Chemodynamics of newly identified giants with globular cluster like abundance patterns in the bulge, disk, and halo of the Milky Way

TL;DR

This study identifies and characterizes 31 nitrogen-rich giant stars in the Milky Way, revealing their unique chemical patterns and possible origins from globular clusters or disrupted dwarf galaxies, using APOGEE survey data.

Contribution

It uncovers a new population of nitrogen-rich giants with distinct chemical and orbital properties, linking them to globular clusters and the Galaxy's accretion history.

Findings

31 nitrogen-rich giants identified with high [N/Fe]

Some stars share orbital properties with the bulge/bar

Chemistry suggests origins from globular clusters or dwarf galaxies

Abstract

The latest edition of the APOGEE-2/DR14 survey catalogue and the first \texttt{Payne} data release of APOGEE abundance determinations by Ting et al. are examined. We identify 31 previously unremarked metal-poor giant stars with anomalously high levels of nitrogen in the chemical space defined by [Fe/H] and [N/Fe]. The APOGEE chemical abundance patterns of such objects revealed that these are chemically distinct from the Milky Way (MW) in most chemical elements. We have found all these objects have a [N/Fe]$>+0.5$, and are thus identified here as nitrogen-rich stars. An orbital analysis of these objects revealed that a handful of them shares the orbital properties of the bar/bulge, and possibly linked to tidal debris of surviving globular clusters trapped into the bar component. 3 of the 31 stars are actually halo interlopers into the bulge area, which suggests that halo contamination is not insignificant when studying N-rich stars found in the inner Galaxy, whereas the rest of the N-rich stars share orbital properties with the halo population. Most of the newly identified population exhibit chemistry similar to the so-called \textit{second-generation} globular cluster stars (enriched in aluminum, [Al/Fe]$>+0.5$), whereas a handful of them exhibit lower abundances of aluminum, [Al/Fe]$<+0.5$, which are thought to be chemically associated with the \textit{first-generation} of stars, as seen in globular clusters, or compatible with origin from a tidally disrupted dwarf galaxy.

Tables

Table 1. Table 1: Adopted atmospheric parameters of our target stars, radial velocity scatter information ( R ​ V S ​ C ​ A ​ T ​ T ​ E ​ R 𝑅 subscript 𝑉 𝑆 𝐶 𝐴 𝑇 𝑇 𝐸 𝑅 RV_{SCATTER} ), and frequency of observation per object (N visits ).

APOGEE$-$ID	Payne [Fe/H]	$J_{2MASS}-K_{s,2MASS}$	$⟨A_K^{WISE}⟩$	E(B-V)	T${}_{\mathrm{eff}}{}^{}{}_{}{}^{pho}$	logiso g	Payne Teff	Payne log g	RVSCATTER	Nvisits
	K	mag	mag		K	dex	K	dex	km s-1
2M01121802$+$6219193	$-1.421$	1.044	0.336	…	…	…	4931.82	2.253	0.08	3
2M02000451$-$0229333	$-1.289$	0.699	0.045	0.028	4614.73	1.499	4738.89	2.032	0.19	6
2M06273068$-$0440140	$-0.797$	0.798	0.151	0.420	5103.98	2.938	4752.06	2.160	0.07	3
2M11062158$-$0712222	$-0.893$	0.572	0.042	0.038	5039.55	2.673	4820.19	2.416	0.14	5
2M11514952$+$2015267	$-1.225$	0.644	0.071	0.048	4822.40	1.970	4726.44	2.235	0.06	3
2M12010401$-$0058306	$-1.009$	0.612	0.033	0.024	4880.99	2.247	4779.53	2.461	1.52	3
2M12042878$+$1949535	$-1.384$	0.645	0.026	0.022	4767.64	1.707	4824.94	2.208	0.15	3
2M12092246$+$0545111	$-1.289$	0.762	0.107	0.016	4412.57	1.131	4599.00	1.830	0.44	4
2M12444724$-$0207405	$-0.931$	0.615	0.067	0.033	4885.23	2.342	4859.61	2.439	0.15	3
2M13481355$-$0040484	$-1.014$	0.698	0.055	0.028	4618.69	1.731	4914.06	2.445	0.21	4
2M13503160$+$4411389	$-1.082$	0.499	0.061	0.012	5250.21	3.114	5142.27	3.201	0.17	3
2M14082554$+$4711096	$-1.118$	0.533	0.053	0.015	5128.05	2.719	5103.23	2.716	0.00	1
2M14582162$+$4117544	$-1.012$	0.876	0.091	0.013	4128.17	0.857	4204.34	1.434	0.00	1
2M15082716$+$6710075	$-1.302$	0.812	0.038	0.033	4309.77	0.947	4186.79	1.355	0.80	26
2M15183589$+$0027100	$-1.217$	0.769	0.095	0.058	4468.69	1.317	4444.12	1.643	0.35	13
2M15193208$+$0025293	$-0.760$	0.718	0.089	0.061	4625.32	1.916	4551.84	2.092	0.09	7
2M15195065$+$0221533	$-0.777$	0.679	0.070	0.041	4701.46	2.058	4583.81	1.918	0.00	1
2M15535831$+$4333280	$-1.256$	0.675	0.108	0.013	4656.55	1.576	4835.53	2.118	0.34	4
2M16362792$+$3901180	$-0.842$	0.668	0.055	0.018	4694.92	2.046	4628.36	2.247	0.04	2
2M16464310$+$4731033	$-1.013$	0.842	0.093	0.021	4221.58	1.023	4497.21	1.729	0.37	12
2M17294680$-$2644220	$-0.912$	1.486	0.493	…	…	…	4486.78	1.743	0.25	2
2M18022601$-$3106232	$-0.835$	0.977	0.326	…	…	…	4642.16	1.829	0.27	7
2M18110406$-$2602142	$-0.713$	1.117	0.190	…	…	…	4418.24	1.752	0.00	1
2M18200243$+$0156016	$-0.736$	1.168	0.322	0.710	4570.84	1.902	4047.75	1.449	0.16	3
2M18461977$-$3021506	$-1.002$	0.933	0.156	0.197	4278.82	1.124	4234.47	1.584	0.00	1
2M18472793$-$3033242	$-1.156$	0.783	0.101	0.173	4640.83	1.628	4647.83	1.891	0.00	1
2M18502108$-$2923442	$-1.023$	0.832	0.152	0.162	4484.83	1.490	4598.75	1.866	0.00	1
2M19004420$+$4421082	$-1.079$	0.658	0.088	0.069	4823.72	2.052	4813.71	2.332	0.16	3
2M20124750$+$1818007	$-0.863$	0.763	0.157	0.237	4827.49	2.216	4645.88	2.231	0.22	6
2M21181769$+$0946422	$-1.357$	0.783	0.116	0.049	4412.88	1.047	4624.36	1.525	0.00	1
2M22015914$+$1543129	$-0.795$	0.566	0.045	0.049	5086.80	2.893	4744.41	2.631	0.26	4

Table 2. Table 2: Mean elemental abundances derived for our target stars using the ”abund” module in BACCHUS code, adopting the atmospheric parameters from Payne -APOGEE (abundances labeled as [Fe/H]sp and [X/Fe]sp), and atmospheric parameters from photometry and isochrones (abundances labeled as [Fe/H]pho and [X/Fe]pho).

APOGEE$-$ID	[Fe/H]sp	[C/Fe]sp	[N/Fe]sp	[O/Fe]sp	[Mg/Fe]sp	[Al/Fe]sp	[Si/Fe]sp	[Ce/Fe]sp	[Nd/Fe]sp	[Na/Fe]sp	Classification
2M01121802$+$6219193	$-$1.34	$-$0.03	1.07	0.64	0.12	…	…	0.42	…	…	FG-like/dGs
2M02000451$-$0229333	$-$1.23	$-$0.03	0.89	0.55	0.18	$-$0.02	0.32	0.64	…	…	FG-like/dGs
2M06273068$-$0440140	$-$0.69	$-$0.29	0.79	0.35	0.05	0.19	0.26	0.24	0.83	…	FG-like/dGs
2M11062158$-$0712222	$-$0.82	$-$0.22	0.93	0.33	0.03	0.09	0.21	0.23	…	…	FG-like/dGs
2M11514952$+$2015267	$-$1.21	$-$0.08	0.84	0.40	0.18	0.07	0.38	0.05	…	…	FG-like/dGs
2M12010401$-$0058306	$-$1.12	$-$0.00	1.53	0.48	0.21	0.09	0.44	1.00	…	…	FG-like/dGs
2M12042878$+$1949535	$-$1.32	$-$0.19	1.15	0.59	0.27	0.31	0.24	0.37	1.11	…	FG-like/dGs
2M12092246$+$0545111	$-$1.17	$-$0.51	1.11	0.29	0.02	0.74	0.22	0.22	…	…	SG-like
2M12444724$-$0207405	$-$0.92	$-$0.27	1.20	0.42	0.09	0.39	0.36	0.32	0.76	…	FG-like/dGs
2M13481355$-$0040484	$-$0.91	$-$0.28	1.13	0.61	0.12	0.19	0.25	…	…	…	FG-like/dGs
2M13503160$+$4411389	$-$0.99	$-$0.33	1.34	…	0.01	0.90	0.23	…	…	…	SG-like
2M14082554$+$4711096	$-$1.08	$-$0.26	1.01	0.51	0.18	$-$0.01	0.32	$-$0.02	1.03	…	FG-like/dGs
2M14582162$+$4117544	$-$0.96	$-$0.42	0.62	0.24	0.08	0.16	0.17	0.24	0.28	…	FG-like/dGs
2M15082716$+$6710075	$-$1.49	0.02	1.36	0.58	$-$0.33	…	0.16	0.48	…	…	FG-like/dGs
2M15183589$+$0027100	$-$1.18	$-$0.33	0.95	0.25	0.11	0.16	0.16	0.17	…	…	FG-like/dGs
2M15193208$+$0025293	$-$0.80	0.02	0.88	0.38	0.26	0.24	0.59	0.25	…	0.30	FG-like/dGs
2M15195065$+$0221533	$-$0.83	$-$0.03	0.59	0.50	0.18	0.18	0.67	0.16	…	…	FG-like/dGs
2M15535831$+$4333280	$-$1.19	…	0.99	0.25	$-$0.43	1.07	0.54	0.38	0.84	…	SG-like
2M16362792$+$3901180	$-$0.75	$-$0.22	0.89	0.27	$-$0.02	0.07	0.27	0.25	…	…	FG-like/dGs
2M16464310$+$4731033	$-$0.99	$-$0.51	1.43	0.25	0.11	0.84	0.33	1.13	0.96	…	SG-like
2M17294680$-$2644220	$-$0.87	$-$0.38	0.88	0.42	0.22	0.24	0.32	0.22	…	…	FG-like/dGs
2M18022601$-$3106232	$-$0.82	$-$0.41	1.13	0.24	0.34	0.74	0.67	0.21	0.75	…	SG-like
2M18110406$-$2602142	$-$0.82	$-$0.23	1.09	0.22	0.18	0.46	0.58	0.40	…	…	FG-like/dGs
2M18200243$+$0156016	$-$0.71	$-$0.07	0.56	0.34	0.09	$-$0.07	0.22	$-$0.19	…	…	FG-like/dGs
2M18461977$-$3021506	$-$0.95	$-$0.27	0.84	0.26	0.04	0.13	0.22	0.35	…	0.04	FG-like/dGs
2M18472793$-$3033242	$-$1.06	…	1.06	0.38	0.28	0.58	0.46	0.10	…	…	SG-like
2M18502108$-$2923442	$-$0.97	$-$0.27	1.17	0.46	0.30	0.66	0.53	0.37	…	…	SG-like
2M19004420$+$4421082	$-$1.04	$-$0.46	1.40	0.38	0.13	0.26	0.33	0.67	0.70	…	FG-like/dGs
2M20124750$+$1818007	$-$0.83	$-$0.07	0.92	0.25	0.23	0.30	0.43	0.17	…	…	FG-like/dGs
2M21181769$+$0946422	$-$1.30	$-$0.52	1.29	0.57	0.14	0.26	0.32	0.25	…	0.85	FG-like/dGs
2M22015914$+$1543129	$-$0.78	$-$0.03	0.78	0.22	0.20	0.30	0.32	0.21	…	…	FG-like/dGs
	[Fe/H]pho	[C/Fe]pho	[N/Fe]pho	[O/Fe]pho	[Mg/Fe]pho	[Al/Fe]pho	[Si/Fe]pho	[Ce/Fe]pho	[Nd/Fe]pho	[Na/Fe]pho
2M01121802$+$6219193	…	…	…	…	…	…	…	…	…	…
2M02000451$-$0229333	$-$1.32	$-$0.17	0.90	0.48	0.22	$-$0.02	0.28	0.35	…	…
2M06273068$-$0440140	$-$0.65	$-$0.08	1.10	0.77	$-$0.09	0.15	0.14	0.67	…	…
2M11062158$-$0712222	$-$0.73	$-$0.19	1.09	0.53	0.01	0.10	0.16	0.17	…	…
2M11514952$+$2015267	$-$1.09	$-$0.40	1.10	0.56	0.30	0.11	0.29	$-$0.03	…	…
2M12010401$-$0058306	$-$1.06	0.12	1.40	0.59	0.29	0.12	0.33	0.92	…	…
2M12042878$+$1949535	$-$1.37	…	0.96	0.61	0.35	0.33	0.33	0.22	…	…
2M12092246$+$0545111	$-$1.29	$-$0.44	0.73	0.08	0.07	0.70	0.23	0.20	…	…
2M12444724$-$0207405	$-$0.90	$-$0.33	1.19	0.43	0.11	0.36	0.21	0.28	0.86	…
2M13481355$-$0040484	$-$1.12	$-$0.47	1.18	0.36	0.22	0.17	0.27	0.32	…	…
2M13503160$+$4411389	$-$0.98	$-$0.23	1.56	1.06	0.05	0.92	0.26	…	…	…
2M14082554$+$4711096	$-$1.02	$-$0.01	0.79	0.53	0.16	0.01	0.26	…	1.01	…
2M14582162$+$4117544	$-$1.08	$-$0.51	1.08	0.28	0.08	0.11	0.19	0.14	0.33	…
2M15082716$+$6710075	$-$1.39	$-$0.16	1.58	0.82	0.04	…	0.10	0.26	…	…
2M15183589$+$0027100	$-$1.15	$-$0.57	1.16	0.29	0.21	0.20	0.25	0.07	…	…
2M15193208$+$0025293	$-$0.81	$-$0.01	0.98	0.49	0.33	0.27	0.29	0.05	…	0.33
2M15195065$+$0221533	$-$0.77	$-$0.00	0.65	0.62	0.18	0.20	0.36	0.16	…	…
2M15535831$+$4333280	$-$1.29	…	0.74	0.13	$-$0.42	1.07	0.51	0.32	…	…
2M16362792$+$3901180	$-$0.73	$-$0.31	1.06	0.43	0.09	0.07	0.18	0.14	…	…
2M16464310$+$4731033	$-$1.22	$-$0.66	1.54	0.07	…	0.49	0.36	0.64	…	…
2M17294680$-$2644220	…	…	…	…	…	…	…	…	…	…
2M18022601$-$3106232	…	…	…	…	…	…	…	…	…	…
2M18110406$-$2602142	…	…	…	…	…	…	…	…	…	…
2M18200243$+$0156016	$-$0.56	$-$0.08	1.18	1.17	0.19	0.20	0.25	0.10	…	…
2M18461977$-$3021506	$-$1.00	$-$0.41	1.10	0.45	0.08	0.15	0.21	0.31	…	0.09
2M18472793$-$3033242	$-$1.15	…	1.08	0.47	0.18	0.45	0.28	0.10	…	…
2M18502108$-$2923442	$-$1.02	$-$0.30	1.11	0.37	0.38	0.68	0.52	0.24	…	…
2M19004420$+$4421082	$-$0.98	$-$0.49	1.39	0.38	0.22	0.31	0.28	0.56	…	…
2M20124750$+$1818007	$-$0.79	$-$0.06	1.13	0.54	0.25	0.34	0.20	0.17	…	…
2M21181769$+$0946422	$-$1.42	$-$0.55	1.17	0.34	0.20	0.25	0.35	0.18	…	0.47
2M22015914$+$1543129	$-$0.64	0.07	0.99	0.63	0.27	0.19	0.28	0.10	…	…

Table 3. Table 3: N-rich giants as tracers of extra-tidal features around Galactic globular clusters

APOGEE$-$ID	[Fe/H]	RV	Nearby GC	[Fe/H]gc	RVgc	rt,gc	separation	Extra-tidal N-rich giant
	[dex]	[km s-1]		[dex]	[km s-1]	arcmin	arcmin	candidates
2M15183589+0027100	$-$1.18	$-$56.27$\pm$0.34	Pal 5	$-$1.41	$-$58.6$\pm$0.2	16.28	50.7	likely
2M18110406-2602142	$-$0.82	$-$24.96$\pm$0.01	NGC 6553	$-$0.18	0.7$\pm$0.4	8.16	25.2	unlikely
2M15195065+0221533	$-$0.83	$-$158.58$\pm$0.01	NGC 5904	$-$1.29	53.7$\pm$0.3	28.4	25.8	unlikely
2M16464310+4731033	$-$0.99	$-$139.80$\pm$0.37	NGC 6229	$-$1.47	$-$138.6$\pm$0.8	5.38	2.7	unlikely

Table 4. Table 4: Abundance determination sensitivity to the stellar parameters from our present measurements.

