensitivity to the tensortoscalar ratio.
8.1. Measurement of the lensing Bmode power spectrum
Since the Planck lensing Bmode template covers almost the entire sky, polarization measurements from any Bmode experiment can be crosscorrelated with the template. This ensures a valuable lensing Bmode power spectrum measurement, including the intermediate angular scales, where the lensing signal is of the same order of magnitude or subdominant with respect to the polarized foreground emission (see Planck Collaboration Int. XXX 2016, hereafter referred to as PIPXXX).
For current groundbased experiments, the crosscorrelation with the Planck template is a promising method for measuring the lensing Bmode signal at the largest accessible angular scales. In general, it leads to better results than a crosscorrelation with a lensing Bmode template built out of the Planck lensing potential and each experiment’s Emode map. This can be understood from two different considerations. On the one hand, a study of the lensing Bmode signal kernel (as in Fabbian & Stompor 2013; Simard et al. 2015) reveals that most of the signal at low and intermediate angular scales comes from products of the lensing potential power at low multipoles and the Emode power at higher multipoles. For example, at ℓ = 100 (200), 80% (90%) of the lensing Bmode power arises from Emode power at ℓ > 335. For degreescale experiments, such as BICEP, it would be of little value to use its own Emode data to generate a new lensing Bmode template. On the other hand, in Sect. 6.2, we have found the Bmode template variance to be dominated by the contribution arising from the noise power spectrum of the reconstructed lensing potential ${\mathit{N}}_{\mathrm{L}}^{\mathit{\phi}}$, even for the PlanckEmode noise. For highresolution experiments covering a small fraction of the sky, we do not expect that a better sensitivity in the Emodes compensates for the uncertainties linked to the small sky coverage. We have quantified this effect in using Eqs. (16) and (17) to forecast the template uncertainties, specifically for an ideal experiment providing noiseless Emode measurements for multipoles from 30 to 2000 with a resolution of 1′ and a sky coverage of 1%. We find the uncertainties of the ideal experiment’s Emodebased template to be about five times larger than the Planck template uncertainties up to multipoles of 700 (and still 50% larger than those of the Planck template at ℓ = 2000). We conclude that, for experiments covering less than a percent of the sky, such as SPTpol or POLARBEAR, the synthesis of a lensing Bmode template that combines the experiment’s Emode data with Planckφ estimate would degrade the signaltonoise for measuring the lensing Bmode power spectrum.
8.1.1. Uncertainty forecasting method
We forecast the uncertainties of the lensing Bmode power spectrum measurement that current experiments can obtain from crosscorrelating their Bmode signal with the Planck lensing Bmode template. As in Sect. 7.5, we consider the BICEP2/Keck Array, POLARBEAR, and SPTpol examples. Error bars are evaluated using Eq. (15). They include lensed cosmic variance from the bestfit ΛCDM model and the statistical error from the template (the template autopower spectrum $\mathit{C\u0302}\begin{array}{c}\mathit{B}\mathrm{lens}\\ \mathit{\ell}\end{array}$ factor) and from the experiment (the experiment autospectrum $\mathrm{(}{\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}\mathrm{+}{\mathit{N}}_{\mathit{\ell}}^{\mathit{B}}\mathrm{)}$ factor). To estimate the template variance within the experiment’s field, $\mathit{C\u0302}\begin{array}{c}\mathit{B}\mathrm{lens}\\ \mathit{\ell}\end{array}$ is analytically calculated using the lensing potential and Emode noise power spectra, rescaled to the noise spatial inhomogeneity within the experiment’s field. This rescaling relies on the SMICA hit count map. We use a simplified model for the BB autospectrum of the experiment that includes the lensed CMB Bmodes, polarized dust, white noise, and Gaussian beam. The specific model and analysis choices are detailed below.
