Issue |
A&A
Volume 516, June-July 2010
|
|
---|---|---|
Article Number | A21 | |
Number of page(s) | 4 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/201014740 | |
Published online | 18 June 2010 |
Discovery of a stellar companion to the nearby solar-analogue HD 104304
(Research Note)
C. Schnupp1 - C. Bergfors1 - W. Brandner1 - S. Daemgen2 - D. Fischer3 - G. Marcy4 - Th. Henning1 - S. Hippler1 - M. Janson5
1 - Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
2 - European Southern Observatory, Karl-Schwarzschild-Straße 2, 85748 Garching, Germany
3 - Department of Astronomy, Yale University, New Haven, CT 06520-8101, USA
4 - Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
5 - Department of Astronomy, University of Toronto, 50 St George Street, Toronto, ON M5S 3H4, Canada
Received 6 April 2010 / Accepted 3 May 2010
Abstract
Context. Sun-like stars are promising candidates to host
exoplanets and are often included in exoplanet surveys by radial
velocity (RV) and direct imaging. In this paper we report on the
detection of a stellar companion to the nearby solar-analogue star HD
104304, which previously was considered to host a planetary mass or
brown dwarf companion.
Aims. We searched for close stellar and substellar companions
around extrasolar planet host stars with high angular resolution
imaging to characterize planet formation environments.
Methods. The detection of the stellar companion was achieved by
high angular resolution measurements, using the ``Lucky Imaging''
technique at the ESO NTT 3.5 m with the AstraLux Sur instrument.
We combined the results with VLT/NACO archive data, where the companion
could also be detected. The results were compared to precise RV
measurements of HD 104304, obtained at the Lick and Keck observatories
from 2001-2010.
Results. We confirmed common proper motion of the binary system. A spectral type of M4V of the companion and a mass of 0.21
was derived. Due to comparison of the data with RV measurements of the
unconfirmed planet candidate listed in the Extrasolar Planets
Encyclopaedia, we suggest that the discovered companion is the origin
of the RV trend and that the inclination of the orbit of
explains the relatively small RV signal.
Key words: instrumentation: high angular resolution - astrometry - binaries: general - stars: fundamental parameters - stars: late-type
1 Introduction
HD 104304 (LHS 5206, HIP 58576) is a high proper motion star at a distance of 12.91
0.13 pc (Perryman et al. 1997).
Because of its proximity, brightness, and observability from both
hemispheres, it has been the subject of numerous studies. It is a
chromospherically inactive star with log R'(HK) = -4.933 (Gray et al. 2006) and with an X-ray luminosity of
W (Schmitt & Liefke 2004). It has a spectral type of G8IV to K0IV, log g = 4.35 to 4.15, and [Fe/H] = 0.22 to 0.18 (Cenarro et al. 2007; Gray et al. 2006), and is a thin disk member (Soubiran & Girard 2005). With an age of
8.5 Gyr and a mass of
1.01
(Takeda et al. 2007)
it is considered a close analogue to the Sun at approximately twice its
present age, and is a target of a high-precision Doppler survey aimed
at identifying planetary companions to Sun-like stars (Wright et al. 2004). HD 104304 has also been suggested as a target to search for habitable planets with future space missions (Lopez et al. 2005).
In 2008 we started a high-angular resolution imaging survey of exoplanet hosts stars with the goal to identify close stellar and substellar companions. The first results of this survey were reported by Daemgen et al. (2009). HD 104304 was included in the survey because of the identification of a potential substellar companion by Marcy (2007).
In the following we will use the designation HD 104304A for the primary star and HD 104304B for the companion.
![]() |
Figure 1:
AstraLux z' and NACO/SDI images of the binary using a logarithmic
intensity scale. The field of view is
|
Open with DEXTER |
2 Observations and data reduction
2.1 AstraLux Sur
Observations at the ESO 3.5 m NTT were obtained with
the ``Lucky Imaging'' instrument AstraLux Sur, a high-speed electron multiplying camera for Lucky Imaging observations (Hippler et al. 2009). The instrument is a clone of the common user instrument AstraLux Norte at the Calar Alto 2.2 m telescope (Hormuth et al. 2008). It provides a field of view of 16 16 arcseconds.
HD 104304 was observed as part of a larger sample of (candidate)
exoplanet host stars stars on April 11, 2009, and again on February 6,
2010 in i' and z'-band. Total integration times were 30 s corresponding to the best 10 % of 10000 frames with an individual
s. Figure 1 shows the AstraLux images of the binary as well as the VLT/NACO data (see Sect. 2.2).
The data were reduced by the AstraLux online data reduction pipeline as explained by Hormuth et al. (2008). Pixel scale and image orientation were determined by observations of star clusters with well-determined astrometry.
2.2 VLT/NACO
After the detection of the companion, we searched the VLT archive for
high-angular
resolution observations of HD 104304.
VLT observations of HD 104304 using the Spectral Differential Imager
(SDI) mode of NACO were obtained on January 18, 2006 in service mode
under the programme-ID 076.C-0762(A) for Damien Ségransan, and
retrieved from the ESO archive. NACO/SDI provides four simultaneous images in three different filters in the near infrared H-band.
