Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible
Planck Collaboration, P. A. R. Ade, N. Aghanim, D. Alina, G. Aniano, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A… 展开作者
Planck Collaboration, P. A. R. Ade, N. Aghanim, D. Alina, G. Aniano, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, C. Beichman, 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, R. -R. Chary, H. C. Chiang, P. R. Christensen, S. Colombi, 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, A. de Rosa, 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, L. Fanciullo, F. Finelli, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, S. Galeotta, K. Ganga, T. Ghosh, M. Giard, Y. Giraud-Héraud, 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, K. M. Huffenberger, A. H. Jaffe, T. R. Jaffe, W. C. Jones, M. Juvela, E. Keihänen, 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, 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, C. A. Oxborrow, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, F. Pasian, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, D. Pietrobon, S. Plaszczynski, F. Poidevin, E. Pointecouteau, G. Polenta, L. Popa, G. W. Pratt, S. Prunet, J. -L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, B. Rusholme, 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, G. Umana, L. Valenziano, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, L. A. Wade, B. D. Wandelt, A. Zonca
The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust, bringing new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the visible. Comparison of the polarization of the emission and of the interstellar polarization on selected lines of sight probed by stars provides unique new diagnostics of the emission and light scattering properties of dust. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, $p_V$ , and the optical depth in the V band to the star, $τ_V$. Toward these stars we measure the submillimetre polarized intensity, $P_S$, and total intensity, $I_S$, in the Planck 353 GHz channel. For those lines of sight through the diffuse interstellar medium with comparable values of the estimated column density and polarization directions close to orthogonal, we correlate properties in the submillimetre and visible to find two ratios, $R_{S/V} = (P_S/I_S)/(p_V/τ_V)$ and $R_{P/p} = P_S/p_V$ , the latter focusing directly on the polarization properties of the aligned grain population alone. We find $R_{S/V}$ = 4.2, with statistical and systematic uncertainties 0.2 and 0.3, respectively, and $R_{P/p}$ = 5.4 MJy sr$^{-1}$, with uncertainties 0.2 and 0.3 MJy sr$^{-1}$, respectively. Our estimate of $R_{S/V}$ is compatible with predictions based on a range of polarizing dust models that have been developed for the diffuse interstellar medium. However, our estimate of $R_{P/p}$ is not compatible with predictions, which are too low by a factor of about 2.5. This more discriminating diagnostic, $R_{P/p}$, indicates that changes to the optical properties in the models of the aligned grain population are required.
Planck Early Results XXIV: Dust in the diffuse interstellar medium and the Galactic halo
本文介绍了普朗克与IRAS数据与绿岸望远镜21厘米观测在14个领域覆盖超过800平方度的银河系高纬度的第一个比较结果。对于平均HI柱密度低于2 x 10^20 cm ^-2的场，星系尘埃的辐射与21 cm辐射有很好的相关性。在这些领域中的剩余发射，一旦HI相关的发射被删除，是符合预期的宇宙红外背景波动的统计特性。具有较大列密度的字段显示出显着的过量粉尘排放相比，HI列密度。过量区域位于有组织的结构中，表明存在分子形式的氢，尽管它们并不总是与CO排放相关。从中速云尘埃排放检测具有很高的意义。它的光谱特性是一致的，与当地的ISM值相比，显着更热的尘埃（T~20 K），较低的亚毫米尘埃不透明度，和一个相对丰富的非常小的颗粒大颗粒约四倍高。这些结果与银河系喷泉云的一部分的预期是一致的，其中有尘埃破碎和碎片。相关的灰尘排放在HVC没有检测到的平均99.9%的置信上限的发射率是0.15倍的本地ISM值在857和3000 GHz的，根据气相的证据较低的金属丰度和耗尽在这些云。意外的反相关变化的尘埃温度和每个H原子的发射截面被确定在本地ISM和IVC，一种趋势，继续进入分子环境。这表明，在分子云中看到的通过聚集的尘埃生长在云凝结和恒星形成过程中更早地活跃。