The polarized dust emission has been parametrized by a single free amplitude in power, A_{dust}, which is defined at the reference frequency of 353 GHz and at a multipole of ℓ = 80. Following PIPXXX, the dust power spectrum has been modelled as the power law ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{dust}}\mathrm{\propto}{\mathit{\ell}}^{2.42}$, with a spatially uniform frequency scaling according to a modified blackbody law, assuming a fixed dust temperature T_{d} = 19.6 K and spectral index β_{d} = 1.6. For the BICEP2/Keck Array combination, we have fixed the dust amplitude to the bestfit value obtained in the joint BICEP2/Keck Array and Planck analysis described in BKP, namely A_{dust} = 3 μK^{2}. In PIPXXX, individual dust amplitudes have been fitted for a series of sky patches, and their scaling with the mean 353GHz dust intensity was described using an empirical relation. However, there was a warning about the difficulty in deriving precise dust amplitude estimates from this empirical law. From Fig. 7 of PIPXXX, we can see that, at the low dust intensity values expected in the SPTpol and POLARBEAR fields, the amplitudes range from 0.1 to 10 μK^{2}. For simplicity, we have assumed the level of dust emission in the POLARBEAR and SPTpol fields to be the same as in the BICEP2 field, and so have used the value A_{dust} = 3 μK^{2}. We checked that assuming the more pessimistic A_{dust} = 10 μK^{2} leads to a minor increase in the forecasted BB^{lens} bandpower uncertainties.
The BICEP2/Keck Array combination has been modelled as reaching a noise level of 3.4 μK arcmin over 400 deg^{2}, and as having a Gaussian beam of 31′FWHM for both BICEP2 and Keck Array experiments (BICEP2 and Keck Array Collaborations 2015b,a). POLARBEAR has been modelled as reaching a depth of 8 μK arcmin over an effective sky area of 25 deg^{2} (f_{sky} = 0.06%) with resolution at 150 GHz (The Polarbear Collaboration 2014). For SPTpol, we have modelled the noise spectrum from the characteristics reported in Hanson et al. (2013), by considering the combination of the 95GHz observation ( resolution and 25 μK arcmin noise level) and the 150GHz observation ( resolution and 10 μK arcmin noise level) over a sky area of 100 deg^{2} (f_{sky} = 0.24%). We have used the same multipole binning as chosen by each experiment in existing publications, and have added a lowℓ bin including multipoles up to the largest accessible angular scales defined by the experiment’s sky coverage. For POLARBEAR and SPTpol, we have considered the 100 < ℓ < 2000 multipole range.
8.1.2. Lensing Bmode bandpower forecasts
Fig. 11 Forecasts of lensing Bmode bandpowers from crosscorrelating the Planck lensing Bmode template with external data from Bmode targeted experiments. Blue circles show the BICEP2/Keck Array bandpowers forecasts using the same multipole binning as that of BICEP2/Keck Array data points shown in Fig. 10. BB^{lens} bandpower measurements can be extended to an additional ℓ = 100–500 bin using POLARBEAR (turquoise) and to an additional ℓ = 100–300 bin using the SPTpol (dark orange) in crosscorrelation with the template. 
Figure 11 shows the forecasted BB^{lens} bandpowers over multipoles up to 500, for which the Planck template is the most useful in helping other experiments to measure the lensing Bmode power spectrum. We find that the BICEP2/Keck Array could be used in combination with the Planck template to obtain BB^{lens} bandpowers in the multipole range ℓ = 20–335 measured at a significance level of about 6σ (sensitivity to A_{Blens} of 0.17).Therefore, our forecasted sensitivity to the lensing Bmode signal is comparable to that obtained in the BKP analysis, where a lensing amplitude of A_{lens} = 1.13 ± 0.18 has been measured. However, we show in Sect. 8.3 that we could improve the sensitivity to the lensing Bmode signal by adding the Bmode template to a BICEP2/Keck Array and Planck joint analysis. The Planck template could enables subdegree angular scale experiments, such as BICEP2/Keck Array, to probe the ℓdependence of the lensing Bmode signal over their full multipole range, including multipoles at which the lensinginduced signal is subdominant compared to other sources of Bmode signal (such as polarized dust). Moreover, the crosscorrelation with the template should allow experiments targeting higher multipoles (such as POLARBEAR or SPTpol) to measure the lensing Bmode signal at intermediate angular scales (100 < ℓ < 300), extending their BB^{lens} estimates down to as low multipoles as their sky coverage would permit.
