X-ray survey of the North-America and Pelican star-forming complex   (NGC7000/IC5070)

Francesco Damiani; Ignazio Pillitteri; and Loredana Prisinzano

arXiv:1702.05999·astro-ph.SR·June 28, 2017

X-ray survey of the North-America and Pelican star-forming complex (NGC7000/IC5070)

Francesco Damiani, Ignazio Pillitteri, and Loredana Prisinzano

PDF

TL;DR

This study provides the first comprehensive X-ray analysis of the North-America and Pelican star-forming complex, identifying and characterizing its young stellar population through multi-wavelength data integration.

Contribution

It offers the first extensive X-ray survey of NGC7000/IC5070, combining data from Chandra and XMM-Newton with optical and IR catalogs to identify young stars and analyze their spatial distribution.

Findings

01

Over 700 X-ray sources detected, most with optical/NIR counterparts.

02

Young stars exhibit a wide range of extinction and sometimes IR excesses.

03

Spatial distribution suggests complex subclustering and possible sequential star formation.

Abstract

We present the first extensive X-ray study of the North-America and Pelican star-forming region (NGC7000/IC5070), with the aim of finding and characterizing its young stellar population. X-ray data from Chandra (four pointings) and XMM-Newton (seven pointings) were reduced and source detection was performed on each image. We complement the X-ray data with optical and near-IR data from the IPHAS, UKIDSS, and 2MASS catalogs, and with other published optical and Spitzer IR data. More than 700 X-ray sources are detected, the majority of which have an optical/NIR counterpart. This allows to identify young stars in different stages of formation. Less than 30% of X-ray sources are identified with a previously known young star. We argue that most X-ray sources with an optical/NIR counterpart, except perhaps for a few tens at near-zero reddening, are likely candidate members of the star-forming…

Figures40

Click any figure to enlarge with its caption.

Tables5

Table 1. Table 1: XMM-Newton observing log. Dates are UT, exposure times t e x p subscript 𝑡 𝑒 𝑥 𝑝 t_{exp} in seconds.

ObsId	RA	Dec	PI	PN start date	PN $t_{e x p}$	MOS start date	MOS $t_{e x p}$
0679580101	312.7004	44.85204	Damiani	2011-11-24,00:13:45	25591	2011-11-23,23:51:28	30239
0679580201	313.2083	44.49669	Damiani	2011-11-24,10:32:48	13750	2011-11-24,09:34:44	19092
0679580301	313.6737	44.04564	Damiani	2011-11-24,18:48:44	23827	2011-11-24,18:26:25	28239
0302640201	314.7238	44.25789	Skinner	2005-11-26,21:12:19	21027	2005-11-26,20:50:00	23733
0556050101	313.4454	44.38394	Motch	2008-05-02,11:27:25	14498	2008-05-02,10:58:53	17392
0656780701	314.5710	43.89539	Schartel	2010-11-25,19:29:52	15968	2010-11-25,19:07:30	18237
0656781201	314.5710	43.89539	Schartel	2011-05-26,12:47:35	17560	2011-05-26,12:25:15	21327

Table 2. Table 2: Chandra observing log. Dates are UT, exposure times t e x p subscript 𝑡 𝑒 𝑥 𝑝 t_{exp} in seconds.

ObsId	RA	Dec	PI	Detector	Start date	$t_{e x p}$
13648	314.2114	43.74551	Damiani	ACIS-I	2011-12-26,20:43:50	44588
13647	312.7507	44.35863	Damiani	ACIS-I	2012-11-20,03:37:14	22766
15592	312.7507	44.35863	Damiani	ACIS-I	2012-11-21,17:52:27	20792
14545	314.5673	43.89382	Guedel	ACIS-S	2013-07-17,06:16:36	29677

Table 3. Table 3: Detected X-ray sources in the NAP. Full table in electronic format only.

