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1. Pulmonary inflammation is a feature of human and murine schistosomiasis, promoted by type-2 dendritic cells

Author

Houlder, Emma, Costain, Alice, Nambuya, Irene, Brown, Sheila, Koopman, J. P. R., Langenberg, M. C. C., Janse, J. J., Hoogerwerf, M. A., Ridley, A. J. L., Forde-Thomas, J. E., Colombo, Stefano, Winkel, B. M. F., Galdon, Alicia, Hoffmann, K. F., Cook, Peter, Roestenberg, M., Mpairwe, H., and MacDonald, Andrew

Abstract

Schistosomiasis is a parasitic disease affecting over 200 million people in multiple organs, including the lungs. Despite this, there is little understanding of pulmonary immune responses during schistosomiasis. Here, we show type-2 dominated lung immune responses in both patent (egg producing) and pre-patent (larval lung migration) murine Schistosoma mansoni (S. mansoni) infection. Human pre-patent S. mansoni infection pulmonary (sputum) samples revealed a mixed type-1/type-2 inflammatory cytokine profile, whilst a case-control study showed no significant pulmonary cytokine changes in endemic patent infection. However, schistosomiasis induced expansion of pulmonary type-2 conventional dendritic cells (cDC2s) in human and murine hosts, at both infection stages. Further, cDC2s were required for type-2 pulmonary inflammation in murine pre-patent or patent infection. These data elevate our fundamental understanding of pulmonary immune responses during schistosomiasis, which may be important for future vaccine design, as well as for understanding links between schistosomiasis and other lung diseases.

Published
2023

2. Unintended electromagnetic radiation from Starlink satellites detected with LOFAR between 110 and 188 MHz

Author

Di Vruno, F., Winkel, B., Bassa, C. G., Józsa, G. I. G., Brentjens, M. A., Jessner, A., and Garrington, S.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We report on observations of 68 satellites belonging to the SpaceX Starlink constellation with the LOFAR radio telescope. Radiation associated with Starlink satellites was detected at observing frequencies between 110 and 188 MHz. A combination of broad-band features, covering the entire observed bandwidth, as well as narrow-band (bandwidth < 12.2 kHz) emission at frequencies of 125, 135, 143.05, 150, and 175 MHz, was observed. The presence and properties of both the narrow- and broad-band features vary between satellites at different orbital altitudes. While the narrow-band detections at 143.05 MHz can be attributed to reflections of radar signals from the French GRAVES Space Surveillance Radar, the signal properties of the broad- and narrow-band features at the other frequencies suggest that this radiation is intrinsic to the Starlink satellites and it is seen for 47 out of the 68 Starlink satellites that were observed. We observed spectral power flux densities vary from 0.1 to 10 Jy for broad-band radiation, to 10 to 500 Jy for some of the narrow-band radiation, equivalent to electric field strengths of up to 49 dB[uV/m] (as measured at a 10 m distance from the satellites, with a measurement bandwidth of 120 kHz). In addition, we present equivalent power flux density simulations of the full Starlink phase 1 constellation, as well as other satellite constellations, for one frequency band allocated to radio astronomy by the International Telecommunication Union (ITU). With these, we calculate the maximum radiation level that each satellite constellation would need to have to comply with regulatory limits for intended emissions in that band. However, these limits do not apply if the radiation is unintended, that is to say if it does not originate from intentionally radiated signals for radio communication or other purposes. (shortened), 20 pages, 14 figures, in press

Published
2023
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3. Out-of-focus holography at the Effelsberg telescope

Author

Cassanelli, T., Bach, U., Winkel, B., and Kraus, A.

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Optics (physics.optics), Physics - Optics
Abstract

Out-of-focus (OOF) holography can be used to determine aperture deformations of radio telescopes that lead to errors in the phase of the complex aperture distribution. In contrast to traditional holography, OOF can be done without a reference antenna, which has a number of practical advantages. The aim of this work is to develop a standard procedure for OOF holography at the Effelsberg telescope. This includes performing OOF holography observations and the development of a software, the pyoof package, to compute aberrations of the telescope's optical system. Based on the OOF holography method developed by Nikolic et al. (2007a), we adapted the approach to the Effelsberg 100-m telescope in order to determine the aberrations of the aperture phase distribution (phase-error maps). The developed OOF holography software is presented as well as the results from observations performed at Effelsberg. Early results reveal a possible gravitationally-caused residual deformation not contained in the previously existing aperture and pointing model, and hence we propose to make changes to the model to counteract aberrations in the telescope's surface. The OOF holography method (observations and pyoof package) works as expected at the Effelsberg 100-m telescope and is able to validate the good performance of the existing finite element model. Test measurements show that slight improvements of the aperture efficiency and gain elevation dependence are possible with a more extensive OOF holography campaign., Submitted to Astronomy & Astrophysics (A&A)

Published
2021

4. A global view on star formation: The GLOSTAR Galactic plane survey

Author

Brunthaler, A., Menten, K., Dzib, S., Cotton, W., Wyrowski, F., Dokara, R., Gong, Y., Medina, S.-N., Müller, P., Nguyen, H., Ortiz-León, G., Reich, W., Rugel, M., Urquhart, J., Winkel, B., Yang, A., Beuther, H., Billington, S., Carrasco-Gonzalez, C., Csengeri, T., Murugeshan, C., Pandian, J., Roy, N., FEMIS 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; Aims. Surveys of the Milky Way at various wavelengths have changed our view of star formation in our Galaxy considerably in recent years. In this paper we give an overview of the GLOSTAR survey, a new survey covering large parts (145 square degrees) of the northern Galactic plane using the Karl G. Jansky Very Large Array in the frequency range 4−8 GHz and the Effelsberg 100-m telescope. This provides for the first time a radio survey covering all angular scales down to 1.5 arcsecond, similar to complementary near-IR and mid-IR galactic plane surveys. We outline the main goals of the survey and give a detailed description of the observations and the data reduction strategy. Methods. In our observations we covered the radio continuum in full polarization, as well as the 6.7 GHz methanol maser line, the 4.8 GHz formaldehyde line, and seven radio recombination lines. The observations were conducted in the most compact D configuration of the VLA and in the more extended B configuration. This yielded spatial resolutions of 18″ and 1.5″ for the two configurations, respectively. We also combined the D configuration images with the Effelsberg 100-m data to provide zero spacing information, and we jointly imaged the D- and B-configuration data for optimal sensitivity of the intermediate spatial ranges. Results. Here we show selected results for the first part of the survey, covering the range of 28° < l

Published
2021

5. GLOSTAR: Radio Source Catalog I. 28° < ℓ < 36° and | b | < 1°

Author

Medina, S.-N., Urquhart, J., Dzib, S., Brunthaler, A., Cotton, B., Menten, K., Wyrowski, F., Beuther, H., Billington, S., Carrasco-Gonzalez, C., Csengeri, T., Gong, Y., Hofner, P., Nguyen, H., Ortiz-León, G., Ott, J., Pandian, J., Roy, N., Sarkar, E., Wang, Y., Winkel, B., Max-Planck-Institut für Radioastronomie (MPIFR), Max Planck Institute for Radio Astronomy, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, FORMATION STELLAIRE 2020, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2019

6. GLOSTAR: Radio Source Catalog I. 28 degrees < l < 36 degrees and vertical bar b vertical bar < 1 degrees

Author

Medina, S-N X, Urquhart, J S, Dzib, S A, Brunthaler, A, Cotton, B, Menten, K M, Wyrowski, F, Beuther, H, Billington, S J, Carrasco-Gonzalez, C, Csengeri, T, Gong, Y, Hofner, P, Nguyen, H, Ortiz-Leon, G N, Ott, J, Pandian, J D, Roy, N, Sarkar, E, Wang, Y, and Winkel, B

Subjects
Physics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. Radio continuum surveys of the Galactic plane are an excellent way to identify different source populations such as planetary nebulae, H II regions, and radio stars and characterize their statistical properties. The Global View of Star Formation in the Milky Way (GLOSTAR) survey will study the star formation in the Galactic plane between -2 degrees < l < 85 degrees and vertical bar b vertical bar < 1 degrees with unprecedented sensitivity in both flux density (similar to 40 mu Jy beam(-1)) and range ofangular scales (similar to 1 `'.5 to the largest radio structures in the Galaxy). Aims. In this paper we present the first results obtained from a radio continuum map of a 16-square-degree-sized region of the Galactic plane centered on l = 32 degrees and b = 0 degrees (28 degrees < l < 36 degrees and vertical bar b vertical bar < 1 degrees). This map has a resolution of 18 `' and a sensitivity of similar to 60-150 mu Jy beam(-1). Methods. We present data acquired in 40 h of observations with the VLA in D-configuration. Two 1 GHz wide sub-bands were observed simultaneously and they were centered at 4.7 and 6.9 GHz. These data were calibrated and imaged using the Obit software package. The source extraction was performed using the BLOBCAT software package and verified through a combination of visual inspection and cross-matching with other radio and mid-infrared surveys. Results. The final catalog consists of 1575 discrete radio sources and 27 large scale structures (including W43 and W44). By cross-matching with other catalogs and calculating the spectral indices (S(nu) alpha nu(alpha)), we have classified 231 continuum sources as H II regions, 37 as ionization fronts, and 46 as planetary nebulae. The longitude and latitude distribution and negative spectral indices are all consistent with the vast majority of the unclassified sources being extragalactic background sources. Conclusions. We present a catalog of 1575 radio continuum sources and discuss their physical properties, emission nature, and relation to previously reported data. These first GLOSTAR results have increased the number of reliable H II regions in this part of the Galaxy by a factor of four.

Published
2019
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7. GLOSTAR -- Radio Source Catalog I: $28^{\circ}< \textit{l} < 36^{\circ}$ and $|b| < 1^{\circ}$

Author

Medina, S. N. X., Urquhart, J. S., Dzib, S. A., Brunthaler, A., Cotton, B., Menten, K. M., Wyrowski, F., Beuther, H., Billington, S. J., Carrasco-Gonzalez, C., Csengeri, T., Gong, Y., Hofner, P., Nguyen, H., Ortiz-León, G. N., Ott, J., Pandian, J. D., Roy, N., Sarkar, E., Wang, Y., and Winkel, B.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

The GLOSTAR survey will study the star formation in the Galactic plane between $-2^{\circ}< \textit{l}< 85^{\circ}$ and $|b| < 1^{\circ}$ with unprecedented sensitivity in both, flux density ($\sim$ 40 $\mu Jy$ beam$^{-1}$) and range of angular scales ($\sim$ 1."5 to the largest radio structures in the Galaxy). In this paper we present the first results obtained from a radio continuum map of a 16 square degree sized region of the Galactic plane centered on $\textit{l} = 32^{\circ}$ and $b = 0^{\circ}$ ($28^{\circ} < \textit{l} < 36^{\circ}$ and $|b| < 1^{\circ}$). This map has a resolution of 18" and sensitivity of $\sim$ 60-150 $\mu Jy$ beam$^{-1}$. We present data acquired with the VLA in D-configuration. Two 1 GHz wide sub-bands were observed simultaneously and centred at 4.7 and 6.9 GHz. These data were calibrated and imaged using the $\textit{Obit}$ software package. The source extraction has been performed using the BLOBCAT software package and verified through a combination of visual inspection and cross-matching with other radio and mid-infrared surveys. The final catalog consists of 1575 discrete radio sources and 27 large scale structures (including W43 and W44). By cross-matching with other catalogs and calculating the spectral indices ($S(\nu) \propto \nu^\alpha$), we have classified 231 continuum sources as HII regions, 37 as ionization fronts, and 46 as planetary nebulae. The longitude and latitude distribution and negative spectral indices are all consistent with the vast majority of the unclassified sources being extragalactic background sources. We present a catalog of 1575 radio continuum sources and discuss their physical properties, emission nature and relation with previously reported. These first GLOSTAR results have increased the number of reliable HII regions in this part of the Galaxy by a factor of four., Comment: 24 pages, 23 figures, Accepted by Astronomy & Astrophysics journal

Published
2019

8. GLOSTAR: Radio Source Catalog I. 28° < ℓ < 36° and |b| < 1°

Author

Medina, S., Urquhart, J., Dzib, S., Brunthaler, A., Cotton, B., Menten, K., Wyrowski, F., Beuther, H., Billington, S., Carrasco-Gonzalez, C., Csengeri, T., Gong, Y., Hofner, P., Nguyen, H., Ortiz-León, G., Ott, J., Pandian, J., Roy, N., Sarkar, E., Wang, Y., and Winkel, B.

Abstract

Context. Radio continuum surveys of the Galactic plane are an excellent way to identify different source populations such as planetary nebulae, H II regions, and radio stars and characterize their statistical properties. The Global View of Star Formation in the Milky Way (GLOSTAR) survey will study the star formation in the Galactic plane between -2° < ℓ < 85° and |b| < 1° with unprecedented sensitivity in both flux density (~40 μJy beam-1) and range ofangular scales (~1".5 to the largest radio structures in the Galaxy). Aims: In this paper we present the first results obtained from a radio continuum map of a 16-square-degree-sized region of the Galactic plane centered on ℓ = 32° and b = 0° (28° < ℓ < 36° and |b| < 1°). This map has a resolution of 18″ and a sensitivity of ~60-150 μJy beam-1. Methods: We present data acquired in 40 h of observations with the VLA in D-configuration. Two 1 GHz wide sub-bands were observed simultaneously and they were centered at 4.7 and 6.9 GHz. These data were calibrated and imaged using the Obit software package. The source extraction was performed using the BLOBCAT software package and verified through a combination of visual inspection and cross-matching with other radio and mid-infrared surveys. Results: The final catalog consists of 1575 discrete radio sources and 27 large scale structures (including W43 and W44). By cross-matching with other catalogs and calculating the spectral indices (S(ν) ∝ να), we have classified 231 continuum sources as H II regions, 37 as ionization fronts, and 46 as planetary nebulae. The longitude and latitude distribution and negative spectral indices are all consistent with the vast majority of the unclassified sources being extragalactic background sources. Conclusions: We present a catalog of 1575 radio continuum sources and discuss their physical properties, emission nature, and relation to previously reported data. These first GLOSTAR results have increased the number of reliable H II regions in this part of the Galaxy by a factor of four. Full version of Table 7 and data from Figs. 7, 9, and 17 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/A175

Published
2019

9. GLOSTAR: Radio Source Catalog I. 28° < ℓ < 36° and |b| < 1°⋆

Author

Medina, S. X. (S.-N. X.), Urquhart, J. S. (J. S.), Dzib, S. A. (S. A.), Brunthaler, A. (A.), Cotton, B. (B.), Menten, K. M. (K. M.), Wyrowski, F. (F.), Beuther, H. (H.), Billington, S. J. (S. J.), Carrasco-Gonzalez, C. (C.), Csengeri, T. (T.), Gong, Y. (Y.), Hofner, P. (P.), Nguyen, H. (H.), Ortiz-León, G. N. (G. N.), Ott, J. (J.), Pandian, J. D. (J. D.), Roy, N. (N.), Sarkar, E. (E.), Wang, Y. (Y.), and Winkel, B. (B.)

