Online Material

 

 

Table 1: Selected particulars of the s-a S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
designation	date	$\log T_{\rm eff}$	MV	$\log L/L_{\odot}$	ref.	g?d?	ref.
HD/HDE
AG Car	min 1985-1990	4.46a	-7.7	6.14	96,103	y y	173, 196, 251, 254, 264, 273, 291
= 94910	max 1982	4.13	-9.8	6.22	96
HR Carb	min 1970	4.34	-8.0	5.90	pp	y y	120, 173, 196, 250, 251
= 90177	max 1992	3.90	-9.3	5.62	pp
160529	min 1989.5	4.00	-8.4	5.46	77	n n	173, 250
= 164G Sco	max 1972-1980	3.90	-8.9	5.46	77
WRA751	min 1989-1991	4.48	(-6.0)	(5.50)	pp,114,126	y y	126, 173, 196, 250, 291, 297
	max 1949-1951
R4c	min $\sim$1984	4.43	-5.3d	5.06	67	y y	95, 275
= S6	max $\sim$1988
A-comp		3.98	-5.2d	4.14	67
R40	min $\sim$1959	4.05	-8.7	5.66	9
= 6884	max 1996.3	3.90	-9.5	5.70	137,138
R71	min 1982, 1989	4.24	-8.0	5.80	42	y y	173, 196, 250
= 269006	max 1975	4.10	-9.2	5.92	42
S Dor	min 1965	4.54e	-7.6	6.30	70	? ?	173, 250
= R88	max 1989	3.93e	-10.0	5.96	70
= 35343
R110	min 1957-1962	3.96	-8.4	5.36	7,63	? ?	173, 250
= 269662	max 1993	3.84	-9.2	5.56	7,63
R116f	min 1989-1990	4.29	-8.4	5.92	pp
= 269700	max $\sim$1900
R127	min 1969.9	4.46	-7.4g	6.00	5,7	y y	173, 250, 256
= 269858f	max 1989.8	3.87	-10.0	5.92	7
R143	min 1981-1995	4.23	-8.2	5.70	pp	? ?	173, 250
= 269929	max 1957	3.90	-9.4	5.72	pp
269216h	mean 1970-1993	4.08	-8.2	5.44	64,66
= Sk $-69^{\circ}75$
HV5495i	min 1988-1993	4.46	-7.0	5.80	22	? ?	173, 250
= 269582	max $\sim$1990
= BE294
= MWC112

Notes to Table 1:
^a See the discussion on the temperature scale (70).
^b In the maximum of 1992 (b-y) = 0.83 and with E(b-y) = 0.78E $(B-V)_{\rm J}$ = 0.78, (b-y)₀ = 0.05. Adopting $\log g$ $\sim$1 and a solar abundance, $T_{\rm eff}$ $\sim$8000K (259).
^c R4 consists of two components: an LBV/B[e] star and an A-type star. The latter is presumably constant. See note ^d in Table 3.
^d Adopted value by (67).
^e The temperatures at the visual minimum of 1965 and the visual maximum in 1989 have been derived from the estimated colour $(B-V)_{\rm J}$ $\sim$-0.1 (74) and the observed colour $(B-V)_{\rm J}$ = 0.28, respectively, and corrected for E $(B-V)_{\rm J}$ = 0.20. Vennix et al. (quoted by (71)) using Kurucz models and a different distance and reddening for the same visual maximum found: $\log T_{\rm eff}$ = 3.95 and $\log L/L{\odot}$ = 5.85. Note that the epoch of our chosen visual minimum is not the same as theirs.
^f The spectral type in the visual minimum is according to (9): B1.5Iaeq.
^g The visual minimum which has been used for the determination of M_V has been corrected for the faint companion, see note ^d in Table 2.
^h Spectral type according to (64) and (65) B8I.
ⁱ Spectral type close to visual minimum ($V_{\rm J}$ = 11.88) WN10h by (22).

 

 

Table 2: Selected particulars of the s-a S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)
designation	$E(B-V)_{\rm J}$	ref.	r	ref.	$V_{\rm J}$	$V_{\rm J}$	ref.	add. ref.
HD/HDE			(kpc)		min	max		[Remarks]
AG Car	0.63	97	6	97,98	8.1	6.0	70	29,46,57,76,78,83,99,
								101,109,113,114,116,119,
								121,124,125,127,128,131,
								196,198-201,263
HR Car	1.00	102,107	5.2	110,111	8.7	7.4	7,108	32,46,57,109,112,
								113,114,116,122,123,
								128,196,198-201
160529	1.10	77	2.5	77	6.95	6.4	77	79,80,81,82,198-201,281,293
								[See for BD and
								HD mag note a]
WRA751	1.6	114,115,	$\geq$ 4.5	114,115,	12.3	10.3	114,115,	196
		126		126			117,118
R4	0.07	67			13.0b	12.5b	67	95,134
R40c	0.14	136			10.7c	9.9	9,137	57,83,119,198-201,281
								[HDptg 1900 = 10.8]
R71	0.20	42			11.0	9.9	43,74,197	44,46,47,57,78,83,119,168,
								196,198-201,281
								[HDEptg 1925 = 9.2]
S Dor	0.20	70			11.4	9.0	70	44,57,71,72,73,74,75,78,
								168,198-201,271,281
R110	0.15	62			10.6	9.7	3,7	10,23,51,57,199-201,281
								[HDEptg 1925 = 10.8]
R116	0.15	8			10.6		8	9,10,44,50,51,52
								[HDEptg 1925 = 10.4]
R127	0.12	103			11.2d	8.8	7,88	1,6,9,46,57,76,78,87,
								198-201
								[HDEptg 1925 = 11.1]
R143	0.54	1			12.0	10.6	1,2,85,	3,4,9
							86
269216	0.12	66			10.7e		66	49,65
								[HDEptg 1925 = 11.0]
HV5495	0.24	39			12.2	11.7	22,39,40,	12,23,131,199-201
							41

Notes to Table 2:
^a BD visual magnitude ($\sim$1850) = 6.9. Three HD photometric magnitudes (ptm) in 1897 with an average 6.69 and two in 1899 with an average 6.68. The averages and (the small) residuals are given in H.A.45 and 46, respectively. The HDptg 1900 = 7.6 is more or less consistent with respect to the HDptm above in view of the high reddening amounting to 1.10 (Col. 2).
^b Both components together, see note ^d in Table 3.
^c Note that the HDptg magnitude (see Col. 9) and the $\sim$1959 magnitude $V_{\rm J}$ = 10.73 by (9), are roughly equal. Thus, considering the low reddening, the star was at both epochs at roughly the same minimum brightness. Note that the current SD-activity started after 1959, see (7) and (137).
^d This is the magnitude including the faint field star nearby. After correction $V_{\rm J}$ = 11.4.
^e This is the mean apparent magnitude.

