Issue |
A&A
Volume 506, Number 3, November II 2009
|
|
---|---|---|
Page(s) | 1469 - 1476 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/200911731 | |
Published online | 03 September 2009 |
A&A 506, 1469-1476 (2009)
Extrasolar planets and brown dwarfs around A-F type stars
,![[*]](/icons/foot_motif.png)
VII.
Cygni radial velocity variations: planets or stellar phenomenon?
M. Desort1 - A.-M. Lagrange1 - F. Galland1 - S. Udry2 - G. Montagnier2,1 - H. Beust1 - I. Boisse3 - X. Bonfils1,4 - F. Bouchy3 - X. Delfosse1 - A. Eggenberger1 - D. Ehrenreich1 - T. Forveille1 - G. Hébrard3 - B. Loeillet3,5 - C. Lovis2 - M. Mayor2 - N. Meunier1 - C. Moutou5 - F. Pepe2 - C. Perrier1 - F. Pont6 - D. Queloz2 - N. C. Santos2,4 - D. Ségransan2 - A. Vidal-Madjar3
1 -
Laboratoire d'Astrophysique de Grenoble, UMR5571 CNRS, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France
2 -
Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland
3 - Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre
& Marie Curie, 98bis boulevard Arago, 75014 Paris, France
4 - Centro de Astronomia e Astrofísica da Universidade de Lisboa,
Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa,
Portugal
5 -
Laboratoire d'Astrophysique de Marseille, UMR6110 CNRS, Université de Provence, BP 8, 13376 Marseille Cedex 12, France
6 -
Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
Received 26 January 2009 / Accepted 27 July 2009
Abstract
Aims. In the framework of the search for extrasolar planets and
brown dwarfs around early-type main-sequence stars, we present the
results obtained on the early F-type star Cygni.
Methods. E LODIE and S OPHIE at the Observatoire de
Haute-Provence (OHP) were used to obtain 91 and 162 spectra,
respectively. Our dedicated radial-velocity measurement method was used
to monitor the star's radial velocities over five years. We also used
complementary, high angular resolution and high-contrast images taken
with PUEO at the CFHT.
Results. We show that Cygni radial velocities are quasi-periodically variable, with a
150-day period. These variations are not due to the
0.35-
stellar companion that we detected in imaging at more than 46 AU from the star.
The absence of correlation between the bisector velocity span
variations and the radial velocity variations for this 7 km s
star,
as well as other criteria, indicate that the observed radial velocity
variations do not stem from stellar spots. The observed amplitude of
the bisector velocity span variations also seems to rule out stellar
pulsations. However, we observe a peak in the bisector velocity span
periodogram at the same period as the one found in the radial velocity
periodogram, which indicates a probable link between these radial
velocity variations and the low-amplitude lineshape variations with a
stellar origin. Long-period variations are not expected from this type
of star to our knowledge. If a stellar origin (hence of new type) were
to be confirmed for these long-period radial velocity variations, this
would have several consequences on the search for planets around
main-sequence stars, both in terms of observational strategy and data
analysis.
An alternative explanation for these variable radial velocities is
the presence of at least one planet of a few Jupiter masses orbiting at
less than 1 AU; however, this planet alone does not explain all
observed features, and the Cygni system is obviously more complex than a planetary system with 1 or 2 planets.
Conclusions. The available data do not allow us to distinguish
between these two possible origins. A vigourous follow-up in
spectroscopy and photometry is needed to get a comprehensive view of
the star intrinsic variability and/or its surrounding planetary system.
Key words: techniques: radial velocities - stars: early-type - stars: planetary systems - stars: individual: Cygni
1 Introduction
Radial-velocity (RV) surveys have led to the detection of more than 300 planets
during the past decade. These surveys mainly focus on solar and
later-type main-sequence (hereafter MS) stars (
F7) that exhibit numerous
lines with low rotational broadening, making them ideal targets for classical
velocimetry. However, it is crucial to understand how planetary systems form
over a wide variety of parent stars and to know, in particular, if there is a correlation
between (i) the planet masses and the parent star masses as predicted,
for instance, by Kennedy & Kenyon (2008), in order to constrain formation models such
as those from Ida & Lin (2005) (but also Boss 2006; and
Laughlin et al. 2004 for M dwarfs); and/or between (ii) the planet
existence and the parent star masses. For massive stars, surveys of
subgiant/giant stars have started to provide first information on planets at
orbital distances typically greater than 0.7 AU (e.g., Sato et al. 2008; Johnson et al. 2006; Hatzes et al. 2005; Johnson et al. 2007; Niedzielski et al. 2007; Lovis & Mayor 2007). Closer separations have to be
investigated by observing massive main-sequence stars. In this framework, we
have developed a tool dedicated to searching for planets around early (A-F) type
stars. The method allowing measurement of the RV of rapid rotators is
described by Galland et al. (2005a, hereafter Paper I).
