Issue 
A&A
Volume 571, November 2014
Planck 2013 results



Article Number  A25  
Number of page(s)  21  
Section  Cosmology (including clusters of galaxies)  
DOI  https://doi.org/10.1051/00046361/201321621  
Published online  29 October 2014 
Planck 2013 results. XXV. Searches for cosmic strings and other topological defects
^{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,
Metsähovintie 114, 02540
Kylmälä,
Finland
^{3}
African Institute for Mathematical Sciences,
68 Melrose Road, Muizenberg,
7701
Rondebosch Cape Town, South
Africa
^{4}
Agenzia Spaziale Italiana Science Data Center,
c/o ESRIN, via Galileo Galilei,
00044
Frascati,
Italy
^{5}
Agenzia Spaziale Italiana, Viale Liegi 26, 00198
Roma,
Italy
^{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}
CITA, University of Toronto, 60 St. George St., Toronto, ON
M5S 3H8,
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^{9}
CNRS, IRAP, 9 Av.
colonel Roche, BP
44346, 31028
Toulouse Cedex 4,
France
^{10}
California Institute of Technology, Pasadena, California, USA
^{11}
Centre for Theoretical Cosmology, DAMTP, University of
Cambridge, Wilberforce
Road, Cambridge
CB3 0WA
UK
^{12}
Centro de Estudios de Física del Cosmos de Aragón
(CEFCA), Plaza San Juan 1, planta
2, 44001
Teruel,
Spain
^{13}
Computational Cosmology Center, Lawrence Berkeley National
Laboratory, Berkeley,
California,
USA
^{14}
Consejo Superior de Investigaciones Científicas
(CSIC), Madrid,
Spain
^{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 Física Fundamental, Facultad de Ciencias,
Universidad de Salamanca, 37008
Salamanca,
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 Electrical Engineering and Computer Sciences,
University of California, Berkeley, California, USA
^{23}
Department of Physics & Astronomy, University of British
Columbia, 6224 Agricultural Road,
Vancouver, British
Columbia, Canada
^{24}
Department of Physics and Astronomy, Dana and David Dornsife College
of Letter, Arts andSciences, University of Southern California,
Los Angeles, CA
90089,
USA
^{25}
Department of Physics and Astronomy, University College
London, London
WC1E 6BT,
UK
^{26}
Department of Physics, Gustaf Hällströmin katu 2a, University of
Helsinki, Helsinki,
Finland
^{27}
Department of Physics, Princeton University,
Princeton, New Jersey, USA
^{28}
Department of Physics, University of California,
One Shields Avenue, Davis, California, USA
^{29}
Department of Physics, University of California,
Santa Barbara, California, USA
^{30}
Department of Physics, University of Illinois at
UrbanaChampaign, 1110 West Green
Street, Urbana,
Illinois,
USA
^{31}
Dipartimento di Fisica e Astronomia G. Galilei, Università degli
Studi di Padova, via Marzolo
8, 35131
Padova,
Italy
^{32}
Dipartimento di Fisica e Scienze della Terra, Università di
Ferrara, via Saragat
1, 44122
Ferrara,
Italy
^{33}
Dipartimento di Fisica, Università La Sapienza,
P.le A. Moro 2, 00185
Roma,
Italy
^{34}
Dipartimento di Fisica, Università degli Studi di
Milano, via Celoria,
16, 20133
Milano,
Italy
^{35}
Dipartimento di Fisica, Università degli Studi di
Trieste, via A. Valerio
2, 34127
Trieste,
Italy
^{36}
Dipartimento di Fisica, Università di Roma Tor
Vergata, via della Ricerca Scientifica
1, 00133
Roma,
Italy
^{37}
Discovery Center, Niels Bohr Institute, Blegdamsvej 17, 2100
Copenhagen,
Denmark
^{38}
Dpto. Astrofísica, Universidad de La Laguna (ULL),
38206, La Laguna, Tenerife,
Spain
^{39}
European Space Agency, ESAC, Planck Science Office,
Camino bajo del Castillo s/n, Urbanización
Villafranca del Castillo, 28691 Villanueva de la Cañada, Madrid, Spain
^{40}
European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ
Noordwijk, The
Netherlands
^{41}
Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University
of Helsinki, 00014
Helsinki,
Finland
^{42}
INAF – Osservatorio Astronomico di Padova,
Vicolo dell’Osservatorio 5,
35122
Padova,
Italy
^{43}
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via di Frascati 33, 00040
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^{44}
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via G.B. Tiepolo 11, 34131
Trieste,
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^{45}
INAF/IASF Bologna, via Gobetti 101, 40129
Bologna,
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^{46}
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Milano,
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^{47}
INFN, Sezione di Bologna, via Irnerio 46, 40126
Bologna,
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^{48}
INFN, Sezione di Roma 1, Università di Roma Sapienza,
Piazzale Aldo Moro 2,
00185
Roma,
Italy
^{49}
IPAG: Institut de Planétologie et d’Astrophysique de Grenoble,
Université Joseph Fourier, Grenoble
1/CNRSINSU, UMR 5274, 38041
Grenoble,
France
^{50}
IUCAA, Post Bag 4, Ganeshkhind, Pune University
Campus, 411 007
Pune,
India
^{51}
Imperial College London, Astrophysics group, Blackett
Laboratory, Prince Consort
Road, London,
SW7 2AZ,
UK
^{52}
Infrared Processing and Analysis Center, California Institute of
Technology, Pasadena,
CA
91125,
USA
^{53}
Institut Néel, CNRS, Université Joseph Fourier Grenoble
I, 25 rue des
Martyrs, 38042
Grenoble,
France
^{54}
Institut Universitaire de France, 103 Bd SaintMichel, 75005
Paris,
France
^{55}
Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université
ParisSud 11, Bâtiment
121, 91405
Orsay,
France
^{56}
Institut d’Astrophysique de Paris, CNRS (UMR7095),
98bis Bd Arago, 75014
Paris,
France
^{57}
Institute for Space Sciences, 077125
BucharestMagurale,
Romania
^{58}
Institute of Astronomy and Astrophysics, Academia
Sinica, 10617
Taipei,
Taiwan
^{59}
Institute of Astronomy, University of Cambridge,
Madingley Road, Cambridge
CB3 0HA,
UK
^{60}
Institute of Mathematics and Physics, Centre for Cosmology, Particle
Physics and Phenomenology, 1348 Louvain University, LouvainlaNeuve,
Belgium
^{61}
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Oslo, Blindern,
0315
Oslo,
Norway
^{62}
Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, 38200 La Laguna, Tenerife, Spain
^{63}
Instituto de Física de Cantabria (CSICUniversidad de
Cantabria), Avda. de los Castros
s/n, 39005
Santander,
Spain
^{64}
Jet Propulsion Laboratory, California Institute of
Technology, 4800 Oak Grove
Drive, Pasadena,
California,
USA
^{65}
Jodrell Bank Centre for Astrophysics, Alan Turing Building, School
of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13
9PL, UK
^{66}
Kavli Institute for Cosmology Cambridge,
Madingley Road, Cambridge, CB3 0HA, UK
^{67}
LAL, Université ParisSud, CNRS/IN2P3, 91898
Orsay,
France
^{68}
LERMA, CNRS, Observatoire de Paris, 61 Avenue de l’Observatoire, 75014
Paris,
France
^{69}
Laboratoire AIM,IRFU/Service d’Astrophysique  CEA/DSM  CNRS 
Université Paris Diderot, Bât. 709,
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^{70}
Laboratoire Traitement et Communication de l’Information, CNRS (UMR
5141) and Télécom ParisTech, 46 rue
Barrault, 75634
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^{71}
Laboratoire de Physique Subatomique et de Cosmologie, Université
Joseph Fourier Grenoble I, CNRS/IN2P3, Institut National Polytechnique de
Grenoble, 53 rue des
Martyrs, 38026
Grenoble Cedex,
France
^{72}
Laboratoire de Physique Théorique, Université ParisSud 11 &
CNRS, Bâtiment 210,
91405
Orsay,
France
^{73}
Lawrence Berkeley National Laboratory, Berkeley, California, USA
^{74}
MaxPlanckInstitut für Astrophysik, KarlSchwarzschildStr. 1, 85741
Garching,
Germany
^{75}
MaxPlanckInstitut für Extraterrestrische Physik,
Giessenbachstraße, 85748
Garching,
Germany
^{76}
McGill Physics, Ernest Rutherford Physics Building, McGill
University, 3600 rue
University, Montréal,
QC, H3A 2T8, Canada
^{77}
MilliLab, VTT Technical Research Centre of Finland,
Tietotie 3, 02044
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Finland
^{78}
Niels Bohr Institute, Blegdamsvej 17, 2100
Copenhagen,
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^{79}
Observational Cosmology, Mail Stop 36717, California Institute of
Technology, Pasadena,
CA, 91125, USA
^{80}
Optical Science Laboratory, University College London,
Gower Street, London, UK
^{81}
SBITPLPPC, EPFL, 1015, Lausanne, Switzerland
^{82}
SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy
^{83}
School of Physics and Astronomy, Cardiff University,
Queens Buildings, The Parade,
Cardiff, CF24 3AA, UK
^{84}
School of Physics and Astronomy, University of
Nottingham, Nottingham
NG7 2RD,
UK
^{85}
Space Sciences Laboratory, University of California,
Berkeley, California, USA
^{86}
Special Astrophysical Observatory, Russian Academy of
Sciences, Nizhnij Arkhyz,
Zelenchukskiy region, 369167
KarachaiCherkessian Republic,
Russia
^{87}
Stanford University, Dept of Physics, Varian Physics
Bldg, 382 via Pueblo
Mall, Stanford,
California,
USA
^{88}
SubDepartment of Astrophysics, University of Oxford,
Keble Road, Oxford
OX1 3RH,
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^{89}
Theory Division, PHTH, CERN, 1211
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Switzerland
^{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, 1807
Granada,
Spain
^{93}
University of Miami, Knight Physics Building,
1320 Campo Sano Dr., Coral Gables, Florida, USA
^{94}
Warsaw University Observatory, Aleje Ujazdowskie 4, 00478
Warszawa,
Poland
Received:
1
April
2013
Accepted:
23
January
2014
Planck data have been used to provide stringent new constraints on cosmic strings and other defects. We describe forecasts of the CMB power spectrum induced by cosmic strings, calculating these from network models and simulations using lineofsight Boltzmann solvers. We have studied NambuGoto cosmic strings, as well as field theory strings for which radiative effects are important, thus spanning the range of theoretical uncertainty in the underlying strings models. We have added the angular power spectrum from strings to that for a simple adiabatic model, with the extra fraction defined as f_{10} at multipole ℓ = 10. This parameter has been added to the standard six parameter fit using COSMOMC with flat priors. For the NambuGoto string model, we have obtained a constraint on the string tension of Gμ/c^{2} < 1.5 × 10^{7} and f_{10} < 0.015 at 95% confidence that can be improved to Gμ/c^{2} < 1.3 × 10^{7} and f_{10} < 0.010 on inclusion of highℓ CMB data. For the AbelianHiggs field theory model we find, Gμ_{AH}/c^{2}< 3.2 × 10^{7} and f_{10} < 0.028. The marginalised likelihoods for f_{10} and in the f_{10}–Ω_{b}h^{2} plane are also presented. We have additionally obtained comparable constraints on f_{10} for models with semilocal strings and global textures. In terms of the effective defect energy scale these are somewhat weaker at Gμ/c^{2} < 1.1 × 10^{6}. We have made complementarity searches for the specific nonGaussian signatures of cosmic strings, calibrating with allsky Planck resolution CMB maps generated from networks of postrecombination strings. We have validated our nonGaussian searches using these simulated maps in a Planckrealistic context, estimating sensitivities of up to ΔGμ/c^{2} ≈ 4 × 10^{7}. We have obtained upper limits on the string tension at 95% confidence of Gμ/c^{2} < 9.0 × 10^{7} with modal bispectrum estimation and Gμ/c^{2} < 7.8 × 10^{7} for real space searches with Minkowski functionals. These are conservative upper bounds because only postrecombination string contributions have been included in the nonGaussian analysis.
Key words: cosmic background radiation / cosmological parameters / early Universe / largescale structure of Universe / cosmology: theory / cosmology: observations
© ESO, 2014
1. Introduction
This paper, one of a set associated with the 2013 release of data from the Planck^{1} mission (Planck Collaboration I 2014), describes the constraints on cosmic strings, semilocal strings and global textures. Such cosmic defects are a generic outcome of symmetrybreaking phase transitions in the early Universe (Kibble 1976) and further motivation came from a potential role in largescale structure formation (Zeldovich 1980; Vilenkin 1981a). Cosmic strings appear in a variety of supersymmetric and other grand unified theories, forming at the end of inflation (see, for example, Jeannerot et al. 2003). However, further interest in cosmic (super)strings has been motivated by their emergence in higherdimensional theories for the origin of our Universe, such as brane inflation. These superstring variants come in a number of D − and F −string forms, creating hybrid networks with more complex dynamics (see, e.g., Polchinski 2005). Cosmic strings can have an enormous energy per unit length μ that can give rise to a number of observable effects, including gravitational lensing and a background of gravitational waves. Here, we shall concentrate on the impact of strings on the cosmic microwave background (CMB), which includes the generation of linelike discontinuities in temperature. Comparable effects can also be caused by other types of cosmic defects, notably semilocal strings and global textures. As well as influencing the CMB power spectrum, each type of topological defect should have a counterpart nonGaussian signature giving us the ability distinguish between different defects, alternative scenarios, or systematic effects. The discovery of any of these objects would profoundly influence our understanding of fundamental physics, identifying GUTscale symmetry breaking patterns, perhaps even providing direct evidence for extra dimensions. Conversely, the absence of these objects will tightly constrain symmetry breaking schemes, again providing guidance for high energy theory. For a general introduction to cosmic strings and other defects, refer to Vilenkin & Shellard (2000); Hindmarsh & Kibble (1995); Copeland & Kibble (2010).