 

 

Table 3: Time scales and amplitudes of the light variations of the s-a S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)
designation	L-SD	S-SD	microvar.	ref.	light curve/
HD/HDE	(yr, mag)	(yr, mag)	(d, mag)		light history
AG Car	25	1a	10-41	43,70,78,84,100,	Fig. 1
	1-2	0.2-1.5	0.1	102,247,248
HR Car	10-20	2-3	20-40	7,78,247
	0.5	0.5	0.15
			100
			0.2
160529	30-50	2.7	45-57	77,78,84,b	Fig. 2
	0.5	0.1	0.1
WRA751c	c	c	30.5	115	Fig. 3, Table 16
			0.15
R4d	(25)			67
	(1)
R40	25	3.5	46; 99; 121	7,66,137,247	Table 16
	0.2-0.6	0.02	0.1
R71	10	3, 6	14-24; 76	7,43,69,76,84,247	Fig. 4, Table 16
	1	0.25	0.1
			100-200
			0.2
S Dore	35	6.8e	$\sim$100; 131; 195	70,76,247,248
	1-2	0.5-1.2	0.2
R110	20	2-3	50-100	7,63,247	Fig. 5, Table 16
	0.3-0.6	0.1-0.3	0.02-0.1
R116	(25-50)		(10-40)	8	Fig. 6, Table 16
	1.4
R127	>13	1.4	$\sim$100; 111	7,78,247	Fig. 7, Table 16
	1.7	0.5	0.1
R143	>30				Fig. 8, Table 16
	(1.5)
269216		1.6	(16)	66	Fig. 9
		0.4	0.1
HV5495	20	2.2		39,40,41	Fig. 10, Table 16
	1.2	0.3-0.5

Notes to Table 3:
^a The primary period P₀ = 371.4d shows a beat of 21.6yr (70), see Fig. 1 and Sect. 1.5.3.
^b According to the analysis of spectroscopic time series (293), a dominant period of 92.5d is present for the photospheric line profile variations, which is about twice the photometric periods, and a period of 114-127d for the wind line profile vriations.
^c It is unknown to what type of SD-phase (S-SD or L-SD) the long-term light variation belongs with an approximate amplitude of $2^{\rm m}$ (Fig. 3).
^e Although the colour index $(U-B)_{\rm J}$ becomes bluer during brightening (67), while this should be just like the $(B-V)_{\rm J}$ redder, we are yet most likely dealing with an SD-phase. This blueing can be explained by the presence of the A-type companion of which the contribution in the UV channels becomes dominant when the S Dor star becomes cooler than its companion. For example: if $V_{\rm J}$ (S Dor star in min) = 13.9, and $V_{\rm J}$ (A star) = 14.0, the blueing in $(U-B)_{\rm J}$ can be explained if the rise in the visual due to an SD-phase amounts to $\sim$$1^{\rm m}$.
^d The reported brightening in 1999 by (271) is nothing else then a new S-SD phase, confirming the established cyclicity amounting to on the average 6.8yr (70).

 

 

Table 4: Selected particulars of the w-a S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)
designation	Sp.	date	$\log T_{\rm eff}$	MV	$\log L/L_{\odot}$	ref.	g?d?	ref.
HD/HDE
$\eta$ Cara		1970-2000	4.36-4.18	-7--9	5.14-6.34	181,182,183,	y y	b
= 93308						184,186,194
P Cyg	B1Ia+	min 1980-2000	4.26	-7.9	5.70	142	y n	149,173,196,
= 193237								240,250,255
168607	B9.4Ia+	1970-1990	3.97	-8.4	5.38	38,48	n n	173
= V4029 Sgr
Cyg OB2#12	B5Ie	1990	4.11	(-10.4)	(6.42)	162
R74	BIe	1988-1990	4.11	-7.8	5.40	8
= 268939
R81	B2.5eqIa+	min 1960-1995c	4.30	-8.6	6.04	139
= 269128
R85d	B5Iaed	min 1960	4.13	-8.2	5.54	pp,9
= 269321		max 1983-1990	4.00	-8.5	5.50	pp,63,272
R99e	WN10	1960-1990	4.50	-8.3	6.42	93	? ?	173,250
= 269445
R123e	Bpec	1980-1990	4.54	-8.5	6.60	94
= 37836
R149	Be+neb	1960-1985	4.30	-6.4	5.16	pp
= -69$^{\circ}$ 476f
34664	B[e]	1982-1990	(4.39)g	-7.4	(5.80)g	pp	- y	21
= S22			4.18h	-7.4	5.32h	pp
38489i	Be	min 1960 & 1984	4.52	-8.0	6.36	pp	- y	95
= S134		max 1966	4.05	-8.4	5.52	pp