8.2. Direct delensing capabilities
“Delensing” consists of subtracting the lensing Bmode template from the Bmode map of an experiment in order to try to highlight the primordial Bmodes. Because of the noise level of the template, poor efficiency is expected from a direct delensing approach (e.g. Marian & Bernstein 2007). We have quantified the expected impact on the tensortoscalar ratio uncertainty in calculating the improvement factor as defined in Smith et al. (2009b) as $\mathit{\alpha}\mathrm{=}\frac{{\mathit{C}}_{\mathit{\ell}}^{\mathit{B,}\mathrm{lens}}\mathrm{+}{\mathit{N}}_{\mathit{\ell}}^{\mathit{B}}}{{\mathit{C}}_{\mathit{\ell}}^{\mathit{B,}\mathrm{res}}\mathrm{+}{\mathit{N}}_{\mathit{\ell}}^{\mathit{B}}}\mathrm{\xb7}$(18)Here ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B,}\mathrm{lens}}$ and ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B,}\mathrm{res}}$ are the lensing Bmode power spectrum, and its residual after subtraction of the template from the external data, while ${\mathit{N}}_{\mathit{\ell}}^{\mathit{B}}$ is the noise power spectrum of the experiment. We find a maximum improvement factor (corresponding to ${\mathit{N}}_{\mathit{\ell}}^{\mathit{B}}\mathrm{=}\mathrm{0}$) of 5% at ℓ < 200, reaching a maximum of 10% around ℓ = 300, in agreement with the expectations derived in Smith et al. (2009b).
8.3. Improvement of the parameter accuracies
We now go beyond the lensing Bmode power spectrum measurement and quantify whether the use of the template as an additional data set (together with other Bmode data and the Planck dust template) can tighten cosmological parameter constraints, and in particular, the amplitude of the lensing potential power spectrum that scales the lensinginduced Bmodes, A_{lens}. We discuss whether more precise measurements of the lensing scaling translate into tightened constraints on the tensortoscalar ratio.
We derive forecasts for particular experiments by performing a Fisher analysis^{9} (for a description of this method, see e.g. Tegmark et al. 1997). We consider a threeparameter model, { r,A_{lens},A_{dust} }, consisting of the tensortoscalar ratio and the amplitudes of the lensing potential and polarized dust power spectra. We compare the parameter constraints obtained in two cases: (1) the data sets consist of B^{exp}, the external data from the Bmode targeted experiment, and , the PlanckBmode data at 353 GHz, considered as a polarized dust template; and (2) the Planck lensing Bmode template, , is used in combination with the other two data sets. As examples of external experiments, we consider the BICEP2/Keck Array combination, hereafter referred to as BK, described in BICEP2 and Keck Array Collaborations (2015a); and a wide sky coverage experiment, such as LiteBIRD (Matsumura et al. 2014). The rationale driving these choices is twofold. Because of the lensing Bmode template noise level in a 1% sky area and from the results obtained above, we do not expect the inclusion of the template to bring a large improvement of the sensitivity to r for BK. However, we will be able to validate our simple fiducial analysis by comparing “Case 1” to the floating lensing amplitude analysis described in BKP. By contrast, a more substantial improvement is expected for a large sky coverage Bmode experiment such as LiteBIRD. For definiteness, we consider two different fiducial cosmologies in what follows, which consist of a r = 0.05 model and r = 10^{4} model.