X-ray	CXO Id	XMM Id	RA	Dec	Pos. err.	Count rate	Rate error	HR1	HR2	HR1	HR2	$\log L_{X}$
no.	(CXOU)	(XMMU)	(J2000)	(J2000)	(arcsec)	(cts/ksec)	(cts/ksec)	ACIS	ACIS	XMM	XMM	(erg/sec)
1	J205004.0+442249		312.51677	44.38037	1.87	0.428	0.226	0.33	0.60
2	J205006.2+442505		312.52597	44.41824	2.34	2.067	0.322	0.31	-0.06			30.09
3	J205013.5+441910		312.55631	44.31957	2.56	0.402	0.161	0.00	0.88
4	J205017.6+442318		312.57358	44.38850	1.48	0.759	0.239	1.00	0.81
5	J205019.0+442630		312.57958	44.44189	2.45	0.550	0.208	-0.90	0.50
6	J205020.3+442557		312.58466	44.43271	1.73	0.488	0.185	0.45	-0.07			29.99
7	J205021.7+442425		312.59051	44.40696	1.08	1.937	0.264	0.48	-0.07			30.76
8	J205021.8+442101		312.59113	44.35048	1.12	0.192	0.103	-0.20	0.20			29.02
9	J205022.4+441918		312.59365	44.32169	1.08	1.939	0.258	0.53	-0.24			30.39
10	J205022.9+442224		312.59556	44.37350	1.12	0.181	0.123	NaN	1.00			29.79
11	J205024.1+442222		312.60066	44.37301	1.12	0.221	0.128	0.20	0.14			29.71
12	J205025.6+442633		312.60667	44.44274	2.81	0.361	0.163	-0.14	-0.09
13	J205026.3+442606		312.60990	44.43526	1.94	0.413	0.184	0.67	-0.43			29.91
14	J205028.2+442205		312.61784	44.36821	0.83	0.158	0.104	NaN	1.00
15	J205028.8+442301		312.62006	44.38378	0.79	0.177	0.109	-1.00	NaN			28.80
16	J205030.1+441501		312.62557	44.25049	1.40	0.355	0.225	-1.00	1.00
17	J205030.5+442520		312.62709	44.42243	0.86	1.127	0.192	0.90	0.22			31.23
18	J205031.1+442427		312.62987	44.40758	1.15	0.536	0.185	0.33	0.80			30.34
19	J205033.1+441539		312.63798	44.26084	1.69	1.498	0.235	0.30	-0.28			30.19
20	J205035.0+442514		312.64602	44.42077	1.44	0.232	0.109	-1.00	1.00
21	J205035.6+441815		312.64838	44.30433	0.86	0.460	0.169	1.00	0.78
22	J205035.8+442324		312.64924	44.39015	0.54	0.144	0.078	1.00	0.60
23	J205035.8+441819		312.64958	44.30541	0.83	0.153	0.086	1.00	-0.56			30.18
24	J205036.9+442050		312.65413	44.34725	0.50	0.255	0.121	0.56	-0.40			29.40
25	J205037.0+441825		312.65431	44.30700	0.58	5.570	0.415	0.42	-0.30			30.76
26	J205037.3+442053		312.65580	44.34813	0.32	2.800	0.287	0.13	-0.59			30.32
27	J205037.8+441746		312.65766	44.29612	1.26	0.958	0.174	0.75	-0.05
28	J205037.9+442512		312.65823	44.42022	0.47	3.010	0.301	0.61	-0.31			30.77
29	J205038.6+441049		312.66086	44.18029	2.66	0.546	0.259	1.00	0.71			30.36
30	J205039.7+442003		312.66583	44.33426	0.43	0.648	0.241	0.33	-0.82			29.63
31	J205040.4+442022		312.66864	44.33951	0.36	0.632	0.197	0.50	-0.67			29.70
32	J205040.5+442051		312.66897	44.34751	0.36	0.173	0.086	0.00	-0.50			29.30
33	J205041.9+441825		312.67467	44.30722	0.50	2.151	0.265	0.94	0.24			31.58
34	J205042.0+442149		312.67531	44.36379	0.47	0.305	0.128	0.00	-0.25			29.80
35	J205042.8+442156		312.67844	44.36561	0.25	2.231	0.270	0.39	0.34			30.86
36	J205042.9+442204		312.67875	44.36791	0.94	0.250	0.107	-0.11	-0.33			29.08
37	J205042.9+442559		312.67875	44.43319	0.72	0.770	0.229	0.73	-0.36			30.38
38	J205043.5+441552		312.68150	44.26465	1.08	0.670	0.218	0.22	-0.22			29.70
39	J205044.0+442058		312.68356	44.34958	0.40	0.499	0.163	1.00	0.58
40	J205044.4+442535		312.68526	44.42643	0.90	0.146	0.118	-1.00	1.00
41	J205044.5+441540		312.68579	44.26125	1.98	0.311	0.135	0.33	0.64			30.01
42	J205044.8+441718		312.68684	44.28860	0.65	1.161	0.231	0.86	-0.11
43	J205044.9+441554		312.68725	44.26522	0.86	1.605	0.225	0.09	-0.57			30.23
44	J205045.9+442446		312.69138	44.41302	0.47	0.794	0.150	1.00	0.89			31.44
45	J205045.9+442555		312.69160	44.43202	0.61	0.751	0.296	0.67	0.23			30.36
46	J205046.0+441910		312.69201	44.31950	0.36	2.527	0.264	0.03	-0.82			30.27
47	J205046.5+442446		312.69384	44.41304	0.76	0.196	0.103	1.00	0.50
48	J205047.0+441729		312.69588	44.29159	0.47	2.614	0.274	0.33	-0.43			30.31
49	J205047.5+441413		312.69832	44.23716	2.56	0.438	0.192	0.33	0.14			29.67
50	J205047.6+441956		312.69862	44.33233	0.61	0.279	0.107	1.00	0.67
51	J205048.1+442428		312.70079	44.40804	0.61	0.726	0.289	0.67	0.17			30.73
52	J205048.5+441702		312.70228	44.28406	1.08	0.200	0.102	1.00	0.11			28.97
53	J205048.5+442104		312.70243	44.35134	0.47	0.281	0.115	0.60	0.00			29.47
54	J205048.6+442025		312.70252	44.34034	0.32	1.271	0.361	0.31	-0.31			29.91
55	J205048.7+442053		312.70304	44.34820	0.43	0.324	0.121	-0.06	-1.00			29.49
56	J205048.8+441923		312.70334	44.32325	0.22	3.915	0.378	0.26	-0.43			30.55
57	J205048.9+442829		312.70395	44.47478	1.44	0.243	0.142	1.00	0.43
58	J205049.6+442441		312.70689	44.41161	0.40	0.470	0.165	1.00	0.65			31.25
59	J205049.7+442015		312.70727	44.33777	0.25	0.184	0.089	1.00	0.50
60	J205050.2+442433		312.70943	44.40926	0.54	0.531	0.171	1.00	0.33
61	J205050.2+442421		312.70957	44.40602	0.22	4.242	0.464	0.79	0.17			31.42
62	J205050.5+442507		312.71061	44.41864	0.58	0.457	0.155	1.00	-0.10			30.82
63	J205050.7+441725		312.71157	44.29053	0.61	0.142	0.113	NaN	1.00
64	J205050.8+441852		312.71186	44.31447	0.65	0.295	0.118	1.00	0.56
65	J205051.3+442518		312.71407	44.42190	0.43	0.984	0.172	1.00	0.30			30.90
66	J205051.7+442539		312.71577	44.42767	0.43	0.421	0.173	1.00	0.07			30.14
67	J205051.9+442441		312.71660	44.41155	0.40	0.457	0.162	1.00	0.47			31.29
68	J205052.4+442342		312.71839	44.39517	0.32	0.104	0.078	-1.00	NaN
69	J205052.6+441645		312.71920	44.27919	0.76	2.193	0.268	0.18	-0.32			30.22
70	J205053.1+442353		312.72157	44.39825	0.54	0.167	0.084	0.00	-0.50			29.21
71	J205053.2+442450		312.72178	44.41394	0.43	0.314	0.120	NaN	1.00
72	J205053.3+442414		312.72228	44.40415	0.72	0.174	0.083	NaN	1.00
73	J205053.4+442435		312.72264	44.40995	0.54	0.527	0.173	0.33	0.20			30.19
74	J205053.4+442427		312.72279	44.40761	0.43	0.334	0.129	0.75	-0.17			29.89
75	J205053.5+442101		312.72327	44.35035	0.22	4.207	0.515	0.30	-0.30			30.42
76	J205053.6+442430		312.72357	44.40854	0.40	0.487	0.158	1.00	-0.24			30.16
77	J205053.7+442118		312.72381	44.35522	0.25	1.726	0.218	0.39	-0.68
78	J205053.9+442118		312.72484	44.35522	0.25	0.696	0.229	0.04	-0.62
79	J205054.8+441758		312.72859	44.29947	0.32	0.126	0.101	-1.00	NaN
80	J205054.8+442013		312.72861	44.33697	0.40	0.476	0.166	0.80	-0.12			29.45
81	J205054.8+442258		312.72874	44.38300	0.47	0.223	0.098	NaN	1.00			29.43
82	J205055.4+441746		312.73107	44.29634	0.40	0.452	0.159	0.22	-0.57			29.49
83	J205055.6+441750		312.73198	44.29732	0.47	3.098	0.289	0.18	-0.43			30.48
84	J205055.7+442144		312.73213	44.36239	0.25	0.670	0.309	0.60	0.00			29.61
85	J205055.7+441828		312.73229	44.30800	0.54	0.520	0.170	-0.05	-0.82			29.60
86	J205055.8+442420		312.73263	44.40570	0.54	0.151	0.075	1.00	0.67
87	J205056.2+441926		312.73446	44.32396	0.25	2.807	0.293	-0.36	-0.85			30.00
88	J205056.6+441706		312.73619	44.28501	0.47	0.257	0.129	-0.14	-0.50			29.24
89	J205056.8+442527		312.73682	44.42440	0.68	0.245	0.107	NaN	1.00
90	J205057.0+441643		312.73757	44.27863	0.79	0.162	0.089	-0.14	-0.50			29.02
91	J205057.3+442450		312.73901	44.41401	0.32	0.995	0.164	0.41	-0.09			30.33
92	J205057.4+442445		312.73951	44.41275	0.29	4.768	0.353	0.67	-0.15
93	J205057.7+442138		312.74082	44.36083	0.58	0.144	0.079	0.33	0.20			29.09
94	J205057.9+442309		312.74162	44.38611	0.43	0.357	0.131	1.00	0.27			29.85
95	J205058.0+442959		312.74195	44.49976	1.48	2.542	0.313	0.15	-0.30			30.20
96	J205058.3+441432		312.74324	44.24237	1.12	1.924	0.304	0.25	-0.48			29.96
97	J205058.4+441444		312.74365	44.24582	1.08	1.990	0.278	0.11	-0.50			30.16
98	J205058.5+441221		312.74407	44.20597	2.02	0.360	0.224	-1.00	1.00			29.95
99	J205058.7+441731		312.74467	44.29202	0.36	7.317	0.473	0.61	-0.02			30.78
100	J205058.7+442317		312.74478	44.38828	0.29	0.517	0.177	0.00	-0.38			29.74
101	J205059.4+441728		312.74769	44.29138	0.61	0.141	0.086	-0.33	-1.00			28.70
102	J205059.4+441939		312.74788	44.32768	0.61	0.680	0.261	0.56	-0.75			29.87
103	J205059.6+443015		312.74834	44.50444	1.48	1.149	0.370	0.72	-0.56			30.09
104	J205100.2+442141		312.75097	44.36162	0.36	0.355	0.173	1.00	0.80
105	J205100.3+442436		312.75127	44.41020	0.29	1.169	0.180	0.15	-0.68			29.88
106	J205101.4+441331		312.75594	44.22531	3.35	1.615	0.277	0.26	0.11			30.07
107	J205101.4+442504		312.75613	44.41782	0.54	0.561	0.182	1.00	0.29
108	J205101.4+441534		312.75615	44.25963	0.61	0.413	0.161	0.33	-0.60			29.50
109	J205101.5+441542		312.75654	44.26177	0.50	3.359	0.385	0.44	-0.22			30.47
110	J205102.1+442009		312.75905	44.33601	0.36	0.629	0.197	0.25	-0.67			29.61
111	J205102.3+442009		312.75993	44.33597	0.29	0.110	0.067	0.00	-0.33			28.74
112	J205102.5+442743		312.76053	44.46211	1.04	0.239	0.126	0.25	-1.00			28.93
113	J205102.8+442822		312.76207	44.47302	0.97	0.318	0.166	1.00	0.33
114	J205103.0+442403		312.76291	44.40087	0.22	4.505	0.361	0.84	0.09			30.53
115	J205103.3+442415		312.76388	44.40439	0.25	2.553	0.301	0.69	-0.14			30.41
116	J205103.3+441310		312.76412	44.21966	1.40	0.330	0.151	0.00	-0.14			29.07
117	J205103.8+442720		312.76623	44.45574	0.97	0.292	0.129	1.00	0.80
118	J205104.4+442919		312.76867	44.48867	1.76	0.522	0.200	0.27	-0.27			29.51
119	J205104.5+442351		312.76884	44.39751	0.47	0.135	0.085	0.33	-0.14			29.28
120	J205104.6+442350		312.76936	44.39731	0.36	0.635	0.201	0.44	-0.24			29.95
121	J205105.3+441522		312.77246	44.25636	1.37	1.119	0.316	0.45	0.57			30.43
122	J205105.7+441358		312.77376	44.23287	3.17	0.689	0.232	0.39	-0.39			29.83
123	J205105.7+441632		312.77378	44.27577	0.61	1.694	0.274	0.40	-0.42			30.25
124	J205106.1+441758		312.77543	44.29946	0.68	0.830	0.157	-0.45	-0.64			29.47
125	J205106.6+442141		312.77768	44.36141	0.25	1.742	0.207	0.01	-0.71			29.89
126	J205107.0+442103		312.77932	44.35088	0.86	0.339	0.129	1.00	0.27
127	J205108.5+442433		312.78563	44.40929	0.47	0.822	0.156	-0.08	-0.16			29.67
128	J205108.9+441642		312.78739	44.27847	0.61	1.284	0.210	0.29	0.00			29.91
129	J205109.0+442315		312.78762	44.38760	0.61	0.123	0.072	0.50	-1.00			29.03
130	J205109.3+442248		312.78894	44.38018	0.76	0.174	0.087	0.00	0.00			28.79
131	J205110.6+442618		312.79433	44.43843	2.48	0.399	0.155	0.20	0.50			29.62
132	J205112.4+441943		312.80181	44.32878	0.47	0.238	0.104	0.50	-1.00			29.14
133	J205112.5+441809		312.80238	44.30272	1.12	0.493	0.163	0.07	-0.45			29.48
134	J205112.6+441845		312.80259	44.31273	0.36	7.343	0.455	0.13	-0.50			30.49
135	J205113.4+442448		312.80600	44.41335	0.50	0.285	0.133	1.00	0.60
136	J205113.7+442225		312.80733	44.37372	0.58	0.876	0.310	-0.71	0.00			29.66
137	J205113.9+441814		312.80802	44.30402	0.58	0.187	0.125	1.00	0.67
138	J205114.7+442746		312.81154	44.46285	1.26	0.420	0.174	0.71	0.08			29.71
139	J205114.9+442125		312.81233	44.35707	1.80	0.329	0.131	-0.33	0.56			29.32
140	J205115.1+441818		312.81313	44.30505	0.68	1.029	0.286	0.35	-0.62			29.88
141	J205115.7+442950		312.81548	44.49739	1.66	0.724	0.275	0.07	0.00			29.41
142	J205115.7+441457		312.81567	44.24929	1.69	1.635	0.409	0.60	-0.24			30.14
143	J205116.4+442258		312.81873	44.38292	0.40	1.559	0.220	0.20	-0.89			29.95
144	J205117.4+441914		312.82282	44.32071	0.86	0.376	0.143	0.08	-0.75			29.39
145	J205117.7+441829		312.82375	44.30826	0.58	0.162	0.094	1.00	-0.33			29.17
146	J205118.6+442454		312.82791	44.41510	0.61	0.146	0.117	NaN	1.00			29.50
147	J205119.4+441931		312.83097	44.32536	0.61	0.358	0.131	0.56	-0.40			29.57
148	J205120.4+442035		312.83529	44.34321	0.36	0.113	0.104	0.50	-1.00
149	J205120.5+442032		312.83581	44.34245	0.32	3.245	0.326	0.28	-0.46			30.32
150	J205120.9+442619		312.83746	44.43887	0.65	3.421	0.334	0.40	-0.41			30.37
151	J205121.3+442405		312.83915	44.40162	0.47	3.327	0.314	0.16	-0.70			30.08
152	J205122.6+442108		312.84445	44.35224	0.50	2.623	0.285	0.44	-0.20			30.41
153	J205122.9+442326		312.84573	44.39078	0.83	0.188	0.104	NaN	1.00
154	J205123.6+441542		312.84838	44.26186	0.83	0.606	0.221	0.33	-0.50			29.79
155	J205124.0+442024		312.85012	44.34014	0.72	0.228	0.109	1.00	0.25			29.49
156	J205124.1+441757		312.85050	44.29917	1.12	0.644	0.215	0.55	-0.48			29.92
157	J205124.7+441755		312.85298	44.29875	0.76	0.245	0.137	0.14	-1.00			29.25
158	J205124.7+441820		312.85303	44.30556	1.01	0.801	0.157	0.31	-0.48			29.93
159	J205126.0+442439		312.85853	44.41105	1.01	0.844	0.258	1.00	0.62
160	J205127.3+441958		312.86414	44.33286	0.83	0.186	0.126	-0.50	-1.00
161	J205127.7+442541		312.86550	44.42833	1.30	0.443	0.176	1.00	0.38			29.90
162	J205128.5+442601		312.86878	44.43374	1.48	0.931	0.286	0.62	-0.26			30.24
163	J205128.5+441545		312.86906	44.26252	1.87	1.349	0.371	0.26	-0.22			30.01
164	J205128.9+441507		312.87066	44.25208	1.44	0.273	0.147	0.33	0.33			29.60
165	J205129.4+442437		312.87270	44.41046	1.66	0.471	0.166	0.71	0.33			29.33
166	J205129.4+442202		312.87288	44.36742	1.01	0.257	0.118	1.00	-0.33			29.74
167	J205131.5+442543		312.88156	44.42869	2.09	0.842	0.261	0.33	0.70			29.96
168	J205133.2+442423		312.88853	44.40662	1.44	0.275	0.127	1.00	0.27			29.61
169	J205133.4+442637	J205133.2+442636	312.88925	44.44376	1.58	1.893	0.292	0.21	-0.13	0.43	-0.37	30.26
170	J205137.6+442005		312.90673	44.33487	0.83	0.586	0.219	0.12	-0.64			29.62
171	J205138.2+441707		312.90936	44.28548	1.48	0.278	0.160	0.33	0.20
172	J205139.1+442429	J205139.2+442425	312.91318	44.40810	1.98	2.038	0.597	0.44	-0.44	0.03	-0.50	30.15
173	J205141.8+441607		312.92445	44.26875	1.98	1.191	0.349	0.58	-0.19			29.90
174	J205145.4+441606		312.93934	44.26861	2.12	0.360	0.265	0.00	0.67			29.46
175	J205145.9+441917		312.94137	44.32144	3.20	0.773	0.266	0.33	0.56			30.68
176	J205547.0+434216		313.94598	43.70464	2.48	0.584	0.226	0.16	-0.38			29.32
177	J205558.5+434557		313.99378	43.76610	2.56	0.654	0.246	0.60	0.62
178	J205559.5+434532		313.99818	43.75911	1.51	2.390	0.312	-0.33	-0.50			29.93
179	J205559.9+434030		313.99968	43.67509	3.20	0.738	0.251	0.33	0.53			30.44
180	J205603.8+434033		314.01593	43.67594	1.15	6.858	0.530	-0.07	-0.56			30.39
181	J205603.8+434448		314.01591	43.74679	1.84	1.151	0.229	0.73	0.58
182	J205606.0+434628		314.02520	43.77449	1.76	0.476	0.187	0.50	-0.20			29.78
183	J205612.6+434531		314.05253	43.75880	1.30	1.209	0.207	0.71	-0.07			30.31
184	J205613.0+434109		314.05434	43.68609	1.22	0.417	0.164	0.00	0.76
185	J205613.5+434120		314.05633	43.68894	1.44	0.294	0.150	0.00	0.64
186	J205614.6+434528		314.06089	43.75794	0.97	0.246	0.112	-0.56	-1.00			29.44
187	J205616.5+434630		314.06881	43.77508	1.12	0.193	0.120	-1.00	1.00
188	J205616.7+434142		314.06982	43.69525	1.12	0.216	0.121	1.00	0.11			29.71
189	J205618.0+434812		314.07533	43.80334	0.90	2.649	0.510	0.75	-0.40
190	J205618.8+433908		314.07842	43.65234	1.30	4.114	0.406	1.00	0.36			31.19
191	J205619.1+434743		314.07963	43.79537	1.40	0.254	0.115	-1.00	1.00
192	J205619.5+434539		314.08163	43.76084	0.65	1.007	0.278	0.39	-0.64			30.23
193	J205622.1+434031		314.09218	43.67536	0.94	0.281	0.131	1.00	0.80
194	J205622.3+435007		314.09296	43.83540	1.44	0.263	0.134	1.00	-0.27			30.12
195	J205622.7+434328		314.09496	43.72463	0.58	1.244	0.179	0.92	0.13			30.71
196	J205624.4+434757		314.10192	43.79925	0.86	0.154	0.129	-0.33	0.00
197	J205626.2+434051		314.10938	43.68107	0.65	0.304	0.130	1.00	0.82
198	J205626.2+434330		314.10956	43.72526	0.61	0.142	0.101	-0.33	0.00			28.73
199	J205626.3+434325		314.10986	43.72366	0.61	0.151	0.108	-1.00	1.00
200	J205627.2+434558		314.11337	43.76626	0.47	0.971	0.155	0.55	-0.60			30.31
201	J205627.7+434536		314.11544	43.76002	0.54	0.482	0.158	0.50	-0.12			30.18
202	J205628.4+433859		314.11859	43.64986	2.59	0.732	0.286	0.60	0.62
203	J205629.4+434705		314.12290	43.78483	0.58	0.149	0.086	1.00	0.33
204	J205629.9+434253		314.12491	43.71485	0.86	0.405	0.151	1.00	0.22			30.45
205	J205629.9+435106		314.12492	43.85184	1.44	2.640	0.312	0.49	-0.18			30.47
206	J205631.0+434921		314.12930	43.82257	0.83	0.173	0.105	1.00	0.71
207	J205631.4+434447		314.13117	43.74647	0.32	0.861	0.159	1.00	-0.22			30.53
208	J205632.5+434808		314.13570	43.80225	0.58	0.170	0.121	-1.00	1.00			29.21
209	J205633.9+434755		314.14139	43.79867	1.01	0.214	0.104	-0.20	0.33			29.28
210	J205635.4+434240		314.14763	43.71138	0.40	0.138	0.076	-1.00	1.00
211	J205635.7+435313		314.14906	43.88721	1.80	0.478	0.221	0.00	0.83			30.49
212	J205636.0+434821		314.15003	43.80610	0.58	0.146	0.099	0.00	0.33
213	J205636.2+435005		314.15104	43.83473	1.22	0.448	0.167	0.00	0.09			29.79
214	J205636.9+434822		314.15377	43.80617	0.47	0.778	0.147	1.00	0.14
215	J205638.0+435133		314.15874	43.85937	0.94	3.558	0.344	0.77	0.45
216	J205638.5+434843		314.16069	43.81218	0.76	0.169	0.086	-0.50	0.00			28.78
217	J205639.1+434723		314.16328	43.78998	0.36	0.117	0.091	1.00	0.67
218	J205639.6+434840		314.16505	43.81115	0.76	0.187	0.095	0.00	0.67
219	J205640.5+433826		314.16902	43.64067	1.51	0.686	0.216	0.00	0.85
220	J205641.7+434718		314.17410	43.78850	0.47	0.273	0.113	0.25	0.00			29.76
221	J205642.2+435426		314.17585	43.90738	2.95	1.142	0.354	0.33	0.16			29.67
222	J205643.0+434935		314.17940	43.82645	0.72	0.251	0.136	1.00	0.50
223	J205643.7+434845		314.18219	43.81250	0.72	0.232	0.108	NaN	1.00
224	J205643.9+434607		314.18301	43.76863	0.40	0.152	0.088	1.00	0.60
225	J205643.9+434600		314.18332	43.76680	0.22	1.182	0.177	-0.19	-0.78			29.77
226	J205644.0+434945		314.18344	43.82937	0.72	0.776	0.238	0.70	-0.48			30.12
227	J205645.7+434147		314.19048	43.69665	0.58	0.131	0.073	1.00	0.67
228	J205645.7+434240		314.19077	43.71115	0.32	0.125	0.105	-1.00	NaN
229	J205646.4+434518		314.19368	43.75513	0.36	0.625	0.192	-1.00	1.00
230	J205646.6+434602		314.19443	43.76734	0.22	4.626	0.337	0.18	-0.61			30.44
231	J205646.7+434609		314.19475	43.76927	0.18	2.620	0.262	0.10	-0.58			30.39
232	J205647.0+434929		314.19607	43.82484	0.47	0.385	0.185	0.50	-0.50			29.64
233	J205647.0+435022		314.19614	43.83952	0.94	0.295	0.126	0.50	0.45			29.80
234	J205647.4+435143		314.19758	43.86207	1.30	0.356	0.151	1.00	0.38
235	J205647.8+434847		314.19944	43.81309	0.61	0.146	0.118	1.00	0.33
236	J205648.2+435355		314.20085	43.89882	2.02	0.433	0.230	-1.00	1.00
237	J205648.5+434852		314.20236	43.81455	0.61	0.136	0.107	-1.00	1.00
238	J205648.7+434707		314.20306	43.78530	0.32	0.140	0.120	-1.00	NaN
239	J205648.8+434640		314.20358	43.77778	0.22	4.689	0.366	0.72	-0.28			31.12
240	J205648.9+434722		314.20413	43.78949	0.43	0.323	0.123	-1.00	1.00			29.06
241	J205649.4+434528		314.20588	43.75804	0.97	0.263	0.113	0.00	0.75
242	J205649.6+434933		314.20702	43.82607	0.76	0.720	0.224	0.78	0.33			30.67
243	J205650.4+434610		314.21031	43.76954	0.32	0.129	0.102	-0.33	-1.00
244	J205651.1+434705		314.21309	43.78474	0.32	0.236	0.104	NaN	1.00
245	J205651.3+434655		314.21396	43.78212	0.32	0.111	0.085	-1.00	1.00
246	J205651.3+434632		314.21405	43.77558	0.40	0.487	0.170	0.67	0.41
