$\begin{figure}\includegraphics[angle=270,width=15cm,clip]{H2019b1.eps}\end{figure}$

Figure B1: Static (or very low amplitude variable) giant stars. BS4432: K4.5; BS4371: M0; BS3923: M1, BS5301: M2 (= ET Vir, SRb, $\delta V=0.2$ , P=80), BS4267: M5; BS1492: M8 (= R Dor, SRb, $\delta V=1$ ). Due to partial saturation of the detector during the observation of R Dor, the apparently strong and unusually shaped TiO absorption at 1.25 $\mu$ m and the dip around 1.65 $\mu$ m require confirmation. Shaded areas are those that could not (in general) be corrected for telluric absorption in a satisfactory way

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b2.eps}\end{figure}$

Figure B2: Supergiant stars. Spectral types from the literature are, from top to bottom are: M0I, M1I, M2-3I, M2I, M4I

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b3.eps}\end{figure}$

Figure B3: Supergiant stars. Spectral types from the literature are, from top to bottom are: M4.5I, M5I, M4-5I, M4I, M3-4I. UY Sct, V774 Sgr, CL Car and EV Car are known low amplitude semi-regular variables. The absorption line near 1.08 $\mu$ m in CL Car is real

B.2. Small amplitude O-rich LPVs

$\begin{figure}\includegraphics[angle=270,width=15cm,clip]{H2019b4.eps}\end{figure}$

Figure B4: KV Car: P=150.0, $\delta V=0.8$ . For display purposes, the spectra with the coolest energy distribution are placed at the bottom, the hottest ones at the top (here and in all further graphs). As for SYVel (Fig. B6), comparison with giant and supergiant spectra suggests that KV Car may be a relatively massive and luminous AGB star

$\begin{figure}\par\includegraphics[angle=270,width=15cm,clip]{H2019b5.eps}\end{figure}$

Figure B5: SV Lib: P=402.7, $\delta V=1.3$ (see however Appendix A). Note the clean CO spectrum between 1.55 and 1.7 $\mu$ m, reminiscent of the S/C Mira BH Cru (Fig. B28). Phases: see Appendix A

$\begin{figure}\par\includegraphics[angle=270,width=15cm,clip]{H2019b6.eps}\end{figure}$

Figure B6: SY Vel: P=63.0, $\delta V=1.3$ . Comparison with the giant BS4267 (Fig. B1) and with the supergiant HD115283 (Fig. B2) suggests this may be a relatively massive/luminous AGB star

B.3. Other solar neighbourhood O-rich LPVs

$\begin{figure} \includegraphics[angle=270,width=15cm,clip]{H2019b7.eps}\end{figure}$

Figure B7: S Car: P=149.5, $\delta V=5.4$ . Cycle to cycle variations are obvious: the three top spectra correspond to maximum light in successive cycles, the two bottom ones to minimum light. Approx. AAVSO/AFOEV phases from top to bottom: 0.1-0.0-0.9-0.4-0.2-0.4-0.5-0.6

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b8.eps}\end{figure}$

Figure B8: RZ Car: P=272.8, $\delta V=6.2$ . GCVS phases from top to bottom: 0.0-0.8-0.2-0.7-0.6

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b9.eps}\end{figure}$

Figure B9: T Cen: P=90.4, $\delta V=3.5$ . GCVS phases from top to bottom: 0.0-0.8-0.4-0.3

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b10.eps}\end{figure}$

Figure B10: R Cha: P=334.6, $\delta V=6.7$ . GCVS phases from top to bottom: 0.1-0.2-0.6-0.3-0.3 (doubtful values)

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b11.eps}\end{figure}$

Figure B11: RY Cra (Jun. 95, GCVS phase 0.9): P=195, $\delta V=1.9$ ; CM Car (Jan. 96, GCVS phase 0.4): P=335, $\delta V=2.5$ . CM Car resembles X Men at a phase close to 0.5, and RY Cra resembles X Men at maximum

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b12.eps}\end{figure}$

Figure B12: U Crt: P=169.0, $\delta V=4$ . The single VI spectrum plotted to illustrate the cool temperatures reached by this star. The available data covers the range M1-M7 in spectral type (instead of staying close to M0 as given in the GCVS). GCVS phases from top to bottom: 0.2-0.5-0.9-0.8 (doubtful values; probably too high by about 0.3 cycles)

