A Search for L/T Transition Dwarfs With Pan-STARRS1 and WISE. III. Young L Dwarf Discoveries and Proper Motion Catalogs in Taurus and Scorpius-Centaurus

TL;DR

This paper reports the discovery of young L and M dwarfs in Taurus and Scorpius-Centaurus, including the lowest mass free-floating objects, and provides proper motion catalogs to aid in understanding their formation and membership.

Contribution

It introduces new young L and M dwarf discoveries with detailed characterization and proper motion data, enhancing knowledge of low-mass objects in star-forming regions.

Findings

Discovery of the coolest Taurus L2 dwarf to date.

Identification of free-floating planetary-mass objects (~6 M_Jup).

Compilation of precise proper motion catalogs for low-mass members.

Abstract

We present the discovery of eight young M7-L2 dwarfs in the Taurus star-forming region and the Scorpius-Centaurus OB Association, serendipitously found during a wide-field search for L/T transition dwarfs using Pan-STARRS1 (optical) and WISE (mid-infrared) photometry. We identify PSO J060.3200+25.9644 (near-infrared spectral type L1) and PSO J077.1033+24.3809 (L2) as new members of Taurus based on their VL-G gravity classifications, the consistency of their photometry and proper motions with previously known Taurus objects, and the low probability of contamination by field objects. PSO J077.1033+24.3809 is the coolest substellar member of Taurus found to date. Both Taurus objects are among the lowest mass free-floating objects ever discovered, with estimated masses $\approx$6 M$_{\rm Jup}$, and provide further evidence that isolated planetary-mass objects can form as part of normal star-formation processes. PSO J060.3200+25.9644 (a.k.a. DANCe J040116.80+255752.2) was previously identified as a likely member of the Pleiades (age $\approx125$ Myr) based on photometry and astrometry, but its VL-G gravity classification and near-infrared photometry imply a much younger age and thus point to Taurus membership. We have also discovered six M7-L1 dwarfs in outlying regions of Scorpius-Centaurus with photometry, proper motions, and low-gravity spectral signatures consistent with membership. These objects have estimated masses $\approx$15-36 M$_{\rm Jup}$. The M7 dwarf, PSO J237.1470-23.1489, shows excess mid-infrared flux implying the presence of a circumstellar disk. Finally, we present catalogs of Pan-STARRS1 proper motions for low-mass members of Taurus and Upper Scorpius with median precisions of $\approx$3 mas yr$^{-1}$, including 67 objects with no previous proper motion and 359 measurements that improve on literature values.

Figures

Tables

Table 1. Table 1: Pan-STARRS1  and AllWISE Photometry

Name	$i_{\mathrm{P1}}$	$z_{\mathrm{P1}}$	$y_{\mathrm{P1}}$	AllWISE Name	$W1$	$W2$	$W3$	$W4$
	(mag)	(mag)	(mag)		(mag)	(mag)	(mag)	(mag)
Taurus Discoveries
PSO J060.3200+25.9644	$21.61\pm 0.04$	$20.06\pm 0.02$	$19.02\pm 0.02$	J040116.80+255752.0	$14.99\pm 0.04$	$14.32\pm 0.05$	$>11.98$	$8.58\pm 0.39$
PSO J077.1033+24.3809	$21.62\pm 0.10$	$20.18\pm 0.05$	$19.21\pm 0.06$	J050824.81+242251.3	$15.15\pm 0.05$	$14.49\pm 0.07$	$>11.78$	$>8.61$
Taurus (previously known)
2MASS J04373705+2331080aaDiscovered by Luhman et al. (2009). Also known as PSO J069.4044+23.5186.	$\cdots$	$20.75\pm 0.03$	$19.67\pm 0.10$	J043737.06+233107.3	$14.45\pm 0.03$	$13.90\pm 0.05$	$>11.68$	$>9.10$
Scorpius-Centaurus Discoveries
PSO J228.6773$-$29.7088	$21.41\pm 0.04$	$19.87\pm 0.05$	$18.74\pm 0.03$	J151442.59$-$294231.9	$14.82\pm 0.03$	$14.22\pm 0.05$	$>11.83$	$>8.90$
PSO J229.2353$-$26.6737	$21.36\pm 0.05$	$20.14\pm 0.04$	$18.97\pm 0.02$	J151656.49$-$264025.3	$14.73\pm 0.04$	$14.37\pm 0.06$	$>12.34$	$>8.98$
PSO J231.7899$-$26.4494	$20.73\pm 0.04$	$19.10\pm 0.02$	$18.06\pm 0.02$	J152709.57$-$262658.0	$14.18\pm 0.03$	$13.79\pm 0.04$	$>12.55$	$>8.99$
PSO J231.8942$-$29.0600	$20.40\pm 0.06$	$18.81\pm 0.02$	$17.71\pm 0.01$	J152734.62$-$290335.8	$13.88\pm 0.03$	$13.43\pm 0.03$	$>11.79$	$>8.35$
PSO J237.1470$-$23.1489	$18.69\pm 0.01$	$17.41\pm 0.01$	$16.61\pm 0.01$	J154835.30$-$230855.5	$12.92\pm 0.03$	$12.40\pm 0.03$	$10.93\pm 0.15$	$8.75\pm 0.45$
PSO J239.7015$-$23.2665	$20.88\pm 0.05$	$19.26\pm 0.01$	$18.24\pm 0.02$	J155848.37$-$231559.1	$14.43\pm 0.03$	$13.94\pm 0.05$	$>12.26$	$>8.41$

Table 2. Table 2: Near-Infrared Photometry

	2MASS Photometry					MKO Photometry
Name	2MASS Name	$J_{2MASS}$	$H_{2MASS}$	$K_{S,2MASS}$		$J_{\mathrm{MKO}}$	$H_{\mathrm{MKO}}$	$K_{\mathrm{MKO}}$
		(mag)	(mag)	(mag)		(mag)	(mag)	(mag)
Taurus Discoveries
PSO J060.3+25	J04011678+2557527	$16.81\pm 0.17$	$15.73\pm 0.14$	$15.36\pm 0.17$		$16.93\pm 0.04$	$16.10\pm 0.03$	$\left[15.53\pm 0.07\right]$
PSO J077.1+24	J05082480+2422518	$16.93\pm 0.14$	$16.47\pm 0.25$	$15.82\pm 0.22$		$17.06\pm 0.04$	$16.31\pm 0.04$	$15.59\pm 0.03$
Taurus (previously known)
2MASS J0437+2331	J04373705+2331080	$17.38\pm 0.19$	$16.13\pm 0.15$	$15.44\pm 0.15$		$17.24\pm 0.02$aaFrom the UKIDSS Galactic Plane Survey (DR6; Lucas et al., 2012).	$16.16\pm 0.01$aaFrom the UKIDSS Galactic Plane Survey (DR6; Lucas et al., 2012).	$15.20\pm 0.02$bbFrom the UKIDSS Galactic Clusters Survey (DR9; Lawrence et al., 2013).
Scorpius-Centaurus Discoveries
PSO J228.6$-$29	J15144258$-$2942315	$16.79\pm 0.19$	$15.95\pm 0.15$	$15.31\pm 0.16$		$16.72\pm 0.05$	$16.18\pm 0.05$	$\left[15.37\pm 0.11\right]$
PSO J229.2$-$26	J15165651$-$2640251	$16.46\pm 0.13$	$15.98\pm 0.18$	$15.18\pm 0.15$		$16.76\pm 0.03$	$15.85\pm 0.02$	$\left[15.14\pm 0.08\right]$
PSO J231.7$-$26	J15270961$-$2626574	$15.96\pm 0.08$	$15.21\pm 0.11$	$14.62\pm 0.10$		$15.98\pm 0.02$	$15.25\pm 0.03$	$\left[14.64\pm 0.05\right]$
PSO J231.8$-$29	J15273464$-$2903354	$15.77\pm 0.09$	$14.83\pm 0.07$	$14.33\pm 0.08$		$\left[\left[15.72\pm 0.09\right]\right]$	$\left[\left[14.91\pm 0.08\right]\right]$	$\left[\left[14.29\pm 0.08\right]\right]$
PSO J237.1$-$23	J15483530$-$2308557	$14.79\pm 0.05$	$14.13\pm 0.07$	$13.60\pm 0.05$		$\left[\left[14.73\pm 0.06\right]\right]$	$\left[\left[14.19\pm 0.07\right]\right]$	$\left[\left[13.57\pm 0.06\right]\right]$
PSO J239.7$-$23	J15584839$-$2315589	$16.30\pm 0.11$	$15.35\pm 0.11$	$15.00\pm 0.13$		$16.25\pm 0.02$	$15.54\pm 0.02$	$\left[15.02\pm 0.07\right]$

Table 3. Table 3: IRTF/SpeX Observations

Object	Date	Slit	R	$t_{\mathrm{int}}$	S/NaaMean $J$-band (1.20–1.31 $\mu$m) S/N per resolution element.	A0 V Standard
	(UT)	(”)	($\lambda /\Delta \lambda$)	(s)
	2013 Jan 25	0.8	75	1920		HD 27761
PSO J060.3+25bbWe present a combined spectrum and S/N from the two observations (Section 3).					37
	2013 Nov 23	0.8	75	960		HD 31069
	2013 Jan 26	0.8	75	840		HD 34977
PSO J077.1+24bbWe present a combined spectrum and S/N from the two observations (Section 3).					34
	2013 Nov 23	0.8	75	1320		HD 38245
PSO J228.6$-$29	2013 Apr 18	0.8	75	720	24	HD 146880
PSO J229.2$-$26	2013 Apr 17	0.8	75	2880	26	HD 143822
PSO J231.7$-$26	2015 May 18	0.5	120	1440	49	HD 133466
PSO J231.8$-$29	2015 May 29	0.5	120	3600	84	HD 146606
PSO J237.1$-$23	2015 May 18	0.5	120	720	79	HD 133466
PSO J239.7$-$23	2013 Apr 18	0.8	75	720	33	HD 147013

Table 4. Table 4: Index-Based Spectral Types from Allers & Liu ( 2013a )

	Index-Derived Spectral Types
					Avg.	Visual	Adopted
Name	H2O	H2OD	H2O–1	H2O–2	SpTaaCalculated as the weighted average of the spectral types from Monte Carlo trials for all indices, excluding those that fell outside the valid range for each index.	SpTbbSpectral types determined by visual comparison with the vl-g spectral standards proposed by Allers & Liu (2013a). Uncertainties for these visual spectral types are $\pm 1$ subtype for all objects.	SpTccThe index-based average spectral types rounded to the nearest subtype, which we adopt as the final spectral types for our discoveries with uncertainties of $\pm 1$ subtype.
Taurus Discoveries
PSO J060.3+25	L1.3${}_{}{}^{+1.4}{}_{-1.4}{}^{}$	$\cdots$	L0.8${}_{}{}^{+1.2}{}_{-1.2}{}^{}$	L0.5${}_{}{}^{+1.1}{}_{-1.2}{}^{}$	L0.9${}_{}{}^{+0.9}{}_{-0.9}{}^{}$	L0.5	L1
PSO J077.1+24	L2.0${}_{}{}^{+1.2}{}_{-1.2}{}^{}$	$\cdots$	L0.1${}_{}{}^{+1.2}{}_{-1.2}{}^{}$	L1.5${}_{}{}^{+0.8}{}_{-1.0}{}^{}$	L1.7${}_{}{}^{+0.9}{}_{-0.9}{}^{}$	L1	L2
Taurus (previously known)
2MASS J0437+2331ddClassified as L0 by (Luhman et al., 2009) using an optical spectrum.	L1.5${}_{}{}^{+1.3}{}_{-1.4}{}^{}$	$\cdots$	L0.1${}_{}{}^{+1.3}{}_{-1.3}{}^{}$	L0.0${}_{}{}^{+1.2}{}_{-1.2}{}^{}$	L0.9${}_{}{}^{+0.9}{}_{-0.9}{}^{}$	L1.5	L1
Scorpius-Centaurus Discoveries
PSO J228.6$-$29	L1.4${}_{}{}^{+1.9}{}_{-2.2}{}^{}$	L1.7${}_{}{}^{+1.4}{}_{-1.4}{}^{}$	L1.1${}_{}{}^{+1.4}{}_{-1.4}{}^{}$	M9.5${}_{}{}^{+1.7}{}_{-1.9}{}^{}$	L0.8${}_{}{}^{+1.1}{}_{-1.3}{}^{}$	L0.5	L1
PSO J229.2$-$26	$\cdots$	$\cdots$	M9.8${}_{}{}^{+1.3}{}_{-1.3}{}^{}$	$\cdots$	M9.8${}_{}{}^{+1.3}{}_{-1.3}{}^{}$	L0	L0
PSO J231.7$-$26	M9.9${}_{}{}^{+0.9}{}_{-0.9}{}^{}$	$\cdots$	M9.6${}_{}{}^{+1.1}{}_{-1.2}{}^{}$	L0.0${}_{}{}^{+0.9}{}_{-0.9}{}^{}$	M9.9${}_{}{}^{+0.6}{}_{-0.6}{}^{}$	L0	L0
PSO J231.8$-$29	L0.3${}_{}{}^{+0.6}{}_{-0.6}{}^{}$	$\cdots$	L1.0${}_{}{}^{+1.1}{}_{-1.1}{}^{}$	M9.9${}_{}{}^{+0.6}{}_{-0.6}{}^{}$	L0.2${}_{}{}^{+0.4}{}_{-0.4}{}^{}$	L0	L0
PSO J237.1$-$23	M7.1${}_{}{}^{+0.5}{}_{-0.6}{}^{}$	$\cdots$	M7.3${}_{}{}^{+1.2}{}_{-1.2}{}^{}$	M7.1${}_{}{}^{+0.6}{}_{-0.6}{}^{}$	M7.1${}_{}{}^{+0.4}{}_{-0.4}{}^{}$	M7.5	M7
PSO J239.7$-$23	L0.1${}_{}{}^{+1.2}{}_{-1.2}{}^{}$	$\cdots$	M9.5${}_{}{}^{+1.3}{}_{-1.3}{}^{}$	L0.1${}_{}{}^{+1.3}{}_{-1.4}{}^{}$	L0.0${}_{}{}^{+0.9}{}_{-0.9}{}^{}$	M9	L0

Table 5. Table 5: Index-Based Spectral Types from Burgasser et al. ( 2006 ) for L dwarfs

	Index Values (Derived Spectral Types)aaSpectral types calculated using the polynomials defined in Burgasser (2007).
						Avg.	Adopted
Name	H2O-$J$	CH4-$J$	H2O-$H$	CH4-$H$	CH4-$K$	SpT	SpTbbFor description see Section 4.2 and Table 4.
Taurus Discoveries
PSO J060.3+25	0.867 (L2.3)	0.933 (T0)	0.780 (L3.4)	1.118 (T1)	1.122 (L0)	L2.8$\pm$0.8	L1
PSO J077.1+24	0.946 (L0.4)	0.924 (T0)	0.803 (L2.5)	1.167 (T1)	1.137 (L0)	L1.5$\pm$1.4	L2
Taurus (previously known)
2MASS J0437+2331ddClassified as L0 by Luhman et al. (2009) using an optical spectrum.	0.810 (L3.9)	0.942 (T0)	0.788 (L3.1)	1.190 (T1)	1.147 (L0)	L3.5$\pm$0.6	L1
Scorpius-Centaurus Discoveries
PSO J228.6$-$29	0.852 (L2.7)	0.837 (T0)	0.735 (L5.2)	1.126 (T1)	1.146 (L0)	L3.9$\pm$1.8	L1
PSO J229.2$-$26	0.918 (L1.0)	0.969 (T0)	0.755 (L4.4)	1.119 (T1)	1.111 (L0)	L2.7$\pm$2.4	L0
PSO J231.7$-$26	0.920 (L1.0)	0.927 (T0)	0.841 (L1.0)	1.167 (T1)	1.135 (L0)	L1.0$\pm$0.5ccThe two contributing index-based spectral types are both L1.0, so we adopt an uncertainty of 0.5 subtypes.	L0
PSO J231.8$-$29	0.923 (L0.9)	0.905 (T0)	0.821 (L1.7)	1.150 (T1)	1.136 (L0)	L1.3$\pm$0.6	L0
PSO J237.1$-$23	0.978 (L0)	0.918 (T0)	0.929 (L0)	1.053 (T1)	1.026 (L0)	$\cdots$	M7
PSO J239.7$-$23	0.971 (L0.0)	0.913 (T0)	0.810 (L2.2)	1.071 (T1)	1.106 (L0)	L1.1$\pm$1.5	L0

Table 6. Table 6: Low-Resolution Gravity Indices from Allers & Liu ( 2013a )

					Index	Gravity	Gravity	Adopted
Name	FeHz	VOz	KIJ	H-cont	ScoresaaScores in parentheses were determined using the original AL13 classification scheme, in which objects with index values corresponding to int-g but within $1\sigma$ of the fld-g value are classified with a score of “?”.	ScorebbThe overall gravity score and the 68% confidence limits were calculated as described in Aller et al. (2016).	Class	SpT
Taurus Discoveries
PSO J060.3+25	1.006${}_{}{}^{+0.035}{}_{-0.036}{}^{}$	1.203${}_{}{}^{+0.032}{}_{-0.034}{}^{}$	1.038${}_{}{}^{+0.016}{}_{-0.016}{}^{}$	0.971${}_{}{}^{+0.022}{}_{-0.023}{}^{}$	2122 (2122)	2.0${}_{}{}^{+0.0}{}_{-0.5}{}^{}$	vl-g	L1
PSO J077.1+24	1.043${}_{}{}^{+0.039}{}_{-0.042}{}^{}$	1.196${}_{}{}^{+0.029}{}_{-0.030}{}^{}$	0.994${}_{}{}^{+0.017}{}_{-0.017}{}^{}$	0.977${}_{}{}^{+0.025}{}_{-0.026}{}^{}$	2122 (2122)	2.0${}_{}{}^{+0.0}{}_{-0.5}{}^{}$	vl-g	L2
Scorpius-Centaurus Discoveries
PSO J231.7$-$26	1.075${}_{}{}^{+0.020}{}_{-0.021}{}^{}$	1.214${}_{}{}^{+0.015}{}_{-0.015}{}^{}$	1.032${}_{}{}^{+0.011}{}_{-0.011}{}^{}$	0.993${}_{}{}^{+0.015}{}_{-0.015}{}^{}$	2n22 (2n22)	2.0${}_{}{}^{+0.0}{}_{-0.0}{}^{}$	vl-g	L0
PSO J231.8$-$29	1.075${}_{}{}^{+0.011}{}_{-0.011}{}^{}$	1.239${}_{}{}^{+0.009}{}_{-0.009}{}^{}$	1.061${}_{}{}^{+0.006}{}_{-0.006}{}^{}$	0.995${}_{}{}^{+0.008}{}_{-0.008}{}^{}$	2122 (2122)	2.0${}_{}{}^{+0.0}{}_{-0.0}{}^{}$	vl-g	L0
PSO J237.1$-$23	1.056${}_{}{}^{+0.019}{}_{-0.019}{}^{}$	1.045${}_{}{}^{+0.014}{}_{-0.014}{}^{}$	1.026${}_{}{}^{+0.009}{}_{-0.009}{}^{}$	0.999${}_{}{}^{+0.007}{}_{-0.007}{}^{}$	2n22 (2n22)	2.0${}_{}{}^{+0.0}{}_{-0.0}{}^{}$	vl-g	M7
PSO J239.7$-$23	1.032${}_{}{}^{+0.034}{}_{-0.035}{}^{}$	1.101${}_{}{}^{+0.025}{}_{-0.025}{}^{}$	1.065${}_{}{}^{+0.019}{}_{-0.019}{}^{}$	0.974${}_{}{}^{+0.025}{}_{-0.026}{}^{}$	2n12 (2n12)	2.0${}_{}{}^{+0.0}{}_{-1.0}{}^{}$	vl-g	L0

Table 7. Table 7: Proper Motions, Luminosities, and Masses

Name	SpT	${\mu }_{\alpha }\cos \delta$aaProper motions from Pan-STARRS1 Processing Version 3.2, calculated using PS1, 2MASS, and Gaia DR1 astrometry (Section 4.4).	${\mu }_{\delta }$aaProper motions from Pan-STARRS1 Processing Version 3.2, calculated using PS1, 2MASS, and Gaia DR1 astrometry (Section 4.4).	${\chi }_{\nu }^2$	$N_{\mathrm{ep}}$	$\Delta t$		log($L_{\mathrm{bol}}$/$L_{\odot }$)	MassbbMasses estimated using $L_{\mathrm{bol}}$ and the Lyon/DUSTY evolutionary models (Chabrier et al., 2000) as described in Sections 5 and 6.
		(mas yr-1)	(mas yr-1)			(yr)		(dex)	($M_{\mathrm{Jup}}$)
Taurus (age $=1.5\pm 0.5$ Myr, distance $=145\pm 15$ pc)
PSO J060.3+25	L1	$19.0\pm 8.2$	$-38.1\pm 8.2$	0.8	43	17.2		$-{3.32}_{-0.10}^{+0.09}$	${6.0}_{-0.8}^{+0.9}$
		$14.3\pm 3.1$ccFrom Bouy et al. (2015). We adopt this proper motion for our analysis in Section 5.	$-26.4\pm 3.2$ccFrom Bouy et al. (2015). We adopt this proper motion for our analysis in Section 5.		29ccFrom Bouy et al. (2015). We adopt this proper motion for our analysis in Section 5.	12.9ccFrom Bouy et al. (2015). We adopt this proper motion for our analysis in Section 5.
PSO J077.1+24	L2	$14.1\pm 12.5$	$-27.1\pm 12.1$	0.6	27	16.0		$-{3.34}_{-0.10}^{+0.09}$	${5.9}_{-0.8}^{+0.9}$
2MASS J0437+2331	L1	$15.9\pm 13.5$	$-54.8\pm 13.4$	0.5	16	15.0		$-{3.17}_{-0.10}^{+0.09}$	${7.1}_{-1.0}^{+1.1}$
Upper Centaurus-Lupus (age $=16\pm 1$ Myr, distance $=140\pm 15$ pc)
PSO J228.6$-$29	L1	$-18.4\pm 11.5$	$-25.6\pm 11.0$	1.3	18	15.4		$-{3.29}_{-0.10}^{+0.10}$	${15.1}_{-0.6}^{+0.6}$
PSO J229.2$-$26	L0	$-30.8\pm 10.9$	$-38.4\pm 10.3$	0.9	29	15.3		$-{3.18}_{-0.11}^{+0.09}$	${15.7}_{-1.5}^{+1.6}$
PSO J231.7$-$26	L0	$-25.8\pm 5.5$	$-28.1\pm 5.4$	1.0	35	16.2		$-{2.93}_{-0.10}^{+0.10}$	${20}_{-4}^{+4}$
PSO J231.8$-$29	L0	$-21.1\pm 2.8$	$-36.3\pm 2.3$	0.5	36	16.5		$-{2.82}_{-0.11}^{+0.10}$	${25}_{-6}^{+8}$
Upper Scorpius (age $=11\pm 2$ Myr, distance $=145\pm 15$ pc)
PSO J237.1$-$23	M7	$-11.4\pm 2.8$	$-19.7\pm 2.8$	2.1	34	16.6		$-{2.43}_{-0.11}^{+0.10}$	${36}_{-10}^{+15}$
PSO J239.7$-$23	L0	$-0.1\pm 7.2$	$-23.0\pm 3.5$	0.6	38	15.7		$-{3.10}_{-0.10}^{+0.09}$	${16.2}_{-1.2}^{+1.4}$

