The aim of this paper is to study the inner Galaxy where the four emission components at radio and millimetre wavelengths peak in a narrow latitude band. Intermediate Science Results Between the initial release of results in January 2011, and the release of the first full-sky maps planned for early 2013, the Planck Collaboration has produced a number of intermediate science results. Planck intermediate results. There are 600 complete signal, noise and systematics simulations of the full-frequency and detector-set maps. The majority of the planet ﬂux density ... Planck, and the two gas giants outshine any PCCS2 object by at We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5 < S/N < 5.3 in the same 10-month survey maps used in the construction of the Early SZ sample. Reduction of large-scale systematic effects in HFI polarization maps and estimation of the reionization optical depth journal , … The characterisation of the physical properties of the three components has allowed us to build a template model to extract the total SZ signal of this system with Planck data. These results clarify a recurrent disparity in the -ray versus dust calibration of X CO, but they Early astrophysics results are given in Planck Collaboration VIII{XXVI 2011, based on data taken be-tween 13 August 2009 and 7 June 2010. cosmology. Large-scale Galactic magnetic ﬁelds Planck Collaboration: ... Planck data The results presented in this paper are based on the 2015 data release2 described in Planck Collaboration I (2016), Planck Collaboration II (2016), and Planck Collaboration Planck measurements have shown that galaxy clusters come in all sorts of shapes and sizes, and discovered the first ever seen triple-system of galaxy clusters. ... which are consistent with the kSZ evidence found in individual Planck raw frequency maps, although lower than found in the WMAP-9yr W band ($3.3\sigma$). The Planck mission results are presented inPlanck Collaboration I(2014) and the in-ﬂight performance of the two focal plane instruments, the HFI (High Frequency We present the results from a deep XMM-Newton re-observation of PLCKG214.6+37.0, part of a multi-wavelength programme to investigate Planck discovered superclusters. These results primarily involve the investigation of diffuse emission from our own Galaxy, and the study of other galaxies and clusters of galaxies. Intermediate results are presented in a series of papers based on Planck data. Fainter CO cannot account for the brightness of the excesses seen othe Galactic plane (Planck Collaboration XIX2011). E- and B-modes of dust polarization from the magnetized ﬁlamentary structure of the interstellar medium Planck Collaboration: P. A. R. Ade81, N. Aghanim55, M. Arnaud69, M. Ashdown66;5, J. Aumont55, C. Baccigalupi80, A. J. Banday89;9, Detection of velocity dispersion ... Planck Collaboration Int. Planck intermediate results. LIII. Proﬁle likelihoods for cosmological parameters ... demonstrating the robustness of the Planck results to the statistical methodology. Planck intermediate results. A&A 550, A128 (2013) DOI: 10.1051/0004-6361/201219361 c ESO 2013 Astronomy & Astrophysics Planck intermediate results II. From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H 0 = (67.8 ± 0.9) km s -1 Mpc -1, a matter density parameter Ω m = 0.308 ± 0.012, and a tilted scalar spectral index with n s = 0.968 ± 0.006, consistent with the 2013 analysis. These data consist of a set of maps of the Stokes Q After modelling and subtracting the tSZ effect and X-ray emission for each cluster in the pair, we studied the residuals on both the SZ and X-ray maps. Reduction of large-scale systematic effects in HFI polarization maps and estimation of the reionization optical depth Planck Collaboration: N. Aghanim53, M. Ashdown63;6, J. Aumont53, C. Baccigalupi75, M. Ballardini29;45;48, A. J. Banday85;9, R. B. Barreiro58, XLII. By combining the Planck data with observations from NASA’s WMAP satellite astronomers suspect that the haze is due to emission from unusually high energy electrons moving through the Galaxy’s magnetic field. Probably the most important high-level result from the Planck satellite1 (Planck Collaboration I2016) is the good agreement Further validation of new Planck clusters with XMM-Newton … Astrophysical Observatory, Astrophysics - Cosmology and Nongalactic Astrophysics. Evidence of unbound gas from the kinetic Sunyaev-Zeldovich effect. Structure of the Galactic magnetic field from dust polarization maps of the southern Galactic cap Structure of the Galactic magnetic field from dust polarization maps of the southern Galactic cap Notice, Smithsonian Terms of Planck intermediate results XLVI. Agreement NNX16AC86A, Is ADS down? The papers are available online, and links to each are provided below. Comparison of Sunyaev-Zeldovich measurements from Planck For component-separation purposes, important improvements include: maps that retain the CMB Solar dipole, allowing for high-precision relative calibration in higher-level analyses; well-defined single-detector maps, allowing for robust CO extraction; and HFI temperature maps between 217 and 857 GHz that are binned into 0'.9 pixels (Nside = 4096), ensuring that the full angular information in the data is represented in the maps even at the highest Planck resolutions. The haze is a distinct but mysterious component of diffuse Galactic emission, the origin of which is unknown. Planck released the Early Release Compact Source Catalogue in January 2011; further investigation has examined the sources that are brightest at higher frequencies (above 100GHz) The sources have been classified into galaxies dominated by thermal emission from dust, and those dominated by synchrotron emission from electrons in magnetic fields. Relevant properties of Planck are summarized for each We present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LF As a Planck first, these simulations include full time-domain processing of the beam-convolved CMB anisotropies. We present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. @article{Aghanim2016PlanckIR, title={Planck intermediate results - XXXIV. Planck intermediate results XLVII. Results using Planck and XMM-Newton measurements have shown that galaxy clusters come in all sorts of shapes and sizes, and that common assumptions may not be valid. Constraints on peculiar velocities XXXIII. (or is it just me...), Smithsonian Privacy If you use any of these results for presentations, please acknowledge the corresponding paper, ESA/Planck, and the Planck Collaboration. In the past the components have The release of NPIPE maps and simulations is accompanied with a complete suite of raw and processed time-ordered data and the software, scripts, auxiliary data, and parameter files needed to improve further on the analysis and to run matching simulations. We introduce results from the Wendelstein Weak Lensing (WWL) pathfinder project, in which we have observed three intermediate-redshift Planck clusters of galaxies with the new 30 arcmin × 30 arcmin wide field imager at the 2 m Fraunhofer Telescope at Wendelstein Observatory. As-Trophysics results are being presented in a number of scientific papers planck intermediate results here here for detailed. Nine Planck frequencies for cosmological parameters... demonstrating the robustness of the Planck maps of planets. 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