Investigating anomalous microwave emission near G107.2+5.20 in Ku-band with the Green Bank Telescope
Abstract
Anomalous microwave emission (AME) is 30 GHz-peaking continuum emission thought to arise from spinning dust grains. Observations suggest that the local environment shapes the AME spectral energy distribution (SED), so building a spatially resolved sample of AME regions is a key step towards understanding its emission mechanism. Using the Green Bank Telescope Ku-band receiver, we obtained a ~1 arcmin resolution map of radius 1.25 deg centered on G107.2+5.20. Our first objective was to constrain the low-frequency side of the AME SED with 13 GHz data. Using matched-resolution aperture photometry, we measure the SED from 408 MHz-3 THz and fit two emission models: one including spinning dust, the other optically thick free-free emission. We find that the spinning dust model is superior, with an amplitude of 14.1±1.1 Jy and a peak frequency of 27±2 GHz. Our second objective was to spatially locate excess 13 GHz emission consistent with spinning dust. We compare our Ku-band map to multi-wavelength gas and dust tracers at ~4 arcmin resolution. We observe two sources of 13 GHz excess at 3σ significance consistent with spinning dust emission, though potential contributions from optically thick free-free emission remain ambiguous. ``Region A'' (G106.95+5.19) is spatially coincident with peak dust radiance. ``Region B'' (G107.08+4.90) is spatially coincident with peak PAH abundance. If regions A and B are indeed sources of spinning dust emission, they are a resolved example of how AME-dust correlation varies with environment.
Versions
Related
- Probing Anomalous Microwave Emission with the Square Kilometre Array
- Investigating X-ray emission from radio-detected broad- and narrow-line Seyfert 1 galaxies
- The Canadian Galactic Emission Mapper: A New 8-10 GHz Telescope to Map the Polarization of the Northern Sky
- The Canadian Galactic Emission Mapper (CGEM): A Cosmic Microwave Foreground Experiment
- Extended gamma-ray emission in the vicinity of the Westerlund 1 massive star cluster and Kes 41 supernova remnant seen by the Fermi Large Area Telescope
BibTeX
@misc{shroyer2026investigating,
title = {{Investigating anomalous microwave emission near G107.2+5.20 in Ku-band with the Green Bank Telescope}},
author = {Jordan E. Shroyer and Bradley R. Johnson and Dillon J. Bass and Anna Dignan and Stuart E. Harper and Brian S. Mason and Andrey Moore and Eric J. Murphy},
howpublished = {arXiv},
year = {2026},
month = jul,
doi = {10.48550/arxiv.2607.14084},
eprint = {2607.14084},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2607.14084},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Investigating anomalous microwave emission near G107.2+5.20 in Ku-band with the Green Bank Telescope
AU - Jordan E. Shroyer
AU - Bradley R. Johnson
AU - Dillon J. Bass
AU - Anna Dignan
AU - Stuart E. Harper
AU - Brian S. Mason
AU - Andrey Moore
AU - Eric J. Murphy
PY - 2026
DA - 2026/07/31
PB - arXiv
DO - 10.48550/arxiv.2607.14084
UR - https://arxiv.org/abs/2607.14084
AB - Anomalous microwave emission (AME) is 30 GHz-peaking continuum emission thought to arise from spinning dust grains. Observations suggest that the local environment shapes the AME spectral energy distribution (SED), so building a spatially resolved sample of AME regions is a key step towards understanding its emission mechanism. Using the Green Bank Telescope Ku-band receiver, we obtained a ~1 arcmin resolution map of radius 1.25 deg centered on G107.2+5.20. Our first objective was to constrain the low-frequency side of the AME SED with 13 GHz data. Using matched-resolution aperture photometry, we measure the SED from 408 MHz-3 THz and fit two emission models: one including spinning dust, the other optically thick free-free emission. We find that the spinning dust model is superior, with an amplitude of 14.1±1.1 Jy and a peak frequency of 27±2 GHz. Our second objective was to spatially locate excess 13 GHz emission consistent with spinning dust. We compare our Ku-band map to multi-wavelength gas and dust tracers at ~4 arcmin resolution. We observe two sources of 13 GHz excess at 3σ significance consistent with spinning dust emission, though potential contributions from optically thick free-free emission remain ambiguous. ``Region A'' (G106.95+5.19) is spatially coincident with peak dust radiance. ``Region B'' (G107.08+4.90) is spatially coincident with peak PAH abundance. If regions A and B are indeed sources of spinning dust emission, they are a resolved example of how AME-dust correlation varies with environment.
ER -