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We probe star formation in the environments of massive (~1013M⊙) dark matter haloes at redshifts of z ~ 1. This star formation is linked to a submillimetre clustering signal which we detect in maps of the Planck High Frequency Instrument that are stacked at the positions of a sample of high redshift (z > 2) strongly lensed dusty star-forming galaxies (DSFGs) selected from the South Pole Telescope (SPT) 2500 deg² survey. The clustering signal has submillimetre colours which are consistent with the mean redshift of the foreground lensing haloes (z ~ 1).We report a mean excess of star formation rate (SFR) compared to the field, of (2700 ± 700)M⊙ yr-1 from all galaxies contributing to this clustering signal within a radius of 3.5 arcmin from the SPT DSFGs. The magnitude of the Planck excess is in broad agreement with predictions of a current model of the cosmic infrared background. The model predicts that 80 per cent of the excess emission measured by Planck originates from galaxies lying in the neighbouring haloes of the lensing halo. Using Herschel maps of the same fields, we find a clear excess, relative to the field, of individual sources which contribute to the Planck excess. The mean excess SFR compared to the field is measured to be (370 ± 40)M⊙ yr-1 per resolved, clustered source. Our findings suggest that the environments around these massive z ~ 1 lensing haloes host intense star formation out to about 2 Mpc. The flux enhancement due to clustering should also be considered when measuring flux densities of galaxies in Planck data. [ABSTRACT FROM AUTHOR]

We present an analysis of CO spectroscopy and infrared-to-millimetre dust photometry of 11 exceptionally bright far-infrared (FIR) and sub-mm sources discovered through a combination of the Planck all-sky survey and follow-up Herschel-SPIRE imaging - ''Planck's Dusty Gravitationally Enhanced subMillimetre Sources''. Each source has a secure spectroscopic redshift z = 2.2-3.6 from multiple lines obtained through a blind redshift search with EMIR at the IRAM 30-m telescope. Interferometry was obtained at IRAM and the SMA, and along with optical/near-infrared imaging obtained at the CFHT and the VLT reveal morphologies consistent with strongly gravitationally lensed sources, including several giant arcs. Additional photometry was obtained with JCMT/SCUBA-2 and IRAM/GISMO at 850 yum and 2 mm, respectively. The SEDs of our sources peak near either the 350 yum or 500 yum bands of SPIRE with peak flux densities between 0.35 and 1.14 Jy. All objects are extremely bright isolated point sources in the 18" beam of SPIRE at 250 yum, with apparent FIR luminosities of up to 3 x 1014 Lq (not correcting for the lensing effect). Their morphologies, sizes, CO line widths, CO luminosities, dust temperatures, and FIR luminosities provide additional empirical evidence that these are amongst the brightest strongly gravitationally lensed high-redshift galaxies on the sub-mm sky. Our programme extends the successful wide-area searches for strongly gravitationally lensed high-redshift galaxies (carried out with the South Pole Telescope and Herschel) towards even brighter sources, which are so rare that their systematic identification requires a genuine all-sky survey like Planck. Six sources are above the ^600 mJy 90% completeness limit of the Planck catalogue of compact sources (PCCS) at 545 and 857 GHz, which implies that these must literally be amongst the brightest high-redshift FIR and sub-mm sources on the extragalactic sky. We discuss their dust masses and temperatures, and use additional WISE 22-yum photometry and template fitting to rule out a significant contribution of AGN heating to the total infrared luminosity. Six sources are detected in FIRST at 1.4 GHz, and the others have sensitive upper limits. Four have flux densities brighter than expected from the local FIR-radio correlation, but in the range previously found for high-z sub-mm galaxies, one has a deficit of FIR emission, and 6 are consistent with the local correlation, although this includes 3 galaxies with upper limits. We attribute this to the turbulent interstellar medium of these galaxies, rather than the presence of radio AGN. The global dust-to-gas ratios and star-formation efficiencies of our sources are predominantly in the range expected from massive, metal-rich, intense, high-redshift starbursts. An extensive multi-wavelength follow-up programme is being carried out to further characterize these sources and the intense star formation within them. [ABSTRACT FROM AUTHOR]