In 2005 we started two surveys dedicated to searching for extrasolar planets and brown dwarfs around a volume-limited sample of A-F main-sequence stars i) with the E LODIE fiber-fed echelle spectrograph (Baranne et al. 1996) mounted on the 1.93-m telescope at the Observatoire de Haute-Provence (OHP, France) in the northern hemisphere; and ii) with the H ARPS spectrograph (Pepe et al. 2002) installed on the 3.6-m ESO telescope at La Silla Observatory (Chile) in the southern hemisphere. In 2006, the E LODIE spectrograph was replaced by S OPHIE (Bouchy et al. 2006). We detected a planet around an F6V star with E LODIE (Galland et al. 2005b, Paper II) and a brown dwarf around an A9V star (Galland et al. 2006b, Paper IV), and with H ARPS a two-planet system around an F6IV-V star (Desort et al. 2008, Paper V). We also derived the first statistics of planet existence around A-F stars thanks to our H ARPS survey (Lagrange et al. 2009, Paper VI).
We present and analyse in this paper the RV variations of Cygni.
Section 2 provides the stellar properties and the various
data obtained on this object. In Sect. 3, we discuss the
origin of the observed RV variations.
2 Stellar characteristics and measurements
The star Cygni (HD 185395, HIP 96441, HR 7469) is a
star, with an age estimated at
1.5-0.7+0.6 Gyr (Nordström et al. 2004), and located at
pc from the Sun (ESA 1997; van Leeuwen 2007). We took its rotational velocity
,
effective temperature
,
and surface gravity
from Erspamer & North (2003) and
Gray et al. (2003) (values in Table 1). We assumed
a spectral type F4V, commonly attributed to this star as, e.g., in the Bright
Star Catalogue (Hoffleit et al. 1991) or in the H IPPARCOS catalogue
(ESA 1997).
Table 1:
Cygni stellar properties.
2.1 Spectroscopic data
2.1.1 Description of the data
Between 2003 and 2006, we recorded 91 high S/N spectra of
Cygni with
E LODIE and, between November 2006 and December 2008, we recorded
162 spectra with S OPHIE. The wavelength range is
3850-6800 Å for E LODIE and 3872-6943 Å for S
OPHIE. Typical exposure times were 15 and 3 min for E
LODIE and S OPHIE, respectively, leading to a S/N of
200. The exposures were performed with simultaneous-thorium spectra to
follow and correct for the possible drift of the instrument due to local
temperature/pressure variations (whose impact shows a standard deviation of
2.5 m s
). With S OPHIE we used the high-resolution (
)
mode.
2.1.2 Radial velocity variations
The radial velocities (Fig. 1) were measured using a dedicated tool
(S AFIR) described in Paper I and based on the Fourier interspectrum
method developed in Chelli (2000). The uncertainty associated with
E LODIE data is 9 m s on average, consistent with the value obtained from our
simulations (see Paper I). In the case of S OPHIE data, the uncertainty is
5 m s
on average (taking the photon noise and instrument stability into
account).
As Cygni has a relatively low projected rotational-velocity
(
= 7 km s
), we could also measure the RV using a Gaussian
adjustement to the cross-correlation function (CCF). The results obtained by
the two different methods are found to be consistent.
![]() |
Figure 1:
Radial velocities of |
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E LODIE and S OPHIE RV data show (Fig. 1) a quasi-periodic signal with
peak-to-peak amplitude of about 220 m s,
much larger than the
uncertainties. A drift in the RV curve moreover seems to be present over the
whole data set, which could be attributed to a stellar companion
(Sect. 2.2). We finally note that the amplitude of the RV variations could also be slightly variable.
