Upper limits on the mass flux we find for a hypothetical star as a function of the surface X-ray flux, a proxy for coronal temperature, assuming ECMI emission was detected at 120 MHz. The mass flux is in units of the solar mass flux, which we take to be 2 × 10⁻¹⁴ M_⊙ yr⁻¹/(4π R${}_{\odot }^2$). We calculate the upper limits for three different dipole magnetic field strengths, indicated by the different colours. The shaded regions indicate the allowed regions for each corresponding dipole strength. The data points in black show previous measurements of mass-loss rates on low-mass stars from Lim & White (1996), Lim et al. (1996), Gaidos et al. (2000), Wood et al. (2001, 2002, 2005, 2014), Wood & Linsky (2010), Wood (2018), Jardine & Collier Cameron (2019), and Finley et al. (2019) for reference. No error bars are plotted for the literature values as the uncertainties are not reported in the corresponding papers.