FURTHER DEFINING SPECTRAL TYPE "Y" AND EXPLORING THE LOW-MASS END OF THE FIELD BROWN DWARF MASS FUNCTION

To support the All-Sky data release in 2012 March, the WISE four-band cryogenic data were reprocessed using an improved version of the reduction pipeline, as described in the WISE All-Sky Data Release Explanatory Supplement.⁸ The individual W1, W2, W3, and W4 frames were rerun and atlas images rebuilt by stacking the individual, reprocessed frames. Source detections were made on the atlas images themselves, and source extractions were made on both the individual frames and the atlas images. Our query for cold brown dwarfs used the database of extractions from the atlas images, this database being a union of the WISE All-Sky Source Catalog and the WISE All-Sky Reject Table. This query attempts to improve upon the search we used earlier (Kirkpatrick et al. 2011) and is aimed toward identifying mid-T or later brown dwarfs for further follow-up. The search constraints are given below.

• 1.  
  The W1–W2 color from profile-fit photometry is greater than 2.0 mag, where the W2 measurement is an actual detection. (This criterion guarantees that the W2 signal-to-noise ratio is greater than three.) As Figure 1 of Kirkpatrick et al. (2011) shows, this color is typical of objects of type mid-T and later.
• 2.  
  The source is detected with a signal-to-noise ratio greater than three in at least eight individual W2 frames going into the co-add stack or, if detected only five, six, or seven times, is still detected at a signal-to-noise ratio greater than three in at least 40% of all frames. This criterion is meant to eliminate spurious, co-aligned artifacts in the co-adds.
• 3.  
  The source is either undetected in W3 or, if detected, has a W2–W3 color less than 3.5 mag. This criterion is meant to eliminate very red extragalactic contaminants or sources embedded in star formation regions.
• 4.  
  The source is not flagged as a diffraction spike, star halo, optical ghost, or latent artifact in bands W1 and W2. This criterion is meant to remove known spurious sources. Real sources that are flagged in W1 and W2 as impacted by spikes, halos, ghosts, or latents are, however, retained.
• 5.  
  The source is not blended with another source. This criterion is meant to reduce the number of objects with poorly determined photometry.
• 6.  
  The source has a reduced χ² value from profile-fit photometry that lies between 0.5 and 3.0. This criterion is meant to eliminate sources that are not point-like.
• 7.  
  The source has an absolute Galactic latitude greater than 3° if its Galactic longitude falls within 20° of zero. This criterion is meant to eliminate confused areas toward the Galactic center.

With this list of sources in hand, images of the field were constructed using Digitized Sky Survey 2 (DSS2) BRI (epoch ∼1980s), Sloan Digital Sky Survey (SDSS) ugriz (where available; epoch ∼2000), Two Micron All Sky Survey (2MASS) JHK_s (epoch ∼2000), and WISE four-band data (epoch ∼2010). These image sets, an example of which is shown in Figure 1, show the source across time and across wavelength. By using these images, sources that cannot possibly be cold brown dwarfs, because they are extended, spurious, or detected at wavelengths shortward of 1.0 μm (unless very bright in the WISE W1 and W2 bandpasses), were eliminated from further consideration.

Zoom In Zoom Out Reset image size

To select objects within 20 pc of the Sun, we further restricted the W2 magnitude depending on the color of the source:⁹ W2 ⩽ 14.5 mag for 2.0 ⩽ W1–W2 < 2.4, W2 ⩽ 14.8 mag for 2.4 ⩽ W1–W2 < 2.8, and W2 ⩽ 15.2 mag for 2.8 ⩽ W1–W2 < 2.9. For colors redder than this—W1–W2 = 2.9 being the color of the standard T9 dwarf UGPS J072227.51−054031.2—no W2 magnitude constraint was applied because at the time of candidate selection, the absolute magnitudes of objects with types ⩾T9 were very poorly known. This search results in 534 candidates along with 30 re-discovered T dwarfs identified earlier by other surveys. Candidates have been placed on our photometry and spectroscopy campaigns, as described in the next section. To date, 189 of these 534 candidates have been followed up via ground-based or Hubble Space Telescope imaging, All 534 are on our Spitzer Space Telescope follow-up imaging campaign, and 130 have been observed spectroscopically. This paper focuses on the new Y dwarf discoveries; for newly found T dwarfs, the reader is referred to G. N. Mace et al. (in preparation), C. G. Tinney et al. (in preparation), and Wright et al. (2012).

Cushing et al. (2011) identified the first six Y dwarfs using WISE data, and we confirm seven more here. Coordinates and photometry from the WISE All-Sky Release are given in Table 1 for all 13 of these Y dwarfs. In order to facilitate future investigations, we also provide finder charts for all 13 in Figure 2. These charts show the W1, W2, and W3 discovery images from WISE as well as a deep near-infrared (1.2–1.6 μm) view at higher resolution.

Zoom In Zoom Out Reset image size

Zoom In Zoom Out Reset image size

Zoom In Zoom Out Reset image size

Photometry of the new Y dwarfs is listed in Table 2 along with (in some cases, revised) photometry for the six Y dwarfs from Cushing et al. (2011). Six ground-based instruments and two space-based facilities—in addition to WISE, whose imaging identified these objects originally—were used for this imaging follow-up. Spectra of the new Y dwarfs were obtained in the ∼1.0–1.8 μm region with three different instruments. Details for the spectroscopic observations are given in Table 3.

2.2.1. Mt. Bigelow/2MASS

2.2.2. AAT/IRIS2

2.2.3. CTIO/NEWFIRM

2.2.4. SOAR/SpartanIRC

2.2.5. SOAR/OSIRIS

2.2.6. Magellan/PANIC

2.2.7. Spitzer/IRAC

2.2.8. HST/WFC3

2.2.9. Keck/NIRSPEC

2.2.10. Magellan/FIRE

Our new spectra, along with those from Cushing et al. (2011), are plotted in Figures 3–5. In Figures 3 and 4 we show all of the Y dwarfs except WISE 0535−7500 (which is plotted separately in Figure 5) and compare them to the T9.5 dwarf WISE 0148−7202 and other Y dwarfs. In Figure 5 we plot two versions of the spectrum of WISE 0535−7500. In the first, we show the contaminated spectrum as extracted by the aXe software from the Hubble Space Telescope. In the second, we plot our attempt at correcting the spectrum for the light of the contaminating object. This simplistic correction involves subtracting off a linear slope so that the mean level in the water absorption bands is zero. The resulting, quasi-corrected spectrum is sufficient to provide a crude classification despite the problems with data acquisition.

Zoom In Zoom Out Reset image size

Zoom In Zoom Out Reset image size

Zoom In Zoom Out Reset image size

After examining these plots, several facts become apparent. (1) All seven of the new discoveries have J-band (∼1.27 μm) flux peaks as narrow or narrower than the Y0 standard, WISE 1738+2732, proposed by Cushing et al. (2011). The T9.5 dwarf, in contrast, has a wider J-band peak than any of these. This confirms that all are Y dwarfs, as defined by Cushing et al. (2011). (2) The spectra of WISE 1541−2250 and WISE 0350−5658 have distinctly narrower J-band peaks than the Y0 standard itself, meaning that both of these objects should be typed later than Y0. The plot shown in Figure 6 suggests that the J-band peak of WISE 0350−5658 is sufficiently narrower than WISE 1738+2732 that it should be typed a full subclass later. We therefore propose WISE 0350−5658 to be the tentative Y1 spectral standard, despite its southerly declination, until other Y1 dwarfs are identified. This also means that WISE 1541−2250, which has a slightly broader J-band peak, should be re-typed from Y0 to Y0.5. (3) The spectrum of WISE 1828+2650, though having a low signal-to-noise ratio, is still in a class by itself due to the near-equal heights of the J- and H-band (∼1.58 μm) peaks. Because it is so different from all of the other spectra, we re-classify it to be ⩾Y2.

Zoom In Zoom Out Reset image size

Zoom In Zoom Out Reset image size

Although Cushing et al. (2011) discussed in detail the establishment of the new Y dwarf spectral class, it is worth revisiting this based on the latest discoveries. We compare our set of observational Y dwarf spectra to theoretical expectations prior to the launch of WISE. Specifically, Burrows et al. (2003) used atmospheric models covering this temperature regime to cite five possible triggers that could lead to the introduction of a new class beyond the T dwarfs. We investigate each of these possibilities below.

• 1.  
  The disappearance of alkali resonance lines near 450 K. The resonance lines of Na i and K i fall at optical wavelengths, where cold brown dwarfs have little flux, but the broad wings of these lines extend very far from the line cores and are believed to have an influence on the emergent flux as longward as 1 μm (Burrows & Volobuyev 2003). As discussed in Cushing et al. (2011), the Y-band (∼1.07 μm) peaks for the Y dwarfs whose spectra cover that region generally appear to be as high or higher than the J-band peaks in units of F_λ. This effect is not seen in the spectra of late-T dwarfs (see, e.g., Kirkpatrick et al. 2011). A harbinger of this effect—seen as a blueward trend of Y-J color in the mid- to late-T dwarf regime—was noted by Leggett et al. (2010) and Burningham et al. (2010) and ascribed to a brightening of the Y-band peak due to reduced absorption by the wings of the K i as atomic potassium begins to form into KCl at cooler temperatures (Lodders 1999). Although indirect, this is evidence that we have pushed into the regime where these alkali lines have lost prominence. Further spectroscopic investigation at higher signal-to-noise levels is possible at the Y band using the G102 grism on board HST/WFC3.
• 2.  
  Water cloud formation below 400–500 K. Although long predicted to be a possible trigger of a new spectral class at low temperatures, Burrows et al. (2003) found that the formation of these clouds has very little effect on the emergent spectra in their models. M. Marley (2012, private communication) also finds little effect shortward of 2 μm but finds that at longer wavelengths, for objects with ≲300 K, the effects are quite pronounced. The importance of these clouds should be re-investigated once newer atmospheric models are published for the coldest brown dwarfs.
• 3.  
  The emergence of ammonia absorption below 2.5 μm. As shown in Figure 5 of Kirkpatrick (2008), the theoretical spectra of Burrows et al. (2003) indicate that absorption bands of NH₃, which first appear in the mid-infrared (10.5 μm) near the L/T transition (Cushing et al. 2006), finally appear at the H and K bands starting near 800 K and become prominent by 450 K. As shown in Figure 5 of Cushing et al. (2011), the H-band ammonia feature—the easier of these two to detect because the K-band feature falls within the telluric water band—is itself confused with overlying absorption by H₂O and CH₄ in the brown dwarf atmosphere. Nonetheless, signs of a possible NH₃ signature were noted by Cushing et al. (2011) in the 1.53–1.58 μm region of WISE 1738+2732. This region falls in an area of extremely low flux, so exquisite signal to noise is needed to detect it. Unfortunately, none of the spectra of our new objects has sufficient signal to investigate this feature further. Analyzing the near-infrared spectra of these objects for the presence of NH₃ bands will likely require higher resolution spectra than can be presently obtained.
• 4.  
  Collapse below 350 K of the optical and near-infrared fluxes, relative to those ≳5 μm. Burrows et al. (2003) state that this collapse in flux would manifest itself as a reversal of the blueward trend of J − K (or J − H) colors. Figure 11 in Cushing et al. (2011) shows the J − H color (on the MKO-NIR system) as a function of spectral type. That figure shows that the J − H color stagnates near −0.4 mag for late-T dwarfs and then appears to turn to the red starting at Y0, although there are some blue outliers at Y0. With our new Y dwarf discoveries, new T dwarf discoveries from Mace (et al.), additional near-infrared photometry, and revised photometric reductions of previous Y dwarf discoveries (see footnotes to Table 2), we can revisit this plot. This new photometry, shown in Figure 7, more clearly shows the reversal of the J − H color. After trending to the blue from early- to mid-T and stagnating for late-T types, the J − H color turns to the red starting near Y0. Later Y dwarfs, such as the Y0.5 dwarf WISE 1541−2250 (J − H > 0.54 mag) and the ⩾Y2 dwarf WISE 1828+2650 (J − H = 0.72 ± 0.42 mag), are roughly 1 mag redder than late-T dwarfs.
• 5.  
  The shift in position of the ∼5 μm peak. As shown in Figures 7 and 8 of Kirkpatrick et al. (2011), the J −W2 and H −W2 colors continue to increase from mid-T to early-Y. Figure 11 from that paper shows an indication that the Spitzer ch1−ch2 color may reverse in the Y sequence, but this was based solely on the ch1−ch2 color of WISE 1828+2650. We can also revisit this trend using newly discovered Y dwarfs. Figure 8 shows the J −W2, F140W−W2, and H −W2 colors as a function of the ch1−ch2 color.¹⁴ The ch1−ch2 color shows a broad range (of up to a magnitude) for Y0 dwarfs; similar scatter is seen in the ch1−ch2 colors of late-T dwarfs, which Leggett et al. (2010) attribute to gravity and/or metallicity effects. Dwarfs classified as Y1 or later are generally redder than these. It should be noted that the ⩾Y2 dwarf, WISE 1828+2650, indicates a turn to the blue in ch1−ch2 color at later types. (The J −W2, F140W−W2, and H −W2 colors, nevertheless, still tend to run redder with advancing spectral type and may serve as a proxy for temperature for these early-Y dwarfs.)

Zoom In Zoom Out Reset image size

WISE 1828+2650 satisfies the last two of the possible trigger conditions discussed above. The stark contrast between its spectral morphology and that of T dwarfs—namely, the near-equal heights of the J and H peaks that are manifested as a turn to the red in the J − H color—satisfies the criteria needed to define a new spectral class. Moreover, Beichman et al. have recently measured the trigonometric parallax for this object, establishing it as an instrinsically dim source (see Section 4.3), and model fits by Cushing et al. (2011) suggest that its effective temperature is below 300 K. With more evidence now in hand, we still reach the same conclusion as Cushing et al. (2011) that WISE 1828+2650 should be considered as the archetypal Y dwarf.