Subjects
formation [stars], surveys, Astrophysics::High Energy Astrophysical Phenomena, thermal [radiation mechanisms], general [radio continuum], Astrophysics::Cosmology and Extragalactic Astrophysics, non-thermal [radiation mechanisms], Astrophysics::Galaxy Astrophysics, interferometric [techniques]
Abstract

Context: Radio continuum surveys of the Galactic plane are an excellent way to identify different source populations such as planetary nebulae, H Ⅱ regions, and radio stars and characterize their statistical properties. The Global View of Star Formation in the Milky Way (GLOSTAR) survey will study the star formation in the Galactic plane between −2° < ℓ < 85° and |b| < 1° with unprecedented sensitivity in both flux density (∼40 μJy beam⁻¹) and range ofangular scales (∼1″.5 to the largest radio structures in the Galaxy). Aims: In this paper we present the first results obtained from a radio continuum map of a 16-square-degree-sized region of the Galactic plane centered on ℓ = 32° and b = 0° (28° < ℓ < 36° and |b

Published
2019

10. GLOSTAR -- Radio Source Catalog I: $28^{\circ}< \textit{l} < 36^{\circ}$ and $|b| < 1^{\circ}$

Author

Medina, S. N. X., Urquhart, J. S., Dzib, S. A., Brunthaler, A., Cotton, B., Menten, K. M., Wyrowski, F., Beuther, H., Billington, S. J., Carrasco-Gonzalez, C., Csengeri, T., Gong, Y., Hofner, P., Nguyen, H., Ortiz-Le��n, G. N., Ott, J., Pandian, J. D., Roy, N., Sarkar, E., Wang, Y., and Winkel, B.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The GLOSTAR survey will study the star formation in the Galactic plane between $-2^{\circ}< \textit{l}< 85^{\circ}$ and $|b| < 1^{\circ}$ with unprecedented sensitivity in both, flux density ($\sim$ 40 $��Jy$ beam$^{-1}$) and range of angular scales ($\sim$ 1."5 to the largest radio structures in the Galaxy). In this paper we present the first results obtained from a radio continuum map of a 16 square degree sized region of the Galactic plane centered on $\textit{l} = 32^{\circ}$ and $b = 0^{\circ}$ ($28^{\circ} < \textit{l} < 36^{\circ}$ and $|b| < 1^{\circ}$). This map has a resolution of 18" and sensitivity of $\sim$ 60-150 $��Jy$ beam$^{-1}$. We present data acquired with the VLA in D-configuration. Two 1 GHz wide sub-bands were observed simultaneously and centred at 4.7 and 6.9 GHz. These data were calibrated and imaged using the $\textit{Obit}$ software package. The source extraction has been performed using the BLOBCAT software package and verified through a combination of visual inspection and cross-matching with other radio and mid-infrared surveys. The final catalog consists of 1575 discrete radio sources and 27 large scale structures (including W43 and W44). By cross-matching with other catalogs and calculating the spectral indices ($S(��) \propto ��^��$), we have classified 231 continuum sources as HII regions, 37 as ionization fronts, and 46 as planetary nebulae. The longitude and latitude distribution and negative spectral indices are all consistent with the vast majority of the unclassified sources being extragalactic background sources. We present a catalog of 1575 radio continuum sources and discuss their physical properties, emission nature and relation with previously reported. These first GLOSTAR results have increased the number of reliable HII regions in this part of the Galaxy by a factor of four., 24 pages, 23 figures, Accepted by Astronomy & Astrophysics journal

Published
2019
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12. Circumgalactic Gas at its Extreme: Tidal Gas Streams around the Whale Galaxy NGC 4631 Explored with HST/COS

Author

Richter, P., Winkel, B., Wakker, B.P., Pingel, N.M., Fox, A.J., Heald, G., Walterbos, R.A.M., Fechner, C., Ben Bekhti, N., Gentile, G., and Publica

Abstract

We present a detailed analysis of the absorption properties of one of the tidal gas streams around the "Whale" galaxy NGC 4631 in the direction of the quasar 2MASS J12421031+3214268. Our study is based on ultraviolet spectral data obtained with the Cosmic Origins Spectrograph (COS) on board the Hubble Space Telescope (HST) and 21cm-data from the HALOGAS project and the Green Bank Telescope (GBT). We detect strong H i Lya absorption in the velocity range +550 to +800 km s−1 related to gas from a NGC 4631 tidal stream known as Spur 2. We measure a column density of log (N(H i/cm−2)) = 18.68 ± 0.15, indicating that the quasar sightline traces the outer boundary of Spur 2 as seen in the 21 cm data. Metal absorption in Spur 2 is detected in the lines of O i, C ii, Si ii, and Si iii in a complex absorption pattern that reflects the multiphase nature of the gas. We find that the average neutral gas fraction in Spur 2 toward 2MASS J12421031+3214268 is only 14%. This implies that ionized gas dominates the total mass of Spur 2, which then may comprise more than 109 M ☉. No significant depletion of Si is observed, showing that Spur 2 does not contain significant amounts of dust. From the measured O i/H i column density ratio, we determine an a abundance in Spur 2 of ${0.13}_{-0.05}{+0.07}$ solar ([a/H] = −0.90±0.16), which is substantially lower than what is observed in the NGC 4631 disk. The low metallicity and low dust content suggest that Spur 2 represents metal-deficient gas stripped off a gas-rich satellite galaxy during a recent encounter with NGC 4631.

Published
2018

14. CONTROLLED HUMAN INFECTION WITH SINGLE-SEX SCHISTOSOMA MANSONI CERCARIAE

Author

Langenberg, M., Hoogerwerf, M.A., Janse, J., Kos-van Oosterhoud, J., Feijt, C., Dood, C. de, Ganesh, M., Ozir-Fazalakhan, A., Kruize, Y., Winkel, B., Hardeman, G., Verbeek-Menken, P., Beek, M. van der, Brienen, E., Diepen, A. van, Corstjens, P., Visser, L., Lieshout, L. van, Smits, H., Meij, P., Dam, G. van, Hokke, R., Yazdanbakhsh, M., and Roestenberg, M.

Published
2018

15. Hydrogen in diffuse molecular clouds in the Milky Way

Author

Winkel, B., Wiesemeyer, H., Menten, K., Sato, M., Brunthaler, A., Wyrowski, F., Neufeld, D., Gerin, M., Indriolo, N., Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS Paris)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2017

16. Planck intermediate results. XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies

Author

Planck Collaboration, Abergel, A., Ade, P. A. R., Aghanim, N., Alves, M. I. R., Aniano, G., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoit-L��vy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bobin, J., Bonaldi, A., Bond, J. R., Bouchet, F. R., Boulanger, F., Burigana, C., Cardoso, J. -F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Crill, B. P., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., D��sert, F. -X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Dor��, O., Douspis, M., Dupac, X., Efstathiou, G., En��lin, T. A., Eriksen, H. K., Falgarone, E., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-H��raud, Y., Gonz��lez-Nuevo, J., G��rski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Henrot-Versill��, S., Hern��ndez-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Joncas, G., Jones, A., Jones, W. C., Juvela, M., Kalberla, P., Keih��nen, E., Kerp, J., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., L��hteenm��ki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-V��rnle, M., L��pez-Caniego, M., Lubin, P. M., Mac��as-P��rez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Mart��nez-Gonz��lez, E., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Desch��nes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Savini, G., Spencer, L. D., Starck, J. -L., Sureau, F., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Verstraete, L., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Winkel, B., Yvon, D., Zacchei, A., Zonca, A., Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), PLANCK, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), European Commission, A., Abergel, P. A. R., Ade, N., Aghanim, M. I. R., Alve, G., Aniano, M., Arnaud, M., Ashdown, J., Aumont, C., Baccigalupi, A. J., Banday, R. B., Barreiro, J. G., Bartlett, E., Battaner, K., Benabed, A., Benoit Lévy, J. P., Bernard, M., Bersanelli, P., Bielewicz, J., Bobin, A., Bonaldi, J. R., Bond, F. R., Bouchet, F., Boulanger, C., Burigana, J. F., Cardoso, A., Catalano, A., Chamballu, H. C., Chiang, P. R., Christensen, D. L., Clement, S., Colombi, L. P. L., Colombo, F., Couchot, B. P., Crill, F., Cuttaia, L., Danese, R. J., Davi, P., de Bernardi, A., de Rosa, G., de Zotti, J., Delabrouille, F. X., Désert, C., Dickinson, J. M., Diego, H., Dole, S., Donzelli, O., Doré, M., Douspi, X., Dupac, G., Efstathiou, T. A., Enßlin, H. K., Eriksen, E., Falgarone, F., Finelli, O., Forni, M., Fraili, E., Franceschi, S., Galeotta, K., Ganga, T., Ghosh, M., Giard, Y., Giraud Héraud, J., González Nuevo, K. M., Górski, Gregorio, Anna, A., Gruppuso, V., Guillet, F. K., Hansen, D., Harrison, G., Helou, S., Henrot Versillé, C., Hernández Monteagudo, D., Herranz, S. R., Hildebrandt, E., Hivon, M., Hobson, W. A., Holme, A., Hornstrup, W., Hovest, K. M., Huffenberger, A. H., Jaffe, T. R., Jaffe, G., Jonca, A., Jone, W. C., Jone, M., Juvela, P., Kalberla, E., Keihänen, J., Kerp, R., Keskitalo, T. S., Kisner, R., Kneissl, J., Knoche, M., Kunz, H., Kurki Suonio, G., Lagache, A., Lähteenmäki, J. M., Lamarre, A., Lasenby, C. R., Lawrence, R., Leonardi, F., Levrier, M., Liguori, P. B., Lilje, M., Linden Vørnle, M., López Caniego, P. M., Lubin, J. F., Macías Pérez, B., Maffei, D., Maino, N., Mandolesi, M., Mari, D. J., Marshall, P. G., Martin, E., Martínez González, S., Masi, M., Massardi, S., Matarrese, P., Mazzotta, A., Melchiorri, L., Mende, A., Mennella, M., Migliaccio, S., Mitra, M. A., Miville Deschêne, A., Moneti, L., Montier, G., Morgante, D., Mortlock, D., Munshi, J. A., Murphy, P., Naselsky, F., Nati, P., Natoli, F., Noviello, D., Novikov, I., Novikov, C. A., Oxborrow, L., Pagano, F., Pajot, D., Paoletti, F., Pasian, O., Perdereau, L., Perotto, F., Perrotta, F., Piacentini, M., Piat, E., Pierpaoli, D., Pietrobon, S., Plaszczynski, E., Pointecouteau, G., Polenta, N., Ponthieu, L., Popa, G. W., Pratt, S., Prunet, J. L., Puget, J. P., Rachen, W. T., Reach, R., Rebolo, M., Reinecke, M., Remazeille, C., Renault, S., Ricciardi, T., Riller, I., Ristorcelli, G., Rocha, C., Rosset, G., Roudier, B., Rusholme, M., Sandri, G., Savini, L. D., Spencer, J. L., Starck, F., Sureau, D., Sutton, A. S., Suur Uski, J. F., Sygnet, J. A., Tauber, L., Terenzi, L., Toffolatti, M., Tomasi, M., Tristram, M., Tucci, G., Umana, L., Valenziano, J., Valiviita, B., Van Tent, L., Verstraete, P., Vielva, F., Villa, L. A., Wade, B. D., Wandelt, B., Winkel, D., Yvon, A., Zacchei, A., Zonca, Department of Physics, Helsinki Institute of Physics, APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Abergel, A, Ade, P, Aghanim, N, Alves, M, Aniano, G, Arnaud, M, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartlett, J, Battaner, E, Benabed, K, Benoit-Levy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bobin, J, Bonaldi, A, Bond, J, Bouchet, F, Boulanger, F, Burigana, C, Cardoso, J, Catalano, A, Chamballu, A, Chiang, H, Christensen, P, Clements, D, Colombi, S, Colombo, L, Couchot, F, Crill, B, Cuttaia, F, Danese, L, Davis, R, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Desert, F, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Dore, O, Douspis, M, Dupac, X, Efstathiou, G, Ensslin, T, Eriksen, H, Falgarone, E, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, F, Harrison, D, Helou, G, Henrot-Versille, S, Hernandez-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Jaffe, A, Jaffe, T, Joncas, G, Jones, A, Jones, W, Juvela, M, Kalberla, P, Keihanen, E, Kerp, J, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden-Vornle, M, Lopez-Caniego, M, Lubin, P, Macias-Perez, J, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martinez-Gonzalez, E, Masi, S, Massardi, M, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Noviello, F, Novikov, D, Novikov, I, Oxborrow, C, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rusholme, B, Sandri, M, Savini, G, Spencer, L, Starck, J, Sureau, F, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Verstraete, L, Vielva, P, Villa, F, Wade, L, Wandelt, B, Winkel, B, Yvon, D, Zacchei, A, Zonca, A, Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, and Aalto University

Subjects
SOLAR NEIGHBORHOOD, Astronomy, diffuse backgrounds [Infrared], Astrophysics, cosmic background radiation, 7. Clean energy, 01 natural sciences, Far infrared, Astrophysics::Solar and Stellar Astrophysics, extinction / submillimeter: ISM / local insterstellar matter / infrared: diffuse background / cosmic background radiation, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Physics, education.field_of_study, Spectral index, Dust , extinction, local interstellar matter, extinction, Cosmic background radiation, Dust, extinction, Infrared: diffuse background, Local insterstellar matter, Submillimeter: ISM, Microwave frequencies, Electromagnetic wave emission, Wavelength, MOLECULAR-HYDROGEN, MAGELLANIC STREAM, MILKY-WAY, submillimeter: ISM, Astronomy and Astrophysics, Space and Planetary Science, dust, extinction, dust, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], ANISOTROPY-PROBE, local insterstellar matter, Opacity, DATA RELEASE, Astrophysics::High Energy Astrophysical Phenomena, education, Carbon dust, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, Settore FIS/05 - Astronomia e Astrofisica, diffuse background [infrared], 0103 physical sciences, Emissivity, Black-body radiation, ISM [submillimeter], Astrophysics::Galaxy Astrophysics, MAGNETIC NANOPARTICLES, 010308 nuclear & particles physics, Silicates, Amorphous carbon, BACKGROUND EXPERIMENT SEARCH, CENTIMETER EXCESS, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, infrared: diffuse background, Interstellar medium, GALACTIC EMISSION, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), dust, extinction / submillimeter: ISM / local insterstellar matter / infrared: diffuse background / cosmic background radiation, Hydrogen, isms [Submillimeter], Galaxy Astrophysics
Abstract