We used the CLEAN algorithm (Högbom 1974), applied to Lomb-Scargle periodograms to derive the periodograms of the radial velocities measured with both instruments (Fig. 2). This algorithm removes the aliases associated with temporal sampling of the data, and it deconvolves the window function iteratively from the initial ``dirty'' periodogram to produce the resulting cleaned periodogram.
In the case of E LODIE data, the periodogram shows one peak at a period of
days. The uncertainty is evaluated with the full width at half
maximum of the highest peak. In the case of S OPHIE data, the peak
corresponds to a period of
days.
![]() |
Figure 2:
E LODIE ( top) and S OPHIE ( bottom) CLEAN periodograms of
the radial velocities. On each data set, one peak is observed, either at |
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2.1.3 Line profile variations
S OPHIE Lomb-Scargle periodograms of the BVSs and curvatures (defined as in Hatzes 1996) are presented in Fig. 3, together with false-alarm probabilities (FAP, Kürster et al. 1997). In the case of the S OPHIE data, a peak is seen at approximately 140 days, i.e., not very different from the one measured in the S OPHIE RV variations. No peak is detected on the still noisier E LODIE data.
![]() |
Figure 3:
E LODIE and S OPHIE Lomb-Scargle periodograms of the bisector
velocity spans ( top 2 panels) and curvatures ( bottom 2
panels) with false alarm probabilities. On S OPHIE periodograms, the
period of |
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Figure 4 presents the bisector velocity spans (BVSs) as a
function of RVs for E LODIE and S OPHIE spectra. The amplitude of the BVS
variations is quite small: 50 m s,
much smaller than the amplitude of the RV
variations. No clear correlation is seem between the BVS and RV
variations. It shows that the spectra are mainly shifted in radial velocity
without significant changes in the line shape.
![]() |
Figure 4: Bisector velocity span versus RVs for E LODIE ( top) and S OPHIE ( bottom) data, showing that there is no correlation between line profiles and radial velocities. The dashed lines on S OPHIE data show the minimum effect of short-term variations, see Sect. 2.1.4. |
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![]() |
Figure 5: Top: RVs for 1-h S OPHIE data. Bottom: bisector velocity spans versus RVs for 1-h S OPHIE data. |
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2.1.4 Stellar jitter
Finally, to quantify its short-term variations, we monitored Cygni for 1 h consecutively (as we did for HD 60532, Paper V). High-frequency
variations are due to stellar phenomena and produce a noise (jitter) that has
to be taken into account in the analysis of longer period variations. In
October 2008, 46 consecutive spectra were then taken with S OPHIE under average
observation conditions (airmass below 1.2,
). The resulting RVs
and associated bisector velocity spans are presented in
Fig. 5. It appears that the short-term variations can account
for an RV amplitude of
30 m s
(
m s
)
and that
the total bisector velocity span amplitude over the whole S OPHIE data
(Fig. 4, bottom) set can only be explained with those short-term
variations. In the following attempt to analyse the high-amplitude RV
variations, we adopt increased RV uncertainties (at least
6.4 m s
,
fixed to that value) to take this stellar jitter into account.
2.2 Imaging data
We observed Cygni at high angular resolution and high contrast with the
adaptive-optics (AO) instrument PUEO (Rigaut et al. 1998) mounted on the
3.6-m Canada-France-Hawaii Telescope (CFHT, USA). The near-infrared camera
used, KIR (Doyon et al. 1998), has a field of view of
,
with a scale of
per pixel. We performed
non saturated exposures, as well as 30-s saturated ones, to investigate the vicinity of the star at
a deeper level. Special care was taken to ensure
that the non saturated exposures could be used as references for accurately
measuring the possible companions positions relative to the central star
and as references for measuring the photometric contrast between the
star and the possible companions.
The star Cygni was observed in June 2004, September 2005, and November 2007. The log
of observations is given in Table 2. A classical reduction was
performed using the software E CLIPSE (Devillard 1997). A candidate companion (CC) is seen in non saturated images (see
Fig. 6) with the narrow bandwidth Fe II filter (
m,
m). A deconvolution algorithm
using the method described in Véran (1997) was applied to derive
the contrast and angular separation (
)
between the star and the
companion.