Table 8. Table 8: Proper Motions of Taurus Members

	Photometry				Proper Motion
Name	$i_{\mathrm{P1}}$	$z_{\mathrm{P1}}$	$y_{\mathrm{P1}}$		${\mu }_{\alpha }\cos \delta$	${\mu }_{\delta }$	${\chi }_{\nu }^2$	$N_{\mathrm{ep}}$	$\Delta t$
	(mag)	(mag)	(mag)		(mas yr-1)	(mas yr-1)			(yr)
Reliable fits:
PSO J060.3200+25.9644	$21.61\pm 0.04$	$20.06\pm 0.02$	$19.02\pm 0.02$		$19.0\pm 8.2$	$-38.1\pm 8.2$	0.8	43	17.2
2MASS J04034997+2620382	$16.27\pm 0.01$	$15.28\pm 0.01$	$14.73\pm 0.01$		$15.6\pm 6.3$	$-16.0\pm 5.3$	14	62	15.1
2MASS J04064443+2540182	$15.67\pm 0.01$	$14.68\pm 0.01$	$14.14\pm 0.01$		$12.4\pm 1.3$	$-15.5\pm 1.1$	2.0	87	15.2
2MASS J04080782+2807280	$15.19\pm 0.01$	$14.34\pm 0.01$	$13.91\pm 0.01$		$2.6\pm 1.5$	$-7.7\pm 1.5$	3.5	91	17.2
2MASS J04102834+2051507	$16.90\pm 0.01$	$15.87\pm 0.01$	$15.28\pm 0.01$		$-2.3\pm 2.6$	$-7.3\pm 1.0$	1.7	69	17.2
2MASS J04105425+2501266	$20.00\pm 0.03$	$19.74\pm 0.07$	$18.78\pm 0.04$		$9.2\pm 4.0$	$-15.7\pm 4.0$	0.7	34	17.2
2MASS J04135328+2811233	$20.37\pm 0.03$	$18.33\pm 0.01$	$16.93\pm 0.01$		$13.3\pm 9.9$	$-39.8\pm 12.3$	22	45	17.2
2MASS J04135737+2918193	$14.81\pm 0.08$	$14.79\pm 0.06$	$14.66\pm 0.01$		$5.9\pm 1.3$	$-26.4\pm 1.5$	1.8	64	17.2
2MASS J04141760+2806096	$15.14\pm 0.02$	$14.26\pm 0.02$	$13.64\pm 0.01$		$7.7\pm 3.8$	$-24.6\pm 2.8$	14	67	17.2
2MASS J04142626+2806032	$19.07\pm 0.05$	$17.21\pm 0.05$	$16.29\pm 0.03$		$8.1\pm 2.8$	$-18.4\pm 3.6$	3.4	41	17.2
2MASS J04142639+2805597	$16.51\pm 0.01$	$15.10\pm 0.01$	$14.17\pm 0.02$		$8.3\pm 2.9$	$-20.2\pm 2.6$	4.3	63	17.2
2MASS J04143054+2805147	$15.79\pm 0.03$	$14.63\pm 0.04$	$13.81\pm 0.04$		$11.8\pm 2.2$	$-19.5\pm 1.6$	3.6	61	17.2
2MASS J04144158+2809583	$\cdots$	$20.76\pm 0.12$	$19.68\pm 0.05$		$-4.7\pm 5.9$	$-5.6\pm 5.7$	0.4	15	15.9
2MASS J04151471+2800096	$19.77\pm 0.01$	$18.07\pm 0.02$	$17.09\pm 0.01$		$15.5\pm 2.0$	$-24.3\pm 2.4$	1.1	50	17.2
2MASS J04152409+2910434	$17.90\pm 0.01$	$16.45\pm 0.01$	$15.59\pm 0.01$		$12.3\pm 1.8$	$-9.0\pm 1.8$	4.3	60	17.2
2MASS J04153566+2847417	$19.81\pm 0.02$	$18.62\pm 0.03$	$17.89\pm 0.01$		$8.1\pm 3.6$	$-29.6\pm 5.3$	4.9	45	17.2
2MASS J04154131+2915078	$16.09\pm 0.01$	$14.96\pm 0.01$	$14.34\pm 0.01$		$3.9\pm 3.1$	$-13.2\pm 2.6$	6.1	59	17.2
2MASS J04154269+2909558	$16.96\pm 0.01$	$15.50\pm 0.01$	$14.65\pm 0.01$		$13.9\pm 2.7$	$-1.5\pm 4.5$	11	39	17.2
2MASS J04154807+2911331	$20.61\pm 0.03$	$18.86\pm 0.01$	$17.84\pm 0.02$		$11.7\pm 3.5$	$-14.0\pm 3.5$	0.7	35	17.2
2MASS J04155799+2746175	$14.90\pm 0.01$	$13.83\pm 0.03$	$13.36\pm 0.03$		$9.9\pm 1.9$	$-23.2\pm 1.9$	2.5	60	17.2
2MASS J04161210+2756385	$15.50\pm 0.06$	$14.12\pm 0.01$	$13.55\pm 0.01$		$7.3\pm 2.1$	$-24.8\pm 1.4$	1.4	71	17.2
2MASS J04161885+2752155	$16.36\pm 0.01$	$15.09\pm 0.01$	$14.35\pm 0.01$		$5.0\pm 1.9$	$-24.2\pm 1.5$	1.3	72	17.2
2MASS J04162725+2053091	$14.96\pm 0.01$	$14.03\pm 0.01$	$13.50\pm 0.01$		$2.1\pm 1.2$	$-10.2\pm 1.3$	1.8	98	17.2
2MASS J04163048+3037053	$16.43\pm 0.01$	$15.53\pm 0.01$	$15.07\pm 0.01$		$6.6\pm 1.3$	$-6.2\pm 1.2$	2.1	86	17.0
2MASS J04163911+2858491	$16.42\pm 0.01$	$15.24\pm 0.01$	$14.45\pm 0.01$		$17.8\pm 3.7$	$-4.2\pm 5.4$	17	56	17.2
2MASS J04181710+2828419	$17.71\pm 0.01$	$16.14\pm 0.01$	$15.19\pm 0.01$		$16.2\pm 6.2$	$-19.1\pm 7.7$	18	61	17.2
2MASS J04182909+2826191	$\cdots$	$\cdots$	$19.55\pm 0.06$		$11.8\pm 11.1$	$-21.7\pm 4.8$	1.4	13	15.9
2MASS J04183030+2743208	$14.86\pm 0.01$	$\cdots$	$13.33\pm 0.01$		$9.1\pm 1.7$	$-29.2\pm 2.4$	2.2	48	17.2
2MASS J04183203+2831153	$21.20\pm 0.07$	$19.38\pm 0.05$	$18.55\pm 0.12$		$11.0\pm 3.2$	$-19.3\pm 3.1$	1.3	61	17.2
2MASS J04183444+2830302	$\cdots$	$19.80\pm 0.02$	$18.08\pm 0.03$		$9.9\pm 3.6$	$-22.7\pm 3.4$	1.5	31	17.2
2MASS J04184023+2824245	$21.16\pm 0.03$	$19.03\pm 0.03$	$17.44\pm 0.01$		$2.7\pm 5.9$	$-31.8\pm 4.9$	8.6	54	17.2
2MASS J04184250+2818498	$16.92\pm 0.01$	$15.52\pm 0.01$	$14.59\pm 0.01$		$8.2\pm 2.5$	$-13.1\pm 3.8$	8.0	73	17.2
2MASS J04185115+2814332	$17.75\pm 0.01$	$16.42\pm 0.01$	$15.65\pm 0.01$		$11.7\pm 4.5$	$-27.9\pm 2.9$	4.3	87	17.2
2MASS J04185147+2820264	$16.68\pm 0.03$	$15.54\pm 0.03$	$14.94\pm 0.02$		$2.3\pm 4.6$	$-6.0\pm 7.2$	29	87	17.2
2MASS J04190126+2802487	$20.96\pm 0.04$	$19.51\pm 0.01$	$18.46\pm 0.01$		$7.1\pm 5.6$	$-28.4\pm 5.3$	1.2	53	17.2
2MASS J04190197+2822332	$16.41\pm 0.01$	$15.02\pm 0.01$	$14.17\pm 0.01$		$-2.6\pm 3.8$	$-21.3\pm 4.9$	23	83	17.2
2MASS J04194148+2716070	$18.03\pm 0.04$	$17.33\pm 0.03$	$16.87\pm 0.03$		$29.0\pm 3.3$	$-19.3\pm 2.8$	5.9	78	17.2
2MASS J04201611+2821325	$17.25\pm 0.01$	$15.98\pm 0.01$	$15.26\pm 0.01$		$3.2\pm 4.3$	$-31.1\pm 6.1$	12	73	17.2
2MASS J04202144+2813491	$19.41\pm 0.02$	$18.54\pm 0.08$	$18.32\pm 0.02$		$-17.1\pm 14.9$	$5.2\pm 12.3$	20	60	17.2
2MASS J04202555+2700355	$16.39\pm 0.01$	$15.24\pm 0.01$	$14.58\pm 0.01$		$18.5\pm 3.5$	$-14.9\pm 1.1$	7.3	82	17.2
2MASS J04202583+2819237	$18.37\pm 0.01$	$17.09\pm 0.05$	$16.60\pm 0.03$		$25.2\pm 7.2$	$-36.6\pm 15.7$	35	77	17.2
2MASS J04210795+2702204	$18.21\pm 0.01$	$15.70\pm 0.01$	$14.89\pm 0.07$		$11.5\pm 8.0$	$-7.0\pm 3.3$	11	69	17.2
2MASS J04213459+2701388	$15.74\pm 0.01$	$14.47\pm 0.01$	$13.75\pm 0.01$		$8.1\pm 3.2$	$-13.5\pm 2.7$	3.1	64	17.2
2MASS J04213965+2649143	$16.27\pm 0.01$	$15.05\pm 0.01$	$14.35\pm 0.01$		$14.7\pm 2.7$	$-13.2\pm 5.1$	5.5	68	17.2
2MASS J04214013+2814224	$14.84\pm 0.01$	$13.86\pm 0.01$	$13.34\pm 0.01$		$13.5\pm 2.1$	$-25.3\pm 3.9$	7.0	84	17.2
2MASS J04214631+2659296	$18.11\pm 0.01$	$16.70\pm 0.01$	$15.84\pm 0.01$		$12.1\pm 1.6$	$-18.5\pm 1.8$	1.2	73	17.2
2MASS J04215450+2652315	$20.78\pm 0.02$	$18.87\pm 0.01$	$17.78\pm 0.02$		$12.0\pm 3.5$	$-9.5\pm 3.5$	1.2	57	17.2
2MASS J04215482+2642372	$15.34\pm 0.01$	$14.36\pm 0.01$	$13.84\pm 0.01$		$19.2\pm 7.8$	$-15.9\pm 3.3$	6.4	63	17.2
2MASS J04215851+1520145	$15.69\pm 0.01$	$15.05\pm 0.02$	$14.59\pm 0.01$		$-2.2\pm 3.6$	$2.2\pm 3.0$	5.6	69	17.2
2MASS J04220069+2657324	$18.50\pm 0.04$	$17.90\pm 0.02$	$17.12\pm 0.11$		$-11.3\pm 7.4$	$-12.8\pm 5.4$	7.0	52	17.2
2MASS J04221332+1934392	$16.93\pm 0.01$	$15.52\pm 0.01$	$14.70\pm 0.01$		$8.7\pm 2.1$	$-8.8\pm 1.7$	1.6	90	17.2
2MASS J04221568+2657060	$16.26\pm 0.01$	$15.85\pm 0.01$	$15.48\pm 0.01$		$10.6\pm 4.0$	$-4.0\pm 5.2$	4.6	74	17.2
2MASS J04221644+2549118	$17.07\pm 0.01$	$15.61\pm 0.01$	$14.85\pm 0.01$		$15.9\pm 2.6$	$-22.4\pm 1.3$	2.1	79	17.2
2MASS J04221675+2654570	$15.13\pm 0.07$	$\cdots$	$14.14\pm 0.03$		$12.7\pm 2.1$	$-14.6\pm 3.3$	13	79	17.2
2MASS J04223075+1526310	$18.11\pm 0.01$	$16.85\pm 0.01$	$16.12\pm 0.01$		$1.3\pm 1.8$	$-3.5\pm 1.7$	0.8	62	17.1
2MASS J04224786+2645530	$15.36\pm 0.02$	$14.74\pm 0.13$	$14.27\pm 0.12$		$12.2\pm 1.9$	$-16.7\pm 1.4$	1.6	54	17.2
2MASS J04230607+2801194	$15.55\pm 0.01$	$14.45\pm 0.01$	$13.81\pm 0.01$		$11.5\pm 1.0$	$-25.2\pm 2.1$	3.5	64	17.2
2MASS J04230776+2805573	$16.34\pm 0.03$	$15.37\pm 0.01$	$15.04\pm 0.07$		$9.8\pm 1.2$	$-26.2\pm 2.0$	1.8	78	17.2
2MASS J04231822+2641156	$17.57\pm 0.01$	$16.10\pm 0.01$	$15.16\pm 0.01$		$14.9\pm 1.7$	$-13.1\pm 2.0$	1.9	53	17.2
2MASS J04233539+2503026	$14.76\pm 0.01$	$13.43\pm 0.01$	$12.64\pm 0.02$		$11.2\pm 4.2$	$-15.3\pm 4.8$	23	69	17.2
2MASS J04233573+2502596	$20.19\pm 0.02$	$18.40\pm 0.02$	$17.21\pm 0.01$		$1.4\pm 5.9$	$-31.9\pm 5.5$	4.0	34	17.2
2MASS J04242090+2630511	$16.99\pm 0.01$	$15.75\pm 0.01$	$15.07\pm 0.01$		$12.0\pm 3.1$	$-25.9\pm 1.4$	2.2	47	17.1
2MASS J04242646+2649503	$16.28\pm 0.01$	$15.15\pm 0.01$	$14.50\pm 0.01$		$10.9\pm 1.4$	$-18.3\pm 1.3$	1.2	64	17.1
2MASS J04245021+2641006	$15.60\pm 0.01$	$14.51\pm 0.01$	$13.94\pm 0.01$		$9.3\pm 1.5$	$-13.4\pm 1.6$	1.7	65	17.2
2MASS J04251550+2829275	$14.64\pm 0.01$	$13.48\pm 0.01$	$12.84\pm 0.01$		$10.2\pm 1.5$	$-23.6\pm 1.3$	1.5	72	17.2
2MASS J04262939+2624137	$17.02\pm 0.01$	$15.83\pm 0.01$	$15.08\pm 0.01$		$6.2\pm 2.5$	$-14.8\pm 1.6$	3.1	74	17.1
2MASS J04263055+2443558	$19.51\pm 0.02$	$17.70\pm 0.01$	$16.67\pm 0.01$		$10.2\pm 3.1$	$-15.3\pm 4.1$	2.5	56	17.1
2MASS J04264449+2756433	$15.89\pm 0.01$	$14.77\pm 0.01$	$14.17\pm 0.01$		$4.5\pm 2.0$	$-30.4\pm 3.7$	7.9	102	17.2
2MASS J04265732+2606284	$14.95\pm 0.01$	$13.80\pm 0.01$	$13.09\pm 0.01$		$-1.6\pm 2.1$	$-16.3\pm 1.9$	4.8	79	17.1
2MASS J04270266+2605304	$20.03\pm 0.04$	$19.06\pm 0.03$	$18.41\pm 0.03$		$3.9\pm 10.5$	$-27.0\pm 11.5$	8.1	47	16.0
2MASS J04270739+2215037	$15.49\pm 0.01$	$14.39\pm 0.01$	$13.79\pm 0.01$		$7.9\pm 1.3$	$-15.3\pm 1.4$	1.0	73	17.2
2MASS J04272799+2612052	$20.34\pm 0.02$	$18.58\pm 0.03$	$17.57\pm 0.01$		$-0.9\pm 2.5$	$-25.6\pm 2.5$	1.8	59	17.2
2MASS J04274538+2357243	$19.27\pm 0.01$	$17.75\pm 0.01$	$16.84\pm 0.01$		$9.3\pm 2.9$	$-12.6\pm 2.7$	3.5	62	17.2
2MASS J04275730+2619183	$17.60\pm 0.08$	$16.66\pm 0.04$	$15.94\pm 0.04$		$-6.4\pm 5.4$	$8.1\pm 5.9$	21	73	17.2
2MASS J04284199+1533535	$15.46\pm 0.01$	$14.63\pm 0.01$	$14.20\pm 0.01$		$1.1\pm 1.3$	$-15.1\pm 1.6$	1.9	68	17.2
2MASS J04284263+2714039	$15.33\pm 0.01$	$14.45\pm 0.01$	$13.85\pm 0.01$		$2.5\pm 1.3$	$-15.7\pm 3.1$	5.8	71	17.2
2MASS J04285053+1844361	$14.65\pm 0.01$	$13.46\pm 0.01$	$12.70\pm 0.01$		$9.3\pm 2.9$	$-9.0\pm 3.8$	11	89	17.2
2MASS J04290068+2755033	$17.99\pm 0.01$	$16.55\pm 0.01$	$15.72\pm 0.01$		$8.7\pm 1.9$	$-25.2\pm 1.7$	1.8	57	17.2
2MASS J04290498+2649073	$18.01\pm 0.01$	$17.14\pm 0.02$	$16.64\pm 0.02$		$12.2\pm 5.5$	$-9.4\pm 6.2$	2.8	69	17.2
2MASS J04292165+2701259	$15.67\pm 0.01$	$14.18\pm 0.01$	$13.17\pm 0.02$		$3.9\pm 1.5$	$-18.9\pm 1.5$	1.8	83	17.2
2MASS J04293008+2439550	$18.71\pm 0.04$	$17.92\pm 0.10$	$16.92\pm 0.12$		$18.9\pm 3.3$	$-29.4\pm 3.6$	13	71	17.1
2MASS J04294568+2630468	$16.31\pm 0.01$	$15.05\pm 0.01$	$14.29\pm 0.01$		$7.4\pm 1.2$	$-23.0\pm 1.4$	1.6	65	17.2
2MASS J04295422+1754041	$15.98\pm 0.03$	$15.18\pm 0.05$	$14.46\pm 0.11$		$8.8\pm 4.0$	$-19.5\pm 2.8$	3.1	70	17.2
2MASS J04295950+2433078	$16.00\pm 0.07$	$14.51\pm 0.01$	$14.01\pm 0.03$		$10.0\pm 1.6$	$-15.5\pm 2.3$	1.8	66	17.1
2MASS J04300724+2608207	$19.24\pm 0.01$	$17.70\pm 0.01$	$16.78\pm 0.01$		$4.4\pm 1.6$	$-19.4\pm 1.8$	1.3	63	17.2
2MASS J04302365+2359129	$19.25\pm 0.01$	$17.70\pm 0.01$	$16.79\pm 0.01$		$1.2\pm 2.4$	$-16.3\pm 2.2$	1.6	55	17.2
2MASS J04305171+2441475	$16.63\pm 0.01$	$15.71\pm 0.01$	$15.11\pm 0.04$		$1.8\pm 5.2$	$-16.5\pm 2.5$	11	74	17.1
2MASS J04305718+2556394	$18.55\pm 0.01$	$17.10\pm 0.01$	$16.28\pm 0.01$		$12.6\pm 1.6$	$-21.4\pm 1.9$	1.4	71	17.2
2MASS J04311907+2335047	$17.86\pm 0.01$	$16.35\pm 0.01$	$15.47\pm 0.01$		$6.4\pm 2.2$	$-9.8\pm 2.0$	1.4	58	15.2
2MASS J04312405+1800215	$15.46\pm 0.01$	$14.18\pm 0.01$	$13.39\pm 0.01$		$13.9\pm 4.3$	$-8.8\pm 3.6$	4.7	62	15.2
2MASS J04312669+2703188	$19.25\pm 0.01$	$17.69\pm 0.02$	$16.77\pm 0.01$		$16.7\pm 2.8$	$-17.3\pm 1.6$	0.6	42	17.2
2MASS J04313407+1808049	$19.56\pm 0.03$	$18.37\pm 0.14$	$17.27\pm 0.03$		$-79.0\pm 25.7$	$-28.5\pm 12.6$	39	36	15.2
2MASS J04313613+1813432	$16.81\pm 0.02$	$16.19\pm 0.03$	$15.57\pm 0.03$		$21.5\pm 6.9$	$-18.2\pm 6.8$	22	57	15.2
2MASS J04313747+1812244	$17.71\pm 0.10$	$17.36\pm 0.03$	$17.07\pm 0.10$		$14.8\pm 5.7$	$-22.6\pm 7.5$	27	64	15.2
2MASS J04314644+2506236	$15.13\pm 0.01$	$14.13\pm 0.01$	$13.57\pm 0.01$		$11.3\pm 1.5$	$-27.8\pm 1.4$	1.9	50	17.2
2MASS J04315968+1821305	$16.10\pm 0.02$	$15.08\pm 0.15$	$14.05\pm 0.07$		$5.2\pm 6.7$	$-23.1\pm 3.4$	13	80	14.2
2MASS J04320329+2528078	$15.07\pm 0.01$	$13.91\pm 0.01$	$13.28\pm 0.01$		$2.8\pm 2.0$	$-17.9\pm 2.5$	3.4	44	17.1
2MASS J04321540+2428597	$14.69\pm 0.02$	$13.32\pm 0.09$	$12.59\pm 0.04$		$14.2\pm 4.6$	$-8.3\pm 6.1$	13	69	17.1
2MASS J04321786+2422149	$15.13\pm 0.01$	$13.93\pm 0.01$	$13.23\pm 0.01$		$-1.0\pm 3.2$	$-16.9\pm 2.6$	12	76	17.2
2MASS J04322210+1827426	$14.61\pm 0.01$	$13.69\pm 0.01$	$13.20\pm 0.01$		$16.3\pm 1.8$	$-20.3\pm 1.8$	3.4	81	14.3
2MASS J04322329+2403013	$16.29\pm 0.02$	$14.85\pm 0.01$	$14.08\pm 0.01$		$6.6\pm 2.4$	$-18.8\pm 2.2$	1.9	69	17.2
2MASS J04322415+2251083	$14.55\pm 0.01$	$13.64\pm 0.01$	$13.11\pm 0.01$		$10.8\pm 1.6$	$-19.9\pm 1.6$	1.0	58	14.3
2MASS J04323205+2257266	$\cdots$	$20.05\pm 0.11$	$19.08\pm 0.07$		$13.5\pm 5.1$	$-7.1\pm 5.2$	3.7	18	13.3
2MASS J04324938+2253082	$15.37\pm 0.16$	$13.89\pm 0.01$	$13.16\pm 0.01$		$18.8\pm 6.3$	$-18.8\pm 4.1$	29	78	14.3
2MASS J04325026+2422115	$20.85\pm 0.03$	$18.56\pm 0.02$	$17.12\pm 0.02$		$1.8\pm 2.9$	$-18.1\pm 2.7$	1.2	41	17.2
2MASS J04325119+1730092	$19.08\pm 0.02$	$17.43\pm 0.01$	$16.53\pm 0.01$		$12.6\pm 1.7$	$-20.8\pm 1.6$	0.7	61	17.3
2MASS J04330197+2421000	$14.56\pm 0.01$	$13.32\pm 0.01$	$12.60\pm 0.01$		$4.9\pm 1.8$	$-19.1\pm 2.1$	2.4	51	17.2
2MASS J04330781+2616066	$16.40\pm 0.01$	$14.89\pm 0.01$	$14.00\pm 0.01$		$9.0\pm 1.8$	$-16.0\pm 1.5$	2.3	74	17.2
2MASS J04330945+2246487	$17.51\pm 0.02$	$15.98\pm 0.01$	$15.20\pm 0.01$		$-0.6\pm 3.3$	$-16.8\pm 1.5$	2.3	67	16.2
2MASS J04331435+2614235	$18.61\pm 0.01$	$17.52\pm 0.02$	$16.88\pm 0.01$		$9.7\pm 4.3$	$-10.4\pm 4.1$	3.5	61	17.2
2MASS J04331907+2246342	$15.71\pm 0.04$	$14.64\pm 0.01$	$13.89\pm 0.05$		$7.0\pm 2.4$	$-18.7\pm 1.9$	3.2	74	16.2
2MASS J04332621+2245293	$15.93\pm 0.01$	$14.70\pm 0.01$	$13.93\pm 0.01$		$8.0\pm 2.9$	$-12.4\pm 2.2$	3.9	69	16.2
2MASS J04332789+1758436	$17.90\pm 0.03$	$17.19\pm 0.03$	$16.40\pm 0.07$		$11.5\pm 1.6$	$-14.9\pm 1.6$	0.7	76	17.3
2MASS J04333905+2227207	$16.04\pm 0.01$	$15.53\pm 0.02$	$15.10\pm 0.01$		$6.3\pm 1.9$	$-10.3\pm 4.8$	4.3	77	16.2
2MASS J04334291+2526470	$19.29\pm 0.01$	$17.61\pm 0.01$	$16.61\pm 0.01$		$6.0\pm 2.2$	$-24.5\pm 3.0$	1.3	43	17.2
2MASS J04334465+2615005	$15.98\pm 0.02$	$14.92\pm 0.05$	$13.82\pm 0.03$		$1.8\pm 2.9$	$-17.1\pm 2.7$	6.4	104	17.2
2MASS J04335245+2612548	$20.78\pm 0.02$	$19.03\pm 0.02$	$17.93\pm 0.02$		$9.0\pm 3.6$	$-15.9\pm 3.5$	1.0	73	17.2
2MASS J04340619+2418508	$17.99\pm 0.01$	$16.57\pm 0.01$	$15.75\pm 0.01$		$8.1\pm 2.9$	$-19.9\pm 2.0$	3.2	53	17.2
2MASS J04341527+2250309	$18.78\pm 0.01$	$17.09\pm 0.01$	$16.09\pm 0.01$		$17.5\pm 9.3$	$-12.4\pm 2.8$	13	45	16.2
2MASS J04344544+2308027	$16.14\pm 0.01$	$15.03\pm 0.01$	$14.40\pm 0.01$		$9.7\pm 1.2$	$-16.1\pm 1.2$	1.4	82	16.3
2MASS J04345973+2807017	$19.39\pm 0.02$	$18.22\pm 0.01$	$17.48\pm 0.01$		$7.0\pm 3.5$	$-15.6\pm 3.2$	0.8	37	17.1
2MASS J04350850+2311398	$15.73\pm 0.01$	$14.63\pm 0.01$	$14.01\pm 0.01$		$9.4\pm 1.3$	$-19.8\pm 1.1$	1.2	89	16.3
2MASS J04354093+2411087	$14.85\pm 0.02$	$14.12\pm 0.04$	$13.29\pm 0.03$		$10.9\pm 4.4$	$-7.7\pm 6.2$	16	74	17.2
2MASS J04354183+2234115	$16.26\pm 0.01$	$15.15\pm 0.01$	$14.50\pm 0.01$		$9.6\pm 1.3$	$-16.1\pm 1.5$	1.6	88	16.3
2MASS J04354203+2252226	$14.68\pm 0.01$	$13.59\pm 0.01$	$13.00\pm 0.01$		$8.4\pm 1.9$	$-13.0\pm 1.6$	1.6	71	16.3
2MASS J04354526+2737130	$19.65\pm 0.01$	$17.94\pm 0.01$	$16.99\pm 0.01$		$8.7\pm 4.3$	$-24.7\pm 1.7$	2.0	57	15.2
2MASS J04355143+2249119	$20.23\pm 0.01$	$18.55\pm 0.01$	$17.53\pm 0.02$		$20.7\pm 6.4$	$-14.3\pm 2.5$	2.7	59	16.3
2MASS J04355209+2255039	$14.78\pm 0.01$	$13.74\pm 0.01$	$13.14\pm 0.01$		$5.9\pm 1.9$	$-4.4\pm 2.2$	3.2	71	16.3
2MASS J04355760+2253574	$18.57\pm 0.01$	$17.55\pm 0.01$	$17.00\pm 0.02$		$20.0\pm 5.4$	$-12.6\pm 2.3$	4.6	69	16.3
2MASS J04355949+2238291	$17.21\pm 0.03$	$16.73\pm 0.02$	$16.25\pm 0.01$		$13.8\pm 3.2$	$-14.0\pm 3.8$	4.8	89	16.3
2MASS J04361030+2159364	$19.19\pm 0.01$	$17.65\pm 0.02$	$16.71\pm 0.01$		$7.7\pm 2.8$	$-21.9\pm 2.9$	3.8	70	16.3
2MASS J04361038+2259560	$18.33\pm 0.01$	$16.79\pm 0.01$	$15.84\pm 0.01$		$12.6\pm 3.1$	$-15.1\pm 2.4$	3.1	64	16.3
2MASS J04362151+2351165	$16.02\pm 0.01$	$15.05\pm 0.01$	$14.55\pm 0.01$		$-0.4\pm 1.2$	$-16.7\pm 1.5$	2.7	54	16.3
2MASS J04363248+2421395	$15.57\pm 0.01$	$14.24\pm 0.01$	$13.41\pm 0.01$		$12.3\pm 1.9$	$-10.0\pm 1.4$	1.6	58	14.3
2MASS J04363893+2258119	$18.02\pm 0.01$	$16.48\pm 0.01$	$15.55\pm 0.01$		$13.3\pm 5.7$	$-24.9\pm 6.7$	32	62	16.3
2MASS J04373705+2331080	$\cdots$	$20.75\pm 0.03$	$19.67\pm 0.10$		$15.9\pm 13.5$	$-54.8\pm 13.4$	0.6	16	15.0
2MASS J04374333+3056563	$15.99\pm 0.01$	$15.09\pm 0.01$	$14.56\pm 0.01$		$6.4\pm 3.6$	$-10.6\pm 2.0$	6.5	81	15.1
2MASS J04375670+2546229	$17.21\pm 0.06$	$16.46\pm 0.07$	$16.00\pm 0.06$		$-4.6\pm 1.6$	$7.6\pm 3.4$	4.9	62	16.2
2MASS J04380083+2558572	$15.79\pm 0.01$	$14.34\pm 0.01$	$13.49\pm 0.01$		$-9.0\pm 5.3$	$-35.6\pm 7.5$	15	77	16.2
2MASS J04380191+2519266	$16.87\pm 0.01$	$16.07\pm 0.02$	$15.57\pm 0.01$		$29.6\pm 10.0$	$-45.3\pm 23.5$	35	78	16.2
2MASS J04381486+2611399	$18.98\pm 0.01$	$17.66\pm 0.01$	$16.92\pm 0.01$		$9.5\pm 2.8$	$-17.0\pm 4.6$	4.6	77	16.2
2MASS J04381630+2326402	$14.50\pm 0.01$	$13.65\pm 0.01$	$13.18\pm 0.01$		$8.6\pm 2.9$	$-16.2\pm 1.7$	3.9	69	16.2
2MASS J04382134+2609137	$\cdots$	$14.88\pm 0.07$	$13.82\pm 0.01$		$21.8\pm 2.9$	$-17.1\pm 3.1$	5.7	54	16.2
2MASS J04384725+1737260	$15.57\pm 0.01$	$14.67\pm 0.01$	$14.19\pm 0.01$		$6.0\pm 1.5$	$-19.7\pm 1.8$	1.9	76	17.2
2MASS J04385859+2336351	$14.99\pm 0.01$	$14.00\pm 0.01$	$13.44\pm 0.01$		$11.1\pm 1.5$	$-20.3\pm 2.7$	1.8	62	16.3
2MASS J04385871+2323595	$15.60\pm 0.01$	$14.53\pm 0.01$	$13.94\pm 0.01$		$5.3\pm 1.7$	$-20.0\pm 2.0$	1.6	70	16.3
2MASS J04390396+2544264	$16.74\pm 0.02$	$15.29\pm 0.01$	$14.47\pm 0.01$		$5.2\pm 2.2$	$-25.9\pm 2.7$	4.5	66	16.3
2MASS J04390525+2337450	$14.92\pm 0.02$	$14.57\pm 0.01$	$14.66\pm 0.02$		$31.8\pm 16.2$	$-31.5\pm 5.6$	11	77	16.3
2MASS J04390637+2334179	$15.20\pm 0.01$	$14.11\pm 0.01$	$13.51\pm 0.01$		$4.5\pm 1.2$	$-20.4\pm 1.2$	1.3	67	16.3
2MASS J04394748+2601407	$17.54\pm 0.02$	$15.79\pm 0.01$	$14.68\pm 0.01$		$3.5\pm 2.1$	$-11.1\pm 4.0$	4.7	56	16.3
2MASS J04400067+2358211	$15.70\pm 0.01$	$14.57\pm 0.01$	$13.95\pm 0.01$		$-7.8\pm 4.0$	$-37.2\pm 4.6$	8.7	64	16.3
2MASS J04400174+2556292	$18.99\pm 0.01$	$17.25\pm 0.01$	$16.08\pm 0.02$		$2.3\pm 3.9$	$3.9\pm 10.1$	15	46	16.3
2MASS J04400800+2605253	$18.34\pm 0.01$	$16.66\pm 0.01$	$15.68\pm 0.01$		$-2.2\pm 2.6$	$-11.4\pm 2.8$	2.1	47	16.3
2MASS J04403979+2519061	$15.89\pm 0.01$	$14.59\pm 0.01$	$13.81\pm 0.01$		$-0.1\pm 5.8$	$-8.2\pm 9.8$	17	89	16.3
2MASS J04410826+2556074	$16.98\pm 0.02$	$16.25\pm 0.03$	$15.86\pm 0.04$		$4.9\pm 4.5$	$-16.2\pm 6.6$	19	69	16.3
2MASS J04411078+2555116	$17.90\pm 0.07$	$16.31\pm 0.07$	$15.57\pm 0.04$		$-11.8\pm 7.4$	$-25.9\pm 4.1$	20	68	16.3
2MASS J04413882+2556267	$15.09\pm 0.02$	$14.21\pm 0.02$	$13.46\pm 0.05$		$0.0\pm 5.5$	$-27.4\pm 4.2$	23	79	16.3
2MASS J04414489+2301513	$18.37\pm 0.01$	$16.96\pm 0.01$	$16.10\pm 0.01$		$6.9\pm 2.2$	$-19.9\pm 1.5$	1.4	59	16.2
2MASS J04414825+2534304	$17.81\pm 0.02$	$16.82\pm 0.01$	$15.77\pm 0.02$		$10.9\pm 2.4$	$-16.6\pm 2.7$	3.6	69	16.3
2MASS J04422101+2520343	$14.61\pm 0.01$	$13.60\pm 0.01$	$13.03\pm 0.01$		$4.6\pm 2.2$	$-18.3\pm 2.0$	16	64	16.3
2MASS J04440164+1621324	$16.64\pm 0.01$	$15.52\pm 0.01$	$14.89\pm 0.01$		$11.3\pm 2.0$	$-21.0\pm 2.3$	5.3	85	17.2
2MASS J04442713+2512164	$14.95\pm 0.03$	$13.91\pm 0.08$	$13.53\pm 0.04$		$4.2\pm 1.7$	$-15.3\pm 1.5$	2.6	84	16.2
2MASS J04480632+1551251	$17.47\pm 0.01$	$16.31\pm 0.01$	$15.59\pm 0.01$		$13.8\pm 2.0$	$-19.0\pm 1.2$	3.4	71	17.2
2MASS J04484189+1703374	$17.09\pm 0.01$	$15.84\pm 0.01$	$15.13\pm 0.01$		$3.8\pm 1.8$	$-14.8\pm 2.0$	3.5	76	17.2
2MASS J04485745+2913521	$14.97\pm 0.01$	$13.94\pm 0.01$	$13.38\pm 0.01$		$12.9\pm 6.1$	$-17.5\pm 6.3$	21	71	17.1
2MASS J04485789+2913548	$16.59\pm 0.01$	$15.73\pm 0.04$	$15.31\pm 0.01$		$8.7\pm 6.5$	$-24.0\pm 6.3$	19	70	17.1
2MASS J04520668+3047175	$19.42\pm 0.02$	$18.21\pm 0.03$	$17.31\pm 0.01$		$9.2\pm 2.6$	$-31.6\pm 1.9$	3.9	65	17.0
2MASS J04520970+3037454	$16.02\pm 0.03$	$15.40\pm 0.05$	$15.02\pm 0.10$		$1.9\pm 1.3$	$-29.8\pm 2.0$	3.0	82	17.0
2MASS J04552333+3027366	$16.55\pm 0.01$	$15.38\pm 0.01$	$14.70\pm 0.01$		$-6.1\pm 4.5$	$-23.6\pm 1.8$	6.5	71	17.0
2MASS J04554046+3039057	$15.63\pm 0.01$	$14.70\pm 0.01$	$14.19\pm 0.01$		$5.0\pm 1.6$	$-22.9\pm 1.5$	2.7	73	17.0
2MASS J04554801+3028050	$16.45\pm 0.01$	$15.37\pm 0.01$	$14.74\pm 0.01$		$4.2\pm 4.0$	$-22.9\pm 2.4$	3.1	69	17.0
2MASS J04554969+3019400	$15.93\pm 0.01$	$14.88\pm 0.01$	$14.29\pm 0.01$		$5.8\pm 1.7$	$-22.5\pm 1.4$	1.8	49	17.0
2MASS J04555288+3006523	$14.51\pm 0.01$	$13.61\pm 0.01$	$13.07\pm 0.01$		$10.8\pm 2.1$	$-8.7\pm 1.1$	1.8	53	16.9
2MASS J04555636+3049374	$14.79\pm 0.01$	$13.88\pm 0.01$	$13.40\pm 0.01$		$5.9\pm 0.9$	$-23.6\pm 2.1$	4.6	77	17.0
2MASS J04574903+3015195	$20.54\pm 0.03$	$18.82\pm 0.02$	$17.80\pm 0.01$		$-5.2\pm 4.1$	$-24.1\pm 4.0$	0.9	48	17.0
2MASS J04591661+2840468	$18.14\pm 0.01$	$17.54\pm 0.08$	$17.56\pm 0.02$		$3.1\pm 3.3$	$3.1\pm 2.3$	1.1	48	17.0
2MASS J05052286+2531312	$14.86\pm 0.12$	$13.71\pm 0.07$	$13.40\pm 0.08$		$-0.2\pm 2.8$	$-17.9\pm 4.7$	21	79	14.9
2MASS J05064662+2104296	$14.90\pm 0.01$	$13.95\pm 0.01$	$13.44\pm 0.01$		$8.6\pm 2.3$	$-18.2\pm 2.2$	4.3	53	17.1
2MASS J05073903+2311068	$14.75\pm 0.01$	$14.08\pm 0.01$	$13.55\pm 0.01$		$6.5\pm 1.7$	$-17.4\pm 3.2$	3.6	36	17.2
PSO J077.1033+24.3809	$21.62\pm 0.10$	$20.18\pm 0.05$	$19.21\pm 0.06$		$14.1\pm 12.5$	$-27.1\pm 12.1$	0.6	27	16.0
Unreliable fits: ${\chi }_{\nu }^2\le 0.3$ or ${\chi }_{\nu }^2\ge 40$
2MASS J04141188+2811535	$16.76\pm 0.05$	$15.78\pm 0.03$	$14.99\pm 0.01$		$11.8\pm 5.5$	$-25.0\pm 19.5$	81	53	17.2
2MASS J04174955+2813318	$15.70\pm 0.02$	$15.00\pm 0.01$	$14.47\pm 0.01$		$-6.0\pm 4.4$	$-3.3\pm 12.2$	59	90	17.2
2MASS J04180796+2826036	$15.14\pm 0.01$	$13.91\pm 0.01$	$13.21\pm 0.01$		$15.0\pm 3.9$	$1.1\pm 12.1$	51	87	17.2
2MASS J04185813+2812234	$17.16\pm 0.02$	$16.04\pm 0.08$	$15.40\pm 0.06$		$25.4\pm 6.3$	$-81.7\pm 36.5$	61	97	17.2
2MASS J04292373+2433002	$15.51\pm 0.04$	$14.93\pm 0.10$	$14.41\pm 0.14$		$-23.6\pm 14.6$	$68.5\pm 27.1$	66	71	17.1
WISE J043835.50+261041.9	$16.20\pm 0.04$	$15.69\pm 0.07$	$15.12\pm 0.02$		$2.2\pm 6.1$	$-21.7\pm 7.0$	44	65	5.1aaThis object does not have a 2MASS detection.
2MASS J04391389+2553208	$\cdots$	$\cdots$	$19.75\pm 0.14$		$-2.0\pm 462.7$	$-5.4\pm 65.0$	0.2	7	15.0

