The Elusive Majority of Young Moving Groups. I. Young Binaries and Lithium-Rich Stars in the Solar Neighborhood

TL;DR

This study systematically identifies and characterizes young, active low-mass stars within 100 parsecs, revealing new members of known young moving groups and discovering numerous close binaries for future dynamical studies.

Contribution

It provides a comprehensive all-sky survey of young, active low-mass stars near the Sun, including new members of young moving groups and a catalog of close binaries for mass measurements.

Findings

58 stars with strong lithium indicating ages 10-200 Myr

Over 600 stars identified as potential young stars

More than 200 new close binaries discovered

Abstract

Young stars in the solar neighborhood serve as nearby probes of stellar evolution and represent promising targets to directly image self-luminous giant planets. We have carried out an all-sky search for late-type ($\approx$K7$-$M5) stars within 100 pc selected primarily on the basis of activity indicators from $GALEX$ and $ROSAT$. Approximately two thousand active and potentially young stars are identified, over 600 of which we have followed up with low-resolution optical spectroscopy and over 1000 with diffraction-limited imaging using Robo-AO at the Palomar 1.5-m telescope. Strong lithium is present in 58 stars, implying ages spanning $\approx$10$-$200 Myr. Most of these lithium-rich stars are new or previously known members of young moving groups including TWA, $\beta$ Pic, Tuc-Hor, Carina, Columba, Argus, AB Dor, Upper Centaurus Lupus, and Lower Centaurus Crux; the rest appear to be young low-mass stars without connections to established kinematic groups. Over 200 close binaries are identified down to 0.2$''$ $-$ the vast majority of which are new $-$ and will be valuable for dynamical mass measurements of young stars with continued orbit monitoring in the future.

Figures

Tables

Table 1. Table 1: Spectroscopic Observations

2MASS	Date	Telescope/		Res.	Exp.	H$\alpha$ EW	Li EW	Na EW	TiO5	Hammer	Vis.
Name	(UT)	Instrument	Grating	Power	(s)	(Å)aaNegative values indicate emission. Uncertainties are estimated to be 10% of the quoted values.	(Å)aaNegative values indicate emission. Uncertainties are estimated to be 10% of the quoted values.	(Å)aaNegative values indicate emission. Uncertainties are estimated to be 10% of the quoted values.	Index	SpTbbSpectral types from Hammer have been shown to have a systematic offset of about one spectral subclass for cool stars. Uncertainties are $\pm$1 subclass. Our visual spectral types are more robust and have uncertainties of $\pm$0.5 subclasses.	SpTbbSpectral types from Hammer have been shown to have a systematic offset of about one spectral subclass for cool stars. Uncertainties are $\pm$1 subclass. Our visual spectral types are more robust and have uncertainties of $\pm$0.5 subclasses.
J00022714–4601439	2014–06–27	SOAR/Goodman	SYZY400	1800	300	–1.0	$\cdots$	2.2	0.65	M1	M2
J00104302–2039067	2013–12–06	SOAR/Goodman	SYZY400	1800	120	–3.5	$\cdots$	3.1	0.48	M3	M3
J00104302–2039067	2013–12–06	SOAR/Goodman	RALC1200	5900	240	–3.2	$\cdots$	$\cdots$	0.49	M3	M3
J00114643–1139553	2013–12–06	SOAR/Goodman	SYZY400	1800	150	0.3	$\cdots$	3.6	0.75	M0	M0
J00120761–1550327	2013–12–31	Mayall/RC-Spec	BL420	2600	30	–3.2	$\cdots$	1.1	0.93	K:	G/K:
J00141709–6139237	2013–12–05	SOAR/Goodman	SYZY400	1800	300	–1.7	$\cdots$	3.1	0.52	M2	M3
J00141709–6139237	2013–12–05	SOAR/Goodman	RALC1200	5900	500	–1.8	$\cdots$	$\cdots$	0.55	M2	M2
J00144767–6003477	2014–06–25	SOAR/Goodman	SYZY400	1800	300	–5.1	$\cdots$	3.4	0.39	M4	M4
J00151561+0247373	2014–06–26	SOAR/Goodman	SYZY400	1800	240	0.4	$\cdots$	1.3	0.88	K5	K7
J00153670–2946003	2013–12–05	SOAR/Goodman	SYZY400	1800	300	–9.2	$\cdots$	3.5	0.34	M4	M5
$\cdots$

Table 2. Table 2: Robo-AO Observations

2MASS	UT Date		Exp.	FWHM
ID	(Y-M-D)	Filter	(s)	(′′)
J00055520+4129289	2014-08-24	SDSS $i^{\prime }$	60	0.28
J00074264+6022543	2013-10-25	LP600	120	0.26
J00074264+6022543	2014-11-08	SDSS $i^{\prime }$	60	0.16
J00080642+4757025	2013-10-25	SDSS $i^{\prime }$	120	0.20
J00085391+2050252	2013-10-24	SDSS $i^{\prime }$	120	0.25
J00085391+2050252	2014-11-06	SDSS $i^{\prime }$	60	0.13
J00114643–1139553	2014-08-28	SDSS $i^{\prime }$	60	0.26
J00120761–1550327	2014-08-29	SDSS $i^{\prime }$	60	0.35
J00133841+5245050	2014-08-26	SDSS $i^{\prime }$	60	0.21
J00133841+5245050	2014-11-06	SDSS $i^{\prime }$	60	0.13
$\cdots$

Table 3. Table 3: Properties of Lithium-Rich Stars

2MASS		SpT	RV	RV	${\mu }_{\alpha }\cos \left(\delta \right)$aaProper motions and parallactic distance from $Gaia$ DR2, unless otherwise noted.	${\mu }_{\delta }$aaProper motions and parallactic distance from $Gaia$ DR2, unless otherwise noted.	DistanceaaProper motions and parallactic distance from $Gaia$ DR2, unless otherwise noted.	BANYAN $\Sigma$	Literature	Adopted	YMG
Name	SpT	Ref.	(km/s)	Ref.	(mas yr-1)	(mas yr-1)	(pc)	Best Hyp.	YMG	YMG	Ref.
J00233468+2014282	M0	TW	–2.2 $\pm$ 0.6	Sh17	65.97 $\pm$ 0.10	–37.38 $\pm$ 0.11	62.89 $\pm$ 0.25	Field	$\beta$ Pic	$\beta$ Pic	Le09, Ma13, Ma14a, Sh17
J00345120–6154583	K7	TW	11 $\pm$ 5	Kr14	88.69 $\pm$ 0.04	–52.66 $\pm$ 0.04	44.50 $\pm$ 0.05	Tuc-Hor	Tuc-Hor	Tuc-Hor	Zu00, Zu01a, To08, Kr14
J00501752+0837341	M5	TW	2.15 $\pm$ 2.0	Sh17	68.02 $\pm$ 0.26	–35.05 $\pm$ 0.13	60.86 $\pm$ 0.52	Field	$\beta$ Pic	$\beta$ Pic	Sh17
J01001613+1251007	K5	TW	$\cdots$	$\cdots$	47.41 $\pm$ 0.08	–31.57 $\pm$ 0.06	94.15 $\pm$ 0.41	Field	$\cdots$	Field	$\cdots$
J01373940+1835332	K7	TW	0.7 $\pm$ 1.9	Sh17	74.76 $\pm$ 0.22	–43.35 $\pm$ 0.15	52.15 $\pm$ 0.28	$\beta$ Pic	$\beta$ Pic/Col?	$\beta$ Pic	Sch10, Ma14b, Sh17
J01540267–4040440	K7	TW	12.7 $\pm$ 0.2	Ma14a	48.72 $\pm$ 0.03	–15.14 $\pm$ 0.03	88.93 $\pm$ 0.21	Field	Col	Col	Ma14a
J02490228–1029220	M2	TW	$\cdots$	$\cdots$	44.1 $\pm$ 1.9bbProper motion from UCAC4 (Zacharias et al. 2013).	–21.7 $\pm$ 2.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	Field	$\beta$ Pic?	$\beta$ Pic?	Ber15
J03451450+5615353	K7	TW	–9 $\pm$ 3	GC18	27.55 $\pm$ 0.20	–33.06 $\pm$ 0.19	112.64 $\pm$ 1.88	Field	$\cdots$	Field	$\cdots$
J03520223+2439479	K7	TW	3.7 $\pm$ 0.1	Ng12	31.15 $\pm$ 0.93	–41.46 $\pm$ 0.87	450 $\pm$ 161ccLikely SB2.	Field	Pleiades	Pleiades	St07
J04071148–2918342	M1	TW	21.2 $\pm$ 0.3	Ma14a	42.0 $\pm$ 1.1bbProper motion from UCAC4 (Zacharias et al. 2013).	–6.9 $\pm$ 1.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	Col	Col	Col	Ro13, Ma13, Ma14a
J04174964+0011455	K7	TW	19 $\pm$ 3	GC18	33.08 $\pm$ 0.19	–26.49 $\pm$ 0.12	99.72 $\pm$ 1.10	Field	$\cdots$	Field	$\cdots$
J04214271–1657543	M1	TW	10 $\pm$ 3	GC18	30.9 $\pm$ 1.7bbProper motion from UCAC4 (Zacharias et al. 2013).	–8.0 $\pm$ 2.1bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	Field	$\cdots$	Field	$\cdots$
J04412079–1947356	K7	TW	$\cdots$	$\cdots$	37.61 $\pm$ 1.19	–12.11 $\pm$ 1.16	139.81 $\pm$ 14.84	Field	$\cdots$	Field	$\cdots$
J04435686+3723033	M2	TW	6.4 $\pm$ 0.2	Ma14a	22.87 $\pm$ 0.10	–61.84 $\pm$ 0.06	71.6 $\pm$ 0.26	Field	$\beta$ Pic	$\beta$ Pic?	Sch10, Ma14b, Me17, Sh17
J04522204+4006347	M0	TW	$\cdots$	$\cdots$	17.16 $\pm$ 0.14	–50.82 $\pm$ 0.09	89.1 $\pm$ 0.41	Field	$\cdots$	Field	$\cdots$
J04580897+4333010	G/K:	TW	11 $\pm$ 8	GC18	22.28 $\pm$ 0.17	–55.80 $\pm$ 0.13	99.04 $\pm$ 1.08	Field	$\cdots$	Field	$\cdots$
J05004928+1527006	K7	TW	18.1 $\pm$ 0.9	Wh07	18.13 $\pm$ 0.08	–58.83 $\pm$ 0.05	53.41 $\pm$ 0.12	$\beta$ Pic	$\beta$ Pic?	$\beta$ Pic	Sch12c, Sch12a
J05053647–5755359	K4	TW	$\cdots$	$\cdots$	26.34 $\pm$ 0.15	15.83 $\pm$ 0.14	94.22 $\pm$ 0.67	Field	$\cdots$	Field	$\cdots$
J05182904–3001321	K7	TW	21.0 $\pm$ 0.5	El14	37.14 $\pm$ 0.08	0.13 $\pm$ 0.10	67.01 $\pm$ 0.26	Tuc-Hor	Tuc-Hor	Tuc-Hor	To08
J05214684+2400444	G7	Li98	13.1 $\pm$ 0.5	Kr17	10.87 $\pm$ 0.08	–46.14 $\pm$ 0.05	88.27 $\pm$ 0.32	118 Tau	118 Tau	118 Tau	Ma16
J05234246+0651581	M0	TW	12 $\pm$ 6	GC18	9.75 $\pm$ 0.06	–33.46 $\pm$ 0.05	96.37 $\pm$ 0.36	32 Ori	32 Ori	32 Ori	Bel15
J05363633+2139330	M2	TW	$\cdots$	$\cdots$	10.65 $\pm$ 0.19	–41.23 $\pm$ 0.14	108.22 $\pm$ 1.59	118 Tau	118 Tau, Taurus	118 Tau	Ma16, Kr17
J05374649+0231264	K5	El14	20.8 $\pm$ 2.8	GC18	18.28 $\pm$ 0.06	–39.52 $\pm$ 0.06	68.44 $\pm$ 0.19	Field	Col	Col	DaS09, El16
J05500858+0511536	M2	TW	18 $\pm$ 4	GC18	17.07 $\pm$ 0.07	–42.18 $\pm$ 0.06	64.45 $\pm$ 0.17	Col	$\cdots$	Col?	TW
J08040534–6316396	M2	TW	$\cdots$	$\cdots$	–17.33 $\pm$ 0.05	32.35 $\pm$ 0.05	78.10 $\pm$ 0.14	Car	Car?	Car?	Ga18c
J08410608–6216063	M0	TW	$\cdots$	$\cdots$	–17.1 $\pm$ 1.1bbProper motion from UCAC4 (Zacharias et al. 2013).	21.8 $\pm$ 1.1bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	Field	$\cdots$	Field	$\cdots$
J08443188–7846311	M0	TW	17.32 $\pm$ 0.11	El14	–30.30 $\pm$ 0.06	26.86 $\pm$ 0.05	98.18 $\pm$ 0.30	$\eta$ Cha	$\eta$ Cha	$\eta$ Cha	Ma99, To08
J09595765–7221472	K7	TW	17.0 $\pm$ 0.2	El14	–27.92 $\pm$ 0.03	28.95 $\pm$ 0.03	83.66 $\pm$ 0.13	Field	Car	Car	El15
J10260210–4105537	M2	TW	$\cdots$	$\cdots$	–46.38 $\pm$ 0.04	–1.85 $\pm$ 0.04	84.88 $\pm$ 0.21	Field	TWA, LCC?	TWA	Pe16, Ga17
J11594608–6101132	K4	TW	15 $\pm$ 3	GC18	–34.21 $\pm$ 0.05	–7.88 $\pm$ 0.04	119.45 $\pm$ 0.43	LCC	LCC	LCC	Pe16
J12000160–1731308	M4	TW	2 $\pm$ 4	GC18	–78.72 $\pm$ 0.14	–28.21 $\pm$ 0.07	53.12 $\pm$ 0.25	Field	$\cdots$	Field	$\cdots$
J12002750–3405371	M5	TW	$\cdots$	$\cdots$	–58.75 $\pm$ 0.12	–21.69 $\pm$ 0.07	72.79 $\pm$ 0.48	TWA	TWA	TWA	Mu15, Ga15b, Ga17
J12003688–6337055	M0	TW	14.3 $\pm$ 1.8	GC18	–40.36 $\pm$ 0.04	–8.18 $\pm$ 0.04	101.2 $\pm$ 0.28	LCC	$\cdots$	LCC	TW
J12124890–6230317	K7	TW	$\cdots$	$\cdots$	–41.6 $\pm$ 1.4bbProper motion from UCAC4 (Zacharias et al. 2013).	–4.4 $\pm$ 1.8bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	LCC	LCC	LCC	So12, El15
J12164593–7753333	M3	TW	14.0 $\pm$ 0.2	El14	–39.83 $\pm$ 0.07	–9.07 $\pm$ 0.07	101.8 $\pm$ 0.40	$ϵ$ Cha	$ϵ$ Cha	$ϵ$ Cha	Lo13, Mu13
J12220147–5737565	M2	TW	$\cdots$	$\cdots$	–36.09 $\pm$ 0.06	–11.25 $\pm$ 0.06	106.45 $\pm$ 0.57	LCC	LCC	LCC	Be18
J12264842–5215070	K7	TW	11.6 $\pm$ 2.5	GC18	–39.69 $\pm$ 0.11	–13.20 $\pm$ 0.10	97.18 $\pm$ 1.03	LCC	LCC	LCC	Pe16
J12281909–7306346	M0	TW	14.6 $\pm$ 1.2	GC18	–36.36 $\pm$ 0.31	–7.18 $\pm$ 0.32	107.35 $\pm$ 2.3	$ϵ$ Cha	$\cdots$	$ϵ$ Cha/LCC	TW
J12383556–5916438	K5	TW	$\cdots$	$\cdots$	–38.01 $\pm$ 0.10	–11.17 $\pm$ 0.07	100.62 $\pm$ 0.77	LCC	LCC	LCC	So12
J12445897–6026409	M1	TW	11.67 $\pm$ 0.14	GC18	–32.60 $\pm$ 0.44	–9.55 $\pm$ 0.54	100.15 $\pm$ 3.09	LCC	$\cdots$	LCC	TW
J13343188–4209305	K3	TW	4.3 $\pm$ 2.6	GC18	–38.78 $\pm$ 0.08	–27.57 $\pm$ 0.11	92.81 $\pm$ 0.42	UCL	LCC?	UCL/LCC	So12, De15
J13390189–2141278	M4	TW	2.8 $\pm$ 1.6	Ma14a	–41.98 $\pm$ 0.12	–26.91 $\pm$ 0.13	83.81 $\pm$ 0.54	Field	$\cdots$	Field	$\cdots$
J13493313–6818291	M3	TW	$\cdots$	$\cdots$	–31.05 $\pm$ 0.21	–19.71 $\pm$ 0.23	99.76 $\pm$ 1.51	LCC	Arg?	LCC	Ma13, TW
J15093920–1332119	M5	TW	$\cdots$	$\cdots$	–53.01 $\pm$ 0.17	–49.11 $\pm$ 0.12	52.65 $\pm$ 0.23	Field	$\cdots$	Field	$\cdots$
J15202415–3037317	M0	TW	$\cdots$	$\cdots$	–27.78 $\pm$ 0.10	–33.12 $\pm$ 0.07	123.92 $\pm$ 0.93	UCL	UCL	UCL	Pe16
J15354856–2958551	M4	TW	$\cdots$	$\cdots$	–32.7 $\pm$ 1.7bbProper motion from UCAC4 (Zacharias et al. 2013).	–38.1 $\pm$ 1.7bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	Field	USco-B	UCL?	Ko00, TW
J15443518+0423075	M2	TW	–22 $\pm$ 5	GC18	–25.42 $\pm$ 0.06	–27.19 $\pm$ 0.05	91.96 $\pm$ 0.28	Field	$\cdots$	Field	$\cdots$
J15451903–4431361	M3	TW	$\cdots$	$\cdots$	–20.41 $\pm$ 1.16	–30.90 $\pm$ 1.10	89.33 $\pm$ 3.68	UCL	$\cdots$	UCL?	TW
J15594951–3628279	K5	TW	–0.3 $\pm$ 1.2	So12	–28.47 $\pm$ 0.10	–43.12 $\pm$ 0.06	86.62 $\pm$ 0.42	UCL	UCL	UCL	So12, Pe16
J16082845–0607345	M4	TW	$\cdots$	$\cdots$	–18.77 $\pm$ 0.16	–26.39 $\pm$ 0.08	86.55 $\pm$ 0.53	Field	$\cdots$	Field	$\cdots$
J16430128–1754274	M1	TW	–9.3 $\pm$ 0.4	Ma14a	–29.13 $\pm$ 0.10	–52.03 $\pm$ 0.05	71.05 $\pm$ 0.26	Field	$\beta$ Pic	Field	Ki10, Bi14, Sh17
J16455062+0343014	M2	TW	–21.7 $\pm$ 1.8	GC18	–37.67 $\pm$ 0.08	–105.38 $\pm$ 0.07	44.89 $\pm$ 0.08	AB Dor	AB Dor?	AB Dor?	Sch12a, Sch12b, Bi15b
J16521087–3359333	M0	TW	$\cdots$	$\cdots$	–20.3 $\pm$ 2.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–42.7 $\pm$ 1.2bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	UCL	UCL	UCL	So12
J17213497–2152283	M4	TW	$\cdots$	$\cdots$	–11.82 $\pm$ 0.15	–32.99 $\pm$ 0.09	101.04 $\pm$ 0.73	UCL	$\cdots$	Sco-Cen?	TW
J17513421–4854558	M2	TW	$\cdots$	$\cdots$	2.14 $\pm$ 0.47	–66.85 $\pm$ 0.41	66.46 $\pm$ 1.17	$\beta$ Pic	USco, $\beta$ Pic	$\beta$ Pic	So12, Ga18c
J17520173–2357571	M2	TW	$\cdots$	$\cdots$	0.22 $\pm$ 0.09	–52.24 $\pm$ 0.07	63.52 $\pm$ 0.20	Field	$\cdots$	Field	$\cdots$
J17563029–2448128	M2	TW	$\cdots$	$\cdots$	–6.58 $\pm$ 0.10	–37.02 $\pm$ 0.08	95.60 $\pm$ 0.58	Field	$\cdots$	Field	$\cdots$
J23093711–0225551	K4	To06	–12.7 $\pm$ 0.4	GC18	60.84 $\pm$ 0.11	–45.96 $\pm$ 0.11	52.60 $\pm$ 0.41	Field	Car	Field?	El15, El16