High resolution numerical simulations of cosmic strings using the NambuGoto action indicate that cosmological networks tend towards a scaleinvariant solution with typically tens of long strings stretching across each horizon volume. These strings continuously source gravitational perturbations on subhorizon scales, the magnitude of that are determined by the dimensionless parameter: (1)where η is the energy scale of the stringforming phase transition and is the Planck mass. String effects on the CMB power spectrum have been estimated using a phenomenological string model and, with WMAP and SDSS data, these estimates yield a 2σ upper bound of Gμ/c^{2} < 2.6 × 10^{7} (Battye & Moss 2010). A consequence is that strings can be responsible for no more than 4.4% of the CMB anisotropy signal at multipole ℓ = 10.
As we shall discuss, the evolution of NambuGoto string networks is computationally challenging and quantitative uncertainties remain, notably in characterising the string smallscale structure and loop production. An alternative approach has been to use field theory simulations of cosmological vortexstrings. These yield a significantly lower number of strings per horizon volume (less than half), reflecting the importance of radiative effects on the microphysical scales being probed numerically. The degree of convergence with NambuGoto string simulations is difficult to determine computationally at present, but there are also global strings for which radiative effects of comparable magnitude are expected to remain important on cosmological scales. It is prudent in this paper, therefore, to constrain both varieties of strings, labelling the field theory constraints as AH from the AbelianHiggs (local U(1)) model used to describe them. Given these quantitative differences, such as the lower density, field theory strings produce a weaker constraint Gμ_{AH}/c^{2} < 5.7 × 10^{7} using WMAP data alone (Bevis et al. 2008) and (Urrestilla et al. 2011). The shape of the stringinduced power spectrum also has a different shape, which allows up to a 9.5% contribution at ℓ = 10. These WMAP constraints can be improved by adding smallscale CMB anisotropy in a joint analysis. The NambuGoto strings limit improves to become Gμ/c^{2} < 1.7 × 10^{7} (using SPT data, Dvorkin et al. 2011) and field theory strings yield Gμ_{AH}/c^{2} < 4.2 × 10^{7} (Urrestilla et al. 2011). Powerspectrum based constraints on global textures were studied in Bevis et al. (2004) and (Urrestilla et al. 2008), with the latter paper giving a 95% limit of Gμ/c^{2} < 4.5 × 10^{6}. Urrestilla et al. (2008) also provide constraints on semilocal strings, Gμ/c^{2} < 5.3 × 10^{6}.
Constraints on cosmic strings from nonGaussianity require high resolution realisations of stringinduced CMB maps that are extremely challenging to produce. Low resolution smallangle and fullsky CMB maps calculated with the full recombination physics included, have indicated some evidence for a significant kurtosis from strings (Landriau & Shellard 2011). More progress has been made in creating high resolution maps from string lensing after recombination (see Ringeval & Bouchet (2012) and references therein) and identifying, in principle, the bispectrum and trispectrum, which can be predicted for strings analytically (Hindmarsh et al. 2009, 2010; Regan & Shellard 2010). The first WMAP constraint on cosmic strings using the analytic CMB trispectrum yielded Gμ/c^{2} < 1.1 × 10^{6} at 95% confidence (Fergusson et al. 2010b). An alternative approach is to fit pixelspace templates to a map, this method was applied to global textures templates in Cruz et al. (2007) and Feeney et al. (2013, 2012).
The most stringent constraints that are claimed for the string tension arise from predicted backgrounds of gravitational waves that are created by decaying loops (Vilenkin 1981b). However, these constraints are strongly dependent on uncertain string physics, most notably the network loop production scale and the nature of string radiation from cusps, i.e., points on the strings approaching the speed of light c. The most optimistic constraint based on the European Pulsar Timing Array is Gμ/c^{2} < 4.0 × 10^{9} (van Haasteren et al. 2011), but a much more conservative estimate of Gμ/c^{2} < 5.3 × 10^{7} can be found in Sanidas et al. (2012), together with a string parameter constraint survey and an extensive discussion of these uncertainties. Such gravitational wave limits do not apply to global strings or to strings for which other radiative channels are available.
Alternative topological defects scenarios also have strong motivations and we report limits on textures and global monopoles in this paper as well. Of particular recent interest are hybrid networks of cosmic strings where the correlation length is reduced by having several interacting varieties (e.g., F and Dstrings) or a small reconnection probability, p < 1. We expect to investigate these models using the Planck full mission data.
The outline of this paper is as follows. In Sect. 2 we briefly describe the different types of topological defects that we consider, and their impact on the CMB anisotropies. We also discuss how the CMB power spectrum is computed and how we obtain CMB maps with a cosmic string contribution. In Sect. 3 we present the defect constraints from the CMB power spectrum (with numbers given in Table 2), while Sect. 4 discusses searches for topological defects with the help of their nonGaussian signature. We finally present the overall conclusions in Sect. 5.
2. Theoretical modelling and forecasting
2.1. Cosmic strings and their cosmological consequences
2.1.1. String network evolution
A detailed quantitative understanding of the cosmological evolution of string networks is an essential prerequisite for making accurate predictions about the cosmological consequences of strings. Fortunately, all string network simulations to date have demonstrated convincingly that the largescale properties of strings approach a selfsimilar scaleinvariant regime soon after formation. If we treat the string as a onedimensional object, then it sweeps out a twodimensional worldsheet in spacetime (2)where the worldsheet parameters ζ^{0} and ζ^{1} are timelike and spacelike respectively. The NambuGoto action that governs string motion then becomes (3)where γ_{ab} = g_{μν}∂_{a}x^{μ}∂_{b}x^{ν} is the twodimensional worldsheet metric (γ = det(γ_{ab})) induced by the spacetime metric g_{μν}. The NambuGoto action Eq. (3) can be derived systematically from a field theory action, such as that for the AbelianHiggs model describing U(1) vortexstrings: (4)where φ is a complex scalar field, F^{μν} is the U(1) field strength and D_{μ} = ∂_{μ} + iA_{μ} is the gaugecovariant derivative with e and λ dimensionless coupling constants. The transverse degrees of freedom in φ can be integrated out provided the string is not strongly curved, that is, the string width δ ≈ ħc/η ≪ L where L is the typical radius of curvature. For a cosmological string network today with Gμ/c^{2} ~ 10^{7}, these two lengthscales are separated by over 40 orders of magnitude, so this should be a valid approximation.
In an expanding universe, the NambuGoto action Eq. (3) yields a Hubbledamped wave equation governing the string motion. These equations can be solved numerically, provided “kinks” or velocity discontinuities are treated carefully. However, they can also be averaged analytically to describe the scaleinvariant evolution of the whole string network in terms of two quantities, the energy density ρ and the rms velocity v. Any string network divides fairly neatly into two distinct populations of long (or “infinite”) strings ρ_{∞} stretching beyond the Hubble radius and the small loops ρ_{l} with length l ≪ H^{1} that the long strings create Kibble (1985). Assuming the long strings form a Brownian random walk characterised by a correlation length L, we have (5)and the averaged equations of motion become simply (6) where measures the network loop production rate and k(v) is a curvature parameter with . This is the velocitydependent onescale (VOS) model and, with a single parameter , it provides a good fit to both Nambu and field theory simulations, notably through the radiationmatter transition (Martins & Shellard 1996).
A general consensus has emerged from the three main simulation codes describing NambuGoto string networks (Martins & Shellard 2006; Ringeval et al. 2007; BlancoPillado et al. 2011). These independent codes essentially solve for left and rightmoving modes along the string using special techniques to handle contact discontinuities or kinks, including “shock fronting”, artificial compression methods and an exact solver for piecewise linear strings, respectively. The consistency between simulations is shown in Table 1 for the string density parameter ζ defined in Eq. (5). Averaging yields the radiation era density ζ = 10.7 and a matter era value ζ = 3.3. Note that these asymptotic values and the intervening matterradiation transition can be welldescribed by the VOS model Eq. (6) with . The matter era VOS value appears somewhat anomalous from the other two simulations, but this is obtained from larger simulations in a regime where convergence is very slow, so it may more closely reflect the true asymptotic value. These simulations have also advanced the study of string smallscale structure and the loop distribution, about which there had been less consensus (see, e.g., BlancoPillado et al. 2011). However, note that CMB anisotropy is far less sensitive to this issue compared to constraints from gravitational waves.
Field theory simulations using lattice gauge techniques have also been employed to study the evolution of string networks in an expanding universe. Comparatively, these threedimensional simulations are constrained to a lower dynamic range and the simulations require the solution of modified field equations to prevent the string core width shrinking below the lattice resolution. On the other hand, field theory simulations include field radiation and therefore provide a more complete account of the string physics. In Table 1 the lower string densities obtained from two sets of AbelianHiggs simulations are given (Moore et al. 2002; Bevis et al. 2007b). The evolution can be fitted with a VOS model Eq. (6) with , which is 150% higher than for NambuGoto strings. Field theory simulations have further important applications, particularly for describing delocalised topological defects such as textures, for describing models that do not form stable defects like semilocal strings, and because they include radiative effects naturally. Radiative effects observed in current AbelianHiggs simulations are comparable to the radiative damping anticipated for cosmological global strings and so the AH analysis below should offer some insight into this case.
95% upper limits on the constrained parameter f_{10} and the derived parameter Gμ/c^{2} for the five defect models discussed in the text.
2.1.2. String gravity and the CMB
Despite the enormous energy per unit length μ, the spacetime around a straight cosmic string is locally flat. The string has an equation of state p_{z} = −ρ, p_{x} = p_{y} = 0 (for one lying along the zdirection), so there is no source term in the relativistic version of the Poisson equation ∇^{2}Φ = 4πG(ρ + p_{x} + p_{y} + p_{z}). The straight string exhibits no analogue of the Newtonian pull of gravity on any surrounding matter. But this does not mean the string has no gravitational impact; on the contrary, a moving string has dramatic effects on nearby matter or propagating CMB photons.
The spacetime metric about a straight static string takes the simple form, (7)that looks like Minkowski space in cylindrical coordinates, but for the fact that the azimuthal coordinate θ has a restricted range 0 ≤ θ ≤ 2π(1−4Gμ). The spacetime is actually conical with a global deficit angle Δ = 8πGμ, that is, an angular wedge of width Δ is removed from the space and the remaining edges identified (see Fig. 1). This means that distant galaxies on the opposite side of a cosmic string can be gravitationally lensed to produce characteristic double images.
Fig. 1
The spacetime around a cosmic string is conical, as if a narrow wedge were removed from a flat sheet and the edges identified. For this reason cosmic strings can create double images of distant objects. Strings moving across the line of sight will cause linelike discontinuities in the CMB radiation. 

