Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization
Planck Collaboration, P. A. R. Ade, M. I. R. Alves, G. Aniano, C. Armitage-Caplan, M. Arnaud, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B.… 展开作者
Planck Collaboration, P. A. R. Ade, M. I. R. Alves, G. Aniano, C. Armitage-Caplan, M. Arnaud, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, K. Benabed, A. Benoit-Lévy, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. J. Bock, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, C. Burigana, J. -F. Cardoso, A. Catalano, A. Chamballu, H. C. Chiang, L. P. L. Colombo, C. Combet, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, G. de Zotti, J. Delabrouille, F. -X. Désert, C. Dickinson, J. M. Diego, S. Donzelli, O. Doré, M. Douspis, J. Dunkley, X. Dupac, T. A. Enßlin, H. K. Eriksen, E. Falgarone, F. Finelli, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, S. Galeotta, K. Ganga, T. Ghosh, M. Giard, J. González-Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, V. Guillet, F. K. Hansen, D. L. Harrison, G. Helou, C. Hernández-Monteagudo, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, A. Hornstrup, A. H. Jaffe, T. R. Jaffe, W. C. Jones, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, M. Kunz, H. Kurki-Suonio, G. Lagache, J. -M. Lamarre, A. Lasenby, C. R. Lawrence, J. P. Leahy, R. Leonardi, F. Levrier, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. Macías-Pérez, B. Maffei, A. M. Magalhães, D. Maino, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, S. Matarrese, P. Mazzotta, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, F. Noviello, D. Novikov, I. Novikov, N. Oppermann, C. A. Oxborrow, L. Pagano, F. Pajot, D. Paoletti, F. Pasian, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, L. Popa, G. W. Pratt, J. P. Rachen, W. T. Reach, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, J. A. Rubiño-Martín, B. Rusholme, E. Salerno, M. Sandri, G. Savini, D. Scott, L. D. Spencer, V. Stolyarov, R. Stompor, R. Sudiwala, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, L. Valenziano, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, B. D. Wandelt, A. Zacchei, A. Zonca
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26 pages, 15 figures, 9 tables; updated version; small changes to match the published version
Planck has mapped the intensity and polarization of the sky at microwave frequencies with unprecedented sensitivity. We make use of the Planck 353 GHz I, Q, and U Stokes maps as dust templates, and cross-correlate them with the Planck and WMAP data at 12 frequencies from 23 to 353 GHz, over circular patches with 10 degree radius. The cross-correlation analysis is performed for both intensity and polarization data in a consistent manner. We use a mask that focuses our analysis on the diffuse interstellar medium at intermediate Galactic latitudes. We determine the spectral indices of dust emission in intensity and polarization between 100 and 353 GHz, for each sky-patch. The mean values, $1.59\pm0.02$ for polarization and $1.51\pm0.01$ for intensity, for a mean dust temperature of 19.6 K, are close, but significantly different ($3.6\,σ$). We determine the mean spectral energy distribution (SED) of the microwave emission, correlated with the 353 GHz dust templates, by averaging the results of the correlation over all sky-patches. We find that the mean SED increases for decreasing frequencies at $ν< 60$ GHz, for both intensity and polarization. The rise of the polarization SED towards low frequencies may be accounted for by a synchrotron component correlated with dust, with no need for any polarization of the anomalous microwave emission. We use a spectral model to separate the synchrotron and dust polarization and to characterize the spectral dependence of the dust polarization fraction. The polarization fraction ($p$) of the dust emission decreases by $(21\pm6)$ % from 353 to 70 GHz. The decrease of $p$ could indicate differences in polarization efficiency among components of interstellar dust (e.g., carbon versus silicate grains). Our observational results provide inputs to quantify and optimize the separation between Galactic and cosmological polarization.