Table 4. Table 4: Robo-AO Point Source Detections

2MASS	UT Date		Candidate		Sep	P.A.	Significance	Performance
ID	(Y-M-D)	Filter	Name	$\Delta$mag	(′′)	($°$)	($\sigma$)	MetricaaImage performance metrics assessed from the PSF core size. These are divided into three groups: high-performance (“H”), medium-performaance (“M”), and low-performance (“L”). Typical contrasts for each group are described in detail in Section 3.4.
J00074264+6022543	2014-11-08	$i^{\prime }$	CC1	0.30 $\pm$ 0.05	0.86 $\pm$ 0.03	94 $\pm$ 2	12.5	H
J00133841+5245050	2014-08-26	$i^{\prime }$	CC1	2.76 $\pm$ 0.03	3.13 $\pm$ 0.03	110 $\pm$ 3	11.5	H
J00133841+5245050	2014-11-06	$i^{\prime }$	CC1	2.39 $\pm$ 0.05	3.16 $\pm$ 0.04	109 $\pm$ 2	7.2	M
J00133841+5245050	2014-11-06	$i^{\prime }$	CC1	2.74 $\pm$ 0.02	3.16 $\pm$ 0.04	109 $\pm$ 3	6.4	H
J00133841+5245050	2014-11-06	$i^{\prime }$	CC2	3.41 $\pm$ 0.04	0.86 $\pm$ 0.03	94 $\pm$ 2	5.9	M
J00160486+2319090	2014-11-06	$i^{\prime }$	CC1	0.41 $\pm$ 0.05	2.66 $\pm$ 0.05	94 $\pm$ 2	9.6	M
J00164045+3000598	2014-08-24	$i^{\prime }$	CC1	2.47 $\pm$ 0.03	0.98 $\pm$ 0.03	174 $\pm$ 1	12.4	H
J00165678+2003551	2014-11-06	$i^{\prime }$	CC1	0.21 $\pm$ 0.03	1.03 $\pm$ 0.05	102 $\pm$ 3	4.2	H
J00171046+2931520	2013-10-23	$i^{\prime }$	CC1	2.07 $\pm$ 0.05	1.02 $\pm$ 0.02	218 $\pm$ 1	10.5	H
J00171046+2931520	2014-08-28	$i^{\prime }$	CC1	2.03 $\pm$ 0.04	1.03 $\pm$ 0.04	221 $\pm$ 6	12.7	H
J00215781+4912379	2013-10-24	$i^{\prime }$	CC1	2.48 $\pm$ 0.05	2.27 $\pm$ 0.02	303 $\pm$ 2	9.1	H
J00215781+4912379	2014-08-22	$i^{\prime }$	CC1	2.24 $\pm$ 0.02	2.29 $\pm$ 0.05	301 $\pm$ 3	8.3	H
J00215781+4912379	2014-08-22	$i^{\prime }$	CC1	2.50 $\pm$ 0.03	2.23 $\pm$ 0.04	301 $\pm$ 2	9.9	H
J00215781+4912379	2014-08-22	$i^{\prime }$	CC1	2.51 $\pm$ 0.03	2.29 $\pm$ 0.05	301 $\pm$ 2	8.1	H
J00215781+4912379	2014-08-22	$i^{\prime }$	CC2	3.02 $\pm$ 0.03	2.66 $\pm$ 0.01	94 $\pm$ 2	7.0	H
J00233468+2014282	2013-10-23	$i^{\prime }$	CC1	1.08 $\pm$ 0.02	1.73 $\pm$ 0.04	136 $\pm$ 2	14.1	H
J00285391+5022330	2013-10-24	$i^{\prime }$	CC1	0.80 $\pm$ 0.16	0.32 $\pm$ 0.05	85 $\pm$ 2	6.6	H
J00302927+0420204	2014-08-23	$i^{\prime }$	CC1	2.39 $\pm$ 0.02	1.70 $\pm$ 0.03	66 $\pm$ 2	17.4	H
J00323480+0729271	2013-10-25	$i^{\prime }$	CC1	1.01 $\pm$ 0.03	0.74 $\pm$ 0.04	338 $\pm$ 4	8.2	H
J00323480+0729271	2014-08-23	$i^{\prime }$	CC1	0.98 $\pm$ 0.03	0.71 $\pm$ 0.04	336 $\pm$ 2	10.7	H
J00340843+2523498	2013-10-23	$i^{\prime }$	CC1	0.09 $\pm$ 0.05	1.55 $\pm$ 0.04	100 $\pm$ 3	12.1	H
J00340843+2523498	2014-08-24	$i^{\prime }$	CC1	0.05 $\pm$ 0.05	1.54 $\pm$ 0.05	101 $\pm$ 3	11.0	H
J00414141+4410530	2013-10-22	$LP600$	CC1	0.33 $\pm$ 0.04	0.59 $\pm$ 0.01	17 $\pm$ 1	7.2	H
J00414141+4410530	2014-11-06	$i^{\prime }$	CC1	1.01 $\pm$ 0.03	0.51 $\pm$ 0.05	14 $\pm$ 2	4.7	H
J00423409+5439048	2014-08-22	$i^{\prime }$	CC1	6.16 $\pm$ 0.05	3.04 $\pm$ 0.02	95 $\pm$ 2	8.8	H
J00423409+5439048	2014-11-06	$i^{\prime }$	CC1	5.77 $\pm$ 0.11	3.04 $\pm$ 0.05	95 $\pm$ 2	6.9	H
J00423409+5439048	2014-11-06	$i^{\prime }$	CC1	6.24 $\pm$ 0.05	2.98 $\pm$ 0.07	96 $\pm$ 5	6.4	H
J00425668+2239350	2014-11-06	$i^{\prime }$	CC1	2.58 $\pm$ 0.05	2.96 $\pm$ 0.02	336 $\pm$ 4	9.1	H
J00485822+4435091	2013-10-22	$i^{\prime }$	CC1	0.46 $\pm$ 0.04	1.04 $\pm$ 0.03	254 $\pm$ 2	9.1	H
J00485822+4435091	2014-11-06	$i^{\prime }$	CC1	0.45 $\pm$ 0.03	0.97 $\pm$ 0.04	256 $\pm$ 2	6.6	M
J00503319+2449009	2013-10-23	$LP600$	CC1	0.87 $\pm$ 0.03	1.02 $\pm$ 0.04	322 $\pm$ 3	10.4	H
J00503319+2449009	2014-11-06	$i^{\prime }$	CC1	0.82 $\pm$ 0.03	0.94 $\pm$ 0.05	324 $\pm$ 3	5.7	H
J00530648+4829385	2014-08-22	$i^{\prime }$	CC1	1.76 $\pm$ 0.04	1.31 $\pm$ 0.04	49 $\pm$ 3	9.5	H
J01001331+2135328	2013-10-23	$i^{\prime }$	CC1	1.45 $\pm$ 0.03	2.63 $\pm$ 0.02	148 $\pm$ 1	11.2	H
J01001613+1251007	2013-10-24	$i^{\prime }$	CC1	2.30 $\pm$ 0.05	1.11 $\pm$ 0.03	359 $\pm$ 3	12.0	H
J01001613+1251007	2014-08-23	$i^{\prime }$	CC1	2.39 $\pm$ 0.04	1.10 $\pm$ 0.03	0 $\pm$ 1	12.5	H
J01034013+4051288	2014-11-06	$i^{\prime }$	CC1	0.91 $\pm$ 0.04	2.53 $\pm$ 0.03	97 $\pm$ 3	9.2	M
J01071194–1935359	2014-11-08	$i^{\prime }$	CC1	0.32 $\pm$ 0.04	0.47 $\pm$ 0.02	166 $\pm$ 3	8.4	H
J01093915+2931112	2014-11-06	$i^{\prime }$	CC1	1.05 $\pm$ 0.02	0.56 $\pm$ 0.04	125 $\pm$ 1	5.1	M
J01102943–1510071	2014-11-08	$i^{\prime }$	CC1	0.24 $\pm$ 0.05	2.38 $\pm$ 0.03	65 $\pm$ 3	9.8	H
J01105436+5822133	2014-08-22	$i^{\prime }$	CC1	1.99 $\pm$ 0.05	0.73 $\pm$ 0.05	81 $\pm$ 5	8.4	H
J01112542+1526214	2013-10-23	$LP600$	CC1	0.86 $\pm$ 0.15	0.33 $\pm$ 0.05	240 $\pm$ 4	8.7	H
J01121854+4238358	2013-10-22	$i^{\prime }$	CC1	6.05 $\pm$ 0.04	2.93 $\pm$ 0.03	279 $\pm$ 1	9.3	H
J01121854+4238358	2014-08-22	$i^{\prime }$	CC1	5.79 $\pm$ 0.15	2.94 $\pm$ 0.04	279 $\pm$ 3	9.8	H
J01121854+4238358	2014-08-22	$i^{\prime }$	CC1	6.14 $\pm$ 0.04	2.94 $\pm$ 0.03	279 $\pm$ 3	10.5	H
J01121854+4238358	2014-08-22	$i^{\prime }$	CC2	6.20 $\pm$ 0.09	0.73 $\pm$ 0.04	81 $\pm$ 3	6.6	H
J01131976+5855224	2013-10-25	$i^{\prime }$	CC1	3.58 $\pm$ 0.02	2.10 $\pm$ 0.05	212 $\pm$ 3	10.1	H
J01131976+5855224	2014-08-27	$i^{\prime }$	CC1	3.53 $\pm$ 0.04	2.08 $\pm$ 0.05	212 $\pm$ 1	10.2	H
J01132958–0738088	2014-11-08	$i^{\prime }$	CC1	5.15 $\pm$ 0.05	3.02 $\pm$ 0.04	228 $\pm$ 2	11.8	H
J01244246–1540454	2014-11-08	$i^{\prime }$	CC1	0.47 $\pm$ 0.09	0.26 $\pm$ 0.04	228 $\pm$ 4	7.6	H
J01281337–2319278	2014-11-08	$i^{\prime }$	CC1	0.64 $\pm$ 0.03	1.11 $\pm$ 0.02	356 $\pm$ 2	7.7	H
J01304065–1027506	2014-08-28	$i^{\prime }$	CC1	0.31 $\pm$ 0.03	0.96 $\pm$ 0.05	89 $\pm$ 3	12.2	H
J01373940+1835332	2013-10-23	$i^{\prime }$	CC1	0.09 $\pm$ 0.02	1.73 $\pm$ 0.06	23 $\pm$ 3	5.2	H
J01373940+1835332	2014-08-22	$i^{\prime }$	CC1	0.17 $\pm$ 0.02	1.71 $\pm$ 0.05	24 $\pm$ 4	4.7	H
J01535076–1459503	2014-11-08	$i^{\prime }$	CC1	0.03 $\pm$ 0.04	2.87 $\pm$ 0.03	291 $\pm$ 3	6.7	H
J01592349+5831162	2013-10-24	$i^{\prime }$	CC1	6.86 $\pm$ 0.05	3.96 $\pm$ 0.04	91 $\pm$ 2	25.7	H
J01592349+5831162	2014-08-22	$i^{\prime }$	CC2	5.87 $\pm$ 0.05	1.71 $\pm$ 0.04	24 $\pm$ 1	8.1	H
J01592349+5831162	2014-08-22	$i^{\prime }$	CC1	7.22 $\pm$ 0.14	3.65 $\pm$ 0.02	89 $\pm$ 1	31.2	H
J01592349+5831162	2014-08-22	$i^{\prime }$	CC1	7.31 $\pm$ 0.12	3.59 $\pm$ 0.04	89 $\pm$ 2	7.1	H
J01592349+5831162	2014-08-22	$i^{\prime }$	CC1	8.20 $\pm$ 0.48	3.59 $\pm$ 0.03	89 $\pm$ 3	8.0	H
J01592349+5831162	2014-11-08	$i^{\prime }$	CC1	7.05 $\pm$ 0.06	3.61 $\pm$ 0.03	88 $\pm$ 1	109.2	H
J02155892–0929121	2014-11-08	$i^{\prime }$	CC1	1.09 $\pm$ 0.17	0.51 $\pm$ 0.03	286 $\pm$ 5	5.5	H
J02155892–0929121	2014-11-08	$i^{\prime }$	CC2	5.47 $\pm$ 0.04	3.36 $\pm$ 0.04	298 $\pm$ 2	24.7	H
J02205082+3320479	2013-10-23	$i^{\prime }$	CC1	1.95 $\pm$ 0.04	1.48 $\pm$ 0.04	338 $\pm$ 2	13.5	H
J02205082+3320479	2014-08-22	$i^{\prime }$	CC1	1.87 $\pm$ 0.03	1.50 $\pm$ 0.02	338 $\pm$ 2	6.4	M
J02233670–1056138	2014-08-28	$i^{\prime }$	CC1	0.98 $\pm$ 0.05	2.66 $\pm$ 0.02	223 $\pm$ 4	17.7	H
J02284694+1538535	2014-11-07	$i^{\prime }$	CC1	1.54 $\pm$ 0.05	0.84 $\pm$ 0.04	147 $\pm$ 3	7.9	H
J02335984–1811525	2014-11-08	$i^{\prime }$	CC1	0.19 $\pm$ 0.03	0.87 $\pm$ 0.03	232 $\pm$ 5	8.1	H
J02490228–1029220	2014-11-08	$i^{\prime }$	CC1	0.52 $\pm$ 0.18	0.51 $\pm$ 0.03	213 $\pm$ 1	5.6	H
J02490228–1029220	2014-11-08	$i^{\prime }$	CC1	0.75 $\pm$ 0.10	0.72 $\pm$ 0.03	217 $\pm$ 3	7.5	H
J02560096+1220457	2014-08-28	$i^{\prime }$	CC1	0.80 $\pm$ 0.03	0.89 $\pm$ 0.04	282 $\pm$ 1	6.7	H
J03033668–2535329	2014-11-08	$i^{\prime }$	CC1	2.89 $\pm$ 0.21	0.85 $\pm$ 0.05	357 $\pm$ 4	6.7	H
J03092643+6732425	2013-10-25	$i^{\prime }$	CC1	6.08 $\pm$ 0.04	2.78 $\pm$ 0.03	357 $\pm$ 1	12.6	H
J03144720+1127272	2014-08-22	$i^{\prime }$	CC1	1.76 $\pm$ 0.17	0.70 $\pm$ 0.03	179 $\pm$ 2	6.4	H
J03144720+1127272	2014-11-08	$i^{\prime }$	CC1	2.47 $\pm$ 0.05	0.59 $\pm$ 0.05	186 $\pm$ 3	5.7	H
J03175221+5847431	2013-10-24	$i^{\prime }$	CC1	5.39 $\pm$ 0.03	2.43 $\pm$ 0.02	67 $\pm$ 1	10.5	H
J03175221+5847431	2014-08-22	$i^{\prime }$	CC1	4.87 $\pm$ 0.03	2.43 $\pm$ 0.03	66 $\pm$ 6	11.1	H
J03175221+5847431	2014-08-22	$i^{\prime }$	CC1	5.67 $\pm$ 0.05	2.43 $\pm$ 0.05	66 $\pm$ 2	10.7	H
J03240643+2347073	2013-10-22	$LP600$	CC1	0.78 $\pm$ 0.02	2.55 $\pm$ 0.04	340 $\pm$ 3	14.6	H
J03240643+2347073	2014-08-29	$i^{\prime }$	CC1	0.76 $\pm$ 0.05	2.63 $\pm$ 0.03	341 $\pm$ 3	9.6	H
J03240643+2347073	2014-11-06	$i^{\prime }$	CC1	0.74 $\pm$ 0.05	2.62 $\pm$ 0.04	341 $\pm$ 1	6.1	H
J03240643+2347073	2014-11-08	$i^{\prime }$	CC1	0.77 $\pm$ 0.03	2.63 $\pm$ 0.02	341 $\pm$ 3	18.1	H
J03323578+2843554	2013-10-23	$i^{\prime }$	CC1	0.34 $\pm$ 0.05	0.47 $\pm$ 0.05	103 $\pm$ 2	7.0	H
J03340048+5835551	2014-08-27	$i^{\prime }$	CC1	1.41 $\pm$ 0.03	0.81 $\pm$ 0.02	110 $\pm$ 2	6.3	H
J03434696+5725557	2013-10-24	$i^{\prime }$	CC1	2.93 $\pm$ 0.16	3.54 $\pm$ 0.02	241 $\pm$ 3	5.2	M
J03520223+2439479	2014-11-06	$i^{\prime }$	CC1	1.81 $\pm$ 0.25	0.45 $\pm$ 0.05	316 $\pm$ 3	7.3	H
J04053888+0544408	2013-10-25	$i^{\prime }$	CC1	0.84 $\pm$ 0.04	0.81 $\pm$ 0.02	253 $\pm$ 3	11.0	H
J04053888+0544408	2014-08-23	$i^{\prime }$	CC1	0.75 $\pm$ 0.04	0.78 $\pm$ 0.03	253 $\pm$ 4	8.5	H
J04074484+0945220	2014-08-23	$i^{\prime }$	CC1	2.06 $\pm$ 0.04	0.77 $\pm$ 0.03	279 $\pm$ 2	6.7	H
J04112810+7544231	2014-11-08	$i^{\prime }$	CC1	1.02 $\pm$ 0.03	0.27 $\pm$ 0.06	104 $\pm$ 1	7.9	H
J04132663–0139211	2014-11-08	$i^{\prime }$	CC1	0.60 $\pm$ 0.02	0.72 $\pm$ 0.04	175 $\pm$ 1	9.8	H
J04134585–0509049	2014-11-08	$i^{\prime }$	CC1	4.92 $\pm$ 0.04	3.37 $\pm$ 0.04	104 $\pm$ 3	9.9	H
J04171645+1213557	2013-10-24	$LP600$	CC1	0.68 $\pm$ 0.05	0.73 $\pm$ 0.04	92 $\pm$ 2	4.6	H
J04171645+1213557	2014-08-23	$i^{\prime }$	CC1	0.68 $\pm$ 0.05	0.73 $\pm$ 0.02	96 $\pm$ 2	7.5	H
J04174337–1754222	2014-08-30	$i^{\prime }$	CC1	2.74 $\pm$ 0.02	2.78 $\pm$ 0.02	359 $\pm$ 2	16.0	H
J04174431+4103137	2013-10-22	$i^{\prime }$	CC1	1.89 $\pm$ 0.04	2.46 $\pm$ 0.04	248 $\pm$ 4	25.6	H
J04174431+4103137	2014-08-26	$i^{\prime }$	CC1	1.91 $\pm$ 0.03	2.52 $\pm$ 0.04	247 $\pm$ 2	11.7	H
J04214271–1657543	2014-08-30	$i^{\prime }$	CC1	0.64 $\pm$ 0.14	0.41 $\pm$ 0.03	55 $\pm$ 2	8.5	H
J04244805+1552292	2013-10-23	$LP600$	CC1	0.35 $\pm$ 0.12	0.30 $\pm$ 0.04	347 $\pm$ 3	9.2	H
J04244805+1552292	2014-11-06	$i^{\prime }$	CC1	0.69 $\pm$ 0.10	0.31 $\pm$ 0.03	344 $\pm$ 1	9.2	H
J04251456+1858250	2014-11-06	$i^{\prime }$	CC1	3.14 $\pm$ 0.03	0.83 $\pm$ 0.02	140 $\pm$ 2	9.5	H
J04282878+1741453	2013-10-23	$i^{\prime }$	CC1	1.82 $\pm$ 0.04	1.72 $\pm$ 0.02	74 $\pm$ 4	13.2	H
J04282878+1741453	2014-11-06	$i^{\prime }$	CC1	1.82 $\pm$ 0.05	1.71 $\pm$ 0.04	75 $\pm$ 1	7.8	H
J04285080+1617204	2013-10-23	$i^{\prime }$	CC1	4.41 $\pm$ 0.02	2.00 $\pm$ 0.04	175 $\pm$ 2	15.7	H
J04285080+1617204	2014-08-22	$i^{\prime }$	CC1	3.86 $\pm$ 0.04	1.97 $\pm$ 0.04	175 $\pm$ 3	15.6	H
J04285080+1617204	2014-08-22	$i^{\prime }$	CC1	4.41 $\pm$ 0.03	1.97 $\pm$ 0.04	175 $\pm$ 3	15.0	H
J04285080+1617204	2014-08-22	$i^{\prime }$	CC2	5.56 $\pm$ 0.05	0.73 $\pm$ 0.03	96 $\pm$ 3	8.5	H
J04311384+2053436	2014-08-28	$i^{\prime }$	CC1	2.74 $\pm$ 0.27	0.65 $\pm$ 0.03	217 $\pm$ 2	9.8	H
J04325718+7407002	2014-08-23	$i^{\prime }$	CC1	1.42 $\pm$ 0.03	2.86 $\pm$ 0.05	323 $\pm$ 2	10.8	H
J04343992+1512325	2014-11-06	$i^{\prime }$	CC1	3.63 $\pm$ 0.04	1.05 $\pm$ 0.04	175 $\pm$ 2	7.4	H
J04350255+0839304	2013-10-25	$i^{\prime }$	CC1	1.04 $\pm$ 0.24	0.32 $\pm$ 0.04	97 $\pm$ 4	8.9	H
J04381255+2813001	2013-10-23	$i^{\prime }$	CC1	0.45 $\pm$ 0.02	1.15 $\pm$ 0.04	303 $\pm$ 1	9.9	H
J04381255+2813001	2014-11-06	$i^{\prime }$	CC1	0.51 $\pm$ 0.03	1.15 $\pm$ 0.04	303 $\pm$ 2	3.9	M
J04385352+2147549	2014-11-06	$i^{\prime }$	CC1	0.56 $\pm$ 0.03	1.27 $\pm$ 0.02	123 $\pm$ 3	5.6	M
J04412780+1404340	2013-10-23	$i^{\prime }$	CC1	1.09 $\pm$ 0.33	0.26 $\pm$ 0.04	262 $\pm$ 2	8.7	H
J04485498+5527185	2013-10-22	$i^{\prime }$	CC1	1.93 $\pm$ 0.17	0.51 $\pm$ 0.03	262 $\pm$ 3	7.3	H
J04492947+4828459	2013-10-22	$LP600$	CC1	0.56 $\pm$ 0.07	0.62 $\pm$ 0.04	246 $\pm$ 3	8.0	H
J04492947+4828459	2014-11-08	$i^{\prime }$	CC1	0.74 $\pm$ 0.03	0.63 $\pm$ 0.01	250 $\pm$ 2	8.1	H
J04495635+2341029	2013-10-24	$i^{\prime }$	CC1	0.79 $\pm$ 0.05	2.51 $\pm$ 0.03	88 $\pm$ 2	10.9	H
J04495635+2341029	2014-08-28	$i^{\prime }$	CC1	0.87 $\pm$ 0.04	2.46 $\pm$ 0.05	89 $\pm$ 2	16.5	H
J05024924+7352143	2014-11-08	$i^{\prime }$	CC1	0.91 $\pm$ 0.16	0.34 $\pm$ 0.03	74 $\pm$ 1	8.9	H
J05122408+1824086	2014-08-28	$i^{\prime }$	CC1	0.10 $\pm$ 0.04	1.50 $\pm$ 0.03	97 $\pm$ 2	12.5	H
J05195513–0723399	2014-11-11	$i^{\prime }$	CC1	2.16 $\pm$ 0.33	0.53 $\pm$ 0.03	286 $\pm$ 2	6.4	H
J05252028+6510544	2013-10-25	$LP600$	CC1	1.88 $\pm$ 0.03	1.63 $\pm$ 0.03	230 $\pm$ 1	11.6	H
J05285650+1231539	2014-08-28	$i^{\prime }$	CC1	1.23 $\pm$ 0.12	0.23 $\pm$ 0.05	162 $\pm$ 2	9.5	H
J05341064+4732033	2013-10-22	$i^{\prime }$	CC1	0.97 $\pm$ 0.03	2.53 $\pm$ 0.01	14 $\pm$ 3	9.1	H
J05341064+4732033	2014-11-06	$i^{\prime }$	CC1	0.98 $\pm$ 0.03	2.47 $\pm$ 0.04	16 $\pm$ 2	8.7	H
J05341064+4732033	2015-03-08	$i^{\prime }$	CC1	1.02 $\pm$ 0.03	2.47 $\pm$ 0.03	16 $\pm$ 2	14.8	H
J05345873+6521435	2014-11-06	$i^{\prime }$	CC1	0.10 $\pm$ 0.05	1.17 $\pm$ 0.03	276 $\pm$ 3	7.3	H
J05494518+2513331	2013-10-25	$i^{\prime }$	CC1	2.10 $\pm$ 0.05	2.79 $\pm$ 0.03	192 $\pm$ 1	17.2	H
J05494518+2513331	2014-08-27	$i^{\prime }$	CC1	2.03 $\pm$ 0.04	2.89 $\pm$ 0.04	193 $\pm$ 2	10.4	H
J05554690+5123592	2014-11-06	$i^{\prime }$	CC1	3.41 $\pm$ 0.05	1.90 $\pm$ 0.05	272 $\pm$ 2	10.6	H
J05554690+5123592	2015-03-08	$i^{\prime }$	CC1	3.53 $\pm$ 0.02	1.88 $\pm$ 0.03	272 $\pm$ 3	20.7	H
J06073185+4712266	2014-03-25	$i^{\prime }$	CC1	6.50 $\pm$ 0.14	3.45 $\pm$ 0.03	11 $\pm$ 2	6.9	H
J06084814+4257182	2013-12-17	$LP600$	CC1	0.70 $\pm$ 0.07	1.34 $\pm$ 0.04	357 $\pm$ 1	3.9	M
J06084814+4257182	2014-03-25	$i^{\prime }$	CC1	0.83 $\pm$ 0.03	1.30 $\pm$ 0.04	354 $\pm$ 2	10.8	H
J06084814+4257182	2014-08-28	$i^{\prime }$	CC1	0.83 $\pm$ 0.05	1.28 $\pm$ 0.04	352 $\pm$ 3	9.2	H
J06084814+4257182	2015-03-08	$i^{\prime }$	CC1	0.84 $\pm$ 0.03	1.29 $\pm$ 0.03	355 $\pm$ 4	11.9	H
J06101580+2119569	2013-10-23	$i^{\prime }$	CC1	4.88 $\pm$ 0.10	1.93 $\pm$ 0.03	51 $\pm$ 3	13.8	H
J06101580+2119569	2014-08-29	$i^{\prime }$	CC1	4.81 $\pm$ 0.06	1.91 $\pm$ 0.05	46 $\pm$ 1	9.2	H
J06101580+2119569	2014-08-30	$i^{\prime }$	CC1	4.91 $\pm$ 0.07	1.93 $\pm$ 0.03	45 $\pm$ 4	2386.5	H
J06101580+2119569	2014-08-30	$i^{\prime }$	CC2	4.99 $\pm$ 0.04	1.28 $\pm$ 0.03	352 $\pm$ 2	23.3	H
J06101580+2119569	2014-08-30	$i^{\prime }$	CC1	4.99 $\pm$ 0.04	1.93 $\pm$ 0.02	45 $\pm$ 2	69.9	H
J06133437+4914051	2013-10-22	$i^{\prime }$	CC1	1.71 $\pm$ 0.12	0.79 $\pm$ 0.03	25 $\pm$ 1	4.4	H
J06133437+4914051	2014-11-06	$i^{\prime }$	CC1	2.31 $\pm$ 0.02	0.81 $\pm$ 0.04	25 $\pm$ 4	6.8	H
J06133437+4914051	2015-03-08	$i^{\prime }$	CC1	2.27 $\pm$ 0.13	0.79 $\pm$ 0.05	27 $\pm$ 4	4.9	H
J06462622+0521150	2014-11-06	$i^{\prime }$	CC1	6.21 $\pm$ 0.03	4.17 $\pm$ 0.03	256 $\pm$ 4	10.0	H
J06584690+2843004	2014-03-25	$i^{\prime }$	CC1	3.54 $\pm$ 0.19	1.08 $\pm$ 0.06	247 $\pm$ 3	7.7	H
J06584690+2843004	2014-09-03	$i^{\prime }$	CC1	3.34 $\pm$ 0.05	1.08 $\pm$ 0.02	247 $\pm$ 2	9.5	H
J06584690+2843004	2014-09-03	$i^{\prime }$	CC1	4.03 $\pm$ 0.06	1.11 $\pm$ 0.04	250 $\pm$ 3	9.3	H
J06584690+2843004	2014-09-03	$i^{\prime }$	CC1	4.06 $\pm$ 0.11	1.04 $\pm$ 0.05	249 $\pm$ 3	9.8	H