Open with DEXTER 
Fig. 2
Characteristic CMB temperature discontinuity created by a cosmic string. Here, the simulated NambuGoto string has produced a cusp, a small region on the string that approaches the speed of light, which has generated a localised CMB signal. 

Open with DEXTER 
Cosmic strings create linelike discontinuities in the CMB signal. As the string moves across the line of sight, the CMB photons are boosted towards the observer, causing a relative CMB temperature shift across the string, given by (Gott III 1985; Kaiser & Stebbins 1984) (8)where v_{s} is the transverse velocity of the string and . This rather simple picture, however, is complicated in an expanding universe with a wiggly string network and relativistic matter and radiation components. The energymomentum tensor T_{μν}(x,t) essentially acts as a source term for the metric fluctuations that perturb the CMB photons and create temperature anisotropies. Essentially, the problem can be recast using Green’s (or transfer) functions G^{μν} that project forward the contributions of strings from early times to today: (9)where is the lineofsight direction for photon propagation and x_{obs} is the observer position. The actual quantitative solution of this problem entails a sophisticated formalism to solve the Boltzmann equation and then to follow photon propagation along the observer’s lineofsight. An example of the linelike discontinuity signal created by a cosmic string in the CMB is shown in Fig. 2. In this case, a string cusp has formed on the string, causing a strongly localised signal and reflecting the Lorentz boost factor in Eq. (9).
2.2. Semilocal strings
The tight constraints on the presence of cosmic strings that we will discuss later in this paper start to put pressure on the wide class of inflation models that generate such defects (Hindmarsh 2011). The power of these constraints would be reduced if the strings could be made unstable. This is the basic motivation behind semilocal strings: a duplication of the complex scalar field φ in the AbelianHiggs action (4), occurring naturally in a range of inflation models (Urrestilla et al. 2004; Dasgupta et al. 2004, 2007; Achucarro et al. 2006), transforms the stable cosmic strings into nontopological semilocal strings (Vachaspati & Achucarro 1991) as the vacuum manifold becomes S^{3}, which is simplyconnected. The existence and stability of the semilocal strings is thus a question of dynamics rather than due to the topology of the vacuum manifold. In general we do not expect to form long strings, but rather shorter string segments, as the semilocal strings can have ends. The evolution of these segments is very complicated and arises directly from the field evolution, so that it is only practicable to simulate these defects with the help of field theory (Urrestilla et al. 2008).
2.3. Global defects
A large alternative class of defects is due to the breaking of a global O(N) symmetry (rather than a gauge symmetry as in the case of cosmic strings) of a Ncomponent scalar field φ. The energy density of global defects is significantly less localised than those that result from gauge symmetry breaking due to the absence of the screening by a gauge field, and there are thus longrange forces between the defects. The field selfordering is therefore very efficient for all types of defects with N ≥ 2, leading to a generic scaling of the defect energy density with the background energy density (see e.g., Durrer et al. 2002). For this reason global monopoles (N = 3) do not overclose the Universe as their local counterparts would. In this paper we study specifically the case N = 4 called “texture”, which can arise naturally in many multifield inflation models that involve a nonzero vacuum expectation value and symmetry breaking. In this case there are no stable topological defects present, but contrary to local texture, global texture can have a nonnegligible impact on the perturbations in the cosmos, with the field selfordering leading to “unwinding events”. In spite of their nontopological nature, the field evolution is closely related to the one of lowerdimensional stable global defects due to the longrange nature of the forces. This is similar to the case of the nontopological semilocal strings of the previous section, and indeed the semilocal example can be seen as an intermediate case between cosmic strings and global texture: Starting from the semilocal action, we can on the one hand revert to the cosmic string action by removing one of the complex scalar fields, and on the other hand we find the texture action if we remove the gauge field.
The normalisation of global defects is usually given in terms of the parameter ε = 8πGη^{2}/c^{2} when using an action like Eq. (4) (with a second complex scalar field but without the gauge fields). However, for a simpler comparison with the cosmic string results we can recast this in terms of Gμ/c^{2} ≡ ε/ 4 and quote limits on Gμ/c^{2} also for the texture model, as in Urrestilla et al. (2008).
2.4. CMB power spectra from cosmic defects
The CMB power spectrum from topological defects, like strings, is more difficult to compute than the equivalent for inflationary scenarios that predict a spectrum dominated by an adiabatic component with a possible, but highly constrained, isocurvature component. In defectbased scenarios the perturbations are sourced continuously throughout the history of the Universe, as opposed to adiabatic and isocurvature modes that are the result of initial conditions. In principle this requires knowledge of the source, quantified by the unequaltime correlator (UETC) of the defect stressenergy tensor, from the time of defect formation near the GUT scale to the present day – a dynamic range of about 10^{52} – something that will never be possible to simulate. Fortunately, we can use the scaling assumption to extrapolate the results of simulations with substantially smaller dynamic range. This has allowed a qualitative picture to emerge of the characteristics of the power spectra from defects, though quantitative predictions differ. Here, we will focus on spectra calculated in two different ways for cosmic strings, as well as spectra from semilocal strings and texture models.
Defectbased power spectra are dominated by different physical effects across the range of angular scales. (i) On large angular scales the spectra are dominated by an integrated SachsWolfe (ISW) component due to the strings along the lineofsight between the time of last scattering and the present day. The scaling assumption implies that this component will be close to scale invariant, although in practice it typically has a mildly blue spectrum. (ii) At intermediate scale the dominant contribution comes from anisotropies created at the time of last scattering. In contrast to the strong series of acoustic peaks created in adiabatic and isocurvature models, defects produce only a broad peak because their contributions are not coherent. (iii) At very small angular scales, the spectra are again dominated by the ISW effect because, rather than decaying exponentially due to the effects of Silk damping, there is only powerlaw decay with the exponent being a characteristic of the specific type of defect.
The standard lore is to treat the defect stress energy tensor, θ_{μν}, as being covariantly conserved at first order, which is known as the “stiff approximation”. In principle, this means that it is necessary to measure two independent quantities from the simulations, or model them. The other two component are then computed from the conservation equations. In practice things are a little more complicated since it is necessary to provide the UETC (10)where τ is the conformal time and k is the wavenumber. Once one has the UETC, then there two ways to proceed. The first involves creating realisations of the defect stressenergy whose power spectra are computed then averaged to give the total power spectrum. The other approach involves diagonalization of the UETC. During pure matter or radiation domination, the scaling property of defect evolution means that quantities are measured relative to the horizon scale, so that the UETC is only a function of x = kτ and x′ = kτ′. These functions U(x,x′) can be discretized and then are symmetric matrices that we can diagonalize. The resulting eigenvectors can be inserted as sources into a Boltzmann code, and the resulting C_{ℓ} are then summed up, weighted by the eigenvalues (Pen et al. 1997; Durrer et al. 2002). Even though the power spectrum resulting from each “eigensource” exhibits a series of acoustic peaks, the summation over many such spectra smears them out, as they are not coherent (unlike inflationary perturbations). This smearingout explains why defect power spectra generically are smooth, as mentioned above.
Fig. 3
Cosmic string power spectra used in this analysis: NAMBU (black dashed), AHmimic (blue dotted) and AH (red solid). The spectra have been set to equal power at ℓ = 10. When normalised to 850 μK at ℓ = 10 they correspond to string tensions of Gμ/c^{2} = 1.17 × 10^{6}, 1.89 × 10^{6} and 2.04 × 10^{6} respectively. Note that the limits discussed in this paper mean that the CMB spectra presented here are less than 3% of the overall power spectrum amplitude and hence the differences observed at high ℓ do not have a large effect. 

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There are also several methods to obtain predictions for the UETCs of cosmic strings and other topological defects. The first approach we will consider for cosmic strings is to use what has become known as the Unconnected Segment Model (USM; Albrecht et al. 1997, 1999; Pogosian & Vachaspati 1999). In its simplest form this models the cosmic string energy momentum tensor as that of an ensemble of line segments of correlation length ξd_{H}(t), moving with an rms velocity ⟨ v^{2} ⟩ ^{1/2}, where d_{H}(t) is the horizon distance. In addition one can take into account the effects of string “wiggles” due to smallscale structure via a coefficient, β = μ_{eff}/μ quantifying the ratio of the renormalised mass per unit length to the true value. The model parameters ξ, ⟨ v^{2} ⟩ ^{1/2} and β are computed from simulations. In our calculations we link the USM sources to the lineofsight Boltzmann solver CMBACT (Pogosian & Vachaspati 1999) to create an ensemble of realisations from which we find an averaged angular power spectrum.
There are two USMbased models that we will use in this analysis which we believe span the realistic possibilities – we note a more general approach marginalising over three string parameters is proposed in Foreman et al. (2011) (see also recent work in Avgoustidis et al. 2012). The first USM model, which we will refer to as NAMBU, is designed to model the observational consequences of simulations of cosmic string simulations performed in the NambuGoto approximation. In these simulations the scaling regime is different in the radiation and matter eras, with (ξ, ⟨ v^{2} ⟩ ^{1/2}/c,β)_{rad} = (0.13,0.65,1.9) and (ξ, ⟨ v^{2} ⟩ ^{1/2}/c,β)_{mat} = (0.21,0.60,1.5) and the extrapolation between the two is modelled by using the velocity dependent onescale model (Martins & Shellard 1996). In the second, which we will refer to as AHmimic, we attempt to model the field theory simulations using the AbelianHiggs model described below, with (ξ, ⟨ v^{2} ⟩ ^{1/2}/c,β) = (0.3,0.5,1) independent of time.
The other approach that we will consider is to measure the UETC directly from a simulation of cosmic strings in the AbelianHiggs model, which we will refer to as AH. The AbelianHiggs model involves a complex scalar field φ and a gauge field A_{μ} described earlier Eq. (4), for which the dimensionless coupling constants e and λ are chosen with λ = 2e^{2}, so that the characteristic scales of the magnetic and scalar energies are equal, (see Bevis et al. (2007b,a) for further details about the model). We then simulate the evolution of the fields on a grid, starting from random initial conditions designed to mimic a phase transition, followed by a brief period of diffusive evolution, to rapidly reach a scaling solution expected to be typical of the configuration found long after the phase transition. As the simulation is performed in comoving coordinates, the string width is effectively decreasing as time passes. To enlarge the dynamical range available, we partially compensate this shrinking with an artificial string fattening. We perform runs for various values of the fattening parameter to ensure that the results are not affected by it.
Fig. 4
Comparison between global texture (black dashed) and semilocal (blue dotted) string power spectra and the AH field theory strings (red solid), normalised to unity at ℓ = 10. As expected, the SL spectrum lies in between the TX and the AH spectra. The AH spectrum was recomputed for the Planck cosmological model with sources from Bevis et al. (2010), and the SL and TX spectra were taken from Urrestilla et al. (2008). 