247	J205651.5+434224		314.21470	43.70689	0.47	0.646	0.124	-1.00	1.00
248	J205651.6+434252		314.21537	43.71459	0.29	1.248	0.181	-0.28	-0.89			29.65
249	J205651.9+433333		314.21659	43.55931	3.28	2.226	0.361	0.43	0.62
250	J205652.0+434240		314.21676	43.71119	0.29	0.124	0.079	-1.00	1.00
251	J205652.0+434434		314.21682	43.74285	0.32	0.152	0.125	1.00	-1.00
252	J205652.5+434955		314.21887	43.83201	1.76	0.345	0.133	0.56	-0.08			30.44
253	J205652.5+434646		314.21911	43.77964	0.40	0.157	0.086	0.20	-0.20
254	J205652.9+434643		314.22043	43.77865	1.04	0.208	0.099	0.50	0.33
255	J205653.7+434804		314.22407	43.80115	0.29	0.159	0.104	NaN	1.00
256	J205653.7+433749		314.22411	43.63041	0.97	3.493	0.351	0.89	0.48
257	J205654.2+434356		314.22595	43.73249	0.32	0.124	0.106	1.00	0.00
258	J205654.8+434605		314.22857	43.76831	0.29	0.124	0.079	-1.00	1.00			28.66
259	J205654.9+434856		314.22908	43.81558	0.65	0.345	0.140	0.78	-0.45			30.40
260	J205655.1+435135		314.22995	43.85988	1.48	0.860	0.271	0.60	0.47
261	J205655.3+434028		314.23072	43.67451	0.68	0.291	0.124	NaN	1.00
262	J205656.1+434748		314.23406	43.79688	0.32	0.926	0.185	1.00	0.44
263	J205656.2+434637		314.23436	43.77705	0.32	0.829	0.236	1.00	0.86
264	J205656.4+434313		314.23517	43.72048	0.47	0.488	0.208	1.00	0.43
265	J205656.5+434248		314.23556	43.71359	0.25	6.008	0.840	1.00	0.99
266	J205656.6+434910		314.23585	43.81948	0.47	0.814	0.162	0.66	-0.41			30.09
267	J205657.0+434812		314.23756	43.80359	0.47	0.927	0.260	0.33	0.75
268	J205657.6+434339		314.24029	43.72761	0.32	0.103	0.077	1.00	-1.00
269	J205658.2+434917		314.24271	43.82148	0.47	2.781	0.284	0.73	0.22			30.96
270	J205658.2+433955		314.24273	43.66541	0.86	0.337	0.126	-1.00	1.00
271	J205658.8+434016		314.24514	43.67128	0.79	0.487	0.166	-0.33	-0.43			29.24
272	J205659.0+435023		314.24620	43.83978	0.79	0.207	0.158	-1.00	1.00
273	J205659.3+434753		314.24717	43.79816	0.43	0.341	0.135	-0.27	-0.33			29.23
274	J205659.5+434637		314.24816	43.77698	0.29	2.397	0.412	0.93	0.02			31.33
275	J205700.3+435028		314.25145	43.84112	0.83	0.541	0.196	1.00	0.45
276	J205700.3+434207		314.25166	43.70216	0.43	0.376	0.148	0.71	0.08			30.16
277	J205701.2+433822		314.25529	43.63971	1.44	0.255	0.121	-0.60	0.71
278	J205701.5+434325		314.25664	43.72380	0.18	7.161	0.570	0.92	0.42
279	J205701.6+434139		314.25669	43.69430	0.40	0.138	0.078	-0.20	-1.00			28.93
280	J205701.7+434738		314.25736	43.79400	0.54	0.875	0.279	1.00	0.71
281	J205702.2+434826		314.25932	43.80747	0.58	1.372	0.204	0.83	0.32
282	J205703.3+434144		314.26380	43.69578	0.40	0.576	0.196	0.75	0.22			30.08
283	J205703.5+434500		314.26487	43.75001	0.25	0.712	0.213	0.64	0.28			30.78
284	J205704.3+434840		314.26823	43.81124	0.72	0.671	0.208	1.00	0.31
285	J205704.4+434853		314.26862	43.81476	0.90	0.974	0.175	0.88	0.30			31.09
286	J205704.7+434411		314.26997	43.73646	0.50	0.178	0.085	1.00	0.71
287	J205704.9+434700		314.27070	43.78346	0.54	0.199	0.097	1.00	0.50
288	J205705.5+434045		314.27303	43.67919	0.54	6.294	0.436	1.00	0.89
289	J205705.8+434910		314.27436	43.81960	1.15	1.355	0.220	0.80	-0.25			30.66
290	J205706.3+434229		314.27643	43.70823	1.01	0.186	0.087	0.60	-0.33			30.83
291	J205706.9+434924		314.27894	43.82351	1.73	0.434	0.165	1.00	-0.06			30.07
292	J205707.0+434752		314.27948	43.79799	1.01	0.234	0.107	NaN	1.00
293	J205707.2+435007	J205707.1+435004	314.28036	43.83544	0.90	3.731	0.357	-0.35	-0.66	-0.70	0.02	30.13
294	J205707.4+434242		314.28120	43.71176	0.86	0.373	0.137	0.71	0.37			30.49
295	J205707.5+434159		314.28149	43.69997	0.65	0.932	0.254	-0.35	-0.50			29.95
296	J205708.4+434819	J205708.4+434816	314.28526	43.80548	0.61	4.190	0.359	0.96	0.53	0.22	0.29
297	J205710.9+434251		314.29559	43.71436	0.58	0.139	0.087	-1.00	1.00
298	J205710.9+433805		314.29557	43.63482	1.40	0.284	0.151	-0.20	0.33			30.28
299	J205711.6+434804		314.29860	43.80123	0.94	0.849	0.166	1.00	0.43			31.53
300	J205712.1+434615		314.30061	43.77090	0.61	0.154	0.131	-1.00	NaN
301	J205712.8+434912	J205712.6+434909	314.30334	43.82012	1.01	0.822	0.244	1.00	0.10	0.17	0.20	30.78
302	J205713.0+434718		314.30441	43.78859	2.20	0.645	0.213	0.08	0.52
303	J205713.8+433947		314.30756	43.66324	1.22	0.480	0.181	1.00	0.05			30.52
304	J205713.9+434808		314.30824	43.80249	0.94	0.291	0.123	0.56	-0.27			30.16
305	J205714.8+434537		314.31199	43.76041	0.86	0.377	0.142	0.83	-0.29			30.10
306	J205715.7+434722	J205715.5+434719	314.31549	43.78968	1.08	1.768	0.245	-0.33	0.97	-0.12	0.60
307	J205716.3+434200		314.31829	43.70016	0.86	0.177	0.151	NaN	1.00
308	J205717.5+434829		314.32323	43.80816	0.86	0.447	0.180	0.82	-0.18
309	J205718.5+434719	J205718.3+434714	314.32711	43.78870	0.86	1.321	0.215	0.80	0.00	0.38	0.11	31.19
310	J205718.6+434726	J205718.3+434714	314.32755	43.79057	1.15	0.573	0.200	0.75	-0.27	0.38	0.11	30.45
311	J205719.0+434854		314.32957	43.81512	1.73	0.466	0.173	0.45	-0.07			30.52
312	J205719.1+434931	J205719.1+434930	314.32985	43.82546	2.05	0.880	0.269	0.33	-0.29	0.27	0.07	30.26
313	J205721.4+434400		314.33941	43.73359	1.08	0.196	0.100	1.00	0.71
314	J205724.2+434103		314.35114	43.68431	1.94	0.981	0.280	0.88	0.23			30.97
315	J205725.1+434209		314.35482	43.70264	1.37	2.896	0.325	0.84	0.25			31.34
316	J205726.1+434235		314.35913	43.70999	1.04	0.211	0.105	1.00	0.78
317	J205727.6+435625	J205727.6+435622	314.36516	43.94040	3.17	3.097	0.462	-0.44	-0.26	-0.58	0.16	30.05
318	J205731.6+435956		314.38198	43.99893	1.98	0.646	0.326	0.00	0.00			30.16
319	J205742.5+435449	J205742.3+435447	314.42724	43.91371	1.19	3.195	0.444	0.88	0.57	0.27	0.38
320	J205743.9+435857		314.43299	43.98268	2.34	2.968	0.480	0.64	0.76			30.88
321	J205744.1+435355	J205744.0+435352	314.43402	43.89869	1.58	3.266	0.455	1.00	0.76	0.39	0.49
322	J205751.1+435232	J205750.7+435231	314.46299	43.87558	0.61	0.226	0.181	NaN	1.00	-0.10	0.49
323	J205751.9+435252		314.46647	43.88124	0.83	0.228	0.126	1.00	0.50
324	J205754.1+435326		314.47549	43.89061	0.36	0.170	0.171	NaN	1.00
325	J205756.4+435235	J205756.4+435233	314.48539	43.87663	0.50	3.651	0.459	-0.06	-0.55	-0.48	0.17	30.12
326	J205757.7+435837		314.49065	43.97709	1.98	0.617	0.277	1.00	0.50			29.82
327	J205759.8+435326	J205759.7+435324	314.49924	43.89058	0.61	1.987	0.335	0.50	-0.11	-0.10	0.04	30.29
328	J205801.6+435848		314.50685	43.98005	1.76	2.455	0.463	0.49	-0.30			30.46
329	J205801.6+435349		314.50703	43.89699	0.32	0.186	0.176	1.00	-0.33
330	J205801.8+435349		314.50784	43.89700	0.40	0.855	0.284	1.00	0.04			30.75
331	J205809.3+435632		314.53899	43.94236	0.32	0.212	0.162	-1.00	NaN
332	J205806.1+435300	J205805.9+435259	314.52547	43.88360	0.25	2.756	0.331	-0.09	-0.57	-0.14	-0.17	30.23
333	J205810.8+435308	J205810.6+435306	314.54506	43.88563	0.25	1.083	0.214	-0.31	-0.33	-0.22	-0.22	30.01
334	J205814.2+435304		314.55944	43.88458	0.40	0.252	0.133	0.00	-1.00			29.24
335	J205816.2+435334		314.56767	43.89304	0.36	0.336	0.159	0.71	-0.33
336	J205816.3+435320	J205816.4+435322	314.56819	43.88908	0.22	0.556	0.237	1.00	-0.09	0.23	0.11
337	J205816.7+435335		314.56987	43.89320	0.43	0.523	0.197	0.50	-0.20			30.92
338	J205817.0+435343		314.57091	43.89534	0.22	0.547	0.217	1.00	0.87			29.80
339	J205817.0+435315	J205816.4+435322	314.57117	43.88776	0.14	2.311	0.317	0.86	-0.49	0.23	0.11
340	J205817.1+435336		314.57127	43.89335	0.40	0.276	0.154	0.14	-0.60			29.29
341	J205817.9+435344	J205818.6+435345	314.57461	43.89557	0.22	1.274	0.230	0.63	-0.10	0.07	0.05	30.39
342	J205818.3+435323		314.57656	43.88983	0.22	1.309	0.235	1.00	0.22
343	J205818.8+435354	J205818.6+435345	314.57837	43.89846	0.29	0.271	0.151	0.67	-0.67	0.07	0.05	29.44
344	J205819.0+435244		314.57957	43.87894	0.22	0.502	0.211	1.00	0.85
345	J205819.5+435344	J205818.6+435345	314.58127	43.89571	0.22	0.738	0.293	0.17	-0.27	0.07	0.05
346	J205819.5+435354		314.58144	43.89846	0.29	0.206	0.129	0.00	-1.00			29.42
347	J205819.5+435400		314.58157	43.90006	0.29	0.179	0.113	0.00	0.33			29.03
348	J205821.5+435344		314.58977	43.89578	0.29	0.702	0.237	1.00	0.29			30.02
349	J205821.7+435330		314.59042	43.89184	0.25	0.260	0.149	0.20	-0.50			29.71
350	J205823.2+435258	J205823.2+435301	314.59701	43.88300	0.14	5.072	0.450	0.11	-0.66	-0.13	-0.19	30.63
351	J205823.3+435253	J205823.2+435301	314.59714	43.88165	0.50	0.305	0.144	1.00	0.33	-0.13	-0.19
352	J205823.3+434915	J205823.0+434913	314.59733	43.82093	1.08	0.250	0.125	-0.50	0.50	0.39	0.36	30.22
353	J205823.6+435255	J205823.2+435301	314.59848	43.88207	0.22	1.429	0.251	-0.22	-0.80	-0.13	-0.19
354	J205823.7+435256	J205823.2+435301	314.59909	43.88243	0.36	0.309	0.149	0.11	-0.43	-0.13	-0.19
355	J205823.7+435311		314.59915	43.88649	0.18	4.116	0.413	0.16	-0.48			30.63
356	J205823.8+435447		314.59922	43.91316	0.32	0.169	0.127	-1.00	1.00
357	J205823.9+435354	J205823.8+435353	314.59999	43.89848	0.14	9.721	0.617	0.37	-0.41	-0.27	-0.04	30.98
358	J205824.9+434851		314.60400	43.81417	0.79	0.211	0.127	0.00	0.50
359	J205825.4+434834		314.60611	43.80951	0.83	0.220	0.153	1.00	0.50
360	J205825.5+435328	J205825.4+435327	314.60640	43.89129	0.25	2.329	0.303	0.33	-0.41	-0.01	-0.15	30.50
361	J205825.7+435216		314.60720	43.87114	0.32	0.158	0.134	1.00	0.33
362	J205827.0+435320		314.61257	43.88890	0.18	3.689	0.398	0.55	-0.39			30.53
363	J205827.0+435110		314.61289	43.85291	0.40	0.245	0.144	1.00	0.75
364	J205828.6+434855		314.61939	43.81533	1.19	0.564	0.202	0.75	0.12			30.65
365	J205830.3+435359		314.62663	43.89978	0.25	0.328	0.150	0.33	-0.71			29.59
366	J205830.5+435408		314.62716	43.90249	0.32	0.159	0.124	0.50	-1.00			29.11
367	J205832.3+435617		314.63481	43.93828	1.33	0.335	0.151	-0.50	0.71			29.83
368	J205840.6+435303		314.66925	43.88426	0.54	0.240	0.140	-0.33	0.50			29.80
369	J205842.2+434926		314.67598	43.82397	2.41	0.554	0.206	0.00	-0.29			29.30
370	J205842.9+435451		314.67885	43.91431	0.90	0.494	0.200	0.60	0.60
371	J205844.5+435358		314.68556	43.89960	0.68	0.437	0.218	1.00	0.00
372	J205846.9+435151	J205846.6+435153	314.69554	43.86436	1.04	2.896	0.370	1.00	0.63	-0.18	0.34	31.24
373	J205847.7+435141	J205847.5+435141	314.69898	43.86147	1.15	2.104	0.323	-0.53	-0.62	-0.41	0.21	29.88
374	J205848.9+435316	J205848.7+435315	314.70416	43.88791	0.83	0.619	0.222	-0.29	-0.20	-0.04	0.15	29.75
375	J205849.1+435035		314.70477	43.84325	2.16	0.961	0.309	0.56	0.24
376	J205849.8+435204		314.70783	43.86799	1.40	1.140	0.332	0.24	0.04
377	J205852.6+435451	J205852.3+435448	314.71944	43.91439	2.81	1.315	0.387	-0.52	0.26	-0.60	0.24
378	J205853.3+435400	J205853.2+435358	314.72223	43.90019	1.55	2.502	0.356	0.62	0.00	0.21	-0.05	30.43
379		J205855.4+440336	314.73100	44.06010	1.22	230.150	5.214			-0.79	-0.69	31.29
380		J205835.7+440512	314.64882	44.08682	3.67	5.312	1.024			-0.08	0.23	29.91
381		J205932.7+440550	314.88627	44.09747	5.44	10.522	2.225			0.17	0.04	30.83
382		J205900.8+440710	314.75364	44.11951	1.80	117.830	5.745			0.51	0.23	31.14
383		J205901.4+440740	314.75620	44.12795	2.63	5.762	1.128			-0.35	-0.14	29.69
384		J205943.3+440748	314.93043	44.13002	3.78	6.522	1.333			-0.58	0.32	29.74
385		J205813.7+440800	314.55729	44.13334	2.66	3.907	0.807			0.19	0.30	30.08
386		J205932.7+440834	314.88643	44.14278	1.55	2.617	0.697			0.39	-0.59	29.85
387		J205804.3+440918	314.51806	44.15508	4.14	12.950	1.648			-0.09	-0.27
388		J205914.8+440930	314.81201	44.15860	3.10	7.197	1.018			-0.86	0.61	29.79
389		J205932.9+440946	314.88725	44.16283	2.81	13.153	1.546			0.04	-0.11	30.72
390		J205812.9+440951	314.55383	44.16419	4.10	3.469	0.822			-0.58	0.12	29.49
391		J205743.1+441037	314.42987	44.17698	4.82	8.945	2.838			-0.30	0.07	29.88
392		J205917.3+441040	314.82216	44.17793	5.22	5.078	0.996			0.13	0.30	30.16
393		J205819.0+441058	314.57950	44.18298	3.24	6.054	0.931			-0.61	0.13	29.71
394		J205902.3+441112	314.75997	44.18671	3.31	4.441	0.708			0.04	0.45	30.15
395		J205935.4+441120	314.89775	44.18895	5.26	6.058	1.193			-0.51	0.39	29.72
396		J205910.6+441142	314.79437	44.19507	2.45	12.933	1.149			-0.57	-0.21	30.04
397		J205740.9+441155	314.42053	44.19880	3.89	6.729	2.679			-0.44	-0.40	29.76
398		J205906.8+441231	314.77851	44.20870	4.14	2.268	0.551			-0.05	0.46	29.64
399		J205954.7+441246	314.97817	44.21282	4.86	9.075	1.558			-0.18	0.62	30.35
400		J205806.0+441250	314.52511	44.21398	3.46	19.769	1.774			-0.52	0.01
401		J205916.6+441311	314.81958	44.21976	3.46	4.342	0.747			0.06	-0.06
402		J205913.1+441318	314.80484	44.22186	3.20	6.304	0.946			-0.17	-0.22	30.05
403		J205925.2+441345	314.85520	44.22926	4.00	3.031	0.685			0.31	0.06	29.59
404		J205737.7+441350	314.40734	44.23077	5.15	22.230	4.260			-0.50	-0.32
405		J205925.7+441420	314.85722	44.23893	2.48	3.832	0.686			-0.17	0.05	30.03
406		J205931.0+441508	314.87944	44.25225	3.64	14.698	1.439			-0.30	0.10	30.10
407		J205819.9+441547	314.58306	44.26331	3.10	6.423	0.905			-0.02	0.38
408		J205839.6+441614	314.66537	44.27076	1.98	24.220	1.424			-0.10	-0.32	30.57
409		J205912.7+441626	314.80319	44.27389	2.23	17.035	1.275			0.16	-0.27
410		J210002.9+441637	315.01210	44.27722	4.28	16.592	2.216			-0.01	-0.05	30.39
411		J205816.7+441729	314.56969	44.29158	3.46	4.879	0.846			-0.24	-0.12	29.75
412		J205803.6+441735	314.51517	44.29314	2.12	3.013	0.763			0.09	-0.46
413		J205900.4+441757	314.75184	44.29941	2.59	9.906	0.995			-0.66	-0.08	29.93
414		J205906.6+441822	314.77783	44.30616	2.99	6.607	0.858			-0.38	0.05	30.13
415		J205827.2+441830	314.61334	44.30856	2.81	2.730	0.610			0.28	0.01
416		J205842.6+441857	314.67783	44.31584	2.20	19.181	1.417			-0.52	-0.38	30.23
417		J205840.4+441936	314.66847	44.32689	2.02	7.520	0.910			-0.16	-0.43
418		J205903.4+441957	314.76454	44.33256	2.59	3.468	0.671			-0.28	-0.28	29.77
419		J205900.6+442041	314.75273	44.34475	3.67	4.163	0.809			-0.54	0.18	29.73
420		J205903.5+442046	314.76474	44.34636	3.60	4.496	0.836			-0.63	0.05	29.58
421		J205814.7+442051	314.56157	44.34753	1.91	4.137	0.854			0.56	0.31	29.72
422		J205812.0+442054	314.55021	44.34845	4.07	4.059	0.955			-0.11	0.01	29.97
423		J205944.8+442114	314.93675	44.35406	3.56	13.980	2.564			-0.57	-0.14	30.07
424		J205806.2+442146	314.52595	44.36283	3.24	9.435	1.451			0.23	0.30	29.94
425		J205755.9+442321	314.48327	44.38921	4.39	17.624	2.496			-0.36	0.07	30.18
426		J205841.5+442325	314.67307	44.39043	2.23	4.042	1.132			0.75	0.11	29.78
427		J205916.1+442621	314.81709	44.43921	3.10	4.005	1.074			-0.03	0.24	29.53
428		J205905.9+442654	314.77467	44.44859	2.95	15.519	2.015			0.29	-0.20	30.43
429		J205946.5+442716	314.94380	44.45460	5.40	13.484	2.828			-0.64	0.42	30.06
430		J205839.5+434307	314.66468	43.71865	5.22	7.131	1.397			-0.21	0.16	29.86
431		J205800.8+434515	314.50366	43.75429	4.36	3.879	1.019			0.05	0.16	30.13
432		J205834.5+434520	314.64384	43.75570	3.28	6.054	0.940			0.16	0.39
433		J205809.8+434536	314.54124	43.76002	4.28	8.268	1.106			-0.02	0.15	30.34
434		J205808.6+434658	314.53612	43.78294	1.98	25.479	1.486			0.58	-0.09	30.89
435		J205741.9+434721	314.42465	43.78932	3.10	6.580	0.935			-0.47	0.23	29.76
436		J205744.8+434839	314.43700	43.81098	2.38	13.879	1.161			-0.46	-0.01	30.07
437		J205854.5+434904	314.72710	43.81803	5.44	4.525	0.950			-0.05	0.45	30.43
438		J205754.4+434931	314.47701	43.82539	4.03	8.857	1.059			-0.49	0.34	29.88
439		J205805.8+434931	314.52437	43.82541	2.56	8.019	0.792			-0.37	0.06	30.11
440		J205849.6+435006	314.70695	43.83511	2.34	12.767	1.061			0.07	-0.12	30.39
441		J205757.3+435007	314.48891	43.83541	2.20	13.232	0.978			-0.63	0.12	30.10
442		J205748.5+435022	314.45214	43.83961	1.91	31.113	1.703			-0.68	-0.17	30.42
443		J205726.8+435037	314.36202	43.84370	6.80	8.424	1.418			-0.22	0.30	29.85
444		J205727.9+435144	314.36637	43.86239	2.05	2.152	0.507			-0.81	0.70	29.26
445		J205716.2+435156	314.31751	43.86577	4.25	11.163	1.479			0.07	0.15	30.98
446		J205709.9+435226	314.29161	43.87409	5.15	7.504	1.437			0.09	0.14	31.08
447		J205928.7+435459	314.86965	43.91659	3.24	16.822	2.573			-0.22	-0.20	30.34
448		J205746.7+435633	314.44498	43.94252	2.95	1.868	0.453			0.31	0.06	30.00
449		J205818.6+435652	314.57770	43.94798	3.38	3.017	0.503			-0.31	0.22	29.64
450		J205905.7+435701	314.77385	43.95038	1.37	112.750	3.186			-0.40	-0.42	31.14
451		J205722.1+435751	314.34209	43.96427	2.09	31.320	2.066			-0.50	-0.09	30.43
452		J205844.3+435810	314.68494	43.96965	3.49	4.085	0.717			-0.01	0.24	30.01
453		J205826.2+440015	314.60920	44.00434	5.47	3.826	0.811			-0.26	0.35	29.60
454		J205839.5+440133	314.66470	44.02605	4.97	6.969	1.251			-0.03	0.26	30.69
455		J205717.8+440227	314.32417	44.04099	4.36	8.421	2.217			-0.34	0.07	29.92
456		J205821.6+440305	314.59029	44.05149	5.36	5.109	1.052			-0.12	0.38	30.10
457		J205833.5+440333	314.63972	44.05929	2.63	17.160	1.760			-0.15	-0.04
458		J205748.6+440525	314.45256	44.09041	2.30	16.083	2.527			-0.16	-0.39	30.35
459		J205421.4+435043	313.58949	43.84545	2.02	190.240	5.560			0.54	-0.06	31.80
460		J205440.6+435243	313.66932	43.87867	3.06	2.748	0.716			-0.63	0.12	29.37
461		J205403.1+435455	313.51331	43.91536	5.18	5.067	0.986			-0.11	0.01	30.10
462		J205414.9+435457	313.56228	43.91601	7.09	5.775	1.056			-0.06	0.20	30.58
463		J205438.8+435528	313.66201	43.92462	2.88	8.813	1.080			-0.49	-0.19	29.87
464		J205530.2+435653	313.87620	43.94818	3.17	8.992	1.333			-0.74	-0.07	29.88
465		J205455.5+435653	313.73136	43.94833	2.66	10.627	1.130			-0.72	-0.14	29.96
466		J205516.9+435706	313.82065	43.95187	3.71	4.254	0.839			-0.57	0.32	29.56
467		J205348.1+435711	313.45078	43.95327	6.08	11.561	1.569			0.12	0.44	30.99
468		J205511.0+435713	313.79604	43.95381	1.76	4.376	0.787			-0.19	-0.55	29.79
469		J205458.3+435713	313.74328	43.95388	2.81	8.806	1.022			-0.71	-0.07	29.87
470		J205421.1+435802	313.58815	43.96728	2.84	2.014	0.465			-0.45	0.03	29.28
471		J205412.0+435806	313.55006	43.96836	4.79	4.672	0.783			0.05	0.31	29.95
472		J205353.3+435807	313.47230	43.96862	2.88	9.923	1.212			-0.60	-0.08	29.93
473		J205425.8+435820	313.60767	43.97248	2.05	19.842	1.270			-0.65	-0.39	30.23
474		J205401.3+435851	313.50548	43.98087	4.50	6.684	0.993			-0.33	-0.14	29.75
475		J205538.6+435905	313.91103	43.98479	2.34	96.706	3.923			0.70	0.32	31.47
476		J205441.8+435939	313.67449	43.99420	1.91	6.224	0.669			0.62	0.47	30.80
477		J205413.4+435945	313.55616	43.99589	3.06	1.491	0.393			-0.20	0.55	29.55
478		J205526.1+435945	313.85916	43.99597	7.85	5.244	1.145			-0.23	0.06	29.80
479		J205503.1+440008	313.76318	44.00237	3.38	3.592	0.593			0.32	0.21	30.84
480		J205416.5+440037	313.56903	44.01044	3.71	2.762	0.540			0.31	-0.23	29.82
481		J205541.2+440038	313.92179	44.01066	6.41	11.616	1.739			0.23	0.01	30.58
482		J205436.2+440039	313.65096	44.01095	3.67	2.186	0.423			-0.05	0.35	30.17