J06584690+2843004	2014-09-03	$i^{\prime }$	CC1	4.80 $\pm$ 0.04	1.04 $\pm$ 0.02	249 $\pm$ 3	8.2	H
J06584690+2843004	2015-03-08	$i^{\prime }$	CC1	3.93 $\pm$ 0.15	1.03 $\pm$ 0.04	255 $\pm$ 2	10.0	H
J07120481+5423473	2014-03-25	$i^{\prime }$	CC1	$\cdots$	1.07 $\pm$ 0.02	336 $\pm$ 3	8.8	H
J07120481+5423473	2014-09-03	$i^{\prime }$	CC1	$\cdots$	1.13 $\pm$ 0.03	338 $\pm$ 3	9.5	H
J07120481+5423473	2015-03-08	$i^{\prime }$	CC1	0.27 $\pm$ 0.04	1.04 $\pm$ 0.04	332 $\pm$ 4	9.4	H
J07140450+5043334	2014-03-25	$i^{\prime }$	CC1	3.54 $\pm$ 0.05	1.91 $\pm$ 0.04	257 $\pm$ 1	10.7	H
J07140450+5043334	2014-09-03	$i^{\prime }$	CC1	3.03 $\pm$ 0.05	1.90 $\pm$ 0.02	256 $\pm$ 4	9.9	H
J07140450+5043334	2014-09-03	$i^{\prime }$	CC1	3.52 $\pm$ 0.03	1.90 $\pm$ 0.04	256 $\pm$ 2	9.4	H
J07140450+5043334	2014-09-03	$i^{\prime }$	CC2	4.42 $\pm$ 0.04	1.11 $\pm$ 0.03	250 $\pm$ 4	9.1	H
J07140450+5043334	2014-11-06	$i^{\prime }$	CC1	3.01 $\pm$ 0.02	1.90 $\pm$ 0.06	256 $\pm$ 1	9.9	H
J07140450+5043334	2014-11-06	$i^{\prime }$	CC1	3.45 $\pm$ 0.05	1.85 $\pm$ 0.03	256 $\pm$ 2	7.8	H
J07140450+5043334	2014-11-06	$i^{\prime }$	CC1	3.48 $\pm$ 0.05	1.90 $\pm$ 0.03	256 $\pm$ 3	9.2	H
J07140450+5043334	2014-11-06	$i^{\prime }$	CC1	4.26 $\pm$ 0.08	1.90 $\pm$ 0.04	256 $\pm$ 3	7.4	H
J07140450+5043334	2015-03-08	$i^{\prime }$	CC1	3.52 $\pm$ 0.04	1.89 $\pm$ 0.04	255 $\pm$ 2	11.1	H
J07161207+3315154	2014-09-03	$i^{\prime }$	CC1	5.42 $\pm$ 0.04	1.84 $\pm$ 0.04	52 $\pm$ 4	12.7	H
J07161207+3315154	2014-11-06	$i^{\prime }$	CC1	5.87 $\pm$ 0.19	1.82 $\pm$ 0.03	52 $\pm$ 5	8.2	H
J07161207+3315154	2015-03-08	$i^{\prime }$	CC1	5.41 $\pm$ 0.04	1.84 $\pm$ 0.01	53 $\pm$ 2	289.6	H
J07194218+2954390	2014-03-25	$i^{\prime }$	CC1	3.24 $\pm$ 0.26	0.48 $\pm$ 0.01	119 $\pm$ 3	5.7	H
J07315773+3613102	2013-12-17	$i^{\prime }$	CC1	2.61 $\pm$ 0.04	1.55 $\pm$ 0.04	190 $\pm$ 2	14.1	H
J07315773+3613102	2015-03-08	$i^{\prime }$	CC1	2.62 $\pm$ 0.05	1.58 $\pm$ 0.04	190 $\pm$ 2	11.4	H
J07505369+4428181	2013-12-13	$i^{\prime }$	CC1	0.99 $\pm$ 0.03	2.08 $\pm$ 0.04	142 $\pm$ 3	10.2	H
J07505369+4428181	2014-11-06	$i^{\prime }$	CC1	1.03 $\pm$ 0.02	2.11 $\pm$ 0.04	143 $\pm$ 2	11.4	H
J07505369+4428181	2015-03-08	$i^{\prime }$	CC1	1.02 $\pm$ 0.04	2.11 $\pm$ 0.03	142 $\pm$ 2	19.6	H
J08010582+0334064	2015-03-08	$i^{\prime }$	CC1	6.39 $\pm$ 0.03	2.25 $\pm$ 0.03	351 $\pm$ 4	7.0	H
J08014318+4959455	2013-12-16	$i^{\prime }$	CC1	1.07 $\pm$ 0.04	1.12 $\pm$ 0.03	163 $\pm$ 2	4.2	L
J08014318+4959455	2014-03-25	$i^{\prime }$	CC1	0.80 $\pm$ 0.04	1.15 $\pm$ 0.04	163 $\pm$ 3	9.4	H
J08014318+4959455	2014-11-06	$i^{\prime }$	CC1	0.79 $\pm$ 0.02	1.16 $\pm$ 0.03	162 $\pm$ 2	6.8	M
J08014318+4959455	2015-03-08	$i^{\prime }$	CC1	0.76 $\pm$ 0.02	1.16 $\pm$ 0.04	164 $\pm$ 3	9.6	H
J08083284+5304377	2014-03-25	$i^{\prime }$	CC1	0.47 $\pm$ 0.04	1.26 $\pm$ 0.05	139 $\pm$ 3	10.8	H
J08083284+5304377	2014-11-06	$i^{\prime }$	CC1	0.52 $\pm$ 0.02	1.26 $\pm$ 0.01	141 $\pm$ 3	7.8	M
J08083284+5304377	2015-03-08	$i^{\prime }$	CC1	0.50 $\pm$ 0.02	1.23 $\pm$ 0.05	136 $\pm$ 2	9.3	H
J08095207+0301106	2014-11-11	$i^{\prime }$	CC1	0.58 $\pm$ 0.03	2.43 $\pm$ 0.02	34 $\pm$ 2	12.8	H
J08095207+0301106	2015-03-08	$i^{\prime }$	CC1	0.48 $\pm$ 0.04	2.41 $\pm$ 0.04	35 $\pm$ 1	13.1	H
J08310177+4012115	2013-10-23	$i^{\prime }$	CC1	0.24 $\pm$ 0.03	1.93 $\pm$ 0.03	119 $\pm$ 2	9.0	L
J08310177+4012115	2014-11-06	$i^{\prime }$	CC1	0.24 $\pm$ 0.02	1.94 $\pm$ 0.04	121 $\pm$ 3	7.7	M
J08310177+4012115	2015-03-08	$i^{\prime }$	CC1	0.22 $\pm$ 0.03	1.94 $\pm$ 0.04	120 $\pm$ 4	9.1	H
J08444213+0044159	2014-11-11	$i^{\prime }$	CC1	3.90 $\pm$ 0.02	3.26 $\pm$ 0.03	116 $\pm$ 3	12.0	H
J08444213+0044159	2015-03-08	$i^{\prime }$	CC1	3.91 $\pm$ 0.05	3.26 $\pm$ 0.02	116 $\pm$ 2	13.5	H
J08504234+0751517	2014-11-10	$i^{\prime }$	CC1	0.30 $\pm$ 0.02	1.20 $\pm$ 0.04	176 $\pm$ 2	5.7	H
J08504234+0751517	2014-11-11	$i^{\prime }$	CC1	0.22 $\pm$ 0.04	1.23 $\pm$ 0.04	178 $\pm$ 3	9.0	H
J08504234+0751517	2015-03-08	$i^{\prime }$	CC1	0.24 $\pm$ 0.04	1.21 $\pm$ 0.05	178 $\pm$ 2	12.9	H
J08593592+5343505	2015-03-08	$i^{\prime }$	CC1	1.03 $\pm$ 0.23	0.37 $\pm$ 0.04	210 $\pm$ 3	8.0	H
J09062111+1659235	2015-03-08	$i^{\prime }$	CC1	0.04 $\pm$ 0.02	0.88 $\pm$ 0.03	280 $\pm$ 2	7.9	H
J09132383+6852305	2014-11-11	$i^{\prime }$	CC1	0.22 $\pm$ 0.03	0.60 $\pm$ 0.04	227 $\pm$ 4	9.7	H
J09132383+6852305	2015-03-08	$i^{\prime }$	CC1	0.31 $\pm$ 0.03	0.63 $\pm$ 0.04	224 $\pm$ 1	6.7	H
J09174473+4612246	2013-12-17	$i^{\prime }$	CC1	0.86 $\pm$ 0.15	0.19 $\pm$ 0.03	348 $\pm$ 2	10.2	H
J09192291+6203170	2014-03-25	$i^{\prime }$	CC1	3.88 $\pm$ 0.34	0.79 $\pm$ 0.04	189 $\pm$ 3	7.1	H
J09200048+3052397	2014-03-25	$i^{\prime }$	CC1	0.45 $\pm$ 0.04	0.42 $\pm$ 0.03	66 $\pm$ 3	10.3	H
J09200048+3052397	2014-11-06	$i^{\prime }$	CC1	1.02 $\pm$ 0.04	0.43 $\pm$ 0.05	72 $\pm$ 3	7.7	H
J09200048+3052397	2015-03-08	$i^{\prime }$	CC1	0.32 $\pm$ 0.03	0.45 $\pm$ 0.03	70 $\pm$ 3	10.7	H
J09214911+4330284	2014-03-25	$i^{\prime }$	CC1	0.35 $\pm$ 0.05	0.72 $\pm$ 0.02	126 $\pm$ 3	8.6	H
J09214911+4330284	2015-03-08	$i^{\prime }$	CC1	0.37 $\pm$ 0.05	0.71 $\pm$ 0.02	124 $\pm$ 3	8.2	M
J10024936+4827333	2014-03-25	$i^{\prime }$	CC1	0.41 $\pm$ 0.18	0.20 $\pm$ 0.02	306 $\pm$ 3	7.4	M
J10043276+0533412	2014-03-25	$i^{\prime }$	CC1	0.61 $\pm$ 0.11	0.30 $\pm$ 0.04	324 $\pm$ 4	7.8	H
J10043276+0533412	2015-03-08	$i^{\prime }$	CC1	0.61 $\pm$ 0.04	0.32 $\pm$ 0.02	327 $\pm$ 2	12.0	H
J10143153+0213174	2015-03-08	$i^{\prime }$	CC1	2.62 $\pm$ 0.10	0.67 $\pm$ 0.04	157 $\pm$ 3	10.9	H
J10143194+0606409	2014-03-25	$i^{\prime }$	CC1	0.28 $\pm$ 0.04	2.13 $\pm$ 0.03	268 $\pm$ 2	18.3	H
J10143194+0606409	2015-03-08	$i^{\prime }$	CC1	0.24 $\pm$ 0.04	2.16 $\pm$ 0.02	268 $\pm$ 2	23.8	H
J10150690+3125110	2014-03-25	$i^{\prime }$	CC1	0.37 $\pm$ 0.03	1.81 $\pm$ 0.03	305 $\pm$ 1	9.5	H
J10150690+3125110	2015-03-08	$i^{\prime }$	CC1	0.39 $\pm$ 0.03	1.77 $\pm$ 0.04	306 $\pm$ 4	13.5	H
J10150690+3125110	2015-06-05	$i^{\prime }$	CC1	0.44 $\pm$ 0.05	1.80 $\pm$ 0.03	307 $\pm$ 4	10.8	M
J10452148+3830422	2015-06-12	$i^{\prime }$	CC1	1.53 $\pm$ 0.10	0.68 $\pm$ 0.03	232 $\pm$ 2	7.1	H
J10482887+5852005	2014-03-25	$i^{\prime }$	CC1	3.69 $\pm$ 0.04	1.20 $\pm$ 0.03	2 $\pm$ 2	11.4	H
J10482887+5852005	2014-11-07	$i^{\prime }$	CC2	3.13 $\pm$ 0.04	1.80 $\pm$ 0.03	307 $\pm$ 2	11.1	H
J10482887+5852005	2014-11-07	$i^{\prime }$	CC1	3.66 $\pm$ 0.04	1.24 $\pm$ 0.01	6 $\pm$ 4	13.1	H
J10482887+5852005	2014-11-07	$i^{\prime }$	CC1	3.90 $\pm$ 0.03	1.24 $\pm$ 0.04	6 $\pm$ 3	14.0	H
J10482887+5852005	2015-03-08	$i^{\prime }$	CC1	3.76 $\pm$ 0.07	1.25 $\pm$ 0.04	11 $\pm$ 2	10.0	H
J10482887+5852005	2015-06-05	$i^{\prime }$	CC1	4.26 $\pm$ 0.34	1.29 $\pm$ 0.02	14 $\pm$ 3	8.1	H
J10571139+0544547	2014-03-25	$i^{\prime }$	CC1	1.18 $\pm$ 0.05	1.01 $\pm$ 0.04	152 $\pm$ 2	11.2	H
J10571139+0544547	2015-03-08	$i^{\prime }$	CC1	1.23 $\pm$ 0.04	1.04 $\pm$ 0.05	152 $\pm$ 3	6.6	H
J10571139+0544547	2015-03-09	$i^{\prime }$	CC1	1.17 $\pm$ 0.03	1.02 $\pm$ 0.03	155 $\pm$ 2	9.2	H
J10571139+0544547	2015-06-05	$i^{\prime }$	CC1	1.17 $\pm$ 0.04	1.04 $\pm$ 0.04	152 $\pm$ 2	9.4	H
J11030845+1517518	2014-03-25	$i^{\prime }$	CC1	1.03 $\pm$ 0.25	0.39 $\pm$ 0.04	57 $\pm$ 2	8.7	H
J11030845+1517518	2015-03-08	$i^{\prime }$	CC1	1.22 $\pm$ 0.13	0.44 $\pm$ 0.03	56 $\pm$ 3	7.8	H
J11030845+1517518	2015-06-05	$i^{\prime }$	CC1	1.38 $\pm$ 0.02	0.47 $\pm$ 0.04	57 $\pm$ 2	10.4	H
J11161238+4942112	2014-03-25	$i^{\prime }$	CC1	0.95 $\pm$ 0.06	0.79 $\pm$ 0.03	160 $\pm$ 4	11.6	H
J11161238+4942112	2015-03-08	$i^{\prime }$	CC1	1.05 $\pm$ 0.03	0.82 $\pm$ 0.05	159 $\pm$ 4	10.5	H
J11161238+4942112	2015-06-05	$i^{\prime }$	CC1	1.05 $\pm$ 0.02	0.84 $\pm$ 0.06	163 $\pm$ 2	10.2	H
J11432359+2518137	2014-03-24	$i^{\prime }$	CC1	1.10 $\pm$ 0.05	0.48 $\pm$ 0.03	113 $\pm$ 3	6.4	H
J11432359+2518137	2015-03-08	$i^{\prime }$	CC1	1.02 $\pm$ 0.06	0.48 $\pm$ 0.04	111 $\pm$ 3	6.2	H
J11470543+7001588	2015-03-09	$i^{\prime }$	CC1	0.06 $\pm$ 0.03	0.91 $\pm$ 0.03	138 $\pm$ 3	8.9	H
J11474897+0459160	2014-03-25	$i^{\prime }$	CC1	4.95 $\pm$ 0.07	1.68 $\pm$ 0.02	292 $\pm$ 2	7.0	H
J11474897+0459160	2014-06-13	$i^{\prime }$	CC1	4.28 $\pm$ 0.03	1.68 $\pm$ 0.04	292 $\pm$ 3	5.4	H
J11474897+0459160	2014-06-13	$i^{\prime }$	CC1	5.11 $\pm$ 0.03	1.68 $\pm$ 0.02	294 $\pm$ 2	6.1	H
J11474897+0459160	2014-06-13	$i^{\prime }$	CC1	5.47 $\pm$ 0.03	1.68 $\pm$ 0.03	294 $\pm$ 2	5.6	H
J11474897+0459160	2015-03-09	$i^{\prime }$	CC1	5.03 $\pm$ 0.05	1.71 $\pm$ 0.05	293 $\pm$ 3	5.9	H
J11474897+0459160	2015-06-05	$i^{\prime }$	CC1	4.97 $\pm$ 0.07	1.71 $\pm$ 0.04	292 $\pm$ 3	5.8	H
J11503435+2903407	2014-03-24	$i^{\prime }$	CC1	0.60 $\pm$ 0.05	0.51 $\pm$ 0.04	352 $\pm$ 1	7.0	H
J11503435+2903407	2015-03-08	$i^{\prime }$	CC1	0.65 $\pm$ 0.07	0.49 $\pm$ 0.05	357 $\pm$ 3	9.2	H
J11503435+2903407	2015-06-04	$i^{\prime }$	CC1	0.59 $\pm$ 0.11	0.49 $\pm$ 0.04	357 $\pm$ 2	6.4	M
J11504306+3312180	2014-03-25	$i^{\prime }$	CC2	4.26 $\pm$ 0.05	2.58 $\pm$ 0.04	91 $\pm$ 2	12.6	H
J11504306+3312180	2014-06-13	$i^{\prime }$	CC1	2.09 $\pm$ 0.02	0.59 $\pm$ 0.01	118 $\pm$ 2	7.5	H
J11504306+3312180	2014-06-13	$i^{\prime }$	CC3	3.18 $\pm$ 0.14	0.49 $\pm$ 0.05	357 $\pm$ 2	7.9	H
J11504306+3312180	2014-06-13	$i^{\prime }$	CC1	4.52 $\pm$ 0.04	0.59 $\pm$ 0.03	118 $\pm$ 1	34.3	H
J11504306+3312180	2015-03-08	$i^{\prime }$	CC1	2.09 $\pm$ 0.07	0.59 $\pm$ 0.04	120 $\pm$ 2	6.6	H
J12115308+1249135	2015-03-08	$i^{\prime }$	CC1	0.08 $\pm$ 0.04	1.17 $\pm$ 0.02	3 $\pm$ 2	10.2	H
J12121136+4849032	2015-06-10	$i^{\prime }$	CC1	1.86 $\pm$ 0.04	2.85 $\pm$ 0.02	167 $\pm$ 3	9.8	H
J12161505+5053376	2015-06-10	$i^{\prime }$	CC1	0.89 $\pm$ 0.05	1.90 $\pm$ 0.03	188 $\pm$ 3	6.6	M
J12174539+0653230	2015-06-12	$i^{\prime }$	CC1	3.37 $\pm$ 0.04	2.63 $\pm$ 0.04	21 $\pm$ 3	6.4	H
J12225061–0404462	2015-06-05	$i^{\prime }$	CC1	1.45 $\pm$ 0.09	0.24 $\pm$ 0.02	29 $\pm$ 2	7.1	H
J13020587+1222215	2014-06-15	$i^{\prime }$	CC1	2.45 $\pm$ 0.05	2.93 $\pm$ 0.03	88 $\pm$ 2	15.2	H
J13020587+1222215	2015-03-08	$i^{\prime }$	CC1	2.47 $\pm$ 0.03	2.95 $\pm$ 0.03	86 $\pm$ 3	12.3	H
J13020587+1222215	2015-06-04	$i^{\prime }$	CC1	2.44 $\pm$ 0.04	2.90 $\pm$ 0.04	87 $\pm$ 3	12.1	H
J13034595+2837205	2015-06-06	$i^{\prime }$	CC1	6.28 $\pm$ 0.29	1.86 $\pm$ 0.03	161 $\pm$ 2	6.3	H
J13061537+2043444	2015-06-08	$i^{\prime }$	CC1	1.88 $\pm$ 0.03	1.61 $\pm$ 0.03	197 $\pm$ 3	5.8	H
J13120689+3213179	2015-06-06	$i^{\prime }$	CC1	0.77 $\pm$ 0.21	0.24 $\pm$ 0.03	315 $\pm$ 3	8.3	H
J13151846–0249516	2015-06-12	$i^{\prime }$	CC1	1.54 $\pm$ 0.15	0.29 $\pm$ 0.03	100 $\pm$ 4	11.4	H
J13162169+2905548	2015-03-08	$i^{\prime }$	CC2	0.96 $\pm$ 0.05	2.40 $\pm$ 0.03	72 $\pm$ 3	11.7	M
J13162169+2905548	2015-03-08	$i^{\prime }$	CC1	1.44 $\pm$ 0.09	0.29 $\pm$ 0.03	81 $\pm$ 3	12.5	M
J13162169+2905548	2015-06-04	$i^{\prime }$	CC2	0.94 $\pm$ 0.04	2.42 $\pm$ 0.05	72 $\pm$ 4	11.5	M
J13162169+2905548	2015-06-04	$i^{\prime }$	CC1	1.22 $\pm$ 0.08	0.30 $\pm$ 0.03	77 $\pm$ 2	11.8	M
J13252836+3743098	2014-06-14	$i^{\prime }$	CC1	2.83 $\pm$ 0.07	2.91 $\pm$ 0.02	96 $\pm$ 3	10.2	H
J13252836+3743098	2015-03-08	$i^{\prime }$	CC1	2.88 $\pm$ 0.09	2.91 $\pm$ 0.03	98 $\pm$ 4	13.0	H
J13252836+3743098	2015-06-04	$i^{\prime }$	CC1	2.84 $\pm$ 0.08	2.89 $\pm$ 0.03	98 $\pm$ 1	10.7	H
J13252836+3743098	2015-06-04	$i^{\prime }$	CC1	2.99 $\pm$ 0.17	2.57 $\pm$ 0.06	96 $\pm$ 3	7.9	H
J13260267+2735021	2015-06-06	$i^{\prime }$	CC1	0.70 $\pm$ 0.03	1.49 $\pm$ 0.05	218 $\pm$ 3	9.7	H
J13282890+0514353	2014-06-15	$i^{\prime }$	CC1	3.18 $\pm$ 0.26	0.93 $\pm$ 0.01	250 $\pm$ 4	8.2	H
J13324347+1114521	2014-06-14	$i^{\prime }$	CC1	3.78 $\pm$ 0.06	1.45 $\pm$ 0.05	86 $\pm$ 1	9.6	H
J13324347+1114521	2014-07-13	$i^{\prime }$	CC1	3.11 $\pm$ 0.03	1.44 $\pm$ 0.04	87 $\pm$ 1	11.6	H
J13324347+1114521	2014-07-13	$i^{\prime }$	CC1	3.52 $\pm$ 0.05	1.44 $\pm$ 0.03	87 $\pm$ 3	10.5	H
J13324347+1114521	2014-07-13	$i^{\prime }$	CC1	4.47 $\pm$ 0.04	1.44 $\pm$ 0.01	87 $\pm$ 5	8.0	H
J13324347+1114521	2015-03-08	$i^{\prime }$	CC1	3.62 $\pm$ 0.02	1.45 $\pm$ 0.05	83 $\pm$ 3	9.9	H
J13324347+1114521	2015-06-04	$i^{\prime }$	CC1	3.67 $\pm$ 0.07	1.45 $\pm$ 0.04	86 $\pm$ 1	11.0	H
J13324460+1648397	2015-06-08	$i^{\prime }$	CC1	0.38 $\pm$ 0.04	2.83 $\pm$ 0.04	53 $\pm$ 3	10.6	H
J13373037–1048346	2015-06-12	$i^{\prime }$	CC1	1.28 $\pm$ 0.21	0.41 $\pm$ 0.02	325 $\pm$ 2	5.9	H
J13375120+4808174	2014-06-15	$i^{\prime }$	CC1	0.74 $\pm$ 0.03	1.63 $\pm$ 0.04	334 $\pm$ 4	13.1	H
J13375120+4808174	2014-06-15	$i^{\prime }$	CC1	0.75 $\pm$ 0.04	1.64 $\pm$ 0.03	334 $\pm$ 3	13.2	H
J13375120+4808174	2015-03-08	$i^{\prime }$	CC1	0.74 $\pm$ 0.05	1.66 $\pm$ 0.06	337 $\pm$ 3	12.1	H
J13375120+4808174	2015-06-03	$i^{\prime }$	CC1	0.72 $\pm$ 0.04	1.63 $\pm$ 0.04	336 $\pm$ 2	6.8	H
J13420990–1600233	2015-06-05	$i^{\prime }$	CC1	1.00 $\pm$ 0.04	0.62 $\pm$ 0.03	40 $\pm$ 2	5.7	H
J13435058+5030053	2014-06-15	$i^{\prime }$	CC1	$\cdots$	1.08 $\pm$ 0.03	53 $\pm$ 4	13.2	H
J13435058+5030053	2015-03-08	$i^{\prime }$	CC1	0.27 $\pm$ 0.04	1.06 $\pm$ 0.06	50 $\pm$ 3	11.9	H
J13435058+5030053	2015-06-03	$i^{\prime }$	CC1	$\cdots$	1.07 $\pm$ 0.04	52 $\pm$ 3	5.9	L
J13474241+2127374	2015-06-07	$i^{\prime }$	CC1	2.00 $\pm$ 0.03	1.33 $\pm$ 0.04	150 $\pm$ 3	6.6	H
J13534589+5210298	2015-06-08	$i^{\prime }$	CC1	0.23 $\pm$ 0.05	1.06 $\pm$ 0.03	349 $\pm$ 3	6.6	H
J14040922+2044314	2014-03-23	$i^{\prime }$	CC1	0.77 $\pm$ 0.04	0.43 $\pm$ 0.05	359 $\pm$ 4	6.5	H
J14040922+2044314	2014-06-13	$i^{\prime }$	CC1	1.26 $\pm$ 0.04	0.46 $\pm$ 0.03	358 $\pm$ 4	7.6	H
J14040922+2044314	2014-07-19	$i^{\prime }$	CC1	0.25 $\pm$ 0.02	0.40 $\pm$ 0.03	354 $\pm$ 2	10.9	H
J14040922+2044314	2015-03-08	$i^{\prime }$	CC1	0.46 $\pm$ 0.05	0.42 $\pm$ 0.02	2 $\pm$ 3	9.8	H
J14105956+0751398	2014-06-15	$i^{\prime }$	CC1	$\cdots$	1.38 $\pm$ 0.03	298 $\pm$ 2	7.4	H
J14105956+0751398	2015-03-09	$i^{\prime }$	CC1	0.23 $\pm$ 0.03	1.33 $\pm$ 0.05	294 $\pm$ 5	5.1	H
J14105956+0751398	2015-06-04	$i^{\prime }$	CC1	$\cdots$	1.34 $\pm$ 0.04	297 $\pm$ 3	5.6	L
J14141700–1521125	2015-03-09	$i^{\prime }$	CC1	1.76 $\pm$ 0.04	1.61 $\pm$ 0.02	76 $\pm$ 2	10.0	H
J14141700–1521125	2015-06-05	$i^{\prime }$	CC1	1.73 $\pm$ 0.04	1.61 $\pm$ 0.02	76 $\pm$ 3	10.5	H
J14170294+3142472	2015-03-08	$i^{\prime }$	CC1	0.95 $\pm$ 0.10	0.27 $\pm$ 0.03	175 $\pm$ 3	8.1	H
J14170837+5000081	2014-03-23	$i^{\prime }$	CC1	1.45 $\pm$ 0.06	1.70 $\pm$ 0.03	41 $\pm$ 3	4.6	L
J14170837+5000081	2014-06-13	$i^{\prime }$	CC1	1.55 $\pm$ 0.04	1.75 $\pm$ 0.05	39 $\pm$ 2	7.4	M
J14170837+5000081	2015-03-09	$i^{\prime }$	CC1	1.63 $\pm$ 0.05	1.69 $\pm$ 0.04	41 $\pm$ 2	12.3	H
J14170837+5000081	2015-06-04	$i^{\prime }$	CC1	1.65 $\pm$ 0.05	1.72 $\pm$ 0.03	41 $\pm$ 1	10.2	H
J14243178–0257158	2015-06-05	$i^{\prime }$	CC1	5.99 $\pm$ 0.08	3.85 $\pm$ 0.04	217 $\pm$ 3	37.5	H
J14303394+0305440	2015-06-08	$i^{\prime }$	CC1	2.81 $\pm$ 0.13	2.69 $\pm$ 0.02	160 $\pm$ 3	9.1	H
J14373999+6745316	2015-06-04	$i^{\prime }$	CC1	1.34 $\pm$ 0.06	0.88 $\pm$ 0.04	112 $\pm$ 2	4.1	M
J14373999+6745316	2015-06-04	$i^{\prime }$	CC1	1.42 $\pm$ 0.06	0.85 $\pm$ 0.03	112 $\pm$ 4	3.9	M
J14433804–0414354	2015-03-08	$i^{\prime }$	CC1	0.27 $\pm$ 0.03	1.01 $\pm$ 0.02	286 $\pm$ 3	5.4	H
J14433804–0414354	2015-06-05	$i^{\prime }$	CC1	0.25 $\pm$ 0.02	1.04 $\pm$ 0.03	286 $\pm$ 1	6.2	H
