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Up: A catalogue of symbiotic

4 Classification notes and comments on particular objects

Symbiotic stars

004=SMC3 V magnitude during outburst.

005=SMC N60 IR-type S -Kenyon 1986,Mürset et al. 1996, D -Allen 1984.

008=AX Per Incorrect coordinates given by Allen 1984,Kenyon 1986.

009=V471 Per This star appears in previous symbiotic catalogs Allen 1984,Kenyon 1986 as V741 Per. The correct name is V471 Per as given in the General Catalog of Variable Stars Kholopov 1985.


 
Table 2: continued
No. Cool-star spectrum Radio IRAS IRAS References
    [mJy] F12[Jy] F25[Jy]  
s01 C(Westerlund et al. 1991)       Meyssonnier & Azzopardi 1993 (fc) Westerlund et al. 1991 (spc) Belczynski 2000 (class)
s02 G-K(Morgan et al. 1992)       Bohannan 1974 (fc) Morgan et al. 1992 (class)
s03 C(Downes & Keyes 1988)       Downes & Keyes 1988 (spc) Belczynski 2000 (class)
s04     0.53 0.25L Jorissen 2000 (class)
s05 F2:(Meinunger 1980)       Meinunger 1980 (fc) Kenyon 1986 (class)
s06 M6,M5(Iijima 1984,Taranova 1986)   6.60 2.65 Tshernova 1949 (fc) Iijima 1984 (spc) Belczynski 2000 (class)
s07 C6.2(Keenan & Morgan 1941)   3.28 0.84 Greene & Wing 1971 (spc) Dalmeri et al. 1997 (class) Johnson et al. 1988 (parm)
s08 S?,M?(MacConnell 1983)   2.33 0.69 Belczynski 2000 (class)
s09 late M,M6,M(Allen 1978,Seal 1995,Pereira et al. 1998)   0.90 0.28L Allen 1984 (fc,class) Pereira et al. 1998 (spc)
s10 late M,M9(Downes & Wallace 1996,Kirkpatrick et al. 1997)       Downes & Wallace 1996 (fc,spc) Belczynski 2000 (class)
s11     1.14 0.41L Jorissen 2000 (class)
s12         Milone 1990 (fc) Kilkenny 1989 (spc,class)
s13 M3,M4(Schulte-Ladbeck 1988,van Genderen 1979)       van Genderen et al. 1974,Schulte-Ladbeck 1988 (spc) Kenyon 1986 (class) van Genderen 1979 (parm)
s14 M3-5(Liller & Jones 1996)       Duerbeck 1987 (fc) Belczynski 2000 (class) Liller & Jones 1996 (spc,parm)
s15 M3(Garcia et al. 1983) <0.8(20  cm) 2.8 0.74 Garcia et al. 1983 (fc,spc,class) Tomasella et al. 1997 (parm)
s16 Mep?(Sanduleak & Stephenson 1973) 2.54(6  cm)     Belczynski 2000 (class)
s17 M2p(Bond 1978)       Meinunger 1980 (fc) Bond 1978 (spc) Kenyon 1986 (class)
s18 K0-M3(Corradi 1995) 21(6  cm) 3.42 12.57 Kohoutek 1982 (fc) Corradi 1995 (spc) Belczynski 2000 (class)
s19 K5(Miko\lajewska et al. 1997)       Miko\lajewska et al. 1997 (spc,class,parm)
s20 M1(Miko\lajewska et al. 1997) <0.21(6  cm) 0.67L 0.28L Allen 1984 (fc,spc,class)
s21 G?,G2-K0(Cieslinski et al. 1997,Cieslinski et al. 1998)       Cieslinski et al. 1997 (fc,spc) Belczynski 2000 (class)
s22         Kilkenny 1989 (spc,class)
s23         Perek & Kohoutek 1967 (fc) Miko\lajewska et al. 1997 (class,spc)
s24   26.4(6  cm) 1.24 1.10 Perek & Kohoutek 1967 (fc) Belczynski 2000 (class)
s25 K2,G-K(Lutz 1977,Stenholm & Acker 1987) 9.0(6  cm) 0.69L 1.67: Perek & Kohoutek 1967 (fc) Aller et al. 1987 (spc) Belczynski 2000 (class)
s26 Mira?,C(Dahlmark 1994,Munari et al. 1998)   1.79 0.62 Dahlmark 1994 (fc) Munari et al. 1998 (spc,class)
s27 Mira?,late(Bond 1976,Acker et al. 1987) 4(2  cm) 5.96 2.66 Perek & Kohoutek 1967 (fc) Belczynski 2000 (class)
s28   6.0(6  cm)     Perek & Kohoutek 1967 (fc) Belczynski 2000 (class) Archipova et al. 1985 (spc,parm)
s29 OH/IR (Seaquist & Ivison 1994) 0.44 (3.6  cm) 42.9 46.0 Seaquist & Ivison 1994 (class,parm)
s30 Mira M2,M4(Kolotilov et al. 1996,Josselin et al. 1998) <9(2  cm) 189.4 170.4 Herbig & Rao 1972 (fc) Kolotilov et al. 1996 (spc,class) Kolotilov et al. 1991 (parm)


010=o Ceti Cool component is Mira Whitelock 1988 of type M2-7 III Karovska et al. 1997, UV spectrum shows emission lines with ionization potentials up to 54.4 eV Karovska et al. 1993 and in the optical spectrum there are emission lines of H I and He I Yamashita & Maehara 1977. Preliminary orbit with orbital period of 400 yrs was

reported in Baize 1980, but recent high precision interferometric observations show that the apparent binary separation is much larger than predicted, and imply orbital period much longer then 400 yrs Karovska et al. 1993.

011=BD Cam Cool component is S giant of type S5.3 Keenan 1954; UV spectra shows emission lines with ionization potential up to 77.5 eV Ake et al. 1993. 24.76-day periodicity estimated from BVRI photometry; pulsational origin has been suggested Adelman 1998.

016=UV Aur Although there has been some controversy over the interpretation of the 395-day period sometimes attributed to orbital motion (e.g. Blair et al. 1983), we believe that it is due to pulsation (see Groenewegen & Whitelock 1996 for discussion). The object is thus classified as a C-rich symbiotic Mira with little dust (S-type). The broad-band polarimetric data show a periodicity of $\sim 14$yrs which may be due to orbital motion Khudyakova 1985.

017=V1261 Ori Cool component is S giant of type S4.1 Jorissen et al. 1996; UV spectrum shows emission lines with ionization potential up to 77.5 eV Ake et al. 1991.

018=LMC1 IUE spectra described in Mürset et al. 1996.

020=Sanduleak's star In the optical spectrum, there is an emission feature at 6825 Å Morgan 1992; moreover, there are emission lines with an ionization potential up to 108.8 eV Morgan 1992,Allen 1980 including lines of H I and He I Mürset et al. 1996. The IUE spectra are described in Mürset et al. 1996.

023=BX Mon IRAS data from Kenyon et al. 1988.

024=V694 Mon Object in permanent outburst Maran et al. 1991; contains M3-5 giant Panferov et al. 1997,Allen 1978; optical spectrum shows emission lines of H I and He I with highly blueshifted ( $\sim 2000-7000$km s-1) shell absorption Allen 1978,Panferov et al. 1997,Meier et al. 1996 and emission lines of singly-ionised metals Panferov et al. 1997 over an A-B type continuum Panferov et al. 1997. VK magnitudes are appropriate for the outburst.


 

Table 3. Orbital photometric ephemerides for symbiotic and suspected symbiotic stars

No. Star Ephemeris Eclipse Ref.
003 EG And Min(UV) = JD 2445380 + 481$\times$E Yes Vogel 1991
008 AX Per Min( $m_{\rm vis}/m_{\rm pg}$) = JD 2436667 + 680.8$\times$E Yes Miko\lajewska & Kenyon 1992
017 V1261 Ori Min(Vyb) = JD 2445494 + 642$\times$E Yes Jorissen et al. 1992,Jorissen 1997
023 BX Mon Min( $m_{\rm pg}$) JD 2449530 + 1401$\times$E Yes Dumm et al. 1998
024 V694 Mon Min( $ m_{\rm pg}/B$) = JD 2437455 + 1930$\times$E No Doroshenko et al. 1993
033 SY Mus Min( $ m_{\rm vis}$) = JD 2450176 + 625$\times$E Yes Dumm et al. 1999
045 RW Hya Min(UV) = JD 2445072 + 370.2$\times$E Yes Kenyon & Miko\lajewska 1995
050 V417 Cen Min( $m_{\rm pg}$) = JD 2427655 + 245.7$\times$E ? van Winckel et al. 1994
057 T CrB Min(UBV) = JD 2435687.6 + 227.67$\times$E No Lines et al. 1988
058 AG Dra Max(U) = JD 2443886 + 554$\times$E No Meinunger 1979
071 CL Sco Min( $m_{\rm pg}$) = JD 2427020 + 624.7$\times$E No Kenyon 1986
092 RT Ser Max(B) = JD 2446600 + 4500$\times$E No Shugarov et al. 1997
093 AE Ara Min( $ m_{\rm vis}$) = JD 2448571 + 830$\times$E ? Miko\lajewska et al. 2000
132 YY Her Min(V) = JD 2448945 + 590$\times$E No Munari et al. 1997
133 V2756 Sgr Min( $m_{\rm pg}$) = JD 2437485 + 243$\times$E Yes? Hoffleit 1970
134 FG Ser Min(B) = JD 2448492 + 650$\times$E Yes Munari et al. 1992
142 AR Pav Min( $m_{\rm vis}/m_{\rm pg}$) = JD 2411265.6 + 604.46$\times$E Yes Skopal et al. 2000
145 V443 Her Min(U) = JD 2443660 + 594$\times$E No Kolotilov et al. 1995
149 V2601 Sgr Min( $m_{\rm pg}$) = JD 2429850 + 850$\times$E Yes? Hoffleit 1968
156 FN Sgr Min( $ m_{\rm vis}$) = JD 2441750 + 567.2$\times$E Yes Miko\lajewska et al. 2000
160 V1413 Aql Min(B) = JD 2446650 + 434.1$\times$E Yes Munari 1992
166 BF Cyg Min(V) = JD 2415058 + 756.8$\times$E Yes Miko\lajewska et al. 1989
167 CH Cyg Min(U) = JD 2446275 + 5700$\times$E Yes Miko\lajewski et al. 1988
172 CI Cyg Min( $ m_{\rm pg}/B$) = JD 2442687.1 + 855.6$\times$E Yes Miko\lajewska 1997
176 PU Vul Min( $ m_{\rm vis}$) = JD 2444550 + 4900$\times$E Yes Nussbaumer & Vogel 1996
177 LT Del Min(U) = JD 2445910 + 478.5$\times$E No Arkhipova et al. 1995
181 V1329 Cyg Min(V) = JD 2444890.0 + 956.5$\times$E Yes Schild & Schmid 1997
185 AG Peg Max(V) = JD 2442710.1 + 816.5$\times$E No Fernie 1985
187 Z And Min( $ m_{\rm vis}$) = JD 2442666 + 758.8$\times$E No Formiggini & Leibowitz 1994
s13 V748 Cen Min(V) = JD 2441917 + 566.5$\times$E Yes van Genderen et al. 1974