483		J205338.6+440041	313.41109	44.01145	5.29	5.559	1.120			0.01	0.28	29.83
484		J205406.8+440045	313.52874	44.01251	2.95	7.086	0.896			0.10	-0.29	30.20
485		J205443.9+440045	313.68320	44.01276	2.23	13.007	0.977			-0.73	-0.20	30.04
486		J205454.8+440052	313.72851	44.01471	2.84	1.635	0.376			0.09	0.57	30.03
487		J205502.7+440149	313.76141	44.03042	3.31	3.605	0.573			-0.46	-0.11	29.49
488		J205458.6+440205	313.74448	44.03491	1.55	54.015	1.965			-0.72	-0.52	30.66
489		J205526.8+440225	313.86207	44.04039	3.42	4.945	0.832			0.04	0.53	29.97
490		J205434.6+440241	313.64434	44.04494	2.99	1.422	0.357			-0.28	-0.28	29.08
491		J205543.3+440310	313.93064	44.05292	3.28	8.065	1.272			0.12	-0.19	29.84
492		J205338.9+440332	313.41217	44.05899	2.05	11.071	1.362			0.21	-0.11	30.34
493		J205409.3+440336	313.53893	44.06005	2.09	1.885	0.468			0.47	0.33	29.82
494		J205334.4+440412	313.39337	44.07005	2.95	11.702	1.515			0.22	0.57	30.60
495		J205447.7+440419	313.69881	44.07221	3.49	3.041	0.533			0.33	-0.11	30.24
496		J205518.2+440419	313.82599	44.07218	3.71	3.641	0.712			-0.40	-0.07	29.50
497		J205404.3+440458	313.51795	44.08278	1.98	2.234	0.500			0.60	0.54
498		J205531.2+440606	313.88009	44.10170	4.00	3.936	0.891			0.52	0.22	29.86
499		J205327.2+440606	313.36357	44.10169	2.88	20.478	2.519			0.11	-0.28	30.24
500		J205506.7+440745	313.77796	44.12936	2.20	1.840	0.489			-0.14	0.65	30.55
501		J205522.6+440800	313.84449	44.13361	2.38	5.768	0.952			0.77	0.47	30.32
502		J205520.2+440902	313.83458	44.15069	2.99	2.742	0.695			0.24	0.52	30.57
503		J205445.5+441015	313.68976	44.17107	2.95	8.285	1.049			-0.60	0.02	29.87
504		J205404.6+441022	313.51918	44.17301	2.81	15.851	1.862			0.23	-0.07	30.63
505		J205346.6+441058	313.44418	44.18284	6.55	14.013	2.196			-0.04	0.33	31.01
506		J205355.6+441108	313.48178	44.18563	4.68	9.431	1.497			0.15	0.05	30.33
507		J205450.8+441134	313.71170	44.19285	4.18	10.664	1.378			0.18	-0.02	30.55
508		J205346.6+441156	313.44432	44.19915	5.80	6.038	1.427			-0.22	0.31	30.17
509		J205446.6+441206	313.69451	44.20186	3.42	6.442	1.087			0.33	-0.05
510		J205428.0+441330	313.61673	44.22518	6.52	11.652	1.810			-0.03	0.33	32.06
511		J205414.6+441424	313.56098	44.24000	3.78	6.214	1.274			-0.41	0.28	29.72
512		J205432.2+441438	313.63421	44.24392	4.93	9.077	1.601			-0.25	0.10	29.89
513		J205410.3+441457	313.54295	44.24934	4.10	5.759	1.376			-0.29	0.23	30.52
514		J205438.1+441526	313.65889	44.25738	3.10	3.859	1.023			-0.40	0.33	29.52
515		J205428.0+441614	313.61697	44.27057	1.40	4.685	1.063			-0.51	0.27
516		J205318.0+441208	313.32529	44.20238	8.50	38.845	9.815			-0.11	0.12	31.18
517		J205420.8+441528	313.58696	44.25804	3.89	30.555	3.467			0.08	0.19	30.77
518		J205313.5+441600	313.30631	44.26682	7.02	23.701	4.263			-0.06	0.31	31.23
519		J205351.9+441706	313.46657	44.28503	1.58	54.105	2.056			0.23	-0.08	31.19
520		J205429.2+441817	313.62167	44.30482	3.17	15.577	2.272			-0.12	0.30	30.70
521		J205242.4+441919	313.17708	44.32202	3.35	32.224	2.717			-0.02	0.06	31.01
522		J205301.9+441921	313.25821	44.32274	1.55	48.971	3.521			0.12	0.40
523		J205432.8+442013	313.63705	44.33703	6.16	26.184	3.660			0.12	0.20	30.99
524		J205324.3+442034	313.35159	44.34279	2.23	20.719	1.570			0.12	-0.07	30.58
525		J205341.5+442137	313.42328	44.36034	1.69	34.199	1.454			-0.02	-0.26	30.47
526		J205309.7+442151	313.29048	44.36442	2.63	8.194	1.605			-0.04	0.30	30.68
527		J205305.2+442206	313.27196	44.36849	2.74	7.638	1.651			-0.19	0.41	30.67
528		J205309.7+442220	313.29078	44.37229	2.59	7.723	1.504			-0.19	0.32	30.64
529		J205253.1+442221	313.22134	44.37259	3.85	12.069	2.558			-0.11	0.35	30.65
530		J205409.3+442258	313.53890	44.38303	0.90	17.420	1.613			0.06	0.38
531		J205346.6+442302	313.44431	44.38399	1.44	58.784	1.906			0.08	-0.18	30.70
532		J205424.8+442305	313.60368	44.38488	5.00	12.151	2.188			-0.18	0.29	30.01
533		J205313.4+442322	313.30592	44.38948	2.12	44.933	3.070			-0.58	0.06
534		J205418.6+442323	313.57777	44.38999	2.48	11.720	1.100			-0.29	0.12	30.03
535		J205330.9+442325	313.37895	44.39055	2.92	7.831	0.981			-0.04	0.02	30.24
536		J205323.9+442342	313.34966	44.39515	2.09	22.329	1.476			0.38	0.12	31.28
537		J205438.1+442402	313.65903	44.40062	2.20	6.084	0.859			0.26	0.07	30.30
538		J205450.0+442409	313.70870	44.40266	7.16	23.254	4.307			-0.21	0.35	30.30
539		J205337.7+442422	313.40746	44.40632	4.90	12.705	2.203			-0.00	0.04	30.44
540		J205413.4+442432	313.55606	44.40914	1.51	70.825	2.323			0.28	0.01	31.37
541		J205417.5+442532	313.57310	44.42580	4.57	17.471	2.696			0.03	0.19	30.67
542		J205358.2+442534	313.49268	44.42620	2.59	2.769	0.535			0.10	-0.01	30.27
543		J205438.2+442543	313.65949	44.42876	5.90	14.789	1.918			-0.21	0.28	30.10
544		J205339.7+442550	313.41560	44.43059	1.87	24.785	1.290			0.27	-0.09	30.69
545		J205346.4+442707	313.44366	44.45218	4.61	7.577	1.173			0.06	0.10	30.32
546		J205325.4+442716	313.35590	44.45453	2.56	17.985	1.769			0.08	-0.01	30.72
547		J205322.1+442747	313.34250	44.46333	1.84	43.370	2.166			0.09	-0.35	30.57
548		J205224.6+442814	313.10254	44.47082	6.30	17.672	2.557			-0.05	0.16	30.62
549		J205345.5+442816	313.43980	44.47123	5.90	28.958	3.758			-0.02	0.21	30.92
550		J205405.7+442842	313.52394	44.47845	5.36	11.297	2.330			-0.08	0.27	30.68
551		J205319.8+442844	313.33274	44.47903	2.27	24.859	1.902			0.14	-0.15	30.65
552		J205250.0+442902	313.20839	44.48402	6.62	32.892	5.248			-0.06	0.28	31.52
553		J205244.9+442912	313.18745	44.48675	4.90	24.652	4.279			-0.01	0.23	30.82
554		J205357.4+442940	313.48949	44.49450	4.00	35.950	4.266			0.31	-0.22	30.97
555		J205406.2+443025	313.52602	44.50721	2.95	28.979	3.759			0.26	-0.28
556		J205347.2+443038	313.44678	44.51061	6.19	7.915	2.125			0.33	0.16	30.67
557		J205343.2+443108	313.43016	44.51891	5.11	15.111	5.315			0.32	0.06	31.75
558		J205340.9+443146	313.42068	44.52955	8.06	43.540	10.058			0.53	0.15	31.95
559		J205444.7+443146	313.68639	44.52948	7.60	46.772	9.622			0.01	-0.00	30.69
560		J205435.3+443235	313.64711	44.54321	5.33	36.610	7.437			0.02	0.08	30.89
561		J205358.1+443238	313.49248	44.54406	4.43	25.754	3.745			0.17	-0.11	31.24
562		J205434.3+443309	313.64328	44.55263	5.11	14.533	5.091			-0.11	0.09	30.55
563		J205343.0+443345	313.42947	44.56262	3.89	11.858	2.564			0.62	0.04	30.96
564		J205340.3+443727	313.41829	44.62441	3.78	30.947	3.276			0.53	-0.15	31.18
565		J205226.7+441705	313.11152	44.28491	3.46	19.545	3.363			-0.07	0.06	30.54
566		J205211.3+441753	313.04747	44.29832	7.02	46.920	15.696			0.39	-0.22	30.90
567		J205249.8+441900	313.20785	44.31688	3.35	12.278	1.980			-0.11	0.08	30.53
568		J205301.5+441904	313.25642	44.31780	3.85	7.106	1.509			0.03	0.22	30.41
569		J205235.5+441910	313.14802	44.31953	4.68	13.853	2.209			0.06	0.14	30.36
570		J205212.7+441925	313.05309	44.32370	1.66	594.620	12.284			0.22	-0.07	31.70
571		J205212.7+442054	313.05307	44.34841	3.46	8.200	1.426			0.32	0.20	30.66
572		J205228.0+442112	313.11675	44.35352	3.71	6.192	1.209			-0.04	0.12	30.29
573		J205217.6+442114	313.07361	44.35404	3.60	6.978	1.310			0.03	-0.31	30.06
574		J205216.2+442157	313.06762	44.36590	9.50	10.814	3.334			0.03	0.14	30.49
575		J205242.7+442219	313.17823	44.37215	5.04	7.235	1.332			-0.20	0.25	29.82
576		J205146.2+442222	312.94278	44.37287	2.70	13.923	2.878			0.24	-0.31	30.39
577		J205348.5+442226	313.45239	44.37412	1.94	12.565	2.685			-0.43	-0.14	30.50
578		J205215.1+442307	313.06321	44.38536	4.18	12.262	1.588			-0.47	0.00	30.02
579		J205205.6+442334	313.02357	44.39302	3.13	10.400	1.507			-0.50	-0.11	29.95
580		J205212.1+442347	313.05077	44.39645	6.48	3.245	1.676			0.00	0.30	30.02
581		J205230.1+442410	313.12569	44.40301	2.70	4.122	0.871			0.04	0.02	29.90
582		J205208.2+442416	313.03447	44.40445	5.29	2.187	1.396			0.18	0.28	30.06
583		J205159.1+442543	312.99660	44.42872	3.82	20.294	2.188			-0.12	-0.40	30.63
584		J205225.0+442554	313.10458	44.43172	2.38	5.711	0.931			0.02	0.14	30.07
585		J205253.4+442557	313.22271	44.43265	5.58	5.182	1.148			-0.11	0.18	30.17
586		J205250.9+442556	313.21227	44.43248	4.21	2.468	0.620			-0.11	0.25	29.32
587		J205256.9+442600	313.23732	44.43361	3.82	3.599	0.752			0.02	0.16	30.22
588		J205209.6+442604	313.04005	44.43455	2.48	21.554	1.960			-0.06	-0.36	30.26
589		J205243.1+442611	313.17960	44.43640	4.28	2.634	0.681			0.10	0.10	29.82
590		J205144.6+442616	312.93622	44.43788	6.19	8.855	2.356			0.32	-0.38	30.10
591		J205232.5+442632	313.13583	44.44249	2.52	4.035	0.749			-0.01	-0.04	29.96
592		J205312.1+442635	313.30072	44.44308	3.38	5.139	0.863			0.04	0.10	30.20
593		J205331.5+442739	313.38159	44.46084	4.14	13.744	1.756			-0.04	0.18	30.55
594		J205212.6+442741	313.05289	44.46146	6.01	3.586	1.649			0.19	0.17	29.76
595		J205317.4+442802	313.32273	44.46728	3.64	15.871	1.575			0.14	0.14
596		J205215.1+442813	313.06308	44.47047	3.17	2.372	0.653			-0.05	-0.27	29.77
597		J205251.7+442814	313.21556	44.47072	3.38	4.591	0.764			0.03	0.16	30.10
598		J205235.1+442819	313.14627	44.47212	1.87	10.430	1.100			-0.31	-0.13	29.95
599		J205145.5+442836	312.93996	44.47680	7.24	10.624	2.004			0.06	0.01	30.46
600		J205314.3+442904	313.30999	44.48463	4.36	2.487	0.658			0.01	0.29	29.87
601		J205334.7+442916	313.39492	44.48793	3.74	6.579	1.320			0.02	-0.15	30.58
602		J205233.9+442917	313.14151	44.48809	5.00	10.869	1.961			-0.02	0.12	30.35
603		J205206.4+442921	313.02696	44.48927	3.10	4.148	1.112			0.23	-0.23	29.85
604		J205227.9+442939	313.11660	44.49420	2.27	21.445	1.631			-0.70	-0.17
605		J205231.6+442958	313.13168	44.49968	2.23	21.377	1.616			0.15	-0.28	30.71
606		J205207.9+443003	313.03307	44.50099	1.94	55.600	3.116			0.75	0.41	31.59
607		J205220.1+443029	313.08377	44.50826	5.47	4.359	1.710			0.35	0.45	30.17
608		J205231.0+443032	313.12918	44.50910	4.28	3.195	0.829			0.16	0.24	29.93
609		J205324.2+443040	313.35107	44.51137	3.64	5.386	1.020			0.53	0.12	30.76
610		J205312.2+443103	313.30112	44.51753	4.79	5.571	0.934			0.18	0.02	30.41
611		J205200.3+443118	313.00126	44.52167	2.70	18.065	1.977			0.42	-0.07	30.74
612		J205340.5+443129	313.41888	44.52474	3.92	70.084	4.118			0.53	0.16	32.32
613		J205254.6+443134	313.22757	44.52618	2.34	5.149	0.830			0.19	-0.05	30.16
614		J205143.7+443218	312.93220	44.53852	5.11	10.419	1.976			0.07	0.04	30.25
615		J205201.3+443236	313.00546	44.54358	5.04	26.455	2.513			0.00	-0.28	30.58
616		J205307.0+443255	313.27943	44.54866	5.90	3.365	0.829			-0.04	0.34	29.99
617		J205235.1+443318	313.14653	44.55513	2.70	11.734	1.281			0.29	-0.28	30.59
618		J205315.9+443321	313.31641	44.55609	3.78	5.219	1.068			0.09	0.15	30.50
619		J205241.6+443407	313.17338	44.56865	2.45	1.660	0.533			0.22	-0.17	29.63
620		J205226.0+443426	313.10864	44.57408	2.70	15.293	1.640			0.32	-0.31	30.44
621		J205158.4+443504	312.99348	44.58445	7.31	11.147	2.148			-0.29	0.08	30.03
622		J205245.1+443524	313.18820	44.59005	2.16	3.203	0.834			0.07	-0.15	29.90
623		J205229.0+443604	313.12108	44.60123	3.38	7.386	1.238			0.19	-0.11	30.02
624		J205322.6+443608	313.34456	44.60232	5.40	6.811	1.426			0.30	0.02	30.52
625		J205250.3+443645	313.20983	44.61253	4.03	14.466	1.727			-0.73	0.32	30.09
626		J205300.7+443658	313.25295	44.61637	2.41	101.920	4.419			0.45	-0.24
627		J205226.6+443706	313.11084	44.61853	3.02	43.592	3.046			0.43	-0.19	31.10
628		J205158.3+443725	312.99300	44.62373	3.92	7.105	1.566			0.17	-0.08	30.25
629		J205224.5+443755	313.10223	44.63199	4.75	10.685	1.761			0.34	-0.14	29.96
630		J205215.4+443802	313.06420	44.63407	7.20	10.626	1.999			-0.13	0.26	29.96
631		J205317.0+443834	313.32097	44.64297	2.23	45.448	3.400			0.60	-0.16	31.26
632		J205229.4+443840	313.12257	44.64471	2.70	5.821	1.216			0.60	-0.29	30.32
633		J205322.2+443852	313.34281	44.64800	2.84	21.781	2.603			0.12	-0.27	30.64
634		J205243.7+443859	313.18243	44.64983	4.28	4.565	1.164			0.35	-0.16	30.51
635		J205329.9+443934	313.37471	44.65962	4.00	8.368	1.900			0.27	-0.13	30.36
636		J205251.5+443952	313.21497	44.66471	4.32	15.932	2.182			0.02	0.62	30.92
637		J205336.6+443952	313.40274	44.66465	3.20	25.520	3.887			0.31	-0.13	30.79
638		J205208.2+444027	313.03421	44.67440	8.60	9.045	4.220			0.13	0.20	30.77
639		J205311.9+444033	313.29990	44.67598	8.68	7.447	3.536			0.35	0.00	30.36
640		J205256.9+444045	313.23747	44.67917	5.51	8.053	3.207			0.23	-0.15	30.32
641		J205301.1+444057	313.25483	44.68251	5.04	12.235	2.262			-0.16	0.11	30.22
642		J205329.5+444106	313.37293	44.68513	8.75	11.678	5.608			0.07	-0.16	30.27
643		J205310.3+444130	313.29302	44.69190	3.46	44.266	3.991			-0.48	-0.24	30.58
644		J205310.8+444218	313.29521	44.70508	5.04	14.061	2.593			0.10	0.01	30.58
645		J205239.9+441615	313.16647	44.27085	6.66	19.823	3.203			-0.11	0.38	31.08
646		J205433.9+442010	313.64149	44.33612	2.95	8.771	1.136			0.17	0.09	30.43
647		J205431.7+442016	313.63219	44.33799	2.20	6.265	0.883			0.22	0.12	30.36
648		J205223.1+442218	313.09652	44.37169	8.50	8.802	2.229			-0.03	0.20	30.48
649		J205223.8+442308	313.09921	44.38570	8.39	9.967	2.476			-0.08	0.29	30.91
650		J205353.4+442311	313.47279	44.38665	0.50	8068.400	19.930			-0.43	-0.52
651		J205333.5+442514	313.38965	44.42063	6.37	8.268	1.222			0.01	0.19	30.27
652		J205342.1+442658	313.42554	44.44966	5.18	17.506	1.761			-0.17	0.08
653		J205355.5+443038	313.48155	44.51059	8.64	12.374	3.219			0.17	0.02	30.69
654		J205337.4+443458	313.40597	44.58292	4.57	2.630	1.347			0.35	0.16
655		J205054.0+443808	312.72513	44.63561	4.46	17.339	2.528			0.10	-0.13	30.73
656		J205044.6+443838	312.68605	44.64403	5.26	6.040	1.207			-0.01	0.08
657		J205053.1+443856	312.72155	44.64906	3.02	3.363	0.856			0.16	0.56	30.28
658		J205040.3+443929	312.66816	44.65827	4.61	8.472	1.309			0.28	0.43	30.03
659		J205134.8+443939	312.89526	44.66094	4.54	40.933	6.136			0.48	0.08	31.10
660		J205052.1+444004	312.71743	44.66793	3.46	6.326	1.088			0.52	0.23	30.67
661		J205118.2+444027	312.82600	44.67420	4.72	11.075	1.800			0.03	-0.08	30.40
662		J205059.4+444047	312.74787	44.67990	2.12	64.128	4.381			0.51	-0.15	31.31
663		J205030.8+444054	312.62862	44.68178	2.56	16.742	1.610			0.45	0.57	30.72
664		J205027.6+444119	312.61514	44.68881	2.81	2.775	0.624			0.29	-0.07	29.50
665		J205057.8+444307	312.74107	44.71880	4.43	7.593	1.090			0.29	-0.05	30.64
666		J205037.1+444315	312.65486	44.72085	3.46	4.876	0.842			-0.34	0.09	29.62
667		J205109.9+444346	312.79126	44.72964	6.44	8.110	1.228			-0.22	0.26	29.84
668		J205047.5+444355	312.69825	44.73204	5.26	3.817	0.755			0.18	0.14	30.39
669		J205029.9+444548	312.62495	44.76352	5.47	2.842	0.606			0.11	0.42	29.77
670		J205043.5+444627	312.68132	44.77426	3.28	3.838	0.599			-0.55	0.14	29.51
671		J204939.4+444626	312.41419	44.77401	1.84	3.554	1.296			-0.78	0.20
672		J205126.4+444722	312.86014	44.78963	3.71	4.071	0.799			-0.08	0.46	30.48
673		J205027.7+444729	312.61575	44.79153	4.10	1.863	0.442			0.27	0.31	29.73
674		J205049.3+444753	312.70564	44.79810	2.16	13.645	0.948			0.63	0.49	30.90
675		J205105.7+444753	312.77387	44.79816	6.98	4.352	0.773			0.12	0.13	30.82
676		J205043.6+444805	312.68168	44.80161	2.20	3.513	0.499			0.31	0.47	29.79
677		J205014.5+444820	312.56082	44.80582	4.86	4.486	0.767			-0.12	0.34	29.92
678		J205041.2+444838	312.67186	44.81073	2.84	1.580	0.357			-0.54	-0.03	29.13
679		J204950.9+444913	312.46209	44.82033	3.02	2.305	0.585			0.40	0.19	29.88
680		J205042.6+444917	312.67758	44.82150	3.82	2.005	0.418			-0.02	0.40	29.73
681		J205016.0+444919	312.56698	44.82216	5.26	4.001	0.794			-0.08	0.47	29.95
682		J205124.6+444932	312.85254	44.82556	3.13	5.523	0.796			0.54	0.25	31.17
683		J205132.3+444933	312.88499	44.82585	1.94	2.046	0.805			1.00	0.57	30.63
684		J205045.4+444934	312.68925	44.82633	1.91	1.616	0.336			-0.62	-0.50	29.14
685		J204958.5+444937	312.49406	44.82722	1.80	3.353	0.615			0.30	0.60	29.86
686		J205031.8+444946	312.63267	44.82955	2.20	13.947	0.991			-0.65	-0.04	30.07
687		J205002.9+444946	312.51227	44.82968	4.86	5.057	0.865			-0.49	0.30	29.63
688		J204958.1+444952	312.49245	44.83134	5.11	14.337	1.393			-0.17	0.34	31.21
689		J205042.7+445014	312.67804	44.83741	4.03	1.611	0.367			0.10	0.26	30.01
690		J205118.2+445034	312.82605	44.84301	2.92	5.874	0.734			0.50	0.44
691		J205039.3+445052	312.66395	44.84799	3.02	4.013	0.546			0.18	0.46	30.24
692		J205018.2+445055	312.57620	44.84881	2.56	2.628	0.501			-0.36	0.02	30.13
693		J205105.4+445058	312.77258	44.84954	2.20	1.071	0.290			0.33	-0.33	29.82
694		J205034.1+445104	312.64222	44.85129	2.30	11.214	0.882			-0.56	-0.23	29.98
695		J205211.4+445107	313.04771	44.85201	2.92	7.136	1.715			-0.39	-0.05	29.78
696		J205109.8+445124	312.79088	44.85673	3.13	4.275	0.613			0.38	0.00	31.21
697		J205051.4+445144	312.71448	44.86246	3.82	1.902	0.393			-0.32	0.17	29.21
698		J205032.3+445147	312.63468	44.86325	4.61	4.269	0.659			0.12	0.38	31.63
699		J205045.2+445201	312.68848	44.86701	7.70	3.080	0.653			0.06	0.23	30.32
700		J205047.9+445258	312.69997	44.88284	2.81	5.814	0.674			-0.61	0.05	29.69
701		J205149.6+445309	312.95684	44.88601	4.90	8.071	1.402			-0.47	0.20	29.87
702		J205108.9+445311	312.78711	44.88657	1.55	14.544	1.060			0.76	0.42	31.66
703		J205033.7+445347	312.64072	44.89647	3.92	7.109	0.812			0.28	0.43	31.05
704		J205101.5+445419	312.75664	44.90542	4.21	5.951	0.774			0.09	0.45	31.11
705		J205000.0+445421	312.50023	44.90601	5.04	5.013	0.926			-0.27	0.10
706		J205154.4+445433	312.97707	44.90932	3.35	29.540	2.483			-0.58	0.06	30.42
707		J205045.5+445453	312.68964	44.91486	1.62	48.216	1.925			0.67	0.64
708		J205032.8+445456	312.63691	44.91557	2.38	3.367	0.560			0.58	0.57	30.03
709		J205025.0+445509	312.60424	44.91938	2.77	31.650	1.854			-0.42	-0.07	30.43
710		J205045.6+445512	312.69035	44.92007	1.48	1.435	0.355			0.38	-0.08
711		J205030.2+445513	312.62611	44.92050	2.02	1.586	0.363			0.60	0.36	29.63
712		J205040.0+445518	312.66689	44.92178	2.70	7.931	0.855			-0.66	0.16	29.83
713		J205105.1+445532	312.77159	44.92572	3.53	3.446	0.618			-0.42	0.16	29.47
714		J205137.5+445617	312.90630	44.93815	2.30	2.264	0.667			-0.60	0.43	30.19
715		J204943.0+445702	312.42937	44.95061	3.67	6.247	1.202			0.45	0.27	30.72
716		J205008.8+445812	312.53678	44.97020	4.25	10.012	1.321			-0.34	0.06	29.93
717		J205105.8+445950	312.77429	44.99732	5.58	4.861	1.073			-0.45	0.55	29.62
718		J205043.9+450126	312.68328	45.02394	4.46	9.305	1.363			-0.39	0.23	29.93
719		J205055.3+450335	312.73068	45.05983	2.30	44.973	3.659			-0.67	-0.40	30.58
720		J205122.5+450402	312.84381	45.06749	4.43	22.880	3.272			0.25	0.45	30.56
721		J205033.7+450434	312.64048	45.07638	1.44	4.004	0.929			-0.85	0.00	29.69