APOGEE$-$ID	$X$	${\sigma }_{\left[X/H\right],T_{\mathrm{eff}}}$	${\sigma }_{\left[X/H\right],logg}$	${\sigma }_{\left[X/H\right],{\xi }_t}$	${\sigma }_{mean}$	${\sigma }_{total}$
2M01121802$+$6219193	Fe	0.048	0.010	0.015	0.102	0.114
2M01121802$+$6219193	C	0.011	0.085	0.117	0.315	0.347
2M01121802$+$6219193	N	0.158	0.092	0.138	0.169	0.285
2M01121802$+$6219193	O	0.134	0.027	0.012	0.051	0.147
2M01121802$+$6219193	Mg	0.061	0.041	0.025	0.022	0.082
2M01121802$+$6219193	Al	..	..	..	..	..
2M01121802$+$6219193	Si	..	..	..	..	..
2M01121802$+$6219193	Ce	0.054	0.090	0.098	..	0.144
2M01121802$+$6219193	Nd	..	..	..	..	..
2M01121802$+$6219193	Na	..	..	..	..	..
2M02000451$-$0229333	Fe	0.040	0.010	0.005	0.101	0.109
2M02000451$-$0229333	C	0.081	0.179	0.032	0.102	0.224
2M02000451$-$0229333	N	0.080	0.143	0.054	0.111	0.205
2M02000451$-$0229333	O	0.123	0.021	0.005	0.131	0.181
2M02000451$-$0229333	Mg	0.058	0.055	0.007	0.011	0.081
2M02000451$-$0229333	Al	0.056	0.017	0.006	0.074	0.094
2M02000451$-$0229333	Si	0.022	0.020	0.011	0.081	0.088
2M02000451$-$0229333	Ce	0.118	0.045	0.015	0.042	0.134
2M02000451$-$0229333	Nd	0.0	..	..	..	..
2M02000451$-$0229333	Na	..	..	..	..	..
2M06273068$-$0440140	Fe	0.047	0.024	0.024	0.087	0.105
2M06273068$-$0440140	C	0.012	0.094	0.010	0.050	0.108
2M06273068$-$0440140	N	0.168	0.118	0.005	0.067	0.216
2M06273068$-$0440140	O	0.102	0.034	0.017	0.185	0.215
2M06273068$-$0440140	Mg	0.072	0.106	0.031	0.026	0.135
2M06273068$-$0440140	Al	0.063	0.063	0.027	0.030	0.098
2M06273068$-$0440140	Si	0.022	0.007	0.008	0.118	0.120
2M06273068$-$0440140	Ce	0.066	0.036	0.053	0.133	0.162
2M06273068$-$0440140	Nd	0.041	0.124	0.019	0.154	0.203
2M06273068$-$0440140	Na	..	..	..	..	..
2M11062158$-$0712222	Fe	0.066	0.015	0.026	0.058	0.094
2M11062158$-$0712222	C	0.015	0.025	0.044	0.137	0.147
2M11062158$-$0712222	N	0.155	0.016	0.064	0.038	0.173
2M11062158$-$0712222	O	0.150	0.022	0.017	0.128	0.200
2M11062158$-$0712222	Mg	0.093	0.072	0.022	0.033	0.125
2M11062158$-$0712222	Al	0.092	0.026	0.030	0.077	0.127
2M11062158$-$0712222	Si	0.060	0.037	0.027	0.074	0.106
2M11062158$-$0712222	Ce	0.018	0.057	0.013	0.115	0.130
2M11062158$-$0712222	Nd	..	..	..	..	..
2M11062158$-$0712222	Na	..	..	..	..	..
2M11514952$+$2015267	Fe	0.053	0.035	0.046	0.084	0.115
2M11514952$+$2015267	C	0.035	0.128	0.065	0.073	0.165
2M11514952$+$2015267	N	0.162	0.147	0.129	0.087	0.269
2M11514952$+$2015267	O	0.138	0.073	0.072	0.135	0.219
2M11514952$+$2015267	Mg	0.084	0.085	0.060	0.034	0.139
2M11514952$+$2015267	Al	0.071	0.049	0.061	0.073	0.129
2M11514952$+$2015267	Si	0.028	0.013	0.031	0.061	0.075
2M11514952$+$2015267	Ce	0.044	0.069	0.036	0.020	0.092
2M11514952$+$2015267	Nd	..	..	..	..	..
2M11514952$+$2015267	Na	..	..	..	..	..
2M12010401$-$0058306	Fe	0.042	5.421	0.008	0.122	0.129
2M12010401$-$0058306	C	0.047	0.087	0.004	0.072	0.123
2M12010401$-$0058306	N	0.082	0.054	0.016	0.087	0.133
2M12010401$-$0058306	O	0.137	0.023	0.006	0.180	0.228
2M12010401$-$0058306	Mg	0.086	0.072	0.008	0.044	0.121
2M12010401$-$0058306	Al	0.066	0.017	0.011	0.112	0.132
2M12010401$-$0058306	Si	0.034	0.035	0.015	0.145	0.154
2M12010401$-$0058306	Ce	0.057	0.123	0.033	0.089	0.166
2M12010401$-$0058306	Nd	..	..	..	..	..
2M12010401$-$0058306	Na	..	..	..	..	..
2M12042878$+$1949535	Fe	0.050	0.015	0.002	0.103	0.116
2M12042878$+$1949535	C	0.036	0.084	0.001	..	0.091
2M12042878$+$1949535	N	0.250	0.084	0.002	0.119	0.289
2M12042878$+$1949535	O	0.132	0.029	9.994	0.087	0.161
2M12042878$+$1949535	Mg	0.085	0.065	0.006	0.057	0.122
2M12042878$+$1949535	Al	0.081	0.034	0.005	0.043	0.098
2M12042878$+$1949535	Si	0.037	0.023	0.036	0.093	0.109
2M12042878$+$1949535	Ce	0.075	0.116	0.009	0.111	0.177
2M12042878$+$1949535	Nd	0.067	0.092	0.022	0.024	0.118
2M12042878$+$1949535	Na	..	..	..	..	..
2M12092246$+$0545111	Fe	0.047	0.021	0.009	0.096	0.110
2M12092246$+$0545111	C	0.064	0.110	0.030	0.016	0.132
2M12092246$+$0545111	N	0.190	0.093	0.030	0.059	0.222
2M12092246$+$0545111	O	0.141	0.027	0.010	0.193	0.241
2M12092246$+$0545111	Mg	0.067	0.044	0.010	0.005	0.081
2M12092246$+$0545111	Al	0.092	0.051	0.014	0.063	0.123
2M12092246$+$0545111	Si	0.027	0.036	0.019	0.094	0.106
2M12092246$+$0545111	Ce	0.164	0.158	0.004	..	0.228
2M12092246$+$0545111	Nd	..	..	..	..	..
2M12092246$+$0545111	Na	..	..	..	..	..

Table 5. Table 5: (continued)

APOGEE$-$ID	$X$	${\sigma }_{\left[X/H\right],T_{\mathrm{eff}}}$	${\sigma }_{\left[X/H\right],logg}$	${\sigma }_{\left[X/H\right],{\xi }_t}$	${\sigma }_{mean}$	${\sigma }_{total}$
2M12444724$-$0207405	Fe	0.043	0.012	0.005	0.089	0.100
2M12444724$-$0207405	C	0.043	0.083	0.082	0.075	0.146
2M12444724$-$0207405	N	0.106	0.053	0.089	0.140	0.204
2M12444724$-$0207405	O	0.113	0.018	0.002	0.172	0.207
2M12444724$-$0207405	Mg	0.065	0.078	0.006	0.035	0.108
2M12444724$-$0207405	Al	0.073	0.035	0.013	0.063	0.104
2M12444724$-$0207405	Si	0.070	0.066	0.073	0.119	0.170
2M12444724$-$0207405	Ce	0.012	0.038	0.014	0.093	0.102
2M12444724$-$0207405	Nd	0.106	0.001	0.031	..	0.110
2M12444724$-$0207405	Na	..	..	..	..	..
2M13481355$-$0040484	Fe	0.055	0.018	0.015	0.083	0.102
2M13481355$-$0040484	C	0.056	0.076	0.032	…	0.099
2M13481355$-$0040484	N	0.167	0.059	0.045	0.057	0.192
2M13481355$-$0040484	O	0.145	0.043	0.026	0.175	0.233
2M13481355$-$0040484	Mg	0.076	0.073	0.010	0.027	0.110
2M13481355$-$0040484	Al	0.065	0.021	0.011	0.045	0.083
2M13481355$-$0040484	Si	0.037	0.034	0.013	0.048	0.071
2M13481355$-$0040484	Ce	..	..	..	..	..
2M13481355$-$0040484	Nd	..	..	..	..	..
2M13481355$-$0040484	Na	..	..	..	..	..
2M13503160$+$4411389	Fe	0.051	0.021	0.014	0.110	0.124
2M13503160$+$4411389	C	0.049	0.220	0.100	0.089	0.263
2M13503160$+$4411389	N	0.054	0.164	0.007	0.137	0.221
2M13503160$+$4411389	O	..	..	..	..	..
2M13503160$+$4411389	Mg	0.073	0.077	0.006	0.010	0.108
2M13503160$+$4411389	Al	0.085	0.095	0.006	0.120	0.176
2M13503160$+$4411389	Si	0.033	0.012	0.025	0.075	0.087
2M13503160$+$4411389	Ce	..	..	..	..	..
2M13503160$+$4411389	Nd	..	..	..	..	..
2M13503160$+$4411389	Na	..	..	..	..	..
2M14082554$+$4711096	Fe	0.047	0.016	0.041	0.088	0.110
2M14082554$+$4711096	C	0.132	0.152	0.117	..	0.134
2M14082554$+$4711096	N	0.246	0.102	0.052	0.161	0.316
2M14082554$+$4711096	O	0.129	0.032	0.035	0.162	0.212
2M14082554$+$4711096	Mg	0.068	0.075	0.036	0.021	0.110
2M14082554$+$4711096	Al	0.060	0.027	0.055	0.075	0.114
2M14082554$+$4711096	Si	0.036	0.015	0.022	0.089	0.100
2M14082554$+$4711096	Ce	0.001	0.001	0.009	..	0.009
2M14082554$+$4711096	Nd	0.043	0.043	0.049	..	0.078
2M14082554$+$4711096	Na	..	..	..	..	..
2M14582162$+$4117544	Fe	0.031	0.056	0.022	0.083	0.107
2M14582162$+$4117544	C	0.018	0.073	0.002	0.151	0.169
2M14582162$+$4117544	N	0.211	0.227	0.181	0.038	0.362
2M14582162$+$4117544	O	0.164	0.039	0.025	0.119	0.208
2M14582162$+$4117544	Mg	0.066	0.045	0.030	0.042	0.095
2M14582162$+$4117544	Al	0.079	0.040	0.030	0.027	0.098
2M14582162$+$4117544	Si	0.069	0.113	0.065	0.044	0.154
2M14582162$+$4117544	Ce	0.048	0.111	0.014	0.042	0.129
2M14582162$+$4117544	Nd	0.027	0.006	0.008	..	0.029
2M14582162$+$4117544	Na	..	..	..	..	..
2M15082716$+$6710075	Fe	0.040	0.048	0.018	0.167	0.180
2M15082716$+$6710075	C	0.014	0.041	0.008	0.086	0.097
2M15082716$+$6710075	N	0.115	0.051	0.012	0.122	0.176
2M15082716$+$6710075	O	0.146	0.042	0.012	0.087	0.176
2M15082716$+$6710075	Mg	0.064	0.001	0.014	0.044	0.079
2M15082716$+$6710075	Al	..	..	..	..	..
2M15082716$+$6710075	Si	0.026	0.039	0.081	0.014	0.095
2M15082716$+$6710075	Ce	0.044	0.089	0.025	0.100	0.144
2M15082716$+$6710075	Nd	..	..	..	..	..
2M15082716$+$6710075	Na	..	..	..	..	..
2M15183589$+$0027100	Fe	0.030	0.009	0.009	0.095	0.101
2M15183589$+$0027100	C	0.095	0.122	0.002	0.233	0.280
2M15183589$+$0027100	N	0.038	0.112	0.012	0.145	0.188
2M15183589$+$0027100	O	0.148	0.016	0.001	0.111	0.186
2M15183589$+$0027100	Mg	0.062	0.048	0.017	0.047	0.093
2M15183589$+$0027100	Al	0.064	0.019	0.016	0.060	0.091
2M15183589$+$0027100	Si	0.060	0.064	0.034	0.067	0.116
2M15183589$+$0027100	Ce	0.018	0.060	0.009	0.061	0.088
2M15183589$+$0027100	Nd	..	..	..	..	..
2M15183589$+$0027100	Na	..	..	..	..	..
2M15193208$+$0025293	Fe	0.037	0.021	0.005	0.085	0.095
2M15193208$+$0025293	C	0.029	0.075	0.012	0.192	0.209
2M15193208$+$0025293	N	0.070	0.049	0.014	0.053	0.103
2M15193208$+$0025293	O	0.108	0.015	0.002	0.107	0.153
2M15193208$+$0025293	Mg	0.086	0.108	0.009	0.031	0.142
2M15193208$+$0025293	Al	0.086	0.061	0.010	0.090	0.139
2M15193208$+$0025293	Si	0.078	0.083	0.115	0.091	0.187
2M15193208$+$0025293	Ce	0.069	0.032	0.080	0.065	0.128
2M15193208$+$0025293	Nd	..	..	..	..	..
2M15193208$+$0025293	Na	0.021	0.014	..	..	0.025
2M15195065$+$0221533	Fe	0.087	0.082	0.005	0.134	0.180
2M15195065$+$0221533	C	0.052	0.082	0.007	0.217	0.238
2M15195065$+$0221533	N	0.069	0.037	0.021	0.045	0.093
2M15195065$+$0221533	O	0.128	0.046	0.002	0.105	0.172
2M15195065$+$0221533	Mg	0.159	0.160	0.009	0.035	0.229
2M15195065$+$0221533	Al	0.107	0.097	0.010	0.070	0.162
2M15195065$+$0221533	Si	0.018	0.018	0.127	0.065	0.145
2M15195065$+$0221533	Ce	0.043	0.129	8.498	0.009	0.136
2M15195065$+$0221533	Nd	..	..	..	..	..
2M15195065$+$0221533	Na	..	..	..	..	..

Table 6. Table 6: (continued)

APOGEE$-$ID	$X$	${\sigma }_{\left[X/H\right],T_{\mathrm{eff}}}$	${\sigma }_{\left[X/H\right],logg}$	${\sigma }_{\left[X/H\right],{\xi }_t}$	${\sigma }_{mean}$	${\sigma }_{total}$
2M15535831$+$4333280	Fe	0.025	0.002	0.017	0.084	0.090
2M15535831$+$4333280	C	..	..	..	..	..
2M15535831$+$4333280	N	0.037	0.058	0.034	0.109	0.134
2M15535831$+$4333280	O	0.069	0.086	0.047	0.225	0.255
2M15535831$+$4333280	Mg	0.026	0.017	0.026	0.074	0.085
2M15535831$+$4333280	Al	0.054	0.051	0.022	0.016	0.079
2M15535831$+$4333280	Si	0.011	0.032	0.010	0.091	0.098
2M15535831$+$4333280	Ce	0.013	0.233	0.080	0.015	0.247
2M15535831$+$4333280	Nd	0.011	0.066	0.041	..	0.078
2M15535831$+$4333280	Na	..	..	..	..	..
2M16362792$+$3901180	Fe	0.039	0.016	0.018	0.074	0.087
2M16362792$+$3901180	C	0.022	0.093	0.024	0.053	0.112
2M16362792$+$3901180	N	0.084	0.080	0.060	0.070	0.149
2M16362792$+$3901180	O	0.105	0.042	0.049	0.178	0.216
2M16362792$+$3901180	Mg	0.052	0.074	0.032	0.121	0.155
2M16362792$+$3901180	Al	0.077	0.039	0.006	0.048	0.099
2M16362792$+$3901180	Si	0.047	0.048	0.011	0.121	0.139
2M16362792$+$3901180	Ce	0.042	0.160	0.045	0.051	0.179
2M16362792$+$3901180	Nd	..	..	..	..	..
2M16362792$+$3901180	Na	..	..	..	..	..
2M16464310$+$4731033	Fe	0.036	0.031	0.010	0.132	0.141
2M16464310$+$4731033	C	0.069	0.089	0.119	0.046	0.170
2M16464310$+$4731033	N	0.118	0.066	0.146	0.112	0.229
2M16464310$+$4731033	O	0.110	0.041	0.020	0.071	0.139
2M16464310$+$4731033	Mg	0.071	0.033	0.016	0.098	0.127
2M16464310$+$4731033	Al	0.098	0.038	0.018	0.039	0.114
2M16464310$+$4731033	Si	0.021	0.065	0.028	0.104	0.128
2M16464310$+$4731033	Ce	0.046	0.154	0.029	0.131	0.210
2M16464310$+$4731033	Nd	0.058	0.060	0.100	..	0.130
2M16464310$+$4731033		..	..	..	..	..
2M17294680$-$2644220	Fe	0.031	0.040	0.020	0.065	0.086
2M17294680$-$2644220	C	0.016	0.075	0.007	0.151	0.170
2M17294680$-$2644220	N	0.144	0.056	0.037	0.123	0.202
2M17294680$-$2644220	O	0.115	0.040	0.022	0.069	0.142
2M17294680$-$2644220	Mg	0.080	0.126	0.036	0.036	0.158
2M17294680$-$2644220	Al	0.062	0.062	0.019	0.054	0.105
2M17294680$-$2644220	Si	0.075	0.089	0.005	0.140	0.182
2M17294680$-$2644220	Ce	0.023	0.071	0.010	0.065	0.099
2M17294680$-$2644220	Nd	..	..	..	..	..
2M17294680$-$2644220	Na	..	..	..	..	..
2M18022601$-$3106232	Fe	0.077	0.065	0.052	0.070	0.134
2M18022601$-$3106232	C	0.031	0.160	0.022	0.141	0.216
2M18022601$-$3106232	N	0.099	0.177	0.086	0.070	0.231
2M18022601$-$3106232	O	0.084	0.079	0.077	0.140	0.197
2M18022601$-$3106232	Mg	0.120	0.123	0.061	0.075	0.198
2M18022601$-$3106232	Al	0.112	0.091	0.050	0.116	0.192
2M18022601$-$3106232	Si	0.012	0.007	0.015	0.088	0.090
2M18022601$-$3106232	Ce	0.019	0.069	0.022	0.048	0.089
2M18022601$-$3106232	Nd	0.080	0.001	0.044	0.154	0.179
2M18022601$-$3106232	Na	0.027	..	0.009	..	0.028
2M18110406$-$2602142	Fe	0.115	0.085	0.005	0.102	0.176
2M18110406$-$2602142	C	0.049	0.143	0.035	0.145	0.213
2M18110406$-$2602142	N	0.235	0.103	0.049	0.075	0.272
2M18110406$-$2602142	O	0.141	0.027	0.014	0.040	0.150
2M18110406$-$2602142	Mg	0.213	0.150	0.011	0.025	0.262
2M18110406$-$2602142	Al	0.225	0.163	0.011	0.040	0.281
2M18110406$-$2602142	Si	0.076	0.063	0.097	0.116	0.181
2M18110406$-$2602142	Ce	0.030	0.050	0.005	0.060	0.084
2M18110406$-$2602142	Nd	..	..	..	..	..
2M18110406$-$2602142	Na	..	..	..	..	..
2M18200243$+$0156016	Fe	0.028	0.045	0.038	0.092	0.113
2M18200243$+$0156016	C	0.053	0.126	0.017	0.093	0.167
2M18200243$+$0156016	N	0.190	0.112	0.086	0.054	0.244
2M18200243$+$0156016	O	0.130	0.045	0.038	0.068	0.158
2M18200243$+$0156016	Mg	0.061	0.070	0.051	0.034	0.111
2M18200243$+$0156016	Al	0.101	0.007	0.077	0.098	0.161
2M18200243$+$0156016	Si	0.048	0.057	0.135	0.133	0.204
2M18200243$+$0156016	Ce	0.137	0.112	0.026	0.081	0.197
2M18200243$+$0156016	Nd	..	..	..	..	..
2M18200243$+$0156016	Na	..	..	..	..	..
2M18461977$-$3021506	Fe	0.041	0.044	0.022	0.098	0.117
2M18461977$-$3021506	C	0.051	0.074	0.022	0.035	0.100
2M18461977$-$3021506	N	0.114	0.077	0.053	0.119	0.190
2M18461977$-$3021506	O	0.152	0.023	0.013	0.094	0.181
2M18461977$-$3021506	Mg	0.069	0.063	0.025	0.065	0.117
2M18461977$-$3021506	Al	0.087	0.047	0.026	0.094	0.139
2M18461977$-$3021506	Si	0.071	0.078	0.046	0.056	0.128
2M18461977$-$3021506	Ce	0.019	0.168	0.028	0.024	0.174
2M18461977$-$3021506	Nd	..	..	..	..	..
2M18461977$-$3021506	Na	0.006	0.009	0.004	..	0.012
2M18472793$-$3033242	Fe	0.036	0.015	0.028	0.156	0.163
2M18472793$-$3033242	C	..	..	..	..	..
2M18472793$-$3033242	N	0.126	0.036	0.026	0.114	0.176
2M18472793$-$3033242	O	0.124	0.021	0.022	0.175	0.217
2M18472793$-$3033242	Mg	0.078	0.067	0.027	0.073	0.130
2M18472793$-$3033242	Al	0.107	0.092	0.019	0.102	0.176
2M18472793$-$3033242	Si	0.070	0.079	0.032	0.111	0.157
2M18472793$-$3033242	Ce	0.018	0.075	0.012	0.018	0.081
2M18472793$-$3033242	Nd	..	..	..	..	..
2M18472793$-$3033242	Na	..	..	..	..	..