Table 9. Table 9: Proper Motions of Upper Scorpius Members

	Photometry				Proper Motion
Name	$i_{\mathrm{P1}}$	$z_{\mathrm{P1}}$	$y_{\mathrm{P1}}$		${\mu }_{\alpha }\cos \delta$	${\mu }_{\delta }$	${\chi }_{\nu }^2$	$N_{\mathrm{ep}}$	$\Delta t$
	(mag)	(mag)	(mag)		(mas yr-1)	(mas yr-1)			(yr)
Reliable fits:
2MASS J15350863$-$2532397	$17.98\pm 0.01$	$16.86\pm 0.01$	$16.28\pm 0.01$		$-10.2\pm 6.8$	$-13.5\pm 4.8$	4.7	47	16.5
2MASS J15355111$-$2021008	$18.73\pm 0.01$	$17.32\pm 0.01$	$16.50\pm 0.01$		$-11.2\pm 1.6$	$-17.6\pm 2.2$	1.2	38	16.6
2MASS J15411302$-$2308161	$18.14\pm 0.01$	$17.02\pm 0.01$	$16.40\pm 0.01$		$-12.1\pm 2.2$	$-22.8\pm 1.9$	1.1	48	15.3
2MASS J15420830$-$2621138	$16.83\pm 0.01$	$15.85\pm 0.01$	$15.32\pm 0.01$		$-10.9\pm 3.3$	$-16.8\pm 6.6$	3.7	53	15.7
2MASS J15423609$-$2108428	$18.39\pm 0.01$	$17.02\pm 0.01$	$16.22\pm 0.01$		$-11.1\pm 6.3$	$-13.5\pm 5.0$	6.3	37	16.6
2MASS J15433947$-$2535549	$20.47\pm 0.03$	$18.85\pm 0.02$	$17.83\pm 0.02$		$-15.9\pm 4.5$	$-16.6\pm 4.4$	0.7	41	15.3
2MASS J15442275$-$2136092	$18.29\pm 0.01$	$17.23\pm 0.01$	$16.60\pm 0.01$		$-13.2\pm 2.2$	$-28.2\pm 2.1$	0.9	52	16.6
2MASS J15453662$-$2510493	$17.85\pm 0.01$	$16.70\pm 0.01$	$16.05\pm 0.01$		$-10.9\pm 1.8$	$-20.2\pm 2.1$	2.0	55	15.7
2MASS J15465432$-$2556520	$15.93\pm 0.01$	$14.93\pm 0.01$	$14.40\pm 0.01$		$-11.3\pm 1.9$	$-15.3\pm 4.1$	4.2	64	15.7
2MASS J15470494$-$2137403	$15.55\pm 0.01$	$14.68\pm 0.01$	$14.21\pm 0.01$		$-5.9\pm 3.7$	$-8.5\pm 3.3$	4.0	51	16.6
2MASS J15472282$-$2139141	$20.13\pm 0.02$	$18.72\pm 0.02$	$17.83\pm 0.03$		$-9.2\pm 2.3$	$-21.1\pm 2.3$	1.0	45	16.6
2MASS J15472572$-$2609185	$17.22\pm 0.02$	$16.10\pm 0.01$	$15.45\pm 0.01$		$-13.2\pm 2.0$	$-27.5\pm 2.6$	2.0	54	15.3
2MASS J15480057$-$1815003	$18.72\pm 0.01$	$17.38\pm 0.01$	$16.62\pm 0.01$		$-10.8\pm 2.3$	$-21.7\pm 2.3$	1.2	37	15.9
PSO J237.1470$-$23.1489	$18.69\pm 0.01$	$17.41\pm 0.01$	$16.61\pm 0.01$		$-11.4\pm 2.8$	$-19.7\pm 2.8$	2.1	34	16.6
2MASS J15490414$-$2120150	$17.14\pm 0.01$	$16.03\pm 0.01$	$15.43\pm 0.01$		$-6.6\pm 2.2$	$-8.5\pm 2.5$	2.0	59	16.6
2MASS J15490803$-$2839550	$16.39\pm 0.01$	$15.49\pm 0.01$	$15.02\pm 0.01$		$-20.4\pm 3.2$	$-18.2\pm 1.9$	4.9	67	15.7
2MASS J15491602$-$2547146	$15.92\pm 0.01$	$14.97\pm 0.01$	$14.49\pm 0.01$		$-21.2\pm 1.8$	$-18.0\pm 2.3$	2.3	47	15.3
2MASS J15492260$-$2146574	$14.61\pm 0.01$	$13.87\pm 0.01$	$13.49\pm 0.01$		$-17.1\pm 1.6$	$-18.2\pm 1.4$	2.2	66	16.6
2MASS J15492909$-$2815384	$16.01\pm 0.01$	$15.03\pm 0.01$	$14.47\pm 0.01$		$-15.9\pm 1.5$	$-22.4\pm 3.4$	2.2	54	15.3
2MASS J15493660$-$2815141	$16.31\pm 0.01$	$15.35\pm 0.01$	$14.86\pm 0.01$		$-14.5\pm 1.2$	$-14.9\pm 4.1$	2.1	66	15.7
2MASS J15493784$-$2514102	$18.73\pm 0.01$	$17.38\pm 0.01$	$16.60\pm 0.01$		$-22.8\pm 2.0$	$-26.0\pm 3.7$	1.5	45	15.7
2MASS J15495069$-$2233511	$17.51\pm 0.01$	$16.20\pm 0.01$	$15.47\pm 0.01$		$24.4\pm 14.9$	$-13.6\pm 5.8$	10	54	16.1
2MASS J15495733$-$2201256	$16.69\pm 0.01$	$15.59\pm 0.01$	$14.98\pm 0.01$		$-9.1\pm 12.7$	$-18.5\pm 2.6$	8.8	59	16.6
2MASS J15501958$-$2805237	$17.78\pm 0.01$	$16.70\pm 0.01$	$16.11\pm 0.01$		$-14.6\pm 1.4$	$-16.3\pm 4.8$	4.3	71	15.7
2MASS J15511870$-$2145235	$14.76\pm 0.01$	$13.98\pm 0.01$	$13.57\pm 0.01$		$-10.6\pm 2.3$	$-19.6\pm 4.7$	9.4	60	16.6
2MASS J15514032$-$2146103	$14.70\pm 0.01$	$13.88\pm 0.01$	$13.45\pm 0.01$		$-13.1\pm 2.9$	$-17.1\pm 2.0$	4.1	58	16.6
2MASS J15514709$-$2113234	$16.44\pm 0.08$	$15.61\pm 0.07$	$15.32\pm 0.01$		$-9.6\pm 1.0$	$-15.3\pm 1.6$	1.3	70	16.6
2MASS J15514758$-$2329332	$18.31\pm 0.01$	$16.96\pm 0.01$	$16.17\pm 0.01$		$-11.5\pm 1.5$	$-16.8\pm 3.8$	1.4	45	16.6
2MASS J15521088$-$2125372	$17.22\pm 0.01$	$16.90\pm 0.12$	$16.73\pm 0.19$		$-9.9\pm 3.9$	$-16.1\pm 2.6$	2.3	64	16.6
2MASS J15522255$-$2313361	$17.33\pm 0.01$	$16.11\pm 0.01$	$15.45\pm 0.01$		$-16.5\pm 1.5$	$-17.8\pm 5.0$	1.7	55	16.6
2MASS J15524857$-$2621453	$16.25\pm 0.01$	$15.30\pm 0.01$	$14.78\pm 0.01$		$-16.0\pm 1.3$	$-13.9\pm 7.8$	6.3	46	15.7
2MASS J15530132$-$2114135	$14.78\pm 0.01$	$13.93\pm 0.01$	$13.47\pm 0.01$		$-9.5\pm 1.5$	$-20.8\pm 1.9$	1.5	59	16.3
2MASS J15541998$-$2135428	$19.00\pm 0.01$	$17.56\pm 0.01$	$16.70\pm 0.01$		$-7.3\pm 3.0$	$-24.1\pm 2.7$	1.0	42	16.3
2MASS J15543065$-$2536054	$18.67\pm 0.01$	$17.41\pm 0.01$	$16.73\pm 0.01$		$-10.6\pm 2.3$	$-19.0\pm 4.6$	1.6	47	15.7
2MASS J15543190$-$2221564	$17.95\pm 0.01$	$16.65\pm 0.01$	$15.92\pm 0.01$		$-18.3\pm 3.5$	$-18.5\pm 3.0$	2.8	38	16.6
2MASS J15544486$-$2843078	$17.16\pm 0.01$	$16.15\pm 0.01$	$15.62\pm 0.01$		$-21.1\pm 4.3$	$-31.7\pm 3.6$	5.4	64	15.1
2MASS J15550531$-$2117402	$15.52\pm 0.01$	$14.59\pm 0.01$	$14.08\pm 0.01$		$-10.8\pm 1.7$	$-18.1\pm 2.6$	3.7	50	16.3
2MASS J15551960$-$2751207	$17.45\pm 0.01$	$16.30\pm 0.01$	$15.64\pm 0.01$		$-17.7\pm 2.3$	$-33.9\pm 2.0$	1.5	56	15.1
2MASS J15552561$-$1817484	$15.69\pm 0.01$	$14.56\pm 0.01$	$13.95\pm 0.01$		$-8.2\pm 1.4$	$-20.2\pm 1.7$	2.8	73	16.6
2MASS J15553243$-$2308171	$15.57\pm 0.01$	$15.12\pm 0.02$	$14.87\pm 0.01$		$35.9\pm 7.9$	$31.8\pm 11.5$	19	57	16.6
2MASS J15555600$-$2045187	$16.99\pm 0.01$	$16.13\pm 0.05$	$15.37\pm 0.01$		$-11.2\pm 1.6$	$-24.4\pm 1.6$	1.3	60	16.1
2MASS J15560104$-$2338081	$17.18\pm 0.01$	$16.04\pm 0.01$	$15.43\pm 0.01$		$-13.6\pm 1.5$	$-20.0\pm 3.2$	2.4	75	16.6
2MASS J15560497$-$2106461	$17.82\pm 0.01$	$16.52\pm 0.01$	$15.77\pm 0.01$		$-13.8\pm 1.1$	$-16.9\pm 4.6$	1.5	50	16.6
2MASS J15561216$-$2354076	$\cdots$	$\cdots$	$12.51\pm 0.02$		$-19.7\pm 3.9$	$-30.0\pm 3.0$	3.3	28	15.7
2MASS J15561978$-$2423288	$16.26\pm 0.01$	$15.32\pm 0.01$	$14.83\pm 0.01$		$-3.1\pm 10.5$	$-19.0\pm 3.8$	21	76	15.7
2MASS J15562060$-$2336099	$\cdots$	$\cdots$	$12.62\pm 0.01$		$-12.1\pm 3.1$	$-14.2\pm 3.8$	3.6	64	16.6
2MASS J15563425$-$2003332	$14.63\pm 0.01$	$13.73\pm 0.01$	$13.26\pm 0.01$		$-11.3\pm 1.9$	$-17.9\pm 2.8$	3.5	51	16.6
2MASS J15570641$-$2206060	$14.93\pm 0.01$	$14.06\pm 0.01$	$13.65\pm 0.01$		$-11.3\pm 2.9$	$-17.1\pm 2.8$	3.0	50	15.7
2MASS J15571279$-$2343465	$16.64\pm 0.01$	$15.59\pm 0.01$	$14.99\pm 0.01$		$-11.9\pm 1.4$	$-15.7\pm 2.2$	2.5	52	15.7
2MASS J15572343$-$2924290	$18.30\pm 0.01$	$17.08\pm 0.01$	$16.37\pm 0.01$		$-17.9\pm 2.6$	$-29.1\pm 3.6$	2.0	39	15.1
2MASS J15572692$-$2715094	$16.45\pm 0.01$	$15.57\pm 0.01$	$15.11\pm 0.01$		$-21.5\pm 1.8$	$-48.6\pm 2.8$	2.6	62	14.9
2MASS J15572849$-$2219051	$15.37\pm 0.01$	$14.48\pm 0.01$	$14.01\pm 0.01$		$-16.0\pm 5.2$	$-14.6\pm 3.1$	12	51	14.6
2MASS J15572919$-$2215237	$16.00\pm 0.01$	$15.22\pm 0.01$	$14.82\pm 0.01$		$-29.4\pm 3.5$	$-8.1\pm 2.6$	14	53	14.6
2MASS J15572986$-$2258438	$14.77\pm 0.01$	$13.94\pm 0.01$	$13.51\pm 0.01$		$-26.4\pm 12.0$	$-11.2\pm 4.6$	17	73	14.6
2MASS J15573718$-$2245251	$15.65\pm 0.01$	$15.06\pm 0.01$	$14.77\pm 0.01$		$-9.8\pm 1.6$	$-12.0\pm 1.5$	1.8	65	14.1
2MASS J15574250$-$2226055	$14.73\pm 0.01$	$14.03\pm 0.01$	$13.67\pm 0.01$		$-13.2\pm 1.5$	$-21.0\pm 2.7$	3.2	53	14.6
2MASS J15574757$-$2444121	$15.66\pm 0.01$	$14.81\pm 0.01$	$14.40\pm 0.01$		$-12.7\pm 1.3$	$-19.1\pm 5.0$	2.6	62	15.7
2MASS J15581571$-$2021368	$14.66\pm 0.01$	$13.81\pm 0.01$	$13.39\pm 0.01$		$-11.1\pm 2.0$	$-21.5\pm 2.9$	4.4	63	15.7
2MASS J15581884$-$1915448	$\cdots$	$\cdots$	$12.57\pm 0.01$		$-8.2\pm 2.3$	$-16.7\pm 3.9$	3.0	76	15.7
2MASS J15582337$-$2151588	$15.19\pm 0.01$	$14.25\pm 0.01$	$13.73\pm 0.01$		$-7.5\pm 2.2$	$-19.1\pm 3.2$	2.1	57	15.1
2MASS J15582376$-$2721435	$15.96\pm 0.01$	$15.04\pm 0.01$	$14.56\pm 0.01$		$-6.4\pm 2.1$	$-22.9\pm 2.3$	1.9	66	15.1
2MASS J15582981$-$2310077	$14.96\pm 0.01$	$14.08\pm 0.01$	$13.67\pm 0.01$		$-9.4\pm 1.5$	$-18.0\pm 4.9$	3.6	66	15.7
2MASS J15583162$-$2402538	$16.07\pm 0.03$	$15.16\pm 0.01$	$14.65\pm 0.01$		$-13.5\pm 4.2$	$-21.1\pm 4.2$	9.1	45	15.1
2MASS J15583598$-$2348136	$15.88\pm 0.01$	$14.96\pm 0.01$	$14.46\pm 0.01$		$-10.3\pm 3.0$	$-24.2\pm 2.4$	23	68	15.1
2MASS J15584813$-$2141338	$16.49\pm 0.01$	$15.51\pm 0.01$	$15.00\pm 0.01$		$-21.9\pm 1.7$	$-30.0\pm 4.0$	2.1	45	15.7
PSO J239.7015$-$23.2665	$20.88\pm 0.05$	$19.26\pm 0.01$	$18.24\pm 0.02$		$-0.1\pm 7.2$	$-23.0\pm 3.5$	0.7	38	15.7
2MASS J15590193$-$2616329	$14.84\pm 0.01$	$13.97\pm 0.01$	$13.52\pm 0.01$		$-13.7\pm 1.2$	$-17.1\pm 5.4$	2.8	50	16.5
2MASS J15591135$-$2338002	$17.89\pm 0.01$	$16.66\pm 0.01$	$15.97\pm 0.01$		$-11.0\pm 1.1$	$-20.9\pm 2.3$	3.1	56	14.6
2MASS J15591244$-$2236502	$15.64\pm 0.01$	$14.73\pm 0.01$	$14.21\pm 0.01$		$-10.7\pm 2.1$	$-16.7\pm 2.9$	4.8	60	14.6
2MASS J15591513$-$2840411	$15.58\pm 0.01$	$14.79\pm 0.01$	$14.39\pm 0.01$		$-13.9\pm 2.2$	$-16.5\pm 2.2$	4.0	61	16.5
2MASS J15592591$-$2305081	$15.64\pm 0.01$	$14.58\pm 0.01$	$14.01\pm 0.01$		$-9.1\pm 1.6$	$-27.3\pm 1.9$	2.4	60	15.1
2MASS J15594366$-$2014396	$17.93\pm 0.01$	$16.63\pm 0.01$	$15.87\pm 0.01$		$-11.9\pm 2.3$	$-24.0\pm 2.0$	2.0	54	15.1
2MASS J15594439$-$1928191	$18.37\pm 0.01$	$17.02\pm 0.01$	$16.25\pm 0.01$		$-23.6\pm 16.0$	$-20.2\pm 3.3$	23	41	15.1
2MASS J15594802$-$2227162	$17.80\pm 0.01$	$16.56\pm 0.01$	$15.85\pm 0.01$		$-9.8\pm 2.0$	$-16.3\pm 3.2$	1.4	57	15.7
2MASS J15594970$-$2301576	$15.74\pm 0.01$	$14.78\pm 0.01$	$14.25\pm 0.01$		$-5.7\pm 1.9$	$-21.4\pm 1.9$	2.2	68	15.1
2MASS J15595868$-$1836520	$16.83\pm 0.01$	$15.67\pm 0.01$	$15.05\pm 0.01$		$-7.6\pm 3.0$	$-16.9\pm 1.8$	1.5	61	15.7
2MASS J16000713$-$2224066	$15.86\pm 0.01$	$15.17\pm 0.01$	$14.83\pm 0.01$		$-26.4\pm 2.1$	$-3.2\pm 1.7$	3.3	55	15.7
2MASS J16001610$-$1726071	$18.04\pm 0.01$	$16.78\pm 0.01$	$16.07\pm 0.01$		$-8.5\pm 1.2$	$-10.6\pm 1.9$	1.4	84	16.7
2MASS J16001730$-$2236504	$\cdots$	$\cdots$	$12.61\pm 0.04$		$-16.4\pm 7.7$	$-30.0\pm 11.8$	13	40	15.7
2MASS J16001944$-$2256287	$18.33\pm 0.01$	$17.00\pm 0.01$	$16.24\pm 0.01$		$-11.0\pm 2.1$	$-19.2\pm 4.8$	1.5	56	15.7
2MASS J16002323$-$2329595	$18.40\pm 0.02$	$17.04\pm 0.01$	$16.23\pm 0.02$		$51.4\pm 32.0$	$-46.1\pm 16.0$	23	36	15.7
2MASS J16002631$-$2259412	$15.31\pm 0.01$	$14.32\pm 0.01$	$13.78\pm 0.01$		$-10.0\pm 1.8$	$-23.5\pm 2.0$	2.7	69	15.1
2MASS J16002669$-$2056316	$16.45\pm 0.01$	$15.50\pm 0.01$	$14.97\pm 0.01$		$-3.4\pm 3.1$	$-11.1\pm 5.5$	7.0	75	15.7
2MASS J16003023$-$2334457	$15.85\pm 0.01$	$14.83\pm 0.01$	$14.30\pm 0.01$		$-10.8\pm 1.1$	$-15.6\pm 2.7$	2.7	57	15.7
2MASS J16004318$-$2229143	$19.17\pm 0.01$	$17.77\pm 0.01$	$17.00\pm 0.01$		$-10.8\pm 1.6$	$-17.2\pm 3.4$	1.5	54	15.7
2MASS J16005065$-$1927502	$15.71\pm 0.01$	$14.61\pm 0.02$	$13.95\pm 0.01$		$-4.2\pm 2.1$	$-18.1\pm 2.2$	4.5	69	15.1
2MASS J16005265$-$2812087	$16.65\pm 0.01$	$15.66\pm 0.01$	$15.10\pm 0.01$		$-6.8\pm 1.6$	$-28.8\pm 1.6$	1.5	73	15.9
2MASS J16010605$-$2215246	$14.90\pm 0.01$	$14.12\pm 0.01$	$13.70\pm 0.01$		$-8.1\pm 1.9$	$-29.2\pm 2.8$	2.7	57	15.1
2MASS J16011915$-$2306394	$16.86\pm 0.01$	$15.78\pm 0.01$	$15.19\pm 0.01$		$-16.6\pm 2.3$	$-27.9\pm 3.7$	3.4	50	15.1
2MASS J16012238$-$2708194	$18.80\pm 0.01$	$17.38\pm 0.01$	$16.55\pm 0.01$		$-6.7\pm 2.4$	$-20.1\pm 3.8$	2.1	58	16.5
2MASS J16012902$-$2509069	$\cdots$	$\cdots$	$12.67\pm 0.01$		$-10.9\pm 1.6$	$-100.6\pm 32.4$	27	69	16.5
2MASS J16014157$-$2111380	$15.88\pm 0.02$	$14.89\pm 0.04$	$14.38\pm 0.01$		$-10.2\pm 1.4$	$-17.5\pm 2.2$	1.7	76	16.5
2MASS J16014528$-$2138551	$18.91\pm 0.01$	$17.64\pm 0.01$	$16.92\pm 0.01$		$-6.3\pm 2.3$	$-10.4\pm 1.7$	1.8	64	16.5
2MASS J16014769$-$2441011	$16.85\pm 0.01$	$15.89\pm 0.01$	$15.38\pm 0.01$		$-7.9\pm 1.7$	$-15.7\pm 5.7$	2.1	46	16.5
2MASS J16014955$-$2351082	$15.64\pm 0.01$	$14.76\pm 0.01$	$14.30\pm 0.01$		$-10.4\pm 1.9$	$-19.3\pm 1.7$	4.1	54	16.5
2MASS J16015498$-$2131230	$16.22\pm 0.01$	$15.23\pm 0.01$	$14.69\pm 0.01$		$-14.6\pm 3.4$	$-23.2\pm 1.6$	12	66	16.0
2MASS J16015976$-$1952202	$15.29\pm 0.01$	$14.36\pm 0.01$	$13.89\pm 0.01$		$-15.3\pm 2.0$	$-27.8\pm 2.2$	3.1	66	16.0
2MASS J16020287$-$2236139	$14.77\pm 0.01$	$14.32\pm 0.01$	$14.10\pm 0.01$		$-22.0\pm 8.6$	$-50.3\pm 9.1$	15	50	16.5
2MASS J16020429$-$2050425	$16.05\pm 0.01$	$14.98\pm 0.01$	$14.38\pm 0.01$		$-5.1\pm 1.6$	$-18.0\pm 3.9$	2.8	79	16.5
2MASS J16021096$-$2007495	$15.16\pm 0.01$	$14.28\pm 0.01$	$13.83\pm 0.01$		$-6.0\pm 1.6$	$-13.9\pm 3.6$	3.1	78	16.5
2MASS J16021489$-$2438325	$14.93\pm 0.01$	$14.01\pm 0.01$	$13.52\pm 0.01$		$-16.8\pm 1.5$	$-34.8\pm 2.9$	2.4	41	15.9
2MASS J16022357$-$2259332	$14.89\pm 0.01$	$13.91\pm 0.01$	$13.38\pm 0.01$		$-10.8\pm 2.0$	$-17.2\pm 5.1$	2.9	56	16.5
2MASS J16022616$-$2002403	$14.65\pm 0.01$	$13.79\pm 0.01$	$13.34\pm 0.01$		$-6.9\pm 1.1$	$-14.2\pm 7.5$	4.4	83	16.5
2MASS J16023185$-$2132340	$15.65\pm 0.01$	$14.73\pm 0.01$	$14.20\pm 0.01$		$-7.2\pm 3.6$	$-16.6\pm 3.4$	4.5	39	16.5
2MASS J16023227$-$2200486	$16.57\pm 0.01$	$15.48\pm 0.01$	$14.88\pm 0.01$		$-10.4\pm 1.5$	$-20.2\pm 1.8$	1.4	64	16.0
2MASS J16023418$-$2200354	$16.25\pm 0.01$	$15.02\pm 0.01$	$14.37\pm 0.01$		$-11.9\pm 1.7$	$-22.9\pm 1.3$	1.7	70	16.0
2MASS J16023587$-$2320170	$\cdots$	$\cdots$	$12.53\pm 0.01$		$-10.8\pm 3.4$	$-27.7\pm 6.3$	8.8	39	16.5
2MASS J16024142$-$2248419	$16.20\pm 0.01$	$15.17\pm 0.01$	$14.56\pm 0.01$		$-10.9\pm 2.0$	$-20.1\pm 6.2$	3.6	42	16.5
2MASS J16024152$-$2138245	$15.05\pm 0.01$	$14.22\pm 0.01$	$13.72\pm 0.01$		$-11.7\pm 1.6$	$-13.9\pm 2.8$	3.5	71	16.5
2MASS J16024448$-$2543323	$14.68\pm 0.01$	$13.93\pm 0.01$	$13.57\pm 0.01$		$-12.5\pm 3.3$	$-16.2\pm 4.2$	5.9	75	16.5
2MASS J16024544$-$1930377	$15.08\pm 0.01$	$14.12\pm 0.01$	$13.60\pm 0.01$		$-6.7\pm 1.1$	$-14.9\pm 2.6$	3.0	87	16.0
2MASS J16024546$-$1946034	$15.25\pm 0.01$	$14.65\pm 0.01$	$14.33\pm 0.01$		$-3.5\pm 1.1$	$6.5\pm 5.5$	3.1	95	16.5
2MASS J16024575$-$2304509	$15.35\pm 0.01$	$14.38\pm 0.01$	$13.87\pm 0.01$		$-21.3\pm 1.8$	$-26.6\pm 6.1$	3.3	56	16.5
2MASS J16025116$-$2401502	$15.67\pm 0.01$	$14.65\pm 0.01$	$14.04\pm 0.01$		$-16.5\pm 5.6$	$-10.1\pm 12.3$	24	46	16.5
2MASS J16025214$-$2121296	$18.52\pm 0.01$	$17.10\pm 0.02$	$16.34\pm 0.01$		$-5.4\pm 1.9$	$-17.6\pm 1.9$	2.1	54	16.5
2MASS J16025529$-$1922431	$16.06\pm 0.01$	$14.95\pm 0.01$	$14.33\pm 0.01$		$-11.0\pm 1.8$	$-19.5\pm 1.5$	2.2	97	16.0
2MASS J16030161$-$2207523	$15.70\pm 0.01$	$14.78\pm 0.01$	$14.27\pm 0.01$		$-9.1\pm 2.1$	$-18.7\pm 4.4$	4.1	51	16.5
2MASS J16031329$-$2112569	$14.98\pm 0.01$	$14.12\pm 0.01$	$13.62\pm 0.01$		$-9.5\pm 1.9$	$-19.3\pm 3.1$	3.3	83	16.5
2MASS J16031491$-$2234454	$14.59\pm 0.01$	$13.62\pm 0.01$	$13.13\pm 0.01$		$-9.7\pm 1.4$	$-19.0\pm 7.0$	3.9	51	16.5
2MASS J16032625$-$2155378	$15.46\pm 0.01$	$14.56\pm 0.01$	$14.05\pm 0.01$		$-11.3\pm 1.5$	$-19.1\pm 2.9$	2.2	67	16.5
2MASS J16032940$-$1955038	$14.62\pm 0.01$	$13.81\pm 0.01$	$13.39\pm 0.01$		$-3.9\pm 1.1$	$-12.8\pm 2.8$	5.2	93	16.5
2MASS J16033471$-$1829303	$15.54\pm 0.01$	$14.56\pm 0.01$	$14.02\pm 0.01$		$-7.0\pm 1.0$	$-16.5\pm 1.5$	2.3	84	16.5
2MASS J16034030$-$2335237	$14.79\pm 0.01$	$14.01\pm 0.01$	$13.61\pm 0.01$		$-10.2\pm 2.9$	$-16.9\pm 6.9$	5.6	51	16.5
2MASS J16035175$-$2140154	$14.57\pm 0.01$	$13.55\pm 0.01$	$13.00\pm 0.01$		$-9.3\pm 1.5$	$-24.4\pm 2.1$	2.1	70	16.0
2MASS J16035404$-$2509393	$14.91\pm 0.01$	$14.08\pm 0.01$	$13.64\pm 0.01$		$-10.5\pm 2.0$	$-21.9\pm 5.4$	6.3	61	16.5
2MASS J16035652$-$2357250	$16.51\pm 0.01$	$15.59\pm 0.01$	$15.08\pm 0.01$		$-8.6\pm 1.1$	$-16.1\pm 4.2$	1.9	47	16.5
2MASS J16041792$-$1941505	$16.65\pm 0.01$	$15.47\pm 0.01$	$14.91\pm 0.01$		$-5.7\pm 1.4$	$-16.2\pm 2.2$	1.5	78	16.5
2MASS J16042796$-$1904337	$14.77\pm 0.01$	$13.93\pm 0.01$	$13.46\pm 0.01$		$-1.8\pm 1.7$	$-16.9\pm 4.4$	8.5	78	16.5
2MASS J16043565$-$1948302	$15.02\pm 0.01$	$14.10\pm 0.01$	$13.58\pm 0.01$		$-9.1\pm 1.7$	$-21.8\pm 2.3$	3.2	70	15.9
2MASS J16044026$-$2254323	$18.00\pm 0.01$	$16.72\pm 0.01$	$16.18\pm 0.04$		$-10.6\pm 3.3$	$-17.4\pm 2.7$	5.0	49	16.5
2MASS J16044068$-$1946538	$16.56\pm 0.01$	$15.53\pm 0.01$	$14.96\pm 0.01$		$-5.8\pm 1.9$	$-14.8\pm 3.5$	5.7	91	16.5
2MASS J16044075$-$1936525	$17.04\pm 0.01$	$15.84\pm 0.01$	$15.15\pm 0.01$		$-8.7\pm 2.9$	$-16.5\pm 4.8$	2.0	74	16.5
2MASS J16044303$-$2318258	$17.14\pm 0.01$	$15.98\pm 0.01$	$15.31\pm 0.01$		$-8.7\pm 1.5$	$-17.9\pm 2.4$	1.5	88	16.5
2MASS J16044930$-$2045581	$19.21\pm 0.01$	$17.76\pm 0.01$	$16.90\pm 0.01$		$-6.0\pm 1.6$	$-16.9\pm 2.4$	1.4	47	16.5
2MASS J16044997$-$2038353	$14.86\pm 0.01$	$13.90\pm 0.01$	$13.40\pm 0.01$		$-6.9\pm 2.0$	$-16.1\pm 5.2$	4.8	74	16.5
2MASS J16045199$-$2224108	$17.85\pm 0.01$	$16.44\pm 0.01$	$15.65\pm 0.01$		$-9.1\pm 2.1$	$-20.4\pm 2.1$	1.0	52	15.9
2MASS J16045379$-$2002271	$16.38\pm 0.01$	$15.40\pm 0.01$	$14.87\pm 0.01$		$-7.8\pm 0.8$	$-16.1\pm 2.0$	1.6	81	16.5
2MASS J16045581$-$2307438	$17.38\pm 0.01$	$16.14\pm 0.01$	$15.42\pm 0.01$		$-6.4\pm 3.6$	$-18.2\pm 5.7$	2.4	72	16.5
2MASS J16045716$-$2104160	$15.07\pm 0.01$	$14.27\pm 0.01$	$13.84\pm 0.01$		$-7.5\pm 2.2$	$-19.5\pm 5.8$	2.5	67	16.5
2MASS J16050231$-$1941554	$15.14\pm 0.01$	$14.32\pm 0.01$	$13.89\pm 0.01$		$-7.2\pm 2.3$	$-14.8\pm 6.0$	7.1	79	16.5
2MASS J16050474$-$1956274	$\cdots$	$\cdots$	$12.54\pm 0.01$		$-0.7\pm 4.7$	$-17.4\pm 5.6$	24	81	16.5
2MASS J16051403$-$2406524	$16.16\pm 0.01$	$15.01\pm 0.01$	$14.39\pm 0.01$		$-12.0\pm 1.4$	$-24.1\pm 1.7$	1.6	80	16.0
2MASS J16051615$-$1938310	$15.03\pm 0.01$	$14.21\pm 0.01$	$13.80\pm 0.01$		$-6.0\pm 2.3$	$-18.3\pm 5.3$	3.4	59	16.5
2MASS J16052556$-$2035397	$15.05\pm 0.01$	$14.09\pm 0.01$	$13.57\pm 0.01$		$-5.8\pm 3.2$	$-33.3\pm 6.8$	4.7	71	16.5
2MASS J16052787$-$2115510	$15.87\pm 0.01$	$15.00\pm 0.01$	$14.51\pm 0.01$		$-7.2\pm 1.8$	$-14.1\pm 2.6$	2.5	85	16.5
2MASS J16053077$-$2246200	$17.18\pm 0.01$	$16.03\pm 0.01$	$15.38\pm 0.01$		$-12.1\pm 3.0$	$-21.9\pm 2.2$	2.1	71	15.1
2MASS J16053128$-$1926240	$15.35\pm 0.01$	$14.43\pm 0.01$	$13.93\pm 0.01$		$-8.4\pm 2.1$	$-21.1\pm 1.7$	1.6	64	15.1
2MASS J16053215$-$1933159	$15.49\pm 0.01$	$14.67\pm 0.01$	$14.28\pm 0.01$		$-7.4\pm 1.2$	$-15.6\pm 3.4$	2.0	57	15.7
2MASS J16054416$-$2155054	$14.91\pm 0.01$	$13.94\pm 0.01$	$13.40\pm 0.01$		$-14.0\pm 2.0$	$-36.0\pm 4.4$	4.3	67	15.1
2MASS J16054565$-$1948353	$15.49\pm 0.01$	$14.61\pm 0.01$	$14.14\pm 0.01$		$-7.5\pm 1.4$	$-15.4\pm 4.4$	2.6	64	15.7
2MASS J16054778$-$1945263	$14.88\pm 0.01$	$14.05\pm 0.01$	$13.63\pm 0.01$		$-5.2\pm 1.1$	$-13.6\pm 4.8$	2.9	76	15.7
2MASS J16055407$-$1818443	$16.78\pm 0.01$	$15.64\pm 0.01$	$15.00\pm 0.01$		$-4.8\pm 2.0$	$-14.7\pm 1.4$	1.6	68	15.7
2MASS J16055409$-$1818488	$21.26\pm 0.10$	$19.66\pm 0.03$	$18.71\pm 0.09$		$-16.2\pm 6.2$	$-31.7\pm 5.9$	1.2	15	14.1
2MASS J16060374$-$2219298	$20.55\pm 0.04$	$18.94\pm 0.02$	$17.97\pm 0.01$		$7.4\pm 7.9$	$-13.3\pm 2.7$	0.9	36	15.7
2MASS J16060391$-$2056443	$17.34\pm 0.01$	$16.02\pm 0.01$	$15.27\pm 0.01$		$-8.6\pm 2.1$	$-20.0\pm 4.4$	2.9	62	15.1
2MASS J16060629$-$2335133	$20.70\pm 0.04$	$19.23\pm 0.01$	$18.28\pm 0.01$		$-7.5\pm 6.5$	$-18.1\pm 6.4$	1.0	31	15.1
2MASS J16061144$-$1935405	$15.82\pm 0.03$	$14.96\pm 0.01$	$14.32\pm 0.01$		$-4.7\pm 3.4$	$-13.1\pm 1.7$	2.4	65	15.7
2MASS J16061199$-$1935331	$15.05\pm 0.01$	$14.05\pm 0.01$	$13.50\pm 0.01$		$-6.0\pm 1.7$	$-15.0\pm 1.7$	2.2	62	15.7
2MASS J16061935$-$1923326	$15.20\pm 0.01$	$14.31\pm 0.01$	$13.84\pm 0.01$		$-4.1\pm 2.8$	$-25.2\pm 2.7$	5.1	71	15.1