The dust-Hi correlation is used to characterize the emission properties of dust in the diffuse interstellar medium (ISM) from far infrared wavelengths to microwave frequencies. The field of this investigation encompasses the part of the southern sky best suited to study the cosmic infrared and microwave backgrounds. We cross-correlate sky maps from Planck, the Wilkinson Microwave Anisotropy Probe (WMAP), and the diffuse infrared background experiment (DIRBE), at 17 frequencies from 23 to 3000 GHz, with the Parkes survey of the 21 cm line emission of neutral atomic hydrogen, over a contiguous area of 7500 deg2 centred on the southern Galactic pole. We present a general methodology to study the dust-H i correlation over the sky, including simulations to quantify uncertainties. Our analysis yields four specific results. (1) We map the temperature, submillimetre emissivity, and opacity of the dust per H-atom. The dust temperature is observed to be anti-correlated with the dust emissivity and opacity. We interpret this result as evidence of dust evolution within the diffuse ISM. The mean dust opacity is measured to be (7.1 ± 0.6) × 10-27 cm2 H-1 × (v/353 GHz) 1.53 ± 0.03for 100 ≤ v ≤ 353 GHz. This is a reference value to estimate hydrogen column densities from dust emission at submillimetre and millimetre wavelengths. (2) We map the spectral index βmm of dust emission at millimetre wavelengths (defined here as v ≤ 353GHz), and find it to be remarkably constant at βmm = 1.51 ± 0.13. We compare it with the far infrared spectral index βFIR derived from greybody fits at higher frequencies, and find a systematic difference, βmm -βFIR = -0.15, which suggests that the dust spectral energy distribution (SED) flattens at v ≤ 353 GHz. (3) We present spectral fits of the microwave emission correlated with Hi from 23 to 353 GHz, which separate dust and anomalous microwave emission (AME). We show that the flattening of the dust SED can be accounted for with an additional component with a blackbody spectrum. This additional component, which accounts for (26 ± 6)% of the dust emission at 100GHz, could represent magnetic dipole emission. Alternatively, it could account for an increasing contribution of carbon dust, or a flattening of the emissivity of amorphous silicates, at millimetre wavelengths. These interpretations make different predictions for the dust polarization SED. (4) We analyse the residuals of the dust-Hi correlation. We identify a Galactic contribution to these residuals, which we model with variations of the dust emissivity on angular scales smaller than that of our correlation analysis. This model of the residuals is used to quantify uncertainties of the CIB power spectrum in a companion Planck paper.© ESO 2014., The Planck Collaboration acknowledges support from: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement nº 267934.

Published
2014

17. HI4PI: A full-sky HI survey based on EBHIS and GASS

Author

Ben, Bekhti N., Floer, L., Keller, R., Kerp, J., Lenz, D., Winkel, B., Bailin, J., Calabretta, M. R., Dedes, L., Ford, H. A., Gibson, B. K., Haud, U., Janowiecki, S., Kalberla, P. M. W., Lockman, F. J., McClure-Griffiths, N. M., Murphy, T., Pisano, D. J., Staveley-Smith, L., and Nakanishi, Hiroyuki

Subjects
Physics, Brightness, 010308 nuclear & particles physics, Third revision, media_common.quotation_subject, HEALPix, Milky Way, Sampling (statistics), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, ISM: atoms, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, surveys, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Angular resolution, Map projection, 010303 astronomy & astrophysics, techniques: spectroscopic, media_common
Abstract

著者人数: 20名, Accepted: 2016-09-07, 資料番号: SA1160234000

Published
2016
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18. HERSCHEL SURVEY OF GALACTIC OH + , H 2 O + , AND H 3 O + : PROBING THE MOLECULAR HYDROGEN FRACTION AND COSMIC-RAY IONIZATION RATE

Author

Iffrig, Olivier, Hennebelle, Patrick, Indriolo, Nick, Neufeld, D., Gerin, M., Schilke, P., Benz, A., Winkel, B., Menten, K., Chambers, E., Black, John, Bruderer, S., Falgarone, E., Godard, B., Goicoechea, J., Gupta, H., Lis, D., Ossenkopf, V., Persson, C., Sonnentrucker, P., Van Der Tak, F., Van Dishoeck, E., Wolfire, Mark, Wyrowski, F., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Onsala space observatory (oso), Chalmers University of Technology [Göteborg], Max-Planck-Institut für Extraterrestrische Physik (MPE), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Laboratoire Univers et Théories (LUTH (UMR_8102)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Materials Science and Engineering, KTH (KTH), Department of Materials Science and Engineering, KTH, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Onsala Space Observatory (OSO), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), National Aeronautics and Space Administration (US), Ministerio de Ciencia e Innovación (España), Ministerio de Economía y Competitividad (España), and Kapteyn Astronomical Institute

Subjects
Hydrogen, Astrophysics::High Energy Astrophysical Phenomena, Interstellar cloud, Continuum (design consultancy), chemistry.chemical_element, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ion, cosmic rays, Ionization, Disc, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], astrochemistry, Galactic Center, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, chemistry, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrochemistry - cosmic rays, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

In diffuse interstellar clouds the chemistry that leads to the formation of the oxygen-bearing ions OH+, H2O+, and H3O+ begins with the ionization of atomic hydrogen by cosmic rays, and continues through subsequent hydrogen abstraction reactions involving H2. Given these reaction pathways, the observed abundances of these molecules are useful in constraining both the total cosmic-ray ionization rate of atomic hydrogen (ζH) and molecular hydrogen fraction ($f_{\rm H_2}$). We present observations targeting transitions of OH+, H2O+, and H3O+ made with the Herschel Space Observatory along 20 Galactic sight lines toward bright submillimeter continuum sources. Both OH+ and H2O+ are detected in absorption in multiple velocity components along every sight line, but H3O+ is only detected along 7 sight lines. From the molecular abundances we compute $f_{\rm H_2}$ in multiple distinct components along each line of sight, and find a Gaussian distribution with mean and standard deviation 0.042 ± 0.018. This confirms previous findings that OH+ and H2O+ primarily reside in gas with low H2 fractions. We also infer ζH throughout our sample, and find a lognormal distribution with mean log (ζH) = –15.75 (ζH = 1.78 × 10–16 s–1) and standard deviation 0.29 for gas within the Galactic disk, but outside of the Galactic center. This is in good agreement with the mean and distribution of cosmic-ray ionization rates previously inferred from H$_3^+$ observations. Ionization rates in the Galactic center tend to be 10-100 times larger than found in the Galactic disk, also in accord with prior studies., Support for this work was provided by NASA through an award issued by JPL/Caltech. N.I. and D.A.N. are funded by NASA Research Support Agreement No. 1393741 provided through JPL. J.R.G. thanks the Spanish MINECO for funding support under grants CSD2009-00038 and AYA2012- 32032.

Published
2015

21. Pregnancy outcome following maternal exposure to Mirtazapine: Preliminary results of a collaborative ENTIS study

Author

Winterfeld, U., Buclin, T., Klinger, G., Panchaud, A., Stephens, S., Arnon, J., Malm, H., te Winkel, B., Clementi, M., Pistelli, A., Manáková, A., Eleftheriou, G., Merlob, P., Kaplan, Y.C., and Rothuizen, L.E.

Abstract

Introduction: Mirtazapine is a noradrenergic and serotonergic antidepressant mainly acting through blockade of presynaptic alpha-2 receptors. Published data on pregnancy outcome after exposure to mirtazapine are scarce. This study addresses the risk associated with exposure to mirtazapine during pregnancy. Patients (or Materials) and Methods: Multicenter (n = 11), observational prospective cohort study comparing pregnancy outcomes after exposure to mirtazapine with 2 matched control groups: exposure to any selective serotonin reuptake inhibitor (SSRI) as a diseasematched control group, and general controls with no exposure to medication known to be teratogenic or to any antidepressant. Data were collected by members of the European Network of Teratology Information Services (ENTIS) during individual risk counseling between 1995 and 2011. Standardized procedures for data collection were used in each center. Results: A total of 357 pregnant women exposed to mirtazapine at any time during pregnancy were included in the study and compared with 357 pregnancies from each control group. The rate of major birth defects between the mirtazapine and the SSRI group did not differ significantly (4.5% vs 4.2%; unadjusted odds ratio, 1.1; 95% confidence interval, 0.5-2.3, P = 0.9). A trend toward a higher rate of birth defects in the mirtazapine group compared with general controls did not reach statistical significance (4.2% vs 1.9%; OR, 2.4; 95% CI, 0.9-6.3; P = 0.08). The crude rate of spontaneous abortions did not differ significantly between the mirtazapine, the SSRI, and the general control groups (9.5% vs 10.4% vs 8.4%; P = 0.67), neither did the rate of deliveries resulting in live births (79.6% vs 84.3% in both control groups; P = 0.15). However, a higher rate of elective pregnancy-termination was observed in the mirtazapine group compared with SSRI and general controls (7.8% vs 3.4% vs 5.6%; P = 0.03). Premature birth (< 37 weeks) (10.6% vs 10.1% vs 7.5%; P = 0.38), gestational age at birth (median, 39 weeks; interquartile range (IQR), 38-40 in all groups; P = 0.29), and birth weight (median, 3320 g; IQR, 2979-3636 vs 3230 g; IQR, 2910-3629 vs 3338 g; IQR, 2967-3650; P = 0.34) did not differ significantly between the groups. Conclusion: This study did not observe a statistically significant difference in the rate of major birth defects between mirtazapine, SSRI-exposed, and nonexposed pregnancies. A slightly higher rate of birth defects was, however, observed in the mirtazapine and SSRI groups compared with the low rate of birth defects in our general controls. Overall, the pregnancy outcome after mirtazapine exposure in this study is very similar to that of the SSRI-exposed control group.

Published
2013

22. An absorption-selected survey of neutral gas in the Milky Way halo

Author

Bekhti, N. Ben, Winkel, B., Richter, P., Kerp, J., Klein, U., and Murphy, M. T.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We aim at analysing systematically the distribution and physical properties of neutral and mildly ionised gas in the Milky Way halo, based on a large absorption-selected data set. Multi-wavelength studies were performed combining optical absorption line data of CaII and NaI with follow-up HI 21-cm emission line observations along 408 sight lines towards low- and high-redshift QSOs. We made use of archival optical spectra obtained with UVES/VLT. HI data were extracted from the Effelsberg-Bonn HI survey and the Galactic All-Sky survey. For selected sight lines we obtained deeper follow-up observations using the Effelsberg 100-m telescope. CaII (NaI) halo absorbers at intermediate and high radial velocities are present in 40-55% (20-35%) of the sightlines, depending on the column density threshold chosen. Many halo absorbers show multi-component absorption lines, indicating the presence of sub-structure. In 65% of the cases, absorption is associated with HI 21-cm emission. The CaII (NaI) column density distribution function follows a power-law with a slope of -2.2 (-1.4). Our absorption-selected survey confirms our previous results that the Milky Way halo is filled with a large number of neutral gas structures whose high column density tail represents the population of common HI high- and intermediate-velocity clouds seen in 21-cm observations. We find that CaII/NaI column density ratios in the halo absorbers are typically smaller than those in the Milky Way disc, in the gas in the Magellanic Clouds, and in damped Lyman-alpha systems. The small ratios (prominent in particular in high-velocity components) indicate a lower level of Ca depletion onto dust grains in Milky Way halo absorbers compared to gas in discs and inner regions of galaxies., 17 pages, 20 figures, accepted by A&A

Published
2012

23. An absorption-selected survey of neutral gas in the Milky Way halo New results based on a large sample of Ca II, Na I, and H I spectra towards QSOs

Author

Ben Bekhti, Nadya, Winkel, B., Richter, P., Kerp, J., Klein, U., and Murphy, M. T.

Subjects
Institut für Physik und Astronomie, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Aims. We aim at analysing systematically the distribution and physical properties of neutral and mildly ionised gas in the Milky Way halo, based on a large absorption-selected data set. Methods. Multi-wavelength studies were performed combining optical absorption line data of Ca II and Na I with follow-up H I 21-cm emission line observations along 408 sight lines towards low-and high-redshift QSOs. We made use of archival optical spectra obtained with UVES/VLT. H I data were extracted from the Effelsberg-Bonn H I survey and the Galactic All-Sky survey. For selected sight lines we obtained deeper follow-up observations using the Effelsberg 100-m telescope. Results. Ca II (Na I) halo absorbers at intermediate and high radial velocities are present in 40-55% (20-35%) of the sightlines, depending on the column density threshold chosen. Many halo absorbers show multi-component absorption lines, indicating the presence of sub-structure. In 65% of the cases, absorption is associated with H I 21-cm emission. The Ca II (Na I) column density distribution function follows a power-law with a slope of beta approximate to -2.2 (-1.4). Conclusions. Our absorption-selected survey confirms our previous results that the Milky Way halo is filled with a large number of neutral gas structures whose high column density tail represents the population of common H I high-and intermediate-velocity clouds seen in 21-cm observations. We find that Na I/Ca II column density ratios in the halo absorbers are typically smaller than those in the Milky Way disc, in the gas in the Magellanic Clouds, and in damped Lyman a systems. The small ratios (prominent in particular in high-velocity components) indicate a lower level of Ca depletion onto dust grains in Milky Way halo absorbers compared to gas in discs and inner regions of galaxies.

