004 =SMC3 V magnitude during outburst.
005 =SMC N60 IR-type S -[137, 236], D -[18].
008 =AX Per Incorrect coordinates given by [18, 137].
009 =V471 Per This star appears in previous symbiotic catalogs [18, 137]. The 
009 correct name is V471 Per as given in the General Catalog of Variable 
009 Stars [147].
010 =o Ceti Cool component is Mira [313] of type M2-7 III [313], UV spectrum 
010 shows emission lines with ionization potentials up to 54.4eV [133] and in 
010 the optical spectrum there are emission lines of H I and He I [320]. 
010 Preliminary orbit with orbital period of 400 yrs was reported in [28], but 
010 recent high precision interferometric observations show that the apparent 
010 binary separation is much larger than predicted, and imply orbital period 
010 much longer then 400 yrs [133].
011 =BD Cam Cool component is S giant of type S5.3 [135]; UV spectra shows 
011 emission lines with ionization potential up to 77.5eV [8]. 24.76-day 
011 periodicity estimated from BVRI photometry; pulsational origin has been 
011 suggested [5].
016 =UV Aur Although there has been some controversy over the interpretation of 
016 the 395-day period sometimes attributed to orbital motion (e.g. [36]), we 
016 believe that it is due to pulsation (see [87] for discussion). The object is
016 thus classified as a C-rich symbiotic Mira with little dust (S-type). The 
016 broad-band polarimetric data show a periodicity of ~14yrs which may be due 
016 to orbital motion [148].
017 =V1261 Ori Cool component is S giant of type S4.1 [127] UV spectrum shows 
017 emission lines with ionization potential up to 77.5eV [7].
018 =LMC1 IUE spectra described in [236].
020 =Sanduleak's star In the optical spectrum, there is an emission feature at 
020 6825{AA} [215]; moreover, there are emission lines with an ionization 
020 potential up to 108.8eV [215, 13] including lines of H I and He I [236]. 
020 The IUE spectra are described in [236].
023 =BX Mon IRAS data from [142].
024 =V694 Mon Object in permanent outburst [176]; contains M3-5 giant [243, 11];
024 optical spectrum shows emission lines of H I and He I with highly 
024 blueshifted (~2000-7000km/s) shell absorption [11, 243, 188] and emission 
024 lines of singly-ionised metals [243] over an A-B type continuum [243]. 
024 VK magnitudes are appropriate for the outburst.
026 =RX Pup Highly variable radio emission [114]. Nebula resolved at optical and
027 radio wavelengths with a possible jet-like feature in the [N II] line 
027 ([53] and references therein).
027 =Hen 3-160 IRAS data from [142].
028 =AS 201 A spherical nebula detected in H{alpha} and [N II] lines ([53] and 
028 references therein).
029 =KM Vel Cool component is Mira [313, 75] of M spectral type [274]; optical 
029 spectrum shows emission lines with ionization potential up to 41.0eV [21] 
029 and emission lines of H I and He I [275]. Finding chart in [248] is 
029 incorrect and no other has been published.
032 =SS73 29 IUE observations reported in [142]. IRAS data from [142].
033 =SY Mus The system inclination, i=101.1{deg}+/-2.5{deg}, and the position 
033 angle of the line-of-nodes, {Omega}=58.6{deg}+/-1.7{deg}, has been derived 
033 from spectropolarimetric studies of the Raman-scattered O VI emission 
033 lines [91, 89].
034 =BI Cru A bipolar nebula resolved in the optical ([53] and references 
034 therein) with the bipolar lobes and associated outflows perpendicular to the
034 position angle of intrinsic scattering polarization [88].
036 =TX CVn Low ionization potential (IP_max_=13.6eV), but this is a confirmed 
036 symbiotic star ([138]: combination spectrum of late B + early M, emission 
036 lines of HI and singly-ionised metals). Classification is also based on its 
036 light curve showing eruptions as in other symbiotics (with {Delta}m_up_ 
036 to ~3^m^). Since the 1970's, the star is in permanent outburst with P-Cyg 
036 type spectrum.
038 =Hen 3-828 IRAS data from [142].