The European Space Agency's Planck satellite, dedicated to studying the early Universe and its subsequent evolution, was launched 14 May 2009 and has been scanning the microwave and submillimetre sky continuously since 12 August 2009. In March 2013, ESA and the Planck Collaboration released the initial cosmology products based on the first 15.5 months of Planck data, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the mission and its performance, the processing, analysis, and characteristics of the data, the scientific results, and the science data products and papers in the release. The science products include maps of the cosmic microwave background (CMB) and diffuse extragalactic foregrounds, a catalogue of compact Galactic and extragalactic sources, and a list of sources detected through the Sunyaev-Zeldovich effect. The likelihood code used to assess cosmological models against the Planck data and a lensing likelihood are described. Scientific results include robust support for the standard six-parameter ΛCDM model of cosmology and improved measurements of its parameters, including a highly significant deviation from scale invariance of the primordial power spectrum. The Planck values for these parameters and others derived from them are significantly different from those previously determined. Several large-scale anomalies in the temperature distribution of the CMB, first detected by WMAP, are confirmed with higher confidence. Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at greater than 25σ. Planck finds no evidence for non-Gaussianity in the CMB. Planck's results agree well with results from the measurements of baryon acoustic oscillations. Planck finds a lower Hubble constant than found in some more local measures. Some tension is also present between the amplitude of matter fluctuations (σ8) derived from CMB data and that derived from Sunyaev-Zeldovich data. The Planck and WMAP power spectra are offset from each other by an average level of about 2% around the first acoustic peak. Analysis of Planck polarization data is not yet mature, therefore polarization results are not released, although the robust detection of E-mode polarization around CMB hot and cold spots is shown graphically. [ABSTRACT FROM AUTHOR]

We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 100 to 857 GHz frequency channel maps from the Planck survey. This map shows an obvious galaxy cluster tSZ signal that is well matched with blindly detected clusters in the Planck SZ catalogue. To characterize the signal in the tSZ map we have computed its angular power spectrum. At large angular scales (ࡁ < 60), the major foreground contaminant is the diffuse thermal dust emission. At small angular scales (ࡁ > 500) the clustered cosmic infrared background and residual point sources are the major contaminants. These foregrounds are carefully modelled and subtracted. We thus measure the tSZ power spectrum over angular scales 0.17° ≲ θ ≲ 3.0° that were previously unexplored. The measured tSZ power spectrum is consistent with that expected from the Planck catalogue of SZ sources, with clear evidence of additional signal from unresolved clusters and, potentially, diffuse warm baryons. Marginalized band-powers of the Planck tSZ power spectrum and the best-fit model are given. The non-Gaussianity of the Compton parameter map is further characterized by computing its 1D probability distribution function and its bispectrum. The measured tSZ power spectrum and high order statistics are used to place constraints on σ8. [ABSTRACT FROM AUTHOR]

We describe the all-sky Planck catalogue of clusters and cluster candidates derived from Sunyaev-Zeldovich (SZ) effect detections using the first 15.5 months of Planck satellite observations. The catalogue contains 1227 entries, making it over six times the size of the Planck Early SZ (ESZ) sample and the largest SZ-selected catalogue to date. It contains 861 confirmed clusters, of which 178 have been confirmed as clusters, mostly through follow-up observations, and a further 683 are previously-known clusters. The remaining 366 have the status of cluster candidates, and we divide them into three classes according to the quality of evidence that they are likely to be true clusters. The Planck SZ catalogue is the deepest all-sky cluster catalogue, with redshifts up to about one, and spans the broadest cluster mass range from (0.1 to 1.6) × 1015 M☉. Confirmation of cluster candidates through comparison with existing surveys or cluster catalogues is extensively described, as is the statistical characterization of the catalogue in terms of completeness and statistical reliability. The outputs of the validation process are provided as additional information. This gives, in particular, an ensemble of 813 cluster redshifts, and for all these Planck clusters we also include a mass estimated from a newly-proposed SZ-mass proxy. A refined measure of the SZ Compton parameter for the clusters with X-ray counter-parts is provided, as is an X-ray flux for all the Planck clusters not previously detected in X-ray surveys. [ABSTRACT FROM AUTHOR]

