Microturbulent velocity from stellar spectra: a comparison between different approaches (Research Note)

Abstract

Context --- The classical method to infer microturbulent velocity in stellar spectra requires that the abundances of the iron lines are not correlated with the observed equivalent widths. An alternative method, requiring the use of the expected line strength, is often used to by-pass the risk of spurious slopes due to the correlation between the errors in abundance and equivalent width. Aims --- To compare the two methods and identify pros and cons and applicability to the typical practical cases. Methods --- I performed a test with a grid of synthetic spectra, including instrumental broadening and Poissonian noise. For all these spectra, microturbulent velocity has been derived by using the two approaches and compared with the original value with which the synthetic spectra have been generated. Results --- The two methods provide similar results for spectra with SNR$ > 70, while for lower SNR both approaches underestimate the true microturbulent velocity, depending of the SNR and the possible selection of the lines based on the equivalent width errors. Basically, the values inferred by using the observed equivalent widths better agree with those of the synthetic spectra. In fact, the method based on the expected line strength is not totally free from a bias that can heavily affect the determination of microturbulent velocity. Finally, I recommend to use the classical approach (based on the observed equivalent widths) to infer this parameter. In cases of full spectroscopical determination of all the atmospherical parameters, the difference between the two approaches is reduced, leading to an absolute difference in the derived iron abundances of less than 0.1 dex.