Jacqueline K. Faherty , Adric R. Riedel Erini Lambrides ... · Erini Lambrides 2, Haley Fica ,...
Transcript of Jacqueline K. Faherty , Adric R. Riedel Erini Lambrides ... · Erini Lambrides 2, Haley Fica ,...
Draft version May 26, 2016Preprint typeset using LATEX style emulateapj v. 01/23/15
POPULATION PROPERTIES OF BROWN DWARF ANALOGS TO EXOPLANETS∗
Jacqueline K. Faherty1,2,9, Adric R. Riedel2,3, Kelle L. Cruz2,3,11, Jonathan Gagne1, 10, Joseph C. Filippazzo2,4,11,Erini Lambrides2, Haley Fica2, Alycia Weinberger1, John R. Thorstensen8, C. G. Tinney7,12, Vivienne
Baldassare2,5, Emily Lemonier2,6, Emily L. Rice2,4,11
Draft version May 26, 2016
ABSTRACT
We present a kinematic analysis of 152 low surface gravity M7-L8 dwarfs by adding 18 new parallaxes(including 10 for comparative field objects), 38 new radial velocities, and 19 new proper motions.We also add low- or moderate-resolution near-infrared spectra for 43 sources confirming their low-surface gravity features. Among the full sample, we find 39 objects to be high-likelihood or new bonafide members of nearby moving groups, 92 objects to be ambiguous members and 21 objects thatare non-members. Using this age calibrated sample, we investigate trends in gravity classification,photometric color, absolute magnitude, color-magnitude, luminosity and effective temperature. Wefind that gravity classification and photometric color clearly separate 5-130 Myr sources from > 3 Gyrfield objects, but they do not correlate one-to-one with the narrower 5 -130 Myr age range. Sourceswith the same spectral subtype in the same group have systematically redder colors, but they aredistributed between 1-4σ from the field sequences and the most extreme outlier switches betweenintermediate and low-gravity sources either confirmed in a group or not. The absolute magnitudes oflow-gravity sources from J band through W3 show a flux redistribution when compared to equivalently typed field brown dwarfs that is correlated with spectral subtype. Low-gravity late-type L dwarfsare fainter at J than the field sequence but brighter by W3. Low-gravity M dwarfs are > 1 magbrighter than field dwarfs in all bands from J through W3. Clouds, which are a far more dominantopacity source for L dwarfs, are the likely cause. On color magnitude diagrams, the latest-type low-gravity L dwarfs drive the elbow of the L/T transition up to 1 magnitude redder and 1 magnitudefainter than field dwarfs at MJ but are consistent with or brighter than the elbow at MW1 andMW2. We conclude that low-gravity dwarfs carry an extreme version of the cloud conditions of fieldobjects to lower temperatures, which logically extends into the lowest mass directly imaged exoplanets.Furthermore, there is an indication on CMD’s (such as MJ versus (J-W2)) of increasingly reddersequences separated by gravity classification although it is not consistent across all CMD combinations.Examining bolometric luminosities for planets and low-gravity objects, we confirm that (in general)young M dwarfs are overluminous while young L dwarfs are normal compared to the field. Usingmodel extracted radii, this translates into normal to slightly warmer M dwarf temperatures comparedto the field sequence while lower temperatures for L dwarfs with no obvious correlation with assignedmoving group.Keywords: Astrometry– stars: low-mass– brown dwarfs
∗THIS PAPER INCLUDES DATA GATHERED WITH THE 6.5METER MAGELLAN TELESCOPES LOCATED AT LAS CAM-PANAS OBSERVATORY, CHILE.
1 Department of Terrestrial Magnetism, Carnegie Institu-tion of Washington, Washington, DC 20015, USA; [email protected]
2 Department of Astrophysics, American Museum of NaturalHistory, Central Park West at 79th Street, New York, NY 10034;[email protected]
3 Department of Physics & Astronomy, Hunter College, 695 ParkAvenue, New York, NY 10065, USA
4 Department of Engineering Science & Physics, College ofStaten Island, 2800 Victory Blvd., Staten Island, NY 10301 USA
5 Department of Astronomy, University of Michigan, 1085 S.University, Ann Arbor, MI 48109
6 Department of Physics & Astronomy, Columbia University,Broadway and 116th St., New York, NY 10027 USA
7 School of Physics, UNSW Australia, 2052. Australia8 Department of Physics and Astronomy, Dartmouth College,
Hanover NH 03755, USA9 Hubble Fellow10 Sagan Fellow11 Physics Program, The Graduate Center, City University of
New York, New York, NY 1001612 Australian Centre for Astrobiology, UNSW Australia, 2052.
Australia
1. INTRODUCTION
At masses <∼ 75 MJup – the H-burning mass limit– , the interior of a source changes significantly. Belowthis mass limit, electron degeneracy pressure sufficientlyslows contraction that the core of a given object is pre-vented from ever reaching the temperatures required fornuclear fusion (Hayashi & Nakano 1963, Kumar 1963).As a consequence, the evolution of substellar mass ob-jects produces a temperature, age, and mass degeneracythat leads to an important, and at times completely in-distinguishable, overlap in the physical properties of thelowest mass stars, brown dwarfs and planets.
Objects with masses <∼ 75 MJup cool through theirlives with spectral energy distributions evolving as theiratmospheric chemistry changes with decreasing tempera-tures. The spectral classification for sources in the range(3000 K > Teff > 250 K) corresponds to late-type M, L,T and Y with each class defined by the effects of chang-ing molecular species available in the photosphere (Kirk-patrick 2005, Burgasser et al. 2002a, Cushing et al. 2011).At the warmest temperatures, the atmosphere is too hot
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for the condensation of solids (Allard & Hauschildt 1995;Lodders 1999). But as the Teff falls below 2500 K, bothliquid (e.g. Fe) and solid (e.g. CaTiO3, VO) mineraland metal condensates settle into discrete cloud layers(Ackerman & Marley 2001; Tsuji et al. 1996b,a; Woitke& Helling 2004; Allard et al. 2001).
As temperatures cool further, cloud layers form at suchdeep levels in the photosphere that they have little orno impact on the emergent spectrum. This transitionbetween “cloudy” to “cloudless” objects occurs rapidlyover a narrow temperature range (1200-1400 K, corre-sponding to the transition between L-type and T-typespectra) and drives extreme photometric, spectroscopic,and luminosity changes (Burgasser et al. 2002b, Tinneyet al. 2003, Faherty et al. 2012, 2014a, Dupuy & Liu2012, Radigan et al. 2012, Artigau et al. 2009). Violentstorms (like those seen on Jupiter), along with magnetic-activity-inducing aurorae, have been noted as environ-mental conditions likely to be present at the L-T transi-tion ( Metchev et al. 2015, Radigan et al. 2012, Apai et al.2013, Hallinan et al. 2015, Buenzli et al. 2014,Gillon et al.2013, Buenzli et al. 2015, Faherty et al. 2014a, Burgasseret al. 2014).
Confounding our understanding of cloud formation inlow-temperature atmospheres is mounting evidence fora correlation between cloud properties and youth. Lowsurface gravity brown dwarfs, thought to be young, haveunusually red near to mid-infrared colors and a fainterabsolute magnitude through ∼ 2.5 µm when compared totheir older spectral counterparts with field surface grav-ities (Faherty et al. 2012, Faherty et al. 2013, Filippazzoet al. 2015, Liu et al. 2013, Gagne et al. 2015b). Metchev& Hillenbrand (2006) made the first connection betweenage and cloudiness in their study of the young companionHD 203030B, whose transition to the cloud-free T spec-tral class appears to be delayed by the presence of thickclouds. In a detailed study of the prototypical isolated,young brown dwarf 2M0355+1133, Faherty et al. (2013)found that the deviant colors and fainter absolute mag-nitudes were best explained by enhanced dust, or thickphotospheric clouds, shifting flux to longer wavelengths.At the coldest temperatures, where clouds should allbut have dispersed below the photosphere in field browndwarfs, Burgasser et al. (2010b) studied the T8 dwarfRoss 458 C and found clouds must be considered as animportant opacity source for young T dwarfs.
Exoplanet studies have independently found similartrends with age and cloud properties. The young plan-etary mass companions 2M1207 b (< 10 MJup) andHR8799 b (< 10 MJup), are exceedingly red in the near-infrared and up to 2 magnitudes fainter than field browndwarfs of similar Teff (Marois et al. 2008, 2010, Mohantyet al. 2007). To reproduce their anomalous observables,theorists have developed “enhanced” cloudy atmosphericmodels with non-equilibrium chemistry (Marley et al.2012, Barman et al. 2011a,b, Madhusudhan et al. 2011)in which lower surface gravity alters the vertical mixingwhich then leads to high altitude clouds with differingphysical composition (e.g. thicker or thinner aggrega-tions).
In general, M, L, T, and Y classifications identifybrown dwarfs. If the source is older (> 2 - 3 Gyr),late-type M and early L dwarfs are stars. But if thesource is young (< 1 Gyr), even those warmer classifi-
cations will describe an object that is < 75 MJup. Todate, all directly imaged giant exoplanets have observ-able properties which lead to their classification squarelyin this well-studied regime. Planetary mass companionssuch as 2M1207 b, 51 Eri b, β Pictoris b, ROXs 42Bb, and the giant planets orbiting HR8799, have observ-ables that are similar to L or T brown dwarfs (Chauvinet al. 2004, Macintosh et al. 2015, Lagrange et al. 2010,Marois et al. 2008, 2010, Currie et al. 2014, Kraus et al.2014). Furthermore, there exists a population of “classi-cal” brown dwarfs that overlap in effective temperature,age – many in the same moving group – , and mass withdirectly observed planetary mass companions (e.g. PSO318, SDSS1110, 0047+6803, Liu et al. 2013, Gagne et al.2015c, Gizis et al. 2012, 2015). Studies of these two pop-ulations in concert may resolve questions of the forma-tion of companions versus isolated equivalents as well asuntangle atmosphere, temperature, age, and metallicityeffects on the observables.
In this work we examine this new population of sus-pected young, low surface gravity sources that are ex-cellent exoplanet analogs. In section 2 we explain thesample examined in this work and in section 3 we de-scribe the imaging and spectral data acquired. In section4 we review new near-infrared spectral types designatedin this work and in section 5 we discuss how we measurednew radial velocities. In section 6 we assess the likelihoodof membership in nearby moving groups such as β Pic-toris, AB Doradus, Argus, Columba, TW Hydrae, andTucana Horologium. In section 7 we review the diversityof the whole sample in spectral features, infrared colors,absolute magnitudes, bolometric luminosities and effec-tive temperatures. In section 8 we place the young browndwarf sample in context with directly imaged planetarymass companions. Conclusions are presented in section9.
2. THE SAMPLE
Given the age-mass degeneracy of substellar mass ob-jects and an age range of ∼5 - 130 Myr for groups suchas TW Hydrae (5-15 Myr; Weinberger et al. 2013), βPictoris (20-26 Myr; Binks & Jeffries 2014, Malo et al.2014), and AB Doradus (110 - 130 Myr; Barenfeld et al.2013, Zuckerman et al. 2004) the target temperature forour sample was Teff < 3000 K, or, equivalently, sourceswith spectral types of M7 or later. This cut-off restrictedus to < 0.07 M� or the classic brown dwarf boundary(Kumar 1963, Hayashi & Nakano 1963).
The suspicion of membership in a nearby moving groupshould be accompanied by observed signatures of youthas kinematics alone leave doubt about chance contami-nation from the field sample. As such, for this work wefocused on > M7 objects with confirmed spectral signa-tures of low-gravity in either the optical or the infrared.We note that while there are isolated T dwarfs thoughtto be young (e.g. SDSS 1110, Gagne et al. 2015a, CF-BDSIR 2149, Delorme et al. 2012), their spectral pecu-liarities appear to be subtle making them more difficultto identify and investigate (see also Best et al. 2015).
For isolated late-type M and L dwarfs suspected tobe young, there are strong spectral differences in thestrength of the alkali lines and metal oxide absorptionbands as well as the shape of the near-infrared H- band(∼1.65 µm) compared to older field age counterparts (e.g.
Brown Dwarf Analogs to Exoplanets 3
Lucas et al. 2001; Gorlova et al. 2003; Luhman et al.2004; McGovern et al. 2004; Allers et al. 2007; Rice et al.2010, 2011, Patience et al. 2012; Faherty et al. 2013).Physically this can be explained by a change in the bal-ance between ionized and neutral atomic and molecularspecies, as a result of lower surface gravity and, con-sequently, lower gas densities in the photospheric lay-ers (Kirkpatrick et al. 2006). Furthermore, a lower sur-face gravity is linked to an increase in collision inducedH2 absorption (see e.g. Canty et al. 2013, Tokunaga &Kobayashi 1999). Changes in the amount of this absorp-tion result in the K- band (∼ 2.2 µm) being suppressed(or enhanced) and the shape of the H band being mode-ified to cause the “peaky” H band relative to water opac-ity seen in young sources (see Rice et al. 2011).
The collection of brown dwarfs with spectral signaturesof a low-surface gravity is increasing13. Gagne et al.(2014c, 2015b,c) presented a bayesian analysis of thebrown dwarf population looking for potential new mov-ing group members and uncovered numerous low-gravitysources. Allers & Liu (2013) presented a near-infraredspectroscopic study of a large number of known sources.Aside from those extensive studies, objects have been re-ported singly in paper (e.g. Kirkpatrick et al. 2006, Liuet al. 2013, Gagne et al. 2014a,b, 2015a, Faherty et al.2013, Rice et al. 2010, Gizis et al. 2012, Gauza et al.2015) or included as a subset to a larger compilation offield objects (e.g. Cruz et al. 2007, Kirkpatrick et al.2010, Reid et al. 2007, Thompson et al. 2013). The ob-jects within this paper were drawn from the literatureas well as our ongoing search for new low-surface gravityobjects.
The 15214 low-surface gravity objects examined in thiswork are listed in Table 1 with their coordinates, spectraltypes, gravity classifications (optical and infrared as ap-plicable), 2MASS and WISE photometry. There are 48sources in this sample that are lacking an optical spectraltype and 8 sources lacking an infrared spectral type. Ofthe 96 objects with both optical and near-infrared data,there are 67 sources (70%) that have a different opticalspectral type than the infrared although the majority arewithin 1 subtype of each other.
For assigning a gravity designation, there are two clas-sification systems based on spectral features. The Cruzet al. (2009) system uses optical spectra and assigns alow-surface gravity (γ), intermediate gravity (β), or fieldgravity (‘—’ in Table 1 and throughout) based on thestrength of metal oxide absorption bands and alkali lines.In certain cases a classification of δ is also used for ob-jects that look more extreme than γ (see Gagne et al.2015b). In this work we label objects as δ in tables butplot them and discuss them along with γ sources. On theCruz et al. (2009) scheme, γ and β objects are thought tobe younger than the Pleiades (age < ∼ 120 Myr, Staufferet al. 1998). The Allers & Liu (2013) system uses near-infrared spectra and evaluates spectral indices to assigna very low-gravity (vl-g), intermediate gravity (int-g), or
13 Our group maintains a listing of known isolated field ob-jects noted as having gravity sensitive features on a web-basedcompendiumhttp : //www.bdnyc.org/young bds
14 While this paper was awaiting acceptance, Aller et al. (2016)reported a sample of AB Doradus late-type M and L dwarfs. Thoseobjects are not included in this analysis but should be consideredin future work.
field gravity (fld-g) to a given source. As discussed inAllers & Liu (2013), the optical and near-infrared grav-ity systems are broadly consistent. However, to anchoreither requires an age-calibrated sample to ground thegravity designations as age-indicators.
Figure 1 shows a histogram distribution of the spec-tral subtypes in the optical and the infrared highlightingthe gravity classification. There are 51 objects classifiedoptically as γ and 80 with the equivalent infrared clas-sification. There are 27 objects classified optically as βand 57 with the equivalent infrared classification. Of theobjects which have both optical and infrared gravity des-ignations, 16 sources (17%) have different gravity classifi-cations from the two methods and 23 objects (24%) havea low-gravity infrared classification but are not noted aspeculiar in the optical. For simplification of the text (andin large part because the two systems are generally con-sistent), we have adopted the convention that any objectclassified as vl-g or int-g in the infrared is referred to asγ or β (respectively) in the text, Tables, and Figures.
3. DATA
The sample of 152 M7-L8 ultracool dwarfs comprisingour sample were placed on follow-up programs – eitherimaging (parallax, proper motion), spectroscopy (radialvelocity) or both – to determine kinematic membershipin a nearby moving group. Below we describe the datacollected for the suspected young brown dwarf sample.
3.1. Parallax and Proper Motion Imaging
The astrometric images for this program were obtainedusing three different instruments and telescopes in thenorthern and southern hemispheres. We report paral-laxes for eight low-gravity and ten field dwarfs. For 19objects, we report proper motion alone as we lack enoughepochs to decouple parallaxes. An additional 13 objectshave not yet been imaged by either the northern or south-ern instruments, and so we report proper motions usingthe time baseline between 2MASS and WISE.
3.1.1. Northern Hemisphere Targets
For Northern Hemisphere astrometry targets, we ob-tained I-band images with the MDM Observatory 2.4mHiltner telescope on Kitt Peak, Arizona. Parallaxes arebeing measured for both low-surface gravity and field ul-tracool dwarfs and for this work we report 5 of the formerand 10 of the latter (field dwarfs used for comparison inthe analysis discussed in Section 7).
For most observations at MDM, we used a thinnedSITe CCD detector (named “echelle”) with 2048x2048pixels and an image scale of 0′′.275 pixel−1. This suf-fered a hardware failure and was unavailable for someof the runs. As a substitute, we began using “Nellie”, athick, frontside-illuminated STIS CCD which gave 0′′.240pixel−1. The change in instrument made no discernibledifference to the astrometry. Table 2 gives the perti-nent astrometric information. In addition to the parallaximaging, we took V -band images and determined V − Icolors for the field stars for use in the parallax reductionand analysis. For a single target field (1552+2948) weused SDSS colors instead. The reduction and analysiswas similar to that described in Thorstensen (2003) andThorstensen et al. (2008), with some modifications.
4 Faherty et al.
Parallax observations through a broadband filter aresubject to differential color refraction (DCR). The effec-tive wavelength of the light reaching the detector for eachstar will depend on its spectral energy distribution. Con-sequently, the target and reference stars can be observedto have different positions depending on how far fromthe zenith the target is observed at each epoch. In previ-ous studies we approximated the I-band DCR correctionas a simple linear trend with V − I color, amountingto 5 mas per unit V − I per unit tan z (where z is thezenith distance of each observation). We checked this byexplicitly computing the correction for stars of varyingcolor using library spectra from Pickles (1998), a tab-ulation of the I passband from Bessell (1990), and theatmospheric refraction as a function of wavelength ap-propriate to the observatory’s elevation. The synthesizedcorrections agreed very well with the empirically-derivedlinear correction. However, the library spectra did notextend to objects as red as the present sample and mostare so faint in V that we could not measure V − I ac-curately. We therefore computed DCR corrections usingthe spectral classifications of our targets and spectra ofL and T-dwarfs assembled by Neill Reid15. The result-ing corrections typically amounted to ∼ 25 mas per unittan z, that is, the DCR expected on the basis of the linearrelation for a star with (V − I) ≈ 5.
To minimize DCR effects, we restricted the parallaxobservations to hour angles within ±2 h of the meridian.The effect of DCR on parallax is mainly along the east-west (or X) direction, and the X-component of refractionis proportional to tan z sin p, where p is the parallacticangle. This quantity averaged 0.12 for our observations,reflecting a slight westward bias in hour angle, and itsstandard deviation was 0.15. We are therefore confidentthat the DCR correction is not affecting our results un-duly.
As in previous papers, we used our parallax observa-tions to estimate distances using a Bayesian formalismthat takes into account proper motion, parallax, anda plausible range of absolute magnitude (Thorstensen2003). For these targets we assumed a large spread inabsolute magnitude, so that it had essentially no effecton the distance, and used a velocity distribution char-acteristic of a disk population to formulate the proper-motion prior. For most of the targets, the parallax πwas precise enough that the Lutz-Kelker correction andother Bayesian priors had little effect on the estimateddistance, which was therefore close to 1/π.
Table 3 lists our measured parallaxes and proper mo-tions and Table 4 shows the comparison with literaturevalues for four sources with previously reported values.In the case of MDM measured proper motions, they arerelative to the reference stars, and not absolute. Al-though the formal errors of the proper motions are typi-cally 1-2 mas yr−1, this precision is spurious in that thedispersion of the reference star proper motions is usuallyover 10 mas yr−1, so the relative zero point is correspond-ingly uncertain.
3.1.2. Southern Hemisphere Targets
We observed 16 of the most southernly targets withthe Carnegie Astrometric Planet Search Camera (CAP-
15 Available at http://www.stsci.edu/∼inr/ultracool.html
SCam) on the 100-inch du Pont telescope and five withthe FourStar imaging camera (Persson et al. 2013) on theMagellan Baade Telescope. In the case of both programs,we are continually imaging objects for the purpose ofmeasuring parallaxes. However, for this work we reportparallaxes (and proper motions) for only 3 objects withCAPScam. The remaining 18 objects (13 – CAPScam, 5– FourStar) need more epochs to decouple parallax fromproper motion and will be the subject of a future paper.
A description of the CAPSCam instrument and the ba-sic data reduction techniques are described in Boss et al.(2009) and Anglada-Escude et al. (2012). CAPSCam uti-lizes a Hawaii-2RG HyViSI detector filtered to a band-pass of 100 nm centered at 865 nm with 2048 x 2048pixels, each subtending 0.196′′ on a side. CAPSCam wasbuilt to simultaneously image bright target stars in a 64x 64 pixel guide window allowing short exposures whileobtaining longer exposures of fainter reference stars inthe full frame window (e.g. Weinberger et al. 2013). Thebrown dwarfs targeted in this program were generallyfainter than the astrometric reference stars so we workedwith only the full frame window. Data were processedas described in Weinberger et al. (2013). For exposuretimes, we used 30s - 120s for our bright targets and 150s- 300s for our faint targets with no coadds in an 8 - 12point dither pattern contained in a 15′′ box. Pertinentastrometric information for parallax targets is given inTable 2.
FourStar is a near-infrared mosaic imager (Perssonet al. 2013) with four 2048 x 2048 Teledyne HAWAII-2RG arrays that produce a 10.9′ x 10.9′ field of view at aplate scale of 0.159′′ pixel−1. Each target was observedwith the J3 (1.22–1.36µm) narrow band filter and cen-tered in chip 2. This procedure has proven successful inour astrometric program for late-T and Y dwarfs (e.g.Tinney et al. 2012, 2014, Faherty et al. 2014b). Expo-sure times of 15s with 2 coadds in an 11 point ditherpattern contained in a 15′′ box were used for each tar-get. The images were processed as described in Tinneyet al. (2014).
In the case of the 18 proper motion only targets fromeither CAPSCam or FourStar, we combine our latest im-age with that of 2MASS (∆t listed in Table 5). Propermotions were calculated using the astrometric strategydescribed in Faherty et al. (2009). Results are listed inTable 5.
For three CAPSCam targets there is sufficient data tosolve for both proper motions and parallaxes. For thesesources, the astrometric pipeline described in Weinbergeret al. (2013) was employed. Table 3 lists our measuredparallaxes and proper motions and Table 4 shows thecomparison with literature values for 0241-0326.
3.2. Low and Medium Resolution Spectroscopy
3.2.1. FIRE
We used the 6.5m Baade Magellan telescope and theFolded-port InfraRed Echellette (FIRE; Simcoe et al.2013) spectrograph to obtain near-infrared spectra of 36sources. Observations were made over 7 runs between2013 July and 2014 September. For all observations, weused the echellette mode and the 0.6′′ slit (resolutionλ/∆λ ∼ 6000) covering the full 0.8 - 2.5 µm band witha spatial resolution of 0.18′′/pixel. Exposure times for
Brown Dwarf Analogs to Exoplanets 5
each source and number of images acquired are listedin Table 6. Immediately after each science image, weobtained an A star for telluric correction and obtained aThAr lamp spectra. At the start of the night we obtaineddome flats and Xe flash lamps to construct a pixel-to-pixel response calibration. Data were reduced using theFIREHOSE package which is based on the MASE andSpeX reduction tools (Bochanski et al. 2009, Cushinget al. 2004, Vacca et al. 2003).
3.2.2. IRTF
We used the 3m NASA Infrared Telescope Facil-ity (IRTF) to obtain low-resolution near-infrared spec-troscopy for 10 targets. We used either the 0.′′5 slit orthe 0.′′8 slit depending on conditions. All observationswere aligned to the parallactic angle to obtain R ≡ λ /∆λ ≈ 120 spectral data over the wavelength range of 0.7– 2.5 µm. Exposure times for each source and number ofimages acquired are listed in Table 6. Immediately aftereach science observation we observed an A0 star at a sim-ilar airmass for telluric corrections and flux calibration,as well as an exposure of an internal flat-field and Ar arclamp. All data were reduced using the SpeXtool packageversion 3.4 using standard settings (Cushing et al. 2004,Vacca et al. 2003).
3.2.3. TSpec
We used the Triple Spectrograph (TSpec) at the 5 mHale Telescope at Palomar Observatory to obtain near-infrared spectra of two targets. TSpec uses a 1024 x2048 HAWAII-2 array to cover simultaneously the rangefrom 1.0 to 2.45µm (Herter et al. 2008). With a 1.1x 43′′ slit, it achieves a resolution of ∼2500. Observa-tions were acquired in an ABBA nod sequence with anexposure time per nod position of 300s (see Table 6) soas to mitigate problems with changing OH backgroundlevels. Observations of A0 stars were taken near in timeand near in airmass to the target objects and were usedfor telluric correction and flux calibration. Dome flatswere taken to calibrate the pixel-to-pixel response. Datawere reduced using a modified version of Spextool (seeKirkpatrick et al. 2011).
3.3. High Resolution Spectroscopy
3.3.1. Keck II NIRSPEC
The Keck II near-infrared SPECtrograph (NIRSPEC)is a Nasmyth focus spectrograph designed to obtain spec-tra at wavelengths from 0.95 – 5.5µm (McLean et al.1998). It offers a choice of low-resolution and cross-dispersed high resolution spectrographic modes, with op-tional adaptive optics guidance. In high-resolution mode,it can achieve resolving powers of up to R=25000 usinga 3 pixel entrance slit, with two orders visible on theoutput spectrum (selectable by filter).
Multiple observations of 17 sources were taken in highresolution mode on Keck II on 14, 15, and 16 September2008, using the NIRSPEC-5 filter to obtain H-band spec-tra in Order 49 (1.545 – 1.570µm). Observational datafor each source are listed in Table 7. The data were re-duced using the IDL-based spectroscopy reduction pack-age REDSPEC. Many of our observations had very lowsignal-to-noise, and so multiple exposures were co-addedbefore extracting spectra. We tested this procedure by
using objects with sufficient signal-to-noise prior to co-adding, and by comparing individual against co-addedspectra. The resulting individual exposure spectra werealmost identical to those obtained by co-adding prior torunning REDSPEC reductions. Heliocentric radial ve-locity corrections were calculated with the IRAF taskrvcorrect , and applied using custom python code.
3.3.2. Gemini South Phoenix
The Phoenix instrument (previously on Gemini South)is a long-slit, high resolution infrared echelle spectro-graph, designed to obtain spectra between 1 – 5 µm atresolutions between R=50000 and R=80000. Spectra arenot cross-dispersed, leaving only a narrow range of a sin-gle order selectable by order-sorting filters.
Observations of 18 sources were taken during semester2007B and 2009B using the H6420 filter to select H-bandspectra in Order 36 (1.551 – 1.558 µm). Spectra werereduced using the supplied IDL Phoenix reduction codes.Observational data for each source are listed in Table 7.
3.3.3. Magellan Clay MIKE
The Magellan Inamori Kyocera Echelle (MIKE) on theMagellan II (Clay) telescope is a cross-dispersed, highresolution optical spectrograph, designed to cover the en-tire optical spectrum range (divided into two channels,blue: 0.32 – 0.48 µm, and red: 0.44 – 1.00 µm) at aresolving power of R∼28,000 (blue) and R∼22,000 (red)using the 1.0” slit. The output spectra contain a largerange of overlapping echelle orders, each covering roughly0.02µm of the red optical spectrum.
Red-side spectra were taken on 4 July 2006, 1 Novem-ber 2006, and 2 November 2006. The observations com-prise 17 target and standard spectra, with additionalB-type and white dwarf flux calibrators. Observationaldata for each source are listed in Table 7. Spectra werereduced using the IDL MIKE echelle pipeline16, and or-ders 38 – 52 (0.92 – 0.65µm) were extracted from everyspectrum. Many of those orders were unusable for ourpurposes, and were not used in the final solutions. Tel-luric atmospheric features dominate the wavebands cov-ered by orders 38 (telluric O2), 45 (A band), and 50 (Bband). The orders higher (bluer) than 44 typically hadinsufficient signal due to the extreme faint and red colorsof the target objects.
4. NEW NEAR-INFRARED SPECTRAL TYPES
We obtained spectra with FIRE, SpeX, and TSpecfor 43 targets to investigate near-infrared signatures ofyouth. Each object had either demonstrated optical low-surface gravity features, but were missing (or had poor)near infrared data, or had low signal to noise near in-frared spectra. Determining the spectral type and grav-ity classification for peculiar sources has its difficulties.Primarily because one wants to ground the peculiar ob-ject type by comparing to an equivalent field source.However, as will be seen in section 7, the low grav-ity sequence does not easily follow from the field se-quence. In the infrared, Allers & Liu (2013) have pre-sented a method for determining gravity classification us-ing indices. Alternatively, the population of low gravity
16 http://web.mit.edu/burles/www/MIKE/ checked 19 JUNE2014
6 Faherty et al.
sources (especially earlier L types) has grown in numbersuch that templates of peculiar sources can be made forcomparison (e.g. Gagne et al. 2015b, Cruz et al. submit-ted). For this work, we have defaulted to a visual matchto templates or known sources – grounded by their opti-cal data – as our primary spectral typing method. How-ever we also check each source against indices to ensureconsistency.
In the case of each new spectrum, we visually comparedto the library of spectra in the SpeX prism library17 aswell as the low gravity templates discussed in Gagne et al.2015b. For the FIRE and TSpec echelle spectra, we firstbinned them to prism resolution (∼ 120). This visualcheck to known objects gave the match we found mostreliable for this work in both type and gravity classifi-cation and it is listed in the “SpT adopted” column inTable 9. Figures 3 - 4 show two example spectra (prismand binned down FIRE data) compared visually to bothfield and very low gravity sources, as representations ofour spectral typing method.
As a secondary check, we report the indices analysisof each object. A near infrared spectral subtype is arequired input for evaluating the gravity classificationwith the Allers & Liu (2013) system so we first appliedthe subtype indices (as described in Allers & Liu 2013)and list the results in the “SpT Allers13” column in Table9. Once we had determined the closest near infraredtype, we evaluated the medium resolution (for FIRE andTSpec data) and/or the low resolution gravity indices(for Prism data). We list the results of each in Table9. In general we found that matching visually to lowgravity templates or known objects versus using indiceswere consistent within 1 subtype.
5. RADIAL VELOCITIES
Radial velocities from NIRSPEC, Phoenix, and MIKEwere calculated using a custom python routine, whichuses cross-correlation with standard brown dwarfs toachieve 1 km s−1 radial velocity precision. Useable spec-tra have resolving power of R=20,000 or higher, and gen-erally signal-to-noise of at least 20. All data were cor-rected to heliocentric radial velocity by shifting the wave-length grid. Brown dwarf standards – sourced primarilyfrom Blake et al. (2010) – were observed and correctedwith the same settings as the targets, and paired withobjects of matching spectral type. Given that our radialvelocity sample is bimodal with peaks at L0 and L4, ourspectra are fit against relatively few standards.
The python code calculates radial velocities on the fly,and operates on optical and infrared data without modi-fication. The radial velocity inputs were the wavelength,flux, and uncertainty data as three one-dimensional ar-rays, for both the target and the standard. The targetand standard spectra were first cropped to only the por-tion where they overlap, and then interpolated onto alog-normal wavelength grid.
From there, 5000 trials were conducted with differ-ent randomized Gaussian noise added to the wavelengthgrids of the target and standard, according to the per-element uncertainties. This was done to account for theuncertainties on the fluxes and to provide a method ofquantifying the uncertainty on the output radial velocity.
17 http://pono.ucsd.edu/∼adam/browndwarfs/spexprism/
For each of the 5000 trials, the two spectra were cross-correlated to produce a wavelength shift between them.A small 400-element region around the peak of the cross-correlation function was fit with a Gaussian and a linearterm, to locate the exact peak of the cross-correlationon a sub-element basis. The widths (and therefore per-measurement errors) of the cross-correlation peak werediscarded, assumed to be accounted for in the actualspread of the resulting set of peaks.
The results of the 5000 trials formed (in well-determined cases) a Gaussian histogram centered on theradial velocity shift between the two systems. The widthof that Gaussian was taken to represent the uncertaintyin the measured radial velocity. This pixel shift was con-verted into km s−1 radial velocity, and corrected for theknown velocity of the standard. Semi-independent verifi-cation of the radial velocities was accomplished by mea-suring the velocity relative to two different standards,or where available, using multiple orders from the samespectrum.
The process was sensitive to virtually all unwanted pro-cesses that produce features in the brown dwarf spectra.Chief among these were cosmic rays and detector hot pix-els, which were pixel-scale events removed from the spec-tra prior to interpolation onto the grid and provide verylittle signal in the RV correlation. The most importanteffect was telluric lines, which appeared like normal spec-tral features but did not track the radial velocity of thestar. These were dealt with by identifying orders whosecontamination was severe enough to produce discordantradial velocities and avoiding them in the analysis.
Table 7 lists the final radial velocity values for eachsource. Table 8 shows a comparison of sources for whichthere was a literature value.
5.1. Instrument-specific Differences
MIKE data has multiple echelle orders, and allstars were measured against two L2 dwarf standards:LHS 2924 and BRI 1222-1221 (Mohanty et al. 2003). Allorders were examined by eye, and determinations weremade as to whether they contained sufficient signal fora believable radial velocity. This was corroborated bycross-checking the result against other orders from thesame star and radial velocity. Some orders had broadercross-correlation functions, and the Gaussian was fit toa 200 pixel region around the peak rather than the stan-dard 100 pixels. In other orders, a small a-physical sec-ondary peak in the final results appeared, and was re-moved from the Gaussian fit for the final radial velocityfor that order.
After visual inspection, the most consistent orders –both within the match between the two stars, and be-tween the two standards – were combined into a weightedmean and weighted standard deviation. For all stars,the results of orders 39-44, collectively covering 0.77µm– 0.89µm – were deemed sufficiently reliable (despite thepresence of telluric water features) to be used in the finalresult.
6. COMPUTING KINEMATIC PROBABILITIES IN NEARBYYOUNG MOVING GROUPS
Among the 152 brown dwarfs investigated for kine-matic membership in this work, we report 37 new radialvelocities, 8 new parallaxes, and 33 new proper motions
Brown Dwarf Analogs to Exoplanets 7
(13 of which are reported as new from 2MASS to WISEproper motion measurements). In total 27 targets havefull kinematics (a parallax, proper motion and radial ve-locity), and the remaining 123 have only partial kine-matics – 16 have a parallax and proper motion but noradial velocity, 26 have radial velocity and proper mo-tion but no parallax, and 81 have proper motions but noparallax or radial velocity measurement. All astrometricinformation for this sample is listed in Table 10.
As discussed in Section 2, there are 51 objects classifiedoptically as γ and 80 with the equivalent infrared clas-sification. There are also 27 objects classified opticallyas β and 57 with the equivalent infrared classification.Given the gravity indications, we regard each object asa potentially young source and investigate membershipin a group within 100 pc of the Sun. To assess the likeli-hood of membership, we employed four different tools toexamine the available kinematic data:
• BANYAN-I Bayesian statistical calculator (Maloet al. 2013) and its successor,
• BANYAN-II (Gagne et al. 2014d),
• LACEwING (Riedel 2015), and
• Convergent point method of Rodriguez et al.(2013).
The plurality of measurements in combination with avisual inspection of an objects kinematics against bonafide members listed in (Malo et al. 2013) along with theindividual kinematic boxes of Zuckerman & Song (2004)drove our decision on group membership.
The four different methods test for membership in dif-ferent sets of groups - LACEwING considers 14 distinctgroups, BANYAN I and II consider 7 groups (or 8 in-cluding the “Old” object classification), and the conver-gence method tests for membership in 6 groups. Eachmethod has its benefits and flaws. For instance BanyanI is a fast bayesian formalism that uses flat priors butassumes (probably unrealistically) that radial velocity,and proper motion in a given direction are Gaussian.Banyan II deals better with transforming measurementsto probabilities based on the distribution of known mem-bers (does not assume a Gaussian distribution) howeverit likely has incomplete/imperfect lists of bonafide mem-bers. LACEwING is similar to Banyan I in its assump-tion that radial velocity, and proper motion in a givendirection are Gaussian but it requires fitting a model to a(arguably much cleaner list of) bonafide members of mul-tiple groups not covered by the other methods. The con-vergent point method is a simple yet different approachthat estimates the probability of membership in a knowngroup by measuring the proper motions in directions par-allel and perpendicular to the location of a given groupsconvergent point. Unfortunately, this method does nottake into account measured radial velocities or distances.Given the benefits and flaws of each method, we chose totake the output of each into consideration as we decidedon membership for each target. For an adequate com-parison, we only considered membership in six groups:TW Hydrae, β Pictoris, Tucana Horologium, Columba,Argus (which is not tested by the Convergence code),and AB Doradus. All other groups could not be consis-tently checked. Therefore they may be mentioned (e.g.
Chamaeleon near, Octans, Hyades) but are only consid-ered tentative until further kinematic investigation.
Furthermore, the output of each code should be viewedslightly differently. In Malo et al. (2013), the authorsadopt a membership probability threshold of 90% to re-cover bona fide members. Banyan II supplements with acontamination probability and finds this number shouldbe < a few percent with a high membership probability(we impose > 90% based on Banyan I) in order to recoverbona fide members (Gagne et al. 2014d). LACEwING (asdescribed in Riedel 2015) finds < 20% - 60% is low prob-ability and > 60% is high probability for group member-ship. Convergent point reports distinct probabilities foreach group between 0 - 100% (hence objects can have >90% probability of membership in more than one group).As with Banyan I, we impose > 90% as a high probabilitythreshold for membership on convergent point as well.
In assessing the membership probability, we found fourdifferent categories for describing an object:
• Non-member, NM: An object that is kinematicallyeliminated from falling into a nearby group regard-less of future astrometric measurements
• Ambiguous member, AM: An object that requiresupdated astrometric precision because it could ei-ther belong to more than one group or it can notbe differentiated from the field
• High-likelihood member, HLM: An object thatdoes not have full kinematics but is regarded ashigh confidence (> 90% in Banayan I, > 90% inBanyan II with < 5% contamination, > 90% inconvergent point, > 60% in LACEwING) in threeof the four codes, and
• Bona fide member, BM: An object regarded as ahigh-likelihood member with full kinematics (paral-lax, proper motion, radial velocity) demonstratingthat it is in line with known higher mass bona fidemembers of nearby groups.
6.1. Full Kinematic Sample
For the 28 targets with full kinematics, we compute theXYZ spatial positions and UVW velocities following theformalism of Johnson & Soderblom (1987), which em-ploys U/X in the direction of the Galactic center, pro-viding a right-handed coordinate system. In general, theresulting values are limited by the parallax precision. Forthese 28 objects, visual inspection against the positionsand velocities of the bona fide members in each group (aslisted by Malo et al. 2013) gave an obvious and strongindication of membership. We used the four other meth-ods listed above as confirmation for the visual inspec-tion. The XYZ spatial positions and UVW velocities forsystems with full kinematic information are given in Ta-ble 11. A visual example of the phase-space motions of0045+1634, a new bona fide member of Argus, is shownin Figure 2. Among the full kinematic sample, we found11 objects stand out as bona fide members, 9 objectsare classified as ambiguous, and 8 are classified as non-members. The outcome of assessing the likelihood ofmembership from each kinematic method is listed in Ta-ble 12.
8 Faherty et al.
6.2. Partial Kinematic Sample
Having only partial kinematics for 124 objects limitsour ability to definitively place these targets in a nearbygroup. As stated above, the BANYAN I/II, ConvergentPoint, and LACEwING methods use varying techniquesto yield membership probabilities. We list the outcomesof assessing the likelihood of membership for each sourcein Table 12. As can be seen from this tabulation, theresults varied across methods. In the case of an objectlike 2322-6151, all methods yield a probability of mem-bership in the Tucana Horologium moving group withthree of the 4 yielding > 90% membership. The mostdifficult cases were objects like 1154-3400, where eachmethod yielded a moderate to high probability in a dif-ferent group (Banyan I and Banyan II both predict Ar-gus, LACEwING predicts TW Hydrae, and Convergentpoint predicts Chameleon-near). Our approach to theanalysis was to be conservative with group membershipto eliminate assigning objects to groups that were un-certain. In all we concluded that there were 28 objectsto be regarded as high likelihood members (HLM) of aknown group, 83 objects that were ambiguous (AM), and13 objects that were non-members (NM). Adding thefull kinematic sample the final tally is 28 high likelihoodmembers (HLM), 11 bona fide group members (BM), 92ambiguous (AM), and 21 non-members (NM).
6.3. Comparison with Previous Works
Among the 152 brown dwarfs examined in this work,11 are newly identified as low-gravity and 141 have beenpreviously discussed in the literature for membership ina nearby moving group (e.g. Gagne et al. 2015b,c). Sev-eral of the objects – 2M0355, PSO318, 0047+6803, 1741-4642, 2154-1055, 0608-2753 – have been the subject ofsingle-object papers (Faherty et al. 2013, Liu et al. 2013,Schneider et al. 2014, Gagne et al. 2014a,b, Rice et al.2010). The remaining 129 objects were examined formembership in a nearby group primarily by Gagne et al.(2014d) – hereafter G14 – , and Gagne et al. 2015b –hereafter G15 – using BANYAN II.
There are 69 objects from our sample included in G14,73 objects in G15 and 6 in both. In G14, there is a hi-erarchical probability structure that categorizes poten-tial members as: (1) Bona fide, (2) High probability, (3)Moderate probability and, (4) Low Probability18. Thatstructure is not used in G15, but replaced by noting theprobability of membership in a group (multiple groups ifdeemed necessary) along with its contamination poten-tial.
Of the 69 objects from our sample examined in G14,three objects – 2M0355, 2M0123, and TWA 26 – weredeclared bona fide members of AB Doradus, TucanaHorologium, and TW Hydrae respectively. A further 29objects were deemed high probability members of Argus(2), AB Doradus (5), β Pictoris (4), Columba (4), andTucana Horologium (14). Ten objects were deemed mod-est probability members of AB Doradus (3), β Pictoris(3), Columba (1), Argus (1), and Tucana Horologium(2). Eight objects were deemed low probability mem-bers of Argus (1), AB Doradus (1), β Pictoris (4), and
18 See the G14 paper for a detailed description of how to inter-pret each probability category’
TW Hydrae (2). There were also 16 objects designatedas young field sources (aka “no group membership pos-sible”) and 3 objects designated as peripheral membersor contaminants in a group.
In Table 12, we use our new kinematics and show thepredictions from BANYAN I, BANYAN II, LACEwING,the convergent point and our plurality decision based onreviewing the results from all four methods with updatedastrometric measurements for many of the sources. Forthe G14 overlap, we agree with 2M0355, 2M0123, andTWA 26 being considered bona fide members. Amongthe high-likelihood sample from G14 we add a new ra-dial velocity, parallax, and/or proper motion to 19 ofthe 29 objects and confirm 11 objects as high-likelihoodmembers and demote 5 objects to ambiguous or non-member. Our re-evaluation of the kinematics also leadsus to demote 3 objects to ambiguous members ratherthan considering them high-likelihood sources in a givengroup. Among the moderate and low probability objectsin G14, we add new kinematics to 8 objects and find 5remain ambiguous and 3 are demoted to non-members.Our re-evaluation of the kinematics finds that 15 of thelow or moderate probability sources are ambiguous there-fore we can not say anything about membership. Theremaining 19 sources that were young field, periphery, orcontaminants in G14 are ambiguous or non-members inour analysis.
For the 67 objects in G15, we add three new kinematicpoints. One object is deemed high-likelihood while theother 2 are ambiguous. Otherwise, our re-evaluation ofthe kinematics leads us to classify 13 objects as high-likelihood members of groups while the remaining 54 areambiguous (52) or non-members (2).
In all, we find that when the Bayesian II analysis pre-dictions find group members have a high-likelihood ofmembership in a single group (> 99%) while yielding acontamination probability of <1%, the various kinematicmethods are consistent in their predictions and we takethis to mean that the source is a reliable member.
7. DIVERSITY OF YOUNG BROWN DWARFS
Each one of these moving group members is a possiblebenchmark for examining the evolutionary properties ofthe brown dwarf and directly imaged exoplanet popula-tions. In this section we evaluate the homogeneity anddiversity of the sample as a whole as well as the subsam-ples from each moving group.
7.1. Do Gravity Classifications Correspond With Age?
In total there are 51 optically classified γ objects (80infrared classified equivalents) as well as 27 optically clas-sified β objects ( 57 infrared equivalents). We confirm 20(28) of the γ objects and 5 (7) of the β objects respec-tively as high confidence or bona fide members of movinggroups. There are an additional 19 (44) γ objects and17 (41) β objects regarded as ambiguous members to aknown group, and 12 (10) γ objects and 5 (8) β objectsfound to be non members. As stated in Section 2, γclassified sources have spectral features indicating thatthey are a lower surface gravity than the β classified ob-jects. Furthermore, β classified sources are subtly butdistinctively different from the field sample, indicating– as noted in Allers & Liu 2013 and Cruz et al. 2009–that they are also younger but not to the extent of the γ
Brown Dwarf Analogs to Exoplanets 9
objects. The age calibrated sample allows us to test howwell gravity features trace the age of an object.
In Table 13, we list the new members of each groupas well as their optical and/or near-infrared spectral andgravity classification. As stated in section 6.1, nine bonafide objects have full kinematics. For the 28 sources miss-ing a radial velocity or parallax but regarded as highconfidence members to a group, we list the kinematicallypredicted radial velocity and/or parallax from BANYANII – checked to be consistent with LACEwING predic-tions – in parentheses in Table 13.
In TW Hydrae and β Pictoris, which are the twoyoungest groups at ∼ 10 and ∼ 20 Myr respectively, thereare nine M7 or later objects, all of which have a gravityclassification of γ in both the infrared and optical. InAB Doradus, the oldest association at ∼110 - 130 Myr,there are eight sources with 4 optical γ (6 infrared) and1 optical β (2 infrared) objects. Similarly, in TucanaHorologium, where we have the most number of bonafide or high-likelihood members, 20 M7 or later, thereare 9 optical γ (10 infrared) and 3 optical β (5 infrared)objects.
Splitting the sample of BM/HLM objects into < 25Myr (β Pictoris, TW Hydrae), ∼ 40 Myr (TucanaHorologium, Columba, Argus), and > 100 Myr (AB Do-radus) categories, and using the default spectral typeand gravity classes used in plots within this text, we findthere are (9 γ, 0 β) in < 25 Myr, (14 γ, 8 β) in ∼ 40Myr, and (6γ, 2 β) in > 100 Myr associations. Whilethese are still small numbers, the lack of a correlation ofnumbers of (γ, β) objects as a function of bin, indicatesthat spectral features do not correspond one to one withage. We note that there are 25 objects that have both aninfrared and optical spectral type and while 6 have dif-fering gravity classifications, 19 are consistent with eachother affirming the diversity. Clearly, what have beenassigned as gravity sensitive features are influenced bysecondary parameters (see also discussions in Allers &Liu 2013, Liu et al. 2013, G15).
7.2. Photometric Properties: What Do the Colors TellUs?
The majority of flux for a brown dwarf emerges in theinfrared. Interestingly, an enormous amount of diversityamong the population can be found by examining in-frared colors alone (e.g. Kirkpatrick et al. 2008, Fahertyet al. 2009, 2013, Schmidt et al. 2010).
As quantified in Tables 15 - 16 and visualized in Fig-ures 5 - 14, the scatter for “normal” sources is pro-nounced, especially among the mid- to late- L dwarfs.Past works have attributed this to variations in effectivetemperature, metallicity, age, or atmosphere conditions(Faherty et al. 2013, Kirkpatrick et al. 2008, Patten et al.2006, Knapp et al. 2004).
In Figures 5 - 14 we plot infrared color combinationsfor the population. These can be used to examine trendsor lack thereof among the new age-calibrated sample.The spread for “normal” objects (grey shaded area) inFigures 5 - 14 was created by isolating sources withoutpeculiar spectral features (e.g. subdwarfs, low-gravityobjects, and unresolved binaries were eliminated), andonly keeping sources with photometric uncertainties inthe color shown < 0.2 mag. The list was gathered from
the dwarfarchives19 compendium and supplemented withthe large ultra cool dwarf surveys from Schmidt et al.(2010), Mace et al. (2013), Kirkpatrick et al. (2011), andWest et al. (2008) (for M dwarfs).
For the low gravity sample, spectral types, as well asgravity classifications, are from optical data unless onlyinfrared was available. We note that most sources plot-ted have spectral type uncertainties of 0.5. However, ascan be seen in Table 1, low-gravity sources can have upto a 2 type difference in subtype, as well as differinggravity indications between the optical and the infrared.We investigated whether isolating the smaller samplesof optical only or infrared only yielded different trendsthan this mixed sample, but found similar results in allcases. Hence we default to optical classifications anddesignations where available, as this is the wavelengthrange where the original spectral typing schemes for thisexpected temperature range were created.
Overplotted on the grey field sequences in Figures 5 -14 are the individual γ or β low-gravity objects. We havecolor coded each source by the group it has been assignedor labeled it as “young field?” for those with ambiguousor non conforming group kinematics. We have also giventhe β and γ objects different symbols so their trendscould be highlighted. Tables 17 - 18 give the infraredcolor of each source as well as its deviation from themean (see Tables 15 - 16) of normal objects in its spectralsubtype.
In general, the γ and β sources are systematically red-der than the mean for their subtype with the deviationfrom “normal” increasing with later spectral subtypes.Objects are most deviant from normal in the (J-W2)color (Figure 8) where they are an average of 2σ (orup to 1.85 mag) redder than the subtype mean valueacross all types, and least deviant in the (J-H) color(Figure 5) where they are an average of ∼ 0.7σ (or upto 0.6 mag) redder than the subtype mean value acrossall types. Typically, the γ sources mark the extreme redphotometric outliers for each subtype bin, although thereare a handful of extreme β sources (e.g. 0153-6744, aninfrared L3 β).
The difference in age between the oldest moving groupinvestigated and the average age for field sources is morethan ∼ 3 Gyr (field age references Burgasser et al. 2015,Seifahrt et al. 2010, Faherty et al. 2009). As shown inFigures 5 - 14, the difference in photometric propertiesacross this large age gap is distinct. We also investigatedthe more subtle age difference changes to the photometricproperties across the 5 - 130 Myr sample. Isolating thesources that are confidently associated with a movinggroup, we conclude that there is no obvious correlationbetween the extreme color of an object and the age of thegroup. For example, 5-15 Myr TW Hydrae late-type Mand L dwarfs, 25 Myr β Pictoris spectral equivalents and30 -50 Myr Tucana Horologium spectral equivalents havesimilar photometric colors. The exceptions are TWA27Aand TWA28, which are 2-5σ redder than similar objectsin several colors. We note that Schneider et al. (2012a,b)postulate that these sources may have disks hence theirsurroundings may be contributing to the colors.
Comparing internally within the same moving group(assumed to have the same age and metallicity) we find
19 http://www.dwarfarchives.org
10 Faherty et al.
that objects of the same spectral subtype show a largediversity in their photometric colors. The best exampleis at L0 where there are 5 Tucana Horologium members.The objects have systematically redder colors, but theyare distributed between 1-4σ from the field mean indicat-ing that since this is a coeval group, diversity must bedriven by yet another parameter. We note that depend-ing on the exact formation mechanism, metallicity varia-tions can not be completely outruled as also contributingto the diversity among objects in the same group.
Plotted as grey symbols throughout Figures 5 - 14 areobjects that are kinematically ambiguous or unassociatedwith any known group. Many of these sources, (such asthe L4γ 1615+4953 and the very oddly reddened M8γ0435-1441 – see discussion in Allers & Liu 2013 and Cruzet al. 2003), are among the reddest objects for their spec-tral bins and rival the associated kinematic members intheir spectral and photometric peculiarities. Conversely,there are several β sources, such as the L2β 0510-1843,that fall within the normal range in each color and areonly subtly spectrally different than field sources. Unfor-tunately, with no group association, we can not commenton the likelihood of age differences driving the diversity.It is likely that within this sample, there are objects inmoving groups not yet recognized, as well as sources thatare not young but mimic low surface gravity features dueto secondary parameters (e.g. atmosphere or metallicityvariations).
7.3. Flux Redistribution to Longer Wavelengths forYounger Objects
As discussed in section 7.2 above, low surface gravitybrown dwarfs are systematically redder for their givenspectral types. Hence, one might expect that they wouldnot logically follow the absolute magnitude sequence offield equivalents. Figures 15 - 20 show MJ through MW3
versus spectral type for all low surface gravity sourceswith parallaxes or, in a select few cases, with kinematicdistances. In Table 13 we mark the 25 sources for whichwe lack a parallax but have assumed the kinematic dis-tance to a moving group since the object was assessedas a high-likelihood member. The grey area throughouteach figure is the polynomial relation for the field pop-ulation at each band recalculated with all known browndwarfs with parallaxes. We list all new relations for bothfield and low gravity objects used in or calculated for thiswork in Table 19. Throughout Figures 15 - 20, individ-ual low surface gravity objects are over plotted and colorcoded by group membership and given a symbol repre-senting their gravity designation. The lower portion ofeach figure shows the deviation of each low-gravity sourcefrom the mean absolute magnitude value of the spectralsubtype.
7.3.1. Trends with Spectral Type
Focusing on the objects associated with known groups,there is a distinct difference between the behavior oflow-gravity late-type M dwarfs and L dwarfs. In Fig-ure 15, which shows the MJ band trend, the TW Hy-drae and Tucana Horologium late-type M’s are ∼ 2 mag-nitudes brighter than the field relations whereas the Ldwarfs are normal to ∼1 mag fainter than the field rela-tions. Moving to longer wavelengths, the flux shifts. By
MW3, nearly all sources regardless of spectral type havebrighter absolute magnitudes than the field polynomial.One plausible explanation for this redistribution of fluxis dust grains in the photosphere that absorb and rera-diate at cooler temperatures (hence longer wavelengths).Equally likely is the possibility that there exists thickerclouds or that there are higher lying clouds in the at-mospheres of these sources (e.g. Marocco et al. 2013,Hiranaka et al. 2015, Faherty et al. 2013).
One main consequence of the young sources deviat-ing from the field in some bands and not in others,is that the polynomial relations that use spectral typeand photometry to obtain distances, are inappropriatefor low-surface gravity objects. At bluer near-infraredbands, they would over estimate distances, whereas atredder near-infrared bands they would under-estimate.In Table 19 we have taken this into account and presentnew spectrophotometric polynomials for suspected youngsources at J through W3 bands. As discussed in Filip-pazzo et al. (2015), the flux redistribution hinges aroundK band. As a result, we recommend this spectral dis-tance polynomial relation for suspected young sources.
7.3.2. Trends with Age
Overall, we find that there is a clear difference in thebehavior of the absolute magnitudes as a function ofspectral type for the > ∼ 3 Gyr field trends in eachband compared to the behavior of the low surface grav-ity sources. Narrowing in on the 5 - 130 Myr range andcomparing equivalent spectral type sources in differinggroups (such as the L7 sources in AB Doradus and β Pic-toris or the Tucana Horologium late- M and L dwarfs)we find that there is no obvious correlation with age andabsolute magnitude trend. In the case of PSO318 (∼ 25Myr), 1119-1137, and 1147-2040 (∼ 5 -15 Myr) versus0047+6803 (∼ 110-130 Myr) or TWA 27A (∼ 5-15 Myr)versus 0123-6921 (∼30-50 Myr), the sources switch inbrightness depending on the band, but stay within 1σ ofeach other from J (∼ 1.25µ m) through W2 (∼ 4.6µ m).By MW3 (∼ 11.56µ m), TWA 27 A is over 1 magnitudebrighter than 0123-6921 although this might be due to adisk and not due to the source (Schneider et al. 2012a,b).Regardless, it does not appear that the younger sourcesshow an extreme version of the overall trend indicatingthat whatever causes the flux redistribution compared tothe field (> 3 Gyr sample) has a near equal impact from∼5-15 Myr through ∼110-130 Myr.
7.3.3. Trends with Non-Group Members and ExpandedExplanations for Diversity
The sources with non-conforming group kinematics(grey points) do not all trace the behavior of the bonafide/high-likelihood members. For instance, all but 2 ofthe γ or β “Young Field?” M7-L1 objects stay withinthe polynomial for each band. Furthermore, all but oneof those are classified as β, which is the more subtly al-tered gravity type. Conversely, the L3 and L4 γ and βsources move from within the field polynomial band tobeing 1-2σ brighter than equivalent sources between MJ
and MW3.There are several explanations for why a spectroscop-
ically classified low gravity object looks normal in otherparameters. Photometric variability may contributeslightly to their position on spectrophotometric diagrams
Brown Dwarf Analogs to Exoplanets 11
(e.g. Allers et al. 2016) but it is unlikely to contributein a significant way. As shown in works such as Radiganet al. (2014), and Metchev et al. (2015), large amplitudephotometric variations (> 5%) among brown dwarfs arerare. Alternatively, rotational velocity could contributein a substantial way because it influences global circu-lation on a given source which causes or disrupts cloudpatterns. In this same vein, the distribution of cloudsby latitude on a given object may not be homogeneousin structure or grain size. Consequently, (as first pro-posed by Kirkpatrick et al. 2010) our viewing angle (e.g.pole-on or equatorial on) would impact the spectral andphotometric appearance. Unfortunately, there is littleinformation on the rotational velocity distribution of theyoung brown dwarf sample so testing this parameter willrequire additional data.
The simplest explanation is that sources falling within“normal” absolute magnitude and luminosity plots withnon-conforming kinematics to any known group may notbe young. Aganze et al. (2016) showed this to be thecase for the d/sdM7 object GJ 660.1B that had a pe-culiar near infrared spectrum which hinted that it wasyoung. However this object was co-moving with a highermass, low-metallicity star refuting that suggestion. Inthe case of GJ 660.1 B, a low-metallicity likely helpedto mimic certain spectral features of youth. In lieu ofthe fact that there may be some older contaminants inthe sample, we present all new relations in Table 19 tobe inclusive of all objects in this work with parallaxes aswell as only objects that are considered bonafide or highlikely members of groups.
7.4. Color Magnitude Trends for Young Brown Dwarfs
Color magnitude diagrams have been discussed atlength in the literature as a diagnostic of temperature,gravity, metallicity, and atmosphere properties of thebrown dwarf population (e.g. Liu et al. 2013, Fahertyet al. 2012, 2013, Filippazzo et al. 2015, G15, Dupuy& Liu 2012, Patten et al. 2006). Figures 21 - 31 showthe full suite of infrared color magnitude diagrams us-ing JHK (2MASS) and W1W2 (WISE) photometry forthe field parallax sample omitting binaries, subdwarfs,spectrally peculiar sources and those with absolute mag-nitude uncertainties > 0.5 in any band. On each plotwe color code objects by spectral ranges of < M9, L0-L4,L5-L9, T0-T4, and >T5 and we highlight the low surfacegravity objects by their gravity classification. The latesttype sources in our sample are labeled on each plot. Onselect plots, we have also labeled the M dwarf membersof β Pictoris and TW Hydrae.
For completeness of the discussion, we have includedthe one confirmed isolated T dwarf member of a mov-ing group in the analysis (SDSS1110, T5.5, Gagne et al.2015a) as well as the L7 wide companion VHS 1256 B(Gauza et al. 2015). While the latest-type L dwarfs pushthe elbow of the L/T transition to an extreme red/faintcolor/magnitude, SDSS 1110 falls near spectral equiva-lents on all color magnitude diagrams. As discussed inGagne et al. 2015c and Filippazzo et al. 2015, this sourceappears ∼150 K cooler than equivalents but does notexhibit the extreme color-magnitude properties as seenwith the L dwarfs.
Looking at a given absolute magnitude across all plotsand comparing field objects to low surface gravity ob-
jects, we find that the latter can be more than a 1 mag-nitude redder. The most extreme behavior can be seenon Figures 24 and 25 which exploits the largest wave-length difference in color (J −W2) and as discussed insection 7.2 is where the low-gravity objects are the mostextreme photometric outliers.
As was discussed in section 7.3, there is a distinct dif-ference in the diversity of absolute magnitudes betweenyoung M dwarfs and L dwarfs. Using the color codingas a visual queue in Figures 21 - 31, the M dwarfs fallredder than the field sequence but they also scatter tobrighter magnitudes. For the W2 color difference plots(e.g. MJHK vs (J-W2), (H-W2), or (K-W2)), we la-bel the position of the M dwarfs in TW Hydrae and βPictoris as they are strikingly red and bright at thesewavelengths and well separated from the field popula-tion.
Comparatively, the L dwarfs flip in their behavior andcan be seen as redder but fainter than field sources.Focusing on Figures 21 - 22, and 26 which use JHKphotometry only, the latest type sources (e.g. PSO318,0047+6803, 2244+2043, 1119-1137, 1147-2040) are notonly redder but they also drive the elbow of the L/Ttransition ∼ 1 magnitude fainter than the field (notablyin MJ). Moving to longer wavelengths, this behaviorreverses. By Figures that evaluate colors against MW1
(∼ 3.4µ m) or MW2 (e.g. Figure 23 or 28) the latesttype sources are consistent with or slightly brighter thanthe elbow. Hence as discussed in section 7.3 and Filip-pazzo et al. (2015), the flux redistribution of young Ldwarfs seems to hinge very close to the K band. Indeedthe color magnitude diagram that appears to smoothlyand monotonically transition objects from late- M to Tdwarfs is the MK vs (K-W2) plot in Figure 30. Thereis a 10 magnitude difference between the warmest to thecoolest objects and the magnitude seems to monotoni-cally decrease with reddening color showing only a hintof an L/T transition elbow at MK=13/MW2=12. Onthis plot, the low-surface gravity sequence lies ∼ 1 mag-nitude brighter than the field with the exception of asmall fraction of the sample appearing normal (includ-ing the AB Doradus T dwarf SDSS1110).
The L/T transition induces a turning elbow on mostcolor magnitude plots. This feature is brought on whenthe clouds dissipate as one moves from warmer L dwarfsto cooler T dwarfs and CH4 begins to dominate as anopacity source all conspiring to drive the source colorsblueward. The demonstration that these young sourcesare redder and fainter than the field sequence in the near-infrared indicates that the clouds must persist throughlower temperatures (fainter) and represent an extremeversion of the conditions present for field age equivalents(redder). The brightening of sources at W1 and W2 atextreme red colors likely holds clues to the compositionand structure of the clouds as it is a reflection of theflux redistribution to longer wavelengths as discussed insection 7.3 above.
For colors and magnitudes evaluated across JH or Kand W1 or W2 (e.g. Figure 27 which shows MH vs H-W1), the latest type objects pull the low-gravity sequenceredder than the field while maintaining a small spread inabsolute magnitude from 0103+1935 through PSO318.Interestingly this indicates similarities in these sourcesnot readily apparent in current spectral data.
12 Faherty et al.
Lastly, on Figures 21 - 31 we have given γ and β clas-sified sources different symbols to investigate whethertrends between the two could be identified. Throughout,there is a hint that the sequence of γ classified objects isredder than that of the β sources. This is most prominenton Figures 23 - 24 where only four β L dwarfs rival γsources in color and/or magnitude. On other figures suchas 21, there appears to be more mixing between the twogravity classifications. As has been stated throughoutthis work, spectral type and the corresponding gravityclassification are difficult to evaluate and can differ be-tween optical and infrared spectra or from low resolutionto medium resolution data. The data as viewed in thiswork, seems to indicate that the γ classified sources aredistinct on color magnitude diagrams from the β classi-fied sources with some mixing likely due to a non-uniformspectral typing methodology.
7.5. The Bolometric Luminosities and EffectiveTemperatures of Young Objects
One expects that younger brown dwarfs should have in-flated radii compared to equivalent temperature sourcesgiven that they are still contracting. Consequently, onewould expect that γ and β objects would be overlumi-nous when compared to their field age equivalents. Arough estimate using the Burrows et al. (2001) evolution-ary models indicates that 10 Myr (50 Myr) objects withmasses ranging from 10 to 75 MJup have radii that are25% to 75% (13% to 50%) larger than 1 -3 Gyr dwarfswith equivalent temperatures. Since Lbol scales as R2,one might expect that this age difference translates intoyounger objects being 1.5x - 3.0x (1.3x - 2.3x) overlumi-nous compared to the field.
Initially, studies categorized low surface gravity browndwarfs as “underluminous” compared to field sourcesbased on examining near-infrared absolute magnitudetrends alone (e.g. Faherty et al. 2012). However as dis-cussed in section 7.3, flux shifts to longer wavelengths be-yond the H and K bands at lower gravities, so that someabsolute magnitude bands might be fainter but Lbol’sare not underluminous compared to the field (Fahertyet al. 2013, Filippazzo et al. 2015). In fact, Filippazzoet al. (2015) carefully evaluated Lbol values for all browndwarfs with parallaxes (or kinematic distances in the caseof high likelihood moving group members) and presentedup to date relations between observables and calculatedLbols. In that work, β and γ objects were found to splitalong the M/L transition whereby M dwarfs were over-luminous and L dwarfs were within to slightly below thesequence when compared to field objects.
To investigate Lbol trends among the age calibratedsample, we first calculate values for sources reportedhere-in using the technique described in Filippazzo et al.(2015). In that work, the authors integrate underthe combined optical and near-infrared photometry andspectra as well as the WISE photometry and mid infraredspectra where available. As described in previous sec-tions, we use parallaxes where available but supplementwith kinematic distances when a source was regarded asa high likelihood member to a group (see values in paren-theses in Tables 13 and 10). All Lbol, Teff , and Massvalues are listed in Table 14 as well as Table 13 formembers only.
Figure 32 shows Lbol as a function of spectral type for
all objects compared to the field polynomial from Filip-pazzo et al. (2015). Also overplotted is the polynomialfit for objects in groups (labeled as GRP in Table 19).We highlight bona fide and high-likelihood brown dwarfmoving group members as well as the unassociated γ andβ objects with differing symbols and colors.
Focusing on the age calibrated sample, we find thatlate-type M dwarfs assigned to groups are overluminouscompared to the field. The L dwarfs assigned to agroup are mixed, with the majority falling within thefield polynomial relations and a small number fallingslightly above. Comparing group-to-group differences,the 5-15 Myr TW Hydrae M8 and M9 objects are ∼5xmore luminous than the field while the 30-50 Myr TucanaHorologium source is ∼2x more luminous. Interestingly,the TW Hydrae, β Pictoris, and AB Doradus L7’s havenear equal Lbol values, all near the mean value for theirsubtype.
Comparing the γ and β gravity sources without mem-bership to the field and high-likelihood group members,we find that – with the exception of the M7.5 0335+2342which is highly suspect to be a β Pictoris member (seenote in Table 13) – all non-members fall within the poly-nomial relations for the field. This trend indicates thatthe late- M non-member γ and β sources may not beyoung (see discussion in subsection 7.3.3 and section 7.6).Indeed, 1022+0200 is a late-M non-member with fullkinematics. When we compare the UV velocity of thissource to that of the Eggen & Iben (1989) criterion foryoung stars, we find it falls outside of it hinting that itmay be drawn from the older disk population. It remainsunclear how to interpret the non-member L dwarfs as thistrend is in line with group assigned equivalents.
The result of Lbol’s for γ and β gravity L dwarfs lookinglike field sources or in some cases underluminous, impliesthat they are cooler than their field spectral equivalents.In other words, low-gravity or atmospheric conditionspotentially induced at a younger age, mimic spectral fea-tures of a warmer object. As young sources are typed ona scheme anchored by field objects, they are incorrectlygrouped with warmer sources. They certainly stand outin photometric, spectroscopic, and band by band abso-lute magnitude comparisons with field sources (e.g. allof section 7). However the low gravity sequence doesnot logically or easily follow off of the field sequence.Figure 33 shows the Teff values for γ and β sources cal-culated using the method described in Filippazzo et al.(2015) along with the polynomial and residuals for fieldobjects (from Filippazzo et al. 2015) and group members(from Table 19). As noted in Filippazzo et al. (2015) –with the exception of a few – while M dwarfs are sim-ilar if not warmer for their given spectral subtype, theL dwarfs are up to 100-300K cooler. Examining the 5-130 Myr age calibrated objects within this sample, wecan not isolate a trend of younger objects being increas-ingly cooler than older equivalent sources. For exam-ple, PSO318 and 0047+6803 are equivalent temperatureseven though there is a ∼100 Myr difference in age.
7.6. Unmatched objects with Signatures of Youth
Among the 152 objects in this sample with reportedspectral signatures of youth in either the optical or thenear-infrared, we confidently find that 39 (∼25%) arehigh-likelihood or bona fide members of nearby mov-
Brown Dwarf Analogs to Exoplanets 13
ing groups. There are 92 (∼61%) dubbed ambiguouseither because their kinematics overlap with more thanone group (including the old field) and they need betterastrometric measurements to differentiate, or there is notstrong enough evidence with the current astrometry todefinitively call it high-likelihood or bona fide. There are21 objects (∼ 14%) for which we have enough informationto declare them as non-members to any known group as-sessed in this work. Among the non-members, there are 4optically classified (3 infrared classified) M dwarfs and 15optically classified (17 infrared classified) L dwarfs with12 optically (10 infrared) classified γ objects and 5 op-tically (8 infrared) classified β objects. Several of theseobjects have extreme infrared colors (see Figures 5 - 14).For instance, 1615+4953 is classified in the optical as anL4γ and rivals the most exciting late-type objects in itsdeviant infrared colors. However, current kinematics donot show a high probability of membership in any groupdespite its having a proper motion and radial velocity.Similarly, 0435-1441 is strikingly red in JHK, showsboth optical and infrared signatures of youth, and itsspectrum needs to be de-reddened (E(B-V)=1.8). Whileit is in the direction of the nearby star-forming regionMBM 20, the distance noted for that cluster (112 - 161pc) would drive unrealistic absolute magnitudes and Lbolvalues for this source.
The current census of young, but, unassociated late- Mand L dwarfs is similar to what has emerged in studiesof early M dwarfs with multiple signatures of youth (e.g.X-ray, UV and IR-excess, Lithium). A significant por-tion of objects in the studies of Rodriguez et al. (2013)and Shkolnik et al. (2011, 2012) are strong candidatesfor being 5 -130 Myr objects via their spectral and pho-tometric properties but their kinematics are inconclusiveand their age cannot be determined by a group assign-ment. Likely, there are a number of groups waiting tobe uncovered that may account for this overabundance ofyoung, low mass objects. Alternatively, after 5 - 130 Myrsources have been dynamically moved from their originssuch that tracing back their history to any collection ofobjects is beyond our capability.
8. COMPARISONS WITH DIRECTLY IMAGEDEXOPLANETS
Several of the objects discussed herein are in the samemoving groups as directly imaged exoplanets or plane-tary mass companions. For example, there are two bonafide or high-likelihood brown dwarfs in the β Pictorismoving group, home to the 11-13 Jupiter mass planetβ Pictoris b and the newly discovered 2 - 3 Jupitermass planet 51 Eri b (Bonnefoy et al. 2013, 2014, Maleset al. 2014, Macintosh et al. 2015), 20 in the TucanaHorologium association which houses the 10 - 14 MJup
planetary mass companion AB Pictoris b (Chauvin et al.2005, Bonnefoy et al. 2010) as well as the 12 - 15 MJup
planetary mass companion 2M0219 b (Artigau et al.2015), and seven in the TW Hydrae Association whichis the home of the 3 - 7 MJup planetary mass companion2M1207 b (Chauvin et al. 2004, Patience et al. 2012).As such, the brown dwarfs discussed herein should beconsidered siblings of the directly imaged planets as onecan assume that they are co-eval, and share formationconditions and dynamical histories. The mode of for-mation for the brown dwarfs versus the directly imaged
exoplanets remains a question but will likely drive dis-tinct differences in the observables of each population.In this section, we look to place the young brown dwarfsample in context with related exoplanet members.
8.1. Similarities of Brown Dwarfs and ImagedExoplanets on Color Magnitude Diagrams
Young isolated brown dwarfs are far easier to accumu-late data on than directly imaged exoplanet equivalentsbecause they do not have a bright star to block whenobserving. The collection of currently known giant ex-oplanets, generally have only infrared (J,H,K,L′,M ′)photometric measurements. Near-infrared spectroscopyis possible for some although this requires considerabletelescope time and advanced instrumentation (e.g. Op-penheimer et al. 2013, Macintosh et al. 2015, Hinkleyet al. 2015, Bonnefoy et al. 2013, Patience et al. 2012).
Figures 35 - 41 show a full suite of near-infrared colormagnitude diagrams with the same brown dwarf sampleas in Figures 21 - 31 however we now compliment eachwith directly imaged exoplanets and color code sourcesby their respective moving groups. For L’ band photom-etry of the brown dwarfs, we have used the small sam-ple of MLT sources with measured MKO L’ – primarilyfrom Golimowski et al. (2004) – to convert the WISEW1 band photometry which has comparable wavelengthcoverage. The polynomial relation used for convertingbetween bands is listed in Table 19.
As with the young brown dwarfs discussed herein, anobservable feature of note for the exoplanets is that theyare redder and fainter than the field brown dwarf popu-lation in near-infrared color magnitude diagrams. Thisis exemplified by the positions of HR8799 b and 2M1207b both of which sit ∼ 1 mag below the L dwarf sequencein Figures 35 36, and 37. To explain their position onnear-infrared color magnitude diagrams, several authorshave proposed thick or high-lying photospheric clouds intheir atmospheres (Bowler et al. 2010b, Madhusudhanet al. 2011, Hinz et al. 2010, Marley et al. 2012, Skemeret al. 2012, Currie et al. 2011). An alternative theory pro-posed by Tremblin et al. (2016) has recently emerged thatproposes cloudless atmospheres with thermo-chemical in-stabilities may invoke some of the features seen here-in.Further investigation of those models is required beforewe can appropriately comment on how well they mayreproduce the large sample presented in this work.
The young brown dwarf sequence in many ways mirrorsthat of the directly imaged exoplanets but for warmer(or older) objects. From the warmest (at M7) to thecoolest (at L7) the low-gravity brown dwarfs are redderand fainter than their field counterparts. As can be seenon each Figure, the low-gravity sequence appears to log-ically extend through many of the directly imaged exo-planets. Interestingly, the youngest exoplanets (those inTaurus, Upper Scorpius, and ρ Ophiuchus; Kraus et al.2014, Currie et al. 2014) are redder than either the fieldor the low-gravity sequences indicating that – assumingformation differences do not drastically alter the avail-able compositions – the atmosphere or gravity effects aremost pronounced close to formation.
By color combinations using L’ band, the youngestplanetary mass objects such as ROXs12 b, DH Tau b,and GQ Lup b are nearly 2 magnitudes redder and >2 magnitudes brighter than the field sequence. Con-
14 Faherty et al.
versely, the lowest temperature planets around HR8799fall within or close to the T dwarf sequence. The excep-tion is HR8799 b which has a singificantly redder (J-L)color than the field sequence as well as the young browndwarf sequence. It is also ∼ 2 magnitudes fainter in ML
than the low-gravity sequence which extends redward inFigure 38 with minimal scatter in ML. Skemer et al.(2012) have noted that the 3.3µm photometry (not plot-ted) for the HR8799 planets is brighter than predictedby evolutionary or atmosphere models. As in Barmanet al. (2011a), Skemer et al. (2012) use thick cloudy non-equilibrium chemistry models and remove CH4 to fit thedata. Similarly, none of the isolated late-type L dwarfslabeled on Figures 35 - 41 have CH4 in their near infraredspectra even though 1119-1137, 1147-2040, PSO318 and0047+6803 have calculated Teff s which should allow fordetectable CH4. Interestingly only the planetary masscompanion 2M1207 b rivals the far reaching red sequenceof the young brown dwarfs, yet that source is lacking anL’ or equivalent band detection. Hence at this point thelate-type young brown dwarf sequence prevails over theexoplanet sequence in their extreme L’ colors even as theearliest type youngest planetary mass sources prevail atslightly bluer magnitudes.
The latest-type low-gravity brown dwarfs, and theknown directly imaged exoplanets push the L/T transi-tion to cooler temperatures and redder colors. Interest-ingly we have two sets of objects in the same group thatspan either side of the famed L/T transition. 0047+6803(Teff=1227± 30 K, Mass= 9 - 15 MJup) and SDSS1110(Teff= 926 ± 18, Mass= 7 - 11 MJup) are both in the∼110 - 130 Myr AB Doradus moving group. PSO318(Teff= 1210 ± 41, Mass= 5 - 9 MJup) and 51 Eri b(Teff= 675 ± 75, Mass= 2 - 12MJup) are both in the ∼25 Myr β Pictoris moving group. The two sets differ by∼100 Myr in age. Comparing 0047+6803 to PSO318 wefind they have similar spectral types, have Teff within1σ but may differ in mass by up to ∼10 MJup . Bothpush the L/T transition redder on multiple color mag-nitude diagrams in Figures 21 - 31 and Figures 35 - 41.Overall PSO318 and 0047+6803 have similar absolutemagnitudes (see Figures 15 - 20) although PSO318 canbe significantly redder in specific colors. 51 Eri b andSDSS1110 are thought to have similar spectral types butdiffer in mass and Teff by as much as 344 K and 5 MJup
respectively. Interestingly, 51 Eri b is ∼ 2 mag fainter inMJHL than SDSS 1110. Comparing its position on Fig-ures 35, 38 and 40, 51 Eri b appears much more like theT8 Ross 458 C thought to be 150 - 800 Myr (Burgasseret al. 2010b). Regardless for both groups we see that bythe time we have reached the mid to late-T dwarf phase,sources are back on or very close to, the field sequence.As cloud clearing is thought to happen at the L/T tran-sition, we surmise this is further evidence that much ofthe diversity seen among the young, warm exoplanet andbrown dwarf population is atmosphere related.
A note of caution when looking for similarities on colormagnitude diagrams between brown dwarfs and giant ex-oplanets comes in the way of comparing the newly discov-ered L7 companion VHS1256 B to HR8799 b. In Gauzaet al. (2015), the authors noted a similarity of this com-panion and the giant exoplanet. On Figure 37, the twohave enticingly similar near-infrared values. However,Figure 42 shows the near-infrared spectrum of each ob-
ject as well as a field L7 to demonstrate strong differencesin H-band. Clearly there is some commonality betweenthe two sources, but color magnitude combinations alonedo not give a full enough picture to draw conclusions.
The directly imaged companion GJ 504 b is anotherexample of how we require multiple color magnitude di-agram plots to begin exploring the potential characteris-tics of a single object (Kuzuhara et al. 2013). GJ 504 bis nearly 1 magnitude redder than late-type T dwarfs inMJHK vs (J-K) or (H-K) diagrams (Figures 37 and 39),but it appears normal inMJH vs (J-H) plots (Figure 35).Recent work by Fuhrmann & Chini (2015) suggest theprimary may not be young therefore this source may notbe planetary mass. Regardless it is a low mass T dwarforbiting at < 50 AU, potentially formed in a disk arounda nearby star hence it may be characteristically differentthan equivalent temperature T dwarfs (see e.g. Skemeret al. 2015).
8.1.1. Bolometric Luminosities
Comparing the bolometric luminosities (Lbol) acrossthe sample of field objects, new bona fide or high-likelihood moving group members, and directly imagedexoplanets allows us to investigate how the flux variesacross the sample. For the directly imaged exoplanets,we use the Lbol values reported in the literature (seeMales et al. 2014, Bonnefoy et al. 2014, Currie et al.2014).
As discussed in both section 7.5 and Filippazzo et al.(2015), the young M dwarfs are overluminous for theirspectral type while the young L’s are normal to slightlyunderluminous. Several authors have noted this pe-culiarity among the directly imaged exoplanets as well(e.g. Bowler et al. 2013, Males et al. 2014). Examin-ing the two populations together allows us to investigatewhether there is an obvious age-associated correlationwithin the scatter. The youngest objects in Figure 43are the directly imaged exoplanets such as ROXs 42B b,and 1RXS1609 b which belong to star forming regionsat just a few Myr of age. These sources appear overlu-minous in comparison to equivalent sources regardless ofhow late their spectral type (e.g. 1RXS1609b which isthought to resemble an L4). The latest type planets thathave direct, comparable data – 2M1207 b, HR8799 b, 51Eri b – are all ∼ 1 σ or more below the field sequenceindicating that they are either far cooler than the latestL dwarfs or there is unaccounted flux in the bolometricluminosity calculations. Interestingly, this appears to bewhere the young brown dwarf and the directly imagedexoplanet comparisons diverge. The latest type exoplan-ets in equivalent age groups to the isolated brown dwarfs,are either far cooler than any currently discovered youngbrown dwarf equivalent, or the physical conditions di-verge (e.g. atmosphere conditions, chemistry, other).
8.1.2. Masses from combining Evolutionary Models withLBol, and Age
In Figure 34, we combine the Lbol values with the agesof the moving group members to estimate masses. InTable 14 we also list masses calculated from the spec-tral energy distribution analysis as described in Filip-pazzo et al. (2015). Over-plotted on Figure 34 with theyoung brown dwarfs are directly imaged planetary andbrown dwarf mass companions with Lbol values collected
Brown Dwarf Analogs to Exoplanets 15
from the literature. The models from Saumon & Mar-ley (2008)(solid) and Baraffe et al. (2015) (dashed) areshown with lines of equal mass color coded as stars (>75 MJup, blue) brown dwarfs (> 13 MJup, green) andplanets (< 13 MJup, red).
It is unclear how each one of the objects in this sampleformed however, using the 13 MJup boundary as a massdistinguisher between brown-dwarf and planet-type ob-jects, we find that there are close to 9 solitary objectswith masses < 13 MJup. Several of those sources lie in anambiguous area where low mass brown dwarfs and plan-etary mass objects cross (30 - 130 Myr between massesof 10 - 20 MJup).
With the exception of Y type objects whose age isstill undetermined (e.g. W0855, Luhman 2014), 1119-1137, 1147-2040, and PSO318 are the lowest mass iso-lated sources categorized. PSO 318 has a lower lumi-nosity than β Pictoris b, the 11 - 13 MJup planet inthe same association while 1119-1137 and 1147-2040 aresignificantly more luminous than their sibling exoplanet2M1207b. Interestingly, the AB Doradus equivalentlytyped L7 member, 0047+6803, is higher mass than allof these sources even though its bolometric luminosity iscomparable. Similarly, 0355+1133 which is in the samegroup as 0047+6803, shares photometric anomalies withPSO318 (near-infrared and mid infrared color) and spec-tral anomalies with 2M1207b yet it is much higher mass.
The overlap in masses of the directly imaged exoplan-ets and isolated brown dwarfs invites questions of forma-tion given co-evolving groups. Whether the latter wasformed via star formation processes or ejected after plan-etary formation processes is yet to be seen and requiresfurther investigation.
9. CONCLUSIONS
In this work we investigate the kinematics and fun-damental properties of a sample of 152 suspected youngbrown dwarfs. We present near-infrared spectra and con-firm low-surface gravity features for 43 of the objectsdesignating them either intermediate (β) or very low (γ)gravity sources. We report 18 new parallaxes (10 fieldobjects for comparison and 8 low surface gravity), 19new proper motions, and 38 new radial velocities and in-vestigate the likelihood of membership in a nearby mov-ing group. We use four kinematic membership codes (1)BANYAN I, (2) BANYAN II, (3) LACEwING, and (4)Convergent method, as well as a visual check of the avail-able space motion for each target against known membersof well known nearby kinematic groups to determine thelikelihood of co-membership for our sources. We cate-gorize objects as (1) bona fide –BM, (2) high-likelihood–HLM, (2) ambiguous –AM, or (3) non-member –NM ofnearby moving groups. We find 39 sources are bona fideor high-likelihood members of known associations (8 inAB Doradus, 1 in Argus, 2 in β Pictoris, 1 in Columba,7 in TW Hydrae, and 20 in Tucana Horologium). A fur-ther 92 objects have an ambiguous status and 21 objectsare not members of any known group evaluated in thiswork.
Examining the distribution of gravity classificationsbetween different groups we find that the youngest as-sociation (TW Hydrae) has only very low-gravity (γ)sources associated with it but slightly older groups suchas Tucana Horologium (9 optically classified, 10 infrared
classified γ objects and 3 optically classified, 5 infraredclassified β objects) and AB Doradus (4 optically classi-fied, 6 infrared classified γ objects and 1 optically classi-fied, 2 infrared classified β objects) show a mix of bothintermediate (β) and very low-gravity sources. This di-versity is evidence that classically delegated gravity fea-tures in the spectra of brown dwarfs are influenced byother parameters such as metallicity or (more likely) at-mospheric conditions.
We investigate colors for the full sample acrossthe suite of MKO, 2MASS and WISE photometry(J,H,Ks,W1,W2,W3). In color versus spectral typediagrams, we find that the γ and β classified objects aredistinct from the field (> 3 Gyr sources). They are mostdeviant from the field sequence in the (J-W2) color wherethey are an average of 2σ redder than the subtype mean.They are least deviant in the (J-H) color where they arean average of 0.7σ redder than the subtype mean. Basedon the 5 -130 Myr age calibrated sample, we concludethat the extent of deviation in infrared color is not in-dicative of the age of the source (meaning redder doesnot translate to younger). In any given color a γ or aβ object – whether confirmed in a group or not – maymark the extreme outlier for a given subtype. We findthat the L0 dwarfs in Tucana Horologium (expected tohave the same, Teff , age and metallicity) deviate fromthe field sequence of infrared colors by between 1 and 4 σ(depending on the particular color examined). Assumingclouds are the source of the diversity, we conclude thatthere is a variation in cloud properties between otherwisesimilar objects.
Examination of the absolute magnitudes for the par-allax sample indicates a clear flux redistribution for low-and intermediate-gravity brown dwarfs (compared tofield brown dwarfs) from near-infrared to wavelengthsat (and longer than) the WISE W3 band. There is alsoa clear correlation of this trend with spectral subtype.The M dwarfs are 1-2σ brighter than field equivalents atJ band but 4-5σ brighter at W3. The L dwarfs are 1-2σfainter at J band but 1-2σ brighter atW3. Clouds, whichare a far more dominant opacity source for L dwarfs, arelikely the cause.
Sources that are not confirmed in groups do not alltrace the same behavior in absolute magnitude or colorindicating that some sources may not be young. Varia-tions in atmospheric conditions or metallicity likely drivethe diversity.
On color-magnitude diagrams, the low-surface gravitybrown dwarfs pull the elbow of the field L/T transitionsignificantly redder and fainter with the most extremecase being the MJ vs (J-W2) plot where young objectsare up to 1 mag redder than the field sequence. Con-versely, the MK versus (K-W2) plot shows a 10 magni-tude difference between the warmest and coolest browndwarfs yet seems to monotonically decrease in magnitudewith reddening color. On this figure there is little evi-dence for an L/T transition elbow and the young objectsform a secondary sequence that is ∼1 mag redder thanthe field sequence. Interestingly as we move to longerwavelengths the effect reverses and the latest type ob-jects pull the elbow of the L/T transition back up asthey are equivalent or slightly brighter than field equiv-alents at MW1,W2. Comparing the sequence of γ and βclassified sources on CMD’s compared to the field, we
16 Faherty et al.
find a hint that the two are distinct with the former red-der than the latter. This trend is clearest on the MJ
versus (J-W2) figure although there is still a small mixof γ and β sources at extreme colors for a given absolutemagnitude.
Comparing the low-gravity sample with directly im-aged exoplanets on color magnitude diagrams we findthat the former sequence logically extends through thelatest type planets on multiple color magnitude dia-grams. The small collection of hot, planetary mass ob-jects in star forming regions such as ρ Ophiuchus andTaurus are strikingly red, bright, and luminous comparedto either the field sequence or the low-gravity objects in-dicating that the atmosphere and/or gravity effects thatdrive the population diversity may be pronounced closeto formation. Comparing β Pictoris members 51 Eri b(mid T dwarf) and PSO318 (late L dwarf) with AB Do-radus members SDSS1110 (mid T dwarf) and 0047+6803(late L dwarf) we find that even though the members dif-fer by ∼ 100 Myr, the late-type L’s similarly push the el-bow of the L/T transition redder and fainter whereas theT dwarfs appear on or very close to the field sequence.We surmise that this behavior, seen in two sets of ob-jects at different ages across the L/T transition wherecloud clearing is thought to be significant, is evidencethat much of the diversity seen among young warm exo-planet and brown dwarfs is atmosphere related.
Brown Dwarf Analogs to Exoplanets 17
γGravity
β# γ/β
3/7
4/8
12/9
17/9
14/6
5/5
9/5
6/3
2/3
1/1
5/1
M7 M9 L1 L3 L5 L7SpT (NIR)
05
1015202530
Num
ber
M7 M9 L1 L3 L5 L7SpT (NIR)
05
1015202530
Num
ber
M7 M9 L1 L3 L5 L7SpT (Opt)
0
5
10
15
20
Num
ber
M7 M9 L1 L3 L5 L7SpT (Opt)
0
5
10
15
20
Num
ber
γGravity
β
1/1
5/3
8/7
15/4
2/3 4/1 3/2
7/2
2/3
0/12/0
# γ/β
Figure 1. The distribution of objects analyzed in this work organized by spectral subtype and gravity classification in either the near-infrared (left) or optical (right). For ease of labels in this work, we have chosen to label VL-G and INT-G objects classified using the Allers& Liu (2013) spectral indices as γ and β respectively. On this plot we also show the number of γ and β at each subtype as a ratio of # γ/ # β.
18 Faherty et al.
−25 −20 −15 −10 −5 0U (km s−1)
−30
−25
−20
−15
−10
V (
km
s−
1)
AB Doradus
Tuc Hor
β Pictoris
Columba
Argus
TW Hya
−25 −20 −15 −10 −5 0U (km s−1)
−20
−15
−10
−5
0
5
W (
km
s−
1)
−35 −30 −25 −20 −15 −10V (km s−1)
−20
−15
−10
−5
0
5
W (
km
s−
1)
Figure 2. The UVW properties of 0045+1634 (black filled triangle) compared to those of the members of the nearby young groups. Solidrectangles surround the furthest extent of highly probable members from Torres et al. (2008) but their distribution does not necessarily fillthe entire rectangle.
Brown Dwarf Analogs to Exoplanets 19
Figure 3. The SpeX prism spectrum of 0055+0134 over-plotted with a sample of field and very low-gravity subtype equivalents.
20 Faherty et al.
Figure 4. The FIRE spectrum of 0421-6306 binned to prism resolution and over-plotted with a sample of field and very low-gravitysubtype equivalents.
Brown Dwarf Analogs to Exoplanets 21
M8 L0 L2 L4 L6 L8 Spectral Type
0.4
0.6
0.8
1.0
1.2
1.4
1.6
1.8
J−
H
AB DoradusTucana Horologiumβ PictorisColumba and CarinaArgusTW HydraeYoung Field?
γ
β
Figure 5. The distribution of J-H color as a function of spectral type. The black filled circle at each subtype is the mean value and thegrey filled area marks the standard deviation spread. The isolated sources that compose this “normal” sample have no spectral peculiarities(e.g. subdwarfs, low-gravity, unresolved binarity), and were only included if they had a photometric uncertainty in each band < 0.2 mag.The full list was gathered from the dwarfarchives compendium and supplemented with the large ultra cool dwarf surveys from Schmidtet al. (2010), Mace et al. (2013), Kirkpatrick et al. (2011), and West et al. (2008) (for M dwarfs). Individual filled squares or five-pointstars are γ or β (respectively) classified objects. Spectral types, as well as gravity classifications, are from optical data unless only infraredwas available. We note that most sources plotted have spectral type uncertainties of 0.5. Objects are color coded by group assignments(or lack-thereof) discussed in this work. 2MASS photometry is used for JHKs bands.
22 Faherty et al.
M8 L0 L2 L4 L6 L8 Spectral Type
1.0
1.5
2.0
2.5
3.0
J−
Ks
AB DoradusTucana Horologiumβ PictorisColumba and CarinaArgusTW HydraeYoung Field?
γ
β
Figure 6. The distribution of J-Ks color as a function of spectral type. Symbols are as described in Figure 5.
Brown Dwarf Analogs to Exoplanets 23
M8 L0 L2 L4 L6 L8 Spectral Type
1.0
1.5
2.0
2.5
3.0
3.5
4.0
J−
W1
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW HydraeYoung Field?
γ
β
Figure 7. The distribution of J-W1 color as a function of spectral type. Symbols are as described in Figure 5.
24 Faherty et al.
M8 L0 L2 L4 L6 L8 Spectral Type
2
3
4
5
J−
W2
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW Hydrae
Young Field?
γβ
Figure 8. The distribution of J-W2 color as a function of spectral type. Symbols are as described in Figure 5.
Brown Dwarf Analogs to Exoplanets 25
M8 L0 L2 L4 L6 L8 Spectral Type
0.2
0.4
0.6
0.8
1.0
1.2
H−
Ks
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW HydraeYoung Field?
γ
β
Figure 9. The distribution of H-Ks color as a function of spectral type. Symbols are as described in Figure 5.
26 Faherty et al.
M8 L0 L2 L4 L6 L8 Spectral Type
0.5
1.0
1.5
2.0
2.5
H−
W1
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW HydraeYoung Field?
γ
β
Figure 10. The distribution of H-W1 color as a function of spectral type. Symbols are as described in Figure 5.
Brown Dwarf Analogs to Exoplanets 27
M8 L0 L2 L4 L6 L8 Spectral Type
1.0
1.5
2.0
2.5
3.0
H−
W2
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW HydraeYoung Field?
γ
β
Figure 11. The distribution of H-W2 color as a function of spectral type. Symbols are as described in Figure 5.
28 Faherty et al.
M8 L0 L2 L4 L6 L8 Spectral Type
0.2
0.4
0.6
0.8
1.0
1.2
1.4
Ks−
W1
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW HydraeYoung Field?
γ
β
Figure 12. The distribution of Ks-W1 color as a function of spectral type. Symbols are as described in Figure 5.
Brown Dwarf Analogs to Exoplanets 29
M8 L0 L2 L4 L6 L8 Spectral Type
0.5
1.0
1.5
2.0
Ks−
W2
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW HydraeYoung Field?
γβ
Figure 13. The distribution of Ks-W2 color as a function of spectral type. Symbols are as described in Figure 5.
30 Faherty et al.
M8 L0 L2 L4 L6 L8 Spectral Type
0.2
0.4
0.6
0.8
W1
−W
2
AB DoradusTucana Horologiumβ PictorisColumbaArgusTW HydraeYoung Field?
γβ
Figure 14. The distribution of W1-W2 color as a function of spectral type. Symbols are as described in Figure 5.
Brown Dwarf Analogs to Exoplanets 31
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
16
15
14
13
12
11
10
9
MJ (2
MAS
S)
AB DoradusTucana Horologium` PictorisColumba and CarinaArgusTW HydraeYoung Field?
a `
Figure 15. The spectral type versus MJ plot. The field polynomial listed in Table 19 is represented by the grey area. All JHK photometryis from 2MASS. Over-plotted are objects in this work with measured parallaxes or estimated kinematic distances from high confidencegroup membership. Symbols distinguish very low (γ) from intermediate (β) gravity sources. Objects are color coded by group membership.For demonstration on the MJ plot only, we also overplot individual field objects (with MJer < 0.5) as black filled circles. Residuals ofindividual γ and β objects against the field polynomial are shown in the lower panel.
32 Faherty et al.
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
15
14
13
12
11
10
9
8
MH
(2M
ASS)
AB DoradusTucana Horologium` PictorisColumba and CarinaArgusTW HydraeYoung Field?
a `
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
Figure 16. The spectral type versus MH plot with residuals against polynomial relations (lower panel). Symbols are as described inFigure 15.
Brown Dwarf Analogs to Exoplanets 33
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
14
13
12
11
10
9
8
MKs
(2M
ASS)
AB DoradusTucana Horologium` PictorisColumba and CarinaArgusTW HydraeYoung Field?
a `
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
Figure 17. The spectral type versus MKs plot with residuals against polynomial relations (lower panel). Symbols are as described inFigure 15.
34 Faherty et al.
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
12
11
10
9
8
MW
1 (W
ISE)
AB DoradusTucana Horologium` PictorisColumba and CarinaArgusTW HydraeYoung Field?
a `
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
012
Res
idua
ls
Figure 18. The spectral type versus MW1 plot with residuals against polynomial relations (lower panel). Symbols are as described inFigure 15.
Brown Dwarf Analogs to Exoplanets 35
36 Faherty et al.
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
12
11
10
9
8
7
MW
2 (W
ISE)
AB DoradusTucana Horologium` PictorisColumba and CarinaArgusTW HydraeYoung Field?
a `
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
0123
Res
idua
ls
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
0123
Res
idua
ls
Figure 19. The spectral type versus MW2 plot with residuals against polynomial relations (lower panel). Symbols are as described inFigure 15.
Brown Dwarf Analogs to Exoplanets 37
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
10
9
8
7
6
5
MW
3 (W
ISE)
AB DoradusTucana Horologium` PictorisColumba and CarinaArgusTW HydraeYoung Field?
a `
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
01234
Res
idua
ls
M7 M8 M9 L0 L1 L2 L3 L4 L5 L6 L7 L8Spectral Type
−2−1
01234
Res
idua
ls
Figure 20. The spectral type versus MW3 plot with residuals against polynomial relations (lower panel). Symbols are as described inFigure 15.
PSO318
0047
0355
2244
0326
SDSS1110
VHS 1256 b
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1147
1119
−0.5 0.0 0.5 1.0 1.5 2.0(J − H) (2MASS)
18
16
14
12
10
MJ (
2MAS
S)
−0.5 0.0 0.5 1.0 1.5 2.0(J − H) (2MASS)
18
16
14
12
10
MJ (
2MAS
S)
PSO318
0047
0355
2244
0326
SDSS1110
VHS 1256 b
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1147
1119
−0.5 0.0 0.5 1.0 1.5 2.0(J − H) (2MASS)
20
18
16
14
12
10
8
MH (2
MAS
S)
−0.5 0.0 0.5 1.0 1.5 2.0(J − H) (2MASS)
20
18
16
14
12
10
8
MH (2
MAS
S)
Figure 21. The (J-H) versus MJ (left) and MH (right) color magnitude diagram for late-type M through T dwarfs (Y dwarfs wherephotometry is available). All JHK photometry is on the MKO system. Objects have been color coded by spectral subtype. Binaries,subdwarfs, spectrally peculiar sources and those with absolute magnitude uncertainties > 0.5 have been omitted. Low-gravity objects arehighlighted as bold filled circles throughout. Objects of interest discussed in detail within the text have been labeled.
38 Faherty et al.
1119
0047
0355
2244
0326
SDSS1110
VHS 1256 b
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1147
PSO318
−1 0 1 2 3(J − K) (2MASS)
18
16
14
12
10
MJ (
2MAS
S)
−1 0 1 2 3(J − K) (2MASS)
18
16
14
12
10
MJ (
2MAS
S)
−1 0 1 2 3(J − K) (2MASS)
18
16
14
12
10
8
MK
(2M
ASS)
−1 0 1 2 3(J − K) (2MASS)
18
16
14
12
10
8
MK
(2M
ASS)
1119
0355
2244
0326
SDSS1110
VHS 1256 b
1147
PSO318
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
Figure 22. The (J-K) versus MJ (left) and MK (right) color magnitude diagram. Symbols are as described in Figure 21.
SDSS1110
PSO318
0047
0355
2244
0326
0103
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1119
1147
0 1 2 3 4(J − W1)
18
16
14
12
10
MJ (
2MAS
S)
0 1 2 3 4(J − W1)
18
16
14
12
10
MJ (
2MAS
S)
0 1 2 3 4(J − W1)
18
16
14
12
10
8
MW
1
0 1 2 3 4(J − W1)
18
16
14
12
10
8
MW
1
SDSS1110 PSO318
0047
0355
2244
0326
0103
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1119
1147
Figure 23. The (J-W1) versus MJ (left) and MW1 (right) color magnitude diagram. Symbols are as described in Figure 21.
Brown Dwarf Analogs to Exoplanets 39
SDSS1110 PSO318
22440355
0047
0326
0103
TWA 28TWA 27ATWA 26
TWA 292M2000
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1147
1119
1 2 3 4 5(J − W2)
18
16
14
12
10
MJ (
2MAS
S)
1 2 3 4 5(J − W2)
18
16
14
12
10
MJ (
2MAS
S)
Figure 24. The (J-W2) versus MJ color magnitude diagram. Symbols are as described in Figure 21.
40 Faherty et al.
1 2 3 4 5(J − W2)
14
12
10
8
MW
2 (W
ISE)
1 2 3 4 5(J − W2)
14
12
10
8
MW
2 (W
ISE)
SDSS1110
PSO3180047
0355
2244
0326
0103
TWA 28TWA 27ATWA 26
TWA 292M2000
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1147 1119
Figure 25. The (J-W2) versus MW2 (right) color magnitude diagram. Symbols are as described in Figure 21.
PSO318
11190355
2244
0326
SDSS1110 VHS 1256 b
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
−0.5 0.0 0.5 1.0 1.5(H − K) (2MASS)
20
18
16
14
12
10
8
MH (2
MAS
S)
−0.5 0.0 0.5 1.0 1.5(H − K) (2MASS)
20
18
16
14
12
10
8
MH (2
MAS
S)
11470047
−0.5 0.0 0.5 1.0 1.5(H − K) (2MASS)
18
16
14
12
10
8
MK
(2M
ASS)
−0.5 0.0 0.5 1.0 1.5(H − K) (2MASS)
18
16
14
12
10
8
MK
(2M
ASS)
PSO318
11190355
2244
0326
SDSS1110VHS 1256 b
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
11470047
Figure 26. The (H-K) versus MH (left) and MK (right) color magnitude diagram. Symbols are as described in Figure 21.
Brown Dwarf Analogs to Exoplanets 41
0.0 0.5 1.0 1.5 2.0 2.5(H − W1)
20
18
16
14
12
10
8M
H (2
MAS
S)
0.0 0.5 1.0 1.5 2.0 2.5(H − W1)
20
18
16
14
12
10
8M
H (2
MAS
S)
SDSS1110 PSO3180047
0355
2244
0326
0103
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1147 1119
0.0 0.5 1.0 1.5 2.0 2.5(H − W1)
18
16
14
12
10
8
MW
1
0.0 0.5 1.0 1.5 2.0 2.5(H − W1)
18
16
14
12
10
8
MW
1
SDSS1110
PSO318
11190355
2244
0326
0103
< M9L0 - L4L5 - L9T0 - T4
>T5 !" 1147
0047
Figure 27. The (H-W1) versus MH (left) and MW1 (right) color magnitude diagram. Symbols are as described in Figure 21.
1 2 3 4 5(H − W2)
20
18
16
14
12
10
8
MH (2
MAS
S)
1 2 3 4 5(H − W2)
20
18
16
14
12
10
8
MH (2
MAS
S)
SDSS1110
PSO3181119
0355
2244
0326
TWA 28TWA 27ATWA 26TWA 292M2000
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1147
0047
1 2 3 4 5(H − W2)
14
12
10
8M
W2 (
WIS
E)
1 2 3 4 5(H − W2)
14
12
10
8M
W2 (
WIS
E)
SDSS1110
PSO318
11190355
2244
0326
TWA 28TWA 27ATWA 26
TWA 292M2000
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
11470047
Figure 28. The (H-W2) versus MH (left) and MW2 (right) color magnitude diagram. Symbols are as described in Figure 21.
0.0 0.5 1.0 1.5 2.0(K − W1)
18
16
14
12
10
8
MK
(2M
ASS)
0.0 0.5 1.0 1.5 2.0(K − W1)
18
16
14
12
10
8
MK
(2M
ASS)
SDSS1110
PSO31811470355
2244
0326
0103
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
0.0 0.5 1.0 1.5 2.0(K − W1)
18
16
14
12
10
8
MW
1 (W
ISE)
0.0 0.5 1.0 1.5 2.0(K − W1)
18
16
14
12
10
8
MW
1 (W
ISE)
SDSS1110
PSO3181147
0355
22440103
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
0047
Figure 29. The (K-W1) versus MK (left) and MW1 (right) color magnitude diagram. Symbols are as described in Figure 21.
42 Faherty et al.
Brown Dwarf Analogs to Exoplanets 43
1 2 3 4 5(K − W2)
18
16
14
12
10
8
MK
(2M
ASS)
1 2 3 4 5(K − W2)
18
16
14
12
10
8
MK
(2M
ASS)
SDSS1110
PSO318
0355
2244
0326
TWA 28TWA 27ATWA 26TWA 292M2000
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
1 2 3 4 5(K − W2)
14
12
10
8
MW
2 (W
ISE)
1 2 3 4 5(K − W2)
14
12
10
8
MW
2 (W
ISE)
SDSS1110
PSO318
0047
0355
2244
0326
0103
TWA 28TWA 27A
TWA 26
TWA 292M2000
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
Figure 30. The (K-W2) versus MK (left) and MW2 (right) color magnitude diagram. Symbols are as described in Figure 21.
0.5 1.0 1.5 2.0(W1 − W2)
18
16
14
12
10
8
MW
1 (W
ISE)
0.5 1.0 1.5 2.0(W1 − W2)
18
16
14
12
10
8
MW
1 (W
ISE)
SDSS1110
PSO318
0047
0355
2244
0326
0103
TWA 28TWA 27A
TWA 2922000
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
0.5 1.0 1.5 2.0(W1 − W2)
14
12
10
8
MW
2 (W
ISE)
0.5 1.0 1.5 2.0(W1 − W2)
14
12
10
8
MW
2 (W
ISE)
< M9L0 - L4L5 - L9T0 - T4
>T5 !"
SDSS1110
PSO318
0047
0355
2244
0326
0103
TWA 28TWA 27A
TWA 292M2000
TWA 26
Figure 31. The (W1-W2) versus MW1 (left) and MW2 (right) color magnitude diagram. Symbols are as described in Figure 21.
44 Faherty et al.
M6 M8 L0 L2 L4 L6 L8 SpT
−5.0
−4.5
−4.0
−3.5
−3.0
−2.5
log
(Lbo
l/LSu
n)
M6 M8 L0 L2 L4 L6 L8 SpT
−5.0
−4.5
−4.0
−3.5
−3.0
−2.5
log
(Lbo
l/LSu
n)
AB DoradusTuc Hor` PictorisColumbaArgusTW HyaYoung Field? a `
TWA29
TWA26TWA28
PSO318
0045
2M2244
0047
0355
0326
VHS1256 B
2206
14250153
2235
FieldLow-G
1207
0714
1119, 1147
Figure 32. The spectral type versus bolometric luminosity plot. The field polynomial and residuals from Filippazzo et al. (2015) isrepresented by the grey area. Over-plotted are objects in this work with measured parallaxes or estimated kinematic distances from highconfidence group membership. Lbol values were calculated as described in Filippazzo et al. (2015). Symbols distinguish very low (γ) fromintermediate (β) gravity sources. Objects are color coded by group membership.
Brown Dwarf Analogs to Exoplanets 45
M6 M8 L0 L2 L4 L6 L8 SpT
1000
1500
2000
2500
3000
T eff (
K)
M6 M8 L0 L2 L4 L6 L8 SpT
1000
1500
2000
2500
3000
T eff (
K)
AB DoradusTuc Hor` PictorisColumbaArgusTW HyaYoung Field? a `
TWA29TWA26
TWA28
PSO318
0045
2244
0047
0326
0355
VHS1256 B
220614250153
2235
FieldLow-G
1119, 1147
Figure 33. The spectral type versus Teff plot. Symbols are as described in Figure 32.
46 Faherty et al.
6.5 7.0 7.5 8.0 8.5log Age[yr]
−5.5
−5.0
−4.5
−4.0
−3.5
−3.0
−2.5
L bol
(Lsu
n)
51 Eri B
2M0219 b
β Pic b
AB Pic B
LP261-75 B
HD203030 B
HN Peg BGU Psc bHR8799 b
HR8799 d2M1207 b
1RXS 1609 b𝜅 And B
SDSS1110 VHS 1256 B
PSO 318
VHS 1256 A
CD 35-2722 b
TWA 27"TWA 28
1207-39
TWA 29
0032
004710 MJup
2 MJup
1147, 1119
0123
03552M0122 B
Figure 34. The age versus bolometric luminosity plot with model isochrone tracks at constant mass from Saumon & Marley (2008) (solidlines) and Baraffe et al. (2015) (dashed lines). We have color coded <13 MJup tracks in red, 13 MJup < M < 75 MJup tracks in greenand > 75 MJup blue. Over-plotted are both the young brown dwarfs discussed in this work and directly imaged exoplanets with measuredquantities.
Brown Dwarf Analogs to Exoplanets 47
−1.0 −0.5 0.0 0.5 1.0 1.5 2.0(J − H) (MKO)
18
16
14
12
10
8
MJ (
MKO
)
−1.0 −0.5 0.0 0.5 1.0 1.5 2.0(J − H) (MKO)
18
16
14
12
10
8
MJ (
MKO
)
GJ 504 b
VHS 1256 B 2M1207 b
PSO318
2M0355
SDSS1110GU Psc b
HN Peg b
HR8799 cdb
2M0122 B
ROXs12 b
HD1160 B
USco1610-1913 b2M0219A
β Pic b
2M0219 B
DH Tau b
51 Eri b
GQ Lup b
AB Pic B
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
Ross 458 C
Figure 35. The (J-H) versus MJ color magnitude diagram for brown dwarfs and directly imaged planetary mass companions. Allphotometry is on the MKO system. For the brown dwarfs lacking MKO L’ photometry, WISE W1 mags were converted using a polynomiallisted in Table 19. Objects have been color coded by nearby moving group membership and those of interest discussed in detail within thetext have been labeled.
48 Faherty et al.
−1.0 −0.5 0.0 0.5 1.0 1.5 2.0(J − H) (MKO)
20
18
16
14
12
10
8
MH (M
KO)
−1.0 −0.5 0.0 0.5 1.0 1.5 2.0(J − H) (MKO)
20
18
16
14
12
10
8
MH (M
KO)
GJ 504 b
VHS 1256 B2M1207 b
PSO318
2M0355
SDSS1110
GU Psc b
HN Peg b
HR8799 cdb
2M0122 B
ROXs12 bHD1160 B
USco1610-1913 b
2M0219A
β Pic b
2M0219 B
DH Tau b
51 Eri b
GQ Lup b
AB Pic B
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
Ross 458 C
Figure 36. The (J-H) versus MH (right) color magnitude diagram for brown dwarfs and directly imaged planetary mass companions.Symbols are as described in Figure 35.
−1 0 1 2 3(J − K) (MKO)
18
16
14
12
10
8
MJ (
MKO
)
−1 0 1 2 3(J − K) (MKO)
18
16
14
12
10
8
MJ (
MKO
)
GJ 504 bVHS 1256 B
2M1207 b
PSO318
2M0355
SDSS1110GU Psc b
HN Peg b
HR8799 cdb
2M0122 B
ROXs12 b
HD1160 B
USco1610-1913 b2M0219A
β Pic b
DH Tau b
GQ Lup b
AB Pic B
2M0103 B
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
Ross 458 C
−1 0 1 2 3(J − K) (MKO)
18
16
14
12
10
8
MK
(MKO
)
−1 0 1 2 3(J − K) (MKO)
18
16
14
12
10
8
MK
(MKO
)
Ross 458 C
GJ 504 b
VHS 1256 B
2M1207 b
PSO318
2M0355
SDSS1110
GU Psc b
HN Peg b
HR8799 cdb
2M0122 B
ROXs12 bHD1160 B
USco1610-1913 bDH Tau bGQ Lup b
AB Pic B
2M0103 B
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
Figure 37. The (J-K) versus MJ (left) and MK (right) color magnitude diagram for brown dwarfs and directly imaged planetary masscompanions. Symbols are as described in Figure 35.
Brown Dwarf Analogs to Exoplanets 49
1 2 3 4(J − L) (MKO)
18
16
14
12
10
8M
J (M
KO)
1 2 3 4(J − L) (MKO)
18
16
14
12
10
8M
J (M
KO)
GJ 504 b
PSO318
2M0355
SDSS1110
ROXs12 b
USco1610-1913 b
DH Tau b
51 Eri b
GQ Lup b
RXS1609 b
W0047
2M2244HR8799 cdb
GSC6214-210 bFU Tau b
ROXs42B b
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
2M0122 B
1 2 3 4(J − L) (MKO)
16
14
12
10
8
6
ML (
MKO
)
1 2 3 4(J − L) (MKO)
16
14
12
10
8
6
ML (
MKO
)
GJ 504 b
PSO318
2M0355
SDSS1110
ROXs12 b
USco1610-1913 b
DH Tau b
51 Eri b
GQ Lup b
W0047
2M2244
HR8799 cdb
GSC6214-210 bFU Tau b
ROXs42B b
RXS1609 b
2M0122 B
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
Figure 38. The (J-L) versus MJ (left) and ML (right) color magnitude diagram for brown dwarfs and directly imaged planetary masscompanions. Symbols are as described in Figure 35.
−1.0 −0.5 0.0 0.5 1.0 1.5(H − K) (MKO)
20
18
16
14
12
10
8
MH (M
KO)
−1.0 −0.5 0.0 0.5 1.0 1.5(H − K) (MKO)
20
18
16
14
12
10
8
MH (M
KO)
GJ 504 b
VHS 1256 B
2M1207 b
PSO318
2M0355
SDSS1110GU Psc b
HN Peg b
HR8799 ecdb
2M0122 B
ROXs12 bFU Tau b
USco1610-1913 b2M0219A
β Pic b2M0219 B
DH Tau b
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
Ross 458 C
−0.5 0.0 0.5 1.0 1.5(H − K) (MKO)
18
16
14
12
10
8M
K (M
KO)
−0.5 0.0 0.5 1.0 1.5(H − K) (MKO)
18
16
14
12
10
8M
K (M
KO)
GJ 504 b
VHS 1256 B
2M1207 b
PSO3182M0355
SDSS1110
GU Psc b
HN Peg b
2M0122 B
ROXs12 bFU Tau b
USco1610-1913 b2M0219A
β Pic b2M0219 B
DH Tau b
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
HR8799 ecdb
Ross 458 C
Figure 39. The (H-K) versus MH (left) and MK (right) color magnitude diagram for brown dwarfs and directly imaged planetary masscompanions. Symbols are as described in Figure 35.
0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0(H − L) (MKO)
20
18
16
14
12
10
8
MH (M
KO)
0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0(H − L) (MKO)
20
18
16
14
12
10
8
MH (M
KO)
GJ 504 b
PSO318
2M0355
SDSS1110HR8799 ecdb
ROXs12 b
USco1610-1913 b
DH Tau b
51 Eri b
GQ Lup b
RXS1609 b
W0047
2M2244
2M0122 B
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0(H − L) (MKO)
16
14
12
10
8
6
ML (
MKO
)
0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0(H − L) (MKO)
16
14
12
10
8
6
ML (
MKO
)
GJ 504 b
PSO318
2M0355
SDSS1110
HR8799 ecd
ROXs12 b
USco1610-1913 b
DH Tau b
51 Eri b
GQ Lup b
W0047
2M2244
2M0122 BRXS1609 b
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
HR8799 b
Figure 40. The (H-L) versus MH (left) and ML (right) color magnitude diagram for brown dwarfs and directly imaged planetary masscompanions. Symbols are as described in Figure 35.
50 Faherty et al.
0 1 2 3(K − L) (MKO)
18
16
14
12
10
8
MK
(MKO
)
0 1 2 3(K − L) (MKO)
18
16
14
12
10
8
MK
(MKO
)
GJ 504 b
PSO318
SDSS1110
ROXs12 b
USco1610-1913 bDH Tau b
GQ Lup b
RXS1609 b
W0047
2M2244
GSC6214-210 b
2M0355
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
HR8799 ecdb
0.5 1.0 1.5 2.0 2.5 3.0 3.5(K − L) (MKO)
16
14
12
10
8
6
ML (
MKO
)
0.5 1.0 1.5 2.0 2.5 3.0 3.5(K − L) (MKO)
16
14
12
10
8
6
ML (
MKO
)
GJ 504 b
PSO318
SDSS1110
ROXs12 b
USco1610-1913 bGQ Lup b
2M2244
GSC6214-210 b
RXS1609 b2M0355
W0047
!AB Doradus"β Pictoris"Tucana Horologium"Columba"TW Hydrae"< 8 Myr"!!PMC"
!"
HR8799 ecdb
Figure 41. The (K-L) versus MK (left) and ML (right) color magnitude diagram for brown dwarfs and directly imaged planetary masscompanions. Symbols are as described in Figure 35.
HR8799 b VHS1256 B
Field L7
1.4 1.6 1.8 2.0 2.2 2.4 2.6Wavelength (µm)
0.2
0.4
0.6
0.8
1.0
Nor
mal
ized
Fh
1.4 1.6 1.8 2.0 2.2 2.4 2.6Wavelength (µm)
0.2
0.4
0.6
0.8
1.0
Nor
mal
ized
Fh
Figure 42. The near-infrared spectrum comparison of HR8799 b (black, from Oppenheimer et al. 2013, Barman et al. 2011a), VHS 1256B (red, from Gauza et al. 2015), and a field L7 (Gagne et al. (2015b)).
Brown Dwarf Analogs to Exoplanets 51
M6 M8 L0 L2 L4 L6 L8 T0 T2 T4 T6 T8 SpT
−6
−5
−4
−3
log
(Lbo
l/LSu
n)
M6 M8 L0 L2 L4 L6 L8 T0 T2 T4 T6 T8 SpT
−6
−5
−4
−3
log
(Lbo
l/LSu
n)
AB DoradusTuc Hor` PictorisColumbaArgusTW Hya< 10 Myr?Young Field? a `
FieldLow-G
SDSS1110
1RXS1609 b
Roxs 42 Bb
CD 35-2722 B
β Pic b
2M0219 bAB Pic b
2M0122 B
LP261-75 B
51 Eri b
Ross 458 C
HN Peg b2M1207 b
HD203030 B Gu Psc b
HR8799 db
Figure 43. The spectral type versus bolometric luminosity plot for brown dwarfs and directly imaged planets. Lbol values and spectraltypes for planets have been taken from the literature with the exception of HR8799bd and 2M1207b which we delegate as L8 objects torepresent their nature as late-type objects. Symbols are as in Figure 32.
52 Faherty et al.Table
1P
hoto
metr
icP
rop
ert
ies
of
Low
Surf
ace
Gra
vit
yD
warf
s
2M
ASS
Desi
gnati
on
SpT
SpT
JH
KW
1W
2W
3W
4O
pT
IR2M
ASS
2M
ASS
2M
ASS
WIS
EW
ISE
WIS
EW
ISE
Refe
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
00011217+
1535355
––
L4β
15.5
22±
0.0
61
14.5
05±
0.0
52
13.7
1±
0.0
43
12.9
38±
0.0
23
12.5
17±
0.0
26
11.4
98±
0.1
77
8.9
53±
–5
00040288-6
410358
L1γ
L1γa
15.7
86±
0.0
71
14.8
31±
0.0
73
14.0
10±
0.0
45
13.3
70±
0.0
25
12.9
37±
0.0
27
12.1
78±
0.2
44
9.1
61±
–15
,27
00182834-6
703130
––
L0γ
15.4
57±
0.0
57
14.4
8±
0.0
61
13.7
11±
0.0
39
13.1
71±
0.0
25
12.7
68±
0.0
26
12.7
63±
0.4
45
9.0
46±
–5
00191296-6
226005
––
L1γ
15.6
4±
0.0
614.6
18±
0.0
54
13.9
57±
0.0
51
13.3
51±
0.0
25
12.8
83±
0.0
26
12.3
78±
0.2
62
9.1
14±
–5
00192626+
4614078
M8
–M
8β
12.6
03±
0.0
17
11.9
40±
0.0
21
11.5
02±
0.0
11
11.2
60±
0.0
23
11.0
01±
0.0
20
10.8
57±
0.0
70
9.4
01±
–7,
500274197+
0503417
M9.5β
L0βa
16.1
89±
0.0
92
15.2
88±
0.0
99
14.9
60±
0.1
15
14.6
19±
0.0
36
14.1
35±
0.0
54
12.2
39±
–8.8
90±
–6,
27,
36
00303013-1
450333
L7
–L
4-L
6β
16.2
78±
0.1
11
15.2
73±
0.1
14.4
81±
0.1
13.6
57±
0.0
28
13.2
63±
0.0
34
12.2
75±
–9.1
49±
–18,
500325584-4
405058
L0γ
L0β
14.7
76±
0.0
32
13.8
57±
0.0
32
13.2
70±
0.0
35
12.8
20±
0.0
25
12.4
90±
0.0
25
11.7
26±
0.1
87
9.2
89±
–2,
6,
27
003323.8
6-1
52130
L4β
L1
15.2
86±
0.0
56
14.2
08±
0.0
51
13.4
10±
0.0
39
12.8
01±
0.0
25
12.4
79±
0.0
27
11.8
88±
0.2
47
8.8
79±
–2,
6,
27
00344300-4
102266
––
L1β
15.7
07±
0.0
66
14.8
07±
0.0
64
14.0
84±
0.0
56
13.4
98±
0.0
26
13.0
98±
0.0
312.5
96±
0.3
94
9.2
85±
–5
00374306-5
846229
L0γ
––
15.3
74±
0.0
50
14.2
59±
0.0
51
13.5
90±
0.0
44
13.1
25±
0.0
26
12.7
38±
0.0
27
12.5
57±
0.3
80
9.3
24±
–2
00381489-6
403529
––
M9.5β
14.5
23±
0.0
313.8
67±
0.0
45
13.3
95±
0.0
33
12.9
04±
0.0
24
12.5
39±
0.0
24
11.7
46±
0.1
75
9.3
74±
–5
00425923+
1142104
––
M9β
14.7
54±
0.0
36
14.0
74±
0.0
42
13.5
14±
0.0
27
13.2
37±
0.0
26
12.9
18±
0.0
312.1
75±
–9.1
51±
–5
00452143+
1634446
L2β
L2γa
13.0
59±
0.0
18
12.0
59±
0.0
34
11.3
70±
0.0
19
10.7
68±
0.0
23
10.3
93±
0.0
19
9.7
35±
0.0
40
8.4
24±
0.2
61
2,
6,
27
00464841+
0715177
M9β
L0δ
13.8
85±
0.0
26
13.1
78±
0.0
34
12.5
50±
0.0
25
12.0
70±
0.0
26
11.6
38±
0.0
22
11.1
39±
0.1
81
9.0
24±
–1,
5,
27
00470038+
6803543
L7
(γ?)
L6-L
8γ
15.6
04±
0.0
68
13.9
68±
0.0
41
13.0
53±
0.0
29
11.8
76±
0.0
23
11.2
68±
0.0
20
10.3
27±
0.0
72
9.0
95±
0.4
53
34,
35
00550564+
0134365
L2γ
L2γa
16.4
36±
0.1
14
15.2
70±
0.0
74
14.4
40±
0.0
68
13.6
82±
0.0
27
13.2
04±
0.0
33
11.9
88±
–8.4
77±
–27,
36
00584253-0
651239
L0
–L
1β
14.3
11±
0.0
23
13.4
44±
0.0
28
12.9
04±
0.0
32
12.5
62±
0.0
25
12.2
48±
0.0
27
11.6
92±
0.4
11
8.7
39±
–18,
501033203+
1935361
L6β
L6β
16.2
88±
0.0
79
14.8
97±
0.0
55
14.1
49±
0.0
58
13.1
78±
0.0
24
12.6
96±
0.0
27
12.2
34±
0.3
25
8.2
90±
–8,
501174748-3
403258
L1β
L1βa
15.1
78±
0.0
34
14.2
09±
0.0
38
13.4
90±
0.0
36
13.0
28±
0.0
25
12.6
23±
0.0
26
11.8
02±
0.1
86
9.2
15±
–7,
6,
27
01205114-5
200349
––
L1γ
15.6
42±
0.0
71
14.6
6±
0.0
72
13.7
52±
0.0
53
13.2
3±
0.0
26
12.7
78±
0.0
26
11.8
47±
0.1
68
8.9
49±
–5
01231125-6
921379
M7.5γ
––
12.3
20±
0.0
19
11.7
11±
0.0
24
11.3
23±
0.0
24
11.0
60±
0.0
23
10.8
18±
0.0
21
10.5
95±
0.0
62
9.4
26±
–4
01244599-5
745379
L0γ
L0γa
16.3
08±
0.1
04
15.0
59±
0.0
88
14.3
20±
0.0
88
13.7
73±
0.0
26
13.3
42±
0.0
32
12.4
49±
0.3
13
8.9
08±
–2,
27
01262109+
1428057
L4γ
L2γ
17.1
08±
0.2
14
16.1
72±
0.2
18
15.2
80±
0.1
45
14.2
37±
0.0
29
13.7
02±
0.0
37
12.3
79±
–9.1
27±
–21,
601294256-0
823580
M5
–M
7β
10.6
55±
0.0
21
10.0
85±
0.0
23
9.7
71±
0.0
23
9.5
45±
0.0
22
9.3
27±
0.0
29.2
06±
0.0
32
8.8
91±
0.4
58
17,
501415823-4
633574
L0γ
L0γ
14.8
32±
0.0
41
13.8
75±
0.0
24
13.1
00±
0.0
30
12.5
51±
0.0
24
12.1
70±
0.0
22
11.9
21±
0.2
12
9.2
43±
–2,
6,
28
01531463-6
744181
L2
–L
3β
16.4
12±
0.1
34
15.1
09±
0.0
86
14.4
24±
0.1
03
13.7
13±
0.0
26
13.2
16±
0.0
28
12.5
14±
0.2
89.3
35±
–1,
502103857-3
015313
L0γ
L0γa
15.0
66±
0.0
47
14.1
61±
0.0
44
13.5
00±
0.0
42
13.0
03±
0.0
26
12.6
52±
0.0
26
11.9
34±
0.1
95
9.3
55±
–5,
27
02212859-6
831400
M8β
––
13.9
65±
0.0
33
13.2
75±
0.0
32
12.8
06±
0.0
37
12.4
71±
0.0
24
12.1
92±
0.0
23
11.6
04±
0.1
07
9.6
14±
–27
02215494-5
412054
M9β
––
13.9
02±
0.0
31
13.2
21±
0.0
31
12.6
70±
0.0
30
12.3
25±
0.0
24
11.9
63±
0.0
22
11.4
40±
0.1
22
9.4
81±
–1,
13,
27
02235464-5
815067
L0γ
––
15.0
70±
0.0
48
14.0
03±
0.0
36
13.4
20±
0.0
42
12.8
19±
0.0
24
12.4
31±
0.0
24
11.6
44±
0.1
54
9.4
66±
–2
02251947-5
837295
M9β
M9γa
13.7
38±
0.0
25
13.0
58±
0.0
25
12.5
60±
0.0
26
12.2
34±
0.0
24
11.9
26±
0.0
23
11.9
94±
0.1
90
9.2
18±
–27,
36
02265658-5
327032
––
L0δ
15.4
03±
0.0
44
14.3
46±
0.0
513.7
52±
0.0
45
13.2
19±
0.0
25
12.7
83±
0.0
26
11.5
8±
0.1
48.6
4±
0.2
56
502292794-0
053282
––
L0γ
16.4
90±
0.0
99
15.7
46±
0.0
99
15.1
82±
0.1
38
14.7
20±
0.0
32
14.3
28±
0.0
45
12.6
79±
–8.7
24±
–6
02340093-6
442068
L0γ
L0βγa
15.3
25±
0.0
62
14.4
42±
0.0
55
13.8
50±
0.0
69
13.2
47±
0.0
25
12.9
05±
0.0
26
12.6
19±
0.2
79
9.4
94±
–15,
27
02410564-5
511466
––
L1γ
15.3
87±
0.0
57
14.3
26±
0.0
52
13.7
39±
0.0
38
13.1
85±
0.0
23
12.8
09±
0.0
26
12.2
49±
0.2
42
9.3
49±
–5
02411151-0
326587
L0γ
L1γ
15.7
99±
0.0
64
14.8
11±
0.0
53
14.0
40±
0.0
49
13.6
38±
0.0
25
13.2
56±
0.0
29
12.7
66±
0.4
15
9.0
00±
–14,
6
02501167-0
151295f
––
M7β
12.8
86±
0.0
26
12.2
78±
0.0
21
11.9
09±
0.0
17
11.6
91±
0.0
23
11.4
51±
0.0
22
11.0
35±
0.1
58
8.8
27±
–5
02530084+
1652532d
M6.5
–M
7βd
8.3
94±
0.0
21
7.8
83±
0.0
37
7.5
85±
0.0
43
7.3
22±
0.0
27
7.0
57±
0.0
26.8
97±
0.0
17
6.7
18±
0.0
76
20,
25,
502535980+
3206373
M7β
M6β
13.6
16±
0.0
21
12.9
31±
0.0
20
12.5
50±
0.0
23
12.3
24±
0.0
25
12.1
27±
0.0
24
11.8
08±
0.2
50
8.5
09±
–27,
36
02583123-1
520536
––
L3β
15.9
08±
0.0
72
14.8
66±
0.0
614.1
92±
0.0
55
13.6
23±
0.0
25
13.1
94±
0.0
28
12.5
78±
0.3
05
9.5
42±
–5
03032042-7
312300
L2γ
––
16.1
37±
0.1
07
15.0
96±
0.0
85
14.3
20±
0.0
84
13.7
77±
0.0
25
13.3
50±
0.0
26
12.2
88±
0.1
67
9.3
44±
0.3
41
15
03164512-2
848521
L0
–L
1β
14.5
78±
0.0
39
13.7
72±
0.0
35
13.1
14±
0.0
35
12.6
49±
0.0
23
12.3
12±
0.0
23
11.7
43±
0.1
25
9.3
64±
–7,
503231002-4
631237
L0γ
L0γa
15.3
89±
0.0
69
14.3
21±
0.0
61
13.7
00±
0.0
50
13.0
75±
0.0
24
12.6
65±
0.0
24
11.9
39±
0.1
60
9.1
80±
–2,
27
03264225-2
102057
L5β
L5βγa
16.1
34±
0.0
93
14.7
93±
0.0
75
13.9
20±
0.0
65
12.9
50±
0.0
24
12.4
35±
0.0
23
12.1
73±
0.2
03
9.6
63±
–5,
27
03350208+
2342356
M8.5
–M
7.5β
12.2
50±
0.0
17
11.6
55±
0.0
20
11.2
61±
0.0
14
11.0
44±
0.0
23
10.7
67±
0.0
20
10.7
62±
0.1
30
8.9
32±
–12,
603393521-3
525440
M9β
L0β
10.7
25±
0.0
18
10.0
17±
0.0
20
9.5
50±
0.0
21
9.1
33±
0.0
22
8.8
08±
0.0
19
8.2
72±
0.0
17
7.9
97±
0.1
10
12,
6,
27
03420931-2
904317
––
L0β
15.9
18±
0.0
85
15.3
53±
0.1
06
14.3
78±
0.0
85
13.9
69±
0.0
27
13.5
4±
0.0
32
12.6
73±
–9.2
37±
–5
03421621-6
817321
L4γ
––
16.8
54±
0.1
38
15.3
86±
0.0
86
14.5
41±
0.0
89
13.9
55±
0.0
25
13.4
82±
0.0
25
12.9
94±
0.4
05
9.7
23±
–5
03550477-1
032415
M8.5
–M
8.5β
13.0
8±
0.0
25
12.4
62±
0.0
24
11.9
75±
0.0
23
11.7
12±
0.0
24
11.4
25±
0.0
22
10.8
65±
0.0
95
8.6
27±
0.3
09
5,
36
03552337+
1133437
L5γ
L3-L
6γ
14.0
50±
0.0
20
12.5
30±
0.0
29
11.5
30±
0.0
19
10.5
28±
0.0
23
9.9
43±
0.0
21
9.2
94±
0.0
38
8.3
17±
–2,
5,
21
03572695-4
417305
L0β
L0β
14.3
67±
0.0
29
13.5
31±
0.0
25
12.9
10±
0.0
26
12.4
75±
0.0
23
12.0
86±
0.0
21
11.6
00±
0.0
84
9.3
18±
–14,
27
04062677-3
812102
L0γ
L1γ
16.7
68±
0.1
26
15.7
11±
0.1
01
15.1
10±
0.1
16
14.4
49±
0.0
30
14.1
00±
0.0
41
12.5
20±
–9.0
97±
–15,
604185879-4
507413
––
L3γ
16.1
63±
0.0
84
15.0
46±
0.0
74
14.5
95±
0.0
88
13.8
64±
0.0
27
13.4
55±
0.0
312.7
83±
–9.6
42±
–5
04210718-6
306022
L5β
L5γa
15.5
65±
0.0
48
14.2
84±
0.0
40
13.4
50±
0.0
42
12.5
58±
0.0
22
12.1
35±
0.0
21
11.5
98±
0.0
95
9.2
45±
–2,
27
04351455-1
414468
M8γ
M7γa
11.8
79±
0.0
29
10.6
22±
0.0
27
9.9
51±
0.0
21
9.7
11±
0.0
24
9.2
68±
0.0
21
9.1
36±
0.0
34
8.5
14±
0.3
10
27,
36
Brown Dwarf Analogs to Exoplanets 53Table
1—
Continued
2M
ASS
Desi
gnati
on
SpT
SpT
JH
KW
1W
2W
3W
4O
pT
IR2M
ASS
2M
ASS
2M
ASS
WIS
EW
ISE
WIS
EW
ISE
Refe
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
04362788-4
114465
M8β
M9γ
13.0
97±
0.0
23
12.4
30±
0.0
20
12.0
50±
0.0
24
11.7
40±
0.0
23
11.4
60±
0.0
21
11.1
11±
0.0
82
9.1
84±
–13,
6,
27
04400972-5
126544
––
L0γ
15.6
85±
0.0
69
14.7
79±
0.0
56
14.1
71±
0.0
613.5
85±
0.0
24
13.1
93±
0.0
26
12.3
71±
0.2
11
8.9
29±
–5
04433761+
0002051
M9γ
M9γ
12.5
07±
0.0
23
11.8
04±
0.0
22
11.2
20±
0.0
19
10.8
26±
0.0
24
10.4
76±
0.0
21
10.0
31±
0.0
54
8.4
23±
–3,
604493288+
1607226
––
M9γ
14.2
72±
0.0
26
13.4
9±
0.0
313.0
77±
0.0
29
12.7
3±
0.0
25
12.4
23±
0.0
27
11.5
07±
0.2
16
8.8
71±
–5
05012406-0
010452
L4γ
L3γa
14.9
82±
0.0
36
13.7
13±
0.0
33
12.9
60±
0.0
34
12.0
50±
0.0
24
11.5
18±
0.0
22
10.9
52±
0.1
07
9.1
65±
–2,
6,
27
05104958-1
843548
––
L2β
15.3
52±
0.0
56
14.3
41±
0.0
53
13.8
13±
0.0
55
13.2
56±
0.0
25
12.9
4±
0.0
29
12.6
8±
–9.1
88±
–5
05120636-2
949540
L5γ
L5βa
15.4
63±
0.0
55
14.1
56±
0.0
47
13.2
90±
0.0
41
12.3
78±
0.0
23
11.9
21±
0.0
23
11.3
29±
0.1
05
9.1
03±
–14,
5,
27
05181131-3
101529
M6.5
–M
7β
11.8
78±
0.0
26
11.2
34±
0.0
22
10.9±
0.0
19
10.6
41±
0.0
23
10.4
03±
0.0
19
10.1
11±
0.0
43
9.1
27±
0.4
57
26,
505184616-2
756457
L1γ
L1γ
15.2
62±
0.0
41
14.2
95±
0.0
45
13.6
20±
0.0
39
13.0
45±
0.0
24
12.6
61±
0.0
26
12.5
81±
0.3
49
9.2
19±
–3,
605264316-1
824315
––
M7β
12.3
58±
0.0
19
11.8
36±
0.0
22
11.4
48±
0.0
21
11.2
01±
0.0
23
10.9
44±
0.0
21
10.7
9±
0.0
81
8.9
84±
–5
05341594-0
631397
M8γ
M8γ
16.0
54±
0.0
76
15.3
69±
0.0
96
14.9
40±
0.0
97
14.7
85±
0.0
36
14.2
56±
0.0
56
11.5
90±
–8.2
65±
0.2
95
27,
36
05361998-1
920396
L2γ
L2γa
15.7
68±
0.0
73
14.6
93±
0.0
70
13.8
50±
0.0
61
13.2
62±
0.0
26
12.7
89±
0.0
27
12.5
51±
0.3
95
9.2
42±
–3,
6,
27
05402325-0
906326
––
M9β
14.5
86±
0.0
37
13.8
49±
0.0
35
13.3
3±
0.0
47
13.0
3±
0.0
25
12.7
44±
0.0
28
11.9
67±
0.2
67
8.9
38±
–5
05575096-1
359503
M7
–M
7γ
12.8
71±
0.0
19
12.1
45±
0.0
26
11.7
32±
0.0
21
11.3
36±
0.0
23
10.8
03±
0.0
20
7.8
89±
0.0
17
5.0
20±
0.0
25
27,
36
06023045+
3910592
L1
–L
1β
12.3
00±
0.0
18
11.4
51±
0.0
19
10.8
65±
0.0
18
10.4
35±
0.0
22
10.1
24±
0.0
22
9.5
91±
0.0
40
8.4
28±
–24,
606085283-2
753583
M8.5γ
L0γ
13.5
95±
0.0
26
12.8
97±
0.0
24
12.3
70±
0.0
24
11.9
76±
0.0
24
11.6
23±
0.0
21
11.3
14±
0.1
13
9.0
93±
–14,
606272161-5
308428
––
L0βγ
16.3
85±
0.1
13
15.2
34±
0.0
91
14.6
9±
0.0
87
13.8
83±
0.0
26
13.5
02±
0.0
29
13.3
92±
0.5
04
9.7
4±
–5
06322402-5
010349
L3β
L4γ
15.0
24±
0.0
41
14.0
31±
0.0
38
13.3
37±
0.0
29
12.6
10±
0.0
23
12.1
69±
0.0
22
11.7
29±
0.1
46
8.9
19±
–5
06524851-5
741376
M8β
––
13.6
32±
0.0
25
12.9
65±
0.0
22
12.4
50±
0.0
21
12.1
53±
0.0
23
11.8
57±
0.0
21
11.0
41±
0.0
53
9.6
00±
0.3
73
1,
13
07123786-6
155528
L1β
L1γa
15.2
96±
0.0
62
14.3
92±
0.0
42
13.6
70±
0.0
48
12.9
91±
0.0
24
12.6
26±
0.0
22
11.4
78±
0.0
95
9.5
12±
–2,
27
07140394+
3702459
M8
–M
7.5β
11.9
76±
0.0
19
11.2
52±
0.0
28
10.8
38±
0.0
17
10.5
66±
0.0
24
10.3
46±
0.0
210.2
02±
0.0
57
8.7
98±
–4,1
,13,
27
08095903+
4434216
––
L6p
16.4
37±
0.1
14
15.1
84±
0.0
97
14.4
17±
0.0
58
13.3
44±
0.0
26
12.8
1±
0.0
28
11.7
85±
0.2
06
9.0
55±
–5
08561384-1
342242
––
M8γ
13.6
02±
0.0
23
12.9
76±
0.0
28
12.4
89±
0.0
23
12.1
54±
0.0
23
11.6
2±
0.0
22
9.8
82±
0.0
46
8.3
76±
0.2
71
508575849+
5708514
L8
–L
8–
15.0
38±
0.0
38
13.7
9±
0.0
41
12.9
62±
0.0
28
12.0
19±
0.0
24
11.4
15±
0.0
21
10.3
76±
0.0
58
8.5
69±
0.2
714,
509451445-7
753150
––
M9β
13.8
93±
0.0
28
13.2
32±
0.0
29
12.7
87±
0.0
29
12.5
12±
0.0
22
12.2
79±
0.0
22
12.2
16±
–9.3
43±
–5
09532126-1
014205
M9γ
M9βa
13.4
69±
0.0
26
12.6
44±
0.0
26
12.1
40±
0.0
21
11.7
57±
0.0
23
11.4
04±
0.0
21
10.7
61±
0.1
00
8.7
19±
–3,
5,
27
09593276+
4523309
––
L3γ
15.8
80±
0.0
70
14.7
59±
0.0
68
13.6
73±
0.0
44
12.8
60±
0.0
25
12.3
63±
0.0
25
11.6
54±
0.1
70
9.0
44±
–27
G196-3
BL
3β
L3γ
14.8
31±
0.0
45
13.6
48±
0.0
42
12.7
78±
0.0
33
–±
––±
––±
––±
–14,
510212570-2
830427
––
L4βγ
16.9
14±
0.1
54
15.8
51±
0.1
12
14.9
81±
0.1
24
14.1
58±
0.0
313.6
77±
0.0
38
12.4
31±
–9.2
47±
–5
10220489+
0200477
M9β
M9β
14.1
00±
0.0
29
13.3
98±
0.0
30
12.9
00±
0.0
30
12.6
12±
0.0
25
12.3
40±
0.0
29
11.9
65±
0.4
11
8.5
31±
–1,8
,610224821+
5825453
L1β
L1β
13.4
99±
0.0
23
12.6
42±
0.0
31
12.1
60±
0.0
23
11.7
62±
0.0
23
11.4
96±
0.0
21
11.2
00±
0.1
09
9.1
33±
–14,
6T
WA
28
M8.5γ
M9γa
13.0
34±
0.0
21
12.3
56±
0.0
20
11.8
90±
0.0
23
11.4
35±
0.0
24
10.7
93±
0.0
21
9.3
85±
0.0
33
8.0
21±
0.1
86
23,
6,
27
11064461-3
715115
––
M9γ
14.4
87±
0.0
28
13.8
45±
0.0
26
13.3
39±
0.0
38
13.0
72±
0.0
25
12.7
53±
0.0
27
12.1
9±
–9.0
49±
–5
11083081+
6830169
L1γ
L1γ
13.1
23±
0.0
212.2
35±
0.0
19
11.5
83±
0.0
17
11.1
03±
0.0
24
10.7
54±
0.0
21
10.2
05±
0.0
43
9.4
94±
–5
11193254-1
137466c
––
L7γ
17.4
74±
0.0
58
15.7
88±
0.0
34
14.7
51±
0.0
12
13.5
48±
0.0
26
12.8
83±
0.0
27
12.2
44±
0.4
11
8.9
40±
–32,
33
11271382-3
735076
––
L0δ
16.4
69±
0.0
97
15.5
68±
0.1
07
15.2
29±
0.1
55
14.4
62±
0.0
32
14.1
03±
0.0
47
11.8
04±
0.1
85
9.2
29±
–5
TW
A26
M9γ
M9γ
12.6
86±
0.0
26
11.9
96±
0.0
22
11.5
03±
0.0
23
11.1
55±
0.0
23
10.7
93±
0.0
20
10.6
26±
0.0
75
8.4
79±
–1,
6,
5114724.1
0-2
04021.3
c–
–L
7γ
17.6
37±
0.0
58
15.7
64±
0.1
12
14.8
72±
0.0
11
13.7
18±
0.0
26
13.0
90±
0.0
30
12.1
55±
–8.9
13±
–31
11480096-2
836488
––
L1β
16.1
13±
0.0
79
15.1
86±
0.0
81
14.5
63±
0.0
84
14.1
39±
0.0
29
13.7
74±
0.0
39
12.2
29±
–9.2
4±
–5
11544223-3
400390
L0β
L1βa
14.1
95±
0.0
31
13.3
31±
0.0
27
12.8
50±
0.0
32
12.3
50±
0.0
23
12.0
37±
0.0
23
11.3
69±
0.1
06
9.5
48±
–14,
5,
27
TW
A27A
M8γ
M8γ
13.0
00±
0.0
30
12.3
90±
0.0
30
11.9
50±
0.0
30
11.5
56±
0.0
23
11.0
09±
0.0
20
9.4
56±
0.0
27
8.0
29±
0.1
33
10,
6,
27
12074836-3
900043
L0γ
L1γ
15.4
94±
0.0
58
14.6
08±
0.0
49
14.0
40±
0.0
60
13.6
34±
0.0
25
13.2
15±
0.0
28
13.2
02±
0.5
30
9.1
96±
–19
12271545-0
636458
M9
–M
8.5β
14.1
95±
0.0
25
13.3
89±
0.0
32
12.8
84±
0.0
34
12.5
16±
0.0
312.2
59±
0.0
27
11.8
51±
0.2
79
9.0
36±
–7,
5T
WA
29
M9.5γ
L0γ
14.5
18±
0.0
32
13.8
00±
0.0
33
13.3
69±
0.0
36
12.9
94±
0.0
23
12.6
23±
0.0
23
12.5
62±
–9.0
93±
–11,
6,
27
12474428-3
816464
––
M9γ
14.7
85±
0.0
33
14.0
96±
0.0
36
13.5
73±
0.0
39
13.1
08±
0.0
24
12.5
23±
0.0
25
10.9
53±
0.0
77
8.8
41±
0.2
93
19
12535039-4
211215
––
M9.5γ
16.0
02±
0.1
04
15.3±
0.1
04
14.7
39±
0.1
06
14.2
79±
0.0
27
13.9
2±
0.0
36
12.5
91±
–9.6
6±
–5
12563961-2
718455
––
L4βa
16.4
16±
0.1
28
15.3
74±
0.1
22
14.7
09±
0.0
93
14.0
88±
0.0
27
13.6
95±
0.0
34
12.4
74±
0.3
13
9.4
52±
–5,
27
14112131-2
119503
M9β
M8βa
12.4
37±
0.0
18
11.8
26±
0.0
26
11.3
30±
0.0
19
11.0
77±
0.0
23
10.8
15±
0.0
22
10.6
48±
0.0
65
8.8
12±
–7,
5,
27
14252798-3
650229
L3
–L
4γ
13.7
47±
0.0
28
12.5
75±
0.0
22
11.8
05±
0.0
27
10.9
98±
0.0
22
10.5
76±
0.0
20
10.0
10±
0.0
42
9.5
66±
–1,
515104786-2
818174
M9
–M
9β
12.8
38±
0.0
28
12.1
1±
0.0
32
11.6
87±
0.0
311.3
15±
0.0
25
11.0
12±
0.0
24
11.0
78±
0.1
96
8.2
5±
–1,
515291017+
6312539
––
M8β
11.6
43±
0.0
21
10.9
37±
0.0
28
10.5
54±
0.0
23
10.2
9±
0.0
23
10.0
58±
0.0
21
9.7
19±
0.0
27
9.2
41±
0.3
31
515382417-1
953116
L4γ
L4γa
15.9
34±
0.0
63
14.8
52±
0.0
60
14.0
00±
0.0
48
13.1
72±
0.0
27
12.7
21±
0.0
29
11.3
69±
0.1
77
8.8
08±
–27,
36
15470557-1
626303A
––
M9β
13.8
64±
0.0
29
13.2
43±
0.0
29
12.7
35±
0.0
27
12.4
37±
0.0
24
12.1
44±
0.0
26
11.7
15±
–8.5
49±
–5
15474719-2
423493
M9γ
L0β
13.9
70±
0.0
26
13.2
71±
0.0
32
12.7
40±
0.0
23
12.4
07±
0.0
25
12.1
05±
0.0
32
12.1
11±
–8.7
39±
–1
15515237+
0941148
L4γ
>L
5γa
16.3
19±
0.1
10
15.1
14±
0.0
71
14.3
10±
0.0
57
13.6
00±
0.0
25
13.1
21±
0.0
30
12.6
77±
0.4
78
9.1
56±
–1,
27
15525906+
2948485
L0β
L0β
13.4
78±
0.0
23
12.6
06±
0.0
24
12.0
20±
0.0
26
11.5
44±
0.0
23
11.2
07±
0.0
20
10.6
64±
0.0
49
9.0
03±
–2,
615575011-2
952431
M9δ
L1γa
16.3
16±
0.1
19
15.4
50±
0.1
04
14.8
50±
0.1
11
14.4
35±
0.0
37
14.0
66±
0.0
58
12.1
54±
0.3
44
8.6
68±
–15,
6,
27
16154255+
4953211
L4γ
L3-L
6γ
16.7
89±
0.1
37
15.3
32±
0.0
98
14.3
10±
0.0
69
13.2
02±
0.0
24
12.6
21±
0.0
22
12.1
31±
0.1
30
9.3
05±
–3,
6
54 Faherty et al.Table
1—
Continued
2M
ASS
Desi
gnati
on
SpT
SpT
JH
KW
1W
2W
3W
4O
pT
IR2M
ASS
2M
ASS
2M
ASS
WIS
EW
ISE
WIS
EW
ISE
Refe
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
17111353+
2326333
L0γ
L1βa
14.4
99±
0.0
24
13.6
68±
0.0
30
13.0
60±
0.0
26
12.5
81±
0.0
24
12.2
26±
0.0
24
11.6
62±
0.1
52
9.3
34±
–3,
6,
27
17260007+
1538190
L3.5γ
L3γa
15.6
69±
0.0
63
14.4
65±
0.0
45
13.6
60±
0.0
49
13.0
71±
0.0
25
12.6
94±
0.0
26
11.5
56±
0.1
57
9.3
09±
–5,
27
17410280-4
642218
––
L6-L
8γa
15.7
86±
0.0
75
14.5
34±
0.0
54
13.4
38±
0.0
35
12.3
01±
0.0
25
11.6
75±
0.0
23
11.4
32±
0.1
90
8.5
41±
–5,
27
18212815+
1414010
L4.5
—L
4p
eca
13.4
31±
0.0
21
12.3
96±
0.0
17
11.6
50±
0.0
19
10.8
53±
0.0
23
10.4
75±
0.0
20
9.9
28±
0.0
52
9.0
67±
0.5
34
27,
29,
30
19350976-6
200473
––
L1γ
16.2
54±
0.1
05
15.2
93±
0.0
94
14.7
24±
0.0
98
14.0
59±
0.0
29
13.6
5±
0.0
39
12.8
81±
–8.5
59±
–5
19355595-2
846343
M9γ
M9γa
13.9
53±
0.0
24
13.1
80±
0.0
20
12.7
10±
0.0
28
12.3
47±
0.0
26
11.9
10±
0.0
25
10.5
19±
0.0
76
8.6
36±
–27,
36
19564700-7
542270
L0γ
L2γa
16.1
54±
0.1
02
15.0
36±
0.0
96
14.2
30±
0.0
66
13.6
93±
0.0
27
13.2
49±
0.0
31
12.6
78±
–9.1
71±
–2,
27
20004841-7
523070
M9γ
M9γa
12.7
34±
0.0
23
11.9
67±
0.0
26
11.5
10±
0.0
24
11.1
08±
0.0
23
10.7
97±
0.0
20
10.5
50±
0.0
69
8.5
48±
–4,
5,
27
20025073-0
521524
L5β
L5-L
7γa
15.3
16±
0.0
49
14.2
78±
0.0
50
13.4
20±
0.0
35
12.5
32±
0.0
23
12.0
90±
0.0
26
11.4
41±
0.2
09
8.8
18±
–3,
5,
27
20113196-5
048112
––
L3γ
16.4
23±
0.1
09
15.2
57±
0.0
81
14.5
77±
0.0
82
14.0
09±
0.0
31
13.6
68±
0.0
38
12.4
31±
–9.0
84±
–5
20135152-2
806020
M9γ
L0γa
14.2
42±
0.0
28
13.4
61±
0.0
27
12.9
40±
0.0
26
12.5
25±
0.0
28
12.1
63±
0.0
27
11.8
77±
0.2
76
8.6
63±
–1,
6,
27
20282203-5
637024
––
M8.5γ
13.8
37±
0.0
21
13.2
43±
0.0
27
12.7
1±
0.0
27
12.4
72±
0.0
22
12.1
73±
0.0
24
12.2
98±
0.3
15
8.6
69±
–5
20334473-5
635338
––
L0γ
15.7
18±
0.0
88
15.1
37±
0.1
09
14.2
44±
0.0
81
13.8
17±
0.0
27
13.4
15±
0.0
34
12.3
76±
–9.2
7±
–5
20391314-1
126531
M8
–M
7β
13.7
92±
0.0
24
13.1
29±
0.0
38
12.6
8±
0.0
28
12.4
65±
0.0
23
12.1
66±
0.0
24
12.5
96±
0.5
38
9.0
4±
–7,
520575409-0
252302
L1.5
–L
2β
13.1
21±
0.0
21
12.2
68±
0.0
22
11.7
24±
0.0
23
11.2
61±
0.0
22
10.9
81±
0.0
20
10.4
31±
0.0
79
8.9
06±
–7,
25,
27
21140802-2
251358bc
––
L6-L
8γa
17.2
94±
0.0
815.6
24±
0.0
414.4
35±
0.0
413.2
16±
0.0
26
12.4
61±
0.0
31
11.8
38±
0.3
58
8.5
81±
–9,
27
21265040-8
140293
L3γ
L3γa
15.5
42±
0.0
55
14.4
05±
0.0
53
13.5
50±
0.0
41
12.9
10±
0.0
24
12.4
72±
0.0
23
11.8
85±
0.1
61
9.3
57±
–2,
27
21324036+
1029494
––
L4β
16.5
94±
0.1
38
15.3
66±
0.1
13
14.6
34±
0.1
14.0
3±
0.0
33
13.5
78±
0.0
42
12.3
83±
0.3
79
8.5
12±
–5
21543454-1
055308
L4β
L5γa
16.4
40±
0.1
21
15.0
69±
0.0
82
14.2
00±
0.0
68
13.3
67±
0.0
26
12.9
17±
0.0
29
12.0
54±
0.3
16
8.4
26±
–22,
27
21544859-7
459134
––
M9.5β
14.2
88±
0.0
29
13.5
68±
0.0
42
13.0
84±
0.0
32
12.7
08±
0.0
25
12.3
76±
0.0
25
11.9
91±
0.2
11
8.9
13±
–5
21572060+
8340575
L0
–M
9γ
13.9
72±
0.0
26
13.0
66±
0.0
33
12.5
84±
0.0
25
12.0
88±
0.0
23
11.6
81±
0.0
21
11.0
07±
0.0
79
8.7
62±
–5
22025794-5
605087
––
M9γ
14.3
56±
0.0
34
13.6
16±
0.0
35
13.1
6±
0.0
36
12.8
09±
0.0
25
12.5
55±
0.0
25
11.7
28±
0.1
89.3
22±
–5
22064498-4
217208
L4γ
L4γa
15.5
55±
0.0
65
14.4
47±
0.0
61
13.6
10±
0.0
55
12.8
23±
0.0
24
12.3
76±
0.0
25
11.8
87±
0.2
22
9.2
59±
–5,
27
22081363+
2921215
L3γ
L3γ
15.7
97±
0.0
84
14.7
93±
0.0
70
14.1
50±
0.0
73
13.3
54±
0.0
27
12.8
88±
0.0
27
12.5
84±
0.3
91
9.2
98±
–14,
522134491-2
136079
L0γ
L0γ
15.3
76±
0.0
32
14.4
04±
0.0
55
13.7
60±
0.0
38
13.2
29±
0.0
27
12.8
32±
0.0
29
11.5
52±
0.2
03
9.0
70±
–14,
622351658-3
844154
––
L1.5γ
15.1
83±
0.0
51
14.2
72±
0.0
46
13.6
31±
0.0
44
13.0
07±
0.0
24
12.6
47±
0.0
27
12.5
35±
0.4
36
8.7
73±
–5
22353560-5
906306
––
M8.5β
14.2
81±
0.0
29
13.5
92±
0.0
37
13.1
68±
0.0
32
12.6
91±
0.0
24
12.3
63±
0.0
26
12.0
8±
0.3
09
9.0
94±
–5
22443167+
2043433
L6.5
p–
L6-L
8γa
16.4
76±
0.1
40
14.9
99±
0.0
65
14.0
22±
0.0
73
12.7
77±
0.0
24
12.1
08±
0.0
24
11.1
36±
0.1
15
9.3
01±
–14,
6,
27
22495345+
0044046
L4γ
L3βa
16.5
87±
0.1
24
15.4
21±
0.1
09
14.3
60±
0.0
70
13.5
76±
0.0
27
13.1
44±
0.0
50
11.2
84±
–7.6
87±
–14,
6,
27
23153135+
0617146
L0γ
L0γa
15.8
61±
0.0
82
14.7
57±
0.0
69
14.0
70±
0.0
63
13.5
52±
0.0
26
13.0
95±
0.0
31
11.6
71±
0.2
30
8.5
92±
–27,
36
23224684-3
133231
L0β
L2β
13.5
77±
0.0
27
12.7
89±
0.0
23
12.3
24±
0.0
24
11.9
74±
0.0
23
11.7
07±
0.0
23
11.2
53±
0.1
28
9.1
53±
–1,
623225299-6
151275
L2γ
L3γa
15.5
45±
0.0
61
14.5
35±
0.0
62
13.8
60±
0.0
42
13.2
43±
0.0
26
12.8
41±
0.0
29
12.6
79±
0.3
91
9.3
78±
–2,
5,
27
23231347-0
244360
M8.5
–M
8β
13.5
8±
0.0
23
12.9
25±
0.0
312.4
81±
0.0
26
12.2
37±
0.0
25
11.9
54±
0.0
24
12.2
28±
0.3
91
8.5
12±
–3,
523255604-0
259508
L3
–L
1γ
15.9
61±
0.0
77
14.9
35±
0.0
69
14.1
15±
0.0
56
13.6
95±
0.0
27
13.3
48±
0.0
34
11.8
83±
–8.6
77±
–16,
523360735-3
541489
––
M9β
14.6
51±
0.0
25
13.8
09±
0.0
25
13.3
85±
0.0
41
13.0
02±
0.0
24
12.6
47±
0.0
26
12.5
18±
0.4
18
9.1
77±
–5
23433470-3
646021
––
L3-L
6γ
16.5
68±
0.1
315.0
11±
0.0
63
14.1
94±
0.0
64
13.1
21±
0.0
24
12.6
12±
0.0
27
11.6
98±
0.1
88
9.1
38±
–5
23453903+
0055137
M9
–M
9β
13.7
71±
0.0
27
13.1
17±
0.0
26
12.5
81±
0.0
28
12.2
12±
0.0
25
11.8
79±
0.0
23
11.4
65±
0.2
03
8.9
41±
–1,
523520507-1
100435
M7
–M
8β
12.8
4±
0.0
18
12.1
66±
0.0
211.7
42±
0.0
18
11.4
4±
0.0
25
11.1
46±
0.0
22
10.8
49±
0.1
09
8.8
77±
–3,
5
Note.
—R
efe
rences:
1=
Reid
et
al.
(2008),
2=
Cru
zet
al.
(2009),
3=
Cru
zet
al.
(2007),
4=
Sch
mid
tet
al.
(2007),
5=
Gagne
et
al.
(2015b),
6=
Allers
&L
iu(2
013),
7=
Cru
zet
al.
(2003),
8=
Fahert
yet
al.
(2012),
9=
Liu
et
al.
(2013),
10=
Giz
is(2
002),
11=
Loop
er
et
al.
(2007)
12=
Reid
et
al.
(2002),
13=
Fahert
yet
al.
(2009),
14=
Kir
kpatr
ick
et
al.
(2008),
15=
Kir
kpatr
ick
et
al.
(2010),
16=
Burg
ass
er
et
al.
(2010a),
17=
Reid
et
al.
(2007),
18=
Kir
kpatr
ick
et
al.
(2000),
19=
Gagne
et
al.
(2014a),
20=
Teegard
en
et
al.
(2003),
21=
Fahert
yet
al.
(2013),
22=
Gagne
et
al.
(2014b),
23=
Sch
olz
et
al.
(2005)
24=
Salim
&G
ould
(2003),
25=
Burg
ass
er
et
al.
(2008),
26=
Cri
foet
al.
(2005),
27=
This
pap
er,
28=
Kir
kpatr
ick
et
al.
(2006),
29=
Loop
er
et
al.
(2008),
30=
Sahlm
ann
et
al.
(2016),
31=
Sch
neid
er
et
al.
(2016),
32=
Kellogg
et
al.
(2016),
33=
Kellogg
et
al.
(2015),
34=
Giz
iset
al.
(2012),
35=
Giz
iset
al.
(2015),
36=
Cru
zet
al.
inpre
pa
These
sourc
es
have
new
infr
are
dsp
ectr
apre
sente
din
this
pap
er.
Inth
em
ajo
rity
of
case
sw
euse
the
infr
are
dsp
ectr
al
typ
eand
gra
vit
ycla
ssifi
cati
on
dia
gnose
din
this
work
.If
an
ob
ject
had
Sp
eX
data
we
defa
ult
toth
ere
sult
ant
typ
eand
cla
ssifi
cati
on
wit
hth
at
data
.b
This
sourc
eis
refe
rred
toas
PSO
318
for
the
rem
ain
der
of
the
text
cT
he
sourc
es
PSO
318,
2M
1119,
and
2M
1147
have
photo
metr
yre
port
ed
on
the
MK
Osy
stem
that
we
have
convert
ed
to2M
ASS
usi
ng
the
rela
tions
inSte
phens
et
al.
(2009).
Inth
ecase
of
PSO
318,
JH
Kw
as
convert
ed
toM
KO
where
as
for
2M
119,
Jand
Hw
ere
convert
ed
and
for
2M
1147
only
Jw
as
convert
ed.
dT
eegard
ens
Sta
r.e
Refe
rences
are
for
the
spectr
al
data
and
gra
vit
yanaly
sis
(if
diff
ere
nt
then
the
ori
gin
al
spectr
al
data
refe
rence).
fR
efe
rred
toas
TV
LM
831-1
54910
inT
inney
et
al.
(1995).
Brown Dwarf Analogs to Exoplanets 55
Table 2Details on Parallax Targets and Observations
2MASS Designation SpT SpT Nights Framesa Ref Starsa ∆t Telescope Noteb RefOpT IR (yr)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
00452143+1634446 L2β L2γ 4 26 24 3.0 MDM LG 1,201410321+1804502 L1 L4.5 4 23 26 3.3 MDM N 3,4,02132880+4444453 L1.5 — 5 34 81 3.0 MDM N 502235464-5815067 L0γ — 5 48 26 4.9 DuPont LG 102411151-0326587 L0γ L1γ 6 55 20 4.9 DuPont LG 2,1302535980+3206373 M7β M6 5 28 53 3.9 MDM LG 1403140344+1603056 L0 — 5 31 37 3.0 MDM N 605002100+0330501 L4 — 5 30 61 2.8 MDM N 606023045+3910592 L1 L1β 7 77 71 9.9 MDM LG 2,1506154934-0100415 L2 — 5 34 62 2.2 MDM N 706523073+4710348 L4.5 — 5 27 49 3.0 MDM N 509111297+7401081 L0 — 4 24 35 2.9 MDM N 610224821+5825453 L1β L1β 6 30 15 4.9 MDM LG 2,1310484281+0111580 L1 L4 3 17 14 3.0 MDM N 8,913004255+1912354 L1 L3 5 47 10 2.4 MDM N 10,1114162408+1348263 L6 L6 5 29 11 3.3 MDM N 1215525906+2948485 L0β L0β 6 27 33 5.3 MDM LG 1,221265040-8140293 L3γ L3γ 6 90 38 5.4 DuPont LG 1
Note. — References: 1=Cruz et al. (2009), 2=Allers & Liu (2013), 3=Wilson et al. (2003), 4=Cruz et al. (2007), 5=Cruz et al. (2003), 6=Reidet al. (2008), 7=Phan-Bao et al. (2008), 8=Hawley et al. (2002), 9=Kendall et al. (2004), 10=Gizis et al. (2000), 11=Burgasser et al. (2008),12=Bowler et al. (2010a), 13=Kirkpatrick et al. (2008), 14=This paper, 15=Salim & Gould (2003)a
The number of reference stars and individual image frames used in the parallax solutionb
LG is a low surface gravity object and N is a field object
Table 3Results of Parallax Program
Name SpT SpT µαa µδ
a πabsOpT IR ′′yr−1 ′′yr−1 mas
(1) (2) (3) (4) (5) (6)
00452143+1634446 L2β L2γ 0.355 ± 0.01 -0.04 ± 0.01 62.5 ± 3.701410321+1804502 L1 L4.5 0.41 ± 0.01 -0.047 ± 0.01 41.0 ± 2.802132880+4444453 L1.5 — -0.054 ± 0.01 -0.147 ± 0.01 50.0 ± 2.102235464-5815067 L0γ — 0.0986 ± 0.0008 -0.0182 ± 0.0009 27.4 ± 2.602411151-0326587 L0γ L1γ 0.0737 ± 0.001 -0.0242 ± 0.0019 26.7 ± 3.302535980+3206373 M7β M6 0.087 ± 0.01 -0.096 ± 0.01 17.7 ± 2.503140344+1603056 L0 — -0.247 ± 0.01 -0.05 ± 0.01 69.0 ± 2.405002100+0330501 L4 — 0.008 ± 0.01 -0.353 ± 0.01 75.2 ± 3.706023045+3910592 L1 L2β 0.157 ± 0.01 -0.504 ± 0.01 88.5 ± 1.606154934-0100415 L2 — 0.197 ± 0.01 -0.055 ± 0.01 49.8 ± 2.806523073+4710348 L4.5 — -0.118 ± 0.01 0.136 ± 0.01 114.9 ± 4.009111297+7401081 L0 — -0.2 ± 0.01 -0.145 ± 0.01 45.2 ± 3.110224821+5825453 L1β L1β -0.807 ± 0.01 -0.73 ± 0.01 54.3 ± 2.510484281+0111580 L1 L4 -0.436 ± 0.01 -0.218 ± 0.01 71.9 ± 7.413004255+1912354 L1 L3 -0.793 ± 0.01 -1.231 ± 0.01 70.4 ± 2.514162408+1348263 L6 L6 0.088 ± 0.01 0.136 ± 0.01 107.5 ± 3.515525906+2948485 L0β L0β -0.162 ± 0.01 -0.06 ± 0.01 48.8 ± 2.721265040-8140293 L3γ L3γ 0.0556 ± 0.0014 -0.1018 ± 0.003 31.3 ± 2.6
aThe proper motions from MDM are not corrected to absolute and have zero-point uncertainties of ∼ 10 mas yr−1; see Weinberger et al. (2013)
for a discussion of the du Pont proper motions.
56 Faherty et al.
Table 4Literature Parallax Comparisons
2MASS Designation SpT SpT µα µδ π Ref′′yr−1 ′′yr−1 mas
(1) (2) (3) (4) (5) (6) (7)
00452143+1634446 L2β L2γ 0.355 ± 0.01 -0.04 ± 0.01 62.5 ± 3.7 10.3562 ± 0.00137 -0.035 ± 0.0109 57.3 ± 2.0 2
02411151-0326587 L0γ L1γ 0.0737 ± 0.001 -0.0242 ± 0.0019 26.7 ± 3.3 10.084 ± 0.0117 -0.0224 ± 0.0086 21.4 ± 2.6 2
10224821+5825453 L1β L1β -0.807 ± 0.01 -0.73 ± 0.01 54.3 ± 2.5 1-0.799 ± 0.0064 -0.7438 ± 0.0132 46.3 ± 1.3 2
14162408+1348263 L6 L6 0.088 ± 0.01 0.136 ± 0.01 107.5 ± 3.5 10.0951 ± 0.003 0.1303 ± 0.003 109.9 ± 1.8 2
15525906+2948485 L0β L0β -0.162 ± 0.01 -0.06 ± 0.01 48.8 ± 2.7 1-0.1541 ± 0.0053 -0.0622 ± 0.0106 47.7 ± 0.9 3
Note. — References: (1) This work (2) Osorio et al. 2014 (3) Dupuy & Liu 2012
Brown Dwarf Analogs to Exoplanets 57
Table 5New Proper Motion Measurements
2MASS SpT SpT µRA µDEC Ref ∆t
OpT NIR ′′ yr−1 ′′ yr−1 yr(1) (2) (3) (4) (5) (6) (7)
00040288-6410358 L1γ L1γ 0.064 ± 0.012 -0.047 ± 0.012 WISE-2MASS 10.0200374306-5846229 L0γ — 0.057 ± 0.01 0.017 ± 0.005 FourStar 14.1501174748-3403258 L1β L1β 0.084 ± 0.015 -0.045 ± 0.008 FourStar 15.0801262109+1428057 L4γ L2γ 0.07 ± 0.012 -0.008 ± 0.012 WISE-2MASS 9.6801415823-4633574 L0γ L0γ 0.105 ± 0.01 -0.049 ± 0.01 FourStar 14.2902103857-3015313 L0γ L0γ 0.145 ± 0.036 -0.04 ± 0.007 FourStar 14.3902340093-6442068 L0γ L0βγ 0.088 ± 0.012 -0.015 ± 0.012 WISE-2MASS 10.5303032042-7312300 L2γ — 0.043 ± 0.012 0.003 ± 0.012 WISE-2MASS 10.4803231002-4631237 L0γ L0γ 0.066 ± 0.008 0.001 ± 0.016 FourStar 14.3004062677-3812102 L0γ L1γ 0.009 ± 0.012 0.029 ± 0.012 WISE-2MASS 9.7905120636-2949540 L5γ L5β -0.01 ± 0.013 0.08 ± 0.015 CAPSCam 15.1405341594-0631397 M8γ M8γ 0.002 ± 0.012 -0.007 ± 0.012 WISE-2MASS 9.5209532126-1014205 M9γ M9β -0.07 ± 0.007 -0.06 ± 0.009 CAPSCam 15.0609593276+4523309 – L3γ -0.087 ± 0.009 -0.126 ± 0.012 WISE-2MASS 11.33TWA 28 M8.5γ M9γ -0.06 ± 0.008 -0.014 ± 0.009 CAPSCam 14.9011544223-3400390 L0β L1β -0.161 ± 0.008 0.012 ± 0.007 CAPSCam 14.8914112131-2119503 M9β M8β -0.078 ± 0.009 -0.073 ± 0.011 CAPSCam 15.7714482563+1031590 L4 L4pec 0.223 ± 0.017 -0.118 ± 0.013 CAPSCam 13.8215382417-1953116 L4γ L4γ 0.026 ± 0.007 -0.045 ± 0.007 CAPSCam 15.6915474719-2423493 M9γ L0β -0.135 ± 0.009 -0.127 ± 0.008 CAPSCam 14.7915575011-2952431 M9δ L1γ -0.01 ± 0.012 -0.028 ± 0.012 WISE-2MASS 11.0416154255+4953211 L4γ L3-L6γ -0.08 ± 0.012 0.018 ± 0.012 WISE-2MASS 12.1117111353+2326333 L0γ L1β -0.063 ± 0.015 -0.035 ± 0.012 CAPSCam 16.8518212815+1414010 L4.5 L4pec 0.226 ± 0.008 -0.24 ± 0.007 CAPSCam 15.0719355595-2846343 M9γ M9γ 0.034 ± 0.012 -0.058 ± 0.012 CAPSCam 14.7919564700-7542270 L0γ L2γ 0.009 ± 0.012 -0.059 ± 0.012 WISE-2MASS 9.7220004841-7523070 M9γ M9γ 0.069 ± 0.012 -0.11 ± 0.004 CAPSCam 13.7920025073-0521524 L5β L5-L7γ -0.098 ± 0.005 -0.11 ± 0.008 CAPSCam 15.5420135152-2806020 M9γ L0γ 0.043 ± 0.012 -0.068 ± 0.012 WISE-2MASS 11.0321543454-1055308 L4β L5γ 0.175 ± 0.012 0.009 ± 0.012 WISE-2MASS 11.7722064498-4217208 L4γ L4γ 0.128 ± 0.013 -0.181 ± 0.008 CAPSCam 15.5223153135+0617146 L0γ L0γ 0.056 ± 0.012 -0.039 ± 0.012 WISE-2MASS 9.9623225299-6151275 L2γ L3γ 0.062 ± 0.01 -0.085 ± 0.009 FourStar 14.07
58 Faherty et al.
Table 6near-infrared Spectral Data
2MASS Date-Observed Instrument Mode Slit Int time Images(1) (2) (3) (4) (5) (6) (7)
00040288-6410358 11-Sept-2014 FIRE Echelle 0.6 900 200274197+0503417 08-Aug-2014 FIRE Echelle 0.6 900 200452143+1634446 08-Aug-2014 FIRE Echelle 0.6 900 200550564+0134365 04-Sept-2003 SpeX Prism 0.8 180 201174748-3403258 12-Sept-2014 FIRE Echelle 0.6 900 201174748-3403258(2) 11-Sept-2014 FIRE Echelle 0.6 600 201244599-5745379 11-Sept-2014 FIRE Echelle 0.6 900 202103857-3015313 11-Sept-2014 FIRE Echelle 0.6 750 202103857-3015313(2) 29-Dec-2009 TripleSpec — 1.1x43” 300 602251947-5837295 28-July-2013 FIRE Echelle 0.6 600 202340093-6442068 28-July-2013 FIRE Echelle 0.6 750 203231002-4631237 13-Nov-2007 SpeX Prism 0.5 180 503264225-2102057 13-Nov-2007 SpeX Prism 0.5 180 604210718-6306022 11-Sept-2014 FIRE Echelle 0.6 900 204351455-1414468 13-Nov-2007 SpeX SXD 0.5 200 405012406-0010452 12-Oct-2007 SpeX Prism 0.5 90 605120636-2949540 15-Nov-2013 FIRE Echelle 0.6 500 205120636-2949540(2) 08-Dec-2011 SpeX Prism 0.5 180 805361998-1920396 13-Dec-2013 FIRE Echelle 0.6 650 207123786-6155528 15-Nov-2013 FIRE Echelle 0.6 650 209532126-1014205 02-March-2009 TripleSpec — 1.1x43” 300 609593276+4523309 30-Dec-2009 SpeX Prism 0.5 180 311020983-3430355 12-May-2014 FIRE Echelle 0.6 600 211544223-3400390 12-May-2014 FIRE Echelle 0.6 750 212563961-2718455 12-May-2014 FIRE Echelle 0.6 900 214112131-2119503 12-May-2014 FIRE Echelle 0.6 500 214482563+1031590 13-May-2014 FIRE Echelle 0.6 900 215382417-1953116 28-July-2013 FIRE Echelle 0.6 900 215382417-1953116(2) 04-Sept-2003 SpeX Prism 0.8 180 615515237+0941148 15-Aug-2013 FIRE Echelle 0.6 900 215575011-2952431 28-July-2013 FIRE Echelle 0.6 900 217111353+2326333 12-May-2014 FIRE Echelle 0.6 800 217260007+1538190 12-May-2014 FIRE Echelle 0.6 800 217410280-4642218 11-Sept-2014 FIRE Echelle 0.6 1500 218212815+1414010 12-May-2014 FIRE Echelle 0.6 650 219355595-2846343 08-Aug-2014 FIRE Echelle 0.6 600 219564700-7542270 28-July-2013 FIRE Echelle 0.6 900 420004841-7523070 28-July-2013 FIRE Echelle 0.6 300 320025073-0521524 28-July-2013 FIRE Echelle 0.6 600 220135152-2806020 12-May-2014 FIRE Echelle 0.6 600 220135152-2806020(2) 08-Aug-2014 FIRE Echelle 0.6 600 2PSO318 13-Dec-2013 FIRE Echelle 0.6 900 421265040-8140293 15-Aug-2013 FIRE Echelle 0.6 900 221265040-8140293(2) 12-May-2014 FIRE Echelle 0.6 800 221543454-1055308 08-Aug-2014 FIRE Echelle 0.6 1200 222064498-4217208 12-May-2014 FIRE Echelle 0.6 700 222064498-4217208(2) 08-Aug-2014 FIRE Echelle 0.6 750 222064498-4217208(3) 21-Aug-2006 SpeX Prism 0.5 180 522443167+2043433 11-Sept-2014 FIRE Echelle 0.6 900 222495345+0044046 08-Aug-2014 FIRE Echelle 0.6 1200 223153135+0617146 08-Aug-2014 FIRE Echelle 0.6 750 223153135+0617146(2) 14-Nov-2007 SpeX Prism 0.5 180 6
Note. —
Brown Dwarf Analogs to Exoplanets 59Table
7R
adia
lV
elo
cit
ies
Nam
eT
ele
scop
eR
eso
lvin
gP
ow
er
Date
-obs
Sta
ndard
sU
sed
R.V
.R
.V.
final
(1)
(2)
(3)
(4)
(5)
(6)
(7)
00325584-4
405058
Magellan
Cla
yM
IKE
25000
01-N
ov-2
006
4,5
12.9
5±
1.9
212.9
5±
1.9
200332386-1
521309
Gem
ini
South
Phoenix
50000
28-O
ct-
2009
6,7
-6.3
7±
0.4
0-6
.37±
0.4
000374306-5
846229
Gem
ini
South
Phoenix
50000
20-N
ov-2
007
6,7
6.6
3±
0.0
86.6
2±
0.0
700374306-5
846229
Gem
ini
South
Phoenix
50000
23-D
ec-2
007
6,7
6.0
1±
0.7
400452143+
1634446
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
1,3
3.1
6±
0.8
33.1
6±
0.8
300464841+
0715177
Keck
IIN
IRSP
EC
20000
14-S
ep-2
008
1,2
,3-2
.75±
0.2
7-2
.75±
0.2
700550564+
0134365
Keck
IIN
IRSP
EC
20000
14-S
ep-2
008
1,2
,3-1
.21±
0.3
8-1
.21±
0.3
801415823-4
633574
Magellan
Cla
yM
IKE
25000
02-N
ov-2
006
4,5
6.4
1±
1.5
66.4
1±
1.5
602103857-3
015313
Gem
ini
South
Phoenix
50000
22-D
ec-2
007
6,7
7.6
3±
0.3
57.8
2±
0.2
702103857-3
015313
Gem
ini
South
Phoenix
50000
24-D
ec-2
007
6,7
7.0
5±
0.4
502103857-3
015313
Gem
ini
South
Phoenix
50000
26-D
ec-2
007
6,7
7.9
6±
0.1
602215494-5
412054
Gem
ini
South
Phoenix
50000
27-O
ct-
2009
6,7
10.1
8±
0.1
010.1
8±
0.1
002235464-5
815067
Gem
ini
South
Phoenix
50000
05-D
ec-2
007
6,7
9.5
5±
0.6
210.3
6±
0.2
302235464-5
815067
Gem
ini
South
Phoenix
50000
25-D
ec-2
007
6,7
10.4
2±
0.1
802340093-6
442068
Gem
ini
South
Phoenix
50000
27-O
ct-
2009
6,7
12.5
6±
0.1
411.7
6±
0.7
202340093-6
442068
Gem
ini
South
Phoenix
50000
29-O
ct-
2009
6,7
11.1
1±
0.1
302411151-0
326587
aK
eck
IIN
IRSP
EC
20000
13-S
ep-2
008
1,2
,36.3
4±
7.9
86.3
4±
7.9
803231002-4
631237
Gem
ini
South
Phoenix
50000
21-D
ec-2
007
6,7
13.0
2±
0.1
313.0
0±
0.0
503231002-4
631237
Gem
ini
South
Phoenix
50000
23-D
ec-2
007
6,7
12.9
0±
0.2
903393521-3
525440
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
4,5
7.4
3±
0.7
27.4
3±
0.7
203572695-4
417305
Magellan
Cla
yM
IKE
25000
01-N
ov-2
006
4,5
10.7
3±
4.6
010.7
3±
4.6
004210718-6
306022
Gem
ini
South
Phoenix
50000
14-D
ec-2
007
6,7
15.8
1±
0.5
314.7
0±
0.3
304210718-6
306022
Gem
ini
South
Phoenix
50000
15-D
ec-2
007
6,7
14.6
0±
0.1
604351455-1
414468
Magellan
Cla
yM
IKE
25000
01-N
ov-2
006
4,5
16.1
6±
1.7
616.1
6±
1.7
604362788-4
114465
Magellan
Cla
yM
IKE
25000
02-N
ov-2
006
4,5
14.9
7±
1.4
514.9
7±
1.4
504433761+
0002051
Magellan
Cla
yM
IKE
25000
01-N
ov-2
006
4,5
16.9
7±
0.7
616.9
7±
0.7
605012406-0
010452
Magellan
Cla
yM
IKE
25000
02-N
ov-2
006
4,5
21.2
9±
0.8
521.7
7±
0.6
605012406-0
010452
Gem
ini
South
Phoenix
50000
28-O
ct-
2009
6,7
22.6
8±
1.1
605184616-2
756457
Keck
IIN
IRSP
EC
20000
13-S
ep-2
008
1,2
24.5
2±
0.4
124.3
5±
0.1
905184616-2
756457
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
1,2
24.1
5±
0.4
506085283-2
753583
Magellan
Cla
yM
IKE
25000
02-N
ov-2
006
4,5
28.0
8±
1.9
326.3
5±
0.0
706085283-2
753583
Gem
ini
South
Phoenix
50000
28-O
ct-
2009
6,7
26.3
5±
0.0
815474719-2
423493
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
4,5
-6.5
2±
0.3
5-6
.52±
0.3
515525906+
2948485
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
4,5
-19.9
0±
1.3
8-1
9.9
0±
1.3
816154255+
4953211a
Keck
IIN
IRSP
EC
20000
13-S
ep-2
008
1,2
,3-2
5.5
9±
3.1
8-2
5.5
9±
3.1
817111353+
2326333
Keck
IIN
IRSP
EC
20000
14-S
ep-2
008
1,2
,3-2
0.6
9±
0.7
5-2
0.6
9±
0.7
517260007+
1538190
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
1,2
,3-2
0.5
4±
0.8
4-2
0.5
4±
0.8
418212815+
1414010
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
2,3
9.0
8±
0.1
79.0
8±
0.1
7
19350976-6
200473b
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
20004841-7
523070
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
4,5
4.4
0±
2.8
44.4
0±
2.8
420135152-2
806020
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
4,5
-6.5
3±
0.2
4-6
.53±
0.2
421265040-8
140293
Gem
ini
South
Phoenix
50000
29-O
ct-
2009
6,7
10.0
3±
0.4
910.0
3±
0.4
922081363+
2921215
Keck
IIN
IRSP
EC
20000
13-S
ep-2
008
1,2
,3-1
5.5
9±
1.9
3-1
5.5
9±
1.9
322134491-2
136079
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
4,5
-4.9
2±
4.1
8-4
.92±
4.1
822495345+
0044046
Keck
IIN
IRSP
EC
20000
13-S
ep-2
008
1,2
,3-3
.26±
0.9
0-3
.26±
0.9
023153135+
0617146
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
1,2
,3-1
4.6
9±
0.5
2-1
4.6
9±
0.5
223224684-3
133231
Gem
ini
South
Phoenix
50000
27-O
ct-
2009
6,7
33.8
6±
1.1
133.8
6±
1.1
123225299-6
151275
Gem
ini
South
Phoenix
50000
28-O
ct-
2009
6,7
7.2
0±
0.4
66.7
5±
0.7
523225299-6
151275
Gem
ini
South
Phoenix
50000
29-O
ct-
2009
6,7
5.5
2±
0.7
6
00242463-0
158201c
Gem
ini
South
Phoenix
50000
24-D
ec-2
007
6,7
11.6
5±
1.6
011.6
5±
1.6
01224522-1
23835c
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
4-2
.87±
0.5
9-2
.87±
0.5
901062285-5
933185c
Gem
ini
South
Phoenix
50000
27-J
ul-
2007
6,7
1.1
8±
0.4
41.1
8±
0.4
405233822-1
403022c
Gem
ini
South
Phoenix
50000
27-O
ct-
2009
612.4
8±
0.4
112.4
8±
0.4
105361998-1
920396c
Keck
IIN
IRSP
EC
20000
14-S
ep-2
008
1,2
22.0
7±
0.7
022.0
7±
0.7
014284323+
3310391c
Magellan
Cla
yM
IKE
25000
04-J
ul-
2006
5-3
9.1
4±
0.3
8-3
9.1
4±
0.3
818284076+
1229207ac
Keck
IIN
IRSP
EC
20000
14-S
ep-2
008
151.9
5±
15.0
451.9
5±
15.0
4
60 Faherty et al.Table
7—
Continued
Nam
eT
ele
scop
eR
eso
lvin
gP
ow
er
Date
-obs
Sta
ndard
sU
sed
R.V
.R
.V.
final
(1)
(2)
(3)
(4)
(5)
(6)
(7)
21041491-1
037369c
Gem
ini
South
Phoenix
50000
28-O
ct-
2009
6,7
-30.9
0±
1.5
8-3
0.9
0±
1.5
821481633+
4003594c
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
1,2
,3-1
4.5
2±
0.7
1-1
4.5
2±
0.7
122244381-0
158521c
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
1,2
-36.4
8±
0.0
1-3
6.4
8±
0.0
122344161+
4041387c
Keck
IIN
IRSP
EC
20000
15-S
ep-2
008
1,2
,3-1
2.4
9±
0.4
2-1
2.4
9±
0.4
2
23515044-2
537367acd
Gem
ini
South
Phoenix
50000
28-O
ct-
2009
6,7
-5.6
8±
1.8
2-5
.68±
1.8
2
Note.
—D
ata
from
2M
ASS
Cutr
iet
al.
(2003)
and
AL
LW
ISE
Cutr
i&
et
al.
(2013).
Sta
ndard
stars
are
as
follow
s:1.)
2M
ASS
J18212815+
1414010
(+9.7
8B
lake
et
al.
2010),
2.)
2M
ASS
J00452143+
1634446
(+3.2
9B
lake
et
al.
2010),
3.)
2M
ASS
J22244381-0
158521
(-37.5
5B
lake
et
al.
2010),
4.)
LH
S2924
(-37.4
Mohanty
et
al.
2003),
5.)
BR
I1222-1
221
(-4.8
Mohanty
et
al.
2003),
6.)
2M
ASS
J11553952-3
727350
(+45.0
Seif
ahrt
et
al.
2010),
7.)
2M
ASS
J05233822-1
403022
(+11.8
2B
lake
et
al.
2007)
aL
ow
Quality
Sp
ectr
um
bN
oU
seable
Sp
ectr
um
cN
oSp
ectr
osc
opic
Sig
ns
of
Youth
dT
his
ob
ject
islist
ed
inF
ilip
pazzo
et
al.
(2015)
wit
ha
dis
tance
and
refe
rence
toFahert
y+
inpre
p.
The
valu
ein
that
pap
er
was
spectr
ophoto
metr
icand
should
not
be
regard
ed
as
apara
llax.
Brown Dwarf Analogs to Exoplanets 61
Table 8Comparison of new and previously published RVs.
Name Telescope RVours RVothers RV RVothers RV RVothers RV RVothers RV
kms−1 kms−1 ref. kms−1 ref. kms−1 ref. kms−1 ref.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
00242463-0158201 Gemini South Phoenix +11.65±1.60 +10.4±3 3 +16±2 700452143+1634446 Keck II NIRSPEC +3.16±0.83 +3.29±0.43 101415823-4633574 Magellan Clay MIKE +6.41±1.56 +12±15 203393521-3525440 Magellan Clay MIKE +7.43±0.72 +7.6±3 3 +6±2 8 +5.8±2.4 5 +10±2 9
04433761+0002051 Magellan Clay MIKE +16.97±0.76 +17.1±3 305233822-1403022 Gemini South Phoenix +12.48±0.41 +12.21±0.21 106085283-2753583 Magellan Clay MIKE +26.35±0.07 +24±1 4
1224522-123835 Magellan Clay MIKE −2.87±0.59 −5.8±3 3 −4.8±2 714284323+3310391 Magellan Clay MIKE −39.14±0.38 −37.4±2 715525906+2948485 Magellan Clay MIKE −19.90±1.38 −18.43±0.11 118212815+1414010 Keck II NIRSPEC +9.08±0.17 +9.78±0.21 120004841-7523070 Magellan Clay MIKE +4.40±2.84 +8±2.4 5 +11.77±0.97 621041491-1037369 Gemini South Phoenix −30.90±1.58 −21.09±0.41 1 −21.2±2.2 522244381-0158521 Keck II NIRSPEC −36.48±0.01 −37.55±0.21 123515044-2537367 Gemini South Phoenix −5.68±1.82 −10±3 3 −12.3±2.6 5
Note. — References: 1. Blake et al. (2010), 2. Kirkpatrick et al. (2006), 3. Reiners (2009), 4. Rice et al. (2010), 5. Burgasser et al. (2015), 6.Galvez-Ortiz et al. (2010), 7. Mohanty et al. (2003), 8. Basri (2000), 9. Reid et al. (2002)
Table 9Adopted near-infrared Spectral Types
Name SpT SpT Gravity Score Gravity Type Gravity Score Gravity TypeAdopted Allers13 MedRes MedRes LowRes LowRes
(1) (2) (3) (4) (5) (6) (7)
00040288-6410358 L1 γ L2.3 ± 0.3 2221 VL-G 2211 VL-G00274197+0503417 M8 β M9.0 ± 0.8 2n11 INT-G 2n01 INT-G00452143+1634446 L0 β L1.5 ± 0.4 1211 INT-G 1211 INT-G00550564+0134365 L2γ L1.0 ± 0.9 — — 2122 VL-G01174748-3403258 L1 γ L2.2 ± 0.5 1211 INT-G 1211 INT-G
01174748-3403258(2) L1 γ L1.9 ± 0.5 2212 VL-G 2222 VL-G01244599-5745379 L0 γ L0.7 ± 0.5 2222 VL-G 2222 VL-G02103857-3015313 L0 γ L1.0 ± 0.3 2211 VL-G 2211 VL-G
02103857-3015313(2) L0 γ L2.2 ± 0.1 2112 VL-G 1122 VL-G02251947-5837295 M9 γ M9.4 ± 0.1 1n11 INT-G 1n11 INT-G02340093-6442068 L0 β/γ L0.8 ± 0.3 2211 VL-G 2211 VL-G03231002-4631237 L0γ M9.0±0.4 — — 2222 VL-G03264225-2102057 L5β γ L4.1±0.1 — — 0n01 FLD-G04210718-6306022 L5 γ L4.2 ± 0.1 0n11 INT-G 0n01 FLD-G04351455-1414468 M7γa M6.8±0.4 2n22 VL-G 2n22 VL-G05012406-0010452 L4γ L2.4±0.1 — — 2212 VL-G05120636-2949540 L4 pec L4.1 ± 0.8 2010 FLD-G 2010 FLD-G
05120636-2949540(2) L5βγ L4.3 ± 0.4 — — 0n01 FLD-G05361998-1920396 L1 γ L2.1 ± 0.3 1222 VL-G 1212 VL-G07123786-6155528 L1 γ L1.5 ± 0.5 2211 VL-G 2221 VL-G09532126-1014205 M9β M9.7±0.3 2n12 VL-G 2n02 VL-G09593276+452330911020983-3430355 M9 γ M8.3 ± 1.0 2n22 VL-G 2n22 VL-G11544223-3400390 L1 β L0.8 ± 0.5 1111 INT-G 1101 INT-G12563961-2718455 L4 β L3.4 ± 0.4 1211 INT-G 1201 INT-G14112131-2119503 M8 β M8.3 ± 0.1 1n11 INT-G 1n01 INT-G14482563+1031590 L4 pec L4.7 ± 0.8 2010 FLD-G 1010 FLD-G15382417-1953116 L4 γ L3.5 ± 0.9 2211 VL-G 2211 VL-G
15382417-1953116(2) L4γ L2.1±0.6 — — 1021 INT-G15515237+0941148 > L5 γ L3.3 ± 0.2 — — — —15575011-2952431 L1 γ L2.3 ± 0.6 2222 VL-G 2212 VL-G17111353+2326333 L0 pec L0.4 ± 0.6 2211 VL-G 2211 VL-G17260007+1538190 L3 β/γ L2.6 ± 0.3 1121 INT-G 1121 INT-G17410280-4642218 > L5 γ L5.3 ± 0.8 — — — —18212815+1414010 L4 pec L3.5 ± 1.3 1111 INT-G 0101 FLD-G19355595-2846343 M9 γ M9.3 ± 0.4 2n21 VL-G 2n11 INT-G19564700-7542270 L2 γ L0.9 ± 0.2 2222 VL-G 2222 VL-G20004841-7523070 M9 γ L0.2 ± 1.1 2n21 VL-G 2n21 VL-G20025073-0521524 > L5 β/γ L5.5 ± 0.2 — — — —20135152-2806020 L0 γ L0.0 ± 0.4 2122 VL-G 2122 VL-G
20135152-2806020(2) L0 γ L0.0 ± 0.3 2122 VL-G 2122 VL-GPSO318 L6-L8 γ L6.8 ± 0.8 — — — —
21265040-8140293 L3 γ L2.4 ± 0.1 1221 VL-G 1221 VL-G21265040-8140293(2) L3 γ L2.4 ± 0.2 1221 VL-G 1221 VL-G
21543454-1055308 L5 γ L5.5 ± 0.8 2n11 INT-G 2n01 INT-G22064498-4217208 L4 β/γ L3.3 ± 0.2 1111 INT-G 1111 INT-G
22064498-4217208(2) L3-4 β/γ L2.7 ± 0.2 — — — —
62 Faherty et al.
Table 9 — Continued
Name SpT SpT Gravity Score Gravity Type Gravity Score Gravity TypeAdopted Allers13 MedRes MedRes LowRes LowRes
(1) (2) (3) (4) (5) (6) (7)
22064498-4217208(3) L3γ L1.7 ± 0.8 — — 1?12 INT-G22443167+2043433 L6-L8 γ L6.7 ± 0.8 — — — —22495345+0044046 L1 γ L3.1 ± 0.3 2011 INT-G 2011 INT-G23153135+0617146 L0 γ L1.0 ± 0.5 2222 VL-G 2212 VL-G
23153135+0617146(2) L0γ M9.9±0.5 — — 2222 VL-G
aReddening E(B-V)=1.8 and SPT = M7 are a good solution, but spt/reddening is almost degenerate.
Brown Dwarf Analogs to Exoplanets 63Table
10
Kin
em
ati
cdata
on
Low
Surf
ace
Gra
vit
yD
warf
s
2M
ASS
Desi
gnati
on
SpT
SpT
µRA
cosDEC
µDEC
πR
V(R
ef)
(OpT
)(I
R)
(′′
yr−
1)
(′′
yr−
1)
(mas)
(km
s−1)
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
00011217+
1535355
—-
L4β
0.1
352±
0.0
107
-0.1
696±
0.0
137
––
10
00040288-6
410358
L1γ
L1γa
0.0
64±
0.0
12
-0.0
47±
0.0
12
(17±
1)
(6.0
7±
2.8
9)
100182834-6
703130
—-
L0γ
0.0
66±
0.0
04
-0.0
523±
0.0
126
––
1,1
000191296-6
226005
—-
L1γ
0.0
541±
0.0
047
-0.0
345±
0.0
121
(21±
6)
(6.7±
2.5
)1,1
000192626+
4614078
M8–
M8β
0.1
4000±
0.0
6-0
.1±
0.0
5(3
1±
3)
-19.5±
22,4
00274197+
0503417
M9.5β
L0β
0.0
105±
0.0
004
-0.0
008±
0.0
003
13.8±
1.6
–3
00303013-1
450333
L7–
L4-L
6β
0.2
497±
0.0
141
-0.0
053±
0.0
15
37.4
2±
4.5
0–
10,1
100325584-4
405058
L0γ
L0β
0.1
2830±
0.0
034
-0.0
934±
0.0
03
21.6±
7.2
12.9
5±
1.9
21,5
003323.8
6-1
521309
L4β
L1
0.3
0950±
0.0
104
0.0
289±
0.0
183
24.8±
2.5
-6.3
7±
0.4
01,6
00344300-4
102266
—-
L1β
0.0
939±
0.0
079
-0.0
412±
0.0
108
––
10
00374306-5
846229
L0γ
—-
0.0
5700±
0.0
10.0
17±
0.0
05
–6.6
2±
0.0
71
00381489-6
403529
—-
M9.5β
0.0
871±
0.0
038
-0.0
353±
0.0
105
(23±
5)
(7.2
7±
2.8
1)
1,1
000425923+
1142104
—-
M9β
0.0
929±
0.0
17
-0.0
758±
0.0
152
––
10
00452143+
1634446
L2β
L2γ
0.3
5500±
0.0
1-0
.04±
0.0
162.5±
3.7
3.1
6±
0.8
31
00464841+
0715177
M9β
L0δ
0.0
9800±
0.0
22
-0.0
51±
0.0
1–
-2.7
5±
0.2
71,2
00470038+
6803543
L7(γ
?)
L6-L
8γ
0.3
8700±
0.0
04
-0.1
97±
0.0
04
82±
3-2
0±
1.4
700550564+
0134365
L2γ
L2γ
0.0
4400±
0.0
24
-0.0
82±
0.0
24
–-1
.21±
0.3
81,2
00584253-0
651239
L0–
L1β
0.1
367±
0.0
02
-0.1
226±
0.0
018
33.8±
4.0
–5
01033203+
1935361
L6β
L6β
0.2
9300±
0.0
046
0.0
277±
0.0
047
46.9±
7.6
–8
01174748-3
403258
L1β
L1βa
0.0
84±
0.0
15
-0.0
45±
0.0
08
(20±
3)
(3.9
6±
2.0
9)
101205114-5
200349
—-
L1γ
0.0
921±
0.0
058
-0.0
404±
0.0
102
(24±
4)
(7.2
2±
2.5
)1,1
001231125-6
921379
M7.5γ
—-
0.0
8278±
0.0
0174
-0.0
2646±
0.0
0139
21.6±
3.3
10.9±
34,9
01244599-5
745379
L0γ
L0γ
-0.0
0300±
0.0
10.0
18±
0.0
19
––
201262109+
1428057
L4γ
L2γ
0.0
7000±
0.0
12
-0.0
08±
0.0
12
––
101294256-0
823580
M5–
M7β
0.1
007±
0.0
084
-0.0
564±
0.0
09
––
10
01415823-4
633574
L0γ
L0γ
0.1
05±
0.0
1-0
.049±
0.0
1(2
5±
3)
6.4
09±
1.5
61
01531463-6
744181
L2–
L3β
0.0
71±
0.0
037
-0.0
166±
0.0
127
(21±
7)
(10.4
1±
2.7
1)
1,1
002103857-3
015313
L0γ
L0γa
0.1
45±
0.0
36
-0.0
4±
0.0
07
(32±
8)
7.8
2±
0.2
74
102212859-6
831400
M8β
—-
0.0
5390±
0.0
044
0.0
137±
0.0
045
25.4±
3.6
–8
02215494-5
412054
M9β
—-
0.1
36±
0.0
1-0
.01±
0.0
17
(31±
5)
10.1
8±
0.0
97
1,2
02235464-5
815067
L0γ
—-
0.0
9860±
0.0
008
-0.0
182±
0.0
009
27.4±
2.6
10.3
6±
0.2
31
02251947-5
837295
M9β
M9γ
0.0
8500±
0.0
1-0
.03±
0.0
18
––
202265658-5
327032
—-
L0δ
0.0
936±
0.0
053
-0.0
028±
0.0
107
––
1,1
002292794-0
053282
—-
L0γ
-0.0
0900±
0.0
98
-0.0
54±
0.2
02
––
102340093-6
442068
L0γ
L0βγ
0.0
88±
0.0
12
-0.0
15±
0.0
12
(21±
5)
11.7
62±
0.7
21
102410564-5
511466
—-
L1γ
0.0
965±
0.0
052
-0.0
123±
0.0
106
(24±
4)
(11.7
3±
2.4
4)
1,1
002411151-0
326587
L0γ
L1γ
0.0
7370±
0.0
01
-0.0
242±
0.0
019
21.4±
2.6
6.3
4±
7.9
81
02501167-0
151295
—-
M7β
0.0
627±
0.0
087
-0.0
306±
0.0
09
30.2±
4.5
–25,
10
02530084+
1652532
—-
M7β
1.5
124±
0.0
406
0.4
305±
0.0
447
260.6
3±
2.6
9–
24
02535980+
3206373
M7β
M6β
0.0
8700±
0.0
1-0
.096±
0.0
117.7±
2.5
–1
02583123-1
520536
—-
L3β
0.0
625±
0.0
098
-0.0
581±
0.0
097
––
1,1
003032042-7
312300
L2γ
—-
0.0
4300±
0.0
12
0.0
03±
0.0
12
––
103164512-2
848521
L0–
L1β
0.0
952±
0.0
082
-0.0
81±
0.0
094
––
10
03231002-4
631237
L0γ
L0γa
0.0
66±
0.0
08
0.0
01±
0.0
16
(17±
3)
13.0
01±
0.0
45
103264225-2
102057
L5β
L5βγa
0.1
08±
0.0
14
-0.1
46±
0.0
15
(41±
1)
(22.9
1±
2.0
7)
1,2
03350208+
2342356
M8.5
–M
7.5β
0.0
5400±
0.0
1-0
.056±
0.0
123.6±
1.3
15.5±
1.7
12
03393521-3
525440
M9β
L0β
0.3
0580±
0.0
004
0.2
70548±
0.0
004
155.8
9±
1.0
36.9
2±
1.0
51,1
303420931-2
904317
—-
L0β
0.0
671±
0.0
1-0
.0207±
0.0
122
––
1,1
003421621-6
817321
L4γ
—-
0.0
653±
0.0
028
0.0
185±
0.0
091
(21±
9)
(13.8
7±
2.6
2)
103550477-1
032415
M8.5
–M
8.5β
0.0
464±
0.0
072
-0.0
265±
0.0
065
––
10
03552337+
1133437
L5γ
L3-L
6γ
0.2
2500±
0.0
132
-0.6
3±
0.0
15
110.8±
4.3
11.9
2±
0.2
26,1
4
03572695-4
417305b
L0β
L0β
0.0
6400±
0.0
13
-0.0
2±
0.0
19
–10.7
3±
4.6
01,2
04062677-3
812102
L0γ
L1γ
0.0
0900±
0.0
12
0.0
29±
0.0
12
––
104185879-4
507413
—-
L3γ
0.0
533±
0.0
084
-0.0
082±
0.0
126
––
10
04210718-6
306022
L5β
L5γ
0.1
4600±
0.0
08
0.1
91±
0.0
18
–14.7
0±
0.3
31,2
04351455-1
414468
M8γ
M7γ
0.0
0900±
0.0
14
0.0
16±
0.0
14
–16.1
6±
1.7
61,2
64 Faherty et al.Table
10
—Continued
2M
ASS
Desi
gnati
on
SpT
SpT
µRA
cosDEC
µDEC
πR
V(R
ef)
(OpT
)(I
R)
(′′
yr−
1)
(′′
yr−
1)
(mas)
(km
s−1)
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
04362788-4
114465
M8β
M9γ
0.0
73±
0.0
12
0.0
13±
0.0
16
(23±
6)
14.9
72±
1.4
46
1,2
04400972-5
126544
—-
L0γ
0.0
458±
0.0
062
0.0
078±
0.0
105
––
10
04433761+
0002051b
M9γ
M9γ
0.0
2800±
0.0
14
-0.0
99±
0.0
14
–16.9
7±
0.7
61,2
04493288+
1607226
—-
M9γ
0.0
196±
0.0
094
-0.0
38±
0.0
092
––
10
05012406-0
010452
L4γ
L3γ
0.1
9030±
0.0
095
-0.1
428±
0.0
125
51±
3.7
21.7
7±
0.6
61,6
05104958-1
843548
—-
L2β
0.0
882±
0.0
095
-0.0
399±
0.0
106
––
10
05120636-2
949540
L5γ
L5β
-0.0
1000±
0.0
13
0.0
8±
0.0
15
––
105181131-3
101529
M6.5
–M
7β
0.0
416±
0.0
068
0.0
008±
0.0
081
––
10
05184616-2
756457
L1γ
L1γ
0.0
2860±
0.0
042
-0.0
16±
0.0
04
21.4±
6.9
24.3
5±
0.1
91,8
05264316-1
824315
—-
M7β
0.0
247±
0.0
093
-0.0
227±
0.0
095
––
10
05341594-0
631397
M8γ
M8γ
0.0
0200±
0.0
12
-0.0
07±
0.0
12
––
105361998-1
920396
L2γ
L2γ
0.0
2460±
0.0
053
-0.0
306±
0.0
05
25.6±
9.4
22.0
65±
0.6
95
1,8
05402325-0
906326
—-
M9β
0.0
376±
0.0
098
-0.0
292±
0.0
097
––
10
05575096-1
359503
M7–
M7γ
0.0
0000±
0.0
05
0±
0.0
05
1.9±
130.3±
2.8
12
06023045+
3910592
L1–
L1β
0.1
5700±
0.0
1-0
.504±
0.0
188.5±
1.6
–1
06085283-2
753583
M8.5γ
L0γ
0.0
0890±
0.0
035
0.0
107±
0.0
035
32±
3.6
26.3
5±
0.0
71,8
06272161-5
308428
—-
L0βγ
0.0
104±
0.0
066
0.0
651±
0.0
123
––
10
06322402-5
010349
L3β
L4γ
-0.1
0020±
0.0
052
-0.0
046±
0.0
088–
––
1,1
006524851-5
741376
M8β
—-
0.0
0100±
0.0
034
0.0
292±
0.0
033
31.3±
3.2
–8
07123786-6
155528
L1β
L1γ
-0.0
3570±
0.0
049
0.0
791±
0.0
048
22.9±
9.1
–8
07140394+
3702459
M8–
M7.5β
-0.0
984±
0.0
069
-0.1
71±
0.0
089
80.1
0±
4.8
–26
08095903+
4434216
—-
L6p
-0.1
833±
0.0
081
-0.2
019±
0.0
13
––
10
08561384-1
342242
—-
M8γ
-0.0
576±
0.0
078
-0.0
194±
0.0
081
––
10
08575849+
5708514
L8–
L8—
-0.4
181±
0.0
044
-0.3
706±
0.0
113
––
10
09451445-7
753150
—-
M9β
-0.0
345±
0.0
016
0.0
436±
0.0
119
––
10
09532126-1
014205
M9γ
M9β
-0.0
7000±
0.0
07
-0.0
6±
0.0
09
––
109593276+
4523309
—-
L3γ
-0.0
8700±
0.0
09
-0.1
26±
0.0
12
–2.7±
0.7
1G
196-3
BL
3β
L3γ
-0.1
3230±
0.0
107
-0.2
021±
0.0
137
41±
4.1
–6
10212570-2
830427
—-
L4βγ
-0.0
526±
0.0
131
-0.0
375±
0.0
163
––
10
10220489+
0200477
M9β
M9β
-0.1
5620±
0.0
066
-0.4
29±
0.0
068
26.4±
11.5
-7.9±
4.8
810224821+
5825453
L1β
L1β
-0.8
0700±
0.0
1-0
.73±
0.0
154.3±
2.5
19.2
9±
0.1
11
TW
A28
M8.5γ
M9γ
-0.0
6720±
0.0
006
-0.0
14±
0.0
006
18.1±
0.5
(13.3±
1.8
)18
11064461-3
715115
—-
M9γ
-0.0
408±
0.0
076
-0.0
066±
0.0
102
––
10
11083081+
6830169
L1γ
L1γ
-0.2
389±
0.0
026
-0.1
922±
0.0
092
––
10
11193254-1
137466
—-
L7γ
-.1451±
0.0
149
-0.0
724±
0.0
16
(35±
5)
8.5±
3.3
27
11271382-3
735076
—-
L0δ
-0.0
613±
0.0
138
0.0
132±
0.0
208
––
10
TW
A26
M9γ
M9γ
-0.0
8120±
0.0
039
-0.0
277±
0.0
021
23.8
2±
2.5
811.6±
215,1
6114724.1
0-2
04021.3
—-
L7γ
-0.1
221±
0.0
12
-0.0
745±
0.0
113
(32±
4)
(9.6
1±
)28
11480096-2
836488
—-
L1β
-0.0
743±
0.0
135
-0.0
194±
0.0
161
––
10
11544223-3
400390
L0β
L1β
-0.1
6100±
0.0
08
0.0
12±
0.0
07
––
1T
WA
27A
M8γ
M8γ
-0.0
6300±
0.0
02
-0.0
23±
0.0
03
19.1±
0.4
11.2±
216,1
912074836-3
900043
L0γ
L1γ
-0.0
572±
0.0
079
-0.0
248±
0.0
105
(15±
3)
(9.4
8±
1.9
1)
17
12271545-0
636458
M9–
M8.5β
-0.1
141±
0.0
111
-0.0
646±
0.0
109
––
10
TW
A29
M9.5γ
L0γ
-0.0
4030±
0.0
117
-0.0
203±
0.0
17
12.6
6±
2.0
7(7
.74±
2.0
4)
15
12474428-3
816464
—-
M9γ
-0.0
3320±
0.0
071
-0.0
166±
0.0
095
––
17
12535039-4
211215
—-
M9.5γ
-0.0
388±
0.0
09
-0.0
121±
0.0
132
––
10
12563961-2
718455
—-
L4β
-0.0
674±
0.0
102
-0.0
565±
0.0
127
––
10
14112131-2
119503
M9β
M8β
-0.0
7800±
0.0
09
-0.0
73±
0.0
11
–-0
.9±
2.5
114252798-3
650229
L3–
L4γ
-0.2
8489±
0.0
014
-0.4
6308±
0.0
01
86.4
5±
0.8
35.3
7±
0.2
513,1
415104786-2
818174
M9–
M9β
-0.1
092±
0.0
081
-0.0
399±
0.0
098
––
10
15291017+
6312539
—-
M8β
-0.1
132±
0.0
033
0.0
447±
0.0
091
––
10
15382417-1
953116
L4γ
L4γ
0.0
2600±
0.0
07
-0.0
45±
0.0
07
––
115470557-1
626303A
—-
M9β
-0.0
539±
0.0
087
-0.1
253±
0.0
09
––
10
15474719-2
423493
M9γ
L0β
-0.1
3500±
0.0
09
-0.1
27±
0.0
08
–-6
.52±
0.3
51
15515237+
0941148
L4γ
>L
5γ
-0.0
7000±
0.0
22
-0.0
5±
0.0
22
––
215525906+
2948485
L0β
L0β
-0.1
6200±
0.0
1-0
.06±
0.0
148.8±
2.7
-18.4
3±
0.1
11,1
415575011-2
952431
M9δ
L1γ
-0.0
1000±
0.0
12
-0.0
28±
0.0
12
––
116154255+
4953211
L4γ
L3-L
6γ
-0.0
8000±
0.0
12
0.0
18±
0.0
12
–-2
5.5
9±
3.1
81
Brown Dwarf Analogs to Exoplanets 65Table
10
—Continued
2M
ASS
Desi
gnati
on
SpT
SpT
µRA
cosDEC
µDEC
πR
V(R
ef)
(OpT
)(I
R)
(′′
yr−
1)
(′′
yr−
1)
(mas)
(km
s−1)
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
17111353+
2326333
L0γ
L1β
-0.0
6300±
0.0
15
-0.0
35±
0.0
12
–-2
0.6
9±
0.7
51
17260007+
1538190
L3.5γ
L3γ
-0.0
4310±
0.0
071
-0.0
557±
0.0
052
28.6±
2.9
-20.5
4±
0.8
41,6
17410280-4
642218
—-
L6-L
8γ
-0.0
2040±
0.0
092
-0.3
43±
0.0
137
–-5
.7±
5.1
20
18212815+
1414010
L4.5
—L
4p
ec
0.2
3027±
0.0
0016
-0.2
4149±
0.0
0012
106.6
5±
0.2
39.0
8±
0.1
71,2
219350976-6
200473
—-
L1γ
-0.0
043±
0.0
063
-0.0
533±
0.0
162
––
10
19355595-2
846343
M9γ
M9γ
0.0
3400±
0.0
12
-0.0
58±
0.0
12
––
119564700-7
542270
L0γ
L2γ
0.0
0900±
0.0
12
-0.0
59±
0.0
12
––
120004841-7
523070
M9γ
M9γa
0.0
69±
0.0
12
-0.1
1±
0.0
04
(31±
1)
4.3
97±
2.8
42
120025073-0
521524
L5β
L5-L
7γ
-0.0
9800±
0.0
05
-0.1
1±
0.0
08
––
120113196-5
048112
—-
L3γ
0.0
213±
0.0
081
-0.0
713±
0.0
145
––
10
20135152-2
806020
M9γ
L0γ
0.0
4300±
0.0
12
-0.0
68±
0.0
12
–-6
.53±
0.2
41
20282203-5
637024
—-
M8.5γ
0.0
233±
0.0
053
-0.0
604±
0.0
106
––
10
20334473-5
635338
—-
L0γ
0.0
16±
0.0
061
-0.0
731±
0.0
125
––
10
20391314-1
126531
M8–
M7β
0.0
485±
0.0
09
-0.0
898±
0.0
09
––
10
20575409-0
252302
L1.5
–L
2β
0.0
0160±
0.0
038
-0.0
863±
0.0
039
70.1±
3.7
-24.6
8±
0.6
18
PSO
318
—-
L6-L
8γ
0.1
3730±
0.0
013
-0.1
387±
0.0
014
40.7±
2.4
−6.0
+0.8
−1.1
21,2
321265040-8
140293
L3γ
L3γ
0.0
5560±
0.0
014
-0.1
018±
0.0
03
31.3±
2.6
10.0
3±
0.4
91
21324036+
1029494
—-
L4β
0.1
078±
0.0
164
0.0
297±
0.0
181
––
10
21543454-1
055308
L4β
L5γ
0.1
7500±
0.0
12
0.0
09±
0.0
12
––
121544859-7
459134
—-
M9.5β
0.0
407±
0.0
022
-0.0
796±
0.0
122
(21±
7)
(6.2
1±
3.1
)1,1
021572060+
8340575
L0–
M9γ
0.1
248±
0.0
008
0.0
441±
0.0
154
––
10
22025794-5
605087
—-
M9γ
0.0
496±
0.0
052
-0.0
696±
0.0
103
––
10
22064498-4
217208
L4γ
L4γa
0.1
28±
0.0
13
-0.1
81±
0.0
08
(35±
2)
(7.6±
2.0
)1
22081363+
2921215
L3γ
L3γ
0.0
9070±
0.0
03
-0.0
162±
0.0
037
21.2±
0.7
-15.5
9±
1.9
31,6
22134491-2
136079
L0γ
L0γ
0.0
6000±
0.0
11
-0.0
63±
0.0
17
–-4
.92±
4.1
81,2
22351658-3
844154
—-
L1.5γ
0.0
505±
0.0
078
-0.0
757±
0.0
109
(22±
2)
(-4.9±
3.1
)10
22353560-5
906306
—-
M8.5β
0.0
556±
0.0
051
-0.0
81±
0.0
108
(23±
5)
(1.7
1±
3.1
4)
1,1
022443167+
2043433
L6.5
p–
L6-L
8γa
0.2
52±
0.0
14
-0.2
14±
0.0
11
(54±
4)
(-15.5±
1.7
)1,2
22495345+
0044046
L4γ
L3β
0.0
7500±
0.0
18
0.0
26±
0.0
18
–-3
.26±
0.9
01,2
23153135+
0617146
L0γ
L0γ
0.0
5600±
0.0
12
-0.0
39±
0.0
12
–-1
4.6
9±
0.5
21
23224684-3
133231
L0β
L2β
-0.1
9480±
0.0
074
-0.5
273±
0.0
075
58.6±
5.6
33.8
6±
1.1
11,8
23225299-6
151275
L2γ
L3γa
0.0
62±
0.0
1-0
.085±
0.0
09
(22±
1)
6.7
47±
0.7
51
23231347-0
244360
M8.5
–M
8β
0.0
859±
0.0
097
-0.0
435±
0.0
106
––
10
23255604-0
259508
L3–
L1γ
0.0
783±
0.0
127
-0.0
958±
0.0
11
––
10
23360735-3
541489
—-
M9β
0.0
696±
0.0
082
-0.0
807±
0.0
099
––
10
23433470-3
646021
—-
L3-L
6γ
0.0
87±
0.0
083
-0.0
987±
0.0
125
––
10
23453903+
0055137
M9–
M9β
0.0
841±
0.0
134
-0.0
461±
0.0
117
––
10
23520507-1
100435
M7–
M8β
0.0
881±
0.0
09
-0.1
145±
0.0
085
––
10
Note.
—R
efe
rences:
1=
This
Pap
er,
2=
Fahert
yet
al.
(2009),
3=
Dahn
et
al.
(2002),
4=
Rein
ers
&B
asr
i(2
009),
5=
Maro
cco
et
al.
(2013),
6=
Zapate
roO
sori
oet
al.
(2014),
7=
Giz
iset
al.
(2015),
8=
Fahert
yet
al.
(2012),
9=
Rie
del
(2015),
10=
Gagne
et
al.
(2015b),
11=
Vrb
aet
al.
(2004),
12=
Shkoln
iket
al.
(2012),
13=
Die
teri
chet
al.
(2014),
14=
Bla
ke
et
al.
(2010),
15=
Wein
berg
er
et
al.
(2013),
16=
Mohanty
et
al.
(2003),
17=
Gagne
et
al.
(2014a),
18=
Teix
eir
aet
al.
(2008),
19=
Ducoura
nt
et
al.
(2014),
20=
Sch
neid
er
et
al.
(2014),
21=
Liu
et
al.
(2013),
22=
Sahlm
ann
et
al.
(2016),
23=
Allers
et
al.
(2016),
24=
Henry
et
al.
(2006),
25=
Tin
ney
et
al.
(1995),
26=
Dit
tmann
et
al.
(2014),
27=
Kellogg
et
al.
(2016),
28=
Sch
neid
er
et
al.
(2016)
aT
hese
sourc
es
have
new
infr
are
dsp
ectr
apre
sente
din
this
pap
er.
Inth
em
ajo
rity
of
case
sw
euse
the
infr
are
dsp
ectr
al
typ
eand
gra
vit
ycla
ssifi
cati
on
dia
gnose
din
this
work
.If
an
ob
ject
had
Sp
eX
data
we
defa
ult
toth
ere
sult
ant
typ
eand
cla
ssifi
cati
on
wit
hth
at
data
.b
These
sourc
es
were
list
ed
inF
ilip
pazzo
et
al.
(2015)
as
mem
bers
of
ass
ocia
tions
but
as
has
been
note
din
Table
12,
we
have
dow
ngra
ded
them
toam
big
uos
young
ob
jects
66 Faherty et al.
Table 11Kinematics for target dwarfs
Name U V W X Y Z(1) (2) (3) (4) (5) (6) (7)
00325584-4405058 -10.77 ± 3.85 -32.08 ± 8.55 -8.34 ± 2.26 8.96 ± 2.59 -9.24 ± 2.67 -41.15 ± 11.89003323.86-1521309 -52.85 ± 5.68 -26.91 ± 3.93 3.23 ± 0.86 -1.86 ± 0.18 8.46 ± 0.82 -39.09 ± 3.800452143+1634446 -22.62 ± 1.47 -14.31 ± 1.21 -5.02 ± 0.84 -5.66 ± 0.33 9.48 ± 0.55 -11.54 ± 0.6700470038+6803543 -8.58 ± 1.06 -27.83 ± 1.22 -13.53 ± 0.49 -6.52 ± 0.24 10.23 ± 0.37 1.1 ± 0.0401231125-6921379 -7.92 ± 1.96 -20.39 ± 2.71 -1.82 ± 2.42 14.9 ± 2.11 -27.1 ± 3.84 -33.76 ± 4.7802235464-5815067 -7.94 ± 0.86 -18.46 ± 1.19 -1.11 ± 0.7 4.29 ± 0.4 -20.41 ± 1.88 -29.71 ± 2.7402411151-0326587 -9.68 ± 4.71 -11.49 ± 1.49 -1.39 ± 6.56 -21.39 ± 2.55 1.63 ± 0.19 -30.27 ± 3.603350208+2342356 -16.91 ± 1.77 -11.46 ± 2.11 -8.08 ± 1.95 -36.8 ± 2.02 10.13 ± 0.55 -18.31 ± 103393521-3525440 -13.32 ± 0.35 -4.95 ± 0.52 -0.1 ± 0.85 -2.1 ± 0.01 -3.19 ± 0.02 -5.15 ± 0.0303552337+1133437 -5.53 ± 0.4 -26.32 ± 1.18 -15.34 ± 0.62 -7.72 ± 0.3 0.25 ± 0.01 -4.64 ± 0.1805012406-0010452 -15.15 ± 0.83 -27 ± 1.74 -1.08 ± 1.07 -16.76 ± 1.16 -6.02 ± 0.42 -8.06 ± 0.5605184616-2756457 -10.99 ± 0.93 -21.09 ± 1.55 -8.64 ± 1.37 -23.81 ± 6.57 -28.98 ± 8 -23.02 ± 6.3505361998-1920396 -10.85 ± 1.41 -18.95 ± 1.83 -7.49 ± 1.06 -24 ± 7.34 -22.27 ± 6.81 -15.21 ± 4.6505575096-1359503 -22.15 ± 7.41 -18.46 ± 8.29 -9.3 ± 9.91 -309.69 ± 83.51 -257.52 ± 69.45 -131.51 ± 35.4606085283-2753583 -15.51 ± 0.45 -19.93 ± 0.34 -7.79 ± 0.51 -16.84 ± 1.82 -23.54 ± 2.54 -11.12 ± 1.210220489+0200477 14.87 ± 4.49 -53.28 ± 19.96 -49.14 ± 14.81 -11.07 ± 3.8 -20.45 ± 7.02 24.35 ± 8.3610224821+5825453 -69.35 ± 2.74 -67.62 ± 3.48 0.1 ± 0.87 -10.57 ± 0.48 5.61 ± 0.26 13.98 ± 0.64TWA26 -9.02 ± 1.5 -18.29 ± 1.94 -3.52 ± 1.42 9.92 ± 1.02 -35.32 ± 3.63 19.9 ± 2.04TWA27A -7.62 ± 0.94 -18.24 ± 1.77 -3.52 ± 1.03 19.49 ± 0.41 -44.22 ± 0.94 20.06 ± 0.4214252798-3650229 -5.23 ± 0.21 -26.29 ± 0.27 -14.11 ± 0.19 8.56 ± 0.08 -6.42 ± 0.06 4.39 ± 0.0415525906+2948485 -9.73 ± 0.88 -22.44 ± 1.11 -4.71 ± 0.78 8.78 ± 0.47 9.7 ± 0.52 15.74 ± 0.8517260007+1538190 -8.66 ± 1.05 -21.01 ± 1.34 -6.26 ± 1.11 24.62 ± 2.4 19.25 ± 1.88 15.1 ± 1.4818212815+1414010 12.91 ± 0.12 4.62 ± 0.11 -11.30 ± 0.06 6.74 ± 0.01 6.17 ± 0.01 2.11 ± 0.0120575409-0252302 -12.44 ± 0.45 -19.97 ± 0.5 9.47 ± 0.39 8.66 ± 0.45 8.9 ± 0.47 -6.96 ± 0.36PSO318 -10.4 ± 0.7 -16.4 ± 0.6 -9.8 ± 0.8 15.2 ± 0.6 7.2 ± 0.3 -14.6 ± 0.621265040-8140293 -7.02 ± 1.07 -18.57 ± 1.09 -3.67 ± 0.39 17.55 ± 1.41 -20.48 ± 1.64 -16.95 ± 1.3622081363+2921215 -15.2 ± 0.87 -18.97 ± 1.83 -8.76 ± 1.13 3.64 ± 0.12 43.76 ± 1.4 -17.14 ± 0.55232246843133231 40.26 ± 2.74 -30.87 ± 3.18 -24.72 ± 1.27 5.55 ± 0.51 1.46 ± 0.13 -15.97 ± 1.47
Note. — Data is only presented for targets with measured parallax, or measured parallax and radial velocity. While the actual uncertaintiesare best described by a radially-oriented ellipsoid, they are given here for comparison to other values.
Brown Dwarf Analogs to Exoplanets 67Table
12
Movin
gG
roup
mem
bers
hip
pro
babilit
ies
BA
NY
AN
IIL
AC
Ew
ING
Converg
ence
BA
NY
AN
IN
am
eSpT
SpT
Pro
b.
Conta
m.
Gro
up
Pro
b.
Gro
up
Pro
b.
Gro
up
Pro
b.
Gro
up
Decis
ion
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
00011217+
1535355
––
L4β
97.4
1.1
AB
DO
R35.1
2A
BD
OR
43.1
AB
DO
R99.0
4A
BD
OR
AM
00040288-6
410358
L1γ
L1γa
99.6
0T
UC
-HO
R38.7
6T
UC
-HO
R100
TU
C-H
OR
100
TU
C-H
OR
HL
M00182834-6
703130
––
L0γ
99.9
<0.1
TU
C-H
OR
48.7
1T
UC
-HO
R76.7
TU
C-H
OR
99.8
3T
UC
-HO
RA
M00191296-6
226005
––
L1γ
99.7
<0.1
TU
C-H
OR
0N
ON
E99.7
TU
C-H
OR
89.4
4T
UC
-HO
RH
LM
00192626+
4614078
M8
–M
8β
72
13.3
AB
DO
R66.4
2A
BD
OR
99
AB
DO
R99
AB
DO
RH
LM
00274197+
0503417
M9.5β
L0βa
0100
AR
GU
S0
NO
NE
100
CH
A-N
EA
R100
OL
DA
M00303013-1
450333
L7
–L
4-L
6β
26.5
2.6
AR
GU
S29.6
5A
BD
OR
98.1
CH
A-N
EA
R97.8
7A
RG
US
AM
00325584-4
405058
L0γ
L0β
67.3
1T
UC
-HO
R91.3
AB
DO
R96
AB
DO
R100
AB
DO
RH
LM
003323.8
6-1
52130.9
L4β
L1
099.8
CO
LU
MB
A0
NO
NE
60
CH
A-N
EA
R100
OL
DN
M00344300-4
102266
––
L1β
98.7
<0.1
TU
C-H
OR
41.9
1T
UC
-HO
R70.1
TW
HY
A70.4
8T
UC
-HO
RA
M00374306-5
846229
L0γ
––
099.3
BE
TA
PIC
0N
ON
E71
CH
A-N
EA
R100
OL
DN
M00381489-6
403529
––
M9.5β
99.9
<0.1
TU
C-H
OR
62.8
3T
UC
-HO
R58
TU
C-H
OR
95.9
1T
UC
-HO
RH
LM
00425923+
1142104
––
M9β
19.6
53.1
AB
DO
R0
NO
NE
64.9
AB
DO
R83.0
2B
ET
AP
ICA
M00452143+
1634446
L2β
L2γa
99.9
0.1
AR
GU
S99.4
2A
RG
US
37
CH
A-N
EA
R100
AR
GU
SB
M00464841+
0715177
M9β
L0δ
31.3
48.8
CO
LU
MB
A24.4
4A
BD
OR
99
TW
HY
A99
CO
LU
MB
AA
M00470038+
6803543
L7
(γ?)
L6-L
8γ
100
0.1
AB
DO
R99.9
5A
BD
OR
56
AB
DO
R100
AB
DO
RB
M00550564+
0134365
L2γ
L2γa
9.2
48.3
BE
TA
PIC
0N
ON
E68
AB
DO
R100
OL
DN
M00584253-0
651239
L0
–L
1β
96.5
0.3
AB
DO
R52.5
AB
DO
R14.3
CO
LU
MB
A91.6
5B
ET
AP
ICA
M01033203+
1935361
L6β
L6β
51.2
15.7
AR
GU
S36.9
5H
yades
16
CH
A-N
EA
R96
OL
DA
M01174748-3
403258
L1β
L1βa
98.4
0T
UC
-HO
R30.6
3T
UC
-HO
R100
TU
C-H
OR
91
TU
C-H
OR
HL
M01205114-5
200349
––
L1γ
>99.9
<0.1
TU
C-H
OR
64.5
4T
UC
-HO
R100
TU
C-H
OR
95.1
8T
UC
-HO
RH
LM
01231125-6
921379
M7.5γ
––
100
0T
UC
-HO
R99.9
7T
UC
-HO
R100
TU
CH
OR
100
TU
CH
OR
BM
01244599-5
745379
L0γ
L0γa
099.3
CO
LU
MB
A0
NO
NE
0N
ON
E100
OL
DN
M01262109+
1428057
L4γ
L2γ
099.9
BE
TA
PIC
0N
ON
E99
CH
A-N
EA
R100
OL
DA
M01294256-0
823580
M5
–M
7β
95.9
18.9
BE
TA
PIC
0N
ON
E100
CO
LU
MB
A72.4
6C
OL
UM
BA
AM
01415823-4
633574
L0γ
L0γ
100
0T
UC
-HO
R99.8
4T
UC
-HO
R83.5
TU
C-H
OR
100
TU
C-H
OR
HL
M01531463-6
744181
L2
–L
3β
>99.9
<0.1
TU
C-H
OR
33.2
5T
UC
-HO
R98.8
TU
C-H
OR
99.4
9T
UC
-HO
RH
LM
02103857-3
015313
L0γ
L0γa
99.4
0T
UC
-HO
R96.3
4T
UC
-HO
R56
TU
C-H
OR
100
TU
C-H
OR
HL
M02212859-6
831400
M8β
––
0.8
99.4
AB
DO
R0
NO
NE
84
CH
A-N
EA
R62
AB
DO
RA
M02215494-5
412054
M9β
––
99.8
0T
UC
-HO
R99.9
1T
UC
-HO
R61
TU
C-H
OR
100
TU
C-H
OR
HL
M02235464-5
815067
L0γ
––
100
0T
UC
-HO
R99.9
8T
UC
-HO
R95
TU
CH
OR
100
TU
CH
OR
BM
02251947-5
837295
M9β
M9γa
57.5
1.2
BE
TA
PIC
40.5
2A
BD
OR
68
TU
C-H
OR
57
TU
C-H
OR
AM
02265658-5
327032
––
L0δ
>99.9
<0.1
TU
C-H
OR
65.9
TU
C-H
OR
43
TU
C-H
OR
77.5
7T
UC
-HO
RA
M02292794-0
053282
––
L0γ
79.8
1.3
BE
TA
PIC
81.0
2A
BD
OR
96
AB
DO
R100
OL
DA
M02340093-6
442068
L0γ
L0βγa
100
0T
UC
-HO
R99.5
6T
UC
-HO
R80
TU
C-H
OR
100
TU
C-H
OR
HL
M02410564-5
511466
––
L1γ
>99.9
<0.1
TU
C-H
OR
71.2
4T
UC
-HO
R99.9
TU
C-H
OR
95.3
6T
UC
-HO
RH
LM
02411151-0
326587
L0γ
L1γ
48.5
0T
UC
-HO
R0
NO
NE
35
CH
A-N
EA
R90
OL
DA
M02501167-0
151295
––
M7β
92.9
1.1
BE
TA
PIC
0N
ON
E98.8
TU
C-H
OR
67.1
OL
DA
M02530084+
1652532
––
M7β
...
...
FIE
LD
0N
ON
E0
NO
NE
100
OL
DN
M02535980+
3206373
M7β
M6β
57.8
26.5
BE
TA
PIC
20.6
1A
BD
OR
100
BE
TA
PIC
97
BE
TA
PIC
AM
02583123-1
520536
––
L3β
88.9
<0.1
TU
C-H
OR
0N
ON
E77.4
AB
DO
R49.8
2B
ET
AP
ICA
M03032042-7
312300
L2γ
––
40.7
0T
UC
-HO
R31.4
4T
UC
-HO
R98
TU
C-H
OR
87
OL
DA
M03164512-2
848521
L0
–L
1β
96.9
3.2
AB
DO
R50.9
9T
UC
-HO
R99.8
AB
DO
R99.2
5A
BD
OR
AM
03231002-4
631237
L0γ
L0γa
99.7
0T
UC
-HO
R73.0
8T
UC
-HO
R92
TU
C-H
OR
100
TU
C-H
OR
HL
M03264225-2
102057
L5β
L5βγa
99.4
1A
BD
OR
44.8
9A
BD
OR
66
AB
DO
R99
AB
DO
RH
LM
03350208+
2342356
M8.5
–M
7.5β
76.2
4.9
BE
TA
PIC
32.4
8A
RG
US
98
CO
LU
MB
A79
OL
DA
M03393521-3
525440
M9β
L0β
40.2
0.2
AR
GU
S43.8
2C
OM
AB
ER
0N
ON
E100
OL
DA
M03420931-2
904317
––
L0β
99.7
<0.1
TU
C-H
OR
27.8
6T
UC
-HO
R96.5
TU
C-H
OR
51.9
2C
OL
UM
BA
AM
03421621-6
817321
L4γ
––
99.8
<0.1
TU
C-H
OR
28.3
3T
UC
-HO
R99.7
TU
C-H
OR
98.7
1T
UC
-HO
RH
LM
03550477-1
032415
M8.5
–M
8.5β
93.8
<0.1
TU
C-H
OR
0N
ON
E99.9
TW
HY
A93.2
4C
OL
UM
BA
AM
03552337+
1133437
L5γ
L3-L
6γ
99.6
1.1
AB
DO
R100
AB
DO
R18
AB
DO
R100
AB
DO
RB
M03572695-4
417305c
L0β
L0β
99.2
0T
UC
-HO
R54.8
4T
UC
-HO
R62
TU
C-H
OR
53
TU
C-H
OR
AM
04062677-3
812102
L0γ
L1γ
0.3
79.6
CO
LU
MB
A41.0
7O
cta
ns
75
CH
A-N
EA
R100
OL
DA
M04185879-4
507413
––
L3γ
92.7
<0.1
TU
C-H
OR
28.9
7A
BD
OR
91.6
AB
DO
R64.9
AB
DO
RA
M04210718-6
306022
L5β
L5γa
99.5
2.4
BE
TA
PIC
52.7
4T
UC
-HO
R96
BE
TA
PIC
99
BE
TA
PIC
AM
04351455-1
414468
M8γ
M7γa
0.5
93.8
BE
TA
PIC
0N
ON
E89
CH
A-N
EA
R100
OL
DN
M04362788-4
114465
M8β
M9γ
99
0T
UC
-HO
R87.9
7T
UC
-HO
R87
TU
C-H
OR
100
TU
C-H
OR
HL
M
68 Faherty et al.Table
12
—Continued
BA
NY
AN
IIL
AC
Ew
ING
Converg
ence
BA
NY
AN
IN
am
eSpT
SpT
Pro
b.
Conta
m.
Gro
up
Pro
b.
Gro
up
Pro
b.
Gro
up
Pro
b.
Gro
up
Decis
ion
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
04400972-5
126544
––
L0γ
86.7
<0.1
TU
C-H
OR
27.1
9A
BD
OR
99.8
AB
DO
R72.2
5A
BD
OR
AM
04433761+
0002051c
M9γ
M9γ
99.7
3.4
BE
TA
PIC
59.7
3A
BD
OR
96
AB
DO
R79
BE
TA
PIC
AM
04493288+
1607226
––
M9γ
1.6
98.2
BE
TA
PIC
0N
ON
E99.9
TW
HY
A82.2
4B
ET
AP
ICA
M05012406-0
010452
L4γ
L3γa
20.8
0.4
CO
LU
MB
A82.8
7A
BD
OR
99
TU
C-H
OR
100
OL
DA
M05104958-1
843548
––
L2β
68.6
6.6
CO
LU
MB
A23.7
3T
UC
-HO
R89.6
TW
HY
A87.1
CO
LU
MB
AA
M05120636-2
949540
L5γ
L5βa
53.1
1B
ET
AP
IC0
NO
NE
6C
HA
-NE
AR
88
OL
DA
M05181131-3
101529
M6.5
–M
7β
96.2
8.8
CO
LU
MB
A0
NO
NE
90.4
CO
LU
MB
A91.2
3C
OL
UM
BA
AM
05184616-2
756457
L1γ
L1γ
99.4
0.1
CO
LU
MB
A74.9
1C
OL
UM
BA
13
CO
LU
MB
A87
CO
LU
MB
AB
M05264316-1
824315
––
M7β
93.5
12.8
CO
LU
MB
A0
NO
NE
83.1
CO
LU
MB
A88.6
6C
OL
UM
BA
AM
05341594-0
631397
M8γ
M8γ
099.8
CO
LU
MB
A0
NO
NE
100
BE
TA
PIC
99
OL
DA
M05361998-1
920396
L2γ
L2γa
99.2
0.1
CO
LU
MB
A35.2
3C
OL
UM
BA
78
BE
TA
PIC
57
BE
TA
PIC
AM
05402325-0
906326
––
M9β
72
16.1
CO
LU
MB
A0
NO
NE
95
TU
C-H
OR
87.3
CO
LU
MB
AA
M05575096-1
359503
M7
–M
7γ
36.4
0T
WH
YA
0N
ON
E99
TW
HY
A76
TW
HY
AA
M06023045+
3910592
L1
–L
1β
2.4
0.8
AB
DO
R46.3
3A
BD
OR
37
CO
LU
MB
A98
OL
DA
M06085283-2
753583
M8.5γ
L0γ
0100
BE
TA
PIC
0N
ON
E94
CH
A-N
EA
R49
BE
TA
PIC
AM
06272161-5
308428
––
L0βγ
87.2
9.1
CA
RIN
A37.7
2A
BD
OR
90.5
CH
A-N
EA
R84.7
CO
LU
MB
AA
M06322402-5
010349
L3β
L4γ
29.5
76.7
AB
DO
R41.7
7A
BD
OR
NO
NE
94.8
9N
ON
EA
M06524851-5
741376
M8β
––
2.9
85.4
AB
DO
R0
NO
NE
98
CH
A-N
EA
R98
AB
DO
RA
M07123786-6
155528
L1β
L1γa
78.7
37.6
BE
TA
PIC
39.1
2A
BD
OR
78
BE
TA
PIC
58
BE
TA
PIC
AM
07140394+
3702459
M8
–M
7.5β
88.9
0.5
AR
GU
S0
NO
NE
10.9
CH
A-N
EA
R87.3
5A
RG
US
AM
08095903+
4434216
––
L6p
80.7
27.4
AR
GU
S21.4
9A
BD
OR
15.7
CH
A-N
EA
R92.7
9A
RG
US
AM
08561384-1
342242
––
M8γ
4.9
<0.1
TW
HY
A0
NO
NE
78.8
TW
HY
A95.9
2O
LD
AM
08575849+
5708514
L8
–L
8–
...
...
FIE
LD
30.2
1H
ER
-LY
Rr
4.7
CH
A-N
EA
R93.9
8A
RG
US
AM
09451445-7
753150
––
M9β
90.4
2.8
CA
RIN
A41.8
6O
cta
ns
88.3
CH
A-N
EA
R67.5
6O
LD
AM
09532126-1
014205
M9γ
M9βa
28.7
0T
WH
YA
87.4
CO
MA
BE
R69
TU
C-H
OR
76
OL
DA
M09593276+
4523309
––
L3γ
2.1
0.3
TW
HY
A0
NO
NE
92
AB
DO
R69
OL
DN
MG
196-3
BL
3β
L3γ
41
23.3
AB
DO
R20.1
9A
BD
OR
42
CO
LU
MB
A95
AB
DO
RA
M10212570-2
830427
––
L4βγ
92.4
<0.1
TW
HY
A0
NO
NE
97.2
AB
DO
R99.3
TW
HY
AA
M10220489+
0200477
M9β
M9β
2.6
6.1
AB
DO
R0
NO
NE
0N
ON
E100
OL
DN
M10224821+
5825453
L1β
L1β
099.9
AB
DO
R0
NO
NE
14
AB
DO
R100
OL
DN
MT
WA
28
M8.5γ
M9γa
99.9
0T
WH
YA
100
TW
HY
A97
TW
HY
A100
TW
HY
AH
LM
11064461-3
715115
––
M9γ
94.6
<0.1
TW
HY
A0
NO
NE
99.5
CO
LU
MB
A99.8
5T
WH
YA
AM
11083081+
6830169
L1γ
L1γ
689.9
CA
RIN
A25.0
5A
BD
OR
77.6
CO
LU
MB
A96.6
3A
BD
OR
AM
11193254-1
137466
––
L7γ
92
0.0
005
TW
HY
A16
TW
HY
A90.4
TW
HY
A95.8
7T
WH
YA
HL
M11271382-3
735076
––
L0δ
92.5
<0.1
TW
HY
A0
NO
NE
99.7
CH
A-N
EA
R99.3
9T
WH
YA
AM
TW
A26
M9γ
M9γ
100
0T
WH
YA
100
TW
HY
A98
TW
HY
A100
TW
HY
AB
M114724.1
0-2
04021.3
––
L7γ
91.2
<0.1
TW
HY
A19
TW
HY
A90
TW
HY
A98
TW
HY
AH
LM
11480096-2
836488
––
L1β
68.9
<0.1
TW
HY
A91.5
3T
WH
YA
91
TW
HY
A99.9
3T
WH
YA
AM
11544223-3
400390
L0β
L1βa
91
0.6
AR
GU
S76.3
1T
WH
YA
99
CH
A-N
EA
R98
AR
GU
SA
MT
WA
27A
M8γ
M8γ
100
0T
WH
YA
100
TW
HY
A97
TW
HY
A100
TW
HY
AB
M12074836-3
900043
L0γ
L1γ
99.6
0T
WH
YA
99.7
2T
WH
YA
92
TW
HY
A100
TW
HY
AH
LM
12271545-0
636458
M9
–M
8.5β
1.5
0.6
TW
HY
A0
NO
NE
100
CO
LU
MB
A72.6
2T
WH
YA
AM
TW
A29
M9.5γ
L0γ
91.6
0T
WH
YA
76.8
6T
WH
YA
99
TW
HY
A95
TW
HY
AH
LM
12474428-3
816464
––
M9γ
36.4
0T
WH
YA
0N
ON
E99
TW
HY
A76
TW
HY
AA
M12535039-4
211215
––
M9.5γ
59.3
0T
WH
YA
0N
ON
E97.2
CO
LU
MB
A86.1
8T
WH
YA
AM
12563961-2
718455
––
L4βa
15.9
<0.1
TW
HY
A58.0
5T
WH
YA
75.8
AB
DO
R99.1
4T
WH
YA
AM
14112131-2
119503
M9β
M8βa
0.1
27.8
TW
HY
A65.1
6T
WH
YA
86
BE
TA
PIC
83
TW
HY
AA
M14252798-3
650229
L3
–L
4γ
99.9
0.1
AB
DO
R99.9
9A
BD
OR
39
AB
DO
R100
AB
DO
RB
M15104786-2
818174
M9
–M
9β
59.1
60.2
AR
GU
S0
NO
NE
99.1
CH
A-N
EA
R90.4
5A
RG
US
AM
15291017+
6312539
––
M8β
24.6
79.2
AB
DO
R0
NO
NE
81.4
AB
DO
R93.1
6A
BD
OR
AM
15382417-1
953116
L4γ
L4γa
0100
BE
TA
PIC
0N
ON
E0
NO
NE
100
OL
DN
M15470557-1
626303
A–
–M
9β
10.6
63.4
AB
DO
R0
NO
NE
97.1
AB
DO
R78.0
3A
BD
OR
AM
15474719-2
423493
M9γ
L0β
098.8
BE
TA
PIC
34.2
3A
BD
OR
17
TU
C-H
OR
97
OL
DN
M15515237+
0941148
L4γ
>L
5γa
0.1
99.1
AB
DO
R94.6
5C
OM
AB
ER
100
BE
TA
PIC
93
OL
DA
M15525906+
2948485
L0β
L0β
092.7
AB
DO
R21.9
5H
ER
-LY
Rr
19
TU
C-H
OR
80
OL
DA
M15575011-2
952431
M9δ
L1γa
0100
BE
TA
PIC
0N
ON
E100
AB
DO
R100
OL
DN
M16154255+
4953211
L4γ
L3-L
6γ
13.7
69
AB
DO
R31.8
2A
BD
OR
92
CO
LU
MB
A63
AB
DO
RA
M17111353+
2326333
L0γ
L1βa
0100
BE
TA
PIC
0N
ON
E94
BE
TA
PIC
96
BE
TA
PIC
NM
Brown Dwarf Analogs to Exoplanets 69Table
12
—Continued
BA
NY
AN
IIL
AC
Ew
ING
Converg
ence
BA
NY
AN
IN
am
eSpT
SpT
Pro
b.
Conta
m.
Gro
up
Pro
b.
Gro
up
Pro
b.
Gro
up
Pro
b.
Gro
up
Decis
ion
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
17260007+
1538190
L3.5γ
L3γa
099.8
AB
DO
R0
NO
NE
65
BE
TA
PIC
80
OL
DN
M17410280-4
642218
––
L6-L
8γa
99.7
1.8
BE
TA
PIC
78.7
8A
RG
US
94
BE
TA
PIC
100
BE
TA
PIC
AM
18212815+
1414010
L4.5
—L
4p
eca
0100
NO
NE
0N
ON
E0
NO
NE
100
OL
DN
M19350976-6
200473
––
L1γ
20.8
0.2
TU
C-H
OR
0N
ON
E100
TU
C-H
OR
97.3
2T
UC
-HO
RA
M19355595-2
846343
M9γ
M9γa
25.3
12.6
AR
GU
S0
NO
NE
100
CH
A-N
EA
R93
OL
DA
M19564700-7
542270
L0γ
L2γa
53.3
0T
UC
-HO
R26.8
TU
C-H
OR
97
CO
LU
MB
A97
TU
C-H
OR
AM
20004841-7
523070
M9γ
M9γa
99.4
3.5
BE
TA
PIC
84.0
5T
UC
-HO
R71
BE
TA
PIC
100
BE
TA
PIC
HL
M20025073-0
521524
L5β
L5-L
7γa
047.8
BE
TA
PIC
0N
ON
E0
NO
NE
100
OL
DN
M20113196-5
048112
––
L3γ
42.6
<0.1
TU
C-H
OR
0N
ON
E96.5
CO
LU
MB
A66.5
3T
UC
-HO
RA
M20135152-2
806020
M9γ
L0γa
77.6
39.5
BE
TA
PIC
28.9
4B
ET
AP
IC100
BE
TA
PIC
100
BE
TA
PIC
AM
20282203-5
637024
––
M8.5γ
44.3
<0.1
TU
C-H
OR
0N
ON
E94.6
AB
DO
R69.8
5T
UC
-HO
RA
M20334473-5
635338
––
L0γ
93.4
<0.1
TU
C-H
OR
0N
ON
E81.7
TU
C-H
OR
99.8
5T
UC
-HO
RA
M20391314-1
126531
M8
–M
7β
2.2
46.6
AB
DO
R0
NO
NE
100
CO
LU
MB
A71.2
4A
BD
OR
AM
20575409-0
252302
L1.5
–L
2β
0100
TU
C-H
OR
0N
ON
E0
NO
NE
100
OL
DN
MP
SO
318
––
L6-L
8γa
99.7
0.1
BE
TA
PIC
60.7
7A
RG
US
99
BE
TA
PIC
100
BE
TA
PIC
BM
21265040-8
140293b
L3γ
L3γa
9.3
1.4
BE
TA
PIC
76.5
1B
ET
AP
IC26
CH
A-N
EA
R94
TU
C-H
OR
AM
21324036+
1029494
––
L4β
30.8
61.6
AR
GU
S0
NO
NE
92.8
CH
A-N
EA
R53.4
4A
RG
US
AM
21543454-1
055308
L4β
L5γa
16.3
5.6
AR
GU
S0
NO
NE
29
CH
A-N
EA
R70
AR
GU
SA
M21544859-7
459134
––
M9.5β
99.4
<0.1
TU
C-H
OR
44.3
4T
UC
-HO
R100
TU
C-H
OR
99.9
4T
UC
-HO
RH
LM
21572060+
8340575
L0
–M
9γ
30.8
62.9
AB
DO
R0
NO
NE
63.3
AB
DO
R84
AB
DO
RA
M22025794-5
605087
––
M9γ
98.4
<0.1
TU
C-H
OR
32.4
9T
UC
-HO
R41.7
TU
C-H
OR
98.7
5T
UC
-HO
RA
M22064498-4
217208
L4γ
L4γa
99.1
1.4
AB
DO
R41.7
5A
BD
OR
89
AB
DO
R96
AB
DO
RH
LM
22081363+
2921215
L3γ
L3γ
0.2
91.2
BE
TA
PIC
0N
ON
E99
TW
HY
A66
BE
TA
PIC
NM
22134491-2
136079
L0γ
L0γ
35.4
45.8
BE
TA
PIC
0N
ON
E100
CO
LU
MB
A72
BE
TA
PIC
AM
22351658-3
844154
––
L1.5γ
96.2
<0.1
TU
C-H
OR
20.7
TU
C-H
OR
93.6
TU
C-H
OR
94.0
1T
UC
-HO
RH
LM
22353560-5
906306
––
M8.5β
99.8
<0.1
TU
C-H
OR
50.7
4T
UC
-HO
R99.7
TU
C-H
OR
99.9
5T
UC
-HO
RH
LM
22443167+
2043433
L6.5
p–
L6-L
8γa
99.4
0.5
AB
DO
R38.3
8A
BD
OR
69
AB
DO
R99
AB
DO
RH
LM
22495345+
0044046
L4γ
L3βa
0.2
96.1
AR
GU
S0
NO
NE
61
CH
A-N
EA
R100
OL
DN
M23153135+
0617146
L0γ
L0γa
099.6
CO
LU
MB
A0
NO
NE
92
CO
LU
MB
A100
OL
DN
M23224684-3
133231
L0β
L2β
054.5
AB
DO
R0
NO
NE
0N
ON
E100
OL
DN
M23225299-6
151275
L2γ
L3γa
99.9
0T
UC
-HO
R98.8
8T
UC
-HO
R34
TU
C-H
OR
100
TU
C-H
OR
HL
M23231347-0
244360
M8.5
–M
8β
30.6
54.4
BE
TA
PIC
0N
ON
E99.9
TW
HY
A55.2
8O
LD
AM
23255604-0
259508
L3
–L
1γ
73.4
12.3
AB
DO
R21.2
8A
BD
OR
91.2
AB
DO
R98.5
AB
DO
RA
M23360735-3
541489
––
M9β
50.8
30.3
AB
DO
R30.1
7T
UC
-HO
R74.5
AB
DO
R60.8
9T
UC
-HO
RA
M23433470-3
646021
––
L3-L
6γ
68.9
4.8
AB
DO
R38.4
6T
UC
-HO
R65.9
AB
DO
R56.1
7T
UC
-HO
RA
M23453903+
0055137
M9
–M
9β
...
...
FIE
LD
0N
ON
E99.6
BE
TA
PIC
40.3
9C
OL
UM
BA
AM
23520507-1
100435
M7
–M
8β
90.6
4A
BD
OR
27.2
2A
BD
OR
57.2
AB
DO
R97.8
5A
BD
OR
AM
Note.
—C
om
puta
tions
of
BA
NY
AN
Iand
IIw
ere
done
wit
hth
ew
eb
calc
ula
tor,
wit
hout
photo
metr
icdata
.B
AN
YA
NII
and
LA
CE
wIN
Gw
ere
com
pute
dass
um
ing
the
ob
jects
are
young.
The
pre
dic
ted
dis
tance
and
RV
(as
pre
dic
ted
by
LA
CE
wIN
Gfo
rth
efinal
gro
up)
should
be
com
pare
dto
the
valu
es
inT
able
10.
aT
hese
sourc
es
have
new
infr
are
dsp
ectr
apre
sente
din
this
pap
er.
Inth
em
ajo
rity
of
case
sw
euse
the
infr
are
dsp
ectr
al
typ
eand
gra
vit
ycla
ssifi
cati
on
dia
gnose
din
this
work
.If
an
ob
ject
had
Sp
eX
data
we
defa
ult
toth
ere
sult
ant
typ
eand
cla
ssifi
cati
on
wit
hth
at
data
.b
Deacon
et
al.
(2016)
use
the
para
llax
rep
ort
ed
inth
isw
ork
tosh
ow
that
this
sourc
eis
co-m
ovin
gw
ith
the
Mdw
arf
TY
C9486-9
27-1
.In
that
work
they
rep
ort
alikelihood
of
mem
bers
hip
in
theβ
pic
tori
sm
ovin
ggro
up,
how
ever
we
find
this
unlikely
wit
hth
egiv
en
kin
em
ati
cs.
The
mem
bers
hip
of
this
inte
rest
ing
wid
esy
stem
rem
ain
sunknow
n.
cT
hese
sourc
es
were
list
ed
inF
ilip
pazzo
et
al.
(2015)
as
mem
bers
of
ass
ocia
tions
but
as
has
been
note
din
Table
12,
we
have
dow
ngra
ded
them
toam
big
uos
young
ob
jects
dT
he
sourc
e0335+
2342
islist
ed
as
ab
onafide
mem
ber
ofβ
Pic
tori
sin
Gagne
et
al.
(2014d)
usi
ng
a2M
ASS
toW
ISE
pro
per
moti
on.
Asi
de
from
the
Shkoln
iket
al.
(2012)
pro
per
moti
on
use
din
this
work
,th
isso
urc
eals
ohas
aP
PM
XL
pro
per
moti
on.
Dep
endin
gon
whic
hvalu
eis
use
din
the
kin
em
ati
canaly
sis,
the
pro
babilit
yof
mem
bers
hip
vari
es.
Base
don
its
posi
tion
on
the
vari
ous
photo
metr
icand
abso
lute
magnit
ude
dia
gra
ms
inth
isw
ork
,w
esu
spect
this
sourc
eis
aβ
Pic
tori
sm
em
ber.
How
ever
refined
kin
em
ati
cs
will
confirm
this
.Furt
herm
ore
,A
llers
&L
iu
(2013)
list
this
ob
ject
as
an
M7
VL
Gso
urc
ehow
ever
we
have
chose
nto
list
itas
an
M7.5β
base
don
the
analy
sis
inG
agne
et
al.
(2014d).
70 Faherty et al.Table
13
Hig
hC
onfidence
Movin
gG
roup
Mem
bers
2M
ASS
SpT
SpT
µRA
µDEC
πR
VLBol
Teff
Mass
aR
ef
OpT
NIR
′′yr−
1′′
yr−
1m
as
km
s−1
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
AB
DORADUS
00192626+
4614078
M8
–M
8β
0.1
4000±
0.0
6-0
.1±
0.0
5(3
1±
3)
-19.5±
2-2
.773±
0.1
29
2637.0±
371.0
66.6
2±
48.9
92,4
00325584-4
405058
L0γ
L0β
0.1
2830±
0.0
034
-0.0
934±
0.0
03
21.6±
7.2
12.9
5±
1.9
2-3
.388±
0.2
89
2066.0±
413.0
41.6
4±
29.4
71,5
00470038+
6803543
L7
(γ?)
L6-L
8γ
0.3
8700±
0.0
04
-0.1
97±
0.0
04
82±
3-2
0±
1.4
-4.4
29±
0.0
33
1230.0±
27.0
11.8
4±
2.6
37
03264225-2
102057
L5β
L5βγa
0.1
08±
0.0
14
-0.1
46±
0.0
15
(41±
1)
(22.9
1±
2.0
7)
-4.2
35±
0.0
22
1346.0±
26.0
13.7
7±
2.6
1,2
03552337+
1133437
L5γ
L3-L
6γ
0.2
2500±
0.0
132
-0.6
3±
0.0
15
110.8±
4.3
11.9
2±
0.2
2-4
.104±
0.0
34
1478.0±
58.0
21.6
2±
6.1
46,1
414252798-3
650229
L3
–L
4γ
-0.2
8489±
0.0
014
-0.4
6308±
0.0
01
86.4
5±
0.8
35.3
7±
0.2
5-4
.038±
0.0
09
1535.0±
53.0
22.5
2±
6.0
713,1
422064498-4
217208
L4γ
L4γa
0.1
28±
0.0
13
-0.1
81±
0.0
08
(35±
2)
(7.6±
2.0
)-3
.997±
0.0
09
1566.0±
59.0
23.1
5±
6.3
71
22443167+
2043433
L6.5
p–
L6-L
8γa
0.2
52±
0.0
14
-0.2
14±
0.0
11
(54±
4)
(-15.5±
1.7
)-4
.503±
0.0
07
1184.0±
10.0
10.4
6±
1.4
91,2
ARG
US
00452143+
1634446
L2β
L2γa
0.3
5500±
0.0
1-0
.04±
0.0
162.5±
3.7
3.1
6±
0.8
3-3
.405±
0.0
31
2059.0±
45.0
24.9
8±
4.6
21
βPictoris
20004841-7
523070
M9γ
M9γa
0.0
69±
0.0
12
-0.1
1±
0.0
04
(31±
1)
4.3
97±
2.8
42
-2.9
72±
0.0
28
2375.0±
74.0
24.2
8±
5.6
31
PSO
318
––
L6-L
8γa
0.1
3730±
0.0
013
-0.1
387±
0.0
014
40.7±
2.4
−6.0
+0.8
−1.1
-4.3
9±
0.0
52
1213.0±
38.0
6.4
4±
1.2
921
COLUM
BA
05184616-2
756457
L1γ
L1γ
0.0
2860±
0.0
042
-0.0
16±
0.0
04
21.4±
6.9
24.3
5±
0.1
9-3
.575±
0.2
81808.0±
301.0
19.9
4±
9.2
31,8
TUCAN
AH
OROLOG
IUM
00040288-6
410358
L1γ
L1γa
0.0
64±
0.0
12
-0.0
47±
0.0
12
(17±
1)
(6.0
7±
2.8
9)
-3.4
8±
0.0
51
1904.0±
63.0
16.1
1±
2.9
100191296-6
226005
––
L1γ
0.0
541±
0.0
047
-0.0
345±
0.0
121
(21±
6)
(6.7±
2.5
)-3
.644±
0.2
48
1755.0±
258.0
14.8
8±
4.5
21,1
000381489-6
403529
––
M9.5β
0.0
871±
0.0
038
-0.0
353±
0.0
105
(23±
5)
(7.2
7±
2.8
1)
-3.4
23±
0.1
89
1957.0±
226.0
22.0
3±
9.3
91,1
001174748-3
403258
L1β
L1βa
0.0
84±
0.0
15
-0.0
45±
0.0
08
(20±
3)
(3.9
6±
2.0
9)
-3.4
77±
0.1
31902.0±
152.0
16.3
6±
3.6
91
01205114-5
200349
––
L1γ
0.0
921±
0.0
058
-0.0
404±
0.0
102
(24±
4)
(7.2
2±
2.5
)-3
.737±
0.1
45
1685.0±
145.0
13.9
7±
3.5
11,1
001231125-6
921379
M7.5γ
––
0.0
8278±
0.0
0174
-0.0
2646±
0.0
0139
21.6±
3.3
10.9±
3-2
.525±
0.1
33
2743.0±
317.0
55.5
6±
33.2
14,9
01415823-4
633574
L0γ
L0γ
0.1
05±
0.0
1-0
.049±
0.0
1(2
5±
3)
6.4
09±
1.5
6-3
.485±
0.1
04
1899.0±
123.0
16.2±
3.4
101531463-6
744181
L2
–L
3β
0.0
71±
0.0
037
-0.0
166±
0.0
127
(21±
7)
(10.4
1±
2.7
1)
-3.9
1±
0.2
91545.0±
264.0
11.8
9±
5.3
61,1
002103857-3
015313
L0γ
L0γa
0.1
45±
0.0
36
-0.0
4±
0.0
07
(32±
8)
7.8
2±
0.2
74
-3.8
26±
0.2
17
1610.0±
207.0
13.0
3±
4.3
11
02215494-5
412054
M9β
––
0.1
36±
0.0
1-0
.01±
0.0
17
(31±
5)
10.1
8±
0.0
97
——
—1,2
02235464-5
815067
L0γ
––
0.0
9860±
0.0
008
-0.0
182±
0.0
009
27.4±
2.6
10.3
6±
0.2
3-3
.509±
0.0
82
1879.0±
98.0
15.9
1±
3.1
21
02340093-6
442068
L0γ
L0βγ
0.0
88±
0.0
12
-0.0
15±
0.0
12
(21±
5)
11.7
62±
0.7
21
-3.5
38±
0.2
07
1848.0±
229.0
15.9
7±
4.2
91
02410564-5
511466
––
L1γ
0.0
965±
0.0
052
-0.0
123±
0.0
106
(24±
4)
(11.7
3±
2.4
4)
-3.6
79±
0.1
45
1731.0±
151.0
14.4
9±
3.4
91,1
003231002-4
631237
L0γ
L0γa
0.0
66±
0.0
08
0.0
01±
0.0
16
(17±
3)
13.0
01±
0.0
45
-3.3
48±
0.1
53
2031.0±
201.0
23.1
7±
9.7
51
03421621-6
817321
L4γ
––
0.0
653±
0.0
028
0.0
185±
0.0
091
(21±
9)
(13.8
7±
2.6
2)
-3.8
48±
0.3
72
1590.0±
349.0
12.3
8±
6.1
11
04362788-4
114465
M8β
M9γ
0.0
73±
0.0
12
0.0
13±
0.0
16
(23±
6)
14.9
72±
1.4
46
-2.8
72±
0.2
27
2452.0±
404.0
38.5±
22.5
91,2
21544859-7
459134
––
M9.5β
0.0
407±
0.0
022
-0.0
796±
0.0
122
(21±
7)
(6.2
1±
3.1
)-3
.219±
0.2
92118.0±
385.0
28.5
1±
15.1
51,1
022351658-3
844154
––
L1.5γ
0.0
505±
0.0
078
-0.0
757±
0.0
109
(22±
2)
(-4.9±
3.1
)—
——
10
22353560-5
906306
––
M8.5β
0.0
556±
0.0
051
-0.0
81±
0.0
108
(23±
5)
(1.7
1±
3.1
4)
-3.2
94±
0.1
89
2076.0±
251.0
25.1
3±
11.5
81,1
023225299-6
151275
L2γ
L3γa
0.0
62±
0.0
1-0
.085±
0.0
09
(22±
1)
6.7
47±
0.7
5-3
.606±
0.0
41793.0±
50.0
15.0
5±
2.6
61
TW
HYDRAE
TW
A28
M8.5γ
M9γa
-0.0
6720±
0.0
006
-0.0
14±
0.0
006
18.1±
0.5
(13.3±
1.8
)-2
.561±
0.0
24
2664.0±
81.0
35.3
9±
10.2
318
TW
A26
M9γ
M9γ
-0.0
8120±
0.0
039
-0.0
277±
0.0
021
23.8
2±
2.5
811.6±
2-2
.587±
0.0
94
2641.0±
192.0
35.3±
13.7
315,1
6T
WA
27A
M8γ
M8γ
-0.0
6300±
0.0
02
-0.0
23±
0.0
03
19.1±
0.4
11.2±
2-2
.602±
0.0
18
2635.0±
73.0
33.0
4±
9.3
216,1
911193254-1
137466
––
L7γ
-.1451±
0.0
149
-0.0
724±
0.0
16
(35±
5)
8.5±
3.3
-4.3
63±
0.1
24
1223.0±
90.0
6.5
7±
1.9
427
114724.1
0-2
04021.3
––
L7γ
-0.1
221±
0.0
12
-0.0
745±
0.0
113
(32±
4)
(9.6
1±
)-4
.346±
0.1
09
1235.0±
80.0
6.6
4±
1.8
928
12074836-3
900043
L0γ
L1γ
-0.0
572±
0.0
079
-0.0
248±
0.0
105
(15±
3)
(9.4
8±
1.9
1)
-3.4
85±
0.0
76
1882.0±
84.0
13.7
5±
0.7
517
TW
A29
M9.5γ
L0γ
-0.0
4030±
0.0
117
-0.0
203±
0.0
17
12.6
6±
2.0
7(7
.74±
2.0
4)
-2.9
05±
0.1
42
2394.0±
236.0
24.7
4±
8.4
315
Note.
—a
These
sourc
es
have
new
infr
are
dsp
ectr
apre
sente
din
this
pap
er.
Inth
em
ajo
rity
of
case
sw
euse
the
infr
are
dsp
ectr
al
typ
eand
gra
vit
ycla
ssifi
cati
on
dia
gnose
din
this
work
.If
an
ob
ject
had
Sp
eX
data
we
defa
ult
toth
ere
sult
ant
typ
eand
cla
ssifi
cati
on
wit
hth
at
data
.
