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arXiv:astro-ph/0302399v1 19 Feb 2003
Radial Velocity Studies of Close Binary Stars. VIII1
Slavek M. Rucinski, Christopher C. Capobianco2
, Wenxian Lu3
, Heide DeBond, J. R. Thomson,
Stefan W. Mochnacki, R. Melvin Blake
David Dunlap Observatory, University of Toronto
P.O.Box 360, Richmond Hill, Ontario, Canada L4C 4Y6
(rucinski,capobian,lu,debond,jthomson,mochnacki,blake)@astro.utoronto.ca
and
Waldemar Og loza
Mt. Suhora Observatory of the Pedagogical University
ul. Podchora˙zych 2, 30-084 Cracow, Poland
ogloza@ap.krakow.pl
and
Greg Stachowski
Copernicus Astronomical Center, Bartycka 18, 00–716 Warszawa, Poland
gss@camk.edu.pl
and
P. Rogoziecki
Adam Mickiewicz University Observatory, S loneczna 36, 60–286 Pozna´n, Poland
progoz@moon.astro.amu.edu.pl
ABSTRACT
Radial-velocity measurements and sine-curve fits to the orbital velocity variations
are presented for the seventh set of ten close binary systems: V410 Aur, V523 Cas,
QW Gem, V921 Her, V2357 Oph, V1130 Tau, HN UMa, HX UMa, HD 93917, NSV 223.
All systems, but three (V523 Cas, HD 93917, NSV 223), were discovered photometri-
cally by the Hipparcos mission. All systems are double-lined (SB2) binaries and all,
but the detached, very close system V1130 Tau, are contact binaries. The broadening-
function permitted improvement of the orbital elements for V523 Cas, which was the
only system observed before for radial velocity variations. Spectroscopic/visual com-
panions were detected for V410 Aur and HX UMa. Several of the studied systems are
prime candidates for combined light and radial-velocity synthesis solutions.
– 2 –
Subject headings: stars: close binaries - stars: eclipsing binaries – stars: variable stars
1. INTRODUCTION
This paper is a continuation in a series of papers of radial-velocity studies of close binary stars
(Lu & Rucinski 1999; Rucinski & Lu 1999; Rucinski et al. 2000; Lu et al. 2001; Rucinski et al. 2001,
2002a) and presents data for the seventh group of ten close binary stars observed at the David
Dunlap Observatory. Selection of the targets is quasi-random: At a given time, we observe a few
dozen close binary systems with periods shorter than one day, brighter than 11 magnitude and
with declinations >−20◦; we publish the results in groups of ten systems as soon as reasonable
orbital elements are obtained from measurements evenly distributed in orbital phases. For technical
details and conventions, and for preliminary estimates of errors and uncertainties, see the interim
summary paper Rucinski (2002b, Paper VII).
This paper is structured in the same way as the previous papers in that most of the data for
the observed binaries are in two tables consisting of the radial-velocity measurements (Table 1) and
their sine-curve solutions (Table 2). Section 2 of the paper contains brief summaries of previous
studies for individual systems and comments on the new data. Figures 1 – 3 show the radial velocity
data and solutions. While in the previous papers we showed only some most interesting broadening
functions (BF), Figure 4 in this paper shows the BF’s for all systems; the functions have been
selected from among the best defined ones around the orbital phase of 0.25.
The observations reported in this paper have been collected between March 2000 and April
2002; the ranges of dates for individual systems can be found in Table 1. All systems discussed in
this paper, except V523 Cas, have been observed for radial-velocity variations for the first time. We
have derived the radial velocities in the same way as described in previous papers; see Paper VII for
a discussion of the broadening-function approach used in the derivation of the radial-velocity orbit
parameters: the amplitudes, Ki, the center-of-mass velocity, V0, and the time-of-eclipse epoch, T0.
The data in Table 2 are organized in the same manner as in previous papers. In addition to
the parameters of spectroscopic orbits, the table provides information about the relation between
the spectroscopically observed epoch of the primary-eclipse T0and the recent photometric deter-
minations in the form of the O−Cdeviations for the number of elapsed periods E. It also contains
our new spectral classifications of the program objects.
1Based on the data obtained at the David Dunlap Observatory, University of Toronto.
2Current address: Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, STN CSC,
Victoria BC, V8W 3P6, Canada
3Current address: Dept. of Geography and Meteorology and Dept. of Physics and Astronomy, Valparaiso Univer-
sity, Valparaiso, IN 46383
– 3 –
2. RESULTS FOR INDIVIDUAL SYSTEMS
2.1. V410 Aur
V410 Aur was discovered by the Hipparcos satellite. The somewhat sparsely covered Hipparcos
light curve is rather typical for a W UMa-type system; it has an amplitude of about 0.33 mag.
Total eclipses are entirely possible, given the large semi-amplitudes Kiof our solution, suggesting
an orbital inclination i≃90 degrees. The system is a spectroscopic triple, with the third component
having the relative brightness of L3/(L1+L2) = 0.26 ±0.01. The photometric amplitude corrected
for the third light is 0.43 mag, which actually is large and inconsistent with the the mass-ratio
qsp = 0.14; the maximum amplitude for the inclination of i= 90 degrees is expected to be around
0.33 – 0.38 mag. (Rucinski 2001).
The individual velocities of the third component did not show any trace of a “cross-talk” (i.e.
did not correlate with the binary phase) although the third-star peak in the broadening function was
strong and always projected into the broadening function signature of the primary component (see
Figure 4) making the orbital solution somewhat poorer than for similar systems without companions
(see Figure 1). The radial velocity observations of the third component are given in Table 3. Our
observations were made in two groups, around HJD 2,451,870 and HJD 2,452,280. The average
velocities of the third component for these groups were V3= 48.38 ±0.30 km s−1and 43.90 ±0.43
km s−1; both differ significantly from the mean velocity of the close binary, V0= 36.94 ±3.10
km s−1. Unfortunately, we do not have enough observations and they are not accurate enough to
check if the difference in the average V3is reflected in a change of the binary center-of-mass velocity
V0; our solution for the binary uses one constant value for V0.
The orbital ephemeris based on the Hipparcos data shows a large O−Cdeviation of 0.10 days.
We arbitrarily reduced the O−Cby shifting the time of the primary eclipse by that amount under
an assumption that V410 Aur is a contact binary of the A type (i.e. that the hotter component is
the more massive one).
The third body in the system was probably the reason for a large error in the Hipparcos
parallax, 4.77±5.39 mas, so that we have no distance estimate for the system. There is a discrepancy
between the Vmax estimated from the Hipparcos HP= 9.98 and from the Tycho–2 (Hog et al. 2000)
photometry, Vmax = 10.18 (transformed from VT). Our estimate of the spectral type, G0/2V, is
consistent with the average (B−V) = 0.56 from Tycho–2.
2.2. V523 Cas
V523 Cas is the only system in this group which was observed spectroscopically before our
observations (Milone et al. 1985). The system is an interesting one because – with its very short
orbital period of 0.237 days, right next to CC Com at 0.221 days – it is very close to the still-
unexplained abrupt cutoff in the orbital period distribution of contact binaries. Several photometric
– 4 –
studies of V523 Cas have been recently rediscussed by Lister et al. (2000) where all previous
references are given. The photometric solutions encountered the common problem of a featureless
light curve poorly constraining the geometrical parameters, with the crucial parameter of the mass
ratio taking a large range of values, with the photometric ones usually above the value determined
by Milone et al. of qsp = 0.42 ±0.02.
Our radial velocity results are well defined (Figure 1). The broadening function (Figure 4)
very clearly shows the more compact and slightly hotter (or having a higher surface brightness)
less-massive component. The disparity of the component shapes is quite striking in the broadening
function; it seems as if the secondary were a detached component (but still quite large) in a semi-
detached binary. Our spectroscopic mass ratio, qsp = 0.516 ±0.008, is very close to the photometric
value determined most recently by Lister et al. (2000), qph = 0.53 ±0.02, hopefully ending the long
dispute about the qsp versus qph disparity (Maceroni 1986).
