Planck 2011 Conference the Millimeter And

PLANCK 2011 CONFERENCE

THE MILLIMETER AND SUBMILLIMETER SKY IN THE PLANCK MISSION ERA

10-14 January 2011 Paris, Cité des Sciences

(Abstracts version Jan 14th)

Planck mission status, Performances, Cross-calibration

Herschel - update with a Planck perspective Pilbratt Goran, European Space Agency The Herschel Space Observatory was launched together with Planck on 14 May 2009. Herschel carries a 3.5 m diameter Cassegrain telescope and three instruments: PACS, SPIRE, and HIFI. It covers the wavelength range ~55-671 um for photometry and spectroscopy, with an angular resolution of approximately 7"/100 um. Early Herschel science performance and science results will be presented, with an attempt of a Planck perspective. The observing opportunities for follow-up of Planck results, in particular the ERCSC, will be outlined.

Radio sources

A Bayesian technique to detect point sources in CMB maps Argueso Francisco, Departamento de Matematicas. Universidad de Oviedo and E. Salerno, D. Herranz, J. L. Sanz, E. Kuruoglu, K. Kayabol; IFCA, CSIC, Santander, Spain. ISTI, CNR, Pisa, Italy The detection and flux estimation of point sources in cosmic microwave background (CMB) maps is a very important task in order to clean the maps and also to obtain relevant astrophysical information. We propose a new strategy based on Bayesian methodology which can be applied to the blind detection of point sources in CMB maps. The method incorporates three prior distributions: a uniform distribution on the source locations, an extended power law on the source fluxes, following the De Zotti counts model, and a Poisson distribution on the number of point sources per patch. Together with a Gaussian likelihood, these priors produce a posterior distribution. We maximize this posterior with respect to the source fluxes in order to estimate them. At the same time, we show that the detected sources must be in the peaks of the matched-filtered maps. Finally, we choose the number of sources which maximizes the posterior for the estimated fluxes. In this way, we give a non- arbitrary method to select the number of point sources. To check the performance of our method, we carry out flat CMB simulations for the Planck channels from 30 to 100 GHz. For simplicity, we have excluded the foregrounds in our simulations. We compare our Bayesian strategy with the application of a matched filter with a typical 5 sigma cut. The percentage of spurious sources is always below 5% from 0. 2 Jy on for both methods and the completeness is much better for the Bayesian method.

The 10C survey of Radio Sources - First Results. Scaife Anna, Dublin Institute for Advanced Studies on behalf of the AMI Consortium; Cavendish Laboratory, University of Cambridge

1 I present first results from the Tenth Cambridge (10C) Survey of Radio Sources at an observing frequency of 15.7GHz. The survey fields cover an area of 27 sq. degrees to a flux density completeness of 1mJy, and include deeper areas covering 12 sq. degrees complete to 0.5mJy. The 10C survey is the deepest radio survey of any significant extent (>0.2 sq. degrees) above 1.4GHz. The 10C source catalogue contains 1897 entries and is reasonably parameterized by a single power law. At S<60mJy the measured counts are found to be lower than those predicted by de Zotti et al. (2005). Matching the 10C catalogue to the 1.4GHz FIRST and NVSS results provides evidence that the spectral indices of the sub-mJy population at 15.7GHz are flatter than those of the super-mJy population. I will discuss these results in detail as well as providing a technical overview of the survey itself.

Spectral energy distributions and radio continuum spectra of northern extragalactic radio sources Lahteenmaki Anne, Aalto University, Metsahovi Radio Observatory (invited on Planck early paper) SEDs, based on Planck ERCSC and simultaneous multifrequency data, of a northern sample of extragalactic radio sources are presented. The large frequency coverage of Planck also allows a look at the more detailed radio continuum spectra. SED modelling methods are briefly discussed, with an emphasis on proper modelling of the synchrotron component.

Ground based radio observations for Planck Massardi Marcella, INAF-Osservatorio Astronomico di Padova Planck is performing an all-sky, low resolution, survey in nine bands from 30 to 857 GHz detecting a large sample of extragalactic radio sources. We will discuss the role of extragalactic radio sources in Planck data and the synergies of Planck with some of the major ground-based observational facilities (ATCA, Efferlsberg, Medicina, Metsahovi, RATAN, VLA) investigating the radio source population properties in total intensity and polarisation. By joining almost simultaneous ground-based observations at frequencies lower or comparable to the Planck ones it is now possible to reconstruct the SEDs across the radio and FIR bands to investigate the population properties and improve the models that describe the physics of radio sources without any effect due to variability. On one hand Planck benefits from observations close in time and frequency to the lower Planck ones to validate the quality of the source extraction techniques in total intensity and polarisation. On the other hand, Planck flux density calibration based on the CMB dipole are being used to solve the absolute calibration difficulties for the ground-based telescopes due to AGN variability and to the fact that planets have complicated emission and are resolved for interferometers. Here we show some of the results of these observational campaigns, focussing on those obtained by the Planck-ATCA Co-eval Observations project for the Southern sky and by the Simultaneous Medicina-Planck Experiment for the Northern sky.

The CMB Polarization Foreground of Radio-loud AGNs Wiesemeyer Helmut, Max Planck Institute for Radio Astronomy and I. Agudo (1), C. Thum (2); (1) IAA Granada (Spain) /Institute for Astrophysical Research, Boston (USA), (2) IRAM Grenoble (France) Out of the Galactic plane, the most important contribution to the contamination of CMB polarization measurements by foreground sources is from radio-loud AGNs. Monitoring their polarization properties at mm (rather than radio) wavelengths during the Planck mission is a valuable tool both for studying the intrinsic polarization properties of AGN (owing to the weakness of Faraday rotation) and for the correction of the corresponding foreground signal in Planck's HFI survey. The polarization of AGNs at mm wavelengths is dominated by the emission from the compact, innermost regions of their relativistic jets, whereas the bright emission at cm wavelengths is from jet regions further downstream, because of synchrotron opacity effects. We have observed 145 flat-radio-spectrum AGNs with flux density exceeding 1 Jy, using the XPOL polarimeter at the IRAM 30m telescope at 86 GHz. 76 % and 6 % of our source sample (dominated by blazars) show linear, respectively circular polarization above detection thresholds of 1.5 % and 0.3 %, respectively. The linear polarization at 86 GHz exceeds that at 15 GHz by a factor of ~2, and the jet luminosity is anti-correlated with the fractional linear polarization. No correlation was found between the position angles of the linear polarization and those of the jet axis, most likely due to the asymmetry of the 3mm emission region of the jets. Here we will discuss the relevance of our results for the accurate removal of foregrounds in CMB surveys.