J14445989+5309251	2015-06-03	$i^{\prime }$	CC1	0.43 $\pm$ 0.03	0.86 $\pm$ 0.03	54 $\pm$ 2	5.3	H
J14514497–0530407	2015-06-05	$i^{\prime }$	CC1	1.38 $\pm$ 0.04	0.48 $\pm$ 0.02	48 $\pm$ 4	8.4	H
J15005557+4525343	2015-06-06	$i^{\prime }$	CC1	3.13 $\pm$ 0.04	2.03 $\pm$ 0.03	165 $\pm$ 2	9.8	H
J15072382+4333531	2014-06-13	$i^{\prime }$	CC1	0.98 $\pm$ 0.14	0.55 $\pm$ 0.04	312 $\pm$ 3	4.9	M
J15072382+4333531	2014-07-16	$i^{\prime }$	CC1	1.06 $\pm$ 0.12	0.57 $\pm$ 0.03	311 $\pm$ 3	8.1	H
J15072382+4333531	2015-03-08	$i^{\prime }$	CC1	1.13 $\pm$ 0.13	0.55 $\pm$ 0.04	317 $\pm$ 3	6.7	H
J15072382+4333531	2015-06-03	$i^{\prime }$	CC1	1.25 $\pm$ 0.11	0.60 $\pm$ 0.02	322 $\pm$ 4	5.5	M
J15114542+1014222	2015-06-08	$i^{\prime }$	CC1	0.86 $\pm$ 0.05	1.92 $\pm$ 0.03	250 $\pm$ 3	11.0	H
J15123818+4543464	2014-03-24	$i^{\prime }$	CC1	0.74 $\pm$ 0.13	0.54 $\pm$ 0.03	217 $\pm$ 2	6.0	H
J15123818+4543464	2015-03-08	$i^{\prime }$	CC1	0.77 $\pm$ 0.09	0.54 $\pm$ 0.05	217 $\pm$ 3	6.5	H
J15123818+4543464	2015-06-03	$i^{\prime }$	CC1	1.00 $\pm$ 0.05	0.56 $\pm$ 0.04	217 $\pm$ 3	5.8	M
J15154371–0725208	2015-06-05	$i^{\prime }$	CC1	0.07 $\pm$ 0.03	0.60 $\pm$ 0.03	193 $\pm$ 3	5.7	H
J15233660+3837489	2014-03-23	$i^{\prime }$	CC1	0.47 $\pm$ 0.07	0.62 $\pm$ 0.02	356 $\pm$ 4	5.4	H
J15233660+3837489	2014-06-13	$i^{\prime }$	CC1	0.65 $\pm$ 0.04	0.64 $\pm$ 0.05	357 $\pm$ 2	6.5	H
J15233660+3837489	2014-07-16	$i^{\prime }$	CC1	0.69 $\pm$ 0.05	0.67 $\pm$ 0.03	0 $\pm$ 1	13.4	H
J15233660+3837489	2015-03-08	$i^{\prime }$	CC1	0.60 $\pm$ 0.04	0.64 $\pm$ 0.04	1 $\pm$ 3	6.8	H
J15233660+3837489	2015-06-03	$i^{\prime }$	CC1	0.86 $\pm$ 0.05	0.69 $\pm$ 0.06	5 $\pm$ 2	5.4	M
J15402840–1841460	2015-03-09	$i^{\prime }$	CC1	1.09 $\pm$ 0.05	0.76 $\pm$ 0.03	37 $\pm$ 4	5.9	H
J15422038+5936528	2014-06-15	$i^{\prime }$	CC1	3.48 $\pm$ 0.07	1.58 $\pm$ 0.04	247 $\pm$ 1	10.2	M
J15422038+5936528	2014-07-16	$i^{\prime }$	CC1	3.12 $\pm$ 0.04	1.66 $\pm$ 0.03	245 $\pm$ 2	13.1	M
J15422038+5936528	2014-07-16	$i^{\prime }$	CC1	3.40 $\pm$ 0.05	1.66 $\pm$ 0.04	245 $\pm$ 1	10.4	M
J15422038+5936528	2015-03-08	$i^{\prime }$	CC1	3.61 $\pm$ 0.04	1.72 $\pm$ 0.04	245 $\pm$ 3	9.6	L
J15422038+5936528	2015-06-03	$i^{\prime }$	CC1	3.22 $\pm$ 0.21	1.52 $\pm$ 0.03	246 $\pm$ 2	4.4	L
J15424184+8005306	2015-03-08	$i^{\prime }$	CC1	0.24 $\pm$ 0.03	2.08 $\pm$ 0.02	240 $\pm$ 3	7.2	M
J15424184+8005306	2015-06-05	$i^{\prime }$	CC1	0.22 $\pm$ 0.05	2.05 $\pm$ 0.06	242 $\pm$ 1	9.2	H
J15452354+7514548	2015-06-12	$i^{\prime }$	CC1	0.58 $\pm$ 0.04	0.96 $\pm$ 0.03	143 $\pm$ 2	6.3	M
J15521824+3414537	2014-03-23	$i^{\prime }$	CC1	0.15 $\pm$ 0.03	1.80 $\pm$ 0.03	107 $\pm$ 3	6.5	H
J15521824+3414537	2015-03-08	$i^{\prime }$	CC1	0.15 $\pm$ 0.04	1.82 $\pm$ 0.03	108 $\pm$ 2	6.4	M
J15521824+3414537	2015-06-03	$i^{\prime }$	CC1	0.16 $\pm$ 0.03	1.87 $\pm$ 0.02	107 $\pm$ 3	5.2	H
J15553178+3512028	2014-03-25	$i^{\prime }$	CC1	2.07 $\pm$ 0.02	1.64 $\pm$ 0.04	252 $\pm$ 1	10.4	H
J15553178+3512028	2014-06-13	$i^{\prime }$	CC1	2.04 $\pm$ 0.02	1.61 $\pm$ 0.04	253 $\pm$ 3	12.1	H
J15553178+3512028	2014-06-13	$i^{\prime }$	CC1	2.10 $\pm$ 0.02	1.61 $\pm$ 0.04	253 $\pm$ 3	11.9	H
J15553178+3512028	2014-06-13	$i^{\prime }$	CC2	2.21 $\pm$ 0.06	1.87 $\pm$ 0.03	107 $\pm$ 2	8.0	L
J15553178+3512028	2015-03-08	$i^{\prime }$	CC1	2.13 $\pm$ 0.03	1.57 $\pm$ 0.04	253 $\pm$ 2	8.5	M
J15553178+3512028	2015-06-03	$i^{\prime }$	CC1	2.03 $\pm$ 0.03	1.67 $\pm$ 0.04	252 $\pm$ 1	7.6	H
J15575497+6010263	2014-06-16	$i^{\prime }$	CC1	0.62 $\pm$ 0.04	0.70 $\pm$ 0.03	297 $\pm$ 2	3.6	H
J15575497+6010263	2014-07-18	$i^{\prime }$	CC1	0.45 $\pm$ 0.04	0.73 $\pm$ 0.03	300 $\pm$ 4	5.7	H
J15575497+6010263	2015-03-08	$i^{\prime }$	CC1	0.46 $\pm$ 0.04	0.70 $\pm$ 0.02	299 $\pm$ 2	4.7	H
J15575497+6010263	2015-06-03	$i^{\prime }$	CC1	0.46 $\pm$ 0.03	0.72 $\pm$ 0.05	299 $\pm$ 4	4.6	H
J16015690+1825127	2014-03-24	$i^{\prime }$	CC1	4.79 $\pm$ 0.05	1.25 $\pm$ 0.04	156 $\pm$ 2	10.0	H
J16043736+7022142	2015-06-12	$i^{\prime }$	CC1	0.72 $\pm$ 0.02	0.76 $\pm$ 0.05	5 $\pm$ 2	4.7	H
J16060319+0333215	2014-06-15	$i^{\prime }$	CC1	1.02 $\pm$ 0.14	0.56 $\pm$ 0.05	305 $\pm$ 3	5.7	H
J16060319+0333215	2015-03-08	$i^{\prime }$	CC1	1.10 $\pm$ 0.10	0.60 $\pm$ 0.02	304 $\pm$ 5	4.9	H
J16060319+0333215	2015-06-04	$i^{\prime }$	CC1	0.96 $\pm$ 0.10	0.59 $\pm$ 0.04	298 $\pm$ 2	4.4	M
J16102225+4509347	2014-06-14	$i^{\prime }$	CC1	3.10 $\pm$ 0.04	2.43 $\pm$ 0.03	59 $\pm$ 3	7.1	M
J16102225+4509347	2014-07-16	$i^{\prime }$	CC1	3.13 $\pm$ 0.02	2.39 $\pm$ 0.03	60 $\pm$ 2	13.8	H
J16102225+4509347	2015-03-08	$i^{\prime }$	CC1	3.10 $\pm$ 0.02	2.38 $\pm$ 0.03	59 $\pm$ 4	9.6	H
J16102225+4509347	2015-06-03	$i^{\prime }$	CC1	3.24 $\pm$ 0.05	2.41 $\pm$ 0.05	60 $\pm$ 2	8.1	M
J16171135+7733477	2015-06-05	$i^{\prime }$	CC1	1.95 $\pm$ 0.04	0.81 $\pm$ 0.04	263 $\pm$ 2	8.3	H
J16250150–1215254	2015-03-08	$i^{\prime }$	CC1	0.99 $\pm$ 0.10	0.31 $\pm$ 0.03	105 $\pm$ 3	7.0	H
J16455062+0343014	2014-06-15	$i^{\prime }$	CC1	3.52 $\pm$ 0.04	2.06 $\pm$ 0.05	188 $\pm$ 3	17.6	H
J16455062+0343014	2014-07-17	$i^{\prime }$	CC1	3.48 $\pm$ 0.02	2.05 $\pm$ 0.03	189 $\pm$ 2	29.8	H
J16455062+0343014	2014-07-17	$i^{\prime }$	CC1	3.48 $\pm$ 0.03	2.02 $\pm$ 0.04	188 $\pm$ 4	31.5	H
J16455062+0343014	2014-07-17	$i^{\prime }$	CC1	3.48 $\pm$ 0.03	2.05 $\pm$ 0.03	187 $\pm$ 1	25.6	H
J16455062+0343014	2015-03-08	$i^{\prime }$	CC1	3.47 $\pm$ 0.03	2.04 $\pm$ 0.03	188 $\pm$ 3	10.4	H
J16455062+0343014	2015-06-04	$i^{\prime }$	CC1	3.45 $\pm$ 0.04	2.10 $\pm$ 0.05	187 $\pm$ 3	7.7	H
J16510995+3555071	2014-06-15	$i^{\prime }$	CC1	1.55 $\pm$ 0.09	1.07 $\pm$ 0.04	316 $\pm$ 2	7.2	L
J16510995+3555071	2014-07-13	$i^{\prime }$	CC1	1.70 $\pm$ 0.04	1.08 $\pm$ 0.04	320 $\pm$ 2	13.2	M
J16510995+3555071	2015-03-08	$i^{\prime }$	CC1	1.60 $\pm$ 0.08	1.04 $\pm$ 0.02	316 $\pm$ 3	7.5	H
J16510995+3555071	2015-06-03	$i^{\prime }$	CC1	1.65 $\pm$ 0.04	1.09 $\pm$ 0.04	318 $\pm$ 3	7.3	L
J16582055+0733079	2015-06-02	$i^{\prime }$	CC1	1.08 $\pm$ 0.11	0.50 $\pm$ 0.03	131 $\pm$ 4	5.1	M
J16582055+0733079	2015-06-04	$i^{\prime }$	CC1	1.07 $\pm$ 0.11	0.52 $\pm$ 0.03	136 $\pm$ 4	5.9	M
J17021204+5103284	2014-07-18	$i^{\prime }$	CC1	0.33 $\pm$ 0.05	0.78 $\pm$ 0.02	62 $\pm$ 3	11.9	H
J17021204+5103284	2015-03-09	$i^{\prime }$	CC1	0.34 $\pm$ 0.03	0.75 $\pm$ 0.03	61 $\pm$ 3	9.2	H
J17021204+5103284	2015-06-03	$i^{\prime }$	CC1	0.50 $\pm$ 0.04	0.81 $\pm$ 0.04	60 $\pm$ 2	7.8	L
J17035283+3211456	2015-03-08	$i^{\prime }$	CC1	2.18 $\pm$ 0.04	1.44 $\pm$ 0.03	150 $\pm$ 1	5.7	H
J17035283+3211456	2015-03-09	$i^{\prime }$	CC1	1.96 $\pm$ 0.02	1.43 $\pm$ 0.04	149 $\pm$ 3	9.8	H
J17035283+3211456	2015-06-06	$i^{\prime }$	CC1	2.13 $\pm$ 0.05	1.40 $\pm$ 0.03	148 $\pm$ 2	5.4	H
J17152512+1328342	2015-06-04	$i^{\prime }$	CC1	0.53 $\pm$ 0.05	0.74 $\pm$ 0.05	222 $\pm$ 2	6.1	M
J17183470+3400290	2015-06-02	$i^{\prime }$	CC1	2.05 $\pm$ 0.03	1.32 $\pm$ 0.03	83 $\pm$ 4	6.3	M
J17183470+3400290	2015-06-03	$i^{\prime }$	CC1	2.15 $\pm$ 0.04	1.20 $\pm$ 0.03	84 $\pm$ 3	6.3	M
J17340562+4447082	2014-03-25	$i^{\prime }$	CC1	0.35 $\pm$ 0.05	0.59 $\pm$ 0.04	145 $\pm$ 2	7.4	H
J17340562+4447082	2015-03-08	$i^{\prime }$	CC1	0.42 $\pm$ 0.02	0.63 $\pm$ 0.03	143 $\pm$ 1	8.0	H
J17340562+4447082	2015-06-03	$i^{\prime }$	CC1	0.47 $\pm$ 0.03	0.64 $\pm$ 0.02	144 $\pm$ 3	6.4	L
J17380077+3329457	2014-03-24	$i^{\prime }$	CC1	0.87 $\pm$ 0.03	0.97 $\pm$ 0.04	151 $\pm$ 3	9.3	H
J17380077+3329457	2015-03-08	$i^{\prime }$	CC1	0.88 $\pm$ 0.03	1.00 $\pm$ 0.04	151 $\pm$ 4	8.5	H
J17380077+3329457	2015-06-03	$i^{\prime }$	CC1	0.83 $\pm$ 0.02	0.97 $\pm$ 0.05	151 $\pm$ 2	5.9	H
J17530062+1655029	2015-06-05	$i^{\prime }$	CC1	0.44 $\pm$ 0.05	0.88 $\pm$ 0.04	112 $\pm$ 3	4.8	H
J17544786+4109310	2014-06-13	$i^{\prime }$	CC1	3.81 $\pm$ 0.21	0.83 $\pm$ 0.03	101 $\pm$ 4	9.0	H
J17544786+4109310	2014-07-13	$i^{\prime }$	CC1	3.17 $\pm$ 0.27	0.84 $\pm$ 0.03	104 $\pm$ 4	7.5	H
J17544786+4109310	2014-07-13	$i^{\prime }$	CC1	3.54 $\pm$ 0.19	0.84 $\pm$ 0.05	104 $\pm$ 4	8.6	H
J17544786+4109310	2014-07-13	$i^{\prime }$	CC1	5.12 $\pm$ 0.58	0.84 $\pm$ 0.03	104 $\pm$ 2	8.0	H
J17544786+4109310	2015-03-08	$i^{\prime }$	CC1	3.67 $\pm$ 0.31	0.80 $\pm$ 0.04	104 $\pm$ 1	7.8	H
J18132028+0751536	2015-06-12	$i^{\prime }$	CC1	0.19 $\pm$ 0.04	0.98 $\pm$ 0.02	34 $\pm$ 3	5.0	H
J18254891+0409280	2014-08-28	$i^{\prime }$	CC1	5.12 $\pm$ 0.05	3.62 $\pm$ 0.03	181 $\pm$ 1	21.1	H
J18320290+2030581	2015-06-02	$i^{\prime }$	CC1	0.78 $\pm$ 0.21	1.38 $\pm$ 0.02	19 $\pm$ 2	3.7	L
J18320290+2030581	2015-06-07	$i^{\prime }$	CC1	0.42 $\pm$ 0.04	1.43 $\pm$ 0.04	18 $\pm$ 3	5.0	L
J19011166+2550384	2015-06-06	$i^{\prime }$	CC1	1.73 $\pm$ 0.05	1.34 $\pm$ 0.04	142 $\pm$ 1	5.8	H
J19031729+6359341	2014-08-27	$i^{\prime }$	CC1	2.36 $\pm$ 0.04	3.69 $\pm$ 0.03	64 $\pm$ 2	19.9	H
J19133270+5644363	2015-06-08	$i^{\prime }$	CC1	0.56 $\pm$ 0.05	1.17 $\pm$ 0.03	167 $\pm$ 3	5.7	H
J19205158+1903362	2015-06-10	$i^{\prime }$	CC1	1.11 $\pm$ 0.08	0.51 $\pm$ 0.04	196 $\pm$ 1	5.1	M
J19370113+3147214	2014-08-23	$i^{\prime }$	CC1	0.20 $\pm$ 0.08	0.51 $\pm$ 0.02	303 $\pm$ 3	5.1	H
J19370113+3147214	2015-06-05	$i^{\prime }$	CC1	0.30 $\pm$ 0.03	0.48 $\pm$ 0.04	296 $\pm$ 2	5.7	H
J19433674+3225206	2014-09-03	$i^{\prime }$	CC1	0.78 $\pm$ 0.09	0.40 $\pm$ 0.03	73 $\pm$ 2	13.3	H
J19471438+6402377	2014-09-03	$i^{\prime }$	CC1	1.14 $\pm$ 0.14	0.17 $\pm$ 0.03	203 $\pm$ 4	5.4	H
J19515537+3811071	2015-06-08	$i^{\prime }$	CC1	2.34 $\pm$ 0.04	2.32 $\pm$ 0.03	69 $\pm$ 2	9.6	H
J19543755+2013065	2014-09-03	$i^{\prime }$	CC1	5.47 $\pm$ 0.05	4.20 $\pm$ 0.03	113 $\pm$ 3	5.9	H
J20013373+2814101	2013-10-25	$i^{\prime }$	CC1	0.25 $\pm$ 0.02	1.54 $\pm$ 0.05	119 $\pm$ 2	7.6	H
J20013373+2814101	2014-08-24	$i^{\prime }$	CC1	0.27 $\pm$ 0.05	1.52 $\pm$ 0.03	120 $\pm$ 1	6.9	H
J20013373+2814101	2015-06-05	$i^{\prime }$	CC1	0.24 $\pm$ 0.03	1.54 $\pm$ 0.04	121 $\pm$ 4	5.2	H
J20194925+2256367	2014-08-24	$i^{\prime }$	CC1	1.81 $\pm$ 0.02	1.96 $\pm$ 0.02	357 $\pm$ 3	26.3	H
J20322012+5047455	2014-07-18	$i^{\prime }$	CC1	1.47 $\pm$ 0.03	0.82 $\pm$ 0.02	157 $\pm$ 1	11.1	H
J20393474+4822450	2014-07-16	$i^{\prime }$	CC1	1.85 $\pm$ 0.03	1.86 $\pm$ 0.04	122 $\pm$ 1	9.8	H
J20393474+4822450	2015-06-08	$i^{\prime }$	CC1	1.74 $\pm$ 0.05	1.84 $\pm$ 0.03	122 $\pm$ 3	5.6	H
J20395460+0620118	2014-08-26	$i^{\prime }$	CC1	4.41 $\pm$ 0.21	2.48 $\pm$ 0.05	334 $\pm$ 2	5.4	H
J20422203+5311332	2014-07-16	$i^{\prime }$	CC1	1.34 $\pm$ 0.12	0.29 $\pm$ 0.03	36 $\pm$ 2	7.5	H
J20424915+4122599	2014-07-16	$i^{\prime }$	CC1	0.91 $\pm$ 0.08	0.48 $\pm$ 0.04	143 $\pm$ 3	8.3	M
J20424915+4122599	2014-08-22	$i^{\prime }$	CC1	1.34 $\pm$ 0.07	0.57 $\pm$ 0.01	141 $\pm$ 1	6.5	M
J20560274–1710538	2014-08-28	$i^{\prime }$	CC1	2.62 $\pm$ 0.04	2.21 $\pm$ 0.04	139 $\pm$ 1	13.1	H
J21000529+4004136	2015-06-06	$i^{\prime }$	CC1	1.77 $\pm$ 0.03	0.89 $\pm$ 0.05	56 $\pm$ 1	7.5	H
J21010182+2615397	2014-07-16	$i^{\prime }$	CC1	0.19 $\pm$ 0.05	0.43 $\pm$ 0.03	99 $\pm$ 2	6.7	H
J21143673+1952557	2013-10-25	$i^{\prime }$	CC1	3.93 $\pm$ 0.03	2.86 $\pm$ 0.04	133 $\pm$ 3	12.3	H
J21143673+1952557	2014-07-16	$i^{\prime }$	CC1	3.93 $\pm$ 0.04	2.86 $\pm$ 0.02	132 $\pm$ 3	16.2	H
J21143673+1952557	2014-11-07	$i^{\prime }$	CC1	3.51 $\pm$ 0.03	2.86 $\pm$ 0.02	133 $\pm$ 3	14.8	H
J21143673+1952557	2014-11-07	$i^{\prime }$	CC1	3.89 $\pm$ 0.05	2.86 $\pm$ 0.04	133 $\pm$ 2	14.7	H
J21175904+3404301	2014-07-13	$i^{\prime }$	CC1	1.59 $\pm$ 0.06	1.12 $\pm$ 0.02	293 $\pm$ 3	5.5	H
J21175904+3404301	2015-06-05	$i^{\prime }$	CC1	1.57 $\pm$ 0.05	1.12 $\pm$ 0.04	292 $\pm$ 1	5.0	H
J21294054+6405399	2014-08-22	$i^{\prime }$	CC1	2.14 $\pm$ 0.05	2.44 $\pm$ 0.03	320 $\pm$ 3	11.0	M
J21322198+2433419	2014-07-16	$i^{\prime }$	CC1	0.25 $\pm$ 0.04	1.55 $\pm$ 0.03	240 $\pm$ 2	9.1	H
J21363852+3927206	2013-10-24	$LP600$	CC1	1.31 $\pm$ 0.02	1.09 $\pm$ 0.02	263 $\pm$ 3	11.9	H
J21374019+0137137	2014-07-17	$i^{\prime }$	CC1	0.90 $\pm$ 0.19	0.42 $\pm$ 0.03	345 $\pm$ 4	8.8	H
J21411161–1011001	2014-11-11	$i^{\prime }$	CC1	1.24 $\pm$ 0.02	1.02 $\pm$ 0.02	14 $\pm$ 2	6.5	H
J21501406+0922295	2014-11-08	$i^{\prime }$	CC1	3.06 $\pm$ 0.04	1.51 $\pm$ 0.02	332 $\pm$ 4	11.1	H
J21512893–0238147	2014-08-22	$i^{\prime }$	CC1	1.72 $\pm$ 0.04	1.43 $\pm$ 0.02	255 $\pm$ 4	8.5	H
J21521039+0537356	2014-07-17	$i^{\prime }$	CC1	1.99 $\pm$ 0.22	0.64 $\pm$ 0.01	16 $\pm$ 4	6.3	H
J21543507+5445122	2014-07-13	$i^{\prime }$	CC1	1.23 $\pm$ 0.03	3.19 $\pm$ 0.05	72 $\pm$ 4	23.1	H
J21552437+5938371	2014-08-23	$i^{\prime }$	CC1	1.72 $\pm$ 0.09	0.36 $\pm$ 0.02	76 $\pm$ 3	16.9	H
J22073842–0650034	2014-11-10	$i^{\prime }$	CC1	1.87 $\pm$ 0.06	0.95 $\pm$ 0.05	287 $\pm$ 3	8.2	H
J22300418+4851347	2013-10-25	$i^{\prime }$	CC1	1.21 $\pm$ 0.04	2.32 $\pm$ 0.04	251 $\pm$ 4	16.2	H
J22413501+1849277	2014-11-06	$i^{\prime }$	CC1	2.64 $\pm$ 0.22	0.23 $\pm$ 0.03	264 $\pm$ 3	6.5	H
J22413577+2602128	2013-07-25	$i^{\prime }$	CC1	6.81 $\pm$ 0.08	3.70 $\pm$ 0.04	72 $\pm$ 2	13.4	H
J22413577+2602128	2014-08-22	$i^{\prime }$	CC1	7.11 $\pm$ 0.22	3.62 $\pm$ 0.04	74 $\pm$ 2	9.2	H
J22413577+2602128	2014-08-22	$i^{\prime }$	CC1	7.60 $\pm$ 0.43	3.62 $\pm$ 0.02	74 $\pm$ 2	5.7	H
J22424884+1330532	2014-07-13	$i^{\prime }$	CC1	0.23 $\pm$ 0.03	2.24 $\pm$ 0.03	309 $\pm$ 2	13.1	H
J22594127+2154070	2014-07-12	$i^{\prime }$	CC1	2.88 $\pm$ 0.05	2.28 $\pm$ 0.04	36 $\pm$ 3	6.2	H
J22594127+2154070	2014-08-22	$i^{\prime }$	CC1	3.02 $\pm$ 0.04	2.28 $\pm$ 0.04	36 $\pm$ 1	8.9	H
J22594127+2154070	2014-08-23	$i^{\prime }$	CC1	3.02 $\pm$ 0.06	2.27 $\pm$ 0.02	36 $\pm$ 2	11.9	H
J22594127+2154070	2014-11-06	$i^{\prime }$	CC1	3.01 $\pm$ 0.04	2.24 $\pm$ 0.04	36 $\pm$ 1	7.1	H
J23002791–2618431	2014-11-11	$i^{\prime }$	CC1	0.56 $\pm$ 0.03	2.27 $\pm$ 0.04	237 $\pm$ 2	8.0	H
J23024391+7506019	2014-11-10	$i^{\prime }$	CC1	0.91 $\pm$ 0.04	3.73 $\pm$ 0.04	208 $\pm$ 2	16.6	H
J23040837+0318214	2014-07-17	$i^{\prime }$	CC1	4.23 $\pm$ 0.04	2.16 $\pm$ 0.05	300 $\pm$ 2	8.2	H
J23040837+0318214	2014-08-22	$i^{\prime }$	CC1	3.65 $\pm$ 0.05	2.20 $\pm$ 0.05	300 $\pm$ 1	9.5	H
J23040837+0318214	2014-08-22	$i^{\prime }$	CC1	4.33 $\pm$ 0.03	2.20 $\pm$ 0.04	300 $\pm$ 2	8.8	H
J23040837+0318214	2014-08-22	$i^{\prime }$	CC2	5.73 $\pm$ 0.04	3.73 $\pm$ 0.02	208 $\pm$ 3	6.4	H
J23060295–1556151	2014-11-10	$i^{\prime }$	CC1	0.22 $\pm$ 0.04	0.81 $\pm$ 0.05	25 $\pm$ 3	6.8	H
J23062378+1236269	2013-10-24	$i^{\prime }$	CC1	0.47 $\pm$ 0.06	0.46 $\pm$ 0.04	329 $\pm$ 4	6.9	H
J23062378+1236269	2014-07-16	$i^{\prime }$	CC1	0.61 $\pm$ 0.05	0.43 $\pm$ 0.03	334 $\pm$ 2	6.8	H
J23220944+5756296	2013-10-25	$i^{\prime }$	CC1	1.62 $\pm$ 0.29	0.35 $\pm$ 0.04	312 $\pm$ 3	9.6	H
J23450477+1458573	2014-07-12	$i^{\prime }$	CC1	0.33 $\pm$ 0.03	1.15 $\pm$ 0.03	180 $\pm$ 4	6.0	H
J23450477+1458573	2014-11-08	$i^{\prime }$	CC1	$\cdots$	1.16 $\pm$ 0.03	178 $\pm$ 2	14.9	H
J23473777–2316060	2014-11-10	$i^{\prime }$	CC1	-0.10 $\pm$ 0.05	1.24 $\pm$ 0.03	64 $\pm$ 2	7.7	H
J23574989+3837468	2013-10-25	$i^{\prime }$	CC1	1.41 $\pm$ 0.21	0.47 $\pm$ 0.05	231 $\pm$ 1	11.0	H
J23574989+3837468	2014-11-06	$i^{\prime }$	CC1	1.80 $\pm$ 0.08	0.48 $\pm$ 0.05	228 $\pm$ 3	6.6	H
J23581366–1724338	2014-11-10	$i^{\prime }$	CC1	0.03 $\pm$ 0.03	2.09 $\pm$ 0.03	176 $\pm$ 2	22.5	H
J23590042+2051387	2014-07-12	$i^{\prime }$	CC1	0.94 $\pm$ 0.05	0.56 $\pm$ 0.03	168 $\pm$ 2	5.9	H