2MASS J16062277$-$2011243	$14.61\pm 0.01$	$13.84\pm 0.01$	$13.42\pm 0.01$		$-8.1\pm 3.3$	$-15.3\pm 2.9$	4.2	80	15.7
2MASS J16062389$-$1941165	$14.77\pm 0.01$	$13.82\pm 0.01$	$13.30\pm 0.01$		$-6.0\pm 1.2$	$-21.9\pm 1.9$	1.7	78	15.1
2MASS J16062637$-$2306113	$16.08\pm 0.01$	$15.17\pm 0.01$	$14.69\pm 0.01$		$-5.8\pm 2.3$	$-14.2\pm 4.2$	2.7	74	15.7
2MASS J16062860$-$2043317	$14.65\pm 0.01$	$13.71\pm 0.01$	$13.16\pm 0.01$		$-12.4\pm 1.2$	$-13.3\pm 4.9$	3.4	87	15.7
2MASS J16062870$-$2856580	$16.54\pm 0.01$	$15.57\pm 0.01$	$15.04\pm 0.01$		$-3.9\pm 1.7$	$-19.4\pm 1.7$	1.7	72	15.9
2MASS J16063210$-$2020538	$15.87\pm 0.01$	$14.95\pm 0.01$	$14.46\pm 0.01$		$-19.5\pm 8.9$	$-9.6\pm 8.1$	18	75	15.8
2MASS J16063461$-$2255043	$14.72\pm 0.01$	$13.86\pm 0.01$	$13.39\pm 0.01$		$-10.0\pm 1.6$	$-21.0\pm 2.4$	2.5	51	15.9
2MASS J16063539$-$2516510	$15.26\pm 0.01$	$14.41\pm 0.01$	$13.97\pm 0.01$		$-9.6\pm 1.4$	$-20.6\pm 5.1$	3.5	53	16.5
2MASS J16063922$-$2248340	$15.09\pm 0.01$	$14.24\pm 0.01$	$13.78\pm 0.01$		$-4.0\pm 2.3$	$-25.8\pm 4.9$	12	77	16.4
2MASS J16064102$-$2455489	$15.70\pm 0.01$	$14.89\pm 0.01$	$14.41\pm 0.01$		$-10.3\pm 1.8$	$-20.0\pm 4.1$	4.7	64	16.5
2MASS J16064266$-$1851140	$18.26\pm 0.01$	$16.86\pm 0.01$	$16.04\pm 0.01$		$-7.4\pm 2.1$	$-20.8\pm 2.1$	1.4	47	15.9
2MASS J16064818$-$2230400	$19.06\pm 0.01$	$17.61\pm 0.01$	$16.75\pm 0.01$		$-8.0\pm 1.4$	$-16.3\pm 4.0$	1.2	42	16.4
2MASS J16065018$-$2309539	$14.57\pm 0.01$	$13.74\pm 0.01$	$13.29\pm 0.01$		$-7.0\pm 1.9$	$-22.4\pm 2.4$	5.2	74	16.4
2MASS J16070009$-$2043102	$14.50\pm 0.01$	$13.70\pm 0.01$	$13.25\pm 0.01$		$-7.9\pm 1.4$	$-20.7\pm 3.8$	6.1	76	15.7
2MASS J16070051$-$2206362	$\cdots$	$13.05\pm 0.01$	$12.71\pm 0.01$		$-12.2\pm 1.1$	$-19.9\pm 2.3$	1.9	92	15.7
2MASS J16070169$-$2028579	$16.67\pm 0.01$	$15.74\pm 0.01$	$15.04\pm 0.01$		$-8.5\pm 2.2$	$-24.7\pm 3.1$	3.2	70	15.1
2MASS J16070474$-$2015557	$15.14\pm 0.01$	$14.32\pm 0.01$	$13.88\pm 0.01$		$-5.0\pm 1.2$	$-14.7\pm 5.0$	3.0	84	15.7
2MASS J16070700$-$2515127	$14.51\pm 0.01$	$13.76\pm 0.01$	$13.37\pm 0.01$		$-11.6\pm 2.2$	$-16.7\pm 9.6$	6.4	48	16.5
2MASS J16070873$-$1927341	$14.71\pm 0.01$	$13.95\pm 0.01$	$13.51\pm 0.01$		$-9.0\pm 2.4$	$-14.3\pm 2.0$	4.3	75	15.7
2MASS J16071007$-$1917046	$15.64\pm 0.01$	$14.66\pm 0.01$	$14.14\pm 0.01$		$-13.6\pm 2.0$	$-23.7\pm 3.1$	3.7	81	15.1
2MASS J16071348$-$2106016	$15.35\pm 0.01$	$14.41\pm 0.01$	$13.89\pm 0.01$		$-10.0\pm 1.3$	$-24.6\pm 2.2$	2.3	85	15.1
2MASS J16071478$-$2321011	$\cdots$	$19.81\pm 0.01$	$18.74\pm 0.02$		$0.2\pm 12.2$	$-16.3\pm 11.0$	0.7	17	14.3
2MASS J16071750$-$1820348	$18.95\pm 0.01$	$17.48\pm 0.01$	$16.72\pm 0.04$		$-4.5\pm 2.6$	$-21.1\pm 3.3$	2.9	50	15.7
2MASS J16072240$-$2011581	$15.75\pm 0.01$	$14.76\pm 0.01$	$14.19\pm 0.01$		$-7.2\pm 1.9$	$-25.8\pm 2.0$	4.8	85	15.1
2MASS J16072382$-$2211018	$19.51\pm 0.02$	$17.93\pm 0.01$	$17.05\pm 0.01$		$-19.5\pm 6.0$	$-21.7\pm 6.9$	4.1	53	15.7
2MASS J16072641$-$2144169	$17.98\pm 0.01$	$16.85\pm 0.01$	$16.21\pm 0.01$		$-9.2\pm 2.4$	$-20.7\pm 4.3$	2.7	62	15.1
2MASS J16072754$-$2018344	$15.76\pm 0.01$	$14.66\pm 0.01$	$14.04\pm 0.01$		$-6.2\pm 3.6$	$-23.6\pm 2.3$	13	70	15.1
2MASS J16072853$-$2407543	$\cdots$	$\cdots$	$12.55\pm 0.01$		$-3.2\pm 13.0$	$-20.8\pm 11.8$	16	62	16.5
2MASS J16073556$-$2027134	$15.80\pm 0.01$	$14.92\pm 0.01$	$14.43\pm 0.01$		$-8.2\pm 1.5$	$-22.8\pm 2.7$	2.6	64	15.1
2MASS J16073799$-$2242468	$\cdots$	$19.99\pm 0.02$	$18.93\pm 0.03$		$-14.4\pm 10.3$	$-16.5\pm 10.3$	0.9	36	14.8
2MASS J16074036$-$2357019	$16.88\pm 0.01$	$15.80\pm 0.01$	$15.21\pm 0.01$		$-7.0\pm 1.8$	$-20.3\pm 2.5$	3.0	73	15.7
2MASS J16074200$-$2107302	$15.12\pm 0.01$	$14.23\pm 0.01$	$13.77\pm 0.01$		$-4.7\pm 2.2$	$-14.4\pm 4.5$	4.5	82	15.7
2MASS J16074522$-$2222574	$15.30\pm 0.01$	$14.41\pm 0.01$	$13.91\pm 0.01$		$-9.7\pm 1.4$	$-11.9\pm 3.6$	3.1	73	15.7
2MASS J16075039$-$2221021	$15.18\pm 0.01$	$14.27\pm 0.01$	$13.79\pm 0.01$		$-8.3\pm 2.8$	$-19.9\pm 3.1$	4.2	70	15.1
2MASS J16075567$-$2443267	$16.75\pm 0.01$	$15.78\pm 0.01$	$15.28\pm 0.01$		$-8.2\pm 7.5$	$-17.1\pm 2.9$	16	60	16.5
2MASS J16075850$-$2039485	$16.88\pm 0.01$	$15.78\pm 0.01$	$15.18\pm 0.01$		$-4.6\pm 3.1$	$-22.6\pm 6.0$	7.2	85	15.7
2MASS J16080051$-$2040289	$15.27\pm 0.01$	$14.33\pm 0.01$	$13.81\pm 0.01$		$-0.7\pm 4.5$	$-28.2\pm 6.3$	13	84	15.1
2MASS J16080217$-$2259057	$15.15\pm 0.01$	$14.18\pm 0.01$	$13.68\pm 0.01$		$-8.4\pm 1.2$	$-14.8\pm 3.7$	2.2	62	15.7
2MASS J16080245$-$2531392	$14.61\pm 0.01$	$13.75\pm 0.01$	$13.28\pm 0.01$		$-14.8\pm 2.7$	$-17.8\pm 3.5$	4.1	57	16.5
2MASS J16080370$-$1812385	$16.78\pm 0.01$	$16.10\pm 0.01$	$15.79\pm 0.01$		$34.8\pm 17.5$	$17.1\pm 11.7$	10	65	15.7
2MASS J16080745$-$2345055	$17.93\pm 0.01$	$16.74\pm 0.01$	$16.05\pm 0.01$		$-5.0\pm 7.0$	$-17.7\pm 4.8$	3.1	63	15.7
2MASS J16081081$-$2229428	$15.62\pm 0.01$	$14.61\pm 0.01$	$14.08\pm 0.01$		$-4.4\pm 2.1$	$-20.7\pm 3.2$	2.0	68	15.7
2MASS J16081758$-$2348508	$16.66\pm 0.01$	$15.64\pm 0.01$	$15.08\pm 0.02$		$-6.5\pm 5.7$	$-18.9\pm 5.2$	3.3	57	15.7
2MASS J16081843$-$2232248	$20.92\pm 0.04$	$19.26\pm 0.02$	$18.18\pm 0.01$		$-11.7\pm 5.6$	$-26.7\pm 5.5$	0.7	46	15.1
2MASS J16082096$-$1832197	$17.66\pm 0.01$	$16.52\pm 0.01$	$15.87\pm 0.01$		$-15.6\pm 1.6$	$-18.3\pm 3.3$	2.7	57	15.7
2MASS J16082229$-$2217029	$15.96\pm 0.01$	$15.00\pm 0.01$	$14.47\pm 0.01$		$-19.1\pm 4.1$	$-25.9\pm 1.9$	11	53	15.7
2MASS J16082751$-$1949047	$14.52\pm 0.01$	$13.61\pm 0.01$	$13.10\pm 0.01$		$10.7\pm 6.2$	$-6.2\pm 8.0$	5.0	74	15.7
2MASS J16082847$-$2315103	$20.03\pm 0.02$	$18.43\pm 0.01$	$17.47\pm 0.01$		$-8.6\pm 4.0$	$-30.8\pm 3.9$	1.2	41	15.1
2MASS J16083048$-$2335109	$19.08\pm 0.01$	$17.58\pm 0.01$	$16.75\pm 0.01$		$-12.3\pm 4.1$	$-18.7\pm 4.4$	1.4	45	15.7
2MASS J16083455$-$2211559	$15.36\pm 0.01$	$14.47\pm 0.01$	$13.97\pm 0.01$		$-9.8\pm 1.7$	$-18.7\pm 3.8$	3.4	81	15.7
2MASS J16083659$-$1802497	$16.26\pm 0.01$	$15.10\pm 0.01$	$14.42\pm 0.01$		$-5.4\pm 1.5$	$-17.7\pm 4.7$	4.1	88	15.7
2MASS J16084171$-$1856107	$15.46\pm 0.01$	$14.38\pm 0.01$	$13.79\pm 0.01$		$-6.5\pm 1.5$	$-18.6\pm 1.6$	1.9	73	15.1
2MASS J16084565$-$2430000	$14.73\pm 0.01$	$13.93\pm 0.01$	$13.54\pm 0.01$		$-10.6\pm 1.4$	$-14.3\pm 5.2$	3.3	75	16.5
2MASS J16084744$-$2235477	$20.14\pm 0.02$	$18.56\pm 0.01$	$17.66\pm 0.01$		$0.1\pm 4.5$	$-27.3\pm 4.5$	0.8	46	15.1
2MASS J16084836$-$2341209	$15.43\pm 0.01$	$14.46\pm 0.01$	$13.98\pm 0.01$		$-9.4\pm 2.3$	$-17.6\pm 4.9$	3.9	72	15.7
2MASS J16085871$-$2449363	$14.86\pm 0.01$	$14.08\pm 0.01$	$13.68\pm 0.01$		$-10.0\pm 1.8$	$-15.4\pm 4.9$	7.2	82	16.5
2MASS J16090002$-$1908368	$14.75\pm 0.01$	$13.87\pm 0.01$	$13.43\pm 0.01$		$-4.9\pm 1.2$	$-19.2\pm 3.8$	2.3	74	15.7
2MASS J16090051$-$2745194	$14.95\pm 0.01$	$14.04\pm 0.01$	$13.53\pm 0.01$		$-14.0\pm 3.0$	$-17.8\pm 3.2$	3.9	58	16.5
2MASS J16090071$-$2029086	$17.83\pm 0.01$	$16.63\pm 0.01$	$15.95\pm 0.01$		$-4.5\pm 3.4$	$-22.4\pm 1.8$	2.2	46	15.7
2MASS J16090168$-$2740521	$16.21\pm 0.01$	$15.08\pm 0.01$	$14.46\pm 0.01$		$-11.3\pm 2.2$	$-24.4\pm 2.1$	2.3	68	15.9
2MASS J16090197$-$2151225	$17.15\pm 0.01$	$15.96\pm 0.01$	$15.29\pm 0.01$		$-8.1\pm 2.7$	$-15.9\pm 2.7$	2.8	59	15.7
2MASS J16090407$-$2417588	$15.01\pm 0.01$	$13.86\pm 0.01$	$13.35\pm 0.02$		$-8.4\pm 2.1$	$-25.6\pm 3.6$	14	74	16.0
2MASS J16090451$-$2224523	$16.60\pm 0.01$	$15.37\pm 0.01$	$14.65\pm 0.01$		$-6.1\pm 2.1$	$-16.5\pm 2.0$	1.4	68	15.1
2MASS J16090776$-$2339545	$15.04\pm 0.01$	$14.09\pm 0.01$	$13.56\pm 0.01$		$-8.4\pm 2.1$	$-26.7\pm 1.9$	2.4	77	15.1
2MASS J16090884$-$2217466	$15.74\pm 0.01$	$14.82\pm 0.01$	$14.36\pm 0.01$		$-15.9\pm 1.7$	$-26.0\pm 3.0$	3.0	73	15.7
2MASS J16091580$-$1937063	$15.03\pm 0.01$	$14.22\pm 0.01$	$13.78\pm 0.01$		$-3.2\pm 1.6$	$-13.5\pm 2.0$	2.3	77	15.7
2MASS J16091689$-$2341324	$14.74\pm 0.01$	$13.83\pm 0.01$	$13.38\pm 0.01$		$-15.2\pm 2.7$	$-15.2\pm 5.7$	5.6	72	15.7
2MASS J16091837$-$2007349	$16.40\pm 0.01$	$15.23\pm 0.01$	$14.61\pm 0.01$		$-11.7\pm 3.4$	$-25.6\pm 3.3$	3.6	47	15.1
2MASS J16092054$-$1926318	$16.32\pm 0.03$	$15.21\pm 0.01$	$14.61\pm 0.01$		$-9.5\pm 3.3$	$-18.6\pm 3.6$	4.8	58	15.7
2MASS J16092136$-$2139342	$15.11\pm 0.01$	$14.12\pm 0.02$	$13.58\pm 0.01$		$-10.2\pm 4.7$	$-6.3\pm 6.0$	28	64	15.1
2MASS J16092619$-$2403030	$14.94\pm 0.01$	$14.09\pm 0.01$	$13.66\pm 0.01$		$-8.0\pm 1.1$	$-18.6\pm 4.1$	2.6	77	16.5
2MASS J16092938$-$2343121	$17.83\pm 0.01$	$16.57\pm 0.01$	$15.87\pm 0.01$		$-8.3\pm 1.4$	$-16.1\pm 2.0$	1.3	59	15.7
2MASS J16093019$-$2059536	$17.30\pm 0.01$	$16.17\pm 0.01$	$15.56\pm 0.01$		$-5.8\pm 3.4$	$-13.7\pm 6.1$	1.9	63	15.7
2MASS J16093245$-$2405593	$16.11\pm 0.01$	$15.05\pm 0.01$	$14.43\pm 0.01$		$-4.8\pm 1.9$	$-17.5\pm 7.9$	8.3	74	16.5
2MASS J16093558$-$1828232	$14.62\pm 0.01$	$13.81\pm 0.01$	$13.38\pm 0.01$		$-2.6\pm 1.4$	$-14.7\pm 5.3$	4.6	90	15.7
2MASS J16093706$-$2052529	$15.82\pm 0.01$	$14.90\pm 0.01$	$14.39\pm 0.01$		$-5.9\pm 1.6$	$-15.4\pm 2.3$	2.0	83	15.1
2MASS J16094634$-$2255335	$14.71\pm 0.01$	$13.87\pm 0.01$	$13.44\pm 0.01$		$-7.1\pm 4.6$	$-15.1\pm 7.7$	5.3	70	15.7
2MASS J16095060$-$1848521	$18.73\pm 0.01$	$17.25\pm 0.01$	$16.37\pm 0.01$		$-6.0\pm 3.6$	$-20.6\pm 3.7$	1.9	41	15.1
2MASS J16095107$-$2722418	$16.72\pm 0.01$	$15.58\pm 0.01$	$14.92\pm 0.01$		$-11.1\pm 3.9$	$-20.1\pm 2.7$	2.9	64	16.5
2MASS J16095217$-$2136277	$16.11\pm 0.01$	$14.91\pm 0.01$	$14.23\pm 0.01$		$-5.1\pm 1.7$	$-27.4\pm 2.2$	2.2	61	15.1
2MASS J16095287$-$2441535	$14.77\pm 0.01$	$13.86\pm 0.01$	$13.35\pm 0.01$		$-7.2\pm 1.7$	$-26.6\pm 2.6$	3.6	63	16.0
2MASS J16095307$-$1948169	$16.04\pm 0.01$	$14.94\pm 0.01$	$14.33\pm 0.01$		$-3.7\pm 2.2$	$-10.6\pm 4.7$	7.0	61	15.1
2MASS J16095361$-$1754474	$15.50\pm 0.01$	$14.56\pm 0.01$	$14.11\pm 0.01$		$-8.3\pm 2.8$	$-17.3\pm 2.6$	3.7	81	15.7
2MASS J16095695$-$2212027	$16.69\pm 0.01$	$15.69\pm 0.01$	$15.13\pm 0.01$		$-6.8\pm 1.1$	$-17.4\pm 4.2$	1.5	73	15.7
2MASS J16095852$-$2345186	$16.09\pm 0.01$	$14.92\pm 0.01$	$14.26\pm 0.01$		$-7.2\pm 2.2$	$-25.2\pm 2.4$	11	87	15.1
2MASS J16095990$-$2155424	$17.54\pm 0.01$	$16.45\pm 0.01$	$15.86\pm 0.01$		$-7.4\pm 1.3$	$-16.4\pm 6.1$	2.0	77	15.7
2MASS J16100129$-$2152243	$15.82\pm 0.01$	$14.78\pm 0.01$	$14.18\pm 0.01$		$-0.7\pm 1.7$	$-25.0\pm 2.3$	3.1	79	15.1
2MASS J16100394$-$2728479	$14.65\pm 0.01$	$13.85\pm 0.01$	$13.44\pm 0.01$		$-7.7\pm 1.2$	$-14.9\pm 3.5$	2.9	68	16.5
2MASS J16100541$-$1919362	$17.93\pm 0.01$	$16.66\pm 0.03$	$15.90\pm 0.02$		$0.5\pm 5.3$	$-13.4\pm 2.6$	7.1	49	15.7
2MASS J16100608$-$2127440	$19.16\pm 0.02$	$17.61\pm 0.01$	$16.73\pm 0.01$		$-6.1\pm 3.6$	$-19.1\pm 2.8$	2.4	46	15.7
2MASS J16100753$-$1810568	$16.16\pm 0.01$	$14.99\pm 0.01$	$14.35\pm 0.01$		$-4.2\pm 1.6$	$-22.2\pm 1.8$	1.7	76	15.1
2MASS J16101100$-$1946040	$15.09\pm 0.01$	$14.22\pm 0.01$	$13.77\pm 0.01$		$-9.3\pm 1.2$	$-15.5\pm 2.6$	4.6	89	15.7
2MASS J16101191$-$2101550	$16.81\pm 0.01$	$15.72\pm 0.01$	$15.06\pm 0.01$		$-5.6\pm 1.7$	$-19.4\pm 1.9$	2.5	79	15.1
2MASS J16101316$-$2856308	$17.53\pm 0.01$	$16.34\pm 0.01$	$15.68\pm 0.01$		$-15.0\pm 2.8$	$-15.2\pm 3.1$	1.3	51	16.5
2MASS J16101445$-$1951377	$\cdots$	$\cdots$	$12.61\pm 0.01$		$-2.3\pm 2.9$	$-15.3\pm 2.6$	1.9	46	15.7
2MASS J16101888$-$2502325	$14.90\pm 0.01$	$14.02\pm 0.01$	$13.59\pm 0.02$		$-28.4\pm 9.0$	$-30.8\pm 8.5$	28	46	16.5
2MASS J16101942$-$2331089	$16.66\pm 0.01$	$15.67\pm 0.01$	$15.13\pm 0.01$		$-5.1\pm 1.2$	$-13.6\pm 2.3$	1.6	62	15.7
2MASS J16102087$-$2331556	$14.76\pm 0.01$	$13.86\pm 0.01$	$13.35\pm 0.01$		$-13.5\pm 2.1$	$-24.2\pm 3.6$	5.0	76	15.1
2MASS J16102564$-$2411250	$18.81\pm 0.01$	$17.46\pm 0.01$	$16.68\pm 0.01$		$-16.2\pm 5.9$	$-20.2\pm 2.4$	1.9	51	16.0
2MASS J16102819$-$1910444	$15.90\pm 0.01$	$14.93\pm 0.01$	$14.40\pm 0.01$		$-6.8\pm 2.4$	$-11.1\pm 1.9$	6.2	80	15.7
2MASS J16102988$-$2403497	$15.65\pm 0.01$	$14.82\pm 0.01$	$14.36\pm 0.01$		$-7.2\pm 3.1$	$-21.4\pm 2.3$	5.9	66	16.0
2MASS J16103008$-$1839065	$14.86\pm 0.01$	$13.86\pm 0.01$	$13.28\pm 0.01$		$-5.8\pm 1.2$	$-19.2\pm 2.8$	3.4	86	15.7
2MASS J16103014$-$2315167	$18.10\pm 0.01$	$16.83\pm 0.01$	$16.09\pm 0.01$		$-6.3\pm 2.0$	$-29.7\pm 2.0$	1.4	64	15.1
2MASS J16103525$-$2029168	$15.73\pm 0.01$	$14.74\pm 0.01$	$14.21\pm 0.01$		$-8.1\pm 1.2$	$-16.7\pm 3.1$	2.4	74	15.7
2MASS J16103876$-$1829235	$17.66\pm 0.01$	$16.46\pm 0.01$	$15.72\pm 0.01$		$-4.0\pm 1.3$	$-12.9\pm 2.0$	1.4	67	15.7
2MASS J16104636$-$1840598	$15.50\pm 0.01$	$14.58\pm 0.01$	$14.01\pm 0.01$		$-0.2\pm 2.7$	$-24.6\pm 2.2$	3.0	82	15.1
2MASS J16104714$-$2239492	$19.75\pm 0.02$	$18.13\pm 0.01$	$17.22\pm 0.01$		$-4.3\pm 3.9$	$-17.0\pm 4.6$	2.4	50	15.7
2MASS J16104996$-$2212515	$15.95\pm 0.01$	$14.89\pm 0.01$	$14.28\pm 0.01$		$-5.0\pm 1.5$	$-18.7\pm 2.8$	2.4	54	15.7
2MASS J16105429$-$2309108	$15.84\pm 0.01$	$14.92\pm 0.01$	$14.45\pm 0.01$		$-21.7\pm 3.2$	$-35.6\pm 3.0$	5.4	78	15.1
2MASS J16105499$-$2126139	$16.05\pm 0.01$	$14.98\pm 0.01$	$14.36\pm 0.01$		$22.8\pm 17.1$	$-11.6\pm 2.9$	37	71	15.1
2MASS J16105728$-$2359540	$15.58\pm 0.01$	$14.72\pm 0.01$	$14.27\pm 0.01$		$-11.4\pm 5.5$	$-12.9\pm 4.0$	6.7	70	16.5
2MASS J16110142$-$1924489	$16.44\pm 0.01$	$15.44\pm 0.01$	$14.87\pm 0.01$		$-4.9\pm 1.7$	$-14.6\pm 1.8$	2.0	83	15.1
2MASS J16110212$-$2335504	$14.63\pm 0.01$	$13.80\pm 0.01$	$13.34\pm 0.01$		$-5.7\pm 1.5$	$-20.5\pm 4.2$	2.9	64	15.7
2MASS J16110360$-$2426429	$18.98\pm 0.01$	$17.46\pm 0.01$	$16.61\pm 0.01$		$-9.1\pm 1.6$	$-24.4\pm 3.8$	5.7	55	14.6
2MASS J16110737$-$2228501	$15.51\pm 0.01$	$14.43\pm 0.01$	$13.83\pm 0.01$		$-3.4\pm 2.0$	$-18.9\pm 2.0$	2.0	73	15.1
2MASS J16111095$-$1933320	$15.08\pm 0.01$	$14.19\pm 0.01$	$13.72\pm 0.01$		$-1.6\pm 1.4$	$-18.0\pm 1.8$	2.9	83	15.7
2MASS J16111237$-$1927374	$16.01\pm 0.01$	$14.93\pm 0.01$	$14.31\pm 0.01$		$-0.8\pm 1.5$	$-17.0\pm 1.6$	2.6	81	15.7
2MASS J16111687$-$2639331	$14.79\pm 0.01$	$14.00\pm 0.01$	$13.62\pm 0.01$		$-7.0\pm 1.5$	$-20.1\pm 2.3$	3.5	57	14.6
2MASS J16111711$-$2217173	$17.96\pm 0.01$	$16.73\pm 0.01$	$16.04\pm 0.01$		$-2.9\pm 1.4$	$-14.7\pm 3.6$	1.4	62	15.7
2MASS J16111744$-$2441203	$\cdots$	$\cdots$	$12.73\pm 0.01$		$-7.9\pm 2.2$	$-18.6\pm 2.8$	3.6	59	14.6
2MASS J16111820$-$1803585	$16.04\pm 0.01$	$14.93\pm 0.01$	$14.32\pm 0.01$		$-9.7\pm 1.6$	$-17.7\pm 2.6$	2.8	76	15.1
2MASS J16111907$-$2319202	$15.67\pm 0.01$	$15.15\pm 0.10$	$13.71\pm 0.03$		$-8.1\pm 1.4$	$-23.9\pm 2.1$	2.0	74	15.1
2MASS J16111935$-$1905080	$17.49\pm 0.01$	$16.21\pm 0.01$	$15.47\pm 0.01$		$-2.9\pm 1.5$	$-17.3\pm 7.0$	2.9	37	15.7
2MASS J16112023$-$1847554	$15.96\pm 0.01$	$14.89\pm 0.01$	$14.32\pm 0.01$		$-1.4\pm 1.7$	$-18.6\pm 2.6$	2.9	81	15.1
2MASS J16112479$-$2655461	$18.50\pm 0.01$	$17.24\pm 0.01$	$16.52\pm 0.01$		$-12.9\pm 2.4$	$-17.6\pm 2.4$	1.1	50	14.6
2MASS J16112630$-$2340059	$16.48\pm 0.01$	$15.51\pm 0.01$	$14.96\pm 0.01$		$-7.1\pm 2.4$	$-13.6\pm 8.3$	7.6	74	15.7
2MASS J16112939$-$1942246	$15.14\pm 0.01$	$14.22\pm 0.01$	$13.67\pm 0.01$		$-4.3\pm 1.2$	$-19.4\pm 4.8$	3.0	76	15.7
2MASS J16112959$-$1900292	$17.37\pm 0.01$	$16.11\pm 0.01$	$15.39\pm 0.01$		$-5.4\pm 1.8$	$-18.5\pm 2.8$	1.3	48	15.7
2MASS J16113180$-$2237082	$15.79\pm 0.01$	$14.83\pm 0.01$	$14.29\pm 0.01$		$-4.8\pm 1.9$	$-17.2\pm 5.2$	3.0	82	15.7
2MASS J16113363$-$1914003	$\cdots$	$\cdots$	$12.57\pm 0.01$		$-12.9\pm 6.2$	$-16.3\pm 2.8$	16	83	15.7
2MASS J16113470$-$2219442	$16.35\pm 0.01$	$15.37\pm 0.01$	$14.83\pm 0.01$		$-7.6\pm 1.5$	$-16.3\pm 5.0$	2.4	81	15.7
2MASS J16113761$-$2346147	$14.81\pm 0.01$	$14.00\pm 0.01$	$13.56\pm 0.01$		$-7.9\pm 0.9$	$-18.3\pm 3.4$	2.5	83	15.7
2MASS J16113837$-$2307072	$17.00\pm 0.01$	$15.95\pm 0.01$	$15.34\pm 0.01$		$-6.5\pm 3.0$	$-21.4\pm 2.3$	4.0	82	15.7
2MASS J16114040$-$2311347	$15.62\pm 0.01$	$14.63\pm 0.01$	$14.09\pm 0.01$		$-15.2\pm 4.4$	$-51.4\pm 16.1$	10	77	15.7
2MASS J16114353$-$2527073	$14.69\pm 0.01$	$13.74\pm 0.01$	$13.23\pm 0.01$		$-13.6\pm 1.9$	$-29.5\pm 2.8$	3.9	48	15.9
2MASS J16114530$-$2254329	$15.99\pm 0.01$	$14.95\pm 0.01$	$14.36\pm 0.01$		$-6.7\pm 1.7$	$-27.4\pm 2.2$	2.4	83	15.1
2MASS J16114534$-$1928132	$16.08\pm 0.01$	$15.02\pm 0.01$	$14.44\pm 0.01$		$-7.6\pm 3.0$	$-14.7\pm 2.7$	4.1	56	15.7
2MASS J16114612$-$1907429	$15.28\pm 0.01$	$14.31\pm 0.01$	$13.79\pm 0.01$		$-7.0\pm 2.0$	$-27.5\pm 2.7$	3.9	75	15.1
2MASS J16114735$-$2242062	$16.45\pm 0.01$	$15.47\pm 0.01$	$14.97\pm 0.01$		$-6.8\pm 3.0$	$-9.7\pm 7.9$	4.3	64	15.7
2MASS J16114920$-$1947431	$14.66\pm 0.01$	$13.76\pm 0.01$	$13.28\pm 0.01$		$-9.1\pm 1.5$	$-18.0\pm 6.5$	4.2	67	15.7
2MASS J16115436$-$2157025	$18.50\pm 0.01$	$17.04\pm 0.01$	$16.18\pm 0.01$		$-2.2\pm 7.1$	$-10.0\pm 7.6$	11	40	15.7
2MASS J16115439$-$2236491	$17.59\pm 0.01$	$16.49\pm 0.01$	$15.89\pm 0.01$		$-8.4\pm 1.1$	$-12.2\pm 5.0$	1.5	68	15.7
2MASS J16115737$-$2215066	$16.78\pm 0.01$	$15.80\pm 0.01$	$15.23\pm 0.01$		$-8.8\pm 1.6$	$-16.4\pm 1.8$	1.3	73	15.1
2MASS J16121016$-$2758305	$18.94\pm 0.02$	$17.63\pm 0.01$	$16.86\pm 0.02$		$32.5\pm 27.6$	$24.4\pm 26.9$	17	42	16.5
2MASS J16121043$-$1932275	$15.29\pm 0.01$	$14.30\pm 0.01$	$13.76\pm 0.01$		$-5.8\pm 1.1$	$-13.6\pm 1.6$	2.9	78	15.7
2MASS J16121185$-$2047267	$17.14\pm 0.01$	$15.95\pm 0.01$	$15.29\pm 0.01$		$-6.6\pm 1.7$	$-22.2\pm 1.4$	1.8	74	15.7
2MASS J16121492$-$2218038	$15.05\pm 0.01$	$14.22\pm 0.01$	$13.78\pm 0.01$		$-5.2\pm 2.4$	$-18.7\pm 4.7$	8.3	67	15.7
2MASS J16121609$-$2344248	$16.11\pm 0.01$	$15.18\pm 0.01$	$14.68\pm 0.01$		$-15.4\pm 2.8$	$-15.4\pm 3.1$	4.9	67	15.7
2MASS J16121723$-$2839082	$14.75\pm 0.01$	$13.94\pm 0.01$	$13.54\pm 0.01$		$-2.6\pm 4.6$	$-15.7\pm 2.5$	11	62	16.5
2MASS J16122737$-$2009596	$15.70\pm 0.01$	$14.68\pm 0.01$	$14.10\pm 0.01$		$-8.3\pm 1.5$	$-23.8\pm 2.7$	2.3	73	15.1
2MASS J16122764$-$2156407	$\cdots$	$20.33\pm 0.02$	$19.44\pm 0.06$		$-5.2\pm 13.6$	$-19.8\pm 13.5$	0.8	17	14.8
2MASS J16122768$-$2406485	$15.94\pm 0.01$	$14.95\pm 0.01$	$14.39\pm 0.01$		$-6.7\pm 1.9$	$-23.9\pm 1.6$	2.4	68	16.0
2MASS J16122895$-$2159358	$\cdots$	$20.32\pm 0.04$	$19.06\pm 0.07$		$-33.1\pm 83.4$	$-36.8\pm 11.5$	1.2	14	13.9
2MASS J16123458$-$2458341	$14.96\pm 0.01$	$13.98\pm 0.01$	$13.46\pm 0.01$		$-8.3\pm 3.1$	$-25.0\pm 4.3$	4.0	67	15.9
2MASS J16123759$-$2349234	$16.93\pm 0.01$	$15.93\pm 0.01$	$15.37\pm 0.01$		$-6.8\pm 1.7$	$-26.5\pm 2.2$	1.7	69	15.1
2MASS J16124374$-$2308231	$14.59\pm 0.01$	$13.79\pm 0.01$	$13.33\pm 0.01$		$-8.3\pm 1.0$	$-23.6\pm 4.8$	4.1	77	15.7
2MASS J16124506$-$2305303	$16.56\pm 0.01$	$15.57\pm 0.01$	$14.99\pm 0.01$		$-8.8\pm 1.0$	$-24.2\pm 3.3$	2.1	70	15.7
2MASS J16124692$-$2338408	$17.00\pm 0.01$	$15.87\pm 0.01$	$15.24\pm 0.01$		$-8.8\pm 2.7$	$-19.3\pm 1.6$	1.9	69	15.1
2MASS J16124726$-$1903531	$16.06\pm 0.01$	$15.01\pm 0.01$	$14.45\pm 0.01$		$-2.2\pm 5.4$	$-29.2\pm 3.0$	6.2	62	15.1
2MASS J16125528$-$2226542	$15.15\pm 0.01$	$14.28\pm 0.01$	$13.81\pm 0.01$		$-14.6\pm 4.9$	$-23.0\pm 3.5$	16	71	15.1
2MASS J16130232$-$2124283	$\cdots$	$20.63\pm 0.04$	$19.50\pm 0.06$		$-9.0\pm 6.2$	$-23.3\pm 6.1$	0.8	24	14.8
2MASS J16130235$-$1904450	$17.72\pm 0.02$	$16.60\pm 0.02$	$15.79\pm 0.02$		$-10.8\pm 2.1$	$-18.0\pm 2.2$	1.0	52	15.1
