We perform an analysis of the diffuse low-frequency Galactic components in the Southern part of the Gould Belt system ( 130 ^ { \circ } \leq l \leq 230 ^ { \circ } and -50 ^ { \circ } \leq b \leq - 10 ^ { \circ } ) .
Strong ultra-violet ( UV ) flux coming from the Gould Belt super-association is responsible for bright diffuse foregrounds that we observe from our position inside the system and that can help us improve our knowledge of the Galactic emission .
Free-free emission and anomalous microwave emission ( AME ) are the dominant components at low frequencies ( \nu < 40 \thinspace GHz ) , while synchrotron emission is very smooth and faint .
We separate diffuse free-free emission and AME from synchrotron emission and thermal dust emission by using Planck data , complemented by ancillary data , using the “ Correlated Component Analysis ” ( CCA ) component separation method and we compare with the results of cross-correlation of foreground templates with the frequency maps .
We estimate the electron temperature T _ { e } from H \alpha and free-free emission using two methods ( temperature-temperature plot and cross-correlation ) and we obtain T _ { e } ranging from 3100 to 5200 K , for an effective fraction of absorbing dust along the line of sight of 30 % ( f _ { d } = 0.3 ) .
We estimate the frequency spectrum of the diffuse AME and we recover a peak frequency ( in flux density units ) of 25.5 \pm 1.5 GHz .
We verify the reliability of this result with realistic simulations that include the presence of biases in the spectral model for the AME and in the free-free template .
By combining physical models for vibrational and rotational dust emission and adding the constraints from the thermal dust spectrum from Planck and IRAS we are able to get a good description of the frequency spectrum of the AME for plausible values of the local density and radiation field .