Brown Dwarf Analogs to Exoplanets 71
Table 14Fundamental Parameters for Young Sources
2MASS SpT SpT π LBolb Teff
b Massb
OpT NIR mas K MJupiter
(1) (2) (3) (4) (5) (6) (7)
00040288-6410358 L1 γ L1 γa (17 ± 1) -3.48±0.051 1904.0±63.0 16.11±2.900191296-6226005 – – L1 γ (21 ± 6) -3.644±0.248 1755.0±258.0 14.88±4.5200192626+4614078 M8 – M8 β (31±3) -2.773±0.129 2637.0±371.0 66.62±48.9900274197+0503417 M9.5β L0β 13.8±1.6 -3.545±0.101 1945.0±197.0 31.64±19.2500303013-1450333 L7– L4-L6β 37.42±4.50 -4.378±0.105 1436.0±131.0 50.89±23.4300325584-4405058 L0γ L0β 21.6±7.2 -3.388±0.289 2066.0±413.0 41.64±29.47003323.86-1521309 L4β L1 24.8±2.5 -3.616±0.088 1880.0±173.0 29.68±17.7100381489-6403529 – – M9.5 β (23 ± 5) -3.423±0.189 1957.0±226.0 22.03±9.3900452143+1634446 L2β L2γ 62.5±3.7 -3.405±0.031 2059.0±45.0 24.98±4.6200470038+6803543 L7(γ?) L6-L8γ 82±3 -4.429±0.033 1230.0±27.0 11.84±2.6300584253-0651239 L0– L1β 33.8±4.0 -3.635±0.103 1860.0±180.0 29.48±17.7601033203+1935361 L6β L6β 46.9±7.6 -4.407±0.141 1223.0±113.0 12.82±8.4301174748-3403258 L1 β L1 βa (20 ± 3) -3.477±0.13 1902.0±152.0 16.36±3.6901205114-5200349 – – L1 γ (24 ± 4) -3.737±0.145 1685.0±145.0 13.97±3.5101231125-6921379 M7.5γ —- 21.6±3.3 -2.525±0.133 2743.0±317.0 55.56±33.2101415823-4633574 L0 γ L0 γ (25 ± 3) -3.485±0.104 1899.0±123.0 16.2±3.401531463-6744181 L2 – L3 β (21 ± 7) -3.91±0.29 1545.0±264.0 11.89±5.3602103857-3015313 L0 γ L0 γa (32 ± 8) -3.826±0.217 1610.0±207.0 13.03±4.3102212859-6831400 M8β —- 25.4±3.6 — — —02215494-5412054 M9 β —- (31 ± 5) — — —02235464-5815067 L0γ —- 27.4±2.6 -3.509±0.082 1879.0±98.0 15.91±3.1202340093-6442068 L0 γ L0β γ (21 ± 5) -3.538±0.207 1848.0±229.0 15.97±4.2902410564-5511466 – – L1 γ (24 ± 4) -3.679±0.145 1731.0±151.0 14.49±3.4902411151-0326587 L0γ L1γ 21.4±2.6 -3.717±0.106 1787.0±172.0 27.68±16.6702501167-0151295 —- M7β 30.2±4.5 -3.001±0.129 2821.0±242.0 103.42±16.1702530084+1652532 —- M7β 260.63±2.69 -3.193±0.121 2641.0±210.0 90.37±13.8802535980+3206373 M7β M6β 17.7±2.5 -2.788±0.123 2627.0±362.0 65.02±47.4803231002-4631237 L0 γ L0 γa (17 ± 3) -3.348±0.153 2031.0±201.0 23.17±9.7503264225-2102057 L5 β L5βγa (41 ± 1) -4.235±0.022 1346.0±26.0 13.77±2.603350208+2342356 M8.5– M7.5β 23.6±1.3 — — —03393521-3525440 M9β L0β 155.89±1.03 -3.563±0.005 1939.0±142.0 29.62±16.6703421621-6817321 L4 γ – – (21 ± 9) -3.848±0.372 1590.0±349.0 12.38±6.1103552337+1133437 L5γ L3-L6γ 110.8±4.3 -4.104±0.034 1478.0±58.0 21.62±6.1404362788-4114465 M8 β M9 γ (23 ± 6) -2.872±0.227 2452.0±404.0 38.5±22.5905012406-0010452 L4γ L3γ 51±3.7 -3.962±0.063 1563.0±116.0 22.15±13.205184616-2756457 L1γ L1γ 21.4±6.9 -3.575±0.28 1808.0±301.0 19.94±9.2305361998-1920396 L2γ L2γ 25.6±9.4 -3.826±0.319 1666.0±334.0 27.71±20.4605575096-1359503 M7– M7γ 1.9±1 — — —06023045+3910592 L1– L1β 88.5±1.6 -3.65±0.016 1857.0±133.0 27.88±15.6306085283-2753583 M8.5γ L0γ 32±3.6 -3.344±0.098 2147.0±228.0 37.85±24.0506524851-5741376 M8β —- 31.3±3.2 — — —07123786-6155528 L1β L1γ 22.9±9.1 -3.598±0.345 1861.0±412.0 35.66±25.807140394+3702459 M8– M7.5β 80.10±4.8 -3.479±0.052 2352.0±97.0 77.81±11.75G196-3B L3β L3γ 41±4.1 -3.752±0.087 1789.0±177.0 32.83±20.2510220489+0200477 M9β M9β 26.4±11.5 -3.323±0.378 2097.0±526.0 47.09±35.0910224821+5825453 L1β L1β 54.3±2.5 -3.682±0.041 1823.0±136.0 27.55±15.72TWA28 M8.5γ M9γ 18.1±0.5 -2.561±0.024 2664.0±81.0 35.39±10.2311193254-1137466 —- L7γ (35±5) -4.363±0.124 1223.0±90.0 6.57±1.94TWA26 M9γ M9γ 23.82±2.58 -2.587±0.094 2641.0±192.0 35.3±13.73114724.10-204021.3 —- L7γ (32±4) -4.346±0.109 1235.0±80.0 6.64±1.89TWA27A M8γ M8γ 19.1±0.4 -2.602±0.018 2635.0±73.0 33.04±9.3212074836-3900043 L0 γ L1 γ (15 ± 3) -3.485±0.076 1882.0±84.0 13.75±0.75TWA29 M9.5γ L0γ 12.66±2.07 -2.905±0.142 2394.0±236.0 24.74±8.4314252798-3650229 L3– L4γ 86.45±0.83 -4.038±0.009 1535.0±53.0 22.52±6.0715525906+2948485 L0β L0β 48.8±2.7 -3.538±0.017 1967.0±153.0 30.34±17.317260007+1538190 L3.5γ L3γ 28.6±2.9 -3.844±0.088 1667.0±146.0 24.82±14.8618212815+1414010 L4.5— L4pec 106.65±0.23 -2.801±0.006 2986.0±23.0 121.27±6.3820004841-7523070 M9 γ M9 γa (31 ± 1) -2.972±0.028 2375.0±74.0 24.28±5.6320575409-0252302 L1.5– L2β 70.1±3.7 -3.767±0.046 2041.0±88.0 69.5±13.04PSO318 —- L6-L8γ 40.7±2.4 -4.39±0.052 1213.0±38.0 6.44±1.2921265040-8140293 L3γ L3γ 31.3±2.6 -3.866±0.072 1651.0±132.0 24.21±14.321544859-7459134 – – M9.5 β (21 ± 7) -3.219±0.29 2118.0±385.0 28.51±15.1522064498-4217208 L4 γ L4 γa (35 ± 2) -3.997±0.009 1566.0±59.0 23.15±6.3722081363+2921215 L3γ L3γ 21.2±0.7 -3.705±0.029 1799.0±131.0 26.96±15.222351658-3844154 – – L1.5 γ (22±2) — — —22353560-5906306 – – M8.5 β (23 ± 5) -3.294±0.189 2076.0±251.0 25.13±11.5822443167+2043433 L6.5p – L6-L8 γa (54 ± 4) -4.503±0.007 1184.0±10.0 10.46±1.4923224684-3133231 L0β L2β 58.6±5.6 -3.85±0.083 1667.0±139.0 24.65±14.6923225299-6151275 L2 γ L3 γa (22 ± 1) -3.606±0.04 1793.0±50.0 15.05±2.66
72 Faherty et al.
Table 14 — Continued
2MASS SpT SpT π LBolb Teff
b Massb
OpT NIR mas K MJupiter
(1) (2) (3) (4) (5) (6) (7)
Note. —b
Lbol, Teff, and Mass are calculated as described in Filippazzo et al. (2015). Values that are slightly different from that work, have been updated
using new data presented in this paper.a
These sources have new infrared spectra presented in this paper. In the majority of cases we use the infrared spectral type and gravity
classification diagnosed in this work. If an object had SpeX data we default to the resultant type and classification with that data.
Brown Dwarf Analogs to Exoplanets 73Table
15
Avera
ge
Infr
are
dC
olo
rsof
late
-typ
eM
and
Ldw
arf
s
SpT
NJ−H
a(J
-H) avg
σ(J
-H)
NJ−K
a(J
-K) avg
σ(J
-K)
NJ−W
1a
(J-W
1) avg
σ(J
-W1)
NJ−W
2a
(J-W
2) avg
σ(J
-W2)
NH−K
a(H
-K) avg
σ(H
-K)
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
M7
1998
0.6
10.0
91976
0.9
70.1
01992
1.1
70.0
91990
1.3
70.1
01976
0.3
60.1
0M
8703
0.6
50.0
9698
1.0
60.1
1692
1.2
70.1
2692
1.4
90.1
3698
0.4
10.0
9M
9430
0.6
90.1
0428
1.1
50.1
1420
1.4
10.1
4420
1.6
50.1
7428
0.4
50.1
0L
0231
0.7
50.1
2223
1.2
20.1
5228
1.5
50.1
7225
1.8
30.1
9210
0.4
80.1
2L
1129
0.8
10.1
4125
1.3
50.1
9114
1.7
10.2
1114
1.9
70.2
3127
0.5
40.1
3L
265
0.9
10.1
466
1.5
10.2
157
1.9
80.2
857
2.2
70.3
265
0.5
90.1
1L
365
0.9
60.1
464
1.6
10.2
259
2.1
10.2
959
2.4
20.3
464
0.6
50.1
5L
439
1.0
70.1
738
1.7
40.2
534
2.4
00.3
433
2.7
40.4
038
0.6
70.1
4L
536
1.0
90.1
436
1.7
50.2
239
2.4
80.2
539
2.8
30.3
036
0.6
60.1
1L
618
1.1
10.2
019
1.8
40.2
821
2.5
90.4
121
3.0
00.5
223
0.7
60.1
6L
712
1.1
10.1
212
1.8
10.1
613
2.5
40.2
613
3.0
10.3
012
0.7
00.0
9L
818
1.1
10.1
219
1.7
80.1
617
2.5
60.2
017
3.1
30.2
420
0.6
70.0
9
aO
nly
norm
al
(non-
low
surf
ace
gra
vit
y,
sub
dw
arf
,or
young)
Ldw
arf
sw
ith
photo
metr
icuncert
ain
ty<
0.1
were
use
din
calc
ula
ting
the
avera
ge.
74 Faherty et al.Table
16
Avera
ge
Infr
are
dC
olo
rsof
late
-typ
eM
and
Ldw
arf
s
SpT
NH−W
1a
(H-W
1) avg
σ(H
-W1)
NH−W
2a
(H-W
2) avg
σ(H
-W2)
NK−W
1a
(K-W
1) avg
σ(K
-W1)
NK−W
2a
(K-W
2) avg
σ(K
-W2)
NW
1−W
2a
(W1-W
2) avg
σ(W
1-W
2)
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
M7
1992
0.5
50.0
91988
0.7
60.1
01970
0.2
00.0
91970
0.4
10.1
01991
0.2
10.0
6M
8692
0.6
20.1
0692
0.8
40.1
2687
0.2
20.0
9687
0.4
40.1
1692
0.2
20.0
6M
9420
0.7
20.1
1420
0.9
60.1
5417
0.2
60.1
0417
0.5
10.1
4421
0.2
40.0
6L
0222
0.8
10.1
3219
1.0
80.1
7223
0.3
40.1
2219
0.6
10.1
3229
0.2
70.0
8L
1113
0.9
10.1
5113
1.1
70.1
8112
0.3
70.1
1111
0.6
30.1
4118
0.2
60.0
6L
256
1.0
50.1
756
1.3
40.2
257
0.4
50.1
257
0.7
40.1
658
0.2
90.0
7L
358
1.1
60.2
058
1.4
70.2
459
0.5
10.1
459
0.8
20.1
863
0.3
10.0
6L
434
1.3
40.2
434
1.6
70.2
934
0.6
80.1
434
1.0
10.1
835
0.3
40.0
7L
540
1.3
90.1
539
1.7
40.2
038
0.7
40.1
237
1.0
80.1
841
0.3
50.0
8L
621
1.4
90.3
021
1.9
20.3
822
0.7
70.2
022
1.1
90.2
623
0.4
10.1
2L
714
1.4
50.1
914
1.9
10.2
414
0.7
60.1
414
1.2
20.1
915
0.4
50.0
9L
819
1.4
60.1
618
2.0
40.1
919
0.8
00.1
118
1.3
70.1
419
0.5
60.1
1
aO
nly
norm
al
(non-
low
surf
ace
gra
vit
y,
sub
dw
arf
,or
young)
Ldw
arf
sw
ith
photo
metr
icuncert
ain
ty<
0.1
were
use
din
calc
ula
ting
the
avera
ge.
Brown Dwarf Analogs to Exoplanets 75Table
17
Infr
are
dC
olo
rsof
low
gra
vit
yla
te-t
yp
eM
and
Ldw
arf
s
Nam
eSpT
SpT
(J-H
)#
ofσ(J−H
)a
(J-K
)#
ofσ(J−K
)a
(J-W
1)
#ofσ(J−W
1)a
(J-W
2)
#ofσ(J−W
2)a
(H-K
)#
ofσ(H−K
)a
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
01231125-6
921379
M7.5γ
––
0.6
1±
0.0
30.0
1.0
0±
0.0
30.3
1.2
6±
0.0
31.0
1.5
0±
0.0
31.3
0.3
9±
0.0
30.3
01294256-0
823580
M5
–M
7β
0.5
7±
0.0
3-0
.40.8
8±
0.0
3-0
.91.1
1±
0.0
3-0
.71.3
3±
0.0
3-0
.40.3
1±
0.0
3-0
.502501167-0
151295
––
M7β
0.6
1±
0.0
30.0
0.9
8±
0.0
30.1
1.2
0±
0.0
30.3
1.4
4±
0.0
30.6
0.3
7±
0.0
30.1
02530084+
1652532
––
M7β
0.5
1±
0.0
4-1
.10.8
1±
0.0
5-1
.61.0
7±
0.0
3-1
.11.3
4±
0.0
3-0
.30.3
0±
0.0
6-0
.602535980+
3206373
M7β
M6β
0.6
9±
0.0
30.8
1.0
7±
0.0
31.0
1.2
9±
0.0
31.4
1.4
9±
0.0
31.2
0.3
8±
0.0
30.2
03350208+
2342356
M8.5
–M
7.5β
0.6
0±
0.0
3-0
.20.9
9±
0.0
20.2
1.2
1±
0.0
30.4
1.4
8±
0.0
31.1
0.3
9±
0.0
20.3
05181131-3
101529
M6.5
–M
7β
0.6
4±
0.0
30.4
0.9
8±
0.0
30.1
1.2
4±
0.0
30.7
1.4
8±
0.0
31.1
0.3
3±
0.0
3-0
.305264316-1
824315
––
M7β
0.5
2±
0.0
3-1
.00.9
1±
0.0
3-0
.61.1
6±
0.0
3-0
.11.4
1±
0.0
30.4
0.3
9±
0.0
30.3
05575096-1
359503
M7–
M7γ
0.7
3±
0.0
31.3
1.1
4±
0.0
31.7
1.5
4±
0.0
34.1
2.0
7±
0.0
37.0
0.4
1±
0.0
30.5
07140394+
3702459
M8–
M7.5β
0.7
2±
0.0
31.3
1.1
4±
0.0
31.7
1.4
1±
0.0
32.7
1.6
3±
0.0
32.6
0.4
1±
0.0
30.5
20391314-1
126531
M8–
M7β
0.6
6±
0.0
40.6
1.1
1±
0.0
41.4
1.3
3±
0.0
31.7
1.6
3±
0.0
32.6
0.4
5±
0.0
50.9
00192626+
4614078
M8
–M
8β
0.6
6±
0.0
30.1
1.1
0±
0.0
20.4
1.3
4±
0.0
30.6
1.6
0±
0.0
30.9
0.4
4±
0.0
20.3
02212859-6
831400
M8β
––
0.6
9±
0.0
50.4
1.1
6±
0.0
50.9
1.4
9±
0.0
41.9
1.7
7±
0.0
42.2
0.4
7±
0.0
50.7
03550477-1
032415
M8.5
–M
8.5β
0.6
2±
0.0
3-0
.41.1
1±
0.0
30.4
1.3
7±
0.0
30.8
1.6
6±
0.0
31.3
0.4
9±
0.0
30.9
04351455-1
414468
M8γ
M7γ
1.2
6±
0.0
46.7
1.9
3±
0.0
47.9
2.1
7±
0.0
47.5
2.6
1±
0.0
48.6
0.6
7±
0.0
32.9
04362788-4
114465
M8β
M9γ
0.6
7±
0.0
30.2
1.0
5±
0.0
3-0
.11.3
6±
0.0
30.7
1.6
4±
0.0
31.1
0.3
8±
0.0
3-0
.305341594-0
631397
M8γ
M8γ
0.6
8±
0.1
20.4
1.1
1±
0.1
20.5
1.2
7±
0.0
80.0
1.8
0±
0.0
92.4
0.4
3±
0.1
40.2
06085283-2
753583
M8.5γ
L0γ
0.7
0±
0.0
40.5
1.2
3±
0.0
41.5
1.6
2±
0.0
42.9
1.9
7±
0.0
33.7
0.5
3±
0.0
31.3
06524851-5
741376
M8β
––
0.6
7±
0.0
30.2
1.1
8±
0.0
31.1
1.4
8±
0.0
31.7
1.7
8±
0.0
32.2
0.5
2±
0.0
31.2
08561384-1
342242
––
M8γ
0.6
3±
0.0
4-0
.31.1
1±
0.0
30.5
1.4
5±
0.0
31.5
1.9
8±
0.0
33.8
0.4
9±
0.0
40.9
TW
A28
M8.5γ
M9γ
0.6
8±
0.0
30.3
1.1
4±
0.0
30.8
1.6
0±
0.0
32.7
2.2
4±
0.0
35.8
0.4
7±
0.0
30.6
TW
A27A
M8γ
M8γ
0.6
1±
0.0
4-0
.41.0
5±
0.0
4-0
.11.4
4±
0.0
41.5
1.9
9±
0.0
43.9
0.4
4±
0.0
40.3
12271545-0
636458
M9–
M8.5β
0.8
1±
0.0
41.7
1.3
1±
0.0
42.3
1.6
8±
0.0
43.4
1.9
4±
0.0
43.4
0.5
0±
0.0
51.1
15291017+
6312539
––
M8β
0.7
1±
0.0
40.6
1.0
9±
0.0
30.3
1.3
5±
0.0
30.7
1.5
9±
0.0
30.7
0.3
8±
0.0
4-0
.320282203-5
637024
––
M8.5γ
0.5
9±
0.0
3-0
.61.1
3±
0.0
30.6
1.3
7±
0.0
30.8
1.6
6±
0.0
31.3
0.5
3±
0.0
41.4
22353560-5
906306
––
M8.5β
0.6
9±
0.0
50.4
1.1
1±
0.0
40.5
1.5
9±
0.0
42.7
1.9
2±
0.0
43.3
0.4
2±
0.0
50.2
23231347-0
244360
M8.5
–M
8β
0.6
5±
0.0
40.1
1.1
0±
0.0
30.4
1.3
4±
0.0
30.6
1.6
3±
0.0
31.0
0.4
4±
0.0
40.4
23520507-1
100435
M7–
M8β
0.6
7±
0.0
30.3
1.1
0±
0.0
30.3
1.4
0±
0.0
31.1
1.6
9±
0.0
31.6
0.4
2±
0.0
30.2
00274197+
0503417
M9.5β
L0β
0.9
0±
0.1
42.1
1.2
3±
0.1
50.7
1.5
7±
0.1
01.1
2.0
5±
0.1
12.4
0.3
3±
0.1
5-1
.200381489-6
403529
––
M9.5β
0.6
6±
0.0
5-0
.31.1
3±
0.0
4-0
.21.6
2±
0.0
41.5
1.9
8±
0.0
42.0
0.4
7±
0.0
60.2
00425923+
1142104
––
M9β
0.6
8±
0.0
6-0
.11.2
4±
0.0
50.8
1.5
2±
0.0
40.8
1.8
4±
0.0
51.1
0.5
6±
0.0
51.1
00464841+
0715177
M9β
L0δ
0.7
1±
0.0
40.2
1.3
4±
0.0
41.7
1.8
2±
0.0
42.9
2.2
5±
0.0
33.5
0.6
3±
0.0
41.8
02215494-5
412054
M9β
––
0.6
8±
0.0
4-0
.11.2
3±
0.0
40.7
1.5
8±
0.0
41.2
1.9
4±
0.0
41.7
0.5
5±
0.0
41.0
02251947-5
837295
M9β
M9γ
0.6
8±
0.0
4-0
.11.1
8±
0.0
40.3
1.5
0±
0.0
30.7
1.8
1±
0.0
31.0
0.5
0±
0.0
40.5
03393521-3
525440
M9β
L0β
0.7
1±
0.0
30.2
1.1
8±
0.0
30.2
1.5
9±
0.0
31.3
1.9
2±
0.0
31.6
0.4
7±
0.0
30.2
04433761+
0002051
M9γ
M9γ
0.7
0±
0.0
30.1
1.2
9±
0.0
31.2
1.6
8±
0.0
31.9
2.0
3±
0.0
32.2
0.5
8±
0.0
31.3
04493288+
1607226
––
M9γ
0.7
8±
0.0
40.9
1.2
0±
0.0
40.4
1.5
4±
0.0
40.9
1.8
5±
0.0
41.2
0.4
1±
0.0
4-0
.405402325-0
906326
––
M9β
0.7
4±
0.0
50.5
1.2
6±
0.0
61.0
1.5
6±
0.0
41.0
1.8
4±
0.0
51.1
0.5
2±
0.0
60.7
09451445-7
753150
––
M9β
0.6
6±
0.0
4-0
.31.1
1±
0.0
4-0
.41.3
8±
0.0
4-0
.21.6
1±
0.0
4-0
.20.4
4±
0.0
4-0
.109532126-1
014205
M9γ
M9β
0.8
2±
0.0
41.3
1.3
3±
0.0
31.6
1.7
1±
0.0
32.2
2.0
7±
0.0
32.4
0.5
0±
0.0
30.5
10220489+
0200477
M9β
M9β
0.7
0±
0.0
40.1
1.2
0±
0.0
40.5
1.4
9±
0.0
40.6
1.7
6±
0.0
40.6
0.5
0±
0.0
40.5
11064461-3
715115
––
M9γ
0.6
4±
0.0
4-0
.51.1
5±
0.0
50.0
1.4
2±
0.0
40.0
1.7
3±
0.0
40.5
0.5
1±
0.0
50.6
TW
A26
M9γ
M9γ
0.6
9±
0.0
30.0
1.1
8±
0.0
30.3
1.5
3±
0.0
30.9
1.8
9±
0.0
31.4
0.4
9±
0.0
30.4
TW
A29
M9.5γ
L0γ
0.7
2±
0.0
50.3
1.1
5±
0.0
50.0
1.5
2±
0.0
40.8
1.9
0±
0.0
41.4
0.4
3±
0.0
5-0
.212474428-3
816464
––
M9γ
0.6
9±
0.0
50.0
1.2
1±
0.0
50.6
1.6
8±
0.0
41.9
2.2
6±
0.0
43.6
0.5
2±
0.0
50.7
12535039-4
211215
––
M9.5γ
0.7
0±
0.1
50.1
1.2
6±
0.1
51.0
1.7
2±
0.1
12.2
2.0
8±
0.1
12.5
0.5
6±
0.1
51.1
14112131-2
119503
M9β
M8β
0.6
1±
0.0
3-0
.81.1
1±
0.0
3-0
.41.3
6±
0.0
3-0
.41.6
2±
0.0
3-0
.20.5
0±
0.0
30.5
15104786-2
818174
M9–
M9β
0.7
3±
0.0
40.4
1.1
5±
0.0
40.0
1.5
2±
0.0
40.8
1.8
3±
0.0
41.0
0.4
2±
0.0
4-0
.315470557-1
626303A
––
M9β
0.6
2±
0.0
4-0
.71.1
3±
0.0
4-0
.21.4
3±
0.0
40.1
1.7
2±
0.0
40.4
0.5
1±
0.0
40.6
15474719-2
423493
M9γ
L0β
0.7
0±
0.0
40.1
1.2
3±
0.0
30.7
1.5
6±
0.0
41.1
1.8
7±
0.0
41.3
0.5
3±
0.0
40.8
15575011-2
952431
M9δ
L1γ
0.8
7±
0.1
61.8
1.4
7±
0.1
62.9
1.8
8±
0.1
23.4
2.2
5±
0.1
33.5
0.6
0±
0.1
51.5
19355595-2
846343
M9γ
M9γ
0.7
7±
0.0
30.8
1.2
4±
0.0
40.8
1.6
1±
0.0
41.4
2.0
4±
0.0
32.3
0.4
7±
0.0
30.2
20004841-7
523070
M9γ
M9γa
0.7
7±
0.0
30.8
1.2
2±
0.0
30.7
1.6
3±
0.0
31.5
1.9
4±
0.0
31.7
0.4
6±
0.0
40.1
20135152-2
806020
M9γ
L0γ
0.7
8±
0.0
40.9
1.3
0±
0.0
41.4
1.7
2±
0.0
42.2
2.0
8±
0.0
42.5
0.5
2±
0.0
40.7
21544859-7
459134
––
M9.5β
0.7
2±
0.0
50.3
1.2
0±
0.0
40.5
1.5
8±
0.0
41.2
1.9
1±
0.0
41.5
0.4
8±
0.0
50.3
21572060+
8340575
L0–
M9γ
0.9
1±
0.0
42.2
1.3
9±
0.0
42.2
1.8
8±
0.0
33.4
2.2
9±
0.0
33.8
0.4
8±
0.0
40.3
22025794-5
605087
––
M9γ
0.7
4±
0.0
50.5
1.2
0±
0.0
50.4
1.5
5±
0.0
41.0
1.8
0±
0.0
40.9
0.4
6±
0.0
50.1
76 Faherty et al.Table
17
—Continued
Nam
eSpT
SpT
(J-H
)#
ofσ(J−H
)a
(J-K
)#
ofσ(J−K
)a
(J-W
1)
#ofσ(J−W
1)a
(J-W
2)
#ofσ(J−W
2)a
(H-K
)#
ofσ(H−K
)a
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
23360735-3
541489
––
M9β
0.8
4±
0.0
41.5
1.2
7±
0.0
51.1
1.6
5±
0.0
31.7
2.0
0±
0.0
42.1
0.4
2±
0.0
5-0
.323453903+
0055137
M9–
M9β
0.6
5±
0.0
4-0
.41.1
9±
0.0
40.4
1.5
6±
0.0
41.1
1.8
9±
0.0
41.4
0.5
4±
0.0
40.9
00182834-6
703130
––
L0γ
0.9
8±
0.0
81.9
1.7
5±
0.0
73.5
2.2
9±
0.0
64.3
2.6
9±
0.0
64.5
0.7
7±
0.0
72.4
00325584-4
405058
L0γ
L0β
0.9
2±
0.0
51.4
1.5
1±
0.0
51.9
1.9
6±
0.0
42.4
2.2
9±
0.0
42.4
0.5
9±
0.0
50.9
00374306-5
846229
L0γ
––
1.1
2±
0.0
73.0
1.7
8±
0.0
73.8
2.2
5±
0.0
64.1
2.6
4±
0.0
64.2
0.6
7±
0.0
71.6
01244599-5
745379
L0γ
L0γ
1.2
5±
0.1
44.2
1.9
9±
0.1
45.1
2.5
4±
0.1
15.8
2.9
7±
0.1
16.0
0.7
4±
0.1
22.2
01415823-4
633574
L0γ
L0γ
0.9
6±
0.0
51.7
1.7
3±
0.0
53.4
2.2
8±
0.0
54.3
2.6
6±
0.0
54.4
0.7
8±
0.0
42.5
02103857-3
015313
L0γ
L0γa
0.9
1±
0.0
61.3
1.5
7±
0.0
62.3
2.0
6±
0.0
53.0
2.4
1±
0.0
53.1
0.6
6±
0.0
61.5
02235464-5
815067
L0γ
––
1.0
7±
0.0
62.6
1.6
5±
0.0
62.9
2.2
5±
0.0
54.1
2.6
4±
0.0
54.3
0.5
8±
0.0
60.9
02265658-5
327032
––
L0δ
1.0
6±
0.0
72.6
1.6
5±
0.0
62.9
2.1
8±
0.0
53.7
2.6
2±
0.0
54.2
0.5
9±
0.0
70.9
02292794-0
053282
––
L0γ
0.7
4±
0.1
4-0
.11.3
1±
0.1
70.6
1.7
7±
0.1
01.3
2.1
6±
0.1
11.7
0.5
6±
0.1
70.7
02340093-6
442068
L0γ
L0βγ
0.8
8±
0.0
81.1
1.4
8±
0.0
91.7
2.0
8±
0.0
73.1
2.4
2±
0.0
73.1
0.5
9±
0.0
90.9
02411151-0
326587
L0γ
L1γ
0.9
9±
0.0
82.0
1.7
6±
0.0
83.6
2.1
6±
0.0
73.6
2.5
4±
0.0
73.8
0.7
7±
0.0
72.4
03231002-4
631237
L0γ
L0γa
1.0
7±
0.0
92.7
1.6
9±
0.0
93.1
2.3
1±
0.0
74.5
2.7
2±
0.0
74.7
0.6
2±
0.0
81.2
03420931-2
904317
––
L0β
0.5
7±
0.1
4-1
.51.5
4±
0.1
22.1
1.9
5±
0.0
92.3
2.3
8±
0.0
92.9
0.9
8±
0.1
44.1
03572695-4
417305
L0β
L0β
0.8
4±
0.0
40.7
1.4
6±
0.0
41.6
1.8
9±
0.0
42.0
2.2
8±
0.0
42.4
0.6
2±
0.0
41.2
04062677-3
812102
L0γ
L1γ
1.0
6±
0.1
62.6
1.6
6±
0.1
72.9
2.3
2±
0.1
34.5
2.6
7±
0.1
34.4
0.6
0±
0.1
51.0
04400972-5
126544
––
L0γ
0.9
1±
0.0
91.3
1.5
1±
0.0
92.0
2.1
0±
0.0
73.2
2.4
9±
0.0
73.5
0.6
1±
0.0
81.1
06272161-5
308428
––
L0βγ
1.1
5±
0.1
53.3
1.7
0±
0.1
43.2
2.5
0±
0.1
25.6
2.8
8±
0.1
25.5
0.5
4±
0.1
30.5
11271382-3
735076
––
L0δ
0.9
0±
0.1
41.3
1.2
4±
0.1
80.1
2.0
1±
0.1
02.7
2.3
7±
0.1
12.8
0.3
4±
0.1
9-1
.211544223-3
400390
L0β
L1β
0.8
6±
0.0
41.0
1.3
5±
0.0
40.8
1.8
5±
0.0
41.7
2.1
6±
0.0
41.7
0.4
8±
0.0
40.0
12074836-3
900043
L0γ
L1γ
0.8
9±
0.0
81.1
1.4
5±
0.0
81.6
1.8
6±
0.0
61.8
2.2
8±
0.0
62.4
0.5
7±
0.0
80.7
15525906+
2948485
L0β
L0β
0.8
7±
0.0
31.0
1.4
6±
0.0
31.6
1.9
3±
0.0
32.3
2.2
7±
0.0
32.3
0.5
9±
0.0
40.9
17111353+
2326333
L0γ
L1β
0.8
3±
0.0
40.7
1.4
4±
0.0
41.5
1.9
2±
0.0
32.2
2.2
7±
0.0
32.3
0.6
1±
0.0
41.1
19564700-7
542270
L0γ
L2γ
1.1
2±
0.1
43.1
1.9
2±
0.1
24.7
2.4
6±
0.1
15.4
2.9
1±
0.1
15.7
0.8
1±
0.1
22.7
20334473-5
635338
––
L0γ
0.5
8±
0.1
4-1
.41.4
7±
0.1
21.7
1.9
0±
0.0
92.1
2.3
0±
0.0
92.5
0.8
9±
0.1
43.4
22134491-2
136079
L0γ
L0γ
0.9
7±
0.0
61.9
1.6
2±
0.0
52.6
2.1
5±
0.0
43.5
2.5
4±
0.0
43.8
0.6
4±
0.0
71.4
23153135+
0617146
L0γ
L0γ
1.1
0±
0.1
13.0
1.7
9±
0.1
03.8
2.3
1±
0.0
94.5
2.7
7±
0.0
94.9
0.6
9±
0.0
91.7
23224684-3
133231
L0β
L2β
0.7
9±
0.0
40.3
1.2
5±
0.0
40.2
1.6
0±
0.0
40.3
1.8
7±
0.0
40.2
0.4
7±
0.0
3-0
.100040288-6
410358
L1γ
L1γa
0.9
6±
0.1
01.0
1.7
8±
0.0
82.2
2.4
2±
0.0
83.4
2.8
5±
0.0
83.8
0.8
2±
0.0
92.2
00191296-6
226005
––
L1γ
1.0
2±
0.0
81.5
1.6
8±
0.0
81.8
2.2
9±
0.0
72.8
2.7
6±
0.0
73.4
0.6
6±
0.0
70.9
00344300-4
102266
––
L1β
0.9
0±
0.0
90.6
1.6
2±
0.0
91.4
2.2
1±
0.0
72.4
2.6
1±
0.0
72.8
0.7
2±
0.0
91.4
00584253-0
651239
L0–
L1β
0.8
7±
0.0
40.4
1.4
1±
0.0
40.3
1.7
5±
0.0
30.2
2.0
6±
0.0
40.4
0.5
4±
0.0
40.0
01174748-3
403258
L1β
L1βa
0.9
7±
0.0
51.1
1.6
9±
0.0
51.8
2.1
5±
0.0
42.1
2.5
6±
0.0
42.5
0.7
2±
0.0
51.4
01205114-5
200349
––
L1γ
0.9
8±
0.1
01.2
1.8
9±
0.0
92.8
2.4
1±
0.0
83.3
2.8
6±
0.0
83.9
0.9
1±
0.0
92.8
02410564-5
511466
––
L1γ
1.0
6±
0.0
81.8
1.6
5±
0.0
71.6
2.2
0±
0.0
62.3
2.5
8±
0.0
62.6
0.5
9±
0.0
60.4
03164512-2
848521
L0–
L1β
0.8
1±
0.0
50.0
1.4
6±
0.0
50.6
1.9
3±
0.0
51.0
2.2
7±
0.0
51.3
0.6
6±
0.0
50.9
05184616-2
756457
L1γ
L1γ
0.9
7±
0.0
61.1
1.6
4±
0.0
61.5
2.2
2±
0.0
52.4
2.6
0±
0.0
52.7
0.6
8±
0.0
61.0
06023045+
3910592
L1–
L1β
0.8
5±
0.0
30.3
1.4
4±
0.0
30.4
1.8
7±
0.0
30.7
2.1
8±
0.0
30.9
0.5
9±
0.0
30.4
07123786-6
155528
L1β
L1γ
0.9
0±
0.0
70.7
1.6
3±
0.0
81.5
2.3
1±
0.0
72.8
2.6
7±
0.0
73.0
0.7
2±
0.0
61.4
10224821+
5825453
L1β
L1β
0.8
6±
0.0
40.3
1.3
4±
0.0
3-0
.11.7
4±
0.0
30.1
2.0
0±
0.0
30.1
0.4
8±
0.0
4-0
.411083081+
6830169
L1γ
L1γ
0.8
9±
0.0
30.6
1.5
4±
0.0
31.0
2.0
2±
0.0
31.5
2.3
7±
0.0
31.7
0.6
5±
0.0
30.9
11480096-2
836488
––
L1β
0.9
3±
0.1
10.8
1.5
5±
0.1
21.1
1.9
7±
0.0
81.3
2.3
4±
0.0
91.6
0.6
2±
0.1
20.6
19350976-6
200473
––
L1γ
0.9
6±
0.1
41.1
1.5
3±
0.1
40.9
2.2
0±
0.1
12.3
2.6
0±
0.1
12.8
0.5
7±
0.1
40.2
22351658-3
844154
––
L1.5γ
0.9
1±
0.0
70.7
1.5
5±
0.0
71.1
2.1
8±
0.0
62.2
2.5
4±
0.0
62.5
0.6
4±
0.0
60.8
23255604-0
259508
L3–
L1γ
1.0
3±
0.1
01.5
1.8
5±
0.1
02.6
2.2
7±
0.0
82.6
2.6
1±
0.0
82.8
0.8
2±
0.0
92.2
00452143+
1634446
L2β
L2γ
1.0
0±
0.0
40.6
1.6
9±
0.0
30.9
2.2
9±
0.0
31.1
2.6
7±
0.0
31.2
0.6
9±
0.0
40.9
00550564+
0134365
L2γ
L2γ
1.1
7±
0.1
41.8
2.0
0±
0.1
32.3
2.7
5±
0.1
22.8
3.2
3±
0.1
23.0
0.8
3±
0.1
02.2
03032042-7
312300
L2γ
––
1.0
4±
0.1
40.9
1.8
2±
0.1
41.5
2.3
6±
0.1
11.4
2.7
9±
0.1
11.6
0.7
8±
0.1
21.7
05104958-1
843548
––
L2β
1.0
1±
0.0
80.7
1.5
4±
0.0
80.1
2.1
0±
0.0
60.4
2.4
1±
0.0
60.4
0.5
3±
0.0
8-0
.605361998-1
920396
L2γ
L2γ
1.0
8±
0.1
01.2
1.9
2±
0.1
01.9
2.5
1±
0.0
81.9
2.9
8±
0.0
82.2
0.8
4±
0.0
92.3
20575409-0
252302
L1.5
–L
2β
0.8
5±
0.0
3-0
.41.4
0±
0.0
3-0
.51.8
6±
0.0
3-0
.42.1
4±
0.0
3-0
.40.5
4±
0.0
3-0
.423225299-6
151275
L2γ
L3γa
1.0
1±
0.0
90.7
1.6
9±
0.0
70.8
2.3
0±
0.0
71.2
2.7
0±
0.0
71.4
0.6
8±
0.0
70.8
01531463-6
744181
L2
–L
3β
1.3
0±
0.1
62.4
1.9
9±
0.1
71.7
2.7
0±
0.1
42.0
3.2
0±
0.1
42.3
0.6
9±
0.1
30.2
02583123-1
520536
––
L3β
1.0
4±
0.0
90.6
1.7
2±
0.0
90.5
2.2
9±
0.0
80.6
2.7
1±
0.0
80.9
0.6
7±
0.0
80.2
04185879-4
507413
––
L3γ
1.1
2±
0.1
11.1
1.5
7±
0.1
2-0
.22.3
0±
0.0
90.7
2.7
1±
0.0
90.8
0.4
5±
0.1
1-1
.306322402-5
010349
L3β
L4γ
0.9
9±
0.0
60.2
1.6
9±
0.0
50.3
2.4
1±
0.0
51.0
2.8
6±
0.0
51.3
0.6
9±
0.0
50.3
09593276+
4523309
––
L3γ
1.1
2±
0.1
01.2
2.2
1±
0.0
82.7
3.0
2±
0.0
73.1
3.5
2±
0.0
73.2
1.0
9±
0.0
82.9
Brown Dwarf Analogs to Exoplanets 77Table
17
—Continued
Nam
eSpT
SpT
(J-H
)#
ofσ(J−H
)a
(J-K
)#
ofσ(J−K
)a
(J-W
1)
#ofσ(J−W
1)a
(J-W
2)
#ofσ(J−W
2)a
(H-K
)#
ofσ(H−K
)a
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
G196-3
BL
3β
L3γ
1.1
8±
0.0
61.6
2.0
5±
0.0
62.0
3.1
3±
0.0
53.5
3.7
0±
0.0
53.8
0.8
7±
0.0
51.5
17260007+
1538190
L3.5γ
L3γ
1.2
0±
0.0
81.7
2.0
1±
0.0
81.8
2.6
0±
0.0
71.7
2.9
8±
0.0
71.6
0.8
1±
0.0
71.0
20113196-5
048112
––
L3γ
1.1
7±
0.1
41.5
1.8
5±
0.1
41.1
2.4
1±
0.1
11.0
2.7
6±
0.1
21.0
0.6
8±
0.1
20.2
21265040-8
140293
L3γ
L3γ
1.1
4±
0.0
81.3
1.9
9±
0.0
71.7
2.6
3±
0.0
61.8
3.0
7±
0.0
61.9
0.8
5±
0.0
71.4
22081363+
2921215
L3γ
L3γ
1.0
0±
0.1
10.3
1.6
5±
0.1
10.2
2.4
4±
0.0
91.1
2.9
1±
0.0
91.4
0.6
4±
0.1
00.0
00011217+
1535355
––
L4β
1.0
2±
0.0
8-0
.31.8
1±
0.0
70.3
2.5
8±
0.0
70.5
3.0
1±
0.0
70.7
0.8
0±
0.0
70.9
003323.8
6-1
521309
L4β
L1
1.0
8±
0.0
80.0
1.8
8±
0.0
70.5
2.4
9±
0.0
60.2
2.8
1±
0.0
60.2
0.8
0±
0.0
60.9
01262109+
1428057
L4γ
L2γ
0.9
4±
0.3
1-0
.81.8
3±
0.2
60.4
2.8
7±
0.2
21.4
3.4
1±
0.2
21.7
0.8
9±
0.2
61.6
03421621-6
817321
L4γ
––
1.4
7±
0.1
62.3
2.3
1±
0.1
62.3
2.9
0±
0.1
41.5
3.3
7±
0.1
41.6
0.8
4±
0.1
21.2
05012406-0
010452
L4γ
L3γ
1.2
7±
0.0
51.2
2.0
2±
0.0
51.1
2.9
3±
0.0
41.6
3.4
6±
0.0
41.8
0.7
5±
0.0
50.6
10212570-2
830427
––
L4βγ
1.0
6±
0.1
90.0
1.9
3±
0.2
00.8
2.7
6±
0.1
61.0
3.2
4±
0.1
61.2
0.8
7±
0.1
71.4
12563961-2
718455
––
L4β
1.0
4±
0.1
8-0
.21.7
1±
0.1
6-0
.12.3
3±
0.1
3-0
.22.7
2±
0.1
30.0
0.6
7±
0.1
50.0
14252798-3
650229
L3–
L4γ
1.1
7±
0.0
40.6
1.9
4±
0.0
40.8
2.7
5±
0.0
41.0
3.1
7±
0.0
31.1
0.7
7±
0.0
30.7
15382417-1
953116
L4γ
L4γ
1.0
8±
0.0
90.1
1.9
3±
0.0
80.8
2.7
6±
0.0
71.1
3.2
1±
0.0
71.2
0.8
5±
0.0
81.3
15515237+
0941148
L4γ
>L
5γ
1.2
1±
0.1
30.8
2.0
1±
0.1
21.1
2.7
2±
0.1
10.9
3.2
0±
0.1
11.1
0.8
0±
0.0
91.0
16154255+
4953211
L4γ
L3-L
6γ
1.4
6±
0.1
72.3
2.4
8±
0.1
53.0
3.5
9±
0.1
43.5
4.1
7±
0.1
43.6
1.0
2±
0.1
22.5
18212815+
1414010
L4.5
—L
4p
ec
1.0
4±
0.0
3-0
.21.7
8±
0.0
30.2
2.5
8±
0.0
30.5
2.9
6±
0.0
30.5
0.7
5±
0.0
30.5
21324036+
1029494
––
L4β
1.2
3±
0.1
80.9
1.9
6±
0.1
70.9
2.5
6±
0.1
40.5
3.0
2±
0.1
40.7
0.7
3±
0.1
50.4
21543454-1
055308
L4β
L5γ
1.3
7±
0.1
51.8
2.2
4±
0.1
42.0
3.0
7±
0.1
22.0
3.5
2±
0.1
22.0
0.8
7±
0.1
11.4
22064498-4
217208
L4γ
L4γa
1.1
1±
0.0
90.2
1.9
5±
0.0
90.8
2.7
3±
0.0
71.0
3.1
8±
0.0
71.1
0.8
4±
0.0
81.2
22495345+
0044046
L4γ
L3β
1.1
7±
0.1
70.6
2.2
3±
0.1
41.9
3.0
1±
0.1
31.8
3.4
4±
0.1
31.8
1.0
6±
0.1
32.8
23433470-3
646021
––
L3-L
6γ
1.5
6±
0.1
42.9
2.3
7±
0.1
42.5
3.4
5±
0.1
33.1
3.9
6±
0.1
33.0
0.8
2±
0.0
91.0
00303013-1
450333
L7–
L4-L
6β
1.0
1±
0.1
5-0
.61.8
0±
0.1
50.2
2.6
2±
0.1
10.6
3.0
2±
0.1
20.6
0.7
9±
0.1
41.2
03264225-2
102057
L5β
L5βγa
1.3
4±
0.1
21.8
2.2
1±
0.1
12.1
3.1
8±
0.1
02.8
3.7
0±
0.1
02.9
0.8
7±
0.1
01.9
03552337+
1133437
L5γ
L3-L
6γ
1.5
2±
0.0
43.1
2.5
2±
0.0
33.5
3.5
2±
0.0
34.2
4.1
1±
0.0
34.3
1.0
0±
0.0
33.1
04210718-6
306022
L5β
L5γ
1.2
8±
0.0
61.4
2.1
2±
0.0
61.7
3.0
1±
0.0
52.1
3.4
3±
0.0
52.0
0.8
3±
0.0
61.6
05120636-2
949540
L5γ
L5β
1.3
1±
0.0
71.5
2.1
7±
0.0
71.9
3.0
9±
0.0
62.4
3.5
4±
0.0
62.4
0.8
7±
0.0
61.9
20025073-0
521524
L5β
L5-L
7γ
1.0
4±
0.0
7-0
.41.9
0±
0.0
60.7
2.7
8±
0.0
51.2
3.2
3±
0.0
61.3
0.8
6±
0.0
61.8
00470038+
6803543
L7(γ
?)