Table 5. Table 5: Binary Common Proper Motion Tests

2MASS	$N_{\mathrm{epochs}}$	$\Delta t$	Cand.	${\chi }_{\nu }^2$	${\chi }_{\nu }^2$	$\nu$	BIC	BIC	$\Delta$BIC	Comp?aaStatus of companion based on differenced Bayesian Information Criterion for the common proper motion and background hypotheses. “SE”=Single Epoch; “BG”=background; “CPM”=Common Proper Motion. See Section 4.2 for details.	Known	Binary
Name		(yr)	Comp.	(BG)	(CPM)		(BG)	(CPM)			Binary?	Ref.
J00074264+6022543	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja14b, Bo15b
J00133841+5245050	3	0.197	CC1	0.352	0.426	2	6.20	6.35	-0.148	BG?	N	$\cdots$
J00133841+5245050	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J00160486+2319090	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J00164045+3000598	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J00165678+2003551	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J00171046+2931520	2	0.847	CC1	0.307	0.293	1	3.77	3.76	0.0133	CPM?	N	$\cdots$
J00215781+4912379	4	0.828	CC1	14.1	0.795	3	49.2	9.32	39.9	CPM	Y	Bo15b
J00215781+4912379	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J00233468+2014282	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J00285391+5022330	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Dae07
J00302927+0420204	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J00323480+0729271	2	0.828	CC1	5.51	0.481	1	8.98	3.95	5.03	CPM	Y	Mc01
J00340843+2523498	2	0.836	CC1	2.49	0.0799	1	5.95	3.55	2.41	CPM?	Y	WDS
J00414141+4410530	2	1.04	CC1	14.9	4.26	1	18.4	7.73	10.6	CPM	Y	Ja12
J00423409+5439048	3	0.208	CC1	0.285	0.357	2	6.06	6.21	-0.144	BG?	N	$\cdots$
J00425668+2239350	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J00485822+4435091	2	1.04	CC1	16.1	2.46	1	19.5	5.93	13.6	CPM	Y	Mc01
J00503319+2449009	2	1.04	CC1	18.8	1.78	1	22.3	5.25	17.0	CPM	Y	WDS, Ja12
J00530648+4829385	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01001331+2135328	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01001613+1251007	2	0.830	CC1	0.670	0.156	1	4.14	3.62	0.515	CPM?	N	$\cdots$
J01034013+4051288	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01071194–1935359	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01093915+2931112	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01102943–1510071	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J01105436+5822133	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01112542+1526214	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Beu04
J01121854+4238358	3	0.833	CC1	2.53	0.0478	2	10.6	5.59	4.97	CPM	N	$\cdots$
J01121854+4238358	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01131976+5855224	2	0.839	CC1	3.17	0.0800	1	6.63	3.55	3.09	CPM	N	$\cdots$
J01132958–0738088	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J01244246–1540454	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01281337–2319278	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01304065–1027506	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J01373940+1835332	2	0.830	CC1	0.703	0.106	1	4.17	3.57	0.597	CPM?	Y	WDS
J01535076–1459503	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ber10
J01592349+5831162	5	1.04	CC1	0.414	49.5	4	9.70	206	-196	BG	N	$\cdots$
J01592349+5831162	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J02155892–0929121	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ber10, Bo15a
J02155892–0929121	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ber10, Bo15a
J02205082+3320479	2	0.830	CC1	8.19	0.200	1	11.7	3.67	7.99	CPM	N	$\cdots$
J02233670–1056138	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J02284694+1538535	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J02335984–1811525	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ber10
J02490228–1029220	2	$\cdots$	CC1	26.8	26.1	1	30.2	29.6	0.659	CPM?	Y	Ber10
J02560096+1220457	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J03033668–2535329	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ber10
J03092643+6732425	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J03144720+1127272	2	0.214	CC1	6.94	7.33	1	10.4	10.8	-0.383	BG?	N	$\cdots$
J03175221+5847431	3	0.828	CC1	2.14	0.114	2	9.77	5.72	4.05	CPM	N	$\cdots$
J03240643+2347073	4	1.05	CC1	7.14	2.50	3	28.3	14.4	13.9	CPM	Y	WDS
J03323578+2843554	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J03340048+5835551	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J03434696+5725557	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J03520223+2439479	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J04053888+0544408	2	0.828	CC1	5.53	0.692	1	9.00	4.16	4.84	CPM	Y	Mc01
J04074484+0945220	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04112810+7544231	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04132663–0139211	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Mc01
J04134585–0509049	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Bo15b
J04171645+1213557	2	0.830	CC1	4.96	2.00	1	8.43	5.47	2.96	CPM?	N	$\cdots$
J04174337–1754222	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04174431+4103137	2	0.844	CC1	2.29	1.17	1	5.76	4.64	1.11	CPM?	N	$\cdots$
J04214271–1657543	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04244805+1552292	2	1.04	CC1	25.9	0.940	1	29.3	4.41	24.9	CPM	Y	WDS
J04251456+1858250	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04282878+1741453	2	1.04	CC1	3.71	0.109	1	7.17	3.57	3.60	CPM	Y	Gu05
J04285080+1617204	3	0.830	CC1	0.643	0.281	2	6.78	6.06	0.724	CPM?	N	$\cdots$
J04285080+1617204	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04311384+2053436	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04325718+7407002	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04343992+1512325	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04350255+0839304	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04381255+2813001	2	1.04	CC1	53.7	0.00	1	57.2	3.47	53.7	CPM	Y	Beu04
J04385352+2147549	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja14b
J04412780+1404340	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04485498+5527185	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J04492947+4828459	2	1.05	CC1	32.4	1.29	1	35.8	4.76	31.1	CPM	Y	Ja14b
J04495635+2341029	2	0.844	CC1	2.28	0.860	1	5.74	4.33	1.42	CPM?	N	$\cdots$
J05024924+7352143	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J05122408+1824086	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J05195513–0723399	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J05252028+6510544	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J05285650+1231539	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J05341064+4732033	3	1.38	CC1	2.00	3.17	2	9.49	11.8	-2.34	BG?	N	$\cdots$
J05345873+6521435	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J05494518+2513331	2	0.839	CC1	7.03	4.20	1	10.5	7.67	2.83	CPM?	N	$\cdots$
J05554690+5123592	2	0.335	CC1	0.167	0.118	1	3.63	3.58	0.0490	CPM?	N	$\cdots$
J06073185+4712266	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J06084814+4257182	4	1.22	CC1	23.6	2.39	3	77.7	14.1	63.6	CPM	N	$\cdots$
J06101580+2119569	4	0.852	CC1	2.71	2.28	3	15.1	13.8	1.31	CPM?	N	$\cdots$
J06101580+2119569	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J06133437+4914051	3	1.38	CC1	1.42	0.198	2	8.33	5.89	2.44	CPM?	N	$\cdots$
J06462622+0521150	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J06584690+2843004	6	0.953	CC1	0.507	1.44	5	11.5	16.1	-4.65	BG	N	$\cdots$
J07120481+5423473	3	0.953	CC1	4.96	2.04	2	15.4	9.57	5.84	CPM	N	$\cdots$
J07140450+5043334	8	0.953	CC1	9.41	0.528	7	76.3	14.1	62.2	CPM	N	$\cdots$
J07140450+5043334	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J07161207+3315154	3	0.510	CC1	7.60	0.105	2	20.7	5.70	15.0	CPM	N	$\cdots$
J07194218+2954390	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J07315773+3613102	2	1.22	CC1	55.7	0.281	1	59.2	3.75	55.4	CPM	Y	Beu04
J07505369+4428181	3	1.23	CC1	12.3	0.359	2	30.1	6.21	23.9	CPM	Y	Ja12
J08010582+0334064	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J08014318+4959455	4	1.23	CC1	4.64	0.697	3	20.8	9.02	11.8	CPM	N	$\cdots$
J08083284+5304377	3	0.953	CC1	1.33	0.547	2	8.16	6.59	1.57	CPM?	N	$\cdots$
J08095207+0301106	2	0.321	CC1	1.03	0.400	1	4.50	3.87	0.634	CPM?	N	$\cdots$
J08310177+4012115	3	1.37	CC1	4.16	0.219	2	13.8	5.93	7.89	CPM	Y	WDS
J08444213+0044159	2	0.321	CC1	1.82	0.00	1	5.29	3.47	1.82	CPM?	N	$\cdots$
J08504234+0751517	3	0.324	CC1	2.84	0.557	2	11.2	6.61	4.57	CPM	Y	WDS
J08593592+5343505	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J09062111+1659235	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Sc98
J09132383+6852305	2	0.321	CC1	8.08	0.811	1	11.5	4.28	7.27	CPM	N	$\cdots$
J09174473+4612246	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J09192291+6203170	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J09200048+3052397	3	0.953	CC1	3.12	1.71	2	11.7	8.91	2.83	CPM?	N	$\cdots$
J09214911+4330284	2	0.953	CC1	60.2	0.347	1	63.7	3.81	59.9	CPM	Y	La08
J10024936+4827333	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J10043276+0533412	2	0.953	CC1	16.0	0.650	1	19.5	4.12	15.3	CPM	N	$\cdots$
J10143153+0213174	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J10143194+0606409	2	0.953	CC1	22.6	0.692	1	26.0	4.16	21.9	CPM	Y	WDS
J10150690+3125110	3	1.20	CC1	9.44	0.495	2	24.4	6.48	17.9	CPM	N	$\cdots$
J10452148+3830422	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J10482887+5852005	5	1.20	CC1	0.273	8.18	4	9.14	40.8	-31.6	BG	N	$\cdots$
J10482887+5852005	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J10571139+0544547	4	1.20	CC1	3.52	0.555	3	17.5	8.60	8.89	CPM	Y	Bo15b
J11030845+1517518	3	1.20	CC1	62.7	1.54	2	131.	8.57	122.	CPM	N	$\cdots$
J11161238+4942112	3	1.20	CC1	1.96	0.651	2	9.41	6.79	2.62	CPM?	N	$\cdots$
J11432359+2518137	2	0.956	CC1	20.8	0.222	1	24.2	3.69	20.5	CPM	N	$\cdots$
J11470543+7001588	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J11474897+0459160	6	1.20	CC1	2.77	0.367	5	22.8	10.8	12.0	CPM	N	$\cdots$
J11503435+2903407	3	1.20	CC1	8500	3.86	2	17000	13.2	17000	CPM	N	$\cdots$
J11504306+3312180	3	0.734	CC1	11.6	0.250	2	28.7	5.99	22.8	CPM	N	$\cdots$
J11504306+3312180	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J11504306+3312180	1	$\cdots$	CC3	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J12115308+1249135	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J12121136+4849032	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J12161505+5053376	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J12174539+0653230	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J12225061–0404462	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Bo15b
J13020587+1222215	3	0.970	CC1	20.6	0.483	2	46.7	6.46	40.3	CPM	Y	WDS
J13034595+2837205	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J13061537+2043444	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J13120689+3213179	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J13151846–0249516	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J13162169+2905548	2	0.241	CC1	0.378	1.29	1	3.84	4.75	-0.908	BG?	N	$\cdots$
J13162169+2905548	2	0.241	CC2	0.0900	0.118	1	3.56	3.58	-0.0276	BG?	Y	WDS
J13252836+3743098	4	0.973	CC1	45.2	9.92	3	142	36.7	106	CPM	Y	WDS
J13260267+2735021	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J13282890+0514353	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J13324347+1114521	6	0.973	CC1	2.49	0.326	5	21.4	10.6	10.8	CPM	N	$\cdots$
J13324460+1648397	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J13373037–1048346	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J13375120+4808174	4	0.967	CC1	1.45	0.258	3	11.3	7.70	3.59	CPM	Y	WDS
J13420990–1600233	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J13435058+5030053	3	0.967	CC1	2.84	0.264	2	11.2	6.02	5.14	CPM	N	$\cdots$
J13474241+2127374	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J13534589+5210298	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja12
J14040922+2044314	4	0.959	CC1	1560	0.735	3	4690	9.14	4680	CPM	Y	WDS
J14105956+0751398	3	0.970	CC1	0.516	1.00	2	6.52	7.50	-0.972	BG?	N	$\cdots$
J14141700–1521125	2	0.241	CC1	1.19	0.00	1	4.65	3.47	1.19	CPM?	N	$\cdots$
J14170294+3142472	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	De99
J14170837+5000081	4	1.20	CC1	1.67	0.435	3	11.9	8.24	3.69	CPM	N	$\cdots$
J14243178–0257158	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J14303394+0305440	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J14373999+6745316	2	$\cdots$	CC1	0.358	0.360	1	3.82	3.83	-0.00247	BG?	N	$\cdots$
J14433804–0414354	2	0.244	CC1	1.60	0.692	1	5.06	4.16	0.904	CPM?	Y	Ja12
J14445989+5309251	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J14514497–0530407	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J15005557+4525343	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J15072382+4333531	4	0.973	CC1	7.35	2.28	3	29.0	13.8	15.2	CPM	N	$\cdots$
J15114542+1014222	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J15123818+4543464	3	1.19	CC1	165.	0.0800	2	336	5.65	331	CPM	Y	Mc01
J15154371–0725208	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J15233660+3837489	5	1.20	CC1	10.1	2.38	4	48.4	17.6	30.8	CPM	N	$\cdots$
J15402840–1841460	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J15422038+5936528	5	0.967	CC1	4.88	3.88	4	27.6	23.6	3.99	CPM	N	$\cdots$
J15424184+8005306	2	0.244	CC1	0.837	0.625	1	4.30	4.09	0.212	CPM?	N	$\cdots$
J15452354+7514548	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J15521824+3414537	3	1.20	CC1	7.31	2.03	2	20.1	9.56	10.5	CPM	N	$\cdots$
J15553178+3512028	5	1.19	CC1	18.7	0.694	4	82.7	10.8	71.9	CPM	Y	Mc01
J15553178+3512028	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J15575497+6010263	4	0.964	CC1	2.41	0.589	3	14.2	8.70	5.48	CPM	N	$\cdots$
J16015690+1825127	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J16043736+7022142	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J16060319+0333215	3	0.970	CC1	17.9	2.28	2	41.2	10.1	31.2	CPM	N	$\cdots$
J16102225+4509347	4	0.970	CC1	0.633	0.850	3	8.83	9.48	-0.651	BG?	N	$\cdots$
J16171135+7733477	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J16250150–1215254	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J16455062+0343014	6	0.970	CC1	0.937	0.224	5	13.6	10.1	3.57	CPM	N	$\cdots$
J16510995+3555071	4	0.967	CC1	8.18	0.971	3	31.5	9.85	21.6	CPM	Y	Ja12
J16582055+0733079	2	0.00549	CC1	1.02	1.00	1	4.49	4.47	0.0177	CPM?	N	$\cdots$
J17021204+5103284	3	0.877	CC1	4.10	0.753	2	13.7	7.00	6.69	CPM	Y	Ja12
J17035283+3211456	3	0.246	CC1	1.24	0.914	2	7.97	7.32	0.648	CPM?	Y	Dae07
J17152512+1328342	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J17183470+3400290	2	0.00281	CC1	8.05	8.04	1	11.5	11.5	0.00714	CPM?	N	$\cdots$
J17340562+4447082	3	1.19	CC1	2.76	1.38	2	11.0	8.26	2.75	CPM?	N	$\cdots$
J17380077+3329457	3	1.19	CC1	4.32	0.141	2	14.1	5.77	8.36	CPM	Y	Ja12
J17530062+1655029	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J17544786+4109310	5	0.734	CC1	0.627	0.511	4	10.6	10.1	0.465	CPM?	N	$\cdots$
J18132028+0751536	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J18254891+0409280	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J18320290+2030581	2	0.0137	CC1	1.20	1.33	1	4.67	4.79	-0.127	BG?	Y	La08
J19011166+2550384	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J19031729+6359341	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J19133270+5644363	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J19205158+1903362	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J19370113+3147214	2	0.784	CC1	2.81	4.22	1	6.28	7.68	-1.41	BG?	N	$\cdots$
J19433674+3225206	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J19471438+6402377	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J19515537+3811071	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J19543755+2013065	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J20013373+2814101	3	1.61	CC1	1.40	0.259	2	8.30	6.01	2.29	CPM?	Y	WDS
J20194925+2256367	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J20322012+5047455	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J20393474+4822450	2	0.896	CC1	0.738	0.160	1	4.20	3.63	0.578	CPM?	N	$\cdots$
J20395460+0620118	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J20422203+5311332	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J20424915+4122599	2	0.101	CC1	9.17	5.16	1	12.6	8.63	4.01	CPM	N	$\cdots$
J20560274–1710538	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Jay01
J21000529+4004136	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J21010182+2615397	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J21143673+1952557	4	1.04	CC1	3.14	0.0185	3	16.4	6.99	9.37	CPM	N	$\cdots$
J21175904+3404301	2	0.896	CC1	0.969	0.100	1	4.43	3.57	0.869	CPM?	N	$\cdots$
J21294054+6405399	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J21322198+2433419	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Mc01
J21363852+3927206	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J21374019+0137137	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja14b
J21411161–1011001	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J21501406+0922295	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J21512893–0238147	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J21521039+0537356	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Jo13
J21543507+5445122	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J21552437+5938371	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja14b
J22073842–0650034	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J22300418+4851347	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Ja14b
J22413501+1849277	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J22413577+2602128	3	1.08	CC1	2.32	3.10	2	10.1	11.7	-1.57	BG?	N	$\cdots$
J22424884+1330532	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J22594127+2154070	4	0.320	CC1	0.224	0.183	3	7.60	7.48	0.123	CPM?	N	$\cdots$
J23002791–2618431	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J23024391+7506019	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	WDS
J23040837+0318214	3	0.0986	CC1	0.156	0.355	2	5.80	6.20	-0.398	BG?	N	$\cdots$
J23040837+0318214	1	$\cdots$	CC2	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J23060295–1556151	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J23062378+1236269	2	0.726	CC1	34.4	1.61	1	37.9	5.08	32.8	CPM	Y	WDS
J23220944+5756296	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J23450477+1458573	2	0.326	CC1	2.72	0.256	1	6.19	3.72	2.47	CPM?	Y	Ja12
J23473777–2316060	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$
J23574989+3837468	2	1.03	CC1	14.6	0.920	1	18.1	4.39	13.7	CPM	Y	Mc01
J23581366–1724338	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	Y	Dae07
J23590042+2051387	1	$\cdots$	CC1	$\cdots$	$\cdots$	0	$\cdots$	$\cdots$	$\cdots$	SE	N	$\cdots$