026=RX Pup Highly variable radio emission Ivison & Seaquist 1994. Nebula resolved at optical and radio wavelengths with a possible jet-like feature in the [N II] line (Corradi et al. 1999 and references therein).

027=Hen 3-160 IRAS data from Kenyon et al. 1988.

028=AS 201 A spherical nebula detected in H$_\alpha$ and [N II] lines (Corradi et al. 1999 and references therein).

029=KM Vel Cool component is Mira Whitelock 1988,Feast et al. 1983 of M spectral type Schwarz et al. 1995; optical spectrum shows emission lines with ionization potential up to 41.0 eV Allen 1976 and emission lines of H I and He I Seal 1990. Finding chart in Perek & Kohoutek 1967 is incorrect and no other has been published.

032=SS73 29 IUE observations reported in Munari & Buson 1994. IRAS data from Kenyon et al. 1988.

033=SY Mus The system inclination, $i=101\hbox{$.\!\!^\circ$ }1 \pm 2\hbox{$.\!\!^\circ$ }5$, and the position angle of the line-of-nodes, $\Omega=58\hbox{$.\!\!^\circ$ }6 \pm 1\hbox{$.\!\!^\circ$ }7$, has been derived from spectropolarimetric studies of the Raman-scattered O VI emission lines Harries & Howarth 2000,Harries & Howarth 1996.

034=BI Cru A bipolar nebula resolved in the optical (Corradi et al. 1999 and references therein) with the bipolar lobes and associated outflows perpendicular to the position angle of intrinsic scattering polarization Harries 1996.

036=TX CVn Low ionization potential (IP $_{\rm max} = 13.6$ eV), but this is a confirmed symbiotic star (Kenyon 1986: combination spectrum of late B + early M, emission lines of HI and singly-ionised metals). Classification is also based on its light curve showing eruptions as in other symbiotics (with $\Delta m_{\rm pg}$ up to $\sim 3^m$). Since the 1970's, the star is in permanent outburst with P-Cyg type spectrum.

038=Hen 3-828 IRAS data from Kenyon et al. 1988.

041=St 2-22 The SIMBAD database uses different name for this object: PN Sa 3-22.

043=V840 Cen IRAS data from Harrison & Gehrz 1994. Finding chart available in McNaught & Dawes 1986 where object is marked as star A Duerbeck & Seitter 1989.

046=Hen 3-916 Finding chart in Allen 1984 is wrong, object is 2 mm ($\sim 20''$) E of marked star Harries & Howarth 1996.

047=V704 Cen Cool component might be Mira Whitelock 1988.

048=V852 Cen Cool component is Mira Whitelock 1988,Feast et al. 1983; optical spectrum shows emission lines with ionization potential up to 100 eV and emission lines of H I and He I Pereira 1995,de Freitas Pacheco & Costa 1996,Miko\lajewska et al. 1997,Lutz & Kaler 1989. Bipolar nebula resolved in the optical (Southern Crab) (Corradi et al. 1999 and references therein).

050=V417 Cen An irregular nebula resolved at optical wavelengths (Corradi et al. 1999 and references therein).

055=HD 330036 This is a yellow symbiotic star; cool component is F5 giant or subgiant Lutz 1984. In UV, there are emission lines with ionization potential up to 77.5 eV Lutz 1984 and in the optical spectrum there are emission lines with ionization potential up to 54.4 eV Miko\lajewska et al. 1997,Lutz 1984. IR-type D' -Belczynski 2000.


 

Table 4. Orbital elements for symbiotic and suspected symbiotic binaries

No. Star P $K_{\rm g}$ $q \equiv M_{\rm g}/M_{\rm h}$ $\gamma_0$ e T0 agsini f(M) Ref.
    [days] [km s-1]   [km s-1]   [JD] [$R_\odot$] [$M_\odot$]  
003 EG And  482.6  7.3    -95 0 2450804(3)  70 0.020  Fekel et al. 2000
008 AX Per  680.8  7.5 2.5 -116.5 0 2445511.8 100 0.030  Miko\lajewska & Kenyon 1992
011 BD Cam  596.21  8.5    -22.3  0.09 2442794(1)  99.7  0.037 Griffin 1984
017 V1261 Ori  642 7.5  3.0  79.7 0.07 2446778(3) 95 0.028 Jorissen & Mayor 1992
023 BX Mon 1401  4.3 6.7   29.1 0.49 2449530 104 0.0076 Dumm et al. 1998
    1259  4.6     29.1 0.44 2449680 103 0.0092 Fekel et al. 2000
033 SY Mus  624.5  7.4     12.9 0 2449082(3)  91 0.026  Schmutz et al. 1994
036 TX CVn  199    5.7      2.3 0.16 2445195.25(1)  22 0.004  Kenyon & Garcia 1989
045 RW Hya  370.2  8.8     12.4 0 2445071.6  65 0.026  Kenyon & Miko\lajewska 1995
     370.4  8.8     12.9 0 2449512   0.026  Schild et al. 1996
051 BD-21 3873  281.6  10.6    203.9 0 2449087.3(3)  59  0.035 Smith et al. 1997
057 T CrB  227.57 23.9 0.6  -27.8 0 2447918.6 107 0.322  Fekel et al. 2000,Belczynski et al. 1998
058 AG Dra  554    5.1   -148.3 0 2446366.4  56 0.008  Miko\lajewska et al. 1995
101 RS Oph  455.7   16.7    -40.2 0 2450154.1(3) 150 0.221  Fekel et al. 2000
134 FG Ser  650    8.3 2.8   71.2 0 2448491 107 0.039  Mürset et al. 2000
142 AR Pav  604.5 9.6 2.7  -68.4 0 2448139 115 0.055   Schild et al. 2000
145 V443 Her  594    3.2    -49.2 0 2446007.7  39 0.002  Dobrzycka et al. 1993
167 CH Cyg 5700    4.9    -57.7 0.47 2445086 478 0.045  Miko\lajewski et al. 1988
     756.0  2.6    -60.6 0 2446643.7  39 0.0014 Hinkle et al. 1993
    5292     4.8     0.06 2445592(1) 500 0.060  Hinkle et al. 1993
172 CI Cyg  855.3  6.7 3   18.4 0 2445241.8 114 0.027  Kenyon et al. 1991
    853.8 6.7     15.0 0.11 2450426.4 112 0.026  Fekel et al. 2000
182 CD-43 14304  1448  4.4    27.6 0 2445929(3) 126 0.013 Schmid et al. 1998
     1442  4.6    27.5 0.22 2445560(1) 128 0.014 Schmid et al. 1998
185 AG Peg  816.5  5.3 4  -15.9 0 2431667.5  84 0.012  Kenyon et al. 1993
     818.2  5.4    -15.9 0.11 2446812  87 0.0135  Fekel et al. 2000
187 Z And  758.8  6.8     -1.8 0 2445703.0 102 0.025  Miko\lajewska & Kenyon 1996
s11 CD-27 8661  763.3  10.5   -5.5 0 2449280.5(3) 158 0.092 Van Eck et al. 2000

(1) T0 - time of the passage through periastron.
(2) Assumed from photometric ephemeris (eclipse).
(3) Time of maximum velocity.


056=Hen 2-139 Only H I emission lines in spectrum according to Allen 1984, but other emission lines (like [O III]) are reported in Allen 1976.

058=AG Dra A secondary periodicity of $\sim 355^{\rm d}$ has been detected in the optical light curve and interpreted in terms of non-radial pulsation of the cool giant Galis et al. 1999. An orbital inclination, $i \sim 120^{\circ}$, has been derived from spectropolarimetric observations Schmid & Schild 1997.

060=V347 Nor An elliptical nebula resolved at optical wavelengths (Corradi et al. 1999 and references therein).

065=Hen 3-1213 IUE observations reported in Gutierrez-Moreno et al. 1997.

066=Hen 2-173 IRAS data from Kenyon et al. 1988.

067=Hen 2-176 Classified as D-type in Allen 1984 based on its very red IR colours. However the IR colours are also consistent with an $\rm M4-M7$ giant and a very high interstellar reddening, $E_{B-V} \sim 2 \div 3$. Such a high reddening is also indicated by permitted and forbidden emission line ratios Miko\lajewska et al. 1997. Moreover both the location in the He I 6678/5876, 7065/5876 diagram Proga et al. 1994 and in the [O III] 5007/H$_\beta$, [O III] 4363/H$_\gamma$ diagram Gutierrez-Moreno et al. 1995 is consistent with S-type system.


