Issue 
A&A
Volume 586, February 2016



Article Number  A140  
Number of page(s)  14  
Section  Cosmology (including clusters of galaxies)  
DOI  https://doi.org/10.1051/00046361/201526328  
Published online  09 February 2016 
Planck intermediate results
XXXVII. Evidence of unbound gas from the kinetic SunyaevZeldovich effect
^{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, PO Box 13000, 00076 Aalto, Finland
^{3} African Institute for Mathematical Sciences, 6–8 Melrose Road, Muizenberg, Cape Town, South Africa
^{4} Agenzia Spaziale Italiana Science Data Center, via del Politecnico snc, 00133 Roma, Italy
^{5} AixMarseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
^{6} Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, UK
^{7} Astrophysics & Cosmology Research Unit, School of Mathematics, Statistics & Computer Science, University of KwaZuluNatal, Westville Campus, Private Bag X54001, 4000 Durban, South Africa
^{8} Atacama Large Millimeter/submillimeter Array, ALMA Santiago Central Offices, Alonso de Cordova 3107, Vitacura, Casilla 763 0355, Santiago, Chile
^{9} CITA, University of Toronto, 60 St. George St., Toronto, ON M5S 3H8, Canada
^{10} CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
^{11} California Institute of Technology, Pasadena, California, USA
^{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, CA 94720, USA
^{14} DSM/Irfu/SPP, CEASaclay, 91191 GifsurYvette Cedex, France
^{15} DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark
^{16} Département de Physique Théorique, Université de Genève, 24 quai E. Ansermet, 1211 Genève 4, Switzerland
^{17} Departamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain
^{18} Departamento de Física, Universidad de Oviedo, Avda. Calvo Sotelo s/n, 33003 Oviedo, Spain
^{19} Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
^{20} Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada
^{21} Department of Physics and Astronomy, Dana and David Dornsife College of Letter, Arts and Sciences, University of Southern California, Los Angeles, CA 90089, USA
^{22} Department of Physics and Astronomy, University College London, London WC1E 6BT, UK
^{23} Department of Physics, Florida State University, Keen Physics Building, 77 Chieftan Way, Tallahassee, Florida, USA
^{24} Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, 00100 Helsinki, Finland
^{25} Department of Physics, Princeton University, Princeton, NJ 08544, USA
^{26} Department of Physics, University of California, Santa Barbara, CA 93106, USA
^{27} Department of Physics, University of Illinois at UrbanaChampaign, 1110 West Green Street, Urbana, Illinois, USA
^{28} Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131 Padova, Italy
^{29} Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, via Saragat 1, 44122 Ferrara, Italy
^{30} Dipartimento di Fisica, Università La Sapienza, P.le A. Moro 2, Roma, Italy
^{31} Dipartimento di Fisica, Università degli Studi di Milano, via Celoria, 16 Milano, Italy
^{32} Dipartimento di Fisica, Università degli Studi di Trieste, via A. Valerio 2, Trieste, Italy
^{33} Dipartimento di Matematica, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1 Roma, Italy
^{34} Discovery Center, Niels Bohr Institute, 17 Blegdamsvej, Copenhagen, Denmark
^{35} European Southern Observatory, ESO Vitacura, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile
^{36} European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, 28692 Villanueva de la Cañada, Madrid, Spain
^{37} European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
^{38} Facoltà di Ingegneria, Università degli Studi eCampus, via Isimbardi 10, 22060 Novedrate (CO), Italy
^{39} Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
^{40} Gran Sasso Science Institute, INFN, viale F. Crispi 7, 67100 L’ Aquila, Italy
^{41} HGSFP and University of Heidelberg, Theoretical Physics Department, Philosophenweg 16, 69120 Heidelberg, Germany
^{42} Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, 00100 Helsinki, Finland
^{43} INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, Italy
^{44} INAF–Osservatorio Astronomico di Roma, via di Frascati 33, Monte Porzio Catone, Italy
^{45} INAF–Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, Trieste, Italy
^{46} INAF/IASF Bologna, via Gobetti 101, Bologna, Italy
^{47} INAF/IASF Milano, via E. Bassini 15, Milano, Italy
^{48} INFN, Sezione di Bologna, via Irnerio 46, 40126 Bologna, Italy
^{49} INFN, Sezione di Roma 1, Università di Roma Sapienza, P.le Aldo Moro 2, 00185 Roma, Italy
^{50} INFN, Sezione di Roma 2, Università di Roma Tor Vergata, via della Ricerca Scientifica, 1, Roma, Italy
^{51} INFN/National Institute for Nuclear Physics, via Valerio 2, 34127 Trieste, Italy
^{52} IPAG: Institut de Planétologie et d’Astrophysique de Grenoble, Université Grenoble Alpes, IPAG, 38000 Grenoble, France
^{53} CNRS, IPAG, 38000 Grenoble, France
^{54} Imperial College London, Astrophysics group, Blackett Laboratory, Prince Consort Road, London, SW7 2AZ, UK
^{55} Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
^{56} Institut d’Astrophysique Spatiale, CNRS (UMR 8617), Université ParisSud 11, Bâtiment 121, Orsay, France
^{57} Institut d’Astrophysique de Paris, CNRS (UMR 7095), 98bis boulevard Arago, 75014 Paris, France
^{58} Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
^{59} Institute of Theoretical Astrophysics, University ofOslo, Blindern, Oslo, Norway
^{60} Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE), Apartado Postal 51 y 216, 72000 Puebla, México
^{61} Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, La Laguna, Tenerife, Spain
^{62} Instituto de Física de Cantabria (CSICUniversidad de Cantabria), Avda. de los Castros s/n, Santander, Spain
^{63} Istituto Nazionale di Fisica Nucleare, Sezione di Padova, via Marzolo 8, 35131 Padova, Italy
^{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 Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
^{67} Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
^{68} Kazan Federal University, 18 Kremlyovskaya St., 420008 Kazan, Russia
^{69} LAL, Université ParisSud, CNRS/IN2P3, Orsay, France
^{70} LERMA, CNRS, Observatoire de Paris, 61 avenue de l’Observatoire, Paris, France
^{71} Laboratoire AIM, IRFU/Service d’Astrophysique – CEA/DSM – CNRS – Université Paris Diderot, Bât. 709, CEASaclay, 91191 GifsurYvette Cedex, France
^{72} Laboratoire Traitement et Communication de l’Information, CNRS (UMR 5141) and Télécom ParisTech, 46 rue Barrault, 75634 Paris Cedex 13, France
^{73} Laboratoire de Physique Subatomique et Cosmologie, Université GrenobleAlpes, CNRS/IN2P3, 53 rue des Martyrs, 38026 Grenoble Cedex, France
^{74} Laboratoire de Physique Théorique, Université ParisSud 11 & CNRS, Bâtiment 210, 91405 Orsay, France
^{75} Lebedev Physical Institute of the Russian Academy of Sciences, Astro Space Centre, 84/32 Profsoyuznaya st., Moscow, GSP7, 117997, Russia
^{76} LeibnizInstitut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
^{77} MaxPlanckInstitut für Astrophysik, KarlSchwarzschildStr. 1, 85741 Garching, Germany
^{78} National University of Ireland, Department of Experimental Physics, Maynooth, Co. Kildare, Ireland
^{79} Nicolaus Copernicus Astronomical Center, Bartycka 18, 00716 Warsaw, Poland
^{80} Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark
^{81} Optical Science Laboratory, University College London, Gower Street, WC1E 6 BT London, UK
^{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} Sorbonne UniversitéUPMC, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
^{85} Space Research Institute (IKI), Russian Academy of Sciences, Profsoyuznaya Str, 84/32, 117997 Moscow, Russia
^{86} Space Sciences Laboratory, University of California, Berkeley, California, USA
^{87} Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Zelenchukskiy region, 369167 KarachaiCherkessian Republic, Russia
^{88} SubDepartment of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
^{89} UPMC Univ Paris 06, UMR 7095, 98bis boulevard Arago, 75014 Paris, France
^{90} Université de Toulouse, UPSOMP, IRAP, 31028 Toulouse Cedex 4, France
^{91} Universities Space Research Association, Stratospheric Observatory for Infrared Astronomy, MS 23211, Moffett Field, CA 94035, USA
^{92} University Observatory, Ludwig Maximilian University of Munich, Scheinerstrasse 1, 81679 Munich, Germany
^{93} University of Granada, Departamento de Física Teórica y del Cosmos, Facultad de Ciencias, 18071 Granada, Spain
^{94} University of Granada, Instituto Carlos I de Física Teórica y Computacional, 18071 Granada, Spain
^{95} Warsaw University Observatory, Aleje Ujazdowskie 4, 00478 Warszawa, Poland
Received: 16 April 2015
Accepted: 7 October 2015
By looking at the kinetic SunyaevZeldovich effect (kSZ) in Planck nominal mission data, we present a significant detection of baryons participating in largescale bulk flows around central galaxies (CGs) at redshift z ≈ 0.1. We estimate the pairwise momentum of the kSZ temperature fluctuations at the positions of the Central Galaxy Catalogue (CGC) samples extracted from Sloan Digital Sky Survey (SDSSDR7) data. For the foregroundcleaned SEVEM, SMICA, NILC, and COMMANDER maps, we find 1.8–2.5σ detections of the kSZ signal, which are consistent with the kSZ evidence found in individualPlanck raw frequency maps, although lower than found in the WMAP9yr Wband (3.3σ). We further reconstruct the peculiar velocity field from the CG density field, and compute for the first time the crosscorrelation function between kSZ temperature fluctuations and estimates of CG radial peculiar velocities. This correlation function yields a 3.0–3.7σ detection of the peculiar motion of extended gas on Mpc scales in flows correlated up to distances of 80–100 h^{1} Mpc. Both the pairwise momentum estimates and the kSZ temperaturevelocity field correlation find evidence for kSZ signatures out to apertures of 8 arcmin and beyond, corresponding to a physical radius of >1 Mpc, more than twice the mean virial radius of halos. This is consistent with the predictions from hydrodynamical simulations that most of the baryons are outside the virialized halos. We fit a simple model, in which the temperaturevelocity crosscorrelation is proportional to the signal seen in a semianalytic model built upon Nbody simulations, and interpret the proportionality constant as an effective optical depth to Thomson scattering. We find τ_{T} = (1.4 ± 0.5) × 10^{4}; the simplest interpretation of this measurement is that much of the gas is in a diffuse phase, which contributes little signal to Xray or thermal SunyaevZeldovich observations.