Herschel observations of interstellar chloronium. II - Detections toward G29.96-0.02, W49N, W51, and W3(OH), and determinations of the ortho-to-para and $^{35}$Cl/$^{37}$Cl isotopic ratios
New insights into the interstellar medium of the dwarf galaxy IC 10: connection between magnetic fields, the radio--infrared correlation and star formation
Investigating ionising sources and the complex interstellar medium of GHZ2 at $z=12.3$
INAF Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Università di Firenze, Dipartimento di Fisica e Astronomia（佛罗伦萨大学物理与天文学系）；INAF – Arcetri Astrophysical Observatory（意大利国家天体物理研究所阿切特里天文台）；European Southern Observatory（欧洲南方天文台）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Department of Space, Earth, & Environment, Chalmers University of Technology（查尔姆斯理工大学空间、地球与环境系）；NSF’s NOIRLab（美国国家科学基金会NOIR实验室）；Institute of Science and Technology Austria (ISTA)（奥地利科学与技术研究所）；IPAC, California Institute of Technology（加州理工学院IPAC）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）
Heavy interstellar scattering toward the near end of the Galactic bar
Crimean Astrophysical Observatory（克里米亚天体物理观测台）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Instituto de Física, Pontificia Universidad Católica de Valparaíso（天主教瓦尔帕莱索大学物理研究所）；Lebedev Physical Institute（列别捷夫物理研究所）；Moscow Institute of Physics and Technology（莫斯科物理技术学院）；Black Hole Initiative at Harvard University（哈佛大学黑洞倡议项目）；Department of Physics, Indian Institute of Science（印度科学学院物理系）；Department of Physics, New Mexico Institute of Mining and Technology（新墨西哥矿业理工学院物理系）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
Laboratory rotational spectroscopy and interstellar search for the protein precursor 4-oxobutanenitrile (HCOCH$_2$CH$_2$CN)
Centro de Astrobiología (CAB, CSIC-INTA)（天体生物学中心）；Universidad del País Vasco (UPV/EHU)（巴斯克大学）；Instituto Biofisika (CSIC, UPV/EHU)（生物物理研究所）；University of Bologna（博洛尼亚大学）
Breakthrough Listen Observations of 3I/ATLAS with the Green Bank Telescope at 1-12 GHz
University of California, Berkeley（加州大学伯克利分校）；Breakthrough Listen, University of Oxford（突破聆听项目，牛津大学）；SETI Institute（搜寻地外文明研究所）；Marshall University（马歇尔大学）；University of Malta（马耳他大学）；University of Manchester（曼彻斯特大学）
The multiphase interstellar medium as a common origin for magnetic misalignment and TB parity violation
LUX, Observatoire de Paris, Université PSL, Sorbonne Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切里天文台）；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，巴黎文理研究大学，索邦大学）；Department of Physics, California Institute of Technology（加州理工学院物理系）；TAPIR, California Institute of Technology（加州理工学院理论天体物理学与相对论研究中心）
Molecular absorption lines toward the Galactic ISM detected at 89 GHz with VLBI
Graduate School of Science and Engineering, Kagoshima University（鹿儿岛大学理工学研究科）；Nobeyama Radio Observatory, National Astronomical Observatory of Japan (NAOJ), National Institutes of Natural Sciences (NINS)（日本国立天文台野边山射电天文台，日本国立自然科学研究所）；Amanogawa Galaxy Astronomy Research Center, Graduate School of Science and Engineering, Kagoshima University（鹿儿岛大学理工学研究科银河天文学研究中心）；Center for General Education, Institute for Comprehensive Education, Kagoshima University（鹿儿岛大学综合教育院通识教育中心）；Korea Astronomy and Space Science Institute（韩国天体宇宙科学研究所）
The dust and [CII] morphologies of redshift ~4.5 sub-millimeter galaxies at ~200pc resolution: The absence of large clumps in the interstellar medium of high-redshift galaxies