High frequency blazar flares: The potential of Planck Rachen Jorg Paul, Max-Planck-Institite for Astrophysics and G. Rocha (1), L. Fuhrmann (2), E. Angelakis (2), T.P. Krichbaum (2), I. Nestoras (2); (1) Jet Propulsion Laboratory, Pasadena, CA; (2) Max-Planck-Institute for Radioastronomy, Bonn, Germany Blazars, the super-class of flat spectrum radio quasrs and BL Lac objects, are the dominant population of extragalactic point sources at millimetre frequencies(about 30 to 200 GHz), known for their strong variability. In flaring phases, some blazars have shown an increase in luminosity of more than an order of magnitude, in which case non-thermal, variable emission may dominate their spectra even in the submillimetre regime and above. Performing more than four full sky surveys over two years, the Planck Surveyor Mission is an ideal instrument 2 to discover blazar flares in the scarcely explored regime above 100 GHz. We briefly present the potential and methods for the Planck mission to investigate variable point sources, and discuss some interesting cases of variability seen from the comparison of Planck ERCSC data with results from an ongoing monitoring program involving the Effelsberg 100m, and the IRAM Pico Veleta 30m telescopes.

(Poster 01) High-frequency predictions for number counts and spectral properties of extragalactic radio sources Tucci Marco, Laboratoire de l'Accelerateur Lineaire (LAL) and Luigi Toffolatti, Enrique Martinez-Gonzalez; Departamento de Fisica, Universidad de Oviedo, Spain; Instituto de Fisica de Cantabria, CSIC, Universidad de Cantabria, Spain In this contribution we present new predictions on number counts of extragalactic radio sources at frequencies >5GHz, by extrapolating observational data coming from surveys at low radio frequencies. Our approach is somewhat different than before, because we provide a statistical characterization of the source spectral behaviours at high radio frequencies that takes into account, at least partially, the main physical mechanisms responsible of the emission. We focus on flat-spectrum radio sources, i.e. the dominant source population in the flux and frequency ranges we are interested in. Models of synchrotron emission from inhomogeneous unresolved relativistic jets predict that, at a particular frequency, jet emissions cease to be dominated by optically-thick synchrotron, and become dominated by synchrotron in optically-thin regime. Spectra then change its slope from ``flat'' to ``steep''. We determine this frequency on the basis of standard models for synchrotron emission in blazars and of typical values for the involved physical parameters. Moreover, we also discuss the contribution from ""inverted-spectrum"" sources, by using a purely statistical approach. We find that predictions of our model on number counts are in very good agreement with observational data, that cover a large frequency range up to ~220 GHz. Moreover, the model seems able to explain well the average steepening currently observed in the spectral slope of flat-spectrum sources at frequencies >~70

3 Clusters of galaxies, Sunyaev-Zeldovich effect

(Invited) SPT SZ observations Christian Reichardt (University of California, Berkeley) The South Pole Telescope (SPT) is a 10-meter telescope designed to survey the millimeter-wave sky, taking advantage of the exceptional observing conditions at the Amundsen-Scott South Pole Station. The telescope and its ground-breaking 960-element bolometric camera were successfully installed at the South Pole in 2007. Since then, SPT has embarked upon a large, three-frequency survey which will cover 6% of the entire sky by the end of 2011. The primary science goal of the survey is to constrain the evolution of dark energy through a mass- limited catalogue of hundreds of SZ clusters. I will report on the status and early results from the survey.

Latest AMI SZ Results Hurley-Walker Natasha, University of Cambridge I present the latest Sunyaev-Zel'dovich measurements of galaxy clusters with the Arcminute Microkelvin Imager, a radio interferometer operating at 15GHz in Cambridge, UK. These include measurements of a 'Bullet- like' cluster, a comparison with weak lensing data for six massive clusters, a summary of observed large samples of clusters and our first blind survey results. I will also discuss the complementarity AMI offers for following up Planck observations, in terms of sensitivity to gas position and distribution.

Statistical analysis of SZ scaling relations for X-ray galaxy clusters Melin Jean-Baptiste, CEA Saclay - IRFU/SPP and Rocco Piffaretti; CEA Saclay, France All sky data from the Planck survey and the Meta-Catalogue of X-ray detected Clusters of galaxies (MCXC) are combined to investigate the relationship between thermal Sunyaev-Zeldovich (SZ) signal and X-ray luminosity. For each X-ray cluster in the sample the SZ signal is extracted and the statistical significance of the measurement is maximised by averaging the SZ signal in X-ray luminosity, total mass, or redshift bins. The SZ signal is clearly detected over ~3 decades in X-ray luminosity. The derived relation between SZ signal and X-ray luminosity is investigated and the measured SZ signal is compared to values predicted from X-ray data.

Calibration of the local galaxy cluster SZ scaling relations from the Planck first sky survey Pointecouteau Etienne, CESR and Pratt; CEA Saclay, France We present precise Sunyaev-Zeldovich (SZ) effect measurements in the direction of 62 nearby galaxy clusters ($z <0.5$) detected at high signal-to-noise in the first \planck\ all-sky dataset. Combining these high quality \planck\ measurements with deep \xmm\ X-ray data, we investigate the relations between $Y_{500}$, the integrated Compton parameter due to the SZ effect, and the X-ray-derived gas mass $\Mgv$, temperature $\TX$, luminosity $\LX$, thermal energy $Y_{\rm X} = M_{\rm gas,500} \times T_X$, and total mass $\M500$. We find results that are in excellent agreement with both X-ray predictions and recently-published ground-based data derived from smaller samples. This sample yields an exceptionally robust, high-quality local reference, and illustrates the superior nature of \planck\ for statistical studies of galaxy clusters, especially due to its all-sky coverage.

Sunyaev-Zel'dovich imaging with Bolocam Sayers Jack, Caltech and S. Golwala, S. Ameglio, N. Czakon, T. Downes, E. Pierpaoli, S. Siegel; USC We will present the results from high S/N SZ images made with Bolocam. To date, we have imaged ~40 clusters to a depth of ~10 uK-arcmin. The images are approximately 6-7 arcmin in radius with 1 arcmin resolution. Our data are of sufficient quality to constrain models without relying on X-ray data, and we are able to study morphologies in individual clusters (e.g., ellipticity). Additionally, we are able to compute the integrated Comptonization out to r_500 in a model-independent way, with ~10% uncertainties limited entirely by systematics. We have also performed joint SZ/X-ray analyses to constrain approximately mass-weighted temperature profiles to beyond r_500, and to examine the scaling between Y_SZ and X-ray observables such as m_gas. Our targets are primarily high-mass (~10^15 M_sun) clusters at moderate redshifts (0.3 - 0.9), and should therefore be contained in, and be representative of, the clusters in the Planck Cluster Catalogue (PCC). Consequently, our data will supplement the PCC with deeper, higher resolution SZ data.

Identification of galaxy clusters in the CMB maps Wuensche Alex, Instituto Nacional de Pesquisas Espaciais - INPE and Camila P. Novaes; The Cosmic Microwave Background (CMB) is considered one of the most important astrophysical observables. The study of their properties is used to understand the mechanisms of structure formation in the Universe. Secondary temperature fluctuations, generated after the recombination, mask the primary signal of the CMB, 4 hindering the study of their intrinsic properties. One such process is known as the Sunyaev-Zel'dovich effect (SZ), caused by inverse Compton scattering of CMB photons. SZ effect measurements are used to estimate cosmological observables such as the Hubble constant, the relationship between angular diameter - distance and the parameter Ω of the equation of state of dark energy. The Planck satellite, launched in 2009 by the European Space Agency, is dedicated to the study of CMB and one of the expected results of data analysis is the separation of signals contaminating the CMB, including the SZ effect. This paper presents the analysis of the distribution of SZ clusters in simulated Planck CMB maps. The clusters were produced with beta-isothermal temperature profiles and combined with synthetic CMB maps and galactic noise to test a noise-sensitive adaptation of an ICA-based algorithm known as JADE. Preliminary results show that the method is effective in identifying the position and intensity of the SZ effect in each cluster.

