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Table 1

List of the observed stars (in order of OH/IR stars, subsequently post-AGB and others and the PN, and finally the massive evolved stars), their IRAS numbers, observation programme, types, morphologies and whether the 69 μm band was detected in the spectrum.

Source name IRAS # pr MM Type Morphology 69 μm OBSID
OH 32.8−0.3 18498−0017 1 1 AGB Outflow1,2,3 + 1342209738
OH 21.5+0.5 18257−1000 2 2 AGB Outflow1,3 + 1342242438
OH 30.1-0.7 18460−0254 3 1 AGB Outflow2,3 + 1342216207
OH 26.5+0.6 18348−0526 4 3 AGB Outflow1,2,3,4,5,6 + 1342207777
OH 127.8+0.0 01304+6211 5 AGB Outflow1,2,3 + combined, see text
AFGL 2403 19283+1944 6 2 AGB Outflow7,8 + 1342245226
IRAS 21554 21554+6204 7 2 AGB Outflow7,9 + 1342247150
AFGL 5379 17411−3154 8 3 AGB Outflow3,4,7 + 1342228537
OH 104.9+2.4 22177+5936 9 1 AGB Outflow2,3,10,11 − 1342212261
AFGL 4259 20043+2653 10 2 AGB Outflow − 1342244918
IRAS 17010 17010−3840 11 1 AGB Outflow2,12 − 1342216176
RAFGL 2374 19192+0922 12 2 AGB Outflow12,13 − 1342244920
WX Psc 01037+1219 13 3 AGB Outflow4,14,15 − 1342202122
IRC +50137 05073+5248 14 2 AGB Outflow7,13,15 − 1342249315
AFGL 2019 17501−2656 15 2 AGB . − 1342252253
RAFGL 4205 14562−5406 16 2 C/O pAGB/pPN Multipolar20 D + 1342249211
AFGL 6815 17150−3224 17 3 pAGB/pPN Bipolar/rings21,22 D + 1342216629
HD 161796 17436+5003 18 3 pAGB/pPN Torus/bipolar16,17 S + 1342208882
IRAS 16342 16342−3814 19 3 pPN Torus/Bipolar18,19 D + 1342216628
CPD −64 2939 14331−6435 20 2 pAGB/pPN .23,24 S + 1342250006
OH 231.8+4.2 07399−1435 21 3 pAGB/pPN Bipolar/binary25,26 D + 1342196695
IRAS 16279 16279−4757 22 3 C/O pAGB Bipolar26,27 D + 1342228204
HDE 330036 15476−4836 23 1 Symbiotic Shells/binary28 + 1342225842
IRAS 09425 09425−6040 24 3 C/O AGB disk?36,40−42 + 1342225564
IRAS 19306 19306+1407 25 2 pAGB/pPN Bipolar29,30 D − 1342244921
HD 331319 19475+3119 26 2 pAGB/pPN Multipolar/torus31 D − 1342245232
Hen 2−90 13064−6103 27 2 pAGB/pPN Torus/binary32 D − 1342248308
Red Rectangle 06176−1036 28 3 pAGB circumbinary disk33−36 + 1342220928
ACHer 18281+2149 29 1 pAGB circumbinary disk37−39 + 1342208896
AR Pup 08011−3627 30 1 RV Tauri circumbinary disk35 − 1342210381
HD 93662 10456−5712 31 1 RV Tauri circumbinary disk35 − 1342211823
IW Car 09256−6324 32 1 RV Tauri circumbinary disk35 − 1342210386
U Mon 07284−0940 33 1 RV Tauri circumbinary disk35 − 1342206993
NGC 6543 17584+6638 34 4 PN Bipolar43,44 + 1342187203
NGC 6302 17103−3702 35 3 PN Bipolar/torus45,46 + 1342230151
NGC 6537 18021−1950 36 3 PN Bipolar, shells47 + 1342231323
CPD –56°8032 17047−5650 37 3 C/O PN Bipolar, torus/disk26,56 + 1342228202
BD +30 3639 19327+3024 38 3 PN Ring50−52 + 1342220601
IRAS 07027 07027−7934 39 2 PN .53,54 − 1342245248
IRAS 17347 17347−3139 40 3 C/O PN Bipolar/torus30,55 − 1342229697
NGC 6720 18517+3257 41 1 PN Bipolar, rings48,49 ? 1342208920
AFGL 4106 10215−5916 42 1 post-RSG Oval/knots26,57 + 1342207818
HD 168625 18184−1623 43 3 pAGB/LBV? Bipolar/torus58,59 + 1342229741
AFGL 2343 19114+0002 44 3 p-AGB/p-RSG Spherical shell26 + 1342208894
AFGL 2298 18576+0341 45 1 Massive Knotty shell60 − 1342207804
IRC +10420 19244+1115 46 3 p-RSG Bipolar61 − 1342208886
NML Cyg − 47 3 Variable Asymmetric62 − 1342198175
V432 Car 11065−6026 48 1 LBV Bipolar63 − 1342212229

Notes. The observation programme numbers refer to: 1) “Forsterite dust in the circumstellar environment of evolved stars”; 2) “Study of the cool forsterite dust around evolved stars”; 3) MESS; 4) “Mapping the distribution of the crystalline silicate forsterite in the Cat’s Eye Nebula (NGC 6543)”.

Reference. (1) Suh & Kwon (2013); (2) de Vries et al. (2010); (3) Justtanont et al. (2006); (4) Justtanont et al. (2012); (5) Chesneau et al. (2005); (6) Groenewegen (2012); (7) De Beck et al. (2010); (8) Begemann et al. (1997); (9) Kemper et al. (2003); (10) Riechers et al. (2004); (11) Riechers et al. (2005); (12) Kwok et al. (1997); (13) Justtanont & Tielens (1992); (14) Decin et al. (2007); (15) Suh (2002); (16) Hoogzaad et al. (2002); (17) Min et al. (2013); (18) Verhoelst et al. (2009); (19) Dijkstra et al. (2003); (20) Sahai et al. (2011); (21) Ramos-Larios et al. (2012); (22) Kwok et al. (1998); (23) Suárez et al. (2006); (24) Gauba & Parthasarathy (2004); (25) Sánchez Contreras et al. (2004); (26) Lagadec et al. (2011); (27) Matsuura et al. (2004); (28) Angeloni et al. (2007); (29) Cerrigone et al. (2009); (30) Sahai et al. (2007); (31) Hsu & Lee (2011); (32) Sahai & Nyman (2000); (33) Waters et al. (1998b); (34) Bujarrabal et al. (2005); (35) de Ruyter et al. (2006); (36) Molster et al. (2001); (37) Van Winckel et al. (1998); (38) Giridhar et al. (2000); (39) Jura & Kahane (1999); (40) Molster et al. (1999b); (41) Molster et al. (2002b); (42) García-Hernández et al. (2006); (43) Waters et al. (1996); (44) Balick (2004); (45) Matsuura et al. (2005c); (46) Kemper et al. (2002); (47) Matsuura et al. (2005b); (48) O’Dell et al. (2007); (49) van Hoof et al. (2010); (50) Gillett et al. (1973); (51) Phillips & Ramos-Larios (2007); (52) Waters et al. (1998a); (53) De Marco & Soker (2002); (54) Zijlstra et al. (1991); (55) de Gregorio-Monsalvo et al. (2004); (56) Cohen et al. (1999); (57) Molster et al. (1999a); (58) Umana et al. (2010); (59) Smith (2007); (60) Buemi et al. (2010); (61) Oudmaijer & de Wit (2013); (62) Monnier et al. (1997); (63) Riera et al. (1995).

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