A new spin on Galactic dust

被引:65
作者
de Oliveira-Costa, A
Tegmark, M
Finkbeiner, DP
Davies, RD
Gutierrez, CM
Haffner, LM
Jones, AW
Lasenby, AN
Rebolo, R
Reynolds, RJ
Tufte, SL
Watson, RA
机构
[1] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA
[2] Princeton Univ, Dept Astron, Princeton, NJ 08544 USA
[3] Univ Manchester, Nuffield Radio Astron Labs, Macclesfield SK11 9DL, Cheshire, England
[4] Inst Astrofis Canarias, Tenerife 38200, Spain
[5] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA
[6] Lewis & Clark Coll, Dept Phys, Portland, OR 97219 USA
[7] Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England
关键词
cosmic microwave background; dust; extinction; infrared : ISM; methods : data analysis; radiation mechanisms : nonthermal; radiation mechanisms : thermal;
D O I
10.1086/338109
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present a new puzzle involving Galactic microwave emission and attempt to resolve it. On one hand, a cross-correlation analysis of the Wisconsin Halpha Mapper map with the Tenerife 10 and 15 GHz maps shows that the well-known DIRBE correlated microwave emission cannot be dominated by free-free emission. On the other hand, recent high-resolution observations in the 8-10 GHz range with the Green Bank 140 foot telescope by Finkbeiner et al. failed to find the corresponding 8 sigma signal that would be expected in the simplest spinning-dust models. So what physical mechanism is causing this ubiquitous dust-correlated emission ? We argue for a model predicting that spinning dust is the culprit after all, but that the corresponding small grains are well correlated with the larger grains seen at 100 mum only on large angular scales. In support of this grain-segregation model, we find that the best spinning-dust template involves higher frequency maps in the range 12-60 mum, in which emission from transiently heated small grains is important. Upcoming cosmic microwave background experiments such as ground-based interferometers, the Microwave Anisotropy Probe, and the Planck low-frequency interferometer with high resolution at low frequencies should allow a definitive test of this model.
引用
收藏
页码:363 / 369
页数:7
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