R Scl Some of these observation of R Scl were published by R Scl Lloyd Evans (1997MNRAS.286..839L) and by R Scl Whitelock et al. (1995MNRAS.276..219W, 1997MNRAS.288..512W). YY Tri Some observations published by YY Tri Whitelock et al. (1994MNRAS.267..711W, 1997MNRAS.288..512W) R For Some observations published by Lloyd Evans (1997MNRAS.286..839L), R For Whitelock et al. (1997MNRAS.288..512W) and R For Olivier et al. (2001MNRAS.326..490O). EV Eri Some observations published by EV Eri Whitelock et al. (1995MNRAS.276..219W, 1997MNRAS.288..512W) V718 Tau Epchtein et al. (1990A&A...227...82E) and 2MASS data obtained V718 Tau before and after SAAO observations, at phases which are similar V718 Tau to our faintest measurements (i.e. not in the gap) suggest that V718 Tau it has been much fainter (K=3.94, 3.88, respectively, e_K~0.7) V718 Tau and redder, than the faintest SAAO measurements. 05418-3224 An observation by Epchtein et al. (1990A&A...227...82E) predating 05418-3224 ours is 3 and 5mag brighter at K and J, respectively. 2MASS 05418-3224 photometry contemporaneous with ours and Fouque et al. 05418-3224 (1992, Cat. ) measurements predating ours are within the 05418-3224 range shown in our light curve. We therefore class this star as 05418-3224 showing obscuration events, but note that the evidence is very 05418-3224 limited. V617 Mon Although Noguchi et al. (1981PASJ...33..373N) present measures V617 Mon distinctly different from ours, a comparison with 2MASS suggests V617 Mon they actually observed BD+08 1312, an M star about 1arcmin away V617 Mon from V617 Mon. V617 Mon The GCVS period is 375d with which the near-infrared observations V617 Mon are not consistent. We use the newly determined 444d which V617 Mon provides a very good fit to our data. 06531-0216 Note that the 2MASS (K=4.45) and Epchtein et al. 06531-0216 (1990A&A...227...82E) (K=2.89) observations do not agree with 06531-0216 the phasing of the SAAO data. The period must therefore be 06531-0216 regarded as uncertain. [ABC89]Car105 The Aaronson et al. (1989ApJS...70..637A) observation (K=5.41), [ABC89]Car105 which predates the SAAO photometry, is much fainter than our [ABC89]Car105 minimum (K=4.48). This may indicate an obscuration event. [W65] c2 While the 2MASS, the 1985 Aaronson et al. (1989ApJS...70..637A) [W65] c2 and the SAAO observations differ by less than 0.1mag at K, the [W65] c2 1988 Aaronson et al. photometry is considerably fainter [W65] c2 (J=9.14, K=7.21). [ABC89]Cir27 The Aaronson et al. (1989ApJS...70..637A) measurement (K=3.87) [ABC89]Cir27 is significantly brighter than the SAAO maximum (K=4.57) and may [ABC89]Cir27 indicate that the source was obscured during the SAAO [ABC89]Cir27 observations. 15471-5644 Too crowded for measurement at JHK, but 2MASS has K=14.8 and 15471-5644 Groenewegen, de Jong & Baas (1993, Cat. ) have 15471-5644 K=11.4, L=4.6, so it is certainly a large amplitude variable. 17446-4048 The Fouque et al. (1992, Cat. ) measurement (K=4.81) is 17446-4048 significantly fainter than the SAAO minimum (K=4.21) and may 17446-4048 indicate that the star was being obscured at the time the 17446-4048 observation was made. 2MASS is also faint (K=4.65) 18036-2344 The Guglielmo et al. (1993, Cat. ) measurement 18036-2344 (K=6.53) is significantly fainter than the SAAO minimum (K=5.81) 18036-2344 and may indicate that the star was in an obscuration phase. 18269-1257 2MASS has K=8.02 on JD2450937, so all our observations are near 18269-1257 maximum and P~700d. R Ori SC star. Some observations published by R Ori Whitelock et al. (2000MNRAS.319..728W). R Lep Some observations published by Whitelock et al. R Lep (1997MNRAS.288..512W) and Lloyd Evans (1997MNRAS.286..839L). ZZ Gem Observations published by Groenewegen et al., 1998MNRAS.293...18G GM CMa Some observations published by GM CMa Whitelock et al. (1997MNRAS.288..512W) RT Gem Observations published by Groenewegen et al., 1998MNRAS.293...18G CL Mon Some observations published by Lloyd Evans (1997MNRAS.286..839L). R CMi SC star. Published by Groenewegen et al. (1998MNRAS.293...18G). VX Gem Observations published by Groenewegen et al., 1998MNRAS.293...18G R Vol Some observations published by R Vol Whitelock et al. (1997MNRAS.288..512W) V346 Pup Some observations published by V346 Pup Olivier et al. (2001MNRAS.326..490O). 08276-5125 Probably not a C star R Pyx Published by Whitelock et al. (2000MNRAS.319..728W) 08439-2734 SC star UW Pyx Observations Published by Whitelock et al. (2000MNRAS.319..728W). UX Pyx Probably not a C star CQ Pyx Some observations published by CQ Pyx Olivier et al. (2001MNRAS.326..490O). CW Leo Some observations published by CW Leo Olivier et al. (2001MNRAS.326..490O) MU Vel Probably not a C star W Sex Some observations published by W Sex Whitelock et al. (2000MNRAS.319..728W) W Sex The difference between the GCVS period of 134d and the Hipparcos W Sex period of 200d was noted by Whitelock et al. W Sex (2000MNRAS.319..728W). Our newly determined period of 195d is W Sex consistent with the Hipparcos value. It is not a Mira. RW LMi Some observations published by RW LMi Olivier et al. (2001MNRAS.326..490O). 