041 =St 2-22 The SIMBAD database uses different name for this object: PN Sa 3-22
043 =V840 Cen IRAS data from [94]. Finding chart available in [184] where object
043 is marked as star A [70].
046 =Hen 3-916 Finding chart in [18] is wrong, object is 2 mm (~20") E of marked
046 star [90].
047 =V704 Cen Cool component might be Mira [313].
048 =V852 Cen Cool component is Mira [313, 75]; optical spectrum shows emission 
048 lines with ionization potential up to 100eV and emission lines of H I and 
048 He I [244, 60, 198, 171]. Bipolar nebula resolved in the optical (Southern 
048 Crab) ([53] and references therein).
050 =V417 Cen An irregular nebula resolved at optical wavelengths ([53] and 
050 references therein).
055 =HD 330036 This is a yellow symbiotic star; cool component is F5 giant or 
055 subgiant [169]. In UV, there are emission lines with ionization potential 
055 up to 77.5eV [169] and in the optical spectrum there are emission lines with
055 ionization potential up to 54.4eV [168, 169]. IR-type D' [1].
056 =Hen 2-139 Only H I emission lines in spectrum according to [18], but other 
056 emission lines (like [O III]) are reported in [21].
058 =AG Dra A secondary periodicity of ~355d has been detected in the optical 
058 light curve and interpreted in terms of non-radial pulsation of the cool 
058 giant [81]. An orbital inclination, i~120{deg}, has been derived from 
058 spectropolarimetric observations [268].
060 =V347 Nor An elliptical nebula resolved at optical wavelengths ([53] and 
060 references therein).
065 =Hen 3-1213 IUE observations reported in [183].
066 =Hen 2-173 IRAS data from [142].
067 =Hen 2-176 Classified as D-type in [18] based on its very red IR colours. 
067 However the IR colours are also consistent with an M4-M7 giant and a very 
067 high interstellar reddening, E_{B-V}_~2/3. Such a high reddening is also 
067 indicated by permitted and forbidden emission line ratios [198]. Moreover 
067 both the location in the He I 6678/5876, 7065/5876 diagram [250] and in the 
067 [O III] 5007/H{beta}, [O III] 4363/H{gamma} diagram [181] is consistent 
067 with S-type system.
068 =KX TrA The finding chart in [18] is wrong: the object is really 3 mm (~25")
068 W of marked star, although tabulated coordinates are correct [90]. The 
068 orbital period, P=1347+/-29days, the system inclination, 
068 i=135{deg}+/-38{deg}, and the position angle of the line-of-nodes, 
068 {Omega}=58{deg}+/-15{deg}, has been derived from spectropolarimetric studies
068 of the Raman-scattered O VI emission lines [91].
071 =CL Sco IRAS data from [92].
073 =V455 Sco An elliptical nebula possibly resolved in [O III] ([53] and 
073 references therein). The orbital period, P=1419+/-39days, the system 
073 inclination, i=93.6{deg}+/-2.3{deg}, and the position angle of the 
073 line-of-nodes, {Omega}=170.1{deg}+/-1.0{deg}, has been derived from 
073 spectropolarimetric studies of the Raman-scattered O VI emission lines [91].
074 =Hen 3-1341 IUE observations reported in [183]. Spectral signatures of 
074 collimated bipolar jets have been found during the 1999 outburst [299].
077 =H 2-5 IR-type D -[198],S -[18, 137].
084 =V2116 Oph Orbital period of 303.8 days is derived from the spin changes of 
084 the X-ray pulsar companion [247, 56].
088 =M 1-21 VK magnitudes - close and fainter companion also measured. The 
088 orbital period, P=892+/40days, the system inclination, i=96{deg}+/-5{deg}, 
088 and the position angle of the line-of-nodes, {Omega}=73.1+/-3{deg}, has been
088 derived from spectropolarimetric studies of the Raman-scattered O VI 
088 emission lines [91].
089 =Hen 2-251 K-band spectrum is practically identical with that of the 
089 symbiotic Mira, RX Pup, as observed during the dust obscuration event, with 
089 strong dust continuum and weak CO 2.3-{mu}m band [204, 196].
092 =RT Ser IRAS data from [142].
093 =AE Ara IRAS data from [142].