 

Table 5. Pulsations ephemerides for Miras in symbiotic and suspected symbiotic stars

No. Star T0 [JD] P [days] Ref.
010 o Ceti Max(V) = 2444839 331.96 Kholopov 1985
016 UV Aur Max( $m_{\rm pg}$) = 2441062 395.42 Kholopov 1985
026 RX Pup Min(J) = 2440214 578 Miko\lajewska et al. 1999
029 KM Vel ? 370 Feast et al. 1983
030 V366 Car ? 433 Feast et al. 1983
034 BI Cru ? 280 Whitelock et al. 1983
048 V852 Cen ? 400 Whitelock 1987
049 V835 Cen ? 450 Feast et al. 1983
060 V347 Nor ? 370-380 Whitelock 1988
100 H 1-36 ? 450-500 Whitelock 1987
169 HM Sge Max(J) = 2446856 527 Yudin et al. 1994
174 V1016 Cyg Min(K) = 2444852 478 Munari 1988
    Max(K) = 2445038 478 Munari 1988
175 RR Tel Max(J/K) = 2442999 387 Feast et al. 1983
183 V407 Cyg Max(B) = 2429710 745 Kolotilov et al. 1998
188 R Aqr Max(V) = 2442398 386.96 Kholopov 1985
s27 V850 Aql Max(V) = 2425888 320 Kholopov 1985
s30 V627 Cas ? 466 Kolotilov et al. 1996



 

Table 6. Hipparcos parallaxes for symbiotic stars Perryman et al. 1997

No. Star $\pi$ [mas]
003 EG And 1.48 $\pm$ 0.97
010 o Ceti 7.79 $\pm$ 1.07
011 BD Cam 6.27 $\pm$ 0.63
017 V1261 Ori 1.32 $\pm$ 0.99
057 T CrB -1.61 $\pm$ 0.63
058 AG Dra -1.72 $\pm$ 0.98
142 AR Pav 3.37 $\pm$ 2.47
167 CH Cyg 3.73 $\pm$ 0.85
172 CI Cyg -0.36 $\pm$ 1.58
185 AG Peg -0.30 $\pm$ 1.17
187 Z And 2.34 $\pm$ 2.91
188 R Aqr 5.07 $\pm$ 3.15



 

Table 7. Flickering and outburst characteristics of symbiotic and suspected symbiotic stars. SyN - symbiotic nova, SyRN - symbiotic recurrent nova, Z And - Z And type outburst

No. Star Flick. Ref. Out. Type of Out. Ref.
002 SMC2     +   Morgan 1992
004 SMC3     +   Morgan 1992
008 AX Per     + Z And Miko\lajewska & Kenyon 1992
010 o Ceti + Warner 1972      
012 S32     +?   Kafatos et al. 1983
013 LMC S154     +?   Remillard et al. 1992
024 V694 Mon + Dobrzycka et al. 1996 +   Maran et al. 1991
026 RX Pup     + SyRN? Miko\lajewska et al. 1999
035 RT Cru + Cieslinski et al. 1994 +   Cieslinski et al. 1994
036 TX CVn     + Z And Mammano & Taffara 1978
043 V840 Cen     +   Liller 1986
050 V417 Cen     +?   van Winckel et al. 1994
057 T CrB + Kenyon 1986 + SyRN Webbink et al. 1987
058 AG Dra     + Z And Miko\lajewska et al. 1995,Greiner et al. 1997
068 KX Tra     +   Liller 1974
074 Hen 3-1341     +   Tomov et al. 2000
084 V2116 Oph + Jablonsky et al. 1997      
092 RT Ser     + SyN Mürset & Nussbaumer 1994
093 AE Ara     + Z And? Miko\lajewska et al. 2000
096 V2110 Oph     +?   Allen 1978
097 V916 Sco     +?   Sanduleak et al. 1978
099 V917 Sco     +   Chaisson 1997
101 RS Oph + Dobrzycka et al. 1996 + SyRN Kenyon 1986
107 Bl 3-14     +   Gutierrez-Moreno & Moreno 1995
110 V745 Sco     + SyRN Sekiguchi et al. 1990
128 V2506 Sgr     +   Duerbeck 1987
132 YY Her     + Z And Munari et al. 1997
134 FG Ser     + Z And Munari et al. 1995
138 V4074 Sgr     +   Herbig & Hoffleit1975
139 V2905 Sgr     +?   Hoffleit 1971
142 AR Pav     + Z And Thackeray et al. 1974
143 V3929 Sgr     +?   Remillard et al. 1992
148 V3890 Sgr     + SyRN Harrison et al. 1993
156 FN Sgr     + Z And Miko\lajewska et al. 2000
158 CM Aql     + Z And Kenyon 1983
160 V1413 Aql     + Z And Munari 1992,Esipov et al. 2000
164 V352 Aql     +   Hoffmeister et al. 1954
166 BF Cyg     + Z And Skopal et al. 1997
167 CH Cyg + Dobrzycka et al. 1996 +   Miko\lajewski et al. 1990
169 HM Sge     + SyN Mürset & Nussbaumer 1994
172 CI Cyg     + Z And Kenyon et al. 1991
174 V1016 Cyg     + SyN Mürset & Nussbaumer 1994
175 RR Tel     + SyN Mürset & Nussbaumer 1994
176 PU Vul     + SyN Kolotilov et al. 1995,Mürset & Nussbaumer 1994
177 LT Del     +   Arkhipova et al. 1997
181 V1329 Cyg     + SyN Mürset & Nussbaumer 1994
183 V407 Cyg     +   Munari et al. 1990
185 AG Peg     + SyN Kenyon et al. 1993,Mürset & Nussbaumer 1994
187 Z And + Sokolski & Bildsten 1999 + Z And Miko\lajewska & Kenyon 1996
188 R Aqr     +   Miko\lajewska & Kenyon 1992
s13 V748 Cen     +   Munari 1997
s14 V345 Nor     +   Duerbeck 1987
s15 V934 Her     +   Tomasella et al. 1997


068=KX TrA The finding chart in Allen 1984 is wrong: the object is really 3 mm ($\sim 25''$) W of marked star, although tabulated coordinates are correct Harries & Howarth 1996. The orbital period, P=1347 $\pm$ 29 days, the system inclination, $i=135^\circ \pm 38^\circ$, and the position angle of the line-of-nodes, $\Omega=58^\circ \pm 15^\circ$, has been derived from spectropolarimetric studies of the Raman-scattered O VI emission lines Harries & Howarth 2000.

071=CL Sco IRAS data from Harrison & Gehrz 1992.

073=V455 Sco An elliptical nebula possibly resolved in [O III] (Corradi et al. 1999 and references therein). The orbital period, P=1419 $\pm$ 39 days, the system inclination, $i=93\hbox{$.\!\!^\circ$ }6 \pm 2\hbox{$.\!\!^\circ$ }3$, and the position angle of the line-of-nodes, $\Omega=170\hbox{$.\!\!^\circ$ }1 \pm 1\hbox{$.\!\!^\circ$ }0$, has been derived from spectropolarimetric studies of the Raman-scattered O VI emission lines Harries & Howarth 2000.

074=Hen 3-1341 IUE observations reported in Gutierrez-Moreno et al. 1997. Spectral signatures of collimated bipolar jets have been found during the 1999 outburst Tomov et al. 2000.

077=H 2-5 IR-type D -Miko\lajewska et al. 1997,S -Allen 1984,Kenyon 1986.

084=V2116 Oph Orbital period of 303.8 days is derived from the spin changes of the X-ray pulsar companion Pereira et al. 1999,Cutler et al. 1986.

088=M 1-21 VK magnitudes - close and fainter companion also measured. The orbital period, P=892 $\pm$ 40 days, the system inclination, $i=96^\circ \pm 5^\circ$, and the position angle of the line-of-nodes, $\Omega=73\hbox{$.\!\!^\circ$ }1 \pm 3^\circ$, has been derived from spectropolarimetric studies of the Raman-scattered O VI emission lines Harries & Howarth 2000.

089=Hen 2-251 K-band spectrum is practically identical with that of the symbiotic Mira, RX Pup, as observed during the dust obscuration event, with strong dust continuum and weak CO 2.3-$\mu$m band Miko\lajewska et al. 2000,Miko\lajewska 1999.

092=RT Ser IRAS data from Kenyon et al. 1988.

093=AE Ara IRAS data from Kenyon et al. 1988.

094=SS73 96 IRAS data from Kenyon et al. 1988. An axisymmetrical nebula resolved at radio wavelengths (Corradi et al. 1999 and references therein).

096=V2110 Oph IRAS data from Kenyon et al. 1988.

100=H 1-36 In Medina Tanco & Steiner 1995 there is an estimate of cool component spectral type M4-5 III based on TiO 7100 Å band depth. However the spectrum of H 1-36 shown on their Fig. A1 does not show any absorption features or red continuum. A complex nebula resolved at optical and radio wavelengths (Corradi et al. 1999 and references therein). The only symbiotic star known to support an OH maser Ivison et al. 1994.

101=RS Oph Bipolar nebula detected in radio range (Corradi et al. 1999 and references therein).

Table 8. Different names for symbiotic and suspected symbiotic stars

001=SMC 1=NAME SMC1=[MH95] 183

002=SMC 2=NAME SMC2

003=EG And=HD 4174=BD+39 167=SAO 36618=GCRV 403=HIC 3494=GEN# +1.00004174= AG+40 66=GC 880=DO 8473=GPM1 20=SKY# 1157=AGKR 609=IRC +40014=JP11 413= PPM 43262=HIP 3494=IRAS 00415+4024

004=SMC 3=NAME SMC3=RX J0048.4-7332

005=SMC N60=LHA 115-N 60=LIN 323=HV 1707(???)