Published
2012

24. Absorption and emission line studies of gas in the Milky Way halo

Author

Bekhti, N. Ben, Richter, P., Winkel, B., Kerp, J., Kalberla, P., Klein, U., and Murphy, M. T.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We perform a systematic study of physical properties and distribution of neutral and ionised gas in the halo of the Milky Way (MW). Beside the large neutral intermediate- and high-velocity cloud (IVC, HVC) complexes there exists a population of partly ionised gaseous structures with low-column densities that have a substantial area filling factor. The origin and nature of these structures are still under debate. We analyse the physical parameters of the MW halo gas and the relation to quasar (QSO) metal-absorption line systems at low and high redshifts. For this purpose we combine new HI 21-cm data from the EBHIS and GASS surveys with optical quasar absorption line data to study the filling factor and distribution of these gaseous clouds in the halo at HI densities below 10^19 1/cm^2. This study is important to understand the evolution of the MW in particular and the gas accretion mechanisms of galaxies in general., 7 pages, 6 figures. To appear in "The Dynamic ISM: A celebration of the Canadian Galactic Plane Survey," ASP Conference Series

Published
2010

25. The Effelsberg-Bonn HI Survey: Milky Way data

Author

Winkel, B., Kerp, J., Kalberla, P. M. W., and Bekhti, N. Ben

Subjects
Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

Since autumn 2008 an L-band 7-Feed-Array is operated for astronomical science at the 100-m radio telescope at Effelsberg. This receiver is used to perform an unbiased, fully sampled HI survey of the whole northern hemisphere observing both the galactic and extragalactic sky in parallel - the Effelsberg-Bonn HI survey (EBHIS). We present first results based on the Milky Way data. Up to now two larger coherent regions were mapped each covering about 2000 square degrees. One of these fields covers the northern part of the high-velocity cloud complex GCN. With the better angular resolution of the EBHIS we resolve the previously detected clouds into isolated compact clumps and find a linewidth-radial velocity relation giving hints on an interaction of accreting material with the Milky Way halo., 7 pages, 6 figures. To appear in "The Dynamic ISM: A celebration of the Canadian Galactic Plane Survey," ASP Conference Series

Published
2010

26. RFI mitigation for the Effelsberg-Bonn HI Survey (EBHIS)

Author

Flöer, L., Winkel, B., and Kerp, J.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

A new L-band 7 feed array at the 100-m telescope is used to perform an unbiased, fully sampled HI survey of the whole northern hemisphere - the Effelsberg-Bonn HI Survey (EBHIS). The use of state-of-the-art digital Fast Fourier Transform spectrometers based on FPGAs - superior in dynamic range and allowing fast dumping of spectra - makes it possible to apply sophisticated RFI mitigation schemes. Based on the current status of the survey we discuss the RFI situation at the 100-m telescope and present a fast algorithm to automatically identify RFI in the raw data output from the spectrometer. Using simulations we show that it is feasible to detect more than 95% of all RFI in excess of 1 sigma amplitude with less than 1% false positives., Comment: 9 pages, 7 figures, accepted for publication in Proc. RFI2010

Published
2010
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27. Bioassays for the ecotoxicological and genotoxicological assessment of contaminated soils (results of a round-robin test). Part 2: Assessment of the habitat function of soils - tests with soil microflora and fauna

Author

Hund-Rinke, K., Kördel, W., Hennecke, D., Achazi, R., Warnecke, D., Wilke, B.-M., Winkel, B., Heiden, S., and Publica

Subjects
microorganism, Fauna, bioassay, ecotoxicity, terrestrial test system, soil assessment
Abstract

For the assessment of contaminated or remediated soils, aside from chemical analyses, ecotoxicological tests are performed which focus on the retention function of soils (determined by tests with aqueous soil extracts) and on the habitat function (determined by tests with soil). Whereas numerous test exist as standardized guidelines for identifying the effect of chemicals, this is not the case for the assessment of soil quality. A round-robin test was performed to monitor the comparability of the results from ecotoxicological test methods on soils and to facilitate the standardization of corresponding test methods. Four contaminated soils were tested using a total number of fifteen test systems, including ecotoxicological and genotoxicological tests with soil extracts and soil. In the second part of this publication series, the results obtained from the tests with soil micro-organisms and soil fauna are presented.

Published
2002

29. Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation

Author

Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoit, A., Benoit-Levy, A., Bernard, J. -P., Bersanelli, M., Bethermin, M., Bielewicz, P., Blagrave, K., Bobin, J., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. -F., Catalano, A., Challinor, A., Chamballu, A., Chen, X., Chiang, H. C., Chiang, L. -Y, Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. -M., Desert, F. -X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Dore, O., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Heraud, Y., Gonzalez-Nuevo, J., Gorski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Helou, G., Henrot-Versille, S., Hernandez-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Kalberla, P., Keihanen, E., Kerp, J., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lacasa, F., Lagache, G., Lahteenmaki, A., Lamarre, J. -M., Langer, M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leonardi, R., Leon-Tavares, J., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P. M., Macias-Perez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martinez-Gonzalez, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschenes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Norgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prezeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan-Robinson, M., Rubino-Martin, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Serra, P., Shellard, E. P. S., Spencer, L. D., Starck, J. -L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Tuerler, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Welikala, N., White, M., White, S. D. M., Winkel, B., Yvon, D., Zacchei, A., Zonca, A., Planck Collaboration, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), PLANCK, Tauber, Jan, Ade, P. A. R., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bethermin, M., Bielewicz, P., Blagrave, K., Bobin, J., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Challinor, A., Chamballu, A., Chen, X., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Kalberla, P., Keihänen, E., Kerp, J., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lacasa, F., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Langer, M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leonardi, R., León Tavares, J., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan Robinson, M., Rubinõ Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Serra, P., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Welikala, N., White, M., White, S. D. M., Winkel, B., Yvon, D., Zacchei, A., Zonca, A., Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Anne Lähteenmäki Group, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Department of Physics, Helsinki Institute of Physics, APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Max-Planck-Gesellschaft-Max-Planck-Gesellschaft

Subjects
Large-scale structure of Universe, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Cosmology: observations, Galaxies: star formation, Infrared: diffuse background, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, 01 natural sciences, Luminosity, Cosmic infrared background, 010303 astronomy & astrophysics, Physics, arge-scale structure of Universe, FORMING GALAXIES, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science::Computers and Society, observations [cosmology], Physics::Space Physics, Physical Sciences, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, astro-ph.CO, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), SIMILAR-TO 2, ANGULAR POWER SPECTRA, 100 MU-M, Dark matter, education, FOS: Physical sciences, observation [Cosmology], SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, observations [osmology], star formation [Galaxies], NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, CONDITIONAL LUMINOSITY FUNCTION, 0103 physical sciences, Planck, Astrophysics::Galaxy Astrophysics, Science & Technology, SOUTH-POLE TELESCOPE, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, Star formation, diffuse background [Infrared], Astronomy and Astrophysic, 115 Astronomy, Space science, infrared: diffuse background, Galaxy, Redshift, 0201 Astronomical And Space Sciences, 13. Climate action, DARK-MATTER HALOES, cosmology: observations, galaxies: star formation, FORMATION RATE DENSITY, Bispectrum
Abstract

We present new measurements of cosmic infrared background (CIB) anisotropies using Planck. Combining HFI data with IRAS, the angular auto-and cross-frequency power spectrum is measured from 143 to 3000 GHz, and the auto-bispectrum from 217 to 545 GHz. The total areas used to compute the CIB power spectrum and bispectrum are about 2240 and 4400 deg2, respectively. After careful removal of the contaminants (cosmic microwave background anisotropies, Galactic dust, and Sunyaev-Zeldovich emission), and a complete study of systematics, the CIB power spectrum is measured with unprecedented signal to noise ratio from angular multipoles â.,> ~ 150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from â.,> ~ 130 to 1100, with a total signal to noise ratio of around 6, 19, and 29 at 217, 353, and 545 GHz, respectively. Two approaches are developed for modelling CIB power spectrum anisotropies. The first approach takes advantage of the unique measurements by Planck at large angular scales, and models only the linear part of the power spectrum, with a mean bias of dark matter haloes hosting dusty galaxies at a given redshift weighted by their contribution to the emissivities. The second approach is based on a model that associates star-forming galaxies with dark matter haloes and their subhaloes, using a parametrized relation between the dust-processed infrared luminosity and (sub-)halo mass. The two approaches simultaneously fit all auto-and cross-power spectra very well. We find that the star formation history is well constrained up to redshifts around 2, and agrees with recent estimates of the obscured star-formation density using Spitzer and Herschel. However, at higher redshift, the accuracy of the star formation history measurement is strongly degraded by the uncertainty in the spectral energy distribution of CIB galaxies. We also find that the mean halo mass which is most efficient at hosting star formation is log (Meff/M) = 12.6 and that CIB galaxies have warmer temperatures as redshift increases. The CIB bispectrum is steeper than that expected from the power spectrum, although well fitted by a power law; this gives some information about the contribution of massive haloes to the CIB bispectrum. Finally, we show that the same halo occupation distribution can fit all power spectra simultaneously. The precise measurements enabled by Planck pose new challenges for the modelling of CIB anisotropies, indicating the power of using CIB anisotropies to understand the process of galaxy formation., The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).

31. ASKAP and MeerKAT surveys of the magellanic clouds

Author

Loon, J. Th, Arce, H., Bailey, A., Bains, I., Begum, A., Bekki, K., Bekhti, N. B., Bland-Hawthorn, J., Brooks, K., Brunt, C., Burton, M., Caswell, J., Cunningham, M., Dickey, J., Douglas, K., Ellingsen, S., English, J., Estalella, R., Ford, A., Foster, T., Gaensler, B., Gallagher, J., Gibson, S., Girart, J., Goldsmith, P., Gómez, J. F., Gómez, Y., Green, A., Green, J., Haffner, M., Heiles, C., Heitsch, F., Hennebelle, P., Hirota, T., Hoare, M., Imai, H., Izumiura, H., Joncas, G., Jones, P., Kalberla, P., Kang, J. -H, Kawamura, A., Kerp, J., Kerton, C., Koo, B. -C, Kothes, R., Kurtz, S., Masa Lakicevic, Landecker, T., Lazarian, A., Lo, N., Lockman, F., Magnani, L., Mcclure-Griffiths, N., Menten, K., Migenes, V., Miville-Deschênes, M. -A, Muller, E., Nakagawa, A., Nakanishi, H., Nakashima, J. -I, Nidever, D., Nigra, L., Peek, J., Pérez-Torres, M., Phillips, C., Putman, M., Remijan, A., Richter, P., Schilke, P., Sofue, Y., Stanimirović, S., Tafoya, D., Taylor, R., Tian, W. -W, Uscanga, L., Loon, J., Voronkov, M., Wakker, B., Walsh, A., Westmeier, T., Winkel, B., Zweibel, E., Bagheri, G., Barway, S., Beletsky, Y., Bernard, J. -P, Bietenholz, M., Booth, R., Bot, C., Brinks, E., Cioni, M. -R, Blok, E., Evans, C., Gibson, B., Goedhart, S., Gómez, J., Gordon, K., Haverkorn, M., Holwerda, B., Indebetouw, R., Israel, F., Koribalski, B., Krumholz, M., Lakićević, M., Meixner, M., Oliveira, J., Sarre, P., Sewiło, M., Sibbons, L., Smith, K., Vlemmings, W., Walter, F., Whitelock, P., and Zijlstra, A.

Abstract

The Magellanic Clouds are a stepping stone from the overwhelming detail of the Milky Way in which we are immersed, to the global characteristics of galaxies both in the nearby and distant universe. They are interacting, gas-rich dwarf galaxies of sub-solar metallicity, not unlike the building blocks that assembled the large galaxies that dominate groups and clusters, and representative of the conditions at the height of cosmic star formation. The Square Kilometre Array (SKA) can make huge strides in understanding galactic metabolism and the ecological processes that govern star formation, by observations of the Magellanic Clouds and other, nearby Magellanic-type irregular galaxies. Two programmes with SKA Pathfinders attempt to pave the way: the approved Galactic ASKAP Spectral Line Survey (GASKAP) includes a deep survey in H I and OH of the Magellanic Clouds, whilst MagiKAT is proposed to perform more detailed studies of selected regions within the Magellanic Clouds - also including Faraday rotation measurements and observations at higher frequencies. These surveys also close the gap with the revolutionizing surveys at far-IR wavelengths with the Spitzer Space Telescope and Herschel Space Observatory.