Notes to Table 4:
^a Total luminosity $\log L/L_{\odot}$ = 6.65 ( $M_{\rm bol} = -11.9$). Physical and photometric parameters in the table are only for the S Dor variable hidden in $\eta$ Car. Their large uncertainty is due to the following facts: (i) most of the visual light is reflected light from the core by the Homunculus; (ii) the internal reddening in the Homunculus is highly uncertain; (iii) the S Dor variable is presumably not single (e.g. 185). The peculiar non-stellar variability (Sect. 3.2.6) is perhaps due to the varying physical conditions of a luminous accretion disk according to (298), perhaps around a hot nearby companion of the S Dor star. The error box in Fig. 20 has been computed from the estimated temperature- and M_V limits of the S Dor star. The spectral type of that object looks like that of P Cyg (186), (294). See for more information the notes to Tables 5 and 6 and Sects. 3.2.2 and 3.2.6.
^b The literature on the Homunculus is overwhelming, see ``add.ref.'' in Table 5 and references therein.
^c Presumably the star is at present in a minimum of SD-phases, but the parameters were taken outside the eclipse (Fig. 12), since R81 is an eclipsing binary (140) of which the revised period $P = 74.55\,d~\pm~0.02$d m.e. (66).
^d The spectral type is from (9) and presumably for the date $\sim\,1959$. According to (272) the spectral type was AIe in October 1996 and somewhat hotter in January 1999: B8Ie. The trend of these three spectral types supports the presumable trend of the L-SD cycle sketched in Fig. 13, thus, in the minimum the star is hotter than in the maximum. For the temperature and luminosity during the maximum (1983-1990), a spectral type A0Ia has been adopted, inspired by the spectrum made some years later by (272). The minimum and maximum apparent magnitudes used for the two M_V values are 10.8 and 10.5, respectively.
^e Possibly having a disk, see references in Col. 7.
^f CPD number. The maximum light amplitude, MLA = 0 $.\!\!^{\rm m}$3, is too high for a normal $\alpha$ Cyg variable, thus, supporting the S Dor membership based on (10) and observations listed in Table 7, see note ^e in Table 5 and note ^f in Table 6.
^g If the spectral type is B0-0.5 according to (14).
^h If the spectral type is B4 according to (13), which agrees better with the photometry than the previous spectral type in note ^g, therefore, the star has been plotted with the matching $T_{\rm eff}$ and L on the HR-diagram in Fig. 20.
ⁱ See Fig. 18 for a correlation $V_{\rm J}$/ $(B-V)_{\rm J}$ which supports the S Dor membership. However, the track on the HR-diagram is abnormally steep (Fig. 20). Perhaps inadequate photometry and/or the presence of much circumstellar material is the cause of its abnormality.

 

 

Table 5: Selected particulars of the w-a S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)
designation	$E(B-V)_{\rm J}$	ref.	r	ref.	$V_{\rm J}$	$V_{\rm J}$	ref.	add.ref.
HD/HDE			(kpc)		mean	min		[Remarks]
$\eta$ Cara	0.50	178,179,	2.3	189,194	a	a		83,119,190,191,193,195,198-201,
		180,181						202,203,206,242,243,269,276,
								278,279,282,283,287,288,289,
								290,292,294,295,296,298,299
P Cyg	0.51	142,145	1.7	142		4.9	147,169,	143,144,146,149,150,151,
							204	152,224,237,238,239,240,
								241,249,280,281
168607b	1.55	38	2.2	132,133	8.2b		38,66,	48,198-201
							80,253	[HDptm 1900 = 8.9;
								$V_{\rm J}$(1956) = 8.29 (89)]
CygOB2#12	3.4	159,162	(1.7)	161,162	11.5		163	160,164
R74	0.15				11.0		8	9,10,11,12
								[HDEptg 1925 = 10.6]
R81	0.14	66,139,				10.3c	198-201	3,9,44,51,66,119
		141
R85	0.17d	pp			10.65	10.8	63	10,57,198-201,272
								[HDEptg 1925 = 10.9]
R99	0.42	91,94,			11.45		91	10,22,57,92
		95						[HDEptg 1925 = 11.6]
R123	0.20	94			10.55	10.7	91	10,44,57,87,93
R149	0.10				12.4e		10	9,165,166,167
34664	0.28	15			11.8		8,15	11,16,17,18,19,20,21
38489		87			11.85f	12.1f	8,85,	10,95
							87	[HDptg 1900 = 11.6]

Notes to Table 5:
^a The apparent visual magnitude of the S Dor variable inside $\eta$ Car is very uncertain, see note ^a below Table 4. See for the integrated magnitudes (thus including the bipolar nebula) the references (182), (178), (188), (187), (184), (192) and (243). Note that the constructed $V_{\rm J}$ scale in (188), (187), (184) and (192) is about 0 $.\!\!^{\rm m}$15 fainter than the constructed $V_{\rm J}$ scale in (182) and (178) and about 0 $.\!\!^{\rm m}$2 fainter than the $V_{\rm J}$, directly obtained with an UBV photometer, from (243). The cause is the use of different filter systems, clearly expressed by the transformation formula and is not due to errors in the photometry. For instance, it is easy to see from the zero points in the transformation equations given for $V_{\rm J,Geneva} (22'')$ and y in Sect. 2 of (184) that the difference between the two systems amounts to 0 $.\!\!^{\rm m}$213. The first is brighter than the second magnitude scale and consequently close to $V_{\rm J}$ directly measured by an UBV photometer. The cause is the emission spectrum of $\eta$ Car and the narrowness of the y passband. See also (277).
^b Note that the HDptg 1900 = 8.7, listed in the HD catalogue, has been derived from the HDptm, by adding the colour index -0.2 (see the Introduction to the HD catalogue), assuming zero reddening. Since the reddening appears to be substantial (Col. 2), the HDptg 1900 must be considered as erroneous.
^c This is the outside-eclipse magnitude, but supposed to be the minimum of possible S Dor phases.
^d Based on the spectral types in minimum light (B5Iae) and maximum light (A0Ia, see note ^d in Table 4) and $(B-V)_{\rm J}$ = 0.1 (9) and 0.18 (63), respectively.
^e VBLUW photometry, made in eight nights in 1975 and 1976 are listed in Table 7. The $V_{\rm J}$ given above is an average based on a compilation in (10), complemented with the data in Table 7 and in (165), (166) and (167).
^f At maximum light the apparent magnitude $V_{\rm J}$ = 11.6. In view of the reddening (Col. 2), the ``HDptm'' could have been between 11.1 and 11.6.

