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| Format: | Preprint |
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2024
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| Online-Zugang: | https://arxiv.org/abs/2405.04383 |
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| author | Harper, Stuart E. Dickinson, Clive Cleary, Kieran A. Hensley, Brandon S. Hoerning, Gabriel A. Paladini, Roberta Rennie, Thomas J. Cepeda-Arroita, Roke Dunne, Delaney A. Eriksen, Hans Kristian Gundersen, Joshua Ott Ihle, Havard T. Lunde, Jonas G. S. Ricci, Roberto Stil, Jeroen Stutzer, Nils-Ole Taylor, A. R. Wehus, Ingunn Kathrine |
| author_facet | Harper, Stuart E. Dickinson, Clive Cleary, Kieran A. Hensley, Brandon S. Hoerning, Gabriel A. Paladini, Roberta Rennie, Thomas J. Cepeda-Arroita, Roke Dunne, Delaney A. Eriksen, Hans Kristian Gundersen, Joshua Ott Ihle, Havard T. Lunde, Jonas G. S. Ricci, Roberto Stil, Jeroen Stutzer, Nils-Ole Taylor, A. R. Wehus, Ingunn Kathrine |
| contents | Anomalous Microwave Emission (AME) is a major component of Galactic emission in the frequency band 10 to 60 GHz and is commonly modelled as rapidly rotating spinning dust grains. The photodissociation region (PDR) at the boundary of the $λ$-Orionis Hii region has been identified by several recent analyses as one of the brightest spinning dust emitting sources in the sky. We investigate the Barnard 30 dark cloud, a dark cloud embedded within the $λ$-Orionis PDR. We use total-power observations of Barnard 30 from the CO Mapping Array Project (COMAP) pathfinder instrument at 26 to 34GHz with a resolution of 4.5 arcminutes alongside existing data from Planck, WISE, IRAS, ACT, and the 1.447GHz GALFACTS survey. We use aperture photometry and template fitting to measure the spectral energy distribution of Barnard 30. We find that the spinning dust is the dominant emission component in the 26 to 34GHz range at the $7 σ$ level ($S_{30GHz} = 2.85\pm0.43$Jy). We find no evidence that polycyclic aromatic hydrocarbons are the preferred carrier for the spinning dust emission, suggesting that the spinning dust carriers are due to a mixed population of very small grains. Finally, we find evidence for variations in spinning dust emissivity and peak frequency within Barnard 30, and that these variations are possibly driven by changes in dust grain population and the total radiation field. Confirming the origin of the variations in the spinning dust spectrum will require both future COMAP observations at 15GHz combined with spectroscopic mid-infrared data of Barnard 30. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_04383 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | COMAP Galactic Science I: Observations of Spinning Dust Emission at 30GHz in Dark Clouds Surrounding the λ-Orionis Hii Region Harper, Stuart E. Dickinson, Clive Cleary, Kieran A. Hensley, Brandon S. Hoerning, Gabriel A. Paladini, Roberta Rennie, Thomas J. Cepeda-Arroita, Roke Dunne, Delaney A. Eriksen, Hans Kristian Gundersen, Joshua Ott Ihle, Havard T. Lunde, Jonas G. S. Ricci, Roberto Stil, Jeroen Stutzer, Nils-Ole Taylor, A. R. Wehus, Ingunn Kathrine Astrophysics of Galaxies Anomalous Microwave Emission (AME) is a major component of Galactic emission in the frequency band 10 to 60 GHz and is commonly modelled as rapidly rotating spinning dust grains. The photodissociation region (PDR) at the boundary of the $λ$-Orionis Hii region has been identified by several recent analyses as one of the brightest spinning dust emitting sources in the sky. We investigate the Barnard 30 dark cloud, a dark cloud embedded within the $λ$-Orionis PDR. We use total-power observations of Barnard 30 from the CO Mapping Array Project (COMAP) pathfinder instrument at 26 to 34GHz with a resolution of 4.5 arcminutes alongside existing data from Planck, WISE, IRAS, ACT, and the 1.447GHz GALFACTS survey. We use aperture photometry and template fitting to measure the spectral energy distribution of Barnard 30. We find that the spinning dust is the dominant emission component in the 26 to 34GHz range at the $7 σ$ level ($S_{30GHz} = 2.85\pm0.43$Jy). We find no evidence that polycyclic aromatic hydrocarbons are the preferred carrier for the spinning dust emission, suggesting that the spinning dust carriers are due to a mixed population of very small grains. Finally, we find evidence for variations in spinning dust emissivity and peak frequency within Barnard 30, and that these variations are possibly driven by changes in dust grain population and the total radiation field. Confirming the origin of the variations in the spinning dust spectrum will require both future COMAP observations at 15GHz combined with spectroscopic mid-infrared data of Barnard 30. |
| title | COMAP Galactic Science I: Observations of Spinning Dust Emission at 30GHz in Dark Clouds Surrounding the λ-Orionis Hii Region |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2405.04383 |