Table 7. Table 7: (continued)

APOGEE$-$ID	$X$	${\sigma }_{\left[X/H\right],T_{\mathrm{eff}}}$	${\sigma }_{\left[X/H\right],logg}$	${\sigma }_{\left[X/H\right],{\xi }_t}$	${\sigma }_{mean}$	${\sigma }_{total}$
2M18502108$-$2923442	Fe	0.037	0.004	0.005	0.073	0.082
2M18502108$-$2923442	C	0.027	0.069	0.001	0.184	0.199
2M18502108$-$2923442	N	0.077	0.036	0.002	0.044	0.096
2M18502108$-$2923442	O	0.127	0.018	0.001	0.083	0.153
2M18502108$-$2923442	Mg	0.084	0.081	0.011	0.054	0.129
2M18502108$-$2923442	Al	0.079	0.041	0.012	0.025	0.093
2M18502108$-$2923442	Si	0.013	0.016	0.018	0.050	0.057
2M18502108$-$2923442	Ce	0.032	0.058	0.013	0.090	0.112
2M18502108$-$2923442	Nd	..	..	..	..	..
2M18502108$-$2923442	Na	..	..	..	..	..
2M19004420$+$4421082	Fe	0.046	0.014	0.018	0.093	0.106
2M19004420$+$4421082	C	0.074	0.108	0.044	0.074	0.157
2M19004420$+$4421082	N	0.098	0.107	0.023	0.030	0.151
2M19004420$+$4421082	O	0.115	0.060	0.012	0.050	0.140
2M19004420$+$4421082	Mg	0.064	0.063	0.022	0.009	0.093
2M19004420$+$4421082	Al	0.073	0.025	0.028	0.052	0.098
2M19004420$+$4421082	Si	0.024	0.018	0.010	0.062	0.070
2M19004420$+$4421082	Ce	0.037	0.091	0.023	0.158	0.188
2M19004420$+$4421082	Nd	0.075	0.001	0.001	0.021	0.078
2M19004420$+$4421082	Na	..	..	..	..	..
2M20124750$+$1818007	Fe	0.039	0.009	0.007	0.118	0.125
2M20124750$+$1818007	C	0.007	0.069	0.001	0.153	0.168
2M20124750$+$1818007	N	0.169	0.042	0.012	0.064	0.186
2M20124750$+$1818007	O	0.133	0.016	0.009	0.180	0.225
2M20124750$+$1818007	Mg	0.082	0.106	0.011	0.038	0.140
2M20124750$+$1818007	Al	0.054	0.016	0.020	0.052	0.080
2M20124750$+$1818007	Si	0.044	0.052	0.056	0.094	0.129
2M20124750$+$1818007	Ce	0.024	0.084	0.001	0.044	0.098
2M20124750$+$1818007	Nd	..	..	..	..	..
2M20124750$+$1818007	Na	..	..	..	..	..
2M21181769$+$0946422	Fe	0.042	0.014	0.018	0.095	0.107
2M21181769$+$0946422	C	0.083	0.061	0.007	0.151	0.183
2M21181769$+$0946422	N	0.052	0.053	0.023	0.050	0.093
2M21181769$+$0946422	O	0.148	0.029	0.018	0.140	0.207
2M21181769$+$0946422	Mg	0.079	0.029	0.027	0.028	0.093
2M21181769$+$0946422	Al	0.055	0.018	0.028	0.090	0.111
2M21181769$+$0946422	Si	0.028	0.045	0.027	0.088	0.107
2M21181769$+$0946422	Ce	0.010	0.064	0.009	0.065	0.092
2M21181769$+$0946422	Nd	..	..	..	..	..
2M21181769$+$0946422	Na	..	..	..	..	..
2M22015914$+$1543129	Fe	0.032	0.010	0.004	0.090	0.096
2M22015914$+$1543129	C	0.038	0.116	0.009	0.036	0.127
2M22015914$+$1543129	N	0.129	0.086	0.009	0.070	0.170
2M22015914$+$1543129	O	0.090	0.026	0.002	0.164	0.189
2M22015914$+$1543129	Mg	0.083	0.113	0.005	0.045	0.148
2M22015914$+$1543129	Al	0.054	0.046	0.011	0.140	0.157
2M22015914$+$1543129	Si	0.023	0.018	0.007	0.048	0.057
2M22015914$+$1543129	Ce	0.015	0.062	0.004	..	0.064
2M22015914$+$1543129	Nd	..	..	..	..	..
2M22015914$+$1543129	Na	..	..	..	..	..

Table 8. Table 8: Orbital elements obtained using a simple Monte Carlo approach for the 31 N-rich stars. The average value of the orbital elements (pericentric and apocentric radii, the eccentricity, the maximum distance the orbit reaches above/below the Galactic plane, as well as the maximum and minimum of the z -component of the angular momentum in the inertial frame, L z subscript 𝐿 𝑧 L_{z} ) was found for the half million realizations, with uncertainty ranges given by the 16th (subscript) and 84th (superscript) percentile values.

