318 results found
Collaboration P, Adam R, Ade PAR, et al., 2016, Planck 2015 results. VII. HFI TOI and beam processing, A, Vol: 594
The Planck High Frequency Instrument (HFI) has observed the full sky at sixfrequencies (100, 143, 217, 353, 545, and 857 GHz) in intensity and at fourfrequencies in linear polarization (100, 143, 217, and 353 GHz). In order toobtain sky maps, the time-ordered information (TOI) containing the detector andpointing samples must be processed and the angular response must be assessed.The full mission TOI is included in the Planck 2015 release. This paperdescribes the HFI TOI and beam processing for the 2015 release. HFI calibrationand map-making are described in a companion paper. The main pipeline has beenmodified since the last release (2013 nominal mission in intensity only), byincluding a correction for the non-linearity of the warm readout and byimproving the model of the bolometer time response. The beam processing is anessential tool that derives the angular response used in all the Planck sciencepapers and we report an improvement in the effective beam window functionuncertainty of more than a factor 10 relative to the 2013 release. Noisecorrelations introduced by pipeline filtering function are assessed usingdedicated simulations. Angular cross-power spectra using datasets that aredecorrelated in time are immune to the main systematic effects.
Collaboration P, Ade PAR, Aghanim N, et al., 2016, Planck 2015 results. XXVI. The Second Planck Catalogue of Compact Sources, Astronomy & Astrophysics, Vol: 594, ISSN: 1432-0746
The Second Planck Catalogue of Compact Sources is a catalogue of sourcesdetected in single-frequency maps from the full duration of the Planck missionand supersedes previous versions of the Planck compact source catalogues. Itconsists of compact sources, both Galactic and extragalactic, detected over theentire sky. Compact sources detected in the lower frequency channels areassigned to the PCCS2, while at higher frequencies they are assigned to one oftwo sub-catalogues, the PCCS2 or PCCS2E, depending on their location on thesky. The first of these catalogues covers most of the sky and allows the userto produce subsamples at higher reliabilities than the target 80% integralreliability of the catalogue. The PCCS2E contains sources detected in skyregions where the diffuse emission makes it difficult to quantify thereliability of the detections. Both the PCCS2 and PCCS2E include polarizationmeasurements, in the form of polarized flux densities, or upper limits, andorientation angles for all seven polarization-sensitive Planck channels. Theimproved data-processing of the full-mission maps and their reduced noiselevels allow us to increase the number of objects in the catalogue, improvingits completeness for the target 80 % reliability as compared with the previousversions, the PCCS and ERCSC catalogues.
Collaboration P, Ade PAR, Aghanim N, et al., 2016, Planck 2015 results. XXVII. The Second Planck Catalogue of Sunyaev-Zeldovich Sources, Astronomy & Astrophysics, Vol: 594, ISSN: 0004-6361
We present the all-sky Planck catalogue of Sunyaev-Zeldovich (SZ) sourcesdetected from the 29 month full-mission data. The catalogue (PSZ2) is thelargest SZ-selected sample of galaxy clusters yet produced and the deepestall-sky catalogue of galaxy clusters. It contains 1653 detections, of which1203 are confirmed clusters with identified counterparts in external data-sets,and is the first SZ-selected cluster survey containing > $10^3$ confirmedclusters. We present a detailed analysis of the survey selection function interms of its completeness and statistical reliability, placing a lower limit of83% on the purity. Using simulations, we find that the Y5R500 estimates arerobust to pressure-profile variation and beam systematics, but accurateconversion to Y500 requires. the use of prior information on the clusterextent. We describe the multi-wavelength search for counterparts in ancillarydata, which makes use of radio, microwave, infra-red, optical and X-raydata-sets, and which places emphasis on the robustness of the counterpartmatch. We discuss the physical properties of the new sample and identify apopulation of low-redshift X-ray under- luminous clusters revealed by SZselection. These objects appear in optical and SZ surveys with consistentproperties for their mass, but are almost absent from ROSAT X-ray selectedsamples.
Collaboration P, Ade PAR, Aghanim N, et al., 2016, Planck 2015 results. XIII. Cosmological parameters, A, Vol: 594
We present results based on full-mission Planck observations of temperatureand polarization anisotropies of the CMB. These data are consistent with thesix-parameter inflationary LCDM cosmology. From the Planck temperature andlensing data, for this cosmology we find a Hubble constant, H0= (67.8 +/- 0.9)km/s/Mpc, a matter density parameter Omega_m = 0.308 +/- 0.012 and a scalarspectral index with n_s = 0.968 +/- 0.006. (We quote 68% errors on measuredparameters and 95% limits on other parameters.) Combined with Plancktemperature and lensing data, Planck LFI polarization measurements lead to areionization optical depth of tau = 0.066 +/- 0.016. Combining Planck withother astrophysical data we find N_ eff = 3.15 +/- 0.23 for the effectivenumber of relativistic degrees of freedom and the sum of neutrino masses isconstrained to < 0.23 eV. Spatial curvature is found to be |Omega_K| < 0.005.For LCDM we find a limit on the tensor-to-scalar ratio of r <0.11 consistentwith the B-mode constraints from an analysis of BICEP2, Keck Array, and Planck(BKP) data. Adding the BKP data leads to a tighter constraint of r < 0.09. Wefind no evidence for isocurvature perturbations or cosmic defects. The equationof state of dark energy is constrained to w = -1.006 +/- 0.045. Standard bigbang nucleosynthesis predictions for the Planck LCDM cosmology are in excellentagreement with observations. We investigate annihilating dark matter anddeviations from standard recombination, finding no evidence for new physics.The Planck results for base LCDM are in agreement with BAO data and with theJLA SNe sample. However the amplitude of the fluctuations is found to be higherthan inferred from rich cluster counts and weak gravitational lensing. Apartfrom these tensions, the base LCDM cosmology provides an excellent descriptionof the Planck CMB observations and many other astrophysical data sets.