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During the simulations, we compute the energymomentum tensor at regular intervals and decompose it into scalar, vector and tensor parts. We store these components once scaling is reached, and compute the UETCs by correlating them with later values of the energymomentum tensor. UETCs from several runs are averaged, diagonalized and then fed into a modified version of the CMBEASY Boltzmann code (Doran 2005) to compute the CMB power spectra (both temperature and polarisation). The spectra used in this paper were derived from fieldtheory simulations on a 1024^{3} grid and used the extrapolation to substring scales described in Bevis et al. (2010), which are expected to be accurate at the 10% level to ℓ_{max} ≈ 4000.
In Figs. 3 and 4 we present the spectra we will use in subsequent analysis. The higher dashed black curve is the spectrum computed using the USM for the NAMBU model, and the smaller dashed blue and solid red curves the AHmimic model and the AH model, respectively. We should note that when normalised to the amplitude of the observed CMB anisotropies on largescales at ℓ = 10, the three models give Gμ/c^{2} = 1.17 × 10^{6}, 1.89 × 10^{6} and 1.9 × 10^{6} for the NAMBU, AHmimic and AH models, respectively. The reasons for differences between the spectra for these two approaches are discussed in Battye & Moss (2010). Briefly, the main reasons for the differences are twofold: First, the overall normalisation, which is due to the NAMBU models having smaller values of ξ, more strings per horizon volume, and larger values of β, with each of the string segments being heavier, than the two AH models. Both these effects mean that a lower value of Gμ/c^{2} is required to achieve the same amplitude for the anisotropies. Secondly, the enhanced peak at small angular scales, which is caused by the value of ξ being smaller in the radiation era than in the matter era, meaning that there are more strings per horizon volume in the radiation era when the smallscale anisotropy is imprinted, and hence more anisotropy on those scales for a given Gμ/c^{2}.
The method used for the semilocal strings (denoted SL) and O(4) global texture (denoted TX) is fundamentally the same as for the AH model: we simulate the field theory on a discretized grid and compute the energymomentum tensor at regular intervals. From these snapshots we derive the UETCs by correlating the scalar, vector and tensor parts at different times. The only difference is the fieldtheory action being used in the simulations. In Fig. 4 we present the spectra we used for the semilocal strings and global textures, taken from Urrestilla et al. (2008). These models are also shown with the AH cosmic string model for comparison.
2.5. Maps of CMB anisotropies from cosmic strings
In order to go further than the twopoint correlation function, we have used numerical simulations of NambuGoto cosmic string evolution in an FLRW spacetime to generate various CMB synthetic maps. The use of simulations is crucial to produce realistic string configurations on our past light cone and have been the subject of various code development in the last twenty years (see Albrecht & Turok 1989; Bennett & Bouchet 1989, 1990; Allen & Shellard 1990; Vincent et al. 1998; Moore et al. 2001; Ringeval et al. 2007; BlancoPillado et al. 2011). Until recently, the underlying numerical challenges have limited the resolution of the full sky maps to an angular resolution of 14′ (corresponding to a HEALPix resolution of N_{side} = 256) in Landriau & Shellard (2003, 2011) (see also early work in Allen et al. 1996). In order to extend the applicability of these maps to the small scales probed by Planck, we have used the maps described in Ringeval & Bouchet (2012) that have an angular resolution of 0.85′ (N_{side} = 4096). This map is obtained by considering the ISW contribution from (10), sourced by the NambuGoto stress tensor, and which can be recast into the form (Stebbins & Veeraraghavan 1995) (11)The integral is performed over all string position vectors X = { X^{i} } intercepting our past line cone (in the transverse temporal gauge). Primes and dots denote differentiation with respect to the spatial and timelike worldsheet coordinates ζ^{1} and ζ^{0} respectively, while dl is the invariant string length element. Taking the limit gives back the small angle and flat sky approximation used in Hindmarsh (1994); Bouchet et al. (1988); Fraisse et al. (2008). For generating the full sky map, Eq. (12) has been evaluated without any other approximation and required more than 3000 NambuGoto string simulations of various sizes to fill the whole comoving volume between the observer and the last scattering surface. We note that the use of different simulations does not induce any visible artefact, essentially because only the subset of strings intercepting our past light cone leaves imprints in the CMB. As a result, the probability of observing an edge remains very small. Discussions of these effects and details on the numerics can be found in Ringeval & Bouchet (2012).
This method therefore includes all string effects from the last scattering surface till today, but does not include the Doppler contributions induced by the strings into the plasma prior to recombination. As a result, our full sky map represents the ISW contribution from strings, which is dominant at large and small scales but underestimates the signal on intermediate length scales where recombination effects on the surface of last scattering dominate (see the discussion in Sect. 2.4). This can be seen directly by making a qualitative comparison between the ISW string power spectrum, obtained from the simulated maps and shown in Fig. 5, with the full CMB string power spectrum predicted for Nambu strings shown in Fig. 3 (dashed line). We therefore expect the string searches based on the simulated maps to be less constraining than those using the power spectrum, though certainly robust as any linelike gravitating object should generate such a signal.
Fig. 5
Integrated SachsWolfe angular power spectra extracted from the full sky cosmic string maps at different resolutions (labelled by N_{side}), with or without applying the antialiasing procedure (see text). The antialiasing filtering gives back the correct power up to ℓ_{max} ≲ 2N_{side}. 

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Calibration and training for the nonGaussian searches of Sect. 4 have required the generation of new full sky and statistically independent cosmic string maps. The numerical challenges underlying the N_{side} = 4096 map (Ringeval & Bouchet 2012) are such that it was numerically too expensive to create another one of the same kind. At this resolution, the computations typically require 800 000 cpuhours, so we have chosen to generate three new maps at a lower resolution of 1.7′, i.e., N_{side} = 2048. Unfortunately, at this lower resolution, the simulated string maps, hereafter referred to as raw maps, exhibit a strong aliasing at small scales that could have induced spurious systematics even after convolution with the Planck beam. This aliasing concerns pixelsized structures and comes from the method used to numerically evaluate Eq. (12). In order to save computing time, the signal associated with each pixel is only computed at the centroid direction . This has the effect of including some extra power associated with string smallscale structure that is below the pixel angular size, thereby aliasing power into the map. In order to address this problem, we have used semianalytical methods to design an optimal antialiasing filter, both in harmonic space and in real space. As discussed in Fraisse et al. (2008); Bevis et al. (2010), the small scale angular temperature power spectrum slowly decays as a power law ℓ^{−p} such that any deviations from this behaviour can only come from the aliasing. For each N_{side} = 2048 raw map, we have performed a multiparameter fit of the power spectrum, and of the onepoint distribution function, to extract, and then removes, its small scale aliasing contribution. In order to validate the procedure, we have checked that the power spectrum of each of the filtered maps matches the one associated of the raw N_{side} = 4096 map, the latter being also being affected but at half the scale. In Fig. 5, we have plotted the power spectra of one of the N_{side} = 2048 maps before and after convolution with our antialiasing filter. As expected, it matches with the one extracted from the N_{side} = 4096 map (here truncated at ℓ = 4096). We note that the string bispectra reconstructed from the antialiased N_{side} = 2048 maps and the N_{side} = 4096 maps are essentially identical, as discussed in Sect. 4.2.2 and shown in Fig. 11. Finally, in order to include the effects associated with the HEALPix pixelization scheme, the antialiased maps have been convolved with the HEALPix pixel window function before being used for further processing.
Fig. 6
All sky Mollweide projection of the simulated cosmic strings CMB sky after convolution by a Gaussian beam of 5′ resolution. The colour scale indicates the range of (ΔT/T)/(Gμ/c^{2}) fluctuations. 

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Fig. 7
A 20° gnomic projection patch extracted from the full sky map and zooming into string induced temperature steps (see Fig. 6). Applying the spherical gradient magnitude operator enhances the temperature steps, and thus the string locations, even more (right). 

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In total, this method has provided four theoretical full sky string maps that have been used in the string searches we will discuss in Sect. 4. As an illustration, we have represented in Fig. 6, one of the filtered string map after convolution by a Gaussian beam of FWHM = 5′. The colour scale traces the relative temperature anisotropies ΔT/T, divided by the string tension Gμ/c^{2}. The anisotropy patterns may look Gaussian at first because most of the string signatures show up on the smallest length scales. In Fig. 7, we have plotted a gnomic projection representing a field of view of 20°, in which the temperature steps are now clearly apparent. The right panel of Fig. 7 represents the magnitude of the spherical gradient, which enhances the steps.
Finally, in order to provide a much larger statistical sample beyond only four string realisations, we have also produced a collection of 1000 small angle patches (7.2°) of the CMB sky derived in the flat sky approximation (Stebbins 1988; Hindmarsh 1994; Stebbins & Veeraraghavan 1995; Bouchet et al. 1988; Fraisse et al. 2008). Although the largescale correlations are lost, these maps have been shown to accurately reproduce various analytically expected nonGaussian string effects such as the onepoint and higher npoints functions by Takahashi et al. (2009), Hindmarsh et al. (2009), Hindmarsh et al. (2010), Regan & Shellard (2010), Yamauchi et al. (2010b), Yamauchi et al. (2010a), Ringeval (2010).
3. Power spectrum constraints on cosmic strings and other topological defects
In order to compute constraints on cosmic string scenarios we just add the angular power spectrum to that for an simple adiabatic model – which assumes that they are uncorrelated – with the fraction of the spectrum contributed by cosmic strings being f_{10} at ℓ = 10. This parameter is then added as an extra parameter to the standard six parameter fit using COSMOMC and the Planck likelihood described in Planck Collaboration XV (2014). We use a Flat ΛCDM cosmology defined through the physical densities of baryons, Ω_{b}h^{2}, and cold dark matter, Ω_{c}h^{2}, the acoustic scale, θ_{MC}, the amplitude, A_{s} and spectral index, n_{s} of density fluctuations and the optical depth to reionization τ. The Hubble constant is a derived parameter and is given by H_{0} = 100 h km s^{1} Mpc^{1}. We use the same priors on the cosmological and nuisance parameters as are used in Planck Collaboration XVI (2014) and use WMAP polarisation data to help fix τ. In addition to just using the Planck data, we have also added highℓ CMB data from SPT and ACT to obtain stronger constraint(Sievers et al. 2013; Hou et al. 2014).
For the USMbased models we use the approach used in Battye et al. (2006) and Battye & Moss (2010). We find that the constraints on the standard six parameters are not significantly affected by the inclusion of the extra string parameter and that there are no significant correlations with other parameters (see Table 3). For the case of Planck data only and using the NAMBU model we find that Gμ/c^{2} < 1.5 × 10^{7} and f_{10} < 0.015, whereas for the AHmimic model we find that Gμ/c^{2} < 3.6 × 10^{7} and f_{10} < 0.033, with all the upper limits being at 95% confidence level. The 1D marginalised likelihoods for f_{10} are presented in the upper panels of Fig. 8. The differences between the upper limits for the NAMBU and AHmimic models is compatible with those seen previously using WMAP 7year and SDSS data (Battye & Moss 2010). The upper limits from this version of the Planck likelihood are better than those computed from WMAP7+SPT (Dvorkin et al. 2011) and WMAP7+ACT (Dunkley et al. 2011) and are significantly better than those from WMAP7+SDSS (Battye & Moss 2010). Based on the Planck “Blue Book” values for noise levels we predicted (Battye et al. 2008) a limit of Gμ/c^{2} < 6 × 10^{8}, while the present limit is about a factor of two worse than this. The main reason for this is that the projected limit ignored the need for nuisance parameters to model high ℓ foregrounds and that not all the frequency channels have been used. The corresponding limits for the AH model are f_{10} < 0.028 and Gμ/c^{2} < 3.2 × 10^{7}.
There is now very little degeneracy between the f_{10} and n_{S} parameters, something that was not the case for WMAP alone (Battye et al. 2006; Bevis et al. 2008; Urrestilla et al. 2011). This has implication for supersymmetric hybrid inflation models as discussed in Battye et al. (2010) that typically require n_{S}> 0.98. The simplest versions of these models appear to be ruled out. The strongest correlation using the NAMBU and AH mimic models is between f_{10} and Ω_{b}h^{2} as illustrated in Fig. 10. For the AH model the correlation between f_{10} and the amplitude of primordial perturbations, A_{s}, is of a comparable magnitude, for all other parameters (including the nuisance parameters) the correlations are even less important. In addition, we find in agreement with Lizarraga et al. (2012), that there are significant correlations between the amount of strings f_{10} in the AH model and the number of relativistic degrees of freedom N_{eff} as well as between f_{10} and the primordial helium abundance Y_{He}. We leave a detailed study of these correlations to later work.
Constraints on the fitted cosmological parameters in the case of Planck alone for the cosmic strings models (NAMBU, AHmimic and AH), semilocal strings (SL) and texture (TX).
Fig. 8
Marginalised constraints on f_{10} for topological defects from Planck data plus polarisation from WMAP (Planck+WP). The left panel show constraints on cosmic strings, with NAMBU in black dashed, AHmimic in blue dotted and AH in red solid. The right panel show the constraints on SL (blue dotted) and TX (black dashed) compared to AH (again solid red). 