007=SMC N73=LHA 115-N 73=LIN 445 a

008=AX Per=MWC 411=HV 5488=CSI+54-01331=GCRV 896=JP11 5465=IRAS 01331+5359

009=V471 Per=PN M 1-2=PK 133-08 1=PN VV 8=LS V +52 1=PN G133.1-08.6=PN ARO 116=CSI+52-01555=PN VV' 11=IRAS 01555+5239

010=o Cet=MIRA=HD 14386=RAFGL 318=SKY# 3428=GC 2796=omi Cet=ADS 1778 AP= IRC +00030=YZ 93 562=MWC 35=BD-03 353=GEN# +1.00014386J= CCDM J02194-0258AP=PLX 477=GCRV 1301=JP11 625=CSI-03 353 1=DO 430= HIC 10826=SAO 129825=68 Cet=HR 681=UBV 21604=LTT 1179=TD1 1361= PPM 184482=JOY 1AP=IRAS 02168-0312

011=BD Cam=HD 22649=BD+62 597=HR 1105=SAO 12874=GC 4383=IRC +60125=FK4 129= UBV 3468=CSS 79=[HFE83] 244=GEN# +1.00022649=AG+63 277=N30 751= GCRV 2027=RAFGL 506=PPM 14446=HIP 17296=SKY# 5606=UBV M 9615=PLX 758= JP11 803=CSV 328=HIC 17296=S1* 60=IRAS 03377+6303

012=S32=StHA 32

013=LMC S154=LHA 120-S 154

014=LMC S147=LHA 120-S 147=[BE74] 484

015=LMC N19=LHA 120-N 19=[BE74] 191=LMC B0503-6803=MC4(0503-680)= PMN J0503-6757

016=UV Aur=HD 34842=BD+32 957=ADS 3934 A=IRC +30110=SAO 57941=HV 3322=Case 9= GEN# +1.0003482A=CGCS 911=IDS 05153+3224 A=AG+32 505=JP11 1034=UBV M 10852= AN 58.1911=LEE 179=RAFGL 735=PPM 70251=HIC 25050=GCRV 3199= DO 11210=CSI+32 957 1=Fuen C 29=CCDM J05218+3231A=C* 318=IRAS 05185+3227

017=V1261 Ori=HD 35155=BD-08 1099=RAFGL 736=SAO 132035=GCRV 56103=YZ 98 1455= HIC 25092=GEN# +1.00035155=GC 6602=HERZ 11764=CSS 133=HIP 25092=SKY# 8520= IRC -10086=PPM 187990=S1* 98=IRAS 05199-0842

019=LMC N67=CH-95=LHA 120-N 67=[HC88] 95

021=LMC S63=LHA 120-S 63=HV 12671

022=SMP LMC 94=LHA 120-S 170=LM 2-44

023=BX Mon=AS 150=HV 10446=MHA 61-12=JP11 5448=SS73 4

024=V694 Mon=MWC 560=SS73 5=LS 391=CSI-07-07234=GSC 05396-01135= MHA 61-14=IRAS 07233-0737

025=WRAY 15-157=IRAS 08045-2823

026=RX Pup=HD 69190=WRAY 16-17=HV 3372=CPD-41 2287=Hen 3-138=AN 88.1914=SS73 8= JP11 1653=PK 258-03 1=CD-41 3911=IRAS 08124-4133

027=Hen 3-160=SS73 9=WRAY 15-208

028=AS 201=MHA 382-43=Hen 3-172=SCM 38=PK 249+06 1=PDS 32=PN SaSt 1-1= PN G249.0+06.9=IRAS 08296-2735

029=KM Vel=Hen 2-34=WRAY 16-56=PK 274+02 1=ESO 212-13=PN G274.1+02.5= SS73 14=IRAS 09394-4909

030=V366 Car=Hen 2-38=PK 280-02 1=PN SaSt 1-3=ESO 167-11=WRAY 16-62= IRAS 09530-5704

031=Hen 3-461=PK 283+06 2=IRAS 10370-5108

033=SY Mus=HD 100336=SS73 32=HV 3376=WRAY 15-824=TD1 15706=Hen 3-667= AN 118.1914=CPD-65 11298=CSI-65-11298=SPH 127=IRAS 11299-6508

034=BI Cru=Hen 3-782=SVS 1855=IRAS 12206-6221

035=RT Cru=HV 1245=AN 131.1906

036=TX CVn=BD+37 2318=UBV M 2779=PPM 76696=JP11 5415=CDS 866=FB 110= Case A-F 788=AG+37 1208=SAO 63173=GEN# +0.03702318=IRAS 12423+3702

037=Hen 2-87=SS73 36=PK 302-00 1=WRAY 16-119=ESO 95-16=IRAS 12423-6244 -0.3cm

038=Hen 3-828=SS73 37=WRAY 15-1022 -0.3cm

039=SS73 38=CD-64 665=CGCS 3295=DJM 390=IRAS 12483-6443 -0.3cm

041=St 2-22=PN Sa 3-22=PK 305+03 1 -0.3cm

042=CD-36 8436=NSV 06160=Hen 3-886=JP11 311=PK 308+25 6=IRAS 13131-3644 -0.3cm

043=V840 Cen=LILLER'S OBJECT -0.3cm

044=Hen 3-905=SS73 40=WRAY 15-1108 -0.3cm

045=RW Hya=HD 117970=MWC 412=CPD-24 5101=YZ 115 9978=SAO 181760=CD-24 10977= GCRV 8034=HV 3237=PPM 261808=GEN# +1.00117970=JP11 2404=AN 51.1910= FAUST 3820=IRAS 13315-2507 -0.3cm

046=Hen 3-916=SS73-42=WRAY 15-1123 -0.3cm

047=V704 Cen=Hen 2-101=PK 311+03 1=PN G311.1+03.4=WRAY 16-141=ESO 133-7= IRAS 13515-5812 -0.3cm

048=V852 Cen=Hen 2-104=PK 315+09 1=ESO 221-31=PN G315.4+09.4=SS73 43= NAME SOUTHERN CRAB=WRAY 16-147=SCM 78=IRAS 14085-5112 -0.3cm

049=V835 Cen=Hen 2-106=WRAY 16-148=PK 312-02 1=ESO 97-14=SCM 79=NSV 06587= IRAS 14103-6311 -0.3cm

050=V417 Cen=HV 6516=IRAS 14122-6139 -0.3cm

052=Hen 2-127=SS73 45=PK 325+04 2=ESO 224-2=SCM 94=WRAY 16-180= IRAS 15210-5139 -0.3cm

053=Hen 3-1092=Hen 2-134=SS73 46=PK 319-09 1=WRAY 16-186=LS 3391=ESO 99-10= JP11 5230=CSI-66-15425 -0.3cm

054=Hen 3-1103=SS73 47=WRAY 15-1359 -0.3cm

055=HD 330036=BD-48 10371=PN Cn 1-1=PK 330+04 1=CD-48 10371=HIP 77662= ESO 225-1=HIC 77662=WRAY 15-1364=PN G330.7+04.1=IRAS 15476-4836 -0.3cm

056=Hen 2-139=PK 326-01 1=WRAY 16-193=ESO 178-2=IRAS 15508-5520 -0.3cm

057=T CrB=HD 143454=MWC 413=GC 21491=IDS 15553+2612 AB=DO 15377=PPM 104498= GEN# +1.00143454J=BD+26 2765=GCRV 9203=SAO 84129=NOVA CrB 1866= CCDM J15595+2555AB=AG+26 1536=HR 5958=SBC 558=NOVA CrB 1946=HIC 78322= HIP 78322=IRAS 15574+2603 -0.3cm

058=AG Dra=AG+66 715=CDS 889=SAO 16931=HIC 78512=1ES 1601+66.9= BPS BS 16087-0012=BD+67 922=GCRV 9231=UBV 13635=GEN# +0.06700922= 2E 1601.3+6656=2RE J1601+664=HIP 78512=JP11 236=SVS 1155=PPM 19692= 2E 3573=2RE J160133+664805=IRAS 16013+6656 -0.3cm

059=WRAY 16-202=PN Sa 3-33=PK 332+01 1 -0.3cm

060=V347 Nor=Hen 2-147=WRAY 16-208=PK 327-04 1=ESO 178-13=PN G327.9-04.3= IRAS 16099-5651 -0.3cm

061=UKS Ce-1=UKS-Ce1=UKS Ce1=UKS 1612-22.0 -0.3cm

062=QS Nor=Hen 2-156=SS73 53=WRAY 15-1461=PK 338+05 2=SCM 111=ESO 331-2= CSV 2635 -0.3cm

063=WRAY 15-1470=Hen 3-1187=SS73 55 -0.3cm

064=Hen 2-171=SS73 59=WRAY 16-226=PK 346+08 1=PN G346.0+08.5=ESO 390-7= IRAS 16307-3459 -0.3cm

065=Hen 3-1213=SS73 60=WRAY 15-1511 -0.3cm

066=Hen 2-173=SS73 61=WRAY 15-1518=PK 342+05 1=ESO 331-7 -0.3cm

067=Hen 2-176=PK 339+00 1=WRAY 16-230=ESO 277-5=IRAS 16379-4507 -0.3cm

068=KX TrA=Hen 3-1242=PN Cn 1-2=Hen 2-177=PK 326-10 1=WRAY 16-233= ESO 101-10=JP11 5232=PN StWr 1-1=JP11 5233=IRAS 16401-6231 -0.3cm

