A&A 435, L5-L8 (2005)
DOI: 10.1051/0004-6361:200500101
T. Forveille1,2 - J.-L. Beuzit2 - P. Delorme1,2 - D. Ségransan3 - X. Delfosse2 - G. Chauvin4 - T. Fusco5 - A.-M. Lagrange2 - M. Mayor3 - G. Montagnier2 - D. Mouillet6 - C. Perrier2 - S. Udry3 - J. Charton2 - P. Gigan7 - J.-M. Conan5 - P. Kern2 - G. Michet7
1 - Canada-France-Hawaii Telescope Corporation, PO Box 1597,
Kamuela, HI 96743, USA
2 - Laboratoire d'Astrophysique de Grenoble, BP 53X, 38041
Grenoble Cedex, France
3 - Observatoire de Genève, 51 Chemin des Maillettes, 1290, Switzerland
4 - European Southern Observatory, Casilla 19001, Santiago 19, Chile
5 - ONERA-DOTA, 92322 Châtillon, France
6 - Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées, Tarbes, France
7 - Laboratoire d'Études Spatiales et d'Instrumentation en Astrophysique, 5 place Jules Janssen, 92195 Meudon Cedex, France
Received 7 January 2005 / Accepted 19 March 2005
Abstract
We present the discovery of a tight M8V binary, with a
separation of only 1.2 astronomical units, obtained with the
PUEO and NACO adaptive optics systems, respectively at the CFHT
and VLT telescopes. The estimated period of LP 349-25 is
approximately 5 years, and this makes it an excellent candidate for a
precise mass measurement.
Key words: stars: binaries: visual - stars: individual: LP 349-25 - stars: low-mass, brown dwarfs
Thanks to persistent efforts with ground-based adaptive optics
and spectroscopy (Forveille et al. 1999; Delfosse et al. 1999a,b; Ségransan et al. 2000), as well as with HST (Torres et al. 1999; Benedict et al. 2000, 2001;
Hershey & Taff 1998), over 30 M dwarfs now have published masses
with 10% precision or better. As a result, the empirical Mass-Luminosity
relation is now fairly well constrained down to 0.1 solar mass
(Delfosse et al. 2000). The near-IR relations for M dwarfs are tight and
agree very well with theoretical predictions (Baraffe et al. 1998). By contrast,
the V band relation diverges significantly from those models below
0.5 solar mass, and has considerable intrinsic dispersion.
The motivation for additional measurements in that mass range is therefore
now shifting towards characterizing - and understanding - that
dispersion around the mean relation.
Below 0.1 solar mass on the other hand, empirical masses are much
scarcer. Many binaries are now known in that mass range,
and their separations are on average much tighter (typically <10 AU)
than in more massive systems (e.g. Close et al. 2003; Bouy et al. 2003).
Nonetheless, those that are currently known mostly have moderately
long periods, 20 years and beyond, which reflect typical distances of
20-30 pc and the resolution limit of the observations. To our knowledge,
the only objects with published dynamical masses well below 0.1 solar mass
are the components of Gl 569BC (Lane et al. 2001; Zapatero Osorio et al. 2004)
and 2MASSW J0746425+2000321 (Bouy et al. 2004).
Both orbits are still preliminary, with grade 4 in the Washington
Double Star catalog. The observations of 2MASS0746 only cover 35%
of its period, albeit at a very favourable phase, while Gl 569BC has full
orbital coverage but still somewhat sparse sampling.
Perhaps more importantly, both systems are young enough that at least one
of their components is actually below the Brown Dwarf limit (0.070 solar
mass, Chabrier et al. 2000), in spite of only moderately late spectral
types. The age of 2MASS0746 is not independently determined, and the
properties of Gl 569A can only constrain that of Gl 569BC to a broad
interval (Zapatero Osorio et al. 2004), over which the model luminosity of
the brown dwarf evolves by an order of magnitude.
In any comparison with theory, age therefore enters as an unwelcome
free parameter, and reduces the diagnostic value of those two
binaries. A few additional systems are being followed, such as LHS 1070
(Leinert et al. 1994, 2001) and Gl 494 (Beuzit et al. 2004),
but identifying additional late-M dwarfs binaries with periods under
10 years remains critically important.
Here we present the discovery of one such system, LP 349-25, using the adaptive optics systems of the CFHT and VLT telescopes. Section 2 presents the observations and the data analysis, while Sect. 3 briefly discusses the properties of the system.
The discovery observations were carried out on July 3rd 2004 at
the 3.6-m Canada-France-Hawaii Telescope (CFHT), using the CFHT
Adaptive Optics Bonnette (AOB) and the KIR infrared camera. The AOB,
also called PUEO after the sharp-visioned Hawaiian owl, is a
general-purpose adaptive optics (AO) system based on F. Roddier's
curvature concept (Roddier et al. 1991). It is mounted at the telescope
F/8 Cassegrain focus, and cameras or other instruments are then
attached to it (Arsenault et al. 1994; Rigaut et al. 1998). The
atmospheric turbulence is analysed by a 19-element wavefront curvature
sensor and the correction applied by a 19-electrode bimorph mirror.
Modal control and continuous mode gain optimization
(Gendron & Léna 1994; Rigaut et al. 1994) maximize the quality of the AO correction for the current atmospheric turbulence and guide star magnitude. For our observations a dichroic mirror diverted the visible light to the wavefront sensor while the KIR science camera (Doyon et al. 1998, named after a cocktail drink) recorded near-infrared light. The KIR plate scale is 34.85
0.10 per pixel, for a total field size of
(KIR on-line users manual). Excellent
atmospheric conditions prevailed during the observation (
0.55'' seeing
in the V band). The observation sequence consisted of 5 individual 15 s exposures at
each position of an 8'' square+center offset pattern.
The resulting images are excellent in spite of LP 349-25's faintness
(V = 17.5, and 40 ADUs/cycle on the wavefront sensor), and its duplicity
was obvious in real time at the telescope.
Confirmation observations of LP 349-25 were performed on September 26th 2004 with the NACO instrument at VLT UT4 (ESO Very Large Telescope, Paranal Chile). NACO consists of the NAOS adaptive optics system (Rousset et al. 2003; Lagrange et al. 2003), providing
diffraction-limited images in the near infrared, and of the CONICA
science camera (Lenzen et al. 1998), equipped with a 1024 1024
ALLADIN detector covering the 1-5
m spectral domain. The main
technical features of NAOS are a piezo-stack deformable mirror with
185 actuators and a separate tip-tilt mirror, two selectable
Shack-Hartmann wavefront sensors operating either in the optical
(450-950 nm) or in the near-IR (800-2500 nm) range, both featuring up
to 14
14 subapertures. The LP 349-25 observations used the
NAOS IR wavefront sensor, under clear sky and average turbulence
conditions (0.6'' seeing and 7 ms coherence time). They were performed
through the standard H broad-band filter and used the S13 CONICA camera, which provides a 13.27 mas/pixel sampling (NACO on-line users manual). The observation sequence consisted of pairs of 7s exposures acquired on a 7 positions random offset pattern within a 5'' jitter box.
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Figure 1: Adaptive optics images of LP 349-25 with CFHT through a K' filter ( left) and with the VLT through an H filter ( right). The scale is indicated by a 0.2'' bar, and North is up and East left. |
Open with DEXTER |
The reduction was performed within the ECLIPSE package (Devillard 1997). The individual raw data were flat-fielded using a normalised gain map, derived from images of the illuminated dome at CFHT, and from sky images taken at sunset for the VLT. The sky signal was estimated from a median across the jittered images. The individual flat-fielded images were then corrected from the sky image and stacked using a cross correlation algorithm.
After this cosmetic processing, we used the point-source mode of the
MISTRAL myopic deconvolution package (Mugnier et al. 2004) to extract
the coordinates and intensities of the two stars, from which we
derived the parameters of interest, separation, PA and relative
photometry. The astrometric calibration was derived from the standard
Orion field (McCaughrean & Stauffer 1994) and the HIP 482 wide binary.
This verified the expected pixel scale of both instruments.