Table 6. Table 6: Properties of Robo-AO Visual Binaries

2MASS	${\mu }_{\alpha }\cos \left(\delta \right)$aaProper motions and parallactic distance from $Gaia$ DR2, unless oherwise noted.	${\mu }_{\delta }$aaProper motions and parallactic distance from $Gaia$ DR2, unless oherwise noted.	DistanceaaProper motions and parallactic distance from $Gaia$ DR2, unless oherwise noted.	Cand.	Proj. Sep.	BANYAN $\Sigma$	Literature	YMG
Name	(mas yr-1)	(mas yr-1)	(pc)	Comp.	(”)	Best Hyp.	YMG	Ref.
J00074264+6022543	321.81 $\pm$ 1.48	–5.61 $\pm$ 1.18	16.48 $\pm$ 0.25	CC1	0.86	Field	$\cdots$	$\cdots$
J00133841+5245050	61.36 $\pm$ 0.04	–42.18 $\pm$ 0.03	54.63 $\pm$ 0.09	CC1/CC2	3.13/0.86	Field	$\cdots$	$\cdots$
J00160486+2319090	140.26 $\pm$ 0.14	–45.65 $\pm$ 0.17	37.88 $\pm$ 0.14	CC1	2.66	Field	$\cdots$	$\cdots$
J00164045+3000598	223.82 $\pm$ 0.29	23.70 $\pm$ 0.21	41.56 $\pm$ 0.30	CC1	0.98	Field	$\cdots$	$\cdots$
J00165678+2003551	212.24 $\pm$ 0.44	–28.39 $\pm$ 0.58	39.06 $\pm$ 0.38	CC1	1.03	Field	$\cdots$	$\cdots$
J00171046+2931520	76.01 $\pm$ 0.08	–90.22 $\pm$ 0.06	54.96 $\pm$ 0.16	CC1	1.02	AB Dor	$\cdots$	$\cdots$
J00215781+4912379	208.77 $\pm$ 0.10	–35.03 $\pm$ 0.07	29.56 $\pm$ 0.05	CC1/CC2	2.29/2.66	Field	Car?	Shk12
J00233468+2014282	65.97 $\pm$ 0.10	–37.38 $\pm$ 0.11	62.89 $\pm$ 0.25	CC1	1.73	Field	$\beta$ Pic	Le09, Ma13, Ma14a, Sh17
J00285391+5022330	447.86 $\pm$ 1.18	132.93 $\pm$ 0.94	13.48 $\pm$ 0.17	CC1	0.32	Field	$\cdots$	$\cdots$
J00302927+0420204	72.51 $\pm$ 0.08	–1.00 $\pm$ 0.05	59.35 $\pm$ 0.15	CC1	1.70	Field	$\cdots$	$\cdots$
J00323480+0729271	104.47 $\pm$ 0.29	–63.63 $\pm$ 0.18	35.60 $\pm$ 0.20	CC1	0.71	$\beta$ Pic	$\beta$ Pic?	Sch12b, Sch12a, Bi15a, Me17
J00340843+2523498	82.28 $\pm$ 0.18	–97.32 $\pm$ 0.08	47.68 $\pm$ 0.28	CC1	1.54	AB Dor	AB Dor	Sch10, Ma13, Ma14a
J00414141+4410530	–44.5 $\pm$ 2.4bbProper motion from UCAC4 (Zacharias et al. 2013).	–27.1 $\pm$ 2.9bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.51	Field	$\cdots$	$\cdots$
J00423409+5439048	140.72 $\pm$ 0.19	–12.91 $\pm$ 0.24	57.44 $\pm$ 0.59	CC1	2.98	Field	$\cdots$	$\cdots$
J00425668+2239350	400.51 $\pm$ 0.37	21.95 $\pm$ 0.25	31.68 $\pm$ 0.12	CC1	2.96	Field	$\cdots$	$\cdots$
J00485822+4435091	120.30 $\pm$ 1.82	–130.67 $\pm$ 1.24	32.99 $\pm$ 0.87	CC1	0.97	AB Dor	AB Dor	Sch12a, Sch12b
J00503319+2449009	203.42 $\pm$ 0.23	–31.92 $\pm$ 0.18	14.97 $\pm$ 0.03	CC1	0.94	Field	Arg	Ma14a
J00530648+4829385	229.28 $\pm$ 0.14	–143.59 $\pm$ 0.17	65.24 $\pm$ 0.46	CC1	1.31	Field	$\cdots$	$\cdots$
J01001331+2135328	77.77 $\pm$ 0.14	12.67 $\pm$ 0.25	82.07 $\pm$ 0.68	CC1	2.63	Field	$\cdots$	$\cdots$
J01001613+1251007	47.41 $\pm$ 0.08	–31.57 $\pm$ 0.06	94.15 $\pm$ 0.41	CC1	1.10	Field	$\cdots$	$\cdots$
J01034013+4051288	116.61 $\pm$ 0.12	–161.31 $\pm$ 0.12	31.06 $\pm$ 0.08	CC1	2.53	AB Dor	AB Dor	Shk12
J01071194–1935359	64.4 $\pm$ 1.6bbProper motion from UCAC4 (Zacharias et al. 2013).	–39.5 $\pm$ 1.2bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.47	Field	$\beta$ Pic/Tuc-Hor/Col?	Ki10, Pe13, Ma13, Kr14, Sh17
J01093915+2931112	150.8 $\pm$ 4.8bbProper motion from UCAC4 (Zacharias et al. 2013).	5.8 $\pm$ 5.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.56	Field	$\cdots$	$\cdots$
J01102943–1510071	174.19 $\pm$ 0.10	23.95 $\pm$ 0.08	43.51 $\pm$ 0.10	CC1	2.38	Field	$\cdots$	$\cdots$
J01105436+5822133	85.25 $\pm$ 0.23	–50.22 $\pm$ 0.25	44.54 $\pm$ 0.45	CC1	0.73	Field	$\cdots$	$\cdots$
J01112542+1526214	192.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–130.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.33	Col	$\beta$ Pic	Ma13, Ma14b, Ri14, Sh17
J01121854+4238358	93.74 $\pm$ 0.09	17.82 $\pm$ 0.08	100.11 $\pm$ 0.57	CC1/CC2	2.94/0.73	Field	$\cdots$	$\cdots$
J01131976+5855224	163.84 $\pm$ 0.04	–132.77 $\pm$ 0.05	27.71 $\pm$ 0.03	CC1	2.08	AB Dor	AB Dor?	Sch12a
J01132958–0738088	74.65 $\pm$ 0.08	–68.29 $\pm$ 0.06	65.08 $\pm$ 0.22	CC1	3.02	Field	AB Dor?	Ma13
J01244246–1540454	188.2 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–22.8 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.26	Field	$\cdots$	$\cdots$
J01281337–2319278	207.97 $\pm$ 0.16	–5.95 $\pm$ 0.14	60.94 $\pm$ 0.29	CC1	1.11	Field	$\cdots$	$\cdots$
J01304065–1027506	120.56 $\pm$ 2.03	4.37 $\pm$ 1.33	33.95 $\pm$ 1.57	CC1	0.96	Field	$\cdots$	$\cdots$
J01373940+1835332	74.76 $\pm$ 0.22	–43.35 $\pm$ 0.15	52.15 $\pm$ 0.28	CC1	1.71	$\beta$ Pic	$\beta$ Pic/Col?	Sch10, Ma14b, Sh17
J01535076–1459503	106.65 $\pm$ 0.17	–40.79 $\pm$ 0.21	33.84 $\pm$ 0.14	CC1	2.87	$\beta$ Pic	$\beta$ Pic	Ma13, Ma14a, Sh17
J01592349+5831162	320.58 $\pm$ 0.10	–192.69 $\pm$ 0.10	13.13 $\pm$ 0.01	CC1/CC2	3.96/1.71	Col	Car/Col?	Shk12, Br14
J02155892–0929121	96.6 $\pm$ 1.9bbProper motion from UCAC4 (Zacharias et al. 2013).	–46.5 $\pm$ 2.6bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1/CC2	0.51/3.36	Tuc-Hor	Tuc-Hor/$\beta$ Pic?/Col?	Ma13, Kr14, Bo15a, Na17
J02205082+3320479	144.35 $\pm$ 0.09	–111.33 $\pm$ 0.09	53.11 $\pm$ 0.14	CC1	1.50	Field	$\cdots$	$\cdots$
J02233670–1056138	99.61 $\pm$ 0.07	–41.99 $\pm$ 0.08	121.33 $\pm$ 0.61	CC1	2.66	Field	$\cdots$	$\cdots$
J02284694+1538535	170.91 $\pm$ 0.18	–9.17 $\pm$ 0.17	35.05 $\pm$ 0.14	CC1	0.84	Field	$\cdots$	$\cdots$
J02335984–1811525	72.97 $\pm$ 0.79	–30.34 $\pm$ 0.62	80.56 $\pm$ 2.67	CC1	0.87	Field	Col/$\beta$ Pic	Ro13, Ma14a, Sh17
J02490228–1029220	44.1 $\pm$ 1.9bbProper motion from UCAC4 (Zacharias et al. 2013).	–21.7 $\pm$ 2.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.72	Field	$\beta$ Pic?	Ber15
J02560096+1220457	162.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–67.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.89	Field	$\cdots$	$\cdots$
J03033668–2535329	217.89 $\pm$ 0.30	106.94 $\pm$ 0.31	35.44 $\pm$ 0.20	CC1	0.85	Field	Arg	Ma13
J03092643+6732425	–67.07 $\pm$ 0.35	54.41 $\pm$ 0.44	50.54 $\pm$ 0.71	CC1	2.78	Field	$\cdots$	$\cdots$
J03144720+1127272	60.98 $\pm$ 0.67	–46.18 $\pm$ 0.48	58.90 $\pm$ 0.96	CC1	0.59	Field	$\cdots$	$\cdots$
J03175221+5847431	72.68 $\pm$ 0.04	–6.71 $\pm$ 0.06	100.28 $\pm$ 0.34	CC1	2.43	Field	$\cdots$	$\cdots$
J03240643+2347073	215.05 $\pm$ 0.10	–120.24 $\pm$ 0.07	20.71 $\pm$ 0.02	CC1	2.63	Car-Near	Car-Near?, Arg	Zu06, El16
J03323578+2843554	58.8 $\pm$ 2.6bbProper motion from UCAC4 (Zacharias et al. 2013).	–81.0 $\pm$ 3.5bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.47	$\beta$ Pic	$\beta$ Pic?	Sch12a, Ma14a, Ja14, Sh17
J03340048+5835551	292.12 $\pm$ 0.68	–172.80 $\pm$ 0.51	39.16 $\pm$ 0.65	CC1	0.81	Field	$\cdots$	$\cdots$
J03434696+5725557	–84.37 $\pm$ 0.06	42.56 $\pm$ 0.06	29.45 $\pm$ 0.03	CC1	3.54	Field	$\cdots$	$\cdots$
J03520223+2439479	31.15 $\pm$ 0.93	–41.46 $\pm$ 0.87	450.29 $\pm$ 161.04	CC1	0.45	Field	Pleiades	St07
J04053888+0544408	47.90 $\pm$ 2.03	–53.21 $\pm$ 2.04	36.73 $\pm$ 1.62	CC1	0.78	$\beta$ Pic	$\cdots$	$\cdots$
J04074484+0945220	64.68 $\pm$ 0.88	–13.94 $\pm$ 0.58	44.66 $\pm$ 0.71	CC1	0.77	Field	$\cdots$	$\cdots$
J04112810+7544231	14.8 $\pm$ 2.4bbProper motion from UCAC4 (Zacharias et al. 2013).	–29.9 $\pm$ 2.1bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.27	Field	$\cdots$	$\cdots$
J04132663–0139211	138.76 $\pm$ 0.57	–19.20 $\pm$ 0.38	30.01 $\pm$ 0.33	CC1	0.72	Field	Arg?	Ma13
J04134585–0509049	177.39 $\pm$ 0.29	–110.10 $\pm$ 0.17	29.62 $\pm$ 0.19	CC1	3.37	Field	$\cdots$	$\cdots$
J04171645+1213557	31.4 $\pm$ 1.9bbProper motion from UCAC4 (Zacharias et al. 2013).	–11.8 $\pm$ 1.9bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.73	Field	$\cdots$	$\cdots$
J04174337–1754222	27.77 $\pm$ 0.04	17.10 $\pm$ 0.04	73.31 $\pm$ 0.19	CC1	2.78	Field	$\cdots$	$\cdots$
J04174431+4103137	67.51 $\pm$ 0.16	–209.25 $\pm$ 0.09	30.55 $\pm$ 0.07	CC1	2.52	AB Dor	AB Dor?	Sch12a
J04214271–1657543	30.9 $\pm$ 1.7bbProper motion from UCAC4 (Zacharias et al. 2013).	–8.0 $\pm$ 2.1bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.41	Field	$\cdots$	$\cdots$
J04244805+1552292	121.40 $\pm$ 2.00	–17.82 $\pm$ 1.27	143.58 $\pm$ 15.23	CC1	0.31	Field	$\cdots$	$\cdots$
J04251456+1858250	97.98 $\pm$ 0.11	–28.35 $\pm$ 0.09	52.95 $\pm$ 0.20	CC1	0.83	Hyades	Hyades	Ro11
J04282878+1741453	108.16 $\pm$ 0.62	–41.79 $\pm$ 0.36	46.88 $\pm$ 0.57	CC1	1.71	Field	Hyades	Ro11
J04285080+1617204	101.21 $\pm$ 2.14	–10.38 $\pm$ 2.13	54.45 $\pm$ 3.41	CC1/CC2	1.97/0.73	Field	Hyades	Ro11
J04311384+2053436	23.11 $\pm$ 0.29	–114.21 $\pm$ 0.19	33.98 $\pm$ 0.16	CC1	0.65	Field	$\cdots$	$\cdots$
J04325718+7407002	78.38 $\pm$ 0.06	–124.92 $\pm$ 0.09	33.85 $\pm$ 0.05	CC1	2.86	Col	Col?	Ga18c
J04343992+1512325	103.56 $\pm$ 0.27	–35.76 $\pm$ 0.14	48.07 $\pm$ 0.31	CC1	1.05	Field	Hyades	Ro11
J04350255+0839304	90.95 $\pm$ 1.26	–0.74 $\pm$ 0.96	59.34 $\pm$ 2.64	CC1	0.32	Hyades	Hyades	Ro11
J04381255+2813001	395.65 $\pm$ 0.97	–92.04 $\pm$ 0.79	13.62 $\pm$ 0.09	CC1	1.15	Field	$\cdots$	$\cdots$
J04385352+2147549	187.71 $\pm$ 0.64	–213.61 $\pm$ 0.47	41.00 $\pm$ 0.65	CC1	1.27	Field	$\cdots$	$\cdots$
J04412780+1404340	95.71 $\pm$ 0.92	–23.97 $\pm$ 0.65	49.21 $\pm$ 1.24	CC1	0.26	Hyades	Hyades	Ro11
J04485498+5527185	91.74 $\pm$ 0.93	–105.93 $\pm$ 0.88	43.59 $\pm$ 1.27	CC1	0.51	Field	$\cdots$	$\cdots$
J04492947+4828459	180.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–195.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.63	Field	$\cdots$	$\cdots$
J04495635+2341029	37.18 $\pm$ 0.19	–170.12 $\pm$ 0.11	41.05 $\pm$ 0.16	CC1	2.46	AB Dor	$\cdots$	$\cdots$
J05024924+7352143	47.67 $\pm$ 1.90	–56.70 $\pm$ 1.90	57.39 $\pm$ 4.50	CC1	0.34	Field	$\cdots$	$\cdots$
J05122408+1824086	64.29 $\pm$ 0.13	–31.91 $\pm$ 0.09	53.09 $\pm$ 0.19	CC1	1.50	Hyades	Hyades	Ro11
J05195513–0723399	62.97 $\pm$ 1.06	–47.16 $\pm$ 0.85	57.73 $\pm$ 2.10	CC1	0.53	Field	$\cdots$	$\cdots$
J05252028+6510544	–108.75 $\pm$ 0.04	19.51 $\pm$ 0.04	38.05 $\pm$ 0.04	CC1	1.63	Field	$\cdots$	$\cdots$
J05285650+1231539	93.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–211.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.23	Col	$\cdots$	$\cdots$
J05341064+4732033	–58.07 $\pm$ 0.07	36.85 $\pm$ 0.06	33.25 $\pm$ 0.05	CC1	2.47	Field	$\cdots$	$\cdots$
J05345873+6521435	47.63 $\pm$ 0.09	–118.80 $\pm$ 0.11	52.15 $\pm$ 0.21	CC1	1.17	Field	$\cdots$	$\cdots$
J05494518+2513331	12.68 $\pm$ 0.10	–47.88 $\pm$ 0.08	103.46 $\pm$ 0.62	CC1	2.89	Field	$\cdots$	$\cdots$
J05554690+5123592	34.31 $\pm$ 0.06	–105.94 $\pm$ 0.05	60.88 $\pm$ 0.14	CC1	1.88	Field	$\cdots$	$\cdots$
J06073185+4712266	37.77 $\pm$ 0.16	–188.43 $\pm$ 0.14	28.30 $\pm$ 0.09	CC1	3.45	Col	AB Dor?	Sch12a
J06084814+4257182	39.22 $\pm$ 0.12	–238.52 $\pm$ 0.10	47.62 $\pm$ 0.14	CC1	1.29	Field	$\cdots$	$\cdots$
J06101580+2119569	54.64 $\pm$ 0.24	–193.47 $\pm$ 0.20	59.12 $\pm$ 0.30	CC1/CC2	1.93/1.28	Field	$\cdots$	$\cdots$
J06133437+4914051	33.20 $\pm$ 0.44	–39.40 $\pm$ 0.42	90.54 $\pm$ 2.29	CC1	0.79	Field	$\cdots$	$\cdots$
J06462622+0521150	59.68 $\pm$ 0.08	–0.69 $\pm$ 0.07	42.84 $\pm$ 0.09	CC1	4.17	Field	$\cdots$	$\cdots$
J06584690+2843004	–30.11 $\pm$ 1.24	–116.93 $\pm$ 1.10	41.75 $\pm$ 1.21	CC1	1.03	Field	$\cdots$	$\cdots$
J07120481+5423473	12.61 $\pm$ 0.81	–108.40 $\pm$ 0.66	76.90 $\pm$ 3.81	CC1	1.04	Field	$\cdots$	$\cdots$
J07140450+5043334	–130.35 $\pm$ 0.05	–269.34 $\pm$ 0.04	28.43 $\pm$ 0.03	CC1/CC2	1.90/1.11	Field	$\cdots$	$\cdots$
J07161207+3315154	–80.56 $\pm$ 0.10	–182.04 $\pm$ 0.07	28.62 $\pm$ 0.06	CC1	1.84	Field	$\cdots$	$\cdots$
J07194218+2954390	–22.79 $\pm$ 0.81	–90.88 $\pm$ 0.73	52.16 $\pm$ 1.32	CC1	0.48	Field	$\cdots$	$\cdots$
J07315773+3613102	–249.50 $\pm$ 0.08	–246.33 $\pm$ 0.07	12.00 $\pm$ 0.01	CC1	1.58	Field	$\cdots$	$\cdots$
J07505369+4428181	66.25 $\pm$ 0.06	–140.52 $\pm$ 0.05	49.98 $\pm$ 0.09	CC1	2.11	Field	$\cdots$	$\cdots$
J08010582+0334064	–176.78 $\pm$ 0.08	–124.53 $\pm$ 0.05	46.96 $\pm$ 0.10	CC1	2.25	Field	$\cdots$	$\cdots$
J08014318+4959455	–77.62 $\pm$ 0.36	–68.60 $\pm$ 0.25	56.63 $\pm$ 0.85	CC1	1.16	Field	$\cdots$	$\cdots$
J08083284+5304377	–89.35 $\pm$ 0.32	–91.10 $\pm$ 0.30	35.00 $\pm$ 0.31	CC1	1.23	Field	$\cdots$	$\cdots$
J08095207+0301106	–15.16 $\pm$ 0.06	–39.24 $\pm$ 0.04	97.73 $\pm$ 0.34	CC1	2.43	Field	$\cdots$	$\cdots$
J08310177+4012115	–88.34 $\pm$ 0.09	–124.43 $\pm$ 0.07	33.67 $\pm$ 0.07	CC1	1.94	Field	$\cdots$	$\cdots$
J08444213+0044159	–108.18 $\pm$ 0.07	–9.32 $\pm$ 0.04	65.04 $\pm$ 0.16	CC1	3.26	Field	$\cdots$	$\cdots$
J08504234+0751517	–43.41 $\pm$ 0.10	–26.49 $\pm$ 0.07	17.80 $\pm$ 0.02	CC1	1.21	Field	$\cdots$	$\cdots$
J08593592+5343505	–268.16 $\pm$ 1.92	–194.23 $\pm$ 1.69	13.46 $\pm$ 0.19	CC1	0.37	Field	$\cdots$	$\cdots$
J09062111+1659235	–96.6 $\pm$ 1.6bbProper motion from UCAC4 (Zacharias et al. 2013).	–34.2 $\pm$ 2.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.88	Field	$\cdots$	$\cdots$
J09132383+6852305	–154.9 $\pm$ 2.3bbProper motion from UCAC4 (Zacharias et al. 2013).	–233.2 $\pm$ 2.2bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.60	AB Dor	AB Dor?	Sch12a, Ga18b
J09174473+4612246	–129.87 $\pm$ 0.70	–17.50 $\pm$ 0.75	33.45 $\pm$ 0.48	CC1	0.19	Field	$\cdots$	$\cdots$
J09192291+6203170	–288.35 $\pm$ 0.06	–386.15 $\pm$ 0.08	38.10 $\pm$ 0.07	CC1	0.79	Field	$\cdots$	$\cdots$
J09200048+3052397	–74.3 $\pm$ 6.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–33.6 $\pm$ 3.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.42	Field	$\cdots$	$\cdots$
J09214911+4330284	–295.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–121.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.71	Field	$\cdots$	$\cdots$
J10024936+4827333	–321.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–280.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.20	Field	$\cdots$	$\cdots$
J10043276+0533412	–77.7 $\pm$ 1.7bbProper motion from UCAC4 (Zacharias et al. 2013).	–102.2 $\pm$ 2.2bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.30	AB Dor	$\cdots$	$\cdots$
J10143153+0213174	–29.73 $\pm$ 0.39	–46.01 $\pm$ 0.46	85.23 $\pm$ 1.27	CC1	0.67	Field	$\cdots$	$\cdots$
J10143194+0606409	–144.00 $\pm$ 0.09	–69.54 $\pm$ 0.09	32.36 $\pm$ 0.06	CC1	2.13	Field	$\cdots$	$\cdots$
J10150690+3125110	–55.05 $\pm$ 0.11	–213.17 $\pm$ 0.15	33.56 $\pm$ 0.08	CC1	1.81	Field	$\cdots$	$\cdots$
J10452148+3830422	–38.26 $\pm$ 0.29	154.35 $\pm$ 0.45	13.70 $\pm$ 0.05	CC1	0.68	Field	$\cdots$	$\cdots$
J10482887+5852005	–199.46 $\pm$ 0.04	–55.92 $\pm$ 0.05	43.91 $\pm$ 0.06	CC1/CC2	1.20/1.80	Field	$\cdots$	$\cdots$
J10571139+0544547	–59.14 $\pm$ 0.84	–37.78 $\pm$ 0.90	104.94 $\pm$ 4.92	CC1	1.01	Field	$\beta$ Pic?	Sch12c
J11030845+1517518	–419.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–84.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.39	Car-Near	$\cdots$	$\cdots$
J11161238+4942112	–74.48 $\pm$ 0.46	–0.37 $\pm$ 0.49	79.19 $\pm$ 2.29	CC1	0.79	Field	$\cdots$	$\cdots$
J11432359+2518137	–233.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–31.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.48	Car-Near	$\cdots$	$\cdots$
J11470543+7001588	–342.70 $\pm$ 0.69	–33.53 $\pm$ 0.64	30.68 $\pm$ 0.37	CC1	0.91	Field	$\cdots$	$\cdots$
J11474897+0459160	–134.93 $\pm$ 0.09	–95.43 $\pm$ 0.06	38.03 $\pm$ 0.08	CC1	1.68	Field	$\cdots$	$\cdots$
J11503435+2903407	–213.0 $\pm$ 10.2bbProper motion from UCAC4 (Zacharias et al. 2013).	18.4 $\pm$ 6.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.51	Field	$\cdots$	$\cdots$
J11504306+3312180	–209.71 $\pm$ 1.44	5.62 $\pm$ 1.62	49.01 $\pm$ 1.97	CC1/CC2/CC3	0.59/2.58/0.49	Field	$\cdots$	$\cdots$
J12115308+1249135	–71.62 $\pm$ 0.13	–57.64 $\pm$ 0.07	61.02 $\pm$ 0.30	CC1	1.17	Field	$\beta$ Pic?	Sch12a
J12121136+4849032	197.82 $\pm$ 0.03	–314.46 $\pm$ 0.04	26.59 $\pm$ 0.02	CC1	2.85	Field	$\cdots$	$\cdots$
J12161505+5053376	–79.57 $\pm$ 0.07	34.16 $\pm$ 0.09	38.04 $\pm$ 0.10	CC1	1.90	Field	$\cdots$	$\cdots$
J12174539+0653230	–103.31 $\pm$ 0.10	42.01 $\pm$ 0.05	49.48 $\pm$ 0.11	CC1	2.63	Field	$\cdots$	$\cdots$
J12225061–0404462	–255.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–65.7 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.24	Field	$\cdots$	$\cdots$
J13020587+1222215	–217.30 $\pm$ 0.20	–95.69 $\pm$ 0.12	30.22 $\pm$ 0.07	CC1	2.93	Field	$\cdots$	$\cdots$
J13034595+2837205	–33.15 $\pm$ 0.05	20.25 $\pm$ 0.04	214.34 $\pm$ 1.67	CC1	1.86	Field	$\cdots$	$\cdots$
J13061537+2043444	–55.82 $\pm$ 0.07	94.57 $\pm$ 0.05	19.65 $\pm$ 0.02	CC1	1.61	Field	$\cdots$	$\cdots$
J13120689+3213179	114.5 $\pm$ 2.3bbProper motion from UCAC4 (Zacharias et al. 2013).	–89.0 $\pm$ 4.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.24	Field	$\cdots$	$\cdots$
J13151846–0249516	165.2 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–165.2 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.29	Field	$\cdots$	$\cdots$
J13162169+2905548	–157.77 $\pm$ 0.09	–107.31 $\pm$ 0.10	59.68 $\pm$ 0.26	CC1/CC2	0.29/2.42	Field	$\cdots$	$\cdots$
J13252836+3743098	–197.94 $\pm$ 0.05	57.35 $\pm$ 0.04	33.79 $\pm$ 0.04	CC1	2.91	Field	$\cdots$	$\cdots$
J13260267+2735021	–2.97 $\pm$ 0.17	73.12 $\pm$ 0.14	45.20 $\pm$ 0.16	CC1	1.49	Field	$\cdots$	$\cdots$
J13282890+0514353	–63.87 $\pm$ 0.11	–51.28 $\pm$ 0.08	111.34 $\pm$ 0.68	CC1	0.93	Field	$\cdots$	$\cdots$
J13324347+1114521	–165.62 $\pm$ 0.11	9.66 $\pm$ 0.06	51.07 $\pm$ 0.11	CC1	1.45	Field	$\cdots$	$\cdots$
J13324460+1648397	287.56 $\pm$ 0.27	–206.79 $\pm$ 0.12	16.58 $\pm$ 0.03	CC1	2.83	Field	$\cdots$	$\cdots$
J13373037–1048346	90.5 $\pm$ 2.8bbProper motion from UCAC4 (Zacharias et al. 2013).	–152.7 $\pm$ 2.4bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.41	Field	$\cdots$	$\cdots$
J13375120+4808174	–241.53 $\pm$ 0.05	–137.72 $\pm$ 0.05	21.19 $\pm$ 0.01	CC1	1.63	Field	$\cdots$	$\cdots$
J13420990–1600233	–496.64 $\pm$ 0.70	–49.15 $\pm$ 0.58	21.06 $\pm$ 0.23	CC1	0.62	Field	$\cdots$	$\cdots$
J13435058+5030053	–80.04 $\pm$ 0.49	–10.50 $\pm$ 0.53	62.45 $\pm$ 1.49	CC1	1.08	Field	$\cdots$	$\cdots$
J13474241+2127374	79.92 $\pm$ 0.08	–89.26 $\pm$ 0.06	29.94 $\pm$ 0.04	CC1	1.33	Field	$\cdots$	$\cdots$
J13534589+5210298	–2.78 $\pm$ 1.40	–130.26 $\pm$ 1.42	56.15 $\pm$ 2.83	CC1	1.06	Field	$\cdots$	$\cdots$
J14040922+2044314	–130.5 $\pm$ 3.3bbProper motion from UCAC4 (Zacharias et al. 2013).	–20.4 $\pm$ 1.8bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.43	Field	$\cdots$	$\cdots$
J14105956+0751398	–51.03 $\pm$ 0.14	9.05 $\pm$ 0.13	34.27 $\pm$ 0.11	CC1	1.38	Field	$\cdots$	$\cdots$
J14141700–1521125	–120.12 $\pm$ 0.11	–197.14 $\pm$ 0.10	28.65 $\pm$ 0.05	CC1	1.61	AB Dor	$\beta$ Pic?	El16, Sh17
J14170294+3142472	–589.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–143.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.27	Field	$\cdots$	$\cdots$
J14170837+5000081	–105.79 $\pm$ 0.13	42.29 $\pm$ 0.12	64.36 $\pm$ 0.36	CC1	1.70	Field	$\cdots$	$\cdots$
J14243178–0257158	–66.95 $\pm$ 0.55	–33.15 $\pm$ 0.46	131.53 $\pm$ 4.92	CC1	3.85	Field	$\cdots$	$\cdots$
J14303394+0305440	44.15 $\pm$ 0.85	11.18 $\pm$ 0.78	57.41 $\pm$ 1.36	CC1	2.69	Field	$\cdots$	$\cdots$
J14373999+6745316	–213.52 $\pm$ 0.67	184.48 $\pm$ 0.73	41.03 $\pm$ 0.53	CC1	0.88	Field	$\cdots$	$\cdots$
J14433804–0414354	–101.85 $\pm$ 0.29	–69.61 $\pm$ 0.28	51.62 $\pm$ 0.53	CC1	1.01	Field	$\cdots$	$\cdots$
J14445989+5309251	–102.14 $\pm$ 1.00	11.01 $\pm$ 1.10	58.93 $\pm$ 2.17	CC1	0.86	Field	$\cdots$	$\cdots$
J14514497–0530407	–63.37 $\pm$ 0.74	–2.92 $\pm$ 0.86	83.81 $\pm$ 2.88	CC1	0.48	Field	$\cdots$	$\cdots$
J15005557+4525343	224.77 $\pm$ 0.06	328.98 $\pm$ 0.06	11.71 $\pm$ 0.01	CC1	2.03	Field	$\cdots$	$\cdots$
J15072382+4333531	79.64 $\pm$ 0.88	39.88 $\pm$ 1.07	30.83 $\pm$ 0.55	CC1	0.55	Field	$\cdots$	$\cdots$
J15114542+1014222	–35.99 $\pm$ 0.12	22.12 $\pm$ 0.08	108.90 $\pm$ 0.56	CC1	1.92	Field	$\cdots$	$\cdots$
J15123818+4543464	–387.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	352.0 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.54	Field	$\cdots$	$\cdots$
J15154371–0725208	–150.7 $\pm$ 4.3bbProper motion from UCAC4 (Zacharias et al. 2013).	–277.8 $\pm$ 9.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.60	AB Dor	$\cdots$	$\cdots$
J15233660+3837489	–108.0 $\pm$ 1.2bbProper motion from UCAC4 (Zacharias et al. 2013).	–51.2 $\pm$ 1.5bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.62	AB Dor	AB Dor?	Sch12a
J15402840–1841460	–60.85 $\pm$ 0.58	–148.75 $\pm$ 0.36	38.15 $\pm$ 0.38	CC1	0.76	AB Dor	AB Dor	Zu04, To08
J15422038+5936528	–88.40 $\pm$ 0.06	20.80 $\pm$ 0.08	44.52 $\pm$ 0.07	CC1	1.58	Field	$\cdots$	$\cdots$
J15424184+8005306	–45.97 $\pm$ 0.03	67.33 $\pm$ 0.03	76.43 $\pm$ 0.11	CC1	2.08	Field	$\cdots$	$\cdots$
J15452354+7514548	–28.94 $\pm$ 1.69	–63.38 $\pm$ 1.80	49.50 $\pm$ 2.31	CC1	0.96	Field	$\cdots$	$\cdots$
J15521824+3414537	–78.99 $\pm$ 0.03	191.13 $\pm$ 0.04	45.64 $\pm$ 0.04	CC1	1.80	Field	$\cdots$	$\cdots$
J15553178+3512028	–232.36 $\pm$ 0.06	155.98 $\pm$ 0.09	27.82 $\pm$ 0.03	CC1/CC2	1.61/1.87	Field	Arg?	Ma13, Ma14a
J15575497+6010263	–63.9 $\pm$ 1.4bbProper motion from UCAC4 (Zacharias et al. 2013).	31.0 $\pm$ 0.9bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.70	Field	$\cdots$	$\cdots$
J16015690+1825127	–36.35 $\pm$ 0.05	–87.74 $\pm$ 0.05	65.28 $\pm$ 0.22	CC1	1.25	Field	$\cdots$	$\cdots$
J16043736+7022142	46.60 $\pm$ 2.01	15.84 $\pm$ 2.41	48.38 $\pm$ 2.75	CC1	0.76	Field	$\cdots$	$\cdots$
J16060319+0333215	–104.9 $\pm$ 2.7bbProper motion from UCAC4 (Zacharias et al. 2013).	–95.4 $\pm$ 2.6bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.56	Field	$\cdots$	$\cdots$
J16102225+4509347	–11.05 $\pm$ 0.08	29.87 $\pm$ 0.10	100.96 $\pm$ 0.48	CC1	2.43	Field	$\cdots$	$\cdots$
J16171135+7733477	–38.27 $\pm$ 0.14	39.80 $\pm$ 0.18	72.57 $\pm$ 0.44	CC1	0.81	Field	AB Dor?/$\beta$ Pic?	Sch12a
J16250150–1215254	–184.8 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–173.6 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.31	Field	$\cdots$	$\cdots$
J16455062+0343014	–37.67 $\pm$ 0.08	–105.38 $\pm$ 0.07	44.89 $\pm$ 0.08	CC1	2.06	AB Dor	AB Dor?	Sch12a, Sch12b, Bi15b
J16510995+3555071	–74.28 $\pm$ 0.12	175.23 $\pm$ 0.15	34.93 $\pm$ 0.08	CC1	1.07	Field	$\cdots$	$\cdots$
J16582055+0733079	35.1 $\pm$ 2.7bbProper motion from UCAC4 (Zacharias et al. 2013).	–14.4 $\pm$ 3.4bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.50	Field	$\cdots$	$\cdots$
J17021204+5103284	–37.50 $\pm$ 1.61	77.33 $\pm$ 1.55	60.65 $\pm$ 2.80	CC1	0.78	Field	$\cdots$	$\cdots$
J17035283+3211456	192.41 $\pm$ 0.64	99.97 $\pm$ 0.66	19.13 $\pm$ 0.12	CC1	1.44	Field	$\cdots$	$\cdots$
J17152512+1328342	30.40 $\pm$ 0.96	23.22 $\pm$ 0.92	53.97 $\pm$ 1.44	CC1	0.74	Field	$\cdots$	$\cdots$
J17183470+3400290	–14.62 $\pm$ 0.04	172.98 $\pm$ 0.05	50.56 $\pm$ 0.07	CC1	1.32	Field	$\cdots$	$\cdots$
J17340562+4447082	–97.2 $\pm$ 4.1bbProper motion from UCAC4 (Zacharias et al. 2013).	20.1 $\pm$ 2.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.59	Field	$\cdots$	$\cdots$
J17380077+3329457	–121.22 $\pm$ 0.21	54.06 $\pm$ 0.22	52.62 $\pm$ 0.32	CC1	0.97	Field	$\cdots$	$\cdots$
J17530062+1655029	–243.94 $\pm$ 2.13	–240.05 $\pm$ 2.24	22.65 $\pm$ 0.52	CC1	0.88	Field	$\cdots$	$\cdots$
J17544786+4109310	–15.03 $\pm$ 0.71	93.65 $\pm$ 0.68	67.10 $\pm$ 1.70	CC1	0.83	Field	$\cdots$	$\cdots$
J18132028+0751536	24.04 $\pm$ 1.47	62.82 $\pm$ 1.54	53.10 $\pm$ 3.06	CC1	0.98	Field	$\cdots$	$\cdots$
J18254891+0409280	7.88 $\pm$ 0.06	–90.95 $\pm$ 0.06	54.99 $\pm$ 0.10	CC1	3.62	Field	$\cdots$	$\cdots$
J18320290+2030581	–47.48 $\pm$ 0.27	–214.65 $\pm$ 0.40	31.20 $\pm$ 0.17	CC1	1.38	Field	$\cdots$	$\cdots$
J19011166+2550384	–11.18 $\pm$ 0.08	36.69 $\pm$ 0.09	48.87 $\pm$ 0.14	CC1	1.34	Field	$\cdots$	$\cdots$
J19031729+6359341	63.7 $\pm$ 2.5bbProper motion from UCAC4 (Zacharias et al. 2013).	112.1 $\pm$ 1.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	3.69	AB Dor	$\cdots$	$\cdots$
J19133270+5644363	–5.84 $\pm$ 0.33	33.94 $\pm$ 0.29	69.23 $\pm$ 0.67	CC1	1.17	Field	$\cdots$	$\cdots$
J19205158+1903362	67.8 $\pm$ 2.3bbProper motion from UCAC4 (Zacharias et al. 2013).	63.9 $\pm$ 3.4bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.51	Field	$\cdots$	$\cdots$
J19370113+3147214	80.5 $\pm$ 1.3bbProper motion from UCAC4 (Zacharias et al. 2013).	100.5 $\pm$ 0.7bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.51	Field	$\cdots$	$\cdots$
J19433674+3225206	43.90 $\pm$ 0.05	–5.46 $\pm$ 0.05	47.75 $\pm$ 0.07	CC1	0.40	Field	$\cdots$	$\cdots$
J19471438+6402377	92.18 $\pm$ 0.09	23.13 $\pm$ 0.07	67.20 $\pm$ 0.15	CC1	0.17	Field	$\cdots$	$\cdots$
J19515537+3811071	–14.19 $\pm$ 0.04	–143.40 $\pm$ 0.04	43.86 $\pm$ 0.05	CC1	2.32	Field	$\cdots$	$\cdots$
J19543755+2013065	–38.09 $\pm$ 0.04	–62.76 $\pm$ 0.04	27.42 $\pm$ 0.03	CC1	4.20	Field	$\cdots$	$\cdots$
J20013373+2814101	114.16 $\pm$ 0.07	79.54 $\pm$ 0.07	33.90 $\pm$ 0.06	CC1	1.54	Field	$\cdots$	$\cdots$
J20194925+2256367	83.53 $\pm$ 0.10	106.69 $\pm$ 0.09	29.34 $\pm$ 0.06	CC1	1.96	Field	$\cdots$	$\cdots$
J20322012+5047455	–10.02 $\pm$ 0.61	61.38 $\pm$ 0.63	57.40 $\pm$ 1.27	CC1	0.82	Field	$\cdots$	$\cdots$
J20393474+4822450	88.11 $\pm$ 0.06	48.72 $\pm$ 0.05	76.65 $\pm$ 0.20	CC1	1.86	Field	$\cdots$	$\cdots$
J20395460+0620118	89.41 $\pm$ 0.19	–104.27 $\pm$ 0.13	36.36 $\pm$ 0.16	CC1	2.48	Field	AB Dor	Sch10, Ma14a
J20422203+5311332	50.6 $\pm$ 1.8bbProper motion from UCAC4 (Zacharias et al. 2013).	83.7 $\pm$ 1.8bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.29	Field	$\cdots$	$\cdots$
J20424915+4122599	67.3 $\pm$ 1.6bbProper motion from UCAC4 (Zacharias et al. 2013).	–31.1 $\pm$ 2.3bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.48	AB Dor	AB Dor?	Sch12a
J20560274–1710538	57.31 $\pm$ 0.11	–62.14 $\pm$ 0.07	45.93 $\pm$ 0.21	CC1	2.21	$\beta$ Pic	$\beta$ Pic	Zu01b, To08, Sh17
J21000529+4004136	614.4 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	–247.2 $\pm$ 8.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.89	AB Dor	$\cdots$	$\cdots$
J21010182+2615397	63.5 $\pm$ 2.4bbProper motion from UCAC4 (Zacharias et al. 2013).	–6.7 $\pm$ 2.5bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.43	Field	$\cdots$	$\cdots$
J21143673+1952557	85.76 $\pm$ 0.08	–48.51 $\pm$ 0.09	122.07 $\pm$ 0.95	CC1	2.86	Field	$\cdots$	$\cdots$
J21175904+3404301	51.54 $\pm$ 0.08	–23.68 $\pm$ 0.10	43.48 $\pm$ 0.12	CC1	1.12	Field	$\cdots$	$\cdots$
J21294054+6405399	90.90 $\pm$ 0.06	28.79 $\pm$ 0.06	43.83 $\pm$ 0.07	CC1	2.44	Field	$\cdots$	$\cdots$
J21322198+2433419	229.54 $\pm$ 0.09	–8.71 $\pm$ 0.10	20.55 $\pm$ 0.03	CC1	1.55	Field	$\cdots$	$\cdots$
J21363852+3927206	–212.30 $\pm$ 0.25	–158.28 $\pm$ 0.30	20.71 $\pm$ 0.08	CC1	1.09	Field	$\cdots$	$\cdots$
J21374019+0137137	80.3 $\pm$ 2.8bbProper motion from UCAC4 (Zacharias et al. 2013).	–59.4 $\pm$ 3.1bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.42	$\beta$ Pic	$\beta$ Pic	Sch12b, Sch12a, Sch12c, Sh17
J21411161–1011001	–0.91 $\pm$ 1.15	–74.24 $\pm$ 1.27	62.53 $\pm$ 2.78	CC1	1.02	Field	$\cdots$	$\cdots$
J21501406+0922295	201.51 $\pm$ 0.07	–295.38 $\pm$ 0.08	44.36 $\pm$ 0.11	CC1	1.51	Field	$\cdots$	$\cdots$
J21512893–0238147	30.45 $\pm$ 0.09	–34.47 $\pm$ 0.09	46.23 $\pm$ 0.11	CC1	1.43	Field	$\cdots$	$\cdots$
J21521039+0537356	109.8 $\pm$ 1.5bbProper motion from UCAC4 (Zacharias et al. 2013).	–150.0 $\pm$ 2.0bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.64	AB Dor	AB Dor	To08, DaS09, Shk12, Ma13
J21543507+5445122	171.35 $\pm$ 0.05	142.35 $\pm$ 0.05	71.25 $\pm$ 0.16	CC1	3.19	Field	$\cdots$	$\cdots$
J21552437+5938371	113.0 $\pm$ 2.2bbProper motion from UCAC4 (Zacharias et al. 2013).	22.5 $\pm$ 1.8bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.36	Field	$\beta$ Pic?	Sch12a
J22073842–0650034	146.34 $\pm$ 0.35	–2.57 $\pm$ 0.32	63.98 $\pm$ 0.80	CC1	0.95	Field	$\cdots$	$\cdots$
J22300418+4851347	–73.66 $\pm$ 0.10	–61.55 $\pm$ 0.09	33.26 $\pm$ 0.07	CC1	2.32	Field	$\cdots$	$\cdots$
J22413501+1849277	256.83 $\pm$ 1.00	95.46 $\pm$ 0.92	31.40 $\pm$ 0.65	CC1	0.23	Field	$\cdots$	$\cdots$
J22413577+2602128	–20.90 $\pm$ 0.10	59.67 $\pm$ 0.08	30.19 $\pm$ 0.05	CC1	3.70	Field	$\cdots$	$\cdots$
J22424884+1330532	57.15 $\pm$ 0.08	–34.62 $\pm$ 0.10	69.09 $\pm$ 0.33	CC1	2.24	Field	Col	Ma13, Ma14a
J22594127+2154070	127.97 $\pm$ 0.09	–59.09 $\pm$ 0.06	38.02 $\pm$ 0.07	CC1	2.28	Field	$\cdots$	$\cdots$
J23002791–2618431	116.72 $\pm$ 0.09	–159.84 $\pm$ 0.07	31.86 $\pm$ 0.05	CC1	2.27	AB Dor	AB Dor	Zu04, Ma13
J23024391+7506019	285.30 $\pm$ 0.05	22.95 $\pm$ 0.04	53.16 $\pm$ 0.07	CC1	3.73	Field	$\cdots$	$\cdots$
J23040837+0318214	104.94 $\pm$ 0.08	–53.34 $\pm$ 0.06	85.89 $\pm$ 0.34	CC1/CC2	2.20/3.73	Field	$\cdots$	$\cdots$
J23060295–1556151	124.2 $\pm$ 1.7bbProper motion from UCAC4 (Zacharias et al. 2013).	–11.5 $\pm$ 1.7bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.81	Field	$\cdots$	$\cdots$
J23062378+1236269	301.1 $\pm$ 4.4bbProper motion from UCAC4 (Zacharias et al. 2013).	–52.6 $\pm$ 2.1bbProper motion from UCAC4 (Zacharias et al. 2013).	$\cdots$	CC1	0.46	Field	$\cdots$	$\cdots$
J23220944+5756296	–6.25 $\pm$ 1.79	–27.82 $\pm$ 1.87	166.06 $\pm$ 32.14	CC1	0.35	Field	$\cdots$	$\cdots$
J23450477+1458573	237.55 $\pm$ 0.29	–28.93 $\pm$ 0.14	71.79 $\pm$ 0.75	CC1	1.15	Field	$\cdots$	$\cdots$
J23473777–2316060	155.46 $\pm$ 0.24	–66.18 $\pm$ 0.26	44.87 $\pm$ 0.35	CC1	1.24	Field	$\cdots$	$\cdots$
J23574989+3837468	–155.61 $\pm$ 1.87	–145.25 $\pm$ 1.57	21.14 $\pm$ 0.67	CC1	0.47	Field	UMa?	Sh12
J23581366–1724338	225.77 $\pm$ 0.14	19.74 $\pm$ 0.09	33.45 $\pm$ 0.08	CC1	2.09	Car-Near	Hyades?, Arg?	Sh12, Ma13, El16
J23590042+2051387	228.92 $\pm$ 1.25	–104.85 $\pm$ 0.57	66.85 $\pm$ 3.56	CC1	0.56	Field	$\cdots$	$\cdots$

Equations

$$J-H>-(H-K_S)+0.65\mathrm{mag}$$

$$J-H<-(H-K_S)+1.05\mathrm{mag}$$

$$NUV-W1<7.0(J-W2)+5.5\mathrm{mag}$$

$$NUV-W1<13\mathrm{mag}$$

$${\chi }_{\mathrm{CPM}}^2=\sum _{i=1}^{N-1}\left(\frac{({\theta }_{\mathrm{meas},i}-{\theta }_{\mathrm{ref},i}{)}^2}{{\sigma }_{\theta ,\mathrm{meas},i}^2+{\sigma }_{\theta ,\mathrm{ref},i}^2}+\frac{({\rho }_{\mathrm{meas},i}-{\rho }_{\mathrm{pred},i}{)}^2}{{\sigma }_{\rho ,\mathrm{meas},i}^2+{\sigma }_{\rho ,\mathrm{ref},i}^2}\right),$$

$${\chi }_{\mathrm{BG}}^2=\sum _{i=1}^{N-1}\left(\frac{({\theta }_{\mathrm{meas},i}-{\theta }_{\mathrm{pred},i}{)}^2}{{\sigma }_{\theta ,\mathrm{meas},i}^2+{\sigma }_{\theta ,\mathrm{pred},i}^2}+\frac{({\rho }_{\mathrm{meas},i}-{\rho }_{\mathrm{pred},i}{)}^2}{{\sigma }_{\rho ,\mathrm{meas},i}^2+{\sigma }_{\rho ,\mathrm{pred},i}^2}\right).$$

$$\mathrm{BIC}={\chi }^2+k\ln n$$

Full text

binaries: visual—stars: low-mass—stars: pre-main sequence

††facilities: Mayall (RC-Spec), SOAR (Goodman Spectrograph), PO:1.5m (Robo-AO), UH:2.2m (SNIFS)

1 Introduction

Since the initial recognition of young moving groups (YMGs) about two decades ago (e.g., Kastner et al. 1997; Zuckerman & Webb 2000; Torres et al. 2000), these nearby associations of intermediate-age ($\approx$10–200 Myr) stars have been the subject of increasing interest in the stellar, substellar, and exoplanet communities (e.g., Torres et al. 2008; Mamajek 2016b; Bowler 2016). These loose, relatively sparse (N$$\sim50–300), kinematically comoving groups in the solar neighborhood ($\lesssim$100 pc) provide a link between the youngest T Tauri stars and the older population of field stars.