069=AS 210=MHA 276-52=Hen 3-1265=SS73 66=JP11 5249=WRAY 16-237=PK 355+11 1= IRAS 16482-2555 -0.3cm

070=HK Sco=HV 4493=AS 212=MHA 71-6=Hen 3-1280=SS73 68=WRAY 15-1563 -0.3cm

071=CL Sco=HV 4035=AS 213=MHA 71-5=Hen 3-1286=SS73 69=WRAY 15-1564= CD-30 13603 -0.3cm

072=PN MaC 1-3=PK 339-03 1 -0.3cm

073=V455 Sco=HV 7869=AS 217=MHA 71-15=Hen 3-1334=SS73 74=PN H 2-2= PK 351+03 1=ESO 392-3=WRAY 16-252=Haro 3-2=PN VV' 162=IRAS 17040-3401 -0.3cm

074=Hen 3-1341=NSV 08226=SS73 75 -0.3cm

075=Hen 3-1342=SS73 77 -0.3cm

076=AS 221=MHA 276-12=Hen 3-1348=SS73 79=PN H 2-4=PK 352+03 1=WRAY 15-1637= PN VV' 166=Haro 3-4=ESO 392-4=IRAS 17087-3230 -0.3cm

077=PN H 2-5=PK 354+04 2=PN VV' 172=ESO 454-3=WRAY 15-1655=Haro 3-5= IRAS 17121-3131 -0.3cm

078=PN Sa 3-43=PK 355+04 1 -0.3cm

079=Draco C-1=Irwin Dra 22025=Stetson 3203=McClure C1=[ALS82] C1 -0.3cm

080=PN Th 3-7=PK 356+04 3=PN ARO 249=ESO 454-12 -0.3cm

081=PN Th 3-17=PK 357+03 3=WRAY 17-81=ESO 454-30=PN Sa 3-54 -0.3cm

082=PN Th 3-18=PK 358+03 5=ESO 454-32=WRAY 17-83=Hen 2-228 -0.3cm

083=Hen 3-1410=PN Th 3-20=PK 357+02 3=PN ARO 251=NSV 08805=WRAY 15-1714= ESO 454-37 -0.3cm

084=V2116 Oph=GX 1+04=PK 001+04 1=4U 1728-24=1M 1728-247=H 1728-247= PN MaC 1-5=2S 1728-247=GX 2+05=2U 1728-24=3U 1728-24=3A 1728-247= 1H 1728-247 -0.3cm

085=PN Th 3-29=WRAY 17-89=PN Sa 3-61=PK 358+02 3=ESO 455-15= IRAS 17299-2905 -0.3cm

086=PN Th 3-30=PK 359+02 1=ESO 455-18=WRAY 17-90=Hen 2-243=PN Sa 3-63 -0.3cm

087=PN Th 3-31=PK 358+01 2=ESO 455-19=Hen 2-245=WRAY 17-91= IRAS 17312-2926 -0.3cm

088=PN M 1-21=SS73 90=Hen 2-247=PK 006+07 1=PN VV' 216=PN VV 103= ESO 588-7=IRAS 17313-1909 -0.3cm

089=Hen 2-251=PK 358+01 3=PN H 1-25=PN VV' 218=Haro 2-25=WRAY 16-289= SS73 92=SCM 151=ESO 455-22=PN Bl A=IRAS 17321-2943 -0.3cm

090=PN Pt 1=PK 003+03 3=EQ 1735-2352=ESO 520-12 -0.3cm

091=PN K 6-6=WR 99=LuSt 1=PN G359.8+01.5=Terz V 2955 -0.3cm

092=RT Ser=MWC 265=SS73 94=CSI-11-17371=NOVA Ser 1909=NOVA Ser 1917= GCRV 10203=AN 7.1917 -0.3cm

093=AE Ara=HV 5491=MWC 591=Hen 3-1451=SS73 95=WRAY 15-1754=PN PC 18= PK 344-08 1=GSC 08347-01978=ESO 279-5 -0.3cm

095=UU Ser=AS 237=SS73 98=AN 720.1936=HV 8771=CSV 2420 -0.3cm

096=V2110 Oph=AS 239=MHA 79-52=Hen 3-1465=JP11 5250 -0.3cm

097=V916 Sco=SSM 1=EQ 1740-360 -0.3cm

098=Hen 2-275=WRAY 16-304=PK 351-05 1=ESO 334-8 -0.3cm

099=V917 Sco=Hen 3-1481=SS73 103 -0.3cm

100=PN H 1-36=PK 353-04 1=Hen 2-289=PN Sa 2-249=PN G353.5-04.9= ESO 393-31=PN VV' 259=Haro 2-36=IRAS 17463-3700 -0.3cm

101=RS Oph=HD 162214=MWC 414=BD-06 4661=NOVA Oph 1898=AN 20.1901= PPM 201101=GCRV 10316=HV 164=SS73 106=JP11 2898=NOVA Oph 1933= IRAS 17474-0641 -0.3cm

102=WRAY 16-312=PN Sa 3-80=PK 358-01 2 -0.3cm

103=V4141 Sgr=PN Th 4-4=PK 008+03 2=ESO 589-10=PN ARO 260=IRAS 17477-1948 -0.3cm

104=ALS 2=[ALS88] 2=SS 324=EQ 174755.9-174710=PK 010+04 7 -0.3cm

105=AS 245=MHA 359-110=Hen 3-1501=SS73 107=PN H 2-28=PK 006+02 2= ESO 589-13=PN VV' 268=PN ARO 261=Haro 3-28=IRAS 17479-2218 -0.3cm

106=Hen 2-294=PK 357-03 1=ESO 394-1=WRAY 16-318=IRAS 17483-3250 -0.3cm

107=PN Bl 3-14=PK 000-01 4=ESO 455-55 -0.3cm

108=PN Bl 3-6=PK 358-02 2=PN Sa 3-85=ESO 456-4=IRAS 17496-3120 -0.3cm

109=PN Bl L=PK 359-02 1=PN Sa 3-86=ESO 456-6 -0.3cm

110=V745 Sco=NOVA Sco 1937 -0.3cm

111=PN MaC 1-9=PK 013+05 2 -0.3cm

112=AS 255=MHA 363-45=Hen 3-1525=SS73 111=IRAS 17537-3513 -0.3cm

113=V2416 Sgr=PN M 3-18=SS73 112=PK 007+01 2=ESO 589-24=PN VV' 295= Hen 2-312=Ve 2-61=IRAS 17542-2142 -0.3cm

114=PN H 2-34=PN Sa 3-105=PK 001-02 1=ESO 456-28=PN VV' 304=Haro 3-34 -0.3cm

116=AS 269=PN H 1-49=SS73 119=PK 358-05 2=Hen 2-331=MHA 304-52=ESO 394-23= WRAY 16-356=Haro 2-49=PN VV' 323=SCM 178=IRAS 18001-3242 -0.3cm

117=PN Ap 1-8=SS73 121=PK 002-03 1=ESO 456-47=IRAS 18013-2821 -0.3cm

118=SS73 122=PN KFL 6=IRAS 18015-2709 -0.3cm

119=AS 270=Hen 3-1581=SS73 126=IRAS 18026-2025 -0.3cm

120=PN H 2-38=SS73 128=PK 002-03 4=Hen 2-343=WRAY 17-108=ESO 456-51= PN VV' 342=Haro 3-38=IRAS 18028-2817 -0.3cm

121=SS73 129=PK 001-04 3=T 17=PN KFL 8=IRAS 18038-2932 -0.3cm

122=Hen 3-1591=SS73 132=T 53=NSV 10219=IRAS 18044-2558 -0.3cm

123=V615 Sgr=Hen 2-349=PK 356-07 1=SS73 131=ESO 394-29=WRAY 15-1840= HV 7199=IRAS 18044-3610 -0.3cm

124=Ve 2-57=SS 134=NSV 10241 -0.3cm

125=AS 276=Hen 3-1595=SS73 135=MHA 363-7=IRAS 18058-4108 -0.3cm

126=PN Ap 1-9=SS73 137=PK 003-04 2=Hen 2-356=WRAY 16-377=ESO 456-63= SCM 186=IRAS 18073-2753 -0.3cm

127=AS 281=MHA 208-83=SS73 138=PN Ap 1-10=PK 003-04 1=WRAY 16-378= ESO 456-65=Hen 2-357=IRAS 18076-2757 -0.3cm

128=V2506 Sgr=AS 282=MHA 304-113=Hen 2-358=SS73 139=PN Ap 1-11= PK 003-04 6=WRAY 16-379=ESO 456-66 -0.3cm

129=SS73 141=PK 359-07 2=WRAY 16-384 -0.3cm

130=AS 289=Hen 3-1627=SS73 143=F1-11=IRAS 18095-1140 -0.3cm

131=Y CrA=HD 166813=Hen 3-1632=CSI-42-18107=SS73 144=HV 169= PK 350-11 1=AN 25.1901=IRAS 18110-4252 -0.3cm

132=YY Her=AS 297=CSI+20-18124=GSC 01579-00381=AN 6.1919=JP11 5444= MHA 352-34 -0.3cm

133=V2756 Sgr=AS 293=MHA 304-122=Hen 2-370=SS73 145=PK 002-05 1=ESO 456-79= WRAY 16-392 -0.3cm

134=FG Ser=AS 296=D 143-2=SS73 148=SON 10363=JP11 5251=IRAS 18125-0019 -0.3cm

135=HD 319167=PN CnMy 17=Hen 2-373=SS73 146=PK 001-06 1=WRAY 16-395= SCM 195=ESO 456-81 -0.3cm