${\Omega }_{bar}$	APOGEE$-$ID	RA	DEC	$RV\pm \Delta$	$d\pm \Delta$	${\mu }_{\alpha }\pm \Delta$	${\mu }_{\delta }\pm \Delta$	$⟨r_{min}⟩$	$⟨r_{max}⟩$	$⟨e⟩$	$⟨Z_{max}⟩$	$⟨L_{z,min}⟩$	$⟨L_{z,max}⟩$
km s-1 kpc-1		(∘)	(∘)	km s-1	kpc	mas yr-1	mas yr-1	kpc	kpc		kpc	km s-1 kpc-1	km s-1 kpc-1
35	2M01121802$+$6219193	18.075099	62.322044	$-$256.06$\pm$0.07	4.02$\pm$0.39	5.369$\pm$0.031	$-$1.376$\pm$0.035	0.05${}_{0.02}{}^{}{}_{}{}^{0.10}$	11.73${}_{11.51}{}^{}{}_{}{}^{12.04}$	0.99${}_{0.98}{}^{}{}_{}{}^{0.99}$	0.37${}_{0.35}{}^{}{}_{}{}^{0.40}$	$-$9.0${}_{-15.0}{}^{}{}_{}{}^{0.0}$	11.0${}_{7.0}{}^{}{}_{}{}^{21.0}$
40								0.06${}_{0.02}{}^{}{}_{}{}^{0.10}$	12.59${}_{11.48}{}^{}{}_{}{}^{12.70}$	0.99${}_{0.98}{}^{}{}_{}{}^{0.99}$	0.37${}_{0.35}{}^{}{}_{}{}^{0.40}$	$-$15.0${}_{-20.0}{}^{}{}_{}{}^{-5.0}$	9.0${}_{3.0}{}^{}{}_{}{}^{18.0}$
45								0.05${}_{0.02}{}^{}{}_{}{}^{0.12}$	12.29${}_{11.86}{}^{}{}_{}{}^{13.49}$	0.99${}_{0.97}{}^{}{}_{}{}^{0.99}$	0.39${}_{0.36}{}^{}{}_{}{}^{0.44}$	$-$12.0${}_{-24.0}{}^{}{}_{}{}^{-10.0}$	4.0${}_{-4.0}{}^{}{}_{}{}^{12.0}$
50								0.09${}_{0.04}{}^{}{}_{}{}^{0.18}$	13.81${}_{13.50}{}^{}{}_{}{}^{14.02}$	0.98${}_{0.97}{}^{}{}_{}{}^{0.99}$	0.37${}_{0.36}{}^{}{}_{}{}^{0.42}$	$-$26.0${}_{-35.0}{}^{}{}_{}{}^{-13.0}$	7.0${}_{-1.2}{}^{}{}_{}{}^{21.0}$
35	2M02000451$-$0229333	30.018804	$-$2.492584	68.68$\pm$0.19	7.89$\pm$1.13	3.701$\pm$0.076	$-$4.492$\pm$0.048	1.28${}_{0.36}{}^{}{}_{}{}^{2.27}$	14.45${}_{13.69}{}^{}{}_{}{}^{15.38}$	0.83${}_{0.71}{}^{}{}_{}{}^{0.95}$	11.62${}_{8.79}{}^{}{}_{}{}^{15.23}$	$-$56.0${}_{-93.0}{}^{}{}_{}{}^{-14.0}$	$-$45.0${}_{-84.0}{}^{}{}_{}{}^{-2.0}$
40								1.11${}_{0.39}{}^{}{}_{}{}^{2.13}$	14.84${}_{13.98}{}^{}{}_{}{}^{15.68}$	0.86${}_{0.73}{}^{}{}_{}{}^{0.94}$	11.74${}_{8.99}{}^{}{}_{}{}^{15.05}$	$-$56.0${}_{-96.0}{}^{}{}_{}{}^{-17.0}$	$-$39.0${}_{-78.0}{}^{}{}_{}{}^{-7.0}$
45								1.09${}_{0.33}{}^{}{}_{}{}^{2.00}$	14.25${}_{13.76}{}^{}{}_{}{}^{15.13}$	0.85${}_{0.74}{}^{}{}_{}{}^{0.95}$	11.64${}_{8.83}{}^{}{}_{}{}^{14.68}$	$-$54.0${}_{-94.0}{}^{}{}_{}{}^{-14.0}$	$-$37.0${}_{-72.0}{}^{}{}_{}{}^{1.0}$
50								1.15${}_{0.38}{}^{}{}_{}{}^{2.20}$	14.25${}_{13.64}{}^{}{}_{}{}^{17.16}$	0.85${}_{0.72}{}^{}{}_{}{}^{0.95}$	11.30${}_{9.17}{}^{}{}_{}{}^{15.38}$	$-$59.0${}_{-93.0}{}^{}{}_{}{}^{-20.8}$	$-$41.0${}_{-81.0}{}^{}{}_{}{}^{-5.8}$
35	2M06273068$-$0440140	96.877869	$-$4.67057	66.63$\pm$0.06	7.94$\pm$1.05	$-$0.260$\pm$0.046	$-$0.057$\pm$0.045	13.27${}_{12.38}{}^{}{}_{}{}^{14.19}$	15.86${}_{14.67}{}^{}{}_{}{}^{17.10}$	0.08${}_{0.08}{}^{}{}_{}{}^{0.09}$	1.28${}_{1.05}{}^{}{}_{}{}^{1.56}$	$-$339.0${}_{-362.0}{}^{}{}_{}{}^{-317.0}$	$-$339.0${}_{-361.0}{}^{}{}_{}{}^{-317.0}$
40								13.24${}_{12.40}{}^{}{}_{}{}^{14.18}$	15.89${}_{14.65}{}^{}{}_{}{}^{17.15}$	0.09${}_{0.08}{}^{}{}_{}{}^{0.10}$	1.28${}_{1.05}{}^{}{}_{}{}^{1.56}$	$-$339.0${}_{-362.0}{}^{}{}_{}{}^{-317.0}$	$-$339.0${}_{-362.0}{}^{}{}_{}{}^{-317.0}$
45								13.26${}_{12.34}{}^{}{}_{}{}^{14.16}$	15.89${}_{14.69}{}^{}{}_{}{}^{17.19}$	0.09${}_{0.08}{}^{}{}_{}{}^{0.09}$	1.28${}_{1.05}{}^{}{}_{}{}^{1.56}$	$-$339.0${}_{-362.0}{}^{}{}_{}{}^{-317.0}$	$-$339.0${}_{-362.0}{}^{}{}_{}{}^{-317.0}$
50								13.25${}_{12.35}{}^{}{}_{}{}^{14.18}$	15.90${}_{14.68}{}^{}{}_{}{}^{17.15}$	0.09${}_{0.08}{}^{}{}_{}{}^{0.10}$	1.28${}_{1.05}{}^{}{}_{}{}^{1.56}$	$-$339.0${}_{-362.0}{}^{}{}_{}{}^{-317.0}$	$-$339.0${}_{-362.0}{}^{}{}_{}{}^{-317.0}$
35	2M11062158$-$0712222	166.589953	$-$7.206176	43.25$\pm$0.13	3.86$\pm$0.36	$-$13.358$\pm$0.057	$-$6.870$\pm$0.041	2.88${}_{2.78}{}^{}{}_{}{}^{2.95}$	10.56${}_{10.04}{}^{}{}_{}{}^{11.24}$	0.56${}_{0.54}{}^{}{}_{}{}^{0.60}$	8.78${}_{7.54}{}^{}{}_{}{}^{10.0}$	$-$90.0${}_{-96.0}{}^{}{}_{}{}^{-84.0}$	$-$85.0${}_{-88.0}{}^{}{}_{}{}^{-80.0}$
40								2.90${}_{2.78}{}^{}{}_{}{}^{3.03}$	10.83${}_{10.33}{}^{}{}_{}{}^{11.47}$	0.57${}_{0.54}{}^{}{}_{}{}^{0.59}$	8.83${}_{7.75}{}^{}{}_{}{}^{9.93}$	$-$92.0${}_{-102.0}{}^{}{}_{}{}^{-83.0}$	$-$86.0${}_{-92.0}{}^{}{}_{}{}^{-78.0}$
45								2.87${}_{2.77}{}^{}{}_{}{}^{2.95}$	10.48${}_{10.02}{}^{}{}_{}{}^{11.72}$	0.57${}_{0.54}{}^{}{}_{}{}^{0.61}$	8.73${}_{7.41}{}^{}{}_{}{}^{10.3}$	$-$90.0${}_{-95.0}{}^{}{}_{}{}^{-85.0}$	$-$83.0${}_{-87.0}{}^{}{}_{}{}^{-78.0}$
50								2.88${}_{2.79}{}^{}{}_{}{}^{2.97}$	10.88${}_{10.01}{}^{}{}_{}{}^{11.31}$	0.57${}_{0.54}{}^{}{}_{}{}^{0.60}$	9.09${}_{7.43}{}^{}{}_{}{}^{10.25}$	$-$92.0${}_{-98.0}{}^{}{}_{}{}^{-84.0}$	$-$84.0${}_{-87.0}{}^{}{}_{}{}^{-80.0}$
35	2M11514952$+$2015267	177.956372	20.257444	10.85$\pm$0.05	2.25$\pm$0.20	$-$3.249$\pm$0.083	$-$15.064$\pm$0.061	1.57${}_{1.37}{}^{}{}_{}{}^{1.75}$	9.55${}_{9.23}{}^{}{}_{}{}^{10.96}$	0.71${}_{0.67}{}^{}{}_{}{}^{0.76}$	2.33${}_{2.05}{}^{}{}_{}{}^{2.64}$	$-$94.0${}_{-106.0}{}^{}{}_{}{}^{-78.0}$	$-$60.0${}_{-68.0}{}^{}{}_{}{}^{-53.0}$
40								2.00${}_{1.54}{}^{}{}_{}{}^{2.37}$	9.87${}_{9.77}{}^{}{}_{}{}^{9.96}$	0.66${}_{0.60}{}^{}{}_{}{}^{0.73}$	2.61${}_{2.51}{}^{}{}_{}{}^{3.04}$	$-$88.0${}_{-101.0}{}^{}{}_{}{}^{-75.0}$	$-$73.0${}_{-84.0}{}^{}{}_{}{}^{-57.0}$
45								1.90${}_{1.51}{}^{}{}_{}{}^{2.22}$	9.43${}_{9.33}{}^{}{}_{}{}^{9.68}$	0.66${}_{0.61}{}^{}{}_{}{}^{0.72}$	3.58${}_{3.37}{}^{}{}_{}{}^{3.71}$	$-$84.0${}_{-95.0}{}^{}{}_{}{}^{-71.0}$	$-$65.0${}_{-75.0}{}^{}{}_{}{}^{-54.0}$
50								1.87${}_{1.43}{}^{}{}_{}{}^{2.32}$	10.06${}_{9.73}{}^{}{}_{}{}^{10.29}$	0.68${}_{0.61}{}^{}{}_{}{}^{0.75}$	2.74${}_{2.41}{}^{}{}_{}{}^{3.14}$	$-$93.0${}_{-101.0}{}^{}{}_{}{}^{-81.0}$	$-$69.0${}_{-83.0}{}^{}{}_{}{}^{-54.0}$
35	2M12010401$-$0058306	180.26672	$-$0.975172	145.41$\pm$1.52	1.69$\pm$0.10	3.765$\pm$0.077	$-$20.473$\pm$0.039	0.46${}_{0.08}{}^{}{}_{}{}^{1.09}$	9.70${}_{9.58}{}^{}{}_{}{}^{9.78}$	0.90${}_{0.79}{}^{}{}_{}{}^{0.98}$	5.56${}_{5.39}{}^{}{}_{}{}^{5.75}$	$-$49.0${}_{-57.0}{}^{}{}_{}{}^{-42.0}$	$-$13.0${}_{-36.2}{}^{}{}_{}{}^{20.0}$
40								1.07${}_{0.85}{}^{}{}_{}{}^{1.36}$	9.84${}_{9.71}{}^{}{}_{}{}^{10.23}$	0.80${}_{0.75}{}^{}{}_{}{}^{0.84}$	5.68${}_{5.59}{}^{}{}_{}{}^{5.85}$	$-$52.0${}_{-61.0}{}^{}{}_{}{}^{-47.0}$	$-$39.0${}_{-47.0}{}^{}{}_{}{}^{-32.0}$
45								1.05${}_{0.79}{}^{}{}_{}{}^{1.29}$	10.94${}_{10.82}{}^{}{}_{}{}^{11.20}$	0.82${}_{0.78}{}^{}{}_{}{}^{0.86}$	5.53${}_{5.31}{}^{}{}_{}{}^{6.19}$	$-$67.0${}_{-74.0}{}^{}{}_{}{}^{-58.0}$	$-$37.0${}_{-45.0}{}^{}{}_{}{}^{-29.0}$
50								0.79${}_{0.53}{}^{}{}_{}{}^{0.97}$	9.97${}_{9.68}{}^{}{}_{}{}^{10.27}$	0.85${}_{0.82}{}^{}{}_{}{}^{0.89}$	5.90${}_{5.35}{}^{}{}_{}{}^{6.45}$	$-$52.0${}_{-63.0}{}^{}{}_{}{}^{-46.0}$	$-$25.0${}_{-34.0}{}^{}{}_{}{}^{-18.0}$
35	2M12042878$+$1949535	181.119949	19.831541	83.82$\pm$0.14	2.93$\pm$0.31	$-$6.604$\pm$0.072	$-$13.721$\pm$0.053	0.20${}_{0.05}{}^{}{}_{}{}^{1.01}$	9.18${}_{8.77}{}^{}{}_{}{}^{9.55}$	0.95${}_{0.80}{}^{}{}_{}{}^{0.98}$	4.83${}_{4.22}{}^{}{}_{}{}^{5.64}$	$-$32.0${}_{-56.0}{}^{}{}_{}{}^{-7.8}$	8.5${}_{-36.0}{}^{}{}_{}{}^{33.0}$
40								0.30${}_{0.05}{}^{}{}_{}{}^{0.99}$	9.05${}_{8.84}{}^{}{}_{}{}^{9.35}$	0.93${}_{0.79}{}^{}{}_{}{}^{0.98}$	5.02${}_{4.28}{}^{}{}_{}{}^{5.39}$	$-$28.0${}_{-49.0}{}^{}{}_{}{}^{-9.0}$	$-$8.0${}_{-37.0}{}^{}{}_{}{}^{8.0}$
45								0.35${}_{0.11}{}^{}{}_{}{}^{0.99}$	9.71${}_{9.47}{}^{}{}_{}{}^{9.91}$	0.93${}_{0.81}{}^{}{}_{}{}^{0.97}$	4.18${}_{3.79}{}^{}{}_{}{}^{4.83}$	$-$32.0${}_{-57.0}{}^{}{}_{}{}^{-12.0}$	$-$12.0${}_{-37.0}{}^{}{}_{}{}^{2.0}$
50								0.41${}_{0.05}{}^{}{}_{}{}^{1.07}$	9.33${}_{8.96}{}^{}{}_{}{}^{10.01}$	0.91${}_{0.80}{}^{}{}_{}{}^{0.98}$	5.96${}_{4.66}{}^{}{}_{}{}^{6.26}$	$-$34.0${}_{-60.0}{}^{}{}_{}{}^{-7.0}$	$-$13.0${}_{-38.0}{}^{}{}_{}{}^{7.0}$
35	2M12092246$+$0545111	182.34361	5.7531	1.44$\pm$0.43	10.80$\pm$1.93	$-$1.320$\pm$0.060	$-$1.700$\pm$0.031	3.58${}_{2.97}{}^{}{}_{}{}^{4.22}$	14.47${}_{12.66}{}^{}{}_{}{}^{16.38}$	0.60${}_{0.50}{}^{}{}_{}{}^{0.69}$	10.94${}_{8.82}{}^{}{}_{}{}^{12.99}$	$-$126.0${}_{-137.0}{}^{}{}_{}{}^{-114.8}$	$-$119.0${}_{-133.0}{}^{}{}_{}{}^{-106.0}$
40								3.41${}_{2.86}{}^{}{}_{}{}^{4.27}$	13.86${}_{13.49}{}^{}{}_{}{}^{15.59}$	0.60${}_{0.52}{}^{}{}_{}{}^{0.68}$	10.61${}_{9.41}{}^{}{}_{}{}^{12.50}$	$-$120.0${}_{-144.1}{}^{}{}_{}{}^{-107.0}$	$-$110.0${}_{-134.0}{}^{}{}_{}{}^{-99.0}$
45								3.51${}_{2.93}{}^{}{}_{}{}^{4.12}$	14.03${}_{12.39}{}^{}{}_{}{}^{15.50}$	0.60${}_{0.49}{}^{}{}_{}{}^{0.67}$	10.75${}_{8.68}{}^{}{}_{}{}^{12.49}$	$-$120.0${}_{-134.0}{}^{}{}_{}{}^{-108.8}$	$-$116.0${}_{-126.0}{}^{}{}_{}{}^{-102.0}$
50								3.51${}_{2.92}{}^{}{}_{}{}^{4.16}$	14.19${}_{12.36}{}^{}{}_{}{}^{15.79}$	0.60${}_{0.49}{}^{}{}_{}{}^{0.69}$	10.69${}_{8.81}{}^{}{}_{}{}^{12.56}$	$-$120.0${}_{-135.0}{}^{}{}_{}{}^{-110.0}$	$-$116.0${}_{-132.0}{}^{}{}_{}{}^{-102.0}$
35	2M12444724$-$0207405	191.196857	$-$2.127943	105.54$\pm$0.15	5.06$\pm$0.56	$-$1.419$\pm$0.051	$-$8.712$\pm$0.030	0.08${}_{0.03}{}^{}{}_{}{}^{0.47}$	9.26${}_{8.86}{}^{}{}_{}{}^{9.98}$	0.98${}_{0.90}{}^{}{}_{}{}^{0.99}$	7.49${}_{6.69}{}^{}{}_{}{}^{8.57}$	$-$4.0${}_{-23.0}{}^{}{}_{}{}^{9.0}$	13.0${}_{8.0}{}^{}{}_{}{}^{30.0}$
40								0.22${}_{0.06}{}^{}{}_{}{}^{0.57}$	9.26${}_{8.98}{}^{}{}_{}{}^{9.80}$	0.95${}_{0.88}{}^{}{}_{}{}^{0.98}$	7.28${}_{6.75}{}^{}{}_{}{}^{7.58}$	$-$3.5${}_{-26.0}{}^{}{}_{}{}^{13.0}$	15.0${}_{-9.0}{}^{}{}_{}{}^{30.0}$
45								0.18${}_{0.04}{}^{}{}_{}{}^{0.60}$	9.23${}_{8.88}{}^{}{}_{}{}^{9.67}$	0.96${}_{0.87}{}^{}{}_{}{}^{0.99}$	7.77${}_{6.54}{}^{}{}_{}{}^{9.02}$	$-$7.0${}_{-23.2}{}^{}{}_{}{}^{11.0}$	5.0${}_{-6.0}{}^{}{}_{}{}^{22.0}$
50								0.27${}_{0.05}{}^{}{}_{}{}^{0.53}$	9.60${}_{8.99}{}^{}{}_{}{}^{10.35}$	0.94${}_{0.89}{}^{}{}_{}{}^{0.98}$	7.58${}_{6.89}{}^{}{}_{}{}^{8.52}$	$-$8.0${}_{-34.0}{}^{}{}_{}{}^{13.0}$	7.0${}_{-10.0}{}^{}{}_{}{}^{28.0}$
35	2M13481355$-$0040484	207.056489	$-$0.680118	210.41$\pm$0.20	4.81$\pm$0.70	$-$6.905$\pm$0.056	$-$2.524$\pm$0.045	0.65${}_{0.35}{}^{}{}_{}{}^{1.07}$	8.56${}_{8.23}{}^{}{}_{}{}^{9.19}$	0.85${}_{0.76}{}^{}{}_{}{}^{0.92}$	8.69${}_{8.03}{}^{}{}_{}{}^{9.33}$	$-$41.0${}_{-55.0}{}^{}{}_{}{}^{-27.0}$	$-$12.0${}_{-25.0}{}^{}{}_{}{}^{-4.0}$
40								1.20${}_{0.72}{}^{}{}_{}{}^{1.81}$	8.59${}_{8.01}{}^{}{}_{}{}^{9.35}$	0.75${}_{0.62}{}^{}{}_{}{}^{0.85}$	8.36${}_{7.83}{}^{}{}_{}{}^{9.47}$	$-$36.0${}_{-50.0}{}^{}{}_{}{}^{-27.0}$	$-$30.0${}_{-44.2}{}^{}{}_{}{}^{-17.0}$
45								1.18${}_{0.74}{}^{}{}_{}{}^{1.80}$	8.48${}_{7.99}{}^{}{}_{}{}^{9.17}$	0.75${}_{0.63}{}^{}{}_{}{}^{0.85}$	8.58${}_{7.84}{}^{}{}_{}{}^{9.30}$	$-$36.0${}_{-49.0}{}^{}{}_{}{}^{-27.0}$	$-$31.0${}_{-45.0}{}^{}{}_{}{}^{-19.0}$
50								1.15${}_{0.66}{}^{}{}_{}{}^{1.79}$	8.73${}_{7.87}{}^{}{}_{}{}^{9.33}$	0.76${}_{0.62}{}^{}{}_{}{}^{0.86}$	8.43${}_{7.56}{}^{}{}_{}{}^{9.22}$	$-$36.0${}_{-48.0}{}^{}{}_{}{}^{-25.0}$	$-$29.0${}_{-43.0}{}^{}{}_{}{}^{-15.0}$
35	2M13503160$+$4411389	207.6317	44.194141	20.54$\pm$0.16	2.00$\pm$0.05	2.079$\pm$0.017	$-$13.203$\pm$0.019	5.35${}_{5.28}{}^{}{}_{}{}^{5.41}$	10.09${}_{10.05}{}^{}{}_{}{}^{10.17}$	0.30${}_{0.30}{}^{}{}_{}{}^{0.31}$	3.58${}_{3.41}{}^{}{}_{}{}^{3.66}$	$-$166.0${}_{-167.0}{}^{}{}_{}{}^{-164.0}$	$-$159.0${}_{-160.0}{}^{}{}_{}{}^{-157.0}$
40								5.32${}_{5.19}{}^{}{}_{}{}^{5.37}$	10.29${}_{10.27}{}^{}{}_{}{}^{10.32}$	0.31${}_{0.31}{}^{}{}_{}{}^{0.33}$	3.62${}_{3.44}{}^{}{}_{}{}^{3.77}$	$-$166.0${}_{-168.0}{}^{}{}_{}{}^{-165.0}$	$-$156.0${}_{-157.0}{}^{}{}_{}{}^{-154.0}$
45								5.31${}_{5.24}{}^{}{}_{}{}^{5.35}$	10.30${}_{10.26}{}^{}{}_{}{}^{10.36}$	0.31${}_{0.31}{}^{}{}_{}{}^{0.32}$	3.63${}_{3.45}{}^{}{}_{}{}^{3.71}$	$-$165.0${}_{-166.0}{}^{}{}_{}{}^{-163.0}$	$-$159.0${}_{-160.0}{}^{}{}_{}{}^{-157.0}$
50								5.34${}_{5.28}{}^{}{}_{}{}^{5.42}$	10.95${}_{10.93}{}^{}{}_{}{}^{10.97}$	0.34${}_{0.33}{}^{}{}_{}{}^{0.34}$	3.84${}_{3.71}{}^{}{}_{}{}^{3.96}$	$-$169.0${}_{-171.0}{}^{}{}_{}{}^{-168.0}$	$-$155.0${}_{-157.0}{}^{}{}_{}{}^{-153.0}$
35	2M14082554$+$4711096	212.106431	47.186001	$-$62.76$\pm$0.00	0.49$\pm$0.01	$-$151.479$\pm$0.033	$-$10.543$\pm$0.034	0.26${}_{0.20}{}^{}{}_{}{}^{0.30}$	14.22${}_{13.93}{}^{}{}_{}{}^{14.34}$	0.96${}_{0.95}{}^{}{}_{}{}^{0.97}$	3.59${}_{2.45}{}^{}{}_{}{}^{4.04}$	6.0${}_{3.0}{}^{}{}_{}{}^{8.0}$	21.0${}_{18.0}{}^{}{}_{}{}^{24.0}$
40								0.08${}_{0.04}{}^{}{}_{}{}^{0.13}$	16.45${}_{15.80}{}^{}{}_{}{}^{16.75}$	0.98${}_{0.98}{}^{}{}_{}{}^{0.99}$	3.59${}_{2.34}{}^{}{}_{}{}^{4.06}$	$-$11.0${}_{-19.2}{}^{}{}_{}{}^{-4.0}$	25.0${}_{21.0}{}^{}{}_{}{}^{30.0}$
45								0.24${}_{0.15}{}^{}{}_{}{}^{0.33}$	13.97${}_{13.75}{}^{}{}_{}{}^{14.32}$	0.96${}_{0.95}{}^{}{}_{}{}^{0.97}$	3.83${}_{3.37}{}^{}{}_{}{}^{4.21}$	9.0${}_{5.0}{}^{}{}_{}{}^{12.0}$	43.0${}_{34.0}{}^{}{}_{}{}^{50.0}$
50								0.28${}_{0.21}{}^{}{}_{}{}^{0.31}$	14.06${}_{13.88}{}^{}{}_{}{}^{14.29}$	0.96${}_{0.95}{}^{}{}_{}{}^{0.97}$	3.60${}_{3.29}{}^{}{}_{}{}^{3.97}$	11.0${}_{6.0}{}^{}{}_{}{}^{13.0}$	25.0${}_{24.0}{}^{}{}_{}{}^{27.0}$
35	2M14582162$+$4117544	224.590099	41.298454	$-$73.89$\pm$0.00	3.57$\pm$0.33	$-$13.150$\pm$0.057	$-$6.297$\pm$0.064	0.13${}_{0.05}{}^{}{}_{}{}^{0.39}$	9.05${}_{8.69}{}^{}{}_{}{}^{9.45}$	0.97${}_{0.92}{}^{}{}_{}{}^{0.98}$	5.17${}_{3.78}{}^{}{}_{}{}^{6.58}$	0.0${}_{-28.0}{}^{}{}_{}{}^{9.0}$	26.0${}_{18.8}{}^{}{}_{}{}^{40.0}$
40								0.08${}_{0.03}{}^{}{}_{}{}^{0.32}$	9.03${}_{8.74}{}^{}{}_{}{}^{9.32}$	0.98${}_{0.93}{}^{}{}_{}{}^{0.99}$	4.87${}_{3.66}{}^{}{}_{}{}^{6.11}$	$-$6.0${}_{-20.0}{}^{}{}_{}{}^{9.0}$	15.0${}_{9.0}{}^{}{}_{}{}^{27.0}$
45								0.09${}_{0.02}{}^{}{}_{}{}^{0.49}$	9.04${}_{8.64}{}^{}{}_{}{}^{9.38}$	0.97${}_{0.89}{}^{}{}_{}{}^{0.99}$	4.61${}_{3.79}{}^{}{}_{}{}^{5.13}$	$-$7.0${}_{-18.0}{}^{}{}_{}{}^{16.2}$	8.0${}_{-2.0}{}^{}{}_{}{}^{28.0}$
50								0.17${}_{0.04}{}^{}{}_{}{}^{0.43}$	8.72${}_{8.45}{}^{}{}_{}{}^{9.20}$	0.96${}_{0.90}{}^{}{}_{}{}^{0.98}$	4.97${}_{4.39}{}^{}{}_{}{}^{5.75}$	1.0${}_{-19.0}{}^{}{}_{}{}^{13.0}$	17.0${}_{-2.0}{}^{}{}_{}{}^{27.0}$
35	2M15082716$+$6710075	227.113188	67.168762	$-$233.12$\pm$0.79	54.34$\pm$4.20	$-$0.203$\pm$0.089	0.112$\pm$0.085	4.77${}_{2.14}{}^{}{}_{}{}^{7.54}$	58.43${}_{35.40}{}^{}{}_{}{}^{82.86}$	0.82${}_{0.70}{}^{}{}_{}{}^{0.93}$	58.14${}_{34.06}{}^{}{}_{}{}^{81.48}$	$-$126.5${}_{-195.0}{}^{}{}_{}{}^{27.2}$	$-$126.0${}_{-195.0}{}^{}{}_{}{}^{27.2}$
40								4.76${}_{2.18}{}^{}{}_{}{}^{7.46}$	58.43${}_{35.40}{}^{}{}_{}{}^{82.86}$	0.82${}_{0.70}{}^{}{}_{}{}^{0.93}$	58.12${}_{34.10}{}^{}{}_{}{}^{81.30}$	$-$126.0${}_{-195.0}{}^{}{}_{}{}^{27.2}$	$-$126.0${}_{-195.0}{}^{}{}_{}{}^{27.2}$
45								4.76${}_{2.14}{}^{}{}_{}{}^{7.43}$	58.43${}_{35.40}{}^{}{}_{}{}^{82.86}$	0.82${}_{0.70}{}^{}{}_{}{}^{0.93}$	58.13${}_{34.10}{}^{}{}_{}{}^{81.30}$	$-$126.5${}_{-195.0}{}^{}{}_{}{}^{27.2}$	$-$126.0${}_{-195.0}{}^{}{}_{}{}^{27.2}$
50								4.71${}_{2.15}{}^{}{}_{}{}^{7.43}$	58.43${}_{35.39}{}^{}{}_{}{}^{82.86}$	0.82${}_{0.70}{}^{}{}_{}{}^{0.93}$	58.13${}_{34.10}{}^{}{}_{}{}^{81.32}$	$-$126.5${}_{-195.0}{}^{}{}_{}{}^{27.2}$	$-$126.0${}_{-195.0}{}^{}{}_{}{}^{27.2}$
35	2M15183589$+$0027100	229.649545	0.452789	$-$56.27$\pm$0.34	18.16$\pm$2.53	$-$2.689$\pm$0.071	$-$2.806$\pm$0.063	1.05${}_{0.23}{}^{}{}_{}{}^{2.21}$	13.59${}_{11.51}{}^{}{}_{}{}^{16.27}$	0.85${}_{0.75}{}^{}{}_{}{}^{0.95}$	13.58${}_{11.38}{}^{}{}_{}{}^{15.07}$	$-$46.0${}_{-77.0}{}^{}{}_{}{}^{-17.0}$	$-$33.0${}_{-69.0}{}^{}{}_{}{}^{-3.0}$
40								0.98${}_{0.20}{}^{}{}_{}{}^{2.29}$	14.09${}_{11.75}{}^{}{}_{}{}^{15.79}$	0.87${}_{0.74}{}^{}{}_{}{}^{0.96}$	13.37${}_{11.46}{}^{}{}_{}{}^{14.86}$	$-$43.5${}_{-76.2}{}^{}{}_{}{}^{-20.0}$	$-$32.0${}_{-75.0}{}^{}{}_{}{}^{-3.0}$
45								0.78${}_{0.17}{}^{}{}_{}{}^{2.26}$	13.26${}_{12.16}{}^{}{}_{}{}^{15.91}$	0.88${}_{0.74}{}^{}{}_{}{}^{0.97}$	13.11${}_{11.59}{}^{}{}_{}{}^{14.82}$	$-$35.5${}_{-76.2}{}^{}{}_{}{}^{-19.0}$	$-$24.0${}_{-74.2}{}^{}{}_{}{}^{-1.0}$
50								0.92${}_{0.16}{}^{}{}_{}{}^{2.30}$	13.27${}_{11.65}{}^{}{}_{}{}^{16.37}$	0.86${}_{0.74}{}^{}{}_{}{}^{0.97}$	13.33${}_{11.85}{}^{}{}_{}{}^{15.16}$	$-$37.0${}_{-78.2}{}^{}{}_{}{}^{-17.0}$	$-$28.0${}_{-76.0}{}^{}{}_{}{}^{-1.0}$