The ephemeris used to phase the observations was based on two sources: The period, as given
in Table 2, is from Nelson (2001) while the initial epoch, T0= 2,451,822.4267, was taken from
Pribulla et al. (2001).
V523 Cas does not have a trigonometric parallax and was apparently too faint to be included
in the Tycho–2 project. Thus, we refrain from a full discussion of its parameters, noting only that
our spectral type, K4V, confirms previous classifications and agrees with (B−V) = 1.07 measured
by Bradstreet (1981); in that work Vmax = 10.59. The (extrapolated) calibration of Rucinski &
Duerbeck (1997, RD97) gives MV= 6.15 so that V523 Cas is one of the faintest known contact
binaries. This gives a rather small distance to the binary, about 77 pc.
2.3. QW Gem
This contact system has been discovered by Hipparcos. It is somewhat faint for our telescope, so
that the individual broadening functions are noisy, but the orbital solution is well defined (Figure 1).
This contact system is of the W-type when the Hipparcos ephemeris is used; this ephemeris gives
a very small O−Cdeviations. The light curve has a moderately large amplitude of 0.41 mag.
The maximum light brightness, Vmax = 10.3±0.1, is estimated from the transformed HP
data and the Tycho–2 average data; this estimate is very approximate. The Hipparcos parallax
has a large error, 4.09 ±5.42, which may indicate some undiscovered companions or just reflects
the relative faintness of the star. Our spectral type, F8V, is consistent with the Tycho–2 average
(B−V) = 0.48. MV= 3.36 determined from the very uncertain parallax is in agreement with
MV(cal) = 3.55 derived using the RD97 calibration.
– 5 –
2.4. V921 Her
V921 Her is another Hipparcos discovery. This contact system is of the A-type with the more
massive component eclipsed during the deeper minimum. The Hipparcos light curve is well defined,
with an amplitude of 0.36 mag. The system is interesting in that it has a relatively long period of
0.877 days which is rather infrequent among contact binaries. The color index estimated from the
Tycho–2 data, (B−V) = 0.27, points at a spectral type slightly later than our new classification,
A7IV (the SIMBAD type is an even earlier A5), but there may be some interstellar reddening. The
Hipparcos parallax, 2.39 ±0.97 mas and Vmax = 9.37, with an assumption of no reddening, give
MV= 1.3±0.9, which is consistent with the extrapolated RD97 calibration, MV(cal) = 1.1. This
is one of the most luminous contact systems with P < 1 day.
The components are only barely resolved in the broadening function which may indicate a low
orbital inclination (a small sini). The orbit is moderately well defined (Figure 1), partly due to
the early spectral type and dearth of lines; both factors tend to increase the velocity errors. An
interesting feature is a relatively large (in the absolute sense) mean systemic velocity of V0=−79
km s−1; the Hipparcos tangential velocities are small so that the large radial velocity is the main
contributor to the spatial velocity of 81 km s−1.
2.5. V2357 Oph
This variable was discovered by Hipparcos. It was classified as a pulsating star with a period of
0.208 day which is two times shorter than the actual orbital period. The Hipparcos ephemeris was
for the maximum light. Assuming that the Hipparcos initial epoch corresponded to the minimum
just before the maximum used in the ephemeris (T0= 2,448,500.0451), the resulting O−Cis quite
small, see Table 2.
The orbit is only moderately well defined (Figure 2), partly because the system is a bit faint
for our instrumentation, and partly because of the small separation of the components in the
broadening functions. The small radial velocity semi-amplitudes Kiand the small photometric
amplitude of 0.12 mag. are all consistent with the low orbital inclination.
The Hipparcos parallax, 5.37 ±2.01 mas and Vmax = 10.43 lead to MV= 4.08 ±0.82, while
MV(cal) = 4.23 (RD97) for the average (B−V) = 0.80, as indicated by the Tycho–2 data. This
color index is approximately consistent with our spectral type, G5V.
2.6. V1130 Tau
This bright (Vmax = 6.56) system was discovered by Hipparcos. It is the only non-contact
system in this group of ten binaries. The broadening functions are exceptionally well defined and
– 6 –
show (Figure 4) two large, but detached components of similar size and brightness. The mass ratio
resulting from our orbit (Figure 2) is q= 0.919 ±0.008. The photometric variations observed by
Hipparcos define a very nice light curve with rounded maxima, and an amplitude of of 0.38 mag. The
distinction of which component is the hotter one and thus which of the minima should be called the
primary minimum is not well established from the Hipparcos light curve. The broadening functions
show the fainter component eclipsed during the Hipparcos’ primary minimum, which may indicate
that the identification of the eclipses is actually incorrect.
The system begs to be analyzed in detail as it is one of the shortest period detached systems
with the spectral type F3V. This spectral type is in agreement with the average (B−V) = 0.34,
as derived from the Tycho–2 data. The Hipparcos parallax is relatively large (in fact the largest in
this group of binaries) and well determined, 15.35 ±0.78 mas, leading to MV= 2.49 ±0.12. The
contact-binary calibration of RD97 obviously does not apply in this case; we can only note that the
combined brightness corresponds to some 0.6 mag. above the Main Sequence, which simply reflects
the detached binary nature of two similar stars.
We note that (M1+M2) sin3i= 2.41 ±0.03 M⊙for V1130 Tau is relatively large so that the
orbital inclination must be close to 90 degrees.
2.7. HN UMa
Another Hipparcos discovery, HN UMa, is a rather commonly-looking contact system seen at
moderately low orbital inclination because both the photometric variations (0.12 mag.) as well as
the radial velocity semi-amplitudes, Ki, are rather small (Figure 2).
The spectral type of F8V is somewhat early for the average (B−V) = 0.46 derived from
the Tycho–2 data. The Hipparcos parallax, 5.81 ±1.39 mas, with the adopted Vmax = 9.80, give
MV= 3.62±0.53, while MV(cal) = 3.36 (RD97). The proper motion of the system (Tycho–2 data)
is comparatively large, µαcos(δ) = +54.0±1.9 mas and µδ=−36.9±1.8 mas, which together with
V0=−37.1 km s−1results in a relatively large spatial velocity of 65.0 km s−1.
2.8. HX UMa
The variability of HX UMa was discovered by Hipparcos. The light curve is of a typical W UMa-
type system with an amplitude of 0.17 mag. Apparently, the ephemeris of Hipparcos predicts the
photometric minima quite well with a very small O−Cshift; the deeper one corresponds to the
eclipse of the more massive star.
A close companion at the distance of 0.63 arcsec was discovered by Hipparcos. The re-
determination by Fabricius & Makarov (2000) gave an average magnitude difference between the
components of 3.00 mag. in the HPsystem; our determination of a weak third-light peak in the
– 7 –
broadening function gives L3/(L1+L2) = 0.049 ±0.004 or ∆m= 3.27 ±0.10 at the bandpass of
our spectroscopy at 5184 ˚
A. The signature of the third body was just barely detectable (Figure 4)
and, if not for the persistence through the orbital phases of the binary, it could be easily taken for
noise in the broadening function. The radial velocity data for the third component are given in
Table 3. The average velocity, V3=−23.59 ±0.77 km s−1, is slightly different from the center of
mass velocity of the binary, V0=−19.88±0.39 km s−1, but the difference may be of no significance
as we cannot exclude any systematic bias in the measurements of V3on top of the much stronger
feature of the close binary system. We do not see any “cross-talk” in the velocity determinations
in the sense that V3does not depend on the orbital phase of the close binary (see Paper VII for
a discussion of cases when such a dependence is observed). Our observations were made in two
groups, centered on HJD 2,451,697.4 and 2,451,986.9 (see Table 3). We do not see any significant
change in V3between these epochs, with the average values of −22.95 ±1.12 and −24.56 ±1.00
km s−1.