136=Hen 2-374=SS73 147=PK 009-02 1=ESO 590-10=IRAS 18126-2135 -0.3cm

137=Hen 2-376=AS 294=NSV 10435=PK 004-05 2=MHA 304-123=WRAY 16-396= PN Sa 3-126=ESO 457-1 -0.3cm

138=V4074 Sgr=AS 295B=Hen 3-1641=HIC 89526=HIP 89526 -0.3cm

139=V2905 Sgr=AS 299=SS73 151=GEN# +6.20010299=MHA 208-92 -0.3cm

141=Hen 3-1674=SS73 153=T 21=WRAY 15-1864=PN KFL 17 -0.3cm

142=AR Pav=MWC 600=CPD-66 3307=GCRV 10756=HIC 89886=HV 7860=PPM 363277= HIP 89886=SBC 668=GSC 09080-00788=IRAS 18157-6609 -0.3cm

143=V3929 Sgr=Hen 2-390=SS73 154=CSV 4026=PK 005-05 2=ESO 522-19= PN ARO 274=PN StWr 2-3=SCM 202=HV 9397=P 4629=IRAS 18178-2649 -0.3cm

144=V3804 Sgr=AS 302=MHA 304-33=Hen 3-1676=SS73 155=IRAS 18182-3133 -0.3cm

145=V443 Her=MWC 603=GCRV 68111=CSI+23-18201=JP11 5216=FB 171= IRAS 18200+2325 -0.3cm

146=V3811 Sgr=Hen 2-396=ESO 590-19=PK 010-03 1=SS73 160=IRAS 18206-2157 -0.3cm

147=V4018 Sgr=CD-28 14567=AS 304=Hen 3-1691=SS73 162=PN KFL 20= GSC 06869-00806=IRAS 18221-2837 -0.3cm

148=V3890 Sgr=NOVA Sgr 1962=SS 390 -0.3cm

149=V2601 Sgr=AS 313=MHA 208-51=SS73 171=IRAS 18349-2244 -0.3cm

150=PN K 3-9=PN Sa 3-142=PK 023-01 1=IRAS 18376-0846 -0.3cm

151=AS 316=MHA 208-58=Hen 2-417=SS73 172=PK 012-07 1=ESO 591-14 -0.3cm

152=DQ Ser=CSV 4342 -0.3cm

153=MWC 960=MHA 204-22=Hen 3-1726=SS73 174 -0.3cm

154=AS 323=PN K 4-7=PK 026-02 2=MHA 369-39=PN ARO 292 -0.3cm

155=AS 327=MHA 208-67=Hen 3-1730=SS73 176=PK 011-11 1=JP11 5253=WRAY 16-421 -0.3cm

156=FN Sgr=AS 329=SS73 177=CSI-19-18509=NOVA Sgr 1925=GCRV 11342=JP11 5475 -0.3cm

157=PN Pe 2-16=PK 029-02 1=PN Th 1-F=PN ARO 296=PN VV' 464 -0.3cm

159=V919 Sgr=AS 337=MHA 227-6=SS73 178=AN 237.1932 -0.3cm

160=V1413 Aql=AS 338=MHA 305-6=Hen 3-1737=PN K 4-12=PK 048+04 1=SS 428= IRAS 19015+1625 -0.3cm

162=PN Ap 3-1=PK 037-02 1=SCM 231=PN ARO 145 -0.3cm

163=PN MaC 1-17=PK 030-07 1 -0.3cm

164=V352 Aql=PN K 3-25=PK 037-03 3=PN ARO 306=AN 279.1931=IRAS 19111+0212 -0.3cm

165=ALS 1=[ALS88] 1=EQ 191333.1-082308=PK 028-09 3 -0.3cm

166=BF Cyg=MWC 315=LS II +29 5=JP11 5433=CSI+29-19219 2=GCRV 11847= AN 112.1914 -0.3cm

167=CH Cyg=HD 182917=SAO 31632=BD+49 2999=GCRV 11865=JP11 3103=RAFGL 2383= HIC 95413=GEN# +1.00182917=AG+50 1370=DO 37228=YZ 50 6001=HIP 95413= SKY# 36122=GC 26820=CDS 1064=IRC +50294=AN 24.1924=PPM 37375= IRAS 19232+5008 -0.3cm

169=HM Sge=PK 053-03 2=2E 1939.7+1637=SVS 2183=2E 4280=IRAS 19396+1637 -0.3cm

170=Hen 3-1761=NSV 12264=IRAS 19373-6814 -0.3cm

171=QW Sge=AS 360=MHA 80-5=Hen 3-1771=JP11 5254=NSV 12383 -0.3cm

172=CI Cyg=MWC 415=HV 3625=CSI+35-19484=JP11 5434=HIP 97594=GCRV 12195= AN 10.1922=HIC 97594=IRAS 19483+3533 -0.3cm

173=StHA 169=NSV 12466 -0.3cm

174=V1016 Cyg=AS 373=CSI+39-19553=JP11 5437=2E 1955.3+3941=PK 075+05 1= JP11 5438=2E 4302=GCRV 70112=MHA 328-116=IRAS 19553+3941 -0.3cm

175=RR Tel=Hen 3-1811=SKY# 37701=AN 166.1908=2E 4313=CSI-55-20003= GCRV 6924 E=HV 3181=2E 2000.3-5552=IRAS 20003-5552 -0.3cm

176=PU Vul=NOVA Vul 1979=KUWANO-HONDA=IRAS 20189+2124 -0.3cm

177=LT Del=Hen 2-467=PK 063-12 1=PN ARO 353=StHA 179 -0.3cm

179=Hen 2-468=PK 075-04 1=PN ARO 355 -0.3cm

180=ER Del=BD+08 4506=AG+08 2842=SVS 654 -0.3cm

181=V1329 Cyg=HBV 475=PK 077-05 1=UBV M 46710=VES 248=IRAS 20492+3518 -0.3cm

182=CD-43 14304=Hen 3-1924 -0.3cm

183=V407 Cyg=AS 453=MHA 289-90=AN 148.1940=NOVA Cyg 1936 -0.3cm

184=StHA 190=RJHA 120=IRAS 21392+0230 -0.3cm

185=AG Peg=HD 207757=MWC 379=AGKR 19529=JP11 3412=TD1 28516=SKY# 41636= HIC 107848=GEN# +1.00207757=BD+11 4673=SAO 107436=DO 7622=HIP 107848= AG+12 2570=PLX 5279=GCRV 13724=YZ 12 8693=SBC 879=PPM 140717= IRAS 21486+1223 -0.3cm

186=LL Cas=PN K 4-46=PK 108-05 1=AN 207.1940=PN ARO 379 -0.3cm

187=Z And=HD 221650=MWC 416=PLX 5697=SAO 53146=2E 2331.6+4834=GEN# +1.00221650= BD+48 4093=GCRV 14773=HV 193=PPM 64386=2E 4735=AG+48 2087=JP11 3636= AN 41.1901=HIC 116287=HIP 116287=IRAS 23312+4832 -0.3cm

188=R Aqr=HD 222800=SAO 165849=HR 8992=GCRV 14862=MWC 400=SKY# 44830= GC 32948=YZ 105 8733=PPM 242022=HIP 117054=GEN# +1.00222800=IRC -20642= BD-16 6352=RAFGL 3136=HIC 117054=IRAS 23412-1533 -0.3cm

s01=RAW 1691=[MA93] 1858=LIN 521 -0.3cm

s04=CD-28 3719=CSS 294=Hen 3-21=Hen 4-18=S1* 200=IRAS 06591-2902 -0.3cm

s05=GH Gem=CSV 950=AN 241.1943 -0.3cm

s06=ZZ CMi=BD+09 1633=IRC +10162=AN 306.1934=GCRV 4915=HIP 35915=HIC 35915= IRAS 07214+0859 -0.3cm

s07=NQ Gem=HD 59643=BD+24 1686=SAO 79474=N30 1687=DO 13087=YZ 24 2992= GEN# +1.00059643=AG+24 848=YZ 0 823=PPM 97628=CGCS 1737=SKY# 13794= UBV M 13339=GCRV 5014=UBV 7255=LEE 197=HIC 36623=HIP 36623= C* 779=IRAS 07288+2436 -0.3cm

s08=WRAY 16-51=PK 271+03 1=IRAS 09316-4621 -0.3cm

s09=Hen 3-653=SS73 30=PK 323-08 1=WRAY 15-807=IRAS 11232-5940 -0.3cm

s10=NSV 05572=Ross 234=G 241-60=GD 407=LTT 16957 -0.3cm

s11=CD-27 8661=CSS 792=Hen 3-785=Hen 4-121=S1* 443=IRAS 12219-2802 -0.3cm

s12=AE Cir=HV 5112 -0.3cm

s13=V748 Cen=CD-32 10517=CSV 2229=SON 5003=[OM87] 145632.12-331309.6 -0.3cm

s14=V345 Nor=HV 8827=NSV 07429=CSV 2543 -0.3cm

s15=V934 Her=HD 154791=BD+24 3121=3A 1703+241=SKY# 30847=AG+24 1704= YZ 24 5850=1E 1704.4+2402=2A 1704+241=2E 1704.4+2402=AT 1700+239= AGKR 15254=PPM 105555=1H 1706+241=2E 3831=HIP 83714=SAO 84844=DO 15788= 4U 1700+24=HIC 83714=1ES 1704+24.0=IRAS 17044+2402 -0.3cm

s16=Hen 3-1383=SS73 82=WRAY 15-1680 -0.3cm

s18=WSTB 19W032=PK 359+01 3=ESO 455-139=SCM 152=PN G359.2+01.2= IRAS 17358-2854 -0.3cm

s19=WRAY 16-294=PK 002+02 1 -0.3cm

s20=AS 241=PN H 2-19=WRAY 16-302=PK 351-04 1=MHA 363-30=PN Sa 3-70=ESO 334-7= PN VV' 238=Haro 3-19=IRAS 17415-3816 -0.3cm