10226-5229 Probably not a C star [ABC89]Car10 This is an S star TV Vel Light curve published by Groenewegen et al. (1998MNRAS.293...18G) TV Vel GCVS records this as variability type M with P=365d and no TV Vel indication of any uncertainty. There is no clear source for the TV Vel period. We also classify TV Vel as a Mira, but it is certainly TV Vel a border-line case. Our data are inconsistent with the 365-d TV Vel period. TU Car Not a C star V Hya Some observations published by Lloyd Evans (1997MNRAS.286..839L) V Hya and Olivier et al. (2001MNRAS.326..490O) V354 Cen Probably not a C star [ABC89]Cen50 Probably not a C star BH Cru SC star. Some observations published by BH Cru Whitelock et al. (2000MNRAS.319..728W) BH Cru This is known to have a lengthening period BH Cru (Bateson et al., 1988, RASNZ Publ. Var. Star Sec., 15, 70; BH Cru Walker et al., 1995, Southern Stars, 36, 123; BH Cru Zijlstra et al. 2004MNRAS.352..325Z) and our data, which were BH Cru obtained in two batches with a gap in the middle, suggest a BH Cru change from 491 to 524 d, between 1984/1989 and 1997/2004. RU Vir Some observations published by Whitelock et al. RU Vir (2000MNRAS.319..728W) and Olivier et al. (2001MNRAS.326..490O) V Cru Some observations published by V Cru Whitelock et al. (1997MNRAS.288..512W, 2000MNRAS.319..728W) TT Cen SC star. Some observations published by TT Cen Whitelock et al. (1997MNRAS.288..512W) RV Cen C star with silicate shell. Some observations published by RV Cen Whitelock et al. (1997MNRAS.288..512W, 2000MNRAS.319..728W) II Lup Some observations published by Feast et al. (2003MNRAS.346..878F) V Oph Data published by Whitelock et al. (2000MNRAS.319..728W) 16316-5026 Probably not a C star V2548 Oph Some observations published by V2548 Oph Olivier et al. (2001MNRAS.326..490O). SZ Ara Some observations published by SZ Ara Whitelock et al. (2000MNRAS.319..728W) V833 Her Some observations published by V833 Her Olivier et al. (2001MNRAS.326..490O) FX Ser Some observations published by FX Ser Olivier et al. (2001MNRAS.326..490O) V1280 Sgr Some observations published by Lloyd Evans (1997MNRAS.286..839L). V5104 Sgr Some observations published by V5104 Sgr Olivier et al. (2001MNRAS.326..490O) V1076 Her Some observations published by V1076 Her Olivier et al. (2001MNRAS.326..490O) V1417 Aql Some observations published by V1417 Aql Olivier et al. (2001MNRAS.326..490O) V821 Her Some observations published by V821 Her Olivier et al. (2001MNRAS.326..490O) VX Aql SC star V1418 Aql Some observations published by V1418 Aql Olivier et al. (2001MNRAS.326..490O) 18595-3947 This is not a C star. V1420 Aql Some observations published by V1420 Aql Olivier et al. (2001MNRAS.326..490O) V1293 Aql This is not a C star. V1965 Cyg Some observations published by V1965 Cyg Olivier et al. (2001MNRAS.326..490O) V1965 Cyg The original period is from Jones et al. (1990ApJS...74..785J) V1965 Cyg (who incorrectly associates AFGL 2417 with V1129 Cyg) and there V1965 Cyg is evidence for rather erratic behaviour in both their and our V1965 Cyg light curves. Analysing the two data sets together (using only V1965 Cyg the six observations actually listed in their paper) suggests a V1965 Cyg period of 617d. R Cap Some observations published by Lloyd Evans (1997MNRAS.286..839L) R Cap and Groenewegen et al. (1998MNRAS.293...18G) V442 Vul Some observations published by V442 Vul Olivier et al. (2001MNRAS.326..490O) RV Aqr Some observations published by RV Aqr Olivier et al. (2001MNRAS.326..490O) LL Peg Some observations published by Olivier et al. LL Peg (2001MNRAS.326..490O), Whitelock et al. (1994MNRAS.267..711W) IZ Peg Some observations published by Feast et al. (1985MNRAS.215p..63F) IZ Peg and Whitelock et al. (1994MNRAS.267..711W, 1997MNRAS.288..512W). V477 Mon The original period is from Maffei (1966MmSAI..37..475M) who V477 Mon indicated it as 'M?P=820::days'. The near-infrared V477 Mon observations are not consistent with this value, and we use the V477 Mon newly determined 619 d which provides a very good fit to these V477 Mon data. FU Car The GCVS variability type and period of M: and P=365d, FU Car respectively, come from Luyten (1927BHarO.842....9L) who records FU Car FU Car's variability along with that of another star and notes. FU Car 'The available plates are insufficient for a determination of FU Car the light curves, but the possibility is indicated that both FU Car variables have a period of nearly 1yr, and a range of at least FU Car two magnitudes'. This is consistent with our determination of FU Car 431d and our assertion that it is not a Mira. RT Cap This is not a Mira, and the GCVS period of 393d is inconsistent RT Cap with the 359 d derived here. V518 Pup The 448-d period comes from the all-sky automated survey (ASAS) V518 Pup data base of Pojmaski (2002, Cat. ) who also classifies V518 Pup it as a Mira. The 228-d period derived from the infrared data is V518 Pup inconsistent with the ASAS data. While 228d is the best fit to V518 Pup the infrared photometry, 448d is also a possible solution. In V518 Pup this case, 448d would be preferred and is in fact the value we V518 Pup adopt, but the Mira classification must be regarded as uncertain