Collaboration P, Ade PAR, Aghanim N, et al., 2016, Planck 2015 results. XXVIII. The Planck Catalogue of Galactic Cold Clumps, Astronomy & Astrophysics, Vol: 594, ISSN: 1432-0746
We present the Planck Catalogue of Galactic Cold Clumps (PGCC), an all-skycatalogue of Galactic cold clump candidates detected by Planck. This catalogueis the full version of the Early Cold Core (ECC) catalogue, which was madeavailable in 2011 with the Early Release Compact Source Catalogue (ERCSC) andcontained 915 high S/N sources. It is based on the Planck 48 months missiondata that are currently being released to the astronomical community. The PGCCcatalogue is an observational catalogue consisting exclusively of Galactic coldsources. The three highest Planck bands (857, 545, 353 GHz) have been combinedwith IRAS data at 3 THz to perform a multi-frequency detection of sourcescolder than their local environment. After rejection of possible extragalacticcontaminants, the PGCC catalogue contains 13188 Galactic sources spread acrossthe whole sky, i.e., from the Galactic plane to high latitudes, following thespatial distribution of the main molecular cloud complexes. The mediantemperature of PGCC sources lies between 13 and 14.5 K, depending on thequality of the flux density measurements, with a temperature ranging from 5.8to 20 K after removing sources with the 1% largest temperature estimates. Usingseven independent methods, reliable distance estimates have been obtained for5574 sources, which allows us to derive their physical properties such as theirmass, physical size, mean density and luminosity. The PGCC sources are locatedmainly in the solar neighbourhood, up to a distance of 10.5 kpc towards theGalactic centre, and range from low-mass cores to large molecular clouds.Because of this diversity and because the PGCC catalogue contains sources invery different environments, the catalogue is useful to investigate theevolution from molecular clouds to cores. Finally, the catalogue also includes54 additional sources located in the SMC and LMC.
Errard J, Feeney SM, Peiris HV, et al., 2016, Robust forecasts on fundamental physics from the foreground-obscured, gravitationally-lensed CMB polarization, JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, ISSN: 1475-7516
Inoue Y, Ade P, Akiba Y, et al., 2016, POLARBEAR-2: An instrument for CMB polarization measurements, ISSN: 0277-786X
© 2016 SPIE. POLARBEAR-2 (PB-2) is a cosmic microwave background (CMB) polarization experiment that will be located in the Atacama highland in Chile at an altitude of 5200 m. Its science goals are to measure the CMB polarization signals originating from both primordial gravitational waves and weak lensing. PB-2 is designed to measure the tensor to scalar ratio, r, with precision σ(r) > 0:01, and the sum of neutrino masses, Σmz, with σ(Σmv) < 90 meV. To achieve these goals, PB-2 will employ 7588 transition-edge sensor bolometers at 95 GHz and 150 GHz, which will be operated at the base temperature of 250 mK. Science observations will begin in 2017.
Jaffe A, 2016, Physics: Finding the time, Nature, Vol: 537, ISSN: 0028-0836
© 2016 SPIE. The Simons Array is a next generation cosmic microwave background (CMB) polarization experiment whose science target is a precision measurement of the B-mode polarization pattern produced both by inflation and by gravitational lensing. As a continuation and extension of the successful POLARBEAR experimental program, the Simons Array will consist of three cryogenic receivers each featuring multichroic bolometer arrays mounted onto separate 3.5m telescopes. The first of these, also called POLARBEAR-2A, will be the first to deploy in late 2016 and has a large diameter focal plane consisting of dual-polarization dichroic pixels sensitive at 95 GHz and 150 GHz. The POLARBEAR-2A focal plane will utilize 7,588 antenna-coupled superconducting transition edge sensor (TES) bolometers read out with SQUID amplifiers using frequency domain multiplexing techniques. The next two receivers that will make up the Simons Array will be nearly identical in overall design but will feature extended frequency capability. The combination of high sensitivity, multichroic frequency coverage and large sky area available from our mid-latitude Chilean observatory will allow Simons Array to produce high quality polarization sky maps over a wide range of angular scales and to separate out the CMB B-modes from other astrophysical sources with high fidelity. After accounting for galactic foreground separation, the Simons Array will detect the primordial gravitational wave B-mode signal to r > 0.01 with a significance of > 5σ and will constrain the sum of neutrino masses to 40 meV (1σ) when cross-correlated with galaxy surveys. We present the current status of this funded experiment, its future, and discuss its projected science return.