s22=V618 Sgr=HV 7203=AN 313.1933 -0.3cm

s23=AS 280=SS73 136=PK 358-06 1=Hen 2-354=WRAY 16-375=MHA 304-17=ESO 394-32 -0.3cm

s24=AS 288=PN H 2-43=PK 003-04 9=ESO 456-75=PN G003.4-04.8=MHA 304-119= WRAY 16-388=PN VV' 367=Hen 2-366=Haro 3-43=IRAS 18095-2820 -0.3cm

s25=Hen 2-379=SS73 150=PN M 1-44=PK 004-04 2=PN VV 165=WRAY 16-399=SCM 198= ESO 522-11=PN G004.9-04.9=PN VV' 380=IRAS 18131-2705 -0.3cm

s26=V335 Vul=AS 356=MHA 215-33=Case 452=LD 120=GSC 02128-00676= C* 2728=CGCS 4253=IRAS 19211+2421 -0.3cm

s27=V850 Aql=PN K 4-26=PK 037-06 2=CSV 4646=PN ARO 320=IRAS 19210+0032 -0.3cm

s28=Hen 2-442=PN M 4-16=PK 061+02 1=PN G061.8+02.1=PN ARO 157 -0.3cm

s30=V627 Cas=AS 501=RAFGL 2999=MHA 73-59=HBC 316=IRAS 22556+5833

102=WRAY 16-312 IRAS and JHKL colours confirm earlier suggestions Whitelock 1987,Whitelock 1988 that cool component of this system is a Mira Belczynski 2000. In the optical spectrum presented in Allen 1984 there are emission lines with ionization potential up to 108.8 eV and moreover lines of H I and He I are present Belczynski 2000. IRAS data from Kenyon et al. 1988.

103=V4141 Sgr Classified as S-type in Allen 1984,Munari et al. 1992, but in the near-IR/IRAS colour diagrams (e.g. Kenyon & Fernandez-Castro 1987,Whitelock 1988) it falls in the region occupied by symbiotic Miras Miko\lajewska et al. 1997. K-band spectrum shows strong CO 2.3-$\mu$m band consistent with an M6 giant Miko\lajewska et al. 2000. Spectral type of cool component also estimated in MacConnell 1983,Allen 1984 to be mid or late M.

105=AS 245 Classified as S-type in Allen 1980,Miko\lajewska et al. 1997 but in the near-IR/IRAS colour diagrams (e.g. Kenyon & Fernandez-Castro 1987,Whitelock 1988) it falls in the region occupied by symbiotic Miras Whitelock 1988.

107=Bl 3-14 The finding chart in Allen 1984 is good, but the coordinates are reported to disagree with the measured position: $\alpha=17^{\rm h} 52^{\rm m} 06^{\rm s}.4, \delta= -29^{\rm\circ} 45' 49''$ (1950) Harries & Howarth 1996 (if this is right, our coordinates should also be corrected).

110=V745 Sco VK magnitudes during decline from outburst Sekiguchi et al. 1990.

112=AS 255 IR-type S -Allen 1984,Allen 1982, D -Kenyon 1986,Luud & Tuvikene 1987.

114=H2-34 Spectral type M5 is estimated by comparing "by eye'' the depths of TiO $\lambda\,6180$ and $\lambda\,7100$ Å in the spectrum in Fig. 2 in Miko\lajewska et al. 1997 with those of spectral standards.

115=SS73 117 IRAS data from Kenyon et al. 1988.

116=AS 269 This is a yellow symbiotic star, cool component is G-K giant Miko\lajewska et al. 1997,Acker et al. 1987. In the optical spectrum there are emission lines with ionization potential up to 54.4 eV Kaler 1976.

118=SS73 122 IR-type D -Kenyon et al. 1988, others note only possible S type (Allen 1984,Kenyon 1986).

120=H 2-38 There was a report of a pulsational period of 433 days for this star in Munari 1997, but this is a mistake and the reported number is the pulsation period of another symbiotic star: V366 Car (Hen 2-38). The spectral type of the cool component is estimated in Allen 1980 to be M8.5.

122=Hen 3-1591 IR-type D -Allen 1984,Munari et al. 1992, S -Kenyon 1986,Allen 1975.

124=Ve 2-57 Cool component is M star Allen 1978. In the optical spectrum there are emission lines with ionization potential up to 35.1 eV or probably up to 54.4 eV Allen 1978.

125=AS 276 IR-type S -Allen 1984,Allen 1982, D -Kenyon 1986. There is also a D' classification in Luud & Tuvikene 1987, but it doesn't look reliable.

128=V2506 Sgr IRAS data from Harrison & Gehrz 1992.

132=YY Her IRAS data from Kenyon et al. 1988.

133=V2756 Sgr Finding chart in Perek & Kohoutek 1967 is incorrect (Stenholm & Acker 1987).

134=FG Ser K magnitude during outburst. Coordinates taken from Henden & Munari2000 - SIMBAD coordinates are not correct.

138=V4074 Sgr IUE observations reported in Meier et al. 1994.

139=V2905 Sgr IRAS data from Harrison & Gehrz 1992. Spectral type of cool component also estimated in Pereira et al. 1998 to be K/M.

146=V3811 Sgr Mis-identified in Perek & Kohoutek 1967 and in Allen 1974 (see Allen 1975).

148=V3890 Sgr Cool component is M4-8 giant (Harrison et al. 1993,Williams et al. 1991,Sekiguchi 1995). In the optical spectrum there are emission lines with an ionization potential up to 361 eV Williams et al. 1991. This object was earlier classified as recurrent nova with M type companion Sekiguchi 1995,Harrison et al. 1993. The spectrum is also presented in Williams et al. 1994.

156=FN Sgr IRAS data from Harrison & Gehrz 1992.

160=V1413 Aql Spectral type M4 estimated from the TiO $\lambda$ 7100 band depth as observed during mid-eclipse Miko\lajewska 2000.

162=Ap 3-1 Short description of optical spectrum is given in Allen 1984. The object was identified with the 2U 1907+2 X ray source Cahn 1973 but so far there is no ROSAT detection, so this identification might not be correct.

166=BF Cyg IRAS data from Kenyon et al. 1988.

167=CH Cyg Complex nebula with jet-like features resolved at optical and radio wavelengths (Corradi et al. 1999 and references therein). Both the light curves and the radial velocity curves show multiple periodicities: a $\sim 100^{\rm d}$ photometric period has been attributed to radial pulsation of the giant Miko\lajewski et al. 1992, while the nature of the secondary period of $\sim 756^{\rm d}$ also present in the radial velocity curve, is not clear Munari et al. 1996. There is controversy about whether the system is triple or binary Feibelman 1991, and whether the symbiotic pair is the inner binary Skopal et al. 1996 or the white dwarf is on the longer orbit Mikkola & Tanikawa 1998,Ezuka et al. 1998.

169=HM Sge Mean K magnitude during outburst. A complex nebula with possible jet-like features resolved at optical and radio wavelengths (Corradi et al. 1999 and references therein, Richards et al. 1999). The nebula is aligned with the binary orientation deduced from spectropolarimetry of the Raman scattered O VI lines Schmid et al. 2000.

170=Hen 3-1761 IRAS data from Kenyon et al. 1988. IUE observations reported in Gutierrez-Moreno et al. 1997.

171=QW Sge IRAS data from Kenyon et al. 1988 although Munari & Buson 1991 report no IRAS detection.

172=CI Cyg Coordinates from VLA observations Miko\lajewska & Ivison 2000.

174=V1016 Cyg A complex nebula with possible jet-like features resolved at optical and radio wavelengths (Bang et al. 1992,Corradi et al. 1999 and references therein).

176=PU Vul V mag during the decline from outburst (XI 1994) Kolotilov et al. 1995. In Yoon & Honeycutt 2000 $\sim 211^{\rm d}$ periodicity has been reported.

177=LT Del IRAS data from Harrison & Gehrz 1992. Spectral type of cool component also estimated in Lutz 1977 to be G5.

180=ER Del Cool component is S star of type S5.5/2.5 Ake 1979. In the UV, there are emission lines with an ionization potential up to 47.9 eV and a strong UV continuum indicates the presence of a hot companion Johnson & Ake 1989; in the optical spectrum there are emission lines of H I Johnson & Ake 1989.

181=V1329 Cyg The system inclination, $i=86^{\circ} \pm 2^{\circ}$, and the position angle of the orbital plane, $11^{\circ}$, has been derived from spectropolarimetric studies. An extended nebulosity detected in the [O III] $\lambda 5007$ line is aligned with the orbital plane Schild & Schmid 1997.

182=CD-43 14304 The system inclination, $i=58^\circ \pm 6^\circ$, and the position angle of the line-of-nodes, $\Omega=103^\circ \pm 7^\circ$, has been derived from spectropolarimetric studies of the Raman-scattered O VI emission lines Harries & Howarth 2000.

183=V407 Cyg IRAS data from Harrison & Gehrz 1994. IR-type S -Ivison et al. 1995, D -Munari et al. 1990 and also there is D' estimate in Ivison et al. 1991. In Munari et al. 1990 there is an estimate of the orbital period of 43 yrs.

184=StHA 190 In Schmid & Nussbaumer 1993 there is a suggestion, based on the IRAS ratio of F12/F25, that the cool component in this system is a Mira variable. Comparison of IRAS fluxes with diagnostic diagrams in Kenyon et al. 1988 shows that this object is among or close to D' systems, and the VJHKL colours are consistent with a G-K giant, so there is no reason to think that a Mira variable is present in this binary. The authors of Schmid & Nussbaumer 1993 argue that F12/F25>1.0 suggests the presence of a Mira but it may be merely the signature of dust around the system.

185=AG Peg VK magnitudes during outburst. A complex nebula with possible bipolar structure detected at optical and radio wavelengths (Corradi et al. 1999 and references therein).