Key words: cosmic background radiation / cosmology: observations / largescale structure of Universe / galaxies: clusters: intracluster medium
© ESO, 2016
1. Introduction
The kinetic SunyaevZeldovich effect (hereafter kSZ, Sunyaev & Zeldovich 1972, 1980) describes the Doppler boost experienced by a small fraction of the photon bath of the cosmic microwave background (CMB) radiation when scattering off a cloud of moving electrons. In the limit of Thomson scattering, where there is no energy exchange between the electrons and the CMB photons, the kSZ effect is equally efficient for all frequencies and gives rise to relative brightness temperature fluctuations in the CMB that are frequency independent. The exact expression for this effect was first written as Eq. (15) of Sunyaev & Zeldovich (1970), and reads (1)In this expression, the integral is performed along the line of sight, n_{e} denotes the electron number density, σ_{T} is the Thomson crosssection, and represents the line of sight component of the electron peculiar velocity in units of the speed of light c. The equation above shows that the kSZ effect is sensitive to the peculiar momentum of the free electrons, since it is proportional to both their density and peculiar velocity. A few previous studies (HernándezMonteagudo et al. 2006b; Bhattacharya & Kosowsky 2008; Ma & Zhao 2014; Keisler & Schmidt 2013; Li et al. 2014) have proposed that it be used to trace the growth of velocities throughout cosmic history and its connection to dark energy and modified gravity. Zhang & Stebbins (2011) and Planck Collaboration Int. XIII (2014) have also used the kSZ effect to test the Copernican Principle and the homogeneity of the Universe. In addition, the impact of the kSZ effect on subcluster scales has also been investigated (Inogamov & Sunyaev 2003; Dolag & Sunyaev 2013).
With these motivations, there have been previous attempts to detect the kSZ effect in existing CMB data (Kashlinsky et al. 2008, 2010; Lavaux et al. 2013; Hand et al. 2012). The results of Kashlinsky et al. (2008, 2010), which point to the existence of a bulk flow of large amplitude (800–1000 km s^{1}) extending to scales of at least 800 Mpc, have been disputed by a considerable number of authors (e.g., Keisler 2009; Osborne et al. 2011; Mody & Hajian 2012; Planck Collaboration Int. XIII 2014; Feindt et al. 2013). On the other hand, Lavaux et al. (2013) have claimed the detection of the local bulk flow (within 80 h^{1} Mpc) by using the kSZ in WMAP data in the direction of nearby galaxies. While these results remain at a low (roughly 1.7σ) significance level, they are also in slight tension with the results that we present here. On the other hand, the work of Hand et al. (2012) constitutes the first clear detection of the kSZ effect (using the “pairwise” momentum approach that we describe below), and no other group has confirmed their results to date. In addition, Sayers et al. (2013) have provided a first claimed detection of the kSZ effect in a single source. After the first data release of the Planck mission, some disagreement has been claimed between the cosmological frame set by Planck and measurements of peculiar velocities as inferred from redshift space distortions (Macaulay et al. 2013). More recently, Mueller et al. (2015) forecasted the detectability of the neutrino mass with the kSZ pairwise momentum estimator by using Atacama Cosmology Telescope (ACTPol) and Baryon Oscillation Spectroscopic Survey (BOSS) data.
This work represents the second contribution of the Planck^{1} collaboration to the study of the kSZ effect, in which we focus on constraining the “missing baryons” with this signal (DeDeo et al. 2005; HernándezMonteagudo & Sunyaev 2008; Ho et al. 2009; HernándezMonteagudo & Ho 2009; Shao et al. 2011). Numerical simulations (Cen & Ostriker 2006) have shown that most of the baryons lie outside galactic halos, and in a diffuse phase, with temperature in range of 10^{5}–10^{7} K. This “warmhot” intergalactic medium is hard to detect in Xray observations due to the relatively low temperature. Thus, most of the baryons are “missing” in the sense that they are neither hot enough (T< 10^{8} K) to be seen in Xray observations, nor cold enough (T> 10^{3} K) to be made into stars and galaxies. However, as we can see in Eq. (1), the kSZ signal is proportional to the gas density and peculiar velocity, and thus the gas temperature is irrelevant. Therefore the kSZ effect has been proposed as a “leptometer”, since it is sensitive to the ionized gas in the Universe while most of the baryons remain undetected.
In this work, we measure the kSZ effect through two distinct statistics: the kSZ pairwise momentum, which was used in Hand et al. (2012) to detect kSZ effect for the first time; and the crosscorrelation between the kSZ temperature fluctuations with the reconstructed radial peculiar velocities inferred from a galaxy catalogue. These analyses allow us to probe the amount of gas generating the kSZ signal and provide direct evidence of the elusive missing baryons in the local Universe. In Sect. 2 we describe the CMB data and the Central Galaxy Catalogue that will be used in our analysis. In Sect. 3 we describe two statistical tools we use. Section 4 presents and explains our results and illustrates the physical meaning of the significance. The conclusions and discussion is presented in the last section. Throughout this work we adopt the cosmological parameters consistent with Planck Collaboration XIII (2015): Ω_{m} = 0.309; Ω_{Λ} = 0.691; n_{s} = 0.9608; σ_{8} = 0.809; and h = 0.68, where the Hubble constant is H_{0} = 100 h km s^{1} Mpc^{1}.
2. Data description
2.1. Planck data
This work uses Planck data that are available publicly, both raw frequency maps and the CMB foreground cleaned maps^{2}. The kSZ effect should give rise to frequencyindependent temperature fluctuations and hence constitutes a secondary effect with identical spectral behaviour as for the intrinsic CMB anisotropies. Therefore the kSZ effect should be present in all CMB frequency channels and in all CMB foregroundcleaned maps. However, one must take into account the different effective angular resolutions of each band, particularly when searching for a typically smallscale signal such as the kSZ effect. The raw frequency maps used here are the LFI 70 GHz map, and the HFI 100, 143, and 217 GHz maps. These have effective FWHM values of 13.01, 9.88, 7.18, and 4.87 arcmin for the 70, 100, 143, and 217 GHz maps, respectively.
The FWHM of the foreground cleaned products is 5 arcmin for the maps used in this work, namely the SEVEM, SMICA, NILC, and COMMANDER maps. These maps are the output of four different componentseparation algorithms. While the NILC map is the result of an internal linear combination technique, SMICA uses a spectral matching approach, SEVEM a templatefitting method and COMMANDER a parametric, pixel based Monte Carlo Markov Chain technique to project out foregrounds. We refer to the Planck component separation papers for details in the production of these maps (Planck Collaboration IX 2015; Planck Collaboration X 2015). In passing, we note that the foreground subtraction in those maps is not perfect, and that there exist traces of residuals, particularly on the smallest angular scales, related to radio, dust, and thermal SunyaevZel’dovich [tSZ] emission.
For comparison purposes, we examine 9year data from the Wilkinson Microwave Anisotropy Probe (WMAP)^{3}. In particular, we downloaded from the LAMBDA site^{4} the WMAP satellite 9year Wband (94 GHz) map, with an effective FWHM of 12.4 arcmin.
2.2. Central Galaxy Catalogue
We define a galaxy sample in an attempt to trace the centres of dark matter halos. Using as a starting point the seventh data release of the Sloan Digital Sky Survey (SDSS/DR7 Abazajian et al. 2009), the Central Galaxy Catalogue (CGC) is composed of 262 673 spectroscopic sources brighter than r = 17.7 (the rband extinctioncorrected Petrosian magnitude). These sources were extracted from the SDSS/DR7 New York University Value Added Galaxy Catalogue (Blanton et al. 2005)^{5}, and we have applied the following isolation criterion: no brighter (in rband) galaxies are found within 1.0 Mpc in the transverse direction and with a redshift difference smaller than 1000 km s^{1}. The Sloan photometric sample has been used to remove all possible nonspectroscopic sources that may violate the isolation requirements. By using the “photometric redshift 2” catalogue (photoz2, Cunha et al. 2009), all spectroscopic sources in our isolated sample with potential photometric companions within 1.0 Mpc in projected distance, and with more than 10% probability of having a smaller redshift than that of the spectroscopic object, are dropped from the Central Galaxy Catalogue.
Information provided in the NYUVAGC yields estimates of the stellar mass content in this sample, and this enables us to make a direct comparison to the output of numerical simulations (Planck Collaboration Int. XI 2013). We refer to this paper for further details on the scaling between total halo mass and stellar mass for this galaxy sample.