ADE PAR, AKIBA Y, ANTHONY AE, et al., 2015, A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND B-MODE POLARIZATION WITH POLARBEAR, Publications of The Korean Astronomical Society, Vol: 30, Pages: 625-628, ISSN: 1225-1534
Ade PAR, Aghanim N, Ahmed Z, et al., 2015, Joint Analysis of BICEP2/Keck Array and Planck Data, Physical Review Letters, Vol: 114, ISSN: 1079-7114
Ade PAR, Aghanim N, Alina D, et al., 2015, Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence, ASTRONOMY & ASTROPHYSICS, Vol: 576, ISSN: 1432-0746
Ade PAR, Aghanim N, Alina D, et al., 2015, Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust, ASTRONOMY & ASTROPHYSICS, Vol: 576, ISSN: 1432-0746
Ade PAR, Aghanim N, Alina D, et al., 2015, Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible, ASTRONOMY & ASTROPHYSICS, Vol: 576, ISSN: 1432-0746
Ade PAR, Aghanim N, Alves MIR, et al., 2015, Planck intermediate results XXIII. Galactic plane emission components derived from Planck with ancillary data, ASTRONOMY & ASTROPHYSICS, Vol: 580, ISSN: 1432-0746
Ade PAR, Aghanim N, Aniano G, et al., 2015, Planck intermediate results XXVIII. Interstellar gas and dust in the Chamaeleon clouds as seen by Fermi LAT and Planck, ASTRONOMY & ASTROPHYSICS, Vol: 582, ISSN: 1432-0746
Ade PAR, Aghanim N, Armitage-Caplan C, et al., 2015, Planck 2013 results. XXXII. The updated Planck catalogue of Sunyaev-Zeldovich sources, ASTRONOMY & ASTROPHYSICS, Vol: 581, ISSN: 1432-0746
Ade PAR, Aghanim N, Arnaud M, et al., 2015, Planck intermediate results. XXVI. Optical identification and redshifts of Planck clusters with the RTT150 telescope, ASTRONOMY & ASTROPHYSICS, Vol: 582, ISSN: 1432-0746
Ade PAR, Aghanim N, Arnaud M, et al., 2015, Planck intermediate results XXV. The Andromeda galaxy as seen by Planck, ASTRONOMY & ASTROPHYSICS, Vol: 582, ISSN: 1432-0746
Ade PAR, Aghanim N, Arnaud M, et al., 2015, Planck intermediate results XXIV. Constraints on variations in fundamental constants, ASTRONOMY & ASTROPHYSICS, Vol: 580, ISSN: 1432-0746
Ade PAR, Alves MIR, Aniano G, et al., 2015, Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization, ASTRONOMY & ASTROPHYSICS, Vol: 576, ISSN: 1432-0746
Ade PAR, Arnold K, Atlas M, et al., 2015, POLARBEAR constraints on cosmic birefringence and primordial magnetic fields, PHYSICAL REVIEW D, Vol: 92, ISSN: 2470-0010
Aghanim N, Altieri B, Arnaud M, et al., 2015, Planck intermediate results XXVII. High-redshift infrared galaxy overdensity candidates and lensed sources discovered by Planck and confirmed by Herschel-SPIRE, ASTRONOMY & ASTROPHYSICS, Vol: 582, ISSN: 1432-0746
Errard J, Ade PAR, Akiba Y, et al., 2015, MODELING ATMOSPHERIC EMISSION FOR CMB GROUND-BASED OBSERVATIONS, ASTROPHYSICAL JOURNAL, Vol: 809, ISSN: 0004-637X
Jaffe AH, 2015, Concluding Remarks from a Cosmologist, Proceedings of the International Astronomical Union, Vol: 10, Pages: 407-411, ISSN: 1743-9213
© International Astronomical Union 2015. I conclude the SCCC21 conference highlighting some of the contrasts we heard about, some specific topics (the statistics of random fields), and discuss how some of these play out in the analysis of cosmic microwave background data. I conclude with a hopeful look at the efficacy of blind analyses in the CMB and elsewhere in cosmology.
Paykari P, Pires S, Starck J-L, et al., 2015, Sparsely sampling the sky: Regular vs. random sampling, ASTRONOMY & ASTROPHYSICS, Vol: 581, ISSN: 1432-0746
Abergel A, Ade PAR, Aghanim N, et al., 2014, Planck 2013 results. XI. All-sky model of thermal dust emission, ASTRONOMY & ASTROPHYSICS, Vol: 571, ISSN: 1432-0746
Abergel A, Ade PAR, Aghanim N, et al., 2014, Planck intermediate results XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies, ASTRONOMY & ASTROPHYSICS, Vol: 566, ISSN: 1432-0746
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