2MASS J16130306$-$1929319	$16.72\pm 0.01$	$15.64\pm 0.01$	$15.03\pm 0.01$		$-9.7\pm 1.5$	$-25.3\pm 1.7$	1.7	71	15.1
2MASS J16130762$-$1703524	$16.74\pm 0.01$	$15.73\pm 0.01$	$15.17\pm 0.01$		$-22.6\pm 10.1$	$-4.9\pm 5.9$	32	68	15.2
2MASS J16130996$-$1904269	$14.52\pm 0.03$	$13.68\pm 0.01$	$13.23\pm 0.01$		$-5.5\pm 1.6$	$-17.3\pm 2.9$	2.9	67	15.7
2MASS J16131082$-$2313514	$15.23\pm 0.01$	$14.36\pm 0.01$	$13.90\pm 0.01$		$-13.9\pm 1.3$	$-33.2\pm 1.7$	1.6	71	15.1
2MASS J16131211$-$2305031	$17.55\pm 0.01$	$16.35\pm 0.01$	$15.68\pm 0.01$		$-6.0\pm 2.1$	$-24.5\pm 2.1$	2.3	69	15.1
2MASS J16132665$-$2230348	$16.97\pm 0.01$	$15.80\pm 0.01$	$15.18\pm 0.01$		$-3.9\pm 2.2$	$-17.6\pm 5.3$	2.0	48	15.7
2MASS J16132809$-$1924524	$16.22\pm 0.01$	$15.14\pm 0.01$	$14.53\pm 0.01$		$-3.9\pm 1.3$	$-19.8\pm 3.3$	1.9	77	15.7
2MASS J16133476$-$2328156	$16.40\pm 0.01$	$15.49\pm 0.01$	$14.98\pm 0.01$		$-5.9\pm 1.1$	$-14.9\pm 2.7$	1.9	75	15.7
2MASS J16133647$-$2327353	$15.05\pm 0.01$	$14.12\pm 0.01$	$13.63\pm 0.01$		$-10.0\pm 1.2$	$-24.5\pm 2.2$	2.1	74	15.1
2MASS J16133834$-$2158518	$14.58\pm 0.01$	$13.79\pm 0.01$	$13.36\pm 0.01$		$-1.5\pm 3.9$	$-11.7\pm 2.5$	7.5	58	15.7
2MASS J16133840$-$2443309	$\cdots$	$13.09\pm 0.01$	$12.72\pm 0.01$		$-12.2\pm 3.0$	$-15.9\pm 3.1$	5.4	64	16.5
2MASS J16134045$-$2233156	$16.02\pm 0.01$	$14.99\pm 0.01$	$14.42\pm 0.01$		$-2.5\pm 1.8$	$-23.6\pm 2.1$	4.0	64	15.1
2MASS J16134079$-$2219459	$18.60\pm 0.01$	$17.25\pm 0.01$	$16.47\pm 0.01$		$-2.7\pm 2.7$	$-20.7\pm 3.1$	2.4	43	15.1
2MASS J16134264$-$2301279	$16.98\pm 0.01$	$15.91\pm 0.01$	$15.31\pm 0.01$		$-5.3\pm 1.6$	$-14.8\pm 3.6$	1.4	84	15.7
2MASS J16134490$-$2434143	$\cdots$	$\cdots$	$12.58\pm 0.01$		$-6.5\pm 2.4$	$-19.2\pm 5.9$	4.1	55	16.5
2MASS J16134880$-$2509006	$16.84\pm 0.01$	$15.75\pm 0.01$	$15.19\pm 0.01$		$-5.3\pm 1.9$	$-18.3\pm 3.8$	1.6	70	16.5
2MASS J16135765$-$2053447	$17.18\pm 0.01$	$16.12\pm 0.01$	$15.54\pm 0.01$		$-22.8\pm 2.8$	$-30.4\pm 1.8$	1.4	56	15.1
2MASS J16140514$-$2042017	$18.04\pm 0.02$	$16.79\pm 0.01$	$16.09\pm 0.01$		$-9.4\pm 2.4$	$-18.8\pm 2.4$	1.4	56	15.1
2MASS J16141352$-$2244578	$15.03\pm 0.01$	$14.22\pm 0.01$	$13.81\pm 0.01$		$-10.8\pm 7.5$	$-13.8\pm 7.5$	31	70	15.7
2MASS J16141484$-$2427081	$15.66\pm 0.01$	$14.58\pm 0.01$	$14.00\pm 0.01$		$0.5\pm 2.6$	$-20.1\pm 2.3$	7.6	71	16.5
2MASS J16141974$-$2428404	$17.13\pm 0.01$	$16.01\pm 0.01$	$15.37\pm 0.01$		$-9.9\pm 2.8$	$-15.0\pm 3.4$	5.1	49	16.5
2MASS J16142144$-$2339146	$18.53\pm 0.01$	$17.31\pm 0.01$	$16.64\pm 0.01$		$-16.0\pm 3.2$	$-15.9\pm 2.9$	2.5	51	15.1
2MASS J16142312$-$2219338	$14.82\pm 0.01$	$13.86\pm 0.01$	$13.30\pm 0.01$		$-2.8\pm 3.3$	$-19.6\pm 3.4$	10	56	15.7
2MASS J16142478$-$1733329	$18.86\pm 0.01$	$17.47\pm 0.01$	$16.68\pm 0.01$		$-11.1\pm 2.5$	$-22.0\pm 2.7$	2.1	45	15.2
2MASS J16143287$-$2242133	$17.81\pm 0.01$	$16.57\pm 0.01$	$15.90\pm 0.01$		$-4.4\pm 7.0$	$-18.7\pm 6.7$	3.7	53	15.7
2MASS J16143751$-$1858240	$14.92\pm 0.01$	$14.27\pm 0.01$	$13.95\pm 0.01$		$-20.6\pm 2.2$	$-33.9\pm 4.5$	14	75	15.7
2MASS J16144169$-$2351058	$20.96\pm 0.05$	$19.29\pm 0.01$	$18.23\pm 0.03$		$-15.6\pm 7.7$	$-16.2\pm 7.2$	1.3	30	15.1
2MASS J16145258$-$2017133	$19.59\pm 0.02$	$18.07\pm 0.01$	$17.19\pm 0.01$		$-1.2\pm 4.9$	$-16.6\pm 3.0$	2.5	51	15.7
2MASS J16145392$-$2504305	$14.94\pm 0.01$	$14.09\pm 0.01$	$13.64\pm 0.01$		$-5.2\pm 1.5$	$-22.0\pm 4.0$	2.5	51	16.5
2MASS J16145928$-$2459308	$14.80\pm 0.01$	$13.99\pm 0.01$	$13.55\pm 0.01$		$-7.3\pm 1.9$	$-17.8\pm 1.7$	2.8	45	16.5
2MASS J16150524$-$2459351	$15.63\pm 0.01$	$14.64\pm 0.01$	$14.09\pm 0.01$		$-5.4\pm 1.9$	$-21.2\pm 2.3$	3.7	57	15.9
2MASS J16150702$-$2535528	$17.63\pm 0.01$	$16.44\pm 0.01$	$15.78\pm 0.01$		$-9.0\pm 1.7$	$-17.3\pm 1.9$	1.4	73	15.9
2MASS J16150891$-$2345048	$14.89\pm 0.01$	$14.08\pm 0.01$	$13.68\pm 0.01$		$-9.3\pm 2.0$	$-17.4\pm 2.4$	3.5	58	15.7
2MASS J16151116$-$2420153	$17.43\pm 0.01$	$16.39\pm 0.01$	$15.78\pm 0.01$		$-7.9\pm 1.9$	$-12.1\pm 4.6$	1.7	52	16.5
2MASS J16151239$-$2420091	$15.97\pm 0.01$	$15.06\pm 0.01$	$14.57\pm 0.01$		$-14.0\pm 2.1$	$-19.3\pm 2.4$	2.1	53	15.9
2MASS J16151361$-$2304261	$18.30\pm 0.01$	$17.11\pm 0.01$	$16.45\pm 0.01$		$-14.4\pm 1.5$	$-17.2\pm 3.4$	1.7	56	15.7
2MASS J16151602$-$2345103	$15.31\pm 0.01$	$14.36\pm 0.01$	$13.83\pm 0.01$		$-6.8\pm 3.1$	$-17.4\pm 8.1$	7.1	56	15.7
2MASS J16151667$-$2340462	$20.44\pm 0.03$	$18.71\pm 0.01$	$17.70\pm 0.01$		$-8.0\pm 5.0$	$-19.5\pm 4.6$	1.1	35	15.1
2MASS J16152009$-$2333545	$16.24\pm 0.01$	$15.15\pm 0.01$	$14.53\pm 0.01$		$-2.3\pm 2.1$	$-20.9\pm 2.0$	1.7	61	15.1
2MASS J16152750$-$2627281	$14.76\pm 0.01$	$14.01\pm 0.01$	$13.60\pm 0.01$		$-3.6\pm 2.5$	$-15.6\pm 2.8$	4.3	51	16.5
2MASS J16152819$-$2315439	$15.88\pm 0.01$	$15.04\pm 0.01$	$14.60\pm 0.01$		$-13.5\pm 1.2$	$-24.5\pm 4.2$	2.2	79	15.7
2MASS J16153648$-$2315175	$16.92\pm 0.01$	$15.98\pm 0.01$	$15.49\pm 0.01$		$-7.9\pm 1.6$	$-23.3\pm 1.6$	1.8	54	15.1
2MASS J16153844$-$2341558	$14.93\pm 0.01$	$14.11\pm 0.01$	$13.69\pm 0.01$		$-7.9\pm 5.3$	$-12.2\pm 6.0$	8.3	86	15.7
2MASS J16153866$-$2240371	$15.51\pm 0.01$	$14.57\pm 0.01$	$14.10\pm 0.01$		$-10.1\pm 5.6$	$-17.1\pm 4.6$	7.5	60	15.7
2MASS J16153913$-$1917005	$15.13\pm 0.01$	$14.04\pm 0.01$	$13.42\pm 0.01$		$-2.8\pm 1.1$	$-22.4\pm 2.2$	3.3	89	15.1
2MASS J16155507$-$2444365	$16.92\pm 0.01$	$15.73\pm 0.01$	$15.05\pm 0.01$		$-9.6\pm 2.4$	$-25.2\pm 3.5$	2.5	49	15.9
2MASS J16155926$-$2329363	$14.94\pm 0.01$	$14.11\pm 0.01$	$13.69\pm 0.01$		$-10.4\pm 1.4$	$-16.3\pm 2.6$	3.2	78	15.7
2MASS J16160080$-$2214192	$14.72\pm 0.01$	$13.80\pm 0.01$	$13.34\pm 0.01$		$-6.3\pm 1.5$	$-16.0\pm 2.2$	2.8	57	15.7
2MASS J16161183$-$2316268	$15.60\pm 0.01$	$14.70\pm 0.01$	$14.25\pm 0.01$		$-11.0\pm 1.6$	$-24.1\pm 2.3$	2.4	61	15.1
2MASS J16161948$-$2405301	$15.63\pm 0.01$	$14.75\pm 0.01$	$14.29\pm 0.01$		$-9.2\pm 1.7$	$-20.4\pm 2.1$	3.6	70	15.9
2MASS J16162399$-$2408301	$16.16\pm 0.01$	$15.20\pm 0.01$	$14.67\pm 0.01$		$-10.4\pm 3.5$	$-18.1\pm 3.4$	7.4	64	15.9
2MASS J16162531$-$2412057	$16.60\pm 0.01$	$15.65\pm 0.02$	$15.03\pm 0.01$		$-8.1\pm 1.3$	$-13.2\pm 3.3$	1.6	62	16.5
2MASS J16162598$-$2112227	$17.36\pm 0.01$	$16.33\pm 0.01$	$15.78\pm 0.01$		$-11.7\pm 2.8$	$-8.5\pm 3.1$	3.1	51	15.7
2MASS J16163068$-$2512201	$15.95\pm 0.01$	$14.96\pm 0.01$	$14.46\pm 0.01$		$-8.2\pm 1.7$	$-16.2\pm 1.9$	3.3	65	15.9
2MASS J16163226$-$2205201	$16.81\pm 0.01$	$15.76\pm 0.01$	$15.20\pm 0.01$		$-3.7\pm 2.3$	$-17.8\pm 2.4$	1.8	43	15.1
2MASS J16163343$-$2327210	$15.23\pm 0.01$	$14.27\pm 0.01$	$13.76\pm 0.01$		$-15.9\pm 3.2$	$-19.2\pm 2.2$	15	84	15.1
2MASS J16163345$-$2521505	$\cdots$	$\cdots$	$12.60\pm 0.01$		$-6.8\pm 2.8$	$-20.5\pm 3.1$	3.1	56	16.5
2MASS J16163503$-$2057551	$15.28\pm 0.01$	$14.27\pm 0.01$	$13.73\pm 0.01$		$-6.6\pm 1.3$	$-24.4\pm 1.7$	1.9	74	15.1
2MASS J16164539$-$2333413	$16.82\pm 0.01$	$15.82\pm 0.01$	$15.30\pm 0.01$		$-13.2\pm 1.5$	$-29.9\pm 1.8$	1.9	102	15.1
2MASS J16165158$-$2048537	$14.77\pm 0.01$	$13.95\pm 0.01$	$13.53\pm 0.01$		$-5.4\pm 2.6$	$-15.3\pm 2.7$	6.6	59	15.7
2MASS J16165430$-$2459590	$14.56\pm 0.01$	$13.75\pm 0.01$	$13.30\pm 0.01$		$-8.2\pm 2.9$	$-14.8\pm 8.3$	23	67	16.5
2MASS J16170606$-$2225414	$14.79\pm 0.01$	$13.98\pm 0.01$	$13.58\pm 0.01$		$-7.5\pm 2.3$	$-0.6\pm 4.5$	7.9	58	15.1
2MASS J16171901$-$2137129	$16.69\pm 0.01$	$15.63\pm 0.01$	$15.03\pm 0.01$		$-3.6\pm 1.5$	$-21.2\pm 1.9$	2.1	76	15.1
2MASS J16172505$-$2350380	$17.09\pm 0.01$	$16.01\pm 0.01$	$15.40\pm 0.01$		$-4.5\pm 1.5$	$-16.9\pm 4.6$	1.7	58	15.7
2MASS J16173103$-$2050469	$16.49\pm 0.01$	$15.31\pm 0.01$	$14.65\pm 0.01$		$-5.9\pm 2.1$	$-23.6\pm 2.3$	2.7	68	15.1
2MASS J16173236$-$2040362	$18.06\pm 0.01$	$16.85\pm 0.01$	$16.11\pm 0.01$		$-1.2\pm 2.2$	$-14.3\pm 2.4$	1.4	55	15.1
2MASS J16173786$-$2119159	$14.96\pm 0.01$	$14.11\pm 0.01$	$13.68\pm 0.01$		$-12.3\pm 1.2$	$-20.4\pm 2.7$	2.2	65	15.7
2MASS J16174366$-$2111552	$17.11\pm 0.01$	$16.30\pm 0.01$	$15.87\pm 0.01$		$-7.7\pm 2.3$	$-8.5\pm 2.3$	1.2	55	15.1
2MASS J16174539$-$2353360	$17.53\pm 0.01$	$16.33\pm 0.01$	$15.66\pm 0.01$		$-7.1\pm 5.6$	$-29.6\pm 2.4$	3.8	55	15.9
2MASS J16174583$-$2414436	$16.72\pm 0.01$	$15.72\pm 0.01$	$15.16\pm 0.01$		$-2.5\pm 1.3$	$-20.0\pm 1.8$	3.4	57	16.5
2MASS J16181201$-$2413326	$15.82\pm 0.01$	$14.81\pm 0.01$	$14.26\pm 0.01$		$-6.2\pm 2.1$	$-11.3\pm 2.7$	3.6	67	15.9
2MASS J16181568$-$2347084	$16.24\pm 0.01$	$15.00\pm 0.01$	$14.29\pm 0.01$		$-27.4\pm 6.9$	$-28.6\pm 2.1$	3.8	73	15.7
2MASS J16181600$-$2437266	$14.79\pm 0.01$	$13.78\pm 0.01$	$13.24\pm 0.01$		$-4.2\pm 1.6$	$-17.8\pm 2.1$	2.1	57	15.9
2MASS J16181618$-$2619080	$15.41\pm 0.01$	$14.41\pm 0.01$	$13.84\pm 0.01$		$-18.5\pm 3.5$	$-22.7\pm 2.0$	10	70	15.9
2MASS J16181904$-$2028479	$15.35\pm 0.01$	$14.36\pm 0.01$	$13.82\pm 0.01$		$-1.4\pm 1.7$	$-20.6\pm 1.8$	2.1	78	15.1
2MASS J16182082$-$2401502	$18.46\pm 0.01$	$17.24\pm 0.01$	$16.56\pm 0.01$		$-9.3\pm 2.2$	$-23.6\pm 2.6$	1.4	54	15.9
2MASS J16182501$-$2338106	$17.23\pm 0.01$	$16.08\pm 0.01$	$15.45\pm 0.01$		$-7.0\pm 2.0$	$-25.1\pm 1.8$	1.5	78	15.1
2MASS J16183317$-$2517504	$16.21\pm 0.01$	$15.07\pm 0.02$	$14.37\pm 0.01$		$39.1\pm 20.8$	$30.7\pm 23.2$	24	62	16.5
2MASS J16183618$-$2425333	$14.82\pm 0.01$	$13.97\pm 0.01$	$13.52\pm 0.01$		$-1.3\pm 2.8$	$-15.8\pm 3.3$	2.2	69	16.5
2MASS J16184074$-$2209482	$17.22\pm 0.01$	$16.05\pm 0.01$	$15.38\pm 0.01$		$-11.3\pm 3.5$	$-21.9\pm 2.4$	4.4	50	15.7
2MASS J16184955$-$2541499	$19.11\pm 0.01$	$17.82\pm 0.01$	$17.04\pm 0.01$		$-4.0\pm 4.9$	$-14.1\pm 4.0$	1.9	55	16.5
2MASS J16185037$-$2424319	$16.84\pm 0.01$	$15.77\pm 0.01$	$15.16\pm 0.01$		$-6.6\pm 1.9$	$-27.0\pm 1.6$	1.5	57	15.9
2MASS J16185430$-$2346075	$18.88\pm 0.01$	$17.65\pm 0.01$	$16.92\pm 0.01$		$-6.0\pm 1.6$	$-15.5\pm 4.5$	1.0	46	15.7
2MASS J16190341$-$2344085	$17.98\pm 0.01$	$16.72\pm 0.01$	$16.01\pm 0.01$		$-6.7\pm 1.4$	$-24.3\pm 4.5$	1.6	61	15.7
2MASS J16190474$-$2307526	$16.21\pm 0.01$	$15.14\pm 0.01$	$14.56\pm 0.01$		$2.6\pm 3.1$	$-27.7\pm 4.2$	3.6	52	15.1
2MASS J16191521$-$2417241	$15.22\pm 0.01$	$14.24\pm 0.01$	$13.70\pm 0.01$		$-14.1\pm 1.2$	$-15.3\pm 2.8$	1.8	59	16.5
2MASS J16191646$-$2347235	$18.95\pm 0.01$	$17.58\pm 0.01$	$16.78\pm 0.01$		$-7.6\pm 1.5$	$-14.3\pm 1.8$	1.2	75	15.7
2MASS J16192634$-$2412444	$16.93\pm 0.01$	$15.80\pm 0.01$	$15.18\pm 0.01$		$-9.7\pm 2.0$	$-8.9\pm 8.1$	4.7	62	16.5
2MASS J16192988$-$2440469	$18.39\pm 0.01$	$16.90\pm 0.01$	$16.07\pm 0.01$		$-7.4\pm 1.2$	$-24.4\pm 3.7$	1.5	59	16.5
2MASS J16192992$-$2425540	$14.63\pm 0.01$	$13.70\pm 0.01$	$13.21\pm 0.01$		$-7.3\pm 1.5$	$-23.6\pm 2.3$	2.7	77	15.9
2MASS J16193976$-$2145349	$16.58\pm 0.01$	$15.43\pm 0.01$	$14.77\pm 0.01$		$-5.1\pm 1.6$	$-22.7\pm 2.4$	3.4	59	15.1
2MASS J16194210$-$2504323	$18.87\pm 0.01$	$17.58\pm 0.01$	$16.86\pm 0.01$		$-15.7\pm 8.0$	$-12.5\pm 6.2$	15	62	16.5
2MASS J16194309$-$2216175	$14.73\pm 0.01$	$13.99\pm 0.01$	$13.62\pm 0.01$		$-15.0\pm 3.4$	$-18.8\pm 4.1$	2.5	70	15.7
2MASS J16194836$-$2212519	$\cdots$	$\cdots$	$12.53\pm 0.01$		$-6.5\pm 1.8$	$-14.6\pm 5.4$	5.2	77	15.7
2MASS J16195143$-$2241332	$18.28\pm 0.01$	$16.99\pm 0.01$	$16.21\pm 0.01$		$-5.3\pm 1.5$	$-13.2\pm 5.6$	1.8	51	15.7
2MASS J16195827$-$2832276	$20.98\pm 0.04$	$19.37\pm 0.02$	$18.27\pm 0.03$		$-17.7\pm 6.5$	$-19.9\pm 6.5$	0.9	49	15.7
2MASS J16200757$-$2359150	$16.76\pm 0.01$	$15.55\pm 0.01$	$14.87\pm 0.01$		$-14.4\pm 3.7$	$-22.7\pm 2.0$	2.8	63	14.4
2MASS J16201318$-$2425014	$16.25\pm 0.01$	$15.49\pm 0.01$	$15.10\pm 0.01$		$-3.7\pm 2.0$	$-5.8\pm 1.2$	4.2	61	14.8
2MASS J16202128$-$2120289	$16.65\pm 0.01$	$15.55\pm 0.01$	$14.90\pm 0.01$		$-5.6\pm 1.0$	$-16.6\pm 3.6$	1.3	67	15.7
2MASS J16202163$-$2005348	$14.94\pm 0.01$	$14.03\pm 0.01$	$13.56\pm 0.01$		$-16.5\pm 2.8$	$-23.9\pm 3.6$	10	76	15.1
2MASS J16202523$-$2316033	$17.89\pm 0.01$	$16.72\pm 0.01$	$16.08\pm 0.01$		$-9.5\pm 1.3$	$-20.3\pm 2.0$	1.7	60	15.7
2MASS J16203456$-$2430205	$18.93\pm 0.01$	$17.26\pm 0.01$	$16.29\pm 0.01$		$8.0\pm 7.5$	$-18.7\pm 3.7$	5.7	38	14.2
2MASS J16204144$-$2425491	$18.44\pm 0.01$	$17.08\pm 0.01$	$16.29\pm 0.01$		$-11.8\pm 3.3$	$-15.2\pm 2.0$	1.5	60	14.8
2MASS J16210222$-$2358395	$18.87\pm 0.01$	$17.51\pm 0.01$	$16.70\pm 0.01$		$-7.4\pm 2.6$	$-16.7\pm 3.0$	2.9	54	15.7
2MASS J16211563$-$2436117	$14.54\pm 0.01$	$13.95\pm 0.01$	$13.67\pm 0.01$		$-27.7\pm 1.8$	$-15.9\pm 1.6$	3.9	64	15.5
2MASS J16211920$-$2425525	$15.75\pm 0.01$	$14.66\pm 0.01$	$14.00\pm 0.01$		$-0.5\pm 1.6$	$-14.5\pm 1.6$	1.8	70	15.1
2MASS J16212488$-$2426145	$16.17\pm 0.01$	$15.15\pm 0.01$	$14.57\pm 0.01$		$-6.5\pm 2.4$	$-17.3\pm 1.0$	2.3	74	15.5
2MASS J16212953$-$2529431	$\cdots$	$\cdots$	$12.54\pm 0.01$		$-5.1\pm 2.1$	$-18.8\pm 2.3$	2.3	77	15.5
2MASS J16212961$-$2129038	$15.02\pm 0.01$	$14.07\pm 0.01$	$13.61\pm 0.01$		$-3.1\pm 3.0$	$-18.7\pm 11.6$	21	71	15.7
2MASS J16213591$-$2355035	$17.65\pm 0.01$	$16.40\pm 0.01$	$15.67\pm 0.01$		$-9.6\pm 1.3$	$-17.8\pm 2.2$	1.6	72	15.7
2MASS J16214853$-$2517266	$\cdots$	$\cdots$	$12.53\pm 0.01$		$-8.1\pm 1.9$	$-20.0\pm 1.4$	1.2	58	16.8
2MASS J16215975$-$2706366	$14.68\pm 0.01$	$13.91\pm 0.01$	$13.51\pm 0.01$		$-9.0\pm 1.6$	$-22.1\pm 2.2$	2.5	66	16.2
2MASS J16221693$-$1825131	$\cdots$	$\cdots$	$17.80\pm 0.04$		$-25.9\pm 14.2$	$-0.6\pm 11.2$	24	14	14.3
2MASS J16222160$-$2217307	$16.56\pm 0.01$	$15.51\pm 0.01$	$14.96\pm 0.01$		$-22.7\pm 3.3$	$-18.6\pm 2.6$	4.0	66	15.1
2MASS J16222521$-$2405139	$18.27\pm 0.01$	$17.00\pm 0.01$	$16.23\pm 0.01$		$-13.9\pm 1.7$	$-3.4\pm 6.2$	3.7	62	16.8
2MASS J16223834$-$2541017	$18.50\pm 0.01$	$17.28\pm 0.03$	$16.53\pm 0.02$		$-8.8\pm 4.0$	$-13.0\pm 3.4$	1.6	59	16.8
2MASS J16224385$-$1951057	$16.63\pm 0.01$	$15.14\pm 0.01$	$14.25\pm 0.01$		$3.2\pm 4.1$	$-21.4\pm 2.9$	7.2	51	15.7
2MASS J16230646$-$2528419	$19.09\pm 0.01$	$17.71\pm 0.01$	$16.90\pm 0.01$		$-14.9\pm 2.6$	$-24.4\pm 2.6$	1.0	50	16.0
2MASS J16232202$-$2609553	$18.88\pm 0.02$	$17.66\pm 0.01$	$16.89\pm 0.03$		$-6.8\pm 2.6$	$-18.5\pm 4.5$	1.2	49	16.8
2MASS J16235155$-$2317270	$17.43\pm 0.01$	$16.07\pm 0.01$	$15.24\pm 0.01$		$-14.1\pm 9.4$	$-26.7\pm 4.1$	3.9	59	15.7
2MASS J16235470$-$2438319	$17.23\pm 0.01$	$15.94\pm 0.01$	$15.17\pm 0.01$		$-2.2\pm 2.7$	$-17.0\pm 4.3$	1.4	61	16.8
2MASS J16250277$-$3006556	$18.31\pm 0.01$	$17.14\pm 0.01$	$16.50\pm 0.01$		$-7.0\pm 4.2$	$-22.3\pm 6.7$	4.2	50	16.5
2MASS J16252860$-$1658509	$17.44\pm 0.01$	$16.14\pm 0.01$	$15.40\pm 0.01$		$-6.3\pm 3.2$	$-8.5\pm 2.5$	1.6	63	16.7
2MASS J16252969$-$2214543	$16.52\pm 0.01$	$15.42\pm 0.01$	$14.82\pm 0.01$		$-5.9\pm 2.0$	$-15.7\pm 1.8$	1.7	51	15.7
2MASS J16253274$-$2611386	$14.63\pm 0.01$	$13.76\pm 0.01$	$13.30\pm 0.01$		$-7.1\pm 4.8$	$-14.6\pm 4.6$	11	90	16.5
2MASS J16253672$-$2224285	$17.03\pm 0.01$	$15.88\pm 0.01$	$15.16\pm 0.01$		$-5.2\pm 2.7$	$-15.8\pm 7.4$	2.1	47	15.7
2MASS J16254322$-$2230026	$15.98\pm 0.01$	$15.02\pm 0.01$	$14.49\pm 0.01$		$-5.9\pm 3.1$	$-18.2\pm 2.3$	3.1	58	15.7
2MASS J16254808$-$2154195	$14.63\pm 0.01$	$13.87\pm 0.01$	$13.46\pm 0.01$		$-9.4\pm 2.4$	$-18.6\pm 3.6$	2.6	72	15.7
2MASS J16255066$-$2155454	$17.24\pm 0.01$	$16.26\pm 0.01$	$15.74\pm 0.01$		$-16.1\pm 13.2$	$-24.1\pm 2.2$	11	66	15.7
2MASS J16260625$-$2334030	$16.90\pm 0.01$	$15.69\pm 0.01$	$14.96\pm 0.01$		$2.0\pm 2.7$	$-31.9\pm 3.5$	3.3	80	15.3
2MASS J16263026$-$2336551	$17.68\pm 0.03$	$16.27\pm 0.01$	$15.50\pm 0.04$		$-3.5\pm 1.1$	$-16.9\pm 4.5$	1.4	55	15.7
2MASS J16263276$-$2622589	$14.50\pm 0.01$	$13.49\pm 0.01$	$12.92\pm 0.01$		$-6.8\pm 1.8$	$-27.2\pm 4.9$	4.5	53	15.1
2MASS J16265619$-$2213519	$16.84\pm 0.01$	$15.72\pm 0.01$	$15.05\pm 0.01$		$-7.9\pm 1.8$	$-20.6\pm 2.3$	1.6	62	15.3
2MASS J16270217$-$2542346	$18.98\pm 0.01$	$17.59\pm 0.01$	$16.72\pm 0.01$		$-10.2\pm 1.7$	$-13.0\pm 2.7$	1.1	32	15.7
2MASS J16270942$-$2148457	$16.30\pm 0.01$	$15.22\pm 0.03$	$14.79\pm 0.02$		$-8.7\pm 1.7$	$-18.4\pm 1.7$	2.4	70	15.7
2MASS J16272034$-$2844302	$18.47\pm 0.01$	$17.31\pm 0.04$	$16.54\pm 0.01$		$-30.5\pm 10.5$	$-34.7\pm 5.1$	18	57	15.3
2MASS J16272553$-$2138036	$15.10\pm 0.01$	$14.24\pm 0.01$	$13.80\pm 0.01$		$-7.6\pm 1.3$	$-17.7\pm 3.7$	2.8	69	15.7
2MASS J16274799$-$2457134	$17.47\pm 0.01$	$16.19\pm 0.01$	$15.42\pm 0.01$		$-6.7\pm 1.8$	$-21.6\pm 1.9$	1.1	64	15.3
2MASS J16281808$-$2428358	$16.61\pm 0.01$	$15.30\pm 0.01$	$14.54\pm 0.01$		$-3.5\pm 1.3$	$-25.2\pm 1.9$	1.1	62	15.7
2MASS J16284703$-$2428138	$16.65\pm 0.04$	$15.81\pm 0.01$	$15.19\pm 0.02$		$-6.6\pm 1.6$	$-18.5\pm 1.9$	1.9	58	15.7
2MASS J16292211$-$1742091	$15.41\pm 0.01$	$14.49\pm 0.01$	$14.02\pm 0.01$		$-25.0\pm 7.5$	$-22.3\pm 2.2$	6.3	61	16.7
2MASS J16293624$-$2456527	$16.51\pm 0.01$	$15.52\pm 0.01$	$14.90\pm 0.01$		$-12.8\pm 4.2$	$-19.5\pm 2.6$	4.6	80	15.7
2MASS J16293662$-$1708413	$14.83\pm 0.01$	$13.94\pm 0.01$	$13.47\pm 0.01$		$-2.3\pm 1.2$	$-19.5\pm 3.7$	2.5	75	16.7
2MASS J16293934$-$1614570	$14.54\pm 0.01$	$13.89\pm 0.01$	$13.57\pm 0.01$		$-26.2\pm 2.4$	$-6.0\pm 2.2$	5.2	72	16.7
2MASS J16294879$-$2137086	$15.50\pm 0.01$	$14.55\pm 0.01$	$14.02\pm 0.01$		$-4.0\pm 5.5$	$-17.6\pm 4.7$	15	64	15.7
2MASS J16302673$-$2359087	$16.07\pm 0.01$	$14.95\pm 0.02$	$14.30\pm 0.01$		$-1.5\pm 1.8$	$-24.4\pm 4.0$	3.0	61	15.1
2MASS J16303390$-$2428062	$14.72\pm 0.01$	$13.76\pm 0.01$	$13.22\pm 0.01$		$-4.3\pm 1.7$	$-19.3\pm 1.9$	1.8	63	15.1
2MASS J16305349$-$2424538	$15.69\pm 0.01$	$14.61\pm 0.01$	$13.99\pm 0.01$		$-1.6\pm 2.1$	$-21.9\pm 1.6$	1.9	79	16.1
2MASS J16310240$-$2408431	$14.73\pm 0.01$	$13.78\pm 0.01$	$13.24\pm 0.01$		$0.9\pm 1.8$	$-22.0\pm 2.1$	2.3	69	16.1
2MASS J16313519$-$2542261	$18.41\pm 0.01$	$17.05\pm 0.01$	$16.26\pm 0.01$		$-11.8\pm 5.9$	$-18.7\pm 8.1$	4.1	43	14.6
2MASS J16320136$-$2237081	$17.70\pm 0.01$	$16.50\pm 0.01$	$15.78\pm 0.01$		$-5.1\pm 2.3$	$-17.2\pm 3.7$	2.2	55	16.0
2MASS J16324221$-$2316562	$14.66\pm 0.01$	$13.66\pm 0.01$	$13.14\pm 0.01$		$-16.6\pm 2.3$	$-34.1\pm 1.7$	2.7	62	16.2
2MASS J16324727$-$2059375	$16.55\pm 0.01$	$15.53\pm 0.02$	$14.97\pm 0.01$		$-12.4\pm 8.0$	$-17.3\pm 3.0$	19	65	16.6
2MASS J16332000$-$2741076	$17.80\pm 0.01$	$16.71\pm 0.01$	$16.12\pm 0.01$		$-13.2\pm 2.2$	$-17.8\pm 1.8$	2.4	54	16.5
2MASS J16342850$-$2201119	$16.81\pm 0.01$	$15.64\pm 0.01$	$14.99\pm 0.01$		$-8.9\pm 1.8$	$-25.8\pm 2.2$	1.9	62	16.1
2MASS J16370753$-$2432395	$19.35\pm 0.01$	$17.69\pm 0.01$	$16.67\pm 0.01$		$-2.9\pm 2.4$	$-13.6\pm 4.1$	1.3	50	16.5
Unreliable fits: ${\chi }_{\nu }^2\le 0.3$ or ${\chi }_{\nu }^2\ge 40$
2MASS J16002535$-$2644060	$16.03\pm 0.01$	$15.09\pm 0.01$	$14.54\pm 0.01$		$-23.2\pm 6.0$	$19.9\pm 21.0$	64	64	15.9
2MASS J16070211$-$2019387	$15.74\pm 0.02$	$14.82\pm 0.04$	$14.35\pm 0.04$		$102.4\pm 41.2$	$48.9\pm 28.7$	89	79	15.7
2MASS J16090405$-$1934000	$14.85\pm 0.02$	$14.02\pm 0.03$	$13.49\pm 0.01$		$-70.2\pm 36.1$	$95.5\pm 54.7$	130	65	15.7
2MASS J16125723$-$2428013	$15.80\pm 0.01$	$14.89\pm 0.01$	$14.41\pm 0.01$		$-8.5\pm 5.8$	$1.0\pm 31.0$	110	70	16.5
2MASS J16273320$-$2821097	$\cdots$	$\cdots$	$12.67\pm 0.01$		$-17.2\pm 11.7$	$-9.8\pm 7.3$	58	65	15.7

