Abstract
| Original language | English |
|---|---|
| Article number | A20 |
| Number of pages | 17 |
| Journal | Astronomy and Astrophysics |
| Volume | 536 |
| DOIs | |
| Publication status | Published - 2011 |
| MoE publication type | A1 Journal article-refereed |
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Keywords
- Galaxy: general
- ISM: general
- radiation mechanisms
- general
- radio continuum
- ISM
- submillimeter: ISM
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Planck early results. XX : New light on anomalous microwave emission from spinning dust grains. / Tuovinen, Jussi; Varis, Jussi; Dickinson, C. (Corresponding Author); Planck Collaboration.
In: Astronomy and Astrophysics, Vol. 536, A20, 2011.Research output: Contribution to journal › Article › Scientific › peer-review
TY - JOUR
T1 - Planck early results. XX
T2 - New light on anomalous microwave emission from spinning dust grains
AU - Ade, P.A.R.
AU - Aghanim, N.
AU - Arnaud, M.
AU - Tuovinen, Jussi
AU - Varis, Jussi
AU - Dickinson, C.
AU - Planck Collaboration
N1 - Project code: 18080
PY - 2011
Y1 - 2011
N2 - Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range ~10–60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and ρ Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. The spinning dust spectra are the most precisely measured to date, and show the high frequency side clearly for the first time. The spectra have a peak in the range 20–40 GHz and are detected at high significances of 17.1σ for Perseus and 8.4σ for ρ Ophiuchi. In Perseus, spinning dust in the dense molecular gas can account for most of the AME; the low density atomic gas appears to play a minor role. In ρ Ophiuchi, the ~30 GHz peak is dominated by dense molecular gas, but there is an indication of an extended tail at frequencies 50–100 GHz, which can be accounted for by irradiated low density atomic gas. The dust parameters are consistent with those derived from other measurements. We have also searched the Planck map at 28.5 GHz for candidate AME regions, by subtracting a simple model of the synchrotron, free-free, and thermal dust. We present spectra for two of the candidates; S140 and S235 are bright Hii regions that show evidence for AME, and are well fitted by spinning dust models.
AB - Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range ~10–60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and ρ Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. The spinning dust spectra are the most precisely measured to date, and show the high frequency side clearly for the first time. The spectra have a peak in the range 20–40 GHz and are detected at high significances of 17.1σ for Perseus and 8.4σ for ρ Ophiuchi. In Perseus, spinning dust in the dense molecular gas can account for most of the AME; the low density atomic gas appears to play a minor role. In ρ Ophiuchi, the ~30 GHz peak is dominated by dense molecular gas, but there is an indication of an extended tail at frequencies 50–100 GHz, which can be accounted for by irradiated low density atomic gas. The dust parameters are consistent with those derived from other measurements. We have also searched the Planck map at 28.5 GHz for candidate AME regions, by subtracting a simple model of the synchrotron, free-free, and thermal dust. We present spectra for two of the candidates; S140 and S235 are bright Hii regions that show evidence for AME, and are well fitted by spinning dust models.
KW - Galaxy: general
KW - ISM: general
KW - radiation mechanisms
KW - general
KW - radio continuum
KW - ISM
KW - submillimeter: ISM
U2 - 10.1051/0004-6361/201116470
DO - 10.1051/0004-6361/201116470
M3 - Article
VL - 536
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A20
ER -