094 =SS73 96 IRAS data from [142]. An axisymmetrical nebula resolved at radio 
094 wavelengths ([53] and references therein).
096 =V2110 Oph IRAS data from [142].
100 =H 1-36 In [186] there is an estimate of cool component spectral type 
100 M4-5 III based on TiO 7100{AA} band depth. However the spectrum of H 1-36 
100 shown on their Fig. A1 does not show any absorption features or red 
100 continuum. A complex nebula resolved at optical and radio wavelengths ([53] 
100 and references therein). The only symbiotic star known to support an 
100 OH maser [116].
101 =RS Oph Bipolar nebula detected in radio range ([53] and references therein)
102 =WRAY 16-312 IRAS and JHKL colours confirm earlier suggestions [312, 313] 
102 that cool component of this system is a Mira [1]. In the optical spectrum 
102 presented in [18] there are emission lines with ionization potential up to 
102 108.8eV and moreover lines of H I and He I are present [1]. 
102 IRAS data from [142].
103 =V4141 Sgr Classified as S-type in [18, 233], but in the near-IR/IRAS colour
103 diagrams (e.g. [141, 313]) it falls in the region occupied by symbiotic 
103 Miras [198]. K-band spectrum shows strong CO 2.3-{mu}m band consistent with 
103 an M6 giant [204]. Spectral type of cool component also estimated 
103 in [174, 18] to be mid or late M.
105 =AS 245 Classified as S-type in [14, 198] but in the near-IR/IRAS colour 
105 diagrams (e.g. [141, 313]) it falls in the region occupied by symbiotic 
105 Miras [313].
107 =Bl 3-14 The finding chart in [18] is good, but the coordinates are reported
107 to disagree with the measured position: {alpha}=17h} 52min 06.4s, 
107 {delta}= -29{deg} 45' 49'' (1950) [90] (if this is right, our coordinates 
107 should also be corrected).
110 =V745 Sco VK magnitudes during decline from outburst [284].
112 =AS 255 IR-type S -[18, 16], D -[137, 172].
114 =H2-34 Spectral type M5 is estimated by comparing "by eye" the depths of 
114 TiO {lambda},6180 and {lambda,7100} {AA} in the spectrum in Fig. 2 in [198] 
114 with those of spectral standards.
115 =SS73 117 IRAS data from [142].
116 =AS 269 This is a yellow symbiotic star, cool component is G-K giant 
116 [198, 3]. In the optical spectrum there are emission lines with ionization 
116 potential up to 54.4eV [130].
118 =SS73 122 IR-type D -[142], others note only possible S type ([18, 137]).
120 =H 2-38 There was a report of a pulsational period of 433 days for this star
120 in [221], but this is a mistake and the reported number is the pulsation 
120 period of another symbiotic star: V366 Car (Hen 2-38). The spectral type of 
120 the cool component is estimated in [14] to be M8.5.
122 =Hen 3-1591 IR-type D -[18, 233], S -[137, 20].
124 =Ve 2-57 Cool component is M star [11]. In the optical spectrum there are 
124 emission lines with ionization potential up to 35.1eV or probably up 
124 to 54.4eV [11].
125 =AS 276 IR-type S -[18, 16], D -[137]. There is also a D' classification 
125 in [172], but it doesn't look reliable.
128 =V2506 Sgr IRAS data from [92].
132 =YY Her IRAS data from [142].
133 =V2756 Sgr Finding chart in [248] is incorrect ([293]).
134 =FG Ser K magnitude during outburst. Coordinates taken from [96] - 
134 SIMBAD coordinates are not correct.
138 =V4074 Sgr IUE observations reported in [187].
139 =V2905 Sgr IRAS data from [92]. Spectral type of cool component also 
139 estimated in [245] to be K/M.
146 =V3811 Sgr Mis-identified in [248] and in [19] (see [20]).
148 =V3890 Sgr Cool component is M4-8 giant ([95, 316, 283]). In the optical 
148 spectrum there are emission lines with an ionization potential up to 
148 361eV [316]. This object was earlier classified as recurrent nova with 
148 M type companion [283, 95]. The spectrum is also presented in [317].
156 =FN Sgr IRAS data from [92].