We expect most of our CGs to be the central galaxies of their dark matter halos (again see Planck Collaboration Int. XI 2013), just as bright field galaxies lie at the centres of their satellite systems and cD galaxies lie near the centres of their clusters. They are normally the brightest galaxies in their system. By applying the same isolation criteria to a mock galaxy catalogue based on the Munich semianalytic galaxy formation model (see Sect. 2.3 for more details), we found that at stellar masses above 10^{11} M_{⊙}, more than 83% of CGs in the mock galaxy catalogue are truly central galaxies. For those CGs that are satellites, we have checked that at log (M_{∗}/M_{⊙}) > 11 about twothirds are brighter than the true central galaxies of their halos, while the remainder are fainter, but are considered isolated because they are more than 1 Mpc (transverse direction) from their central galaxies (60%) or have redshifts differing by more than 1000 km s^{1} (40%).
A case with stricter isolation criteria has been tested, in which we require no brighter galaxies to be found within 2.0 Mpc in the transverse direction and with a redshift difference smaller than 2000 km s^{1}. Applying these stricter criteria to the same parent SDSS spectroscopic catalogue, we end up with a total of 110 437 CGs, out of which which 58 105 galaxies are more massive than 10^{11} M_{⊙}. Thus about 30% of the galaxies with log (M_{∗}/M_{⊙}) > 11 have been eliminated from the sample. This new sample of CGs has a slightly higher fraction of centrals, reaching about 87% at log (M_{∗}/M_{⊙}) > 11. The improvement is small because (as we have checked) most of the satellite galaxies in the 1 Mpc sample are brighter than the central galaxies of their own halos, and with the stricter criteria they are still included. Considering a balance between the sample size, which directly affects the signaltonoise ratio in our measurements, and the purity of central galaxies, we choose the 1 Mpc isolation criteria and the corresponding CGC sample in our analysis from here on. This sample amounts to 262 673 sources over the DR7 footprint (about 6300 deg^{2}, f_{sky} = 0.15).
2.3. Numerical simulations
In order to compare measurements derived from observations to theoretical predictions, we make use of two different numerical simulations of the largescalestructure. We first look at the combination of two hydrodynamical simulations, combining a constrained realization of the local Universe and a large cosmological simulation covering 1200 h^{1} Mpc. The simulations were performed with the GADGET3 code (Springel et al. 2001; Springel 2005), which makes use of the entropyconserving formulation of smoothedparticle hydrodynamics (SPH; Springel & Hernquist 2002). These simulations include radiative cooling, heating by a uniform redshiftdependent UV background (Haardt & Madau 1996), and a treatment of star formation and feedback processes. The latter is based on a subresolution model for the multiphase structure of the interstellar medium (Springel & Hernquist 2003) with parameters that have been fixed to obtain a wind velocity of around 350 km s^{1}. We used the code SMAC (Dolag et al. 2005) to produce full sky maps from the simulations. For the innermost shell (up to 90 h^{1} Mpc from the observer) we use the simulation of the local Universe, whereas the rest of the shells are taken from the large, cosmological box. We construct full sky maps of the thermal and kinetic SZ signals, as well as halo catalogues, by stacking these consecutive shells through the cosmological boxes taken at the evolution time corresponding to their distance. In this way, the simulations reach out to a redshift of 0.22 and contain 13 058 objects with masses above 10^{14}M_{⊙}. Provided that our CGC lies at a median redshift of 0.12, this combined simulation should be able to help us interpret the clustering properties of peculiar velocities of highly biased, massive halos, on the largest scales. For more details on the procedure for using the simulations see Dolag & Sunyaev (2013). This simulated catalogue will hereafter be referred to as the CLUSTER catalogue.
We have also used a mock galaxy catalogue, based on the semianalytic galaxy formation simulation of Guo et al. (2013), which is implemented on the very large dark matter Millennium simulation (Springel et al. 2005). The Millennium simulation follows the evolution of cosmic structure within a box of side 500 h^{1} Mpc (comoving), whose merger trees are complete for subhalos above a mass resolution of 1.7 × 10^{10}h^{1} M_{⊙}. Galaxies are assigned to dark matter halos following the model recipes described in Guo et al. (2011). The rescaling technique of Angulo & White (2010) has been adopted to convert the Millennium simulation, which is originally based on WMAP1 cosmology, to the WMAP7 cosmology. The galaxy formation parameters have been adjusted to fit several statistical observables, such as the luminosity, stellar mass, and correlation functions for galaxies at z = 0.
We project the simulation box along one axis, and assign every galaxy a redshift based on its line of sight (LOS) distance and peculiar velocity, i.e., parallel to the LOS axis. In this way we can select a sample of galaxies from the simulation using criteria exactly analogous to those used for our CGC based on SDSS. A galaxy is selected if it has no brighter companions within 1 Mpc in projected distance and 1000 km s^{1} along the LOS. This sample of simulated galaxies will be referred as the GALAXY catalogue.
3. Methodology
We will search for kSZ signatures in Planck temperature maps by implementing two different statistics on the CMB data. The first statistic aims to extract the kSZ pairwise momentum by following the approach of Hand et al. (2012), which was inspired by Groth et al. (1989) and Juszkiewicz et al. (1998). The second statistic correlates the kSZ temperature anisotropies estimated from Planck temperature maps with estimates of the radial peculiar velocities. These velocity estimates are obtained after inverting the continuity equation relating galaxy density with peculiar velocities, as suggested by DeDeo et al. (2005) and Ho et al. (2009). The particular inversion methods applied to our data are described in Kitaura et al. (2012a, hereafter K12). Throughout this work we use the HEALPix software (Górski et al. 1998)^{6} to deal with the CMB maps.
3.1. The pairwise kSZ momentum estimator
Ferreira et al. (1999) developed an estimator for pairwise momentum with weights depending only on lineofsight quantities. With this motivation we use a similar weighting scheme on our CMB maps. The pairwise momentum estimator combines information on the relative spatial distance of pairs of galaxies with their kSZ estimates in a statistic that is sensitive to the gravitational infall of those objects. Specifically we use (2)where the weights c_{i,j} are given by (3)Here r_{i} and r_{j} are the vectors pointing to the positions of the ith and jth galaxies on the celestial sphere, r_{i} and r_{j} are the comoving distances to those objects, and r_{i,j} = r_{i}−r_{j} is the distance vector for this galaxy pair. The hat symbol () denotes a unit vector in the direction of r, and θ is the angle separating and . We also note that means (r_{i}−r_{j}) /  r_{i}−r_{j} . The sum is over all galaxy pairs lying a distance r_{i,j} falling in the distance bin assigned to r. The quantity δT_{i} denotes a relative kSZ temperature estimate at the position of the ith galaxy: (4)In this equation, the symbol corresponds to the kSZ amplitude estimate obtained at the angular position of the ith galaxy with an aperture photometry (AP) filter, while denotes the average kSZ estimate obtained from all galaxies after weighting by a Gaussian of width σ_{z} centred on z_{i}: (5)In this AP approach one computes the average temperature within a given angular radius θ, and subtracts from it the average temperature in a surrounding ring of inner and outer radii [ θ,fθ ], with f> 1. In our case we use (see, e.g., Planck Collaboration Int. XIII 2014). If we knew accurately the spatial gas distribution on these scales there would clearly be room for more optimal approaches, like a matched filter technique (Li et al. 2014). But on these relatively small scales the density profile in halos seems to be significantly less regular than the pressure profile (see, e.g., Arnaud et al. 2010), and this adds to the fact that gas outside halos, not necessarily following any given profile, also contributes to the signal. Furthermore, we would like to conduct an analysis that is as model independent as possible, and thus blind to any specific model for the gas spatial distribution.
The correction by a redshiftaveraged quantity introduced in the last equation above was justified by Hand et al. (2012) through the need to correct for possible redshift evolution of the tSZ signal in the sources. In practice, this correction allows us to measure relative changes in temperature anisotropies between nearby galaxy pairs after minimizing other noise sources, such as CMB residuals.
Fig. 1 Absolute value of versus distance to the observer after obtaining AP kSZ temperature estimates on the real positions of CGs (black line) and on a rotated CG configuration (red line). The green line provides the theoretical expectation for the rms of , and the blue histogram displays the radial distribution of the CGs (see text for further details). 
We next conduct an analysis into the motivation behind this zdependent monopole correction. In Fig. 1 we display the amplitude of for σ_{z} = 0.01 versus the comoving distance to the observer r. The value of the aperture chosen in this exercise is 8 arcmin. The black line refers to the real position of the CGs, while the red line refers to a rotatedonthesky configuration of the CGs. Since we are plotting absolute values of , the solid (dashed) parts of these lines refer to positive (negative) values of . The amplitude of these curves is close to the solid green line, which corresponds to the theoretical prediction for the rms of under the assumption that the AP temperature estimates are dominated by CMB residuals. That is, the amplitude of the green curve equals , where σ [ δT ] ≃ 20 μK is the rms of the 8 arcmin AP kSZ estimates and N_{CG}(r) is the number of CGs effectively falling under the redshift Gaussian window given in Eq. (5). While σ [ δT ] ≃ 20 μK is computed from real data, its amplitude is very close to the theoretical predictions of Fig. 6 in HernándezMonteagudo et al. (2006b), for an angular aperture of 8 arcmin after considering the CMB exclusively. We can see that the amplitude of is lowest for those distances where the number density of CGs is highest (as displayed, in arbitrary units, by the blue histogram in Fig. 1).
Therefore Fig. 1 shows not only that AP kSZ estimates are dominated by CMB residuals, but also that the difference in for CG pair members lying 50–100 h^{1} Mpc away in radial distance typically amounts to few times 0.01 μK. We shall show below that this amplitude is not completely negligible when compared to the typical kSZ pairwise momentum amplitude between CGs at large distances, and thus subtracting becomes necessary. However, this should not be the case when crosscorrelating AP kSZ measurements with estimates of radial peculiar velocities (see Sect. 3.2 below), since in this case the residual will not be correlated with those velocities and should not contribute to this crosscorrelation.