Table 4. Table 4: Optical/NIR photometry for X-ray sources.

X-ray	$i$	$r - i$	$r - H α$	$J$	$H$	$K$	IR	H $α$	RGS11
no.							excess	excess	number
1
2				13.52	12.70	12.35
3
4
5
6				14.21	12.81	12.10
7				13.22	11.53	10.51			98
8				15.82	15.15	14.60
9	17.06	1.93	2.14	13.92	12.74	12.12		Y	101
10				20.00	18.12	17.21
11				14.92	13.32	12.63
12
13				14.38	12.96	12.35
14
15				11.25	11.06	11.00
16
17				14.88	11.85	9.75			116
18				19.55	17.59	16.59
19	16.07	1.44	1.24	13.80	12.78	12.15		Y	121
20									124
21									127
22
23				16.57	13.71	12.27
24				12.09	11.03	10.56
25				11.27	10.21	9.66			130
26				11.86	10.94	10.51			131
27									134
28	16.45	2.38	0.66	12.85	11.39	10.87
29				20.34	18.24	17.47
30	14.69	1.45	0.68	12.59	11.69	11.38
31	16.41	2.08	1.18	13.73	12.81	12.33			140
32				12.75	11.56	11.10			141
33				18.18	14.89	13.02
34				14.63	13.20	12.43
35				12.35	10.57	9.55
36				15.52	14.87	14.40
37				15.62	13.78	12.95
38				13.39	12.46	12.05			146
39
40
41				17.76	15.88	15.03
42									150
43				12.14	11.09	10.48			152
44				16.83	13.20	11.19			156
45				14.00	12.14	11.37
46				12.93	11.95	11.64			157
47
48				12.48	11.55	11.11
49				17.11	16.02	15.49
50
51				16.45	14.02	12.69
52				13.76	13.01	11.77	Y		163
53				14.02	12.96	12.37			164
54	16.57	1.67	0.81	14.30	13.42	13.10
55				13.12	12.10	11.62			166
56				12.95	11.96	11.48			167
57
58				16.55	12.76	10.49			171
59
60
61				15.23	13.10	11.93
62				15.95	12.82	11.00
63
64
65				15.20	12.67	11.27
66				15.39	13.60	12.58
67				20.04	15.82	13.50
68
69				12.19	11.31	10.79			177
70	15.62	1.88	1.05	13.46	12.41	11.95			178
71
72
73				14.62	12.80	12.03
74				12.64	11.18	10.20
75				11.85	11.01	10.64			180
76				12.80	11.11	10.09			181
77									185
78
79
80	17.37	2.11	1.49	14.62	13.81	13.44		Y
81				14.69	13.58	12.90
82				14.04	13.12	12.78
83				12.36	11.36	10.81			188
84	17.41	2.10	1.20	14.79	13.97	13.59
85	16.02	2.08	0.85	13.42	12.43	12.12
86
87	13.09	0.50	0.35	12.16	11.69	11.57
88	16.75	1.88	0.79	14.45	13.55	13.21
89
90	16.13	1.86	0.81	13.85	12.98	12.63
91				13.92	12.46	11.67
92
93				17.36	16.34	15.98
94				18.98	17.55	16.94
95				13.23	12.36	12.05
96				12.54	11.76	11.53			196
97				11.65	10.73	10.34			197
98				16.83	15.19	14.42
99	14.77	1.24	0.85	12.58	11.65	11.15		Y	199
100				14.33	13.31	12.65
101	17.51	1.89	1.07	15.56	14.94	14.68
102	16.16	1.53	1.39	13.75	12.69	12.08		Y	202
103				14.63	13.49	13.04
104
105				13.48	12.63	12.23
106				14.31	13.37	13.02
107
108	15.23	1.31	0.68	13.10	12.11	11.81
109	14.23	1.03	0.95	12.41	11.45	10.95		Y	210
110				14.20	13.37	12.92			213
111				14.79	14.09	13.69
112	17.53	1.95	0.89	15.58	14.99	14.71
113
114				13.64	12.69	12.32			218
115				13.34	12.28	11.77			220
116	13.78	0.49	0.30	13.00	12.69	12.55
117
118	16.24	2.12	0.93	13.58	12.74	12.38
119				11.99	10.86	10.04			224
120				11.99	10.86	10.04			224
121				20.42	18.64	18.19			227
122				13.12	12.08	11.59			228
123	14.52	1.28	0.55	11.83	10.81	10.18			230
124	14.68	0.96	0.55	13.37	12.75	12.55
125				13.32	12.57	12.35
126
127				14.04	13.32	12.82			238
128	16.37	2.11	0.93	13.82	12.97	12.59
129				15.38	14.40	13.94
130				11.79	11.57	11.40
131				16.42	15.33	14.82
132	16.66	2.53	0.95	13.83	13.04	12.66
133	16.26	1.30	0.56	14.32	13.44	13.17
134				10.87	10.15	9.94
135
136	16.50	2.43	0.95	13.76	13.01	12.63
137
138	17.09	1.97	0.32	13.70	12.51	11.99
139	17.05	1.88	0.93	14.79	13.92	13.58
140	15.31	1.24	0.64	13.19	12.24	11.56	Y		257
141				15.59	15.01	14.68
142	15.82	1.38	0.69	12.28	11.31	10.87
143	14.55	0.88	0.87	12.76	11.99	11.59		Y	259
144				14.97	14.06	13.76
145	16.09	1.58	1.09	13.31	12.39	11.79		Y	263
146				17.63	16.10	15.41
147	15.57	1.29	1.00	13.71	12.60	11.76	Y	Y	269
148
149	15.40	1.83	0.91	13.13	12.24	11.90
150	14.16	1.17	1.17	11.88	10.96	10.30	Y	Y	271
151	12.43	0.76	0.39	11.18	10.66	10.45
152	14.88	1.12	1.06	12.78	11.70	10.99	Y	Y	278
153
154	16.20	1.43	1.26	13.85	12.83	12.25		Y	284
155				15.64	14.39	13.83
156				14.45	13.36	12.55			287
157	16.20	1.95	0.95	13.84	12.91	12.54
158	16.49	1.92	1.17	13.88	12.85	12.22			290
159
160
161				20.21	18.75	18.30
162	15.96	1.37	0.65	15.10	13.69	12.75	Y		301
163				14.01	13.10	12.65			303
164				18.10	16.81	16.25
165				14.58	13.87	13.57
166				15.48	14.07	13.20			304
167				17.65	16.52	16.03
168				19.69	18.57	17.68
169				11.65	10.68	10.09			319
170	16.20	1.80	0.73	13.80	12.88	12.52
171
172	13.89	1.22	0.52	11.75	10.92	10.41			328
173	14.89	1.14	0.93	12.85	11.94	11.20	Y	Y	334
174				15.73	14.78	14.35
175				16.07	13.86	12.87
176	16.10	1.57	0.83	14.46	13.83	13.59
177
178				11.34	11.03	10.94
179				17.28	15.33	14.42
180				11.53	11.07	10.98
181
182	17.87	1.97	0.84	14.92	13.69	13.18
183				13.10	11.84	11.06			853
184
185
186	18.19	2.11	0.95	15.19	14.02	13.56
187
188				15.93	14.31	13.56
189	16.06	2.04	0.66
190				13.96	12.06	11.04			862
191
192				14.42	13.12	12.42			866
193
194				17.99	15.87	14.92
195				13.72	11.72	10.78
196
197
198	18.03	1.88	0.96	16.10	15.49	15.16
199
200	17.57	2.08	1.25	13.87	12.46	11.66			881
201				16.16	14.34	13.46
202
203
204				16.89	14.54	13.37
205				14.71	13.54	13.07			884
206
207				14.81	12.87	11.89			887
208				16.45	15.40	14.97
209	17.45	1.67	0.68	14.85	13.83	13.44
210
211				16.70	14.60	13.24			895
212
213				14.26	12.98	12.48
214
215
216				17.04	16.45	16.25
217
218
219									907
220				15.86	14.33	13.70			909
221	19.15	1.40	0.84	13.88	13.20	12.94
222
223
224
225	15.96	2.48	1.17	13.29	12.54	12.21
226				15.54	14.16	13.60
227
228
229									922
230	15.40	2.07	1.25	12.83	11.99	11.68		Y	923
231	15.59	1.58	0.69	13.23	12.18	11.78			925
232				15.33	14.22	13.62
233				20.10	18.48	18.01
234
235
236
237
238
239	17.05	2.91	0.84	12.14	10.37	9.58
240				9.87	9.51	9.38
241									944
242				17.37	15.06	14.01
243
244
245
246									951
247
248				12.83	12.21	12.05
249									957
250
251
252				17.96	15.35	14.08
253									961
254									962
255
256									967
257									972
258	16.53	1.65	0.84	14.73	14.10	13.84
259				16.33	13.85	12.72
260
261
262									979
263
264									981
265									982
266	17.49	2.34	0.67	13.87	12.55	11.99
267									983
268
269				15.13	13.25	12.40
270
271	13.89	0.53	0.31	13.00	12.51	12.42
272
273	16.57	1.96	0.98	14.19	13.46	13.10
274				15.53	12.77	11.46
275
276				15.46	13.56	12.51
277
278									997
279	16.53	2.34	1.37	13.84	13.08	12.59		Y
280									998
281
282	16.47	1.59	0.86	14.30	12.80	11.91	Y		1005
283				17.08	14.46	13.06
284
285				17.46	14.39	12.76			1012
286									1013
287
288									1018
289				14.39	12.53	11.59			1021
290				19.00	15.22	13.22			1023
291	17.89	2.52	0.86	13.75	12.06	11.19			1027
292
293				10.47	9.83	9.65
294				16.00	13.38	12.03			1030
295				13.45	12.45	11.91
296
297
298				15.57	13.20	12.19			1043
299				18.13	14.20	11.82			1046
300
301				14.74	12.43	10.97			1049
302									1051
303				16.83	14.45	13.37
304				15.23	13.11	12.17
305				15.89	13.98	13.18
306
307
308									1065
309				16.44	13.39	11.88			1067
310				15.12	13.08	12.01
311				16.14	13.81	12.44			1069
312	18.22	2.58	1.09	13.98	12.47	11.86
313
314				16.35	13.60	12.05			1079
315				16.66	14.14	12.97
316
317				12.12	11.52	11.40
318				19.92	18.37	17.64
319
320				14.21	12.47	11.79
321
322
323
324
325	14.75	0.93	0.50	13.47	12.85	12.65
326				19.50	18.25	18.02
327				11.85	10.87	10.25			1128
328	17.28	1.97	0.91	14.60	13.39	12.95
329
330				15.71	13.53	12.20			1132
331
332	15.32	1.41	0.76	13.41	12.58	12.21			1139
333				12.32	11.28	10.87			1148
334	17.12	2.47	1.54	14.10	13.27	12.74		Y
335
336									1158
337				17.31	14.19	12.16			1163
338				13.25	12.21	11.46			1164
339									1165
340				14.38	13.55	13.00
341				11.77	10.41	9.70			1172
342									1176
343				14.30	13.30	12.65
344
345
346				12.69	11.49	10.92			1179
347				14.57	13.82	13.33
348	15.21	1.51	1.31	12.80	11.49	10.71	Y	Y	1185
349				14.09	12.70	11.98
350				12.77	11.81	11.34
351
352				15.68	13.54	12.09			1188
353
354
355				10.56	9.62	8.84			1190
356
357	14.48	1.36	0.83	12.23	11.16	10.69		Y	1192
358
359
360	16.88	1.88	1.31	13.60	12.40	11.73		Y	1196
361
362	16.47	1.27	1.06	13.85	12.82	12.14	Y	Y	1198
363
364				17.68	15.11	13.79
365	16.88	1.87	1.16	15.04	13.84	13.05	Y	Y
366	15.79	1.66	1.10	13.76	12.82	12.37		Y	1203
367				17.83	16.46	15.67
368				18.61	16.90	16.14
369	16.52	1.74	0.88	14.75	14.18	13.88
370
371
372				15.25	13.07	11.35	Y		1222
373				12.00	11.43	11.28
374	16.84	1.55	0.63	14.33	13.30	12.91
375
376
377
378	16.07	1.79	0.51	13.27	12.12	11.67
379				5.09	4.46	4.45
380	18.06	1.40	0.85	15.94	15.10	14.78
381	14.42	2.16	0.55	10.50	8.94	8.23
382	17.54	1.14	0.52	15.90	15.23	14.81
383	14.56	0.73	0.42	13.54	12.93	12.81
384				10.71	10.44	10.41
385				17.85	16.69	16.22
386				13.88	12.77	12.37
387	16.53	1.60	0.61
388	16.66	2.06	1.01	13.13	12.52	12.26
389				12.67	11.48	10.73			1245
390	17.48	2.07	0.98	15.42	14.81	14.49
391	17.05	1.82	1.06	15.24	14.62	14.35
392	17.37	1.41	0.54	16.84	15.76	15.25
393				10.83	10.45	10.40
394				17.08	15.93	15.38
395	16.80	1.90	1.00	14.95	14.34	14.05
396	15.52	1.65	0.88	13.85	13.28	13.01
397	16.75	1.85	0.89	14.96	14.37	14.07
398	17.79	1.54	0.41	15.30	14.38	13.97
399	18.03	1.13	0.41	16.75	15.74	15.30
400
401
402	18.17	1.40	0.58	13.42	12.49	12.17
403				16.40	15.65	15.31
404
405	16.94	1.75	0.68	14.21	13.11	12.66
406	16.22	1.92	0.99	14.22	13.62	13.33
407
408	18.13	1.11	0.39	11.71	10.91	10.52			1214
409
410				13.57	12.73	12.44
411	15.55	1.01	0.47	13.98	13.22	12.98
412
413				7.67	7.08	6.94
414	16.10	1.20	1.15	14.34	13.41	12.96		Y	1232
415
416	15.32	1.75	0.93	13.55	12.93	12.65
417
418	17.03	1.61	0.75	14.79	13.89	13.58
419	15.75	1.09	0.58	16.88	16.11	15.79
420	15.32	0.89	0.34	11.94	11.71	11.66
421	18.22	1.24	0.62	16.30	15.52	15.23
422	16.39	1.70	0.72	13.93	12.92	12.54			1152
423	16.93	1.02	0.45	12.21	11.79	11.71
424	16.34	1.49	0.62	16.67	16.03	15.76
425	17.70	1.13	0.28	13.05	12.50	12.38
426				13.04	12.19	11.91
427	17.96	1.10	0.42	16.28	15.70	15.51
428	13.68	0.88	0.41	12.21	11.40	10.89			1231
429	18.49	1.11	0.41	13.10	12.49	12.28
430				12.16	11.42	11.24
431	15.24	1.33	1.25	13.11	11.87	11.05	Y	Y	1131
432
433				13.83	12.78	12.29			1147
434				13.35	12.24	11.69			1145
435	17.94	1.93	1.04	15.93	15.31	15.03
436	14.64	0.80	0.47	13.43	12.76	12.63			1099
437				15.10	13.61	12.99
438				11.46	11.12	11.05
439	15.74	1.26	0.83	13.88	13.06	12.64		Y	1138
440				13.97	13.02	12.67
441	15.29	1.14	0.63	13.80	13.09	12.90
442	14.32	1.71	0.92	12.56	11.96	11.72
443				13.75	13.16	12.91
444				11.65	11.38	11.30
445	17.04	1.91	0.61	15.41	13.60	12.71	Y		1062
446				15.23	13.07	12.11
447	14.62	1.26	0.61	12.75	11.94	11.69
448				13.79	12.37	11.79
449				14.72	13.86	13.63
450				10.55	9.85	9.44			1230
451	13.91	0.66	0.42	12.90	12.32	12.20
452				17.14	16.13	15.69
453	17.12	1.75	0.82	15.34	14.67	14.34
454	17.05	0.62	1.38	14.13	12.48	11.23	Y		1212
455				13.64	12.92	12.72
456				16.78	15.77	15.33
457	15.27	1.08	1.33					Y	1206
458				12.71	11.87	11.62
459	15.87	1.68	0.64	15.43	14.22	13.75
460				13.58	13.02	12.77
461	16.79	2.05	0.64	13.99	12.96	12.54
462	18.06	1.60	0.12	16.49	14.89	14.23	Y
463	16.10	1.91	1.05	14.11	13.53	13.24
464				10.35	9.79	9.64
465				10.47	10.13	10.14
466				10.54	10.28	10.26
467	18.17	1.56	0.82	16.04	14.23	13.43	Y
468				13.47	12.67	12.34
469	17.87	1.88	0.57	13.84	13.24	12.99
470				16.95	16.31	16.00
471	18.19	1.75	0.60	15.77	14.88	14.43
472	14.01	0.69	0.42	12.93	12.39	12.15
473	13.16	0.52	0.38	12.21	11.73	11.63
474	15.27	1.75	0.94	13.41	12.85	12.57
475				18.03	16.92	16.37
476				20.47	18.59	17.66
477				16.73	15.73	15.29
478	16.78	1.20	0.69	15.30	14.52	14.29			779
479				16.60	14.37	13.20			760
480	18.05	2.40	0.88	14.41	13.37	13.00
481	14.63	0.57	0.34	12.19	10.99	10.52	Y
482				19.80	18.26	17.39
483				13.56	12.84	12.49
484				13.81	12.80	12.44
485				12.97	12.34	12.12
486				20.05	18.49	17.74
487	17.30	1.93	0.99	15.32	14.75	14.44
488				11.91	11.45	11.33
489				16.61	15.70	15.28
490				8.08	7.66	7.48
491				13.54	12.98	12.88			808
492	17.13	1.90	0.59	14.51	13.58	13.18
493				18.56	17.33	16.82
494				15.76	14.54	14.03
495				15.24	13.78	13.16
496	15.72	1.43	0.76	14.10	13.46	13.22
497
498				16.20	15.35	14.85
499	13.29	0.90	0.40	11.91	11.30	11.19
500				20.90	18.51	17.55
501				17.82	16.57	16.05
502				15.50	13.39	12.49
503				14.41	13.76	13.52
504				13.39	12.26	11.92
505				14.99	13.29	12.56
506	18.33	1.81	0.83	13.60	12.58	12.21
507				13.40	12.24	11.64			742
508				14.26	13.22	12.85
509									732
510				19.91	16.18	14.15			697
511				14.68	14.10	13.80
512				13.42	12.84	12.70
513				17.27	15.80	15.22
514				12.35	12.08	11.94
515
516	14.18	1.37	0.73	15.80	14.51	13.98	Y
517				11.51	10.59	10.19
518	16.40	2.05	0.61	14.58	12.91	12.19			553
519	14.52	1.17	0.48	16.36	15.24	14.78
520				15.14	14.00	13.43
521	16.17	1.55	0.64	15.97	14.86	14.25			485
522
523	15.94	2.06	0.53	12.41	11.19	10.59
524				12.93	11.99	11.67
525	12.65	0.97	0.46	11.16	10.49	10.31
526				14.32	13.00	12.11			541
527				16.07	14.56	13.88
528				16.56	15.14	14.51
529				16.44	15.21	14.65
530
531				9.40	9.03	8.84
532	15.16	1.55	0.83	13.50	12.92	12.65
533
534	17.05	1.62	0.83	15.35	14.71	14.43
535				12.12	11.18	10.70			591
536				13.05	11.32	10.36			573
537				15.85	14.66	14.15
538				11.90	11.63	11.58
539				13.56	12.60	12.18			617
540	15.27	1.63	0.76	12.31	11.18	10.55			680
541	16.47	1.78	0.61	13.72	12.63	12.22
542				13.70	12.16	11.30
543				11.21	10.84	10.73
544	14.29	1.57	0.59	11.78	10.83	10.45
545	16.58	1.97	0.74	13.79	12.65	12.26			639
546				12.78	11.62	11.20
547				9.72	9.21	9.00			568
548	16.88	2.08	0.82	14.10	13.08	12.69
549	16.82	1.66	0.59	13.93	12.81	12.35			634
550				17.24	15.84	15.44
551				12.54	11.62	11.28
552	17.02	1.46	0.70	17.42	15.51	14.66	Y
553				16.47	15.44	14.91
554				12.33	11.27	10.86
555
556	16.60	1.45	0.75	13.88	12.38	11.76
557				17.33	14.17	12.63
558	16.01	2.81	0.72	14.72	12.29	10.69	Y
559	13.09	1.19	0.50	11.25	10.54	10.29			729
560	15.85	1.53	0.64	13.43	12.41	12.10
561	14.12	1.66	0.61	15.99	14.38	13.66	Y
562	15.78	1.67	0.66	13.14	12.13	11.71
563				12.99	11.30	10.49
564	16.14	2.34	0.69	12.37	11.00	10.42
565				11.33	10.52	9.98			439
566	17.06	2.13	0.96	12.90	11.96	11.71
567				12.56	11.52	10.96			500
568				13.32	12.17	11.47			524
569	15.12	1.43	0.70	12.91	12.00	11.73
570				13.58	13.50	13.33
571	15.07	1.44	0.62	13.36	11.94	11.07	Y		405
572	15.65	1.22	1.17	13.73	12.60	12.04		Y	444
573	15.66	1.34	0.62	13.45	12.54	12.27
574				14.78	13.67	13.21
575	16.89	1.88	0.97	14.92	14.31	13.99			487
576	15.22	1.50	0.65	12.62	11.72	11.35
577				16.15	15.14	14.67
578				13.74	13.15	12.88
579				11.73	11.48	11.39
580	17.36	1.70	0.55	17.10	15.97	15.38
581	17.70	2.30	1.12	14.97	14.03	13.65
582	16.47	2.31	0.34	12.71	11.31	10.72
583	17.15	1.29	0.47	11.80	10.89	10.39			374
584	17.19	2.01	0.89	14.54	13.59	13.18
585				14.95	13.82	13.37			501
586				11.64	11.37	11.29			501
587				13.71	12.38	11.78			514
588				7.13	6.86	6.54			402
589	18.15	1.62	0.69	15.91	14.99	14.35
590	15.80	1.23	0.57	13.86	13.04	12.75
591	15.87	1.67	0.64	13.25	12.21	11.89
592				13.59	12.40	11.95
593	16.94	2.26	0.78	13.90	12.86	12.42
594				16.53	15.67	15.32
595									564
596	15.88	1.28	1.45	13.20	12.21	11.73		Y	413
597	16.77	1.79	0.77	14.04	12.92	12.51
598	16.31	1.64	0.86	14.52	13.94	13.67
599	16.30	1.59	1.11	14.00	12.90	12.20	Y	Y	341
600	16.19	1.66	0.73	13.68	12.54	12.04			556
601				12.75	11.37	10.58			605
602	15.85	1.56	0.59	13.53	12.55	12.20
603	15.98	1.48	0.63	13.77	12.89	12.55
604
605	16.72	2.12	0.91	14.04	13.01	12.63
606				20.29	18.47	18.10			397
607	17.71	1.61	0.88	14.49	13.32	12.75			421
608	17.19	1.85	0.64	14.37	13.33	12.83
609				15.64	13.77	12.75
610				13.35	12.05	11.36			547
611	15.57	1.82	0.62	12.52	11.33	10.91
612	16.01	2.81	0.72	16.10	13.16	11.40	Y
613	16.42	1.92	0.72	13.31	12.18	11.77
614				14.20	13.27	12.98
615	15.92	1.64	0.55	12.84	11.99	11.75
616				16.12	15.06	14.47
617	15.93	1.94	0.76	12.79	11.62	11.07			461
618				15.22	13.72	13.05
619	17.37	1.73	0.83	14.66	13.61	13.19			482
620				12.02	11.10	10.75
621	14.75	1.14	0.64	13.34	12.63	12.45
622	16.82	1.70	0.64	14.20	13.16	12.76
623	14.58	1.53	0.55	12.35	11.54	11.22
624				14.17	12.80	12.21
625				11.01	10.71	10.65
626
627	14.86	1.90	0.66	11.92	10.77	10.35
628	15.96	1.67	0.68	13.30	12.25	11.88
629				8.28	7.84	7.64
630				10.96	10.63	10.52
631				12.39	11.13	10.52			563
632	16.60	2.07	0.64	13.57	12.29	11.85
633	14.33	1.57	0.61	11.88	10.88	10.58
634				14.87	13.28	12.41			488
635	17.05	2.13	0.72	13.89	12.80	12.34
636				15.35	13.95	13.36
637	15.18	1.61	0.60	12.77	11.72	11.38
638	16.80	2.58	0.66	12.48	10.86	10.25
639	16.87	1.89	0.62	13.77	12.58	12.15
640	17.60	1.44	0.58	12.88	11.82	11.38			515
641				13.34	12.57	12.21
642	16.14	1.99	0.65	11.21	10.35	10.01			582
643				9.47	9.39	9.36
644	16.58	2.14	0.81	13.55	12.45	12.02
645	17.08	1.66	0.44	13.10	11.58	10.97
646	16.30	1.80	0.70	13.50	12.33	11.86
647	15.94	2.06	0.53	12.41	11.19	10.59
648	17.25	1.55	0.66	16.69	15.50	14.93
649	17.96	1.34	0.76	17.20	15.43	14.67	Y
650
651				13.68	12.68	12.30
652	16.06	1.82	0.74						626
653				14.80	13.52	12.97			656
654
655	15.25	1.30	0.90	13.07	12.02	11.31		Y
656
657				16.65	15.26	14.57
658				16.12	15.38	15.02
659	15.97	1.84	0.74	13.05	11.88	11.41
660				16.28	14.57	13.85
661	15.32	1.69	0.64	12.87	11.85	11.50
662	15.23	1.54	0.73	12.71	11.59	10.98			203
663				16.06	14.93	14.37
664				11.06	10.37	10.02
665	17.05	2.06	0.86	13.52	12.14	11.38			193
666	16.99	1.81	1.05	15.30	14.71	14.42
667				16.51	15.97	15.71			248
668				14.20	12.71	11.88			159
669	16.13	1.45	0.43	16.13	15.15	14.78
670				10.86	10.28	10.18
671
672				18.72	17.01	16.30
673				17.11	16.00	15.50
674				17.75	16.30	15.65
675				15.96	13.94	12.77			229
676				15.93	15.07	14.64
677				16.26	15.26	15.03
678				11.52	11.26	11.24
679				16.52	15.36	14.80
680				16.42	15.36	14.87
681				16.41	15.44	15.00
682				15.23	12.52	11.01			289
683				15.93	13.46	12.33
684				11.75	11.42	11.36
685				16.61	15.65	15.21
686	15.83	1.83	0.96	14.07	13.49	13.23
687				9.14	8.89	8.87
688	17.57	1.73	0.52	17.55	15.56	14.66	Y
689				14.24	12.69	12.01
690									267
691				19.32	17.86	17.54
692				18.36	16.96	16.40
693				14.35	12.80	12.19
694	16.93	1.87	1.05	15.23	14.62	14.34
695				10.30	9.88	9.74
696				17.10	14.02	12.30			244
697				11.02	10.70	10.62
698	15.74	0.93	0.46	20.64	16.79	14.98	Y
699	15.17	0.95	0.54	16.24	14.61	13.88	Y
700	15.43	1.72	0.90	13.61	13.02	12.76
701				12.15	11.49	11.25			347
702				16.71	13.86	12.17			240
703				17.29	15.14	14.17
704				16.33	13.81	12.65
705	12.74	0.51	0.33
706				12.53	11.88	11.64
707
708				17.09	15.93	15.40
709				14.69	14.13	13.89			108
710									155
711				17.60	16.52	16.07
712	15.50	1.98	0.99	13.60	13.06	12.77
713	16.60	2.02	0.99	14.66	14.10	13.79
714				17.49	15.86	15.15
715				16.86	15.07	14.28
716	17.33	2.02	1.00	15.32	14.72	14.42
717				11.92	11.50	11.41
718	15.30	1.01	0.59	14.02	13.34	13.15
719	12.21	1.76	0.88	10.45	9.87	9.59
720	16.46	1.34	0.35	15.90	15.10	14.67
721	17.10	1.49	0.45	14.90	14.15	13.84