Given that the ammonia absorption bands in the near-infrared are obscured by other strong absorption bands, we lack a clear signature that defines the exact onset of the Y class. A gradual change in spectral morphology is the norm, however, at the boundary between spectral classes. For example, there is very little change in the optical morphology of a late-K dwarf and an early-M dwarf, even though mid-K and mid-M spectra are markedly different, and the same is true at the boundary between M and L classes. The L/T transition is unusual in its sudden appearance of a major absorption species that radically alters the appearance of the spectra (over what we now know is a very small temperature range; see Figure 8 of Kirkpatrick 2005). For Y dwarfs, we see a gradual change in the spectral morphology from late-T to early-Y, even though the spectra of a mid-T dwarf and that of WISE 1828+2650 are very different. We have further evidence that this gradual change continues down the Y sequence, as well: the spectrum of our new Y1 dwarf WISE 0350−5658 has as an H-band peak relative to that of the J-band peak that is higher than in the Y0 standard and this presages the effect of equal-peak heights seen in WISE 1828+2650. We therefore see no reason to deviate from the Y dwarf classification scheme presented in Cushing et al. (2011), which has so far been robust to new discoveries.

For early-Y dwarfs, we have based our classifications on the narrowness of the J-band peak using by-eye comparisons to our Y0 and Y1 spectral standards. Can a spectral index be created that distills this same information? A pre-existing index, dubbed W_J, was developed by Warren et al. (2007) to measure this narrowness of J-band for late-T dwarfs, but we find that it has problems in the Y dwarf regime. (See Figure 7 of Cushing et al. 2011 for a graphical representation of this index along with other indices measured for T dwarfs.) All of the Y dwarfs have a W_J index of ∼0.1, except for WISE 1828+2650, which is very noisy. Because the J-band peak is so narrow for Y dwarfs, the numerator of the W_J index (which is the flux integrated from 1.18 to 1.23 μm) is nearing 0. A better measure of the J-band peak can be obtained by moving this region of integration longward so that it still falls in a region with measurable flux nearer the peak. Also, the region used in the denominator of the index (1.26–1.285 μm), which measures the flux in the peak itself, as well as the region used in the numerator (to measure the blueward wing) can be narrowed to reflect the fact that the opacity hole in the spectrum has narrowed for the Y dwarfs.

Mace et al. define a new index, called J-narrow, which is the ratio of the median flux over the 1.245–1.260 μm region to the median flux over 1.260–1.275 μm. We show the results of measuring this index on our collection of WISE-discovered T and Y dwarfs in Figure 9. Note that for most of the T dwarfs, J-narrow has a value greater than 0.85. Y dwarfs have values less than this, the Y0 standard WISE 1728+2732 being the least narrow Y dwarf as measured by this index. (This is because our by-eye classification requires an object to have a J-band peak as least as narrow as that of the Y0 standard for it to be classified as a Y dwarf.) Whittling the wavelength region over which the index operates, though necessary, nonetheless comes at a price: high signal-to-noise spectra are required to make the index measurements robust. This is a difficult requirement to meet because Y dwarfs are notoriously hard to observe given their intrinsic faintness and the ones plotted in Figure 9 are among the closest, brightest Y dwarfs over the entire sky. Even though we present this new index for completeness, we strongly recommend that researchers classify their spectra by overplotting the late-T and early-Y standards rather than resorting to the use of spectral indices, since the latter technique is far more prone to error when spectra have low signal to noise.

Zoom In Zoom Out Reset image size

To understand the intrinsic faintness of Y dwarfs, we have constructed a Hertzsprung–Russell (H-R) diagram at the H band that contains a selection of main-sequence stars and brown dwarfs with spectral types running the gamut from O through Y. Objects were required to have high quality parallaxes and be free of complications such as being heavily reddened (which is mitigated by choosing only the most nearby examples) or belonging to a close multiple system. Our aim was to choose, if possible, at least 25 objects in each spectral class, spread evenly so that all integral subclasses were covered. All H-band magnitudes and errors were taken from 2MASS. Additional details are given below.

O, B, and A dwarfs. Using Jim Kaler's "Stars" Web site,¹⁵ we selected objects identified as O dwarfs and retained those having trigonometric parallaxes from Hipparcos (van Leeuwen 2007) that place them within 600 pc of the Sun and parallax errors less than 1 mas. Only 10 O dwarfs survived the cut, the earliest being the O7 V star 15 Monocerotis. Using the same Web site and Hipparcos parallaxes, we selected B dwarfs lying within 500 pc and A dwarfs lying within 100 pc. Retaining only those with parallax errors under ∼1 mas resulted in a sample of 26 B stars and 42 A stars.

F, G, and K dwarfs. Using SIMBAD, we selected F, G, and K stars whose Hipparcos parallaxes (van Leeuwen 2007) place them within 20.0, 18.2, and 13.4 pc of the Sun (i.e., parallax values exceeding 50, 55, and 75 mas), respectively. We retained those that Jim Kaler's "Stars" Web site confirms as having dwarf luminosity classes. Further requiring that the Hipparcos parallax errors are less than ∼0.5 mas resulted in a list of 35 F dwarfs, 53 G dwarfs, and 28 K dwarfs.

M dwarfs. We selected M dwarfs from the Research Consortium On Nearby Stars' (RECONS) Web page that lists the hundred nearest stellar systems to the Sun.¹⁶ Dropping objects where the 2MASS H-band photometry or measured spectral type is a composite of multiple components resulted in a list of 72 M dwarfs.

L and T dwarfs. We selected from the literature those L and T dwarfs having measured trigonometric parallaxes. The list is available as Table 5 of Kirkpatrick et al. (2011). Retaining only those not known to be multiple systems and having well measured 2MASS H-band magnitudes results in 20 L dwarfs and 21 T dwarfs.

Y dwarfs. Due to the paucity of parallax data currently available for Y dwarfs, we retained all Y dwarfs from Marsh et al. (2012) and Beichman et al. (2012) having trigonometric parallax measurements at least five times the error. This selection yields four Y dwarfs.

The compiled list is illustrated in Figure 10. The trend of ever-dimming H-band magnitude as a function of later spectral type shows two well-known inflection points. The first of these occurs at early-M and is a result of hydrogen associating into H₂ at temperatures below ∼4000 K (Mould 1976; Mould & Hyland 1976). The other inflection point, at late-L to mid-T, is a flattening or brightening of the H-band flux over a range of spectral types near the L/T transition (see, e.g., Looper et al. 2008; Dahn et al. 2002; Vrba et al. 2004; Knapp et al. 2004; the brightening is even more dramatic in the J band). The physical cause for this brightening may be due to patchy clouds in the atmospheres of these objects (Marley et al. 2010). Below this second inflection point, the H-band magnitude plummets. By early-Y the absolute H-band magnitudes are ∼30 mag (or 12 orders of magnitude in flux) fainter than those of late-O dwarfs. As discussed later in this paper, the trend of absolute H-band flux may show another inflection point at early-Y, although more data are required to check this further.

Zoom In Zoom Out Reset image size

To understand the importance of Y dwarfs in the Milky Way, we consider an all-sky, volume-limited sample of the solar neighborhood with which to compare the frequency of Y dwarfs relative to other spectral types. Previous authors have considered different volumes as defining the immediate solar neighborhood. Building on earlier work¹⁷ by Hertzsprung (1907, 1922), van de Kamp (1930, 1940, 1945, 1953, 1969, 1971) considered the sample out to ∼5 pc; Kuiper (1942) considered a volume out ∼10 pc; and Gliese (1956, 1969) and Gliese & Jahreiß (1979) considered a distance limit of ∼20 pc, although this was extended to 25 pc in Gliese & Jahreiß (1991). For our purposes, we will consider a distance limit of 8 pc because this bounds a volume with a sufficient number of objects (∼250) to provide adequate statistics across spectral classes.

Table 4 gives our update of all stars and brown dwarfs known or suspected to lie within 8 pc. This list relies heavily on previous work, most notably the list compiled by Reid & Gizis (1997) with updates in Reid et al. (2004) and I. N. Reid (2012, private communication) and the list of the hundred nearest stars compiled by RECONS at their Web site. The papers by Reid et al. consider only objects with decl. >−30° and do not include several recently discovered, low-luminosity objects uncovered by surveys such as 2MASS, SDSS, DENIS, UKIDSS, and WISE; the RECONS list includes only objects with precisely determined trigonometric parallaxes and only objects within roughly 6.7 pc of the Sun. Therefore, we have combed the literature to uncover more newly discovered objects, suspects with unknown or poorly measured parallaxes, or objects near the outer limits of the 8 pc volume. Other updates in Table 4 include better characterization of previously known or newly identified multiple systems and consistent, MK-based spectral types for stars earlier than late-K (see Gray et al. 2003 and Gray et al. 2006). Further details on each column are given below.