160 =V1413 Aql Spectral type M4 estimated from the TiO {lambda} 7100 band depth 
160 as observed during mid-eclipse [197].
162 =Ap 3-1 Short description of optical spectrum is given in [18]. The object 
162 was identified with the 2U 1907+2 X ray source [44] but so far there is no 
162 ROSAT detection, so this identification might not be correct.
166 =BF Cyg IRAS data from [142].
167 =CH Cyg Complex nebula with jet-like features resolved at optical and radio 
167 wavelengths ([53] and references therein). Both the light curves and the 
167 radial velocity curves show multiple periodicities: a ~100d photometric 
167 period has been attributed to radial pulsation of the giant [211], while the
167 nature of the secondary period of ~756d also present in the radial velocity 
167 curve, is not clear [231]. There is controversy about whether the system is 
167 triple or binary [77], and whether the symbiotic pair is the inner 
167 binary [288] or the white dwarf is on the longer orbit [193, 74].
169 =HM Sge Mean K magnitude during outburst. A complex nebula with possible 
169 jet-like features resolved at optical and radio wavelengths ([53] and 
169 references therein, [253]). The nebula is aligned with the binary 
169 orientation deduced from spectropolarimetry of the Raman scattered O VI 
169 lines [264].
170 =Hen 3-1761 IRAS data from [142]. IUE observations reported in [183].
171 =QW Sge IRAS data from [142] although [222] report no IRAS detection.
172 =CI Cyg Coordinates from VLA observations [203].
174 =V1016 Cyg A complex nebula with possible jet-like features resolved at 
174 optical and radio wavelengths ([29, 53] and references therein).
176 =PU Vul V mag during the decline from outburst (XI 1994) [156]. 
176 In [321] ~211d periodicity has been reported.
177 =LT Del IRAS data from [92]. Spectral type of cool component also estimated 
177 in [168] to be G5.
180 =ER Del Cool component is S star of type S5.5/2.5 [6]. In the UV, there are 
180 emission lines with an ionization potential up to 47.9eV and a strong UV 
180 continuum indicates the presence of a hot companion [119]; in the optical 
180 spectrum there are emission lines of H I [119].
181 =V1329 Cyg The system inclination, i=86{deg}+/-2{deg}, and the position 
181 angle of the orbital plane, 11{deg}, has been derived from 
181 spectropolarimetric studies. An extended nebulosity detected in the 
181 [O III] {lambda} 5007 line is aligned with the orbital plane [261].
182 =CD-43 14304 The system inclination, i=58{deg}+/-6{deg}, and the position 
182 angle of the line-of-nodes, {Omega}=103{deg}+/-7{deg}, has been derived from
182 spectropolarimetric studies of the Raman-scattered O VI emission lines [91].
183 =V407 Cyg IRAS data from [94]. IR-type S -[117], D -[227] and also there 
183 is D' estimate in [112]. In [227] there is an estimate of the orbital period
183 of 43 yrs.
184 =StHA 190 In [266] there is a suggestion, based on the IRAS ratio of 
184 F12/F25, that the cool component in this system is a Mira variable. 
184 Comparison of IRAS fluxes with diagnostic diagrams in [142] shows that this 
184 object is among or close to D' systems, and the VJHKL colours are consistent
184 with a G-K giant, so there is no reason to think that a Mira variable is 
184 present in this binary. The authors of [266] argue that F12/F25>1.0 suggests
184 the presence of a Mira but it may be merely the signature of dust around 
184 the system.
185 =AG Peg VK magnitudes during outburst. A complex nebula with possible 
185 bipolar structure detected at optical and radio wavelengths ([53] and 
185 references therein).
186 =LL Cas The presence of the [Fe VII] 4892{AA} line reported in [159] is not 
186 reliable because of the absence of the strongest [Fe VII] 6087{AA} iron line
186 at that time. In [159], there is a report of a possible pulsational period 
186 for the cool component of this system (286.6 days). This is a plausible 
186 explanation, as the spectrum taken at maximum light shows a more pronounced 
186 late-type continuum than the spectrum taken at minimum (see [159]), 
186 indicating that the cool component is responsible for this variability. 