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b13.eps}\end{figure}$

Figure B13: RS Hor: P=202.9, $\delta V=5.2$ . GCVS phases from top to bottom: 0.8-0.6-0.4

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b14.eps}\end{figure}$

Figure B14: BD Hya: P=117.4, $\delta V=1.8$ . GCVS phases from top to bottom: 0.6-0.2-0.2-0.2 (doubtful values, top spectrum probably closer to maximum

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b15.eps}\end{figure}$

Figure B15: RS Hya: P=338.6, $\delta V=5.2$ . GCVS phases from top to bottom: 0.7-0.6-0.8-0.5-0.5-0.3-0.3 (doubtful values)

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b17.eps}\end{figure}$

Figure B17: S Lib: P=192.9, $\delta V=5.5$ . The unmatched VI spectrum is plotted to illustrate the cool temperatures reached by this star. The 15 days delay between the optical and NIR observations in June 95 may explain the absence of P $\beta$ emission despite the strong H $\alpha$ line. GCVS phases from top to bottom: 0.3-0.5-0.8 (doubtful values; probably too high by about 0.3 cycles)

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b19.eps}\end{figure}$

Figure B19: X Men: P=380.0, $\delta V=3.6$ . GCVS phases from top to bottom: 0.7-0.2-0.3-0.4 (doubtful values; probably too low by about 0.2 cycles)

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b20.eps}\end{figure}$

Figure B20: R Phe: P=269.3, $\delta V=6.9$ . GCVS phases from top to bottom: 0.6-0.9-0.0-0.3-0.5 (in good agreement with AAVSO light curve)

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b21.eps}\end{figure}$

Figure B21: S Phe: P=141.0, $\delta V=2.0$ . GCVS phases from top to bottom: 0.6-0.9-0.1-0.2-0.4 (doubtful values)

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b22.eps}\end{figure}$

Figure B22: WW Sco: P=431, $\delta V=4.1$ . Potentially metal rich star. GCVS phases from top to bottom: 0.3-0.3-0.5

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b23.eps}\end{figure}$

Figure B23: Upper 2 spectra: Z Aql: P=129.2, $\delta V=6.6$ ; bottom 2 spectra; SV Tel: P=225.5, $\delta V=3$ . GCVS phases from top to bottom: 0.5-0.0 for Z Aql, 0.7-0.0 for SV Tel

B.4. Obscured O-rich LPVs

$\begin{figure} \includegraphics[angle=270,width=15cm,clip]{H2019b24.eps}\end{figure}$

Figure B24: OH/IR stars. The quasi-absence of CO absorption in U Equ indicates CO or circumstellar dust emission for this star, while circumstellar dust absorption is probably partly responsible for the red colours of the others

B.5. O-rich LPVs in the Galactic Bulge

B.6. Luminous red O-rich stars in the LMC and SMC

$\begin{figure} \includegraphics[angle=270,width=15cm,clip]{H2019b26.eps}\end{figure}$

Figure B26: Luminous red stars in the LMC (HV2255 and HV2360) and in the SMC (N371R20)

B.7. C-rich LPVs

$\begin{figure} \includegraphics[angle=270,width=15cm,clip]{H2019b27.eps}\end{figure}$

Figure B27: Bottom spectrum: S Cen: P=65, $\delta V=1.5$ . Top 3 spectra: T Cae: P=156, $\delta V=1.8$ . Carbon stars. GCVS phases for T Cae from top to bottom: 0.0-0.8-0.4

$\begin{figure} \par\includegraphics[angle=270,width=15cm,clip]{H2019b28.eps}\end{figure}$

Figure B28: BH Cru: P=520, $\delta V=2.8$ . S/C star whose period increased from 421 to about 535 days over the last 20 years (Bedding et al. 2000). The unmatched optical spectrum taken in March 1996 (not shown) also displays H $\alpha$ emission. GCVS phases from top to bottom: 0.0-0.3-0.4 (in good agreement with AAVSO data)

B.8. Obscured C-rich LPV

$\begin{figure} \includegraphics[angle=270,width=15cm,clip]{H2019b31.eps}\end{figure}$

Figure B31: R Lep: P=427.1, $\delta V=6.2$ . Carbon star. GCVS phases from top to bottom: 0.3-0.9-0.8-0.7 (doubtful values, bottom 3 spectra probably closer to minimum, as also suggested by AFOEV data)

Appendix B: Spectra