The spectral type, F8V, is consistent with (B−V) = 0.44 derived from the Tycho–2 data. The
Hipparcos parallax is poorly determined, 6.68 ±3.01, possibly reflecting the visual-binary nature
of the system, so it cannot be meaningfully compared with the RD97 calibration which predicts
MV(cal) = 3.32.
It was noted by Bartkevicius & Lazauskaite (1997) that HX UMa is not physically related to
the nearby variable star DP UMa (HD 104513).
2.9. HD 93917
The W UMa-type variability of this star has been recently discovered by Lasala–Garcia (2001);
we used the timing data from that work for the values of T0and P. The amplitude of light
variations is 0.34 mag. so it is rather curious that the variability of this bright (Vmax = 9.02) star
went undetected for such a long time. There are more curious circumstances around this star: It
is one of very few HD stars not observed by the main Hipparcos project (but it was observed by
Tycho–2). Also, there existed a large discrepancy between the (B−V) = 0.55 color index, as given
in the SIMBAD database and confirmed by Tycho–2, and the SIMBAD spectral type of K0. We
found that the spectral type is F9.5V which agrees very well with the color index. The predicted
MV(cal) = 3.35 (RD97) cannot be checked because the Tycho parallax is poor, 14.9±11.4 mas.
Our observations define a very good spectroscopic orbit without any peculiarities (Figure 3).
The system belongs to the W-type of contact binaries, i.e. has a hotter less-massive component.
There is absolutely nothing peculiar in the system except for the very fact that, being so bright,
its variability remained undetected for such a long time. We note that Rucinski (2002c) (Sec. 8 &
12) estimated that even among brights stars within the interval 7.5< V < 8.5, perhaps as many
as 45 contact systems still remain to be discovered.
– 8 –
2.10. NSV 223
The variability of NSV 223 was known since the discovery by Strohmeier et al. (1956). Recently,
Verrot & Van Cauteren (2000) obtained a light curve showing a total, long-duration eclipse in the
secondary minimum, which suggests that the mass ratio is small. Our radial velocity data (Figure 3)
fully confirm these predictions: The contact system is indeed of the A-type and the mass ratio is
small, q= 0.136 ±0.011. The large semi-amplitudes Kisuggest that the orbital inclination is close
to 90 degrees. In spite of those properties promising a very good combined solution, the system
is poorly known. What is known is Vmax = 10.86 from Verrot & Van Cauteren (2000); also our
spectral type is F7V. The ephemeris given by the discoverers holds quite well (see Table 2).
3. SUMMARY
This paper presents radial-velocity data and orbital solutions for the seventh group of ten close
binary systems observed at the David Dunlap Observatory. In this series, only V523 Cas has a
history of previous radial-velocity studies. Seven system were discovered photometrically by the
Hipparcos satellite mission while two binary systems, HD 93917 and NSV 223 have been identified
as contact systems only very recently.
All systems of this group, with the exception of the detached binary V1130 Tau, are contact
binaries of the W UMa type. All systems are double-lined (SB2) binaries with visible spectral lines
of both components. V1130 Tau is interesting one because it is a very close yet detached consisting
of two almost identical F3V stars on a tight orbit with P= 0.799 days. In contrast, the early-type
(A7) contact binary V921 Her has a relatively long period of P= 0.877 days. A bright (9 mag.),
recently discovered contact system HD 93917 is rather inconspicuous in its properties except for
the fact that it remained undiscovered for such a long time; this confirms the prediction that many
close binary systems still remain to be discovered among bright stars. V410 Aur and HX UMa
have fainter companions detected spectroscopically.
Support from the Natural Sciences and Engineering Council of Canada to SMR and SWM is
acknowledged with gratitude.
The research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France
and accessible through the Canadian Astronomy Data Centre, which is operated by the Herzberg
Institute of Astrophysics, National Research Council of Canada.
REFERENCES
Bartkevicius, A. & Lazauskaite, R. 1997, Baltic Astr., 6, 499
– 9 –
Bradstreet, D. H. 1981, AJ, 86, 98
European Space Agency. 1997. The Hipparcos and Tycho Catalogues (ESA SP-1200)(Noordwijk:
ESA) (HIP)
Fabricius, C. & Makarov, V. V. 2000, A&A, 356, 141
Hog, E., Fabricius, C., Makarov, V. V., Urban, S., Corbin, T., Wycoff, G., Bastian, U., Schwek-
endiek, P. & Wicenec, A. 2000, A&A, 355, L27 (TYC2)
Lasala–Garcia, A. 2001, Inf. Bull. Var. Stars, 5075
Lister, T. A., McDermid, R. M. & Hilditch, R. W. 2000, MNRAS, 317, 111
Lu, W., & Rucinski, S. M. 1999, AJ, 118, 515 (Paper I)
Lu, W., Rucinski, S. M. & Ogloza, W. 2001, AJ, 122, 402 (Paper IV)
Maceroni, C. 1986, A&A, 170, 43
Milone, E. F., Hrivnak, B. J. & Fisher, W. A. 1985, AJ, 90, 354
Nelson, R. H. 2001, Inf. Bull. Var. Stars, 5040
Pribulla, T., Vanko, M., Parimucha, S. & Chochol, D. 2001, Inf. Bull. Var. Stars, 5056
Rucinski, S. M 2001, AJ, 122, 1007
Rucinski, S. M 2002b, AJ, 124, 1746 (Paper VII)
Rucinski, S. M 2002c, PASP, 114, 1124
Rucinski, S. M., & Duerbeck, H.W. 1997, PASP, 109, 1340 (RD97)
Rucinski, S. M. & Lu, W. 1999, AJ, 118, 2451 (Paper II)
Rucinski, S. M., Lu, W. & Mochnacki, S. W. 2000, AJ, 120, 1133 (Paper III)
Rucinski, S. M., Lu, W., Mochnacki, S. W., Ogloza, W. & Stachowski, G. 2001, AJ, 122, 1974
(Paper V)
Rucinski, S. M., Lu, W., Capobianco, C. C., Mochnacki, S. W., Blake, R. M., Thomson, J. R.,
Ogloza, W. & Stachowski, G. 2002a, AJ, 124, 1738 (Paper VI)
Strohmeier, W., Kippenhahn, R. & Geyer, E. 1956, Kleine Ver¨off. Remeis–Sternwarte Bamberg,
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Verrot, J. P. & Van Cauteren, P. 2000, Inf. Bull. Var. Stars, 4910
This preprint was prepared with the AAS L
A
T
EX macros v5.0.
– 10 –
Captions to figures:
Fig. 1.— Radial velocities of the systems V410 Aur, V523 Cas, QW Gem and V921 Her are plotted
in individual panels versus the orbital phases. The lines give the respective circular-orbit (sine-
curve) fits to the radial velocities. All four systems are contact binaries. V410 Aur and V921 Her
are A-type contact systems, while V523 Cas and QW Gem are W-type contact system. V410 Aur
has a fainter spectroscopic companion whose presence lowered the quality of the measurements and
of the solution. The circles and triangles in this and the next two figures correspond to components
with velocities V1and V2, as listed in Table 1, respectively. The component eclipsed at the minimum
corresponding to T0(as given in Table 2) is the one which shows negative velocities for the phase
interval 0.0−0.5. The open symbols indicate observations contributing half-weight data in the
solutions. Short marks in the lower parts of the panels show phases of available observations which
were not used in the solutions because of the blending of lines. All panels have the same vertical
range, −350 to +350 km s−1, but the display is vertically shifted for V921 Her.