Table 4. The Census of Stars and Brown Dwarfs within 8 pc of the Sun

Discovery Name	Other Name	Gliese Name	πtriga	σπ	π Ref.	Spec.	Spec.	J2000 Coords.	Sys.	Indiv.
			(mas)	(mas)		Type	Ref.		Rank	Rank
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)
Sun	Sol	...	...	...	...	G2 V	51	...	0	0
Proxima Cenb	α Cen C	Gl 551	769.91	0.54	16	M5.5 V	18	1429−6240	1	1
Rigel Kentaurus A	α Cen A	Gl 559 A	754.81	4.11	5	G2 V	50	1439−6050	1	2
Rigel Kentaurus B	α Cen B	Gl 559 B	...	...	...	K2 IV C2+1	50	1439−6050	1	2
Barnard's Star	...	Gl 699	545.4	0.3	16	M4 V	38	1757+0441	2	4
Wolf 359	...	Gl 406	419.1	2.1	6	M6 V	38	1056+0700	3	5
Lalande 21185	...	Gl 411	392.64	0.67	5	M2 V	38	1103+3558	4	6
Sirius A	α CMa A	Gl 244 A	379.21	1.58	5	A0mA1 Va	49	0645−1642	5	7
Sirius B	α CMa B	Gl 244 B	...	...	...	DA2	52	0645−1643	5	7
L 726-8 A	BL Cet	Gl 65 A	373.7	2.7	6	M5.5 V	38	0139−1757	6	9
L 726-8 B	UV Cet	Gl 65 B	...	...	...	M6 V	38	0139−1757	6	9
Ross 154	...	Gl 729	336.72	2.03	5	M3.5 V	21	1849−2350	7	11
Ross 248	...	Gl 905	316.0	1.1	6	M5.5 V	21	2341+4410	8	12
Eri	...	Gl 144	310.94	0.16	5	K2 V (k)	50	0332−0927	9	13
Lacaille 9352	...	Gl 887	305.26	0.70	5	M0.5 V	44	2305−3551	10	14
Ross 128	...	Gl 447	298.2	1.7	6	M4 V	21	1147+0048	11	15
L 789-6 A	...	Gl 866 A	289.5	4.4	6	M5c V	21	2238−1517	12	16
L 789-6 B	...	Gl 866 B	...	...	...	M5.5:d V	45	2238−1515	12	16
L 789-6 C	...	Gl 866 C	...	...	...	M6.5:d V	45	2238−1517	12	16
61 Cyg A	...	Gl 820 A	286.9	1.1	6	K5 V	38	2106+3844	13	19
61 Cyg B	...	Gl 820 B	...	...	...	K7 V	38	2106+3844	13	19
Procyon A	α CMi A	Gl 280 A	284.56	1.26	5	F5 IV-V	49	0739+0513	14	21
Procyon B	α CMi B	Gl 280 B	...	...	...	DA	52	0739+0515	14	21
Σ 2398 A	...	Gl 725 A	280.18	2.18	5	M3 V	41	1842+5937	15	23
Σ 2398 B	...	Gl 725 B	...	...	...	M3.5 V	41	1842+5937	15	23
Groombridge 34 A	...	Gl 15 A	278.76	0.77	5	M1.5 V	21	0018+4401	16	25
Groombridge 34 B	...	Gl 15 B	...	...	...	M3.5 V	21	0018+4401	16	25
Ind A	...	Gl 845 A	276.06	0.28	5	K4 V (k)	50	2203−5647	17	27
Ind Ba	...	Gl 845 Ba	...	...	...	T1	53	2204−5646	17	27
Ind Bb	...	Gl 845 Bb	...	...	...	T6	53	2204−5646	17	27
G 51-15	...	GJ 1111	275.8	3.0	6	M6.5 V	38	0829+2646	18	30
τ Cet	...	Gl 71	273.96	0.17	5	G8.5 V	50	0144−1556	19	31
L 372-58	...	GJ 1061	271.92	1.34	12	M5 V	12	0335−4430	20	32
L 725-32	...	Gl 54.1	268.8	3.2	6	M4.5 V	21	0112−1659	21	33
Luyten's Star	BD+05 1668	Gl 273	262.98	1.39	5	M3.5 V	38	0727+0513	22	34
SCR J1845−6357 A	...	...	259.45	1.11	12	M8.5 V	12	1845−6357	23	35
SCR J1845−6357 B	...	...	...	...	...	T6	54	1845−6357	23	35
Teegarden's Star	SO J025300.5+165258	...	259.25	0.94	74	M6 V	12	0253+1652	24	37
Kapteyn's Star	Z C 5h243bb	Gl 191	255.66	0.91	5	sdM1	44	0511−4501	25	38
Lacaille 8760	...	Gl 825	253.41	0.80	5	K7 V	44	2117−3852	26	39
Krüger 60 A	...	Gl 860 A	251.5	3.7	6	M3 V	39	2228+5741	27	40
Krüger 60 B	...	Gl 860 B	...	...	...	M4 V	39	2227+5741	27	40
DENIS-P J104814.7−395606.1	...	...	247.71	1.55	17	M8.5 V	20	1048−3956	28	42
UGPS J072227.51−054031.2	...	...	246	33	22	T9	4	0722−0540	29	43
Ross 614 A	...	Gl 234 A	242.32	3.12	5	M4-4.5 V	42	0629−0248	30	44
Ross 614 B	...	Gl 234 B	...	...	...	M4.5-6.5 V	42	0629−0248	30	44
WISE J035000.32−565830.2	...	...	238	38	2	Y1	1	0350−5658	31	46
WISEPA J154151.66−225025.2	...	...	238rr	...	1	Y0.5	1	1541−2250	32	47
BD−12 4523	Wolf 1061	Gl 628	232.98	1.60	5	M3 V	21	1630−1239	33	48
van Maanen's Stare	...	Gl 35	232.5	1.9	6	DZ8	52	0049+0523	34	49
Gou 32416bb	CD−37 15492	Gl 1	230.42	0.90	5	M1.5 V	44	0005−3721	35	50
Wolf 424 A	...	Gl 473 A	227.9	4.6	6	M5.5c V	40	1233+0901	36	51
Wolf 424 B	...	Gl 473 B	...	...	...	M5.5: V	46	1233+0901	36	51
L 1159-16	...	Gl 83.1	224.8	2.9	6	M4.5 V	38	0200+1303	37	53
Oe Arg 17415-6bb	BD+68 946	Gl 687	220.84	0.94	5	M3 V	21	1736+6820	38	54
LP 731-58	LHS 292	...	220.3	3.6	6	M6.5 V	40	1048−1120	39	55
Innes (unnumbered)g	CD−46 11540	Gl 674	220.24	1.42	5	M2.5 V	44	1728−4653	40	56
G 208-44 A	...	GJ 1245 A	220.2	1.0	6	M5.5h V	41	1953+4424	41	57
G 208-44 B	...	GJ 1245 C	...	...	...	M6.5:i V	1	1953+4424	41	57
G 208-45	...	GJ 1245 B	...	...	...	M5.5 V	41	1953+4424	41	57
Innes (unnumbered)g	Ci 20 658	Gl 440	215.80	1.25	8	DQ6	52	1145−6450	42	60
Ross 780	...	Gl 876	213.28	2.12	5	M3.5 V	21	2253−1415	43	61
G 158-27	...	GJ 1002	213.0	3.6	6	M5.5 V	21	0006−0732	44	62
L 143-23	LHS 288	...	208.95	2.73	12	M5 V	12	1044−6112	45	62
WISEPC J140518.40+553421.4	...	...	207	39	2	Y0p	4	1405+5534	46	62
Lalande 21258 A	...	Gl 412 A	206.27	1.00	5	M1 V	21	1105+4331	47	65
Lalande 21258 B	...	Gl 412 B	...	...	...	M5.5 V	21	1105+4331	47	65
Groombridge 1618	...	Gl 380	205.21	0.54	5	K7 V	38	1011+4927	48	67
BD+20 2465	G 54-23	Gl 388	204.6	2.8	6	M3 V	21	1019+1952	49	68
DENIS J081730.0−615520	...	...	203	13	23	T6	23	0817−6155	50	69
CD−49 13515	L 354-89	Gl 832	201.87	1.01	5	M1.5 V	44	2133−4900	51	70
LP 944-20	...	...	201.4	4.2	27	M9 V	48	0339−3525	52	71
DENIS-P J025503.3−470049	...	...	201.37	3.89	13	L8	55	0255−4700	53	72
o2 Eri A	...	Gl 166 A	200.62	0.23	5	K0.5 V	50	0415−0739	54	73
o2 Eri B	...	Gl 166 B	...	...	...	DA4	52	0415−0739	54	73
o2 Eri C	...	Gl 166 C	...	...	...	M4.5 V	38	0415−0739	54	73
Innes (unnumbered)g	CD−44 11909	Gl 682	196.90	2.15	5	M3.5 V	44	1737−4419	55	76
70 Oph A	...	Gl 702 A	196.72	0.83	5	K0- V	49	1805+0229	56	77
70 Oph B	...	Gl 702 B	...	0.83	5	K5 V	56	1805+0229	56	77
BD+43 4305	LFT 1737	Gl 873	195.22	1.87	5	M3.5 V	42	2246+4420	57	79
Altair	α Aql	Gl 768	194.95	0.57	5	A7 Vn	49	1950+0852	58	80
WISEPC J150649.97+702736.0	...	...	193	26	2	T6	3	1506+7027	59	81
WISEPC J205628.90+145953.3	...	...	192	...	1	Y0	4	2056+1459	60	82
G 9-38 A	...	GJ 1116 A	191.2	2.5	6	M5.5 V	57	0858+1945	61	83
G 9-38 B	...	GJ 1116 B	...	...	...	M5.5 V	57	0858+1945	61	83
G 99-49	...	...	190.93	1.89	12	M3.5 V	21	0600+0242	62	85
LP 656-38	LHS 1723	...	187.92	1.26	12	M4 V	12	0501−0656	63	86
2MASS J09393548−2448279	...	...	187.3	4.6	28	T8	53	0939−2448	64	87
AC+79 3888	LFT 849	Gl 445	186.86	1.70	5	M3.5 V	21	1147+7841	65	88
Lalande 25372	...	Gl 526	185.49	1.10	5	M1.5 V	21	1345+1453	66	89
Stein 2051 A	...	Gl 169.1A	180.6	0.8	6	M4 V	42	0431+5858	67	90
Stein 2051 B	...	Gl 169.1B	...	...	...	DC5	52	0431+5858	67	90
Wolf 294	...	Gl 251	179.01	1.60	5	M3 V	38	0654+3316	68	92
2MASSI J0415195−093506	...	...	177.3	2.2	76	T8	53	0415−0935	69	93
Strb. 1611s	Wolf 1453	Gl 205	176.77	1.18	5	M1.5 V	38	0531−0340	70	94
2MASSI J1835379+325954	LSR J1835+3259	...	176.5	0.5	31	M8.5 V	31	1835+3259	71	95
WISEPA J174124.26+255319.5	...	...	176	22	2	T9	3	1741+2553	72	96
LP 816-60	...	...	175.03	3.40	5	M4 V	50	2052−1658	73	97
L 449-1	...	...	175	...	14	M4 V	14	0517−3521	74	98
L 668-21 A	...	Gl 229 A	173.81	0.99	5	M1 V	38	0610−2151	75	99
L 668-21 B	...	Gl 229 B	...	...	...	T7 pec	53	0610−2152	75	99
σ Dra	...	Gl 764	173.77	0.18	5	G9 V	49	1932+6939	76	101
Ross 47	...	Gl 213	171.55	3.99	5	M4 V	38	0542+1229	77	102
Innes (unnumbered)g	...	Gl 693	171.48	2.31	5	M2 V	44	1746−5719	78	103
Lalande 27173 A	...	Gl 570 A	171.22	0.94	5	K4 V	50	1457−2124	79	104
Lalande 27173 B	...	Gl 570 B	...	...	...	M1m V	21	1457−2124	79	104
Lalande 27173 C	...	Gl 570 C	...	...	...	M3:n V	57	1457−2124	79	104
2MASSW J1457150−212148	...	Gl 570 D	...	...	...	T7.5	53	1457−2121	79	104
Wolf 1055	...	Gl 752 A	171.2	0.7	6	M3 V	38	1916+0510	80	108
van Biesbroeck 10	...	Gl 752 B	...	...	...	M8 V	41	1916+0509	80	108
WISE J053516.80−750024.9	...	...	170	44	2	⩾Y1:	1	0535−7500	81	110
L 347-14	...	Gl 754	169.03	1.55	17	M3 V	19	1920−4533	82	111
Innes (unnumbered)g	...	Gl 588	168.66	1.30	5	M2.5 V	44	1532−4116	83	112
36 Oph A	...	Gl 663 A	168.54	0.54	5	K0 V	59	1715−2636	84	113
36 Oph B	...	Gl 663 B	...	...	...	K1 V	59	1715−2636	84	113
36 Oph Co	...	Gl 664	...	...	...	K5 V (k)	50	1716−2632	84	113
η Cas A	...	Gl 34 A	167.98	0.48	5	F9 V	58	0049+5748	85	116
η Cas B	...	Gl 34 B	...	...	...	K7 V	21	0049+5749	85	116
Ross 882	...	Gl 285	167.88	2.31	5	M4 V	21	0744+0333	86	118
Lalande 46650	...	Gl 908	167.29	1.23	5	M1 V	21	2349+0224	87	119
2MASS J05332802−4257205	...	...	167	...	32	M4.5 V	32	0533−4257	88	120
2MASS J18450079−1409036p	...	...	167	...	32	M5 V	32	1845−1409	89	121
2MASS J18450097−1409053p	...	...	167	...	32	M5 V	32	1845−1409	89	121
2MASS J20360829−3607115	...	...	167	...	32	M4.5 V	32	2036−3607	90	123
L 722-22 A	...	GJ 1005 A	166.6	∼2	24	M3.5 V	42	0015−1607	91	124
L 722-22 B	...	GJ 1005 B	...	...	...	M4.5-6.5 V	42	0015−1607	91	124
LPM 728 A	...	Gl 783 A	166.25	0.27	5	K2.5 V	50	2011−3606	92	126
LPM 728 B	...	Gl 783 B	...	...	...	M3.5 Vq	56	2011−3606	92	126
WISEPA J025409.45+022359.1	...	...	166	26	2	T8	3	0254+0223	93	128
82 Eri	...	Gl 139	165.47	0.19	5	G8 V	50	0319−4304	94	129
Ross 986 A	...	Gl 268 A	165.2	2.1	6	M4.5c V	38	0710+3831	95	130
Ross 986 B	...	Gl 268 B	...	...	...	M5: V	60	0710+3832	95	130
WISEPA J041022.71+150248.5	...	...	164	24	2	Y0	4	0410+1502	96	132
LP 44-113	...	GJ 1221	164.7	2.4	6	DXP9	52	1748+7052	97	133
δ Pav	...	Gl 780	163.71	0.17	5	G8 IV	50	2008−6610	98	134
2MASSI J0937347+293142	...	...	163.39	1.76	26	T6 pec	53	0937+2931	99	135
BD+53 1320	LFT 634	Gl 338 A	162.8	2.9	6	M0 V	38	0914+5241	100	136
BD+53 1321	LFT 635	Gl 338 B	...	...	...	K7 V	38	0914+5241	100	136
BD+19 5116 A	LFT 1799	Gl 896 A	161.76	1.66	5	M3.5 V	21	2331+1956	101	138
BD+19 5116 B	LFT 1800	Gl 896 B	...	...	...	M4.5 V	21	2331+1956	101	138
LPM 730	...	Gl 784	161.34	1.00	5	M0 V	56	2013−4509	102	140
WISE J014656.66+423410.0	...	...	159	...	1	Y0		0146+4234	103	141
Wolf 1481	...	Gl 555	158.46	2.62	17	M3.5 V	21	1434−1231	104	142
2MASS J15031961+2525196	...	...	157.2	2.2	76	T5	53	1503+2525	105	143
LP 368-128	LHS 2090	...	156.87	2.67	12	M6 V	12	0900+2150	106	144
L 471-42	LHS 337	...	156.78	1.99	12	M4 V	12	1238−3822	107	145
G 99-44	...	Gl 223.2	156.13	0.84	8	DZ9	52	0555−0410	108	146
G 180-60	...	...	156r	4	25	M5 V	65	1631+4051	109	147
SIMP J013656.5+093347	...	...	156	...	34	T2.5	34	0136+0933	110	148
Wolf 630 A	...	Gl 644 A	154.8	0.6	6	M2.5t V	21	1655−0819	111	149
Wolf 630 Ba	...	Gl 644 B	...	...	...	M3:u V	1	1655−0820	111	149
van Biesbroeck 8	...	Gl 644 C	⋅⋅⋅  v	...	...	M7 V	41	1655−0823	111	149
Wolf 630 Bb	...	Gl 644 D	...	...	...	M3.5:u V	1	1655−0820	111	149
Wolf 629	...	Gl 643	⋅⋅⋅  w	...	...	M3.5 V	38	1655−0819	111	149
Wolf 562	BD−7 4003	Gl 581	154.66	2.62	17	M2.5 V	21	1519−0743	112	154
BD+45 2505 A	LFT 1326	Gl 661 A	154.0	3.6	6	M3c V	39	1710+4542	113	155
BD+45 2505 B	LFT 1327	Gl 661 B	...	...	...	M3:x V	64	1712+4539	113	155
LP 71-82	...	...	154f	...	32,36	M5 V	32	1802+6415	114	157
G 202-48	...	Gl 625	153.46	0.99	5	M1.5 V	39	1625+5418	115	158
L 100-115	...	GJ 1128	153.05	2.41	17	M4.5 V	18	0942−6853	116	159
G 161-71	...	...	153j	...	35,72	M5 V	35	0944−1220	117	160
L 1190-34	...	GJ 1156	152.9	3.0	6	M5 V	21	1218+1107	118	161
BD+56 2966	LFT 1767	Gl 892	152.76	0.29	5	K3 V	49	2313+5710	119	162
2MASS J11145133−2618235	...	...	152	...	1	T7.5	53	1114−2618	120	163
Ross 104	...	Gl 408	150.10	1.70	5	M2.5 V	21	1100+2249	121	164
Ross 775 A	...	Gl 829 A	149.15	1.81	5	M3.5c V	39	2129+1738	122	165
Ross 775 B	...	Gl 829 B	...	...	...	M3.5:y V	1	2129+1738	122	165
SCR J1546−5534	...	...	149	...	11	late-Mz V	1	1546−5534	123	167
ξ Boo A	...	Gl 566 A	148.98	0.48	5	G7 V	49	1451+1906	124	168
ξ Boo B	...	Gl 566 B	...	...	...	K4 V	67	1451+1906	124	168
Wolf 358	...	Gl 402	147.92	3.52	5	M4 V	38	1050+0648	125	170
G 41-14 A	...	...	147.66	1.98	12	M3.5c V	21	0858+0828	126	171
G 41-14 B	...	...	...	...	...	M3.5:aa V	1	0858+0828	126	171
G 41-14 C	...	...	...	...	...	M3.5:aa V	1	0858+0828	126	171
Ross 619	...	Gl 299	146.3	3.1	6	M4 V	21	0811+0846	127	174
Ross 671	...	Gl 880	146.09	1.00	5	M1.5 V	39	2256+1633	128	175
LP 914-54	LHS 3003	...	145.30	3.25	15	M7 V	66	1456−2809	129	176
LP 771-95cc	...	...	144.68	2.52	12	M2.5 V	12	0301−1635	130	177
LP 771-96 A	...	...	...	...	...	M3dd V	12	0301−1635	130	177
LP 771-96 B	...	...	...	...	...	M3.5:ee V	1	0301−1635	130	177
L 230-188	...	GJ 1068	143.42	1.92	17	M4.5ff V	44	0410−5336	131	180
WISE J192841.35+235604.9	...	...	143	...	1	T6	78	1928+2356	132	181
L 369-44gg	LP 993-116	...	143	...	32,72	M4 V	32	0245−4344	133	182
L 369-45gg	LP 993-115	...	143	...	32,72	M5:hh V	1	0245−4344	133	182
2MASS J18522528−3730363	...	...	143	...	32	M4.5 V	32	1852−3730	134	184
G 161-7 A	...	...	143k	...	35,72	M5c V	35	0915−1035	135	185
G 161-7 B	...	...	...	...	...	M5:ll V	1	0915−1035	135	185
BD+61 2068 A	LFT 1580 A	Gl 809 A	141.87	0.64	5	M0c V	39	2053+6209	136	187
BD+61 2068 B	LFT 1580 B	Gl 809 B	...	...	...	M?ii V	1	2053+6209	136	187
Ross 446	...	Gl 393	141.50	2.22	5	M2 V	21	1028+0050	137	189
WISE J071322.55−291751.9	...	...	141	...	1	Y0		0713−2917	138	190
WISE J000517.48+373720.5	...	...	141	...	1	T9	78	0005+3737	139	191
WISEPC J121756.91+162640.2	...	...	141	...	1	T9	3	1217+1626	140	192
2MASS J07290002−3954043	...	...	141	...	1	T8p	79	0729−3954	141	193
HR 6426 A	LFT 1336 A	Gl 667 A	139.5	6.3	6	K4- V	50	1718−3459	142	194
HR 6426 B	LFT 1336 B	Gl 667 B	...	...	...	K4 V	56	1718−3459	142	194
HR 6426 C	LFT 1337	Gl 667 C	...	...	...	M1.5 V	44	1718−3459	142	194
HR 753 A	LFT 217 A	Gl 105 A	139.27	0.45	5	K3 V	49	0236+0653	143	197
HR 753 B	LFT 218	Gl 105 B	...	...	...	M3.5 V	21	0236+0652	143	197
HR 753 C	LFT 217 B	Gl 105 C	...	...	...	M7:jj V	68	0236+0653	143	197
SCR J0740−4257	LSR J07401−4257	...	139	...	7	M4.5 V	7	0740−4257	144	200
L 43-72	...	...	139	...	14	M4.5 V	14	1811−7859	145	201
G 157-77	...	GJ 1286	138.3	3.5	6	M5.5 V	21	2335−0223	146	202
LP 229-17kk	...	...	138	40	37	M3 V	37	1834+4007	147	203
LP 71-165	LHS 3376	...	137.5	5.3	6	M4.5 V	21	1818+6611	148	204
2MASSW J1507476−162738	...	...	136.4	0.6	30	L5	61	1507−1627	149	205
WISE J004945.61+215120.0	...	...	135	...	1	T8.5	78	0049+2151	150	206
L 788-34	LHS 3799	...	134.4	4.9	6	M4.5 V	21	2223−1736	151	207
G 203-47 A	...	...	134.31	1.99	5	M3.5 Vc	21	1709+4340	152	208
G 203-47 B	...	...	134.31	1.99	5	D?nn	43	1709+4340	152	208
L 499-56	LHS 3746	...	134.29	1.31	12	M3 V	12	2202−3704	153	210
Lalande 1299	...	Gl 33	134.14	0.51	5	K2 V	49	0048+0516	154	211
β Hyi	...	Gl 19	134.07	0.11	5	G0 V	50	0025−7715	155	212
Ross 556	...	Gl 109	133.16	2.26	5	M3 V	21	0244+2531	156	213
107 Psc	...	Gl 68	132.76	0.50	5	K0 V	49	0142+2016	157	214
G 154-44	...	GJ 1224	132.6	3.7	6	M4.5 V	21	1807−1557	158	215
μ Cas A	...	Gl 53 A	132.38	0.82	5	K1 V Fe-2	49	0108+5455	159	216
μ Cas B	...	Gl 53 B	...	...	...	M3.5:oo V	9	0108+5455	159	216
LTT 9283qq	...	Gl 879	131.42	0.62	5	K4+ V k	50	2256−3133	160	218
Ross 490	...	Gl 514	130.62	1.05	5	M1 V	21	1329+1022	161	219
Vega	...	Gl 721	130.23	0.36	5	A0 Va	49	1836+3847	162	220
Wolf 718	...	Gl 673	129.86	0.73	5	K7 V	21	1725+0206	163	221
Fomalhautpp	...	Gl 881	129.81	0.47	5	A4 V	50	2257−2937	164	222
LP 881-64 Amm	...	GJ 2005 A	129.47	2.48	15	M5.5 V	69	0024−2708	165	223
LP 881-64 B	...	GJ 2005 B	...	...	...	M8.5 V	69	0024−2708	165	223
LP 881-64 C	...	GJ 2005 C	...	...	...	M9 V	69	0024−2708	165	223
L 991-14	...	Gl 701	128.89	1.43	5	M0 V	21	1805−0301	166	226
G 109-35	...	GJ 1093	128.8	3.5	6	M5 V	21	0659+1920	167	227
Innes (unnumbered)g	...	Gl 480.1	128.52	3.90	5	M3 V	44	1240−4333	168	228
WISEP J060738.65+242953.4	...	...	128.2	...	71	L9	1	0607+2429	169	229
2MASS J03480772−602227	...	...	128	...	1	T7	53	0348−6022	170	230
p Eri A	...	Gl 66 A	127.84	2.19	5	K2 V	50	0139−5611	171	231
p Eri B	...	Gl 66 B	...	...	...	K2 V	50	0139−5611	171	231
BD−03 2870	LFT 3734	Gl 382	127.08	1.90	5	M2 V	38	1012−0344	172	233
L 97-12	...	Gl 293	126.25	1.34	8	DQ9	52	0753−6747	173	234
L 1813-21	LHS 1805	...	126.1	3.3	75	M3.5 V	21	0601+5935	174	235
LP 876-10	...	...	126l	...	35,70	M4 V	70	2248−2422	175	236
L 674-15	...	Gl 300	125.60	0.97	12	M3.5 V	21	0812−2133	176	237
AC+65 6955	LFT 1552	Gl 793	125.07	1.08	5	M2.5 V	44	2030+6526	177	238
G 99-47	...	GJ 1087	125.0	3.6	6	DAP9	52	0556+0521	178	239
LP 467-16	...	...	125	...	32,73	M5 V	3	0111+1526	179	240
2MASS J12140866−2345172	...	...	125	...	32	M4.5 V	32	1214−2345	180	241
2MASS J19513587−3510375	...	...	125	...	32	M4 V	32	1951−3510	181	242
SCR J0838−5855	...	...	125	...	7	M6 V	7	0838−5855	182	243