NACO was, as expected, found oriented within 0.1 degree of North,
and KIR was found rotated by -2.0
0.2 degrees. Centroiding errors and imperfect knowledge
of the point-spread function completely dominate our uncertainty
budget at the small separation of LP 349-25.
Figure 1 displays the two reduced images and Table 1 summarizes the extracted parameters.
Table 1: Adaptive optics measurement of LP 349-25.
LP 349-25 is a recent addition to the solar neighborhood inventory, in
spite of its figuring in the Luyten Two Tenth Catalog (Luyten 1980). It was first recognised as a nearby star by Gizis et al. 2000, during a spectroscopic survey of candidate cool nearby stars selected from red 2MASS/POSS colours. They derive an M8V spectral type, and estimate
a photometric distance of 8.4 pc from the relatively insensitive J-Ks colour index. Reid et al. (2003) use narrow band spectral indices and J band photometry to derive a more precise distance, 7.7
0.8 pc. We approximately correct that determination for the new companion, and
adopt a distance for the system of 10.1
1.2 pc.
The companion is bright in the infrared, K' = 10.46, and on that ground
alone it is highly improbable that it is a background star. At the position of
LP 349-25 the density of the 2MASS catalog for K < 11 is 60 sources/square
degree. The probability to find such a bright star within even an arcsecond
of LP 349-25 is therefore only 1.5
10-6. Additionally, the companion
cannot be much bluer than the primary, or the system would
have produced a stronger signal on the visible wavefront sensor.
Galactic reddening behind LP 349-25 (
,
)
is very small (approximately E(B-V) = 0.06,
Burstein & Heiles 1982), and a background star would thus need to be
intrisically as red as LP 349-25. This would make it either an
unrelated red dwarf in the immediate solar neighbourhood, or
a halo giant at
20 kpc. Both possibilities are highly unlikely.
The proper motion and parallax are large (+399.8
5.5 mas/yr and -177.2
5.5 mas/yr Salim & Gould 2003); 130
13 mas, assuming for the sake of this particular argument that
the star is actually single), but largely cancel out between the dates of our two observations, with a total motion of only -19
7 and -47
4 mas. The separation of the two components actually changed by -14
15 mas and -16
15 mas. This is compatible with the expected orbital motion of
30 mas (uncertain by a factor of a few), but only helps excluding a background object at the 2
level.
LP 349-25 however has been previously examined for multiplicity, with the HOKUPAA adaptive optics system on GEMINI (Close et al. 2002), and it was then found unresolved. The two components were most likely less separated at that time (September 18th and 19th 2001), or perhaps for this particular target Close et al. 2002 did not obtain as good an adaptive optics correction as we have. Had the system however been significantly wider than found here, Close et al. (2002) would have been able to resolve it even with degraded correction. Their negative result demonstrates that LP 349-25 is not a long period system, which we would have serendipitously observed close to periastron. It also definitely ensures that the companion is not a background star, which on that date would have been separated by 1.3'', and very obviously resolved. A background star would in addition have been separated by 21.9'' at the 1954 epoch of the blue plate of the first Palomar Survey, and again it would be very easily seen.
For late-M and early-L dwarfs, one spectral subtype corresponds
to approximately 0.35 mag at H band (e.g. Vrba et al. 2004). The
observed contrast therefore indicates that the make-up of the pair is
M7.5V+M8.5V or M8V+M9V. At the 10 pc distance of the system, its 0.12'' separation translates
to 1.2 AU. If the stars have reached the main sequence (age >
1 Gyr),
as implicitly assumed to evaluate the distance, both masses are approximately
0.08
(Baraffe et al. 1998), just above the Brown Dwarf limit.
Adopting the main sequence masses, and correcting for the 1.35 statistical
factor between instantaneous projected separation and semi-major axis
(Duquennoy & Mayor 1991), the orbital period is approximately 5 years.
This estimate obviously has significant uncertainties, but it makes
LP 349-25 one of the best candidates for an accurate mass determination below 0.1
.
We
plan to monitor its relative motion with adaptive optics and will attempt to obtain a spectroscopic orbit, but a precise trigonometric parallax and an astrometric orbit will be equally important for the mass determination.