We present constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude Ω8 and matter density parameter Ωm in a flat ΛCDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that Ω8 = 0:75 ± 0:03, Ωm = 0:29 ± 0:02, and Ω8 (Ωm/0:27) 0:3 = 0:764 ± 0:025. The value of Ω8 is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find Ω8(Ωm/0:27) 0:3 = 0:78 ± 0:01 and a tighter one-dimensional range Ω8 = 0:77 ± 0:02. We find that the larger values of Ω8 and Ωm preferred by Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the ACDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make further progress in this field. [ABSTRACT FROM AUTHOR]

With its unprecedented ability to scrutinise the sub-millimetre (sub-mm) to centimetre full sky, the Planck satellite is uniquely suited to search for the progenitors of clusters of galaxies. The forming massive halos at z ≳1-2 are expected to host massive galaxies with high star formation rates. Clustered in the growing potential well that is being established, these galaxies are within Planck 's reach via their sub-mm emission. We have applied a new colour-based method combining Planck and IRAS data to detect the rarest and brightest sub-mm cold sources on the sky. In this work, we describe the method and present the first confirmations of our high- z candidates, particularly focusing on 17p732, a newly discovered high- z (proto)cluster candidate at z ⋍ 1.7 for which we carried a multi-wavelength follow-up. (© 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) [ABSTRACT FROM AUTHOR]

We study the thermal (tSZ) and kinetic Sunyaev–Zel'dovich (kSZ) effect associated with superclusters of galaxies using the MareNostrum (MNU) universe smoothed particle hydrodynamics (SPH) simulation. In particular, we consider superclusters with characteristics (total mass, overdensity and number density of cluster members) similar to those of the Corona Borealis Supercluster (CrB-SC). This paper has been motivated by the detection at 33 GHz of a strong temperature decrement in the cosmic microwave background towards the core of this supercluster (Génova-Santos et al.). Multifrequency observations with Very Small Array (VSA) and Millimetre & Infrared Testa Grigia Observatory (MITO) suggest the existence of a tSZ effect component in the spectrum of this cold spot, with a Comptonization parameter value of (Battistelli et al.), which would account for roughly 25 per cent of the total observed decrement. From the SPH simulation, we identify nine regions containing superclusters similar to CrB-SC, obtain the associated SZ maps and calculate the probability of finding such SZ signals arising from hot gas within the supercluster. Our results show that the warm/hot intergalactic medium (WHIM) lying in the intercluster regions within the supercluster produces a tSZ effect much smaller than the observed value by MITO/VSA. Neither can, summing the contribution of small clusters and galaxy groups in the region, explain the amplitude of the SZ signal. Our synthetic maps show peak y-values significantly below the observations. Less than 0.3 per cent are compatible at the lower end of the 1σ level, even when considering privileged orientations in which the filamentary structures are aligned along the line of sight (LOS). When we take into account the actual posterior distribution from the observations, the probability that WHIM can cause a tSZ signal like the one observed in the CrB-SC is <1 per cent, rising up to a 3.2 per cent when the contribution of small clusters and galaxy groups is included. If the simulations provide a suitable description of the gas physics, then we must conclude that the tSZ component of the CrB spot most probably arises from an unknown galaxy cluster along the LOS. On the other hand, the simulations also show that the kSZ signal associated with the supercluster cannot provide an explanation for the remaining 75 per cent of the observed cold spot in CrB. [ABSTRACT FROM AUTHOR]

Poster: Clinical track: Sarcoma PO-1233: Perioperative Radiotherapy with a Moderate Dose-Escalation for Retroperitoneal Sarcoma (RPS). M. Nuñez Baez, A. Montero, X. Chen-Zhao, A. Acosta, B. Alvarez, J. Palma, M. Lopez-Gonzalez, E. Sanchez, O. Hernando, J. Valero, R. Ciervide, M. Garcia-Aranda, R. Alonso, M. De la Casa, D. Zucca, J. MartÃ-, I. Flores-Cacho, C. Ruiz-Morales, P. Fernandez-Leton, M. Rubio Rodriguez. [Extracted from the article]