Like Hand et al. (2012), our choice for σ_{z} is σ_{z} = 0.01, although results are very similar if we change this by a factor of 2. Adopting higher values introduces larger errors in the peculiar momentum estimates, and smaller values tend to suppress the power on the largest scales; we adopt σ_{z} = 0.01 as a compromise value. It is worth noting that any effect giving rise to a pair of δT_{i},δT_{j}, whose difference is not correlated to the relative distance of the galaxies r_{i}−r_{j}, should not contribute to Eq. (2).
3.2. Recovering peculiar velocities from the CGC galaxy survey
There is a long history of the use of the density field to generate estimates of peculiar velocities (e.g., Dekel et al. 1993; Nusser & Davis 1994; Fisher et al. 1995; Zaroubi et al. 1995, for some early studies). DeDeo et al. (2005) and Ho et al. (2009) first suggested inverting the galaxy density field into its peculiar velocity field in the context of kSZ studies. In this section, we use the approach of K12 to obtain estimates of the peculiar velocity field from a matter density tracer. The work of K12 is based upon the analysis of the Millennium simulation, where full access to all dark matter particles was possible. In our case the analysis will obviously be limited to the use of the CGC catalogue, and this unavoidably impacts the performance of the algorithms.
Inspired by K12, in our analysis we conduct three different approaches to obtain the velocity field. The first one is a simple inversion of the linear continuity equation of the density contrast obtained from the galaxies in the CGC: this will be hereafter called the LINEAR approach. It makes use of the continuity equation at linear order, (6)where v(x) is the peculiar velocity field and δ(x) is the matter density contrast. In our case, however, we observe the galaxy density contrast δ^{g}(x), and thus the amplitude of the estimated velocity field is modulated by the bias factor b relating δ^{g}(x) and δ(x), δ^{g}(x) = bδ(x). The bias factor b is assumed to be constant on the scales of interest.
The second approach performs the same inversion of the linear continuity equation, but on a linearized estimate of the density field. This linearized field is obtained after computing the natural logarithm of unity plus the density contrast of the galaxy number density field and subsequently removing its spatial average (Neyrinck et al. 2009), (7)In this expression, δ^{g}(x) denotes again the density contrast of the galaxy number density at position x. This approach will be referred to as LOGLINEAR. Finally, secondorder perturbation theory (see, e.g., Bouchet et al. 1995) was applied on this linearized field, yielding a third estimate of the peculiar velocity field (the LOG2LPT approach). We refer to K12 for details on the implementations of the three approaches. For the sake of simplicity, we discuss results for the LINEAR approach, and leave the corresponding discussion of the two other methods for an appendix. We have also tried using the full SDSS spectroscopic sample (rather than the CGC) on the same volume to recover the peculiar velocity field; the full galaxy sample should be a better proxy for the dark matter density field than the CGC. However, after testing this with an enlarged version of the GALAXY catalogue (by considering all halos above a mass threshold of 10^{10.8} M_{⊙}), we obtain negligible differences with respect to the mock CG. Likewise, we obtain practically the same results when using the real CGC and the full spectroscopic sample. Therefore, for the sake of simplicity, we restrict our analysis to the CGC. All these methods make use of FFTs requiring the use of a 3D spatial grid when computing galaxy number densities. We choose to use a grid of 128^{3} cells, each cell being 4 h^{1} Mpc on a side. This cell size is well below the scales where the typical velocity correlations are expected (above 40 h^{1} Mpc), and comparable with the positional shifts induced by the redshift space distortions (about 3 h^{1} Mpc for a radial velocity of 300 km s^{1}).
These distortions will be ignored hereafter, since they affect scales much smaller than those of interest in our study (roughly 20 h^{1} Mpc and above). We note that these distortions can be corrected in an iterative fashion (see the pioneering work of Yahil et al. 1991 within the linear approximation; Kitaura et al. 2012c for the lognormal model, or Kitaura et al. 2012b including nonlocal tidal fields). Nevertheless, our tests performing such kinds of correction on the mock catalogue yield a very minor improvement on the scales of interest.
Fig. 2 Reconstruction of the xcomponent of the peculiar velocity field (arrows) in a narrow slice of the grid containing the CGC over the corresponding density contrast contour 2D plot. 
After aligning the X and Zaxes of the 3D grid with the zero Galactic longitude and zero Galactic colatitude axes, respectively, we place our grid at a distance vector R_{box} = [ −300,−250,150 ] h^{1} Mpc from the observer. This position vector locates the corner of the 3D grid that constitutes the origin for labelling cells within the box. This choice of R_{box} is motivated by a compromise between having as many grid cells in the CGC footprint as possible, and keeping a relatively high galaxy number density. Placing the 3D grid at a larger distance would allow us to have all grid cells inside the CGC footprint, but at the expense of probing distances where the galaxy number density is low (due to the galaxy radial selection function being low as well). Our choice for R_{box} results in about 150 000 CGs being present in the box, and about 82% of the grid cells falling inside the CGC footprint.
The three approaches will provide estimates of the peculiar velocity field in each grid cell, v^{rec}(x). From these, it is straightforward to compute the radial component as seen by the observer, , and to assign it to all galaxies falling into that grid cell. In Fig. 2 arrows show the LINEAR reconstruction of the xcomponent of the peculiar velocity field from the CGC, for a single zslice of data. The coloured contour displays the galaxy density contrast distribution over the same spatial slice.
The methodology outlined in K12 was conducted in the absence of any sky mask or selection function. In our work we address these aspects of the real data by means of a Poissonian data augmentation approach. In a first step, all grid cells falling outside the CGC footprint are populated, via Poissonian realizations, with the average number of galaxies dictated by the CGC radial selection function computed from cells inside the footprint. In this way we fill all holes in the 3D grid. Following exactly the same procedure, we next radially augment the average number of counts in cells in such a way that the radial selection function of the resulting galaxy sample is constant. In this way we avoid radial gradients that could introduce spurious velocities along the line of sight.
In order to test this methodology, we use the GALAXY mock catalogue, in two different scenarios. The first scenario is an ideal one, with no mask or selection function: we apply the three approaches on a box populated with our mock catalogue, and compare the recovered radial velocities with the real ones provided by the catalogue. When performing this comparison, we evaluate a 3D grid for the original galaxy radial velocity by assigning to each cell the radial velocity of the galaxy falling nearest to the cell centre, that is, we adopt a nearest particle (NP) method. For different radial bins of the k wavevector, we evaluate the correlation coefficient (r_{k}) computed from the crosspower spectrum between the recovered and the original radial velocity fields and their respective autospectra: (8)In this expression, P^{X,Y}(k) stands for , that is, the radially averaged power spectrum of the line of sight velocity modes. The superscripts { X,Y } = { orig,rec } stand for “original” and “recovered” components, respectively, and the asterisk denotes the complex conjugate operation.
Fig. 3 Correlation coefficient of the recovered lineofsight velocities with the actual ones in our GALAXY mock catalogue. Solid, dotted, and dashed lines refer to the LINEAR, LOGLINEAR, and LOG2LPT approaches, respectively. The red lines consider the ideal scenario without any sky mask or selection function, while the black ones are for the same sky mask and selection function present in the real CGC. 
In Fig. 3 the red lines display the correlation coefficients for the ideal scenario. Solid, dotted, and dashed lines refer to the LINEAR, LOGLINEAR, and LOG2LPT approaches, respectively. On large scales (low k modes), the three approaches provide correlation coefficients that are very close to unity, while they seem to lose information on small scales in the same way. We note that a direct comparison to the results of K12 is not possible, since, in our case, we do not use the full dark matter particle catalogue, but only a central halo one.
After the real mask and selection function obtained from the CGC is applied to the GALAXY mock catalogue, then the recovery of the peculiar velocities from the three adopted approaches worsens considerably. The black lines in Fig. 3 display, in general, much lower correlation levels than the red ones. The LINEAR approach seems to be the one that retains most information on the largest scales, and it outperforms the LOGLINEAR and the LOG2LPT methods on all scales. We hence expect the LINEAR approach to be more sensitive to the kSZ effect than the other two methods, particularly on the largest scales.
Once the velocity inversion from the CGC density contrast has been performed, we compute the spatial correlation function between the recovered velocities and the kSZ temperature anisotropies, (9)where δT_{i} is estimated as in Eq. (4), and the ensemble average is obtained after running through all galaxy pairs { i,j } lying a distance r away.
3.3. Template fitting
When studying the measurements of the kSZ pairwise momentum and kSZ momentum correlation, we perform fits to estimates obtained from our numerical simulations. That is, we minimize the quantity (10)where the indexes i,j run over different radial bins, ŵ^{X}(r_{i}) is the measured quantity in the ith radial bin (with X either denoting kSZ pairwise momentum or the kSZ temperaturerecovered velocity correlation), and refers to its counterpart measured in the numerical simulation. The symbol C_{ij} denotes the ij component of the covariance matrix C that is computed from the Planck maps after estimating ŵ^{X} for null positions where no SZ effect is expected^{7}. This minimization procedure provides formal estimates for the amplitude A^{X} and its associated errors: Most of the information is located at short and intermediate distances, where the estimated statistic ŵ^{X}(r) differs most from zero, as can be seen in Figs. 4 and 5. We also test the null hypothesis, that is, we measure the χ^{2} statistic (defined in Eq. (10) above) for the particular case of A^{X} = 0 and estimate the significance level at which such a value (denoted by ) is compatible with this null hypothesis. In these cases, we quote the significance as the number of σ with which the null hypothesis is ruled out under Gaussian statistics. The array of distance bins on which the covariance matrix in Eq. (10) is computed is chosen evenly in the range 0–150 h^{1} Mpc. However, we consider only three separate points centred upon 16, 38, and 81 h^{1} Mpc when computing (conservative) statistical significances. In this way we minimize correlation among radial bins to ensure that the inversion of the covariance matrix is stable. We have checked that, for the adopted set of distance bins, random variations at the level of 10% of the measured ŵ^{X}(r) do not compromise the stability of the recovered significance estimates. In other words, we explicitly check that 10% fluctuations on the measured ŵ^{X}(r) introduces fluctuations at a similar level in the χ^{2} estimates (more dramatic changes in the χ^{2} estimates would point to singular or quasisingular inverse covariance matrices).
