Speaker
Description
Low surface brightness galaxies are not that different from known and
well-studied brighter galaxies — they are also a mixture of stars,
gas, and dust (even though only recently we have found IR counterparts for those unfamiliar objects), and they undergo similar processes, such as dust attenuation and emission, which are essential to explain their physical properties. Those faint sources are considered to be dust-poor. However, the last analysis shows that a few per cent of them can be attenuated at the level of 0.8 magnitudes.
Our previous analysis shows that for main-sequence galaxies, LOFAR measurements can easily substitute infrared data to constrain the star formation rate through the spectral energy fitting method. Can we use the same method to study dust-poor and faint LSBs?
In my talk, I will present our study on the NEP multiwavelength data using more than 1000 LSB galaxies with estimated LOFAR fluxes at 144 MHz.