5 Interstellar medium components

CosmoRec: A New Cosmological Recombination Code Chluba Jens, CITA and Rajat Thomas; CITA In this contribution I will introduce CosmoRec, a new cosmological recombination code, which was developed to quickly solve the hydrogen and helium recombination problem, including previously neglected physical processes, such as Lyman-a diffusion and two-photon processes from excited states. CosmoRec is now ready for parameter estimation with CosmoMC, and I will show the results of forecasts for upcoming Planck data. I will also briefly discuss the results of a non-parametric estimation of recombination uncertainties to identify how much we can learn about recombination from CMB data itself.

Studying the Galactic magnetic field in the plane Jaffe Tess, CESR Toulouse We study the magnetic field of the Galaxy in the plane using three complementary observables to disentangle three field components defined as the coherent field, the ordered field, and the isotropic random field. Using a combination of low-frequency radio data to trace total synchrotron intensity, microwave measurements of synchrotron polarized intensity, and Faraday rotation measures, we can separate the field components due to the different geometry of their effects on the three observables. We use our publicly available code to simulate the observables from physical models of the relevant components of the magneto-ionic medium, and an MCMC approach to model selection. This framework allows us to perform a self-consistent analysis with fewer simplifying assumptions, and in particular to study the ordered field that is often neglected as well as realistic models for the cosmic ray distribution. After presenting our results so far, I will discuss the impact Planck will have on this project.

Galactic cold cores with the Planck and Herschel satellites Juvela Mika, University of Helsinki and Isabelle Ristorcelli and the Cold Cores team; CESR, Toulouse In the project ""Galactic Cold Cores"" we are using the combination of Planck and Herschel satellites to study the initial stages of star formation. The sensitive sub-millimetre observations of Planck give, for the first time, the possibility of an unbiased survey of cold starless and pre-stellar cores all over the sky (cf. talk by L. Montier). A representative cross section of this population is being studied in detail with Herschel photometric observations. We will present an overview of the project and its goals, and discuss the first results obtained in the Herschel studies. These confirm the earlier findings on the dust evolution between diffuse and dense clouds and illustrate the great variety in the nature of the cold objects Planck is detecting.

Distribution of Planck Cold Cores - loops and clusters Marton Gabor, Eotvos Lorand University and S. Zahorecz, L. V. Toth, M. Juvela, I. Ristorcelli, L. Montier, D. Marshall and the Planck Cold Core Team; University of Helsinki, CESR We investigated the spatial distribution of clumps from the Cold Core Catalog of Planck Objects (C3PO) and and found it to be highly nonuniform. The large and small scale distribution anomalies were analysed. We identified groups using the Minimum Spanning Tree method and measured their elongation. The number of groups is significantly higher than in random samples with the same source density and the same marginal distributions along l and b. We note that the larger groups are more common in the C3PO than in the random sample.The mean elongation of the groups in the simulated samples does not differ from that in the C3PO. We also compared the distribution of C3PO clumps to the FIR loops in the Konyves et al. (2006) catalog of IRAS Galactic Infrared Loops and Heiles HI shells (1984). We found a significant excess of clumps on the shells. Heiles, C., 1984, ApJS, 55, 585 Konyves, V., Kiss, C., Moor, A., Kiss, Z. T., & Toth, L. V. 2007, A&A, 463, 1227

6 IR galaxies, CIB

(Invited) Infrared and submm galaxies models Gianfranco De Zotti (INAF, Osservatorio Astronomico di Padova) The spectacular success of hierarchical ΛCDM at explaining the large-scale structure (> 1Mpc) has led to the widespread opinion that the formation of visible galaxies parallels that of dark matter halos: small objects form first and merge together to make larger ones; most of the star-formation, and of the black hole accretion, in the early universe is triggered by galaxy interactions and mergers, and therefore occurs in bursts. However, several bodies of evidence sit uncomfortably with, or at least were not predicted by, the simplest bottom-up merger driven scenario drawn from the hierarchical-ΛCDM paradigm. These include: downsizing, a number of correlations among parameters characterizing early type galaxies tight enough to leave little room for random processes, insensitivity of galaxy properties to environment, large stellar mass fraction in fragile disks. Difficulties are more easily overcome if baryon processes, rather than merging, are the main drivers of galaxy evolution after a fast accretion phase (timescale « H(z)-1) in which the potential well is created by major mergers, as found by some high resolution simulations. The subsequent accretion, mostly in the form of minor mergers, generally adds mass in the outskirts of the halo, affecting only weakly the central region where the stellar component resides, although merger-driven starbursts and black-hole accretion episodes occasionally occur. Implications of this scenario are discussed with special reference to far-IR and sub-mm data.

CIB anisotropies modeling Doré Olivier, Jet Propulsion Laboratory Cosmic Infrared Background (CIB) ansiotropies are expected to trace the correlated large-scale structure and thus to probe the clustering properties of galaxies and their associated dark matter halo. To understand the clustering of CIB anisotropies requires a modeling of the connection between dusty star-forming galaxies and the dark matter. It is thus related to the relationship between star-formation and the dark-matter distribution. We will discuss in this context the latest measurements from the Planck data.

Anomalous Dust in Late-Type Galaxies Israel Frank, Sterrewacht Leiden The fully-sampled spectral energy distributions (SEDs) of the Magellanic Clouds exhibit a significant amount of emission in the 10-300 GHz range in excess of extrapolated far-infrared dust ionized gas emission. Such an excess is absent in the fully-sampled qSEDs of the starburst galaxies HC 253 and NGC 4945, but is marginally present in the M 82 SED. Other presently available galaxy SEDs generally lack coverage of the crucial 10-100 GHz range, but far-infrared and submillimeter measurements suggest that millimeter-wavelength excess emission may be common in star-forming dwarf galaxy SEDs. and absent or unimportant in thje SEDs of more massive starburst galaxies and (ultra)luminous infrared galaxies. The nature of the dust responsible for the excess emission is briefly discussed.

ALMA Kneissl Ruediger, ALMA/ESO The Atacama Large Millimeter/submillimeter Array (ALMA) is currently under construction at 5000m in Chile. It will have an array of at least 50 twelve-meter antennas, a compact array of 12 seven-meter antennas and 4 total power antennas to provide imaging on angular scales from arcminutes to tens of milliarcsecs. The frequency range will be 30 to 900 GHz with instantaneous bandwidth of 8 GHz for continuum observations or wide lines, but with spectral resolution as fine as 7.6 kHz available for observing narrow lines. Early science is expected to start in the second half of 2011 with 16 antennas in four bands (band 3: 84 - 116 GHz, band 6: 211 - 275 GHz, band 7: 275 - 373 GHz, band 9: 602 - 720 GHz), two or more array configurations and an initial set of correlator modes. In this presentation I will discuss the current status of construction, opportunities for ALMA observation of compact Planck sources and report about current and future Planck relevant observatory task observations, for example the compilation of a calibrator catalogue.