4. Results
Fig. 4 Computation of the kSZ pairwise momentum for the CGC sample. The top row, from left to right, displays the results for different aperture choices on the raw HFI 217 GHz map, namely 5, 8, 12, and 18 arcmin. The top row also shows the analysis for the foregroundcleaned SEVEM map, displayed with blue squares. The fit to the pairwise momentum templates from the CLUSTER catalogue is also displayed by the solid red line, and the GALAXY catalogue by the green line. The bottom row presents the results at a fixed aperture of 12 arcmin for different frequency maps, including WMAP9 Wband data (red squares). 
4.1. The kSZ pairwise momentum
As mentioned above, the CGC was used previously in Planck Collaboration Int. XI (2013) to trace the tSZ effect versus stellar mass down to halos of size about twice that of the Milky Way. In this case we use the full CGC to trace the presence of the kSZ signal in Planck data, since our attempts with the most massive subsamples of the CGC yield no kSZ signatures. While the tSZ effect is mostly generated in collapsed structures (HernándezMonteagudo et al. 2006a) because it traces gas pressure, the kSZ effect instead is sensitive to all baryons, regardless of whether they belong to a collapsed gas cloud or not. Thus it is expected that not only will the virialized gas in halos contribute to the kSZ signal, but also the baryons surrounding those halos and moving in the same bulk flow. Rather than using a particular gas density profile, we choose not to make any assumption about the spatial distribution of gas around CGs.
We thus adopt an AP filter of varying apertures around the positions of CGC galaxies. The minimum aperture we consider is close to the resolution of Planck (5 arcmin), and we search for signals using increasing apertures of radii 5, 8, 12, and 18 arcmin. This is equivalent to probing spheres of radius ranging from 0.5 up to 1.8 h^{1} Mpc (in physical units) around the catalogue objects. The result of the kSZ pairwise momentum estimation on the raw 217 GHz HFI map is displayed in the top row of Fig. 4 for the four apertures under consideration. The recovered momenta for the raw frequency maps (displayed by black circles) provide some evidence for kSZ signal for apertures smaller than 12 arcmin: below a distance of 60 h^{1} Mpc all points are systematically below zero, some beyond the 2σ level. Although the test does not yield significant values (at 0.4σ,0.3σ,0.7σ and − 1.2σ for 5, 8, 12, and 18 arcmin apertures, respectively), the fits to the GALAXY peculiar momentum template (displayed by the green solid line in the secondfromtheleft panel in the top row) yield S/N = A^{pkSZ}/σ^{pkSZ} = 1.7,1.4,1.9 and 0.1 for 5, 8, 12, and 18 arcmin apertures, respectively. We obtain similar levels for the peculiar momentum template obtained from the CLUSTER simulation (red line in secondfromtheleft panel in top row). When using the SEVEM clean map, these significances go beyond the 2σ level: S/N = A^{pkSZ}/σ^{pkSZ} = 2.5,1.8,2.2 and 0.0 for 5, 8, 12, and 18 arcmin apertures for the GALAXYderived template, respectively. If we repeat the analysis at 12 arcmin aperture for the SMICA NILC and COMMANDER maps, we obtain S/N = A^{pkSZ}/σ^{pkSZ} = 2.1,2.2, and 2.1, respectively.
Fig. 5 Filled circles: measured kSZ pairwise momentum for the kSZ map derived from the CLUSTER simulation after considering different radial apertures on a subset of clusters in the mass range (1−2) × 10^{14}h^{1} M_{⊙}. Black triangles: pairwise momentum computed from the GALAXY mock catalogue (filled triangles) after assigning these galaxies a tSZ amplitude following a mass scaling inspired by the tSZ measurements of the CGC given in Planck Collaboration Int. XI (2013). 
We note at this point that the behaviour of the kSZ evidence for the CGs as displayed in Fig. 4 is significantly different to what is found in Fig. 5 for the CLUSTER simulation with halos in the mass range (1–2) × 10^{14}h^{1} M_{⊙}. In this simulation, most of the kSZ signal is coming from the halos themselves, and thus increasing the aperture to values larger than the virial radius of the clusters results in a dilution of the kSZ pairwise momentum amplitude. For real data, we find that the amplitude of the signal does not show significant changes when increasing the aperture from 5 arcmin up to 12 arcmin. It is worth adding now that the black filled triangles in Fig. 5 represent the peculiar momentum measured on the GALAXY mock catalogue after assigning to these galaxies a tSZ temperature fluctuation following the tSZ versus mass scaling measured in the CGC (Planck Collaboration Int. XI 2013). This tSZ amplitude assumes an observing frequency of ν_{obs} = 100 GHz, and hence provides a conservative estimate of the tSZ contamination, which turns out to be at the level of − 3 × 10^{3} μK, i.e., about a factor of 30 below the measured amplitude on the real CG sample.
We next investigate the spectral stability of the signal for 12 arcmin apertures. This choice is motivated by the fact that the LFI 70 GHz and the HFI 100 and 143 GHz channels have lower angular resolution, comparable or bigger than 8 arcmin, and this may compromise the comparison with the 217 GHz channel. This analysis is shown in the bottom row of Fig. 4. The signal obtained for the raw 217 GHz channel is found to be remarkably similar to what we obtain at 143, 100 GHz in HFI: the fits to the kSZ pairwise momentum template from the GALAXY simulation gives S/N = A^{pkSZ}/σ^{pkSZ} = 2.2 and 2.1, respectively. The LFI 70 GHz channel, on the other hand, seems to show a much flatter pattern, and this could be due to a larger impact of instrumental noise: the tSZ should also be present at 100 and 143 GHz, and, as expected, gives rise to negligible changes. The effective full width half maximum (FWHM) for the 70 GHz channel is close to 13 arcmin, and this may also contribute to the difference with respect to the other HFI channels.
In the bottom row, second panel of Fig. 4, the red squares provide the measurement obtained from the cleaned Wband map of WMAP9. Surprisingly, the level of anticorrelation for distances below 30 h^{1} Mpc appears higher for WMAP data than for the Planck channels: the first three radial bins lie at the 2.3–3.3σ level, and a fit to the GALAXY template of the pairwise momentum yields S/N = A^{pkSZ}/σ^{pkSZ} = 3.3 as well. The angular resolution of the Wband in WMAP is close to that of the LFI 70 GHz channel, and the nonrelativistic tSZ changes by less than 13% between those channels. If any other frequencydependent contaminants (which should be absent in the WMAP Wband) are responsible for this offset, then they should also introduce more changes at the other frequencies. Thus the reason for the deeper anticorrelation pattern found in the Wband of WMAP9 remains unclear. Overall, we conclude that the Planck results for the pairwise peculiar momentum are compatible with a kSZ signal, at a level ranging between 2 and 2.5σ. The output from WMAP9 W band is also compatible with a kSZ signal, with a statistical significance of 3.3σ.
Fig. 6 Measured crosscorrelation function between the kSZ temperature estimates and the recovered radial peculiar velocities, , according to the LINEAR approach. The recovered velocities are divided with their rms dispersion σ_{v} = 310 km s^{1}, so kSZ temperature estimates are correlated to a quantity of variance unity. This plot corresponds to an aperture of 8 arcmin. Filled coloured circles correspond to estimates from different CMB maps (SEVEM, SMICA, NILC, COMMANDER, and the HFI 217 GHz map). The dotted lines display the null estimates obtained after computing kSZ temperature estimates for rotated positions on the SEVEM map, and the thick dashed line displays the average of the dotted lines. Error bars are computed from these null estimates of the correlation function. The solid line provides the best fit of the SEVEM data to the theoretical prediction for obtained from the GALAXY mock catalogue. These predictions are obtained using only a relatively small number of mock halos, and hence their uncertainty must be considered when comparing to the data. 
4.2. Crosscorrelation analysis with estimated peculiar velocities
After reconstructing the CGC density field into a peculiar velocity field in a 3D grid, as explained in Sect. 3.2, we compute the crosscorrelation function for the three inversion approaches using the Planck HFI 217 GHz band, and the SEVEM SMICA NILC and COMMANDER maps (see Fig. 6). Here we are using kSZ temperature estimates obtained with an 8 arcmin aperture. The three inversion approaches (namely, LINEAR, LOGLINEAR, and LOG2LPT) may suffer from different biases that impact the amplitude of the recovered velocities. Thus, in order to avoid issues with the normalization of the recovered velocities and to ease the comparison between different approaches, we normalize the recovered velocities s by their rms before computing the crosscorrelation function. In any case we must keep in mind the different responses of the three approaches on different kscales (see Fig. 3), thus giving rise to different correlation structures. For the sake of clarity, in this section we show results for the LINEAR method only, while in the Appendix we discuss the results for the other two reconstruction methods.
In Fig. 6, filled coloured circles display the results obtained after using the δT kSZ temperature estimates obtained at the real positions of the CGs on the CMB maps. The null tests were obtained by computing the crosscorrelation of the normalized recovered velocities () with temperature estimates (δT) obtained on 50 rotated^{8} positions on the CMB maps. In those cases, the δTs were computed for positions obtained after rotating the real CG angular positions in Galactic longitude. The results from each of these null rotations are displayed by dotted lines in Fig. 6, and their average is given by the thick, dashed line (which lies close to zero at all radii). Both the error bars and the covariance matrix of the correlation function were obtained from these null realizations.