First Light and Reionization Epoch Simulations (FLARES) XXII: UV-dust spatial offsets at the Epoch of Reionisation
University of Hertfordshire（赫特福德大学）；University of Sussex（萨塞克斯大学）；Technical University of Denmark（丹麦技术大学）；Academia Sinica（中央研究院）；University of Cambridge（剑桥大学）
Variance of dust temperature and spectral index in Planck polarization data using spin-moment expansion
Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Sud, Université Paris-Saclay（空间天体物理研究所，法国国家科学研究中心，巴黎南大学，巴黎萨克雷大学）；Laboratoire Univers et Particules de Montpellier, Université de Montpellier, CNRS/IN2P2（蒙彼利埃宇宙与粒子实验室，蒙彼利埃大学，法国国家科学研究中心/法国国家核子和粒子物理研究所）；International School for Advanced Studies (SISSA)（高级国际研究学院）；Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Trieste（意大利国家核物理研究所，的里雅斯特分部）；Institute for Fundamental Physics of the Universe (IFPU)（宇宙基础物理研究所）；IRAP, Université de Toulouse, CNRS, CNES, UPS（天体物理学研究所，图卢兹大学，法国国家科学研究中心，法国国家空间研究中心）；Laboratoire de Physique de l’Ecole Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris（巴黎高等师范学院物理实验室，巴黎高等师范学院，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎大学）；Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，格勒诺布尔理工学院）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所，卡利亚里天文台）；Laboratoire d’Océanographie Physique et Spatiale (LOPS), Univ. Brest, CNRS, Ifremer, IRD（物理与空间海洋学实验室，布雷斯特大学，法国国家科学研究中心，法国海洋开发研究院，法国农业食品与林业研究发展中心）
Separation of polarized dust emission in Planck observations with Scattering Transforms
Laboratoire de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris Cité（巴黎高等师范学院物理实验室，ENS，PSL大学，CNRS，索邦大学，巴黎西岱大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Department of Astronomy and Astrophysics, University of Chicago（芝加哥大学天文学与天体物理学系）；CNRS-UCB International Research Laboratory, Centre Pierre Binétruy, IRL 2007, CPB-IN2P3（CNRS-UCB国际研究实验室，皮埃尔·比内屈中心，IRL 2007，CPB-IN2P3）
Untangling dust emission and cosmic infrared background anisotropies with the scattering transform statistics
National Institute of Science Education and Research（印度科学教育研究所）；Homi Bhabha National Institute（霍米·巴巴国立研究所）；Laboratoire de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris Cité（巴黎高等师范学院物理实验室）；Laboratoire d’Océanographie Physique et Spatiale (LOPS), Univ. Brest, CNRS, Ifremer, IRD（布列斯特大学海洋物理与空间实验室）
Cosmoglobe DR2. V. Spatial correlations between thermal dust and ionized carbon emission in Planck HFI and COBE-DIRBE
Institute of Theoretical Astrophysics, University of Oslo（奥斯陆大学理论天体物理研究所）；Dipartimento di Fisica, Università degli Studi di Milano（米兰大学物理系）；Laboratoire de Physique des 2 infinis – Irène Joliot Curie (IJCLab)（双无穷物理实验室——伊雷娜·约里奥-居里实验室）；Department of Space, Earth and Environment, Chalmers University of Technology（查尔姆斯理工大学空间、地球与环境系）；Università di Trento（特伦托大学）；INFN sezione di Milano（意大利国家核物理研究院米兰分部）
BICEP/Keck XX: Component-separated maps of polarized CMB and thermal dust emission using Planck and BICEP/Keck Observations through the 2018 Observing Season
Cardiff University（卡迪夫大学）；Stanford University（斯坦福大学）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；University of British Columbia（不列颠哥伦比亚大学）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森天体物理中心）；California Institute of Technology（加州理工学院）；University of Cincinnati（辛辛那提大学）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）
Is there a left-handed magnetic field in the solar neighborhood? Exploring helical magnetic fields in the interstellar medium through dust polarization power spectra
Planck's dusty GEMS. IV. Star formation and feedback in a maximum starburst at z=3 seen at 60-pc resolution
我们提出了一个高分辨率的ALMA干涉测量的CO（4-3）线发射和尘埃连续体的“红宝石”（PLCK_G244.8+54.9），一个明亮的，引力透镜星系在z = 3.0发现的普朗克全天巡天。红宝石是普朗克尘埃宝石中最明亮的一颗，它是银河系外亚毫米天空中11个最明亮的引力透镜高红移星系的样本。我们解决了高表面亮度的连续和CO线发射的红宝石在几个扩展块沿部分，近圆形爱因斯坦环直径为1.4”周围的大质量星系在z = 1.5。当地的恒星形成强度高达2000 M $_{\odot}$ yr $^{-1}$ kpc $^{-2}$，其中最高的观测在高红移，显然在最大的恒星爆发的范围。气体质量表面密度为几个$\times$ 10 $^4$ M $_{\odot}$ pc $^{-2}$。红宝石位于施密特-肯尼库特图中的星暴序列之上，甚至部分位于其上方，处于恒星形成的极限，恒星形成是通过辐射压、恒星风和超新星的动能注入而自我调节的。我们发现，这些过程也可以注入足够的动能和动量到气体中来解释湍流线宽，这是符合边缘引力约束的分子云嵌入在一个临界托姆雷稳定盘。恒星形成效率在每自由落体时间的1-10%之间，这与银河系中设定局部恒星形成定律的压力平衡可能在最高恒星形成强度之外是普遍存在的概念一致。活动星系核的反馈对于红宝石星系中恒星的形成并不是必需的，这与活动星系核在红外线和射电波段中没有明亮的成分是一致的。
HI, CO, and Planck/IRAS dust properties in the high-latitude-cloud complex, MBM 53, 54, 55 and HLCG 92-35; Possible evidence for an optically thick HI envelope around the CO clouds