Full text

brown dwarfs — proper motions — stars: formation — stars: individual (PSO J060.3200+25.9644, PSO J077.1033+24.3809, PSO J237.1470$-$23.1489)

††slugcomment: Accepted by The Astrophysical Journal, 2017 January 31

1 Introduction

Brown dwarfs with ages $\lesssim 100$ Myr are valuable laboratories for testing both the youngest substellar evolutionary models and the lowest-gravity (therefore lowest-mass) atmospheric models. For instance, brown dwarfs with T${}_{\rm eff}\lesssim 1400$ K and ages $\lesssim 20$ Myr will have masses $\lesssim 10$ $M_{\mathrm{Jup}}$ (e.g., Chabrier et al., 2000), firmly in the planetary regime ($\lesssim 13$ $M_{\mathrm{Jup}}$). These young, very low mass brown dwarfs therefore serve as vital templates for understanding directly imaged planets.

Star-forming regions and young open clusters offer the opportunity to identify multiple young brown dwarfs in small areas of the sky, at the age when these objects are brightest. Planetary-mass objects in star-forming regions have been discovered both as companions to stars (e.g., Luhman et al., 2006; Lafreniere et al., 2008) and as free-floating objects (e.g., Luhman et al., 2009; Weights et al., 2009). Wide-field, red-sensitive surveys such as the Pan-STARRS1 $3\pi$ Survey (PS1; Kaiser et al., 2010, K. Chambers et al., 2017, in prep), the Two Micron All Sky Survey (2MASS; Skrutskie et al., 2006), the UKIRT Infrared Deep Sky Survey (UKIDSS; Lawrence et al., 2007), and the Wide-Field Infrared Survey Explorer (WISE; Wright et al., 2010) have the ability to detect free-floating very low mass brown dwarfs in nearby star-forming regions (e.g., Lodieu, 2013; Esplin et al., 2014), although interstellar reddening at optical and near-infrared wavelengths can make brown dwarfs difficult to distinguish from background giant stars. More discoveries of these objects would improve our understanding of the early evolution of low mass brown dwarfs and giant planets.

At a distance of $\approx$145 pc and an age of $\approx$1–2 Myr (Kraus & Hillenbrand, 2009), the Taurus-Auriga molecular cloud (hereinafter Taurus) is one of the closest star-forming regions to the Sun. A comprehensive review of Taurus and its observational history can be found in Kenyon et al. (2008). Taurus has been searched extensively for substellar members from optical to mid-infrared wavelengths (e.g., Luhman, 2006; Slesnick et al., 2006; Guieu et al., 2006; Luhman et al., 2009; Quanz et al., 2010; Rebull et al., 2010). Esplin et al. (2014) cataloged 74 members with spectral types M6–L0, which at the young age of Taurus span the full brown dwarf mass regime from the stellar/sub-stellar boundary down to planetary masses ($\lesssim$13 $M_{\mathrm{Jup}}$). The coolest known substellar objects in Taurus to date are the free-floating $\approx$4–7 $M_{\mathrm{Jup}}$ 2MASS J04373705+2331080 (hereinafter 2MASS J0437+2331), discovered and classified as L0 by Luhman et al. (2009), and the planetary-mass companion 2MASS J04414489+2301513 Bb (Todorov et al., 2010), with a near-IR spectral type of L$1\pm 1$ on the Allers & Liu (2013a) system and an estimated mass of $\approx 10\pm 2$ $M_{\mathrm{Jup}}$ Bowler & Hillenbrand (2015).

The Scorpius-Centaurus Association (hereinafter Sco-Cen) is the nearest OB association to the Sun. The Sco-Cen complex, reviewed in detail by Preibisch & Mamajek (2008), has a distance similar to Taurus but an older age ($\approx$10–20 Myr). With no significant ongoing star formation, Sco-Cen is much less affected by interstellar reddening, but any planetary-mass objects will also have cooled and become fainter than equivalent-mass objects in Taurus. The Upper Scorpius subgroup in particular has been the target of many searches for ultracool dwarfs (e.g., Martín et al., 2004; Lodieu et al., 2006, 2011; Slesnick et al., 2006, 2008; Dawson et al., 2014). Lodieu et al. (2008) have probed the deepest into the substellar regime, spectroscopically confirming over 20 M8–L2 dwarfs in Upper Scorpius with masses down to $\approx$15 $M_{\mathrm{Jup}}$.

Here we present the discovery of two early-L dwarfs in Taurus and six M7–L1 dwarfs in Sco-Cen, serendipitously identified in a wide-field search for L/T transition dwarfs in the Pan-STARRS1 and WISE catalogs. In Section 2 we explain how these objects were initially identified, and we describe follow-up observations in Section 3. We detail the observed features of our discoveries in Section 4. We discuss their membership in Taurus (Section 5) or Sco-Cen (Section 6), and provide estimated masses and comparisons with model spectra. We summarize our discoveries in Section 7.

2 Photometric Selection

We conducted a search over $\approx$28,000 deg2 for L/T transition dwarfs in the field using a merged catalog of PS1 and WISE photometry. The search is described in detail in Best et al. (2013, hereinafter Paper I), and the full spectroscopic follow-up results are presented in Best et al. (2015, hereinafter Paper II), including our discovery of 130 ultracool dwarfs. Among these discoveries were 23 late-M and L dwarfs with spectroscopic signs of low gravity, implying youth. This was a surprisingly large number given that we were searching for objects with field ages and cooler spectral types ($\approx$L6–T5) and that objects with ages $\lesssim 200$ Myr should comprise at most a few percent of the local population in a galaxy $\gtrsim$10 Gyr old. In Paper II, we determined that our search could find late-M and L dwarfs with $W1-W2$ colors redder than average for their spectral types, bringing younger objects into our sample.

Our search also specifically avoided the heavily reddened areas of the sky defined in Cruz et al. (2003), which include Taurus and Sco-Cen. The eight discoveries described in this paper lie just outside these reddened regions, with one exception: PSO J060.3200+25.9644 (hereinafter PSO J060.3+25) lies $\approx$2∘ inside the Cruz et al. (2003) Taurus boundaries, but we pursued follow-up observations because its spectral energy distribution (SED) from $z_{\rm P1}$ through $W2$ (0.9–4.6 $\mu$m) strongly suggested an unreddened ultracool object.