Correlations in the (sub)millimeter background from ACT x BLAST Viero Marco, California Institute of Technology and Amir Hajian, Graeme Addison; Canadian Institute for Theoretical Astrophysics, Oxford University Understanding how infrared galaxies are correlated is necessary in order to 1) understand the role of the environment in galaxy formation, and 2) quantify their contribution to the CMB spectrum in order to correctly measure the power from secondary CMB anisotropies, such as the SZ or lensing. However, the vast majority of infrared galaxies in the (sub)millimeter background are unresolved, so that to measure correlations in galaxy population requires measuring the power spectrum of the unresolved background. Furthermore, the multiple contributions to the sky at millimeter wavelengths makes isolating the power from infrared galaxies difficult. Cross-correlations of millimeter maps with submillimeter maps provides a way to identify and isolate the contribution from the infrared galaxies common to both, and in particular to estimate the strength of the clustered term vs. wavelength. Here we present the first measurements of the auto and cross-correlation power 7 spectra of the cosmic submillimeter background at: 250, 350, and 500 µm (1200, 860, and 1200 GHz) from observations made with the Balloon-borne Large Aperture Submillimeter Telescope, BLAST; and at 1380 and 2030 µm (218 and 148 GHz) from observations made with the Atacama Cosmology Telescope, ACT. These results will complement those anticipated from the Planck mission by extending to higher resolution in the millimeter wave regime.

(Poster 02) Modeling the evolution of infrared galaxies: A Parametric backwards evolution model Bethermin Matthieu, IAS and Dole Hervé, Lagache Guilaine, Le Borgne Damien and Pénin Aurélie; IAS, IAP We present a new backwards evolution model. This model reproduces the statistical properties of the infrared galaxies among which the number counts between 15 microns and 1.1 mm, the luminosity functions, and the redshift distributions. This model uses an evolution in density and luminosity of the luminosity function parametrized by broken power-laws with two breaks at redshift ~0.9 and 2, and contains the two populations of the Lagache et al. (2004) model: normal and starburst galaxies. We also take into account the effect of the strong lensing of high-redshift sub-millimeter galaxies. It has 13 free parameters and 8 additional calibration parameters. We fit the parameters to the IRAS, Spitzer, Herschel and AzTEC measurements with a Monte-Carlo Markov chain. Our model ajusted on deep counts at key wavelengths reproduces well recent very discriminating observations like Oliver et al. (2010) Herschel counts and the Jauzac et al. (2010) measured redshift distribution of the CIB. We discuss the contribution to the cosmic infrared background (CIB) and to the infrared luminosity density of the different populations included in the model. We also estimate the effect of the strong lensing on the number counts, and discuss the recent discovery by the South Pole Telescope (SPT) of a very bright population lying at high-redshift.

(Poster 25) Linear bias model for ACT x BLAST clustered IR source power Graeme Addison, University of Oxford We have measured cross-correlation power spectra of the cosmic infrared background using the 8.6 square degrees common to both the BLAST (250, 350 and 500 micron) and ACT (1.38mm - 217 GHz and 2.03mm - 148 GHz) maps. We detect a clustered component at >4 sigma in addition to a Poisson level in the ACTxBLAST cross-correlations. We successfully fit the clustering power in all the cross-spectra simultaneously using a linear bias model with a simple redshift-dependent bias parameterisation and use this model to make predictions for the size of the clustered components we expect in the Planck HFI bands.

8 Dust emission in different phases of the ISM

Planck Early Results: New Light on Anomalous Microwave Emission from Spinning Dust Grains Clive Dickinson (Jodrell Bank Centre for Astrophysics) Planck data, combined with multi-frequency data, has allowed accurate spectra from the radio to far infra-red to be constructed for bright regions in our Galaxy. Spectra for the Perseus and Rho Ophiuchus molecular clouds show strong evidence for Anomalous Microwave Emission (AME) at frequencies 10-100 GHz. The residual spectra, after subtraction of the free-free, CMB and thermal dust components, represent the most precise spectra of AME to date. They show a peaked spectral shape, with a peak at ~30 GHz, as expected from electric dipole radiation from small spinning dust grains. A plausible physical model for the spinning dust can provide a good fit to the data, where the higher density molecular gas accounts for most of the AME, while the lower density atomic gas appears to play a minor role. A search for new AME regions with the Planck data has revealed a number of candidates showing excess emission at 28.5 GHz. Two such regions are presented, which may also be due to spinning dust.

Magnetic field components analysis of the SCUPOL 353GHz polarization data catalog Poidevin Frederick, IAG-USP and Kowal, G., Falceta-GonÁalves, D.(*), Gouveia Del Pino, E. and Magalh„es, A.M.; (*) USP Leste The SCUPOL catalog is a compilation of 83 regions that were observed at JCMT between 1997 and 2005. Polarization maps at 850 microns (353 GHz) are available on 48 star forming regions (SFR), 11 Young stellar Objects (YSO) and 6 Starless Prestellar Cores (SPC). For sufficiently sampled maps, observables are defined that help to characterize the turbulent-to-mean magnetic field ratio, the depolarization slope and the polarization properties of each region. The analogs of such observables ("simulables") are calculated from 2D polarization maps produced with 3D MHD 512 pixel grid simulations which were performed for 6 different MHD regimes, including super-Alfvenic and sub-Alfvenic regimes. The "observables" obtained from the simulations are systematically compared to the observables obtained from the data and tentative classification of the observed regions are derived. The SCUPOL compilation is an interesting catalog to test our technics. Such an approach might be very useful to characterize the magnetic and turbulent properties of the molecular clouds and star- forming regions observed with PLANCK.

The Fermi view of the high-energy interstellar medium and its relevance to Planck Strong Andy, Max-Planck-Institut fuer extraterrestrische Physik on behalf of the Fermi-LAT Collaboration; The Fermi and Planck missions share much Galactic astrophysics related to the interstellar medium. I concentrate on the aspects related to high-energy particles: cosmic-ray electrons in the 1 GeV - 1 TeV range are responsible for the inverse Compton emission measured in gamma rays and the synchrotron emission measured in radio. Fermi also measures the cosmic-ray electron spectrum with unprecedented accuracy, and other new cosmic-ray data are providing tight constraints on models. Thus Fermi and Planck promise to be highly complementary in understanding the high-energy Milky Way. The relevant observables include spectral indices and their variations, and intensity maps in both gamma rays and radio. I will discuss this subject in the context of a detailed model of cosmic-ray propagation and magnetic fields.

