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Table 6

Overview of the evolutionary stage, atmospheric chemistry, pulsational type, spectral type, and stellar parameters of the sample stars.

IRAS OTHER Evol. Chem. Puls. Sp. Type d P T eff Ref. L  ⋆  Ref. R  ⋆  (V−K)0 K mean
Type Type (pc) (days) (K) (L⊙) (R⊙) (mag)
– NML Cyg RSG O SRc M6I 1220 1280 3834 – 272035 – 1183 3.9 12.3
00192-2020 T Cet AGB OS SRb M5/M6Ib/II 237 158 2788 – 4900 – 312 6.5 –0.8
01037+1219 WX Psc AGB O OH/IR M8/10II 740 660 2750 – 13914 – 520 13.3 2.3
01246–3248 R Scl AGB C SRb CII 475 370 2295 – 9527 – 617 6.9 –0.1
01304+6211 V669 Cas AGB O OH/IR M9III 6210 1525 2750 – 38012 – 859 –2.3 13.7
02168–0312 o Cet AGB O MIRA M7e 107 331 2193 – 6099 – 541 8.7 2.4
03507+1115 IK Tau AGB O MIRA M8/10IIe 260 470 2667 – 9258 – 451 13.9 –0.5
04566+5606 TX Cam AGB O MIRA M8.5 380 557 2779 – 11360 – 460 15.4 –0.6
05073+5248 NV Aur AGB O MIRA M10 1200 635 2500 – 13284 – 615 1.6 2.9
05524+0723 Alpha Ori RSG O SRc M2Iab 131 2335 3546 – 508887 – 1891 4.8 –4.3
07209-2540 VY CMa RSG O SRc M2/4II 1500 2000 3605 1 428303 – 1679 –0.4 8.1
09448+1139 R Leo AGB O MIRA M8IIIe 82 309 2890 – 5617 – 299 11 2.5
09452+1330 CW Leo AGB C MIRA C9, 5 120 630 2000 2 9820 – 826 15.1 1.1
10131+3049 RW LMi AGB C SRa Ce 440 640 2000 2 5912 – 641 11.8 1.2
10329–3918 U Ant AGB C LB C5, 3 256 365 2775 – 5640 9 325 5.9 –0.5
10350–1307 U Hya AGB C SRb C6,3 161 450 2982 – 11123 – 395 5.5 –0.7
10491–2059 V Hya AGB C SRa C6, 5e 2160 530 2007 – 5414 – 609 8 –0.1
12427+4542 Y CVn AGB C SRb C7Iab 217 157 2750 – 4853 – 307 5.9 –0.7
13269-2301 R Hya AGB O MIRA M7IIIe 118 388 2128 – 7375 – 631 9 2.4
13462–2807 W Hya AGB O SRa M7e 77 361 3129 – 4525 – 229 10.7 3.1
14219+2555 RX Boo AGB O SRb M7.5e 155 340 3010 – 8912 – 347 –1.7 1.9
15194–5115 II Lup AGB C MIRA C 500 575 2400 2 8933 – 547 4.4 1.7
16269+4159 G Her AGB O SRb M6III 310 89 3297 – 3121 – 171 –5.5 11.4
17123+1107 V438 Oph AGB O SRb M8e 416 169 2890 – 5163 – 286 14.8 0.6
17411–3154 AFGL 5379 AGB O OH/IR (OH) 1190 1440 2750 – 35484 – 830 5.7 9.5
18050–2213 VX Sgr RSG O SRc M4eIa 1570 732 3535 3 102294 – 853 0.4 7.7
18308–0503 AFGL 5502 YSO O YSO – 3100 – – – 21000 10 – 1.5 13.2
18333+0533 NX Ser AGB O MIRA (CO) 2480 795 3300 – 17395 – 403 4.9 3.6
18348–0526 OH 26.5+0.6 AGB O OH/IR (OH) 1370 1570 2750 – 39362 – 874 –0.4 8.1
18397+1738 IRC +20370 AGB C MIRA Ce 600 637 2200 2 9933 – 686 4.6 1.8
18448–0545 R Sct AGB O Rva K0Ibpv 431 146 5000 4 4000 4 84 5.6 12.1
18476–0758 S Sct AGB C SRb C6, 4 398 148 2425 – 4634 – 386 6.6 0.5
19114+0002 AFGL 2343 HYPERGIANT O SRd G5Ia 4080 200 5418 – 199526 11 507 0.3 14.8
19126–0708 W Aql AGB S MIRA S6e 680 490 2800 5 9742 – 419 15.4 0.5
19192+0922 OH 44.8–2.3 AGB O OH/IR (OH) 1130 552 2750 – 11228 – 467 4.2 13.6
19244+1115 IRC +10420 HYPERGIANT O SRd A5Ia 5000 – 4442 – 630957 11 1342 2.2 13.9
19283+1944 AFGL 2403 AGB O OH/IR (OH) 2300 – 2750 – 1574 12 174 3.2 13.3
19486+3247 Chi Cyg AGB S MIRA S6 +/1e 149 408 2000 6 7813 – 737 16 1.9
20075–6005 X Pav AGB O SRb M8III 270 199 2046 – 5849 – 608 9.3 –1.1
20077–0625 IRC –10529 AGB O OH/IR M 620 680 2750 – 14421 – 529 2.3 2.1
20120–4433 RZ Sgr AGB S SRb Se 730 223 2710 7 6396 – 363 12.7 1.2
20396+4757 V Cyg AGB C MIRA C5, 3e 271 421 2581 – 6472 – 402 6.3 0.4
21419+5832 Mu Cep RSG O SRc M2Ia 390 730 3660 8 111215 – 830 –5.9 8.5
21439–0226 EP Aqr AGB O SRb M8IIIv 135 55 2302 – 2145 – 291 8.2 –1.6
21554+6204 GLMP 1048 AGB O OH/IR (OH) 2030 – 2750 – 4984 13 311 3.2 14.8
22177+5936 OH 104.9+2.4 AGB O OH/IR (OH) 2300 1620 2750 – 40871 – 891 1.1 13.9
22196–4612 pi1 Gru AGB S SRb S5, 7e 152 150 2257 – 4683 – 447 8.4 5.8
23166+1655 LL Peg AGB C MIRA C 980 696 2000 2 10887 – 869 2 10.5
23320+4316 LP And AGB C MIRA C 630 614 2000 2 9561 – 815 1.6 3.5
23558+5106 R Cas AGB O MIRA M7IIIe 106 430 3129 – 8331 – 310 16.8 1.8

Notes. Spectral types were taken from (i) the SIMBAD database; (ii) Kwok et al. (1997); (iii) Feast & Whitelock (2000); (iv) Justtanont et al. (1996); (v) Suárez et al. (2006); and (vi) Castro-Carrizo et al. (2007). For each star the following fundamental parameters are specified: distance d, period of pulsation P, effective temperature Teff, luminosity L ⋆ , and stellar radius R ⋆ . Teff and L ⋆  were determined according to the methods presented in Appendix C. (V−K)0is the V−K colour that was dereddened according to the method discussed in Appendix B. Kmean is the mean K-band magnitude.

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