The PS1 $z_{\rm P1}$ and $y_{\rm P1}$, WISE, 2MASS, and MKO photometry for our discoveries was originally presented in Paper II. In Table 1, we update the earlier version of PS1 photometry from Paper II with photometry from the PS1 Data Release 1 (DR1; Chambers et al., 2017, in prep; Magnier et al., 2017, in prep) and include $i_{\rm P1}$ magnitudes. The photometry used in both Paper II and this work is the mean PSF photometry from individually calibrated images; the DR1 photometry in this work includes many more epochs. We also replace the WISE All-Sky photometry (Cutri et al., 2012) used in Paper II with AllWISE magnitudes (Cutri et al., 2014). For reference, we reproduce the 2MASS and MKO photometry here in Table 2. We also include photometry for the previously-identified Taurus L dwarf 2MASS J0437+2331.

3 Near-Infrared Spectroscopy

We obtained near-infrared spectra for our candidates between 2013 January and 2015 May using the NASA Infrared Telescope Facility (IRTF). We used the facility spectrograph SpeX (Rayner et al., 2003) in prism mode with the $0.5^{\prime\prime}$ ($R\approx 120$) and $0.8^{\prime\prime}$ ($R\approx 75$) slits. Details of our observations are listed in Table 3. For each science target we observed a nearby A0V star contemporaneously for telluric calibration. All spectra were reduced in standard fashion using versions 3.4 and 4.0 of the Spextool software package (Vacca et al., 2003; Cushing et al., 2004). These observations were part of a large program (Paper II) in which our desired S/N was $\gtrsim$30, sufficient for accurate spectral typing based on overall spectral morphology but not necessarily for robust analysis of specific features. We therefore observed PSO J060.3+25 and PSO J077.1033+24.3809 (hereinafter PSO J077.1+24) a second time to achieve higher S/N, and for each object we combined the first and second epochs using the Spextool xcombspec routine to obtain a single higher-S/N spectrum, which we present in this paper.

While comparing the spectra of our discoveries to spectral standards, we noticed a small wavelength offset in the spectrum of the field L0 standard 2MASS J03454316+2540233 (hereinafter 2MASS J0345+2540) from Burgasser & McElwain (2006). The offset is large enough to affect calculations of the Allers & Liu (2013a) gravity-sensitive spectral indices that we used to analyze our discoveries (Section 4.2). We therefore used IRTF/SpeX to obtain a new spectrum of 2MASS J0345+2540 with more accurate wavelength calibration, which we used for our analysis. Appendix C presents this new spectrum and provides details of the observations.

4 Results

4.1 Ultracool Discoveries

The SpeX prism spectra for our eight young ultracool discoveries are presented in Figure 1, and their spectral types are listed in Table 4. We show their locations in the sky in Figure 2. PSO J060.3+25 was previously identified by Sarro et al. (2014) and Bouy et al. (2015) as a likely very low-mass member of the Pleiades cluster, based on photometry and astrometry. PSO J237.1471$-$23.1489 (hereinafter PSO J237.1$-$23) was identified by Lodieu (2013) as a photometric and astrometric candidate member of Upper Sco. We independently discovered these objects and present here spectral confirmation of their ultracool nature. We also find that PSO J060.3+25 is more likely to be a Taurus member than a Pleiad (Section 5.1.3). The other six objects are new discoveries.

In Figures 3 and 4 we compare the colors of our discoveries with those of previously known late-M and early-L dwarfs. Our discoveries in Taurus and Sco-Cen have red $W1-W2$ colors compared with field objects of similar spectral types, which led to the fortuitous discovery of these young M7–L2 dwarfs even though our search was designed to find L/T transition dwarfs (spectral types $\approx$ L6–T4). The $y_{\rm P1}-W1$, $y_{\rm P1}-J_{\rm MKO}$ and $(J-H)_{\rm MKO}$ colors of our discoveries are normal compared with field objects of similar spectral types.

4.2 Spectral Indices and Spectral Types

We used three methods to assign spectral types for our discoveries: visual comparison with low-gravity field standards and two index-based methods. Table 4 gives the spectral types calculated from the index-based system of Allers & Liu (2013a, hereinafter AL13). The AL13 indices were designed to assign near-infrared spectral types consistent with optical spectral types, independent of surface gravity. Since all of our discoveries show clear spectral signs of low gravity (Section 4.3), we adopted the AL13 index-based types as our final spectral types, rounded to the nearest subtype and assigned an uncertainty of 1 subtype (following AL13). For confirmation, we visually compared our spectra to the vl-g standards of AL13. All of our visually-determined types are within 1 subtype of the adopted index-based types.

In Table 5, we list the spectral types determined using the index-based system of Burgasser et al. (2006, hereinafter B06), compared with our adopted AL13 spectral types. The B06 and AL13 spectral types are consistent within their $2\sigma$ uncertainties, although the B06 types are mostly 1–3 subtypes later. This is probably a consequence of the fact that the B06 indices are not defined for spectral types earlier than L0, so the B06 spectral types are averages only of L types.

4.3 Low-Gravity Signatures

Low-gravity signatures in ultracool dwarf spectra are a well-established indication of ages $\lesssim$200 Myr (e.g., Kirkpatrick et al., 2008; Allers & Liu, 2013a). We used the AL13 system based on gravity-sensitive near-IR spectral indices to assess whether our spectra display signs of low gravity. In this system, an object is assigned a score of 0 for field gravity (fld-g, ages $\gtrsim 200$ Myr), 1 for intermediate gravity (int-g, ages $\approx 50-200$ Myr), or 2 for very low gravity (vl-g, ages $\approx 10-30$ Myr). We calculated indices and gravity scores for our discoveries following Aller et al. (2016), who adapt AL13 to incorporate Monte Carlo assessment of the uncertainties in the indices and gravity classes. We also visually examined the gravity-sensitive features in our spectra as a check on the gravity scores.

We classify six of our discoveries as vl-g: PSO J060.3+25, PSO J077.1+24, PSO J231.7899$-$26.4494 (hereinafter PSO J231.7$-$26), PSO J231.8942$-$29.0600 (hereinafter PSO J231.8$-$29), PSO J237.1$-$23, and PSO J239.7016$-$23.2664 (hereinafter PSO J239.7$-$23). Table 6 lists their indices and gravity scores. Figure 7 compares the spectra of these six vl-g objects with field standards from Kirkpatrick et al. (2010) and vl-g standards from AL13 having the same spectral types. For the L0 field standard 2MASS J0345+2540, we use our new SpeX prism spectrum (Appendix C). All six of our spectra display weak 0.99 $\mu$m FeH and 1.25 $\mu$m K i absorption, and a triangular H band shape, all signs of youth. PSO J060.3+25, PSO J077.1+24, PSO J231.7$-$26, and PSO J231.8$-$29 also show strong 1.06 $\mu$m VO absorption, which AL13 identify as an additional sign of youth for L0–L4 dwarfs.

For the other two objects, PSO J228.6773$-$29.7088 (hereinafter PSO J228.6$-$29) and PSO J229.2354$-$26.6738 (hereinafter PSO J229.2$-$26), the S/N of our spectra was too low ($\lesssim$30) to yield robust gravity scores from the AL13 indices. Figure 8 shows these spectra, again compared with the appropriate field and vl-g standards. In spite of the measurement uncertainties, visual inspection confirms that both objects have weak 0.99 $\mu$m FeH and 1.25 $\mu$m K i absorption, strong 1.06 $\mu$m VO absorption, and triangular H band shapes, so we regard them as strong candidate vl-g objects.

4.4 Proper Motions

Proper motions are key to establishing membership in star-forming regions and clusters whose bulk motion through space is well defined. We use proper motions from PS1 Processing Version 3.2 (PV3.2), the version used for the photometry and mean positions in PS1 DR1. (PS1 proper motions will be part of a future public release.) PV3.2 astrometry is calibrated to the Gaia DR1 (Gaia Collaboration et al., 2016) astrometric reference frame. We present the proper motions for our discoveries in Table 7, and we discuss their consistency with members of Taurus and Sco-Cen in Sections 5 and 6. We present catalogs of proper motions for low-mass members of Taurus and Upper Sco in Appendices A and B, along with a brief summary of the method used to calculate PS1 proper motions.

4.5 No Candidate Binaries

As in Paper II, we used the spectral index criteria of Bardalez Gagliuffi et al. (2014, hereinafter BG14) and visual inspection to search for spectral features indicating that our discoveries may be unresolved binaries. PSO J228.6$-$29 satisfies only one of the twelve BG14 criteria, and our other seven discoveries meet none of the BG14 criteria. Similarly, we found no evidence of spectral blends via visual inspection. None of these objects appear to be candidate unresolved binaries.

In addition, we investigated whether any of our discoveries could be members of wide binary or multiple systems. We searched for nearby known members of the star-forming regions in which our discoveries reside, using the catalogs of Esplin et al. (2014) for Taurus and Luhman & Mamajek (2012) for Upper Scorpius. As several of our Sco-Cen discoveries lie outside the classical boundaries of Upper Scorpius (Section 6), we also searched across all catalogs in Vizier111http://vizier.u-strasbg.fr/viz-bin/VizieR for objects near these discoveries. We found no known members of Taurus or Sco-Cen within $70^{\prime\prime}$ (corresponding to a projected separation $\approx 10,000$ AU) of our discoveries. At wider separations, it is still possible for a pair of low-mass stars and/or brown dwarfs to be physically bound (Dhital et al., 2010; Deacon et al., 2014). However, such a binary is likely to have formed through capture in the natal cluster rather than as an initially bound system (Kouwenhoven et al., 2010). Thus, we conclude that all of our discoveries are likely to be free-floating brown dwarfs that formed as single objects.

5 Taurus Discoveries

Two of our discoveries, PSO J060.3+25 (L1) and PSO J077.1+24 (L2), reside at the projected outer edges of the nearby Taurus star-forming region. Figure 2 shows their sky locations in Taurus. In Section 5.1 we present confirmation that they are bona fide members of Taurus. We also estimate their masses (Section 5.2) and assess whether they have circumstellar disks (Section 5.3).

We first explore why these objects were not identified in previous studies of Taurus, a region that has been repeatedly searched for ultracool dwarfs. Our objects lie $\approx$8∘ ($\approx$20 pc) from the projected center of Taurus, on opposite sides from each other. Many searches surveyed smaller and/or more central regions of Taurus that did not include our objects (e.g., Guieu et al., 2006; Luhman et al., 2009; Quanz et al., 2010; Rebull et al., 2010). Our objects also lie just outside the footprint of Spitzer images analyzed by Esplin et al. (2014). Our objects are very faint, especially at optical wavelengths, so previous searches using $i$-band photometry (e.g., Slesnick et al., 2006) were not able to detect them. Similarly, both objects lie within the area searched by Esplin et al. (2014) using WISE photometry, but are fainter than the $W1\leq 14$ mag limit used in that search. Luhman (2006) would have detected PSO J077.1+24 in 2MASS photometry, but its $(J-H)_{\rm 2MASS}=0.46\pm 0.28$ mag color is bluer than the $(J-H)_{\rm 2MASS}\geq 0.6$ mag cut used in that search.222We note the large error on this color is due to this object being near the detection limit of 2MASS. Our deeper MKO photometry (Table 2) shows this object has $(J-H)_{\rm MKO}=0.75\pm 0.06$ mag. PSO J060.3+25 lies just outside the Luhman (2006) search area but would also have been excluded due to its relatively blue $(H-K_{S})_{\rm 2MASS}$ color (also having a large error). We note also that Luhman (2006) used previously known low-mass members of Taurus as templates to define color cuts, and many of those members are reddened by local extinction. Our discoveries do not appear to be reddened, as discussed in Sections 5.1.2 and 5.1.5.

5.1 Evidence for Membership

5.1.1 Youth

Both PSO J060.3+25 and PSO J077.1+24 have vl-g gravity classes (Section 4.3). While more work is needed to calibrate the ages of vl-g objects (Allers & Liu, 2013a), the classification suggests an age $\lesssim 30$ Myr, much younger than the field population.

5.1.2 Photometry

Figure 9 compares the photometry of PSO J060.3+25 and PSO J077.1+24 to that of known Taurus members from Esplin et al. (2014). The $J$ vs. $J-K_{S}$ (2MASS) and $y_{\rm P1}$ vs. $y_{\rm P1}-W1$ color-magnitude diagrams for Taurus make evident the significant reddening in this region of the sky. We calculated reddening vectors for these color-magnitude diagrams using the $y_{\rm P1}$ coefficient from Schlafly & Finkbeiner (2011, their Table 6, $R_{V}=3.1$) and the $J/K_{S}/W1$ coefficients from Davenport et al. (2014, their Table 3). We include these reddening vectors, scaled to an extinction of $A_{V}=5$ mag, in Figure 9. Our two discoveries sit at the faint end of the unreddened cluster sequence, consistent with their projected locations on the unobscured outskirts of the region. While some young early-L dwarfs have unusually red $(J-K_{S})_{\rm 2MASS}$ colors for their spectral types (e.g., Gagné et al., 2015b), we note that the $(J-K_{S})_{\rm 2MASS}$ colors of our Taurus discoveries ($1.45\pm 0.24$ mag for PSO J060.3+25, $1.11\pm 0.26$ mag for PSO J077.1+24) are consistent with those of older field dwarfs with the same spectral types (Schmidt et al., 2010; Faherty et al., 2013). However, both PSO J060.3+25 and PSO J077.1+24 have $W1-W2$ colors (Figure 3) that are $3\sigma$ redder than those of field early-L dwarfs, a common sign of low gravity (Gizis et al., 2012).

5.1.3 Proper Motions

To assess the kinematic consistency of our discoveries with previously known members of Taurus, we created a list of proper motions for the Taurus stars and brown dwarfs from Esplin et al. (2014) that are not saturated in PS1. We obtained the proper motions from PS1 Processing Version 3.2 (PV3.2), the same source as the proper motions of our discoveries (Section 4.4). We discuss our complete list of proper motions in detail in Appendix A. Figure 10 compares the proper motions of PSO J060.3+25 and PSO J077.1+24 with all reliable PS1 Taurus proper motions. We calculated a weighted mean proper motion for the known Taurus members of ($\mu_{\alpha}{\rm cos}\,\delta=7.6\pm 0.2,\ \mu_{\delta}=-17.4\pm 0.2$ mas yr*-1*), with a weighted rms of 4.9 mas yr*-1* in R.A. and 6.4 mas yr*-1* in Dec.

PSO J077.1+24 has a proper motion of ($14.1\pm 12.5,-27.1\pm 12.1$ mas yr*-1*), consistent with the mean Taurus proper motion. Because the Taurus region has a number of distinct subgroups, we also compared the proper motion of PSO J077.1+24 to that of the closest subgroup on the sky identified by Luhman et al. (2009), L1544. This subgroup has a median proper motion of ($0.9\pm 1,-17.6\pm 1$ mas yr*-1*; Luhman et al., 2009), consistent with PSO J077.1+24.

For PSO J060.3+25, we adopt the proper motion ($14.3\pm 3.1,-26.4\pm 3.2$ mas yr*-1*) from Bouy et al. (2015). Our PS1 proper motion of ($19.0\pm 8.2,-38.1\pm 8.2$ mas yr*-1*) is consistent, but the Bouy et al. (2015) measurement is more precise. The adopted proper motion is very similar to PSO J077.1+24 and consistent with our mean Taurus proper motion. The closest Taurus subgroup on the sky to PSO J060.3+25 identified by Luhman et al. (2009), B209 ($\approx$4*∘* away), has a mean proper motion of ($6.9\pm 1,-22.3\pm 1$ mas yr*-1*; Luhman et al., 2009), consistent within $1.8\sigma$ in R.A. and $1.0\sigma$ in Dec.

PSO J060.3+25 (a.k.a. DANCe J040116.80+255752.2) was also previously identified by Sarro et al. (2014) and Bouy et al. (2015) as a high-probability (93%) member of the Pleiades cluster, based on $z\,YJHK_{S}$ photometry and astrometry. The Pleiades lie at a mean distance of $136.2\pm 1.2$ pc (Melis et al., 2014), commensurate with the $\approx$145 pc distance to Taurus. The projected center of the Pleiades lies $\approx$3.5∘ away from PSO J060.3+25, or $\approx$8 pc at the distance of the Pleiades, so it is possible that PSO J060.3+25 falls within the $9.5\pm 0.5$ pc tidal radius of the Pleiades (Danilov & Loktin, 2015). The mean proper motion for low-mass brown dwarfs ($0.012-0.025$ $M_{\odot}$) in the Pleiades is ($21.6,-47.6$ mas yr*-1*) with a dispersion of $\sigma_{\mu}=7.5\pm 6.1$ mas yr*-1* (Zapatero Osorio et al., 2014a), so the proper motion of PSO J060.3+25 is intermediate between the bulk motions of Taurus and the Pleiades, and consistent within $2\sigma$ with both groups. Our vl-g classification for PSO J060.3+25 suggests a younger age ($\lesssim 30$ Myr) than for the Pleiades ($\approx$125 Myr; Stauffer et al., 1998b), although the age range of vl-g objects has not been firmly established (e.g., Liu et al., 2016). We note that Allers & Liu (2013b) classified several Pleiades members as vl-g, but they used spectra with mostly lower resolution ($R\approx 50$) and S/N ($\lesssim$20) than the prism spectra we present here for our discoveries, so we regard those classifications as provisional. In Figure 11 we also compare the $J$ and $K$-band photometry of known Taurus members and our discoveries, as a function of spectral type, to known VLM members of the Pleiades. The published spectral types for the Pleiades members are derived from multiple sources and methods and are therefore heterogenous, but classification of these objects using the AL13 system shows a consistent result (Allers & Liu, 2013b). Figure 11 shows that our discoveries have $J$ magnitudes more consistent with the younger, brighter members of Taurus. We therefore find it more likely that PSO J060.3+25 is a member of the 1–2 Myr old Taurus region. A radial velocity measurement would help to further assess the Taurus membership of PSO J060.3+25.

5.1.4 Likelihood of Field Contamination

We investigated the possibility that PSO J060.3+25 or PSO J077.1+24 could be a foreground or background field object in the direction of Taurus by estimating the number of such contaminating field objects from our search. For this estimate, we generously defined the boundaries of the Taurus region to be $4^{\rm h}00^{\rm m}\leq\alpha\leq 5^{\rm h}15^{\rm m}$ and $14^{\circ}\leq\delta\leq 32^{\circ}$ (see Figure 2), covering 309.4 deg2. Our search covered the entire sky between declinations $-30^{\circ}$ and $+70^{\circ}$ except for locations within $3^{\circ}$ of the Galactic plane (Paper II), an area totaling 28,070 deg2. (We noted in Section 2 that our search also avoided reddened regions identified by Cruz et al. 2003, but PSO J060.3+25 actually lies within one of these reddened regions, so we include those regions in this estimate.)

We found a total of fourteen vl-g L0–L2 dwarfs in our search, including two previously known objects and three discoveries that we consider to be strong vl-g candidates. We would therefore expect our search to find 0.15 vl-g L0–L2 dwarfs in an arbitrary Taurus-sized area of sky.

In addition, we assessed the likelihood that an early-L dwarf observed in the direction of Taurus would have a proper motion consistent with members of Taurus (as do PSO J060.3+25 and PSO J077.1+24). We used the Besançon Galactic model333http://model.obs-besancon.fr (Robin et al., 2003) to generate a synthetic population of field M dwarfs in a volume spanning our Taurus boundaries between 50 pc and 240 pc. We assigned uncertainties to the synthetic proper motions using an astrometric error vs. $K_{S}$ relationship derived from our Taurus proper motions (Section 5.1.3). Assuming that early-L dwarfs have the same kinematics as M dwarfs in the field, we used Monte Carlo trials to determine that $20.3\pm 0.2$% of early-L dwarfs in the direction of Taurus will have proper motions within $3\sigma$ of the mean Taurus $\mu_{\alpha}{\rm cos}\,\delta$ and $\mu_{\delta}$.

We would therefore expect our search to find $(3.13\pm 0.03)\times 10^{-2}$ vl-g dwarfs within our Taurus boundaries having proper motions consistent with Taurus membership. Poisson statistics give us a probability of 96.9% that neither PSO J060.3+25 nor PSO J077.1+24 is an interloping field object in the direction of Taurus, and a negligible $5\times 10^{-4}$ probability that both objects are contaminants.

5.1.5 Comparison with 2MASS J04373705+2331080

Prior to our discoveries, 2MASS J0437+2331 was the only known free-floating L dwarf member of Taurus, discovered and classified as L0 by Luhman et al. (2009). We used the SpeX Prism spectrum for 2MASS J0437+2331 from Bowler et al. (2014) to assign a near-infrared spectral type of L$1\pm 1$, based on a calculated type of L$0.9\pm 0.9$ using the AL13 indices (Section 4.2).

Luhman et al. (2009) claimed membership in Taurus for 2MASS J0437+2331 based on weaker Na i and K i absorption features in its red-optical spectrum, which are recognized signs of youth (Kirkpatrick et al., 2006), along with its central projected location in Taurus. Similarly to two of our Sco-Cen discoveries, the spectrum for 2MASS J0437+2331 does not have a high enough S/N for us to confidently assign a gravity class, but Figure 14 shows that it more closely resembles the L1 vl-g standard than the field standard, confirming its young age. Figure 9 shows that the y_{\rm P1}$$JK_{S}W1 photometry of 2MASS J0437+2331 is also similar to that of PSO J060.3+25 and PSO J077.1+24, and consistent with being a slightly reddened member of Taurus. 2MASS J0437+2331 has a proper motion of ($15.9\pm 13.5,-54.8\pm 13.4$ mas yr*-1*), consistent with our mean motion of Taurus in R.A. but nearly $2\sigma$ different in Dec. We note that 2MASS J0437+2331 satisfies all the criteria for our search (Section 2), except that it lies well within the excluded reddened region of Cruz et al. (2003).

We compare the spectrum of 2MASS J0437+2331 to those of PSO J060.3+25 and PSO J077.1+24 in Figures 12 and 13, along with the appropriate field (Kirkpatrick et al., 2010) and vl-g (AL13) standards. Interestingly, the near-IR spectrum of 2MASS J0437+2331 is notably redder than those of our discoveries, and its position in the color-magnitude diagrams in Figure 9 is consistent with an extinction of $A_{V}\approx 2-4$ mag. This redness was also noted by Alves de Oliveira et al. (2013), who calculated an extinction of $A_{V}=2.1-3.3$ mag for 2MASS J0437+2331 based on 2MASS photometry and comparison to the near-IR spectra of other young M and L dwarfs. However, Luhman et al. (2009) found an extinction of $A_{J}=0$ mag for 2MASS J0437+2331 using an optical spectrum, which is more sensitive to dust-induced reddening than longer near-IR wavelengths. Our near-IR spectrum also closely resembles the L2 vl-g standard in color. It therefore appears that the red near-IR colors of 2MASS J0437+2331 are photospheric in nature.

Overall, we find supporting evidence that 2MASS J0437+2331 is a member of Taurus, and we find the photometric and spectral qualities of PSO J060.3+25 and PSO J077.1+24 to be very similar to those of 2MASS J0437+2331. The only notable difference is the redder overall near-infrared spectral slope of 2MASS J0437+2331, which does not appear to be due to interstellar extinction (Luhman et al., 2009).

5.1.6 Membership in Taurus

Because of the locations of PSO J060.3+25 and PSO J077.1+24 on Taurus color-magnitude diagrams, their plausibly consistent proper motions, their vl-g gravity classifications, their photometric and spectral similarity to the known Taurus L1 dwarf 2MASS J0437+2331, and the low probability of contamination by field objects, we consider PSO J060.3+25 and PSO J077.1+24 to be bona fide members of Taurus. Their near-infrared colors, consistent with those of field early-L dwarfs but bluer than 2MASS J0437+2331, confirm that the near-infrared redness observed in some low-gravity early-L dwarfs (e.g., Gizis et al. 2012; Faherty et al. 2013; see also Aller et al. 2016) is not a universal feature even for very young (1–2 Myr) L1 and L2 dwarfs.

5.2 Luminosities and Masses

To estimate the masses of our Taurus discoveries, we assumed a distance of $145\pm 15$ pc and an age of 1–2 Myr (Kraus & Hillenbrand, 2009). We first calculated bolometric luminosities for each object using our spectral types, the $K_{\rm MKO}$ bolometric corrections of Liu et al. (2010, their Table 6), and the distance to Taurus. We then used the Lyon/DUSTY evolutionary models444The more recent BHAC15 models (Baraffe et al., 2015) do not extend to masses below $0.01M_{\odot}\ (\approx 10M_{\mathrm{Jup}})$. (Chabrier et al., 2000) and our $L_{\rm bol}$ values to interpolate masses at the age of Taurus. We propagated the uncertainties on our spectral types ($\pm 1$ subtype), $K_{\rm MKO}$ magnitudes, bolometric correction, distance, and age into our mass determinations using Monte Carlo simulations, and we quote 68% confidence limits. We used normal distributions for each uncertainty except for age, for which we used a uniform distribution spanning 1–2 Myr to avoid unreasonably young ages. We estimate masses of $6.0^{+0.9}_{-0.8}$ $M_{\mathrm{Jup}}$ for PSO J060.3+25 and $5.9^{+0.9}_{-0.8}$ $M_{\mathrm{Jup}}$ for PSO J077.1+24 (Table 7). We also applied this method to 2MASS J0437+2331 using $K_{\rm MKO}=15.20\pm 0.02$ mag from the UKIDSS Galactic Clusters Survey (Lawrence et al., 2007, 2013). We estimate log($L_{\rm bol}$/$L_{\odot}$) $=-3.17^{+0.9}_{-1.0}$ dex and a mass of $7.1^{+1.1}_{-1.0}$ $M_{\mathrm{Jup}}$ for 2MASS J0437+2331, consistent with the masses of our discoveries and the 4–7 $M_{\mathrm{Jup}}$ estimate of Luhman et al. (2009).

With no evidence of companionship to any nearby star or of unresolved binarity (Section 4.5), our discoveries are among the lowest mass free-floating substellar objects ever discovered, similar to 2MASS J0437+2331, the young $\beta$ Pictoris Moving Group L dwarf PSO J318.5338$-$22.8603 ($8.3\pm 0.5$ $M_{\mathrm{Jup}}$; Liu et al., 2013; Allers et al., 2016), the young TW Hydrae Associaton L dwarfs 2MASS J11193254$-$1137466 (4.3–7.6 $M_{\mathrm{Jup}}$; Kellogg et al., 2016) and WISEA J114724.10$-$204021.3 (5–13 $M_{\mathrm{Jup}}$; Schneider et al., 2016), the AB Doradus Moving Group T dwarf SDSS J111010.01+011613.1 ($\approx$10–12 $M_{\mathrm{Jup}}$; Gagné et al., 2015a), and the field Y dwarf WISE J085510.83$-$071442.5 (3–10 $M_{\mathrm{Jup}}$; Luhman, 2014; Leggett et al., 2015). They provide significant evidence that free-floating planetary-mass objects can form as part of normal star-formation processes.

For comparison, we also converted spectral types into effective temperatures, and then used the DUSTY models and our $T_{\rm eff}$ values to estimate masses. No empirically calibrated conversion of spectral type to $T_{\rm eff}$ has been determined for very young L dwarfs, so we extrapolated the scale of Luhman et al. (2003, 2008), arriving at 2000 K for the L1 dwarf and 1800 K for the L2 dwarf. We assumed an error of $\pm 100$ K for each object. With this distance-independent approach, we estimate masses of $7.1^{+1.4}_{-1.1}$ $M_{\mathrm{Jup}}$ for PSO J060.3+25 and $5.2^{+0.9}_{-0.8}$ $M_{\mathrm{Jup}}$ for PSO J077.1+24. If instead we use the field dwarf (i.e., not young) SpT-to-$T_{\rm eff}$ conversion of Stephens et al. (2009, Eq. 3), we find temperatures of $2112\pm 100$ K for the L1 dwarf and $1971\pm 100$ K for the L2 dwarf, resulting in masses of $8.6^{+2.0}_{-1.6}$ $M_{\mathrm{Jup}}$ for PSO J060.3+25 and $6.8^{+1.3}_{-1.1}$ $M_{\mathrm{Jup}}$ for PSO J077.1+24.

We note also that a recent study by Daemgen et al. (2015) identified evidence suggesting an older sub-population of Taurus with an age of $\approx$20 Myr. If confirmed, and our discoveries are in fact members of this sub-population, the older age would lead to a factor of $\approx$3 increase in our mass estimates.

5.3 Evidence for Circumstellar Disks

Many low-mass stellar members of Taurus are known to host circumstellar disks (e.g., Andrews et al., 2013; Esplin et al., 2014). We searched for evidence of elevated fluxes at mid-infrared wavelengths that would indicate the presence of circumstellar disks around our Taurus discoveries. We fit the BT-Settl grid of synthetic spectra from Baraffe et al. (2015) to our 0.85–2.45 $\mu$m prism spectra of PSO J060.3+25, PSO J077.1+24, and 2MASS J0437+2331 following the method of Bowler et al. (2011). In summary, the models are smoothed to the resolving power of the data and resampled to the same wavelength grid. The 1.60–1.65 $\mu$m and 1.8–1.95 $\mu$m regions are ignored to avoid incomplete methane line lists and low S/N portions of our spectra. The spectra are flux-calibrated to each object’s $J$-band photometry. A scale factor, equal to the square of the object’s radius divided by its distance, is calculated by minimizing the $\chi^{2}$ value following Cushing et al. (2008). Assuming a distance of $145\pm 15$ pc to Taurus allows us to simultaneously infer the radius at each grid point.