L6-L
8γ
1.6
4±
0.0
84.4
2.5
5±
0.0
74.6
3.7
3±
0.0
74.6
4.3
4±
0.0
74.4
0.9
1±
0.0
52.4
01033203+
1935361
L6β
L6β
1.3
9±
0.1
01.4
2.1
4±
0.1
01.1
3.1
1±
0.0
81.3
3.5
9±
0.0
81.1
0.7
5±
0.0
8-0
.108095903+
4434216
––
L6p
1.2
5±
0.1
50.7
2.0
2±
0.1
30.6
3.0
9±
0.1
21.2
3.6
3±
0.1
21.2
0.7
7±
0.1
10.0
08575849+
5708514
L8–
L8—
1.2
5±
0.0
61.2
2.0
8±
0.0
51.9
3.0
2±
0.0
42.3
3.6
2±
0.0
42.1
0.8
3±
0.0
51.8
11193254-1
137466
—L
7γ
1.6
7±
0.0
74.7
2.7
1±
0.0
65.6
3.9
1±
0.0
65.3
4.5
8±
0.0
65.2
1.0
4±
0.0
43.7
114724.1
0-2
04021.3
––
L7γ
1.8
7±
0.1
36.4
2.7
7±
0.0
66.0
3.9
2±
0.0
65.3
4.5
5±
0.0
75.1
0.8
9±
0.1
12.1
17410280-4
642218
––
L6-L
8γ
1.2
5±
0.0
91.2
2.3
5±
0.0
83.4
3.4
9±
0.0
83.6
4.1
1±
0.0
83.7
1.1
0±
0.0
64.4
PSO
318
––
L6-L
8γ
1.6
6±
0.0
94.6
2.8
5±
0.0
96.5
4.0
7±
0.0
85.9
4.8
2±
0.0
96.0
1.1
9±
0.0
65.4
22443167+
2043433
L6.5
p–
L6-L
8γa
1.4
8±
0.1
51.8
2.4
5±
0.1
62.2
3.7
0±
0.1
42.7
4.3
7±
0.1
42.6
0.9
8±
0.1
01.4
aV
alu
es
are
the
#ofσ
(as
rep
ort
ed
inT
able
15)
from
the
field
sequence
that
each
ob
ject
diff
ers
.A
negati
ve
(-)
num
ber
indic
ate
sth
at
the
colo
rw
as
blu
ew
ard
of
the
field
sequence
avera
ge
where
as
ap
osi
tive
(+)
num
ber
indic
ate
sth
at
the
colo
rw
as
redw
ard
of
the
field
sequence
avera
ge.
78 Faherty et al.Table
18
Infr
are
dC
olo
rsof
low
gra
vit
yla
te-t
yp
eM
and
Ldw
arf
s
Nam
eSpT
SpT
(H-W
1)
#ofσ(H−W
1)a
(H-W
2)
#ofσ(H−W
2)a
(K-W
1)
#ofσ(K−W
1)a
(K-W
2)
#ofσ(K−W
2)a
(W1-W
2)
#ofσ(W
1−W
2)a
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
01231125-6
921379
M7.5γ
––
0.6
5±
0.0
31.1
0.8
9±
0.0
31.3
0.2
6±
0.0
30.7
0.5
1±
0.0
31.0
0.2
4±
0.0
30.5
01294256-0
823580
M5–
M7β
0.5
4±
0.0
3-0
.10.7
6±
0.0
30.0
0.2
3±
0.0
30.3
0.4
4±
0.0
30.3
0.2
2±
0.0
30.1
02501167-0
151295
––
M7β
0.5
9±
0.0
30.4
0.8
3±
0.0
30.7
0.2
2±
0.0
30.2
0.4
6±
0.0
30.5
0.2
4±
0.0
30.5
02530084+
1652532
––
M7β
0.5
6±
0.0
50.1
0.8
3±
0.0
40.7
0.2
6±
0.0
50.7
0.5
3±
0.0
51.2
0.2
7±
0.0
30.9
02535980+
3206373
M7β
M6β
0.6
1±
0.0
30.6
0.8
0±
0.0
30.4
0.2
3±
0.0
30.3
0.4
2±
0.0
30.1
0.2
0±
0.0
3-0
.203350208+
2342356
M8.5
–M
7.5β
0.6
1±
0.0
30.7
0.8
9±
0.0
31.3
0.2
2±
0.0
30.2
0.4
9±
0.0
20.8
0.2
8±
0.0
31.1
05181131-3
101529
M6.5
–M
7β
0.5
9±
0.0
30.5
0.8
3±
0.0
30.7
0.2
6±
0.0
30.7
0.5
0±
0.0
30.9
0.2
4±
0.0
30.5
05264316-1
824315
––
M7β
0.6
4±
0.0
30.9
0.8
9±
0.0
31.3
0.2
5±
0.0
30.5
0.5
0±
0.0
30.9
0.2
6±
0.0
30.8
05575096-1
359503
M7–
M7γ
0.8
1±
0.0
32.9
1.3
4±
0.0
35.8
0.4
0±
0.0
32.2
0.9
3±
0.0
35.2
0.5
3±
0.0
35.4
07140394+
3702459
M8–
M7.5β
0.6
9±
0.0
41.5
0.9
1±
0.0
31.5
0.2
7±
0.0
30.8
0.4
9±
0.0
30.8
0.2
2±
0.0
30.2
20391314-1
126531
M8–
M7β
0.6
6±
0.0
41.3
0.9
6±
0.0
42.0
0.2
2±
0.0
40.2
0.5
1±
0.0
41.0
0.3
0±
0.0
31.5
00192626+
4614078
M8
–M
8β
0.6
8±
0.0
30.6
0.9
4±
0.0
30.8
0.2
4±
0.0
30.2
0.5
0±
0.0
20.6
0.2
6±
0.0
30.7
02212859-6
831400
M8β
––
0.8
0±
0.0
41.8
1.0
8±
0.0
42.0
0.3
3±
0.0
41.3
0.6
1±
0.0
41.6
0.2
8±
0.0
31.0
03550477-1
032415
M8.5
–M
8.5β
0.7
5±
0.0
31.3
1.0
4±
0.0
31.6
0.2
6±
0.0
30.5
0.5
5±
0.0
31.0
0.2
9±
0.0
31.1
04351455-1
414468
M8γ
M7γ
0.9
1±
0.0
42.9
1.3
5±
0.0
34.3
0.2
4±
0.0
30.2
0.6
8±
0.0
32.2
0.4
4±
0.0
33.7
04362788-4
114465
M8β
M9γ
0.6
9±
0.0
30.7
0.9
7±
0.0
31.1
0.3
1±
0.0
31.0
0.5
9±
0.0
31.4
0.2
8±
0.0
31.0
05341594-0
631397
M8γ
M8γ
0.5
8±
0.1
0-0
.41.1
1±
0.1
12.3
0.1
5±
0.1
0-0
.70.6
8±
0.1
12.2
0.5
3±
0.0
75.2
06085283-2
753583
M8.5γ
L0γ
0.9
2±
0.0
33.0
1.2
7±
0.0
33.6
0.3
9±
0.0
31.9
0.7
5±
0.0
32.8
0.3
5±
0.0
32.2
06524851-5
741376
M8β
––
0.8
1±
0.0
31.9
1.1
1±
0.0
32.2
0.3
0±
0.0
30.9
0.5
9±
0.0
31.4
0.3
0±
0.0
31.3
08561384-1
342242
––
M8γ
0.8
2±
0.0
42.0
1.3
6±
0.0
44.3
0.3
4±
0.0
31.3
0.8
7±
0.0
33.9
0.5
3±
0.0
35.2
TW
A28
M8.5γ
M9γ
0.9
2±
0.0
33.0
1.5
6±
0.0
36.0
0.4
6±
0.0
32.6
1.1
0±
0.0
36.0
0.6
4±
0.0
37.0
TW
A27A
M8γ
M8γ
0.8
3±
0.0
42.1
1.3
8±
0.0
44.5
0.3
9±
0.0
41.9
0.9
4±
0.0
44.6
0.5
5±
0.0
35.4
12271545-0
636458
M9–
M8.5β
0.8
7±
0.0
42.5
1.1
3±
0.0
42.4
0.3
7±
0.0
51.6
0.6
3±
0.0
41.7
0.2
6±
0.0
40.6
15291017+
6312539
––
M8β
0.6
5±
0.0
40.3
0.8
8±
0.0
40.3
0.2
6±
0.0
30.5
0.5
0±
0.0
30.5
0.2
3±
0.0
30.2
20282203-5
637024
––
M8.5γ
0.7
7±
0.0
31.5
1.0
7±
0.0
41.9
0.2
4±
0.0
30.2
0.5
4±
0.0
40.9
0.3
0±
0.0
31.3
22353560-5
906306
––
M8.5β
0.9
0±
0.0
42.8
1.2
3±
0.0
53.2
0.4
8±
0.0
42.9
0.8
1±
0.0
43.3
0.3
3±
0.0
41.8
23231347-0
244360
M8.5
–M
8β
0.6
9±
0.0
40.7
0.9
7±
0.0
41.1
0.2
4±
0.0
40.3
0.5
3±
0.0
40.8
0.2
8±
0.0
31.0
23520507-1
100435
M7–
M8β
0.7
3±
0.0
31.1
1.0
2±
0.0
31.5
0.3
0±
0.0
30.9
0.6
0±
0.0
31.4
0.2
9±
0.0
31.2
00274197+
0503417
M9.5β
L0β
0.6
7±
0.1
1-0
.51.1
5±
0.1
11.3
0.3
4±
0.1
20.8
0.8
3±
0.1
32.3
0.4
8±
0.0
64.1
00381489-6
403529
––
M9.5β
0.9
6±
0.0
52.2
1.3
3±
0.0
52.5
0.4
9±
0.0
42.3
0.8
6±
0.0
42.5
0.3
7±
0.0
32.1
00425923+
1142104
––
M9β
0.8
4±
0.0
51.1
1.1
6±
0.0
51.3
0.2
8±
0.0
40.2
0.6
0±
0.0
40.6
0.3
2±
0.0
41.3
00464841+
0715177
M9β
L0δ
1.1
1±
0.0
43.5
1.5
4±
0.0
43.9
0.4
8±
0.0
42.2
0.9
1±
0.0
32.9
0.4
3±
0.0
33.2
02215494-5
412054
M9β
––
0.9
0±
0.0
41.6
1.2
6±
0.0
42.0
0.3
5±
0.0
40.9
0.7
1±
0.0
41.4
0.3
6±
0.0
32.0
02251947-5
837295
M9β
M9γ
0.8
2±
0.0
30.9
1.1
3±
0.0
31.1
0.3
3±
0.0
40.7
0.6
3±
0.0
30.9
0.3
1±
0.0
31.1
03393521-3
525440
M9β
L0β
0.8
8±
0.0
31.5
1.2
1±
0.0
31.7
0.4
2±
0.0
31.6
0.7
4±
0.0
31.7
0.3
2±
0.0
31.4
04433761+
0002051
M9γ
M9γ
0.9
8±
0.0
32.3
1.3
3±
0.0
32.5
0.3
9±
0.0
31.3
0.7
4±
0.0
31.7
0.3
5±
0.0
31.8
04493288+
1607226
––
M9γ
0.7
6±
0.0
40.4
1.0
7±
0.0
40.7
0.3
5±
0.0
40.9
0.6
5±
0.0
41.0
0.3
1±
0.0
41.1
05402325-0
906326
––
M9β
0.8
2±
0.0
40.9
1.1
1±
0.0
41.0
0.3
0±
0.0
50.4
0.5
9±
0.0
50.5
0.2
9±
0.0
40.8
09451445-7
753150
––
M9β
0.7
2±
0.0
40.0
0.9
5±
0.0
40.0
0.2
8±
0.0
40.2
0.5
1±
0.0
40.0
0.2
3±
0.0
3-0
.109532126-1
014205
M9γ
M9β
0.8
9±
0.0
31.5
1.2
4±
0.0
31.9
0.3
8±
0.0
31.2
0.7
4±
0.0
31.6
0.3
5±
0.0
31.9
10220489+
0200477
M9β
M9β
0.7
9±
0.0
40.6
1.0
6±
0.0
40.7
0.2
9±
0.0
40.3
0.5
6±
0.0
40.4
0.2
7±
0.0
40.5
11064461-3
715115
––
M9γ
0.7
7±
0.0
40.5
1.0
9±
0.0
40.9
0.2
7±
0.0
50.1
0.5
9±
0.0
50.5
0.3
2±
0.0
41.3
TW
A26
M9γ
M9γ
0.8
4±
0.0
31.1
1.2
0±
0.0
31.6
0.3
5±
0.0
30.9
0.7
1±
0.0
31.4
0.3
6±
0.0
32.0
TW
A29
M9.5γ
L0γ
0.8
1±
0.0
40.8
1.1
8±
0.0
41.4
0.3
8±
0.0
41.2
0.7
5±
0.0
41.7
0.3
7±
0.0
32.2
12474428-3
816464
––
M9γ
0.9
9±
0.0
42.4
1.5
7±
0.0
44.1
0.4
7±
0.0
52.1
1.0
5±
0.0
53.9
0.5
9±
0.0
35.8
12535039-4
211215
––
M9.5γ
1.0
2±
0.1
12.7
1.3
8±
0.1
12.8
0.4
6±
0.1
12.0
0.8
2±
0.1
12.2
0.3
6±
0.0
52.0
14112131-2
119503
M9β
M8β
0.7
5±
0.0
30.3
1.0
1±
0.0
30.3
0.2
5±
0.0
3-0
.10.5
2±
0.0
30.0
0.2
6±
0.0
30.4
15104786-2
818174
M9–
M9β
0.8
0±
0.0
40.7
1.1
0±
0.0
40.9
0.3
7±
0.0
41.1
0.6
7±
0.0
41.2
0.3
0±
0.0
31.0
15470557-1
626303A
––
M9β
0.8
1±
0.0
40.8
1.1
0±
0.0
40.9
0.3
0±
0.0
40.4
0.5
9±
0.0
40.6
0.2
9±
0.0
40.9
15474719-2
423493
M9γ
L0β
0.8
6±
0.0
41.3
1.1
7±
0.0
51.4
0.3
3±
0.0
30.7
0.6
4±
0.0
40.9
0.3
0±
0.0
41.0
15575011-2
952431
M9δ
L1γ
1.0
2±
0.1
12.7
1.3
8±
0.1
22.8
0.4
1±
0.1
21.5
0.7
8±
0.1
32.0
0.3
7±
0.0
72.2
19355595-2
846343
M9γ
M9γ
0.8
3±
0.0
31.0
1.2
7±
0.0
32.1
0.3
6±
0.0
41.0
0.8
0±
0.0
42.1
0.4
4±
0.0
43.3
20004841-7
523070
M9γ
M9γa
0.8
6±
0.0
31.3
1.1
7±
0.0
31.4
0.4
0±
0.0
31.4
0.7
1±
0.0
31.4
0.3
1±
0.0
31.2
20135152-2
806020
M9γ
L0γ
0.9
4±
0.0
42.0
1.3
0±
0.0
42.3
0.4
1±
0.0
41.5
0.7
8±
0.0
41.9
0.3
6±
0.0
42.0
21544859-7
459134
––
M9.5β
0.8
6±
0.0
51.3
1.1
9±
0.0
51.5
0.3
8±
0.0
41.2
0.7
1±
0.0
41.4
0.3
3±
0.0
41.5
21572060+
8340575
L0–
M9γ
0.9
8±
0.0
42.3
1.3
9±
0.0
42.8
0.5
0±
0.0
32.4
0.9
0±
0.0
32.8
0.4
1±
0.0
32.8
22025794-5
605087
––
M9γ
0.8
1±
0.0
40.8
1.0
6±
0.0
40.7
0.3
5±
0.0
40.9
0.6
1±
0.0
40.7
0.2
5±
0.0
40.2
Brown Dwarf Analogs to Exoplanets 79Table
18
—Continued
Nam
eSpT
SpT
(H-W
1)
#ofσ(H−W
1)a
(H-W
2)
#ofσ(H−W
2)a
(K-W
1)
#ofσ(K−W
1)a
(K-W
2)
#ofσ(K−W
2)a
(W1-W
2)
#ofσ(W
1−W
2)a
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
23360735-3
541489
––
M9β
0.8
1±
0.0
30.8
1.1
6±
0.0
41.3
0.3
8±
0.0
51.2
0.7
4±
0.0
51.6
0.3
6±
0.0
41.9
23453903+
0055137
M9–
M9β
0.9
1±
0.0
41.7
1.2
4±
0.0
31.9
0.3
7±
0.0
41.1
0.7
0±
0.0
41.4
0.3
3±
0.0
31.6
00182834-6
703130
––
L0γ
1.3
1±
0.0
73.8
1.7
1±
0.0
73.7
0.5
4±
0.0
51.7
0.9
4±
0.0
52.6
0.4
0±
0.0
41.7
00325584-4
405058
L0γ
L0β
1.0
4±
0.0
41.7
1.3
7±
0.0
41.7
0.4
5±
0.0
40.9
0.7
8±
0.0
41.3
0.3
3±
0.0
40.8
00374306-5
846229
L0γ
––
1.1
3±
0.0
62.5
1.5
2±
0.0
62.6
0.4
7±
0.0
51.0
0.8
5±
0.0
51.9
0.3
9±
0.0
41.5
01244599-5
745379
L0γ
L0γ
1.2
9±
0.0
93.7
1.7
2±
0.0
93.7
0.5
5±
0.0
91.7
0.9
8±
0.0
92.8
0.4
3±
0.0
42.0
01415823-4
633574
L0γ
L0γ
1.3
2±
0.0
34.0
1.7
1±
0.0
33.7
0.5
5±
0.0
41.7
0.9
3±
0.0
42.5
0.3
8±
0.0
31.4
02103857-3
015313
L0γ
L0γa
1.1
6±
0.0
52.7
1.5
1±
0.0
52.5
0.5
0±
0.0
51.3
0.8
5±
0.0
51.8
0.3
5±
0.0
41.0
02235464-5
815067
L0γ
––
1.1
8±
0.0
42.9
1.5
7±
0.0
42.9
0.6
0±
0.0
52.2
0.9
9±
0.0
52.9
0.3
9±
0.0
31.5
02265658-5
327032
––
L0δ
1.1
3±
0.0
62.4
1.5
6±
0.0
62.8
0.5
3±
0.0
51.6
0.9
7±
0.0
52.8
0.4
4±
0.0
42.1
02292794-0
053282
––
L0γ
1.0
3±
0.1
01.7
1.4
2±
0.1
12.0
0.4
6±
0.1
41.0
0.8
5±
0.1
51.9
0.3
9±
0.0
61.5
02340093-6
442068
L0γ
L0βγ
1.2
0±
0.0
63.0
1.5
4±
0.0
62.7
0.6
0±
0.0
72.2
0.9
5±
0.0
72.6
0.3
4±
0.0
40.9
02411151-0
326587
L0γ
L1γ
1.1
7±
0.0
62.8
1.5
6±
0.0
62.8
0.4
0±
0.0
60.5
0.7
8±
0.0
61.3
0.3
8±
0.0
41.4
03231002-4
631237
L0γ
L0γa
1.2
5±
0.0
73.4
1.6
6±
0.0
73.4
0.6
3±
0.0
62.4
1.0
4±
0.0
63.3
0.4
1±
0.0
31.8
03420931-2
904317
––
L0β
1.3
8±
0.1
14.4
1.8
1±
0.1
14.3
0.4
1±
0.0
90.6
0.8
4±
0.0
91.8
0.4
3±
0.0
42.0
03572695-4
417305
L0β
L0β
1.0
6±
0.0
31.9
1.4
5±
0.0
32.1
0.4
4±
0.0
30.8
0.8
2±
0.0
31.6
0.3
9±
0.0
31.5
04062677-3
812102
L0γ
L1γ
1.2
6±
0.1
13.5
1.6
1±
0.1
13.1
0.6
6±
0.1
22.7
1.0
1±
0.1
23.1
0.3
5±
0.0
51.0
04400972-5
126544
––
L0γ
1.1
9±
0.0
63.0
1.5
9±
0.0
63.0
0.5
9±
0.0
62.0
0.9
8±
0.0
72.8
0.3
9±
0.0
41.5
06272161-5
308428
––
L0βγ
1.3
5±
0.0
94.2
1.7
3±
0.1
03.8
0.8
1±
0.0
93.9
1.1
9±
0.0
94.4
0.3
8±
0.0
41.4
11271382-3
735076
––
L0δ
1.1
1±
0.1
12.3
1.4
7±
0.1
22.3
0.7
7±
0.1
63.6
1.1
3±
0.1
64.0
0.3
6±
0.0
61.1
11544223-3
400390
L0β
L1β
0.9
8±
0.0
41.3
1.2
9±
0.0
41.3
0.5
0±
0.0
41.3
0.8
1±
0.0
41.6
0.3
1±
0.0
30.5
12074836-3
900043
L0γ
L1γ
0.9
7±
0.0
61.3
1.3
9±
0.0
61.8
0.4
1±
0.0
70.5
0.8
2±
0.0
71.7
0.4
2±
0.0
41.9
15525906+
2948485
L0β
L0β
1.0
6±
0.0
31.9
1.4
0±
0.0
31.9
0.4
8±
0.0
31.1
0.8
1±
0.0
31.6
0.3
4±
0.0
30.8
17111353+
2326333
L0γ
L1β
1.0
9±
0.0
42.1
1.4
4±
0.0
42.1
0.4
8±
0.0
41.2
0.8
3±
0.0
41.7
0.3
5±
0.0
31.1
19564700-7
542270
L0γ
L2γ
1.3
4±
0.1
04.1
1.7
9±
0.1
04.2
0.5
4±
0.0
71.6
0.9
8±
0.0
72.9
0.4
4±
0.0
42.2
20334473-5
635338
––
L0γ
1.3
2±
0.1
13.9
1.7
2±
0.1
13.8
0.4
3±
0.0
90.7
0.8
3±
0.0
91.7
0.4
0±
0.0
41.7
22134491-2
136079
L0γ
L0γ
1.1
8±
0.0
62.8
1.5
7±
0.0
62.9
0.5
3±
0.0
51.6
0.9
3±
0.0
52.4
0.4
0±
0.0
41.6
23153135+
0617146
L0γ
L0γ
1.2
1±
0.0
73.0
1.6
6±
0.0
83.4
0.5
2±
0.0
71.5
0.9
8±
0.0
72.8
0.4
6±
0.0
42.3
23224684-3
133231
L0β
L2β
0.8
2±
0.0
30.0
1.0
8±
0.0
30.0
0.3
5±
0.0
30.1
0.6
2±
0.0
30.1
0.2
7±
0.0
30.0
00040288-6
410358
L1γ
L1γa
1.4
6±
0.0
83.7
1.8
9±
0.0
84.0
0.6
4±
0.0
52.5
1.0
7±
0.0
53.2
0.4
3±
0.0
42.9
00191296-6
226005
––
L1γ
1.2
7±
0.0
62.4
1.7
4±
0.0
63.1
0.6
1±
0.0
62.1
1.0
7±
0.0
63.2
0.4
7±
0.0
43.5
00344300-4
102266
––
L1β
1.3
1±
0.0
72.7
1.7
1±
0.0
73.0
0.5
9±
0.0
62.0
0.9
9±
0.0
62.5
0.4
0±
0.0
42.3
00584253-0
651239
L0–
L1β
0.8
8±
0.0
4-0
.21.2
0±
0.0
40.1
0.3
4±
0.0
4-0
.30.6
6±
0.0
40.2
0.3
1±
0.0
40.9
01174748-3
403258
L1β
L1βa
1.1
8±
0.0
51.8
1.5
9±
0.0
52.3
0.4
6±
0.0
40.8
0.8
7±
0.0
41.7
0.4
1±
0.0
42.4
01205114-5
200349
––
L1γ
1.4
3±
0.0
83.5
1.8
8±
0.0
84.0
0.5
2±
0.0
61.4
0.9
7±
0.0
62.5
0.4
5±
0.0
43.2
02410564-5
511466
––
L1γ
1.1
4±
0.0
61.5
1.5
2±
0.0
61.9
0.5
5±
0.0
41.7
0.9
3±
0.0
52.1
0.3
8±
0.0
31.9
03164512-2
848521
L0–
L1β
1.1
2±
0.0
41.4
1.4
6±
0.0
41.6
0.4
7±
0.0
40.9
0.8
0±
0.0
41.2
0.3
4±
0.0
31.3
05184616-2
756457
L1γ
L1γ
1.2
5±
0.0
52.3
1.6
3±
0.0
52.6
0.5
7±
0.0
51.9
0.9
6±
0.0
52.4
0.3
8±
0.0
42.1
06023045+
3910592
L1–
L1β
1.0
2±
0.0
30.7
1.3
3±
0.0
30.9
0.4
3±
0.0
30.5
0.7
4±
0.0
30.8
0.3
1±
0.0
30.8
07123786-6
155528
L1β
L1γ
1.4
0±
0.0
53.3
1.7
7±
0.0
53.3
0.6
8±
0.0
52.8
1.0
4±
0.0
53.0
0.3
7±
0.0
31.8
10224821+
5825453
L1β
L1β
0.8
8±
0.0
4-0
.21.1
5±
0.0
4-0
.10.4
0±
0.0
30.3
0.6
6±
0.0
30.2
0.2
7±
0.0
30.1
11083081+
6830169
L1γ
L1γ
1.1
3±
0.0
31.5
1.4
8±
0.0
31.7
0.4
8±
0.0
31.0
0.8
3±
0.0
31.4
0.3
5±
0.0
31.5
11480096-2
836488
––
L1β
1.0
5±
0.0
90.9
1.4
1±
0.0
91.3
0.4
2±
0.0
90.5
0.7
9±
0.0
91.1
0.3
7±
0.0
51.8
19350976-6
200473
––
L1γ
1.2
3±
0.1
02.2
1.6
4±
0.1
02.6
0.6
7±
0.1
02.7
1.0
7±
0.1
13.2
0.4
1±
0.0
52.5
22351658-3
844154
––
L1.5γ
1.2
7±
0.0
52.4
1.6
3±
0.0
52.5
0.6
2±
0.0
52.3
0.9
8±
0.0
52.5
0.3
6±
0.0
41.7
23255604-0
259508
L3–
L1γ
1.2
4±
0.0
72.2
1.5
9±
0.0
82.3
0.4
2±
0.0
60.5
0.7
7±
0.0
71.0
0.3
5±
0.0
41.4
00452143+
1634446
L2β
L2γ
1.2
9±
0.0
41.4
1.6
7±
0.0
41.5
0.6
0±
0.0
31.3
0.9
8±
0.0
31.5
0.3
8±
0.0
31.2
00550564+
0134365
L2γ
L2γ
1.5
9±
0.0
83.2
2.0
7±
0.0
83.3
0.7
6±
0.0
72.6
1.2
4±
0.0
83.1
0.4
8±
0.0
42.7
03032042-7
312300
L2γ
––
1.3
2±
0.0
91.6
1.7
5±
0.0
91.8
0.5
4±
0.0
90.8
0.9
7±
0.0
91.4
0.4
3±
0.0
42.0
05104958-1
843548
––
L2β
1.0
9±
0.0
60.2
1.4
0±
0.0
60.3
0.5
6±
0.0
60.9
0.8
7±
0.0
60.8
0.3
2±
0.0
40.4
05361998-1
920396
L2γ
L2γ
1.4
3±
0.0
72.2
1.9
0±
0.0
82.6
0.5
9±
0.0
71.1
1.0
6±
0.0
72.0
0.4
7±
0.0
42.6
20575409-0
252302
L1.5
–L
2β
1.0
1±
0.0
3-0
.31.2
9±
0.0
3-0
.20.4
6±
0.0
30.1
0.7
4±
0.0
30.0
0.2
8±
0.0
3-0
.123225299-6
151275
L2γ
L3γa
1.2
9±
0.0
71.4
1.6
9±
0.0
71.6
0.6
2±
0.0
51.4
1.0
2±
0.0
51.7
0.4
0±
0.0
41.6
01531463-6
744181
L2
–L
3β
1.4
0±
0.0
91.2
1.8
9±
0.0
91.8
0.7
1±
0.1
11.4
1.2
1±
0.1
12.2
0.5
0±
0.0
43.1
02583123-1
520536
––
L3β
1.2
4±
0.0
70.4
1.6
7±
0.0
70.8
0.5
7±
0.0
60.4
1.0
0±
0.0
61.0
0.4
3±
0.0
42.0
04185879-4
507413
––
L3γ
1.1
8±
0.0
80.1
1.5
9±
0.0
80.5
0.7
3±
0.0
91.6
1.1
4±
0.0
91.8
0.4
1±
0.0
41.7
06322402-5
010349
L3β
L4γ
1.4
2±
0.0
41.3
1.8
6±
0.0
41.6
0.7
3±
0.0
41.6
1.1
7±
0.0
41.9
0.4
4±
0.0
32.2
09593276+
4523309
––
L3γ
1.9
0±
0.0
73.7
2.4
0±
0.0
73.9
0.8
1±
0.0
52.2
1.3
1±
0.0
52.7
0.5
0±
0.0
43.1
80 Faherty et al.Table
18
—Continued
Nam
eSpT
SpT
(H-W
1)
#ofσ(H−W
1)a
(H-W
2)
#ofσ(H−W
2)a
(K-W
1)
#ofσ(K−W
1)a
(K-W
2)
#ofσ(K−W
2)a
(W1-W
2)
#ofσ(W
1−W
2)a
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
G196-3
BL
3β
L3γ
1.9
5±
0.0
53.9
2.5
1±
0.0
54.4
1.0
8±
0.0
44.1
1.6
4±
0.0
44.6
0.5
7±
0.0
34.3
17260007+
1538190
L3.5γ
L3γ
1.3
9±
0.0
51.2
1.7
7±
0.0
51.3
0.5
9±
0.0
60.6
0.9
7±
0.0
60.8
0.3
8±
0.0
41.1
20113196-5
048112
––
L3γ
1.2
5±
0.0
90.4
1.5
9±
0.0
90.5
0.5
7±
0.0
90.4
0.9
1±
0.0
90.5
0.3
4±
0.0
50.5
21265040-8
140293
L3γ
L3γ
1.5
0±
0.0
61.7
1.9
3±
0.0
61.9
0.6
4±
0.0
50.9
1.0
8±
0.0
51.4
0.4
4±
0.0
32.1
22081363+
2921215
L3γ
L3γ
1.4
4±
0.0
81.4
1.9
1±
0.0
81.8
0.8
0±
0.0
82.0
1.2
6±
0.0
82.5
0.4
7±
0.0
42.6
00011217+
1535355
––
L4β
1.5
7±
0.0
60.9
1.9
9±
0.0
61.1
0.7
7±
0.0
50.7
1.1
9±
0.0
51.0
0.4
2±
0.0
31.2
003323.8
6-1
521309
L4β
L1
1.4
1±
0.0
60.3
1.7
3±
0.0
60.2
0.6
1±
0.0
5-0
.50.9
3±
0.0
5-0
.40.3
2±
0.0
4-0
.301262109+
1428057
L4γ
L2γ
1.9
4±
0.2
22.5
2.4
7±
0.2
22.8
1.0
4±
0.1
52.6
1.5
8±
0.1
53.2
0.5
4±
0.0
52.8
03421621-6
817321
L4γ
––
1.4
3±
0.0
90.4
1.9
0±
0.0
90.8
0.5
9±
0.0
9-0
.71.0
6±
0.0
90.3
0.4
7±
0.0
41.9
05012406-0
010452
L4γ
L3γ
1.6
6±
0.0
41.3
2.2
0±
0.0
41.8
0.9
1±
0.0
41.6
1.4
4±
0.0
42.4
0.5
3±
0.0
32.7
10212570-2
830427
––
L4βγ
1.6
9±
0.1
21.5
2.1
7±
0.1
21.7
0.8
2±
0.1
31.0
1.3
0±
0.1
31.6
0.4
8±
0.0
52.0
12563961-2
718455
––
L4β
1.2
9±
0.1
2-0
.21.6
8±
0.1
30.0
0.6
2±
0.1
0-0
.41.0
1±
0.1
00.0
0.3
9±
0.0
40.8
14252798-3
650229
L3–
L4γ
1.5
8±
0.0
31.0
2.0
0±
0.0
31.1
0.8
1±
0.0
30.9
1.2
3±
0.0
31.2
0.4
2±
0.0
31.2
15382417-1
953116
L4γ
L4γ
1.6
8±
0.0
71.4
2.1
3±
0.0
71.6
0.8
3±
0.0
61.1
1.2
8±
0.0
61.5
0.4
5±
0.0
41.6
15515237+
0941148
L4γ
>L
5γ
1.5
1±
0.0
80.7
1.9
9±
0.0
81.1
0.7
1±
0.0
60.2
1.1
9±
0.0
61.0
0.4
8±
0.0
42.0
16154255+
4953211
L4γ
L3-L
6γ
2.1
3±
0.1
03.3
2.7
1±
0.1
03.6
1.1
1±
0.0
73.1
1.6
9±
0.0
73.8
0.5
8±
0.0
33.4
18212815+
1414010
L4.5
—L
4p
ec
1.5
4±
0.0
30.8
1.9
2±
0.0
30.9
0.8
0±
0.0
30.8
1.1
8±
0.0
30.9
0.3
8±
0.0
30.5
21324036+
1029494
––
L4β
1.3
4±
0.1
20.0
1.7
9±
0.1
20.4
0.6
0±
0.1
1-0
.51.0
6±
0.1
10.3
0.4
5±
0.0
51.6
21543454-1
055308
L4β
L5γ
1.7
0±
0.0
91.5
2.1
5±
0.0
91.7
0.8
3±
0.0
71.1
1.2
8±
0.0
71.5
0.4
5±
0.0
41.6
22064498-4
217208
L4γ
L4γa
1.6
2±
0.0
71.2
2.0
7±
0.0
71.4
0.7
9±
0.0
60.8
1.2
3±
0.0
61.2
0.4
5±
0.0
31.5
22495345+
0044046
L4γ
L3β
1.8
5±
0.1
12.1
2.2
8±
0.1
22.1
0.7
8±
0.0
80.7
1.2
2±
0.0
91.1
0.4
3±
0.0
61.3
23433470-3
646021
––
L3-L
6γ
1.8
9±
0.0
72.3
2.4
0±
0.0
72.5
1.0
7±
0.0
72.8
1.5
8±
0.0
73.2
0.5
1±
0.0
42.4
00303013-1
450333
L7–
L4-L
6β
1.6
2±
0.1
01.5
2.0
1±
0.1
11.4
0.8
2±
0.1
00.7
1.2
2±
0.1
10.8
0.3
9±
0.0
40.6
03264225-2
102057
L5β
L5βγa
1.8
4±
0.0
83.0
2.3
6±
0.0
83.1
0.9
7±
0.0
71.9
1.4
9±
0.0
72.3
0.5
1±
0.0
32.1
03552337+
1133437
L5γ
L3-L
6γ
2.0
0±
0.0
44.1
2.5
9±
0.0
44.2
1.0
0±
0.0
32.2
1.5
9±
0.0
32.8
0.5
9±
0.0
32.9
04210718-6
306022
L5β
L5γ
1.7
3±
0.0
52.2
2.1
5±
0.0
52.0
0.8
9±
0.0
51.3
1.3
2±
0.0
51.3
0.4
2±
0.0
30.9
05120636-2
949540
L5γ
L5β
1.7
8±
0.0
52.6
2.2
4±
0.0
52.5
0.9
1±
0.0
51.4
1.3
7±
0.0
51.6
0.4
6±
0.0
31.3
20025073-0
521524
L5β
L5-L
7γ
1.7
5±
0.0
62.4
2.1
9±
0.0
62.2
0.8
9±
0.0
41.2
1.3
3±
0.0
41.4
0.4
4±
0.0
31.2
00470038+
6803543
L7(γ
?)
L6-L
8γ
2.0
9±
0.0
53.4
2.7
0±
0.0
53.3
1.1
8±
0.0
43.0
1.7
9±
0.0
43.0
0.6
1±
0.0
31.8
01033203+
1935361
L6β
L6β
1.7
2±
0.0
60.8
2.2
0±
0.0
60.7
0.9
7±
0.0
61.0
1.4
5±
0.0
61.0
0.4
8±
0.0
40.6
08095903+
4434216
––
L6p
1.8
4±
0.1
01.2
2.3
7±
0.1
01.2
1.0
7±
0.0
61.5
1.6
1±
0.0
61.6
0.5
3±
0.0
41.0
08575849+
5708514
L8–
L8—
1.7
7±
0.0
51.9
2.3
8±
0.0
51.8
0.9
4±
0.0
41.3
1.5
5±
0.0
41.3
0.6
0±
0.0
30.4
11193254-1
137466
—L
7γ
2.2
4±
0.0
44.2
2.9
1±
0.0
44.1
1.2
0±
0.0
33.2
1.8
7±
0.0
33.4
0.6
7±
0.0
42.4
114724.1
0-2
04021.3
––
L7γ
2.0
5±
0.1
13.1
2.6
7±
0.1
23.2
1.1
5±
0.0
32.8
1.7
8±
0.0
33.0
0.6
3±
0.0
42.0
17410280-4
642218
––
L6-L
8γ
2.2
3±
0.0
64.1
2.8
6±
0.0
64.0
1.1
4±
0.0
42.7
1.7
6±
0.0
42.9
0.6
3±
0.0
32.0
PSO
318
––
L6-L
8γ
2.4
1±
0.0
55.0
3.1
6±
0.0
55.2
1.2
2±
0.0
53.3
1.9
7±
0.0
54.0
0.7
5±
0.0
43.4
22443167+
2043433
L6.5
p–
L6-L
8γa
2.2
2±
0.0
72.4
2.8
9±
0.0
72.6
1.2
5±
0.0
82.4
1.9
1±
0.0
82.8
0.6
7±
0.0
32.2
aV
alu
es
are
the
#ofσ
(as
rep
ort
ed
inT
able
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the
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ject
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ers
.A
negati
ve
(-)
num
ber
indic
ate
sth
at
the
colo
rw
as
blu
ew
ard
of
the
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where
as
ap
osi
tive
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Brown Dwarf Analogs to Exoplanets 81
Table 19Coefficients of Polynomial Fits for M6 -T9 Dwarfs
MFilter x rms c0 c1 c2 c3 c4 c5 c6
MJ FLD 6.0<SpT <29.0 0.402 -8.350e+00 7.157e+00 -1.058e+00 7.771e-02 -2.684e-03 3.478e-05 · · ·MJ YNG 7.0<SpT <17.0 0.647 4.032e-03 -1.416e-01 2.097e+00 8.478e-01 · · · · · · · · ·MJ GRP 7.0<SpT <17.0 0.660 -3.825e-03 1.370e-01 -9.279e-01 10.141e+00 · · · · · · · · ·MH FLD 6.0<SpT <29.0 0.389 -7.496e+00 6.406e+00 -9.174e-01 6.551e-02 -2.217e-03 2.841e-05 · · ·MH YNG 7.0<SpT <17.0 0.634 2.642e-03 -1.049e-01 1.753e+00 1.207e+00 · · · · · · · · ·MH GRP 7.0<SpT <17.0 0.603 -3.909e-03 1.346e-01 -9.347e-01 9.728e+00 · · · · · · · · ·MKs FLD 6.0<SpT <29.0 0.537 -6.704e+00 5.970e+00 -8.481e-01 5.978e-02 -1.997e-03 2.540e-05 · · ·MKs YNG 7.0<SpT <17.0 0.640 -1.585e-02 7.338e-01 4.537e+00 · · · · · · · · · · · ·MKs GRP 7.0<SpT <17.0 0.556 -4.006e-03 1.378e-01 -1.031e+00 9.916e+00 · · · · · · · · ·MW1 FLD 6.0<SpT <29.0 0.365 -1.664e-01 2.991e+00 -3.603e-01 2.258e-02 -6.897e-04 8.337e-06 · · ·MW1 YNG 7.0<SpT <17.0 0.648 -1.397e-02 5.955e-01 5.247e+00 · · · · · · · · · · · ·MW1 GRP 7.0<SpT <17.0 0.551 -4.483e-03 1.505e-01 -1.208e+00 10.403e+00 · · · · · · · · ·MW2 FLD 6.0<SpT <29.0 0.398 -5.043e-01 3.032e+00 -3.655e-01 2.283e-02 -6.938e-04 8.190e-06 · · ·MW2 YNG 7.0<SpT <17.0 0.694 -1.507e-02 5.944e-01 5.061e+00 · · · · · · · · · · · ·MW2 GRP 7.0<SpT <17.0 0.616 -6.821e-03 2.322e-01 -2.133e+00 13.322e+00 · · · · · · · · ·MW3 FLD 6.0<SpT <29.0 0.446 6.462e+00 3.365e-01 1.520e-02 -2.573e-03 9.477e-05 -1.024e-06 · · ·MW3 YNG 7.0<SpT <17.0 0.717 -1.003e-04 -1.670e-03 2.023e-01 7.529e+00 · · · · · · · · ·MW3 GRP 7.0<SpT <17.0 0.427 -5.684e-03 1.993e-01 -1.987e+00 13.972e+00 · · · · · · · · ·Teff FLD 6.0<SpT <29.0 113.431 4.747e+03 -7.005e+02 1.155e+02 -1.191e+01 6.318e-01 -1.606e-02 1.546e-04Teff YNG 7.0<SpT <17.0 180.457 1.330e+00 -66.8637 1235.42 -10068.8 32766.4 · · · · · ·Teff YNG2 7.0<SpT <28.0 197.737 2.795e+04 -9.183e+03 1.360e+03 -1.066e+02 4.578e+00 -1.016e-01 9.106e-04Teff GRP 7.0<SpT <17.0 172.215 7.383e+00 -344.522 4879.86 · · · · · · · · · · · ·Lbol FLD 7.0<SpT <28.0 0.133 2.787e+00 -2.310e+00 3.727e-01 -3.207e-02 1.449e-03 -3.220e-05 2.736e-07Lbol YNG 7.0<SpT <17.0 0.335 -6.514e-03 2.448e-01 -3.113e+00 9.492e+00 · · · · · · · · ·Lbol YNG2 7.0<SpT <28.0 0.206 2.059e-01 9.585 -3.985 4.923e-01 -3.048e-02 9.134e-04 -1.056e-05Lbol GRP 7.0<SpT <17.0 0.221 6.194e-03 -3.757e-01 2.728e-02 · · · · · · · · · · · ·
MLconverteda 7.0<SpT <28.0 -3.46623e-01 3.40366e-02 -3.072e-03
Note. — Relations use 2MASS or WISE magnitudes. Polynomial fits to optical M/L dwarfs and NIR T dwarfs (L dwarfs with no opticalspectral type have NIR spectral types) excluding subdwarfs, low-gravity dwarfs, and binaries for the field (FLD) relations. We present polynomialsinclusive of (1) all γ and β sources under the YNG polynomials as well as (2) only High Likelihood/bonafide moving group members under the
GRP polynomials (see Table 13). The function is defined as MJ,H,Ks,W1,W2,W3,Lbol,Teff=∑ni=0 ci(SpT)i and is valid for varying spectral types
M6-T9 where 6=M6, 10=L0, 20=T0, etc. An FTEST was used to determine the goodness of fit for each polynomial. In the case of all FLDpolynomials, the sample of Filippazzo et al. (2015) is used. In the case of all YNG or GRP polynomials, they are valid from M7 - L7. We list asecond Lbol and Teff for the YNG polynomial (captioned YNG2) that includes planetary mass companions (e.g. HN Peg b, Gu Psc b, Ross 458C,etc) from Filippazzo et al. (2015) and allows us to extend the polynomial from M7-T8.a
Add W1 photometry to SpT polynomial conversion: MLconverted= W1 +∑ni=0 ci(SpT)i
82 Faherty et al.
This publication has made use of the Carnegie As-trometric Program parallax reduction software as wellas the data products from the Two Micron All-SkySurvey, which is a joint project of the University ofMassachusetts and the Infrared Processing and Anal-ysis Center/California Institute of Technology, fundedby the National Aeronautics and Space Administrationand the National Science Foundation. This researchhas alsp made use of the NASA/ IPAC Infrared ScienceArchive, which is operated by the Jet Propulsion Lab-oratory, California Institute of Technology, under con-tract with the National Aeronautics and Space Admin-istration. Furthermore, this publication makes use ofdata products from the Wide-field Infrared Survey Ex-plorer (WISE), which is a joint project of the Univer-sity of California, Los Angeles, and the Jet PropulsionLaboratory/California Institute of Technology, and NE-OWISE, which is a project of the Jet Propulsion Labora-tory/California Institute of Technology. WISE and NE-OWISE are funded by the US National Aeronautics andSpace Administration. Australian access to the Magel-lan Telescopes was supported through the National Col-laborative Research Infrastructure and Collaborative Re-search Infrastructure Strategies of the Australian FederalGovernment. CGT acknowledges the support in this re-search of Australian Research Council grants DP0774000and DP130102695. JRT gratefully acknowledges supportfrom NSF grants AST-0708810 and AST-1008217
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