 

 

Table 6: Time scales and amplitudes of the light variations of the w-a S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)
designation	L-SD	S-SD	microvar.	ref.	light curve/
HD/HDE	(yr, mag)	(yr, mag)	(d, mag)		light history
$\eta$ Cara		1-6	58.6	84,184,187,188,192,195,205,	Fig. 11b
		0.2-0.4	0.04-0.08	245,246,247,248,277,298
P Cygc		8.2d	17.3	147,148,169,204
		0.06	0.05-0.15
			70-150
			0.2
168607e		1.8d	62	80,253	Table 16
		0.2	0.2
CygOB2#12	(50)		?	163
	(0.2)		0.3
R74			42.1	8
			0.25
R81	>50?		24.1	38	Fig. 12,
	>1		0.17		Table 16
R85	30-40	1.1	15-180	63	Fig. 13
	0.3	0.1	0.01-0.2
R99	30		2.1, 10	91	Fig. 14
	0.3		0.15
R123		0.8	3.9; 1.3	91	Fig. 15,
		0.2	0.13		Table 16
R149		>0.5?	?	166
		0.1	(0.3)f
34664g		7	47.2	8	Fig. 16
		0.04	0.14
38489h				10	Fig. 17

Notes to Table 6:
^a Showed a number of presumable SD-eruptions between 1827 and 1857, and a single SD-eruption around 1870 and once more around 1890, see next note.
^b The historical observations (until 1910) include a few observations between 1600 and 1800. After 1935 a gradual rise set in, called the ``secular rise'' and has been interpreted as largely caused by a decrease of circumstellar extinction by the expanding bipolar nebula (178), see also (206) and (274). In Fig. 11, showing a schematic light curve, all observations after 1970 which are not measured by an UBV photometer are corrected according to our transformation equations to fit the $V_{\rm J}$ directly measured by an UBV photometer. See note ^a in Table 5 and (277). Superimposed on the secular rise (after 1960) the frequent SD-phases with a time scale of 1-6 yr and an amplitude of about 0 $.\!\!^{\rm m}$2 are schematically indicated. The last one of 1999-2000 has an amplitude twice as high (192), (243), (277), (298).
^c Showed a number of SD-eruptions between 1600 and 1700 (150), (151). Balmerline shell ejections were observed on a time scale of a few months to half a year (152), (237), (238) and (249).
^d This very low-amplitude oscillation is possibly an SD-phase: the $(B-V)_{\rm J}$ tends to be red in the maxima and blue in the minima. See for P Cyg the discussion in Sect. 3.2.2.
^e Note that the star was possibly fainter around 1900, see Table 5. The 640d (1.8yr) peak in the Fourier analysis is likely due to an S-SD phase, clearly visible in Fig. 5 of (253) and not an artifact.
^f This relative high amplitude, based on the references mentioned in note ^e in Table 5, may be partly caused by the SD-phase mentioned in Col. 3 of Table 6.
^g Note that the amplitude of the microvariations is larger than that of the S-SD phase, see Fig. 16.
^h It is uncertain to what type the probable long-term light variation (with unknown time scale) with an amplitude of 0 $.\!\!^{\rm m}$5 belongs, see also Fig. 17 and notes ⁱ and ^f in Tables 4 and 5, respectively.

   

Table 7: VBLUW photometry of R149 (in log intensity scale) and the transformed values in the UBV system (in magnitude scale) with subscript J, made in 1975 and 1976

JD -	V	V-B	B-U	U-W	B-L	$V_{\rm J}$	$(B-V)_{\rm J}$
2440000
2712.555	-2.202	-0.003	-0.072	0.13	-0.030	12.39	-0.02
2714.552	-2.208	0.002	-0.080	0.08	-0.042	12.41	0.00
2813.382	-2.200	-0.008	-0.097		-0.047	12.39	-0.03
2818.362	-2.212	-0.005	-0.074		-0.040	12.42	-0.02
2830.282	-2.216	-0.012	-0.103		-0.042	12.43	-0.04
2838.299	-2.205	0.005	-0.089		-0.033	12.40	0.00
2862.288	-2.191	0.017	-0.085		-0.026	12.36	0.03
2869.344	-2.218	-0.004	-0.090		-0.040	12.43	-0.02

 

 

Table 8: Selected particulars of the ex-/dormant S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)
designation	Sp	date	$\log T_{\rm eff}$	MV	$\log L/L_{\odot}$	ref.	g?d?	ref.
HD/HDE
$\zeta^{1}$ Sco	B1.5Ia+	1985-1995	4.29	-8.5	6.02	56,pp
= 152236
168625	B5.6/8Ia+	1982-2000	4.15	-7.3	5.23	36	y y	173,250,252
= V4030 Sgr
326823	B1.5Ie	1960-1990	4.29	-6.0	4.98	68,106
= $-42^{\circ}$ 11834a
He3-519	WN11	1985-1992	4.48	(-7.9)	(6.26)	29,129,	y y	135,173,250,251
						257
316285	BIe	1984-1996	4.18	-8.4	5.44	33
= He3-1482
S61	Ofpe/WN9	1970-2000	4.45	-7.0	5.84	pp,154	y y	173,250
= Sk $-67^{\circ}$ 266
Sk $-69^{\circ}$ 279	O9f	1980-2000	4.48	-6.4	5.68	158,pp	y	155,156,279
S119	WN11h	1970-2000	4.44	-6.8	5.80	22b	y ?	173,250,251,279
= 269687

Notes to Table 8:
^a CoD number.
^b Model B.

 

 

Table 9: Selected particulars of the ex-/dormant S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
designation	$E(B-V)_{\rm J}$	ref	r	ref.	$V_{\rm J}$	ref.	add.ref.
HD/HDE			(kpc)		mean		[Remarks]
$\zeta^{1}$ Scoa	0.65	53,55,	1.8	53,54,	4.75a	57,58,	59,80,207
		208		209		198-201
168625b	1.7	34	1.2	36	8.4b	38,89,	35,37,48,66,198-201
						66,80,	[HDptm 1900 = 9.2,
						253	VJ 1956 = 8.41 (89)]
326823c	1.15	105,106	2	106	9.1	105	32,83,119
He3-519d	1.3	29,129,	(8)	129	11.0d	29,131	24,135
		257					[m$_{\rm pg}$ 1949-1950 $\sim$
							10.5 (130)]
316285	1.81	33	1.85	33	9.1	33	32,211
S61	0.18	92,153			12.0	49	154
Sk $-69^{\circ}$ 279	0.25	pp			12.8	23	157,244
S119e	0.09	1			11.95e	1,23	24,25,244
							[HDEptg 1925 = 11.4]

Notes to Table 9:
^a The star was much brighter in the 18th and 19th century, see (58).
^b Note that the HDptg = 9.0 (listed in the HD catalogue) has been derived from the HDptm = 9.2 by adding the estimated colour index -0.2, assuming that the reddening is zero. Since the reddening appears to be substantial (Col. 2), the HDptg is erroneous. The HDptm 1900 = 9.2 suggests that the star was $\sim$0 $.\!\!^{\rm m}$8 fainter around 1900 than at present.
^c According to (104) and (105) perhaps an ex-S Dor variable on its way to the WN-stage, see note ^c in Table 10.
^d According to (130) the star was possibly brighter in the interval 1949-1950, see [Remarks]. If this is the case, the star could be a w-a S Dor variable.
^e It is not certain whether the magnitude difference with the HDEptg 1925, see the [Remarks], should be taken seriously.