Fig. 2.— Same as for Figure 1, but with the radial velocity orbits for the systems V2357 Oph,
V1130 Tau, HN UMa and HX UMa. All systems, except V1130 Tau, which is a close detached
system, are contact systems of the A-type. HX UMa has a faint companion.
Fig. 3.— Same as for Figure 1, for the systems HD 93917 and NSV 223. The former is a contact
binary of the W-type, while the latter is of the A-type.
Fig. 4.— The broadening functions (BF’s) for all binary systems of this group, all for orbital
phases around 0.25, as in similar figures in the previous papers. V410 Aur has a well defined slowly
rotating companion. A tiny third-body feature in the broadening function of HX UMa could easily
be taken for a small error fluctuation (as in poorly determined cases of fainter systems, such as
NSV 223), if not for its persistence throughout all the phases.
– 11 –
arXiv:astro-ph/0302399v1 19 Feb 2003
Table 1. DDO observations of the seventh group of ten close
binary systems
HJD–2,400,000 Phase V1∆V1V2∆V2
V410 Aur
51849.7638 0.0961 −2.0−15.0 225.5 22.9
51849.7723 0.1193 −1.7−9.9 248.6 12.9
51849.7810 0.1430 −5.9−9.8 270.9 5.7
51849.7912 0.1710 −16.0−15.9 269.7 −23.7
51849.8002 0.1954 2.3 5.0 328.8 17.1
51849.8088 0.2190 4.8 9.2 338.0 14.9
51849.8198 0.2490 −18.3−13.1 321.1 −7.5
51849.8370 0.2959 3.6 7.1 316.8 0.3
51849.8466 0.3221 7.1 8.0 299.8 0.6
51849.8551 0.3454 −6.3−8.5 242.6 −35.1
51849.8637 0.3687 −2.5b
−8.5 239.7b
−11.5
51849.8746 0.3985 ··· ··· ··· ···
51849.8832 0.4222 ··· ··· ··· ···
51849.8919 0.4458 ··· ··· ··· ···
51849.9016 0.4722 ··· ··· ··· ···
51849.9102 0.4956 ··· ··· ··· ···
51849.9187 0.5189 ··· ··· ··· ···
51849.9298 0.5491 ··· ··· ··· ···
51849.9383 0.5725 ··· ··· ··· ···
51849.9469 0.5959 ··· ··· ··· ···
51872.7055 0.7202 68.7 −9.7−252.4−2.8
51872.7197 0.7590 59.3 −19.7−245.8 8.5
51872.7282 0.7822 60.3 −17.9−232.4 16.4
51872.7386 0.8105 61.5 −14.5−208.7 25.3
51872.7478 0.8356 65.3b
−7.8−183.2b30.5
51872.7582 0.8642 68.4b
−0.3−163.1b19.7
51872.7668 0.8875 ··· ··· ··· ···
51961.5285 0.1807 −6.0−4.8 298.9 −2.5
51988.5247 0.8723 ··· ··· ··· ···
51988.5488 0.9382 ··· ··· ··· ···
51988.5596 0.9678 ··· ··· ··· ···
51988.5724 0.0027 ··· ··· ··· ···
51988.5873 0.0434 ··· ··· ··· ···
52273.6790 0.2595 −3.2 1.9 312.5 −15.6
52273.6912 0.2928 −8.7−5.0 332.8 14.7
52273.7038 0.3271 −7.3−6.9 315.5 20.5
52273.7156 0.3595 −6.7−11.1 291.4 29.1
52273.7281 0.3933 −7.4−18.2 251.2 33.1
52273.7394 0.4243 11.5b
−6.1 228.5b58.0
52273.7518 0.4581 ··· ··· ··· ···
52273.7633 0.4894 ··· ··· ··· ···
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
52273.7766 0.5259 ··· ··· ··· ···
52273.7883 0.5577 ··· ··· ··· ···
52273.7994 0.5880 ··· ··· ··· ···
52273.8164 0.6345 56.1b
−12.3−159.9b21.4
52273.8273 0.6642 62.9b
−10.2−152.5b60.8
52273.8391 0.6965 55.6b
−21.2−172.8b65.6
52273.8504 0.7274 77.8b
−0.8−202.5b49.3
52277.5986 0.9589 ··· ··· ··· ···
52277.6095 0.9886 ··· ··· ··· ···
52277.6212 0.0206 ··· ··· ··· ···
52277.6319 0.0497 ··· ··· ··· ···
52277.6439 0.0824 ··· ··· ··· ···
V523 Cas
51860.4869 0.8524 −86.0a13.9 191.4a5.2
51860.4954 0.8891 −77.7 2.9 166.2 17.3
51860.5040 0.9259 −70.4a
−13.2 136.2a32.8
51860.5145 0.9705 ··· ··· ··· ···
51872.4947 0.2352 119.9 1.3 −229.9 7.6
51872.5018 0.2658 119.5 1.0 −226.9 10.4
51872.5091 0.2969 109.0 −4.8−216.7 11.6
51872.5178 0.3340 97.5 −5.0−196.6 9.8
51872.5341 0.4038 72.9a6.3 −136.3a0.3
52183.5382 0.2274 118.5 0.6 −230.2 5.9
52183.5613 0.3262 93.7 −11.7−209.2 2.8
52183.5724 0.3734 74.6 −9.7−172.5−1.5
52183.5847 0.4260 ··· ··· ··· ···
52183.5955 0.4726 ··· ··· ··· ···
52183.6075 0.5238 ··· ··· ··· ···
52183.6181 0.5693 −69.3a
−15.5 112.3a15.3
52183.6303 0.6215 −96.4−9.8 164.3 3.7
52183.6415 0.6693 −112.2−3.3 205.5 1.7
52183.6549 0.7265 −121.6 1.3 233.8 3.0
52183.6658 0.7734 −125.3−2.4 225.3 −5.6
52183.6784 0.8271 −119.0−8.8 209.4 3.2
52183.6895 0.8748 −98.2−9.5 172.6 8.1
52183.7028 0.9316 −62.7−9.5 131.3a35.6
52183.7138 0.9787 ··· ··· ··· ···
52183.7283 0.0408 ··· ··· ··· ···
52183.7408 0.0942 65.2 −0.1−168.3a
−34.1
52183.7536 0.1491 97.0 1.5 −201.3−8.7
52183.7644 0.1952 112.5 0.5 −225.6−0.9
52183.7768 0.2482 113.6 −5.5−236.8 1.7
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
52183.7884 0.2979 104.1 −9.6−224.4 3.5
52183.8014 0.3534 88.8 −5.5−188.9 1.5
52183.8124 0.4007 72.8a4.3 −150.3a
−9.9
52183.8347 0.4960 · · · · · · · · · · · ·
52183.8465 0.5464 · · · · · · · · · · · ·
52183.8585 0.5978 −86.6a
−13.9 138.5a5.0
52183.8697 0.6460 −95.4 3.7 197.6 12.8
52183.8826 0.7011 −118.3 0.2 219.0 −3.4
52183.8941 0.7502 −133.0−8.8 221.5 −11.9
52183.9065 0.8033 −120.8−3.4 216.2 −4.1
52183.9171 0.8486 −101.1 0.5 187.7a
−1.9
52310.4842 0.4444 · · · · · · · · · · · ·
52310.4950 0.4903 · · · · · · · · · · · ·
52310.5088 0.5494 · · · · · · · · · · · ·
52310.5202 0.5982 −109.0a
−36.0 135.5a1.5
52310.5338 0.6564 −94.8 9.0 205.8a12.0
52310.5448 0.7035 −121.4−2.4 223.1 −0.3