Notes. Code for references: (1) this paper, (2) Marsh et al. 2012; (3) Kirkpatrick et al. 2011; (4) Cushing et al. 2011; (5) van Leeuwen 2007; (6) van Altena et al. 1995; (7) Winters et al. 2011; (8) Subasavage et al. 2009; (9) Drummond et al. 1995; (10) Riedel et al. 2011; (11) Boyd et al. 2011; (12) Henry et al. 2006; (13) Costa et al. 2006; (14) Scholz et al. 2005a; (15) Costa et al. 2005; (16) Benedict et al. 1999; (17) Jao et al. 2005; (18) Henry et al. 2002; (19) Hawley et al. 1996; (20) Henry et al. 2004; (21) Henry et al. 1994; (22) Lucas et al. 2010; (23) Artigau et al. 2010; (24) Hershey & Taff 1998; (25) Ducourant et al. 1998; (26) Schilbach et al. 2009; (27) Tinney 1996; (28) Burgasser et al. 2008; (29) Vrba et al. 2004; (30) Dahn et al. 2002; (31) Reid et al. 2003; (32) Riaz et al. 2006; (33) Scholz 2010; (34) Artigau et al. 2006; (35) Scholz et al. 2005b; (36) Reid et al. 2007; (37) Jenkins et al. 2009; (38) Kirkpatrick et al. 1991; (39) Kirkpatrick 1992; (40) Henry et al. 1992; (41) Boeshaar & Tyson 1985; (42) Kirkpatrick & McCarthy 1994; (43) Delfosse et al. 1999; (44) Hawley et al. 1996; (45) Delfosse et al. 1999; (46) Torres et al. 1999; (47) McCarthy et al. 1988; (48) Kirkpatrick et al. 1999; (49) Gray et al. 2003; (50) Gray et al. 2006; (51) Garrison 1994; (52) McCook & Sion 2006; (53) Burgasser et al. 2006a; (54) Kasper et al. 2007; (55) Kirkpatrick et al. 2008; (56) Bidelman 1985; (57) Forveille et al. 1999; (58) Gray et al. 2001; (59) Irwin et al. 1996; (60) Tomkin & Pettersen 1986; (61) Kirkpatrick et al. 2000; (62) Burgasser et al. 2010; (63) Kirkpatrick et al. 2010; (64) Henry & McCarthy 1993; (65) Reid et al. 1995; (66) Kirkpatrick et al. 1995; (67) Wilson & Vainu Bappu 1957; (68) Golimowski et al. 2000; (69) Reiners et al. 2007; (70) Reid et al. 2004; (71) J. E. Gizis 2012, priviate communication; (72) Reid et al. 2002; (73) Reid & Cruz 2002; (74) Gatewood & Coban 2009; (75) Khrutskaya et al. 2010; (76) Dupuy & Liu 2012; (77) G. N. Mace et al., in preparation; (78) Looper et al. 2007. ^aUnless otherwise marked, the parallax for the primary (or for the combined system) is used for all components of the system. ^bProxima Centauri is the third member of the α Centauri system. The error bar quoted here for the parallax is the updated one used in Jao et al. (2005). ^cThe spectral type is a joint type including all objects in the system. ^dThese spectral types are estimates based on the M_V values for the B and C components as measured by Delfosse et al. (1999) and translated into spectral type using Table 3 of Kirkpatrick & McCarthy (1994). ^eThis object is sometimes referred to as van Maanen 2, although in the original discovery paper (van Maanen 1917) it is neither named nor numbered. ^fWe estimate a distance by averaging the 7.1 pc estimate of Reid et al. (2007) and the 6 pc estimate of Riaz et al. (2006). ^gAccording to Luyten (1979), Innes discovered this object. However, Innes did not number his discoveries, so the discovery name is noted here simply as "Innes (unnumbered)." ^hThis is a composite type for G 208-44 AB (GJ 1245 AC). ⁱMcCarthy et al. (1988) give delta(V) ≈ 2.0 mag for the G 208-44 AB pair, so we estimate the spectral type of G 208-44 B to be approximately one subclass later than G 208-44 A (assumed to have a type identical to the composite spectral type of M5.5 V). ^jWe estimate a distance by averaging the 6.9 pc estimate of Scholz et al. (2005b) and the 6.2 pc estimate of Reid et al. (2002). ^kWe estimate a distance by averaging the 7.3 pc estimate of Scholz et al. (2005b) and the 6.7 pc estimate of Reid et al. (2002). ^lWe estimate a distance by averaging the 7.2 pc estimate of Reid et al. (2004) and the 8.7 pc estimate of Scholz et al. (2005b). ^mThis spectral type is a composite type for the Lalande 27173 BC pair. ⁿThis spectral type is estimated from the absolute J, H, K values measured by Forveille et al. (1999) and the absolute magnitudes vs. spectral type relation given in Table 3 of Kirkpatrick & McCarthy (1994). ^oThe parallax for 36 Oph A is assumed for 36 Oph C; an independent Hipparcos parallax for 36 Oph C is 167.49 ± 0.60 mas (van Leeuwen 2007). ^p2MASS J18450079−1409036 and 2MASS J18450097−1409053 appear to be a common proper motion pair based on Digitized Sky Survey R-band images taken in 1951 and again in 1988 (see http://irsa.ipac.caltech.edu/applications/FinderChart/). ^qHawley et al. (1997) say this is an M3 III but Luyten (1979) lists this pair as a common proper motion binary so the giant luminosity classification must be an error. ^rReid et al. (2004) state that they believe this parallax measurement may be in error because the result suggests a location on the H-R diagram significantly below the main sequence despite the fact that this M dwarf's spectrum shows no evidence of the low metallicity expected for such a location. ^sIdentification taken from van de Kamp (1930). ^tThis spectral type is the composite type for Wolf 630 ABaBb. ^uThe spectral type is estimated from the measured mass of this component (Ségransan et al. 2000) and a mapping of mass into spectral type using other objects in this table and their masses as measured in Henry & McCarthy (1993). ^vCosta et al. (2005) measure an independent parallax of 155.43+/−1.33 mas for van Biesbroeck 8. ^wvan Leeuwen (2007) measures a parallax value of 148.92 ± 4.00 mas; an independent Yale parallax gives 169.84 ± 6.6 mas (van Altena et al. 1995). ^xThis spectral type is based on delta J, H, K values measured by Henry & McCarthy (1993) and using the absolute magnitude vs. spectral types tabulate in Table 3 of Kirkpatrick & McCarthy (1994). ^yGiven that the mass ratio is ∼1 (Delfosse et al. 1999), we assume equal spectral types for both components. ^zSCR J1546−5534 has J − Ks = 1.10 mag from 2MASS; WISE photometry is corrupted by a brighter source immediately to the northwest (the Galactic latitude of this source is −0.8 deg) so we can only say that J-W2 < 3.65 and H-W2 < 2.99. The overall photometry from both 2MASS and WISE is consistent with a late-M dwarf. ^aaGiven that Delfosse et al. (1999) find nearly equal masses for components A and B and that component C is ∼0.5 mag fainter than the joint AB pair in adaptive optics imaging, we assume all components are roughly the same spectral type. ^bbIdentification taken from Hertzsprung (1922); Kapteyn's Star is also referred to as Cordoba 5h243 (van Maanen 1943). ^ccThe object LP 771-95 shares common proper motion with LP 771-96 AB. The parallax measured for LP 771-95 is assumed for LP 771-96 AB. ^ddThis is the composite spectral type for LP 771-96 AB. ^eeThis spectral type is estimated from the delta V, R, I values measured in Henry et al. (2006), the measured composite type for LP 771-96 AB, and spectral type vs. absolute magnitude relations given in Table 3 of Kirkpatrick & McCarthy (1994). ^ffRodgers & Eggen (1974) note peculiarities in the blue spectrum of this object. ^ggThese two objects share common proper motion. ^hhKuiper (1943) types this object one spectral subclass later than L 369-44; as Kuiper was probably typing on the Mt. Wilson system, we assign this object a type one subclass later than the type assigned for L 369-44 by Riaz et al. (2006). ⁱⁱBD+61 2068 is noted as a spectroscopic binary by Herbst & Layden (1987) (see also Heintz 1981). No other info is given, so an M spectral type is assumed for the secondary. ^jjThe spectral type is an estimate based on measured broadband colors. ^kkThe object LP 229-17 lies near on the sky and in distance to Vega. ^llMontagnier et al. (2006) show that this is a near equal-magnitude binary, so we estimate a spectral type identical to the joint spectrum. ^mmGJ 2005 D, a fourth component reported elsewhere, may not exist according to Seifahrt et al. (2008). ⁿⁿThis object is believed to be a white dwarf. ^ooThis spectral type is an estimate based on the measured absolute V magnitude. ^ppFomalhaut has common proper motion with LTT 9283 (Gl 879). ^qqThe object LTT 9283 has common proper motion with Fomalhaut but may lie slightly closer to the Sun than Fomalhaut itself. ^rrMarsh et al. (2012) report a parallax of 0087 ± 0054 for this object, whereas Kirkpatrick et al. (2011) report 0351 ± 0108. Given the discrepancies in this measurements, we instead use our spectrophotometric distance estimate from Table 8.