Fig. 7 Same as in Fig. 6, but with the null correlation functions (displayed by dotted lines) being estimated after assigning the recovered linear velocity estimate of a given CG to any other CG in the sample (that is, by “shuffling”). Only the LINEAR approach is displayed in this plot. 
Results at zerolag rotation (i.e., the real sky) lie far from the distribution of the null rotations. There are several individual distance bins lying more than 3σ (up to 3.8σ on the 16 h^{1} Mpc distance bin for the raw 217 GHz frequency map), and the tests rule out the null hypothesis typically at the level of 2.1–2.6σ for the clean maps, and at 3.2σ for the raw 217 GHz frequency map. Likewise, when fitting the observed correlation function to the correlation function obtained from the GALAXY simulation, we obtain values of S/N = A^{wT,v}/σ^{wT,v} = 3.0–3.2 for the clean maps, while for the HFI 217 GHz raw map we find S/N = A^{wT,v}/σ^{wT,v} = 3.8. We explain this apparent mismatch below. A clear, largescale correlation pattern, extending up to about 80h^{1} Mpc, is found in the data. A complementary systematic test can be conducted by computing the crosscorrelation function of the kSZ temperature fluctuations (δT) with shuffled estimates of the recovered lineofsight peculiar velocities, i.e., to each CG we assign a estimate corresponding to a different, randomly selected CG. The result of performing this test for the LINEAR approach is displayed in Fig. 7, and shows that the correlation found between the δTs and the recovered velocities clearly vanishes for all shuffled configurations. By shuffling the recovered velocities we are destroying their coherent, largescale pattern, which couples with large angle CMB residuals, and generates most of the uncertainty in the measured crosscorrelation. This explains the smaller error bars in Fig. 7 when compared to Fig. 6.
Fig. 8 Dependence on the aperture radius of the correlation function obtained in the LINEAR approach for the SEVEM map. Error bars are estimated from the rms of the null correlation functions computed from rotated kSZ temperature estimates. 
Fig. 9 Evaluations of the χ^{2} statistic of the correlation function (with respect to the null hypothesis) for different angular apertures. Only results for the foregroundcleaned SEVEM map are shown. There is evidence for kSZ signal in a wide range of apertures above the FWHM, with a local maximum close to 8 arcmin. This roughly corresponds to a radius of 0.8 h^{1} Mpc from the CG positions at the median redshift of the sample. 
Fig. 10 Variation of the recovered correlation function for the four lowest frequency raw HFI maps after an effective convolution by a Gaussian beam of FWHM = 5 arcmin. Error bars here are computed in the same way as in Figs. 6 and 8. 
Fig. 11 Histogram of the angle subtended by R_{200} of the CGC members. 
We further study the dependence of the measured correlation function on the aperture radius and show the results in Fig. 8. We again restrict ourselves to the LINEAR approach and the SEVEM foregroundcleaned map, and error bars are computed from the null rotations (rather than from shuffling estimates of ). We display results for four apertures ranging from 5 to 18 arcmin: the lower end of this range is given by the angular resolution of the map, while for the higher end the kSZ signal is found to vanish. We find that, as for the kSZ peculiar momentum, the kSZ amplitude at 8 arcmin aperture is very close to the one found at 5 arcmin, and it is still significant at 12 arcmin aperture. We then vary the aperture from 5 to 26 arcmin and calculate the corresponding χ^{2} values, as shown in Fig. 9. These results are for the SEVEM foregroundcleaned map, and provide another view of the angular extent of the signal. For the kSZ peculiar momentum, we have shown in Fig. 4 that there is kSZ evidence for apertures as large as 12 arcmin, in good agreement with what we find now for the correlation function. While this statistic seems to have higher significance than the pairwise momentum, for both statistics we find consistently that most of its signal is again coming from gas not locked in the central regions of halos, but in the intergalactic medium surrounding the CG host halos.
We also test the consistency of our results with respect to frequency on raw Planck raw maps. For that we use the HFI channels ranging from 100 GHz up to 353 GHz and now we fix the aperture at 8 arcmin. Since the 100 and 143 GHz frequency maps have angular resolution comparable or worse than 8 arcmin, we choose to deconvolve all HFI maps under consideration by their respective (approximate) Gaussian beams, and convolve them again with a Gaussian beam of FWHM = 5 arcmin. While this approach may challenge the noise levels for the HFI maps with coarser beams, we find that this is balanced by the large number of CGs on which we compute the correlation function. The results of this analysis are given in Fig. 10, and show how the correlation functions from 100 GHz up to 217 GHz agree closely with each other, with no significance dependence on frequency (as is expected for the kSZ effect). However, the result for the 353 GHz channel is pointing to a significantly higher amplitude of the correlation function, even if the error bars associated with this map are typically 50–70% larger than for the 100 GHz map. At the map level, the main difference between the 353 GHz and lower frequency channels is the significantly larger amount of dust and/or CIB emission in the former map. We have checked that, throughout the rotated configurations, the HFI 353 GHz map has on average no correlation with the estimated radial velocities of the CGs. Therefore, the excess found in the measured amplitude of the correlation function must be due to fortuitous alignment between the estimated radial velocities of the CGs and the dust emission at the position of the CGs. This would also explain the higher amplitude of the correlation function found for the raw HFI 217 GHz map with respect to all other clean maps, as shown in Fig. 6: the raw HFI 217 GHz map should still contain some nonnegligible dust contamination when compared to the foregroundcleaned maps SEVEM, SMICA, NILC, and COMMANDER.
Another potential issue is related to the fact that, as shown in Planck Collaboration Int. XI (2013), about 12% of the CGC members with stellar masses above 10^{10} M_{⊙} are actually not central galaxies, but show some offset with respect to the centres of the host halos. This offset should cause a low bias in the kSZ amplitude estimation. We have simulated the impact of this offset by assuming that 12% of the CGs have uniform probability of lying within a (projected) distance range of 0 to 1 Mpc from the halo centre. After adopting a NFW profile for the gas distribution, we have found that the LOSprojected kSZ signal should be low biased a 10, 8, and 6% for θ_{AP} = 5,10 and 15 arcmin, respectively. Given the limited precision of our measurements, these biases are relatively small and will be ignored hereafter.
To compare our detection with simulations, the solid line in Fig. 6 shows the best fit to the prediction inferred from the GALAXY mock catalogue. This prediction is obtained by applying the LINEAR velocity recovery algorithm on our GALAXY catalogue after imposing the sky mask and the selection function present in the real CGC. Three pseudoindependent estimates of the correlation function of the recovered LOS velocity v_{rec} and the real LOS velocity v_{los} (⟨ v_{los}v_{rec} ⟩ (r) ≡ w^{vrec,v}(r)) are obtained after rotating the 3D grid hosting the mock GALAXY CGC, so that the side facing the observer is different in each case. The solid line corresponds to the average of these three estimates of w^{vrec,v}(r), and the ratio to the observed correlation function can be interpreted as an “effective” optical depth to Thomson scattering: . We obtain τ_{T} = (1.39 ± 0.46) × 10^{4} (i.e., at the 3σ level) for the SEVEM map, with very similar values for all other foregroundcleaned maps. We defer the physical interpretation of the kSZ measurements of this paper to an external publication, (HernándezMonteagudo et al. 2015).
5. Discussion and conclusion
The roughly 2.2σ detection (varying slightly for the different maps) of the pairwise momentum indicates that the baryonic gas is comoving with the underlying matter flows, even though it may lie outside the virial radius of the halos. The aperture of 8 arcmin on the CGs (placed at a median redshift of ) corresponds to a physical radius of around 1 Mpc. As we show next, this is considerably higher than the typical virial radius of the CG host halos. Following the same approach as in Planck Collaboration Int. XI (2013), we compute the R_{200} radius containing an average matter density equal to 200 times the critical density at the halo’s redshift. In Fig. 11 we display the histogram of the angle subtended by the R_{200} values of the 150 000 CGs placed in the 3D grid that we use for the velocity recovery. The red vertical solid line indicates the 8 arcmin aperture, well above the typical angular size of the CGC sources.
The behaviour displayed by the measured kSZ peculiar momentum in the top row panels of Fig. 4 differs significantly from the pattern found in Fig. 5. The fact that the measured kSZ pairwise momentum shows a roughly constant amplitude out to an aperture of 12 arcmin, well above the CG virial size, signals the presence of unbound gas that is contributing to the measurement. The opposite situation is seen in Fig. 5: in this scenario most of the signal comes from the halos rather than from a surrounding gas cloud. This plot displays the kSZ peculiar momentum from a subset of our CLUSTER catalogue, with sources in the range (1−2) × 10^{14} h^{1} M_{⊙}, after considering different aperture radii. As long as the halo remains unresolved (as is the case for these simulated clusters), then as we increase the aperture size the kSZ signal coming from the halo becomes more diluted and hence the amplitude decreases, contrary to what is found in Fig. 4.
We find a similar situation in the kSZ temperaturepeculiar velocity crosscorrelation. By crosscorrelating the reconstructed peculiar velocity field in a 3D box with the kSZ temperature anisotropies, we find a 3.0 σ detection between the two fields for the SEVEM map, at an aperture of 8 arcmin. This again, corresponds to gas clouds with radius roughly 1 Mpc, about twice the mean R_{200} radius (we find that ⟨ R_{200} ⟩ _{CGC} ≃ 0.4 Mpc). Since the peculiar velocity is directly related to the underlying matter distribution, our result suggests that gas inside and outside CG host halos are comoving with the matter flows.
