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Table 1

Properties of the sample of carbon-rich AGB stars observed with Herschel (see Sect. 2.4).

Star IRAS Var. P F6.3 μm νLSR d Δd L ⋆ T ⋆ Ṁ g ν∞,g Ṁg/ ν∞,g
name number type (days) (102 Jy) (km s-1) (pc) (pc) (103L⊙) (K) (M⊙ yr-1) (km s-1) ( )
RW Lmi 10131+3049 SRa 6401 25b –1.816 4108 320–710 8.38 247017 5.2 ×10-618 16.518 3.2 ×10-7
V Hya 10491–2059 SR/Mira 5311 12b –16.09 3406,8 330–2160 8.36 216017 2.7 ×10-615 15.020 1.8 ×10-7
II Lup 15194–5115 Mira 5802 6.0b –15.016 6406 470–640 9.16 2000° 1.5 ×10-518 21.018 7.0 ×10-7
V Cyg 20396+4757 Mira 4211 9.7a 15.016 4207 270–740 6.67 187517 1.7 ×10-618 10.518 1.6 ×10-7
LL Peg 23166+1655 Mira 6962 0.9a –31.016 10506 950–1150 11.06 2000° 1.1 ×10-518 13.518 8.5 ×10-7
LP And 23320+4316 Mira 6141 4.0a –17.016 8406,17 610–870 9.76 204017 2.2 ×10-518 13.518 1.6 ×10-6
V384 Per 03229+4721 Mira 5351 4.6a –16.215 7206,17 560–1060 8.46 182017 4.1 ×10-618 14.518 2.8 ×10-7
R Lep 04573–1452 Mira 4271 4.0b 18.512 4135 250–480 5.25,6 229017 1.3 ×10-618 17.012 8.1 ×10-8
W Ori 05028+0106 SRb 2121 3.3a 18.816 3775 220–460 8.05,8 262517 2.1 ×10-718 12.012 1.8 ×10-8
S Aur 05238+3406 SR/Mira 5961 1.7b –21.012 10106,17 300–1130 9.46 194017 4.5 ×10-618 25.012 1.8 ×10-7
U Hya 10350–1307 SRb 4501 2.8b –31.016 2085 160–980 4.25,8 296517 1.4 ×10-718 7.012 2.0 ×10-8
QZ Mus 11318–7256 Mira 5351 4.0b –2.016 6606 620–720 8.46 2200° 4.8 ×10-615 26.515 1.8 ×10-7
Y CVn⋆ 12427+4542 SRb 1571 3.7a 21.016 3205 170–340 8.75,8 276017 3.2 ×10-718 8.512 3.8 ×10-8
AFGL 4202 14484–6152 Mira 5663 4.4b 24.415 6116,15 570–900 8.96 2200° 4.5 ×10-615 19.015 2.4 ×10-7
V821 Her 18397+1738 Mira 5114 4.4b –0.516 7506 600–900 7.56 2200° 2.8 ×10-618 13.018 2.2 ×10-7
V1417 Aql 18398–0220 Mira 6174 4.2a 3.015 8706 870–950 10.86 2000° 1.7 ×10-519 36.015 4.7 ×10-7
S Cep 21358+7823 Mira 4871 7.0a –15.515 4075 380–720 6.45,6 209517 1.4 ×10-618 21.518 6.4 ×10-8
RV Cyg 21412+3747 SRb 2631 1.1b 17.012 6408 350–850 13.48 267517 2.0 ×10-712 13.012 1.5 ×10-8

Notes. The first six sources are covered in the MESS program; the rest in the OT2 program. Given per source are the IRAS number, variability type (Mira or semiregular), pulsational period (P), 6.3 μm flux (F6.3 μm, with the suffix a for ISO SWS data and b for photometric data), adopted distance (d), range of distance estimates in the literature (Δd), stellar velocity with respect to the local standard of rest (νLSR), stellar luminosity (L⋆), stellar effective temperature (T⋆; with ° added for assumed values), gas mass-loss rate (Ṁg), terminal gas velocity (ν∞,g), and wind density tracer (Ṁg/ ν∞,g). The source denoted with (⋆) is of spectral type CJ and is possibly an extrinsic carbon star (Abia et al. 2010).

Reference.

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