The analysis of high-resolution spectra of blue massive stars has allowed us to firmly ascertain the presence of an important non-rotational broadening in O and B-type stars of all luminosity classes (see e.g. Simon-Diaz et al. 2011, BSRSL, 80, 514). Despite it has been commonly referred to as "macroturbulent broadening", results from the analyses make its interpretation as the effect of turbulent motions quite improbable. An alternative physical mechanism suggested as the origin of this extra broadening relates to oscillations. As indicated by recent simulations by Aerts et al. (2009, A&A, 508, 409) this scenario offers a plausible explanation that is now being tested observationally (e.g. Simon-Diaz et al. 2010, ApJL, 720, 174). In this contribution, I will provide an overview of our present knowledge about this intriguing line-broadening, also summarizing the main results obtained to date in our project aimed at investigating the "macroturbulent" broadening in O and B stars and its possible connection to spectroscopic variability phenomena and stellar oscillations. The following questions will be treated in this contribution: 1) How v*sin i measurements in massive stars are affected when "macroturbulent" broadening is taken into account? 2) Where in the OB star domain is this extra-broadening present? 3) Is there any dependence of the characteristics of the "macroturbulent" broadening with metallicity? 4) Should "macroturbulent" broadening actually be called "pulsational" broadening? 5) Is this spectroscopic feature a single-snapshot alternative to detect and investigate stellar pulsations in the realm of massive stars?