52310.5572 0.7566 −129.3−5.2 231.4 −1.8
52310.5682 0.8038 −106.9 10.4 225.4a5.4
52310.5809 0.8580 −95.8 1.4 183.9 2.8
52310.5921 0.9059 −72.2a
−1.9 157.6a28.6
52346.5305 0.6906 −119.0−3.2 216.8 −0.4
52346.5416 0.7380 −134.7a
−10.8 227.4 a
−5.4
52346.5709 0.8633 −95.6−1.0 182.5 6.4
QW Gem
51634.5372 0.7578 −89.0 1.0 273.9 7.9
51634.5622 0.8277 −78.4 1.3 250.9 15.6
51634.5728 0.8573 −71.1−0.5 225.1 17.0
51634.5850 0.8913 −61.2a
−4.0 195.0a27.0
51634.5956 0.9209 · · · · · · · · · · · ·
51635.5360 0.5468 · · · · · · · · · · · ·
51635.5473 0.5785 · · · · · · · · · · · ·
51635.5612 0.6172 −78.3−17.6 176.8 −1.6
51635.5723 0.6483 −85.6−13.1 210.5 −3.0
51635.5866 0.6881 −87.3−4.0 245.1 −1.2
51635.5988 0.7222 −91.4−2.7 251.7 −10.6
51635.6141 0.7648 −96.4−6.7 255.4 −9.9
51635.6248 0.7949 −88.8a
−2.2 257.8a1.9
51635.6389 0.8343 −82.7−4.8 247.2 17.3
51635.6523 0.8716 −63.6a1.8 205.6a13.4
51964.5223 0.1771 71.1 −7.9−234.8 5.8
51964.5320 0.2041 83.0 −1.6−246.6 10.5
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
51964.5431 0.2351 77.1 −10.7−272.6−5.6
51964.5527 0.2620 77.6 −10.4−263.3 4.2
51964.5656 0.2981 89.5 5.3 −247.6 8.6
51964.5755 0.3255 76.7a
−1.7−235.2a3.6
51964.5866 0.3567 56.6 −12.4−213.9−3.3
51964.5966 0.3846 69.8a11.5 −174.6a3.7
51964.6086 0.4181 ··· ··· ··· ···
51964.6186 0.4460 ··· ··· ··· ···
52273.5855 0.1761 74.0a
−4.8−262.2a
−22.4
52273.5999 0.2161 77.9 −8.3−260.4 1.8
52273.6152 0.2590 87.1 −1.0−263.0 4.8
52273.6293 0.2982 75.7 −8.5−244.9 11.2
52273.6449 0.3419 74.8 1.0 −205.6 19.4
52273.6608 0.3863 62.2a4.6 −178.6a
−2.4
52278.5882 0.1450 83.4 13.9 −230.8−18.8
52278.5990 0.1752 77.6a
−1.0−227.7a11.4
52284.6277 0.0092 ··· ··· ··· ···
52288.7748 0.5890 −50.4a
−2.2 173.7a32.9
V921 Her
51822.4973 0.6757 −35.0−1.9−313.6−31.7
51822.5079 0.6878 −31.6−0.2−324.2−35.1
51822.5196 0.7012 −29.5 0.5 −282.0 13.6
51822.5303 0.7133 −26.7 2.3 −292.7 7.5
51822.5437 0.7286 −31.5−3.5−269.9 34.2
51822.5550 0.7415 −29.3−1.7−310.1−4.2
51822.5679 0.7562 −33.9−6.3−298.4 7.6
51822.5800 0.7700 −33.8−5.8−317.8−13.4
51962.9503 0.7606 −33.4−5.7−297.9 7.8
52002.8190 0.2019 −138.7−10.5 134.1 −3.8
52002.8344 0.2194 −132.8−3.2 134.9 −9.1
52002.8652 0.2546 −135.2−4.8 152.2 4.1
52067.7572 0.2169 −131.3−1.9 143.6 0.3
52067.7682 0.2294 −132.6−2.6 155.0 8.7
52067.7803 0.2432 −129.4 1.0 137.4 −10.6
52067.7924 0.2570 −125.6 4.8 141.5 −6.4
52067.8052 0.2716 −126.9 3.1 149.3 3.3
52067.8160 0.2839 −130.9−1.6 135.8 −7.2
52067.8295 0.2993 −119.7 8.3 140.8 3.5
52067.8402 0.3115 −122.1 4.6 146.4 15.0
52072.7582 0.9169 ··· ··· ··· ···
52072.7899 0.9530 ··· ··· ··· ···
52072.8051 0.9703 ··· ··· ··· ···
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
52073.6553 0.9394 ··· ··· ··· ···
52073.6721 0.9585 ··· ··· ··· ···
52073.7038 0.9946 ··· ··· ··· ···
52073.7214 0.0148 ··· ··· ··· ···
52073.7367 0.0322 ··· ··· ··· ···
52073.7525 0.0501 ··· ··· ··· ···
52073.7854 0.0877 ··· ··· ··· ···
52076.6451 0.3471 −112.4b8.9 138.6b31.5
52076.6603 0.3644 −120.8b
−3.1 145.5b53.5
52076.6910 0.3994 −110.5b
−1.1 123.5b68.3
52076.7065 0.4170 ··· ··· ··· ···
52128.5900 0.5526 ··· ··· ··· ···
52128.6054 0.5702 ··· ··· ··· ···
52128.6215 0.5885 −54.9b
−3.0−272.9b
−73.9
52128.6370 0.6061 −44.5b2.7 −259.8b
−40.3
52128.6522 0.6235 ··· ··· ··· ···
52136.5652 0.6425 −43.7b
−4.8−294.9b
−38.6
52136.5760 0.6549 −31.7 4.8 −252.7 14.1
52136.5881 0.6687 −30.8 3.4 −270.5 6.7
52136.5990 0.6810 −29.1 3.2 −302.7−17.4
52136.6116 0.6954 −28.9 1.7 −282.8 10.2
52136.6225 0.7078 −26.9 2.5 −303.4−5.2
52136.6354 0.7225 −26.7 1.7 −304.0−1.2
52136.6469 0.7356 −31.0−3.2−301.5 3.8
52136.6600 0.7505 −23.2 4.4 −297.3 8.9
52136.6718 0.7640 −28.8−1.0−300.4 4.9
52136.6840 0.7780 −29.7−1.3−283.8 18.9
52136.6949 0.7903 −31.4−2.2−303.5−4.5
52136.7107 0.8083 −26.5 4.5 −293.6−2.4
52136.7260 0.8258 −29.9 3.4 −299.3−18.4
V2357 Oph
51717.6065 0.5778 ··· ··· ··· ···
51717.6172 0.6036 ··· ··· ··· ···
51717.6295 0.6331 ··· ··· ··· ···
51717.6404 0.6593 12.5 −5.6−177.9 1.9
51717.6534 0.6906 9.8 −12.1−195.6 1.4
51717.6640 0.7162 7.8 −16.2−204.6 1.2
51717.6759 0.7448 18.2 −6.8−200.7 9.3
51717.6866 0.7704 18.2 −6.4−197.6 10.9
51717.7000 0.8026 18.9 −3.7−193.7 6.0
51717.7107 0.8284 9.7 −10.1−190.3−2.9
51717.7581 0.9426 ··· ··· ··· ···
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
51717.7699 0.9709 ··· ··· ··· ···
51717.7806 0.9966 ··· ··· ··· ···
51773.5672 0.2384 −68.0a
−4.9 175.4a4.1
51773.6245 0.3764 −53.1a
−3.0··· ···
51785.5732 0.1292 −62.9−11.8··· ···
51793.5581 0.3434 −62.8a
−7.0··· ···
51793.5692 0.3701 ··· ··· ··· ···
51793.5813 0.3994 ··· ··· ··· ···
51793.5926 0.4266 ··· ··· ··· ···
51793.6071 0.4614 ··· ··· ··· ···
51793.6179 0.4875 ··· ··· ··· ···
51806.5195 0.5330 ··· ··· ··· ···
51806.5314 0.5618 ··· ··· ··· ···
51806.5453 0.5953 ··· ··· ··· ···
52039.7951 0.8747 ··· ··· ··· ···
52039.8188 0.9318 ··· ··· ··· ···
52039.8343 0.9690 ··· ··· ··· ···