Because of their proximity and youth, YMGs have become a rich resource to study a broad range of topics: the evolution of stellar dynamos and activity (e.g., Shkolnik & Barman 2014; Ansdell et al. 2015); dynamical masses of intermediate-age stars (e.g., Close et al. 2005; Montet et al. 2015; Nielsen et al. 2016; Janson et al. 2018); the structure and evolution of debris disks (e.g., Wyatt et al. 2014); young brown dwarfs and free-floating planetary-mass objects (Liu et al. 2013; Allers & Liu 2013; Gagné et al. 2014; Aller et al. 2016; Liu et al. 2016; Faherty et al. 2016); multiplicity at young ages (Shan et al. 2017; Janson et al. 2017; Best et al. 2017); and the initial mass function of sparse clusters (Gagné et al. 2017). Members of YMGs have also become favored targets for direct imaging searches for exoplanets (e.g., Biller et al. 2013; Brandt et al. 2014; Bowler et al. 2015a; Chauvin et al. 2015) and, as a result, many of the known directly imaged planets and planetary-mass companions orbit members of these associations (e.g., 2M1207–3932 b, Chauvin et al. 2004; HR 8799 bcde, Marois et al. 2008; $\beta$ Pic b, Lagrange et al. 2010, 51 Eri b, Macintosh et al. 2015; GU Psc b, Naud et al. 2014; 2M2236+4751 b, Bowler et al. 2017). However, the relatively limited number of bona fide members of young moving groups—a few hundred confirmed using fully-constrained space motions together with other independent youth indicators—has gradually become a barrier to measuring more precise occurrence rates with direct imaging and searching for correlations with stellar host mass (Bowler & Nielsen 2018).

Despite numerous dedicated searches to identify nearby young stars, the current census of stellar and substellar members of YMGs is vastly incomplete. Assuming a standard initial mass function, Kraus et al. (2014), Gagné et al. (2017), and Shkolnik et al. (2017) find that tens to hundreds of low-mass stars and brown dwarfs are probably missing from membership lists of Tuc-Hor, TWA, and $\beta$ Pic. The same is likely to be true of other YMGs owing to early, biased searches for bright members using Hipparcos parallaxes and proper motions. This has prompted a number of programs to find new low-mass members spanning the stellar and substellar mass regimes (Gizis 2002; Lépine & Simon 2009; Shkolnik et al. 2009; Schlieder et al. 2010; Schlieder et al. 2012b; Malo et al. 2013; Malo et al. 2014a; Gagné et al. 2014; Kraus et al. 2014; Riedel et al. 2014; Binks & Jeffries 2015; Aller et al. 2016; Riedel et al. 2017; Shkolnik et al. 2017). In spite of these innovative efforts, hundreds of low-mass members likely await discovery.

Motivated by the need for additional targets for high-contrast imaging, we have carried out a broad search for low-mass stars in young moving groups. The goals of this program are highly focused: to identify new, single, relatively bright ($R$ $\lesssim$ 15 mag) YMG members with large proper motions. This facilitates the rapid discrimination of background stars from bound companions for follow-up high-contrast imaging observations. Our strategy is to initially use X-ray and UV activity together with color and proper motion cuts to locate candidate young early-M dwarfs. Having begun this study prior to $Gaia$ data releases, our approach to selecting targets for follow-up observations has relied only on proper motions and sky positions without the advantage of having parallaxes.

This study focuses on the characterization of potential young stars and moving group members based on low-resolution optical spectroscopy together with adaptive optics imaging with Robo-AO at the Palomar 60-inch (1.5-m) telescope. In a separate paper we will present radial velocities from new high-resolution spectroscopy of several hundred potential moving group members as part of a follow-up kinematic analysis. Section 2 summarizes the activity, color, and proper motion cuts used to define our starting sample. Our observations and analysis are described in Sections 3 and 4. Moving group candidates are discussed in Section 5 and our conclusions are summarized in Section 6.

2 Sample Selection

Our starting sample draws from two large catalogs of low-mass stars. The Frith et al. (2013) list of bright M dwarfs (K$$<9 mag) consists of stars between K7–M4 selected from the PPMXL catalog (Roeser et al. 2010). The authors apply a series of optical and NIR color cuts to isolate late spectral types, and reduced proper motions are used to distinguish dwarfs from bright, distant giants. Frith et al. require a S/N of at least 5 for proper motions and remove regions surrounding the galactic plane ($|b|$ $<$ 15*∘*) susceptible to source confusion. Finally, they combine their list with the Lépine & Gaidos (2011) catalog of bright M dwarfs to produce a final catalog of 8479 late-K to mid-M dwarfs.

We also utilize the Haakonsen & Rutledge (2009) list of $ROSAT$ All-Sky Survey Bright Source Catalog (Voges et al. 1999) detections cross-matched with the 2MASS Point Source Catalog (Cutri et al. 2003; Skrutskie et al. 2006). The authors provide probabilities that each X-ray source is uniquely associated with a near-infrared counterpart. Altogether 18,497 ROSAT detections have non-zero probabilities of being associated with a 2MASS sources. For this study we select 6084 targets with $>$90% association probabilities as a supplementary catalog to search for young active M dwarfs.

Both samples are then cross-matched against all-sky photometric and proper motion surveys. Near-infrared $J$-, $H$-, and $K_{S}$-band photometry is extracted from the Two Micron All Sky Survey (2MASS; Skrutskie et al. 2006) with a search radius ($R_{S}$) of 5*′′; $r^{\prime}$-band photometry is from Carlsberg Meridian Catalogue 14 (Evans et al. 2002; $R_{S}$=5′′); $R2$ magnitudes are from USNO-B1.0 (Monet et al. 2003; $R_{S}$=5′′); $NUV$ and $FUV$ photometry is from the latest Galaxy Evolution Explorer ($GALEX$) General Release (GR6/GR7; Martin et al. 2005; Morrissey et al. 2007; $R_{S}$=10′′); W1, W2, W3, and W4 photometry from Wide-field Infrared Survey Explorer ($WISE$; Wright et al. 2010; $R_{S}$=10′′); X-ray count rates and hardness ratios are from the $ROSAT$ All-Sky Survey Bright Source Catalog (Voges et al. 1999) or, if not detected there, then the $ROSAT$ All-Sky Faint Source Catalog (Voges et al. 2000; $R_{S}$=30′′); and $V$-band magnitudes and proper motions are from the USNO CCD Astrograph Catalog 4 (Zacharias et al. 2013; $R_{S}$=5′′*). If there are multiple $GALEX$ detections for the same search position at different epochs then we adopt the weighted mean and uncertainty of these measurements.

We apply a series of color, activity, proper motion, and photometric distance cuts to both catalogs that are specifically designed to identify nearby young M dwarfs for follow-up planet searches with direct imaging. These criteria are primarily intended for the Haakonsen & Rutledge (2009) catalog (hereinafter HR09), which has a diverse mix of non-stellar “contaminants” (active galactic nuclei, cataclysmic variables, galaxy clusters, etc.). On the other hand, the Frith et al. (2013) catalog (hereinafter F13) is well-vetted for M dwarfs, but these are overwhelmingly expected to be old inactive field stars. Below we list the additional filters we have applied to both samples:

• •

Optical brightness cut. Stars with $r^{\prime}$ $>$ 15 mag are excluded. This corresponds to the approximate faintness limit for natural guide star AO instruments like Keck/NIRC2, ensuring an optically-bright sample for the possibility of follow-up high-contrast imaging. If no $r^{\prime}$ measurement is listed in CMC14 then we adopt the $R2$ magnitude from USNO-B1.0 and apply the same brightness cut.

• •

Photometric distance cut. $V$-band photometric distance estimates are computed using the $M_{V}$ versus $V$–$K_{S}$ band polynomial fit to Pleiades stars in Bowler et al. (2013). Most known moving group are located within about 100 pc, so we further restrict our search catalog to photometric distances $<$ 100 pc. Photometric distances will underestimate the true distances for binaries and young stars still descending along the Hayashi track, but this cut excludes most of the distant M dwarfs from the sample.

• •

Near-infrared color cuts. A series of near-infrared color cuts are imposed to further isolate late-K and early-M dwarfs. Only stars with $J$-band, $H$-band, and $K_{S}$-band photometric uncertainties below 0.1 mag are considered. Hipparcos K7V–M3V stars and the Lépine & Gaidos (2011) sample of bright M dwarfs are used to establish typical near-infrared colors of M dwarfs (Figure 1). Based on this locus, we impose the following color cuts:

[TABLE]

[TABLE]

These cuts are depicted in Figure 1 for two control samples from Hipparcos and Lépine & Gaidos (2011), in addition to the F13 and H09 catalogs we consider in this work. M dwarfs have already been color-selected for the F13 catalog, so this cut predominantly affects the H09 catalog.

• •

UV activity cut. Stars with active chromospheres are readily distinguished from their inactive counterparts using $GALEX$ photometry. Following Rodriguez et al. (2013), we use the $J$–$W2$ versus $NUV$–$W1$ diagram to identify active stars (Figure 2):

[TABLE]

[TABLE]

Based on the spectral type-color relation from Rodriguez et al. (2013), we also require that $J$–$W2$ $>$ 0.8 mag to isolate late-type ($\geq$K5) stars (Figure 2). Note that this cut does not remove white dwarf-M dwarf binaries, which can share similar UV-to-infrared colors as young, active M dwarfs (Silvestri et al. 2007; Shkolnik et al. 2011)

• •

Reduced proper motion cut. Reduced proper motions provide a convenient way to separate fast-moving dwarfs from kinematically slow but luminous giants. Following F13, we require $H_{K}$ $>$ 6.0, where the reduced proper motion is $H_{K}$ = $K$ + 5 log($\sqrt{(}\mu_{\alpha}\cos(\delta)^{2}+\mu_{\delta}^{2}))$ + 5; here \mu_{\alpha}$$\cos(\delta) and $\mu_{\delta}$ are the star’s proper motion in arcseconds per year. Finally, we also require the total proper motion to be greater than 25 mas yr*-1* to ensure that candidate planets identified in AO imaging can be distinguished from background stars on short ($\sim$1 year) timescales.

Cross-matching the resulting filtered F13 and H09 samples yields 2060 unique targets which we use as the starting point for our young moving group kinematic selection.

3 Observations

To better characterize our starting sample of 2060 activity-selected late-K and early-M dwarfs, we carried out a follow-up observational program to obtain low-resolution optical spectra of these targets using instruments in the northern and southern hemispheres, together with AO imaging with Robo-AO at the Palomar 60*′′* (1.5-m) telescope in the north. Altogether we acquired 762 optical spectra of 632 stars, plus an additional four nearby stars sharing common proper motions with targets in our sample. We also obtained 1523 AO images of 1011 stars to uncover and characterize close binaries. The broader goals of this program are to identify single young stars for high-contrast imaging, so known binaries from recent high-resolution campaigns (e.g., Janson et al. 2012; Janson et al. 2014a) are deprioritized, leading to an intentionally biased sample which we note is not easily amenable to multiplicity statistics. Details about the instrument setups and data reduction are discussed below.

3.1 Mayall/RC-Spec

Observations with the RC-Spectrograph mounted on the 4-m Mayall telescope at Kitt Peak were carried out over eight nights on UT 2013 December 29–31, UT 2014 May 21–23, and UT 2015 June 16–17. Altogether 478 spectra were obtained for 428 stars. The same instrument setup was used for all observing runs: the BL420 grating in conjunction with the GG-495 filter and 1$\farcs$5 $\times$98*′′* slit dimensions produced an average resolving power ($R\equiv\lambda/\Delta\lambda$) of $\approx$2600 spanning 6200–9200 Å. The T2KA CCD with a gain of 1.4 e*-* ADU*-1* was used for the 2013 and 2014 runs; the T2KB CCD was used with a gain of 1.9 e*-* ADU*-1* during the 2015 observations. Sky conditions were partly clear with intermittent clouds. The slit was oriented in a fixed North-South direction throughout the nights, which means targets observed at large hour angles suffered from wavelength-dependent slit loss from differential atmospheric refraction (Filippenko 1982). Most targets were observed near transit but the continuum slopes of some stars are affected by chromatic slit loss. Our observations are detailed in Table 1.

Each image was bias subtracted, flat fielded, and corrected for bad pixels. Night sky lines were removed with median subtraction using 25-pix regions on either side of the science spectrum. The spectrum was then extracted by summing the central 11-pix region in the spatial direction. Wavelength calibration was carried out with HeNeAr arc lamps acquired 3–5 times per night. About 30 prominent lines are fit with a quadratic function to derive the pixel-to-wavelength solution. Several early-type spectrophotometric standards from Oke (1990), Hamuy et al. (1992), and Hamuy et al. (1994) were observed each night to broadly correct the continuum shape for throughput losses from the atmosphere, optics, grating, and CCD.

3.2 SOAR/Goodman Spectrograph

A total of 244 spectra were obtained for 168 stars with the Goodman High-Throughput Spectrograph (Clemens et al. 2004) at the Southern Astrophysical Research (SOAR) 4.1-m telescope located on Cerro Pachón, Chile. The observations spanned nine nights on three observing runs: UT 2013 December 4–7, UT 2014 June 25–28, and UT 2015 February 16. Details about individual observations can be found in Table 1. Our strategy was to first observe with the 400 l mm*-1* grating (“SYZY400”) in the M2 setup with the 0$\farcs$46 slit, which produces an average resolving power of $\approx$1800 spanning 5000–9000 Å. For a subset of targets — usually those showing strong H$\alpha$ emission or hints of Li absorption — we also obtained a spectrum with the 1200 l mm*-1* grating (“RALC1200”) in the M5 setup with the 0$\farcs$46 slit, which produces an average resolving power of $\approx$5900 spanning 6250–7500 Å. The slit was rotated to parallactic angle for each target on all nights except UT 2013 December 4–5. All observations were carried out with the GG455 order-blocking filter and the Blue Camera CCD, which imprinted strong fringing redward of about 7000 Å. The detector was read out at 400 kHz with 1$\times$1 binning. Quartz lamp flats and arc lamps for wavelength calibration were taken immediately after each science observation at the same position on the sky. At least one spectrophotometric standard was targeted per night.

All observations are reduced using custom scripts. Images are bias-subtracted and corrected for bad pixels. A normalized flat field is created at the same location as the science trace on the CCD and is used to remove pixel-to-pixel variations in the science frame, including most (but not all) of the fringing. Spectra are then optimally extracted following the method described in Horne (1986). Wavelength calibration is carried out by fitting Gaussians to 19 strong emission lines from HgAr for the arc lamp frames using the 400 l mm*-1* grating, and 11 emission lines from CuHeAr for the arc lamp frames using the 1200 l mm*-1* grating in pixel space. A fourth order polynomial fit is used to map pixels to wavelengths in an automated fashion for each target. Finally, the extracted spectrum was divided by a spectrophotometric standard observed on the same night to correct for wavelength-dependent throughput losses.

3.3 UH 2.2-m/SuperNova Integral Field Spectrograph

We acquired low-resolution (R$$\approx1300) optical spectra for 40 stars on UT 2014 January 19 and 21 with the SuperNova Integral Field Spectrograph (SNIFS) at the University of Hawai’i’s 88*′′* (2.2 m) telescope located on Maunakea, Hawai’i. SNIFS is an integral-field spectrograph that uses a microlens array to disperse a 6*′′$\times$6′′* field of view into two channels spanning 3200–11000 Å (Lantz et al. 2004). Multiple O/B standards were observed on each night. After basic image reduction and rectification into data cubes, each spectrum were extracted and wavelength calibrated with the SNIFS reduction pipeline (Aldering et al. 2006; Scalzo et al. 2010). Details for each target are listed in Table 1.

3.4 P60/Robo-AO

We obtained 1523 adaptive optics images of 1011 targets from our parent sample of 2060 active stars with Robo-AO at the Palomar 60*′′* (1.5-m) telescope between July 2013 and June 2015. Robo-AO is an efficient autonomous adaptive optics system that provides diffraction-limited AO observations at optical wavelengths using an ultraviolet laser for wavefront sensing (Baranec et al. 2013; Baranec et al. 2014) and an intelligent queue system for target selection (Riddle et al. 2014).

For each observation, Robo-AO’s EMCCD camera produces a data cube typically composed of 256 fast readouts with short exposures. These frames are combined using a shift-and-add pipeline for each observation to produce a final science image with a field of view of 44*′′$\times$44′′* that has been resampled to 21.6 mas pix*-1*, or half the native plate scale (see Law et al. 2014 for details). The plate scale and north orientation are derived from observations of globular clusters taken on observing runs throughout the same time period as these data. Because targets tend to be faint and red, most of our observations are carried out with the SDSS $i^{\prime}$ filter with integration times of 30–120 s. When possible, we obtained multiple observations of candidate visual binaries to test for common proper motion. Details about our individual observations can be found in Table 2.

FWHM values are calculated using the averaged radial profile of the PSF. When seeing conditions degrade, the shift-and-add procedure locks on to noise spikes and produces a narrow core in the final image. For these images, which would otherwise imply sub-diffraction-limited resolution, we ignore the inner 5 pix for our FWHM measurement. The typical FWHM is about 0$\farcs$18, which compares with the diffraction limit of $\approx$0$\farcs$12 at 750 nm. The median seeing at Palomar Observatory is about 1$\farcs$1. 73% of our observations have FWHM $<$ 0$\farcs$25 and 11% of our observations have FWHM $<$ 0$\farcs$15. These measurements are reported in Table 2.

Image performance metrics and contrast curves are generated for each target following Law et al. (2014) and Ziegler et al. (2017). To summarize, AO correction is assessed using PSF core size. Targets are divided into high-, medium-, or low-performance groups, which vary primarily with target brightness and natural seeing conditions.111Representative contrast curves for each performance group are as follows: High: {0.7, 1.6, 3.9 , 5.5, 6.3, 6.4, 6.4} mag, Medium: {0.7, 1.6, 3.2 , 4.4, 5.0, 5.0, 5.0} mag, and Low: {0.5, 1.1, 2.2 , 3.1, 3.5, 3.5, 3.5} mag at {0$\farcs$1, 0$\farcs$2, 0$\farcs$5 , 1*′′, 2′′, 3′′, 4′′}, respectively. 5$\sigma$ contrast curves are derived using a Monte Carlo injection-recovery analysis of artificial companions generated from the primary’s PSF. Contrast curves from our observations are summarized in Figure 3; we typically reach \Delta$$i^{\prime} $\approx$ 5 mag at 1′′*. In Section 4.2 we discuss the visual binaries and fainter candidate companions in our images.

\startlongtable

4 Results

4.1 Spectral Classification

Spectral types are determined using the Hammer classification package (Covey et al. 2007), which measures a suite of indices and assigns a spectral type by comparing these values to spectral standards. West et al. (2011) show that these classifications are generally accurate to $\pm$1 subclass, but for late-M dwarfs there is an average systematic offset of $\approx$0.4 subtypes towards earlier types. We therefore also assign spectral types using the visual classifying feature in Hammer. These two methods are generally in agreement, but our visual types are found to be more reliable, so we adopt an uncertainty of $\pm$0.5 subtypes for these classifications. As expected from our color cuts, the vast majority of objects for which we obtained spectra fall between K5 and M5. Both the automated (index-based) and visual results are reported in Table 1 together with TiO5 indices, which track the onset and strengthening of TiO absorption in the emergent spectra of M dwarfs (Reid et al. 1995).

4.1.1 H$\alpha$ Emission

H$\alpha$ emission is observed in the vast majority of our spectra. We measure equivalent widths by fitting a Gaussian function centered at 6563 Å using the curve-fitting package MPFIT (Markwardt 2009) and integrating under the best-fit model. Each fit was visually inspected to ensure the emission line peak was correctly identified and modeled. Our threshold for clear line emission is $<$–0.5 Å. For equivalent widths between 0.0 to –0.5 Å, the emission is either very weak or questionable based on visual inspection. Values in this range are less reliable because of the low resolving power of our data and should be treated with caution. High-resolution spectra may be needed to unambiguously search for H$\alpha$ emission in those stars. Equivalent widths $>$0 Å indicate that H$\alpha$ is seen in absorption. H$\alpha$ line strengths are listed in Table 1. Uncertainties are determined by comparing equivalent widths of the same targets on the same night; we estimate errors of 20% for the quoted line strengths.

H$\alpha$ equivalent widths are shown as a function of TiO5 index strength in Figure 4. Our targets trace an envelope of H$\alpha$ emission that increases in strength from about –3 Å at TiO5 values of 0.9 ($\approx$K7) to $>$10 Å at TiO5 values of 0.4 ($\approx$M4). The shape of this envelope bears a close resemblance to other large spectroscopic samples of M dwarfs (e.g., Riaz et al. 2006; Gaidos et al. 2014; Kraus et al. 2014). Barrado y Navascués & Martin (2003) identify an empirical division that separates accretion-induced H$\alpha$ emission from saturated chromospheric activity. Eight stars have exceptionally strong H$\alpha$ emission that falls on or above the saturated chromospheric curve in Figure 4 and may originate in part from disk accretion: 2MASS J10260210–4105537, 2MASS J13314666+2916368, 2MASS J13573397–3139105, 2MASS J14255593+1412101, 2MASS J15354856–2958551, 2MASS J17213497–2152283, 2MASS J18464675+0043260, and 2MASS J19300396–2939322.

4.1.2 Lithium

Li I $\lambda$6708 Å absorption is a well-established indicator of youth in the atmospheres of low-mass stars (e.g., Soderblom et al. 2014). Lithium burning occurs in stellar cores through proton capture reactions at temperatures of about 2.5$\times$106 K, and the depletion of lithium among late-type stars with partially or fully convective envelopes is a strong function of both mass and age (Basri et al. 1996; Chabrier et al. 1996; Bildsten et al. 1997). The presence and strength of lithium therefore acts as a sensitive chronometer for masses between about 0.06–0.6 $M_{\odot}$.

Lithium is apparent in 58 stars from the subset of our parent sample for which we obtained spectra (632 out of 2060 stars; see Tables 1 and 4.1.2). Line profiles are fit with Gaussian functions to calculate equivalent widths. We estimate uncertainties of about 20% based on multiple measurements of the same targets in our sample. Our low-resolution observations are shown in Figure 5 and are sensitive to the strongest lines, so there are likely to be additional stars with weaker levels of lithium below our detection limits (about 50–200 mÅ) that we were not sensitive to.

Equivalent widths range from $\approx$100–600 mÅ and span the full range of spectral types from K5 to M5 (middle panel; Figure 4). The diversity of line strengths implies a range of ages for these stars, with the highest equivalent widths corresponding to ages at least as young as TWA ($\approx$10 Myr) based on empirical lithium depletion boundaries for young clusters (e.g., Neuhäuser 1997; Mentuch et al. 2008). For spectral types $>$K7, all of our stars exhibiting lithium are expected to have ages younger than the Pleaides ($\approx$125 Myr; Stauffer et al. 1998). We note that our lithium stars tend to have high H$\alpha$ emission line strengths (top panel; Figure 4) and the lower sodium values (lower panel), pointing to higher magnetic activity levels, larger physical radii, and lower surface gravities.

\startlongtable

Figure 6 shows the position of our lithium-rich stars in the $Gaia$ color-magnitude diagram (CMD) relative to known members of young moving groups. The $Gaia$ DR2 CMD is constructed largely adhering to recommendations by Lindegren et al. (2018) with the following additional restrictions: parallaxes $>$10 mas; parallax SNR $>$10; and photometric SNR $>$10 in $G$, $G_{B}$, and $G_{R}$ bandpasses. Most of the lithium stars lie above the main sequence and are consistent with the isochrones traced out by AB Dor ($\approx$120 Myr); Tuc-Hor, Argus, Carina, and Columba ($\approx$40–50 Myr); $\beta$ Pic ($\approx$23 Myr); and TWA ($\approx$10 Myr).

4.1.3 Sodium

Like other alkali elements, the relative strength of the Na I doublet at 8183 Å and 8195 Å is sensitive to atmospheric pressure and surface gravity (e.g., Slesnick et al. 2006). Schlieder et al. (2012a) show that this doublet can act as a useful tracer of youth for spectral types $>$M3 because of its prominence relative to the pseudo-continuum at cool temperatures and its stronger dependence on surface gravity at lower masses. We simultaneously fit two Gaussians to these neighboring lines and report the total equivalent width of the pair for each spectrum in Table 1. The bottom panel of Figure 4 shows a general strengthening of the lines at lower temperatures with significant spread for a given spectral type. Beyond M0, stars with lithium tend to lie near the lower envelope of our sodium measurements, in agreement with the expectation of large radii, low surface gravities, and young ages for these objects.

\startlongtable

4.2 Visual Binaries

Point sources are identified in our Robo-AO images following the procedure described in Ziegler et al. (2017). Each image is inspected visually and through an automated source-finding algorithm. We focus on a 4*′′* radius surrounding each star where our AO observations are most advantageous compared to all-sky seeing-limited surveys. Altogether point sources are found near 239 stars with optical contrasts peaking at $\Delta$mag$\approx$0.5 and reaching $\Delta$mag$\approx$7 for the faintest objects identified (Figures 7–10). Relative contrasts are measured using aperture photometry at wide separations and processed images of the companion after PSF subtraction at close separations. Uncertainties in astrometry and contrast are estimated based on systematic errors caused by blending and due to maximum orientation changes during the observing period, which we estimate to be $\pm$1$\fdg$5 using calibration fields. Contrasts, separations, position angles, and estimated uncertainties for all point sources can be found in Table 4. Note that targets reported in our complete list of observations in Table 2 that do not have nearby point sources listed in Table 4 imply that they are single, at least to within our sensitivity limits.