Table 9. Table 9: (continued)

${\Omega }_{bar}$	APOGEE$-$ID	RA	DEC	$RV\pm \Delta$	$d\pm \Delta$	${\mu }_{\alpha }\pm \Delta$	${\mu }_{\delta }\pm \Delta$	$⟨r_{min}⟩$	$⟨r_{max}⟩$	$⟨e⟩$	$⟨Z_{max}⟩$	$⟨L_{z,min}⟩$	$⟨L_{z,max}⟩$
km s-1 kpc-1		(∘)	(∘)	km s-1	kpc	mas yr-1	mas yr-1	kpc	kpc		kpc	km s-1 kpc-1	km s-1 kpc-1
35	2M15193208$+$0025293	229.883704	0.424806	16.79$\pm$0.08	9.21$\pm$0.97	$-$1.542$\pm$0.126	$-$0.608$\pm$0.163	1.15${}_{0.54}{}^{}{}_{}{}^{1.73}$	7.13${}_{6.61}{}^{}{}_{}{}^{8.11}$	0.72${}_{0.58}{}^{}{}_{}{}^{0.87}$	6.97${}_{6.16}{}^{}{}_{}{}^{8.10}$	$-$42.0${}_{-54.0}{}^{}{}_{}{}^{-31.0}$	$-$26.0${}_{-40.0}{}^{}{}_{}{}^{-10.0}$
40								1.09${}_{0.68}{}^{}{}_{}{}^{1.52}$	7.15${}_{6.84}{}^{}{}_{}{}^{7.68}$	0.73${}_{0.64}{}^{}{}_{}{}^{0.83}$	7.18${}_{6.45}{}^{}{}_{}{}^{7.84}$	$-$41.0${}_{-59.0}{}^{}{}_{}{}^{-24.8}$	$-$23.5${}_{-34.0}{}^{}{}_{}{}^{-14.0}$
45								1.40${}_{0.84}{}^{}{}_{}{}^{1.98}$	7.11${}_{6.64}{}^{}{}_{}{}^{7.62}$	0.66${}_{0.54}{}^{}{}_{}{}^{0.80}$	7.09${}_{6.34}{}^{}{}_{}{}^{7.75}$	$-$38.0${}_{-53.0}{}^{}{}_{}{}^{-23.0}$	$-$32.0${}_{-46.0}{}^{}{}_{}{}^{-19.0}$
50								1.36${}_{0.83}{}^{}{}_{}{}^{2.00}$	6.98${}_{6.56}{}^{}{}_{}{}^{7.56}$	0.67${}_{0.53}{}^{}{}_{}{}^{0.80}$	7.04${}_{6.25}{}^{}{}_{}{}^{7.89}$	$-$37.0${}_{-51.0}{}^{}{}_{}{}^{-23.8}$	$-$32.0${}_{-46.0}{}^{}{}_{}{}^{-19.0}$
35	2M15195065$+$0221533	229.961053	2.364827	$-$158.58$\pm$0.01	4.71$\pm$0.39	$-$2.500$\pm$0.072	$-$1.367$\pm$0.065	3.31${}_{3.06}{}^{}{}_{}{}^{3.41}$	8.02${}_{7.83}{}^{}{}_{}{}^{8.15}$	0.41${}_{0.40}{}^{}{}_{}{}^{0.43}$	5.63${}_{5.46}{}^{}{}_{}{}^{5.73}$	$-$113.0${}_{-117.0}{}^{}{}_{}{}^{-109.0}$	$-$79.0${}_{-85.0}{}^{}{}_{}{}^{-74.0}$
40								2.35${}_{2.19}{}^{}{}_{}{}^{3.50}$	7.26${}_{7.05}{}^{}{}_{}{}^{7.46}$	0.50${}_{0.36}{}^{}{}_{}{}^{0.52}$	5.40${}_{5.22}{}^{}{}_{}{}^{5.55}$	$-$95.0${}_{-103.0}{}^{}{}_{}{}^{-88.0}$	$-$53.0${}_{-88.0}{}^{}{}_{}{}^{-50.0}$
45								3.44${}_{3.18}{}^{}{}_{}{}^{3.67}$	7.12${}_{6.88}{}^{}{}_{}{}^{7.41}$	0.34${}_{0.33}{}^{}{}_{}{}^{0.36}$	5.36${}_{5.20}{}^{}{}_{}{}^{5.56}$	$-$93.0${}_{-100.0}{}^{}{}_{}{}^{-86.0}$	$-$85.0${}_{-93.0}{}^{}{}_{}{}^{-77.0}$
50								3.35${}_{3.23}{}^{}{}_{}{}^{3.55}$	8.00${}_{7.33}{}^{}{}_{}{}^{8.17}$	0.40${}_{0.35}{}^{}{}_{}{}^{0.42}$	5.48${}_{5.18}{}^{}{}_{}{}^{5.77}$	$-$98.0${}_{-101.0}{}^{}{}_{}{}^{-90.0}$	$-$88.0${}_{-92.0}{}^{}{}_{}{}^{-80.0}$
35	2M15535831$+$4333280	238.492995	43.557785	$-$182.35$\pm$0.34	5.69$\pm$0.76	$-$6.000$\pm$0.041	$-$0.476$\pm$0.051	0.12${}_{0.04}{}^{}{}_{}{}^{0.60}$	9.35${}_{8.78}{}^{}{}_{}{}^{9.87}$	0.97${}_{0.88}{}^{}{}_{}{}^{0.99}$	8.39${}_{7.68}{}^{}{}_{}{}^{8.87}$	0.0${}_{-13.0}{}^{}{}_{}{}^{16.0}$	21.0${}_{9.0}{}^{}{}_{}{}^{41.0}$
40								0.19${}_{0.05}{}^{}{}_{}{}^{0.55}$	9.39${}_{8.73}{}^{}{}_{}{}^{9.90}$	0.95${}_{0.89}{}^{}{}_{}{}^{0.98}$	8.93${}_{7.96}{}^{}{}_{}{}^{9.60}$	0.0${}_{-15.0}{}^{}{}_{}{}^{14.0}$	15.0${}_{1.0}{}^{}{}_{}{}^{31.0}$
45								0.27${}_{0.05}{}^{}{}_{}{}^{0.76}$	9.25${}_{8.96}{}^{}{}_{}{}^{9.51}$	0.94${}_{0.84}{}^{}{}_{}{}^{0.98}$	8.56${}_{7.68}{}^{}{}_{}{}^{9.33}$	0.0${}_{-14.0}{}^{}{}_{}{}^{22.0}$	14.0${}_{-3.0}{}^{}{}_{}{}^{32.0}$
50								0.23${}_{0.04}{}^{}{}_{}{}^{0.56}$	9.68${}_{9.07}{}^{}{}_{}{}^{10.71}$	0.95${}_{0.89}{}^{}{}_{}{}^{0.99}$	8.46${}_{7.57}{}^{}{}_{}{}^{9.07}$	0.0${}_{-23.0}{}^{}{}_{}{}^{16.0}$	13.0${}_{-1.0}{}^{}{}_{}{}^{34.0}$
35	2M16362792$+$3901180	249.11635	39.021675	$-$191.99$\pm$0.03	4.44$\pm$0.27	$-$8.336$\pm$0.023	1.191$\pm$0.026	0.33${}_{0.13}{}^{}{}_{}{}^{0.49}$	9.16${}_{9.07}{}^{}{}_{}{}^{9.26}$	0.92${}_{0.89}{}^{}{}_{}{}^{0.97}$	5.04${}_{4.90}{}^{}{}_{}{}^{5.32}$	11.0${}_{3.0}{}^{}{}_{}{}^{17.0}$	30.0${}_{26.0}{}^{}{}_{}{}^{35.0}$
40								0.42${}_{0.22}{}^{}{}_{}{}^{0.56}$	9.01${}_{8.89}{}^{}{}_{}{}^{9.13}$	0.90${}_{0.88}{}^{}{}_{}{}^{0.95}$	4.72${}_{4.42}{}^{}{}_{}{}^{4.98}$	14.0${}_{7.0}{}^{}{}_{}{}^{20.2}$	28.0${}_{24.0}{}^{}{}_{}{}^{34.0}$
45								0.28${}_{0.13}{}^{}{}_{}{}^{0.45}$	9.50${}_{9.06}{}^{}{}_{}{}^{9.79}$	0.94${}_{0.90}{}^{}{}_{}{}^{0.97}$	5.03${}_{4.48}{}^{}{}_{}{}^{5.69}$	9.0${}_{1.0}{}^{}{}_{}{}^{14.0}$	25.0${}_{18.0}{}^{}{}_{}{}^{32.0}$
50								0.24${}_{0.12}{}^{}{}_{}{}^{0.42}$	9.64${}_{9.38}{}^{}{}_{}{}^{9.89}$	0.95${}_{0.91}{}^{}{}_{}{}^{0.97}$	4.84${}_{4.68}{}^{}{}_{}{}^{5.06}$	6.0${}_{0.8}{}^{}{}_{}{}^{15.0}$	21.0${}_{15.0}{}^{}{}_{}{}^{30.0}$
35	2M16464310$+$4731033	251.679603	47.517605	$-$139.80$\pm$0.37	20.02$\pm$3.61	$-$1.218$\pm$0.055	$-$0.654$\pm$0.101	1.01${}_{0.71}{}^{}{}_{}{}^{1.38}$	19.82${}_{16.89}{}^{}{}_{}{}^{24.38}$	0.90${}_{0.86}{}^{}{}_{}{}^{0.93}$	15.78${}_{14.47}{}^{}{}_{}{}^{17.71}$	$-$53.0${}_{-68.0}{}^{}{}_{}{}^{-38.0}$	$-$39.0${}_{-54.0}{}^{}{}_{}{}^{-27.0}$
40								1.04${}_{0.72}{}^{}{}_{}{}^{1.39}$	21.09${}_{16.73}{}^{}{}_{}{}^{24.31}$	0.90${}_{0.86}{}^{}{}_{}{}^{0.93}$	16.08${}_{14.35}{}^{}{}_{}{}^{17.66}$	$-$53.0${}_{-69.0}{}^{}{}_{}{}^{-39.0}$	$-$40.0${}_{-56.2}{}^{}{}_{}{}^{-26.0}$
45								1.05${}_{0.70}{}^{}{}_{}{}^{1.40}$	20.58${}_{17.74}{}^{}{}_{}{}^{23.90}$	0.90${}_{0.86}{}^{}{}_{}{}^{0.93}$	15.93${}_{14.62}{}^{}{}_{}{}^{17.82}$	$-$53.0${}_{-68.0}{}^{}{}_{}{}^{-38.0}$	$-$40.0${}_{-56.0}{}^{}{}_{}{}^{-25.0}$
50								1.05${}_{0.68}{}^{}{}_{}{}^{1.39}$	21.14${}_{16.68}{}^{}{}_{}{}^{23.30}$	0.90${}_{0.86}{}^{}{}_{}{}^{0.93}$	16.25${}_{14.40}{}^{}{}_{}{}^{17.95}$	$-$53.0${}_{-67.0}{}^{}{}_{}{}^{-38.8}$	$-$40.0${}_{-55.0}{}^{}{}_{}{}^{-25.0}$
35	2M17294680$-$2644220	262.445037	$-$26.739462	$-$217.76$\pm$0.25	3.65$\pm$0.49	$-$3.679$\pm$0.174	$-$6.375$\pm$0.114	1.10${}_{0.83}{}^{}{}_{}{}^{1.58}$	7.31${}_{6.33}{}^{}{}_{}{}^{8.20}$	0.73${}_{0.67}{}^{}{}_{}{}^{0.77}$	0.96${}_{0.50}{}^{}{}_{}{}^{2.20}$	$-$71.0${}_{-84.0}{}^{}{}_{}{}^{-57.0}$	$-$42.0${}_{-61.0}{}^{}{}_{}{}^{-31.0}$
40								1.16${}_{0.75}{}^{}{}_{}{}^{1.56}$	7.29${}_{6.33}{}^{}{}_{}{}^{9.55}$	0.73${}_{0.70}{}^{}{}_{}{}^{0.78}$	0.58${}_{0.48}{}^{}{}_{}{}^{2.13}$	$-$70.0${}_{-101.0}{}^{}{}_{}{}^{-55.0}$	$-$44.0${}_{-60.0}{}^{}{}_{}{}^{-27.0}$
45								1.11${}_{0.82}{}^{}{}_{}{}^{1.24}$	8.40${}_{6.36}{}^{}{}_{}{}^{8.71}$	0.76${}_{0.74}{}^{}{}_{}{}^{0.78}$	0.54${}_{0.46}{}^{}{}_{}{}^{1.77}$	$-$79.0${}_{-88.0}{}^{}{}_{}{}^{-54.0}$	$-$43.0${}_{-48.0}{}^{}{}_{}{}^{-31.0}$
50								0.88${}_{0.74}{}^{}{}_{}{}^{1.40}$	7.72${}_{7.59}{}^{}{}_{}{}^{8.16}$	0.79${}_{0.70}{}^{}{}_{}{}^{0.81}$	0.50${}_{0.45}{}^{}{}_{}{}^{0.60}$	$-$69.0${}_{-77.2}{}^{}{}_{}{}^{-66.0}$	$-$34.0${}_{-53.0}{}^{}{}_{}{}^{-28.0}$
35	2M18022601$-$3106232	270.608394	$-$31.106453	$-$170.48$\pm$0.26	7.23$\pm$1.15	2.127$\pm$0.126	$-$5.193$\pm$0.104	0.36${}_{0.04}{}^{}{}_{}{}^{0.86}$	2.82${}_{2.16}{}^{}{}_{}{}^{3.97}$	0.75${}_{0.63}{}^{}{}_{}{}^{0.96}$	1.25${}_{1.06}{}^{}{}_{}{}^{1.65}$	$-$43.0${}_{-57.0}{}^{}{}_{}{}^{-21.0}$	$-$8.0${}_{-25.0}{}^{}{}_{}{}^{6.0}$
40								0.38${}_{0.04}{}^{}{}_{}{}^{0.78}$	2.77${}_{2.35}{}^{}{}_{}{}^{4.13}$	0.76${}_{0.66}{}^{}{}_{}{}^{0.96}$	1.28${}_{1.11}{}^{}{}_{}{}^{1.65}$	$-$39.0${}_{-59.0}{}^{}{}_{}{}^{-20.0}$	$-$9.0${}_{-22.0}{}^{}{}_{}{}^{6.0}$
45								0.41${}_{0.04}{}^{}{}_{}{}^{0.69}$	2.75${}_{2.40}{}^{}{}_{}{}^{4.06}$	0.76${}_{0.67}{}^{}{}_{}{}^{0.96}$	1.29${}_{1.17}{}^{}{}_{}{}^{1.65}$	$-$36.0${}_{-65.0}{}^{}{}_{}{}^{-20.0}$	$-$9.5${}_{-19.0}{}^{}{}_{}{}^{7.0}$
50								0.38${}_{0.04}{}^{}{}_{}{}^{0.66}$	2.88${}_{2.34}{}^{}{}_{}{}^{3.92}$	0.76${}_{0.69}{}^{}{}_{}{}^{0.96}$	1.33${}_{1.19}{}^{}{}_{}{}^{1.67}$	$-$35.0${}_{-64.0}{}^{}{}_{}{}^{-20.0}$	$-$8.0${}_{-18.0}{}^{}{}_{}{}^{8.0}$
35	2M18110406$-$2602142	272.766955	$-$26.037289	$-$24.96$\pm$0.01	5.70$\pm$0.54	$-$1.181$\pm$0.100	$-$5.176$\pm$0.079	0.48${}_{0.42}{}^{}{}_{}{}^{0.65}$	2.77${}_{2.21}{}^{}{}_{}{}^{3.26}$	0.68${}_{0.65}{}^{}{}_{}{}^{0.71}$	0.42${}_{0.39}{}^{}{}_{}{}^{0.45}$	$-$47.0${}_{-57.0}{}^{}{}_{}{}^{-28.0}$	$-$13.0${}_{-19.0}{}^{}{}_{}{}^{-10.0}$
40								0.48${}_{0.41}{}^{}{}_{}{}^{0.65}$	2.71${}_{2.23}{}^{}{}_{}{}^{3.27}$	0.68${}_{0.65}{}^{}{}_{}{}^{0.70}$	0.43${}_{0.40}{}^{}{}_{}{}^{0.49}$	$-$48.0${}_{-55.0}{}^{}{}_{}{}^{-33.0}$	$-$13.0${}_{-18.0}{}^{}{}_{}{}^{-10.0}$
45								0.44${}_{0.29}{}^{}{}_{}{}^{0.60}$	2.73${}_{2.24}{}^{}{}_{}{}^{3.36}$	0.68${}_{0.66}{}^{}{}_{}{}^{0.81}$	0.46${}_{0.41}{}^{}{}_{}{}^{0.61}$	$-$46.0${}_{-56.0}{}^{}{}_{}{}^{-36.0}$	$-$11.0${}_{-17.0}{}^{}{}_{}{}^{-6.9}$
50								0.44${}_{0.26}{}^{}{}_{}{}^{0.52}$	2.74${}_{2.25}{}^{}{}_{}{}^{3.37}$	0.73${}_{0.70}{}^{}{}_{}{}^{0.78}$	0.46${}_{0.42}{}^{}{}_{}{}^{0.65}$	$-$47.0${}_{-53.1}{}^{}{}_{}{}^{-37.0}$	$-$11.0${}_{-14.1}{}^{}{}_{}{}^{-6.0}$
35	2M18200243$+$0156016	275.010145	1.933787	73.81$\pm$0.16	11.20$\pm$1.45	$-$2.277$\pm$0.084	$-$9.631$\pm$0.075	5.45${}_{4.40}{}^{}{}_{}{}^{6.74}$	21.52${}_{12.08}{}^{}{}_{}{}^{45.92}$	0.59${}_{0.48}{}^{}{}_{}{}^{0.74}$	6.44${}_{3.47}{}^{}{}_{}{}^{15.0}$	$-$215.0${}_{-298.0}{}^{}{}_{}{}^{-158.0}$	$-$212.0${}_{-294.2}{}^{}{}_{}{}^{-152.0}$