186=LL Cas The presence of the [Fe VII] 4892 Å line reported in Kondrateva 1992 is not reliable because of the absence of the strongest [Fe VII] 6087 Å iron line at that time. In Kondrateva 1992, there is a report of a possible pulsational period for the cool component of this system (286.6 days). This is a plausible explanation, as the spectrum taken at maximum light shows a more pronounced late-type continuum than the spectrum taken at minimum (see Kondrateva 1992), indicating that the cool component is responsible for this variability. IR colours: J=8.90, H=8.03, K=7.55 Allen 1974) with assumed modest amount of interstellar reddening (AK=0.2) give J0=8.44, H0=7.67, K0=7.35 which corresponds to the colours of a normal giant in an S-type symbiotic star, although this might still be a Mira without an IR excess (like the Mira in R Aqr, which is another S-type symbiotic star).

187=Z And Spectral type of cool component also estimated in Huang et al. 1994 to be $\sim$M5.2. An inclination of $i=47 \pm 12^{\circ}$ and an orbit orientation, $\Omega=72 \pm 6^{\circ}$, derived from spectropolarimetry Schmid & Schild 1997. There is a report on 28-minute coherent oscillations observed in Z And Sokolski & Bildsten 1999. We have included Z And in Table 7 as system with flickering, although these oscillations are different from rapid light variations observed for other symbiotics.

188=R Aqr The binary has been spatially resolved and a preliminary orbit (with a period of $\sim 44$ yrs) derived in Hollis et al. 1997,Dougherty et al. 1995. The system is embedded in a complex bipolar nebula with jets (Corradi et al. 1999 and references therein).

Suspected symbiotic stars

s01=RAW 1691 Carbon star Westerlund et al. 1991 + H$_\alpha$ profile as for interacting binary star van Winckel et al. 1993.

s02=[BE74] 583 Suspected in Morgan et al. 1992.

s03=StHA 55 Carbon star Downes & Keyes 1988 + with strong H I emission Downes & Keyes 1988 (too strong for single carbon star).

s04=CD-28 3719 A symbiotic nature of this star has been suggested based on its broad H$_\alpha$ profiles (Jorissen 2000) and blue colors (Van Eck & Jorissen 2000).

s05=GH Gem Suspected in Meinunger 1980,Kenyon 1986.

s06=ZZ CMi This object was classified as symbiotic in Iijima 1984,Bopp 1984. We disagree with this classification because: i) colours are bluer at minimum Zamanov & Tomov 1992, the opposite to what is observed for symbiotics; the light curve looks more like a pulsational curve and not like a symbiotic light curve; ii) the spectrum presented in Iijima 1984 does not look like a symbiotic spectrum (e.g. H $_\gamma > {\rm H}_\beta$) and is noisy ([Ne III] line may not be present (so IP $_{\rm max}=35.1$ eV). However, this object contains a late-type star (though we do not know if the star is giant) and it displays an emission-line spectrum; also, the H$_\alpha$ profile shown in Bopp 1984) looks like a symbiotic star (for comparison see van Winckel et al. 1993). We therefore include this object as suspected symbiotic.

s07=NQ Gem Suspected in Johnson et al. 1988. Highly variable UV continuum with strong C IV] emission and Si III]/C III] ratio similar to symbiotic stars. He II 1640 Å emission line has been detected in 1979 by IUE.

s08=WRAY 16-51 Probable presence of late-type star and emission-type spectrum (H I emission lines) MacConnell 1983.

s09=Hen 3-653 Suspected in Allen 1984,Pereira et al. 1998: late-type star and emission-type spectrum (H I and He I emission lines).

s10=NSV 05572 Late-type giant and emission type-spectrum (H I emission lines).

s11=CD-27 8661 A symbiotic nature of this star has been suggested based on its broad H$_\alpha$ profiles (Jorissen 2000) and blue colors (Van Eck & Jorissen 2000).

s12=AE Cir Suspected in Kilkenny 1989. Periods of 3900 and 100 days are mentioned in Kilkenny 1989 (based on visual photometric observations).

s13=V748 Cen Suspected in Kenyon 1986: M type giant van Genderen 1979,Schulte-Ladbeck 1988 and emission-line spectrum (H I, Fe II, [Fe II], [S II]) van Genderen et al. 1974 and UV excess.

s14=V345 Nor Suspected in Liller & del Mar 1984: M star Liller & Jones 1996 and emission-line spectrum (H I, Fe II) Liller & Jones 1996. Listed as N Nor 1985/2 in Duerbeck 1987.

s15=V934 Her Suspected in Garcia et al. 1983: M bright giant and UV emission lines with ionization potential up to 77.5 eV but no emission lines in optical spectrum and no short-wavelength continuum was found (the 1200-2800 Å integrated flux $< 1.5 \ 10^{-14}$ erg s-1 cm-2 Å-1 at Earth) which excludes the presence of a hot white dwarf companion (although a neutron star is still possible).

s16=Hen 3-1383 Possible M type star Sanduleak & Stephenson 1973 and emission-type spectrum (H I, He I) Allen 1978. Nebula resolved at radio wavelengths (Corradi et al. 1999 and references therein).

s17=V503 Her Suspected in Kenyon 1986: M star Bond 1978 and blue excess in the optical spectra suggesting presence of hot companion.

s18=WSTB 19W032 Late type giant Corradi 1995 and emission-line spectrum: lines of H I, He I and others with ionization potential up to 35.1 eV. But this emission-line spectrum might not be physically connected with the giant Corradi 1995.

s19=WRAY 16-294 Suspected in Miko\lajewska et al. 1997: red continuum typical of reddened K giant and emission-line spectrum (H I, He I and others with ionization potential up to 35.1 eV). WRAY 16-294 appears as WRAY 16-296 in Miko\lajewska et al. 1997.

s20=AS 241 Suspected in Allen 1984: M star Miko\lajewska et al. 1997 and emission-line spectrum (H I, He I) Miko\lajewska et al. 1997. M6 spectral type of cool component and D' IR type from Luud & Tuvikene 1987 are not reliable, as M6 does not agree with IR colours (JHK) and authors do not follow original definition of D'.

s21=DT Ser Considered as symbiotic in Cieslinski et al. 1997,Cieslinski et al. 1998: emission spectrum of H I, He I and other lines with ionization potential up to 54.4 eV plus G? Cieslinski et al. 1997 or G2-K0 III-I Cieslinski et al. 1998 cool component. But there is a report of a G star 5'' from this object, so the cool component may not be connected physically with the source of the emission-line spectrum.

s22=V618 Sgr Presence of late-type component (TiO bands in optical spectrum Kilkenny 1989) and emission-line spectrum (H I, Fe II Kilkenny 1989).

s23=AS 280 Suspected in Miko\lajewska et al. 1997: this object resembles a symbiotic star in outburst.

s24=AS 288 This object shows optical emission-line spectrum (H I, He I and others with ionization potential up to 54.4 eV) but no late-type component has been seen so far, however K magnitude and IRAS fluxes compared to diagnostic diagrams in Kenyon et al. 1988 place this object among symbiotics (of IR type D), emission-line fluxes ([O III]4363, 5007 Å, H$_\beta$, H$_\gamma$) compared to diagnostic diagrams in Gutierrez-Moreno et al. 1995 place this object also among symbiotics (among IR type S but close to D-type objects).

s25=Hen 2-379 Cool component is G-K giant Lutz 1977,Stenholm & Acker 1987 and there is emission-line spectrum: H I, He I and other lines with ionization potential up to 35.1 eV. But K giant might not be physically associated with nebula, which is source of the emission Lutz & Kaler 1983. Finding chart in Perek & Kohoutek 1967 is unclear as reported in Stenholm & Acker 1987.

s26=V335 Vul Suspected in Munari et al. 1998: presence of carbon giant and optical emission-line spectrum (H I) displaying hot continuum in blue. We agree with this classification although this object might be a single pulsating star: (i) the carbon star might pulsate with period of 342 days Dahlmark 1994 and then emission lines behave as for a Mira variable - they disappear near minimum light and show up again at maximum (see spectra in Munari et al. 1998); (ii) H$_\alpha$ is very narrow: 2 Å (90 km s-1) and for a symbiotic star we would expect a width of about 300-500 km s-1; (iii) the Balmer decrement is different than that observed for symbiotic stars (it resembles that of Mira variable), although the authors of Munari et al. 1998 claim that the Balmer decrement resembles that of a symbiotic star.

s27=V850 Aql Probable presence of Mira Bond 1976,Kholopov 1985 or late-type star Acker et al. 1987 in the centre of planetary nebula PK 037-6 2 (see note in Kholopov 1985) with emission-line spectrum (H I lines). In Acker et al. 1987 and Bond 1976 there are notes that in Allen 1974 this object is classified as symbiotic, but this is not true and in Allen 1974 there are only IR colours for V850 Aql.

s28=Hen 2-442 Suspected in Yudin 1983: TiO bands probably present, suggesting cool component Archipova et al. 1985,Yudin 1983 and optical emission-line spectrum: H I, He I and other lines with ionization potential up to 100 eV. Hen 2-442 consists of two PN like objects: Hen 2-442A and Hen 2-442B Archipova et al. 1985 and values in catalogue are for the whole system. Symbiotic nature was suggested for Hen 2-442 A.

s29=IRAS 19558+3333 Suspected in Seaquist & Ivison 1994: OH/IR star, based on IRAS colours, but without an OH maser, so a probable, extreme D-type system. Radio continuum emission implies a hot, ionising companion. Correct coordinates given here for precise radio emission (incorrect coordinates given by Seaquist & Ivison 1994).

s30=V627 Cas Suspected in Kolotilov et al. 1996. Spectral type of cool component also estimated in Kolotilov et al. 1991 to be M2-4.

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