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Home All issues Volume 501 / No 2 (July II 2009) A&A, 501 2 (2009) 609-617 Full HTML
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Table 1:

Details of the sources/SWS spectra used in this study.
SourceIRAS name AOTa TDTb Class.cSP98d Spec. TypeeRemarks
S stars from Stephenson (1994) used in this study
R And00213+3817 01(2) 40201723 2.SEcSE3 S3, 5-8, 8e18 $\mu $m feat. weak
S Cas01159+7220 01(2) 41602133 3.SEpSE3 S3, 4-5, 8e15 $\mu $m feat., 18 $\mu $m feat. absent, C2H2+HCN abs.
W Aql19126-0708 01(2) 16402335 3.SEpSE3 S3, 9-6, 9e15 $\mu $m feat., 18 $\mu $m feat. absent, C2H2+HCN abs.
R Cyg19354+5005 01(1) 42201625 2.SEbSE3 S2.5, 9-6, 9e18 $\mu $m feat. absent, 10 $\mu $m feat. narrow
$\chi $ Cyg19486+3247 01(2) 15900437 2.SEbSE3 S6, 2-10, 4e18 $\mu $m feat. absent, substructure at 10.2 $\mu $m
AA Cyg20026+3640 01(2) 36401817 2.MN S7, 5-7.5, 6:
RZ Sgr20120-4433 01(2) 14100818 2.SEaSE2 S4, 4ep 
$\pi ^1$ Gru22196-4612 01(2) 34402039 2.SEaSE2 S7, 5e18 $\mu $m feat. absent
RX Lac22476+4047 01(1) 78200427 2.SEaSE1 M7.5Se:
Stars from Stephenson (1994) not included in the S star sample
W Cet23595-1457 01(2) 37802225 2.SEa:- S7e1Low SNR
T Cet00192-2020 01(2) 55502308 2.SEaSE1t M5-6S IIeM supergiant, M, MS or S
RW And00445+3224 01(3) 42301901 7SE3: M5-10e(S6,2e)Low SNR
WX Cam03452+5301 01(2) 81002721 1.NO- S5/5.5e2Low SNR
NO Aur05374+3153 01(1) 86603434 2.SEaSE1 M2S IabSupergiant
LY Mus13372-7136 01(2) 13201304 1.NO- M4IIIe1No dust features
II Lup15954-5114 06 29700401 3.CEc1- SCe3Carbon-rich
ST Her15492+4837 01(3) 41901305 2.SEaSE1 M6-7 IIIaSMS
OP Herf17553+4521 01(1) 77800625 1.NON M5 IIb-IIIa(S)No dust features
HD 16577418058-3658 01(2) 14100603 1.NO:- M2II/IIIe1No dust features, low SNR
S Lyr19111+2555 01(1) 52000546 2.CE:SE2 SCeLow SNR
HR Peg22521+1640 01(2) 37401910 1.NO- S5,1e1No dust features
GZ Peg23070+0824 01(3) 37600306 1.NON: M4S IIINo dust features
Supergiants with 10 $\mu $m features resembling the S stars
KK Per02068+5619 01(1) 45701204 2.SEa- M2 Iab18 $\mu $m feat. weak, UIR
V605 Cas02167+5926 01(2) 61301202 2.SEa:- M2 Iabe418 $\mu $m feat. weak, UIR
AD Per02169+5645 01(2) 78800921 2.SEap- M2.5 Iabe518 $\mu $m feat. weak, UIR
NO Aur05374+3153 01(1) 86603434 2.SEaSE1 M2S Iab18 $\mu $m feat. weak, UIR
V1749 Cyg20193+3527 01(2) 73000622 2.SEbSE3t M3 IabUIR
IRC+40 42720296+4028 01(3) 53000406 2.SEap:- M0-2 Ie618 $\mu $m feat. absent, UIR
CIT 1120377+3901 01(1) 40503119 2.SEb- M3: Iab18 $\mu $m feat. weak
V354 Cep22317+5838 01(2) 41300101 2.SEcSE6 M2.7 Iab15 $\mu $m feat., 18 $\mu $m feat. absent
V582 Cas23278+6000 01(1) 38501620 2.SEcSE5 M4 Ie718 $\mu $m feat. weak, UIR:
Other sources used in this study
IRC+50 09603229+4721 01(2) 81002351 3.CE- Ce2Carbon-rich, ``30'' $\mu $m feature
R Hya13269-2301 01(1) 08200502 2.SEaSE2t M6-9eS(Tc) 
TY Dra17361+5746 01(2) 74102309 2.SEcSE8t M5-8 
a Observing mode used (see de Graauw et al. 1996; Clegg et al. 1996). Numbers in brackets correspond to the scanning speed. b TDT number which uniquely identifies each ISO observation. c Classification of the SWS spectrum from Kraemer et al. (2002), except c1 Sloan et al. (2003). d IR classification in the scheme of Sloan & Price (1998). e Spectral types are from Sloan & Price (1998); except e1 Kharchenko (2001); e2 Buscombe (2001); e3 Buscombe (1998); e4 Humphreys (1970); e5 Blanco (1955); e6 Solf (1978) and e7 Winfrey et al. (1994). f This source is only listed in the first edition of general catalogue of S stars (Stephenson 1995) and is classed M star in the second edition.

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