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Fig. 9
Marginalised constraints on f_{10} for topological defects with highℓ CMB data from SPT and ACT added to the Planck + WP constraints data (compare with constraints shown in Fig. 8). The left panel show constraints on cosmic strings, with NAMBU in black dashed, AHmimic in blue dotted and AH in red solid. The right panel show the constraints on SL (blue dotted) and TX (black dashed) compared to AH (solid red). 

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In Fig. 8 we also present the 1D marginalised likelihoods for the texture and semilocal string models (compared to the AH field theory strings). The resulting constraints on the f_{10} parameter are given in Table 2 as well. For the conversion into constraints on Gμ/c^{2} we have that for semilocal strings Gμ_{10}/c^{2} = 5.3 × 10^{6} and for global texture Gμ_{10}/c^{2} = 4.5 × 10^{6}, cf. Urrestilla et al. (2008). We notice that, as expected for a fixed Gμ, semilocal strings lead to significantly less anisotropies than cosmic strings (a factor of about 8 in the C_{ℓ}), and texture are similar to the semilocal strings. We thus expect significantly weaker constraints on Gμ for the SL and TX models, especially since in addition the constraints on f_{10} for these models are weaker. Indeed we find a 95% limit of Gμ/c^{2} < 1.10 × 10^{6} for semilocal strings and Gμ/c^{2} < 1.06 × 10^{6} for global textures.
Fig. 10
Marginalised likelihoods in the f_{10}Ω_{b}h^{2} plane for the NAMBU model in blue and the AH mimic model in red using Planck +WP. This is the strongest correlation with any of the standard cosmological parameters. 

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4. NonGaussian searches for cosmic strings
Cosmic strings and other topological defects generically create nonGaussian signatures in the cosmic microwave sky, counterparts of their inevitable impact on the CMB power spectrum. This is a critical test of differentiating defects from simple inflation, while offering the prospect of direct detection. Searches for these nonGaussian defect signatures are important for two key reasons: on the one hand, constraints from the CMB power spectrum can be susceptible to degeneracies with cosmological parameters in the standard concordance model; on the other hand, any apparent defect detection in the power spectrum should have a welldefined prediction in higherorder correlators or other nonGaussian signals, and vice versa. NonGaussian tests can also be used to distinguish cosmic defects from residual foregrounds or systematic contributions. Below we will present results from NG tests that seek strings in multipole space (bispectrum) and in real space (Minkowski functionals), as well as hybrid methods (wavelets).
4.1. Foregrounds, systematics and validation
It is wellknown that the microwave sky contains not only the CMB signal but also emission from different astrophysical contaminants. In particular, point source emission is expected to be a special cause of confusion for cosmic defects, notably those with high resolution signatures, such as cosmic strings. In addition, systematic effects may also be present in the maps at a certain level. Therefore, before claiming a cosmological origin of a given detection, alternative extrinsic sources should be investigated and discarded. This can be done by performing a number of consistency checks in the data, most of which are common to the other nonGaussianity papers, where they are discussed in greater detail. Here, we provide a brief summary of the main issues.
Foregroundcleaned CMB maps are provided using four different component separation techniques (for further details, see Planck Collaboration XII 2014): SMICA (semiblind approach); NILC (internal linear combination in needlet space);SEVEM (internal template fitting); and Commander/Ruler (CR, parametric method). These four foregroundseparation methods are complimentary in that some work in pixel space while others in harmonic space (or a combination with wavelets). They were tested using the most realistic Planck simulations available, i.e. the Full Focal Plane (FFP) version 6, including demonstration that they preserved nonGaussian signals as we will discuss below. In determining the robustness of a particular constraint, we note that it should be replicated with at least two different cleaned CMB maps. The adoption of different masks that exclude different regions of the sky (ranging from more aggressive to more conservative) has also been used to test the stability of nonGaussian estimators. Further tests entail the use of cleaned maps at different frequencies (for instance, those provided by the SEVEM foreground separation technique). A given detection should be consistent at all frequencies, since the behaviour of contaminants and systematic effects will, in general, vary with frequency. A further test is the study of noise maps constructed from the difference between two Planck maps (either at the same or at different frequencies) smoothed to the same resolution. These maps will not contain the CMB signal and, therefore, any NG detection should vanish on them. The opposite would indicate that the claimed result is due to foreground residuals or to the presence of systematic effects.
The methodologies described below were tested using several approaches, passing through the nonGaussian validation suite, involving realistic FFP6 simulations, and culminating in a series of Planck String Challenges instituted for this purpose. The nonGaussianity validation tests are described in detail elsewhere (see Planck Collaboration XXIV 2014) and the realistic FFP6 simulations also (see Planck Collaboration 2013), nevertheless we include a summary here because of their importance also for the validation of cosmic string searches. A set of 96 nonGaussian maps, with given local, equilateral and orthogonal signals, were created using the methods described in Fergusson et al. (2010a), to which was added coloured and anisotropic noise as specified from the SMICA cleaned map. All NG estimators, notably the modal bispectrum method, were required to identify these (unknown) input signals within the expected precision. Realistic Planck FFP6 simulations, including an unknown nonGaussian signal, were then used for the next level of validation. These simulations are intended to provide a complete description of the full Planck mission for both HFI and LFI instruments, including the best current estimates of foreground templates (CIB, CO, freefree, thermal dust etc.), the lensed primordial CMB signal (using lensPIX), timestream effects, such as satellite pointing, focal plane geometries, and ringbyring detector noise spectra, and finally the simulated timeordered data was synthesised together using the Planck mapmaking pipeline at each frequency. The FFP6 maps were then passed through the four componentseparation pipelines and NG estimators (both modal and MF) were able to detect the (unknown) f_{nl} = 20.4 signal (see Planck Collaboration XXIV 2014). We note the caveat that the FFP simulations continue to evolve and improve by incorporating systematic effects more completely and realistically, including “deglitching” and polarisation effects in the near future. Given the available time and resources, the FFP6 simulation set (on which 15M core hours were expended) represents the current stateoftheart for this first Planck defects analysis, as well as other nonGaussian analysis.
Similar to the nonGaussian validation suite, the Planck String Challenges were blind tests employing postrecombination string simulation maps, with an unknown Gμ/c^{2} (as described in Sect. 2.5), coadded to a Gaussian CMB map (created using WMAP7 cosmological parameters). The effect of a 5 arcmin beam was added, together with anisotropic SEVEM noise, and the same mask was employed as for the nonGaussian analysis (f_{sky} = 0.73) For calibrating the string searches, a further three string simulations were also provided (without noise). A further 1000 ΛCDM Gaussian maps with SEVEM noise and beam effects were also provided for validation and calculating linear correction terms. The second challenge incorporated improvements in the coloured SEVEM noise model and lensed Gaussian CMB maps. The aim was to determine the sensitivity of the proposed nonGaussian tests and to see if the Gμ/c^{2} in the challenge map could be measured accurately. The results from these challenges were an important part of the validation for each of the methods described below. In addition, Gaussian FFP6 simulations pipelines for each of the component separation methods were available for determining whether expected foreground residuals were correlated with the string signal.
4.2. Cosmic string bispectrum
4.2.1. Modal bispectrum methods
The CMB bispectrum is the three point correlator of the a_{lm} coefficients, . For the purposes of a search for cosmic strings we assume the network cumulatively creates a statistically isotropic signal, that is, we can employ the angleaveraged reduced bispectrum b_{ℓ1ℓ2ℓ3}, defined by (12)where h_{ℓ1ℓ2ℓ3} is a weakly scaledependent geometrical factor and is the wellknown Gaunt integral over three Y_{ℓm}s that can be expressed in terms of Wigner3j symbols. The CMB bispectrum b_{ℓ1ℓ2ℓ3} is defined on a tetrahedral domain of multipole triples { ℓ_{1}ℓ_{2}ℓ_{3} } satisfying both a triangle condition and ℓ<ℓ_{max} set by the experimental resolution. When seeking the string bispectrum in the Planck data, we employ the following estimator to find or limit its amplitude: (13)where we assume a nearly diagonal covariance matrix C_{ℓ1m1,ℓ2m2} ≈ C_{ℓ}δ_{ℓ1ℓ2}δ_{m1 − m2} and we modify C_{ℓ} and b_{ℓ1ℓ2ℓ3} appropriately to incorporate instrument beam and noise effects, as well as a cutsky. To simplify Eq. (14), we have ignored the “linear term” (which is included in the analysis). A much more extensive introduction to bispectrum estimation can be found in Planck Collaboration XXIV (2014).
A key step in observational searches for nonseparable bispectra, such as those induced by cosmic strings (denoted by ), is to expand it into separable modes (Fergusson & Shellard 2009; Fergusson et al. 2010a) taking the signaltonoiseweighted form: (14)where the modes are constructed from symmetrized products (the n label a distanceordering for the triples { prs }). The product basis functions Q_{n}(ℓ_{1},ℓ_{2},ℓ_{3}) are not in general orthogonal, so it is very useful to construct a related set of orthonormal mode functions R_{n}(ℓ_{1},ℓ_{2},ℓ_{3}) such that ⟨ R_{n},R_{p} ⟩ = δ_{np}. Substituting the separable mode expansion (15) reduces the estimator (14) to the simple form (15)where the coefficients are found by integrating products of three Planck maps filtered using the basis function (an efficient product with each map multiplied by the separable q_{r}(ℓ)). We can validate this estimator by using the modal methodology to create CMB map realisations for cosmic strings from the predicted with a given Gμ/c^{2} (see Fergusson et al. 2010a). It is easy to show that the expectation value for for such an ensemble of maps in the orthogonal basis should be (16)Alternatively, we can exploit this fact by reconstructing the from given CMB map realisations created directly from string simulations, an approach we will adopt here.
4.2.2. Postrecombination string bispectrum
Fig. 11
Coefficients Eq. (15) for the hybrid Fourier mode expansion of the cosmic string bispectrum Eq. (15). The average value (black line) is in remarkable agreement with all four string simulations as can be seen for n < 30 (lower panel), with each exhibiting better than a 97% correlation overall. 

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In order to estimate the string bispectrum at Planck resolution we employed the modal reconstruction method Eq. (17) on the postrecombination string simulations described in Sect 2.5. These string maps include the accumulated linelike discontinuities induced by the string network on CMB photons propagating from the surface of last scattering to the present day. This work does not include recombination physics, that is, contributions from the surface of last scattering that will increase the string anisotropy signal substantially. As discussed previously, there are four fullsky maps of two different resolutions, which were provided for the purpose of calibrating Planck searches for cosmic strings (Ringeval & Bouchet 2012). For the modal analysis, we have adopted the hybrid polynomial basis augmented with a local shape mode (in total with n_{max} = 600 modes), as well as a hybrid Fourier basis (n_{max} = 300), which are both described in Planck Collaboration XXIV (2014).
To extract the string bispectrum in a Planckrealistic context, we chose a fairly high nonGaussian signal with Gμ/c^{2} = 1 × 10^{6}. As for the Planck String Challenges, described in Sect. 4.1, the normalised string maps were added to noise maps generated by the component separation pipelines of SMICA, NILC and SEVEM, creating twelve sets of 200 simulated string realisations. Each of these maps was then filtered using the modal estimator to find the coefficients appropriate for each componentseparation method. After averaging each set of modal coefficients over the different (unmasked) noise realisations, we found remarkable consistency between the estimated for the four string simulations as shown in Fig. 11 for the Fourier modes. Agreement was good across all the 300 modes determined, as shown in detail for n = 1−30 (see the lower panel of Fig. 11).
Quantitatively, the different string simulations produced bispectrum shapes that had above 97% correlations with each other (i.e., for ). The overall integrated bispectrum amplitudes was consistent to within 4%. Despite only four string map simulations, these are small errors relative to experimental and theoretical uncertainties. This robustness indicates that the overall string bispectrum signal at Planck resolution is a statistical summation of very many contributions from the millions of strings between the observer and the last scattering surface. To ensure the bispectrum C_{l} weighting was not significantly affected by the presence of the large string signal, we repeated the modal extraction procedure for Gμ/c^{2} = 5 × 10^{7} (the string bispectrum amplitude reduced by a factor of 8). For the same string simulation, the shape correlations for different Gμ/c^{2} were 99.4% or above and the amplitude scaled as expected with (Gμ/c^{2})^{3} to within 2%. The string bispectrum shown in Fig. 11 is well converged with random errors from the averaging procedure small relative to the actual signal. We conclude that, assuming the physics and numerical accuracy of the string simulations that are available, we have extracted a string bispectrum of sufficient accuracy for the present nonGaussian analysis.
The overall threedimensional reconstruction of the string bispectrum shape is shown in Fig. 12, normalised in the usual way to approximately illustrate the signaltonoise expected (that is, removing an overall l^{4} scaling, by dividing by the constant SachsWolfe bispectrum shape). The first point to note is that the bispectrum is negative, reflecting the underlying string velocity correlations and curvature correlations that have created it; in the expanding universe, curved strings preferentially collapse, creating a negative temperature fluctuation towards the centre and a positive signal outside. In the overall spectrum, the n = 0 mode is dominant, but it is modulated by other modes providing further interesting structure that could be described as broad arms extending along each axis (see Fig. 11); although somewhat “squeezed”, the correlation with the local model is low. The string simulation power spectrum shown in Fig. 5 can be understood to be quantitatively modulating the string bispectrum away from the axes, with the signal slowly decaying beyond (say) l_{1},l_{2}>500 in the l_{3} direction.
The CMB bispectrum and trispectrum induced by the postrecombination gravitational effects of cosmic strings have been estimated analytically (Hindmarsh et al. 2009, 2010; Regan & Shellard 2010). With simplifying assumptions, these predicted that the constant mode would be dominant with a broad central “equilateral” peak, but not the substructure observed in Fig. 12. In terms of missing physics in this postrecombination string bispectrum, we expect the recombination signal to lie in the range ℓ = 200−1000 (shown in the full NAMBU power spectrum in Fig. 3) and to significantly enhance the overall amplitude of the bispectrum (see also Landriau & Shellard 2011, where recombination physics is included).
The correlation of the postrecombination string bispectrum with standard primordial shapes is small, because it does not contain an oscillatory component from the transfer functions. The local, equilateral and orthogonal bispectrum models correlate with strings at about 6%, 11% and 12%, respectively. There is also a CMB ISWlensing bispectrum arising from the correlation between gravitational lensing and the latetime integrated SachsWolfe effect arising from the underlying dominant Gaussian fluctuations (see, for example, the discussion in Planck Collaboration XXVI 2014). Like the string bispectrum, the ISWlensing bispectrum is also mainly negative, but it is much more squeezed/flattened and correlates at only about 11% with the present string bispectrum. So the predicted ISW signal should provide a small positive bias for string detection of about 0.44σ. Diffuse pointsource contamination is of greater concern because at ℓ_{max} = 2000 this has a 40% anticorrelation with strings (for the simple Poissondistributed point source template with = constant). This close relationship with point sources requires a joint analysis (see below). Other foreground contamination must also be considered, as we shall discuss, and for this we rely on realistic simulated FFP6 foreground residuals provided by the Planck component separation pipelines (see Planck Collaboration XII 2014).
Fig. 12
Modal reconstruction of the postrecombination string bispectrum Eq. (15) extracted from Planck resolution map simulations. This is a 3D view of the allowed tetrahedral set of multipoles (ℓ_{1},ℓ_{2},ℓ_{3}) showing isosurfaces of the bispectrum density with darker blue for more negative values (it is normalised relative to the constant SW bispectrum). 

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4.2.3. Planck string bispectrum results
Using the modal bispectrum estimator, we have searched for the string bispectrum in the Planck CMB maps obtained using the foregroundseparation techniques SMICA, NILC and SEVEM. We note that the modal estimator has passed through the full validation suite of NG tests described in the Planck Collaboration XXIV (2014), where further details about the analysis can be found. In summary, we have used the standard U73 mask, which includes a Galactic cut and a conservative point source mask, together with “inpainting” as in the f_{NL} analysis (essentially apodizing the mask). Together with the SMICA, NILC and SEVEM foreground separated maps, realistic noise simulations as specified for the particular foregroundcleaned map, were used to determine the estimator’s linear correction term and to determine the bispectrum variance, which was very nearly optimal. For calibration purposes, we always compare to the string model with tension Gμ/c^{2} = 1 × 10^{6} defining a string bispectrum parameter and normalising it to have f_{NL} = 1 in this case. The standard deviation Δf_{NL} = 0.2 obtained from this Planck analysis would imply a 5σ detection of Gμ/c^{2} = 1 × 10^{6} strings. The strong scaling of the bispectrum amplitude on the string tension ∝ (Gμ/c^{2})^{3}, implies a given measurement yields Gμ/c^{2} = (f_{NL})^{1/3} × 10^{6}.
The results of the string bispectrum estimation for each of the SMICA, NILC and SEVEM maps are shown in Table 4. As shown by the nonGaussian analysis (see Planck Collaboration XXIV 2014), the Planck data exhibits significant detections of both the predicted ISWlensing bispectrum (above 2σ) and a residual point source signal (over 3σ). Since these may be confused with the string signal, we also quote their measurements in this Fourier mode basis. The ISWlensing signal detection is described at length in Planck Collaboration XXVI 2014. The residual point source (PS) signal is discussed in Planck Collaboration XXIV 2014 where it is modelled as a simple Poissonian distribution. In principle, the PS amplitude can be extrapolated from source count models, but direct comparisons remain a goal for future Planck analysis. An independent analysis of the ISWlensing, point source and string contributions to each map showed no evidence for a cosmic string signal (all estimates were were within 1σ, refer to the third column of Table 4). However, given the large contribution of diffuse point sources and their anticorrelation with the string bispectrum, we have also undertaken a joint analysis of the Planck data (which in this case is the same as marginalising over the point source signal). Before doing so, we subtract the expected ISW lensing signal that provides a f_{NL} = 0.09 string bias. The fifth column in Table 4 shows that marginalising point sources enhances the string signal up to the 2σ level for all component separation methods; essentially the constant mode becomes more strongly negative once the measured point sources are removed.
Other foregrounds, such as dust emission, could potentially produce spurious string signals if not subtracted properly. Foreground contamination has been extensively studied within the Planck simulation pipeline (FFP6) and foreground residual maps have been provided by each component separation team (including those for thermal dust, CO emission, freefree, synchrotron, spinning dust, kinetic and thermal SZ etc). We have analysed these residual FFP6 maps provided by both SMICA and NILC to seek evidence of correlations with the string bispectrum; individually these foregrounds make only small contributions (apart from PS), but cumulatively their effect cannot be neglected. The SMICA combinedresidual map, without point sources and analysed with realistic noise, produces a string bias of f_{NL} = 0.23, which after ISW subtraction becomes f_{NL} = 0.14 (relative to a variance Δf_{NL} = 0.20). After both ISW and foreground residual subtraction, a joint analysis with point sources yields a SMICA string signal f_{NL} = 0.37 ± 0.21 (Col. 5 in Table 4). The apparent string bias in NILC from residual foregrounds was even higher f_{NL} = 0.22 (after ISW subtraction), meaning a joint analysis obtained f_{NL} = 0.23 ± 0.21 (see Table 4).
Modal bispectrum analysis of foregroundseparated SMICA, NILC and SEVEM maps showing f_{NL} from strings, ISWlensing and diffuse point sources.
We conclude, given our present understanding of point sources and foregrounds, that there does not appear to be significant evidence for a string bispectrum signal in the Planck nominal mission maps, so we infer the following postrecombination bispectrum constraint on strings: (17)Here, we have taken the more conservative SMICA result f_{NL} = 0.37 ± 0.21, because of its preferred status for foreground separation techniques in Planck Collaboration XII (2014). The susceptibility of the string bispectrum to point source and other foreground contamination deserves further investigation and will require improved characterisation of the diffuse point source bispectrum (beyond the simple Poisson model), as well as identification of the specific foreground residuals which primarily contribute to the small string bias found in the FFP6 simulations.
The string bispectrum constraint Eq. (18) is a conservative upper limit on the string tension Gμ/c^{2} because we have not included recombination contributions. Although this constraint is weaker than that from the power spectrum, it is an independent test for strings and the first quantitative string bispectrum limit to date. This should be considerably improved in future by inclusion of recombination physics and more precise foreground analysis. A comparison with the power spectrum amplitude indicates the string bispectrum should rise by (2)^{3/2}, which, together with the full mission data, would see the sensitivity improve by a factor of two (allowing constraints around Gμ/c^{2} < 4 × 10^{7}). We note that the bispectrum is not the optimal nonGaussian test for strings, because the string signal is somewhat suppressed by symmetry (the bispectrum cancels for straight strings). This fact motivates further study of the trispectrum, for which the Planck sensitivity is forecast to be ΔGμ/c^{2} ≈ 1 × 10^{7} (Fergusson et al. 2010b), as well as joint analysis of polyspectra.
4.3. Steerable wavelet searches for cosmic strings
Wavelets offer a powerful signal analysis tool due to their ability to localise signal content in scale (cf. frequency) and position simultaneously. Consequently, wavelets are wellsuited for detecting potential CMB temperature contributions due to cosmic strings, which exhibit spatially localised signatures with distinct frequency content. Wavelets defined on the sphere are required to analyse fullsky Planck observations (see, for example, Freeden & Windheuser 1997; Wiaux et al. 2005; Sanz et al. 2006; McEwen et al. 2006; Starck et al. 2006; Marinucci et al. 2008; Wiaux et al. 2008a).
We perform an analysis using the steerable wavelets on the sphere constructed by Wiaux et al. (2005). Here we exploit steerability to dynamically adapt the orientations analysed to the underlying data, performing frequentist hypothesis testing. We apply the first (1GD) and second (2GD) Gaussian derivative steerable wavelets, defined on the sphere through a stereographic projection, in order to search for cosmic strings in the Planck data. A steerable wavelet is a directional filter whose rotation by χ ∈ [ 0,2π) about itself can be expressed in terms of a finite linear combination of nonrotated basis filters. Thus, the analysis of a signal with a given steerable wavelet Ψ naturally identifies a set of wavelet coefficients, W_{Ψ}(ω_{0},χ,R), which describe the local features of the signal at each position ω_{0} on the sphere, for each orientation χ and for each physical scale R. Several local morphological properties can be defined in terms of the wavelet coefficients (Wiaux et al. 2008b), including the signedintensity, (18)This quantity represents the value of the wavelet coefficient at the local orientation that maximizes the absolute value of the wavelet coefficient itself. Let us emphasise that the signedintensity morphological property is a highly nonlinear quantity, i.e., , where a and b are two signals on the sphere.
Fig. 13
Deviation of the kurtosis of the signedintensity as a function of Gμ/c^{2}, normalised to the standard deviation of CMB and noise simulations: ΔK/σ = (K(R,Gμ/c^{2}) − K(R,Gμ/c^{2} = 0)) /σ. The left panel shows results for the 1GD wavelet and the right shows the 2GD wavelet. Each curve corresponds to a wavelet scale, R (arcmin), included in the analysis. The final sensitivity of the method is determined by combining the two wavelets and all the scales. 