(Poster 03) SN turbulence and the formation of high latitude structures†in the halo of the Galaxy De Gouveia Dal Pino Elisabete, IAG-USP and C. Melioli (2), R. Santos-Lima (1), F. Geraissate (1), A. Lazarian (3); (1) IAG-USP, University of S„o Paulo; (2) University of Bologna, Italy; (3) University of Wisconsin, Madison The Milky Way, like other star forming galaxies, exhibits a hot halo with structures that resemble chimneys and fountains extending for up to several kpc above the disk. Observations indicate that they may be produced by SNe. These can blow superbubbles that carve holes in the disk through which high speed material can be injected and expand buoyantly up to a maximum height and then return to the disk pulled by the galaxy gravity. This circulating gas in a fountain tends to condense out forming high-velocity cold clouds and filaments above the galactic disk that could be probed at Planck wavelengths. We will here discuss this mechanism helped by three-dimensional hydrodynamical simulations of the Galaxy and its halo. These indicate that SNe-induced turbulence plays a key role in driving outflows and the formation of observed cold clouds †in the halo, at least in †intermediate latitudes (of a few kpc). PLANCK can also provide important information about the MHD turbulent properties of the molecular clouds and star-forming regions in the galactic disk. In particular, it may be able to probe the real role of the magnetic field in the first stages of star formation. In this talk I will also discuss this issue and show that the diffusion of magnetic field induced by MHD turbulent reconnection is †a very efficient mechanism, especially in the early stages of †clump collapse and star formation.

(Poster 04) Atlas and Catalog of Dark Clouds Based on the 2 Micron All Sky Survey 9 Dobashi Kazuhito, Tokyo Gakugei University and Shimoikura, Tomomi; Tokyo Gakugei University We present an atlas and catalog of dark clouds derived based on the 2 Micron All Sky Survey Point Source Catalog (2MASS PSC). Color excess maps of E(J-H) and E(H-Ks) as well as extinction maps of A_J, A_H, and A_Ks covering all of the sky have been produced at the 1' grid with a changing angular resolution from 1' to 12' depending on the regions in the sky. The maps obtained in this work are presented on various scales in a series of figures that can be used as an atlas of dark clouds for general research purposes including the comparison with the FIR dust emission detected by Planck. Based on the color excess and extinction maps, we further carried out a systematic survey for dark clouds all over the sky, and identified 7614 dark clouds in total. We also searched for their counterparts in the previously published catalog of dark clouds based on the optical photographic plates DSS (Dobashi et al. 2005). Cloud parameters such as the coordinates, the visual extinction, and the counterparts are compiled into a new catalog of dark clouds, which will appear in a special issue of the Publications of the Astronomical Society of Japan (PASJ, Dobashi 2011, in press). Digital version of the data will also be available on the internet (Shimoikura & Dobashi, see a poster presentation in this conference).

(Poster 05) Super CO survey with NANTEN2: A key to understand the foreground emission in the Planck results Fukui Yasuo, Department of Physics, Nagoya University It is the most crucial issue to experimentally test the physics of inflation, the most dramatic rapid expansion over 30 orders of magnitude in the earliest stage of the Big Bang and the detection of the B mode polarization in the CMB is most crucial for this purpose. It is at the same time increasingly recognized that the understanding of foreground emission is crucial in deducing the B mode polarization because the B mode signal is so weak and the foreground Galactic polarized emission is so overwhelming due to dust in the ISM at 100GHz or higher. We intend to make a new almost whole sky CO survey at 3 arcmin resolution with NANTEN2 4m telescope located in Atacama, Chile at 4865m altitude in order to obtain the key data to understand the physical properties of the densest phase of the ISM and to have the best estimate of the contribution of the foreground ISM. The results will provide a powerful to remove the foreground emissions in the Planck results and to deduce the weak polarization signals.

(Poster 06) Galactic foreground simulations and observations at low radio frequencies Jelic Vibor, ASTRON Cosmic microwave background (CMB) and epoch of reionization (EoR) experiments have one major thing in common: prominent Galactic and extragalactic foreground emission that challenges the observations. Properties of these foregrounds are quite different at the CMB (>10 GHz) and EoR (< 200 MHz) observing frequencies. However, multi-frequency observations can help us to constrain and understand the physical origin of the foreground emission, minimize the foreground contamination, and result in success of both cosmological experiments. During this talk I will give: (i) an overview of observational constrains of Galactic emission at the EoR observing frequencies, including a recent results obtained with the WSRT telescope; (ii) present a simulation of the Galactic emission used as a foreground model for the Low Frequency Array (LOFAR)-EoR key science project; and (iii) discuss the mutual benefit of multi-frequency foreground observations. Note that our Galactic model produces total and polarized intensity maps (over 10 deg x 10 deg) of Galactic synchrotron and free-free emission, including all its observed characteristics, e.g., spatial fluctuations of amplitude and spectral index, together with Faraday rotation effects. The model has flexibility to provide maps at any desired frequency.

(Poster 07) Aggregate dust connections and implications for astronomical observations at sub-mm wavelengths Koehler Melanie, Institute d'Astrophysique Spatiale and Vincent Guillet; Anthony Jones Collected interplanetary dust particles show in some cases an aggregate structure. The single monomers are of irregular shape and are connected to neighbouring monomers with certain contact areas. An aggregate structure is also assumed for dust in the denser interstellar medium (ISM). In order to carry out model calculations of aggregates different theories are available to calculate their optical properties: e.g., T-matrix method (TMM), generalized multi-particle Mie theory (GMM) or discrete-dipole approximation. While TMM and GMM give the same results, an enhancement occurs at long wavelengths for silicate and amorphous-carbon grains using DDA. We show that this enhancement is not due to uncertainties in DDA but it is due to a different description of the aggregate. For TMM and GMM monomers are assumed as perfect spheres that connect in a point contact with each other. For DDA monomers are built out of dipoles and the contact between monomers is at least one dipole. This larger contact area increases the dust emissivity where the real part, n, of the refractive index is large. For silicates and amorphous carbon n is large at long wavelengths. The coagulation of monomers into aggregates can then explain the enhanced dust emissivity observed at long wavelengths (FIR to mm) in colder regions of the ISM compared the dust emissivity observed in the diffuse interstellar medium. The model presented here will help in the interpretation of the data from Planck for dust in the ISM.

(Poster 08) Extracting information on magnetic power and helicity from galactic polarization maps at CMB frequencies Oppermann Niels, Max Planck Institute for Astrophysics and Torsten Ensslin, Georg Robbers, Henrik Junklewitz; Correlations in Stokes I, Q and U of galactic synchrotron emission permit to measure magnetic correlation functions like power spectra. We show that it is in principle possible to even infer signatures of magnetic helicity using CMB foreground polarization data in connection with measurements of the Faraday rotation of extragalactic sources. A novel method for this is the LITMUS test (Local Inference Test for Magnetic fields which Uncovers heliceS), for which we present results using WMAP and synthetic data. The advent of both more precise and more highly resolved polarization data from Planck as well as improved Faraday Rotation data, brought along by telescopes such as LOFAR, will permit much more accurate probing of galactic magnetic helicity and other magnetic correlation functions.

(Poster 09) Variations of grain emissivity from far-infrared to millimeter wavelengths Paradis Deborah, CESR and Bernard, J.-Ph, Mény, C.; Dust emissivity and its variations with wavelength and temperature are critical for separating astrophysical foreground emission. Grains are probably affected by different physical processes depending on the environment. Their properties are likely to vary according to the density of the medium. We analysed the evolution in dust emissivities from the FIR (100 µm) to millimeter (3.2 mm) wavelengths. Using DIRBE, ARCHEOPS and WMAP data, we performed a correlation study of the IR emission with gas tracers, in the outer Galactic plane, in preparation of the Herschel and Planck missions. We evidenced that the emissivity spectra are always steeper in the FIR (λ < 600 µm) and flatten in the submm and mm. Recent spectroscopic laboratory data reproduce a similar behavior, promising result for a better understanding of the grain composition. In regions where dust is significantly colder in the molecular phase than in the surrounding atomic medium, we produced an increase in the emissivity by a factor of ≈3 in the FIR. However, we showed that the emissivity increase is restricted to the FIR range; the emissivity spectra for the dust in the HI and CO phases become comparable again in the submm and mm wavelength range. We interpret the FIR emissivity increase in molecular clouds containing cold dust as being caused by the coagulation of large grains into fractal aggregates. A forthcoming study will combine Planck with Herschel data to investigate processes of dust a

(Poster 12) BLAST-Pol Scott Douglas, University of British Columbia for the BLAST-Pol Team; University of Pennsylvania, University of Toronto, Cardiff University, University of Miami, INAOE (Mexico), Brown University, Northwestern University, University of Puerto Rico, INAF (Italy), UCL The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLAST-Pol) is a suborbital mapping experiment designed to study the role played by magnetic fields in the star formation process. BLAST- Pol is the reconstructed BLAST telescope, with the addition of linear polarization capability. Using a 1.8-m Cassegrain telescope, BLAST-Pol images the sky simultaneously at 250, 350, and 500 microns, reaching a resolution of 30" at 250 microns. The polarimeter consists of polarizing grids mounted in front of each detector array, with a rotating 4 K achromatic half-wave plate providing additional polarization modulation. With its unprecedented mapping speed and resolution, BLAST-Pol will produce three-color polarization maps for a large number of molecular clouds. The instrument provides a much needed bridge in spatial coverage between larger- scale, coarse resolution surveys and narrow field of view, and high resolution observations of substructure within molecular cloud cores. The addition of higher-resolution polarization information in essentially the HFI 545 and 857GHz channels means there is a close synergy between BLAST-Pol and Galactic studies carried out with Planck. The first science flight will be from McMurdo Station, Antarctica in December 2010.

(Poster 13) Radio Recombination Line Surveys Alves Marta, Jodrell Bank Centre for Astrophyisics and Rod Davies(1), Clive Dickinson(1), Richard Davis(1), Lister Staveley-Smith(2), Mark Calabretta(3); (1) JBCA, (2) ICRAR, (3) CSIRO Radio Recombination Lines (RRLs), in contrast to Halpha, can be used to obtain the Emission Measure on the Galactic plane directly with no dust absorption or contamination. Once the electron temperature of the ionized emitting gas is known, the line integral can be converted into the underlying free-free emission. The HIPASS/ZOA survey is used to map the free-free emission on the Galactic plane between l=20 and 44 degrees and abs(b)<4 degrees, at 1.4 GHz and 14.8 arcmin resolution. The RRL data give the velocity and distance of the line emitting gas as well as the electron temperature, when the data are combined with the continuum from the same survey. The free-free distribution is combined with WMAP data to derive the contribution of the synchrotron and anomalous dust components on the Galactic ridge. The 100um IRIS/IRAS data is used to obtain

11 the emissivity of the anomalous dust. I will present the results of this project along with other RRL surveys that can help modelling the diffuse ionized emission across the Galaxy.

(Poster 14) AKARI FAR-INFRARED ALL SKY SURVEY Doi Yasuo, Univ. of Tokyo and S. Komugi (2), N. Ikeda (2), D. Kato (2), Y. Kitamura (2), M. Kawada (2), T. Nakagawa (2), M. Tanaka (3), Y. Matsuoka (4), H. Kaneda (4), M. Hattori (5), T. Otsubo (5), M. Etxaluze Azkonaga (6,7), G.; 2) Institute of Space and Astronautical Science, 3) Tsukuba University, 4) Nagoya University, 5) Tohoku University, 6) The Open University, 7) The Rutherford Appleton Laboratory, 8) Osaka University We demonstrate the capability of AKARI for mapping diffuse far-infrared emission and achieved reliability of all-sky diffuse map. We have conducted an all-sky survey for more than 94 % of the whole sky during cold phase of AKARI observation in 2006 Feb. - 2007 Aug. The survey in far-infrared (FIR) waveband covers 50 µm - 180 µm with four bands centered at 65 µm, 90 µm, 140 µm, and 160 µm and spatial resolution of 30" - 40" (FWHM), providing us the first all-sky survey data with high-spatial resolution beyond 100 µm. The data have been released for the project team members and thus can be utilised through collaboration with the AKARI project. We discuss quantitative evaluation of data quality and its possible application for FIR/sub-mm astronomy, in combination with the Planck data.

(Poster 15) Herschel study of the extended dust emission in the cold clouds located by Planck Juvela Mika, University of Helsinki and Isabelle Ristorcelli and the Cold Cores team; CESR, Toulouse The Herschel Open Time Key Programme Galactic Cold Cores is devoted to the follow-up of the cold dust clouds that are detected in the Planck all-sky survey. Within the project, we will characterize this source population, examine the physical properties and structure of the detected cores, and study the variations in the properties of interstellar dust grains. We will present the results from the analysis of the first three fields, concentrating on the main dust properties. The observations show increasing dust opacity towards the dense and cold regions (T~13K or below), as suggested by models of grain coagulation and ice mantle formation. We find an anticorrelation between dust colour temperature and dust spectral index that cannot be explained by noise alone. With the help of radiative transfer models, we show that the observations may underestimate the real intrinsic spectral index variations of the dust grains.

(Poster 16) Constraints on the Polarization of the Anomalous Microwave Emission in the Perseus Molecular Complex from 7-year WMAP data Lopez-Caraballo Carlos Hugo, Instituto Astrofisica Canarias and Rubino-Martin, J. A.; Rebolo, R.; Genova-Santos, R.; IAC We have used the seven year Wilkinson Microwave Anisotropy Probe (WMAP) data in order to update the measurements of the intensity signal in the G159.6-18.5 region within the Perseus Molecular Complex, and to set constraints on the polarization level of the anomalous microwave emission in the frequency range where this emission is dominant. At 23, 33 and 41 GHz, we obtain upper limits on the fractional linear polarization of 1.0, 1.8 and 2.7% respectively (with a 95 per cent confidence level). These measurements rule out a significant number of models based on magnetic dipole emission of grains that consist of a simple domain (Draine & Lazarian 1999) as responsible of the anomalous emission. When combining our results with the measurement obtained with the COSMOSOMAS experiment at 11 GHz(Battistelli et al. 2006), we find consistency with the predictions of the electric dipole and resonance relaxation theory (Lazarian & Draine 2000) at this frequency range.