In Table 4.2 we compare the observed and expected astrometry for candidate binary companions with multi-epoch imaging to test whether they are background stars or physically bound systems. $\chi^{2}$ values for the common proper motion ($\chi^{2}_{\mathrm{CPM}}$) and background ($\chi^{2}_{\mathrm{BG}}$) hypotheses are calculated as follows:

[TABLE]

[TABLE]

Here $\theta_{\mathrm{meas},i}$, $\rho_{\mathrm{meas},i}$, $\sigma_{\theta,\mathrm{meas},i}$, and $\sigma_{\rho,\mathrm{meas},i}$ are the measured P.A., separation, and their respective uncertainties for epoch $i$ of $N$ total epochs; $\theta_{\mathrm{ref},i}$, $\rho_{\mathrm{ref},i}$, $\sigma_{\theta,\mathrm{ref},i}$, and $\sigma_{\rho,\mathrm{ref},i}$ are the same for the reference epoch (here taken to be our first observation of the system); and $\theta_{\mathrm{pred},i}$, $\rho_{\mathrm{pred},i}$, $\sigma_{\theta,\mathrm{pred},i}$, and $\sigma_{\rho,\mathrm{pred},i}$ are the predicted relative astrometry of a stationary background source based on the distance, proper motion, and sky position of the target (Table 5).

The Bayesian Information Criterion (BIC; Schwarz 1978) is used to assess the significance of evidence for or against the background and comoving models. It is constructed to reward better fits but penalize more complex models as follows:

[TABLE]

where $k$ is the number of free parameters in the model and $n$ is the number of epochs. Lower BIC values are preferred. Differenced BIC values ($\Delta$BIC = BICBG – BICCPM) for both bound and unbound scenarios are listed in Table 4.2. Following Kass & Raftery (1995), $\Delta$BIC values between 0–3 are interpreted as modest evidence in favor of common proper motion, $\Delta$BIC values greater than 3 suggest strong evidence for common proper motion, $\Delta$BIC values between 0 and –3 point to modest evidence in favor of the background model, and $\Delta$BIC values less than –3 imply strong evidence for the background model.

\startlongtable

Altogether 252 sources are detected within 4*′′* of 239 stars. A single epoch was acquired for most candidate companions so some sources may be background stars, but the vast majority are expected to be physical binaries based on the low number density of comparably bright stars. We carried out a literature search primarily consulting the Washington Double Star Catalog (Mason et al. 2001) and identified 88 previously known binaries — most of which have undergone significant orbital motion since their discovery – while the rest appear to be new.

4.3 Young Moving Group Members

Among the 58 lithium-rich stars in our sample, 35 are previously known or suspected members of young moving groups or nearby star-forming regions (Table 4.1.2). Similarly, 51 out of 238 visual binaries have been identified as known or candidate YMG members in the literature (Table 5). We used the BANYAN-$\Sigma$ tool from Gagné et al. (2018b) to search for additional YMG members in our our lithium-rich stars and active binary samples. BANYAN-$\Sigma$ is a Bayesian classifier that uses kinematic information to determine an object’s membership probability for young moving groups within 150 pc. Compared to previous versions of BANYAN (Malo et al. 2013; Gagné et al. 2014), this updated package uses a refined model of the galactic disk together with spatial and kinematic constraints for 27 associations with ages $\lesssim$800 Myr, including nearby star-forming regions and intermediate-age open clusters.

Results from the BANYAN analysis using default parameters for association locations and space motions are listed in Tables 4.1.2 and 5. When available, radial velocities from the literature have been used for the lithium-rich sample. We do not make use of an instantaneous radial velocity measurement for the active binaries since long-baseline monitoring is needed to robustly measure the pair’s systemic velocity. The best hypothesis refers to the most probable kinematic and spatial model, including the field. Results from BANYAN broadly agree with previous assessments, but in many cases either identifies the field as the most likely hypothesis or disagrees on the most likely moving group. Altogether an additional seven and ten systems are identified as new candidate moving group members from the lithium-rich and active binary samples, respectively.

5 Notes on Individual Objects

Below we comment on new candidate YMG members, noteworthy individual systems with unusually high H$\alpha$ emission, and objects with discrepancies between BANYAN-$\Sigma$ and literature YMG assessments from Tables 4.1.2 and 5. Our final adopted membership status takes into account lithium line strength, $UVW$ kinematics, spatial position, sky position, and CMD position when possible.

2MASS J00233468+2014282 — Lépine & Simon (2009) first identify this star as a member of $\beta$ Pic, which has been bolstered by several additional studies (Malo et al. 2013; Malo et al. 2014a; Shkolnik et al. 2017). However, the best hypothesis from BANYAN-$\Sigma$ is the field population. We measure modest lithium absorption (EW$$\approx260 mÅ), weak H$\alpha$ emission ($EW$=–1 Å), and a spectral type of M0 from our Mayall spectrum, in close agreement with previous measurements. The observed lithium strength is typical of $\beta$ Pic members of this spectral type. This target is identified as a 1$\farcs$7 binary in the Washington Double Star catalog; we easily recovered this companion with our Robo-AO observations. Using the measured RV of –2.2 $\pm$ 0.6 km s*-1* from Shkolnik et al. (2017) together with $Gaia$ DR2 astrometry, the space velocities of this system are $U$=–11.81 $\pm$ 0.19 km s*-1*, $V$=–17.4 $\pm$ 0.4 km s*-1*, and $W$=–8.8 $\pm$ 0.4 km s*-1*. This is only 1.3 $\sigma$ (2.3 $\pm$ 1.7 km s*-1*) from the locus of $\beta$ Pic members from Torres et al. (2008)222Differential velocities (\Delta$$v) and uncertainties ($\sigma_{\Delta v}$) are calculated as follows: \Delta$$v = $\sqrt{(U-U_{0})^{2}+(V-V_{0})^{2}+(W-W_{0})^{2}}$, $\sigma_{\Delta v}$ = $\sqrt{(U-U_{0})^{2}(\sigma_{U}^{2}+\sigma_{U_{0}}^{2})+(V-V_{0})^{2}(\sigma_{V}^{2}+\sigma_{V_{0}}^{2})+(W-W_{0})^{2}(\sigma_{W}^{2}+\sigma_{W_{0}}^{2})}$ / \Delta$$v. Given the excellent agreement of this system with other established $\beta$ Pic members, we adopt previous membership assessments in this group over BANYAN’s field hypothesis

2MASS J00501752+0837341 — This M5 star was proposed as a $\beta$ Pic member by Shkolnik et al. (2017), who also identify it as an SB2, but the best hypothesis from BANYAN-$\Sigma$ is the field. We measure a lithium EW of $\approx$60 mÅ and strong H$\alpha$ emission. Using the measured RV of 2.15 $\pm$ 2.0 km s*-1* from Shkolnik et al. (2017) together with $Gaia$ DR2 astrometry, the space velocities of this system are $U$=–12.7 $\pm$ 0.6 km s*-1*, $V$=–16.6 $\pm$ 1.0 km s*-1*, and $W$=–7.8 $\pm$ 1.6 km s*-1*. This is 1.5 $\sigma$ (3.0 $\pm$ 2.0 km s*-1*) from the locus of $\beta$ Pic members from Torres et al. (2008). Given the good agreement with known members, we adopt previous membership assessment in $\beta$ Pic over BANYAN’s field hypothesis

2MASS J01540267–4040440 — This K7 star was proposed as a Columba member by Malo et al. (2014a), but the best hypothesis from BANYAN-$\Sigma$ is the field. We measure lithium absorption with a depth of $\approx$160 mÅ from our SOAR/Goodman data. Using the measured RV of 12.7 $\pm$ 0.2 km s*-1* from Malo et al. (2014a) together with $Gaia$ DR2 astrometry, the space velocities of this system are $U$=–11.42 $\pm$ 0.03 km s*-1*, $V$=–21.6 $\pm$ 0.08 km s*-1*, and $W$=–5.8 $\pm$ 0.19 km s*-1*. This is 1.4 $\sigma$ (1.8 $\pm$ 1.3 km s*-1*) from the locus of Columba members from Torres et al. (2008). Given the good kinematic agreement with Columba and appropriate lithium strength for the age of this group, we adopt the previous membership assessment in Columba over BANYAN’s field hypothesis.

2MASS J02490228–1029220 — Bergfors et al. (2015) identify lithium in this resolved triple system (Janson et al. 2012) and find that its kinematics are a good match to $\beta$ Pic, but the best hypothesis from our BANYAN-$\Sigma$ analysis is the field. We detect lithium from our SOAR spectrum with a strength of $\approx$310 mÅ, comparable to what Bergfors et al. measure. RVs for this system are presented in Durkan et al. (2018) and support candidacy in $\beta$ Pic, although a parallax is needed to unambiguously confirm membership. We adopt previous assessments of this system as a candidate in $\beta$ Pic over BANYAN’s field hypothesis

2MASS J03520223+2439479 — This star is a known member of the Pleiades (e.g., Stauffer et al. 2007). It has also been proposed as a member of Taurus, but Kraus et al. (2017) show that its proper motion is inconsistent with that region. Walter et al. (1988) and Soderblom et al. (1993) measure lithium equivalent widths of 350 and 302 mÅ, respectively. The 0$\farcs$45 binary companion we uncovered with Robo-AO was first reported by Leinert et al. (1993). $Gaia$ DR2 reports a parallax of 2.2 $\pm$ 0.7 mas ($\approx$450 pc), but the astrometric excess noise parameter is large (2.5 mas), implying the five-parameter astrometric solution is not an especially good fit to the data. This is likely caused by acceleration from the binary companion so the reported parallax is probably unreliable. We adopt previous assessments of this system as a member of the Pleiades over BANYAN’s field hypothesis.

2MASS J04435686+3723033 — Schlieder et al. (2010) identify this object and its wide ($\approx$9*′′) comoving companion as likely members of the $\beta$ Pic moving group based on their activity and proper motions from SUPERBLINK. $\beta$ Pic membership is reaffirmed in Malo et al. (2014b), Messina et al. (2017), and Shkolnik et al. (2017), but the best hypothesis from our BANYAN-$\Sigma$ analysis is the field. Together with the Gaia distance of 71.65 $\pm$ 0.26 pc and RV of –6.4 $\pm$ 0.2 from Malo et al. (2014b), these proper motions imply $UVW$ space velocities of –10.66 $\pm$ 0.19 km s-1*, –19.08 $\pm$ 0.09 km s*-1*, –8.40 $\pm$ 0.05 km s*-1*. These differ by 3.7 $\sigma$ (3.3 km $\pm$ 0.9 km s*-1*) from the locus of $\beta$ Pic from Torres et al. (2008). The M2 host star shows modest lithium absorption (194 $\pm$ 4 mÅ  from Malo et al. 2014b and $\approx$120 mÅ from our Mayall spectrum), consistent with an age older than TWA but younger than Tuc-Hor. We adopt previous assessments of this system as a candidate member of $\beta$ Pic over BANYAN’s field hypothesis.

2MASS J05363633+2139330 — Li & Hu (1998) first identified this star as a candidate member of Taurus from its activity and strong lithium absorption (480 mÅ). We also detect deep lithium in this star with an EW of $\approx$460 mÅ, but found a spectral type of M2 which differs from the K4 classification by Li & Hu (1998). Mamajek (2016a) suggest this star is a member of the proposed subgroup 118 Tau, which is also suggested as the best hypothesis from BANYAN-$\Sigma$. Membership in the broader Taurus complex was recently confirmed with a detailed analysis by Kraus et al. (2017); they also find this subgroup may be kinematically related to Taurus. The proper motion and distance for this star from $Gaia$ DR2 is $\mu_{\alpha}$cos$\delta$=10.65 $\pm$ 0.19 mas yr*-1*, $\mu_{\delta}$=–41.23 $\pm$ 0.14 mas yr*-1*, 108.22 $\pm$ 1.59 pc, respectively, similar to the other 118 Tau group members from Mamajek (2016a) ($\mu_{\alpha}$cos$\delta$ $\approx$ +4 mas yr*-1*; $\mu_{\delta}$ $\approx$ –39 mas yr*-1*; $d$ $\approx$ 120 pc). Given this consistent sky position, proper motion, and distance, we adopt candidacy in 118 Tau as suggested by Mamajek (2016a) and BANYAN.

\startlongtable

2MASS J05374649+0231264 — da Silva et al. (2009) first identify this lithium-rich ($EW$=300 mÅ) star as a member of Columba, which was bolstered by Elliott et al. (2016). We measure a somewhat lower lithium strength of $\approx$190 mÅ from our low-resolution Mayall spectrum. Using the proper motion, distance (68.44 $\pm$ 0.19 pc), and RV (20.8 $\pm$ 2.8 km s*-1*) from $Gaia$ DR2, the space velocities of this system are $U$=–13.1 $\pm$ 2.5 km s*-1*, $V$=–20.6 $\pm$ 1.0 km s*-1*, and $W$=–6.5 $\pm$ 0.7 km s*-1*. This is 1.0 $\sigma$ (1.3 $\pm$ 1.3 km s*-1*) from the locus of Columba members from Torres et al. (2008). Given the good kinematic agreement with Columba and appropriate lithium strength for the age of this group, we adopt previous membership assessment in Columba over BANYAN’s field hypothesis.

2MASS J05500858+0511536 — We measure modest lithium ($\approx$120 mÅ) in this little-studied active M2 star. The best hypothesis from BANYAN-$\Sigma$ is Columba. Using the proper motion, distance (64.45 $\pm$ 0.17 pc), and RV (18 $\pm$ 4 km s*-1*) from $Gaia$ DR2, the space velocities of this system are $U$=–11.2 $\pm$ 3.7 km s*-1*, $V$=–19.2 $\pm$ 1.4 km s*-1*, and $W$=–5.2 $\pm$ 0.8 km s*-1*. This is 1.3 $\sigma$ (3.3 $\pm$ 2.7 km s*-1*) from the locus of Columba members from Torres et al. (2008). The absolute $V$-band magnitude of 8.6 mag and $V$–$J$ color of 3.3 mag place this star above the main sequence, in good agreement with other Columba members from Bell et al. (2015). Overall this star appears to be an excellent new candidate member of Columba, but a more precise RV and lithium equivalent width measurement is needed for confirmation.

2MASS J09595765–7221472 – Elliott et al. (2014) identify this lithium-rich star as a K4 candidate member of Carina, but the best hypothesis from BANYAN-$\Sigma$ is the field. We find a somewhat later spectral type of K7 from our SOAR spectra. Our lithium measurement ($EW$ $\approx$ 270 mÅ) is comparable to that of Torres et al. (2006) ($EW$ = 330 mÅ) and suggests an age between TWA and AB Dor (e.g., Murphy et al. 2018). The velocities of this system are $U$=–8.8 $\pm$ 0.07 km s*-1*, $V$=—-21.6 $\pm$ 0.18 km s*-1*, and $W$=–2.1 $\pm$ 0.05 km s*-1*. This is 2.5 $\sigma$ (3.0 $\pm$ 1.2 km s*-1*) from the locus of Carina members from Torres et al. (2008). This star is a better match to Tuc-Hor in terms of space motion, but is several tens of parsecs from established members of that group. We adopt previous assessments of this system as a member of Carina over BANYAN’s field hypothesis.

2MASS J10260210–4105537 This lithium-rich early M dwarf was proposed as a member of TWA by Bell et al. (2015), Pecaut & Mamajek (2013), and Naud et al. (2017). Gagné et al. (2017) suggest it is a likely contaminant from Lower Centaurus Crux (LCC). Using the new $Gaia$ DR2 distance of 84.9 $\pm$ 2 pc, the best hypothesis from BANYAN-$\Sigma$ is the field. We measure a spectral type of M2 and strong lithium ($EW$ $\approx$ 410 mÅ), which is slightly less than that found by Rodriguez et al. (2011, $EW$ = 500 $\pm$ 70 mÅ). We also find unusually strong H$\alpha$ (EW$\approx$–10.4 Å) above the envelope of saturated chromospheric emission identified by Barrado y Navascués & Martin (2003), suggesting it may originate from ongoing accretion. The distance and sky position of this object is more consistent with TWA than LCC (e.g., Murphy et al. 2015) so we adopt previous assessments of this system as a likely member of TWA over LCC and BANYAN’s field hypothesis. However, a radial velocity is needed to unambiguously establish group membership.

2MASS J12003688–6337055 — This active, lithium-rich (EW$\approx$480 mÅ) M0 star was flagged as a likely LCC member using BANYAN-$\Sigma$. Using the proper motion, distance (101.2 $\pm$ 0.3 pc), and RV (14.3 $\pm$ 1.8 km s*-1*) from $Gaia$ DR2, the space velocities of this system are $U$=–9.7 $\pm$ 0.8 km s*-1*, $V$=–21.06 $\pm$ 1.6 km s*-1*, and $W$=–8.02 $\pm$ 0.06 km s*-1*. This is 1.1 $\sigma$ (2.7 $\pm$ 2.5 km s*-1*) from the locus of LCC members from Gagné et al. (2018b). The $V$-band absolute magnitude of this star is 7.0 mag, which is about a magnitude above the main sequence at the $V$–$J$ color of this object (2.7 mag; Bell et al. 2015). The sky position, space motion, lithium strength, and overluminosity are in excellent agreement with LCC.

2MASS J12281909–7306346 — This active M0 star has strong lithium absorption — EW$$\approx440 mÅ from our low-resolution Goodman spectrum — and has a best hypothesis of $\epsilon$ Cha from BANYAN-$\Sigma$. It does not appear to be a previously known young star. The space velocities of this system from $Gaia$ DR2 astrometry are $U$=–8.5 $\pm$ 0.7 km s*-1*, $V$=–21.0 $\pm$ 1.0 km s*-1*, and $W$=–7.9 $\pm$ 0.3 km s*-1*. This is 2.4 $\sigma$ (3.7 $\pm$ 1.5 km s*-1*) from the locus of $\epsilon$ Cha members from Gagné et al. (2018b). We also note that this star’s kinematics and distance (107 $\pm$ 2 pc) line up well with the locus of LCC members (0.9 $\sigma$, or 1.9 $\pm$ 2.2 km s*-1*). Its sky position is just beyond the canonical (albeit arbitrarily defined) southern boundary of LCC at $b$=–10, but all other indicators agree well with that association. We conclude that this star could plausibly belong to $\epsilon$ Cha or LCC, though the extended LCC is a better kinematic match.

2MASS J12445897–6026409 — This M1 star was identified as a potential member of LCC using BANYAN-$\Sigma$. We measure strong lithium absorption (EW$$\approx340 mÅ) consistent with LCC members of this spectral type. The space velocities of this system from $Gaia$ DR2 astrometry are $U$=–6.7 $\pm$ 0.4 km s*-1*, $V$=–18.3 $\pm$ 0.3 km s*-1*, and $W$=–4.5 $\pm$ 0.3 km s*-1*. This is 1.1 $\sigma$ (3.8 $\pm$ 3.4 km s*-1*) from the locus of LCC members from Gagné et al. (2018b). We conclude that this star is a previously unrecognized member LCC.

2MASS J13314666+2916368 — We measure unusually strong H$\alpha$ emission of –16.2 Å from this M5 star, suggesting it may originate from ongoing accretion. The parallactic distance from $Gaia$ is 18.3 pc. Riedel et al. (2014) identify this close binary as a possible member of Carina or Columba. If it is a member of either of these groups and if the strong H$\alpha$ originates from ongoing accretion, this would be an unusually long disk dissipation timescale possibly similar to the peculiar system found by Murphy et al. (2018).

2MASS J13493313–6818291 — Malo et al. (2013) identify this active M dwarf as a candidate member of Argus, but we find that the best hypothesis from BANYAN-$\Sigma$ is LCC. Janson et al. (2012) resolve it into a close visual triple. We measure a spectral type of M3 and find strong lithium (EW$$\approx360 mÅ) from our moderate-resolution Goodman spectrum, implying an age significantly younger than Argus ($\approx$40–50 Myr; Zuckerman 2018). The distance (99.8 $\pm$ 1.5 pc) and proper motion ($\mu_{\alpha}$cos$\delta$=–31.1 $\pm$ 0.2 mas yr*-1*, $\mu_{\delta}$=–19.7 $\pm$ 0.2 mas yr*-1*) is in good agreement with LCC. We conclude that this star is most likely an LCC member, but an RV is needed for confirmation.

2MASS J15354856–2958551 — This M4 star is noteworthy for having the strongest H$\alpha$ emission (EW$\approx$–43 Å) of any star for which we obtained a spectrum in this program, indicating active disk accretion. Brandner et al. (1996) resolve this star into a 0$\farcs$9 binary and Barenfeld et al. (2016) detect the disk in continuum and CO line emission with ALMA. Köhler et al. (2000) identify this star as a member of USco, but our BANYAN-$\Sigma$ analysis suggests it is a field star based on the UCAC4 proper motion (no astrometric solution is presented in $Gaia$ DR2). We measure strong lithium with an $EW$ of $\approx$500 mÅ, implying a young age consistent with members of the Sco-Cen complex and certainly less than a few tens of 10 Myr. We note that the sky position and proper motion align with UCL. We conclude that this star is a good candidate for UCL, but an RV and parallax are needed to fully assess membership in this subgroup.

2MASS J15451903–4431361 — This little-studied active M3 star shows strong lithium absorption (EW$$\approx380 mÅ) and was identified as a candidate UCL member using BANYAN-$\Sigma$. The sky position and proper motion are in good agreement with UCL membrs, but the distance from $Gaia$ DR2 of 89.3 $\pm$ 3.7 pc is much closer the vast majority of established members (Wright & Mamajek 2018). However, this does not exclude candidacy in that subgroup because our targets are intentionally biased to closer distances which would naturally sample the closest members of this complex. We also note that the $Gaia$ DR2 excess noise parameter for this target is quite large (3.1 mas), which may point to an unseen companion that could be affecting the five-parameter astrometric fit. We conclude that this star may be an unusually nearby member of UCL, but an RV (and perhaps better parallax solution) is needed for confirmation.

2MASS J16430128–1754274 — This active M1 star has been widely listed as a kinematic member of $\beta$ Pic (e.g., Kiss et al. 2010; Binks & Jeffries 2014; Shkolnik et al. 2017). However, the best hypothesis from BANYAN-$\Sigma$ is the field and it received a low membership probability in $\beta$ Pic by Malo et al. (2013). This star has strong lithium absorption, with $EW$ measurements of 300 $\pm$ 20 mÅ by Kiss et al. (2010), 364 $\pm$ 20 mÅ by Binks & Jeffries (2014), and $\approx$280 mÅ in this work from our low-resolution RC-Spec spectrum. Based on the $Gaia$ DR2 distance of 71.1 $\pm$ 0.3 pc and RV of –9.3 $\pm$ 0.4 km s*-1* from Malo et al. (2014a), the space velocities of this system are $U$=–7.6 $\pm$ 0.4 km s*-1*, $V$=–20.1 $\pm$ 0.08 km s*-1*, and $W$=–5.7 $\pm$ 0.13 km s*-1*. This is 5.0 $\sigma$ (6.0 $\pm$ 1.2 km s*-1*) from the locus of $\beta$ Pic members from Torres et al. (2008). We conclude that this star is a poor match with $\beta$ Pic and does not agree especially well with any other known nearby moving groups.

2MASS J16455062+0343014 — Schlieder et al. (2012b) and Schlieder et al. (2012c) identify this active M dwarf as a likely member of AB Dor, but the best hypothesis from BANYAN-$\Sigma$ is the field. We measure a spectral type of M2 and find modest lithium absorption ($EW$ $\approx$ 120 mÅ). We also resolve this source into a 2*′′* binary with Robo-AO and confirm that the pair are physically bound. Based on the $Gaia$ DR2 distance of 44.89 $\pm$ 0.08 pc and RV of –15.5 $\pm$ 0.7 km s*-1* from Schlieder et al. (2012c), the space velocities of this system are $U$=–2.3 $\pm$ 0.6 km s*-1*, $V$=–26.3 $\pm$ 0.2 km s*-1*, and $W$=–11.2 $\pm$ 0.3 km s*-1*. This is 3.4 $\sigma$ (5.0 $\pm$ 1.5 km s*-1*) from the locus of AB Dor members from Torres et al. (2008). However, when we use the RV of –21.7 $\pm$ 1.8 km s*-1* from $Gaia$ DR2, the space velocities of this system are $U$=–7.4 $\pm$ 1.4 km s*-1*, $V$=–28.2 $\pm$ 0.6 km s*-1*, and $W$=–14.2 $\pm$ 0.9 km s*-1*, or only 0.9 $\sigma$ (1.5 $\pm$ 1.6 km s*-1*) from the locus of AB Dor members. We conclude that this visual and spectroscopic binary remains an excellent candidate member of AB Dor. Longer-baseline RV monitoring will be useful to measure a systemic velocity for this pair.

2MASS J17213497–2152283 — We measure strong H$\alpha$ emission (EW$\approx$–13.4 Å) and lithium absorption (EW$\approx$370 mÅ) in this little-studied active M4 star. The best hypothesis from BANYAN-$\Sigma$ is UCL, but the sky position lies at the eastern edge of USco and disagrees with the UCL subgroup. However, the distance from $Gaia$ DR2 of 101.0 $\pm$ 0.7 pc places it closer than nearly all USco members (Wright & Mamajek 2018). We conclude that this star is likely related to the Sco-Cen complex, but perhaps not directly associated with the canonically defined subgroups.

2MASS J23093711–0225551 — This active K4 star was identified as a candidate member of Carina by Elliott et al. (2014) but the best hypothesis from BANYAN-$\Sigma$ is the field. Based on parallactic distance of 52.6 $\pm$ 0.4 pc and RV of –12.7 $\pm$ 0.4 km s*-1* from $Gaia$ DR2, the space velocities of this star are $U$=–9.64 $\pm$ 0.09 km s*-1*, $V$=–20.8 $\pm$ 0.2 km s*-1*, and $W$=–0.2 $\pm$ 0.3 km s*-1*. This is 3.4 $\sigma$ (4.7 $\pm$ 1.4 km s*-1*) from the locus of Carina members from Torres et al. (2008). The kinematics are in good agreement with Tuc-Hor, but this star would be a spatial outlier if it belongs to that group. We measure weak lithium (EW $\approx$ 130 mÅ) from our low-resolution Goodman spectrum, implying an age older than $\beta$ Pic but consistent with scatter in Tuc-Hor and AB Dor. We conclude that this star is most consistent with the field, but could be a kinematic outlier of Carina or perhaps a spatial outlier of Tuc-Hor.

6 Summary

The goal of this study is to identify new young stars in the solar neighborhood for future direct imaging surveys of exoplanets. We began with a sample of 2060 late-K through early-M dwarfs selected on the basis of X-ray and UV activity cuts, proper motions, NIR color cuts, and optical brightness. Follow-up low-resolution optical spectra were obtained for 632 stars, 58 of which show strong lithium absorption. Among the lithium-rich stars, 34 are previously known members of nearby moving groups while seven are new. The rest appear to be young field stars without any obvious connection to an established kinematic group. We also acquired Robo-AO observations of 1011 northern stars in our sample of active K/M dwarfs; 239 of these have nearby point sources within 4*′′*, the majority of which are likely to be physical companions. Many of these have kinematics consistent with young moving groups which long-baseline RV monitoring can better constrain by measuring systemic RVs.

It is a pleasure to thank Diane Harmer, Sean Points, and all support staff and telescope operators at KPNO and CTIO who helped make these observations possible. CZ is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto. VS was supported part from the John W. Cox Endowment for the Advanced Studies in Astronomy. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://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 publication 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. The Robo-AO system was developed by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, and with the support of the National Science Foundation under Grant Nos. AST-0906060, AST-0960343 and AST-1207891, the Mt. Cuba Astronomical Foundation and by a gift from Samuel Oschin. Ongoing science operation support of Robo-AO is provided by the California Institute of Technology and the University of Hawai‘i. C.B. acknowledges support from the Alfred P. Sloan Foundation. NASA’s Astrophysics Data System Bibliographic Services together with the VizieR catalogue access tool and SIMBAD database operated at CDS, Strasbourg, France, were invaluable resources for this work. Based on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope (NOAO Prop. ID 2013B-0496, 2014A-0019, 2015A-0016; PI: B. Bowler), which is a joint project of the Ministério da Ciência, Tecnologia, Inovaçãos e Comunicaçãoes (MCTIC) do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Based in part on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory (NOAO Prop. ID 2013B-0496, 2014A-0019, 2015A-0016; PI: B. Bowler), which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Institutional allocation for the Robo-AO observations at the P60 telescope was provided based on the prior affiliation of BPB and SH with the California Institute of Technology. The authors are honored to be permitted to conduct astronomical research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham.