ner_tags: O O O B-CelestialObject O O O O O B-Wavelength O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O O O O O B-CelestialObject O O O O O B-Survey O O O O O O O O B-Telescope O O O O O O O B-Wavelength O O B-CelestialObject O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-ObservationalTechniques I-ObservationalTechniques O O O O O O O O O O O O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObjectRegion O B-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O B-CelestialObject O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O B-Wavelength O O O O O
tokens: currently say whether IC10 is an example of the radioFIR conspiracy as the sample size used to determine the radioSFR relation is small with a large scatter. Future studies with a larger sample would reveal the true significance of the deviation. 5 CONCLUSIONS We present high-resolution e-MERLIN observations of the nearby dwarf irregular galaxy IC10 as a part of the LeMMINGs project. Our main conclusions are as follows. Our e-MERLIN observations reveal 11 compact radio sources at 1.5GHz coincident with IC10s star-forming disc, five of which also have detections at 5GHz. Although we cannot conclusively classify all sources on the basis of their spectral index due to differences in sampling the uv plane, we gain insight into the nature of each source through the use of low-resolution multiwavelength data, the positional coincidence with features at other wavelengths such as H and 70m, and an estimate of their brightness temperature. Based on our analysis of the expected background source counts, the number of detected sources is consistent with them all being background sources. However, as some sources closely trace compact emission in maps at other wavelengths, giving us confidence that some of these sources do in fact belong to IC10. We find that of the 11 sources, three likely reside in IC10 (sources 1, 2 and 4), all of which are H ii regions; five are background sources (sources 3, 5, 6, 9, 10) and three are yet to be conclusively classified (sources 7, 8, 11). Based on the time-scale over which SNR are typically observable and the resolution limitations of these high-resolution interferometry observations, we expect that we will not be able to detect any SNR with the present e-MERLIN observations. The only SNe we would expect to be able to detect are very young RSNe, but it is unlikely that we would observe any due to a combination of their short observable time-scales and low SFR observed in IC10. We explore other possible factors that could affect SNR detectability in dwarf irregular galaxies and conclude that e-MERLIN alone is well suited to study SNR in galaxies located at distances greater than 4Mpc due to the spatial frequencies covered by the array. For galaxies closer than 4Mpc, additional VLA observations are required to fully cover the spatial scales that SNR candidates occupy. The same reasons as mentioned above explain why we see no compact sources within the NTSB in IC10 and that the detected sources that belong to IC10 are likely to be compact H ii regions. Based on starburst99 models, we determine lower limits for the stellar cluster masses required to produce these observed compact H ii regions; the largest one is about half the size of 30Doradus in the LMC. We present updated integrated flux densities for IC10, where we subtract the contribution from background sources from literature data. We find a 4percent reduction in the measured flux at 1.5GHz and a 2percent reduction at 4.85GHz. With this updated measurement, we