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The presence of a cosmic string signal in the CMB is expected to leave a nonGaussian signature that induces a modification in the distribution of I(ω_{0},R) with respect to the lensed Gaussian case. We calibrated the dependence of these signatures on the string tension using four simulations of the cosmic string contribution (Ringeval & Bouchet 2012) combined with a set of lensed Gaussian CMB realisations, along with a realistic description of the Planck instrumental properties (refer to Planck Collaboration 2013).
A wide range of string tension values were explored, Gμ/c^{2} ∈ [ 2.0 × 10^{7},1.0 × 10^{6} ], considering several wavelet scales, R = [4.0,4.5,5.0,6.0,8.0,10.0,15.0,20.0] arcmin. We use maps at a HEALPix resolution of N_{side} = 2048, including multipoles up to ℓ_{max} = 2500. We analyse the simulations with the same U73 mask of the Planck CMB map (refer to Planck Collaboration XII 2014), which masks both diffuse and compact foregrounds, leaving 73% of the sky remaining for further analysis (refer to discussion in Sect. 4.2.3). When computing the wavelet coefficients of a masked data set, artefacts are introduced close to the mask borders. We therefore define a set of exclusion masks such that, at each scale R, an extra region of the sky is excluded when computing any statistical measure. At each scale the exclusion mask is obtained by expanding the mask borders by three times the width of the corresponding wavelet.
The string nonGaussian signatures are characterised in terms of the kurtosis of the signedintensity I(ω_{0},R) in Eq. (19) at the different scales R and for both the 1GD and 2GD wavelets. The averaged results from the nonGaussian simulations were used to model the distribution of the kurtosis as functions of Gμ/c^{2}, i.e., K(R,Gμ/c^{2}). Other statistics, such as the skewness and the HigherCriticism (e.g., Donoho & Jin 2004; Cayón et al. 2005), have also been explored. We found that the kurtosis sensitivity to the string tension is higher than the alternative measures. In Fig. 13 we show the difference between the average kurtosis at several Gμ/c^{2} values and the average kurtosis for Gμ/c^{2} = 0, normalised to the standard deviation of the simulations. On the given range of scales, the 2GD wavelet appears to be more sensitive to the string signal. The final sensitivity of the method in recovering the string tension can be assessed from simulated data. We compare each simulation to the averaged model through a χ^{2} test, thus estimating Gμ/c^{2} for the simulation. The test is performed jointly on the two wavelets for all the scales, and taking into account the correlations by means of a covariance matrix estimated from CMB and noise simulations. From the distribution of the Gμ/c^{2} values recovered from the simulations the null hypothesis can be rejected at 95% CL for Gμ/c^{2}> 7 × 10^{7}.
The same χ^{2} test was applied to the SEVEM CMB cleaned map, observing no evidence of a string signal at any of the scales studied. Despite the absence of strings, however, we noted that the χ^{2} of the best fit solution was higher than anticipated, corresponding to a probability to exceed (PTE) of 2%. We identified the cause for such a poor fit to the null result as an incompatibility between the data and simulations at the smallest scales. We note that this incompatibility is not related to the potential presence of a string signal, since it biases the nonGaussian estimators towards the opposite direction, as reflected also in the χ^{2} values. Similar behaviour is also noticed for the skewness of and, to a lesser extent, for the HigherCriticism measure.
We have extensively explored the causes of this incompatibility at small scales. First of all, we verified that such a behaviour is present also in the SMICA CMB solution, as well as SEVEM. We then analysed the halfring halfdifference SEVEM CMB maps, and we compared it to pure noise simulations. Indeed, halfring maps are made from the data in the first half or second half of each stable pointing period, therefore we can obtain an estimate of the noise in the data by taking half of the difference between the two maps. We conclude that the halfring noise estimate and noise simulations look compatible. We evaluated the impact on the estimator of unresolved point sources, both from radio galaxies and submillimetre starforming galaxies, using simulations of these astrophysical components processed through the component separation pipelines (Planck Collaboration XII 2014). We found that at a wavelet scale of R = 4 arcmin, these residual foregrounds induce a shift in the kurtosis, ΔK/σ = 0.03, i.e., a bias that is negligible for the present analysis. This shift only increases to more than ΔK/σ = 0.3 when extending the analysis to wavelet scales as small as R = 2.5 arcmin. Finally, we also studied the SEVEM cleaned maps at 143 and 217 GHz, for which we considered wider galactic cuts (mask G56 and G35 from Planck Collaboration XV 2014). Since the inconsistency does not show a significant dependence on the frequency, there is no clear evidence for residual foreground contamination playing a major role.
At this point, it is worth stressing two important properties of the nonGaussian statistics considered in this section. On the one hand, as mentioned above, it is a very nonlinear estimator and, on the other, it depends on the local orientation of the sky signal. In fact, it is the only estimator considered in this paper that has such orientationdependence. This is a critical point, since it implies that the simulations (lensed CMB, noise and foreground residuals) have to be more sophisticated if they are to capture the corresponding local anisotropic characteristics. This is especially difficult to achieve for the residual foregrounds, which are in part based on foreground models with smallscale fluctuations produced through isotropic and Gaussian extrapolations. As a consequence, we cannot discard completely either instrumental or foreground systematics at the smallest scales causing these incompatibilities. Nevertheless, we note that this lack of anisotropic modelling is not crucial for other estimators, as the angular power spectrum, or even the bispectrum, because these are isotropic quantities.
For the reasons given above, we have restricted our steerable wavelets analysis to scales R ≥ 6 arcmin, where simulations are better understood for our specific purpose and where they appear compatible with the data. Analysing SEVEM on this angular range we find Gμ/c^{2} < 7 × 10^{7} at 95% CL. The next Planck release will continue to improve the modelling of instrumental and foreground properties and, therefore, we expect to be able to fully exploit the steerable wavelet capabilities down to the smallest scales (R = 2.5 arcmin). Based on simulations, this can significantly improve the sensitivity of the estimator, allowing constraints of Gμ/c^{2} < 4 × 10^{7} at 95% CL.
Finally, we note that we have also endeavoured to study the simulated string maps using spherical wavelets, making an extension of previous work (Wiaux et al. 2008a; Hammond et al. 2009) to compute the Bayesian posterior distribution of the string tension. Both the spherical and steerable wavelet methods offer good prospects for improved nonGaussian string constraints from the Planck full mission data.
4.4. Real space tests for cosmic strings
4.4.1. Minkowski functionals method
Minkowski Functionals (MFs) describe morphological properties of the CMB field, and can be used as generic estimators of nonGaussianities (Planck Collaboration XXIII 2014). However, they have been considered to constrain specific NG models such as cosmic strings, for example on gradient temperature maps (see e.g., Gott et al. 1990). Indeed they have sensitivity to nonGaussianity sourced by strings at all orders (i.e., including the kurtosis or trispectrum) and they could prove to be a powerful tool to constrain topological defects in general. For the sake of brevity and conciseness, precise definitions of MFs and analytic formulations are presented in Planck Collaboration XXIII (2014) and, here, we only review how MFs can be used to constrain the string energy density Gμ/c^{2}. We follow the Bayesian method discussed in Ducout et al. (2012) for the local model but which can quite similarly be applied to the string case.
We measure the four normalised^{2} functionals v_{k}(k = 0,3) (respectively Area, Perimeter, Genus and N_{cluster}), computed on n_{th} = 26 thresholds ν, between ν_{min} = −3.5 and ν_{max} = + 3.5 in units of the standard deviation of the map. The four functionals are similarly sensitive to cosmic strings and we build a statistics using the combination of all functionals, forming one vector y (of size n = 104).
The principle of this Bayesian method is to compare measurement of MFs on Planck data ŷ to the MFs model curve for strings at the level Gμ/c^{2}, y(Gμ/c^{2}). The Bayes formula is (19)We take a flat prior for the parameter Gμ/c^{2}, with P(Gμ/c^{2}) being a constant over a reasonable range of values for Gμ/c^{2}, mostly determined from previous experiments (between 0 and 1e6). The evidence ^{∫}P(ŷ  Gμ/c^{2})P(Gμ/c^{2})dGμ/c^{2} is being considered as a normalisation factor.
The likelihood P(ŷ  Gμ/c^{2}) is a multivariate Gaussian: ν_{max} was chosen not too extreme, to avoid sensitivity to rare events, and the map’s filtering allows to probe a sufficient number of independent harmonic modes to keep fluctuations small. The likelihood’s Gaussianity has also been verified systematically at each point, using simulations. More details on the likelihood are discussed in Gott et al. (1990); Ducout et al. (2012). This allows us to define a simple χ^{2} test for Gμ/c^{2} and the posterior becomes (20)with (21)The covariance matrix C is computed from 10^{4} Gaussian simulations^{3}: to verify the Gaussian approximation, tests have been performed using nonGaussian matrices over a dozen values of Gμ/c^{2} and covariance matrices and χ^{2} remained constant within numerical precision; furthermore the number of Gaussian simulations used to estimate the covariance matrix guarantees the stability of the statistics for these threshold values (see convergence tests in Ducout et al. 2012).
The cosmic string model curve is calibrated on 10^{3} realistic lensed Planck simulations, to which we have added a string component at a specified level. These simulations take into account the asymmetry of beams and the component separation process (FFP6 simulations, see Planck Collaboration 2013, for a detailed description). For the string component, we had at our disposal only two high resolution string map simulations (Ringeval & Bouchet 2012), so our model is the averaged curve obtained from this combination of Planck and string simulations.
Due to the nonlinear dependence of MFs on Gμ/c^{2} and the small number of string simulations, the posterior distribution is quite complex and noisy. For this reason, we evaluated the posterior at n_{NL} = 51 values of Gμ/c^{2}, between 0 and 10 × 10^{7}, to obtain our Planck estimate for Gμ/c^{2}. This estimate is stable and has been validated in realistic conditions with the Planck String Challenges described above, and for which we found consistent results with the underlying (unknown) Gμ/c^{2}.
4.4.2. Minkowski functionals results
For the constraint on Gμ/c^{2}, we analysed the foregrounds separated SMICA map at N_{side} = 2048 and ℓ_{max} = 2000, using the U73 mask (f_{sky} = 73% of the sky is unmasked). The smallest point sources holes were inpainted. We applied two specific Wiener filters to the map, designed to enhance the information from the map itself (W_{M}) and from the gradients of the map (). The filters are shown in Fig. 14.
Additionally, we estimated the average impact of some residual foregrounds and secondaries (FG) on Gμ/c^{2}, using the linear properties of MFs and foregrounds models processed through the Planck simulation pipeline (FFP6 simulations). Uncorrelated (Poissonian) unresolved point sources (PS), Cosmic Infrared Background (CIB) and SunyaevZeldovich cluster^{4} (SZ) signals can be introduced as a simple additive bias on MFs’ curves following: (22)These biases are obtained as the average obtained on 100 simulations.
Fig. 14
The two Wiener filters, W_{M} and W_{D1}, used to constrain Gμ/c^{2} with Minkowski functionals. 

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Fig. 15
Posterior distribution of the parameter Gμ/c^{2} obtained with Minkowski functionals. This estimate takes into account the lensing of the data, but not the effects of foreground residuals. 