One way of quantifying the amplitude of our signal is to ask by what factor we need to scale the modelbased w^{vrec,v}(r) in order to match our measured . Interpreting this scaling as an “effective” optical depth to Thomson scattering we find τ_{T} = (1.4 ± 0.5) × 10^{4}, which is a factor of 3 larger than that expected for the gas in typical CG host halos alone. This provides another piece of evidence that the kSZ signal found in Planck data is generated by gas beyond the virialized regions around the CGs, as opposed to the tSZ effect, which is mostly generated inside collapsed structures (HernándezMonteagudo et al. 2006a; Van Waerbeke et al. 2014; Ma et al. 2014).
Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA).
Planck’s Legacy Archive: http://pla.esac.esa.int/pla/aio/planckProducts.html
WMAP: http://map.gsfc.nasa.gov
LAMBDA: http://lambda.gsfc.nasa.gov
NYUVAGC: http://sdss.physics.nyu.edu/vagc/
Acknowledgments
The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSUIN2P3INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/. This research was supported by ERC Starting Grant (No. 307209), by the Marie Curie Career Integration Grant CIG 294183 and by the Spanish Ministerio de Economía y Competitividad project AYA201230789.
References
 Abazajian, K. N., AdelmanMcCarthy, J. K., Agüeros, M. A., et al. 2009, ApJS, 182, 543 [NASA ADS] [CrossRef] [Google Scholar]
 Angulo, R. E., & White, S. D. M. 2010, MNRAS, 405, 143 [NASA ADS] [Google Scholar]
 Arnaud, M., Pratt, G. W., Piffaretti, R., et al. 2010, A&A, 517, A92 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Bhattacharya, S., & Kosowsky, A. 2008, Phys. Rev. D, 77, 083004 [NASA ADS] [CrossRef] [Google Scholar]
 Blanton, M. R., Schlegel, D. J., Strauss, M. A., et al. 2005, AJ, 129, 2562 [NASA ADS] [CrossRef] [Google Scholar]
 Bouchet, F. R., Colombi, S., Hivon, E., & Juszkiewicz, R. 1995, A&A, 296, 575 [NASA ADS] [Google Scholar]
 Cen, R., & Ostriker, J. P. 2006, ApJ, 650, 560 [NASA ADS] [CrossRef] [Google Scholar]
 Cunha, C. E., Lima, M., Oyaizu, H., Frieman, J., & Lin, H. 2009, MNRAS, 396, 2379 [NASA ADS] [CrossRef] [Google Scholar]
 DeDeo, S., Spergel, D. N., & Trac, H. 2005, ArXiv eprints [arXiv:astroph/0511060] [Google Scholar]
 Dekel, A., Bertschinger, E., Yahil, A., et al. 1993, ApJ, 412, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Dolag, K., & Sunyaev, R. 2013, MNRAS, 432, 1600 [NASA ADS] [CrossRef] [Google Scholar]
 Dolag, K., Hansen, F. K., Roncarelli, M., & Moscardini, L. 2005, MNRAS, 363, 29 [NASA ADS] [CrossRef] [Google Scholar]
 Feindt, U., Kerschhaggl, M., Kowalski, M., et al. 2013, A&A, 560, A90 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ferreira, P. G., Juszkiewicz, R., Feldman, H. A., Davis, M., & Jaffe, A. H. 1999, ApJ, 515, L1 [NASA ADS] [CrossRef] [Google Scholar]
 Fisher, K. B., Lahav, O., Hoffman, Y., LyndenBell, D., & Zaroubi, S. 1995, MNRAS, 272, 885 [NASA ADS] [Google Scholar]
 Górski, K. M., Hivon, E., & Wandelt, B. D. 1998, Analysis Issues for Large CMB Data Sets, eds A. J. Banday, R. K. Sheth, & L. Da Costa, ESO, Printpartners Ipskamp, NL, 37 [arXiv:astroph/9812350]; Healpix HOMEPAGE: http://www.eso.org/science/healpix/ [Google Scholar]
 Groth, E. J., Juszkiewicz, R., & Ostriker, J. P. 1989, ApJ, 346, 558 [NASA ADS] [CrossRef] [Google Scholar]
 Guo, Q., White, S., BoylanKolchin, M., et al. 2011, MNRAS, 413, 101 [NASA ADS] [CrossRef] [Google Scholar]
 Guo, Q., White, S., Angulo, R. E., et al. 2013, MNRAS, 428, 1351 [Google Scholar]
 Haardt, F., & Madau, P. 1996, ApJ, 461, 20 [NASA ADS] [CrossRef] [Google Scholar]
 Hand, N., Addison, G. E., Aubourg, E., et al. 2012, Phys. Rev. Lett., 109, 041101 [NASA ADS] [CrossRef] [Google Scholar]
 HernándezMonteagudo, C., & Ho, S. 2009, MNRAS, 398, 790 [NASA ADS] [CrossRef] [Google Scholar]
 HernándezMonteagudo, C., & Sunyaev, R. A. 2008, A&A, 490, 25 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 HernándezMonteagudo, C., Trac, H., Verde, L., & Jimenez, R. 2006a, ApJ, 652, L1 [NASA ADS] [CrossRef] [Google Scholar]
 HernándezMonteagudo, C., Verde, L., Jimenez, R., & Spergel, D. N. 2006b, ApJ, 643, 598 [NASA ADS] [CrossRef] [Google Scholar]
 HernándezMonteagudo, C., Ma, Y.Z., Kitaura, F.S., et al. 2015, Phys. Rev. Lett., 115, 191301 [NASA ADS] [CrossRef] [Google Scholar]
 Ho, S., Dedeo, S., & Spergel, D. 2009, ArXiv eprints [arXiv:0903.2845] [Google Scholar]
 Inogamov, N. A., & Sunyaev, R. A. 2003, Astron. Lett., 29, 791 [NASA ADS] [CrossRef] [Google Scholar]
 Juszkiewicz, R., Fisher, K. B., & Szapudi, I. 1998, ApJ, 504, L1 [NASA ADS] [CrossRef] [Google Scholar]
 Kashlinsky, A., AtrioBarandela, F., Kocevski, D., & Ebeling, H. 2008, ApJ, 686, L49 [NASA ADS] [CrossRef] [Google Scholar]
 Kashlinsky, A., AtrioBarandela, F., Ebeling, H., Edge, A., & Kocevski, D. 2010, ApJ, 712, L81 [NASA ADS] [CrossRef] [Google Scholar]
 Keisler, R. 2009, ApJ, 707, L42 [NASA ADS] [CrossRef] [Google Scholar]
 Keisler, R., & Schmidt, F. 2013, ApJ, 765, L32 [NASA ADS] [CrossRef] [Google Scholar]
 Kitaura, F.S., Angulo, R. E., Hoffman, Y., & Gottlöber, S. 2012a, MNRAS, 425, 2422 [NASA ADS] [CrossRef] [Google Scholar]
 Kitaura, F.S., Erdoǧdu, P., Nuza, S. E., et al. 2012b, MNRAS, 427, L35 [NASA ADS] [Google Scholar]
 Kitaura, F.S., Gallerani, S., & Ferrara, A. 2012c, MNRAS, 420, 61 [NASA ADS] [CrossRef] [Google Scholar]
 Lavaux, G., Afshordi, N., & Hudson, M. J. 2013, MNRAS, 430, 1617 [NASA ADS] [CrossRef] [Google Scholar]
 Li, M., Angulo, R. E., White, S. D. M., & Jasche, J. 2014, MNRAS, 443, 2311 [NASA ADS] [CrossRef] [Google Scholar]
 Ma, Y.Z., & Zhao, G.B. 2014, Phys. Lett. B, 735, 402 [NASA ADS] [CrossRef] [Google Scholar]
 Ma, Y.Z., Van Waerbeke, L., Hinshaw, G., Hojjati, A., & Scott, D. 2014, JCAP, 9, 046 [Google Scholar]
 Macaulay, E., Wehus, I. K., & Eriksen, H. K. 2013, Phys. Rev. Lett., 111, 161301 [NASA ADS] [CrossRef] [Google Scholar]
 Mody, K., & Hajian, A. 2012, ApJ, 758, 4 [NASA ADS] [CrossRef] [Google Scholar]
 Mueller, E.M., de Bernardis, F., Bean, R., & Niemack, M. D. 2015, Phys. Rev. D, 92, 063501 [NASA ADS] [CrossRef] [Google Scholar]
 Neyrinck, M. C., Szapudi, I., & Szalay, A. S. 2009, ApJ, 698, L90 [NASA ADS] [CrossRef] [Google Scholar]
 Nusser, A., & Davis, M. 1994, ApJ, 421, L1 [NASA ADS] [CrossRef] [Google Scholar]
 Osborne, S. J., Mak, D. S. Y., Church, S. E., & Pierpaoli, E. 2011, ApJ, 737, 98 [NASA ADS] [CrossRef] [Google Scholar]
 Planck Collaboration IX. 2015, A&A, submitted [arXiv:1502.05956] [Google Scholar]
 Planck Collaboration X. 2015, A&A, submitted [arXiv:1502.01588] [Google Scholar]
 Planck Collaboration XIII. 2015, A&A, submitted [arXiv:1502.01589] [Google Scholar]
 Planck Collaboration Int. XI. 2013, A&A, 557, A52 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Planck Collaboration Int. XIII. 2014, A&A, 561, A97 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Sayers, J., Mroczkowski, T., Zemcov, M., et al. 2013, ApJ, 778, 52 [NASA ADS] [CrossRef] [Google Scholar]
 Shao, J., Zhang, P., Lin, W., Jing, Y., & Pan, J. 2011, MNRAS, 413, 628 [NASA ADS] [CrossRef] [Google Scholar]
 Springel, V. 2005, MNRAS, 364, 1105 [NASA ADS] [CrossRef] [Google Scholar]
 Springel, V., & Hernquist, L. 2002, MNRAS, 333, 649 [NASA ADS] [CrossRef] [Google Scholar]
 Springel, V., & Hernquist, L. 2003, MNRAS, 339, 289 [Google Scholar]
 Springel, V., Yoshida, N., & White, S. D. M. 2001, New Astron., 6, 79 [Google Scholar]
 Springel, V., White, S. D. M., Jenkins, A., et al. 2005, Nature, 435, 629 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Sunyaev, R. A., & Zeldovich, I. B. 1980, MNRAS, 190, 413 [NASA ADS] [CrossRef] [Google Scholar]
 Sunyaev, R. A., & Zeldovich, Y. B. 1970, Ap&SS, 7, 3 [NASA ADS] [Google Scholar]
 Sunyaev, R. A., & Zeldovich, Y. B. 1972, Comm. Astrophys. Space Phys., 4, 173 [Google Scholar]
 Van Waerbeke, L., Hinshaw, G., & Murray, N. 2014, Phys. Rev. D, 89, 023508 [NASA ADS] [CrossRef] [Google Scholar]
 Yahil, A., Strauss, M. A., Davis, M., & Huchra, J. P. 1991, ApJ, 372, 380 [NASA ADS] [CrossRef] [Google Scholar]
 Zaroubi, S., Hoffman, Y., Fisher, K. B., & Lahav, O. 1995, ApJ, 449, 446 [NASA ADS] [CrossRef] [Google Scholar]
 Zhang, P., & Stebbins, A. 2011, Phys. Rev. Lett., 107, 041301 [NASA ADS] [CrossRef] [Google Scholar]
Appendix A: The three velocity reconstruction methods
In this Appendix we briefly compare the velocity recovery by means of the three approaches explained in this work, namely the LINEAR, the LOGLINEAR, and the LOG2LPT approaches. First of all, as is shown in Fig. 3, the LINEAR method outperforms our implementation of the other two methods in the presence of a mask and selection function (even if all three provide virtually identical correlation coefficients in the absence of a mask and selection functions). This is shown clearly in Fig. A.1.