8.3.1. Fisher analysis
We consider the Fisher information matrix of the form (see e.g. Tegmark et al. 1997) ${\mathit{F}}_{\mathit{ij}}\mathrm{=}\sum _{\mathit{\ell}}\frac{\mathrm{1}}{\mathrm{2}}\mathrm{(}\mathrm{2}\mathit{\ell}\mathrm{+}\mathrm{1}\mathrm{)}{\mathit{f}}_{\mathrm{sky}}\hspace{0.17em}\mathrm{Tr}\mathrm{\left[}\mathrm{C}{\mathrm{C}}_{\mathit{,i}}\mathrm{C}{\mathrm{C}}_{\mathit{,j}}\mathrm{\right]}$(19)for a fiducial data covariance matrix C and its derivatives with respect to the parameters labelled by i and j. Given the data set $\mathrm{\left\{}{\mathit{B}}_{\mathit{\ell m}}^{\mathrm{exp}}\mathit{,}\mathit{B\u0302}\begin{array}{c}\mathrm{dust}\\ \mathit{\ell m}\end{array}\mathit{,}\mathit{B\u0302}\begin{array}{c}\mathrm{lens}\\ \mathit{\ell m}\end{array}\mathrm{\right\}}$, we need to model the Bmode autopower spectra for the external data, ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{exp}}$, for the Planck 353GHz map, ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{353}}$, and for the Planck lensing Bmode template within the experiment’s sky coverage, ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B\u0302}\mathrm{lens}}$, as well as the corresponding crosspower spectra.
The fiducial model consists of an extension of the sixparameter ΛCDM model considered so far, including primordial gravitational waves (GW) of amplitude r, a freely floating amplitude of the lensing potential power spectrum, A_{lens}, and a free polarized dust amplitude in power A_{dust} (defined at the reference frequency of 353 GHz and at a multipole of ℓ = 80). In this fiducial framework, the Bmode autopower spectrum of the experiment under consideration is ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{exp}}\mathrm{=}\frac{\mathit{r}}{{\mathit{r}}_{\mathrm{fid}}}{\mathit{C}}_{\mathit{\ell}}^{\mathrm{GW}\mathit{,r}\mathrm{=}{\mathit{r}}_{\mathrm{fid}}}\mathrm{+}{\mathit{A}}_{\mathrm{lens}}{\mathit{C}}_{\mathit{\ell}}^{\mathrm{lens}}\mathrm{+}\mathit{\alpha}{\mathit{A}}_{\mathrm{dust}}\mathit{R}\mathrm{(}\mathit{\nu ,}\mathrm{353}{\mathrm{)}}^{\mathrm{2}}{\mathit{C}}_{\mathit{\ell}}^{\mathrm{dust}}\mathrm{+}{\mathit{N}}_{\mathit{\ell}}^{\mathrm{exp}}\mathit{,}$(20)where ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{GW}\mathit{,r}\mathrm{=}{\mathit{r}}_{\mathrm{fid}}}$ and ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{lens}}$ are the gravitational wave and lensing power spectra at the fiducial r = r_{fid} and A_{lens} = 1 values. We have considered two different fiducial values for r, either r_{fid} = 0.05 or r_{fid} = 10^{4}. The dust power spectrum, ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{dust}}$, and its frequency scaling with the reference 353GHz frequency, R(ν,353) have been modelled as in Sect. 8.1, following PIPXXX. In addition, for multiband experiments with foregroundcleaning capabilities, the dust power spectrum has been assumed to be cleaned up to a residual level defined by the α factor (α = 1 for a single frequency experiment). Finally, ${\mathit{N}}_{\mathit{\ell}}^{\mathrm{exp}}$ is the Bmode noise power spectrum of each experiment.
The Planck 353GHz Bmode autopower spectrum in each experiment’s sky coverage has been modelled as ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{353}}\mathrm{=}{\mathit{A}}_{\mathrm{dust}}{\mathit{C}}_{\mathit{\ell}}^{\mathrm{dust}}\mathrm{+}{\mathit{N}}_{\mathit{\ell}}^{\mathrm{353}}\mathit{,}$(21)where the fullsky noise power spectrum at 353 GHz has been scaled to take the spatial inhomogeneity within the experimental field into account. We have neglected the subdominant CMB Bmode polarization signal.