186 IR colours: J=8.90, H=8.03, K=7.55 [19]) with assumed modest amount of 
186 interstellar reddening (AK=0.2) give J0=8.44, H0=7.67, K0=7.35 which 
186 corresponds to the colours of a normal giant in an S-type symbiotic star, 
186 although this might still be a Mira without an IR excess (like the Mira in 
186 R Aqr, which is another S-type symbiotic star).
187 =Z And Spectral type of cool component also estimated in [107] to be ~M5.2. 
187 An inclination of i=47+/-12{deg} and an orbit orientation, 
187 {Omega}=72+/-6{deg}, derived from spectropolarimetry [268]. There is a 
187 report on 28-minute coherent oscillations observed in Z And [292]. We have 
187 included Z And in Table 7 as system with flickering, although these 
187 oscillations are different from rapid light variations observed for 
187 other symbiotics.
188 =R Aqr The binary has been spatially resolved and a preliminary orbit (with 
188 a period of ~44yrs) derived in [106, 66]. The system is embedded in a 
188 complex bipolar nebula with jets ([53] and references therein).
s01 =RAW 1691 Carbon star [311] + H{alpha} profile as for interacting binary 
s01 star [303].
s02 =[BE74] 583 Suspected in [218].
s03 =StHA 55 Carbon star [67] + with strong H I emission [67] (too strong for 
s03 single carbon star).
s04 =CD-28 3719 A symbiotic nature of this star has been suggested based on its 
s04 broad H{alpha} profiles ([124]) and blue colors ([305]).
s05 =GH Gem Suspected in [190, 137].
s06 =ZZ CMi This object was classified as symbiotic in [108, 41]. We disagree 
s06 with this classification because: i) colours are bluer at minimum [324], the
s06 opposite to what is observed for symbiotics; the light curve looks more like
s06 a pulsational curve and not like a symbiotic light curve; ii) the spectrum 
s06 presented in [108] does not look like a symbiotic spectrum (e.g. 
s06 H{gamma}>H{beta}) and is noisy ([Ne III] line may not be present (so 
s06 IPmax=35.1eV). However, this object contains a late-type star (though we do 
s06 not know if the star is giant) and it displays an emission-line spectrum; 
s06 also, the H{alpha} profile shown in [41]) looks like a symbiotic star (for 
s06 comparison see [303]). We therefore include this object as suspected 
s06 symbiotic.
s07 =NQ Gem Suspected in [120]. Highly variable UV continuum with strong C IV] 
s07 emission and Si III]/C III] ratio similar to symbiotic stars. He II 1640{AA}
s07 emission line has been detected in 1979 by IUE.
s08 =WRAY 16-51 Probable presence of late-type star and emission-type spectrum 
s08 (H I emission lines) [174].
s09 =Hen 3-653 Suspected in [18, 245]: late-type star and emission-type spectrum
s09 (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 
s11 broad H{alpha} profiles ([124]) and blue colors ([305]).
s12 =AE Cir Suspected in [149]. Periods of 3900 and 100 days are mentioned 
s12 in [149] (based on visual photometric observations).
s13 =V748 Cen Suspected in [137]: M type giant [30, 271] and emission-line 
s13 spectrum (H I, Fe II, [Fe II], [S II]) [302] and UV excess.
s14 =V345 Nor Suspected in[164]: M star [165] and emission-line spectrum (H I, 
s14 Fe II) [165]. Listed as N Nor 1985/2 in [69].
s15 =V934 Her Suspected in [137]: M bright giant and UV emission lines with 
s15 ionization potential up to 77.5eV but no emission lines in optical spectrum 
s15 and no short-wavelength continuum was found (the 1200-2800{AA} integrated 
s15 flux <1.5*10^-14^erg/s/cm^2^/{AA} at Earth) which excludes the presence of a
s15 hot white dwarf companion (although a neutron star is still possible).
s16 =Hen 3-1383 Possible M type star [256] and emission-type spectrum (H I, 
s16 He I) [11]. Nebula resolved at radio wavelengths ([53] and references 
s16 therein).
s17 =V503 Her Suspected in [137]: M star [40] and blue excess in the optical 
s17 spectra suggesting presence of hot companion.