Total integration times were
s. The companion was clearly detected in the NACO images.
We also checked the deeper NACO/SDI frames for additional closer and fainter
companions by reducing the data with a dedicated SDI+ADI pipeline in IDL, see Figure 2.
For details on this pipeline see Janson et al. (2007).
These data would enable us to detect a companion 7.5 mag fainter in H than HD
104304A with a detection limit of 3 sigma at an angular separation of 0.3
(as
assumed for the unconfirmed planet in http://exoplanet.eu).
No evidence for additional companions could be found.
2.3 Determination of binary parameters
Figure 1 shows a comparison of the AstraLux z', and the NACO images of the HD 104304 binary. In the NACO data set, we analysed the four acquisition images with the shortest integration time to derive precise relative astrometry and photometry for both components. For the analysis a pixel scale of 17.32 mas/pixel was assumed. Aperture photometry was conducted to determine the brightness ratio. The position of companion and primary star were determined by fitting a Gaussian profile.
![]() |
Figure 2: With the SDI+ADI pipeline reduced NACO/SDI frames of HD 104304. In the center of the image the residuals of the subtracted primary star can be seen. The white and black dots on the right half side of the image are the companion on the different orientated images. |
Open with DEXTER |
In the AstraLux data set, the procedure to determine the brightness ratio was slightly different, as the companion is situated inside the seeing halo of the parent star. Aperture photometry was conducted, taking also into account the halo background. This background was determined on the opposite site of the primary star from where the companion was situated, assuming a symmetric point spread function (PSF). To determine position angle and separation, PSF subtraction was applied to the primary star. The PSF for subtraction was created by mirroring the half of the primary star without companion to the opposite side. On this PSF subtracted image, the position of the binary companion was determined by fitting a Gaussian profile. The position of the parent star was determined by fitting a Gaussian profile to the original data. The results can be found in Table 1.
Table 1: Binary properties.
3 Physical properties of the HD 104304 binary
3.1 Common proper motion
HD 104304 is a high proper-motion star with
mas/yr and
mas/yr.
In the 3.25 years that passed between the VLT/NACO and the first AstraLux observations, HD 104304 moved
mas to the East, and
mas to the
South. In the same period, the separation between HD 104304A and B changed from
mas to
mas, and the position angle increased from
deg to
deg (see
Table 1). If the companion had been a background object, the corresponding numbers would have been a change in separation to
mas and in position angle to
deg,
which can be exluded with high significance. Thus both sources form a
physical binary, and the change in position angle can be attributed to
orbital motion around the common center of mass of both components.
3.2 Spectral types and component masses
As stated by Kraus & Hillenbrand (2007), the literature on intrinsic magnitudes and basic astrophysical parameters of main-sequence stars comprises a rather heterogeneous set. In order to minimize systematic errors in the determination of the properties of the HD 104304 binary system, we base the following analysis therefore on the homogenized set of parameters as compiled and computed by Kraus & Hillenbrand (2007). Assuming that the average of the brightness differences in the three NACO/SDI spectral bands is close to the brightness difference in H-band, we can derive the absolute H-band magnitudes of both components based on the 2MASS photometry of the unresolved binary star. The absolute H-band magnitude of HD 104304B derived this way is consistent with a spectral type of M4V.
To determine the i' magnitude of the binary companion the magnitudes given by Just & Jahreiß (2008) of the unresolved HD 104304 binary were used. By a comparison of the magnitude with spectral types given by Kraus & Hillenbrand (2007)
the spectral type of the companion was derived. Component A has a
spectral type of G8IV to K0IV which leads also to a spectral type of
M4V of HD 104304B in i'-band. We note that for mid M-dwarfs, i'-band magnitudes vary strongly with spectral type. Thus an uncertainty by +0.4 mag in i' corresponds to an uncertainty by less than half a spectral-subclass. By interpolating the mass scale in Table 5 from Kraus & Hillenbrand (2007) we derive a mass of
0.21+0.03-0.02
for HD 104304B.
The derived absolute magnitudes of both components in H and i'-band are listed in Table 2.
Table 2: Component photometry (absolute magnitudes).
3.3 Orbital parameters
While the projected separation of the binary changed only by a
relatively small
amount from 995 mas to 1104 mas, the position angle increased
quite substantially by 32.83 deg over a period of 3.25 years.
This gives some evidence that the orientation of the orbit is closer to
face-on than to edge-on (i.e.
).
The HIPPARCOS parallax of HD 104304 is
mas
(Perryman et al. 1997), corresponding to a distance of
pc. Hence the angular
separations correspond to projected separations of
12.8 AU
to
14.8 AU.
Taking into account only the change of the position angle during the
3.25 years, assuming a circular orbit and a semimajor axis of 14 AU, we would expect an orbital
period of
36 yr. With these assumed orbital parameters, Kepler's third law yields a system mass of
2.1
.
Hence, the real eccentric orbit has a smaller semimajor axis or the orbital period is larger, as the system has a mass of
1.2
(see Table 2).
To precisely determine the orbital parameters, more astrometric data points are necessary. Therefore astrometric monitoring of the binary over the next years is required.