Finally, the Planck lensing Bmode template autopower spectrum within the experimental field has been analytically calculated using Eq. (17), in which the noise power spectra of the lensing potential ${\mathit{N}}_{\mathrm{L}}^{\mathit{\phi}}$ and of the Emode ${\mathit{N}}_{\mathit{\ell}}^{\mathit{E}}$ have been scaled to deal with the spatial inhomogeneity within the experimental field. The crosscorrelation of the experiment’s data with the 353GHz dust template and lensing Bmode template are $\mathrm{\left(}\mathit{\alpha}{\mathrm{)}}^{\mathrm{0.5}}{\mathit{A}}_{\mathrm{dust}}\mathit{R}\mathrm{\right(}\mathit{\nu ,}\mathrm{353}\mathrm{)}{\mathit{C}}_{\mathit{\ell}}^{\mathrm{dust}}$ and ${\mathit{C}}_{\mathit{\ell}}^{\mathrm{lens}}$. Following the assumptions of the model, we have neglected the subdominant crosscorrelation of the lensing Bmode and 353GHz dust templates.
8.3.2. Examples of BK and LiteBIRD
For existing data, we have used a datadriven model. Both the BK and the Planck 353GHz noise power spectra in the BK field have been extrapolated from the noise bandpowers released along with the BKP likelihood^{10}. For the future project LiteBIRD, we have modelled the noise power spectrum from the foreseen instrumental characteristics defined in Matsumura et al. (2014). Only the 100 and 140GHz bands have been considered, the two lowest and two highest bands being discarded, assuming that they are used for foreground cleaning. Following Matsumura et al. (2014), the 100GHz band reaches a depth of 3.7 μK arcmin and a resolution defined by a Gaussian beam of 45′FWHM, while the 140GHz band has a noise level of 4.7 μK arcmin and 32′FWHM. The polarized dust in each frequency band has been assumed to be cleaned over an effective sky area of 63% up to the same residual level as in the BK field. This corresponds to a mildly conservative (Dunkley et al. 2009) 17% residual level in the map domain (corresponding to α = 2.9% in power) for the dust amplitude A_{dust} = 104.5 μK^{2}, obtained in PIPXXX via a powerlaw fit in the large retained science region “LR63”.
With the fiducial model established and using the numerical analysis method described, we can infer the sensitivity to the parameters as $\mathrm{\Delta}{\mathit{\theta}}_{\mathit{i}}\mathrm{=}\sqrt{\mathrm{(}{\mathit{F}}^{1}{\mathrm{)}}_{\mathit{ii}}}$ for θ_{i} ∈ { r,A_{lens},A_{dust} }. The results for BK and LiteBIRD for the two fiducial values of r and in the two cases considered, depending on whether the lensing Bmode template is used or not, are presented in Table 3.
Fisher analysis inferred parameter uncertainties for the BICEP2/Keck Array experiment and for the LiteBIRD project using the r = 0.05 and r = 10^{4} fiducial models.
