Here we compare veiling and the Brγ line, as we use both as accretion tracers. The veiling and EW are measurements that are both relative to the continuum flux, and are loosely correlated. However, there is a poor connection between veiling and the Brγ line flux (lower panel). It appears to show that targets can have some veiling before they start to show significant Brγ flux in emission. All objects with a high Brγ line flux also have high veiling, but not vice versa. There may be a warm nonaccreting inner disk contributing to the K-band continuum. The color bar reflects the spectral index, which is also accretion related.