![]() |
Figure 3:
Left: Theoretical RV curve of the binary system with a period of P = 48.5 years, an inclination of
|
Open with DEXTER |
3.4 Comparison with data of unconfirmed planet candidate
Based on its RV trend, HD 104304 has been identified as a candidate host of a substellar object (Marcy 2007). This RV trend was measured during 5 years, from 2001-2006. In these 5 years a change of 500 m/s in the RV signal was detected.
We calculated the estimated radial velocity curves for a binary system with 1.22 ,
different orbital periods between P = 35 years and P = 60 years different inclinations from
to
and different eccentricities.
To these theoretical RV curves, we compared precise
RV measurements of HD 104304, taken over a period of 9 years.
RV measurements at the Lick observatory have been obtained during
a period of 6.5 years, from May 2001 to December 2007. At the Keck
observatory, RV measurements have been taken over a period of
3 years, from December 2006 to January 2010. As can be seen on
Fig. 3, the calculated RV curve for an inclination of
,
an eccentricity of e=0.29 and a period of P = 48.5 years compares well with the RV data. The identification of the unconfirmed planet by Marcy (2007)
was also based on these RV measurements from the Lick observatory, only
on a shorter timescale than the RV data presented here. Therefore we
suggest that the unconfirmed extrasolar planet candidate listed in the
Extrasolar Planets Encyclopaedia
is identical with the stellar companion presented in this paper.
While a plausible set of orbital parameters is derived, the analysis also hints that thus far only around 20% of the orbit has been covered by RV monitoring, and less than 10% of the orbit by astrometric observations. Thus further monitoring is required in order to derive a robust set of orbital parameters.
Theoretical calculations were made in order to check if a real planet/brown dwarf companion orbiting HD 104304 would have been visible in the NACO/SDI frames.
The reduced NACO/SDI data (see Fig. 2) would enable us to detect a companion 7.5 mag fainter in H than HD 104304A at an angular separation of 0.3
,
i.e. a source with an absolute magnitude
mag for a detection limit of 3 sigma. In
the age range 5 to 10 Gyr, according to Baraffe et al. (2003), this corresponds to a
star with 83
(0.08
). Thus while we can exclude an
additional stellar companion with a mass
83
at a projected
separation
3.9 AU, a substellar (brown dwarf or planetary mass companion) would
not be visible in the NACO images.
4 Conclusions
The combination of NACO/SDI archival data and AstraLux Sur data made
it possible to confirm the stellar companion around HD 104304. Based on
the photometry, a spectral type of M4V and a mass of 0.21
were derived for HD 104304B.
The primary star is well studied, e.g. it has a known metallicity of [Fe/H] = 0.22 to 0.18 (Gray et al. 2006; Cenarro et al. 2007), an age of 8.5 Gyr (Takeda et al. 2007)
and a mass nearly equal to that of our Sun. This knowledge is a
valuable asset for the further characterisation of any stellar or
substellar companion in this system.
By modeling the theoretical RV curve and comparing it to the
available RV observations obtained over a period of 9 years, we have
shown that the observed RV trend could be explained by the detected
stellar companion. A theoretical RV curve with an eccentricity of e=0.29, an orbital period of P = 48.5 years and an inclination of the orbit of
fits
best the RV measurements. This gives evidence that the planet candidate
listed in the Extrasolar Planets
Encyclopaedia around HD 104304 is identical with the presented stellar
companion. Astrometric monitoring of the binary system over the next
few years is necessary to confirm this statement and to precisely
determine the orbit and its orientation.
In the case of confirmation of a planet around HD 104304, this system would be highly interesting in the context of planet formation and migration around close binaries with solar analogue host stars.
AcknowledgementsWe are particulary grateful to Sam (Karl) Wagner, Armin Huber and Ralf-Rainer Rohloff for their help in preparing and commissioning AstraLux Sur as well as all the technical staff at ESO La Silla and MPIA involved in the project.
References
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Footnotes
- ... HD 104304
- Based on observations made with ESO Telescopes at the La Silla and Paranal Observatory under programme IDs 083.C-0145 and 084.C-0812, and on data obtained from the ESO Science Archive Facility.
- ... NACO/SDI
- For more information on NACO/SDI see http://www.eso.org/sci/facilities/paranal/instruments/naco/inst/
- ... Encyclopaedia
- The Extrasolar Planets Encyclopaedia can be found at http://exoplanet.eu and is maintained by Jean Schneider.
All Tables
Table 1: Binary properties.
Table 2: Component photometry (absolute magnitudes).
All Figures
![]() |
Figure 1:
AstraLux z' and NACO/SDI images of the binary using a logarithmic
intensity scale. The field of view is
|
Open with DEXTER | |
In the text |
![]() |
Figure 2: With the SDI+ADI pipeline reduced NACO/SDI frames of HD 104304. In the center of the image the residuals of the subtracted primary star can be seen. The white and black dots on the right half side of the image are the companion on the different orientated images. |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Left: Theoretical RV curve of the binary system with a period of P = 48.5 years, an inclination of
|
Open with DEXTER | |
In the text |
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