The results of the fits are shown in Figure 16. The best-fit synthetic spectra ($T_{\mathrm{eff}}$=1800 K, log $g$=5.5 dex [cgs] for both of our discoveries and $T_{\mathrm{eff}}$=1600 K, log $g$=5.5 dex for 2MASS J0437+2331) offer relatively poor fits to the data, largely failing to reproduce the observed $H$ and $K$-band spectral shapes. The best-fit models have field-age surface gravities, contrary to the vl-g classes indicated by the observed spectra, so we include synthetic spectra with the same $T_{\rm eff}$ as the best-fit models but with log $g$=3.5 dex (roughly the gravity expected for vl-g objects) in Figure 16 for comparison. The inferred radii for our discoveries are all $\geq$2 $R_{\mathrm{Jup}}$, consistent with expectations for very young objects still undergoing gravitational contraction (e.g., Burrows et al., 1997). Synthetic photometry of the best fitting models is generally consistent with the observed photometry from Pan-STARRS, UKIRT, and the $W1$ (3.4 $\mu$m) filter from WISE, but is significantly lower for the $W2$ (4.6 $\mu$m) channel at the 7–9$\sigma$ level. This may represent evidence of thermal excess from a disk around both objects, but we note that the observed $W2$ photometry is much more consistent with the log $g$=3.5 dex model spectra. The discrepancy at $W2$ is therefore likely to be a consequence of the poor model fits, or possibly a result of a systematic error in the model atmospheres, for example from imperfect opacity sources.

The Taurus objects have photometric upper limits in WISE for the $W3$ (12 $\mu$m) and $W4$ (22 $\mu$m) bands, with one exception. PSO J060.3+25 has a reported $2.6\sigma$ detection in $W4$ that is significantly brighter than the synthetic model photometry. We visually inspected the WISE images of this object and could not confirm that the $W4$ detection is distinct from noise. A clear excess at 22 $\mu$m would indicate the presence of a disk, but this marginal detection requires confirmation by deeper imaging.

We note that Luhman et al. (2009) also found no excess at mid-IR wavelengths in Spitzer photometry that would indicate the presence of a disk around 2MASS J0437+2331.

6 Scorpius-Centaurus Discoveries

The Scorpius-Centaurus Association is the nearest OB association to the Sun. We have discovered six new late-M and early-L members of Sco-Cen. Using the boundaries defined by de Zeeuw et al. (1999), PSO J237.1$-$23 (M7) and PSO J239.7$-$23 (L0) lie within the Upper Scorpius subgroup (hereinafter Upper Sco), while PSO J228.6$-$29 (L1), PSO J229.2$-$26 (L0), PSO J231.7$-$26 (L0), and PSO J231.8$-$29 (L0) sit on the northern outskirts of the Upper Centaurus Lupus subgroup (hereinafter UCL). Figure 2 shows the sky locations of our discoveries. Upper Sco and UCL are among the reddened regions on the sky identified by Cruz et al. (2003) that we excluded from our search, and our discoveries lie just outside the excluded areas.

Like Taurus, the Upper Sco region has been searched multiple times for brown dwarfs. Unlike in Taurus, more than a dozen L0–L2 dwarfs have previously been confirmed in Upper Sco, in particular by Lodieu et al. (2008) using early release data from the UKIDSS Galactic Clusters Survey (GCS). Our discoveries were not found by that search, nor by Lodieu et al. (2006, 2011), because of incomplete coverage of the region by the early version of GCS. They also remained undetected by searches using optical data as part of the selection process (Martín et al., 2004; Slesnick et al., 2006, 2008). The objects were detected in GCS Data Release 8 and later versions, but were only observed in $H$ and $K$ bands, and so were not included in the search of Dawson et al. (2011, 2013) who required $Z$ and $J$ photometry in their selection process. PSO J237.1$-$23 was identified as a candidate member of Upper Sco by Lodieu (2013) as part of their “$HK$-only sample”, but PSO J239.7$-$23 is too faint to qualify for this sample. Searches for young ultracool dwarfs have not focused on UCL, so our four discoveries lie outside regions targeted by previous efforts.

In this Section we follow the structure of Section 5, presenting the evidence that our discoveries are members of Sco-Cen (Section 6.1), estimating their masses (Section 6.2), and comparing their SEDs to model atmospheres to look for evidence of circumstellar disks (Section 6.3).

6.1 Evidence for Membership

6.1.1 Youth

Four of our six Sco-Cen discoveries have vl-g gravity classes, suggesting ages $\lesssim 30$ Myr. The other two, PSO J228.6$-$29 and PSO J229.2$-$26, have lower-S/N spectra that do not permit robust calculation of the AL13 gravity-sensitive indices but nevertheless show clear visual indications of low gravity (Section 4.3).

6.1.2 Photometry

Figure 17 demonstrates the consistency of our six discoveries’ photometry with that of known Upper Sco members from Luhman & Mamajek (2012, hereinafter LM12), Dawson et al. (2014), and Rizzuto et al. (2015), and with photometric/astrometric candidates from unreddened regions in the UKIDSS GCS Data Release 10 (Lodieu, 2013, their Table A1). The LM12 catalog contains a handful of objects that are reddened by interstellar extinction, and we include reddening vectors (Section 5.1.2) scaled to an extinction of $A_{V}=2$ mag in Figure 17. Most of our discoveries lie along the unreddened cluster sequence of the Upper Sco $J$ vs. $J-K$ and $y_{\rm P1}$ vs. $y_{\rm P1}-W1$ color-magnitude diagrams, fully consistent with the reddening-free sample of Lodieu (2013). PSO J237.1$-$23 is redder than the cluster sequence in $y_{\rm P1}-W1$, likely evidence for a circumstellar disk (Section 6.3). As with PSO J060.3+25 and PSO J077.1+24 in Taurus, the Sco-Cen objects have $(J-K_{S})_{\rm 2MASS}$ colors that are consistent with field L0–L1 dwarfs but have $W1-W2$ colors that are 1–3$\sigma$ redder than the field population (Gizis et al., 2012; Faherty et al., 2013).

6.1.3 Proper Motion

We compare the proper motions of our Sco-Cen discoveries to the proper motions of several literature sources in Figure 18. Pecaut et al. (2012) calculated proper motions for F-type stars in Upper Sco and UCL, and Lodieu (2013) calculated proper motions for a list of unreddened photometric/astrometric members and candidates in UKIDSS GCS. LM12 do not quote proper motions for their catalog of Upper Sco members, so we obtained PS1 Processing Version 3.2 (PV3.2) proper motions for these objects as well as those from Dawson et al. (2014) and Rizzuto et al. (2015). From these PS1 proper motions we calculated a weighted mean proper motion for known Upper Sco members of ($\mu_{\alpha}{\rm cos}\,\delta=-8.5\pm 0.1,\ \mu_{\delta}=-19.6\pm 0.1$ mas yr*-1*), with a weighted rms of 4.3 mas yr*-1* in R.A. and 5.6 mas yr*-1* in Dec. Our complete list of PS1 proper motions for objects from this combined catalog that are not saturated in PS1 is described in Appendix B. Figure 18 demonstrates the consistency of the proper motions of our discoveries with all literature sources.

6.1.4 Likelihood of Field Contamination

We estimated the likelihood that any of our Sco-Cen discoveries could be interloping foreground or background field objects, using the same approach as in Section 5.1.4. Upper Sco and UCL are distinct regions with different ages and bulk proper motions (Pecaut et al., 2012), so we considered them separately.

We defined the boundaries of Upper Sco to be $343^{\circ}\leq l\leq 360^{\circ}$ and $10^{\circ}\leq b\leq 30^{\circ}$ (Figure 2). The portion of this region surveyed by PS1 (i.e., north of $\delta=-30^{\circ}$) covers 281.0 deg2. We found that $28.42\pm 0.11$% of a synthetic population (Besançon Galactic model) of field M dwarfs in the direction of Upper Sco will have proper motions within $3\sigma$ of the mean Upper Sco $\mu_{\alpha}{\rm cos}\,\delta$ and $\mu_{\delta}$ (Section 6.1.3). We estimate that our search would find $(3.99\pm 0.02)\times 10^{-2}$ field vl-g dwarfs within the projected boundaries of Upper Sco having proper motions consistent with Upper Sco membership. We find a probability of 96.1% that both PSO J237.1$-$23 and PSO J239.7$-$23 are members of Upper Sco.

For UCL, we used the data for F stars from Pecaut et al. (2012) to calculate a weighted mean proper motion of ($\mu_{\alpha}{\rm cos}\,\delta=-23.0\pm 0.1,\ \mu_{\delta}=-23.8\pm 0.1$ mas yr*-1*) with a weighted rms of 5.7 mas yr*-1* in R.A. and 4.9 mas yr*-1* in Dec. Only 0.51% of our synthetic M dwarf population have proper motions consistent within $3\sigma$ with the mean UCL motion. PSO J228.6$-$29, PSO J229.2$-$26, PSO J231.7$-$26, and PSO J231.8$-$29 all have proper motions consistent with UCL, so the probability that any of them is a field interloper is negligible based on proper motions alone.

6.1.5 Membership in Scorpius-Centaurus

All six of our discoveries in the direction of Sco-Cen have vl-g gravity classifications or clear spectral indications of low gravity. Their positions in color-magnitude diagrams, proper motions, and very low probability of contamination by field objects confirm that they are members of Sco-Cen.

6.2 Luminosities and Masses

We calculated bolometric luminosities and estimated the masses of our Sco-Cen discoveries using the method described in Section 5.2. We adopted a distance of $145\pm 15$ pc (de Zeeuw et al., 1999; Preibisch & Zinnecker, 1999) and an age of $11\pm 2$ Myr (Pecaut et al., 2012) for Upper Sco. The mean distance to UCL is $140\pm 2$ pc (de Zeeuw et al., 1999). de Bruijne (1999) found a substantial depth of $50\pm 20$ pc for UCL, but all four of our UCL discoveries have photometry consistent with members of Upper Sco (Figure 17), so we used the same distance uncertainty as Upper Sco and adopted a UCL distance of $140\pm 15$ pc, along with an age of $16\pm 1$ Myr (Pecaut et al., 2012). We used normal distributions for the age and distance uncertainties in our Monte Carlo simulations. Our luminosity and mass estimates for our Sco-Cen discoveries are listed in Table 7. The masses span $15-36$ $M_{\mathrm{Jup}}$, near the low-mass end of the brown dwarf regime and comparable to the lowest mass members known in these regions (Lodieu et al., 2011; Aller et al., 2013).

6.3 A Candidate Circumstellar Disk

At ages $\gtrsim$10 Myr, our discoveries in Sco-Cen are less likely to harbor circumstellar disks than are the $\approx$1–2 Myr Taurus objects (e.g., Mathews et al., 2012). However, LM12 have demonstrated that $\approx$25% of M5–L0 objects in Upper Sco have disks detectable at mid-infrared wavelengths. They developed color vs. spectral type relationships to identify stars and brown dwarfs with candidate circumstellar disks, using colors including $K_{S}-W2$, $K_{S}-W3$, and $K_{S}-W4$. Our L dwarf discoveries were not detected in $W3$ or $W4$, and LM12 caution that the $K_{S}-W2$ colors do not reliably discriminate between excess flux from a disk and rapidly reddening photospheres beyond spectral type M8.5. We nevertheless checked the $K_{S}-W2$ colors of our L dwarfs (including the Taurus discoveries), and none are redder than the typical colors of Upper Sco M9–L1 dwarfs (LM12), so we cannot identify any candidate disk hosts among these objects.

PSO J237.1$-$23, the lone M dwarf (M7) among our discoveries, has significantly mid-infrared redder colors than those of late-M dwarfs lacking disks, strongly suggesting the presence of a circumstellar disk. The $K_{S}-W2$ and $K_{S}-W3$ colors both satisfy the LM12 criteria by $\gtrsim 5\sigma$. PSO J237.1$-$23 also has a marginal $W4$ detection at $8.75\pm 0.45$ mag, which if real would give the object a $K_{S}-W4$ color over 3.5 mag redder than the LM12 limit for disk-hosting M7 dwarfs. We therefore consider PSO J237.1$-$23 to be a clear candidate circumstellar disk host, joining over a dozen other candidates in Upper Sco with spectral types M7 or later (LM12).

We also looked for evidence of excess mid-infrared fluxes using the method described in Section 5.3, fitting the BT-Settl model spectra (Baraffe et al., 2015) to the prism spectra of our Sco-Cen discoveries. The results are shown in Figure 21. As with our Taurus discoveries, the best-fit synthetic spectra for our Sco-Cen objects have field-age gravities inconsistent with the low-gravity features in the observed spectra, fit the emprical $JHK$-band morphologies fairly poorly, and have radii $\geq 2$ $R_{\mathrm{Jup}}$ (consistent with models). Synthetic photometry from the models is generally consistent with the observed photometry. The significantly lower synthetic flux at $W2$ seen in our Taurus discoveries (Figure 16) is present here for two of the six Sco-Cen objects, although again this is likely to be an consequence of poor model fits. Our disk candidate, PSO J237.1$-$23, does show an excess in observed flux relative to the best-fit and low-gravity models at all four WISE bands, although the model synthetic fluxes are higher than observations in the optical bands, indicating that the fit has failed to correctly capture the observed SED.

7 Summary

As part of a wide-field search for L/T transition dwarfs using the Pan-STARRS1 and WISE surveys, we have serendipitously discovered eight young late-M and early-L dwarfs in the nearby Taurus and Scorpius-Centaurus star-forming regions. PSO J060.3+25 (spectral type L1) and PSO J077.1+24 (L2) are members of Taurus. Both have vl-g gravity classifications indicating ages $\lesssim 30$ Myr, photometry consistent with previously known ultracool members of Taurus, and proper motions consistent with the Taurus population. We estimate the probability that neither object is a foreground (or background) field dwarf to be 97%. The spectral and photometric properties of our two discoveries are also similar to the only previously known free-floating L dwarf in Taurus, 2MASS J0437+2331 (Luhman et al., 2009). At the young ($\approx$1–2 Myr) age of Taurus, PSO J060.3+25 and PSO J077.1+24 have estimated masses of $\approx$6 $M_{\mathrm{Jup}}$, and they join 2MASS J0437+2331 ($\approx$7 $M_{\mathrm{Jup}}$, spectral type L1) as the lowest-mass isolated known members of Taurus. PSO J077.1+24 is additionally the coolest known free-floating object discovered in Taurus to date.

PSO J060.3+25 was previously identified by Sarro et al. (2014) and Bouy et al. (2015) as DANCe J040116.80+255752.2, a likely ultracool member of the Pleiades (age $\approx 125$ Myr) based on its photometry and astrometry. Our spectrum confirms the late spectral type of PSO J060.3+25, but its vl-g gravity class implies an age ($\lesssim$30 Myr) consistent with the much younger Taurus star-forming region, and its near-infrared photometry is more consistent with other VLM members of Taurus.

The other six M7–L1 dwarf discoveries lie on the outskirts of the Upper Scorpius and Upper Centaurus-Lupus associations (ages $\approx 11$–16 Myr), with estimated masses $\approx 15-36$ $M_{\mathrm{Jup}}$. Four have vl-g gravity classifications; our spectra for the other two did not have enough S/N for confident gravity classification, but visual inspection finds they have clear spectral signatures of low gravity. The photometry and proper motions of all six objects are fully consistent with membership in Scorpius-Centaurus. Lodieu (2013) previously identified PSO J237.1$-$23 as an astrometric and photometric candidate member of Upper Sco, which we confirm with our independent discovery and spectroscopy.

We found no spectral indications that any of our discoveries have unresolved companions, nor did we find any comoving objects nearby. The Taurus objects represent strong evidence that normal star formation processes can produce isolated objects with masses as low as $\approx$6 $M_{\mathrm{Jup}}$.

The $J-K$ colors of all seven young L dwarf discoveries are consistent with those of older field L0–L2 dwarfs. This contrasts with the redder $J-K$ colors of some previously discovered young early-L dwarfs, and confirms that near-infrared redness is not a universal feature of very young (1–2 Myr) brown dwarfs. Our discoveries do have $W1-W2$ colors that are redder than those of early-L field objects, which we identify as the primary reason we discovered these objects during a search for L/T transition dwarfs.

We fit BT-Settl synthetic spectra (Baraffe et al., 2015) to our observed spectra and found that the best-fit models reproduce our spectra relatively poorly in the near-infrared. At 4.6 $\mu$m (WISE $W2$ band), all three Taurus objects and two Sco-Cen objects show a significant observed excess flux over the model predictions. These elevated fluxes are suggestive of the presence of a circumstellar disk but may also indicate a source of systematic error in the model atmospheres. The M7 dwarf PSO J237.1$-$23 shows strong excess fluxes at $W2$, $W3$, and possibly at $W4$, making it a likely host for a circumstellar disk.

Our discovery of these eight young brown dwarfs in well-searched regions of the sky, while looking for older objects with cooler spectral types, has a few important implications:

• •

The combination of PS1 and WISE photometry is a powerful tool for identifying young ultracool dwarfs (see also Paper II).

• •

Unusually red $W1-W2$ colors in late-M and early-L dwarfs may indicate the objects are young (Figure 3), providing leverage for searches for young M/L dwarfs.

• •

There are likely to be more young planetary-mass brown dwarfs that could be discovered with focused searches in even well-studied star-forming regions.

We thank the anonymous referee for a helpful critique that improved the quality of this paper. We thank Katelyn Allers, Brian Cabreira, Dave Griep, Tony Matulonis, and Eric Volqardsen for assisting with IRTF observations. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. This project makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of the 2MASS data products; the UKIDSS data products; the VISTA data products; NASA’s Astrophysical Data System; the SIMBAD and Vizier databases operated at CDS, Strasbourg, France, and the Database of Ultracool Parallaxes, maintained by Trent Dupuy at https://www.cfa.harvard.edu/$\sim$tdupuy/plx. WMJB received support from NSF grant AST09-09222. WMBJ, MCL, and EAM received support from NSF grant AST-1313455. Finally, the authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always held within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.

Facilities: IRTF (SpeX), PS1, UKIRT (WFCAM)

Appendix A Proper Motions of Known Low-Mass Taurus Members

A.1 Pan-STARRS1 Proper Motions

We compiled a catalog of proper motions for low-mass members of Taurus using the Pan-STARRS1 $3\pi$ (PS1) Survey, Processing Version 3.2 (PV3.2). Photometry and positions from PV3.2 were publically released as part of PS1 DR1 (K. Chambers et al., 2017, in prep), with proper motions and parallaxes planned for a future PS1 release. PS1 astrometry includes Pan-STARRS1 observations from November 2009 to March 2014, as well as detections from 2MASS (October 1997 to November 2000) and Gaia DR1 (Epoch 2015.0; Gaia Collaboration et al., 2016; Lindegren et al., 2016) lying within 1” of the mean PS1 position. PS1 astrometry, including proper motions, is calibrated to the Gaia DR1 reference frame.

A full description of the proper motion calculations can be found in E. Magnier et al. (2017, in prep). Briefly, all PS1, 2MASS, and Gaia detections for an object were fit simultaneously for position, parallax, and proper motion using iteratively-reweighted least squares regression with outlier clipping. Errors were estimated for each object using a bootstrapping approach, drawing random samples in a Monte Carlo fashion (allowing duplicates) from the set of detections not rejected in the astrometric fit.

A.2 Catalog

To create our catalog, we began with the list of 414 Taurus members from Esplin et al. (2014). Using the 2MASS positions (or WISE positions for the seven objects with no 2MASS detection), we cross-matched this list with the PS1 database using a $3^{\prime\prime}$ matching radius, and found 363 matches with a proper motion measured by PS1. We supplemented these matches with our two Taurus discoveries presented in the paper. We verified that none of the PS1 sources were identified as quasars, transients, periodic variables, or solar system objects in the PS1 database, and we excluded any objects with poor PSF fits ($\tt psf\_qf<0.85$). To avoid saturation in PS1 we also excluded objects having $i_{\rm P1}<14.5$ mag or $y_{\rm P1}<12.5$ mag (corresponding roughly to a spectral type of M3–M4). This left us with 187 members of Taurus having proper motions measured by PS1. Almost every object in the catalog of Esplin et al. (2014) was detected by 2MASS, so the PS1 proper motions have time baselines of $\approx$14–17 years. Our catalog includes 27 objects with no previously published proper motion and 93 measurements that improve on the best available literature values drawn from NOMAD (Zacharias et al., 2005), PPMXL (Roeser et al., 2010), SDSS DR9 (Ahn et al., 2012), UCAC4 (Zacharias et al., 2013), UKIDSS GCS DR9 (Lawrence et al., 2013), URAT1 (Finch & Zacharias, 2016), USNO-B (Monet et al., 2003), and Riaz et al. (2013). It is the largest catalog to date for proper motions of low-mass (spectral types $\gtrsim$ M3) members of Taurus.

We list our proper motions in Table 8, along with the $i_{\rm P1}$ and $y_{\rm P1}$ photometry, the number of epochs used, the reduced $\chi^{2}$, and the time baseline for each proper motion fit. We adopt a photometric precision floor of 0.01 mag for the PS1 photometry, following the analysis of Schlafly et al. (2012). The errors reported in the PS1 database are formal errors that do not include systematics, and are often smaller than 0.01 mag. We do not report photometry with errors larger than 0.2 mag. Figure 22 shows the proper motion errors as a function of the $y_{\rm P1}$ magnitude of each source, and indicates that most of the errors are $\lesssim$5 mas yr*-1*.

In Figure 23 we plot the reduced $\chi^{2}$ for the proper motion fits as a function of $y_{\rm P1}$. Most of our proper motion fits have $\chi^{2}_{\nu}>1$, suggesting that the astrometric uncertainties of the individual PS1 epochs are small compared to the scatter in R.A. and Dec. of the epochs. The proper motion errors may therefore be underestimated (by a factor of $\approx$2).

To assess the reliability of our proper motions, we calculated proper motions and $\chi^{2}_{\nu}$ for objects in a 0.5 deg2 patch of sky near Taurus ($80^{\circ}<\alpha<81^{\circ}$, $5.5^{\circ}<\delta<6.0^{\circ}$), in which more than 97% of objects have proper motions less than 50 mas yr*-1*. We used all 8,962 objects in this patch meeting the same criteria as our Taurus catalog and also having $y_{\rm P1}<19.75$ mag to match the faintness limit of our Taurus catalog. Because the proper motions of this sample are small, the rms of the proper motions gives us an estimate of the quality of the measurements. Figure 24 shows that proper motions measurements with $0.3<\chi^{2}_{\nu}<40$ had rms $\approx 5-15$ mas yr*-1*, while proper motions with larger or smaller $\chi^{2}_{\nu}$ had significantly greater spread. We therefore adopted these $\chi^{2}_{\nu}$ values as the limits between which we regard our proper motions as reliable measurements. Table 8 separates our Taurus proper motions into those we regard as reliable (all but 5 of the objects) and unreliable. We report all of our proper motions for completeness, but when $\chi^{2}_{\nu}\leq 0.3$ or $\chi^{2}_{\nu}\geq 40$ the proper motions should be treated with caution.

Using the reliable proper motions and inverse variance weighting, we calculate a weighted mean proper motion for Taurus of ($\mu_{\alpha}{\rm cos}\,\delta=7.6\pm 0.2,\ \mu_{\delta}=-17.4\pm 0.2$ mas yr*-1*), with a weighted rms of 4.9 mas yr*-1* in R.A. and 6.4 mas yr*-1* in Dec. We compare this to the catalog of brighter Taurus members compiled by Ducourant et al. (2005, hereinafter D05), whose proper motions were similarly calculated using optical and 2MASS data and whose time baselines range from 10 to more than 100 years. Using the proper motions from the full D05 Taurus catalog, we calculate a weighted mean proper motion of ($7.9\pm 1.1,-20.5\pm 1.0$ mas yr*-1*). We note a $\approx$3 mas yr*-1* discrepancy with the mean proper motion for our Taurus list, which is likely due to differences in the astrometric reference frames used for the two samples. The Pan-STARRS1 PV3.2 astrometry is tied to the Gaia DR1 reference frame, while the D05 proper motions use data from many sources with different astrometric reference frames. Only ten Taurus objects in the D05 catalog are not saturated in PS1 and have reliable proper motions, preventing a robust object-by-object comparison of the PS1 proper motions with those from D05. The ten shared objects mostly have proper motions from the two catalogs that are consistent within errors.

Appendix B Proper Motions of Known Upper Scorpius Members

We calculated proper motions for 482 members of Upper Sco from the lists of Luhman & Mamajek (2012), Dawson et al. (2014), Rizzuto et al. (2015), and this paper, that met the same selection criteria we used for Taurus members in Appendix A.2. Our catalog comprises the largest set of proper motions for low-mass (spectral types $\gtrsim$ M3) members of Upper Sco published to date. It includes 40 objects for which no proper motion has previously been published, and 266 that improve on existing literature values, which were drawn from NOMAD (Zacharias et al., 2005), PPMXL (Roeser et al., 2010), SDSS DR9 (Ahn et al., 2012), UCAC4 (Zacharias et al., 2013), UKIDSS GCS DR9 (Lawrence et al., 2013), USNO-B (Monet et al., 2003), Dawson et al. (2011), Lodieu et al. (2007, 2013), and Lodieu (2013). We list our proper motions, number of epochs used, reduced $\chi^{2}$, and time baseline for each proper motion fit in Table 9.

Figure 25 shows the distribution of errors for our Upper Sco proper motions as a function of the $y_{\rm P1}$ magnitude of each source. As with our Taurus sample (Appendix A), most of the errors are $\lesssim$5 mas yr*-1*. Figure 26 shows the reduced $\chi^{2}$ for the proper motion fits as a function of $y_{\rm P1}$. Again like Taurus, most of our proper motion fits have $\chi^{2}_{\nu}>1$, implying that the proper motion errors may be underestimated (by a factor of $\approx$2).

Using the reliable fits from our Upper Sco list, we calculate a weighted mean proper motion for Upper Sco of ($\mu_{\alpha}{\rm cos}\,\delta=-8.5\pm 0.1,\ \mu_{\delta}=-19.6\pm 0.1$ mas yr*-1*), with a weighted rms of 4.3 mas yr*-1* in R.A. and 5.6 mas yr*-1* in Dec. We compare our proper motions to those listed in Pecaut et al. (2012, hereinafter P12) for F stars in Upper Sco, which were determined by Hipparcos (van Leeuwen, 2007) or Tycho-2 (Høg et al., 2000). These stars are all saturated in PS1, so we are not able to measure accurate proper motions using PS1 data and compare them directly to the P12 proper motions. For the P12 Upper Sco catalog, we calculate a weighted mean proper motion of ($-11.5\pm 0.3,-25.0\pm 0.2$ mas yr*-1*). We also cross-matched the P12 objects with the UCAC4 catalog (Zacharias et al., 2013), and using those proper motions obtained a weighted mean of ($-9.9\pm 0.2,-21.6\pm 0.2$ mas yr*-1*). The source of the discrepancy between these two mean proper motion vectors for Upper Sco and our determination from PS1 PV3.2 is unclear, and may indicate a difference in the bulk motions of higher mass stars (from P12) and low mass stars and brown dwarfs (our catalog) in Upper Sco.

Appendix C A New SpeX Prism Spectrum for the L0 Field Standard

We identified a wavelength offset in the spectrum of 2MASS J03454316+2540233 (hereinafter 2MASS J0345+2540) publically available from the SpeX Prism Library555http://pono.ucsd.edu/$\sim$adam/browndwarfs/spexprism. 2MASS J0345+2540 is the field L0 spectral standard for both optical (Kirkpatrick et al., 1999) and near-infrared (Kirkpatrick et al., 2010) wavelengths. The spectrum, first published in Burgasser & McElwain (2006, hereinafter BM06), is shifted $\approx$0.01 $\mu$m toward longer wavelengths (Figure 27). The offset is insignificant when visually compared to other spectra over the full 0.8–2.5 $\mu$m range of SpeX prism spectra, but is large enough to impact calculations of the Allers & Liu (2013a) gravity-sensitive spectral indices that use $\approx$0.02 $\mu$m-wide $J$-band absorption features (Section 4.3). The offset is equivalent to a velocity of $\approx$2,400 km s*-1*, two orders of magnitude larger than the radial velocities typical of nearby late-M and early-L dwarfs (Burgasser et al., 2015), so the offset is almost certainly due to a wavelength calibration error.

To obtain a spectrum for 2MASS J0345+2540 with an accurate wavelength calibration, we observed the object on 2016 February 03 UT with IRTF/SpeX in prism mode, using the 0.5” slit. Conditions were clear. Observations were made at an airmass of 1.01 and comprised six exposures of 120 sec using an ABBA nodding pattern. Immediately after we observed the A0V star HD 19600 for telluric calibration. We reduced the 2MASS J0345+2540 spectrum using Spextool v. 4.0 in standard fashion. The final spectrum has a mean S/N of 115 in $J$ band (1.20–1.31 $\mu$m). Figure 27 shows our spectrum compared with the BM06 spectrum for 2MASS J0345+2540 and the SpeX Prism Library spectrum for the L0 dwarf 2MASS J02281101+2537380 (Burgasser et al., 2008). The redward offset on the BM06 spectrum is evident in the $J$-band absorption features. We therefore used our new spectrum for 2MASS J0345+2540 in our analysis (Sections 4.2 and 4.3).