40								5.42${}_{4.46}{}^{}{}_{}{}^{6.73}$	21.58${}_{12.39}{}^{}{}_{}{}^{45.81}$	0.60${}_{0.49}{}^{}{}_{}{}^{0.74}$	6.47${}_{3.43}{}^{}{}_{}{}^{14.9}$	$-$216.0${}_{-297.2}{}^{}{}_{}{}^{-161.8}$	$-$209.0${}_{-295.2}{}^{}{}_{}{}^{-155.0}$
45								5.42${}_{4.37}{}^{}{}_{}{}^{6.68}$	21.20${}_{12.96}{}^{}{}_{}{}^{45.36}$	0.59${}_{0.49}{}^{}{}_{}{}^{0.74}$	6.32${}_{3.48}{}^{}{}_{}{}^{14.8}$	$-$213.5${}_{-295.3}{}^{}{}_{}{}^{-165.0}$	$-$210.0${}_{-294.2}{}^{}{}_{}{}^{-149.0}$
50								5.41${}_{4.28}{}^{}{}_{}{}^{6.65}$	22.14${}_{12.35}{}^{}{}_{}{}^{44.89}$	0.60${}_{0.49}{}^{}{}_{}{}^{0.74}$	6.62${}_{3.26}{}^{}{}_{}{}^{14.85}$	$-$218.0${}_{-295.2}{}^{}{}_{}{}^{-159.0}$	$-$210.0${}_{-293.3}{}^{}{}_{}{}^{-144.0}$
35	2M18461977$-$3021506	281.582414	$-$30.364075	$-$224.99$\pm$0.00	2.97$\pm$0.35	$-$8.525$\pm$0.077	$-$17.357$\pm$0.066	0.10${}_{0.04}{}^{}{}_{}{}^{0.24}$	9.28${}_{8.29}{}^{}{}_{}{}^{10.19}$	0.97${}_{0.94}{}^{}{}_{}{}^{0.98}$	3.51${}_{3.07}{}^{}{}_{}{}^{3.70}$	$-$18.0${}_{-38.0}{}^{}{}_{}{}^{8.0}$	41.0${}_{36.0}{}^{}{}_{}{}^{52.0}$
40								0.21${}_{0.04}{}^{}{}_{}{}^{0.67}$	8.24${}_{7.65}{}^{}{}_{}{}^{8.94}$	0.94${}_{0.83}{}^{}{}_{}{}^{0.98}$	3.25${}_{2.86}{}^{}{}_{}{}^{3.44}$	7.0${}_{-14.0}{}^{}{}_{}{}^{25.1}$	30.0${}_{15.0}{}^{}{}_{}{}^{44.0}$
45								0.37${}_{0.06}{}^{}{}_{}{}^{0.85}$	7.93${}_{7.37}{}^{}{}_{}{}^{8.37}$	0.91${}_{0.79}{}^{}{}_{}{}^{0.98}$	3.11${}_{2.77}{}^{}{}_{}{}^{3.94}$	14.0${}_{-4.0}{}^{}{}_{}{}^{31.0}$	28.0${}_{12.0}{}^{}{}_{}{}^{43.0}$
50								0.39${}_{0.06}{}^{}{}_{}{}^{0.68}$	8.03${}_{7.67}{}^{}{}_{}{}^{8.51}$	0.90${}_{0.83}{}^{}{}_{}{}^{0.98}$	3.20${}_{3.00}{}^{}{}_{}{}^{3.61}$	14.0${}_{-3.2}{}^{}{}_{}{}^{25.0}$	27.0${}_{10.0}{}^{}{}_{}{}^{41.0}$
35	2M18472793$-$3033242	281.866403	$-$30.556734	87.59$\pm$0.05	8.69$\pm$1.15	0.421$\pm$0.060	$-$6.731$\pm$0.052	0.04${}_{0.02}{}^{}{}_{}{}^{0.28}$	3.19${}_{2.52}{}^{}{}_{}{}^{3.96}$	0.96${}_{0.86}{}^{}{}_{}{}^{0.98}$	2.45${}_{2.15}{}^{}{}_{}{}^{3.07}$	$-$16.0${}_{-26.0}{}^{}{}_{}{}^{-11.0}$	15.0${}_{-4.0}{}^{}{}_{}{}^{23.0}$
40								0.05${}_{0.02}{}^{}{}_{}{}^{0.24}$	2.95${}_{2.18}{}^{}{}_{}{}^{4.56}$	0.95${}_{0.89}{}^{}{}_{}{}^{0.98}$	2.50${}_{2.16}{}^{}{}_{}{}^{3.07}$	$-$17.0${}_{-34.0}{}^{}{}_{}{}^{-12.0}$	3.0${}_{-2.0}{}^{}{}_{}{}^{14.0}$
45								0.07${}_{0.02}{}^{}{}_{}{}^{0.26}$	3.26${}_{2.43}{}^{}{}_{}{}^{4.15}$	0.94${}_{0.87}{}^{}{}_{}{}^{0.98}$	2.52${}_{2.10}{}^{}{}_{}{}^{3.05}$	$-$23.0${}_{-37.0}{}^{}{}_{}{}^{-14.0}$	2.0${}_{-4.0}{}^{}{}_{}{}^{11.0}$
50								0.19${}_{0.04}{}^{}{}_{}{}^{0.33}$	3.54${}_{2.12}{}^{}{}_{}{}^{3.90}$	0.88${}_{0.77}{}^{}{}_{}{}^{0.97}$	2.48${}_{2.07}{}^{}{}_{}{}^{3.09}$	$-$24.0${}_{-33.0}{}^{}{}_{}{}^{-15.0}$	$-$2.0${}_{-5.0}{}^{}{}_{}{}^{6.0}$
35	2M18502108$-$2923442	282.587861	$-$29.395628	$-$31.22$\pm$0.00	1.90$\pm$0.11	$-$16.159$\pm$0.072	$-$15.883$\pm$0.062	0.68${}_{0.37}{}^{}{}_{}{}^{0.98}$	6.75${}_{6.41}{}^{}{}_{}{}^{7.05}$	0.82${}_{0.74}{}^{}{}_{}{}^{0.88}$	3.16${}_{2.86}{}^{}{}_{}{}^{3.28}$	$-$61.0${}_{-68.0}{}^{}{}_{}{}^{-39.0}$	$-$22.0${}_{-32.0}{}^{}{}_{}{}^{-11.0}$
40								0.77${}_{0.57}{}^{}{}_{}{}^{0.90}$	6.63${}_{6.47}{}^{}{}_{}{}^{6.82}$	0.79${}_{0.76}{}^{}{}_{}{}^{0.83}$	3.06${}_{2.72}{}^{}{}_{}{}^{3.70}$	$-$51.0${}_{-56.0}{}^{}{}_{}{}^{-43.0}$	$-$27.0${}_{-32.0}{}^{}{}_{}{}^{-19.0}$
45								0.72${}_{0.57}{}^{}{}_{}{}^{0.86}$	6.65${}_{6.48}{}^{}{}_{}{}^{7.92}$	0.81${}_{0.79}{}^{}{}_{}{}^{0.83}$	3.15${}_{2.69}{}^{}{}_{}{}^{3.32}$	$-$52.0${}_{-74.2}{}^{}{}_{}{}^{-41.0}$	$-$25.0${}_{-29.0}{}^{}{}_{}{}^{-18.0}$
50								0.74${}_{0.44}{}^{}{}_{}{}^{1.28}$	6.49${}_{6.38}{}^{}{}_{}{}^{7.39}$	0.79${}_{0.70}{}^{}{}_{}{}^{0.87}$	2.98${}_{2.78}{}^{}{}_{}{}^{3.56}$	$-$47.0${}_{-69.0}{}^{}{}_{}{}^{-37.0}$	$-$20.0${}_{-40.0}{}^{}{}_{}{}^{-10.0}$
35	2M19004420$+$4421082	285.184205	44.352283	$-$219.58$\pm$0.16	4.04$\pm$0.33	$-$5.337$\pm$0.036	$-$11.575$\pm$0.035	1.13${}_{0.89}{}^{}{}_{}{}^{1.28}$	11.44${}_{10.71}{}^{}{}_{}{}^{12.14}$	0.81${}_{0.80}{}^{}{}_{}{}^{0.84}$	2.80${}_{1.85}{}^{}{}_{}{}^{3.45}$	$-$64.0${}_{-71.0}{}^{}{}_{}{}^{-59.0}$	$-$48.0${}_{-57.0}{}^{}{}_{}{}^{-38.0}$
40								1.00${}_{0.87}{}^{}{}_{}{}^{1.16}$	11.38${}_{10.71}{}^{}{}_{}{}^{12.85}$	0.83${}_{0.82}{}^{}{}_{}{}^{0.85}$	2.84${}_{2.07}{}^{}{}_{}{}^{3.79}$	$-$64.0${}_{-82.0}{}^{}{}_{}{}^{-58.0}$	$-$42.0${}_{-51.0}{}^{}{}_{}{}^{-37.0}$
45								1.21${}_{0.83}{}^{}{}_{}{}^{1.30}$	12.19${}_{11.44}{}^{}{}_{}{}^{12.49}$	0.81${}_{0.80}{}^{}{}_{}{}^{0.86}$	2.15${}_{1.86}{}^{}{}_{}{}^{2.91}$	$-$73.0${}_{-77.0}{}^{}{}_{}{}^{-67.0}$	$-$54.0${}_{-57.0}{}^{}{}_{}{}^{-35.0}$
50								1.06${}_{0.91}{}^{}{}_{}{}^{1.21}$	11.62${}_{10.92}{}^{}{}_{}{}^{12.37}$	0.83${}_{0.82}{}^{}{}_{}{}^{0.85}$	2.66${}_{1.76}{}^{}{}_{}{}^{3.31}$	$-$66.0${}_{-74.0}{}^{}{}_{}{}^{-59.0}$	$-$47.0${}_{-53.0}{}^{}{}_{}{}^{-39.7}$
35	2M20124750$+$1818007	303.197945	18.300213	$-$58.21$\pm$0.22	7.63$\pm$0.59	$-$2.890$\pm$0.036	$-$5.879$\pm$0.030	4.70${}_{4.30}{}^{}{}_{}{}^{4.85}$	8.79${}_{8.54}{}^{}{}_{}{}^{9.15}$	0.30${}_{0.28}{}^{}{}_{}{}^{0.33}$	1.34${}_{1.23}{}^{}{}_{}{}^{1.42}$	$-$169.0${}_{-173.0}{}^{}{}_{}{}^{-167.0}$	$-$134.0${}_{-137.0}{}^{}{}_{}{}^{-127.0}$
40								3.60${}_{3.56}{}^{}{}_{}{}^{5.63}$	8.30${}_{8.21}{}^{}{}_{}{}^{8.55}$	0.39${}_{0.20}{}^{}{}_{}{}^{0.39}$	1.22${}_{1.17}{}^{}{}_{}{}^{1.42}$	$-$154.0${}_{-167.0}{}^{}{}_{}{}^{-147.0}$	$-$105.0${}_{-158.0}{}^{}{}_{}{}^{-103.0}$
45								4.99${}_{4.26}{}^{}{}_{}{}^{5.71}$	8.20${}_{7.98}{}^{}{}_{}{}^{8.66}$	0.24${}_{0.20}{}^{}{}_{}{}^{0.30}$	1.27${}_{1.13}{}^{}{}_{}{}^{1.43}$	$-$152.0${}_{-170.0}{}^{}{}_{}{}^{-142.0}$	$-$142.0${}_{-159.0}{}^{}{}_{}{}^{-127.0}$
50								4.94${}_{4.41}{}^{}{}_{}{}^{5.70}$	8.48${}_{7.84}{}^{}{}_{}{}^{8.64}$	0.26${}_{0.20}{}^{}{}_{}{}^{0.29}$	1.27${}_{1.10}{}^{}{}_{}{}^{1.43}$	$-$155.0${}_{-167.0}{}^{}{}_{}{}^{-139.0}$	$-$138.0${}_{-160.0}{}^{}{}_{}{}^{-129.0}$
35	2M21181769$+$0946422	319.573711	9.7784	$-$115.86$\pm$0.02	5.04$\pm$0.65	1.345$\pm$0.057	$-$5.096$\pm$0.058	1.21${}_{1.10}{}^{}{}_{}{}^{1.34}$	8.10${}_{7.78}{}^{}{}_{}{}^{8.22}$	0.73${}_{0.70}{}^{}{}_{}{}^{0.76}$	2.51${}_{2.07}{}^{}{}_{}{}^{3.33}$	$-$67.0${}_{-71.0}{}^{}{}_{}{}^{-61.0}$	$-$46.0${}_{-51.0}{}^{}{}_{}{}^{-42.0}$
40								1.23${}_{1.05}{}^{}{}_{}{}^{1.42}$	8.31${}_{8.01}{}^{}{}_{}{}^{9.30}$	0.74${}_{0.70}{}^{}{}_{}{}^{0.78}$	2.59${}_{2.10}{}^{}{}_{}{}^{3.02}$	$-$71.0${}_{-91.0}{}^{}{}_{}{}^{-63.0}$	$-$45.0${}_{-49.0}{}^{}{}_{}{}^{-39.0}$
45								1.21${}_{0.81}{}^{}{}_{}{}^{1.33}$	8.60${}_{8.48}{}^{}{}_{}{}^{8.81}$	0.75${}_{0.73}{}^{}{}_{}{}^{0.82}$	2.64${}_{2.41}{}^{}{}_{}{}^{2.91}$	$-$68.0${}_{-77.0}{}^{}{}_{}{}^{-63.0}$	$-$44.0${}_{-49.0}{}^{}{}_{}{}^{-30.0}$
50								1.38${}_{1.20}{}^{}{}_{}{}^{1.56}$	8.37${}_{8.15}{}^{}{}_{}{}^{8.64}$	0.71${}_{0.67}{}^{}{}_{}{}^{0.75}$	2.99${}_{2.84}{}^{}{}_{}{}^{3.31}$	$-$64.0${}_{-70.0}{}^{}{}_{}{}^{-59.0}$	$-$47.0${}_{-50.0}{}^{}{}_{}{}^{-44.0}$
35	2M22015914$+$1543129	330.49643	15.720271	$-$58.32$\pm$0.25	3.29$\pm$0.26	1.341$\pm$0.050	$-$0.273$\pm$0.047	3.54${}_{3.45}{}^{}{}_{}{}^{3.71}$	9.71${}_{9.62}{}^{}{}_{}{}^{9.78}$	0.46${}_{0.44}{}^{}{}_{}{}^{0.47}$	2.16${}_{1.92}{}^{}{}_{}{}^{2.35}$	$-$158.0${}_{-161.0}{}^{}{}_{}{}^{-154.0}$	$-$110.0${}_{-115.0}{}^{}{}_{}{}^{-106.0}$
40								4.47${}_{4.37}{}^{}{}_{}{}^{4.56}$	9.40${}_{9.27}{}^{}{}_{}{}^{9.57}$	0.35${}_{0.34}{}^{}{}_{}{}^{0.37}$	2.07${}_{1.85}{}^{}{}_{}{}^{2.32}$	$-$149.0${}_{-152.0}{}^{}{}_{}{}^{-147.0}$	$-$140.0${}_{-143.0}{}^{}{}_{}{}^{-138.0}$
45								4.45${}_{4.32}{}^{}{}_{}{}^{4.57}$	9.22${}_{9.13}{}^{}{}_{}{}^{9.85}$	0.34${}_{0.33}{}^{}{}_{}{}^{0.38}$	2.06${}_{1.89}{}^{}{}_{}{}^{2.35}$	$-$148.0${}_{-151.0}{}^{}{}_{}{}^{-146.0}$	$-$137.0${}_{-141.0}{}^{}{}_{}{}^{-134.0}$
50								4.50${}_{4.41}{}^{}{}_{}{}^{4.59}$	9.57${}_{9.39}{}^{}{}_{}{}^{9.76}$	0.35${}_{0.34}{}^{}{}_{}{}^{0.37}$	2.13${}_{1.91}{}^{}{}_{}{}^{2.36}$	$-$149.0${}_{-152.0}{}^{}{}_{}{}^{-148.0}$	$-$141.0${}_{-143.0}{}^{}{}_{}{}^{-139.0}$

Full text

1 INTRODUCTION

The advent of large spectroscopic surveys such as APOGEE (Majewski et al., 2017) and its capability to measure the atmospheric composition of $\sim$176,000 giants distributed homogeneously over much of the Milky Way (bulge, disk, and halo), and especially designed to observe where extinction by dust is significantly higher, has opened up a new panoramic window on our Galaxy, providing the precise chemical abundance of more than 23 chemical species (e.g., C, N, O, Na, Mg, Al, Si, P, S, K, Ca, Ti, V, Cr, Mn, Co, Ni, Cu, Ge, Rb, Nd, Ce and Yb).

The detailed and unprecedented precision of most of the stellar elemental abundances provided in the H-band ($\lambda$1.5–1.7$\mu$m) has enabled the discovery of giants with unusual abundance patterns throughout of the Galaxy. For example, Martell et al. (2016); Fernández-Trincado et al. (2016b, 2017); Schiavon et al. (2017a); Reis et al. (2018); Koch et al. (2019) and Fernández-Trincado et al. (2019) have identified many such stars through a simple technique known as ”weak” chemical tagging (Freeman & Bland-Hawthorn, 2002; Ting et al., 2015, 2016; Hogg et al., 2016; Schiavon et al., 2017a), i.e., chemically tagging stars born in the same type of stellar system characterised by an unique detailed abundance pattern. Most of the APOGEE spectra have been re-analyzed manually in the works above, with the conclusion that a significant fraction of giants fell within the bounds of the chemically anomalous stars unique to Galactic and/or extragalactic globular cluster environments. Their number has become increased in recent years (see Recio-Blanco et al., 2017; Tang et al., 2019; Kemp et al., 2018), thanks to other extensive spectroscopic surveys such as LAMOST, , which obtained low-resolution spectra (Zhao et al., 2012; Luo et al., 2012; Deng et al., 2012; Cui et al., 2012), and the Gaia-ESO survey, with both medium- and high-resolution spectra (Gilmore et al., 2012; Randich et al., 2013). So far, these results demonstrate that those inhomogeneities appear to occur in other star-formation environments. Such stars have received significant attention in recent years, primarily because they are considered as evaporated from stellar clusters, and as such, play an important role in deciphering the early history of the Galactic formation process (Martell & Grebel, 2010; Martell et al., 2011; Carollo et al., 2013; Fernández-Trincado et al., 2015a, b, 2016a; Helmi et al., 2018; Khoperskov et al., 2018; Minniti et al., 2018a; Ibata et al., 2019), as well as providing clues on the mechanism responsible for the ejection from stellar clusters and its relation with chemical peculiarity (e.g., Pereira et al., 2017, 2019).

Often, stars with ”anomalous chemistry” have been qualitatively linked to the so–called second-generation111Here, we refer to second-generation to the groups of stars showing enhanced N and Al, and depleted C and O abundances, with respect to other field stars at the same metallicity [Fe/H]. globular cluster stars, which clearly exhibit enhanced N, Na, and Al and depleted C, Mg and O abundances with respect to field stars at the same metallicity (e.g., Bastian & Lardo, 2018), however, this terminology is ambiguous in multiple ways. The implicit assumption, that the unusual abundance patterns result after the chemically mundane stars and have been enriched by a previous generation, has not been fully demonstrated. Here, we refer to the stars with peculiar chemical composition as enriched, and the stars having field-like abundances as primordial.

Furthermore, it is now firmly established that carbon-depleted ([C/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}+0.15) giants beyond the metal-poor tail ([Fe/H]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}-0.7) of the thick disk with N enrichment ([N/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}+0.5, hereafter N-rich stars) are found throughout the Milky Way, and owe their unusual elemental abundances to rare astrophysical events or nucleosynthetic pathways in different environments (Mészáros et al., 2015; Masseron et al., 2019; Schiavon et al., 2017b; Fernández-Trincado et al., 2018, 2019). On the other hand, beyond the intrinsic value of identifying the mechanism responsible for the unusual abundance patterns, which are still far from being understood, the exclusive chemistry of such stars are essentials to more broadly improve our understanding of the chain of physical processes experienced by the Milky Way from early. However, the census of chemically anomalous N-rich stars across the Milky Way is still far from complete, especially beyond the bulge regions. Recently, Martell et al. (2016); Fernández-Trincado et al. (2016b, 2017, 2019) reported the discovery of 18 new N-rich stars in the bulge, disk and inner halo of the Milky Way. The present work, reports the discovery of other 31 new N-rich stars in the bulge, disk and inner halo.

Here we revisit the APOGEE spectra to conduct the largest updated census of N-rich stars throughout the Milky Way. Furthermore, the current version of the APOGEE Stellar Parameters and Chemical Abundance Pipeline (ASPCAP, García Pérez et al., 2016) does not measure the s-process elements, but these are measurable from Ce II and Nd II lines (Hasselquist et al., 2016; Cunha et al., 2017) in the observed spectral window, and carry important information about stellar nucleosynthesis along the RGB and AGB. Here we provide for the first time, measures of the neutron-capture element Ce II (Cunha et al., 2017) for some of these candidates. In particular, studies of s-process elements provide strong evidence either for or against the uniqueness of the progenitor stars to stellar systems. In Section 2 we outline our methods to identify candidates enhanced in nitrogen ([N/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}+0.5) and depleted in carbon ([C/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}+0.15). In Section 3 we discuss our results, and in Section 4 we present our concluding remarks.

2 DATA AND METHODS

2.1 Targets Analysed

The sample analysed in this work consist of red giants from the 14th data release of SDSS (DR14, Abolfathi et al., 2018; Jönsson et al., 2018; Holtzman et al., 2018) of the APOGEE-2 survey (Majewski et al., 2017), which has obtained high-resolution (*R$\sim$*22,500) spectra of $\sim$ 270,000 stars in the H-band ($\sim\lambda$1.5–1.7$\mu$m), using the 300-fiber cryogenic spectrograph installed on the 2.5m Telescope (Gunn et al., 2006) at the Apache Point Observatory, as part of the Sloan Digital Sky Survey IV (Blanton et al., 2017). We refer the reader to Zasowski et al. (2013) and Zasowski et al. (2017) for full details regarding the targeting strategies for APOGEE and APOGEE-2, and Nidever et al. (2015), Zamora et al. (2015), Holtzman et al. (2015) and García Pérez et al. (2016) for more details concerning data reduction of the APOGEE spectra, determination of radial velocities, atmospheric parameters, and stellar abundances, respectively.

In this work, we have selected a sub-sample of metal-poor ([Fe/H]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}-0.7) red giants in the first Payne data release of APOGEE abundances (Ting et al., 2018, hereafter Payne-APOGEE) that satisfy the following quality cuts to further ensure reliable parameter/abundance derivation:

• $\circ$

S/N $>$ 70

• $\circ$

3000 K $<$Teff $<$ 5500 K

• $\circ$

log g $<$ 3.6

• $\circ$

quality_flags $=$ good

The Payne routine (see Ting et al., 2018) simultaneously derives best-fit values for all atmospheric parameters and abundances using neural networks, with the parameter space of the training set restricted to [Fe/H]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}-1.5. For the same reason as in Fernández-Trincado et al. (2016b, 2017, 2019) and Schiavon et al. (2017a), we remove stars with [C/Fe] $>+0.15$, because such stars are not typically found in globular clusters, and we want to minimize the contamination by objects such as CH stars (e.g., Karinkuzhi & Goswami, 2015), leaving us with a total of 6,289 giants with metallicities in the range $-1.5<$ [Fe/H] $<-0.7$.

To search for outliers in the [N/Fe]-[Fe/H] abundance plane (see Figure 1), we binned in [Fe/H] space (0.05 dex bins), and by fitting a 5th order polynomial to the bulk of the stars, select stars that deviate from the fit by more than \raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}2.5\sigma from that curve as nitrogen-rich red giants, i.e., we label all stars with nitrogen abundance more than $\sim$0.4 dex above the mean at a fixed metallicity as ”N-rich”. The bins were chosen to ensure that at least 200 stars occupied each bin (see inner label numbers in Figure 1).

In a similar way as described in Schiavon et al. (2017a), we note that over a more limited metallicity range, a sixth-order polynomical also captures the mean behavior of our data set well, which includes stars located towards the disk, bulge and halo, simultaneously. This is the first time, that such global feature is evaluated across the Milky Way (disk+halo+bulge) to homogeneously identify such anomalous stars. The initial sample contained about 300 N-rich candidates, according to the [N/Fe] versus [Fe/H] abundance plane from Payne-APOGEE determinations. These stars have high [N/Fe] ratios (\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}+0.5).

There was expected to be some contamination by star clusters and other previously reported outliers, which we remove from our sample. We found that 177 out of 284 stars are confirmed cluster stars from Masseron et al. (2019) and (Fernández-Trincado et al., 2018), while 31 out of 284 stars are know N-rich stars previously reported in Martell et al. (2016); Fernández-Trincado et al. (2016b); Schiavon et al. (2017a); Fernández-Trincado et al. (2017) and Fernández-Trincado et al. (2019). This yields 79 stars that are previously overlooked nitrogen-rich objects relative in the final data set. For reasons that are explained below, we remove 48 of those stars from our final analysis.

Figure 1 shows our final data set in the [N/Fe]-[Fe/H] plane against the giants that have unusually high N abundances. After applying a number of stringent selection criteria, this yielded the discovery of 31 further N-rich stars (bona fide chemically anomalous giants), adding to the $\sim 100$ such objects out of $\sim 7,000$ regular disk (thick) and halo stars from previous studies.

2.2 Stellar Parameters and Chemical Abundance

Measurements

In order to examine the reliability of these high-[N/Fe] outliers, we performed a careful inspection of each APOGEE spectrum. We made use of the Brussels Automatic Stellar Parameter (BACCHUS) code (Masseron et al., 2016) to derive the metallicity, broadening parameters, and chemical abundances for the newly identified N-rich sample, making a careful line selection as well as providing abundances based on a line-by-line differential approach.

BACCHUS relies on the radiative transfer code Turbospectrum (Alvarez & Plez, 1998; Plez, 2012) and the MARCS model atmosphere grid (Gustafsson et al., 2008). For each element and each line, the abundance determination proceeds as in Hawkins et al. (2016), Fernández-Trincado et al. (2017, 2018), and Fernández-Trincado et al. (2019), and summarized here for guindance: (i) a spectrum synthesis, using the full set of (atomic and molecular) lines, is used to find the local continuum level via a linear fit; (ii) cosmic and telluric rejections are performed; (iii) the local S/N is estimated; (iv) a series of flux points contributing to a given absorption line are automatically selected; and (v) abundances are then derived by comparing the observed spectrum with a set of convolved synthetic spectra characterised by different abundances. Four different abundance determinations are used: (i) line-profile fitting; (ii) core line-intensity comparison; (iii) global goodness-of-fit estimate; and (iv) equivalent width comparison. Each diagnostic yields validation flags. Based on these flags, a decision tree then rejects the line or accepts it, keeping the best-fit abundance. We adopted the $\chi^{2}$ diagnostic as it is the most robust. However, we store the information from the other diagnostics, including the standard deviation, between all four methods.

The linelist used in this work is the latest internal DR14 atomic/molecular linelist (linelist.20170418). For a more detailed description of these lines, we refer the reader to a forthcoming paper (Holtzman et al., in preparation). The current version of ASPCAP/DR14 and the Payne routine do not determine the s-process elements (Nd II and Ce II). Thus, we determine, for the first time, these elements in our target stars, adopting the linelists provided in Hasselquist et al. (2016) and Cunha et al. (2017).

For the light elements, a mix of heavily CN-cycled and $\alpha$-poor MARCS models were used, as well as the same molecular lines adopted by Smith et al. (2013), were employed to determine the C, N, and O abundances. In addition, we have adopted the C, N, and O abundances that satisfy the fitting of all molecular lines consistently; i.e., we first derive 16O abundances from 16OH lines, then derive 12C from 12C16O lines and 14N from 12C14N lines, and the CNO abundances are derived several times to minimize the OH, CO, and CN dependences (see, e.g., Smith et al., 2013; Fernández-Trincado et al., 2016b, 2017, 2018, 2019).

Atmospheric parameters from spectroscopy: In order to provide a consistent chemical analysis, we re-determine the chemical abundances assuming as input the effective temperature (Teff), surface gravity (log g), and metallicity ([Fe/H]) as derived by the Payne-APOGEE runs (see e.g., Ting et al., 2018).

Atmospheric parameters from photometry: We also applied a simple approach of fixing T${}^{pho}_{\rm eff}$ and log g to values determined independently of spectroscopy, in order to check for any significant deviation in the chemical abundances. For this, the photometric effective temperatures were calculated from the $J_{2MASS}-K_{s,2MASS}$ color relation using the methodology presented in González Hernández & Bonifacio (2009). Photometry is extinction corrected using the Rayleigh Jeans Color Excess (RJCE) method (e.g., Majewski et al., 2011). The results are listed in Table 1. We estimate surface gravity from 10 Gyr PARSEC (Bressan et al., 2012) isochrones, as illustrated in Figure 2, since 10 Gyr is the typical age of Galactic GCs (Harris, 1996). The mean elemental abundances derived with the BACCHUS code are listed in Table 2.

Figure 2 compares the difference between the adopted atmospheric parameters as the stars ascend the giant branch. Figure 3 shows the difference of the derived chemical species from the BACCHUS pipeline for both adopted atmospheric parameters. The same figure indicates that small systematic differences are present between the spectroscopic and atmospheric parameters. However, for a few stars, the Payne-APOGEE raw temperature above $\,\stackrel{{\scriptstyle\textstyle>}}{{\sim}}\,$ 5000 K and below $\,\stackrel{{\scriptstyle\textstyle<}}{{\sim}}\,$ 3500 K in metal-poor stars showed significant, 200–400 K offsets, compared to photometry along with significant surface gravity (0.25–0.7 dex) offsets at the same temperature range, and are thus expected to display large scatter in the abundance analysis, as seen in rows 2, 3, 4 and 5 in Figure 3, which may be the reason for the large scatter in [N/Fe], [O/Fe], [Na/Fe], [Ce II/Fe], and [Nd II/Fe]. It is important to note that BACCHUS recovers the [Fe I/H] abundance ratios of these stars within 0.09 dex for both photometric and spectroscopic temperatures. The adoption of a purely photometry temperature scale enables us to be somewhat idependent of the Payne-APOGEE pipeline and the APOGEE/ASPCAP pipeline, which gives important comparison data for future pipeline validation. The final results presented in this paper are based on the spectroscopic atmospheric parameters provided by Payne-APOGEE, and are use to estimate our final errors (listed in Table 4).

Incidence of false detections: A cautionary note is in order before proceeding with the analysis. Once the atmospheric parameters are determined, for each star the selected 12C14N lines were visually inspected to ensure that the spectral fit was adequate. If the lines were not well-reproduced by the synthesis it were rejected. In addition, for a substantial fraction of our target stars, the 12C14N lines were also rejected if they were flagged as problematic by the BACCHUS pipeline, i.e., they were stronly blended or too weak in the spectra of stars with the typical Teff and metallicity of the N-rich sample to deliver reliable [N/Fe] abundances. This indicates, as confirmed by visual inspection of 45 out of 79 stars in our sample, that the spectral fits are of poor quality, or that the stellar parameters are unreliable or both, suggesting that the abundances for these stars cannot be relied on. In this way, 45 stars were identified as false detections, leaving us with a grand total of 31 newly identified reliable N-rich field stars (white unfilled ’star’ symbols), as illustrated in Figure 1. Figure 4 show examples for a portion of the observed APOGEE spectra in the region around the strong 12C14N bands for our 31 stars.

3 Results and discussion

3.1 Chemical Signatures

In this subsection, we discuss the individual abundance ratios and trends, as function of metallicity, for the 31 newly identified N-rich stars.

Figure 5 shows the distribution of [Al/Fe], [N/Fe], [Mg/Fe], [Si/Fe], and [Fe/H] for all stars that made it through the quality criteria discussed in Section 2.1. These elements were chosen because ”migrants” from globular clusters exhibit clear deficiencies and enrichments in these elemental abundances as compared to most stars in Milky Way (Martell et al., 2016; Schiavon et al., 2017a; Fernández-Trincado et al., 2016b, 2017). Most obvious in this plot are the high-[N/Fe] outliers with [N/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}+0.5, nominally corresponding to a chemically anomalous population, commonly associated with stars possibly removed from a system merged with our Milky Way (unless they are part of a binary system). We did not detect any variation of the radial velocities that would support the hypothesis that these objects formed through the binary channel, however, most of the stars in our sample were observed just once, and those with multiple observations have a short baseline ($<$ 6 months), which makes possible detection of only a small fraction of possible binaries (e.g., Fernández-Trincado et al., 2019). The radial velocity dispersion ($RV{scatter}$) of our sample is listed in Table 1, which is typically less than 1.5 km s*-1* over multiple visits, indicating that most of the newly identified N-rich stars unlikely to be variable stars or part of a binary system.