(Poster 17) Planck Early results: The mm/submm properties of a sample of Galactic cold clumps Ristorcelli Isabelle, IRAP, Universite de Toulouse - CNRS and I.Ristorcelli, M.Juvela, L. Montier, D. Marshall, V.M.Pelkonen, N.Ysard, JPh Bernard, L.Pagani, R.Paladini, J.Malinen, Y.Doi, E.Falgarone and the whole Working Group WG7.7 Cold Cores.; IRAP, University of Helsinki, IPAC, LERMA, We present the first detailed analysis of ten representative sources from the ëCold Cores Catalogue of Planck Objectsí (C3PO). The sources have been selected to cover different types spanning a wide range of mass, temperature, density and luminosity, and to represent different environments from high latitudes cirrus to nearby and far / molecular complexes. We combine the Planck data with available ancillary data and dedicated follow- up observations with Herschel and ground-based radio telescopes. The physical characteristics of the cores are derived and we discuss the morphology and the internal structure of the Planck detections. We show that the C3PO (and its subsample Early release ECC catalogue) contains a wide variety of clump physical properties, probably associated to different evolutionary stages: quiet, cold and starless clumps, prestellar objects to very young protostars still embedded in their cold surrounding cloud.

(Poster 18) Release of the Atlas and Catalog of Dark Clouds Based on 2 MASS Shimoikura Tomomi, Tokyo Gakugei University 12 and Dobashi, Kazuhito; Tokyo Gakugei University We have organized a new website to release the database of the atlas and catalog of dark clouds based on the 2MASS Point Source Catalog (Dobashi et al. 2011, PASJ, in press. See also Dobashi & Shimoikura in this conference). This website (http://astro.u-gakugei.ac.jp/~tenmon/Atlas/index.html or http://darkclouds.u- gakugei.ac.jp) is designed to be simple and user-friendly with CGI, so that the researchers can easily obtain the necessary color excess and extinction maps in the simple FITS format. Noise maps, resolutions maps, and a catalog of 7614 dark clouds identified using the color excess and extinction maps are also available. In addition, an extinction map of Av derived previously from the optical database DSS (Dobashi et al. 2005) is also organized at the same website. The former maps from 2MASS mainly trace relatively dense regions in dark clouds revealing a number of dense cloud cores leading to star formation, while the latter map from DSS is more suited to trace less dense regions and to reveal the global extents of dark clouds. These two datasets are complementary, and all together, they are useful to picture the structures of dark clouds in various density ranges. We also organize some of these data in beautiful images with a general explanation of dark clouds and star formation for the public (in Japanese only), so that they can be used for astronomy and science education at schools.

13 Cosmological requirements and methods for components separation

Modelling the impact of dust evolution on the dust polarised emission Guillet Vincent, IAS and Francois Boulanger, Laurent Verstraete, Alain Abergel, Melanie Koehler, Anthony Jones; The dust polarised emission and its variations are determined by the structure of the magnetic field on the line of sight, the efficiency of dust alignment on the magnetic field lines, and the nature of the aligned and not aligned dust populations (shape, size distribution, and optical constants). As confirmed by Planck Early Papers (Abergel et al.), the FIR and submm dust emissivities can differ from the standard "diffuse" value by a factor of a few, even at low or moderate extinction (Av ~ 1). Coated grains and agregates are known to have increased emissivities per unit mass compared to single grains. These observations are therefore often interpreted as an indication of dust evolution in diffuse clouds by coagulation and/or mantling. Dust evolution may complicate our ability to remove the dust polarised screen from the Planck data. In this talk, we present calculations of the polarised emission and extinction for models of "evolved" dust characterised by an increased emissivity at long wavelength, and compare our results with that obtained with the standard "diffuse" dust.

(Invited) Optical/NIR Starlight Polarization - A Tool for Studying the ISM Magnetic Field Structure A. M. Magalhaes - IAG, Universidade de Sao Paulo In this talk we will show some recent results of optical/NIR starlight polarization data in several environments, as well as point out the interrelation between such data and those of Planck's. We first explore the relationship between the magnetic field in the local Interstellar Medium (ISM) and the heliosphere. We then discuss our ongoing ISM Survey data and their potential for exploring the magnetic field structure in the Galaxy at small and large scales and at high Galactic latitudes. We also discuss the nature of the SMC dust and its magnetic field structure. Finally, we look into intriguing data concerning the relationship between the ambient magnetic field direction and that of disks around young stars in the Galaxy and Magellanic Clouds.

The C-Band All-Sky Survey Jones Michael, University of Oxford for the C-BASS collaboration; Caltech, JPL, Manchester University, Rhodes University, Hartebeesthoek Radio Astronomy Observatory, King Abdulaziz City of Science and Technology The C-Band All-Sky Survey (C-BASS) is a project to provide a deep and accurate survey of the whole sky at 5 GHz, and hence measure the synchrotron component of the Galactic foreground. The instrument consists of single-pixel receivers with correlation polarimeters and radiometers, mounted on two 6-m class telescopes, one at Owens Valley Radio Observatory in California and one at the MeerKAT site in South Africa. The final survey will have a resolution of 0.8 degrees and a sensitivity of better than 0.1 mK over the whole sky. I will report on the project status, including preliminary data from the northern telescope and prospects for improved component separation using Planck and C-BASS data.

Adaptive Langevin Sampler for Bayesian Separation of Cosmological Components Kuruoglu Ercan E., ISTI-CNR and Koray Kayabol, Diego Herranz, Bulent Sankur, Emanuele Salerno, Jose-Luis Sanz; IFCA-Santander Spain, Bogazici University We address the cosmological component separation problem in a full Bayesian framework utilising state of the art sampling methods. In contrast to previous work, we consider the sources as images, i.e. 2D signals rather than 1D signals and hence incorporate local structural information utilising Markov random fields (MRFs). Instead of classical random walks in the context of Markov chain Monte Carlo sampling, we employ Langevin sampling which simulates Brownian motion and provides a more intelligent and economic random walk which gives a computational gain of two orders of magnitude over classical MCMC algorithms. We provide results on simulated Planck data and simulations on WMAP are in progress. The method provides means for error analysis seamlessly and the framework allows one to incorporate any prior information available. The technique can also provide partial results on partial data which can be used as initial points for further analysis as new data is available. Simulation results on synthetic data compared to existing methods demonstrate the success of the method.

Removal of foregrounds from the WMAP 7yr polarization maps using a MLP neural network Norgaard-Nielsen Hans Ulrik, DTU Space In a series af papers (Norgaard ñ Nielsen and Jorgensen (2008), Norgaard ñ Nielsen and Hebert (2009) and Norgaard ñ Nielsen (2010)), it has been demonstrated that a simple neural network can extract the CMB temperature signal from mm/submm observations (both for simulated Planck data and observed WMAP data) to a high accuracy and with very small systematic errors. Here the results of an analysis of the WMAP 7yr polarization data will be presented. It will be shown that the neural network method provides CMB Q and U maps with small systematic errors. The improvement of the polarization power spectra are about 25 per cent compared to the power spectra obtained by the WMAP team. 14 Polarized Components separation methodology and results

PLANCK Component Separation using a Sparsity Prior Starck Jean-Luc, CEA, SAP and Jerome Bobin and Florent Sureau; CEA We briefly review the concept of sparsity, and explain why such a sky modeling could be useful for the PLANCK component separation. We present the GMCA method, which has been designed for PLANCK. GMCA seeks for the sparsest solution in the wavelet domain which is compatible with the data. Finally, we will show results on WMAP7 data and PLANCK simulations.