Figure 7 shows the relative
positions of the CC between 2004 and 2007. Clearly, the CC is
not a background star, but it is bound to Cygni. Given the H IPPARCOS distance, 18.6 pc, we derive a
projected separation of 46.5 AU between the two objects, thus a minimum
period of roughly 230 years, assuming a circular orbit. Moreover, we see in
Fig. 7 that the orbit of the companion is - still very partially
- resolved over a three-year period of observation.
The measured contrast between Cygni and its companion
Cygni B is
mag in H band; in the K band, the measured contrast is
mag. Given the star's apparent magnitudes, provided by Skrutskie et al. (2006), and distance (see above), we deduce H and K absolute magnitudes of
and
mag, respectively. Using the BCA98
evolutionary models (Baraffe et al. 1998), and assuming any age above
100 Myr, we deduce a mass
0.35
for the companion.
The evolutionary effects are negligible. Using the empirical relation given
by Delfosse et al. (2000) for
,
we find a comparable mass
0.33
for the companion.
The source Cygni was classified as a double star (Dommanget & Nys 1994). The Washington
double star (WDS) data (Hartkopf & Mason 2001) indicate a visual companion
detected several times since 1889, with a magnitude of
12, i.e.,
comparable to the visual magnitude expected from a 0.35-
star at
Cygni distance. The relative position of this object varied between 1892
and 1968 (see Table 2), and indicates that this companion is
bound to
Cygni. The companion was not detected by H IPPARCOS
because the contrast with
Cygni was too high. It is reasonable to say that
the WDS companion and the one found with PUEO is the same. Then we can track
its motion over more than a century (Fig. 8), but its orbit
is still very incomplete.
Table 2: Log of WDS observations between 1889 and 1968 followed by the AO observations using PUEO at CFHT between June 2004 and November 2007.
![]() |
Figure 6: High contrast and angular resolution image acquired with the adaptive optics system PUEO installed at CFHT: a companion is clearly visible. |
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![]() |
Figure 7:
Temporal evolution of the separation of the stellar companion of |
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![]() |
Figure 8:
Positions of the companion star with respect to the primary star for more than one century. The star represents the primary |
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3 Origins of the observed RV variations
We investigate hereafter different possible origins for the RV variations: stellar phenomenon (spots, pulsations) and planets. Beforehand, we estimate the possible impact of the stellar companion on the spectroscopic data.
3.1 Impact of the stellar companion on the RV data
The star Cygni B could a priori play a role on the measured radial velocities in
two ways. Firstly, given their separation (
2
)
and given the
usual seeings and the entrance width of the optical fiber, the spectra of the
two stars are superimposed in the E LODIE or S OPHIE data (fiber entrance of
2
and 3
,
respectively). This could introduce a bias in the
measurements. However, the contrast of 4.6 mag in H band translates into
a contrast of 7.9 mag (a flux ratio of
1500) in the V band, hence the
negligible signal of the secondary in our spectra. We expect a
radial-velocity effect below 1 m s
.
If very active, it could still produce a
weak H
signature superimposed on the
Cygni H
line. This
does not affect our results, as this line is not considered in the RV measurements.
With the classical cross-correlation technique, the potential pollution of the spectrum by a stellar companion can be tested using various masks. We therefore checked that the RV amplitudes remain identical when using various masks. Also, the RVs are identical if we use either the red part or the blue part of the spectra to measure them. This confirms that the spectrum of the companion has no impact on the measured radial velocities.
Secondly, the stellar companion of course induces radial velocity variations
in the primary. Given the companion properties and assuming the system seen
edge-on, we estimate the maximum drift possibly induced on the primary star by
plotting the acceleration projected on the line of sight z, with respect to
the true separation r (Fig. 9)
![\begin{displaymath}\frac{{\rm d}^2 z}{{\rm d}t^2} = \frac{G m_2}{r^2} \cos \big[ \arcsin\big(
\frac{\rho}{r}\big) \big] ,\end{displaymath}](/articles/aa/full_html/2009/42/aa11731-09/img51.png)
where G is the gravitational constant, m2 = 0.35







![]() |
Figure 9: Possible drift induced by the stellar companion given the unprojected true separation r to the primary star. |
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3.2 Stellar phenomenon
3.2.1 Stellar spots
We saw in the previous section that there is no correlation between the star
RV variations and the BVS variations. Given the star's projected
rotational-velocity, the instrument resolution, and according to the study
presented in Desort et al. (2007), we can definitely conclude that the
observed RV variations are not due to stellar spots. Indeed, were this the
case, a correlation between the BVS and the RV would be observed. Typically,
given the star's properties, one or more spots on an inclined star would be
needed to reproduce a periodic signal, and a linear correlation coefficient
-0.5 between the bisector velocity spans and the RVs. Given the
observed RV amplitude, the amplitude of the BVS would therefore be much higher
than what is actually observed.