For the BK analysis in Case 1 (without the lensing template) and using the r = 0.05 fiducial model, we find Δr = 0.031, ΔA_{lens} = 0.186 and ΔA_{dust} = 0.7, in agreement with results reported in BKP: $\mathit{r}\mathrm{=}\mathrm{0.04}{\mathrm{8}}_{0.032}^{\mathrm{+}\mathrm{0.035}}$, A_{lens} = 1.13 ± 0.18 (from the free lensing amplitude extended analysis) and ${\mathit{A}}_{\mathrm{dust}}\mathrm{=}\mathrm{3.}{\mathrm{3}}_{0.8}^{\mathrm{+}\mathrm{0.9}}$. This indicates that our fiducial Fisher analysis yields reliable parameter uncertainty estimates despite the underlying simplifying assumptions. The use of the lensing template translates into a 5% improvement of the r constraint, whereas the constraint on A_{lens} is tightened by 36%. Similar results are found using the more pessimistic r = 10^{4} fiducial model; Case 2 yields a 5% improvement of the constraint on r and a 35% improvement of the constraint on A_{lens}, compared to Case 1. Over the multipole range covered by BK, A_{lens} is weakly correlated with both r and A_{dust}, as was noted in the BKP paper, so that the improvement in the A_{lens} constraint translates into modest improvement of the r or A_{dust} constraints. This is verified in Fig. 12, where the twodimensional contours at 68% and 95% are shown in the A_{lens}–r and A_{lens}–A_{dust} planes. However, Fig. 12 also shows that the A_{lens}–r correlation is further reduced when the lensing Bmode template is used, leading to more robust constraints.
Fig. 12 Constraints on the tensortoscalar ratio r and the amplitude of the polarized dust power A_{dust} within a model with free lensing potential amplitude A_{lens}. The twodimensional likelihood contours at 68% and 95% are forecasted for BICEP2/Keck Array (BK, shades of blue) and for LiteBIRD (LB, shades of red), in combination with the Planck 353GHz dust template only (line contours) and the Planck dust and lensing Bmode templates (shaded contours). The lower panels show a zoomin on the LiteBIRD contours. 
For large angular scale experiments whose multipole coverage is limited to ℓ ≲ 200, such as LiteBIRD, the implication of the template slightly differs. For the r = 10^{4} fiducial model, the secondary Bmodes, which fully dominate over the primary Bmodes, are precisely measured even without the help of the template. In the r = 0.05 fiducial model, however, the lack of measurement over a lensing Bmode dominated multipole range increases the parameter degeneracy, in particular between A_{lens} and r, as seen in Fig. 12. As a result, the 20% improvement on the A_{lens} uncertainties, which arises from using the Planck lensing Bmode template, translates into a 15% improvement on the r uncertainties.
9. Conclusions
We have produced a nearly allsky template of the CMB secondary Bmodes using the Planck fullmission foregroundcleaned CMB temperature and Stokes parameter maps. For this purpose, we have developed a dedicated pipeline that has been verified via specific simulations. We show that the constructed template includes the lensing Bmode contribution at all angular scales covered by Planck and shows no contamination from primordial Bmodes. This template has been used to compute the CMB lensing Bmode power spectrum by crosscorrelating it with the total foregroundcleaned Planck polarization Bmode maps (via the publicly available Q and U maps). We find that the resulting CMB lensing Bmode power spectrum is insensitive to foreground contamination and independent of the choice of the foregroundcleaned Planck polarization Bmode map used for the crosscorrelation analysis. Furthermore, we find that the results are in good agreement with the expected CMB lensing Bmode power spectrum computed using the baseline Planck 2015 bestfitting ΛCDM model. We obtain a 12σ detection of the lensing Bmodes, in agreement with the results in the companion Planck Collaboration XV (2016) paper.
Planck provides a unique nearly allsky lensing Bmode template, containing all the lensinduced information from intermediate to large angular scales. This template, which is included as part of the Planck 2015 data release, will be a useful tool for current and future groundbased experiments targeting the measurement of the primordial CMB Bmode power spectrum. Indeed, this template can be used to obtain a reliable measurement of the lensing Bmode power spectrum with future experiments or to improve the precision with which they can detect the lensing Bmodes in their own data, by tightening the constraints on the lensing amplitude. This, in turn, can help in the more challenging endeavour of constraining the tensortoscalar ratio.
Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA).
It is also related to the response function of the quadratic estimator for offdiagonal terms of the CMB covariance ℛ_{L}, as defined in Eq. (A.16) of Planck Collaboration XV (2016), via ${\mathrm{\mathcal{A}}}_{\mathrm{L}}\mathrm{=}{\mathrm{\mathcal{R}}}_{\mathrm{L}}^{1}$.