Table 5. Table 5: Optical/NIR photometry for X-ray undetected stars with IR/H α 𝛼 \alpha excess. Full table in electronic format only.

Seq	RA	Dec	$i$	$r - i$	$r - H α$	$J$	$H$	$K$	IR	H $α$	RGS11
no.									excess	excess	number
722	311.40294	45.08670				14.27	11.12	8.82	Y
723	311.52945	44.78329				18.36	14.83	12.29	Y
724	311.53239	44.77889	17.24	1.39	1.47	14.09	12.99	11.90	Y	Y
725	311.55911	44.87168				16.97	14.68	12.89	Y
726	311.56617	43.70630				14.34	13.48	12.59	Y
727	311.57703	44.74357	18.29	1.23	0.45	14.51	12.68	11.83	Y
728	311.61675	44.04525				15.47	13.82	12.45	Y
729	311.67674	43.75285	17.36	1.98	1.28	15.02	14.15	13.66		Y
730	311.68683	45.21762				14.36	11.17	8.75	Y
731	311.70190	44.18731	16.78	2.17	1.66	13.53	12.46	11.95		Y
732	311.71429	44.92656	17.22	1.64	0.76	14.46	13.38	12.55	Y
733	311.71948	44.91088	15.76	1.25	0.55	13.46	12.46	11.66	Y
734	311.72259	44.39995	18.03	1.46	0.75	16.34	14.26	12.97	Y
735	311.72326	43.76692	17.89	2.21	1.65	15.23	14.54	14.07		Y
736	311.74237	44.89695	16.83	1.11	0.36	14.54	13.45	12.43	Y
737	311.74626	43.68682	16.51	3.19	0.62	12.88	10.21	8.16	Y
738	311.76965	43.22022				16.45	15.01	13.63	Y
739	311.77003	43.81984	17.55	1.16	2.29	15.18	14.26	13.56	Y
740	311.82935	43.36731				17.05	15.70	14.50	Y
741	311.84319	43.83651	15.38	1.16	0.84	13.70	12.73	12.41		Y

Equations24

(J - H)_{c} \equiv (J - H) + 0.526 (H - K)

(J - H)_{c} \equiv (J - H) + 0.526 (H - K)

A_{V} \sim ((J - H)_{c} - 0.75) \times (A_{V} / (E (J - H) + 0.526 E (H - K)))

A_{V} \sim ((J - H)_{c} - 0.75) \times (A_{V} / (E (J - H) + 0.526 E (H - K)))

J_{2 M A S S} - J_{U K I D S S} = 0.0188 (J - H)_{U K I D S S} .

J_{2 M A S S} - J_{U K I D S S} = 0.0188 (J - H)_{U K I D S S} .

(J - H)_{U K I D S S} = 0.9217 (J - H)_{2 M A S S} .

(J - H)_{U K I D S S} = 0.9217 (J - H)_{2 M A S S} .

(H - K)_{U K I D S S} = 1.04236 (H - K)_{2 M A S S} .

(H - K)_{U K I D S S} = 1.04236 (H - K)_{2 M A S S} .

r_{I P H A S} - r_{V P H A S} = 0.02448 + 0.0984 (r - i)_{V P H A S}

r_{I P H A S} - r_{V P H A S} = 0.02448 + 0.0984 (r - i)_{V P H A S}

i_{I P H A S} - i_{V P H A S} = 0.070283 - 0.01477 (r - i)_{V P H A S} .

i_{I P H A S} - i_{V P H A S} = 0.070283 - 0.01477 (r - i)_{V P H A S} .

A_{r} / A_{V} = 0.793

A_{r} / A_{V} = 0.793

A_{i} / A_{V} = 0.601

A_{i} / A_{V} = 0.601

A_{J} / A_{V} = 0.282

A_{J} / A_{V} = 0.282

A_{H} / A_{V} = 0.175

A_{H} / A_{V} = 0.175

A_{K} / A_{V} = 0.1187

A_{K} / A_{V} = 0.1187

Peer Reviews

No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.

Videos

No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.

Full text

11institutetext: INAF - Osservatorio Astronomico di Palermo G.S.Vaiana, Piazza del Parlamento 1, I-90134 Palermo, Italy

11email: [email protected] 22institutetext: Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge MA 02138 USA.

X-ray survey of the North-America and Pelican star-forming complex

(NGC7000/IC5070)

Francesco Damiani 11

Ignazio Pillitteri 1122

and Loredana Prisinzano 11

(Received date / Accepted date)

Abstract

*Aims. * We present the first extensive X-ray study of the North-America and Pelican star-forming region (NGC 7000/IC 5070), with the aim of finding and characterizing the young population of this cloud.

*Methods. * X-ray data from Chandra (four pointings) and XMM-Newton (seven pointings) were reduced and source detection algorithm applied to each image. We complement the X-ray data with optical and near-IR data from the IPHAS, UKIDSS, and 2MASS catalogs, and with other published optical and Spitzer IR data. More than 700 X-ray sources are detected, the majority of which have an optical/NIR counterpart. This allows to identify young stars in different stages of formation.

*Results. * Less than 30% of X-ray sources are identified with a previously known young star. We argue that most X-ray sources with an optical/NIR counterpart, except perhaps for a few tens at near-zero reddening, are likely candidate members of the star-forming region, on the basis of both their optical/NIR magnitudes and colors, and of X-ray properties like spectrum hardness or flux variations. They are characterized by a wide range of extinction, and sometimes near-IR excesses, both of which prevent derivation of accurate stellar parameters. The optical color-magnitude diagram suggests ages between 1-10 Myrs. The X-ray members have a very complex spatial distribution with some degree of subclustering, qualitatively similar to that of previously known members. The detailed distribution of X-ray sources relative to the objects with IR excesses identified with Spitzer is sometimes suggestive of sequential star formation, especially near the “Gulf of Mexico” region, probably triggered by the O5 star which illuminates the whole region. We confirm that around this latter star no enhancement in the young star density is found, in agreement with previous results. Thanks to the precision and depth of the IPHAS and UKIDSS data used, we also determine the local optical/IR reddening law, and compute an updated reddening map of the entire region.

Key Words.:

**Open clusters and associations: individual (NGC7000, IC5070) – stars: pre-main-sequence – X-ray: stars **

1 Introduction

The star-formation region associated with the North-America (NGC 7000) and Pelican (IC 5070) Nebulae in Cygnus have received increased attention in the last decades. The two nebulae are catalogued as separate objects because of their visual appearance, but are now commonly regarded as parts of the same physical gas and dust cloud. The properties of the region were reviewed by Reipurth and Schneider (2008). The ionizing source of the nebulae has remained a mystery for decades, but was at last identified with a highly reddened O5 star (2MASS J20555125+4352246, $A_{V}\sim 9.6$ ) by Comerón and Pasquali (2005), hidden by the dark dust cloud LDN935, lying between NGC 7000 and IC 5070. This star is remarkably isolated according to these authors: there are no other massive stars close to it, or they would have been easily detected even if highly obscured.

Since the work of Herbig (1958, henceforth H58) it was known that several tens young pre-main-sequence (PMS) stars are found in this region. Welin (1973) presented also an objective-spectra study of emission-line stars in the region, and a few more young stars were studied spectroscopically by Corbally, Straižys and Laugalys (2009). Narrow-band filter studies have also revealed many emission-line star candidates (e.g. Witham et al. 2008, Armond et al. 2011), as well as many Herbig-Haro flows (Bally and Reipurth 2003, Armond et al. 2011, and also Bally et al. 2014). The strong obscuration towards many parts of the cloud undoubtedly prevents many other PMS stars to be found optically, but was no obstacle for the sensitive survey for Young Stellar Objects (YSOs) made with the Spitzer Space Observatory (IRAC camera, Guieu et al. 2009; IRAC $+$ MIPS, Rebull et al. 2011, henceforth RGS11). Cambrésy et al. (2002) also studied this region using 2MASS data, tracing spatial extinction variations, and finding nine clusters of near-IR (NIR) objects.