 

 

Table 10: Time scales and amplitudes of the light variations of the ex-/dormant S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)
designation	L-SD	S-SD	microvar.	ref.	light curve/
HD/HDE	(yr, mag)	(yr, mag)	(d, mag)		light history
$\zeta^{1}$ Sco			2000a	56,58,84	Table 16
			0.02
			32
			0.1
			25.7
			0.1
168625b			35	38,66,80,253	Table 16
			0.06
326823c			6	105,119
			0.1
He3-519d					Table 16
316285e			?	33
			0.1
S61
Sk $-69^{\circ}$ 279
S119

Notes to Table 10
^a The colour becomes bluer in the light maximum, thus, this periodicity/cyclicity is presumably no SD-phase.
^b See note ^b in Table 9 on a possible long-term light variation.
^c While the object showed an increasing trend of the brightness between 1990 and 1994, the colour became bluer which is unlike an SD-phase, see note ^c in Table 9. Further, the photometric observations by (105) show a long-term oscillation of 396d and an amplitude of 0 $.\!\!^{\rm m}$2, but it is unknown whether they should be classified as an S-SD phase, in which case the object should be a w-a S Dor variable.
^d See note ^d in Table 9 on a possible long-term light variation.
^e According to (33) hardly variable (  0.1) since 1890, also according to the Hipparcos data quoted by (103).

 

 

Table 11: Selected particulars of the candidate (+ and -) and former candidate (0) S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
designation	Sp.	cand.	date	$\log T_{\rm eff}$	MV	$\log L/L_{\odot}$	ref.	g?d?	ref.
HD/HDE
80077	B2/3Ia+	+	1975-1995	4.23	(-9.4)	(6.30)	38,236
148937	O6.5f	-	1960-1995	4.58	-6.0	5.68	132,170,
							171
WRA977	B1.5Ia+	0	1970-1995	4.28	-8.7	6.06	39,59
= BP Cru
= Hen788
AS314	B9Ia	+	1983-1997	4.01	(-7.0)	(4.9)	222	y y	222,223
= V452 Sct
= LS5017
IRC+10420a	F8Ia+-	+	1975-1994	3.90b	(-10.0)	(5.80)	260,284	y y	176,260,261,262,
	mid-Ab								286
MWC314	< B2	+	1954-1995	4.48	(-8.2)	(6.34)	210,222
= V1492 Aql
= BD+14 3887
G79.29+0.46		+	1983-2000	4.40		(6.3)	60	y	250
G25.5+0.2c		+	1983-1993		c		172	y	250
Pistol Star		+	1994-1998	4.15d	-10.8	6.61d	265	y y	265
				4.33e	-11.3	7.20e	265
S18	B[e]	-	1975-1995	4.40	-6.7	5.58	226
5980f	WN3+OB	+	min of				218,219,
= R14			1950-1980				220
	WN11+OB		max of		(-10.7)		pp
			1994.8
R78	B0Ia	-	1960-1990	4.41	-7.4	5.80	45
= 269050
R84	WN9	-	1960-1995	4.46	-6.8g	5.77	22	? ?	173,250
= 269227
269604	A1Ia+	0	1970-1985	3.96	-8.0	5.20	pp
R128	B2Ia	0	1960-1995	4.24	-8.2	5.76	90
= 269859

Notes to Table 11:
^a Considered as a variable yellow hypergiant by (270) and (284). See the discussion in Sect. 3.2.5 of the present paper.
^b According to (285) the spectral type evolved to mid-A in 1994. The temperature has been determined from that spectrum by (284). See also the discussion in Sect. 3.2.5 of the present paper.
^c M_K = -7 according to (172).
^d Model L of (265).
^e Model H of (265).
^f Showed two SD-type eruptions, one in 1993 and a second in 1994. Since the true nature of the multiple star (including an eclipsing binary), is far from being understood, no proper physical and photometric parameters on the possible S Dor variable in the system can be given.
^g The apparent visual magnitude has been corrected for the faint field stars in the aperture, see (8).

 

 

Table 12: Selected particulars of the candidate and former candidate S Dor variables

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
designation	$E(B-V)_{\rm J}$	ref.	r	ref.	$V_{\rm J}$	ref.	add.ref.
HD/HDE			(kpc)		mean		[Remarks]
80077	1.47	38,235	(3)	232,233	7.5	38,232	66,234
							[HDptm 1900 = 7.9;
							HDptg 1900 = 9.0]
148937	0.60	pp,171	1.38	132	6.7	170	174
WRA977	1.65	39,59	5-8	39,59	10.9	39
AS314	0.9	222	(8)	222
IRC+10420	2.2	175	(5)	175	11.0	175	176,177,270
MWC314	1.84	210	(3)	222	9.9	210
G79.29+0.46	5-2	60,196	2-4	60,196			61
G25.5+0.2	10	172	(14.5)	172			173
Pistol Star	8-11	266	8	268			267
S18a	0.4	225			13.55a	227	228,229,230,231
5980b	0.07	218			c		213,214,216,217,220,221
R78	0.15	pp			11.7	8	9,10,49
							[HDptg 1925 = 11.2]
R84	0.18	26			12.1d	8,27	10,11,21,28,29,30,31
							[HDEptg 1925 = 11.6]
269604	0.10	pp			10.8	10
R128	0.12	90			10.6	90,91	10,57
							[HDEptg 1925 = 10.9]

Notes to Table 12:
^a Star strongly variable, see Table 13 and Fig. 19.
^b There is an eclipsing binary in the system (215), with P = 19.2654d and an amplitude amounting to $\sim$0 $.\!\!^{\rm m}$2 (212).
^c $V_{\rm J}$ (min) = 11.7, $V_{\rm J}$ (max) = 8.5 (83), (213).
^d Corrected for the field stars in the aperture.

 

 

Table 13: Time scales and amplitudes of the light variations of the candidate and former candidate S Dor variables

(1)	(2)	(3)	(4)	(5)
designation	cand	microvar.	ref.	light curve
HD/HDE		(d, mag)
80077a	+	41-66	38,66
		0.2a
148937b	-		170
WRA977	0	11.90c	90
		0.14
AS314	+
IRC+10420	+
MWC314d	+	4.16?	210
		0.1
G79.29+0.46	+
G25.5+0.2	+
Pistol Stare	+
S18f	-			Fig. 19
5980g	+	0.25g	212
		0.1
R78	-	3.6-3.9?	8,9
		0.1
R84	-	h	8
269604	0	?	10
		0.18
R128	0	3.444	91
		0.25

Notes to Table 13:
^a The maximum light amplitude, MLA = 0 $.\!\!^{\rm m}$2, is too high for a normal $\alpha$ Cyg variable (39). Therefore, it is not excluded that it may be partly due to a very weak SD-phase (38). Thus, this is in conflict with the supposition of (235) and (236) that it is no S Dor variable, but a hot blue hypergiant.
^b The apparent magnitude $V_{\rm J}$ became gradually brighter on a long-term basis by $\sim$0 $.\!\!^{\rm m}$1 between 1960 and 1987. Between 1981 and 1987 the star showed microvariations 0 $.\!\!^{\rm m}$01 exclusively in blue and ultraviolet light on a time scale of months (170).
^c This is a quasi-period which appeared to be stable on a time basis of 17yr (39).
^d According to a compilation of optical photometry made between 1954 and 1992 by (210), $V_{\rm J}$ varied by $\sim$0 $.\!\!^{\rm m}$1. However, it is unknown whether this is caused by a long-term variation, or by microvariations, see Col. 3.
^e The light variations in the H and K passbands lie barely outside the errors of the data (265).
^f The long-term light variations with a time scale of months and an amplitude of $1^{\rm m}$, are no SD-phases, see Fig. 19. These observations are based on preliminary VBLUW photometry. The V of this system has been transformed to the V of the UBV system (with subscript J) (231).
^g It is uncertain which of the stars in the system is responsible for the this pulsation-type of light variation (212).
^h No significant light variation was detected during the photometric monitoring between 1988 and 1991.

   

Table 14: Bibliographical references mentioned in the Tables 1-6 and 8-13 are codified as follows

No.	Reference	No.	Reference	No.	Reference
1	L. Smith et al. 1998	50	van Genderen et al. 1982	101	de Koter et al. 1996
2	Parker et al. 1993	51	Appenzeller et al. 1979	102	van Genderen et al. 1990
3	Walraven et al. 1977	53	van Genderen et al. 1984	103	de Koter et al. 1993b
4	Walborn et al. 1997	54	Percy et al. 1991	104	Lopes et al. 1992
5	Stahl et al. 1983	55	Leitherer et al. 1984	105	Sterken et al. 1995b
6	Stahl et al. 1986	56	Rivinius et al. 1997	106	Kozak 1985
7	van Genderen et al. 1997b	57	van Genderen 2000	107	Viotti 1971
8	van Genderen/Sterken 1999	58	Sterken et al. 1997a	108	Wisse et al. 1971
9	Feast et al. 1960	59	Kaper et al. 1995	109	de Koter et al. 1993a
10	Stahl et al. 1984a	60	Higgs et al. 1994	110	Hutsemékers et al. 1991
11	Stahl et al. 1985	61	Waters et al. 1996	111	van Genderen et al. 1991
12	Shore et al. 1984	62	Stahl et al. 1990	112	Clampin et al. 1995
13	Muratorio et al. 1988	63	van Genderen et al. 1998b	113	de Winter et al. 1992
14	Zickgraf et al. 1996b	64	Prinja et al. 1991	114	Hu et al. 1990
15	Zickgraf et al. 1986	65	Schild 1987	115	van Genderen et al. 1992a
16	Zickgraf et al. 1985	66	van Leeuwen et al. 1998	116	de Winter 1996
17	Friedjung et al. 1980	67	Zickgraf et al. 1996a	117	Wray 1966
18	Shore 1990	68	McGregor et al. 1988a	118	Henize 1976
19	Shore 1992	69	van Genderen et al. 1985	119	A. Jones et al. 1997
20	Schulte-Ladbeck et al. 1993	70	van Genderen et al. 1997a	120	Weis et al. 1997
21	Allen et al. 1976	71	Lamers 1995	121	McGregor et al. 1988b
22	Crowther et al. 1997	72	Stahl et al. 1982	122	Nota et al. 1997
23	Isserstedt 1975	73	Leitherer et al. 1985	123	Voors et al. 1997
24	Nota et al. 1995a	74	van Genderen 1979b	124	L Smith et al. 1997
25	Nota et al. 1994	75	Martini 1969	125	Whitelock et al. 1983b
26	Crowther et al. 1995	76	de Koter 1993	126	Garcia-Lario et al. 1998
27	Heydari-Malayeri et al. 1997b	77	Sterken et al. 1991	127	Schulte-Ladbeck et al. 1994
28	Vacca et al. 1990	78	Lamers et al. 1998	128	Shore et al. 1996
29	L. Smith et al. 1994	79	Hiltner 1954	129	Davidson et al. 1993
30	Walborn 1982	80	Sterken 1977	130	Henize 1952
31	Schmutz et al. 1991	81	Sterken 1981	131	Stahl 1986
32	Shore et al. 1990	82	Sterken 1976	132	Humphreys 1978
33	Hillier et al. 1998	83	Sterken et al. 1996c	133	Chini et al. 1980
34	Nota et al. 1996a	84	Sterken et al. 1997b	134	Zickgraf 1997
35	Nota et al. 1996b	85	Westerlund 1961	135	Stroud 1997
36	Robberto et al. 1998	86	Clayton et al. 1985	136	Szeifert et al. 1993
37	Hutsemékers et al. 1994	87	van Genderen 1970	137	Sterken et al. 1998
38	van Genderen et al. 1992b	88	Mendoza 1970	138	Venn 1997
39	van Genderen et al. 1996	89	Hiltner 1956	139	Wolf et al. 1981
40	Hofleit 1933	90	Walborn et al. 1991	140	Stahl et al. 1987
41	Hofleit 1940	91	van Genderen et al. 1998a	141	Brunet 1975
42	Lennon et al. 1994	92	Pasquali et al. 1997a	142	Najarro et al. 1997
43	van Genderen et al. 1988	93	Pasquali et al. 1997b	143	Lamers et al. 1983
44	Thackeray 1974	94	Stahl/Wolf 1987	144	Markova et al. 1997
45	van Genderen et al. 1983	95	Stahl et al. 1984a	145	Turner 1985
46	Spoon et al. 1994	96	Lamers et al. 1989	146	de Groot 1969
47	Voors et al. 1999	97	Humphreys et al. 1989	147	de Groot et al. 2001
48	Chentsov et al. 1990	98	Hoekzema et al. 1992	148	van Genderen 1991b
49	Ardeberg et al. 1972	99	Leitherer et al. 1994	149	Meaburn et al. 1996
50	Code et al. 1958	100	Sterken et al. 1996a	150	Lamers et al. 1992