In Planck Collaboration XV (2016), one of the null tests conducted for checking the robustness of the lensing potential power spectrum has showed mild evidence of a difference from zero, specifically a nonzero signal has been seen in the TT curlmode power spectrum (which contains the TTTT curlmode trispectrum) with a significance above 2σ. This feature, however, has no real impact in the lensinginduced power spectrum being tested here. First, it contains the TTEB trispectrum, which differs from the trispectrum affected by the curlmode nulltest failure. Additionally, any impact on the variance of the lensinginduced Bmode power spectrum, via some TTTT trispectrum dependent terms, would be totally overwhelmed by the dominant Gaussian noise term.
We note that in this approach, the parameter likelihood is assumed to be Gaussian close to its maximum, so that the parameter constraints can be derived by calculating the distribution Hessian taken at the fiducial values of the parameters. Owing to this assumption, parameter confidence contours are ellipses.
Acknowledgments
The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSUIN2P3INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck. This paper made use of the HEALPix software package. We thank the anonymous referee for their helpful comments and thoughtful suggestions that contributed to improve this paper.
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All Tables
Bandpower amplitudes for various analysis masks, which are listed in the first column.
Fisher analysis inferred parameter uncertainties for the BICEP2/Keck Array experiment and for the LiteBIRD project using the r = 0.05 and r = 10^{4} fiducial models.
All Figures
Fig. 1 Wienerfiltered lensing potential estimated from the SMICA foregroundcleaned temperature map using the f_{sky} ≃ 80% lensing mask. The lensing potential estimate, which is shown in Galactic coordinates, is effectively inpainted using a lensing extraction method that relies on an inpainting of the input temperature map, as discussed in Sect. 3.3.1. 

In the text 
Fig. 2 Lensing Bmode power spectrum obtained by crosscorrelating the B^{lens} templates with the corresponding fiducial Bmode simulations (top), and residuals with respect to the model (bottom). Top: averaged BB^{lens} bandpowers using the apodized B70 template mask, with multipole bins of Δℓ ≥ 100 (blue points). The error bars are the standard deviation on the mean of the bandpower estimate set. The dark blue curve is the fiducial Bmode power spectrum of our simulations, which assumes r = 0. Bottom: BB^{lens} bandpower residual with respect to the fiducial model, given in units of the 1σ error of a single realization. For comparison, we also show the bandpower residuals obtained without masking, as discussed in Sect. 5.1 (red points). Dashed lines show the ± 1σ range of 100 realizations, indicating the precision level to which we are able to test against bias. 

In the text 
Fig. 3 Error budget. We compare the MC derived uncertainties σ_{MC} associated with the BB^{lens} measurements to the semianalytical errors σ_{G} obtained using Eq. (15). Top: averaged BB^{lens} bandpowers using either σ_{MC} (blue) or σ_{G} (red) as error estimates. For illustration, we also show the expected sensitivity of the PlanckSMICA CMB polarization map to the BB bandpowers (grey boxes), whose uncertainties are a factor of four larger than those of the BB^{lens} bandpowers using the lensing Bmode template. Bottom: relative difference of σ_{G} with respect to σ_{MC}. Dashed lines show a 15% difference. 

In the text 
Fig. 4 SMICA lensinginduced Q and U templates that have been convolved with a Gaussian beam of 60′FWHM to highlight the large angular scales (corresponding to multipoles below 200). No spurious patterns are observed at large angular scales. 

In the text 
Fig. 5 Planckderived Bmode template map computed using the SMICA foregroundcleaned CMB maps. For illustration, the map has been convolved with a Gaussian beam of 10′ (upper panel) and 60′ (lower panel) FWHM. The grey area represents the L80 mask, which was used at the lensing potential reconstruction stage. No obvious foreground residuals are seen in the highresolution map, nor any obvious systematic effects in the lowresolution one. 