The distance of the cloud was estimated to be in the range 500-600 pc by Laugalys et al. (2006, 2007). The line of sight towards Cygnus is tangent to the corresponding spiral arm, and therefore objects at vastly different distance from the Sun can appear visually close in the sky: the Cyg OB2 association for example, only a few degrees away from NGC7000, lies at a much larger distance $\sim 1.5$ kpc. In the direction of the North-America/Pelican (NAP), Straižys, Corbally and Laugalys (2008) find a larger-than-typical $E(J-H)/E(H-K)$ ratio of 2.0.

The NAP region is also known to host two PMS stars in the FU Ori class: V1057 Cyg and V2493 Cyg. This latter was only known as a Classical T Tauri star (CTTS) named HBC722 before its outburst in 2010, and intensively studied thereafter (Semkov et al. 2010, Covey et al. 2011, Aspin 2011, Miller et al. 2011, Green et al. 2011, Kóspál et al. 2011, 2013, Dunham et al. 2012, Semkov et al. 2012, Liebhart et al. 2014, and Lee et al. 2015). V1057 Cyg was observed in X-rays (but not detected) by Skinner et al. (2007), while a positive X-ray detection of V2493 Cyg was presented by Liebhart et al. (2014). No other published X-ray study exists of this region, to our knowledge.

The strong and nonuniform obscuration towards the cloud, and its large size ( $\sim 2^{\circ}$ ) are formidable difficulties when attempting to characterize the global young-star population of this star-forming region. The Spitzer RGS11 study of YSOs is extremely important in this respect, since it covered basically all the cloud, and was sensitive to even highly obscured objects. Since the selection of YSOs in RGS11 is based on the existence of non-photospheric excess IR emission from circumstellar dust (disks), it is however biased against diskless PMS stars (Class III objects in the SED-based nomenclature, or Weak-line T Tauri stars - WTTS, as opposed to CTTS - in the spectroscopic nomenclature). At typical ages of PMS stars, both CTTS and WTTS are however bright X-ray sources (with X-ray luminosities in the range $\log L_{X}\sim 29-31$ erg/s). Therefore, we have obtained new X-ray observations at selected positions in the NAP Nebula, using both XMM-Newton and Chandra X-ray observatories, with the purpose of obtaining a more complete and unbiased census of the PMS population of this star-forming region. In addition, we analyze here other X-ray datasets from these observatories, which were only partially examined in the published literature.

Moreover, we take advantage of two important wide-area optical and NIR surveys: IPHAS (Drew et al. 2005) and UKIDSS (Lawrence et al. 2007), covering the entire cloud, with limiting magnitudes far deeper than most other optical/NIR catalogues available in the same region.

This paper is structured as follows: Section 2 describes the X-ray data presented, and Section 3 their analysis. Section 4 describes the optical/NIR data also used in this work. Section 5 presents all results obtained. Section 6 is a discussion of the results, and Section 7 summarizes our conclusions.

2 X-ray observations

The log of the X-ray observations used in this work is reported in Tables 1 and 2. We obtained three new XMM-Newton EPIC observations and two new Chandra ACIS-I observations (ACIS-I ObsIds 13647 and 15592 are in fact the same observation split in two segments, while 13648 is a distinct pointing). Four archive XMM-Newton observations are also analyzed (of which ObsIds 0656780701 and 0656781201 nearly co-pointed), as well as one ACIS-S observation: this latter has a different field of view (FOV) than the ACIS-I detector, and a slightly different sensitivity. All XMM-Newton observations, made with the EPIC camera, are composed by a set of three simultaneous observations with the PN, MOS1, and MOS2 detectors, approximately co-pointed but having different FOV shapes; PN is the most sensitive of the three, while the MOS1 (MOS2) effective area is comparable to that of ACIS-I. All XMM-Newton observations were made using the Medium filter. The Chandra ACIS images have an on-axis PSF much narrower ( $\sim 0.5$ arcsec) than XMM-Newton EPIC images ( $\sim 4$ arcsec): this implies not only a better spatial resolving power, but also that less counts are needed for a significant source detection ( $\sim 4$ X-ray counts vs. $\sim 40$ for the PN+MOS combination) because the background contribution in the EPIC images is usually non-negligible, while it is in ACIS images. Far from optical axis, the PSF degrades sensibly in ACIS images, while that of XMM-Newton images is rather uniform across the FOV.

We tried to optimize our X-ray pointings, guided by the large-scale distribution and local spatial density of YSOs from Guieu et al. (2009). Therefore, we have chosen ACIS-I where the YSO density was highest, but preferred XMM-Newton with its larger FOV for the sparser regions. Figure 1 shows a Digital-Sky-Survey (DSS) red image of the region, with indicated all the X-ray observations studied here, and also the RGS11 YSOs, and H58 PMS stars; the illuminating O5 star, and the two FU Ori objects are also indicated, as well as the NIR clusters found by Cambrésy et al. (2002). The sub-regions with the highest YSO density are the so-called “Gulf of Mexico”, covered by our ACIS field 13648, and the “Pelican”, covered by our ACIS fields 13647 and 15592. The less-obscured part of the cloud containing V1057 Cyg, covered by XMM-Newton archive ObsId 0302640201, contains only few YSOs.

Besides the studies mentioned above, more evidences can be presented in favour of the North-America and Pelican Nebulae being part of the same cloud; this is especially important in this part of the sky because of the mentioned tangent-arm geometry, and in this particular nebula to ascertain that the foreground obscuring cloud is physically associated with the bright nebulae and is not much closer along the line of sight. For example, the WISE (Wright et al. 2010) images in four NIR bands at 3.4, 4.6, 12, and 22 $\mu$ demostrate the presence of dense, hot dust behind the dark nebula LDN935 (Figure 2), with a geometry approximately centered on the illuminating O5 star. The distance of the dark cloud from us is therefore the same as the distance of the bright nebulae oscured by it. The region with the highest YSO density, just S-E of the O5 star and inside our ACIS 13648 field, is also seen in the WISE image to be one of highest obscuration.

The same qualitative conclusion that the North-America and Pelican Nebulae are the same physical cloud is reached by inspecting an optical emission-line image, obtained using narrow-band filters centered at the [O III], H $\alpha$ , and [S II] optical lines, shown in Figure 3. The ionization (highest for [O III]) has a global pattern, centered close to the O5 star; there is no other obvious ionization center, based on the optical-line image.

All X-ray images studied here are shown in Figures 4, 5, and 6. In these true-color images, the red (green, blue) intensity is proportional to detected X-ray counts in the soft (medium, hard) X-ray band. Blue sources are typically highly absorbed objects, with a strong low-energy cutoff in their X-ray spectrum. The Chandra FOVs are indicated, as well as the O5 star and the FU Ori objects.

3 X-ray data analysis

The X-ray datasets were processed using standard software packages (CIAO v4.8 for Chandra and SAS v11 for XMM-Newton data), and exposure maps at a representative energy of 1 keV were computed using the same packages. Source detection was made using PWDetect (v1.3.2) for Chandra data, and its XMM-Newton analogue PWXDetect (Damiani et al. 1997a,b). The front- and back-illuminated chips of ACIS-S ObsId 14545 were analyzed separately. ACIS-I ObsIds 13647 and 15592, sharing the same pointing direction and roll angle, were only analyzed jointly. This was also the case for archive XMM ObsIds 0656780701 and 0656781201. Spurious detections associated with diffraction spikes or out-of-time events (Fig. 5, panel $a$ ; Fig. 6, panel $a$ ) were manually eliminated. We then merged all individual X-ray detection lists according to computed position errors, separately for XMM-Newton and Chandra, giving priority to highest-significance detections. Thus, each detected X-ray source receives its IAU-recommended instrument-specific designation. The match and merging of XMM-Newton and Chandra detection lists was made in a subsequent step, taking in mind the much better spatial resolution of this latter, and therefore giving priority to the Chandra source positions and properties in ambiguous cases (see e.g. the tight group of sources near HBC 722 in Fig. 5, panel $c$ , which is unresolved by XMM-Newton in Fig. 6, panel $b$ ). The final X-ray source list comprises 721 objects, of which 378 ACIS detections (of which 34 with an XMM-Newton counterpart), and 343 XMM-Newton-only detections. The chosen detection threshold, corresponding to approximately one spurious detection per field, ensures that no more than $\sim 10$ of the 721 detections are spurious. The positions of all X-ray detections are shown in Figure 7.

4 Auxiliary data: optical and near-IR

We have complemented the X-ray data with data taken from the IPHAS DR2 (Barentsen et al. 2014), 2MASS PSC, and UKIDSS DR10plus GPS (Lawrence et al. 2007; table “reliableGpsPointSource”). All of these surveys cover the entire spatial region considered here. We extracted sources from a region of radius $1.5^{\circ}$ centered on $(RA,Dec)=(313.7,44.4)$ . This yielded 1117062 IPHAS sources, however after applying the recommended screening (keeping only sources with flags a10=1 and a10point=1, i.e. point-like sources with high signal-to-noise ratio in all bands) their number reduces to 161635 sources.

The screened 2MASS PSC source list (flag ph_qual different from E,F,U,X, flag cc_flg different from p,d,s) contains 339774 sources. The UKIDSS source list instead contains 980770 sources. This is much larger than the number of 2MASS sources because of the greater depth of the UKIDSS survey; however, the UKIDSS data do not supersede the 2MASS data, since they saturate at the bright end ( $J\leq 12$ ), where 2MASS still contains reliable data. We therefore use both sets of data, after an examination of their agreement on the sources common to both (see Appendix A). For these latter, the photometric errors are much lower in the UKIDSS than in the 2MASS magnitudes, so we adopt the UKIDSS ones whenever available. At large reddening, often found in this region, the UKIDSS photometry differs from 2MASS, so a slight recalibration was applied to agree with the 2MASS system (Appendix A).

We matched each of these source catalogs with our X-ray source list, up to a maximum offset of $4\sigma$ , where $\sigma$ is the combined positional error from our X-ray detection code, from the 2MASS PSC error err_maj, or set fixed to 0.07*′′* for the IPHAS and UKIDSS sources. There are 568 2MASS, 235 IPHAS, and 300 UKIDSS counterparts to our X-ray sources.

The number of total counterparts using the combined NIR catalog is instead 548, lower than the 2MASS counterparts alone because of incomplete sets of magnitudes for several stars.

115 X-ray sources remained unidentified. The number of spurious matches between X-ray and optical/NIR sources is difficult to evaluate, since assumptions usually made to compute it (uniform spatial distributions of the two matched sets) are not fulfilled here. As we have seen above, X-ray sources are found near regions of strong obscuration, where the optical/NIR source density is much smaller than average, and changes on very small spatial scales. Moreover, the PSF (and source position error) of the XMM-Newton data is much larger than that of the Chandra ACIS data, so that even if the optical/NIR spatial density were uniform there is a higher chance of spurious matches for XMM-Newton X-ray sources than for the Chandra ACIS sources.

Finally, we positionally matched our X-ray source list with the YSOs from RGS11, obtaining 184 matches out of all 802 YSOs falling in our X-ray FOVs (by class: 33/189 for flat-spectrum YSOs, 23/195 for Class I, 123/370 for Class II, 4/23 for Class III, and 1/25 for unclassified YSOs). Of the H58 stars, 45 were falling in the X-ray FOVs and 31 were X-ray detected. It is worth remarking that the ACIS fields yielded larger detection percentages than the XMM-Newton fields, whose higher background resulted in a lower sensitivity. The median threshold X-ray luminosity for ACIS detection was found to be $\log L_{X}\sim 29.9$ erg/s, while the corresponding value for XMM-Newton is $\log L_{X}\sim 30.4$ erg/s, at the average absorption values inferred for these YSOs (see below). Considering all ACIS FOVs, 115 YSOs were detected out of 373 observed (by class: 25/94 flat-spectrum, 17/118 Class I, 72/132 Class II, and 1/8 Class III). The corresponding numbers for the XMM-Newton FOVs are 83 detections out of 551 observed YSOs (by class: 11/136 flat-spectrum, 10/115 Class I, 58/274 Class II, and 3/17 Class III).

Our X-ray source properties and identifications are reported in Tables LABEL:table1 and LABEL:table2.

landscape

5 Results

5.1 Distance

The deep IPHAS photometry enables us to perform a new determination of distance, relying upon the assumption that the obscuring dark cloud LDN935 lies immediately before the star-forming region, as argued above. The method (already used by Prisinzano et al. 2005 to determine the distance of the young cluster NGC 6530) fits the lower envelope of datapoints in the color-magnitude diagram (CMD) to the shape of the main sequence of field stars, which are the lowest-luminosity field stars at each given color. It is therefore independent of any assumption on the cluster age or specific isochrone set. To apply the test we have selected two heavily obscured regions in LDN 935 (12-arcmin radius circles around $(RA,Dec)=(314.2,43.6)$ and $(312.9,44.9)$ , respectively), whose CMD using IPHAS data is shown in Figure 8. Also shown is a 10-Gyr isochrone from Baraffe et al. (2015; henceforth BHAC) at zero reddening and distance of 560 pc, which provides a good fit to the lower envelope of datapoints (solid), at least for $r-i<1$ . The dashed curves ( $\pm 20$ % in distance) moreover suggest that the distance is unlikely to be larger than $\sim 650$ pc. Therefore, the new data are in good agreement with the accepted distance of the complex (560-600 pc, Laugalys et al. 2006, 2007). Since the BHAC tracks are not currently available from the IPHAS filter set we have recalibrated them for this filter set starting from those for the Johnson/Cousin filters, as explained in Appendix B.

5.2 H $\alpha$ -emission stars

The IPHAS survey also provides a $r-H\alpha$ index, useful to select H $\alpha$ -emission objects over wide sky areas. A $r-H\alpha$ vs. $r-i$ diagram for NAP is shown in Figure 9. Datapoints in the upper part of the diagram are emission-line stars. In particular, we show with a dashed line the color-dependent limit used by Kalari et al. (2015) to select CTTS stars. Almost all of the H58 PMS stars, and most of the RGS11 YSOs fall above that limit. We have therefore selected all stars significantly above that line ( $4\sigma$ above errors) as candidate CTTS. However, this choice yielded hundreds objects falling too low in the optical CMD ( $i>18$ , $r-i\sim 1$ , much below the ZAMS at the NAP distance), and mostly in the N-E quadrant of the surveyed region, i.e. spatially far from the known YSOs, that are thus unlikely to be young stars in the NAP. These are probably unrelated emission-line stars at much larger distances, and are therefore not included in our emission-star list, which comprises 153 stars (of which 30 detected in X-rays). The spatial distribution of accepted emission-line stars selected from the $r-H\alpha$ index is shown in Figure 7.

5.3 Optical and near-IR color-color diagrams

Different color-color diagrams can be used to estimate the amount of reddening and the possible presence of non-photospheric color excesses, likely originated in circumstellar dusty disks. The $(J-H,H-K)$ diagram for the entire NAP region is shown in Figure 10. In agreement with Straižys, Corbally and Laugalys (2008), we find that the Rieke and Lebofsky (1985) reddening-vector slope does not adequately describe the slope of datapoints in this diagram; therefore, we devote Appendix C to the careful determination of the reddening vector slopes for all independent color pairs in the NAP optical/NIR catalog. This redetermined reddening vector is shown in Fig. 10 and in all following color-color diagrams. To the right of the main locus of reddened normal photospheres, stars with K-band excess emission are found. We have set a fiducial limit to define such stars as the dashed line in the Figure. Stars significantly ( $>4\sigma$ ) to the right of this line are selected as NIR-excess objects, or candidate CTTSs (orange triangles in the Figure). The complete list of NIR-excess objects includes stars selected from other optical/NIR color-color diagrams (see below), hence the presence of several of them also to the left of the fiducial limit in Fig. 10. It should be remarked that this diagram, although widely used, is not a very efficient tool to select CTTSs: none of the CTTSs found by H58 (green squares) falls to the right of the limiting line in this diagram. Also very few of the RGS11 YSOs are found in the CTTS region of the diagram.

We have studied the properties of several mixed optical/NIR diagrams in the young cluster NGC 6530 (Damiani et al. 2006), which enable the selection of many more NIR-excess stars than the $(J-H,H-K)$ diagram. Therefore, we use similar mixed optical/NIR diagrams also for the NAP stars. Figure 11 is a $(r-i,H-K)$ diagram, where we again have drawn a fiducial line (with the slope of the reddening vector, see Appendix C), sufficiently distant from the bulk of stars, separating normal reddened photospheres (to its left) from NIR-excess stars, whose NIR colors are too red compared to the respective $r-i$ colors for any reddening value. The usefulness of this diagram is immediately seen by considering that here most of the H58 CTTSs and of the optically detected RGS11 YSOs are found to the right of our fiducial limit, together with other tens NIR-excess stars (orange triangles) not present in previously-known catalogs. The bulk of normal field stars are instead found along a reddened-photosphere locus, well reproduced by the available BHAC models (blue lines) and reddening vector. The magenta segment of the BHAC isochrones represents the locus of (unreddened) stars with $M>1M_{\odot}$ ; the upper envelope of datapoints is instead populated by the lowest-mass dwarf stars (isochrones are shown down to a minimum mass $M=0.08M_{\odot}$ ). Most of the X-ray sources in the NAP region do not show NIR excesses, neither from Fig. 11 nor from Fig. 10. Some of them follow well the zero-reddening isochrones, down to the substellar-mass limit, while in general Figs. 10 and 11 suggest that they are characterized by a wide range of reddening. The same conclusion was reached in Section 2 above from the visual inspection of the true-color X-ray images of Figs. 4-6.

Another useful diagram is $r-i$ vs. $J-H$ (Fig. 12) although in this case the number of NIR-excess stars selected is smaller than from Fig. 11. However, this color combination enables us to identify the lowest-mass stars more securely than previous diagrams, as it breaks the near-degeneracy between intrinsic stellar color and reddening, for masses below $\sim 0.3M_{\odot}$ (green curves in Fig. 12 are BHAC evolutionary tracks for the lowest masses), as long as a star has photospheric colors. An even more detailed, non-degenerate determination of mass and reddening for individual stars is made possible by the rarely-used, but very interesting, $(r-i,i-H)$ diagram shown in Figure 13. The high-precision IPHAS and UKIDSS photometry undoubtedly are a major ingredient for this representation being so useful. Dwarf M stars, with $M\leq 0.5M_{\odot}$ , stand out clearly above the main locus of more massive stars, and are therefore effectively selected using this diagram. Most of them are unreddened ( $2<i-H<3$ ), of which 34 detected in X-rays. This diagram indicates that the majority of X-ray sources having an optical counterpart have instead larger reddening, in the range $A_{V}\sim 2-4$ . Only 3-4 of the H58 CTTSs have inferred masses $M\leq 0.5M_{\odot}$ , while all others are more massive (if their $i-H$ color is photospheric, which may not be strictly true, see Fig. 11). The few X-ray sources to the left of the unreddened isochrones are not easily justified by any current model: their discrepant colors might arise from spurious matches between the IPHAS and 2MASS/UKIDSS catalogs, or from variability in the optical or NIR bands.

We have estimated the number of foreground X-ray sources as in Pillitteri et al. (2013), by integrating the field-star X-ray luminosity function (Favata and Micela 2003) up to the NAP distance, and down to the limiting X-ray flux values appropriate to our X-ray observations (see Sect. 5.8 and Fig. 28). We estimate that about 67 foreground sources are detected cumulatively in all XMM pointings, and 18 in all ACIS pointings, for a total of $\sim$ 85 foreground sources not related to the NAP. Being older than the NAP members, these are expected to be found among the softest detected X-ray sources (Güdel et al. 1997). The unreddened M stars found above, and many other X-ray sources found along the unreddened sequence in the diagram of Figure 13, are therefore the best candidates as foreground sources.