CMB, SZ effect, and ISM foregrounds separation with extended ILC approaches Remazeilles Mathieu, APC and Jacques Delabrouille, Jean-Francois Cardoso; The "Internal Linear Combination" (ILC) component separation method has been extensively used on the data of the WMAP space mission, to extract a single component, the cosmic microwave background (CMB), from the WMAP multifrequency data. We extend the ILC approach for reconstructing millimetre astrophysical emissions beyond the CMB alone. In particular, we construct a 'constrained ILC' filter to extract maps of both the CMB and the thermal SunyaevñZeldovich (SZ) effect, with vanishing contamination from the other. We also develop a 'multidimensional ILC' filter, which can be used, for instance, to estimate the diffuse emission of a complex component originating from multiple correlated emissions, such as the total emission of the Galactic interstellar medium (ISM). The performance of these generalised ILC methods is tested on simulations of Planck mission observations, for which we successfully reconstruct independent estimates of the CMB, of the thermal SZ, and of emissions from other foregrounds.

The QUIJOTE-CMB Experiment Rubino-Martin Jose Alberto, Instituto Astrofisica Canarias and The QUIJOTE Collaboration; IAC I will review the current status of the QUIJOTE (Q-U-I JOint Tenerife) CMB Experiment, a new experiment that will operate at the Teide Observatory with the aim of characterizing the polarization of the CMB and other processes of galactic and extragalactic emission in the frequency range of 10-40 GHz and at large angular scales. The first of the two QUIJOTE telescopes and the first instrument will start operations soon at the Teide Observatory. QUIJOTE will be a valuable complement at low frequencies for the PLANCK mission, and will have the required sensitivity to detect a primordial gravitational-wave component if the tensor-to-scalar ratio is larger than r=0.05.

(Poster 19) Detection of extragalactic point sources in 7 year WMAP data by using a multifrequency method. Lanz Luis Fernando, Instituto de FÌsica de Cantabria (CSIC-UC) and Diego Herranz, Marcos Lopez-Caniego, Joaquin Gonzalez-Nuevo, Marcella Massardi; Instituto de Fisica de Cantabria (CSIC-UC), Instituto de Fisica de Cantabria (CSIC-UC), SISSA, Osservatorio Astronomico di Padova (INAF) In this work we deal with the problem of multifrequency detection of extragalactic point sources in 7yr-WMAP data. We have used a linear multifrequency filtering technique that takes into account simultaneously the spatial and frequency behaviour of the sources (but without making any a priori assumption about their spectral indices) and, on the other hand, the cross-power spectrum of the background. This combined approach allows us to significantly improve the detectability of extragalactic point sources. Additionally, we are able to recover the fluxes and spectral indices of the sources with better precision than in previous works. By applying our method to the V and W bands of WMAP we are able to obtain 145 clear 5 sigma detections at 94 GHz.

(Poster 20) WMAP data and unconventional cosmologies Gonzalez-Mestres Luis, B.P. 110 The recent claim by Gurzadyan et al. that the cosmological sky is a weakly random one where "the random perturbation is a minor component of mostly regular signal", if confirmed, would have strong implications for unconventional cosmologies. We discuss prospects for approaches based on Lorentz symmetry violation generated beyond Planck scale and on the superbradyon hypothesis. Besides standard relativity, possible violations of other fundamental principles can be considered.

(Poster 21) Simple map cleaning algorithm for B-mode detection at low multipoles Katayama Nobuhiko, High Energy Accelerator Research Organization (KEK and E. Komatsu; Univ. of Texas at Austin We use a simple map cleaning algorithm to estimate B-mode detection limits at low multipoles for a future CMB satellite experiment. In an ultimate low noise space experiment, the Galactic foregrounds limit the measurement 15 of tensor-scalar ratio ($r$). A simple extension to the internal linear combination technique is proposed to lower the offset caused by the E-mode polarization and the foregrounds. We implement and test a pixel based likelihood function maximization for $r$ detection using the simulated three band data with dust and synchrotron models. We observe an offset of $r\sim0.002$ which limits the measurement of $r$ to $\sim 0.01$ with this method.

(Poster 22) Total foreground maps from Planck by Wiener filtering in the needlet domain. Le Jeune Maude, APC and Cardoso, Jean-Francois; LTCI CNRS We present work on separating the Planck data into three contributions: CMB, foregrounds and noise. Two key features are the use of a flexible non parametric model of the foreground correlation structure and the use of needlets (spherical wavelet) to capture the correlations not only across channels but also across the sky and across multipoles. The underlying model is fitted by maximum likelihood using the SMICA framework. From the resulting fit, one then builds the Wiener filters yielding components with minimum mean square error. In particular we obtain maps of the total foreground emission at each Planck frequency with minimum contamination by CMB and noise. The approach is validated through realistic simulations based on the Planck Sky Model. Those simulations provide guidance for selecting the needlet localisation strategy offering the best separation performance. Finally, we present our best foreground estimates in all Planck channels.

(Poster 23) CBass: The C-Band All Sky Survey Irfan Melis, JBCA, University of Manchester and ; Caltech, Oxford University, HartRAO, KAUST CBASS, the C-Band All Sky Survey, is currently conducting a 5GHz survey of the sky in total intensity and polarization. The resulting polarization map will be a vital tool in the removal of foreground emission from current and next-generation CMB polarization experiments. The survey of the northern hemisphere is currently underway with a telescope situated at OVRO, with commissioning of the southern telescope scheduled for August 2010 in South Africa. Upon completion, the CBASS map will provide a polarized template of Galactic synchrotron emission that is weakly affected by Faraday rotation. Not only will the maps provide polarised foreground measurements for component separation techniques; they shall also probe into the physics of the Galactic interstellar medium. In this era of in-depth exploration of B-modes, gravitational waves and non- Gaussianity, CBass will provide the low frequency foreground maps, necessary to accurately separate polarised foregrounds from measurements of the polarised the CMB. Operations are underway at OVRO, and the first galactic maps of the northern hemisphere are forthcoming. Construction of the second receiver has begun. We present an overview of the telescope setup, its calibration and a display of its mapping capability. We also present a status. This will set the scene for the upcoming release of the northern CBASS maps.

(Poster 24) Component separation for a future CMB polarization space mission Basak Soumen, Laboratoire AstroParticule et Cosmologie (APC) and Jacques Delabrouille; The search and discovery of primordial B modes of Cosmic Microwave Background (CMB) polarization provide a unique window for exploring new physics near the Planck scale. COrE is a medium-class space mission proposed to detect with high significance such polarization signals, which are thought to be generated by the primordial gravity waves, as predicted by many classes of inflationary models of cosmology. The broad frequency coverage proposed for COrE allows the application of highly effective component separation methods at the proper level of sensitivity. We present the estimation of the angular power spectrum of B-modes from COrE-like multi-frequency simulated data. The method used is an implementation of an internal linear combination(ILC) of the COrE channels with minimum error variance on a frame of spherical wavelets called needlets, allowing localized filtering in both pixel space and harmonic space. We have obtained a very low foreground B-mode angular power spectrum, which makes possible the determination of tensor to scalar perturbations at a sensitivity better than T/S=0.001.