33. Planck 2013 results. I. Overview of products and scientific results

Author

J.-P. Bernard, Niraj Welikala, J. A. Murphy, Benjamin D. Wandelt, Julian Borrill, I. Flores-Cacho, Marc Türler, Pavel Naselsky, R. J. Davis, Jean-Baptiste Melin, Jussi Varis, J. Tuovinen, Olivier Forni, M.-A. Miville-Deschênes, J. Dick, Olivier Doré, Paolo Serra, L. Toffolatti, M. C. Falvella, K. Ganga, S. Leach, Jose M. Diego, Anthony Lasenby, F. K. Hansen, C. Li, E. Keihänen, Alessandro Melchiorri, R. A. Burenin, Alain Benoit, Jens Jasche, Antony Lewis, C. Gauthier, Simon D. M. White, Michael W. Peel, F. Piacentini, O. Fabre, Guilaine Lagache, Soumen Basak, George Helou, A. Mangilli, Ben Rusholme, B. Ruiz-Granados, A.-S. Suur-Uski, R. C. Butler, D. Girard, M. López-Caniego, Hervé Bourdin, Pasquale Mazzotta, C. Renault, E. Falgarone, T. Riller, Diego Molinari, A. Coulais, Pablo Fosalba, A. Moneti, William T. Reach, P. Carvalho, D. Tavagnacco, Anthony R. Pullen, Jose Alberto Rubino-Martin, A. Renzi, D. Herranz, C. Hernández-Monteagudo, C. Watson, E. Pierpaoli, F. Matthai, F. Schiavon, Roberta Paladini, Jeffrey Jewell, D. L. Harrison, B. Gandolfo, J. Aumont, Rafael Rebolo, G. Maggio, Ingunn Kathrine Wehus, M. Tucci, Jussi-Pekka Väliviita, S. Fromenteau, Daniel J. Mortlock, T. J. Pearson, X. Dupac, Jan Hamann, A. Ducout, I. J. O'Dwyer, Michele Liguori, Federico Nati, M. Sandri, Massimiliano Lattanzi, G. Patanchon, J. E. Gallegos, F. Paci, B. Cappellini, Luca Terenzi, R. Carr, Martin White, M. Bucher, Barbara Comis, Jun-Qing Xia, D. Sutton, Mariachiara Rossetti, S. Ricciardi, L. Mendes, C. Combet, Sabino Matarrese, Michael L. Brown, M. Bridges, Douglas Scott, L. Popa, R. Miniscalco, G. de Zotti, F. Cuttaia, Loïc Maurin, I. D. Novikov, B. M. Schaefer, Jörg P. Rachen, J.-M. Delouis, Reijo Keskitalo, Gayoung Chon, E. Franceschi, A. Curto, S. Colombi, Krzysztof M. Gorski, Domenico Marinucci, P. R. Christensen, Eloisa Menegoni, James J. Bock, Paul M. Sutter, G. Prézeau, T. Déchelette, T. Poutanen, Shirley Ho, Jean-François Cardoso, C. J. MacTavish, P. M. McGehee, Richard A. Battye, A. Marcos-Caballero, Anna Bonaldi, Charles R. Lawrence, Peter M. W. Kalberla, Mathieu Langer, Nicolas Ponthieu, S. Donzelli, Marius Millea, O. Perdereau, A. Benoit-Lévy, M. Giard, J. Démoclès, Dmitry Pogosyan, F. Pasian, Davide Pietrobon, Matthieu Roman, Matthias Bartelmann, A. Lavabre, Joanna Dunkley, Magnus Hansen, Erminia Calabrese, B. Racine, J. P. Torre, Marat Gilfanov, I. F. Bikmaev, Xun Chen, B. P. Crill, N. Bartolo, Lung-Yih Chiang, A. Riazuelo, A. Hempel, Alessandro Gruppuso, M. Le Jeune, F. Elsner, C. North, G. Umana, P. de Bernardis, C. Rosset, A. Da Silva, Adam Moss, M. Cruz, Ricardo Genova-Santos, Andrea Zacchei, Anne Lähteenmäki, Luigi Danese, J.-L. Puget, N. Morisset, Tomotake Matsumura, George F. Smoot, Theodore Kisner, Todd Gaier, Calvin B. Netterfield, Emanuele Salerno, Radek Stompor, E. Gjerløw, D. Santos, Giorgio Savini, François R. Bouchet, J. Kerp, S. Osborne, Nicola Vittorio, V. Lindholm, S. Galeotta, M. Tristram, R. Barrena, P. Vielva, Mika Juvela, J.-M. Lamarre, Claude Leroy, R. Kneissl, A. Catalano, Mattia Negrello, Marcella Massardi, G. Polenta, M. Linden-Vørnle, Sarah E. Church, Tarun Souradeep, Rashmikant V. Sudiwala, M. Casale, Ranga-Ram Chary, Jean-Luc Starck, Alexandra S. Rahlin, E. P. S. Shellard, Z. Hou, M. Freschi, F. Couchot, F. Noviello, Hannu Kurki-Suonio, G. Hurier, J. F. Macías-Pérez, G. Castex, Herve Aussel, Kevin M. Huffenberger, David Pearson, Irek Khamitov, L. Vibert, Créidhe O'Sullivan, Francine R. Marleau, James R. Fergusson, Lloyd Knox, Graca Rocha, David L. Clements, Georg Robbers, F. Boulanger, Jochen Weller, S. R. Lowe, J. W. Bowyer, Fabrizio Villa, B. Bertincourt, Marian Douspis, J. P. Zibin, C. Armitage-Caplan, W. A. Holmes, G. Roudier, S. Pandolfi, Hans Böhringer, I. Ristorcelli, Althea Wilkinson, W. C. Jones, M. Rowan-Robinson, M. Ashdown, Hiranya V. Peiris, Matteo Viel, A. B. McDonald, H. K. Eriksen, Silvia Masi, C. Filliard, A. Mennella, Nabila Aghanim, M. Tomasi, Laura Bonavera, E. Martínez-González, M. Frailis, Carlo Baccigalupi, E. Hivon, M. Piat, Douglas J. Marshall, Suzanne Foley, Marco Bersanelli, Alan Heavens, J.-F. Sygnet, Christophe Ringeval, Kendrick M. Smith, L. Sanselme, Luca Valenziano, Michael Seiffert, Andrew R. Liddle, M. Tuttlebee, Duncan Hanson, Stéphane Plaszczynski, R. B. Barreiro, Fernando Atrio-Barandela, K. Kiiveri, Michael P. Hobson, Clive Dickinson, Anthony Challinor, G. Giardino, Jonathan León-Tavares, H. Dole, Subhabrata Mitra, J. A. Tauber, S. Ilić, M. Savelainen, Peter Meinhold, J. González-Nuevo, A. A. Fraisse, B. Van Tent, A. J. Banday, P. Platania, Klaus Dolag, Yabebal Fantaye, D. Texier, A. de Rosa, David Taylor, Locke D. Spencer, J. Knoche, Simon Prunet, P. Bielewicz, M. Reinecke, L. Perotto, E. Churazov, Benjamin Winkel, V. Stolyarov, M. Maris, Bruno Maffei, Martin Kunz, Mathieu Remazeilles, F. Pajot, Marcel Clemens, Jon E. Gudmundsson, L. Pagano, François Orieux, N. Mandolesi, Andrew H. Jaffe, Philip Lubin, J. Kim, Jérôme Bobin, Davide Maino, A. Chamballu, Simona Mei, D. Yvon, W. Hovest, Håkon Dahle, Y. Giraud-Héraud, M. Frommert, R. A. Sunyaev, G. Huey, F. Lacasa, Monique Arnaud, J. P. Leahy, R. D. Davies, Nicole P. H. Nesvadba, Pekka Kangaslahti, K. Benabed, P. B. Lilje, Florent Sureau, J. R. Bond, Tuhin Ghosh, Valeria Pettorino, Jacques Delabrouille, Hans Ulrik Nørgaard-Nielsen, Allan Hornstrup, Etienne Pointecouteau, Jason D. McEwen, René J. Laureijs, Fabio Finelli, Christoph Räth, James G. Bartlett, S. R. Hildebrandt, Carlo Burigana, Sophie Henrot-Versille, Paolo Natoli, L. P. L. Colombo, Dmitry Novikov, L. A. Wade, Daniela Paoletti, Bruce Partridge, C. A. Oxborrow, Dipak Munshi, George Efstathiou, M. I. R. Alves, Peter G. Martin, E. Battaner, K. Mikkelsen, Matthieu Béthermin, Julien Lesgourgues, J. Haissinski, Robert A. Watson, Francesca Perrotta, Torsten A. Enßlin, Serge Gratton, F.-X. Désert, Andrea Zonca, A. Gregorio, H. C. Chiang, T. R. Jaffe, M. Migliaccio, Peter A. R. Ade, P. Paykari, R. Leonardi, Alain Blanchard, S. Galli, G. W. Pratt, Gianluca Morgante, L. Montier, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), PLANCK, APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Tauber, Jan, Ade, P. A. R., Aghanim, N., Alves, M. I. R., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Aussel, H., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Barrena, R., Bartelmann, M., Bartlett, J. G., Bartolo, N., Basak, S., Battaner, E., Battye, R., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bertincourt, B., Bethermin, M., Bielewicz, P., Bikmaev, I., Blanchard, A., Bobin, J., Bock, J. J., Böhringer, H., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bourdin, H., Bowyer, J. W., Bridges, M., Brown, M. L., Bucher, M., Burenin, R., Burigana, C., Butler, R. C., Calabrese, E., Cappellini, B., Cardoso, J. F., Carr, R., Carvalho, P., Casale, M., Castex, G., Catalano, A., Challinor, A., Chamballu, A., Chary, R. R., Chen, X., Chiang, H. C., Chiang, L. Y., Chon, G., Christensen, P. R., Churazov, E., Church, S., Clemens, M., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Comis, B., Couchot, F., Coulais, A., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Déchelette, T., Delabrouille, J., Delouis, J. M., Démoclès, J., Désert, F. X., Dick, J., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dunkley, J., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fabre, O., Falgarone, E., Falvella, M. C., Fantaye, Y., Fergusson, J., Filliard, C., Finelli, F., Flores Cacho, I., Foley, S., Forni, O., Fosalba, P., Frailis, M., Fraisse, A. A., Franceschi, E., Freschi, M., Fromenteau, S., Frommert, M., Gaier, T. C., Galeotta, S., Gallegos, J., Galli, S., Gandolfo, B., Ganga, K., Gauthier, C., Génova Santos, R. T., Ghosh, T., Giard, M., Giardino, G., Gilfanov, M., Girard, D., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Gudmundsson, J. E., Haissinski, J., Hamann, J., Hansen, F. K., Hansen, M., Hanson, D., Harrison, D. L., Heavens, A., Helou, G., Hempel, A., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Ho, S., Hobson, M., Holmes, W. A., Hornstrup, A., Hou, Z., Hovest, W., Huey, G., Huffenberger, K. M., Hurier, G., Ilić, S., Jaffe, A. H., Jaffe, T. R., Jasche, J., Jewell, J., Jones, W. C., Juvela, M., Kalberla, P., Kangaslahti, P., Keihänen, E., Kerp, J., Keskitalo, R., Khamitov, I., Kiiveri, K., Kim, J., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lacasa, F., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Langer, M., Lasenby, A., Lattanzi, M., Laureijs, R. J., Lavabre, A., Lawrence, C. R., Le Jeune, M., Leach, S., Leahy, J. P., Leonardi, R., León Tavares, J., Leroy, C., Lesgourgues, J., Lewis, A., Li, C., Liddle, A., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lowe, S., Lubin, P. M., Maciás Pérez, J. F., Mactavish, C. J., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos Caballero, A., Marinucci, D., Maris, M., Marleau, F., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matsumura, T., Matthai, F., Maurin, L., Mazzotta, P., Mcdonald, A., Mcewen, J. D., Mcgehee, P., Mei, S., Meinhold, P. R., Melchiorri, A., Melin, J. B., Mendes, L., Menegoni, E., Mennella, A., Migliaccio, M., Mikkelsen, K., Millea, M., Miniscalco, R., Mitra, S., Miville Deschênes, M. A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Negrello, M., Nesvadba, N. P. H., Netterfield, C. B., Nørgaard Nielsen, H. U., North, C., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Orieux, F., Osborne, S., O'Sullivan, C., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Pandolfi, S., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Paykari, P., Pearson, D., Pearson, T. J., Peel, M., Peiris, H. V., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Platania, P., Pogosyan, D., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Pullen, A. R., Rachen, J. P., Racine, B., Rahlin, A., Räth, C., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Riazuelo, A., Ricciardi, S., Riller, T., Ringeval, C., Ristorcelli, I., Robbers, G., Rocha, G., Roman, M., Rosset, C., Rossetti, M., Roudier, G., Rowan Robinson, M., Rubinõ Martín, J. A., Ruiz Granados, B., Rusholme, B., Salerno, E., Sandri, M., Sanselme, L., Santos, D., Savelainen, M., Savini, G., Schaefer, B. M., Schiavon, F., Scott, D., Seiffert, M. D., Serra, P., Shellard, E. P. S., Smith, K., Smoot, G. F., Souradeep, T., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutter, P., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Taylor, D., Terenzi, L., Texier, D., Toffolatti, L., Tomasi, M., Torre, J. P., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Tuttlebee, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vibert, L., Viel, M., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, C., Watson, R., Wehus, I. K., Welikala, N., Weller, J., White, M., White, S. D. M., Wilkinson, A., Winkel, B., Xia, J. Q., Yvon, D., Zacchei, A., Zibin, J. P., Zonca, A., Universidad de Cantabria, Ade, P, Aghanim, N, Alves, M, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Aussel, H, Baccigalupi, C, Banday, A, Barreiro, R, Barrena, R, Bartelmann, M, Bartlett, J, Bartolo, N, Basak, S, Battaner, E, Battye, R, Benabed, K, Benoît, A, Benoit-Lévy, A, Bernard, J, Bersanelli, M, Bertincourt, B, Bethermin, M, Bielewicz, P, Bikmaev, I, Blanchard, A, Bobin, J, Bock, J, Böhringer, H, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bourdin, H, Bowyer, J, Bridges, M, Brown, M, Bucher, M, Burenin, R, Burigana, C, Butler, R, Calabrese, E, Cappellini, B, Cardoso, J, Carr, R, Carvalho, P, Casale, M, Castex, G, Catalano, A, Challinor, A, Chamballu, A, Chary, R, Chen, X, Chiang, H, Chiang, L, Chon, G, Christensen, P, Churazov, E, Church, S, Clemens, M, Clements, D, Colombi, S, Colombo, L, Combet, C, Comis, B, Couchot, F, Coulais, A, Crill, B, Cruz, M, Curto, A, Cuttaia, F, Da Silva, A, Dahle, H, Danese, L, Davies, R, Davis, R, de Bernardis, P, de Rosa, A, de Zotti, G, Déchelette, T, Delabrouille, J, Delouis, J, Démoclès, J, Désert, F, Dick, J, Dickinson, C, Diego, J, Dolag, K, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dunkley, J, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, T, Eriksen, H, Fabre, O, Falgarone, E, Falvella, M, Fantaye, Y, Fergusson, J, Filliard, C, Finelli, F, Flores-Cacho, I, Foley, S, Forni, O, Fosalba, P, Frailis, M, Fraisse, A, Franceschi, E, Freschi, M, Fromenteau, S, Frommert, M, Gaier, T, Galeotta, S, Gallegos, J, Galli, S, Gandolfo, B, Ganga, K, Gauthier, C, Génova-Santos, R, Ghosh, T, Giard, M, Giardino, G, Gilfanov, M, Girard, D, Giraud-Héraud, Y, Gjerløw, E, González-Nuevo, J, Górski, K, Gratton, S, Gregorio, A, Gruppuso, A, Gudmundsson, J, Haissinski, J, Hamann, J, Hansen, F, Hansen, M, Hanson, D, Harrison, D, Heavens, A, Helou, G, Hempel, A, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Ho, S, Hobson, M, Holmes, W, Hornstrup, A, Hou, Z, Hovest, W, Huey, G, Huffenberger, K, Hurier, G, Ilić, S, Jaffe, A, Jaffe, T, Jasche, J, Jewell, J, Jones, W, Juvela, M, Kalberla, P, Kangaslahti, P, Keihänen, E, Kerp, J, Keskitalo, R, Khamitov, I, Kiiveri, K, Kim, J, Kisner, T, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lacasa, F, Lagache, G, Lähteenmäki, A, Lamarre, J, Langer, M, Lasenby, A, Lattanzi, M, Laureijs, R, Lavabre, A, Lawrence, C, Le Jeune, M, Leach, S, Leahy, J, Leonardi, R, León-Tavares, J, Leroy, C, Lesgourgues, J, Lewis, A, Li, C, Liddle, A, Liguori, M, Lilje, P, Linden-Vørnle, M, Lindholm, V, López-Caniego, M, Lowe, S, Lubin, P, Macías-Pérez, J, Mactavish, C, Maffei, B, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Marcos-Caballero, A, Marinucci, D, Maris, M, Marleau, F, Marshall, D, Martin, P, Martínez-González, E, Masi, S, Massardi, M, Matarrese, S, Matsumura, T, Matthai, F, Maurin, L, Mazzotta, P, Mcdonald, A, Mcewen, J, Mcgehee, P, Mei, S, Meinhold, P, Melchiorri, A, Melin, J, Mendes, L, Menegoni, E, Mennella, A, Migliaccio, M, Mikkelsen, K, Millea, M, Miniscalco, R, Mitra, S, Miville-Deschênes, M, Molinari, D, Moneti, A, Montier, L, Morgante, G, Morisset, N, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Negrello, M, Nesvadba, N, Netterfield, C, Nørgaard-Nielsen, H, North, C, Noviello, F, Novikov, D, Novikov, I, O’Dwyer, I, Orieux, F, Osborne, S, O’Sullivan, C, Oxborrow, C, Paci, F, Pagano, L, Pajot, F, Paladini, R, Pandolfi, S, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Paykari, P, Pearson, D, Pearson, T, Peel, M, Peiris, H, Perdereau, O, Perotto, L, Perrotta, F, Pettorino, V, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Platania, P, Pogosyan, D, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prézeau, G, Prunet, S, Puget, J, Pullen, A, Rachen, J, Racine, B, Rahlin, A, Räth, C, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Riazuelo, A, Ricciardi, S, Riller, T, Ringeval, C, Ristorcelli, I, Robbers, G, Rocha, G, Roman, M, Rosset, C, Rossetti, M, Roudier, G, Rowan-Robinson, M, Rubiño-Martín, J, Ruiz-Granados, B, Rusholme, B, Salerno, E, Sandri, M, Sanselme, L, Santos, D, Savelainen, M, Savini, G, Schaefer, B, Schiavon, F, Scott, D, Seiffert, M, Serra, P, Shellard, E, Smith, K, Smoot, G, Souradeep, T, Spencer, L, Starck, J, Stolyarov, V, Stompor, R, Sudiwala, R, Sunyaev, R, Sureau, F, Sutter, P, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Tavagnacco, D, Taylor, D, Terenzi, L, Texier, D, Toffolatti, L, Tomasi, M, Torre, J, Tristram, M, Tucci, M, Tuovinen, J, Türler, M, Tuttlebee, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Varis, J, Vibert, L, Viel, M, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, Watson, C, Watson, R, Wehus, I, Welikala, N, Weller, J, White, M, White, S, Wilkinson, A, Winkel, B, Xia, J, Yvon, D, Zacchei, A, Zibin, J, Zonca, A, Department of Physics, and Helsinki Institute of Physics