Download table as:  ASCIITypeset images: 1 2 3 4 5

Column 1 of Table 4 is intended to provide homage to the original discoverer or survey/mission responsible for first identifying the star as a nearby object. Exceptions are made in the case of stars with common names (e.g., Altair, Fomalhaut, and Vega), Bayer designations (e.g., α Cen A and B, p Eri AB), Flamsteed designations (e.g., 36 Oph ABC), or designations in old stellar catalogs (e.g., Lalande 21185, Lacaille 9352, AC+79 3888). In some cases, it is difficult to determine whether Willem Luyten or the Lowell Observatory group led by Henry Giclas was the first to discover an object because both groups were undergoing photographic proper motion surveys simultaneously. For such objects, the Luyten designation is used if the Lowell Observatory group lists one in its cross-references (Giclas et al. 1971, 1978), and the Giclas number is used if no Luyten designation is given.¹⁸ Column 2 lists alternate names.

Column 3 of Table 4 gives the running number in Gliese (1956, 1969) or Gliese & Jahreiß (1979). SIMBAD has made it common practice to identify objects from any of these papers with a prefix of "GJ," but this was originally meant for objects only from Gliese & Jahreiß (1979). Moreover, for new objects (identified only by "NN") in Gliese & Jahreiß (1991), SIMBAD has created its own numbering scheme; identifiers with GJ numbers higher than GJ 2159 are solely a SIMBAD creation.¹⁹ Gliese & Jahreiß (1991) do not provide catalog numbers for new objects nor are ones needed because all have published, well-recognized names. Such was not necessarily the case for earlier versions of the catalog—researchers in the early 1900's, notably Robert Innes, did not always affix numbers or names to their discoveries, and readers may not have had, as we do today, easy access to discovery papers. In deference to the intent of the original publications, we give a prefix of "Gl" to objects from Gliese (1956, 1969) and "GJ" only to those objects in Gliese & Jahreiß (1979). For other objects, the field in Column 3 is left blank.

Columns 4–6 of Table 4 give the measured trigonometric parallax, its error, and the reference for the measurement. If more than one group has measured the parallax, we list the published measurement with the smallest quoted error. For cases where the error in Column 5 is blank, the value in Column 4 is actually a spectrophotometric estimate based on the magnitude of the object and its spectral type. Columns 7 and 8 give the spectral type and its reference; cases where the spectral type is estimated are annotated as such. Column 9 provides an abbreviated sexagesimal J2000 position for the object in the form hhmm±ddss. Column 10 gives the rank of the system in distance from the Sun, and Column 11 gives the individual rank of each object; for example, Sirius A is in the fifth-closest stellar system to the Sun but is tied with its companion, Sirius B, as the seventh-closest star.

For reference, objects included in previous compilations of the 8 pc sample but now believed to lie beyond 8 pc are listed in Table 5. Among these is the intriguing multiple system ξ UMa (Alula Australis), in which Wright et al. (2012) have announced the discovery by WISE of a widely separated T8.5 companion.

Figure 11 graphically illustrates the 8 pc sample of Table 4 and shows that the solar neighborhood is dominated by M dwarfs. There are twice as many M dwarfs known as there are all other spectral types combined, although they comprise slightly less than half of the total stellar mass. Dwarfs of types L, T, and Y are much less common. L dwarfs are especially rare—only three examples are known within 8 pc—and represent a mix of old stars at the low-mass end of the stellar mass function and old brown dwarfs at the high-mass end of the substellar mass function.²⁰ The number of brown dwarfs then rises at later types—22 known T dwarfs and 8 known Y dwarfs are thought to lie within this 8 pc volume.

Zoom In Zoom Out Reset image size

The statistics for T and Y dwarfs are still incomplete, however. For T dwarfs, a few late-type isolated objects may yet be found, and it is expected that T dwarf companions to some of the higher mass stars will continue to be uncovered. The number of Y dwarfs is incomplete because follow-up of Y dwarf candidates from WISE is still in its infancy and because the coldest Y dwarfs are likely beyond the detection threshold of all existing surveys. As discussed in the next section, distances to the Y dwarfs are only now being measured for the first time, so many of the Y dwarf distances in Table 4 are estimates only.

We now concentrate on the low-mass tail of the field brown dwarf distribution in an updated attempt to determine the shape of the substellar mass function and its low-mass cutoff. As was done in Kirkpatrick et al. (2011), we focus on objects with spectral types of T6 or later. To sample a sufficiently large number of objects at these types, we consider distances larger than the 8 pc limit of the previous section, but we must keep in mind that samples should be reasonably complete (or completable) out to the distance limit we choose. Toward this end, we will use the depth of the WISE all-sky survey as the arbiter of the distance to which a complete census can be obtained, since it is the survey most capable of finding these coldest brown dwarfs. In Kirkpatrick et al. (2011) we found that a distance limit of 20 pc worked well for integral T6–T6.5, T7–T7.5, and T8–T8.5 bins. At T9–T9.5, it was shown that WISE may only fully sample the entire sky out to ∼15 pc, so this limit was chosen for that spectral bin. The limit for Y dwarfs was chosen to be 10 pc, which we retain here and discuss in more detail in the discussion that follows.

Many of the objects will not have trigonometric parallax measurements, so distances must be estimated spectrophotometrically, i.e., each object's apparent magnitude will be compared to the absolute magnitudes computed for similarly typed objects whose distances have been measured. Apparent magnitudes for these cold brown dwarfs are most easily measured from the ground in the J and H bands and from WISE at W2. Unfortunately, due to big differences in the J-band filters chosen for the two most popular filter systems (2MASS and the MKO-NIR system), fluxes can vary by several tenths of a magnitude for the same object (Stephens & Leggett 2004) because the spectral energy distributions of cold brown dwarfs are so complex at these same wavelengths. Fortunately, the H-band filters are very similar and as a result, H-band measurements show little variation between systems (Stephens & Leggett 2004). We will therefore use H and W2 photometry to estimate distances to objects lacking parallax information.

Table 6 presents a compilation of dwarfs that have measured trigonometric parallaxes, photometry at H and/or W2, and types later than T4. Trigonometric parallaxes for the Y dwarfs are taken from Marsh et al. (2012) and Beichman et al. (2012), although three objects from Marsh et al.—WISE 0359−5401, WISE 1541−2250, and WISE 2056+1459—are omitted here because their parallax values are roughly the size of the errors themselves. Unlike the other objects in these papers, these three objects lack measurements near the maximum parallax factor (or in the case of the WISE data points, have large astrometric uncertainties) and do not yet properly constrain the size of the parallactic motion.

Data in Table 6 are used to plot the absolute magnitude versus spectral type diagrams shown in Figures 12 and 13. Figure 12 shows a sharp drop in the absolute H magnitude near the T/Y transition. The absolute H-band magnitude for our latest object—the ⩾Y2 dwarf WISE 1828+2650—appears to indicate a stagnation or perhaps even a brightening in the H flux for later Y dwarfs relative to ones at Y0 and Y1. Figure 13 shows an even more surprising result: the absolute W2 magnitude plummets at Y0 and Y1 only to rebound appreciably for WISE 1828+2650 at ⩾Y2.

Zoom In Zoom Out Reset image size

Zoom In Zoom Out Reset image size

We suggest three possible scenarios to explain this observed behavior. (1) The parallax value for WISE 1828+2650 is the only one of the Y dwarf parallax measures robust enough to trust. In this case, the plummeting absolute magnitudes and Y0 and Y1 can be discounted until longer timeline astrometric monitoring of these objects has produced results with smaller measurement errors. (2) Despite their large errors, the Y0 and Y1 points indicate a pronounced dimming of the H and, more notably, W2 fluxes; the discrepant point for WISE 1828+2650 merely demonstrates that it (and not the other Y dwarfs) is the oddball, its weirdness being attributable to an unknown physical cause or misclassification due to a peculiar spectral morphology.²¹ (3) All trigonometric parallaxes are credible, and the observed behavior represents a real brightening of the fluxes for later Y dwarfs relative to ones at Y0–Y1.

It is clear that continued astrometric monitoring programs targeting Y dwarfs at improved precisions are critical in determining which of these scenarios is the correct one. For now, we perform weighted least-squares fits to the absolute magnitude versus spectral type diagrams with the caveat that they represent our best determinations at this time and will certainly have to be revised as future data become available. Third-order polynomials were fit to data in these diagrams both with and without WISE 1828+2650; for fits that included WISE 1828+2650, a spectral type of exactly Y2 was assumed for the object. For Figure 12, fits included the two upper limit M_H values by assuming that the limits measured in H band were actual detections with errors equal to the error in the H-band measurement of WISE 1828 (0.24 mag). Although this is an ad hoc assumption, we feel that it is better to fit (conservatively) to available data in that region rather than to drop the information entirely.

The resulting least-square fits to the data are given by the following equations:

$$\begin{eqnarray*} M_H &=& 20.272231 + 1.9695993({\rm type}) + 0.23810003({\rm type})^2\nonumber\\ &&+ 0.015161356({\rm type})^3, \end{eqnarray*}$$

which includes WISE 1828+2650 (red dashed curve in Figure 12) or

$$\begin{eqnarray*} M_H &=& 21.179419 + 2.9205146({\rm type}) + 0.53564210({\rm type})^2\nonumber\\ &&+ 0.043616246({\rm type})^3, \end{eqnarray*}$$

which excludes it (blue solid curve in Figure 12). Also,

$$\begin{eqnarray*} M_{W2} &=& 14.249389 + 0.60675032({\rm type}) + 0.12183371({\rm type})^2\nonumber\\ &&+ 0.014785180({\rm type})^3, \end{eqnarray*}$$

which includes WISE 1828+2650 (red dashed curve in Figure 13) or

$$\begin{eqnarray*} M_{W2} &=& 15.213242 + 1.5891486({\rm type}) + 0.42455282({\rm type})^2\nonumber\\ &&+ 0.043434368({\rm type})^3, \end{eqnarray*}$$

which excludes it (blue solid curve in Figure 13). In each equation, the spectral type is given by type = 0 for Y0, 1 for Y1, −1 for T9, −2 for T8, etc. These relations are considered valid only over the range from T7 to Y1.

For subsequent analyses we have used only the fits that exclude WISE 1828+2650 because these relations are needed solely to estimate distances to objects of earlier type than WISE 1828+2650 itself. In this case, we are explicitly assuming that scenario (1) above is incorrect and that either (2) or (3) is a more credible hypothesis. If we instead discover later that this assumption is incorrect, it will have the effect of increasing the distances to the Y0 and Y1 dwarfs, which will result in a reduction of the computed space density for objects at those types.

Using these fits, we have estimated distances for each of the objects identified in our all-sky census of brown dwarfs with types ⩾T6 (Table 7) using their measured (or assumed) spectral types and measured H and/or W2 magnitudes. These distance estimates are shown in Table 8.

