Catalina amplitudes plotted as a function of pulsation periods for MSRa in the halo. All stars plotted here have |Z| > 5 kpc. Panel a: our sample stars obeying (J − K_s)₀ < 1.3. Panel b: carbon stars. We note the large difference of these two distributions, strongly suggesting that most of the stars in the upper panel are not carbon rich. All stars plotted here have |Z| > 5 kpc.