Also, in such a case, one would expect significant photometric variations. A single spot producing such an RV variation would induce a photometric amplitude between 5 and 30 mmag, depending mainly on the star inclination and the spot location (Desort et al. 2007). The photometry given by H IPPARCOS (ESA 1997) is constant with a scatter of only 0.004 mag. We recognize, however, that the H IPPARCOS data were not recorded simultaneously with the spectroscopic ones, so this photometric argument is certainly weaker than the absence of correlation between RV and BVS variations. No clear emission in the core of the Ca II lines is observed (see Fig. 10 for the Ca II K line) which excludes a high level of activity.
We looked for possible long-term stellar variations using classical
H
indicators. Very faint H
variations are
detected, but they are not correlated with the RV variations. As the H
indexes are moreover quite sensitive to pollution by the thorium lamp, we
cannot attribute them to a stellar origin.
Finally, the stellar rotational period is less than 7 days according to its
and assuming a stellar radius typical for this type of star, a
spot or a set of spots cannot explain RV variations with periods of one
hundred days or more. We can therefore safely conclude that spots are most probably not responsible
for the observed RV variations.
![]() |
Figure 10:
No emission is observed in the Ca II K line for the |
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3.2.2 Granulation
Another source of variation could be the attenuation or suppression of the
convective blueshift due to the presence of plages (e.g., Deming & Plymate 1994; Marquez et al. 1996). The expected convective blueshift expected for Cygni would be in the range
400-800 m s
depending on the line (see Gray 2009 for a F5IV-V,
which is the closest to
Cygni in his sample). The observed variations
could then be due to a cyclic variation with a plage filling factor varying
between 0 and 30%, typically in order to produce the
220 m s
variation. However, such a variation of the convection properties
should lead to a strong variation in the bisectors and in the Ca II
index, which is not the case.
3.2.3 Stellar pulsations
Generally, pulsations induce line-profile variations that strongly affect the
bisector velocity span (Paper VI). Besides, the timescale of the observed
radial-velocity variations (100 days) is far larger than the ones of
pulsations known for this type of main-sequence stars. It is in fact more
characteristic of giant stars variability. Variability periods of a few days
are observed in the case of the pulsating
Doradus stars
(Mathias et al. 2004). Moreover, if we integrate the RVs measured between a
minimum and a maximum of the amplitude for half a period, we end up with a
total displacement close to the stellar radius, which, if even possible, would
lead to detectable photometric variations.
It is therefore unlikely that classical pulsations are responsible for the observed RV variations. However, the presence of a peak at about 150 days in the BVS periodogram and in the RV periodogram indicates that the period of the RV variations is linked in some way to the low amplitude line shape variations. Such a situation has never been reported to our knowledge and is indeed quite puzzling. We cannot at this stage exclude that we could be facing a new type of stellar variability, undetected so far because of a lack of long-term, very-precise RV monitoring of main-sequence stars.
3.3 Planet(s) around
Cygni
The Cygni RV curve shows quasi-periodic variations with a period of
130-150 days, together with a variable positive trend. Moreover, the RV
curve seems to be modulated in amplitude. We now try to see whether these
variations can be attributed to a planet or a planetary system.
We first tried to fit the whole data set (with uncertainties set to
6.4 m s
)
assuming a single planet and allowing a drift. We failed to
correctly reproduce the observed RVs. Figure 11 shows an
example of a fit with a planet on a circular orbit (plus a drift). The planet
that produces such an RV curve has a mass of 2.3
and is on a 0.6 AU
circular orbit (Table 3). The algorithm ends up with a
period of 155 days hung on the S OPHIE data set, but fails to properly fit the
E LODIE data set, as if there was period/phase change with time (clearly
visible as structure in the residuals near the range [3600-3800] days).