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Cosmic microwave background, cosmic microwave backgrounds, Astrophysics, cosmic background radiation, Surveys, CMB, power spectrum, Cosmic background radiation, 7. Clean energy, european space agency, Cosmology, atacama cosmology telescope, space vehicles: instruments, observations [Cosmology], sunyaev-zeldovich effects, detectors [Instrumentation], QB, pre-launch status, instrumentation, Physics, data release, [PHYS]Physics [physics], Instrumentation: detector, Astrophysics::Instrumentation and Methods for Astrophysics, probe wmap observations, microwave background maps, CMB cold spot, Computer Science::Computers and Society, damping tail, component separation, Physics::Space Physics, Physical Sciences, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, symbols, detector [Instrumentation], Baryon acoustic oscillations, Neutrino, hubble-space-telescope, galaxy cluster survey, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: observations, Instrumentation: detectors, Space vehicles: instruments, Astronomy and Astrophysics, Space and Planetary Science, education, gravitational lensing, FOS: Physical sciences, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, in-flight performance, Astronomy & Astrophysics, Space vehicles: instrument, Computer Science::Digital Libraries, NO, instruments [Space vehicles], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, instrument [Space vehicles], systematic uncertainties, Planck, Forschungsgruppe Komplexe Plasmen, extragalactic point sources, Science & Technology, cosmology: observation, instrumentation: detectors, Astronomy and Astrophysic, 115 Astronomy, Space science, Settore MAT/06 - Probabilita' e Statistica Matematica, Gravitational lens, [SDU]Sciences of the Universe [physics], cosmology: observations, space vehicles, south-pole telescope, cosmology, Hubble's law
Abstract

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., Centre National D'etudes Spatiales, CNRS/INSU-IN2P3, Italian Space Agency (ASI), Danish Natural Science Research Council, European Space Agency, CNRS/INSU-IN2P3-INP (France), Italian National Research Council, Istituto Nazionale Astrofisica (INAF), National Aeronautics & Space Administration (NASA), United States Department of Energy (DOE), Science & Technology Facilities Council (STFC), UKSA (UK), Consejo Superior de Investigaciones Cientificas (CSIC), Spanish Government, JA (Spain), Finnish Funding Agency for Technology & Innovation (TEKES), AoF (Finland), CSC (Finland), Helmholtz Association, German Aerospace Centre (DLR), Max Planck Society, CSA (Canada), DTU Space (Denmark), SER/SSO (Switzerland), RCN (Norway), Science Foundation Ireland, Portuguese Foundation for Science and Technology, European Union (EU), Science & Technology Facilities Council (STFC) ST/I002006/1 ST/J000388/1 ST/H001239/1 ST/K000977/1 ST/K002805/1 ST/J001368/1 ST/K00333X/1 ST/I005129/1 ST/J005673/1 ST/K003674/1 ST/L000768/1 ST/G003874/1 ST/H008586/1 ST/L001314/1 ST/K004131/1 ST/M007685/1 ST/K000985/1 ST/K001051/1 ST/K00106X/1 ST/I005765/1 ST/K002899/1 ST/J004812/1

Published
2014

34. Genome-wide association analyses identify novel Brugada syndrome risk loci and highlight a new mechanism of sodium channel regulation in disease susceptibility

Author

Barc, Julien, Tadros, Rafik, Glinge, Charlotte, Chiang, David Y., Jouni, Mariam, Simonet, Floriane, Jurgens, Sean J., Baudic, Manon, Nicastro, Michele, Potet, Franck, Offerhaus, Joost A., Walsh, Roddy, Choi, Seung Hoan, Verkerk, Arie O., Mizusawa, Yuka, Anys, Soraya, Minois, Damien, Arnaud, Marine, Duchateau, Josselin, Wijeyeratne, Yanushi D., Muir, Alison, Papadakis, Michael, Castelletti, Silvia, Torchio, Margherita, Ortuño, Cristina Gil, Lacunza, Javier, Giachino, Daniela F., Cerrato, Natascia, Martins, Raphaël P., Campuzano, Oscar, Van Dooren, Sonia, Thollet, Aurélie, Kyndt, Florence, Mazzanti, Andrea, Clémenty, Nicolas, Bisson, Arnaud, Corveleyn, Anniek, Stallmeyer, Birgit, Dittmann, Sven, Saenen, Johan, Noël, Antoine, Honarbakhsh, Shohreh, Rudic, Boris, Marzak, Halim, Rowe, Matthew K., Federspiel, Claire, Le Page, Sophie, Placide, Leslie, Milhem, Antoine, Barajas-Martinez, Hector, Beckmann, Britt-Maria, Krapels, Ingrid P., Steinfurt, Johannes, Winkel, Bo Gregers, Jabbari, Reza, Shoemaker, Moore B., Boukens, Bas J., Škorić-Milosavljević, Doris, Bikker, Hennie, Manevy, Federico, Lichtner, Peter, Ribasés, Marta, Meitinger, Thomas, Müller-Nurasyid, Martina, Strauch, Konstantin, Peters, Annette, Schulz, Holger, Schwettmann, Lars, Leidl, Reiner, Heier, Margit, Veldink, Jan H., van den Berg, Leonard H., Van Damme, Philip, Cusi, Daniele, Lanzani, Chiara, Rigade, Sidwell, Charpentier, Eric, Baron, Estelle, Bonnaud, Stéphanie, Lecointe, Simon, Donnart, Audrey, Le Marec, Hervé, Chatel, Stéphanie, Karakachoff, Matilde, Bézieau, Stéphane, London, Barry, Tfelt-Hansen, Jacob, Roden, Dan, Odening, Katja E., Cerrone, Marina, Chinitz, Larry A., Volders, Paul G., van de Berg, Maarten P., Laurent, Gabriel, Faivre, Laurence, Antzelevitch, Charles, Kääb, Stefan, Arnaout, Alain Al, Dupuis, Jean-Marc, Pasquie, Jean-Luc, Billon, Olivier, Roberts, Jason D., Jesel, Laurence, Borggrefe, Martin, Lambiase, Pier D., Mansourati, Jacques, Loeys, Bart, Leenhardt, Antoine, Guicheney, Pascale, Maury, Philippe, Schulze-Bahr, Eric, Robyns, Tomas, Breckpot, Jeroen, Babuty, Dominique, Priori, Silvia G., Napolitano, Carlo, Defaye, Pascal, Anselme, Frédéric, Darmon, Jean Philippe, Wiart, François, de Asmundis, Carlo, Brugada, Pedro, Brugada, Ramon, Arbelo, Elena, Brugada, Josep, Mabo, Philippe, Behar, Nathalie, Giustetto, Carla, Molina, Maria Sabater, Gimeno, Juan R., Hasdemir, Can, Schwartz, Peter J., Crotti, Lia, McKeown, Pascal P., Sharma, Sanjay, Behr, Elijah R., Haissaguerre, Michel, Sacher, Frédéric, Rooryck, Caroline, Tan, Hanno L., Remme, Carol A., Postema, Pieter G., Delmar, Mario, Ellinor, Patrick T., Lubitz, Steven A., Gourraud, Jean-Baptiste, Tanck, Michael W., George, Alfred L., MacRae, Calum A., Burridge, Paul W., Dina, Christian, Probst, Vincent, Wilde, Arthur A., Schott, Jean-Jacques, Redon, Richard, Bezzina, Connie R., KORA-Study Group, Nantes Referral Ctr Inherited Card, unité de recherche de l'institut du thorax UMR1087 UMR6291 (ITX), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Nantes Université - UFR de Médecine et des Techniques Médicales (Nantes Univ - UFR MEDECINE), Nantes Université - pôle Santé, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Santé, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Centre de recherche Cardio-Thoracique de Bordeaux [Bordeaux] (CRCTB), Université Bordeaux Segalen - Bordeaux 2-CHU Bordeaux [Bordeaux]-Institut National de la Santé et de la Recherche Médicale (INSERM), CHU Pontchaillou [Rennes], Laboratoire Traitement du Signal et de l'Image (LTSI), Université de Rennes (UR)-Institut National de la Santé et de la Recherche Médicale (INSERM), Santé - François Bonamy, Université de Nantes (UN)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche en Santé de l'Université de Nantes (IRS-UN)-Centre hospitalier universitaire de Nantes (CHU Nantes), Physiologie & médecine expérimentale du Cœur et des Muscles [U 1046] (PhyMedExp), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier), Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Research Unit on Cardiovascular and Metabolic Diseases (ICAN), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Sorbonne Université (SU)-Institut de Cardiométabolisme et Nutrition = Institute of Cardiometabolism and Nutrition [CHU Pitié Salpêtrière] (IHU ICAN), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Laboratoire Maladies Rares: Génétique et Métabolisme (Bordeaux) (U1211 INSERM/MRGM), Université de Bordeaux (UB)-Groupe hospitalier Pellegrin-Institut National de la Santé et de la Recherche Médicale (INSERM), Amsterdam UMC - Amsterdam University Medical Center, The MINE study (J.H.V.) has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement no. 772376—EScORIAL). The collaboration project is cofunded by the PPP Allowance made available by Health~Holland, Top Sector Life Sciences & Health, to stimulate public–private partnerships. This study makes use of data generated by the Wellcome Trust Case-Control Consortium. A full list of the investigators who contributed to the generation of the data is available from www.wtccc.org.uk. Funding for the project was provided by the Wellcome Trust under award 076113, 085475 and 090355. The KORA research platform (KORA, Cooperative Research in the Region of Augsburg) was initiated and financed by the Helmholtz Zentrum München—German Research Center for Environmental Health, which is funded by the German Federal Ministry of Education and Research and by the State of Bavaria. Furthermore, KORA research was supported within the Munich Center of Health Sciences (MC Health), Ludwig-Maximilians-Universität, as part of LMUinnovativ. J. Barc is supported by the research program Etoiles montantes des Pays de la Loire REGIOCARD RPH081-U1087-REG-PDL, ANR JCJC LEARN (R21006NN, RPV21014NNA) and by the H2020-MSCA-IF-2014 Program of the European Commission (RISTRAD-661617). R.T. is supported by the Canadian Heart Rhythm Society’s George Mines Award, the European Society of Cardiology research award, and the Philippa and Marvin Carsley Cardiology Chair. D.Y.C. is supported by Fondation Leducq and National Institutes of Health (NIH) NHGRI T32 (no. 1T32HG010464-01). M. Baudic was supported by IRP—VERACITIES—New Mechanisms for VEntricular ARrhythmia And CardIomeTabolic DIseasES, an I-SITE NExT health and engineering initiative (Ecole Centrale and Nantes University) and by the IRP—GAINES—Genetic Architecture IN cardiovascular disEaSes funded by INSERM and CNRS. R.W. is supported by an Amsterdam Cardiovascular Sciences fellowship. S.C. is supported by the NHLBI BioData Catalyst Fellows Program. C.A.R. is supported by Fondation Leducq, the Dutch Heart Foundation (CVON PREDICT2) and the Innovational Research Incentives Scheme Vidi grant from the Netherlands Organisation for Health Research and Development (ZonMw, 91714371). Y.D.W. is supported by the Robert Lancaster Memorial Fund. M.P. is supported by Cardiac Risk in the Young. S.V.D. is supported by Wetenschappelijk Fonds Willy Gepts VUB-UZ Brussel, project ‘Unravelling the molecular genetic pathways of Brugada Syndrome by cardiomics research’, VUB IRP project ‘IMAGica: an Integrative personalized Medical Approach for Genetic diseases, Inherited Cardia Arrhythmias as a model’ and Innoviris BRIDGE 2017, project ‘IGenCare: Integrated Personalised Medical Genomics Care Solution for Patients with Rare Genetic Diseases’. S.H. is supported by the Barts BRC. B.R. is supported by the DZHK (German Centre for Cardiovascular Research) and by the BMBF (German Ministry of Education and Research). B.G.W. is supported by the Danish Heart Foundation. M.B.S. is supported by K23HL127704. Project MinE Belgium was supported by a grant from IWT (no. 140935), the ALS Liga België, the National Lottery of Belgium and the KU Leuven Opening the Future Fund. D.C. and C.L. are supported by HYPERGENES (HEALTH-F4-2007). D.R. is supported by R01 HL149826, P50 GM115305. P.J.S. acknowledges the support of Leducq Foundation for Cardiovascular Research grant 18CVD05. P.V.D. is supported by the Netherlands CardioVascular Research Initiative (CVON PREDICT2). C.A. is supported by NIH HL47678 and HL138103, W.W. Smith Charitable Trust and Wistar Morris Fund. M.B. is Supported by the DZHK (German Centre for Cardiovascular Research) and by the BMBF (German Ministry of Education and Research). P.D.L. is supported by UCL/UCLH Biomedicine NIHR and Barts BRC. B.L. is supported by GOA—Antigone 33933. J.B. is supported by a Senior Clinical Fellowship of the Flemish Science Foundation (FWO). E.B. is supported by the British Heart Foundation including BHF Clinical Research Training Fellowship (FS/11/71/28918: Future diagnostic role and new genetic loci in SADS), Cardiac Risk in the Young and Robert Lancaster Memorial fund sponsored by McColl’s Ltd. Retail Group. H.L.T. is supported by the European Union’s Horizon 2020 research and innovation program under acronym ESCAPE-NET, registered under grant agreement no. 733381, and the Dutch Heart Foundation (CVON RESCUED and PREDICT2 projects). M.D. is supported by NIH-RO1 HL134328. P.T.E. was supported by the Fondation Leducq (14CVD01), the NIH (1RO1HL092577, R01HL128914, K24HL105780), the American Heart Association (18SFRN34110082) and by a research grant from Bayer AG to the Broad Institute. S.A.L. is supported by NIH grant 1R01HL139731 and American Heart Association 18SFRN34250007. J.-B.G. received a grant from the Fédération Française de Cardiologie (PREVENT project). A.L.G. is supported by the Fondation Leducq. C.A.M.R. is supported by the Leducq Foundation and Burroughs Wellecome Fund. A.A.W. is supported by the Dutch Heart Foundation (CVON PREDICT2 project). J.-J.S. is supported by the Fondation pour la Recherche Médicale (DEQ20140329545). R.R. and P.G. are supported by the National Agency for Research (ANR-GENSUD-14-CE10-0001). C.R.B. is supported by the Dutch Heart Foundation (CVON PREDICT2 project), the Netherlands Organization for Scientific Research (VICI fellowship, 016.150.610) and Fondation Leducq (17CVD02)., Barc, J, Tadros, R, Glinge, C, Chiang, D, Jouni, M, Simonet, F, Jurgens, S, Baudic, M, Nicastro, M, Potet, F, Offerhaus, J, Walsh, R, Hoan Choi, S, Verkerk, A, Mizusawa, Y, Anys, S, Minois, D, Arnaud, M, Duchateau, J, Wijeyeratne, Y, Muir, A, Papadakis, M, Castelletti, S, Torchio, M, Gil Ortuño, C, Lacunza, J, Giachino, D, Cerrato, N, Martins, R, Campuzano, O, Van Dooren, S, Thollet, A, Kyndt, F, Mazzanti, A, Clémenty, N, Bisson, A, Corveleyn, A, Stallmeyer, B, Dittmann, S, Saenen, J, Noël, A, Honarbakhsh, S, Rudic, B, Marzak, H, Rowe, M, Federspiel, C, Le Page, S, Placide, L, Milhem, A, Barajas-Martinez, H, Beckmann, B, Krapels, I, Steinfurt, J, Gregers Winkel, B, Jabbari, R, Shoemaker, M, Boukens, B, Škorić-Milosavljević, D, Bikker, H, Manevy, F, Lichtner, P, Ribasés, M, Meitinger, T, Müller-Nurasyid, M, Group, K, Veldink, J, van den Berg, L, Van Damme, P, Cusi, D, Lanzani, C, Rigade, S, Charpentier, E, Baron, E, Bonnaud, S, Lecointe, S, Donnart, A, Le Marec, H, Chatel, S, Karakachoff, M, Bézieau, S, London, B, Tfelt-Hansen, J, Roden, D, Odening, K, Cerrone, M, Chinitz, L, Volders, P, van de Berg, M, Laurent, G, Faivre, L, Antzelevitch, C, Kääb, S, Al Arnaout, A, Dupuis, J, Pasquie, J, Billon, O, Roberts, J, Jesel, L, Borggrefe, M, Lambiase, P, Mansourati, J, Loeys, B, Leenhardt, A, Guicheney, P, Maury, P, Schulze-Bahr, E, Robyns, T, Breckpot, J, Babuty, D, Priori, S, Napolitano, C, Referral Center for inherited cardiac arrhythmia, N, de Asmundis, C, Brugada, P, Brugada, R, Arbelo, E, Brugada, J, Mabo, P, Behar, N, Giustetto, C, Sabater Molina, M, Gimeno, J, Hasdemir, C, Schwartz, P, Crotti, L, Mckeown, P, Sharma, S, Behr, E, Haissaguerre, M, Sacher, F, Rooryck, C, Tan, H, Remme, C, Postema, P, Delmar, M, Ellinor, P, Lubitz, S, Gourraud, J, Tanck, M, L. George Jr., A, Macrae, C, Burridge, P, Dina, C, Probst, V, Wilde, A, Schott, J, Redon &amp, R, Bezzina, C, Cardiology, Graduate School, Medical Biology, ACS - Amsterdam Cardiovascular Sciences, ACS - Heart failure & arrhythmias, Human Genetics, ACS - Pulmonary hypertension & thrombosis, ARD - Amsterdam Reproduction and Development, APH - Methodology, Epidemiology and Data Science, MUMC+: DA KG Polikliniek (9), RS: Carim - H02 Cardiomyopathy, Cardiologie, MUMC+: MA Med Staf Spec Cardiologie (9), RS: Carim - H04 Arrhythmogenesis and cardiogenetics, and Cardiovascular Centre (CVC)