Fig. A.1 Measured crosscorrelation function between the kSZ temperature estimates and the recovered radial peculiar velocities, , according to the three adopted approaches, LINEAR (left panel), LOGLINEAR (middle panel), and LOG2LPT (right panel). The velocities are normalized with their rms dispersion σ_{v} = 230, 310, and 200 km s^{1}from left to right, respectively. We use an aperture of 8 arcmin when estimating kSZ temperature fluctuations. Filled coloured circles correspond to estimates from different CMB maps (SEVEM, SMICA, NILC, COMMANDER, and the HFI 217 GHz map). The dotted lines display the null estimates obtained after computing kSZ temperature estimates for rotated positions on the SEVEM map, and the thick dashed line displays the average of the dotted lines. Error bars are computed from these null estimates of the correlation function. The solid line provides the best fit to the data of the theoretical prediction for obtained from the GALAXY mock catalogue. These predictions are obtained using only a relatively small number of mock halos, and hence their uncertainty must be considered when comparing to data. 
We apply our algorithms to invert density into velocities after using the three different sides of the cubic grid where we place our GALAXY mock catalogue. For each box side we estimate a recovered velocity field and compute its correlation to the real, underlying velocity field of the mock galaxies, w^{vrec,v}(r). Three different estimations are too few to an average correlation function, but we still use this average function (out of these three boxside estimates) when conducting the fit to real data. Thus the solid lines in Fig. A.1 show the fits to the result of averaging the correlation functions w^{T,v} through the three box orientations. We must keep in mind that we expect a high level of uncertainty in these predictions.
These average w^{T,v}(r) functions show a smooth behaviour for the LINEAR and LOG2LPT implementations, although the LOGLINEAR case displays a slight flattening on 50−80 h^{1} Mpc scales, which is absent in the other two cases and is not well fit by the data. We expect correlation functions obtained from the GALAXY mock catalogue to be noisier than the real ones obtained from the CGC, since typically only about 80 000 mock galaxies survive the mask and the selection function, as opposed to the 150 000 surviving galaxies in the real CG sample. The fits of the real data to the solid lines in Fig. A.1 yield S/N ≡ A^{wv,T}/σ_{Awv,T} = 3.0, 2.0, and 2.1 for the LINEAR, LOGLINEAR, and LOG2LPT approaches, respectively.
All Figures
Fig. 1 Absolute value of versus distance to the observer after obtaining AP kSZ temperature estimates on the real positions of CGs (black line) and on a rotated CG configuration (red line). The green line provides the theoretical expectation for the rms of , and the blue histogram displays the radial distribution of the CGs (see text for further details). 

In the text 
Fig. 2 Reconstruction of the xcomponent of the peculiar velocity field (arrows) in a narrow slice of the grid containing the CGC over the corresponding density contrast contour 2D plot. 

In the text 
Fig. 3 Correlation coefficient of the recovered lineofsight velocities with the actual ones in our GALAXY mock catalogue. Solid, dotted, and dashed lines refer to the LINEAR, LOGLINEAR, and LOG2LPT approaches, respectively. The red lines consider the ideal scenario without any sky mask or selection function, while the black ones are for the same sky mask and selection function present in the real CGC. 

In the text 
Fig. 4 Computation of the kSZ pairwise momentum for the CGC sample. The top row, from left to right, displays the results for different aperture choices on the raw HFI 217 GHz map, namely 5, 8, 12, and 18 arcmin. The top row also shows the analysis for the foregroundcleaned SEVEM map, displayed with blue squares. The fit to the pairwise momentum templates from the CLUSTER catalogue is also displayed by the solid red line, and the GALAXY catalogue by the green line. The bottom row presents the results at a fixed aperture of 12 arcmin for different frequency maps, including WMAP9 Wband data (red squares). 

In the text 
Fig. 5 Filled circles: measured kSZ pairwise momentum for the kSZ map derived from the CLUSTER simulation after considering different radial apertures on a subset of clusters in the mass range (1−2) × 10^{14}h^{1} M_{⊙}. Black triangles: pairwise momentum computed from the GALAXY mock catalogue (filled triangles) after assigning these galaxies a tSZ amplitude following a mass scaling inspired by the tSZ measurements of the CGC given in Planck Collaboration Int. XI (2013). 

In the text 
Fig. 6 Measured crosscorrelation function between the kSZ temperature estimates and the recovered radial peculiar velocities, , according to the LINEAR approach. The recovered velocities are divided with their rms dispersion σ_{v} = 310 km s^{1}, so kSZ temperature estimates are correlated to a quantity of variance unity. This plot corresponds to an aperture of 8 arcmin. Filled coloured circles correspond to estimates from different CMB maps (SEVEM, SMICA, NILC, COMMANDER, and the HFI 217 GHz map). The dotted lines display the null estimates obtained after computing kSZ temperature estimates for rotated positions on the SEVEM map, and the thick dashed line displays the average of the dotted lines. Error bars are computed from these null estimates of the correlation function. The solid line provides the best fit of the SEVEM data to the theoretical prediction for obtained from the GALAXY mock catalogue. These predictions are obtained using only a relatively small number of mock halos, and hence their uncertainty must be considered when comparing to the data. 

In the text 
Fig. 7 Same as in Fig. 6, but with the null correlation functions (displayed by dotted lines) being estimated after assigning the recovered linear velocity estimate of a given CG to any other CG in the sample (that is, by “shuffling”). Only the LINEAR approach is displayed in this plot. 

In the text 
Fig. 8 Dependence on the aperture radius of the correlation function obtained in the LINEAR approach for the SEVEM map. Error bars are estimated from the rms of the null correlation functions computed from rotated kSZ temperature estimates. 

In the text 
Fig. 9 Evaluations of the χ^{2} statistic of the correlation function (with respect to the null hypothesis) for different angular apertures. Only results for the foregroundcleaned SEVEM map are shown. There is evidence for kSZ signal in a wide range of apertures above the FWHM, with a local maximum close to 8 arcmin. This roughly corresponds to a radius of 0.8 h^{1} Mpc from the CG positions at the median redshift of the sample. 

In the text 
Fig. 10 Variation of the recovered correlation function for the four lowest frequency raw HFI maps after an effective convolution by a Gaussian beam of FWHM = 5 arcmin. Error bars here are computed in the same way as in Figs. 6 and 8. 

In the text 
Fig. 11 Histogram of the angle subtended by R_{200} of the CGC members. 

In the text 
Fig. A.1 Measured crosscorrelation function between the kSZ temperature estimates and the recovered radial peculiar velocities, , according to the three adopted approaches, LINEAR (left panel), LOGLINEAR (middle panel), and LOG2LPT (right panel). The velocities are normalized with their rms dispersion σ_{v} = 230, 310, and 200 km s^{1}from left to right, respectively. We use an aperture of 8 arcmin when estimating kSZ temperature fluctuations. Filled coloured circles correspond to estimates from different CMB maps (SEVEM, SMICA, NILC, COMMANDER, and the HFI 217 GHz map). The dotted lines display the null estimates obtained after computing kSZ temperature estimates for rotated positions on the SEVEM map, and the thick dashed line displays the average of the dotted lines. Error bars are computed from these null estimates of the correlation function. The solid line provides the best fit to the data of the theoretical prediction for obtained from the GALAXY mock catalogue. These predictions are obtained using only a relatively small number of mock halos, and hence their uncertainty must be considered when comparing to data. 

In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.