Table 7. Photometry for Objects in the All-sky Late-T and Y Dwarf Census

Discovery Name	Disc.	WISE Designationa	Spec.	Type	H	H	W2	W1–W2	H–W2
	Ref.		Type	Ref.	(mag)	ref.	(mag)	(mag)	(mag)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
T6–T6.5 dwarfs
WISEPC J000849.76−173922.6	1	WISE J000849.75−173922.9	T6	1	17.77 ± 0.13	1	14.56 ± 0.07	1.86 ± 0.12	3.22 ± 0.15
2MASS J00345157+0523050	4	WISE J003452.02+052307.0	T6.5	5	15.44 ± 0.08	57	12.52 ± 0.03	2.54 ± 0.05	2.92 ± 0.09
WISE J003830.54+840517.7	2	WISE J003830.54+840517.7	T6	2	...	-	15.34 ± 0.09	2.19 ± 0.20	...
WISE J013525.64+171503.4	2	WISE J013525.64+171503.4	T6	2	...	-	14.74 ± 0.07	2.45 ± 0.17	...
WISEPA J022105.94+384202.9	1	WISE J022105.97+384203.2	T6.5	1	17.45 ± 0.15	1	14.70 ± 0.08	2.18 ± 0.17	2.76 ± 0.17
CFBDS J022638−072831	56	Not detected	T6.5	56	18.65 ± 0.02	56	...	...	...
2MASSI J0243137−245329	6	WISE J024313.47−245331.9	T6	5	15.14 ± 0.11	57	12.92 ± 0.03	1.75 ± 0.04	2.21 ± 0.11
CFBDS J025401−182529	46	WISE J025401.70−182528. 8	T6.5	46	18.49 ± 0.05	56	15.72 ± 0.12	>2.64	2.77 ± 0.13
UGCS J030013.86+490142.5	7	WISE J030013.76+490141.7	T6.5	7	18.37 ± 0.16	58	15.91 ± 0.20	>2.28	2.46 ± 0.26
CFBDS J030130−104504	46	WISE J030130.46−104504.1	T6	46	...	-	15.32 ± 0.11	1.72 ± 0.16	...
CFBDS J030225−144125	56	Not detected	T6	56	17.97 ± 0.04	56	...	...	...
WISEPA J030533.54+395434.4	1	WISE J030533.51+395434.6	T6	1	17.08 ± 0.12	1	14.69 ± 0.07	2.69 ± 0.25	2.39 ± 0.14
WISEPA J030724.57+290447.6	1	WISE J030724.59+290447.4	T6.5	1	17.70 ± 0.14	1	14.99 ± 0.11	2.23 ± 0.24	2.71 ± 0.18
CFHT J0344+3206b	55	Not detected	(T6:)	55	21.65 ± 0.08	55	...	...	...
WISEPA J041054.48+141131.6	1	WISE J041054.48+141131.1	T6	1	17.26 ± 0.12	1	15.08 ± 0.10	1.95 ± 0.19	2.19 ± 0.16
WISEPA J051317.28+060814.7	1	WISE J051317.27+060814.7	T6.5	1	16.13 ± 0.08	1	13.86 ± 0.05	1.97 ± 0.08	2.28 ± 0.09
WISEPA J052536.33+673952.3	1	WISE J052536.35+673952.6	T6p	1	17.87 ± 0.05	1	15.04 ± 0.09	>2.94	2.83 ± 0.11
SOri70 (J0538−0236)	8	Not detected	T6:	5	20.42 ± 0.11	8	...	...	...
WISEPA J054231.26−162829.1	1	WISE J054231.27−162829.1	T6.5	1	16.57 ± 0.10	1	13.98 ± 0.05	2.41 ± 0.10	2.59 ± 0.11
WISEPA J061213.93−303612.7	1	WISE J061213.85−303612. 5	T6	1	17.06 ± 0.11	1	14.03 ± 0.04	2.32 ± 0.08	3.03 ± 0.12
WISEPA J061407.49+391236.4	1	WISE J061407.49+391235.9	T6	1	16.36 ± 0.25	1	13.65 ± 0.04	2.83 ± 0.12	2.71 ± 0.25
WISEPA J062542.21+564625.5	1	WISE J062542.22+564625.4	T6	1	16.90 ± 0.10	1	14.38 ± 0.06	1.95 ± 0.10	2.52 ± 0.12
WISEPA J062720.07−111428.8	1	WISE J062720.07−111428.0	T6	1	15.44 ± 0.08	1	13.26 ± 0.03	1.74 ± 0.05	2.18 ± 0.08
WISE J073347.94+754439.2	2	WISE J073347.94+754439.2	T6	2	...	-	14.77 ± 0.07	2.39 ± 0.16	...
DENIS J081730.0−615520	9	WISE J081729.74−615504.0	T6	9	13.53 ± 0.03	57	11.24 ± 0.02	1.72 ± 0.03	2.29 ± 0.04
ULAS J081948.09+073323.3	10	Not detected	T6p	10	18.36 ± 0.03	10	...	...	...
ULAS J085342.94+000651.8	10	WISE J085342.83+000650.8	T6p	10	19.21 ± 0.06	58	15.79 ± 0.19	2.23 ± 0.42	3.42 ± 0.20
ULAS J085715.96+091325.3	10	not detected	T6	10	18.89 ± 0.10	10	...	...	...
WISEPC J092906.77+040957.9	1	WISE J092906.77+040957.9	T6.5	1	17.37 ± 0.07	1	14.23 ± 0.06	2.40 ± 0.13	3.14 ± 0.09
2MASSI J0937347+293142	6	WISE J093735.61+293127.7	T6p	5	14.70 ± 0.07	57	11.66 ± 0.02	2.42 ± 0.04	3.05 ± 0.07
WISEPC J095259.29+195507.3	1	WISE J095259.29+195508.1	T6	1	17.22 ± 0.10	1	14.34 ± 0.06	2.53 ± 0.17	2.88 ± 0.12
WISEPA J101905.63+652954.2	1	WISE J101905.62+652954.2	T6	1	16.52 ± 0.12	1	14.03 ± 0.04	2.39 ± 0.08	2.49 ± 0.12
ULAS J103434.52−001553.0	10	Not detected	T6.5p	10	19.00 ± 0.03	10	...	...	...
CFBDS J104209+580856	46	WISE J104209.85+580856.0	T6.5	46	18.21 ± 0.05	56	15.30 ± 0.10	1.95 ± 0.18	2.91 ± 0.11
2MASSI J1047538+212423	11	WISE J104752.37+212417.5	T6.5	5	15.80 ± 0.12	57	12.97 ± 0.03	2.46 ± 0.05	2.83 ± 0.12
WISEPC J112254.73+255021.5	1	WISE J112254.72+255022.2	T6	1	16.64 ± 0.11	1	13.97 ± 0.05	2.22 ± 0.10	2.67 ± 0.12
ULAS J115038.79+094942.9	12	Not detected	T6.5p	12	19.23 ± 0.06	12	...	...	...
ULAS J115338.74−014724.1	10	Not detected	T6	10	17.97 ± 0.02	10	...	...	...
NTTDF1205−0744	13	Not detected	T6:	5	...		...	...	...
ULAS J120744.65+133902.7	10	WISE J120744.63+133903.8	T6	10	18.52 ± 0.05	58	15.79 ± 0.18	>2.08	2.73 ± 0.18
2MASS J12095613−1004008B	52	Not detected	T6.5:	65	18.08 ± 0.26	52	...	...	...
SDSS J121440.95+631643.4B	47	Blended w/component A	(T6)	47	...	-	...	...	...
WISE J122558.86−101345.0	2	WISE J122558.86−101345.0	T6	2	16.46 ± 0.15	2	13.99 ± 0.05	2.35 ± 0.10	...
2MASS J12373919+6526148	11	WISE J123737.38+652608.4	T6.5	5	15.74 ± 0.15	57	12.95 ± 0.03	2.54 ± 0.05	2.79 ± 0.15
WISEPC J132004.16+603426.2	1	WISE J132004.16+603426.3	T6.5	1	16.56 ± 0.13	1	14.41 ± 0.05	2.52 ± 0.12	2.15 ± 0.14
ULAS J132605.18+120009.9	10	WISE J132605.25+120010.2	T6p	10	17.93 ± 0.09	58	15.38 ± 0.10	1.59 ± 0.16	2.55 ± 0.14
SDSSp J134646.45−003150.4	14	WISE J134646.07−003151.4	T6.5	5	15.46 ± 0.12	57	13.57 ± 0.03	1.92 ± 0.06	1.89 ± 0.12
ULAS J144555.24+125735.1	10	Not detected	T6.5	10	19.10 ± 0.05	10	...	...	...
ULAS J150457.66+053800.8c	51	WISE J150457.57+053759.8	T6:p	51	17.05 ± 0.03	51	14.23 ± 0.04	2.25 ± 0.09	2.32 ± 0.05
WISEPC J150649.97+702736.0	1	WISE J150649.98+702736.1	T6	1	13.91 ± 0.04	1	11.27 ± 0.02	2.12 ± 0.03	2.64 ± 0.04
ULAS J152526.25+095814.3	10	WISE J152526.19+095814.9	T6.5	10	19.17 ± 0.03	58	16.44 ± 0.22	>2.50	2.73 ± 0.22
ULAS J152912.23+092228.5	10	Not detected	T6	10	19.13 ± 0.05	10	...	...	...
2MASSI J1553022+153236A	6	WISE J155301.95+153238.8	T6.5	65	16.34 ± 0.03	65	13.02 ± 0.03g	2.28 ± 0.06g	...
WISEPA J161215.94−342027.1	1	WISE J161215.93−342028.5	T6.5	1	16.96 ± 0.03	45	13.96 ± 0.05	>4.23	3.00 ± 0.06
2MASS J16150413+1340079	15	WISE J161504.36+134004.2	T6	15	16.49 ± 0.25	57	14.19 ± 0.05	2.08 ± 0.10	2.30 ± 0.26
WISEPA J162208.94−095934.6	1	WISE J162208.94−095934.4	T6	1	16.05 ± 0.05	1	14.17 ± 0.06	2.34 ± 0.15	1.88 ± 0.08
SDSSp J162414.37+002915.6	16	WISE J162414.09+002915.6	T6	5	15.52 ± 0.10	57	13.09 ± 0.03	2.04 ± 0.05	2.44 ± 0.11
WISEPA J162725.64+325525.5	1,3	WISE J162725.65+325524.6	T6	1	16.40 ± 0.05	1	13.60 ± 0.04	2.65 ± 0.08	2.80 ± 0.06
WISE J172134.46+111739.4	2	WISE J172134.46+111739.4	T6	2	...	-	14.28 ± 0.06	1.62 ± 0.09	...
WISEPA J172844.93+571643.6	1	WISE J172844.93+571642.7	T6	1	17.88 ± 0.07	1	15.01 ± 0.05	2.94 ± 0.19	2.87 ± 0.09
WISE J174640.78−033818.0	2	WISE J174640.78−033818.0	T6	2	17.45 ± 0.04	2	14.79 ± 0.10	>3.23	2.66 ± 0.11
SDSS J175805.46+463311.9d	17	WISE J175805.47+463316.8	T6.5	5	16.25 ± 0.22	57	13.82 ± 0.03	1.86 ± 0.05	2.43 ± 0.22
SCR J1845−6357B	18	Blended w/SCR J1845−6357A	T6	19	...	-	...	...	...
WISEPA J190624.75+450808.2	1	WISE J190624.74+450807.1	T6	1	16.32 ± 0.09	1	13.82 ± 0.04	2.27 ± 0.07	2.51 ± 0.10
WISE J192841.35+235604.9	2	WISE J192841.35+235604.9	T6	2	...	-	12.11 ± 0.03	1.83 ± 0.04	...
2MASS J21543318+5942187	15	WISE J215432.95+594213.8	T6	15	15.77 ± 0.17	57	13.51 ± 0.03	2.14 ± 0.08	2.26 ± 0.17
Ind Bb (J2204−5646)	20	Blended w/ Ind Ba	T6	5	...	-	...	...	...
UDXS J221903.10+002418.2	54	Not detected	(T6:)	54	...	-	...	...	...
2MASS J22282889−4310262	21	WISE J222829.00−431029.5	T6	5	15.36 ± 0.12	57	13.33 ± 0.04	1.94 ± 0.06	2.04 ± 0.12
WISE J223720.39+722833.8	2	WISE J223720.39+722833.8	T6	2	...	-	13.61 ± 0.04	2.06 ± 0.07	...
WISE J230133.32+021635.1	2	WISE J230133.32+021635.1	T6.5	2	...	-	14.34 ± 0.06	1.96 ± 0.10	...
ULAS J230601.02+130225.0	10	WISE J230601.02+130225.3	T6.5	10	18.00 ± 0.02	58	15.07 ± 0.10	3.33 ± 0.51	2.94 ± 0.10
ULAS J231557.61+132256.2	10	WISE J231557.66+132255.5	T6.5	10	18.16 ± 0.05	58	15.47 ± 0.13	2.36 ± 0.34	2.69 ± 0.14
CFBDS J232304−015232	56	WISE J232304.41−015233.8	T6	56	17.46 ± 0.04	56	15.07 ± 0.11	1.61 ± 0.17	2.39 ± 0.12
WISE J234228.98+085620.2	2	WISE J234228.98+085620.2	T6.5	2	...	-	13.97 ± 0.05	2.10 ± 0.09	...
WISEPA J234351.20−741847.0	1	WISE J234351.20−741846.9	T6	1	>16.14	1	13.73 ± 0.04	2.01 ± 0.06	>2.41
WISE J235716.49+122741.8	2	WISE J235716.49+122741.8	T6	2	...	-	13.99 ± 0.05	1.85 ± 0.08	...
T7–T7.5 dwarfs
HD 3651B (J0039−2115)	22,23	Blended w/HD 3651A	T7.5	23	16.75 ± 0.16	22	...	...	...
WISE J004024.88+090054.8	2	WISE J004024.88+090054.8	T7	2	...	-	13.92 ± 0.07	2.14 ± 0.11	...
2MASS J00501994−3322402	24	WISE J005021.03−332228.9	T7	5	15.84 ± 0.19	57	13.55 ± 0.04	1.99 ± 0.06	2.29 ± 0.19
WISEPA J012333.21+414203.9	1	WISE J012333.23+414203.8	T7	1	17.20 ± 0.13	1	15.03 ± 0.07	2.01 ± 0.14	2.18 ± 0.15
ULAS J013939.77+004813.8	25	Not detected	T7.5	25	19.12 ± 0.05	25	...	...	...
ULAS J015024.37+135924.0	10	WISE J015024.39+135923.8	T7.5	10	18.11 ± 0.02	58	15.24 ± 0.09	2.75 ± 0.30	2.87 ± 0.10
WISEPC J022322.39−293258.1	1	WISE J022322.36−293257.1	T7.5	1	17.30 ± 0.11	1	14.03 ± 0.04	3.11 ± 0.13	3.27 ± 0.12
WISEPA J022623.98−021142.8	1	WISE J022623.98−021142.8	T7	1	18.84 ± 0.24	45	14.59 ± 0.06	3.01 ± 0.20	...
WISE J024124.73−365328.0	2	WISE J024124.73−365328.0	T7	2	16.98 ± 0.09	45	14.34 ± 0.04	2.55 ± 0.11	...
CFBDS J030135−161418	56	WISE J030135.16−161417.8	T7	56	18.99 ± 0.10	56	15.59 ± 0.10	3.07 ± 0.41	3.40 ± 0.14
WISE J032547.72+083118.2	2	WISE J032547.72+083118.2	T7	2	16.15 ± 0.08	45	13.49 ± 0.04	1.95 ± 0.07	2.66 ± 0.09
2MASS J03480772−602227	21	WISE J034807.33−602234.9	T7	5	15.56 ± 0.14	57	12.54 ± 0.02	2.47 ± 0.04	3.02 ± 0.15
WISEPA J052844.51−330823.9	1	WISE J052844.51−330823.9	T7p	1	16.97 ± 0.14	1	14.60 ± 0.06	3.13 ± 0.24	2.37 ± 0.15
UGCS J053022.52−052447.4	7	Not detected	T7:	7	19.13 ± 0.29	7	...	...	...
Gl229B (J0610−2152)	27	Blended w/Gl 229A	T7p	5	∼14.3	63	...	...	...
WISE J061437.73+095135.0	2	WISE J061437.73+095135.0	T7	2	16.82 ± 0.10	45	14.29 ± 0.07	2.63 ± 0.20	2.53 ± 0.12
2MASSI J0727182+171001	6	WISE J072719.13+170951.6	T7	5	15.76 ± 0.17	57	12.96 ± 0.03	2.28 ± 0.06	2.79 ± 0.17
ULAS J085910.69+101017.1	12	WISE J085910.63+101014.8	T7	12	18.58 ± 0.06	58	15.28 ± 0.14	2.44 ± 0.35	3.30 ± 0.15
ULAS J090116.23−030635.0	28	WISE J090116.21−030636.0	T7.5	28	18.46 ± 0.13	58	14.60 ± 0.07	3.17 ± 0.32	3.86 ± 0.15
CFBDS J092250+152741	46	Not detected	T7	46	18.81 ± 0.10	56	...	...	...
ULAS J094806.06+064805.0	28	Not detected	T7	28	19.46 ± 0.22	28	...	...	...
WISE J103907.73−160002.9	2	WISE J103907.73−160002.9	T7.5	2	17.19 ± 0.20	45	14.16 ± 0.05	2.49 ± 0.12	3.03 ± 0.21
2MASS J11145133−2618235	24	WISE J111448.79−261827.7	T7.5	5	15.73 ± 0.12	57	12.24 ± 0.03	3.13 ± 0.06	3.50 ± 0.13
WISE J112438.12−042149.7	2	WISE J112438.12−042149.7	T7	2	...	-	14.05 ± 0.05	2.51 ± 0.13	...
2MASSI J1217110−031113	11	WISE J121710.30−031112.1	T7.5	5	15.75 ± 0.12	57	13.20 ± 0.04	2.09 ± 0.06	2.55 ± 0.12
WISP J1232−0033	68	Not detected	T7	68	...	-	...	...	...
ULAS J124804.56+075904.0	10	WISE J124804.49+075903.5	T7	10	18.15 ± 0.08	58	15.37 ± 0.13	1.91 ± 0.24	2.78 ± 0.15
Kelu-1 Abh (J1305−2541)	60	Blended w/components Aa,B	(T7.5)	60	...	-	...	...	...
ULAS J131508.42+082627.4	12	Not detected	T7.5	12	19.50 ± 0.10	12	...	...	...
ULAS J134940.81+091833.3	10	Not detected	T7	10	19.43 ± 0.03	10	...	...	...
ULAS J141623.94+134836.3	29	WISE J141623.94+134836.0	T7.5	30	17.58 ± 0.03	58	12.79 ± 0.04	3.33 ± 0.20	4.79 ± 0.05
WISEPC J145715.03+581510.2	1	WISE J145715.03+581510.2	T7	1	16.64 ± 0.29	1	14.47 ± 0.04	2.36 ± 0.09	2.17 ± 0.29
Gl570D (J1457−2122)	31	WISE J145715.84−212207.9	T7.5	5	15.27 ± 0.09	57	12.11 ± 0.02	2.71 ± 0.04	3.15 ± 0.09
SDSS J150411.63+102718.4	32	WISE J150411.80+102715.7	T7	32	...	-	14.06 ± 0.04	2.33 ± 0.08	...
WISE J152305.10+312537.6	2	WISE J152305.10+312537.6	T7 p	2	18.69 ± 0.18	45	14.39 ± 0.04	3.52 ± 0.22	4.30 ± 0.18
WISE J154459.27+584204.5	2	WISE J154459.27+584204.5	T7.5	2	18.34 ± 0.29	45	15.03 ± 0.06	3.36 ± 0.31	3.31 ± 0.30
2MASSI J1553022+153236B	5	Blended w/component A	T7.5	65	16.72 ± 0.03	65	...	...	...
