A&A 490, 763-768 (2008)
DOI: 10.1051/0004-6361:200810605

Binarity at the L/T brown dwarf transition
(Research Note)

Adaptive optics search for companions[*]

B. Goldman1 - H. Bouy2,3,[*] - M. R. Zapatero Osorio2 - M. B. Stumpf1 - W. Brandner1 - T. Henning1


1 - Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
2 - Instituto de Astrofísica de Canarias, C/ vía Lactéa S/N, 38205 La Laguna, Tenerife, Spain
3 - Astronomy Department, 601 Campbell Hall, UC Berkeley, Berkeley CA-94720-3411, USA

Received 15 July 2008 / Accepted 17 August 2008

Abstract
Context. Current atmospheric models cannot reproduce some of the characteristics of the transition between the L dwarfs with cloudy atmospheres and the T dwarfs with dust-depleted photospheres. It has been proposed that a majority of the L/T transition brown dwarfs could actually be a combinaison of a cloudy L dwarf and a clear T dwarf. Indeed binarity seems to occur more frequently among L/T transition brown dwarfs.
Aims. We aim to refine the statistical significance of the seemingly higher frequency of binaries. Co-eval binaries would also be interesting test-beds for evolutionary models.
Methods. We obtained high-resolution imaging for six mid-L to late-T dwarfs, with photometric distances between 8 and 33 pc, using the adaptive optics systems NACO at the VLT, and the Lick system, both with the Laser Guide Star.
Results. We resolve none of our targets. Combining our data with published results, we obtain a frequency of resolved L/T transition brown dwarfs of 31+21-15%, compared to 21+10-7% and 14+14-7% for mid-L and T dwarfs (90% of confidence level). These fractions do not significantly support, nor contradict, the hypothesis of a larger binary fraction in the L/T transition. None of our targets has companions with effective temperatures as low as 360-1000 K at separations larger than 0 $.\!\!^{\prime\prime}$5.

Key words: stars: low-mass, brown dwarfs - stars: atmospheres - technique: high angular resolution - stars: binaries: general - stars: binaries: visual

1 Introduction

L/T transition brown dwarfs are a class of sub-stellar objects comprising the latest L-type and the earliest T-type dwarfs (Leggett et al. 2000), with spectral types between roughly L8 and T4 (Looper et al. 2008). Historically, the warmest members of the group, the late L dwarfs, were soon identified through their very red near-infrared colours (Kirkpatrick et al. 2000; Martín et al. 1999), but the T-type members of the transition kept escaping detection even after the cooler T dwarfs were identified through their strong molecular absorption (``methane dwarfs''). Indeed the neutral near-infrared colours of cooler L/T transition brown dwarfs concealed them to near-infrared surveys such as 2MASS, while the optical/near-infrared survey DENIS was too shallow to provide a large-enough volume (Phan-Bao et al. 2008). Eventually Leggett et al. (2000) identified the first T members of this group in the SDSS EDR data. Their near-infrared spectra exhibit both CO and CH4 absorption and they have J-K colours filling the gap between those of the red late-type L dwarfs and the blue mid-T dwarfs (i.e. $0\lesssim J-K\lesssim$ 2.0).

The rapid transition between the cloudy atmospheres of the L dwarfs and the dust-depleted atmospheres of the T dwarfs, at nearly constant effective temperature, was quickly recognised asa challenge for our theoretical understanding (Kirkpatrick et al. 2000; Golimowski et al. 2004). A brightening in the J band is even observed for early T dwarfs (Looper et al. 2008; Dahn et al. 2002; Tinney et al. 2003; Vrba et al. 2004). Other pecularities include the resurgence of FeH bands and the restrengthening of 1.2 $\mu$m K  I lines. Several unsuccessful attempts have been made to explain these peculiarities through a global thinning of the dust cover (Tsuji 2005), a variation in the precipitation efficiency (Knapp et al. 2004), and a better description of the condensate cloud structure (Cooper et al. 2003; Burrows et al. 2006). This led Burgasser et al. (2002) to propose that a dynamical cloud fragmentation process takes place in the atmospheres of these objects. So far a characteristic weather-like behaviour that this fragmentation could produce has not been clearly identified (see e.g. Goldman et al. 2008).

Table 1: Summary of targets and references. Tip-tilt star magnitude and separation to the target based on USNO-A2.0 (Monet et al. 1998). All distances are photometric, based on the relations of Knapp et al. (2004) between the spectral type, and MJ, and MK (except for SDSS J2047), assuming non-binarity.

Recent high-resolution imaging surveys have revealed a possibly higher binary frequency among L/T transition objects, compared to other brown dwarfs (Liu et al. 2006; Burgasser et al. 2006b). The factor-of-two excess reported by Burgasser et al. (2006b), given the limited sample size (19 dwarfs over the L7 to T3.5 spectral types in their compilation), would not rule out a constant binary fraction at the 90% confidence level (Burgasser 2007). This latter article demonstrates that such a higher binary fraction is expected where the $M_{\rm bol}/$spectral type relationship flattens, under a wide range of (reasonable) formation histories and mass functions, particularly in magnitude-limited samples. Burgasser et al. (2006b) and Liu et al. (2006) formulated the hypothesis that an higher binary rate among the transition brown dwarfs would explain some of the above characteristics, with Liu et al. (2006) speculating that single $\approx$T2-T4.5 objects may be rare. Their results, as well as the binary 2MASS J14044941-3159329 found by Looper et al. (2008), also demonstrated that the J-band brightening across the L/T transition is real and not an effect of selection bias, as it affects binaries which presumably have the same age and metallicity.

Co-eval binaries also provide interesting tests to evolutionary models, as the usually quite uncertain parameters such as age and metallicity, are now fixed for the pair of objects (Bouy et al. 2008; Looper et al. 2008). Finally, the binary fraction is an important prediction of brown dwarf formation scenarios, and, with other parameters, will eventually allow to discriminate between the various scenarios (Caballero 2007; Billères et al. 2005; Umbreit et al. 2005). In particular, Allen (2007) has analysed several high-resoution imaging surveys using a Bayesian algorithm. He substantiated the high-mass ratio distribution, and argued that the observed fraction of binaries with separation larger than 2.5 AU is too large compared to that predicted by Bate & Bonnell (2005).

Brown dwarfs are too faint in the optical to be good natural guide stars for adaptive optics high-resolution imaging, and even near-infrared sensors are not sensitive enough for most of the brown dwarfs, but the closest ones. Laser Guide Star (LGS) systems have recently extended the fraction of the sky observable with adaptive optics, although their operation does require a nearby star for tip-tilt corrections.

Here we report on an on-going search for binarity among L/T transition objects. In Sect. 2, we present our observations, target list and reduction, and in Sect. 3 our results. Finally in Sect. 4 we interpret our (non) detections.

   
2 Observations and data reduction

2.1 Target selection

We searched through the compendium housed at DwarfArchives.org and chose our targets according to the following criteria:

1.
Availability and characteristics of the tip-tilt star. LGS systems require a natural guide star to correct for the tip-tilt motions. Better Strehl ratios are obtained for brighter guide stars, that are closer to the target. We searched the USNO-A2.0 catalogue (Monet et al. 1998) at CDS, Strasbourg, for appropriate tip-tilt stars. For the ESO laser system PARSEC, we selected targets later than L4, with $R\leq 17.6$ mag, $d<40\hbox{$^{\prime\prime}$ }$ guide stars. For the Lick laser system, we selected targets with $R\leq 17.0$ mag, $d<50\hbox{$^{\prime\prime}$ }$ guide stars.
2.
The targets should not have been observed with high-resolution imagers at ESO and on board HST, and no such observations should have been published.
3.
Spectral type: we gave precedence to dwarfs with spectral type close to T0.
4.
Brightness: for a given spectral type we preferred brighter targets as they are likely to be closer to us and allow detections of closer binaries.
5.
Observability: The Lick run was performed in visitor mode and we selected target with the best observability at the time of the observations. The ESO observations were performed in service mode and we only required that the targets be South of $\delta = +20\deg$.
The targets are described in Table 1.

Table 2: Observing log. Site seeing from the DIMM.


  \begin{figure}
\par\includegraphics[width=18cm]{0605fig1.eps} \end{figure} Figure 1: NACO H-band images.
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2.2 NACO/PARSEC observations

We observed all targets in J and H bands to strengthen any detection and to derive a rough spectral type for the potential companion, based on photometry. We used the S27 camera with a 27-mas pixel size and $28\hbox{$^{\prime\prime}$ }\times28\hbox{$^{\prime\prime}$ }$ field of view. This camera maximises the field of view, while offering a good sampling of the point-spread function. In order to remove, or at least characterise, instrumental effects, we observed each target at two instrumental angles, $0\deg$ and $30\deg$. For each angle, we used a four-position dithering pattern, with one and two exposures/position, respectively in the J and H band, for a total integration time per angle of 4 min and 9.6 min. The observations were performed in service mode. The nights were clear (except on April 2) but the seeing was often highly variable (see Table 2). However, the seeing of the final, stacked images barely varies, within a few percent, with the exception of 2MASS J0939, as well as SDSS J2047 in the H band.

We have used the reduced images produced by the NACO pipeline, version 3.6.0 (see Fig. 1). The pipeline determines the astrometry of the image (WCS), with a typical accuracy of 1% for the pixel scale and $0.4\deg$ for the orientation (Eggenberger et al. 2007).

2.3 Lick observatory adaptive optics observations

We used the Lick Observatory 3 m Shane telescope and its adaptive optics system (Bauman et al. 1999; Lloyd et al. 2000) to observe the L4 subdwarf 2MASS J1626, as well as SIMP J0136, one of the closest T dwarf. With $R\approx$ 20 mag, the target was too faint for the wavefront sensor to close the loop, so that we used the LGS. We acquired three dithered images of 5 min each in the Ks-band. Conditions were average for the site, with a seeing of $\approx$1 $.\!\!^{\prime\prime}$5 and a clear sky.

The images were processed using standard procedures using the Eclipse data reduction package (Devillard 1997), including dark subtraction, flat-fielding, sky extimation and co-addition of the individual frames. The images are shown in Fig. 2.


  \begin{figure}
\par\includegraphics[width=9cm,clip]{0605fig2.eps} \end{figure} Figure 2: Lick Ks-band images. The spike South of 2MASS J1626 is much narrower than the point-spread function and cannot be stellar.
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2.4 New proper motions

Three of our NACO targets have objects in the field of view that have multi-epoch detections (see Sect. 3.3) and which can be used to constrain the image astrometry and to derive the proper motions of our targets. Proper motions are crucial to confirm the association with potential companions. Because there are fluctuations in the NACO pixel scale and orientation of up to 1% and $0.4\deg$ respectively, an accurate astrometry would require two objects with known proper motion. As we only have one, the above uncertainties translate into a 120 mas (200 mas) and 84 mas (140 mas) uncertainty for a field object located at 12 $^{\prime\prime}$ (20 $^{\prime\prime}$ respectively) away from the target. Depending on the time baseline, those uncertainties may be greater than the proper motion uncertainties of the field object.

2.4.1 2MASS J0756

2MASS J0756 has been observed twice by SDSS (Adelman-McCarthy et al. 2008) in $2005.00\pm0.05$ and once by 2MASS (Skrutskie et al. 2006) in 1997.83. We derive the proper motion based on the published positions (see Table 1).

Using that proper motion, we measure that the pixel scale is within 2% of the nominal value of 27.15 mas, while the orientation is within $(0.57\pm0.15)\deg$ of the nominal value.

2.4.2 2MASS J1036

2MASS J1036 has a nearby J=15.15 mag field star, whose (negligible) proper motion we derive from USNO and 2MASS catalogues. Adding this proper motion to the positional shift in our images compared to the 2MASS position, we obtain a proper motion of $\mu_\alpha=(-0.12\pm0.02)$ $^{\prime\prime}$/yr, $\mu_\delta=(-0.43\pm0.02)$ $^{\prime\prime}$/yr for the brown dwarf. We use the nominal pixel scale and orientation, but the large baseline of 7.9 years reduces the impact of those uncertainties (included in the quoted errors).

2MASS J1036 is also detected in 2MASS and DENIS images, separated by 2.1 years. We cross-matched all DENIS detections of Strip 5346 within 5 min of the target, to the 2MASS catalogue (138 objects). We find an average offset of $\Delta\alpha=+159\pm16$ mas and $\Delta\delta=-380\pm20$ mas (stat., $1\sigma$), independent of brightness, nearly constant over the field except for a trend in $\Delta\delta$ with right ascension. An accurate determination of the relative DENIS-2MASS astrometry would require a more detailed treatment and is beyond the scope of this paper. Applying these corrections to the DENIS astrometry improves the proper motion fit of the field star. However the resulting proper motion of 2MASS J1036 is found to be incompatible with the above value, calculated over a longer baseline, which we favour.

2.4.3 SDSS J2047

SDSS J2047 has a nearby J=12.56 mag field star, with negligible proper motion. As above we use the relative SDSS and NACO positions to derive the proper motion of $\mu_\alpha=(-0.00\pm0.02)$ $^{\prime\prime}$/yr, $\mu_\delta=(-0.27\pm0.02)$ $^{\prime\prime}$/yr, with a 7.0-yr baseline.

   
3 Results

3.1 Limit of sensitivity of the adaptive optics observations

We have computed the limit of sensitivity of our observations from the 3 $\sigma $ noise on the radial profile of the PSF of the different images. Figure 3 shows the results. NACO H-band observations are typically sensitive to $\Delta H=5$-6 mag at 0 $.\!\!^{\prime\prime}$5, and $\Delta H\approx 4$ mag at 0 $.\!\!^{\prime\prime}$25. The Lick/AO observation is sensitive to $\Delta K{\rm s}=3$ mag at 0 $.\!\!^{\prime\prime}$5, and $\Delta K{\rm s}=1.5$ mag at 0 $.\!\!^{\prime\prime}$25.


  \begin{figure}
\includegraphics[width=9cm,clip]{0605fig3.eps} \end{figure} Figure 3: Limits of sensitivity $\Delta $Mag vs. separation of the adaptive optics observations performed with VLT/NACO (J and H bands) and Lick/AO (Ks band).
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With these 3 $\sigma $ sensitivities, we calculate the absolute J- and H-band limiting magnitudes at 0 $.\!\!^{\prime\prime}$5, assuming the distances listed in Table 1. We translate these absolute magnitudes into effective temperature for the most sensitive filter, usually the J band for the NACO data, assuming the COND 5 Gyr tracks of Allard et al. (2001, see their Table 3#. We note that, although the Strehl ratio in the J band is worst than in the H band, the sensitivity is equal or better in the J band than in the H band thanks to the smaller Airy disk and the larger J flux for T dwarfs and cooler dwarfs.

Table 3: Sensitivities to ultra-cool companions at 0 $.\!\!^{\prime\prime}$25/0 $.\!\!^{\prime\prime}$5 (3$\sigma $). Lower limits on the effective temperature based on Allard et al. (2001).

3.2 Search for close binaries

We resolve no close companion in any of our images.

For the nearly-equal-brightness binaries that could populate the L/T transition ( $\Delta m<2$), we are sensitive to separations down to about 0 $.\!\!^{\prime\prime}$1 for the NACO data, and 0 $.\!\!^{\prime\prime}$2 for SIMP J0136, corresponding to 1-40 AU. If the targets were equal-brightness binaries (unresolved in our data), they would be 41% further away and the minimum physical separation probed would increase accordingly.

We update the compilation of high-resolution-imaging results of Burgasser (2007), to which we add the two T2.5 targets observed by Looper et al. (2008) (one is resolved) and ours. Over the L8 to T2.5 spectral types, we find a binary fraction of 31+21-15%, compared to 21+10-7% and 14+14-7% for mid-L and T dwarfs (90% of confidence level). The statistical uncertainties are calculated using the formula of Burgasser et al. (2003). A simple $\chi^2$ analysis of the different binarity fractions returns a 50% chance result for a 20% constant binary fraction over the L0 to T8 spectral range.

As mentioned in Burgasser (2007) and Allen (2007), the sensitivity of these surveys, both in terms of depth and spatial resolution, varies greatly. Depth is usually not a critical factor for the nearly-equal-brightness binaries we are concerned with, but the physical separations probed, which depend on the target distance and instrumental performance, are crucial. The binarity fractions of Fig. 4 are obviously lower limits, as very close binaries will not be resolved. Allen (2007) estimates to 3-4% the fraction of ultra-cool dwarfs with a tight companion undetected in the imaging surveys he analyses. If we limit ourselves to a comparison of the binarity fractions with respect to spectral types, we need still to address the biases introduced by the incomplete brown dwarf detection and by the target follow-up selections. For instance, our samples are primarily magnitude-limited; L/T transition brown dwarfs are mostly detected in an optical survey (SDSS) limited over a quarter of the sky; the smaller number of L/T transition brown dwarfs may systematically lead to the study of more distant targets than, e.g., the (also fainter) later T dwarfs. We defer to the presentation of our full sample the evaluation of these statistical biases and survey heterogeneity.


  \begin{figure}
\par\includegraphics[width=9cm,clip]{0605fig4.eps} \end{figure} Figure 4: Close binary fraction vs. spectral type. The short thick lines show the new binary fraction for each L and T spectral type. The longer dashed lines indicate the published fraction, averaged over four groups of subtypes (Burgasser 2007), while the thick lines give the updated average fraction including our results. The bottom numbers indicate the numbers of resolved binaries and total numbers of observed brown dwarfs. The 90% confidence levels for statistical noise are reported as vertical thin lines. We include the results of the Duquennoy & Mayor (1991) survey for G stars and Reid & Gizis (1997). We point out again the different survey sensitivities, in particular Duquennoy & Mayor (1991) is based on the radial-velocity method.
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3.3 Wide binaries

We check if the field stars in the NACO field of view of 28 $^{\prime\prime}$ could be associated with the target.

None of the field stars are resolved. Because the field stars are off-axis, their image quality differs from that of the program star. In the case of SDSS J2047's field star, its full width at half maximum is much larger than that of SDSS J2047 (by $\approx$$50\%$). For the three other targets, the full width at half maximum of the field star is similar or even better than that of the on-axis target.

   
4 Conclusion

We have obtained high-resolution imaging of six brown dwarfs using LGS systems at the VLT and Lick observatories. No targets are resolved in our data set. A slightly larger fraction of L/T transition brown dwarfs are binaries, compared to earlier L and later T dwarfs, using data from the literature and adding our non-detections. The excess is however statistically not significant.

Observations of a larger sample, particularly of L/T transition brown dwarfs, is required. (Nearly) whole-sky multi-band optical surveys, such as PanSTARRS1, and near-infrared proper motion surveys, such as UKIDSS and VHS, using 2MASS as the first epoch, will offer the opportunity to find additional targets close enough to provide a good physical-separation sensitivity.

Acknowledgements

B. Goldman thanks P. Moeller and the ESO staff for its support and for conducting the observations. We thank the referee, A. Burgasser, for his quick review. H. Bouy acknowledges the funding from the European Commission's Sixth Framework Program as a Marie Curie Outgoing International Fellow (MOIF-CT-2005-8389). This Research has made use of the M, L, and T dwarf compendium housed at DwarfArchives.org and maintained by C. Gelino, D. Kirkpatrick, and A. Burgasser, and of the S IMBAD database, operated at CDS, Strasbourg, France.

References

 

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