52039.8450 0.9949 ··· ··· ··· ···
52039.8575 0.0249 ··· ··· ··· ···
52039.8687 0.0518 ··· ··· ··· ···
52123.5806 0.4915 ··· ··· ··· ···
52123.5978 0.5328 ··· ··· ··· ···
52129.5817 0.9323 ··· ··· ··· ···
52129.6083 0.9963 ··· ··· ··· ···
52130.6155 0.4199 ··· ··· ··· ···
52347.8115 0.0684 ··· ··· ··· ···
52347.8224 0.0947 ··· ··· ··· ···
52347.8343 0.1232 −56.6−6.6 123.7a9.3
52361.7795 0.6804 19.6 −1.2−193.3−1.2
52361.7967 0.7218 24.8 0.5 −200.6 6.5
52361.8124 0.7595 29.9 5.0 −198.8 10.9
52361.8279 0.7966 19.7 −3.5−193.0 9.0
52361.8434 0.8340 19.9 0.9 −175.5 8.6
52361.8595 0.8727 ··· ··· ··· ···
52361.8755 0.9114 ··· ··· ··· ···
52382.7577 0.1610 −60.9−4.4 138.1a
−4.6
52382.7683 0.1867 −69.1−9.3 169.8 12.9
52382.7800 0.2147 −64.3−2.2 186.0a18.9
52382.7907 0.2405 −65.1−1.9 171.6 0.1
52382.8027 0.2693 −64.3−1.4 187.1 16.7
52382.8134 0.2950 −65.2−3.7 177.4a13.2
52382.8260 0.3255 −65.1−6.8 173.4 22.6
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
52382.8372 0.3524 −69.4−15.0 139.5a5.8
52382.8505 0.3843 −46.4a2.0 ··· ···
52382.8622 0.4126 ··· ··· ··· ···
V1130 Tau
51870.6818 0.9346 ··· ··· ··· ···
51870.6889 0.9435 ··· ··· ··· ···
51870.6964 0.9530 ··· ··· ··· ···
51920.4691 0.2567 ··· ··· ··· ···
51920.4853 0.2770 134.0 1.7 −164.2 6.3
51920.5010 0.2966 131.2 3.0 −163.4 2.7
51920.5173 0.3171 125.5 3.9 −156.1 2.7
51920.5337 0.3376 117.5 4.8 −148.2 1.0
51920.5504 0.3586 105.7 4.2 −137.6−0.5
51920.5656 0.3775 95.3 5.6 −126.6−2.5
51920.5828 0.3991 81.0 6.5 −111.7−4.1
51920.5994 0.4199 65.3 7.1 −95.8−5.8
51920.6157 0.4403 ··· ··· ··· ···
51920.6313 0.4598 ··· ··· ··· ···
51920.6476 0.4802 ··· ··· ··· ···
51920.6647 0.5015 ··· ··· ··· ···
52283.4936 0.6787 ··· ··· ··· ···
52283.5043 0.6920 −150.6−0.4 132.7 −4.1
52283.5162 0.7070 −153.8 0.8 139.6 −1.9
52283.5271 0.7206 −157.3 0.1 139.9 −4.7
52283.5397 0.7364 −159.5−0.1 142.2 −4.6
52283.5503 0.7497 −159.7 0.2 143.3 −4.1
52283.5622 0.7645 −160.4−1.0 142.9 −3.8
52284.5482 0.9988 ··· ··· ··· ···
52284.6414 0.1154 ··· ··· ··· ···
52284.6519 0.1286 92.2 −1.5−138.0−9.5
52284.6643 0.1441 102.3 −0.8−147.1−8.4
52284.6764 0.1592 111.9 0.7 −153.1−5.6
52284.6882 0.1741 118.4 0.4 −157.8−2.8
52284.6954 0.1831 120.3 −1.4−158.8 0.1
52303.4750 0.6907 −147.5 2.4 136.9 0.5
52303.4908 0.7106 −149.5 6.0 141.6 −0.8
52303.5056 0.7290 −152.0 6.7 142.8 −3.2
52303.5397 0.7718 −152.0 6.6 145.8 −0.1
52303.5562 0.7924 −151.4 3.4 140.6 −1.1
52303.5714 0.8114 −144.7 4.4 135.7 0.1
52303.5870 0.8309 −140.0 1.3 132.1 5.0
52303.6021 0.8498 −133.1−1.2 120.4 3.4
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
52303.6170 0.8685 −124.7−3.7 102.1 −2.9
52317.4927 0.2377 132.4 −1.6−173.4−1.0
52317.5034 0.2511 132.7 −1.8−171.2 1.6
52317.5158 0.2666 133.2 −0.5−169.0 3.0
52317.5272 0.2808 129.9 −1.9−167.9 2.0
52324.4900 0.9966 ··· ··· ··· ···
52324.5059 0.0165 ··· ··· ··· ···
52324.5212 0.0357 ··· ··· ··· ···
52324.5366 0.0550 ··· ··· ··· ···
52324.5521 0.0743 ··· ··· ··· ···
52324.5676 0.0938 70.1 1.0 −113.8−12.1
52324.5841 0.1144 85.1 1.0 −122.7−4.5
52324.6006 0.1350 100.5 2.8 −135.1−2.2
52324.6147 0.1527 111.9 4.1 −144.6−0.7
HN UMa
52030.5778 0.3444 −56.9 4.8 135.2 −3.7
52030.5885 0.3722 ··· ··· ··· ···
52030.6006 0.4041 ··· ··· ··· ···
52030.6115 0.4324 ··· ··· ··· ···
52030.6241 0.4655 ··· ··· ··· ···
52030.6348 0.4934 ··· ··· ··· ···
52030.6469 0.5250 ··· ··· ··· ···
52030.6580 0.5540 ··· ··· ··· ···
52030.6699 0.5851 ··· ··· ··· ···
52030.6824 0.6177 ··· ··· ··· ···
52030.6930 0.6456 −14.5−0.9−211.4−6.1
52030.7059 0.6793 −7.8 2.6 −223.3 5.4
52030.7166 0.7073 −9.7−1.2−245.6−3.8
52030.7290 0.7395 −6.5 1.0 −243.0 5.8
52030.7399 0.7682 −10.1−2.5−250.2−2.2
52030.7518 0.7991 −6.5 2.3 −242.0−2.7
52030.7629 0.8282 −6.9 4.1 −224.9−0.7
52059.5861 0.1617 −61.6 0.7 148.3 5.0
52059.5974 0.1912 −67.3−2.5 160.2 −0.6
52059.6096 0.2231 −70.2−3.8 168.0 −4.1
52059.6202 0.2508 −63.6 3.1 174.5 −0.6
52059.6323 0.2825 −60.7 5.5 176.1 5.4
52065.6223 0.9382 ··· ··· ··· ···
52065.6341 0.9689 ··· ··· ··· ···
52065.6458 0.9996 ··· ··· ··· ···
52065.6566 0.0276 ··· ··· ··· ···
52065.6695 0.0614 ··· ··· ··· ···
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
52065.6803 0.0898 ··· ··· ··· ···
52067.5943 0.0922 ··· ··· ··· ···
52067.6054 0.1212 −58.2−0.6 105.2 −4.1
52067.6176 0.1530 −66.3−4.9 130.9 −6.0
52067.6284 0.1814 −65.9−1.8 157.8 2.1
52067.6414 0.2154 −68.4−2.4 153.5b
−16.6
52067.6525 0.2442 −65.8 1.0 179.7 4.8
52067.6640 0.2745 −61.3 5.1 173.3 0.7
52067.6749 0.3028 −64.9 0.3 160.0 −3.5
HX UMa
51673.6361 0.2920 −77.0 1.5 169.6 −12.5
51673.6461 0.3185 −74.0 1.2 151.8 −18.4
51673.6541 0.3394 −73.3−2.0 141.9 −15.2
51673.6624 0.3615 −58.4 8.0 147.6 7.5
51673.6697 0.3807 −52.1b9.2 155.0b32.3
51673.6769 0.3997 ··· ··· ··· ···
51673.6866 0.4253 ··· ··· ··· ···
51673.6937 0.4441 ··· ··· ··· ···
51673.7009 0.4630 ··· ··· ··· ···
51702.5973 0.6755 33.7 −0.7−207.7−1.1
51702.6061 0.6985 43.6 5.8 −218.1 0.1
