Polarization angular spectra of Galactic synchrotron emission on arcminute scales

被引：27

作者：

Tucci, M

Carretti, E

Cecchini, S

Nicastro, L

Fabbri, R

Gaensler, BM

Dickey, JM

McClure-Griffiths, NM

机构：

[1] Univ Milano Bicocca, Dipartimento Fis G Occhialini, I-20126 Milan, Italy

[2] Ist Nazl Fis Nucl, I-20133 Milan, Italy

[3] Inst Fis Cantabria, Santander 39005, Spain

[4] CNR, Sez Bologna, Inst Astrophys Spatiale, I-40129 Bologna, Italy

[5] CNR, Sez Palermo, Inst Astrophys Spatiale, I-90146 Palermo, Italy

[6] Univ Florence, Dipartimento Fis, I-50019 Sesto Fiorentino, Italy

[7] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[8] Commonwealth Sci & Ind Res Org, Australia Telescope Natl Facil, Epping, NSW 1710, Australia

来源：

ASTROPHYSICAL JOURNAL | 2002年 / 579卷 / 02期

基金：

美国国家科学基金会;

关键词：

cosmic microwave background; methods : statistical; polarization; radio continuum : ISM;

D O I：

10.1086/342793

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the angular power spectra of the polarized component of the Galactic synchrotron emission in the 28 deg(2) test region of the Southern Galactic Plane Survey at 1.4 GHz. These data were obtained by the Australia Telescope Compact Array and allow us to investigate angular power spectra down to arcminute scales. We find that, at this frequency, the polarization spectra for E- and B-modes seem to be affected by Faraday rotation produced in compact foreground screens. A different behavior is shown by the angular spectrum of the polarized intensity PI=(Q(2)+U-2)(1/2). This is well fitted by a power law (C-PIl proportional to l(-alphaPI)) with slopesimilar to1.7, which agrees with higher frequency results and can probably be more confidently extrapolated to the cosmological window.

引用

页码：607 / 615

页数：9