In the text 
Fig. 6 Template map variance budget. The total variance of the template, plotted in dark blue, is split into the contribution of the lens reconstruction noise (orange) and Emode noise (green) crossterms; and the pure noise (yellow) and cosmic variance (light blue) terms defined in Sect. 6.2. 

In the text 
Fig. 7 Crosscorrelation of our Bmode template with the SMICA polarization map using masks of different levels of conservatism. The data points show the lensing ${\mathit{C}}_{\mathit{\ell}}^{\mathit{B}}$ bandpowers estimated using masks that preserve a sky fraction of about 60% (labelled B60), 70% (“B70”), and 80% (“B80”), and that are targeted to the foreground emission in temperature (see Sect. 7.2.1); as well as using the 68% “B70s” mask, which allows for a more conservative masking of the extragalactic objects (see Sect. 7.2.2), and the 68% polarizationtargeted “B70p” mask (see Sect. 7.2.3). The residuals with respect to the model in units of the 1σ bandpower uncertainties are shown in the lower panel. The good agreement of all cases within errorbars provides a robustness test against foregrounds, as discussed in Sect. 7.2. 

In the text 
Fig. 8 Consistency of our results using the four Planck componentseparation algorithms. The data points shown in the upper panel represent the lensing Bmode bandpower measurements obtained by crosscorrelating the lensing Bmode template estimates using the Commander (red), NILC (orange), SEVEM (forest green), and SMICA (blue) cleaned polarization map with the corresponding Bmode map. The residuals with respect to the model in units of the 1σ bandpower uncertainties are shown in the lower panel. The consistency of the four estimates strongly indicates the robustness of our baseline template against polarized foreground residuals, as discussed in Sect. 7.2.3. 

In the text 
Fig. 9 Stability to the change in the observed polarization map. Data points shown in the upper panel are the BB^{lens} bandpowers obtained from the crosscorrelation of our SMICABmode template with the SMICA polarization map (red), and with single frequency polarization maps at 100 GHz (yellow), 143 GHz (green), and 217 GHz (blue), which were corrected for foreground and intensitytopolarization leakage. Residuals with respect to the model in units of the 1σ bandpower uncertainties are shown in the lower panel. 

In the text 
Fig. 10 Consistency with external Bmode power spectrum measurements on the full multipole range (top) and at ℓ< 350 (bottom). We compare our baseline BB^{lens} estimate (red points) to the SPTpol templatebased results (green points; Hanson et al. 2013); and to the BB power spectrum measurements from BICEP2/Keck Array (blue boxes; BICEP2 and Keck Array Collaborations 2015a), POLARBEAR (light blue boxes; The Polarbear Collaboration 2014), and SPTpol (yellow boxes; Keisler et al. 2015), as discussed in Sect. 7.5. The black line shows the theoretical lensing Bmode power spectrum for the base ΛCDM bestfit Planck model (with r = 0). 

In the text 
Fig. 11 Forecasts of lensing Bmode bandpowers from crosscorrelating the Planck lensing Bmode template with external data from Bmode targeted experiments. Blue circles show the BICEP2/Keck Array bandpowers forecasts using the same multipole binning as that of BICEP2/Keck Array data points shown in Fig. 10. BB^{lens} bandpower measurements can be extended to an additional ℓ = 100–500 bin using POLARBEAR (turquoise) and to an additional ℓ = 100–300 bin using the SPTpol (dark orange) in crosscorrelation with the template. 

In the text 
Fig. 12 Constraints on the tensortoscalar ratio r and the amplitude of the polarized dust power A_{dust} within a model with free lensing potential amplitude A_{lens}. The twodimensional likelihood contours at 68% and 95% are forecasted for BICEP2/Keck Array (BK, shades of blue) and for LiteBIRD (LB, shades of red), in combination with the Planck 353GHz dust template only (line contours) and the Planck dust and lensing Bmode templates (shaded contours). The lower panels show a zoomin on the LiteBIRD contours. 

In the text 
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