Investigation of the Origin of the Anomalous Microwave Emission in
  Lambda Orionis
  The anomalous microwave emission (AME) still lacks a conclusive explanation.
This excess of emission, roughly between 10 and 50 GHz, tends to defy attempts
to explain it as synchrotron or free-free emission. The overlap with
frequencies important for cosmic microwave background explorations, combined
with a strong correlation with interstellar dust, drive cross-disciplinary
collaboration between interstellar medium and observational cosmology. The
apparent relationship with dust has prompted a ``spinning dust'' hypothesis.
The typical peak frequency range of the AME profile implicates spinning grains
on the order of 1 nm. This points to polycyclic aromatic hydrocarbons (PAHs).
We use data from the AKARI/Infrared Camera (IRC), due to its thorough PAH-band
coverage, to compare AME from the Planck Collaboration astrophysical component
separation product with infrared dust emission in the Orionis AME-prominent
region. We look also at infrared dust emission from other mid IR and far-IR
bands. The results and discussion contained here apply to an angular scale of
approximately 1{\deg}. We find that certainly dust mass correlates with AME,
and that PAH-related emission in the AKARI/IRC 9 {\mu}m band correlates
slightly more strongly. Using hierarchical Bayesian inference and full dust
spectral energy distribution (SED) modeling we argue that AME in
{\lambda}Orionis correlates more strongly with PAH mass than with total dust
mass, lending support for a spinning PAH hypothesis within this region. We
emphasize that future efforts to understand AME should focus on individual
regions, and a detailed comparison of the PAH features with the variation of
the AME SED.