Subjects
EXPRESSION, [SDV]Life Sciences [q-bio], DIAGNOSIS, GUIDELINES, ANNOTATION, Article, NAV1.5 Voltage-Gated Sodium Channel, Young Adult, MANAGEMENT, Genetics, GWAS, Humans, Genetic Predisposition to Disease, 610 Medicine & health, SCN5A, Alleles, Brugada Syndrome, Allele, [SDV.GEN]Life Sciences [q-bio]/Genetics, HERITABILITY, Microtubule-Associated Protein, Brugada Syndrome, GWAS, SNPs, COMMON VARIANTS, Mutation, Disease Susceptibility, Human medicine, ENRICHMENT, Microtubule-Associated Proteins, SNPs, Human, GENERATION, Genome-Wide Association Study
Abstract

Brugada syndrome (BrS) is a cardiac arrhythmia disorder associated with sudden death in young adults. With the exception of SCN5A, encoding the cardiac sodium channel Na(V)1.5, susceptibility genes remain largely unknown. Here we performed a genome-wide association meta-analysis comprising 2,820 unrelated cases with BrS and 10,001 controls, and identified 21 association signals at 12 loci (10 new). Single nucleotide polymorphism (SNP)-heritability estimates indicate a strong polygenic influence. Polygenic risk score analyses based on the 21 susceptibility variants demonstrate varying cumulative contribution of common risk alleles among different patient subgroups, as well as genetic associations with cardiac electrical traits and disorders in the general population. The predominance of cardiac transcription factor loci indicates that transcriptional regulation is a key feature of BrS pathogenesis. Furthermore, functional studies conducted on MAPRE2, encoding the microtubule plus-end binding protein EB2, point to microtubule-related trafficking effects on Na(V)1.5 expression as a new underlying molecular mechanism. Taken together, these findings broaden our understanding of the genetic architecture of BrS and provide new insights into its molecular underpinnings. Genome-wide association analyses identify new susceptibility loci for Brugada syndrome. Functional studies implicate microtubule-related trafficking effects on sodium channel expression as an underlying molecular mechanism., European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program [772376-EScORIAL]; Health~Holland; Top Sector Life Sciences Health; Wellcome Trust [076113, 085475, 090355]; Helmholtz Zentrum Munchen-German Research Center for Environmental Health - German Federal Ministry of Education and Research; State of Bavaria; Munich Center of Health Sciences (MC Health), Ludwig-Maximilians-Universitat, as part of LMUinnovativ; research program Etoiles montantes des Pays de la Loire [REGIOCARD RPH081-U1087-REG-PDL]; ANR JCJC LEARN [R21006NN, RPV21014NNA]; H2020-MSCA-IF-2014 Program of the European Commission [RISTRAD-661617]; Canadian Heart Rhythm Society's George Mines Award; European Society of Cardiology research award; Philippa and Marvin Carsley Cardiology Chair; Fondation Leducq; National Institutes of Health (NIH) NHGRI T32 [1T32HG010464-01]; IRP-VERACITIES-New Mechanisms for VEntricular ARrhythmia And CardIomeTabolic DIseasES an I-SITE NExT health and engineering initiative (Ecole Centrale); IRP-VERACITIES-New Mechanisms for VEntricular ARrhythmia And CardIomeTabolic DIseasES an I-SITE NExT health and engineering initiative (Nantes University); IRP-GAINES-Genetic Architecture IN cardiovascular disEaSes - INSERM; CNRS; Amsterdam Cardiovascular Sciences fellowship; NHLBI BioData Catalyst Fellows Program; Dutch Heart Foundation [CVON PREDICT2]; Innovational Research Incentives Scheme Vidi grant from the Netherlands Organisation for Health Research and Development (ZonMw) [91714371]; Robert Lancaster Memorial Fund; Cardiac Risk in the Young; Wetenschappelijk Fonds Willy Gepts VUB-UZ Brussel; VUB IRP project `IMAGica: an Integrative personalized Medical Approach for Genetic diseases, Inherited Cardia Arrhythmias as a model' and Innoviris BRIDGE 2017; project `IGenCare: Integrated Personalised Medical Genomics Care Solution for Patients with Rare Genetic Diseases'; Barts BRC; DZHK (German Centre for Cardiovascular Research); BMBF (German Ministry of Education and Research); Danish Heart Foundation; IWT [140935]; ALS Liga Belgie; National Lottery of Belgium; KU Leuven Opening the Future Fund; HYPERGENES [HEALTH-F4-2007]; Leducq Foundation for Cardiovascular Research grant [18CVD05]; Netherlands CardioVascular Research Initiative [CVON PREDICT2]; NIH [HL47678, HL138103, 1RO1HL092577, R01HL128914, K24HL105780]; W.W. Smith Charitable Trust; Wistar Morris Fund; GOA-Antigone [33933]; Senior Clinical Fellowship of the Flemish Science Foundation (FWO); British Heart Foundation; BHF Clinical Research Training Fellowship [FS/11/71/28918]; Cardiac Risk in the Young and Robert Lancaster Memorial fund - McColl's Ltd. Retail Group; European Union's Horizon 2020 research and innovation program under acronym ESCAPE-NET [733381]; Dutch Heart Foundation; Fondation Leducq [14CVD01, 17CVD02]; American Heart Association [18SFRN34110082, 18SFRN34250007]; Bayer AG; NIH grant [1R01HL139731]; Federation Francaise de Cardiologie (PREVENT project); Leducq Foundation; Burroughs Wellecome Fund; Fondation pour la Recherche Medicale [DEQ20140329545]; National Agency for Research [ANR-GENSUD-14-CE10-0001]; Netherlands Organization for Scientific Research (VICI fellowship) [016.150.610]; [K23HL127704]; [R01 HL149826]; [P50 GM115305]; [NIH-RO1 HL134328], We are greatly indebted to the patients included in the study. We thank V. Cotard, C. Goutsmedt, M.-F. Le Cunff and N. Bourgeais for assistance in patient recruitment and L. Beekman for his technical support. We thank the biological resource centre for biobanking (CHU Nantes, Nantes Universite, Centre de ressources biologiques (BB0033-00040), F-44000 Nantes, France) for applying the following guidelines68. We are most grateful to the Genomics and Bioinformatics Core Facility of Nantes (GenoBiRD, Biogenouest, IFB) for its technical support. This research has been conducted using the UK Biobank resource; we are grateful to UK Biobank participants. The MINE study (J.H.V.) has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement no. 772376-EScORIAL). The collaboration project is cofunded by the PPP Allowance made available by Health~Holland, Top Sector Life Sciences & Health, to stimulate public-private partnerships. This study makes use of data generated by the Wellcome Trust Case-Control Consortium. A full list of the investigators who contributed to the generation of the data is available from www.wtccc.org.uk.Funding for the project was provided by the Wellcome Trust under award 076113, 085475 and 090355. The KORA research platform (KORA, Cooperative Research in the Region of Augsburg) was initiated and financed by the Helmholtz Zentrum Munchen-German Research Center for Environmental Health, which is funded by the German Federal Ministry of Education and Research and by the State of Bavaria. Furthermore, KORA research was supported within the Munich Center of Health Sciences (MC Health), Ludwig-Maximilians-Universitat, as part of LMUinnovativ. J. Barc is supported by the research program Etoiles montantes des Pays de la Loire REGIOCARD RPH081-U1087-REG-PDL, ANR JCJC LEARN (R21006NN, RPV21014NNA) and by the H2020-MSCA-IF-2014 Program of the European Commission (RISTRAD-661617). R.T. is supported by the Canadian Heart Rhythm Society's George Mines Award, the European Society of Cardiology research award, and the Philippa and Marvin Carsley Cardiology Chair. D.Y.C. is supported by Fondation Leducq and National Institutes of Health (NIH) NHGRI T32 (no. 1T32HG010464-01). M. Baudic was supported by IRP-VERACITIES-New Mechanisms for VEntricular ARrhythmia And CardIomeTabolic DIseasES, an I-SITE NExT health and engineering initiative (Ecole Centrale and Nantes University) and by the IRP-GAINES-Genetic Architecture IN cardiovascular disEaSes funded by INSERM and CNRS. R.W. is supported by an Amsterdam Cardiovascular Sciences fellowship. S.C. is supported by the NHLBI BioData Catalyst Fellows Program. C.A.R. is supported by Fondation Leducq, the Dutch Heart Foundation (CVON PREDICT2) and the Innovational Research Incentives Scheme Vidi grant from the Netherlands Organisation for Health Research and Development (ZonMw; 91714371). Y.D.W. is supported by the Robert Lancaster Memorial Fund. M.P. is supported by Cardiac Risk in the Young. S.V.D. is supported by Wetenschappelijk Fonds Willy Gepts VUB-UZ Brussel, project `Unravelling the molecular genetic pathways of Brugada Syndrome by cardiomics research', VUB IRP project `IMAGica: an Integrative personalized Medical Approach for Genetic diseases, Inherited Cardia Arrhythmias as a model' and Innoviris BRIDGE 2017, project `IGenCare: Integrated Personalised Medical Genomics Care Solution for Patients with Rare Genetic Diseases'. S.H. is supported by the Barts BRC. B.R.; is supported by the DZHK (German Centre for Cardiovascular Research) and by the BMBF (German Ministry of Education and Research). B.G.W. is supported by the Danish Heart Foundation. M.B.S. is supported by K23HL127704. Project MinE Belgium was supported by a grant from IWT (no. 140935), the ALS Liga Belgie, the National Lottery of Belgium and the KU Leuven Opening the Future Fund. D.C. and C.L. are supported by HYPERGENES (HEALTH-F4-2007). D.R. is supported by R01 HL149826, P50 GM115305. P.J.S. acknowledges the support of Leducq Foundation for Cardiovascular Research grant 18CVD05. P.V.D. is supported by the Netherlands CardioVascular Research Initiative (CVON PREDICT2). C.A. is supported by NIH HL47678 and HL138103, W.W. Smith Charitable Trust and Wistar Morris Fund. M.B. is Supported by the DZHK (German Centre for Cardiovascular Research) and by the BMBF (German Ministry of Education and Research). P.D.L. is supported by UCL/UCLH Biomedicine NIHR and Barts BRC. B.L. is supported by GOA-Antigone 33933. J.B. is supported by a Senior Clinical Fellowship of the Flemish Science Foundation (FWO). E.B. is supported by the British Heart Foundation including BHF Clinical Research Training Fellowship (FS/11/71/28918: Future diagnostic role and new genetic loci in SADS), Cardiac Risk in the Young and Robert Lancaster Memorial fund sponsored by McColl's Ltd. Retail Group. H.L.T. is supported by the European Union's Horizon 2020 research and innovation program under acronym ESCAPE-NET, registered under grant agreement no. 733381, and the Dutch Heart Foundation (CVON RESCUED and PREDICT2 projects). M.D. is supported by NIH-RO1 HL134328. P.T.E. was supported by the Fondation Leducq (14CVD01), the NIH (1RO1HL092577, R01HL128914, K24HL105780), the American Heart Association (18SFRN34110082) and by a research grant from Bayer AG to the Broad Institute. S.A.L. is supported by NIH grant 1R01HL139731 and American Heart Association 18SFRN34250007. J.-B.G. received a grant from the Federation Francaise de Cardiologie (PREVENT project). A.L.G. is supported by the Fondation Leducq. C.A.M.R. is supported by the Leducq Foundation and Burroughs Wellecome Fund. A.A.W. is supported by the Dutch Heart Foundation (CVON PREDICT2 project). J.-J.S. is supported by the Fondation pour la Recherche Medicale (DEQ20140329545). R.R. and P.G. are supported by the National Agency for Research (ANR-GENSUD-14-CE10-0001). C.R.B. is supported by the Dutch Heart Foundation (CVON PREDICT2 project), the Netherlands Organization for Scientific Research (VICI fellowship, 016.150.610) and Fondation Leducq (17CVD02).