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We eventually obtain the posterior distribution of Gμ/c^{2} (Fig. 15). As mentioned previously, the posterior curve is complex and noisy and so as to give an estimate of Gμ/c^{2} we report its credible interval at 95%^{5}. Results are summarized in Table 5, for raw data (lensing only is accounted for and subtracted) and foreground subtracted data (lensing, PS, CIB and SZ are considered). The discrepancy between the two filters can be explained because the derivative filter W_{D1} scans smaller scales than W_{M} so it is more easily biased by foreground residuals. Given the remaining foreground uncertainties, we take the most conservative of the MFs constraints for the cosmic string contribution to the Planck data to be The corresponding posterior is presented in Fig. 15.
Some caveats need to be mentioned that may influence these results. First, for the MF method itself, an important limitation is the small number of string simulations used to calibrate the estimator. The estimator appears to be mostly sensitive to lowredshift strings (infinite strings, with redshifts between 0 and 30), and this is affected by cosmic variance. As lowredshift string simulations are much faster to produce than complete simulations back to recombination, it should be possible to improve the robustness of the constraint using these relatively soon. Secondly, the impact of Galactic residuals should be assessed in further detail, especially for the filter W_{D1} that we have observed to be less robust against residuals than the W_{M} filter.
With advances in studying these experimental effects there are good prospects for the full mission data, the sensitivity of the MFs estimator should improve substantially, with simulations forecasting possible MF cosmic string constraints of Gμ/c^{2} < 3 × 10^{7} at the 95% C.I.
We note that further real space analysis of string map simulations has been undertaken with scaling indices of the pixel temperature distribution (see, e.g., Räth et al. 2011). Extensions calculating a set of anisotropic scaling indices along predefined directions appear to offer good prospects for string detection.
MFs constraints obtained on Gμ/c^{2}, at the 95% C.I.
5. Conclusions
We have reviewed the signatures induced by cosmic strings in the CMB and searched for these in the Planck data, resulting in new more stringent constraints on the dimensionless string tension parameter Gμ/c^{2}. A prerequisite for accurate constraints on cosmic strings is a quantitative understanding of both cosmological string network evolution and the effects they induce in the CMB. These are computationally demanding problems but progress has been made recently on several fronts: first, high resolution simulations of NambuGoto strings have yielded robust results for the scaleinvariant properties of string networks on large scales, while there has been increasing convergence about smallscale structure and loops (for which the CMB predictions are less sensitive). Secondly, postrecombination gravitational effects of strings have been incorporated into fullsky Planck resolution CMB temperature maps that are important for validating nonGaussian search methods. Finally, fast Boltzmann pipelines to calculate CMB power spectra induced by causal sources have been developed and tested at high resolution, whether for field theory simulations of strings or textures or for models of NambuGoto strings. Threedimensional field theory simulations of vortexstrings at sufficient resolution should, in principle, converge towards the onedimensional NambuGoto string simulations, but testing this is not numerically feasible at present. For this reason, we believe it is prudent to also include constraints on field theory strings (labelled Gμ_{AH}), thus encompassing cosmic string models for which radiative effects are important at late times (such as global strings). We believe this brackets the important theoretical uncertainties that remain, that is, we have used the best available information to constrain both NambuGoto strings (NAMBU) and field theory strings (AH). This work has also obtained more stringent constraints on semilocal strings and global textures.
5.1. Cosmic string constraints and the CMB power spectrum
Accurate forecasts for the CMB power spectrum induced by cosmic strings are more difficult to compute than their equivalent for simple adiabatic inflationary scenarios. It requires knowledge of the source, quantified by the unequaltime correlator (UETC) of the defect stressenergy tensor, from well before recombination to the present day, which is not computationally feasible. Fortunately, we can exploit scaleinvariant string evolution to extrapolate the results of simulations with substantially smaller dynamic range. We use two methods to obtain predictions for the UETCs. An unconnected segment model (USM) is used to model the properties of an evolving string network, determining its density from an analytic onescale evolution model, and the sources are coupled to the lineofsight Boltzmann solver CMBACT. A second independent pipeline measures the UETCs directly from string simulations in the AbelianHiggs field theory, passing these to a modified form of the CMBEASY Boltzmann code. The resulting NambuGoto and AbelianHiggs string CMB power spectra are illustrated in Fig. 3. Free parameters in the USM model can be chosen to phenomenologically match the field theory UETCs (denoted the AHmimic model) and the comparison is also shown in Fig. 3, validating the two independent pipelines.
To compute constraints on cosmic string scenarios we have added the angular power spectrum to that for a simple adiabatic model, assuming that they are uncorrelated, with the fraction of the spectrum contributed by cosmic strings being f_{10} at ℓ = 10. This has been added to the standard 6 parameter fit using COSMOMC with flat priors. For the USM models we have obtained the constraint for the NambuGoto string model (23)while for the AbelianHiggs field theory model we find, (24)The marginalised likelihoods for f_{10} and in the f_{10}–Ω_{b}h^{2} plane were presented in Fig. 10. With Planck nominal mission data these limits are already about a factor of two more stringent than the comparable WMAP 7year string constraints and these Planck limits improve further with the inclusion of highℓ data.
5.2. NonGaussian searches for cosmic strings
Complementary searches for nonGaussian signatures from cosmic strings were performed and we have reported constraints from the string bispectrum, steerable wavelets and Minkowski functionals. These methods participated in the Planck String Challenges and have undergone nonGaussian validation tests.
The postrecombination string bispectrum has been reconstructed and calibrated from stringinduced CMB maps using a modal estimator. String challenge analysis with Planckrealistic noise simulations and mask indicated a nominal mission sensitivity of ΔGμ/c^{2} ≈ 5.8 × 10^{7}. Analysis of SMICA, NILC and SEVEM foregroundseparated maps has yielded f_{NL} = 0.37 ± 0.21 for the string bispectrum shape, which translates into a bispectrum constraint on the string tension, Gμ/c^{2} < 9.0 × 10^{7} (95% CL). Steerable wavelet methods have been calibrated on string simulation maps added to Gaussian CMB maps with realistic noise and masking, showing a sensitivity of up to ΔGμ/c^{2} ≈ 4 × 10^{7}. The string signal was shown to have greater impact on the kurtosis of the signedintensity than on its skewness, and no evidence of a string signal was found in the Planck data. Minkowski functionals have been applied to string simulation maps in a Planckrealistic context, computing the four functionals – area, perimeter, genus and N_{cluster} – after application of Weiner filters. Using these distributions, a Bayesian estimator has been constructed to constrain the string tension. Analysis of the SMICA foregroundcleaned maps yielded a MF constraint of Gμ/c^{2} < 7.8 × 10^{7} (95% CL).
NonGaussian searches for strings are complementary to the power spectrum analysis and yield constraints as low as Gμ/c^{2} < 7.8 × 10^{7}, though we note the potential impact of foreground residuals in limiting current precision. These are conservative upper bounds because they only include postrecombination string contributions, unlike the string power spectrum analysis. Having such a broad suite of tools, ranging from multipole space, through wavelets, to real space detection methods, allows crossvalidation and reinforces the conclusion that there is at present no evidence for cosmic strings in the Planck nominal mission data.
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 (in particular the lead countries France and Italy), with contributions from NASA (USA) and telescope reflectors provided by a collaboration between ESA and a scientific consortium led and funded by Denmark.
Raw Minkowski functionals V_{k} depend on the Gaussian part of fields through a normalisation factor A_{k}, that is a function only of the power spectrum shape. We therefore normalise functionals v_{k} = V_{k}/A_{k} to focus on nonGaussianity, see Planck Collaboration XXIII (2014) and references therein.
Acknowledgments
The development of Planck has been supported by: ESA; CNES and CNRS/INSUIN2P3INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We also wish to acknowledge the use of the COSMOS supercomputer, part of the DiRAC HPC Facility funded by STFC and the UK Large Facilities Capital Fund, use of the Andromeda cluster of the University of Geneva, and resources of the National Energy Research Scientific Computing Center.
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All Tables
95% upper limits on the constrained parameter f_{10} and the derived parameter Gμ/c^{2} for the five defect models discussed in the text.
Constraints on the fitted cosmological parameters in the case of Planck alone for the cosmic strings models (NAMBU, AHmimic and AH), semilocal strings (SL) and texture (TX).
Modal bispectrum analysis of foregroundseparated SMICA, NILC and SEVEM maps showing f_{NL} from strings, ISWlensing and diffuse point sources.
All Figures
Fig. 1
The spacetime around a cosmic string is conical, as if a narrow wedge were removed from a flat sheet and the edges identified. For this reason cosmic strings can create double images of distant objects. Strings moving across the line of sight will cause linelike discontinuities in the CMB radiation. 

Open with DEXTER  
In the text 
Fig. 2
Characteristic CMB temperature discontinuity created by a cosmic string. Here, the simulated NambuGoto string has produced a cusp, a small region on the string that approaches the speed of light, which has generated a localised CMB signal. 

Open with DEXTER  
In the text 
Fig. 3
Cosmic string power spectra used in this analysis: NAMBU (black dashed), AHmimic (blue dotted) and AH (red solid). The spectra have been set to equal power at ℓ = 10. When normalised to 850 μK at ℓ = 10 they correspond to string tensions of Gμ/c^{2} = 1.17 × 10^{6}, 1.89 × 10^{6} and 2.04 × 10^{6} respectively. Note that the limits discussed in this paper mean that the CMB spectra presented here are less than 3% of the overall power spectrum amplitude and hence the differences observed at high ℓ do not have a large effect. 

Open with DEXTER  
In the text 
Fig. 4
Comparison between global texture (black dashed) and semilocal (blue dotted) string power spectra and the AH field theory strings (red solid), normalised to unity at ℓ = 10. As expected, the SL spectrum lies in between the TX and the AH spectra. The AH spectrum was recomputed for the Planck cosmological model with sources from Bevis et al. (2010), and the SL and TX spectra were taken from Urrestilla et al. (2008). 

Open with DEXTER  
In the text 
Fig. 5
Integrated SachsWolfe angular power spectra extracted from the full sky cosmic string maps at different resolutions (labelled by N_{side}), with or without applying the antialiasing procedure (see text). The antialiasing filtering gives back the correct power up to ℓ_{max} ≲ 2N_{side}. 

Open with DEXTER  
In the text 
Fig. 6
All sky Mollweide projection of the simulated cosmic strings CMB sky after convolution by a Gaussian beam of 5′ resolution. The colour scale indicates the range of (ΔT/T)/(Gμ/c^{2}) fluctuations. 

Open with DEXTER  
In the text 
Fig. 7
A 20° gnomic projection patch extracted from the full sky map and zooming into string induced temperature steps (see Fig. 6). Applying the spherical gradient magnitude operator enhances the temperature steps, and thus the string locations, even more (right). 

Open with DEXTER  
In the text 
Fig. 8
Marginalised constraints on f_{10} for topological defects from Planck data plus polarisation from WMAP (Planck+WP). The left panel show constraints on cosmic strings, with NAMBU in black dashed, AHmimic in blue dotted and AH in red solid. The right panel show the constraints on SL (blue dotted) and TX (black dashed) compared to AH (again solid red). 

Open with DEXTER  
In the text 
Fig. 9
Marginalised constraints on f_{10} for topological defects with highℓ CMB data from SPT and ACT added to the Planck + WP constraints data (compare with constraints shown in Fig. 8). The left panel show constraints on cosmic strings, with NAMBU in black dashed, AHmimic in blue dotted and AH in red solid. The right panel show the constraints on SL (blue dotted) and TX (black dashed) compared to AH (solid red). 

Open with DEXTER  
In the text 
Fig. 10
Marginalised likelihoods in the f_{10}Ω_{b}h^{2} plane for the NAMBU model in blue and the AH mimic model in red using Planck +WP. This is the strongest correlation with any of the standard cosmological parameters. 

Open with DEXTER  
In the text 
Fig. 11
Coefficients Eq. (15) for the hybrid Fourier mode expansion of the cosmic string bispectrum Eq. (15). The average value (black line) is in remarkable agreement with all four string simulations as can be seen for n < 30 (lower panel), with each exhibiting better than a 97% correlation overall. 

Open with DEXTER  
In the text 
Fig. 12
Modal reconstruction of the postrecombination string bispectrum Eq. (15) extracted from Planck resolution map simulations. This is a 3D view of the allowed tetrahedral set of multipoles (ℓ_{1},ℓ_{2},ℓ_{3}) showing isosurfaces of the bispectrum density with darker blue for more negative values (it is normalised relative to the constant SW bispectrum). 

Open with DEXTER  
In the text 
Fig. 13
Deviation of the kurtosis of the signedintensity as a function of Gμ/c^{2}, normalised to the standard deviation of CMB and noise simulations: ΔK/σ = (K(R,Gμ/c^{2}) − K(R,Gμ/c^{2} = 0)) /σ. The left panel shows results for the 1GD wavelet and the right shows the 2GD wavelet. Each curve corresponds to a wavelet scale, R (arcmin), included in the analysis. The final sensitivity of the method is determined by combining the two wavelets and all the scales. 

Open with DEXTER  
In the text 
Fig. 14
The two Wiener filters, W_{M} and W_{D1}, used to constrain Gμ/c^{2} with Minkowski functionals. 

Open with DEXTER  
In the text 
Fig. 15
Posterior distribution of the parameter Gμ/c^{2} obtained with Minkowski functionals. This estimate takes into account the lensing of the data, but not the effects of foreground residuals. 

Open with DEXTER  
In the text 
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