   

Table 15: Continuation of Table 14

No.	Reference	No.	Reference	No.	Reference
151	de Groot et al. 1992	201	Sterken et al. 1995a	251	L. Smith 1997
152	van Gent et al. 1986	202	Innes 1903	252	Skinner 1997
153	Pasquali et al. 1999	203	de Vaucouleurs et al. 1952	253	Sterken et al. 1999c
154	Bohannan et al. 1989	204	Percy et al. 1988	254	Pacheco et al. 1992
155	Weis et al. 1995	205	Whitelock et al. 1983	255	Skinner et al. 1998
156	Weis 1996	206	Whitelock et al. 1994	256	Appenzeller et al. 1987
157	Conti et al. 1986	207	Burki et al. 1982	257	Humphreys et al. 1994
158	Thompson et al. 1982	208	Schild et al. 1969	258	Walborn et al. 1978
159	Schulte 1958	209	Bieging et al. 1989	259	Lester et al. 1986
160	Reddish et al. 1967	210	Miroschnichenko 1996	260	Blöcker et al. 1999
161	Torres-Dodgen et al. 1991	211	van der Veen et al. 1994	261	Oudmaijer et al. 1994
162	Massey et al. 1991	212	Sterken et al. 1997	262	Klochkova et al. 1997
163	Gottlieb et al. 1978	213	Bateson et al. 1994	263	Hoekzema et al. 1993
164	Souza et al. 1980	214	Breysacher 1997	264	Viotti et al. 1988
165	Dufour et al. 1975	215	Breysacher et al. 1991	265	Figer et al. 1998
166	Warren et al. 1975	216	Moffat et al. 1998	266	Catchpole et al. 1990
167	C. Jones et al. 1974	217	Heydari-Malayeri et al. 1997a	267	Cotera et al. 1996
168	van Genderen et al. 1982	218	Koenigsberger et al. 1998b	268	Kaplan et al. 1970
169	Markova et al. 1998	219	Koenigsberger et al. 1998a	269	Hamann et al. 1994
170	van Genderen et al. 1989	220	Barba et al. 1995	270	de Jager 1998
171	Leitherer et al. 1987	221	Barba et al. 1997	271	Massey 2000
172	Subrahmanyari et al. 1993	222	Miroschnichenko et al. 1999	272	Massey et al. 2000
173	Hutsemékers 1997	223	Dong et al. 1991	273	Robberto et al. 1993
174	Leitherer et al. 1997	224	Vakili et al. 1999	274	Menshchikov 1989
175	T. Jones et al. 1993	225	Zickgraf et al. 1989a	275	Pasquali et al. 2000
176	Kastner et al. 1995	226	Zickgraf et al. 1989b	276	Polomski et al. 1999
177	Oudmaijer et al. 1996	227	Azzopardi et al. 1975	277	Sterken et al. 2001
178	van Genderen et al. 1994	228	McGregor et al. 1989	278	Morris et al. 1999
179	Burgarella et al. 1991	229	Shore et al. 1987	279	Weis 1999
180	Pottasch et al. 1976	230	Nota et al. 1995b	280	Langer et al. 1994
181	Davidson/Humphreys 1997	231	van Genderen/Sterken 2001	281	Stothers 1999b
182	van Genderen et al. 1984	232	Steemers et al. 1986	282	Bohigas et al. 2000
183	P. Cox et al. 1995	233	Moffat et al. 1977	283	Icke 1981
184	van Genderen et al. 1999	234	Knoechel et al. 1982	284	Nieuwenhuijzen et al. 2000
185	Damineli et al. 1997	235	Carpay et al. 1989	285	Oudmaijer 1998
186	Ebbets et al. 1997	236	Carpay et al. 1991	286	Oudmaijer 1995
187	Sterken et al. 1996b	237	Markova 1986	287	Damineli et al. 2000
188	van Genderen et al. 1995	238	Kolka 1983	288	Davidson et al. 2000
189	Meaburn et al. 1993	239	Israelian et al. 1999	289	N. Smith et al. 2000
190	Hillier et al. 1992	240	Barlow et al. 1994	290	Pantin et al. 2000
191	Viotti et al. 1989	241	Meaburn et al. 1999	291	Voors et al. 2000
192	Sterken et al. 1999a	242	Glover et al. 1997	292	Duschl et al. 1995
193	Damineli 1996	243	Davidson et al. 1999	293	Gäng 2000
194	Allen et al. 1993	244	Smith-Neubig et al. 1999	294	Viotti et al. 1999
195	Stothers et al. 1997	245	Sterken et al. 1999b	295	Corcoran et al. 1999
196	Voors 1999	246	de Groot et al. 1997a	296	Duncan et al. 1999
197	van Genderen 1979a	247	de Groot et al. 1997b	297	Weis 2000
198	Manfroid et al. 1991	248	de Groot et al. 1996b	298	van Genderen et al. 2001
199	Sterken et al. 1993	249	Kolka 1999	299	Walsh et al. 2000
200	Manfroid et al. 1994	250	Nota/Clampin 1997

