Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353GHz with optical interstellar polarization
Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353GHz with optical interstellar polarization
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普朗克中间结果。
DOI：
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发表时间：
2014
期刊：
影响因子：
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通讯作者：
A. Zonca
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作者：
P. Ade;N. Aghanim;D. Alina;G. Aniano;C. Armitage;M. Arnaud;M. Ashdown;F. Atrio;J. Aumont;C. Baccigalupi;A. Banday;R. B. Barreiro;E. Battaner;C. Beichman;K. Benabed;S. Colombi;L. Colombo;C. Combet;F. Couchot;A. Coulais;B. Crill;A. Curto;F. Cuttaia;L. Danese;R. Davies;R. Davis;P. Bernardis;A. Rosa;G. Zotti;J. Delabrouille;C. Dickinson;J. Diego;S. Donzelli;M. Douspis;J. Dunkley;X. Dupac;H. Eriksen;E. Falgarone;L. Fanciullo;F. Finelli;O. Forni;M. Frailis;A. Fraisse;E. Franceschi;S. Galeotta;K. Ganga;T. Ghosh;M. Giard;J. Gonz;A. Gregorio;A. Gruppuso;V. Guillet;F. Hansen;D. Harrison;G. Helou;C. Hern;S. Hildebrandt;E. Hivon;M. Hobson;W. Holmes;A. Hornstrup;W. Jones;M. Juvela;R. Keskitalo;T. Kisner;R. Kneissl;J. Knoche;M. Kunz;H. Kurki;G. Lagache;A. Lasenby;R. Leonardi;F. Levrier;M. Liguori;P. Lilje;M. Linden;A. Magalh;D. Maino;N. Mandolesi;M. Maris;D. Marshall;P. Martin;S. Masi;S. Matarrese;P. Mazzotta;A. Melchiorri;L. Mendes;A. Mennella;M. Migliaccio;A. Moneti;L. Montier;G. Morgante;D. Mortlock;D. Munshi;J. Murphy;P. Naselsky;F. Nati;P. Natoli;C. 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. Pratt;S. Prunet;L. Puget;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;L. Spencer;V. Stolyarov;R. Stompor;R. Sudiwala;D. Sutton;J. Tauber;L. Terenzi;M. Tomasi;M. Tristram;M. Tucci;G. Umana;L. Valenziano;Jussi Väliviita;B. Tent;P. Vielva;F. Villa;L. Wade;B. Wandelt;A. Zonca
普朗克的调查提供了史无前例的银河系尘埃亚毫米偏振辐射的全天覆盖。除了有关银河系磁场方向的信息外，这也给尘埃的性质带来了新的制约。发出普朗克所看到的亚毫米辐射的尘埃颗粒也会熄灭和偏振光学系统中的星光。恒星探测的选定视线上发射的偏振和星际偏振的比较提供了对尘埃的发射和光散射性质的独特的新诊断，从而最终提供了重要的模型参数、成分、大小、形状和排列的新诊断。利用星际偏振和星光消光的辅助星表，我们得到了恒星在V波段的偏振度PV和光学厚度V。我们提取了在普朗克353 GHz频道中对这些恒星测量的亚毫米极化强度PS和总强度IS。我们比较了光学测量的偏振方向(位置角)和在353 GHz测量的偏振方向(位置角)，并将柱状密度测量E(B，V)与从亚毫米尘埃光学厚度的普朗克乘积图推断的E(B，V)进行了比较。对于CO积分强度小、偏振方向接近于正交值和估计列密度的可比值的视线，我们将发射时的投射偏振频率QS=IS和US=IS与消光时的QV=V和UV=V相关联，以测量偏振比RS=V=(PS=IS)=(PV=V)。我们发现偏振比RS=V=4：3，统计和系统不确定度分别为0：2和0：4。我们通过一个交替的比率直接关注排列的颗粒布居的偏振性质，相对效率Rp=p=PS=Pv=5：6mJy sr1，统计和系统不确定度分别为0：2和0：4mJy sr1。我们对RS=V的估计与基于目前已开发的一系列尘埃模型的预测相当一致，这些模型是为使用星际介质而开发的，它们之间还不是很有区分性。然而，观测到的Rp=p对极化颗粒群是一个更具区分性的诊断，与预测不相容，观测值高出约2.5倍。来自普朗克的这些新诊断，包括以亚毫米为单位的光谱相关性，对于约束和理解颗粒模型的全部复杂性，以及进一步解释普朗克热尘埃极化和完善宇宙微波背景污染的分离将是重要的。
The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust. In addition to the information on the direction of the Galactic magnetic field, this also brings 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 optical. 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, and therefore ultimately of the important model parameters, composition, size, shape, and alignment. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, pV , and the optical depth in the V band to the star, V . We extract the submillimetre polarized intensity, PS, and total intensity, IS, measured toward these stars in the Planck 353 GHz channel. We compare the polarization direction (position angle) measured in the optical with that measured at 353 GHz, and compare the column density measure E(B V) with that inferred from the Planck product map of the submillimetre dust optical depth. For those lines of sight with little CO integrated intensity, as well as having polarization directions close to orthogonal and comparable values of the estimated column density, we correlate the projected polarization e ciencies in emission, QS=IS and US=IS, with those in extinction, qV= V and uV= V , to measure the polarization ratio RS=V = (PS=IS)=(pV= V ). We find a polarization ratio RS=V = 4:3 with statistical and systematic uncertainties 0:2 and 0:4, respectively. We focus directly on the polarization properties of the aligned grain population alone via an alternative ratio, the relative e ciency RP=p = PS=pV = 5:6 MJy sr 1 , with statistical and systematic uncertainties 0:2 and 0:4 MJy sr 1 , respectively. Our estimate of RS=V is reasonably compatible with predictions based on a range of current dust models that have been developed for the di use interstellar medium, not yet very discriminating among them. However, the observed RP=p is a more discriminating diagnostic for the polarizing grain population and is not compatible with predictions, the observations being higher by a factor of about 2.5. These new diagnostics from Planck, including the spectral dependence in the submillimetre, will be important for constraining and understanding the full complexity of the grain models, and for further interpretation of the Planck thermal dust polarization and refining the separation of this contamination of the cosmic microwave background.