s18 =WSTB 19W032 Late type giant [52] and emission-line spectrum: lines of H I, 
s18 He I and others with ionization potential up to 35.1eV. But this 
s18 emission-line spectrum might not be physically connected with the giant [52]
s19 =WRAY 16-294 Suspected in [198]: red continuum typical of reddened K giant 
s19 and emission-line spectrum (H I, He I and others with ionization potential 
s19 up to 35.1eV). WRAY 16-294 appears as WRAY 16-296 in [198].
s20 =AS 241 Suspected in [18]: M star [198] and emission-line spectrum (H I, 
s20 He I) [198]. M6 spectral type of cool component and D' IR type from [172] 
s20 are not reliable, as M6 does not agree with IR colours (JHK) and authors do 
s20 not follow original definition of D'.
s21 =DT Ser Considered as symbiotic in [49, 50]: emission spectrum of H I, He I 
s21 and other lines with ionization potential up to 54.4eV plus G? [49] or 
s21 G2-K0 III-I [50] cool component. But there is a report of a G star 5'' from 
s21 this object, so the cool component may not be connected physically with the 
s21 source of the emission-line spectrum.
s22 =V618 Sgr Presence of late-type component (TiO bands in optical 
s22 spectrum [149]) and emission-line spectrum (H I, Fe II [149]).
s23 =AS 280 Suspected in [198]: this object resembles a symbiotic star in 
s23 outburst.
s24 =AS 288 This object shows optical emission-line spectrum (H I, He I and 
s24 others with ionization potential up to 54.4eV) but no late-type component 
s24 has been seen so far, however K magnitude and IRAS fluxes compared to 
s24 diagnostic diagrams in [142] place this object among symbiotics (of IR 
s24 type D), emission-line fluxes ([O III]4363, 5007{AA}, H{beta}, H{gamma}) 
s24 compared to diagnostic diagrams in [181] place this object also among 
s24 symbiotics (among IR type S but close to D-type objects).
s25 =Hen 2-379 Cool component is G-K giant [168, 293] and there is emission-line
s25 spectrum: H I, He I and other lines with ionization potential up to 35.1eV. 
s25 But K giant might not be physically associated with nebula, which is source 
s25 of the emission [170]. Finding chart in [248] is unclear as reported 
s25 in [293].
s26 =V335 Vul Suspected in [229]: presence of carbon giant and optical 
s26 emission-line spectrum (H I) displaying hot continuum in blue. We agree with
s26 this classification although this object might be a single pulsating star: 
s26 (i) the carbon star might pulsate with period of 342 days [57] and then 
s26 emission lines behave as for a Mira variable - they disappear near minimum 
s26 light and show up again at maximum (see spectra in [229]); (ii) H{alpha} is 
s26 very narrow: 2{AA} (90km/s) and for a symbiotic star we would expect a width
s26 of about 300-500km/s; (iii) the Balmer decrement is different than that 
s26 observed for symbiotic stars (it resembles that of Mira variable), although 
s26 the authors of [229] claim that the Balmer decrement resembles that of a 
s26 symbiotic star.
s27 =V850 Aql Probable presence of Mira [39, 147] or late-type star [3] in the 
s27 centre of planetary nebula PK 037-6 2 (see note in [147]) with emission-line
s27 spectrum (H I lines). In [3] and [39] there are notes that in [19] this 
s27 object is classified as symbiotic, but this is not true and in [19] there 
s27 are only IR colours for V850 Aql.
s28 =Hen 2-442 Suspected in [323]: TiO bands probably present, suggesting cool 
s28 component [25, 323] and optical emission-line spectrum: H I, He I and other 
s28 lines with ionization potential up to 100eV. Hen 2-442 consists of two PN 
s28 like objects: Hen 2-442A and Hen 2-442B [25] and values in catalogue are for
s28 the whole system. Symbiotic nature was suggested for Hen 2-442 A.
s29 =IRAS 19558+3333 Suspected in [277]: OH/IR star, based on IRAS colours, but 
s29 without an OH maser, so a probable, extreme D-type system. Radio continuum 
s29 emission implies a hot, ionising companion. Correct coordinates given here 
s29 for precise radio emission (incorrect coordinates given by [277]).
s30 =V627 Cas Suspected in [158]. Spectral type of cool component also 
s30 estimated in [154] to be M2-4.