The additional drift needed is 16 m s
yr
,
slightly higher
than the maximum value that the binary companion would probably produce. We
note that a system that fails to fit satisfactorilly the whole
set of data (taken over more than 5 years) would allow the data to be fitted if they
were limited to one or two consecutive periods.
![]() |
Figure 11:
E LODIE and S OPHIE radial velocities and orbital solution for |
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We then tried to simultaneously fit the whole set of data, assuming the
presence of several planets and using a genetic algorithm search. No stable
solution was found. The only satisfactory fits are achieved by unstable
systems with orbits that cross each other. We show an example in
Fig. 12 of a fit obtained with a two-companion plus drift
model. The residuals are still very high, the fit is not improved compared
to the one-companion plus drift model (residual rms 35 m s versus 39 m s
,
and the drift that we get is approximately the same: 17 m s
yr
versus 16 m s
yr
). Moreover, these kinds of configurations
with massive planets on such close orbits are not dynamically stable.
Table 3:
E LODIE/S OPHIE best orbital solution for Cygni, considering one planet and a drift.
![]() |
Figure 12:
E LODIE and S OPHIE radial velocities and orbital solution for |
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The system is then obviously more complex than just consisting of one, two, or even three planets plus a drift. We then explored more exotic configurations:
- instead of harbouring one single planet, the system could consist of a
binary planet system orbiting the star, much like the Pluto-Charo system,
but with higher masses. However, the radial-velocity signal generated by
this configuration would be very close to the one generated by a single
planet having the total mass. The only departure from the pure Keplerian
system would be related to the secular perturbations of the orbit due to the
binary nature of the system. The associated secular period would be at least
several hundred primary orbital periods, i.e., much longer than our
observation time span; hence, we should mainly detect the primary orbital
signal with good accuracy;
- one could also think of 2 co-orbiting planets locked in 1:1 mean-motion
resonance. Such a configuration has been observed in the system of Saturn
satellites. The two satellites orbit Saturn on the same orbit. In the
rotating frame, they have synchronized horseshoe-like libration motions
that prevent them from colliding. The less massive one has the largest
amplitude motion (Yoder et al. 1983). The associated libration period is
here again a few hundred orbital periods of the primaries. Over a
shorter time span, the radial-velocity signal of the whole system will
mainly consist of the sum of the individual signals of the two planets. If
we assume that the two planets have zero eccentricities, the radial velocity
signal will have the form
, where n is the common mean motion of the two planets, A and B are amplitudes related to the masses of the planets, and
is a phase shift that depends on their current mutual configuration. This can be rewritten as
where C and
are new amplitudes and phases that depend on A, B, and
. This is equivalent to the signal generated by one single planet. This remains true if the planets have small eccentricities, and if they have larger eccentricities, the mutual system is not stable. Here again, the only departure from this signal will be the temporal variation of C and
that is related to the mutual libration motion of the two bodies. Hence we should not expect to see changes before several decades. The signal detected over our observation timespan should not be different from that of a single planet.
4 Concluding remarks
The radial velocities obtained with E LODIE and S OPHIE on Cygni are
quasi-periodically variable, with a
150 day period. We
investigated different possible origins to these RV variations, either star or
planet related.
Given knowledge today of stellar activity, using several criteria as usual
in this type of study, we are unable to attribute these variations to the
star itself (spots, pulsations); however, the peak in the
periodogram of the BVSs at 140 days, i.e., close to the period of the
RV variations prevents us from totally excluding a stellar origin.
We tried to fit the data with one planet orbiting at less than 1 AU and with a mass of a few Jupiter masses, also taking the impact of the observed companion star into account. It appears that such an hypothesis allows us to fit only part of the data, recorded over a limited number of periods, but fails to satisfactorily fit the whole set of data (taken over more than 5 years). More complex systems were investigated, but no convincing result was obtained. More observations and detailed studies of gravitational interaction between the 2 planets are needed to understand this sytem.
With the data available, we are then not able to conclude on the origin of
these puzzling RV variations. If a planet origin is confirmed, then Cygni, with a spectral type of F4V,
would be the earliest main-sequence star hosting planets found so
far. Moreover, it would be one of the few low-metallicity stars hosting
planets. Its planetary system would not be simple, and it would in particular
include strongly interacting planets.