A small fraction ($\sim$29%) of our giants exhibit large-enrichment in aluminum, [Al/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}+0.5, which make them more likely to be migrants from globular clusters, as they are not typical giants as seen in dwarf galaxy stars (e.g., Hasselquist et al., 2017, 2019). Such N-/Al-rich stars occupy the same locus as SG-like N-/Al-rich giants found in previous studies (Fernández-Trincado et al., 2016b, 2017), and the second-generation globular cluster stars (Mészáros et al., 2015; Masseron et al., 2019), reinforcing the similarity between such objects and, the globular cluster population. The high levels of Al rule out the possibility that satellite galaxies could have contributed stars to our N-/Al-rich population. These objects exhibit chemical similarities to that the second-generation globular cluster stars, implying that it is possible that a high aluminum and nitrogen abundance could be related to escaped globular cluster stars, or due to metal-poor AGB stars that have experienced strong internal mixing; these chemical properties enable us to classify such objects as SG-like (see Table 2). This unique collection of N-rich stars significantly contributes to the task of compiling a more thorough census of anomalously high levels of [N/Fe] and [Al/Fe] throughout the Milky Way, and portends the promising results to be expected from future spectroscopic follow-up observations, and to reconsider the question of in situ halo formation (Martell et al., 2016). For other light-element chemical planes, the distinction between the newly identified N-/Al-rich stars and Milky Way population appears to be weaker in Mg and weakest in Si. Here, we show that the [Al/Fe]-[N/Fe] and [Al/Fe]-[Mg/Fe] chemical planes are an especially powerful and reliable diagnostic to identify this unique class of stars among the N-rich population (primarily with metallicities [Fe/H]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}-0.7).

At lower [Al/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}+0.5 abundances, there is more overlap in [X/Fe] between the chemistry of Milky Way, dwarf galaxy stars (Hasselquist et al., 2017, 2019), and the so–called First-Generation of globular cluster stars (Mészáros et al., 2015), i.e., 24 out of 31 N-rich stars in our final data set exhibit chemical abundances that are somewhat distinct in the [Fe/H]-[N/Fe], [Mg/Fe]-[Al/Fe] and [N/Fe]-[Al/Fe] planes, as shown in Figure 1 and the top panels in Figure 5, but indistinguishable in other chemical planes from stars having chemistry consistent with the halo and thick disk (left-bottom panel in Figure 5), and are distinctly less Mg-enriched (right-bottom panel in Figure 5). Unfortunately, with only few light-/heavy-elements measured, it is not possible to assign the nucleosynthetic origins of these N-rich/Al-normal stars, and disentangle a dwarf galaxy and globular cluster (stars having peculiar chemical composition like the first population) origins; such objects are classified as FG-like/dGs in Table 2. It is likely that they were contributed by different merger events from a dwarf galaxy such as Gaia-Enceladus (Belokurov et al., 2018; Helmi et al., 2018) and the Sagittarius dSph (Hasselquist et al., 2019), or massive disrupted globular clusters (e.g., Kruijssen, 2015).

Figure 6 displays our N-rich sample and globular cluster star data together on the [Al/Fe] versus [Si/Fe], [Mg/Fe], [N/Fe], and [Ce/Fe] planes. The mildly metal-poor globular cluster stars of Masseron et al. (2019), from M5, M107, and M71 are included in this plot, so that the GCs span as wide a metallicity range as our field sample, and have been homogeneously analyzed in the same manner as the N-rich sample presented in this study. Interestingly, the light-/heavy-elements seen in the globular cluster population matches approximately the abundance values determinated for the newly identified N-rich field population at the same [Fe/H]. This result is consistent with findings from other studies, which have characterised SG and FG stars in GCs as having similar chemistry as field stars of same metallicity (e.g., Lind et al., 2015; Martell et al., 2016; Fernández-Trincado et al., 2016b, 2017, 2019). One obvious exception is the star, 2M15535831$+$4333280, extremely Mg-depleted ($<-0.4$) and has high [Al/Fe] and [N/Fe] ratios, similar to large light-element enrichment seen in TYC 5619-109-1 (Fernández-Trincado et al., 2016b), which clearly fall within the extreme limits for [Mg/Fe] of the ’second- generation’ globular cluster population. Our sample’s [N/Fe] appears definitively anomalous, with a spread in [N/Fe] from around 0.5 to 1.5 dex.

The [Ce/Fe] abundance ratios for stars in our sample also show similar levels to those found for stars residing in globular clusters, with a spread in [Ce/Fe] from around -0.2 to $\sim$1.15. Given the lack of information regarding other neutron-capture elements, it is difficult to assign the nucleosynthetic pathways for such stars, however, we can speculate that the Ce and Nd we have measured are likely to have a pure s-process origin.

The [O/Fe] abundance ratio is uncertain in the $T_{\rm eff}$ regime of our objects. The uncertainty arises because BACCHUS determines these abundances from the strengths of 12C14N and 12C16O lines, which become too weak for hotter stars at relatively low metallicities ([Fe/H] \raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}-0.7). Moreover, our results show that, C, Na, Ce II, and Nd II abundances have mostly upper limits (see Table 2), implying that most of these line become weak and heavily blended to be accurately measured, and therefore the derived abundances strongly depends on the ability of properly reproducing the blend. APOGEE has 10 Nd II and 9 Ce II features detectable (Hasselquist et al., 2016; Cunha et al., 2017), however these lines are highly sensitive to stellar parameters, and therefore, only a few can be used to derive upper limits for a large variety of metal-poor stars. In APOGEE spectra, two Na I lines are visible (1.6373$\mu$m and 1.6388$\mu$m) for a few metal-poor stars, however these lines are weak and heavily blended by telluric features at the typical $T_{\rm eff}$ and metallicity for the stars studied in this work. At this time, we cannot guarantee the quality of the abundances for those elements.

3.2 Extra-tidal features around Galactic globular clusters

For most of the newly identified N-rich stars there are no known globular clusters within an angular separation of one degree, except four giants as listed in Table 3. We find for the first time a N-rich star (2M15183589$+$0027100) which appears likely to be a candidate extra-tidal star (within the errors) associated with Pal 5 based on [Fe/H] metallicity, radial velocity and elemental-abundances. We conclude that 2M15183589$+$0027100 is promising an extra-tidal candidate of Pal 5, which appears to be compatible with the globular cluster escapee scenario, as well as supporting spectroscopic evidence that accretion onto the early Milky Way was significant. For the rest of the three N-rich stars with nearby globular clusters, we find a large spread in metallicity and radial velocity, thus making an extra-tidal origin from nearby GCs for these three N-rich stars very unlikely (see Table 3).

3.3 Possible evolutionary state of the newly identified N-rich stars

Here we qualitatively examine the possible evolutionary state of the newly discovered N-rich stars. To accomplish this, the C, N, O, Mg, Al, Si, Na, Ce II, and Nd II abundances are compared with theoretical AGB nucleosynthesis predictions: FRUITY222FUll-Network Repository of Updated Isotopic Tables and Yields: http://fruity.oa-abruzzo.inaf.it/ models from Cristallo et al. (2015), which we have compared to observations with the FRUITY models of metallicity $Z=2\times{}10^{-3}$, the Monash model of metallicity [Fe/H]$=-1.2$ from Fishlock et al. (2014), and the ATON model ([Fe/H]$=-1.2$) from Ventura et al. (2016), as shown in Figure 8. Based on $\chi^{2}$ fitting of the light-/heavy-elements, we find that the majority of our N-rich stars fit the metal-poor, low-mass (M $<$1.5 – 5 M*⊙) AGB yields from Cristallo et al. (2015), which dominates the production of s-process elements (Ce II and Nd II) in most of the cases, but is at odds with the carbon abundance of the FRUITY database. On the other hand, the more massive AGB nucleosynthesis ATON and Monash models in the range of M $>$ 5 – 7 M⊙* is in better agreement with the observations, with the exception of [O/Fe], which shows a significant deviation from the theoretical predictions, perhaps due to the fact that the abundance of [O/Fe] is uncertain in the $T_{\rm eff}$ regime studied here. It is possible that the high nitrogen abundance could be due to a strong internal mixing process, suggesting that the newly identified N-rich stars are probably evolved objects, possibly an in ”early-AGB” or AGB phase. More detailed AGB nucleosynthesis models will be necessary to explain the puzzle of the neutron-capture elements observed in these stars, as well more observations for further understanding the chemical peculiarities observed in these stars.

3.4 Orbits

In order to provide insight on the origin of our stars across the Milky Way, the positional information of the newly identified N-rich stars was combined with precise proper motions from Gaia DR2 (Lindegren et al., 2018; Arenou et al., 2018), radial velocity from the APOGEE-2 survey(Nidever et al., 2015; Majewski et al., 2017), and the newly-measured spectro-photometric distances from Leung & Bovy (2019) as input data for the new state-of-the-art orbital integration package GravPot16333https://gravpot.utinam.cnrs.fr. Orbits are integrated in both an axisymemtric model, and a model including the perturbations due to a realistic (as far as possible) rotating ”boxy/peanut” bar, which fits the structural and dynamical parameters of the Galaxy to the best we know of the recent knowledge of our Milky Way (Fernandez-Trincado et al. 2019, in prep.). Figures 9, 10, 11, and 12 show the orbits for each individual star, using as initial conditions the central values, both in the case of the axisymmetric potential in the inertial Galactic frame of reference (column 1) and the model with bar (columns 2, 3 and 4) in the noninertial frame, where the bar is at rest. For each star, we plotted the projection of the orbit on the Galactic plane (X–Y) and on the meridional plane (R– Z).

Here, we also provide orbital solutions assuming four different values of the angular velocity of the bar $\Omega_{bar}=$ 35, 40, 45, and 50 km s*-1* kpc*-1*, with a bar mass of 1.1$\times 10^{10}$ M*⊙, and a present-day angle orientation of 20∘*, in the same manner as Fernández-Trincado et al. (2019). To model the uncertainty distributions, we sampled a half million orbits using a simple Monte Carlo scheme, assuming a normal distribution for the uncertainties of the input parameters (positions, distance, radial velocity and proper motions). The results are listed in Table 8; the data presented in this table correspond to a backward time integration of 3 Gyr in our dynamical model. Figure 13 shows a scatter plot of all the possible combinations among the orbital elements in the non-axisymmetric potential model. We see that, in each panel, most the stars are grouped in two regions, indicating that they likely belong to the same component. In this case, one group is confined to the bulge/bar, and a second group is apparently moving outwards from the co-rotation (CR) region.

For guidance, the Galactic convention adopted by this study is: $X-$axis is oriented toward $l=$ 0*∘* and $b=$ 0*∘, and the $Y-$axis is oriented toward $l$ = 90∘* and $b=$0*∘, and the disc rotates toward $l=$ 90∘; the velocities are also oriented in these directions. In this convention, the Sun’s orbital velocity vector is [U⊙,V⊙,W⊙] = [$11.1$, $12.24$, 7.25] km s-1* (Brunthaler et al., 2011). The model has been rescaled to the Sun’s Galactocentric distance, 8.3 kpc, and the local rotation velocity of $239$ km s*-1*.

Most of the newly identified N-rich stars are found to have radial and prograde orbits, with pericenter values less than 3 kpc (inside the bulge region), apocenter values ranging between 6.5–58 kpc, orbital eccentricities larger than 0.5, and maximum vertical excursions from the Galactic plane ranging between 0.5–58 kpc. The orbital parameters clearly show that a few these stars live in the inner Galaxy, while most are in the inner halo of the Milky Way. Figure 7 shows the Aitoff project of our objects, which reveals that 6 out of 31 of our stars are located toward the bulge region, 2M17294680$-$2644220, 2M18022601$-$3106232, 2M18110406$-$2602142, 2M18461977$-$3021506, 2M18472793$-$3033242, and 2M18502108$-$2923442; from this group we found that the orbital properties of three of them suggest that they are actually halo interlopers into the inner Galaxy (2M17294680$-$2644220, 2M18461977$-$3021506, and 2M18502108$-$2923442), while the other three stars appear to have bulge/bar-like prograde orbits. It is very likely that such N-rich stars trapped into the bulge/bar potential could be linked to merger debris of surviving globular clusters in bulge/bar-like orbits, such as M 62 (see e.g., Minniti et al., 2018b).

It is also worth mentioning that there are two other N-rich stars, 2M15535831$+$4333280 (SG-like), 2M16362792$+$3901180 (FG-like/dGs), whose orbits are retrograde with respect to the direction of the Galactic rotation. We found that the abundance patterns of these stars, namely the $\alpha-$elements, neutron-capture elements, and the abundance ratios of [Al/Fe], most resemble the known chemical signature of globular cluster stars. The chemistry and dynamical behaviour of this sub-sample of N-rich stars suggests that they could be the debris of dissipated globular clusters, indicating that there may be a significant population of these peculiar abundance giants residing in the Galactic field.

Lastly, 26 out of 31 N-rich stars appear to behave as halo-like orbits, intriguingly in the prograde sense with respect to the rotation of the bar, suggesting that they were likely formed during the very early stages of the evolution of the Galaxy (e.g., Khoperskov et al., 2018), in a similar way as Galactic globular clusters. It is important to note that prograde orbits have been observed before in the inner halo (Bonaca et al., 2017; Fernández-Alvar et al., 2018; Hayes et al., 2018; Lucey et al., 2019), as well as for other globular clusters (Moreno et al., 2014; Pérez-Villegas et al., 2018), however this is not yet well-understood. We also found that most of the simulated orbits are situated in the inner Galaxy, which means that most of the N-rich stars are on highly eccentric orbits (with eccentricities greater than 0.6), reaching out to a maximum distance from the Galactic plane larger than 3 kpc. On the other hand, a handful of the N-rich stars have energies allowing the star to move inwards from the bar’s corotation radius ($<$ 6.5 kpc). In this region, a class of orbits appears around the Lagrange points on the minor axis of the bar that can be stable, and have a banana-like shape parallel to the bar, as illustrated in a few cases in Figure 9 and 10, while the orbits liberating around Lagrange points aligned with the bar are unstable and are probably chaotic orbits. Our model naturally predicts trajectories indicating that most of the N-rich stars are confined to the Galactic halo.

Additionally, in Table 8 and Figure 13 we show the variation of the z-component of the angular momentum ($L_{z}$), as a function of $\Omega_{bar}$. Since this quantity is not conserved in a model like GravPot16 (with non-axisymmetric structures), we follow the change, {$-L_{z}$,$+L_{z}$}, where negative $L_{z}$ in our reference system means that the cluster orbit is prograde (in the same sense as the disk rotation). Both prograde and prograde-retrograde orbits with respect to the direction of the Galactic rotation are clearly revealed for a few cases, this effect is strongly produced by the presence of the Galactic bar, further indicating a chaotic behavior.

A major limitation of the employed dynamical model is that it ignores secular changes in the Milky Way potential over time, which might be important in understanding of the evolution in the inner Galaxy. An in-depth analysis of such dynamical effects is beyond the scope of this paper, however, the adopted technique shown that the inclusion of a more realistic (as far as possible) bar potential is essential for the description of the dynamical behavior of N-rich stars in the innermost part of the Galaxy.

4 Concluding Remarks

We have taken advantage of the fist Payne data release of APOGEE abundances, which determine best-fit stellar parameters and abundances using neural networks as an emulator. We applied a series of quality cuts on the initial Payne catalogue, ensuring the data have sufficiently high-quality spectra needed to estimate chemical abundances for a wide range of chemical species, as well as re-examined line-by-line each APOGEE spectrum with the BACCHUS pipeline. Our study presents an unique collection of 31 newly identified N-rich stars towards the bulge and inner halo of the Milky Way that exhibit anomalously high levels of [N/Fe] over a narrow range of metallicities (-1.5\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}[Fe/H]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle<}}{{\sim}},}-0.7), below the metal-poor tail of the thick-disk metallicity distribution. Based on their [Al/Fe] abundance ratios, we classified them into two groups, the N-/Al-rich giant-stars ([Al/Fe]\raisebox{-2.15277pt}{,\stackrel{{\scriptstyle\textstyle>}}{{\sim}},}+0.5) with chemical signatures similiar to second-generation globular cluster stars, and a second group, the N-rich/Al-normal ([Al/Fe]$<+0.5$) with chemistry similar to the first generation of stars seen in Galactic globular clusters and the population of stars in dwarf galaxies. For many of them, we determined, for the first time the abundances of s-process elements (Ce II and Nd II).

We did not detect any significant variation of their radial velocities that would support the hypothesis of mass transfer, however most of the chemical species examined, along with the high nitrogen abundances could supports the idea that the process responsible for the stars can be qualitatively explained by massive evolved objects, possibly ”early-AGB” or AGB stars. We hypothesise that massive (M$>$ 5 –7 M*⊙*) AGB stars may produce a [N/Fe] over-abundance in some of our N-rich giant stars within the Milky Way. However, more detailed AGB nucleosynthesis models, as well as more observations, will be necessary to confirm or refute the scenario related to AGB stars. Combining our abundance results, orbital analysis, and the absence of radial velocity variations, we conclude that most of the newly identified objects are associated with the bulge/bar structure and the inner Galactic halo, and are likely escaped members of small satellites that were tidally disrupted and captured by the Milky Way.

Acknowledgments

We thank Szabolcs Mészáros for helpful support computing the photometry $T_{\rm eff}$, and especially grateful for the technical expertise and assistance provided by the Instituto de Astrofísica de Canarias (IAC). This article is based upon work from the “ChETEC” COST Action (CA16117), supported by COST (European Cooperation in Science and Technology). J.G.F-T is supported by FONDECYT No. 3180210. J.G.F-T acknowledges the use of TOPCAT (Taylor, 2005) through out the course of this investigation. T.C.B. acknowledge partial support for this work from grant PHY 14-30152; Physics Frontier Center / JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. B.T. acknowledges support from the one-hundred-talent project of Sun Yat-Sen University. S.L-M acknowledges funding from the Australian Research Council through Discovery grant DP180101791, and from the UNSW Scientia Fellowship program. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. A.P-V acknowledges a FAPESP for the postdoctoral fellowship grant no. 2017/15893-1 and the DGAPA-PAPIIT grant IG100319.

BACCHUS have been executed on computers from the Utinam Institute of the Université de Franche-Comté, supported by the Région de Franche-Comté and Institut des Sciences de l’Univers (INSU).

Funding for the GravPot16 software has been provided by the Centre national d’études spatiales (CNES) through grant 0101973 and UTINAM Institute of the Université de Franche-Comté, supported by the Région de Franche-Comté and Institut des Sciences de l’Univers (INSU). Simulations have been executed on computers from the Utinam Institute of the Université de Franche-Comté, supported by the Région de Franche-Comté and Institut des Sciences de l’Univers (INSU), and on the supercomputer facilities of the Mésocentre de calcul de Franche-Comté.

Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS- IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofìsica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Dame, Observatório Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.