SDSS J162838.77+230821.1	32	WISE J162839.00+230818.0	T7	32	16.11 ± 0.15	57	13.96 ± 0.04	2.47 ± 0.10	2.15 ± 0.16
WISEPA J185215.78+353716.3	1	WISE J185215.76+353716.7	T7	1	>17.41	1	14.24 ± 0.05	2.31 ± 0.11	>3.17
WISE J201404.13+042408.5	2	WISE J201404.13+042408.5	T7 p	2	18.66 ± 0.30	45	15.16 ± 0.12	>2.78	3.50 ± 0.32
WISEPA J201824.96−742325.9	26	WISE J201824.97−742327.5	T7	26	17.17 ± 0.04	-	13.62 ± 0.04	2.92 ± 0.11	3.55 ± 0.06
WISEPC J215751.38+265931.4	1	WISE J215751.35+265931.4	T7	1	17.45 ± 0.04	1	14.48 ± 0.06	2.65 ± 0.16	2.97 ± 0.07
WISEPC J220922.10−273439.5	1	WISE J220922.11−273439.6	T7	1	>16.41	1	13.84 ± 0.05	2.66 ± 0.12	>2.57
WISEPC J221354.69+091139.4	1	WISE J221354.68+091139.4	T7	1	17.09 ± 0.11	1	14.60 ± 0.07	2.10 ± 0.13	2.49 ± 0.13
UDXS J221611.51+003308.1	54	Not detected	(T7.5:)	54	...	-	...	...	...
WISEPC J231939.13−184404.3	1	WISE J231939.14−184404.4	T7.5	1	17.95 ± 0.05	1	13.76 ± 0.05	3.39 ± 0.17	4.19 ± 0.07
ULAS J232123.79+135454.9	33	WISE J232123.83+135453.5	T7.5	10	17.15 ± 0.03	58	14.10 ± 0.06	3.21 ± 0.22	3.05 ± 0.06
ULAS J232802.03+134544.8	10	WISE J232802.12+134545.3	T7	10	18.17 ± 0.02	58	15.39 ± 0.13	2.61 ± 0.40	2.78 ± 0.13
WISE J233543.79+422255.2	2	WISE J233543.79+422255.2	T7	2	...	-	15.31 ± 0.10	3.24 ± 0.52	...
WISEPC J234026.62−074507.2	1	WISE J234026.62−074508.1	T7	1	16.19 ± 0.06	1	13.58 ± 0.04	2.37 ± 0.09	2.61 ± 0.07
WISEPC J234841.10−102844.4	1	WISE J234841.10−102844.1	T7	1	16.93 ± 0.12	1	14.40 ± 0.06	2.49 ± 0.16	2.53 ± 0.14
T8–T8.5 dwarfs
WISE J001505.87−461517.6	2	WISE J001505.87−461517.6	T8	2	...	-	14.25 ± 0.06	2.77 ± 0.16	...
WISE J003231.09−494651.4	2	WISE J003231.09−494651.4	T8.5	2	...	-	15.07 ± 0.09	3.01 ± 0.35	...
ULAS J003402.77−005206.7	35	WISE J003402.78−005208.1	T8.5	36	18.49 ± 0.04	58	14.50 ± 0.08	2.97 ± 0.30	3.99 ± 0.09
WISE J004945.61+215120.0	2	WISE J004945.61+215120.0	T8.5	2	...	-	12.97 ± 0.03	2.50 ± 0.05	...
CFBDS J005910.90−011401.3	37	WISE J005911.08−011400.9	T8.5	36	18.27 ± 0.05	59	13.68 ± 0.04	3.39 ± 0.16	4.59 ± 0.07
CFBDS J013302+023128	56	WISE J013302.44+023128.9	T8.5	56	18.62 ± 0.10	56	15.10 ± 0.09	2.69 ± 0.28	3.52 ± 0.14
WISE J024512.62−345047.8	2	WISE J024512.62−345047.8	T8	2	...	-	14.56 ± 0.06	3.36 ± 0.32	...
WISE J024714.52+372523.5	2	WISE J024714.52+372523.5	T8	2	18.24 ± 0.19	2	14.70 ± 0.08	>3.67	3.54 ± 0.21
WISEPA J025409.45+022359.1	1,42	WISE J025409.51+022358.6	T8	1	16.29 ± 0.04	1	12.74 ± 0.03	3.02 ± 0.06	3.55 ± 0.05
WISEPA J031325.96+780744.2	1	WISE J031325.94+780744.3	T8.5	1	17.63 ± 0.06	1	13.19 ± 0.03	2.69 ± 0.07	4.45 ± 0.07
WISE J031624.35+430709.1	2	WISE J031624.35+430709.1	T8	2	19.70 ± 0.09	45	14.56 ± 0.07j	>3.30j	5.14 ± 0.11j
WISE J032120.91−734758.8	2	WISE J032120.91−734758.8	T8	2	19.06 ± 0.12	2	15.60 ± 0.08	>3.59	...
WISEPC J032337.53−602554.9	1	WISE J032337.53−602554.5	T8.5	1	18.40 ± 0.02	1	14.50 ± 0.05	3.61 ± 0.33	3.90 ± 0.06
WISE J033605.05−014350.4	2	WISE J033605.05−014350.4	T8::	2	...	-	14.54 ± 0.07	>3.423	...
2MASSW J0337036−175807B	53	Blended w/component A	(T8??)	53	...	-	...	...	...
2MASSI J0415195−093506	6	WISE J041521.21−093500.6	T8	5	15.54 ± 0.11	57	12.26 ± 0.03	2.85 ± 0.05	3.28 ± 0.12
WISEPA J045853.89+643452.9A	34	WISE J045853.89+643452.5	T8.5	61	17.41 ± 0.06g	1	13.03 ± 0.03g	3.64 ± 0.12g	4.38 ± 0.07g
WISEPA J050003.05−122343.2	1	WISE J050003.04−122343.2	T8	1	18.13 ± 0.12	1	13.94 ± 0.04	3.72 ± 0.25	4.19 ± 0.13
WISEPA J062309.94−045624.6	1	WISE J062309.94−045624.6	T8	1	17.31 ± 0.11	1	13.82 ± 0.04	3.52 ± 0.20	3.50 ± 0.12
2MASS J07290002−3954043	15	WISE J072859.49−395345.7	T8p	15	15.98 ± 0.18	57	12.96 ± 0.03	2.29 ± 0.05	3.02 ± 0.19
WISEPA J074457.15+562821.8	1	WISE J074457.25+562821.0	T8	1	17.59 ± 0.12	1	14.49 ± 0.06	2.59 ± 0.16	3.10 ± 0.13
WISEPA J075003.84+272544.8	1	WISE J075003.78+272545.4	T8.5	1	19.00 ± 0.06	1	14.46 ± 0.07	>3.65	4.54 ± 0.09
WISEPC J075946.98−490454.0	1	WISE J075946.98−490454.0	T8	1	17.41 ± 0.04	45	13.86 ± 0.04	>4.05	3.55 ± 0.05
WISE J081220.04+402106.2	2	WISE J081220.04+402106.2	T8	2	18.30 ± 0.20	2	15.08 ± 0.10	3.16 ± 0.48	3.22 ± 0.22
WISEPC J083641.12−185947.2	1	WISE J083641.10−185947.0	T8p	1	18.79 ± 0.26	45	15.18 ± 0.10	>3.23	3.61 ± 0.28
WISEPA J085716.25+560407.6	1	WISE J085716.24+560407.6	T8	1	17.49 ± 0.14	1	14.11 ± 0.05	3.37 ± 0.22	3.38 ± 0.15
WISEPA J090649.36+473538.6	1	WISE J090649.35+473538.5	T8	1	17.81 ± 0.16	1	14.65 ± 0.08	2.83 ± 0.24	3.17 ± 0.18
2MASS J09393548−2448279	24	WISE J093935.91−244838.5	T8	5	15.78 ± 0.15	57	11.64 ± 0.02	3.39 ± 0.05	4.16 ± 0.15
ULAS J101721.40+011817.9	38	Not detected	T8p	38	19.07 ± 0.02	38	...	...	...
WISEPC J101808.05−244557.7	1	WISE J101808.04−244557.9	T8	1	18.00 ± 0.23	45	14.17 ± 0.05	3.21 ± 0.22	3.83 ± 0.24
CFBDS J102841+565401e	46	Not detected	T8	46	18.38 ± 0.08	56	...	...	...
WISEPC J104245.23−384238.3	1	WISE J104245.23−384238.3	T8.5	1	19.08 ± 0.11	45	14.52 ± 0.06	>4.06	4.56 ± 0.13
ξ UMa C (J1118+3125)	67	WISE J111838.70+312537.9	T8.5	67	18.15 ± 0.06	67	13.31 ± 0.03	2.85 ± 0.08	2.28 ± 0.06
WISEPC J115013.88+630240.7	1	WISE J115013.85+630241.5	T8	1	>18.01	1	13.40 ± 0.03	3.59 ± 0.11	>4.61
2MASS J12255432−2739466B	64	Blended w/component A	T8	64,65	16.91 ± 0.03	65	...	...	...
ULAS J123828.51+095351.3	38	WISE J123828.38+095352.1	T8	36	19.20 ± 0.02	58	15.22 ± 0.12	>2.79	3.98 ± 0.12
Ross458C (J1300+1221)	39	WISE J130041.65+122114.6	T8	36	17.01 ± 0.04	58	13.74 ± 0.04	2.27 ± 0.08	3.27 ± 0.06
ULAS J130217.21+130851.2	10	WISE J130217.08+130851.0	T8	36	18.60 ± 0.06	58	14.95 ± 0.10	>2.66	3.65 ± 0.11
WISEPA J132233.66−234017.1	1,3	WISE J132233.64−234016.8	T8	1	16.61 ± 0.14	1	13.93 ± 0.04	3.06 ± 0.14	2.68 ± 0.15
ULAS J133553.45+113005.2	38	WISE J133553.41+113004.8	T8.5	36	18.25 ± 0.01	58	13.87 ± 0.04	3.01 ± 0.13	4.39 ± 0.04
WISE J143311.42−083736.4	2	WISE J143311.42−083736.4	T8::	2	19.42 ± 0.21	2	15.23 ± 0.10	>3.51	4.19 ± 0.23
WISEPA J143602.19−181421.8	1	WISE J143602.20−181421.9	T8p	1	>17.62	45	14.71 ± 0.06	2.50 ± 0.16	>2.91
CFBDSIR J145829+101343A	44	WISE J145829.40+101341.7	T8.5	45i	20.18 ± 0.10	66	15.66 ± 0.12g	>3.15g	...
WISE J151721.13+052929.3	2	WISE J151721.13+052929.3	T8	2	18.85 ± 0.15	58	15.13 ± 0.08	>2.97	3.72 ± 0.17
WISEPC J151906.64+700931.5	1	WISE J151906.63+700931.4	T8	1	18.28 ± 0.07	1	14.14 ± 0.03	3.03 ± 0.10	4.15 ± 0.08
WISEPA J161705.75+180714.3	26	WISE J161705.74+180714.2	T8	26	18.23 ± 0.08	1	14.16 ± 0.05	2.96 ± 0.16	4.08 ± 0.09
WISEPA J165311.05+444423.9	1,3	WISE J165311.05+444422.8	T8	1	17.53 ± 0.05	1	13.81 ± 0.04	2.68 ± 0.08	3.72 ± 0.06
WISEPA J171104.60+350036.8	1	WISE J171104.60+350036.8	T8	1	>18.12	1	14.72 ± 0.06	>3.43	>3.40
WISEPA J171717.02+612859.3	1	WISE J171717.02+612859.3	T8	1	18.91 ± 0.09	1	15.09 ± 0.05	3.33 ± 0.20	3.83 ± 0.10
WISE J180901.07+383805.4	2	WISE J180901.07+383805.4	T8	2	...	-	15.18 ± 0.08	>2.84	...
WISEPA J181210.85+272144.3	26	WISE J181210.85+272144.3	T8.5:	1	18.83 ± 0.16	1	14.23 ± 0.05	3.58 ± 0.29	4.60 ± 0.17
WISEPA J195905.66−333833.7	1	WISE J195905.65−333833.5	T8	1	17.18 ± 0.05	1	13.88 ± 0.05	2.56 ± 0.11	3.30 ± 0.07
WISEPC J201546.27+664645.1f	2	Blended w/nearby source	T8	2	17.66 ± 0.23	2	14.68 ± 0.06	2.02 ± 0.11	1.82 ± 0.11
WISE J201920.76−114807.6	2	WISE J201920.76−114807.6	T8.5:	2	18.32 ± 0.11	2	14.32 ± 0.06	2.96 ± 0.22	3.89 ± 0.11
Wolf 940B (J2146−0010)	40	WISE J214638.99−001039.6	T8.5	36	18.77 ± 0.03	58	14.24 ± 0.05	2.49 ± 0.13	4.53 ± 0.06
WISEPC J222623.05+044003.9	1	WISE J222623.05+044004.0	T8	1	16.95 ± 0.17	45	14.71 ± 0.09	2.58 ± 0.24	2.24 ± 0.19
WISEPC J225540.74−311841.8	1	WISE J225540.75−311842.0	T8	1	17.70 ± 0.11	1	14.18 ± 0.06	2.74 ± 0.18	3.52 ± 0.12
WISEPA J231336.40−803700.3	26	WISE J231336.38−803700.2	T8	26	17.28 ± 0.14	45	13.64 ± 0.03	2.65 ± 0.07	3.64 ± 0.14
T9–T9.5 dwarfs
WISE J000517.48+373720.5	2	WISE J000517.48+373720.5	T9	2	...	-	13.27 ± 0.03	3.61 ± 0.12	...
WISE J003829.05+275852.1	2	WISE J003829.05+275852.1	T9	2	18.92 ± 0.04	45	14.38 ± 0.05	3.67 ± 0.29	4.54 ± 0.06
WISEPC J014807.25−720258.7	1,36	WISE J014807.25−720258.7	T9.5	1	19.22 ± 0.04	1	14.69 ± 0.05	>4.25	4.53 ± 0.07
WISE J032517.69−385454.1	2	WISE J032517.69−385454.1	T9	2	...	-	14.98 ± 0.06	3.47 ± 0.31	...
WISE J033515.01+431045.1	2	WISE J033515.01+431045.1	T9::	2	19.60 ± 0.26	45	14.60 ± 0.08	>3.55	5.00 ± 0.27
WISE J041358.14−475039.3	2	WISE J041358.14−475039.3	T9	2	20.12 ± 0.20	2	15.69 ± 0.08	>3.70	...
WISEPA J045853.89+643452.9B	3	Blended w/component A	T9.5	61	...	-	...	...	...
UGPS J072227.51−054031.2	43	WISE J072227.27−054029.9	T9	36	16.15 ± 0.21	57	12.21 ± 0.03	2.97 ± 0.06	3.93 ± 0.21
WISE J072312.44+340313.5	2	WISE J072312.44+340313.5	T9:	2	>18.47	2	14.73 ± 0.08	>3.54	>3.74
WISEPA J075108.79−763449.6	1	WISE J075108.80−763449.5	T9	1	>19.02	1	14.52 ± 0.04	3.01 ± 0.14	>4.50
WISE J081117.81−805141.3	2	WISE J081117.81−805141.3	T9.5:	2	19.88 ± 0.21	2	14.38 ± 0.04	2.91 ± 0.13	...
WISE J105130.01−213859.7	2	WISE J105130.01−213859.7	T9:	2	19.19 ± 0.39	2	14.54 ± 0.06	2.63 ± 0.18	...
WISEPC J121756.91+162640.2	1	WISE J121756.90+162640.8	T9	1	18.18 ± 0.05	1	13.09 ± 0.03	3.71 ± 0.14	5.09 ± 0.06
WISP J1305−2538	68	Not detected	T9.5+	68	...	-	...	...	...
WISEPC J131106.24+012252.4	1	WISE J131106.20+012254.3	T9:	1	19.32 ± 0.23	45	14.76 ± 0.09	3.50 ± 0.47	4.56 ± 0.25
WISE J131833.98−175826.5	2	WISE J131833.98−175826.5	T9:	2	17.71 ± 0.23	2	14.75 ± 0.07	3.35 ± 0.35	2.96 ± 0.24
CFBDSIR J145829+101343B	50	Blended w/A component	T9.5	45	22.51 ± 0.16	66	...	...	...
WISE J154214.00+223005.2	2	WISE J154214.00+223005.2	T9.5	2	21.80 ± 0.80	2	15.02 ± 0.06	>3.86	6.78 ± 0.80
WISEPA J161441.45+173936.7	1,3	WISE J161441.46+173935.5	T9	1	18.47 ± 0.22	1	14.25 ± 0.05	>3.65	4.22 ± 0.22
WISEPA J174124.26+255319.5	1,3,42	WISE J174124.25+255319.6	T9	1,42	16.63 ± 0.03	1	12.33 ± 0.03	3.05 ± 0.06	4.30 ± 0.04
WISEPA J180435.40+311706.1	1	WISE J180435.37+311706.4	T9.5:	1	19.21 ± 0.11	1	14.70 ± 0.06	>3.94	4.51 ± 0.13
WISE J210200.15−442919.5	41	WISE J210200.15−442919.5	T9	41	18.39 ± 0.12	45	14.12 ± 0.05	2.83 ± 0.18	4.26 ± 0.09
WISEPA J213456.73−713743.6	1	WISE J213456.73−713744.5	T9p	1	19.81 ± 0.12	45	13.99 ± 0.05	>3.75	5.82 ± 0.13
WISEPC J232519.54−410534.9	1	WISE J232519.53−410535.0	T9p	1	19.22 ± 0.11	1	14.13 ± 0.05	3.47 ± 0.25	5.09 ± 0.12
WISE J233226.49−432510.6	41	WISE J233226.49−432510.6	T9:	41	19.40 ± 0.18	45	14.99 ± 0.09	>2.89	4.41 ± 0.20
WISEPC J234446.25+103415.8	1	WISE J234446.23+103415.6	T9	1	19.07 ± 0.11	1	15.11 ± 0.12	>2.92	3.96 ± 0.16
Y dwarfs
WISE J014656.66+423410.0	2	WISE J014656.66+423410.0	Y0	2	18.71 ± 0.24	45	15.08 ± 0.07	>3.91	3.63 ± 0.25
WISE J035000.32−565830.2	45	WISE J035000.32−565830.2	Y1	45	>21.5	45	14.73 ± 0.06	>4.17	>6.8
WISE J035934.06−540154.6	45	WISE J035934.06−540154.6	Y0	45	22.20 ± 0.43	45	15.42 ± 0.07	>3.87	6.78 ± 0.44
WISEPA J041022.71+150248.5	1,36	WISE J041022.71+150248.4	Y0	36	19.05 ± 0.09	1	14.18 ± 0.06	>4.15	4.87 ± 0.11
WISE J053516.80−750024.9	45	WISE J053516.80−750024.9	⩾Y1	45	>21.6	45	15.06 ± 0.07	>3.86	>6.5
WISE J071322.55−291751.9	45	WISE J071322.55−291751.9	Y0	45	>19.3	-	14.48 ± 0.06	>3.87	>4.8
WISE J073444.02−715744.0	45	WISE J073444.02−715744.0	Y0	45	...	-	15.36 ± 0.06	>4.06	...
WD 0806−661B	48	Not detected	(Y?)	49	...	-	...	...	...
WISEPC J140518.40+553421.4	1,36	WISE J140518.39+553421.3	Y0p	36	>20.5	1	14.10 ± 0.04	>4.72	>6.4
WISEPA J154151.66−225025.2	1,36	WISE J154151.65−225024.9	Y0.5	36	>20.2	1	14.25 ± 0.06	2.49 ± 0.18	>6.0
WISEPA J173835.53+273258.9	1,36	WISE J173835.53+273259.0	Y0	36	20.39 ± 0.33	1	14.55 ± 0.06	>3.86	5.84 ± 0.34
WISEPA J182831.08+265037.8	1,36	WISE J182831.08+265037.7	⩾Y2	45	22.85 ± 0.24	1	14.39 ± 0.06	>4.08	8.46 ± 0.25
WISEPC J205628.90+145953.3	1,36	WISE J205628.91+145953.2	Y0	36	19.62 ± 0.31	1	13.93 ± 0.05	>4.33	5.69 ± 0.31
WISE J222055.31−362817.4	45	WISE J222055.31−362817.4	Y0	45	20.81 ± 0.30	45	14.66 ± 0.06	>3.99	...

Notes. Code for references: (1) Kirkpatrick et al. 2011; (2) G. N. Mace et al., in preparation; (3) Gelino et al. 2011; (4) Burgasser et al. 2004; (5) Burgasser et al. 2006a; (6) Burgasser et al. 2002; (7) Lodieu et al. 2009; (8) Zapatero Osorio et al. 2002; (9) Artigau et al. 2010; (10) Burningham et al. 2010; (11) Burgasser et al. 1999; (12) Pinfield et al. 2008; (13) Cuby et al. 1999; (14) Tsvetanov et al. 2000; (15) Looper et al. 2007; (16) Strauss et al. 1999; (17) Knapp et al. 2004; (18) Biller et al. 2006; (19) Kasper et al. 2007; (20) Scholz et al. 2003; (21) Burgasser et al. 2003c; (22) Mugrauer et al. 2006; (23) Luhman et al. 2007; (24) Tinney et al. 2005; (25) Chiu et al. 2008; (26) Burgasser et al. 2011; (27) Nakajima et al. 1995; (28) Lodieu et al. 2007; (29) Scholz 2010; (30) Burgasser et al. 2010; (31) Burgasser et al. 2000a; (32) Chiu et al. 2006; (33) Scholz 2010; (34) Mainzer et al. 2011; (35) Warren et al. 2007; (36) Cushing et al. 2011; (37) Delorme et al. 2008; (38) Burningham et al. 2008; (39) Goldman et al. 2010; (40) Burningham et al. 2009; (41) C. G. Tinney et al., in preparation; (42) Scholz et al. 2011; (43) Lucas et al. 2010; (44) Delorme et al. 2010; (45) This paper, (46) Reylé et al. 2010; (47) Geißler et al. 2011; (48) Luhman et al. 2011; (49) Luhman et al. 2012; (50) Liu et al. 2011; (51) Murray et al. 2011; (52) Liu et al. 2010; (53) Stumpf et al. 2010; (54) Lodieu et al. 2009; (55) Burgess et al. 2009; (56) Albert et al. 2011; (57) 2MASS, (58) UKIDSS, (59) CFBDS, (60) Stumpf et al. 2008; (61) Burgasser et al. 2012; (62) Burgasser et al. 2006b; (63) Matthews et al. 1996; (64) Burgasser et al. 2003b; (65) Dupuy & Liu 2012; (66) Liu et al. 2011; (67) Wright et al. 2012; (68) Masters et al. 2012. ^aWISE sources are given designations as follows. The prefix is "WISE" for sources taken from the four-band cryogenic atlas source catalog, "WISER" for sources taken from the four-band cryogenic atlas source reject table, "WISEPC" for sources taken from the first-pass processing operations co-add Source Working Database, or "WISEPA" for objects drawn from the preliminary release Atlas Tile Source Working Database. The suffix is the J2000 position of the source in the format Jhhmmss.ss±ddmmss.s. ^bAlso known as IC348 CH4 2 034449.52+320635.4. ^cAlso known as HIP 73786B or Gl 576B. ^dThis is a companion to G 204-39 from Faherty et al. (2010), d = 13.6 pc. ^eObject is seen on the WISE images but is not successfully extracted. ^fObject is not detected by WISE Pass2 processing, so the quoted WISE photometry comes from Pass1. ^gThese values represent the combined light of the composite system. ^hThis object may not exist. ⁱCushing et al. (2011) assigns this binary a composite type of T9 on the revised late-T dwarf classification scheme. Given the Dupuy & Liu (2012) measurements of the parallax and the Liu et al. (2011) H-band measurements of the individual components, we infer spectral types of T8.5 and T9.5 based on absolute H magnitudes of 17.8 and 20.2 mag. ^jSpitzer/IRAC follow-up of this sources shows that the WISE photometry is blended with a bright, nearby source.

Download table as:  ASCIITypeset images: 1 2 3 4