Testing the models: NIR imaging and spectroscopy of the benchmark T-dwarf binary Eps Indi B M. Kasper European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching, Germany [email protected] 9 0 0 2 A. Burrows n Princeton University, Department of Astrophysical Sciences, Princeton, NJ 08544-1001, USA a and J 4 1 W. Brandner ] R Max-Planck-Institut fu¨r Astronomie, K¨onigstuhl 17, 69117 Heidelberg, Germany S . h p - o ABSTRACT r t The relative roles of metallicity and surface gravity on the near-infrared spectra of late-T s a browndwarfsarenotyetfullyunderstood, andevolutionarymodelsstillneedtobecalibratedin [ order to provide accurate estimates of brown dwarf physical parameters from measured spectra. TheT-typebrowndwarfsEpsIndiBaandBbformingthetightlyboundbinaryEpsIndiB,which 1 v orbits the K4V star Eps Indi A, are nowadays the only such benchmark T dwarfs for which all 7 important physical parameters such as metallicity, age and mass are (or soon will be) known. 9 We present spatially resolved VLT/NACO images and low resolution spectra of Eps Indi B in 9 the J, H and K near-infrared bands. The spectral types of Eps Indi Ba and Bb are determined 1 bydirectcomparisonoftheflux-calibratedJHKspectrawithTdwarfstandardtemplatespectra . 1 and also by NIR spectral indices. Eps Indi Bb is confirmed as a T6 while the spectral type of 0 Eps Indi Ba is T1.5 so somewhat later than the previously reported T1. Constrained values for 9 surface gravity and effective temperature are derived by comparison with model spectra. The 0 v: evolutionarymodelspredictmassesaround∼53MJ forEpsIndiBaand∼34MJ forEpsIndiBb, slightly higher than previously reported values. The suppressed J-band and enhanced K-band i X flux of Eps Indi Ba indicates that a noticeable cloud layer is still present in a T1.5 dwarf while r no clouds are needed to model the spectrum of Eps Indi Bb. a Subject headings: stars: late-type — stars: low-mass, brown dwarfs – stars: binaries: general 1. Introduction samechemicalcomposition,ageandmetallicityof themainsequenceprimarydeterminedbywelles- Multiple stellar systems with one component tablished methods also apply to the brown dwarf being a main sequence star and at least one other companion(s). Furthermore, sufficiently tight bi- component having a mass below the hydrogen- nary systems would allow one to directly measure burninglimit,andhenceresidinginthedomainof thesystemmassbydeterminingtheorbitandeven brown dwarfs are the key to calibrate and bench- to measure the individual component masses via mark brown dwarf evolution models. Since all monitoring of radial velocities. Hence, the mea- components are expected to be coeval and of the 1 sured spectral energy distribution (SED) of such with high precision. While the Eps Indi B binary acompanioncanbeusedtocalibratetheeffective isseparatedfromtheEpsIndiAby1500AU(sev- temperature and surface gravity of evolutionary eralarcminutesonskyatthedistanceof3.626pc), models and provide the required benchmarks. thetwobrowndwarfsareseparatedonlybyabout One such precious object, Eps Indi B, was re- 0.7(cid:48)(cid:48) corresponding to a projected spatial separa- solved into a binary T1/T6 dwarf (McCaughrean tion of 2.6 AU (McCaughrean et al. 2004). This et al. 2004) orbiting the K4.5V primary Eps Indi suggeststhatthesystemmassmightbemeasured A during the commissioning of the Simultaneous fromorbitalmotionwithinafewyears. Frommea- Differential Imager (SDI, Close et al. 2005) at surements on Eps Indi A, the system age is rea- the VLT. Initial mass estimates based on spec- sonably well determined to be in the range 0.8 to tralpropertiesandanassumedageof1.3Gyrwere 2 Gyr (Lachaume et al. 1999), and a near-to-solar 47±10M and28±7M forEpsIndBaandBb, metallicity([Mg/H]=-0.05,[Al/H]=-0.04,[Fe/H] Jup Jup respectively (McCaughrean et al. 2004). Another = -0.06) is reported by Beir˜ao et al. (2005). T6 dwarf companion, SCR 1845 B, was recently found by Biller et al. (2006) around the M8.5 pri- 2. Observations and Data Reduction mary SCR 1845 A using the same instrument and Eps Indi B was observed with NACO mounted characterized by NIR imaging and spectroscopy onUT4oftheVLTon23May2008(imaging)and by Kasper et al. (2007). Both, Eps Indi B and 9 June 2008 (spectroscopy). The Adaptive Optics SCR 1845 B, are extremely nearby (closer than 4 used 90% of the light from the binary as a guide pc), so near that they can efficiently be observed star for its infrared wavefront sensor while 10% withmodernAdaptiveOpticsinstrumentsdespite of the light were directed towards the scientific their intrinsic faintness and rather small orbital camera. In this way, we obtained well corrected distance from the primary. Other benchmark ob- images that easily resolve the 0.58(cid:48)(cid:48) binary (see jects include HN Peg (Leggett et al. 2008), Gl Figure1). 570D (Saumon et al. 2006) and HD 130948 BC (Dupuy et al. 2008; Potter et al. 2002; Goto et al. 2.1. Imaging 2002). It is now widely accepted that, besides T Fortheimagingobservations,theS13cameraof eff (a function of bolometric luminosity and radius NACOwasusedintheJ,H-andKsnear-infrared which are both a function of age), surface gravity filters, with a pixel scale of 13.20±0.05mas per (a function of mass and radius) and metallicity pixel. The target was observed using a standard are centrally important in determining the spec- dithering procedure integrating for three minutes tral energy distribution of late-T dwarfs (Saumon on source in each of the bands. et al. 2007; Liu et al. 2007). The effects of metal- Image data reduction followed standard proce- licity and surface gravity on the NIR spectra are, dures including sky removal, bad pixel cleaning, however,notyetfullyunderstood(Burgasseretal. and flat fielding. Differential photometry and as- 2006a; Liu et al. 2007). Calibration of theoretical trometry were done on the reduced images by si- models against observations has started with the multaneously fitting a model PSF profile to the work by Burgasser et al. (2006a); Saumon et al. binary. The individual magnitudes for Eps Indi (2006); Leggett et al. (2007). Both mass and age, i.e., the main underlying physical parameters for any modelling of brown dwarf evolution and at- mospheres, are, however, still highly uncertain for most known T dwarfs. Precise mass estimates can only be derived for browndwarf,whicharemembersofbinaryormul- tiple systems, and for which orbital parameters Fig. 1.— NACO broad band JHK images of the have been determined. Currently, Eps Indi Bb is 0(cid:48).(cid:48)583 binary Eps Indi Bb. North is up, East is the only late T dwarf for which physical parame- left. ters,andinparticularitsmass,willsoonbeknown 2 Ba and Bb were finally calculated from the rela- ibrated. The halo of Eps Indi Ba at the po- tivemagnitudesandtheintegrated2MASSmagni- sition of Bb was estimated at its opposite po- tudesoftheunresolvedsystem(J=11.91,H=11.31 sition with respect to Eps Indi Ba. The spec- and Ks=11.21). The error introduced by the dif- tra were divided by the telluric calibrator and ference between NACO and 2MASS instrument multiplied by a Kurucz template spectrum of responses has been calculated from the spectra, Vega (http://kurucz.harvard.edu/stars/VEGA/) as described in the next section, and has been smoothed to the actual resolution of the data in taken into account. Table1 displays 2MASS pho- order to remove the hydrogen absorption features tometry of Eps Indi Ba and Bb. On 23 May of the A0V telluric calibrator. Synthetic magni- 2008, the separation between the two components tudeswerecalculatedasdescribedinKasperetal. was 0(cid:48).(cid:48)583±0(cid:48).(cid:48)003, and the position angle was (2007) in order to determine and apply the cor- 153◦.9±0◦.5. The errors of the astrometric posi- rection factors needed to convert the flux ratios tions and the flux are the 95% confidence levels from the NACO to the 2MASS photometric sys- provided by the MATLAB fitting algorithm, and tem. Flux calibration of the spectra was finally the error on position angle is introduced by the established using the calculated 2MASS magni- uncertainty of the NACO FoV orientation. tudes of both components (see table1) and the 2MASSzeromagnitudein-bandflux(Cohenetal. 2.2. Spectroscopy 2003). It was verified that the errors introduced by NACOwasusedinlong-slitspectroscopicmode thedifferenceoftheisophotalwavelengthsforEps to obtain R ≈ 400 spectra in the J and HK spec- Indi B and and the spectral calibrator do not ex- troscopic filters (modes S54-4-SJ and S54-4-SHK, ceed the photometric errors. We also estimated 2nm/px pixel dispersion, S54 camera with 54.3 noise from the standard deviation of the individ- mas/pixel). By turning the Nasmyth adaptor ro- ual spectra that were generated during the data tator, the slit was aligned with the binary axis. analysis and averaged to obtain the final result. Dithering the binary at two positions along the The SNR for each individual data point is around slit, exposures of 26 minutes total in each of the 30 for Eps Indi Ba and most parts of Eps Indi Bb modes were obtained. A telluric calibrator (HIP spectra. In the K-band and in the depression be- 113982, spectral type A0V) has been observed in tween the J-band peaks, the SNR of the Eps Indi a similar manner just after the object at a simi- Bb spectrum drops to 3-10. The deduced NIR lar airmass. The effects of differential slit losses spectrum is consistent with the optical to mid-IR between Eps Indi B and the spectral calibrator spectra presented by King et al. (2008). (Goto et al. 2003) were mitigated by observing both properly centered on the slit with about the 3. Results same orientation of the parallactic angle with re- spect to the dispersion direction. A spectrum of 3.1. Spectral Types the NACO internal Tungsten lamp was recorded for wavelength calibration. The most direct way to determine the spectral Spectroscopicdatareductionfollowedstandard typeofastarisdirectcomparisontospectralstan- procedures. After sky removal, bad pixel clean- dards. Figures2 and 3 plot the NIR spectrum of ing and flat fielding, the spectra from Eps Indi EpsIndiBaandBb(blacklines)ontopofTdwarf Ba and Bb were extracted and wavelength cal- spectra obtained by Knapp et al. (2004); Strauss et al. (1999); Leggett et al. (2000); Chiu et al. (2006) and defined as spectral standards by Bur- gasser et al. (2006b). The NIR spectrum of Eps Table 1: 2MASS photometry of Eps Indi Ba and IndiBafitssomewhatinbetweenthestandardT1 Bb from 23 May 2008 (JD 2454609.9). andT2spectra. Usingthespectralindicesdefined Star J H Ks byBurgasseretal.(2006b),three(H O-J,H O-H, Ba 12.29±0.03 11.52±0.03 11.36±0.03 2 2 CH -K) suggest T1 while CH -H suggests T2 and Bb 13.23±0.03 13.21±0.03 13.47±0.03 4 4 CH -JevenT3. Hence,weslightlyrefinethespec- 4 traltypeofEpsIndiBatoT1.5. Thespectrumof 3 Eps Indi Bb fits the T6 standard well. 3.2. Fitting Models to the Eps Indi Ba+b Data Assuming the Eps Indi B components have the same metallicity (near solar, Beir˜ao et al. (2005)) 3 Eps Indi Ba and age (∼ 0.8−2 Gyr, Lachaume et al. (1999)) 2.5 T1 adlwloawrfseuvsoltuotieoxnplaonredtahtemaocscpuhrearceytohfeobrays.icEbvroowlun- Constant 2 + ttoihtoheneaorr,nyeTthehffaenoadrny,dmpgraorsavsvi,ditaeygse(t,gha)en(mdfoarrpapadiinuggisvbeannetdwm,eeoetnna,ltliohcne- Normalized F λ 1.15 T2 ity). For given T and gravity, we have a pre- eff 0.5 T3 dicted radius, and with the known distance we can then make absolute comparisons between the 0 meaured spectra and theoretical models. For the 1 1.2 1.4 1.6 1.8 2 2.2 2.4 λ [μm] evolutionary theory, we use Burrows et al. (1997). Forthespectralandatmospheretheory,weusethe Fig. 2.— Spectrum of Eps Indi Ba (black line) approach described in Burrows et al. (2006) and plotted on top of T1-3 dwarf spectral standards Sharp & Burrows (2007). The goal is to deter- obtainedfromSandyLeggett’sLandTdwarfdata mineT andgravityforeachobject, andthento eff archive. determinewhetheraconsistenttheoreticalpicture emerges. In particular, we can ascertain whether the models are consistent with the assumption of coevality. These current models have some limitations. First, since Eps Indi Ba is clearly near the L/T transition region above a T of ∼1100 K, it eff is necessary to incorporate the effects of silicate clouds (Ackerman & Marley 2001; Tsuji 2002; Burrows et al. 2006). The modeling of clouds 4 Eps Indi Bb (e.g.,theirmodalparticlesizes,spatialextent,op- 3.5 tpcilrcooaubldlpemrmoapotdeircet.liedNse,esavcnreidrbtehddeelgeirsnese,(oBwfuepraurotscwehstinheeetss”a)Cli.ass2qe0u0Ei6t”e) + Constant 2.35 T5 F λ cwliotuhd15isµamsssupmheedrictaolfboerstceormitpergisreadin.soWfewhinicithiatlhlye malized 1.25 also tested 10 and 20µm particles but did not Nor T6 1 achieve better fits. Second, though the absorp- tionfeatureduetothehotbandsofmethanefrom 0.5 T7 ∼1.6 to ∼1.75µm is a defining signature of brown 0 1 1.5 2 2.5 dwarfs, the strengths of these bands are not well- λ [μm] determined theoretically, and have not been mea- sured in the laboratory. Since it is as good as any Fig. 3.— Spectrum of Eps Indi Bb (black line) credible formulation described in the extant lit- plotted on top of T5-7 dwarf spectral standards erature and though it clearly underestimates the obtainedfromSandyLeggett’sLandTdwarfdata strength of these bands, we use the prescription archive. described in Sharp & Burrows (2007). Finally, thewingsoftheKIresonanceabsorptiondoublet at ∼0.77 µm determine the continuum of brown 4 dwarf spectra out to as far as ∼1.05 µm (Burrows Eps Indi Bb, taken from Burrows et al. (1997), is et al. 2000). The shape of these wings, in particu- ∼0.93 R . Generally, the theoretical radii do not J lartheeffectivecutoffwavelength,isstillasubject vary by more than ∼10%, with lower radii associ- of active investigation. ated with higher values of g. Figure5 displays the Given these caveats, we have identified the measured spectrum together with the best fitting range of spectral models which approximately re- model. produce the observations. For Eps Indi Ba, we ThefitstoEpsIndiBaaresomewhatlessgood, ran grids of models spanning the T range 1150- but constraining. Fitting the Z and J bands was eff 1300Kwitharesolutionof50Kandthelog(g[cm compromisedbyambiguitiesinthecloudopacities s−2]) range 4.9-5.3 with a resolution of 0.1. For and KI wings. To approximately achieve the ob- Eps Indi Bb, we ran grids of models spanning the served flux level in the K band required clouds to T range850-950Kwitharesolutionof25Kand suppress the fluxes in the Z and J bands. With- eff the log(g) range 4.7-5.1 with a resolution of 0.1. out cloud opacity, which naturally is most effica- The models were than compared to the measured cious in these bands, the Z and J fluxes would be spectra by visual inspection looking for the small- too high, while the K band flux would simultane- est residuals between data and model over the ouslybetoolowasshowninfigure4. Cloudslevel complete spectral region. We further calculated out these bands and without clouds there are no least-squares residuals between data and model good fits to Eps Indi Ba. An initial investigation and found that the results agree very well with showed that the best fit modal particle sizes were the by-eye fits. We did not attempt to use more ∼15 ± 5 µm. This is an interesting conclusion, sophisticatednumericalmethodssuchasχ2statis- albeit arrived at in lieu of a robust theory of con- tics(Cushingetal.2008;Burgasseretal.2007)to densates in brown dwarf atmospheres. The three quantifythegoodness-of-fitbecausecurrentbrown bestfittingmodelsarederivedfor(T /log(g))of eff dwarfspectraltheorieshaveyettoomanyunquan- (1250/5.3),(1250/5.2)and(1300/5.3)inorder tified systematic problems that make a rigorous of preference corresponding to masses and ages of numerical treatment difficult and to some extent (55M / 1.7Gyr), (48M / 1.2Gyr) and (56M J J J still arbitrary. Masses and ages were derived for / 1.5Gyr). We finally estimate mass and age of thethreebestfittingmodelsfromtheevolutionary Eps Indi Ba of 53+9−7 M and 1.5+0.8−0.5 Gyr. J tracksofBurrowsetal.(1997)bylinearinterpola- The radius of Eps Indi Ba, taken from Burrows tion. We then determined the final mass and age et al. (1997), is ∼0.83 R . Figure4 displays the J estimate by calculating a weighted average of the measured spectrum together with the best fitting threebestfittingmodelsassigningweightsof1,0.5 model and a plot portraying a model, but with- and0.33inorderofpreference. Errorsonthesefi- out clouds, demonstrating the important role of nal estimates were derived from the mass and age clouds. variationsintroducedbyourlog(g)stepsizeof0.1 There is a remarkable agreement in the best which dominate over the variations introduced by fitting ages of Eps Indi Ba and Bb of 1.5 Gyr, so the chosen Teff resolution. the models are consistent with the assumption of For Eps Indi Bb, no cloud models were nec- coevality. However, the age range over which the essary and we derive well matching fits for (T modelsproducereasonablefitsisoftheorder±0.5 eff / log(g)) of (900 / 5.0), (925 / 5.1) and (875 / Gyr, so in total the modelling results agree well 4.9) in order of preference. The best-fit values of with the age estimate of Eps Indi A of 1.3−0.5+0.7 T andg arecorrelated,withthehighergravities Gyr by Lachaume et al. (1999) suggesting overall eff paired with the higher T s. Using the evolution- spectral and evolutionary model consistency. Our eff ary tracks, the corresponding masses and ages are massestimatesaresomewhathigherthanprevious (34/,M /1.5Gyr),(38M /1.8Gyr)and(30M / estimates (47 and 28 M for Eps Indi Ba and Bb, J J J J 1.1Gyr). Using the weighted average described in respectively, McCaughrean et al. (2004)), but still the previous paragraph, we finally estimate mass consistent with those considering the error bars. andageofEpsIndiBbof34±5MJ and1.5±0.5Gyr There is enough leeway in these fits that does withtheerrorbarsderivedfromthevariationsin- not allow us to further constrain the ages and troduced by the log(g) resolution. The radius of masses beyond this range. Ambiguities in con- 5 densate modeling and the age of Eps Indi A and degeneracies along the T /g line in the spectral eff models are the culprits. Nevertheless, Eps Indi B is the most promising binary brown dwarf system with which to make absolute comparisons and for 1 T =1250K, g=2×105cm/s2, clouds which astronomers can test the general theory of 0.9 eff Teff=1200K, g=1.4×105cm/s2, no clouds browndwarfs. Hence,thesedatashouldbeagoad 0.8 Eps Indi Ba observation to further measurements and a motivation for im- −1m]0.7 CH4 proved theory. −2μW cm 00..56 CH4 4. Conclusions Flux [1e−17 00..34 H2O H2O CH4 H2O newWeH-haavnedpKre-bseanntdedsptehcetr1astofJE-bpasndIndaisBwaellanads 0.2 CH Bb. By comparison with theoretical models we 0.1 4 were able to derive strong constraints on effec- 00.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4 2.6 tive temperature, surface gravity and age of both λ [μm] brown dwarfs. The results confirm the approxi- mate coevality of the stellar and the two brown Fig. 4.— NIR spectrum of Eps Indi Ba. The un- dwarf components of the Eps Indi system. The derlyingsolidgraycurveshowsthebestmodelfit. suppressed J-band and enhanced K-band flux of The dotted line shows a similar model not consid- EpsIndBaindicatesthatanoticeablecloudlayer ering clouds. is still present in a T1.5 dwarf like Eps Indi Ba at an age of ≈1.5Gyr, whereas for an T6 dwarf like Eps Ind Bb clouds become much less impor- tant at the same age as clouds either sink below the photosphere (larger scale heights) or thin out (see, e.g., Cushing et al. (2008)). Once dynam- ical mass estimates derived from monitoring of theorbitalmotionofthesystembecomeavailable, our slightly increased mass predictions (compared to McCaughrean et al. (2004)) of 53+9−7M and 3.5 J T =900K, g=1×105cm/s2 34±5M forEpsIndiBaandBb,respectively,will 3 CH4 Eepfsf Indi Bb observation provideJa crucial test for the validity of our mod- CH 2.5 4 eling. Recent dynamical mass estimates point in- −1m] H2O deed towards a significantly higher system mass −2μm 2 H2O for the Eps Ind Ba/Bb system (Cardoso et al. Flux [1e−18 W c 1.15 CH4 2bb0reo0aw8)nb.ednHwcheanmrfcaeervktoholeubtjEieocpntsafrIoynrdatiensdstyinsattgemmaonsdcpohcnaetrliiinbcurmaestointdog- 0.5 H2O CH4 els. 0 −0.5 This research has made use of data products 0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4 2.6 λ [μm] from the Two Mircon All Sky Survey, a joint project of the University of Massachusetts and Fig. 5.— NIR spectrum of Eps Indi Bb. The IPAC/Caltech, funded by NASA and the NSF. underlying gray curve shows the best model fit. We thank Sandy Leggett for providing electronic M and T dwarf spectra through her Web site. AB would like to acknowledge support from the NASA Astrophysics Theory Program under grant 6 NNX08AU16G. WB acknowledges support by Goto, M., Hayano, Y., Kobayashi, N., et al. 2003, the Deutsches Zentrum fu¨r Luft- und Raumfahrt in Presented at the Society of Photo-Optical (DLR), F¨orderkennzeichen 50 OR 0401. Instrumentation Engineers (SPIE) Conference, Facilities: VLT (NACO). Vol. 4839, Society of Photo-Optical Instrumen- tation Engineers (SPIE) Conference Series, ed. REFERENCES P. L. Wizinowich & D. Bonaccini, 1117–1123 Ackerman, A. S. & Marley, M. S. 2001, ApJ, 556, Goto, M., Kobayashi, N., Terada, H., et al. 2002, 872 ApJ, 567, L59 Beir˜ao, P., Santos, N. C., Israelian, G., & Mayor, Kasper,M.,Biller,B.A.,Burrows,A.,etal.2007, M. 2005, A&A, 438, 251 A&A, 471, 655 Biller, B. A., Kasper, M., Close, L. M., Brandner, King, R. R., McCaughrean, M. J., Homeier, D., W., & Kellner, S. 2006, ApJ, 641, L141 etal.2008,inAIPConfProceedings,CoolStars 15 poster abstract Burgasser, A. J., Burrows, A., & Kirkpatrick, J. D. 2006a, ApJ, 639, 1095 Knapp, G.R., Leggett, S.K., Fan, X., etal.2004, AJ, 127, 3553 Burgasser,A.J.,Cruz,K.L.,&Kirkpatrick,J.D. 2007, ApJ, 657, 494 Lachaume, R., Dominik, C., Lanz, T., & Habing, H. J. 1999, A&A, 348, 897 Burgasser, A. J., Geballe, T. R., Leggett, S. K., Kirkpatrick,J.D.,&Golimowski,D.A.2006b, Leggett,S.K.,Geballe,T.R.,Fan,X.,etal.2000, ApJ, 637, 1067 ApJ, 536, L35 Burrows, A., Marley, M., Hubbard, W. B., et al. Leggett,S.K.,Marley,M.S.,Freedman,R.,etal. 1997, ApJ, 491, 856 2007, ApJ, 667, 537 Burrows, A., Marley, M.S., &Sharp, C.M.2000, Leggett,S.K.,Saumon,D.,Albert,L.,etal.2008, ApJ, 531, 438 ApJ, 682, 1256 Burrows, A., Sudarsky, D., & Hubeny, I. 2006, Liu, M. C., Leggett, S. K., & Chiu, K. 2007, ApJ, ApJ, 640, 1063 660, 1507 Cardoso, C., McCaughrean, M. J., King, R. R., McCaughrean, M. J., Close, L. M., & Scholz, R.- etal.2008,inAIPConfProceedings,CoolStars D. e. a. 2004, A&A, 413, 1029 15 poster abstract Potter, D., Mart´ın, E. L., Cushing, M. C., et al. Chiu, K., Fan, X., Leggett, S. K., et al. 2006, AJ, 2002, ApJ, 567, L133 131, 2722 Saumon, D., Marley, M.S., Cushing, M.C., etal. Close, L. M., Lenzen, R., Guirado, J. C., et al. 2006, ApJ, 647, 552 2005, Nature, 433, 286 Saumon, D., Marley, M. S., Leggett, S. K., et al. 2007, ApJ, 656, 1136 Cohen, M., Wheaton, W. A., & Megeath, S. T. 2003, AJ, 126, 1090 Sharp, C.M.&Burrows, A.2007, ApJS,168, 140 Cushing, M.C., Marley, M.S., Saumon, D., etal. Strauss, M. A., Fan, X., Gunn, J. E., et al. 1999, 2008, ApJ, 678, 1372 ApJ, 522, L61 Dupuy, T. J., Liu, M. C., & Ireland, M. J. 2008, Tsuji, T. 2002, ApJ, 575, 264 ArXiv e-prints This2-columnpreprintwaspreparedwiththeAASLATEX macrosv5.2. 7