Published
2022

35. Enhancing rare variant interpretation in inherited arrhythmias through quantitative analysis of consortium disease cohorts and population controls

Author

Charles Antzelevitch, Ahmad S. Amin, Bo Gregers Winkel, Dan M. Roden, Stefan Kääb, Jonathan R. Skinner, Seiko Ohno, Julien Barc, Birgit Stallmeyer, Carla Giustetto, Connie R. Bezzina, Francesco Mazzarotto, Tomas Robyns, Carlo Napolitano, Stellan Mörner, Doris Škorić-Milosavljević, Sven Dittmann, Kenichiro Yamagata, Sonia Van Dooren, Anniek Corveleyn, Carlo de Asmundis, Ramon Brugada, K Usuda, Yuji Tanaka, Sven Zumhagen, Tadashi Nakajima, Johan Saenen, Elijah R. Behr, Hector Barajas-Martinez, Stéphane Bézieau, Masao Yoshinaga, Georgia Sarquella-Brugada, Paul G.A. Volders, Juan R. Gimeno, Lia Crotti, Charlotte Glinge, Andrea Mazzanti, Ingrid P.C. Krapels, Nicola Whiffin, Sebastian Clauss, Yoshiaki Kaneko, James S. Ware, Minoru Horie, Keiko Shimamoto, Isabelle Denjoy, Pieter G. Postema, Christian Krijger, Takeshi Aiba, Masahiko Kurabayashi, Pyotr G. Platonov, Regina Sebastiano, Cristina Gil Ortuño, Annika Rydberg, Roddy Walsh, Michael J. Ackerman, Hideki Itoh, M. Benjamin Shoemaker, Can Hasdemir, Pascale Guicheney, J. Martijn Bos, Frederic Sacher, Takeru Makiyama, Julieta Lazarte, Maarten P. van den Berg, Dominique Babuty, David J. Tester, Silvia Castelletti, Jacques Mansourati, Antoine Leenhardt, Paul A. van der Zwaag, Sanjay Sharma, Elena Arbelo, Candan Celen, Pier D. Lambiase, Maria Christina Kotta, Johannes Steinfurt, Jean-Baptiste Gourraud, Pedro Brugada, Wataru Shimizu, Josep Brugada, Jørgen K. Kanters, Eline A. Nannenberg, Silvia G. Priori, Mary N. Sheppard, Richard Redon, Morten S. Olesen, Jeroen Breckpot, Britt M. Beckmann, Naomasa Makita, Martin Borggrefe, Rafik Tadros, Jean-Jacques Schott, Jacob Tfelt-Hansen, Steven A. Lubitz, Hatice Şahin, Najim Lahrouchi, Michael Papadakis, Daisuke Hazeki, Kenshi Hayashi, Oscar Campuzano, Katja E. Odening, Federica Dagradi, Eric Schulze-Bahr, Boris Rudic, Hiroki Kimoto, Vincent Probst, Jason D. Roberts, Raphaël P. Martins, Bart Loeys, Daniela F. Giachino, F. Kyndt, Kimie Ohkubo, Taisuke Ishikawa, Catarina Lundin, Lut Van Laer, Patrick T. Ellinor, Maria Sabater Molina, Peter J. Schwartz, Annika Winbo, Wellcome Trust, Rosetrees Trust, British Heart Foundation, Walsh, R, Lahrouchi, N, Tadros, R, Kyndt, F, Glinge, C, Postema, P, Amin, A, Nannenberg, E, Ware, J, Whiffin, N, Mazzarotto, F, Skoric-Milosavljevic, D, Krijger, C, Arbelo, E, Babuty, D, Barajas-Martinez, H, Beckmann, B, Bezieau, S, Bos, J, Breckpot, J, Campuzano, O, Castelletti, S, Celen, C, Clauss, S, Corveleyn, A, Crotti, L, Dagradi, F, de Asmundis, C, Denjoy, I, Dittmann, S, Ellinor, P, Ortuno, C, Giustetto, C, Gourraud, J, Hazeki, D, Horie, M, Ishikawa, T, Itoh, H, Kaneko, Y, Kanters, J, Kimoto, H, Kotta, M, Krapels, I, Kurabayashi, M, Lazarte, J, Leenhardt, A, Loeys, B, Lundin, C, Makiyama, T, Mansourati, J, Martins, R, Mazzanti, A, Morner, S, Napolitano, C, Ohkubo, K, Papadakis, M, Rudic, B, Molina, M, Sacher, F, Sahin, H, Sarquella-Brugada, G, Sebastiano, R, Sharma, S, Sheppard, M, Shimamoto, K, Shoemaker, M, Stallmeyer, B, Steinfurt, J, Tanaka, Y, Tester, D, Usuda, K, van der Zwaag, P, Van Dooren, S, Van Laer, L, Winbo, A, Winkel, B, Yamagata, K, Zumhagen, S, Volders, P, Lubitz, S, Antzelevitch, C, Platonov, P, Odening, K, Roden, D, Roberts, J, Skinner, J, Tfelt-Hansen, J, van den Berg, M, Olesen, M, Lambiase, P, Borggrefe, M, Hayashi, K, Rydberg, A, Nakajima, T, Yoshinaga, M, Saenen, J, Kaab, S, Brugada, P, Robyns, T, Giachino, D, Ackerman, M, Brugada, R, Brugada, J, Gimeno, J, Hasdemir, C, Guicheney, P, Priori, S, Schulze-Bahr, E, Makita, N, Schwartz, P, Shimizu, W, Aiba, T, Schott, J, Redon, R, Ohno, S, Probst, V, Arnaout, A, Amelot, M, Anselme, F, Billon, O, Defaye, P, Dupuis, J, Jesel, L, Laurent, G, Maury, P, Pasquie, J, Wiart, F, Behr, E, Barc, J, Bezzina, C, unité de recherche de l'institut du thorax UMR1087 UMR6291 (ITX), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN), Centre Hospitalier Régional Universitaire de Tours (CHRU TOURS), CIC - CHU Bichat, Institut National de la Santé et de la Recherche Médicale (INSERM), Centre Hospitalier Régional Universitaire de Brest (CHRU Brest), CHU Pontchaillou [Rennes], Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Institute of cardiometabolism and nutrition (ICAN), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [AP-HP], Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Ege Üniversitesi, Cardiovascular Centre (CVC), Nantes Referral Ctr Inherited Car, Cardiology, Graduate School, ACS - Heart failure & arrhythmias, Human Genetics, ACS - Amsterdam Cardiovascular Sciences, ACS - Atherosclerosis & ischemic syndromes, MUMC+: DA KG Polikliniek (9), RS: Carim - H02 Cardiomyopathy, Cardiologie, MUMC+: MA Med Staf Spec Cardiologie (9), RS: Carim - H04 Arrhythmogenesis and cardiogenetics, Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Centre Hospitalier Régional Universitaire de Tours (CHRU Tours), Clinical sciences, Heartrhythmmanagement, Medical Genetics, Reproduction and Genetics, and Cardio-vascular diseases

Subjects
0301 basic medicine, [SDV]Life Sciences [q-bio], Nantes Referral Center for inherited cardiac arrhythmia, Disease, Arrhythmias, 030105 genetics & heredity, ACMG/AMP guidelines, Brugada, LQTS, variant interpretation, Medicine, Genetics (clinical), Brugada Syndrome, Brugada syndrome, Genetics, Genetics & Heredity, education.field_of_study, medicine.diagnostic_test, Molecular pathology, 3. Good health, Long QT Syndrome, Medical genetics, Population Control, Cardiology and Cardiovascular Medicine, Cardiac, Medical Genetics, Life Sciences & Biomedicine, medicine.medical_specialty, congenital, hereditary, and neonatal diseases and abnormalities, Long QT syndrome, Population, 610 Medicine & health, BIO/18 - GENETICA, Article, 03 medical and health sciences, Humans, Genetic Testing, cardiovascular diseases, education, Medicinsk genetik, Genetic testing, 0604 Genetics, Science & Technology, business.industry, Genetic heterogeneity, MUTATIONS, ACMG/AMP guideline, Arrhythmias, Cardiac, 1103 Clinical Sciences, MED/11 - MALATTIE DELL'APPARATO CARDIOVASCOLARE, medicine.disease, Mutation, 030104 developmental biology, Human medicine, business
Abstract

Purpose: Stringent variant interpretation guidelines can lead to high rates of variants of uncertain significance (VUS) for genetically heterogeneous disease like long QT syndrome (LQTS) and Brugada syndrome (BrS). Quantitative and disease-specific customization of American College of Medical Genetics and Genomics/Association for Molecular Pathology (ACMG/AMP) guidelines can address this false negative rate. Methods: We compared rare variant frequencies from 1847 LQTS (KCNQ1/KCNH2/SCN5A) and 3335 BrS (SCN5A) cases from the International LQTS/BrS Genetics Consortia to population-specific gnomAD data and developed disease-specific criteria for ACMG/AMP evidence classes-rarity (PM2/BS1 rules) and case enrichment of individual (PS4) and domain-specific (PM1) variants. Results: Rare SCN5A variant prevalence differed between European (20.8%) and Japanese (8.9%) BrS patients (p = 5.7 x 10(-18)) and diagnosis with spontaneous (28.7%) versus induced (15.8%) Brugada type 1 electrocardiogram (ECG) (p = 1.3 x 10(-13)). Ion channel transmembrane regions and specific N-terminus (KCNH2) and C-terminus (KCNQ1/KCNH2) domains were characterized by high enrichment of case variants and >95% probability of pathogenicity. Applying the customized rules, 17.4% of European BrS and 74.8% of European LQTS cases had (likely) pathogenic variants, compared with estimated diagnostic yields (case excess over gnomAD) of 19.2%/82.1%, reducing VUS prevalence to close to background rare variant frequency. Conclusion: Large case-control data sets enable quantitative implementation of ACMG/AMP guidelines and increased sensitivity for inherited arrhythmia genetic testing., Amsterdam Cardiovascular Sciences fellowship; Dutch Heart Foundation (CVON Predict-2/Concor-genes); Netherlands Organization for Scientific ResearchNetherlands Organization for Scientific Research (NWO) [VICI 016.150.610]; Fondation LeducqLeducq Foundation, R.W. is supported by an Amsterdam Cardiovascular Sciences fellowship. C.R.B. is supported by the Dutch Heart Foundation (CVON Predict-2/Concor-genes), Netherlands Organization for Scientific Research (VICI 016.150.610), and Fondation Leducq. See Supplement for all Acknowledgements.

Published
2020

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