 

 

Table 16: Overview of the presumable trends of the brightness in the intervals before 1950 and between 1950 and 2000, their amplitudes, the duration of the low stages and the time scales, for 17 S Dor variables

designation	category	brightness/activity		ampl.	$t_{\rm trend}$	$t_{\rm low}$	references
HD/HDE		<1950	1950-2000	(mag)	(yr)	(yr)
160529a	s-a	(high)	high	0.5			Fig. 2
WRA751	s-a	high	low	2	35	10	Fig. 3
R40	s-a	low	high	0.8	35		7,137; Tables 2 and 3
R71b	s-a	high	lowb	1.7	25	15	Fig. 4
R110	s-a	(low)	high	1.1	35		Fig. 5
R116	s-a	high	low	1.2	40	40-70	Fig. 6
R127	s-a	low	high	2.4	20	10	Fig. 7
R143	s-a	high	low	1.4	20	10	Fig. 8
HV5495	s-a	high	low	1.5		( 20)	Fig. 10
P Cygc	w-a		low			$\sim$300	147,150,151
168607	w-a	low	high	0.7	55		38,66,80,253;
							Tables 5 and 6
R81	w-a	high	low	0.9	70	50	Fig. 12
R123	w-a	high	low	1.2	50	20	Fig. 15
$\zeta^{1}$ Sco	ex/d	high	low	2	100	100	58; Tables 9 and 10
168625d	ex/d	low	high	0.8	55		38,66,80,253;
							Tables 9 and 10
He3-519	ex/d	(high)	(low)	(0.5)	( 35)		Tables 9 and 10
S119	ex/d	(high)	(low)	(0.5)	( 45)		Tables 9 and 10

Notes to Table 16:
^a According to Fig. 2, the star is probably active since at least 1890, thus $t_{\rm high}$ $\sim$110yr.
^b The star was also ``high'' between 1970 and 1980, but much less than before 1950. After 1980 and until 1995 the star behaved as a w-a S Dor variable. New observations have been made by Sterken after 1995. The results will be published in due course.
<sup>c</sup> It is unknown whether the ``high'' state in the 17th century was only due to SD-eruptions, or whether also SD-phases were involved.
^d This star seems to be brighter at present (thus, in the interval 1950-2000) than around 1900, but there is no SD-activity detected in the present photometry.

 

 

Table 17: Numbers of S Dor variables in the SMC, LMC and the Galaxy (G)

type	$N_{\rm obs}$SMC	$N_{\rm obs}$LMC	$N_{\rm obs}$G	mult.fa	$N_{\rm tot}$G
s-a	2	8	4	4	16
w-a	0	8	4b	22	66
ex-/d	0	3	5	22	110
cand (+)	1	0	7
Total	3	19	20		192

Notes to Table 17:
^a Adopting for the galactic disk a radius of 12kpc.
^b With the omission of He3-519 (r = (8)kpc), it leaves 3 objects for the computation of $N_{\rm tot}$G.

Figure 2: The schematic light curve (ptm and $V_{\rm J}$) versus JD (panel at the left) and JD-2400000 (panel at the right) of the s-a S Dor variable HD160529 in the Galaxy. Note that the scale after 1950 is 2 1/2 times larger than before 1950

Figure 3: The schematic light curve ($V_{\rm J}$) versus JD-2400000 of the s-a S Dor variable WRA751 in the Galaxy. After 1990 the $\alpha$ Cyg-type microvariations are sketched on scale

Figure 4: The schematic light curve (ptm, ptg and $V_{\rm J}$) versus JD of the s-a S Dor variable R71 in the LMC

Figure 5: The schematic light curve (ptg and $V_{\rm J}$) versus JD-2400000 of the s-a S Dor variable R110 in the LMC

Figure 6: The schematic light curve (ptm, ptg and $V_{\rm J}$) versus JD of the s-a S Dor variable R116 in the LMC. The $\alpha$ Cyg-type microvariations observed in detail after 1990 are sketched on scale

Figure 7: The schematic light curve (ptg and $V_{\rm J}$) versus JD-2400000 of the s-a S Dor variable R127 in the LMC

Figure 8: The schematic light curve (($V_{\rm J}$) versus JD-2400000 of the s-a S Dor variable R143 in the LMC

Figure 9: The schematic light curve (ptg and $V_{\rm J}$) versus JD-2400000 of the s-a S Dor variable HDE269216 in the LMC

Figure 10: The schematic light curve (ptg and $V_{\rm J}$) versus JD-2400000 of the s-a S Dor variable HV5495 in the LMC

Figure 12: The schematic light curve (ptm, ptg and $V_{\rm J}$) versus JD of the w-a S Dor variable R81 in the LMC. The two dotted lines labeled ``max'' and ``min'' represent the ranges of the light curve due to the eclipses of the binary

Figure 14: The schematic light curve (ptg and $V_{\rm J}$) versus JD-2400000 showing an L-SD cycle of the w-a S Dor variable R99 in the LMC. The two horizontal line pieces at the right represent the ranges of the $\alpha$ Cyg-type microvariations of which the averages are indicated by the dots

Figure 15: The schematic light curve (ptm and $V_{\rm J}$) versus JD (panel at the left) and JD-2400000 (panel at the right) of the w-a S Dor variable R123 in the LMC. The low-amplitude S-SD phases around 1990 are schematically indicated on scale. Obviously, the star stopped its strong-activity just after 1900

Figure 17: The schematic light curve (ptg and $V_{\rm J}$) versus JD-2400000 of the w-a S Dor variable HD38489 in the LMC

Figure 18: The magnitude-colour diagram of the w-a S Dor variable HD38489 in the LMC

Figure 19: The schematic light curve ($V_{\rm J}$) versus JD-2440000 of the candidate (-) S Dor/B[e] variable S18 in the SMC based on VBLUW photometry. The cause of the variations is still unknown, but they are certainly no SD-phases