51702.6147 0.7213 44.0 4.1 −219.2 6.5
51702.6248 0.7478 44.8 3.9 −229.0 0.0
51702.6564 0.8314 37.2 4.1 −208.7−6.4
51702.6652 0.8545 27.0 −1.3−195.1−9.6
51702.6741 0.8779 13.0b
−9.3−188.4b
−23.3
51702.6836 0.9031 ··· ··· ··· ···
51702.6922 0.9257 ··· ··· ··· ···
51704.6615 0.1198 ··· ··· ··· ···
51704.6723 0.1482 −64.5 4.1 155.5 7.6
51704.6848 0.1811 −58.2 16.8 173.3 3.3
51704.6946 0.2070 −74.7 3.8 190.9 9.1
51964.6466 0.8138 43.7 7.6 −219.4−7.0
51964.6550 0.8362 40.2 8.0 −207.6−8.5
51991.6568 0.0515 ··· ··· ··· ···
51991.6685 0.0825 ··· ··· ··· ···
51991.6834 0.1219 ··· ··· ··· ···
51991.6955 0.1536 −63.8 6.1 152.3 0.2
51991.7105 0.1932 −76.3 0.6 175.6 −0.5
51991.7222 0.2240 −81.3−1.4 185.9 −0.6
51991.7342 0.2557 −87.8−7.2 173.9 −15.2
51991.7451 0.2844 −80.1−0.8 190.9 6.5
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
51994.8330 0.4287 ··· ··· ··· ···
51994.8438 0.4570 ··· ··· ··· ···
51994.8562 0.4899 ··· ··· ··· ···
51994.8755 0.5407 ··· ··· ··· ···
51994.8875 0.5724 ··· ··· ··· ···
51994.8990 0.6026 ··· ··· ··· ···
51994.9114 0.6353 6.6b
−19.2−192.2b
−15.1
51994.9224 0.6645 29.8b
−2.5−203.5b
−3.9
HD 93917
52361.5642 0.5677 ··· ··· ··· ···
52361.5753 0.5928 ··· ··· ··· ···
52361.5886 0.6227 −27.3 7.1 194.6 11.7
52361.5999 0.6482 −43.0−0.8 205.7 −2.2
52361.6126 0.6769 −53.3−4.2 231.4 1.2
52361.6234 0.7013 −54.4−1.0 243.7 −0.1
52361.6368 0.7314 −58.3−1.9 251.5 −1.6
52361.6481 0.7569 −58.7−1.9 249.3 −5.2
52361.6622 0.7887 −55.7−1.0 247.2 −0.6
52361.6730 0.8130 −57.9−6.8 236.7 0.3
52361.6860 0.8423 −52.3−7.5 215.3 −0.6
52361.6976 0.8686 −42.9−5.7 203.8 11.9
52361.7110 0.8988 ··· ··· ··· ···
52361.7217 0.9229 ··· ··· ··· ···
52361.7353 0.9535 ··· ··· ··· ···
52361.7469 0.9796 ··· ··· ··· ···
52368.6321 0.5072 ··· ··· ··· ···
52368.6430 0.5318 ··· ··· ··· ···
52368.6576 0.5646 ··· ··· ··· ···
52368.6690 0.5904 ··· ··· ··· ···
52368.6815 0.6186 −30.5 2.4 189.2 10.8
52368.6931 0.6447 −40.5 0.6 210.5 5.9
52368.7056 0.6729 −53.9−5.5 218.9 −8.6
52368.7160 0.6965 −50.5 2.2 240.8 −0.7
52369.6232 0.7423 −49.9 6.9 247.6 −6.9
52369.6526 0.8086 −55.0−3.1 246.5 7.6
52369.6633 0.8328 −53.2−6.2 228.7 5.3
52369.6753 0.8597 −41.3−1.4 206.6 6.0
52369.6861 0.8841 −33.7−1.7 178.4 3.0
52369.6988 0.9129 ··· ··· ··· ···
52369.7103 0.9387 ··· ··· ··· ···
52369.7225 0.9662 ··· ··· ··· ···
52369.7314 0.9864 ··· ··· ··· ···
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
52375.5337 0.0716 ··· ··· ··· ···
52375.5446 0.0963 ··· ··· ··· ···
52375.5565 0.1230 63.6 −5.7−159.4−11.2
52375.5674 0.1476 74.5 −2.4−176.2−3.8
52375.5777 0.1709 81.3 −1.5−186.4 4.7
52387.5687 0.2129 87.5 −2.3−208.5 5.0
52387.5796 0.2375 85.6 −6.0−216.5 2.6
52387.5915 0.2643 87.1 −4.4−209.6 9.3
52387.6024 0.2889 84.4 −5.2−205.2 7.6
52387.6156 0.3187 83.3 −1.7−193.4 4.7
52387.6265 0.3433 79.2 −0.2−176.8 3.4
52387.6384 0.3701 72.1 0.5 −156.5−1.1
52387.6493 0.3946 ··· ··· ··· ···
52387.6612 0.4216 ··· ··· ··· ···
NSV 223
51804.6324 0.5317 ··· ··· ··· ···
51804.6595 0.6059 ··· ··· ··· ···
51805.5906 0.1489 −55.0−0.8 202.5 −15.8
51805.6057 0.1900 −76.1−16.9 267.0 11.6
51805.6210 0.2320 −63.1−1.4 271.7 −2.7
51805.6363 0.2736 −60.1 1.5 290.7 17.6
51805.6535 0.3208 −57.0 1.1 252.9 5.6
51805.6694 0.3641 −43.3 8.8 204.1 1.1
51805.6864 0.4105 −55.8b
−12.6 186.8b49.5
51805.7021 0.4534 ··· ··· ··· ···
51805.7185 0.4982 ··· ··· ··· ···
51805.7343 0.5414 ··· ··· ··· ···
51805.7506 0.5859 ··· ··· ··· ···
51805.7694 0.6371 −2.3−11.3−272.9−25.1
51805.7847 0.6789 0.4 −14.3−295.2−4.9
51805.8006 0.7226 ··· ··· ··· ···
51805.8164 0.7657 23.4 4.9 −312.3 5.9
51805.8324 0.8093 25.3 9.4 −294.6 4.6
51805.8478 0.8514 11.1 0.3 −260.0 1.2
51846.4848 0.8427 10.9 −1.2−255.7 14.8
51846.4970 0.8760 ··· ··· ··· ···
51846.5091 0.9089 ··· ··· ··· ···
51846.5198 0.9381 ··· ··· ··· ···
51846.5333 0.9750 ··· ··· ··· ···
51846.5450 0.0071 ··· ··· ··· ···
51846.5562 0.0377 ··· ··· ··· ···
51846.5681 0.0700 ··· ··· ··· ···
Table 1—Continued
HJD–2,400,000 Phase V1∆V1V2∆V2
51846.5789 0.0995 ··· ··· ··· ···
51846.5932 0.1388 ··· ··· ··· ···
51846.6048 0.1705 −70.0b
−12.9 241.4b1.5
51846.6188 0.2086 −54.9b5.8 263.6b
−2.7
51846.6295 0.2379 −81.2b
−19.3 280.2b4.7
51846.6420 0.2719 −65.3b
−3.6 262.8b
−10.7
51846.6528 0.3016 ··· ··· ··· ···
51846.6662 0.3382 −63.4−7.4 229.8 −2.0
51846.6775 0.3689 −54.9b
−3.6 230.6b33.6
51846.6904 0.4041 ··· ··· ··· ···
51846.7010 0.4330 ··· ··· ··· ···
51846.7126 0.4648 ··· ··· ··· ···
51846.7231 0.4936 ··· ··· ··· ···
51846.7345 0.5246 ··· ··· ··· ···
51846.7491 0.5646 ··· ··· ··· ···
51846.7599 0.5941 ··· ··· ··· ···
51846.7721 0.6273 ··· ··· ··· ···
51846.7831 0.6573 0.4 −11.6−245.6 24.9
51846.7969 0.6949 ··· ··· ··· ···
51846.8090 0.7282 36.9b18.6 −332.7b
−15.9
51846.8253 0.7727 ··· ··· ··· ···
51846.8360 0.8019 ··· ··· ··· ···
aThe data given 0.5 weight in the orbital solution.
bThe data given 0.25 weight in the orbital solution.
