TY - JOUR
T1 - A Spatially Resolved Radio Spectral Index Study of the Dwarf Irregular Galaxy NGC\,1569
AU - Westcott, Jonathan
AU - Brinks, Elias
AU - Hindson, Luke
AU - Beswick, Robert
AU - Heesen, Volker
N1 - © The Author(s) 2018. Published by Oxford University Press on behalf of The Royal Astronomical Society.
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
PY - 2018/4/21
Y1 - 2018/4/21
N2 - We study the resolved radio continuum spectral energy distribution of the dwarf irregular galaxy, NGC 1569, on a beam-by-beam basis to isolate and study its spatially resolved radio emission characteristics. Utilizing high-quality NRAO Karl G. Jansky Very Large Array observations that densely sample the 1-34 GHz frequency range, we adopt a Bayesian fitting procedure, where we use Hα emission that has not been corrected for extinction as a prior, to produce maps of how the separated thermal emission, non-thermal emission, and non-thermal spectral index vary across NGC1569's main disc. We find a higher thermal fraction at 1 GHz than is found in spiral galaxies (26
-3
+2 per cent) and find an average non-thermal spectral index α =-0.53 ± 0.02, suggesting that a young population of cosmic ray electrons is responsible for the observed non-thermal emission. By comparing our recovered map of the thermal radio emission with literature Hα maps, we estimate the total reddening along the line of sight to NGC1569 to be E(B - V) = 0.49 ± 0.05, which is in good agreement with other literature measurements. Spatial variations in the reddening indicate that a significant portion of the total reddening is due to internal extinction within NGC1569.
AB - We study the resolved radio continuum spectral energy distribution of the dwarf irregular galaxy, NGC 1569, on a beam-by-beam basis to isolate and study its spatially resolved radio emission characteristics. Utilizing high-quality NRAO Karl G. Jansky Very Large Array observations that densely sample the 1-34 GHz frequency range, we adopt a Bayesian fitting procedure, where we use Hα emission that has not been corrected for extinction as a prior, to produce maps of how the separated thermal emission, non-thermal emission, and non-thermal spectral index vary across NGC1569's main disc. We find a higher thermal fraction at 1 GHz than is found in spiral galaxies (26
-3
+2 per cent) and find an average non-thermal spectral index α =-0.53 ± 0.02, suggesting that a young population of cosmic ray electrons is responsible for the observed non-thermal emission. By comparing our recovered map of the thermal radio emission with literature Hα maps, we estimate the total reddening along the line of sight to NGC1569 to be E(B - V) = 0.49 ± 0.05, which is in good agreement with other literature measurements. Spatial variations in the reddening indicate that a significant portion of the total reddening is due to internal extinction within NGC1569.
KW - Cosmic rays -HII regions
KW - ISM: magnetic fields
KW - Methods: data analysis
KW - Radio continuum: galaxies
KW - Techniques: interferometric
UR - http://www.scopus.com/inward/record.url?scp=85046008844&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty028
DO - 10.1093/mnras/sty028
M3 - Article
SN - 0035-8711
VL - 475
SP - 5116
EP - 5132
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -