T     Ant    [A/H] = -0.0. P var, nonlinear elements: Max = 2436120.756
T     Ant    + 5.897915d*E + 4.80d*10^{-8}E^2 [00027].
V     Ant    OH, H_2O, SiO maser.
SZ    Ant    From photometry in [00002], about 12.3m V, const? [00000].
TU    Ant    From photometry in [00002], about 10.6m V, const? [00000].
WY    Ant    [Fe/H] = -1.48. P var, nonlinear elements: Max =
WY    Ant    2439139.40 + 0.574330174d*E + 4.820d*10^{-10}E^2 [00029].
AG    Ant    [Fe/H] = -4.8. A post-AGB star. SB1. Brightness variations with
AG    Ant    the orbital period probably due to variations of circumstellar
AG    Ant    extinction.
AI    Ant    Slow variations with Prot (see Table), oscillations with P about
AI    Ant    15 minutes, several frequencies.
R     Ara    Min II 6.2. The light curve shape outside eclipses varies.
R     Ara    VB A (B 8.2m, 4", 123deg, 1933).
S     Ara    [Fe/H] = -0.71. P var. Max = 2420047.2382 + 0.451888176d*E -
S     Ara    1.36d*10**(-10)*E**2 (2414000 - 2441200) [03126]. For current
S     Ara    elements after 2441000, see Table.
T     Ara    VB A (B 11.0m, 34", 60deg).
RW    Ara    Changes of the shape of the light curve due to gaseous streams
RW    Ara    or to a hot spot are possible.
SZ    Ara    P var [00005].
TV    Ara    In the region of the open cluster NGC 6208.
TX    Ara    VB A (B 16.5m 5" sf). A twice shorter period is possible.
AD    Ara    [A/H] = -0.4.
AW    Ara    Before JD 2417300, Max = 2412600 + 186d*E.
BF    Ara    The superoutburst cycle is given.
CC    Ara    VB A (B 14.9m 7" sp).
CT    Ara    Between JD 2420400 and 2425000, Max = 2413080 + 215d:*E.
DU    Ara    P var.
DZ    Ara    VB A (B 12.9m 12" np).
EH    Ara    VB A (B 14.7m 12" nf).
EK    Ara    VB A (B 15m pg 5" s).
FS    Ara    VB A (B 15.1m V 7" nf).
FT    Ara    VB A (B 15.4m 7" nf).
GI    Ara    VB A (B 10" sp). It is not quite clear which star varies.
GK    Ara    The coordinates in [00051] and the chart in [00034] are
GK    Ara    believed to be wrong.
IN    Ara    [Fe/H] = -1.75.
IW    Ara    VB A (B 15.9m 9" sp).
KP    Ara    VB A (B 14.8m 7" p).
KY    Ara    Only one sharp Max (JD2428715 - 721) was observed [00055].
KZ    Ara    VB A (B 13.5m 13" p).
LW    Ara    As of May 2006, erroneously called LX Ara in [00002].
MQ    Ara    VB A (B = NSV 09784 25" sp).
MR    Ara    [Fe/H] = -1.0.
MS    Ara    [Fe/H] = -1.48.
MT    Ara    VB A (B 13.5m 26" sf).
MV    Ara    VB A (B 17.6m 7" nf), a star 13.5m 18" n.
MX    Ara    VB A (B 15.5m 14" sf).
NU    Ara    VB B (A 16.4m 8" sp).
OY    Ara    Eclipsing variations [00010]: amplitude 1.9m (wide B+V filter),
OY    Ara    Min = 2449862.8220 + 0.155466d*E.
QR    Ara    Marked in the chart for BV 1443. ASAS-3 data do not show
QR    Ara    noticeable variations.
QX    Ara    Erroneously called V675 Ara in [00002].
V0340 Ara    [A/H] = 0.6.
V0341 Ara    X-ray source 1RXS J165743.7-631237. V-Ic between 0.08m and
V0341 Ara    0.20m [00012]. The periods 11.95d [00111], 10.919d [00075],
V0341 Ara    14.11045d [00012] satisfy observations only during some
V0341 Ara    intervals of time.
V0342 Ara    P >= 140d.
V0345 Ara    P >= 180d.
V0355 Ara    P > 220d.
V0356 Ara    P > 170d. VB B (A 12.65m B, 22" nf).
V0360 Ara    Min II - Min I = 0.35P.
V0383 Ara    VB A (B 16.5m 8" nf).
V0419 Ara    Not red [00000].
V0422 Ara    According to [00054] and [00053], UG. The spectral type suggests
V0422 Ara    another type [00013].
V0433 Ara    Eclipses: Min = 2453065.5502 + 0.19573d*E [00014]. According to
V0433 Ara    [00014], the outside-eclipse brightness varies between 16.8m
V0433 Ara    and 18.4m V. The faintest magnitude observed in an eclipse was about 19.6m V.
V0447 Ara    Another possible solution of the data from [00002]:
V0447 Ara    Min = 2451936.878 + 18.146d*E [00015].
V0461 Ara    Identified with a bright IR object in the 2MASS catalogue.
V0520 Ara    No objects with Mira-like colors in the field [00000].
V0528 Ara    Not an RR Lyrae star according to [00006], where no period
V0528 Ara    could be found between 0.25d and 2.0d.
V0539 Ara    VB A (B 9.22m, 12", 269deg). DII = 0.13P. Apsidal motion.
V0539 Ara    Tabulated are: the epoch of MinI based on observations in [00075]
V0539 Ara    and the siderial period from [00017]. In 1982 - 1994,
V0539 Ara    MinI = 2445056.777 + 3.169112d*E,
V0539 Ara    MinII = 2445067.825 + 3.169076d*E, U = 150 years. The fainter
V0539 Ara    component of the eclipsing pair pulsates, the detected periods
V0539 Ara    are 1.36d, 1.78d, 1.08d [00017].
V0544 Ara    VB A (B 14.5m pg, 17" sp).
V0577 Ara    The chart in [00059] leads to a much brighter star than the
V0577 Ara    magnitudes in [00059]; for this brighter star, the data in
V0577 Ara    [00002] permit to suspect type EA, Max 13.1m V, MinI 13.6m V,
V0577 Ara    MinII 13.3:m V, MinI = 2453090.826 + 0.6880d*E, with a large
V0577 Ara    light-curve scatter [00000].
V0583 Ara    The chart in [00059] leads to a much brighter star than the
V0583 Ara    magnitudes in [00059].
V0613 Ara    VB B (A = NSV 10198, 12" np).
V0617 Ara    VB B (A 13.1m Bj, 12" nf). Combined magnitudes of the pair are
V0617 Ara    given.
V0624 Ara    MaxII 11.9 at the phase 0.4.
V0639 Ara    V1 (NGC 6397). Cluster non-member.
V0650 Ara    Individual cycles have amplitudes about 0.7m, the mean
V0650 Ara    brightness level varies.
V0658 Ara    The suggested type is in contradiction with the star's red
V0658 Ara    color [00000].
V0710 Ara    Individual cycles have amplitudes from 0.5m to 1m, secondary
V0710 Ara    cycle about 750d.
V0729 Ara    Type RV with a twice longer period is possible.
V0744 Ara    Not red.
V0755 Ara    The chart in [00112] (BV 1310) shows a different variable star.
V0793 Ara    Not red.
V0801 Ara    MXB 1636-53. Description of the spectrum [00113].
V0801 Ara    Modulation with Porb = 0.15804738d [00020], amplitudes up to
V0801 Ara    0.6m V.
V0816 Ara    Type RR: was suggested in [00053], but the star is red.
V0820 Ara    Epoch of Min is given. Strong magnetic field. Either an
V0820 Ara    eclipsing binary or a white-dwarf oblique rotator.
V0821 Ara    4U 1658-48. Complex behavior. Three X-ray states: off, hard-low,
V0821 Ara    high-soft, poorly correlated with optical variations. The latter
V0821 Ara    consist of flickering, possible low-amplitude quasi-periodic
V0821 Ara    variations, and large-amplitude changes. Porb near 0.7d is
V0821 Ara    suspected.
V0825 Ara    V2 (NGC 6397), cluster non-member.
V0826 Ara    V3 (NGC 6397), cluster non-member.
V0827 Ara    V4 (NGC 6397).
V0829 Ara    SR [00114].
V0829 Ara    According to [00075], ELL, 6.06m - 6.14m Hp,
V0829 Ara    Min = 2448504.951 + 7.5010d*E; these type and
V0829 Ara    period seem improbable for the spectral type.
V0832 Ara    Porb = 5200d.
V0834 Ara    Oscillations: P = 12 minutes.
V0835 Ara    Oscillations: P = 10.75 minutes.
V0837 Ara    Associated with a nebula.
V0839 Ara    Associated with a nebula.
S     Tel    The AAVSO chart, approved by Harvard Observatory in 1951,
S     Tel    corresponds to the star at the coordinates in the Table. Most
S     Tel    observations of S Tel reported in the 20th century probably
S     Tel    refer to this star. There remains doubt if the original
S     Tel    CPD-55 9313 was the same star [00126].
U     Tel    P var [00000]. SiO maser.
RR    Tel    A symbiotic Nova. In 1889 - 1930, 12m - 14m pg (according to
RR    Tel    [00123], irregular variations; according to [00128],
RR    Tel    Max = 2411490 + 384d*E, with irregularities). In 1930 - 1944,
RR    Tel    12.5m - 16.5m pg, Max = 2430145 + 386.73d*E [00125]. An outburst
RR    Tel    from 14m to 7m in October, 1944. On JD2441426 - 2444899,
RR    Tel    5.06m - 6.74m J, P = 387d [00124]. The data in [00002] reveal
RR    Tel    current V-band variations with a small amplitude and nearly
RR    Tel    the same period [00000]. A period of 11.38 years, presumably the
RR    Tel    orbital one, was reported in [00127]. The spectrum in the Max of
RR    Tel    the outburst was F5 without emissions, then a rich emission
RR    Tel    spectrum was formed. Since the 1970s, TiO absorption bands are
RR    Tel    being noted. Radio source, soft X-ray source.
RS    Tel    Semiregular variations, P = 49.0d [00002].
RV    Tel    VB (0.6", 294deg, 1946).
SS    Tel    SiO maser.
ST    Tel    The chart in [00034] is wrong.
SU    Tel    VB B (A 13.6m B, 12" nf).
TY    Tel    OH, SiO maser.
UY    Tel    VB.
YY    Tel    No emission lines in the spectrum.
AG    Tel    VB A (B 13.7m B, 20" sp).
AN    Tel    A secondary period about 27d.
AX    Tel    [A/H] = -0.7.
BB    Tel    Not red [00000].
BI    Tel    [Fe/H] = -1.96.
BL    Tel    [Fe/H] = -0.66. The depth of Min II is about 0.1m. The primary
BL    Tel    component varies approximately between 7.09m and 7.27m V,
BL    Tel    the periods revealed in these pulastins are 92.5d and 64.8d
BL    Tel    [00138].
BO    Tel    [A/H] = -0.3.
CK    Tel    VB B (A 15.0m, 12" s).
DZ    Tel    VB A (B 15.9m, 15" np).
EH    Tel    VB A (B 15.6m R, 5" nf).
EU    Tel    The chart in [00034] is wrong.
FX    Tel    VB (4").
GM    Tel    VB A (B 16.6m, 10" p).
HH    Tel    [Fe/H] = -1.02.
HR    Tel    Type EW with a twice longer period is possible.
HY    Tel    [Fe/H] = -0.17.
KK    Tel    Porb = 0.08453d.
KN    Tel    VB A (B 15.6m B, 13" sf).
LW    Tel    Possibly identical to NSV 10695.
MT    Tel    [Fe/H] = -1.85.
NS    Tel    Strong O'Connell effect.
PS    Tel    V39 (NGC 6584). Cluster non-member?
PS    Tel    P = 0.1422d or 0.1657d is possible.
PT    Tel    V27 (NGC 6584). Cluster non-member.
PU    Tel    V24 (NGC 6584). Cluster non-member.
PV    Tel    SB2.
PX    Tel    V15 (NGC 6584). Cluster non-member.
PZ    Tel    SB2.
QR    Tel    P(osc) = 13.0 min.
QS    Tel    Porb = 0.097187d.
QU    Tel    Multiperiodic, P = 257s is dominant.
QZ    Tel    VB B (A 9" sp). The variability is probably due to the fainter
QZ    Tel    (B) component [00075]. The variability range for combined light
QZ    Tel    is given.
V0340 Tel    The data from [00002] do not confirm the tabulated period
V0340 Tel    [00000].
V0343 Tel    O'Connell effect, MaxII 9.18m.
V0349 Tel    Multiperiodic, P2 = 1.2719d.