Note. — Velocities are expressed in km s−1. The deviations ∆Viare relative
to the simple sine-curve fits to the radial velocity data. Observations leading to
entirely unseparable broadening- and correlation-function peaks are marked by
the “no-data” symbol ( ··· ); these observations may be eventually used in more
extensive modeling of broadening functions. The radial velocities designated as
V1correspond to the component which was stronger and easier to measure in the
analysis of the broadening functions; it was not always the component eclipsed
during the primary minimum at the epoch T0(see Table 2). Figures 1 – 3 should
help in identifying which star is which.
arXiv:astro-ph/0302399v1 19 Feb 2003
– 1 –
Table 2. Spectroscopic orbital elements
Name Type Other names V0K1ǫ1T0– 2,400,000 P (days) q
Sp. type K2ǫ2(O–C)(d) [E] (M1+M2) sin3i
V410 Aur EW/A HD 280332 +36.94(3.10) 42.14(3.73) 11.53 52,061.1068(22) 0.366340 0.144(13)
G0/2V HIP 23337 291.68(4.50) 22.19 +0.1060 [9720] 1.42(10)
V523 Cas EW/W −2.54(0.90) 121.64(1.14) 7.82 52,104.0295(4) 0.233693 0.516(7)
K4V 235.95(1.41) 10.37 +0.0027 [1205] 1.110(24)
QW Gem EW/W HD 264672 −0.90(1.39) 89.17(1.84) 7.79 51,961.2357(11) 0.358127 0.334(9)
F8V HIP 32845 267.30(2.52) 12.14 −0.0096 [9664] 1.685(62)
V921 Her EW/A HD 152172 −79.04(1.05) 51.45(0.89) 4.06 51,979.8304(62) 0.877366 0.226(5)
A7IV: HIP 82344 227.17(1.97) 17.37 +0.0718 [3966] 1.971(61)
V2357 Oph EW/A −19.12(1.64) 44.12(1.63) 7.37 52,050.2364(22) 0.415568a0.231(10)
G5V HIP 82967 190.93(2.90) 9.93 −0.0061 [8543] 0.560(32)
V1130 Tau EA HD 24133 −12.74(0.46) 147.21(0.63) 3.39 52,097.6133(11) 0.798871 0.919(7)
F3V HIP 17988 160.11(0.74) 4.26 −0.0218 [4503] 2.408(32)
HN UMa EW/A BD+38◦2220 −37.11(0.63) 29.65(0.76) 3.02 52,049.9590(8) 0.382608 0.140(4)
F8V HIP 55030 212.22(0.96) 4.42 +0.0439 [9278] 0.562(12)
HX UMa EW/A HD 104425 −19.88(1.11) 60.80(1.45) 6.16 51,835.0458(13) 0.379156 0.291(9)
F4V HIP 58648 209.18(2.07) 9.53 −0.0032 [8795] 0.775(30)
HD 93917 EW/W BD−1◦2452b+17.47(0.79) 74.33(0.91) 4.12 52,374.6151(8) 0.443420 0.313(5)
F9.5 237.30(1.32) 6.12 +0.0095 [810] 1.394(30)
NSV 223 EW/A BD+20◦75 −21.66(2.15) 40.39(2.64) 9.02 50,748.8907(18) 0.366128 0.136(10)
F7V 297.98(4.18) 14.43 −0.0053 [2941] 1.47(9)
aV2357 Oph: The period is twice as long as in the Hipparcos catalogue whare the star was classified as pulsating one. The T0has
been adjusted from the maximum to the minimum of light, as described in the text.
bHD 93917: The variability discovery paper gives BD−1◦2448 while SIMBAD gives BD−1◦2452.
Note. — The spectral types given in column two are all new and relate to the combined spectral type of all components in a system.
The convention of naming the binary components in this table is that the more massive star is marked by the subscript “1”, so that the
mass ratio is defined to be always q≤1. Figures 1 – 3 should help identify which component is eclipsed at the primary minimum. The
standard errors of the circular solutions in the table are expressed in units of last decimal places quoted; they are given in parantheses
after each value. The center-of-mass velocities (V0), the velocity amplitudes (Ki) and the standard unit-weight errors of the solutions
(ǫ) are all expressed in km s−1. The spectroscopically determined moments of primary minima are given by T0; the corresponding
(O−C) deviations (in days) have been calculated from the most recent available ephemerides, as given in the text, using the assumed
periods and the number of epochs given by [E]. The values of (M1+M2) sin3iare in the solar mass units.
arXiv:astro-ph/0302399v1 19 Feb 2003
Table 3. Observations of the spectroscopic companions
HJD–2,450,000 Vr
V410 Aur B
1849.7638 46.9
1849.7723 48.7
1849.7810 51.0
1849.7912 50.8
1849.8002 50.6
1849.8088 48.6
1849.8198 49.7
1849.8370 46.9
1849.8466 49.3
1849.8551 48.4
1849.8637 47.2
1849.8746 49.8
1849.8832 48.2
1849.8919 47.2
1849.9016 48.2
1849.9102 48.3
1849.9187 47.3
1849.9298 49.7
1849.9383 47.8
1849.9469 47.6
1872.7055 51.7
1872.7197 46.9
1872.7282 48.3
1872.7386 45.8
1872.7478 47.9
1872.7582 48.5
1872.7668 44.9
1961.5285 46.8
2273.6790 45.2
2273.6912 46.0
2273.7038 44.6
2273.7156 43.3
2273.7281 45.9
2273.7394 42.2
2273.7518 44.6
2273.7633 42.5
2273.7766 42.5
2273.7883 42.7
2273.7994 42.1
2273.8164 41.3
2273.8273 41.0
Table 3—Continued
HJD–2,450,000 Vr
2273.8391 42.9
2273.8504 42.2
2277.5986 45.3
2277.6095 44.0
2277.6212 47.3
2277.6319 48.4
2277.6439 45.9
2277.6548 41.9
2277.6793 43.9
HX UMa B
1673.6541 −15.6
1673.6624 −28.0
1673.6697 −24.0
1702.5973 −27.5
1702.6061 −21.1
1702.6147 −27.2
1702.6248 −24.3
1702.6564 −25.9
1702.6652 −23.2
1702.6741 −19.2
1702.6836 −22.3
1704.6615 −24.6
1704.6723 −14.7
1704.6848 −28.1
1704.6946 −18.5
1964.6466 −24.9
1964.6550 −24.7
1991.6834 −28.4
1991.6955 −26.9
1991.7105 −24.7
1991.7222 −20.4
1991.7342 −27.1
1991.7451 −25.7
1994.8330 −18.0
1994.9224 −24.9
Note. — Radial velocities
are expressed in km s−1.
