ADS | Latest | ![]() | ![]() | ![]() | ![]() | ![]() |
number | orbit | ('') | ('') | (![]() | (![]() | |
434 | Heintz 1995 | 0.440 ![]() | 0.463 | 192.5
![]() | 193.2 | 0.14 ![]() |
1615 | Scardia 1983 |
1.99 ![]() | 1.847 | 276 ![]() | 274.3 | 0.095 ![]() |
1860 | Heintz 1996 | 3.018 ![]() | 2.55 |
231 ![]() | 231.9 | 1.67 ![]() |
Heintz 1996![]() | 2.555 | 231.7 | 1.67 ![]() | |||
2616 | Luyten 1934 | 0.700
![]() | 0.732 | 1 ![]() | 1.328 | - |
Scardia 1985 | 0.640 | 356.5 | ||||
2755AB | Wierzbinsky 1956 | - | 0.118 | - | 83.12 | - |
3358AB | Hartkopf et al. 1996 | 0.245
![]() | 0.258 | 170.0 ![]() | 170.3 | 0.55 ![]() |
3358AC | 0.830 ![]() | 0.713* | 204.0 ![]() | 204.5* | 1.30 ![]() | |
3358BC | 0.585 ![]() | 212.5 ![]() | 0.95 ![]() | |||
3711 | Baize 1969 | 0.76 ![]() | 0.743 | 323 ![]() | 331.3 | - |
3728 | Muller 1963 | - | 0.218 | - | 357.0 | - |
4115 | Siegrist 1951 | 1.090 ![]() | 1.030 | 47.2 ![]() | 40.92 | 1.55 ![]() |
5447 | Baize 1992 | 0.345 ![]() | 0.387 | 218
![]() | 221.1 | - |
5925 | Mourao 1966 |
0.600 ![]() | 0.727 | 281.6 ![]() | 282.5 | - |
7307 | Arend 1953 | 1.017 ![]() | 1.038 | 279.6 ![]() | 281.7 | 0.25 ![]() |
8035 | Couteau 1958 | 0.565 ![]() | 0.623 | 233 ![]() | 240.9 | 1.78 ![]() |
Heintz 1956 | 0.435 | 225.8 | ||||
10360 | Hartkopf et al. 1989 | 0.132 ![]() | 0.138 | 289.3 ![]() | 108.0 | 0.05 ![]() |
12973 | Hartkopf et al. 1989 | 0.226 ![]() | 0.230 |
157.5 ![]() | 157.3 | 0.65 ![]() |
14073 | Hartkopf et al. 1989 | 0.220 ![]() | 0.199 | 287 ![]() | 278.9 | 0.88 ![]() |
14773 | Hartkopf et al. 1996 | 0.270 ![]() | 0.270 |
27.65 ![]() | 27.5 | 0.83 ![]() |
14787 | Heintz 1970 |
0.787 ![]() | 0.733 | 337.8 ![]() | 340.3 | 3.00 ![]() |
15281 | Hartkopf et al. 1989 | 0.086 ![]() | 0.088 | 193.5 ![]() | 199.2 | 0.08 ![]() |
16057 | Heintz 1991 | 0.250 ![]() | 0.255 | 110 ![]() | 111.1 | 0.1 ![]() |
footnotesize 1: 1st orbit given by Heintz.
2: 2nd orbit given by Heintz.
3: Couteau 1958. 4: Heintz 1956
5: Luyten 1934.
Figure 5: Table on the left gives the residuals in separation ()
and position angle (
). Figure on the right is a graphics
visualization of the residuals in a
plane. Each measurement corresponds to a point in the graph. Error bars in
and
have been drawn to scale. For c Her (ADS 10360) the
residual in
has been taken as 1.3
for the plot (instead of
181.3
)
The measurements are summarized in Table 2 (click here). Positions are compared with those computed from the latest available orbits. Orbital elements are from the catalog of Worley & Heintz (1983) and the Sky Catalogue 2000 Vol. 2 for orbits prior to 1984. Recent orbital elements were found on the home page of Pr. W. Heintz (http://laser.swarthmore.edu/html/ research/heintzr.html) and in the literature (references are given in Col. 2).
This paper presents the first extensive application of speckle techniques based on the probability density functions of specklegrams. This method developed at Nice university is well adapted to the data reduction of binary star speckle data. Relative photometry computed this way (cf Sect. 3.4) is found to be consistent with direct image reconstruction from bispectral techniques (cf Sect. 3.5).
The residuals in and
are given in Fig. 5 (click here).
The cloud of points around
validates the
data reduction. It can however be noticed that several stars are found far
from the expected position computed from the latest available orbit. Clearly
some published orbits have to be reconsidered. This is the case for ADS 3711
(orbit estimated in 1969, period P=199y), ADS 4115 (1951, P=586y),
ADS 5925 (1966, P=512y) and ADS 8035 (Couteau Orbit: 1958, P=44.7y (Sky
Cat. 2000) - Heintz orbit: 1956, P=44.4y (Worley & Heintz
1983)).
The stars ADS 5447 and ADS 14073 are also found far from their expected position, although the orbits are quite recent (1989 for ADS 14073, 1992 for ADS 5447). More observations are clearly needed before giving a conclusion.
For the star ADS 2616, we have computed the position from the ephemeris of Luyten (1934) and Scardia (1985). Surprisingly, we found that the 1934 orbit does better fit the observed position.
The case of c Her (ADS 10360) is interesting since we found a residual of
181.3 on the position angle resulting from a confusion between
components A and B. This may occur when the magnitude difference is close to
zero: measurements of c Her available at the CHARA catalog (
http://www.chara.gsu.edu/CHARA/chara.html) show sometimes a 180
uncertainty on
between successive observations. One could object
that our observation was made in the red domain, but the spectral types of
the two stars are identical (A9 IV) (which should be further investigated),
and the brighter star of the couple is the same whatever the color.
ADS 10360 needs to be observed again in several color bands for confirmation
and to check whether the problem comes from a poor observation or a
difference of spectral type of the two binary components.
Acknowledgements
The authors whish to thank the technical staff of the TBL: André Augé, Christian Decha, Pierre Déréthé, Christian Duthu, Francis Laccassagne, Jean-Marie Lavie-Cambo and Christian Lucuix (Observatoire Midi-Pyrénées) for help during the observations; Michel Aurière (Observatoire Midi-Pyrénées) and Institut National des Sciences de l'Univers for financial support. Thanks are also due to Pr. Wulff Heintz for helping in using the orbital elements from his database. This work made use of the SIMBAD astronomical database and of the CHARA 3rd catalogue of interferometric measurements of binary stars.