If a stellar origin were confirmed, then this would show that, unexpectedly, some main-sequence stars, not classified as active by the usual criteria (e.g., Ca II H&K indexes) or pulsating, may undergo intrinsic variations that produce quasi periodical, large-amplitude, and long-period (more than 100 days) RV variations, with at the same time, low levels of line shape deformations (hence small-amplitude BVS variations). Such situations have not been considered so far in the analysis of RV variations, and would need to be considered in future searches for such long-period planets, both in terms of observational strategy and data analysis.
We can at least conclude that Cygni is an individual complex system
that deserves many more observations to be understood, and it may also
serve as an example for other searches.
We acknowledge support from the French CNRS and the support from the Agence Nationale de la Recherche (ANR grant NT05-4_44463). We are grateful to the Observatoire de Haute-Provence (OHP) and theCFHT for their help during the observations, and to the Programme National de Planétologie (PNP, INSU).
These results have made use of the SIMBAD database, operated at the CDS, Strasbourg, France. They also make use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
We also thank Gérard Zins and Sylvain Cètre for their help in implementing the SAFIR interface.
X.B. acknowledges support from the Fundação para a Ciência e a Tecnologia (Portugal) in the form of a fellowship (reference SFRH/BPD/21710/2005) and a programme (reference PTDC/CTE-AST/72685/2006), as well as the Gulbenkian Foundation for funding through the ``Programa de Estímulo à Investigação''.
N.C.S. would like to acknowledge the support from Fundação para a Ciência e a Tecnologia (Portugal) in the form of a grant (references POCI/CTE-AST/56453/2004 and PPCDT/CTE-AST/56453/2004), and through programme Ciência 2007 (C2007-CAUP-FCT/136/2006).
References
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Footnotes
- ... stars
- Based on observations made with the E LODIE and S OPHIE spectrographs at the Observatoire de Haute-Provence (CNRS, France) and with the PUEO adaptive optics system at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii.
- ...
- Tables of radial velocities are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/1469
- ... decade
- A comprehensive list of known exoplanets is available at http://exoplanet.eu.
All Tables
Table 1:
Cygni stellar properties.
Table 2: Log of WDS observations between 1889 and 1968 followed by the AO observations using PUEO at CFHT between June 2004 and November 2007.
Table 3:
E LODIE/S OPHIE best orbital solution for Cygni, considering one planet and a drift.
All Figures
![]() |
Figure 1:
Radial velocities of |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
E LODIE ( top) and S OPHIE ( bottom) CLEAN periodograms of
the radial velocities. On each data set, one peak is observed, either at |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
E LODIE and S OPHIE Lomb-Scargle periodograms of the bisector
velocity spans ( top 2 panels) and curvatures ( bottom 2
panels) with false alarm probabilities. On S OPHIE periodograms, the
period of |
Open with DEXTER | |
In the text |
![]() |
Figure 4: Bisector velocity span versus RVs for E LODIE ( top) and S OPHIE ( bottom) data, showing that there is no correlation between line profiles and radial velocities. The dashed lines on S OPHIE data show the minimum effect of short-term variations, see Sect. 2.1.4. |
Open with DEXTER | |
In the text |
![]() |
Figure 5: Top: RVs for 1-h S OPHIE data. Bottom: bisector velocity spans versus RVs for 1-h S OPHIE data. |
Open with DEXTER | |
In the text |
![]() |
Figure 6: High contrast and angular resolution image acquired with the adaptive optics system PUEO installed at CFHT: a companion is clearly visible. |
Open with DEXTER | |
In the text |
![]() |
Figure 7:
Temporal evolution of the separation of the stellar companion of |
Open with DEXTER | |
In the text |
![]() |
Figure 8:
Positions of the companion star with respect to the primary star for more than one century. The star represents the primary |
Open with DEXTER | |
In the text |
![]() |
Figure 9: Possible drift induced by the stellar companion given the unprojected true separation r to the primary star. |
Open with DEXTER | |
In the text |
![]() |
Figure 10:
No emission is observed in the Ca II K line for the |
Open with DEXTER | |
In the text |
![]() |
Figure 11:
E LODIE and S OPHIE radial velocities and orbital solution for |
Open with DEXTER | |
In the text |
![]() |
Figure 12:
E LODIE and S OPHIE radial velocities and orbital solution for |
Open with DEXTER | |
In the text |
Copyright ESO 2009