The number of NIR-excess stars is 208 (of which 29 detected in X-rays, and 38 common to the H $\alpha$ -excess list), and their spatial distribution can be seen in Fig. 7, with the maximum density found in the “Pelican” region. The 273 X-ray undetected NIR-excess and H $\alpha$ -excess stars are listed in Table 5.

5.4 Color-magnitude diagrams

Figure 14 is an optical CMD for the whole NAP region. Comparison with Fig. 8 shows that thousands background stars are observed behind the cloud. Since no reddening correction was applied here, the apparent masses of e.g. the H58 stars, which as seen above are reddened by several magnitudes in the $V$ band, are much lower than their actual values, in most cases larger than $0.5M_{\odot}$ as discussed above. The few tens X-ray sources and NIR-excess stars below the 10-Gyr isochrone are not necessarily lying at larger distances: in fact, they share the same position in this CMD as many of the RGS11 YSOs. Below-ZAMS NIR-excess objects were already found in other young clusters like NGC 6530 (Damiani et al. 2006) or NGC 6611 (Guarcello et al. 2010), and may be attributed to photospheres obscured by edge-on disks, seen only in scattered light.

Since datapoints shown in Figure 14 have all errors less than 0.1 mag, attributing their position in the CMD to errors seems instead unlikely.

Considering X-ray sources, there is no clear sequence or cluster locus in the CMD, probably because of the large scatter in extinction from star to star. Estimating individual extinction values is subject to large uncertainties, as we will discuss in the following. Two-thirds of X-ray sources lack an IPHAS counterpart, probably because they are too highly reddened. Figure 15 shows therefore the NIR CMD $(J,J-H)$ . The frequency and intensity of non-photosperic dust emission in these NIR bands is probably lower than in the $K$ band, from the comparison of Figs. 11 and 12. The distribution of datapoints, elongated parallel to the reddening vector, suggests that indeed reddening, rather than $H$ -band excess, is responsible for most of the spread towards red colors, by up to $A_{V}\sim 35$ for the most reddened X-ray sources and YSOs with a NIR counterpart. A considerable number of X-ray sources has inferred $A_{V}\geq 10$ , if indeed their $J-H$ color is photospheric.

Finally, Figure 16 shows the $(H,H-K)$ diagram. The spread towards red colors is here probably due to a combination of reddening and $K$ -band excess emission. The diagram shows that several tens new NIR-excess sources (not identified with a YSO from RGS11) are much fainter objects (with $H>15$ ) than these latter. The majority of X-ray sources has $H-K\leq 0.5$ , no NIR excesses, and $H$ magnitudes fainter than the H58 stars.

In the presence of strong differential reddening, as we discuss below, incompleteness affects the optical CMD much more than the NIR CMD: from Figure 14 we see that while for low reddening the IPHAS photometry reaches down to the sub-stellar limit at the NAP distance and ages $\leq 3$ Myr, the mass completeness limit rises rapidly for increasing extinction (e.g. $\sim 1M_{\odot}$ for $A_{V}\sim 5$ ). Our combined NIR catalog reaches at least 3-4 magnitudes deeper than the substellar limit at the same age, and is moreover much less sensitive to extinction (Figures 15 and 16), which accounts for the much larger number of NIR counterparts to X-ray sources (548) compared to optical counterparts (235).

5.5 Extinction and reddening

The wide range of extinction indicated by the above diagrams may have a local component, arising in the individual circumstellar environments, but also shows definite large-scale patterns, as shown by Cambrésy et al. (2002) using 2MASS data. Here we take advantage of the more precise UKIDSS NIR data to build a more detailed extinction map of the NAP, based on the average $J-H$ color, as shown in Figure 17. Optical extinction is approximately 10 times the average $J-H$ (minus 0.5), so that the most obscured regions correspond to $A_{V}\sim 35$ , and the “green” regions in the map correspond to $A_{V}\sim 15$ .

The $J-H$ color may be considered as the best indicator of reddening for our NAP candidate PMS members, either X-ray detected or from H $\alpha$ - or NIR excess: it is available for most candidate members (548/721 X-ray sources, 817/994 X-ray/H $\alpha$ /NIR-excess sources), is less affected by non-photospheric emission than the $K$ band magnitudes, and normal stars fall within a small $J-H$ color range (Fig. 12), especially for $M<1M_{\odot}$ . The mass dependence of $J-H$ color may moreover be partially compensated by using a “corrected” color, of the form:

[TABLE]

for stars not classified as NIR-excess sources; the intrinsic unreddened value of $(J-H)_{c}$ is $\sim$ 0.75 for all masses in the range $0.08-1M_{\odot}$ , and ages $\geq 20$ Myr, with slight deviations for younger low-mass stars (Figure 18). Individual visual extinction $A_{V}$ , for stars with $(J-H)_{c}>0.75$ , can be estimated therefore as

[TABLE]

where the last factor above is the (constant) reddening vector slope, equal to 7.318 (using the Rieke and Lebofsky 1985 reddening law). For stars more massive than $1M_{\odot}$ this underestimates $A_{V}$ , since their intrinsic $(J-H)_{c}$ color is lower (bluer) than 0.75. Extinction $A_{V}$ for stars with a NIR excess is instead estimated from the $J-H$ color alone (this is again an underestimate for $M>1M_{\odot}$ ).

By using these individual $A_{V}$ values (converted to the IPHAS bands $A_{i}$ and $E(r-i)$ as explained in Appendix C) we have built the dereddened optical CMD, shown in Figure 19. The clustering of X-ray sources at $(r-i)_{0}\sim 1$ is probably an artifact resulting from our underestimated reddening for stars above $1M_{\odot}$ . The bulk of X-ray sources, if lying at the NAP distance, are found in a 2-mag wide strip corresponding to the PMS band, between ages 1-10 Myr, also populated by the majority of H58 stars (on average brighter than the rest of the X-ray-source counterparts) and optically-visible YSOs. Tens of NIR-excess stars are found apparently below the main sequence at the Nebula distance, as remarked above. The unreddened X-ray-detected M stars selected from Fig. 13 have especially reliable positions in this diagram, since they required no dereddening: they do not form a proper sequence in this CMD, but are mixed to other low-mass NAP X-ray sources. They might still be foreground, active M dwarfs, 3 to 10 times closer than the NAP; this diagram does not permit to confirm (nor exclude) their NAP membership.

5.6 Spatial distributions

As found by e.g. Cambrésy et al. (2002) and RGS11, the spatial distribution of young stars in the NAP is highly non-uniform. This non-uniformity also holds for the X-ray source distribution (Figs. 4 to 6). Therefore, we examine here in more detail the properties of each spatial sub-region. The individual panels of Figures 20 and 21 permit a comparison between the spatial distributions of all sets of data considered here. The background greyscale image represents the local density of all optical/NIR objects (in white the lowest densities), which is inversely correlated with the mean reddening (Cambrésy et al. 2002) shown in Fig. 17, but is a somewhat more versatile indicator (e.g. for sources with too noisy or missing $J$ magnitudes). As in Figs. 1 and 7, big solid circles/squares are X-ray FOVs, while RGS11 YSOs are indicated with black plus signs. X-ray sources are here instead color-coded, according to their observed $J-H$ color, with the color scale shown in the upper left panel of Fig. 20. X-ray sources without a NIR counterpart, or with missing $J-H$ , are drawn with a red color, assuming that high extinction is the reason for the missing measurement.

The “Pelican hat”, as in RGS11, is the northernmost field in our survey (Fig. 20, top left), covered by XMM-Newton ObsId 0679580101. The region hosts a local concentration of YSOs (see RGS11), nearly coincident with a region of enhanced obscuration, elongated along N-S direction, through the center of the XMM-Newton FOV. Curiously, most X-ray detected sources in this field lie to the right of center (inside the dashed rectangle in the Figure). Their $J-H$ colors suggest they are an inhomogeneous group, either with very different extinction values, and/or a wide range of masses. Very few of these in-rectangle X-ray sources also possess a NIR excess. At the same time, they are not spread uniformly across the X-ray FOV, as if they were an unrelated field-star population111The XMM-Newton EPIC camera sensitivity dependence on off-axis distance is flat enough that such a central concentration of detections cannot be an instrumental effect. See also Sect. 5.8.

, but closer to the West side of the obscured region. Therefore, these X-ray sources appear to correspond to a sub-population of the NAP which is missed by YSO/CTTS searches, even using Spitzer or mixed optical/IR criteria; they also lack strong H $\alpha$ emission, as are not coincident with IPHAS-selected CTTSs. The properties of this group of X-ray sources are perhaps best interpreted as a group of relatively older WTTS members of the NAP population, and their spatial placement relative to the younger YSOs (and the currently cloud overdensity seen from the star-count map) as an indication of sequential star-formation episodes, proceeding from West to East in this particular region of the NAP.

The upper-right panel of Fig. 20 (“Pelican” field proper) was covered by one new (0679580201) and one archival (0556050101) XMM-Newton observations, and by Chandra ACIS-I ObsIds 13647 and 15592; it hosts most of the H58 stars, and a large number of RGS11 YSOs (though not the highest density). Most of the X-ray sources in the XMM-Newton FOVs (those in the ACIS-I FOV will be discussed below) have intermediate $J-H\sim 1-1.5$ , except for 4-5 higher-reddening X-ray sources falling in a more obscured region, and also coincident with Cluster #6 from Cambrésy et al. (2002; yellow circles).

Next, the lower-left panel of Fig. 20 (LDN 935) shows our XMM-Newton field closest to the most oscured part of the NAP, and also to its illuminating O5 star, which lies just outside of our (ObsId 0679580301) FOV. In proceeding from the Pelican region towards the O5 star, there is an obvious gradual decrease in the YSO spatial density. Also the S-E part of the XMM-Newton FOV, closest to the O star, is almost devoid of X-ray sources. The central and S-W part of this FOV (again marked with a dashed rectangle) contains very few YSOs, but still a few tens X-ray sources, again with a mixture of $J-H$ values.

The “Gulf of Mexico” region (lower-right panel of Fig. 20) hosts a crowded YSO population, and also dense groups of X-ray sources, which the spatial resolution of the XMM-Newton EPIC images was insufficient to resolve. The region, also containing four of Cambrésy’s clusters, shows very definite spatial relationships between the obscuration pattern, the YSO and X-ray populations. Its properties are best examined by looking at the individual Chandra FOVs, as we do below. To conclude with our XMM-Newton observed fields, Fig. 21, upper-left panel, shows the archival ObsId 0302640201, centered on the FU Ori star V1057 Cyg (not detected in X-rays), and containing inconspicuous, low-density populations of both YSOs and X-ray sources. North of it, corresponding to “continental North America”, Figure 17 shows that both the YSO density and the average reddening are very low: although some hot, ionized gas must be there to produce the emission nebula, the total dust column density must be low not to redden background giants (main contributor to the star-count map); a low amount of warm dust there is also evident from Fig. 2, so that we do not expect active star formation in this region.

Our ACIS-I “Pelican” FOV (upper-right panel of Fig. 21) comprises the highest density of H58 PMS stars, and also probes with high spatial resolution the bright-rimmed cloud giving the nebula its shape (see Fig. 2). This cloud is so dense to obscure most background stars behind its illuminated rim (see also Fig. 17). This latter coincides with a cluster from Cambrésy et al. (2002), which is also detected as a small cluster of highly reddened X-ray sources. In the N-E part of the ACIS FOV (dashed square), the X-ray source density is larger than the YSO density, the latter being much more numerous in the southern part of the same FOV.

Both the YSO spatial density and local obscuration reach their maximum inside our “Gulf of Mexico” ACIS-I FOV (lower-left panel of Fig. 21), with YSO falling along arch-like patterns near the border of the obscured region. Many tens X-ray sources are also following the same pattern, indicating that they are also young stars belonging to the NAP population. Some of them have large reddening, especially those coincident with Cambrésy’s Cluster #2 (northernmost yellow circle). The obscuring material here, unlike that in the Pelican nebula, does not coincide with the (southern) bright rim, as it should be evident from comparing Figs. 2 and 17. To the N-W of the most obscured region and the YSO cluster, the YSO density drops abruptly but there are still several tens of X-ray sources (dashed rectangle), which appear to be too little reddened to belong to the background, and too numerous to belong to the foreground of the NAP: they again are good candidates as WTTS members of the NAP. It is worth remarking that their spatial density increases towards the obscured region, while it decreases slightly towards the N-W border of the FOV, in the direction of the O5 star, only 5*′* away. As above, there is not detectable increase of X-ray source density in the neighborhood of the most massive star. It might be argued that the in-rectangle X-ray sources are too lightly reddened to be NAP members, in a region dominated by strong obscuration, and that they are unlikely to lie all on the near edge of the obscuring dust. The reason for their apparent low reddening might then be their higher mass ( $M>1M_{\odot}$ ), causing reddening from $J-H$ to be increasingly underestimated the higher the actual mass is.

Last, in the lower-right panel of Fig. 21 we show a zoom of the central part of archive ACIS-S ObsId 14545, centered on the recently-erupted FU Ori object HBC722, surrounded by a dense group of X-ray sources, known YSOs and PMS stars (H58, Armond et al. 2011; also coincident with Cambrésy’s Cluster #3b): they lie all near the border of a strong-obscuration region.

5.7 X-ray spectra, lightcurves and luminosities

Whenever X-ray sources are detected with a sufficient number of X-ray counts, their X-ray spectra and lightcurves may help to understand their nature. Here we make use of hardness ratios and do not perform a detailed best fit of the spectra of the brightest sources, deferring this to a future paper. Hardness ratios are here defined as $HR1=(M-S)/(M+S)$ , and $HR2=(H-M)/(H+M)$ , where $S$ , $M$ , and $H$ are the source X-ray counts in the soft (0.3-1.2 keV), medium (1.2-2.4 keV), and hard (2.4-8.0 keV) bands, respectively. $HR1$ is most affected by the line-of-sight absorption of soft X-ray photons, while $HR2$ is affected by absorption only at very high column densities, and more often is a measure of intrinsic spectrum hardness (and high plasma temperatures for thermal sources). Figure 22 compares these hardness ratios with the $J-H$ color, separately for XMM-Newton sources (with more than 50 X-ray counts) and ACIS sources (with more than 20 counts). Since the instrumental effective area has a different energy dependence for XMM-Newton and Chandra ACIS, the respective $HR1,2$ must not be mixed together. We have argued above that $J-H$ is dominated by reddening: this is further supported by the fairly good correlation between $HR1$ and this color (left two panels in Fig. 22); the X-ray sources associated with a H58 star or with a RGS11 YSO follow the same relation as the other sources. A much weaker correlation is seen between ACIS $HR2$ and $J-H$ , as expected if $HR2$ is only weakly related to absorption. No relation is seen between XMM-Newton $HR2$ and $J-H$ . Also when considering $HR2$ , the X-rays sources with a H58 star/YSO association are homogeneous with the others. Nearly all of H58 stars have (XMM-Newton or ACIS) $HR2\leq 0$ , indicative of not-too-hot X-ray emitting plasma. Over the same $J-H$ range of the H58 stars, however, the upper-right panel of Fig. 22 shows that about one-half of the RGS11 YSOs have $HR2>0$ , and thus even hotter plasmas, in agreement with previous results on very young Class I/II protostars in Orion (e.g. Prisinzano et al. 2008). The group of unreddened X-ray sources at $J-H\sim 0.6$ , already mentioned with reference to Figs. 12 and 13, is also recognizable in the two upper panels of Fig. 22, their $HR1,2$ also being rather homogeneous. Their low $HR1$ values confirm their low line-of-sight absorption, but not lower than several of the H58 CTTS; their $HR2$ values average to $\sim 0$ , like the bulk of YSOs, which suggests that these X-ray sources have intrinsic spectra no different from the bona-fide population of the NAP, despite that their low reddening/absorption is compatible with being active foreground stars.

We have also examined the X-ray lightcurves of sources detected with enough counts. Some examples are shown in Figure 23, which illustrates the type of variability found. When the count rate is large enough, most sources are found to be variable; in many or most cases, lightcurve shapes are complex, while “simple” flares with impulsive rise and exponential decay are more rare. This is reminiscent of the X-ray lightcurves of YSOs in the $\rho$ Oph star-forming region, from the XMM-Newton DROXO survey (Pillitteri et al. 2010). Panel $e$ shows a probable (double-peaked) flare event, with a long decay time of $\sim 10$ ksec, as found e.g. in the COUP Orion lightcurves (Favata et al. 2005). Some of the XMM-Newton observations have long interruptions in the middle (like in panels $a$ and $d$ ). Large-amplitude variability on timescales of one day may also be seen from the comparison of the co-pointed ACIS-I images ObsId 13647 and 15592, already shown in Fig. 4.

Since X-ray emission decays with stellar age, one possible way of discriminating very young stars in the NAP from foreground/background active non-members is through the use of X-ray-to-optical luminosity ratios, which decrease with mass-dependent timescales (e.g. Preibisch and Feigelson 2005). Ratios of X-ray to bolometric ( $L_{X}/L_{bol}$ ) or X-ray to visual ( $L_{X}/L_{V}$ ) luminosities are commonly used. In our case, the difficulty in obtaining accurate extinction values for individual X-ray sources makes these ratios unsuitable, and has prompted us to search a reddening-free equivalent ratio. It is well known than while the dust absorption decreases from optical to IR wavelengths, the X-ray absorption decreases from the soft to the hard X-ray band, with photons of energy $E=2$ keV being absorbed like NIR photons with $\lambda=2\mu$ , for a typical interstellar gas/dust ratio. Therefore, we searched for an X-ray energy range where absorption is equivalent to that in the $J$ NIR band, which as discussed above is convenient to study our NAP stars. We made several experiments using the PIMMS software222Portable, Interactive Multi-Mission Simulator, available at http://heasarc.gsfc.nasa.gov/docs/software/tools/pimms.html, for different energy bands: 0.8-1.2 keV, 1.0-1.8 keV, and 1.2-2.4 keV, sufficiently wide for being well characterized at the spectral resolution of Chandra/ACIS detector. Three single-temperature APEC thermal models were considered, in the temperature range of Class I/II/III YSOs. Hydrogen column density ( $N_{H}$ ) values were converted to optical extinction using the relation $N_{H}=2.22\cdot 10^{21}A_{V}$ (Gorenstein 1975), while the correspondence between $A_{V}$ and NIR extinction is explained in Appendix C. The results of the experiment is shown in Figure 24, where the ordinate shows the relative flux attenuation. We see that the X-ray band between 1.0-1.8 keV is absorbed by an amount similar to the $J$ band, within a factor of $\sim 50$ % up to $A_{V}\sim 10-12$ . Absorption in the harder 1.2-2.4 keV band is also very close to that in the $H$ band; however, X-ray counts are often less in this higher-energy band than in the 1.0-1.8 keV band, and the NIR $H$ band is more easily affected by non-photosperic contributions than the $J$ band, so that the pair [1.0-1.8 keV]/ $J$ seems preferable to obtain an absorption-independent flux ratio.

A plot of X-ray count-rate in the 1.0-1.8 keV band vs. $J$ is shown in Figure 25, for ACIS-I sources with $J-H<2$ , corresponding roughly to $A_{V}=12$ . In this diagram, absorption causes datapoints to move parallel to the dashed line, and might partially account for the correlation seen in the diagram, while the spread above and below that line reflects the X-ray to photospheric flux ratio. Most of the H58 stars have X-ray/NIR flux ratios within an order of magnitude. Their average ratio is also close to that of the bulk of NAP X-ray sources; only four of them show weaker X-ray/NIR flux ratio. Also the RGS11 YSOs appear well mixed with the non-YSO X-ray sources, and count-rate upper limits for X-ray undetected YSOs (arrows in the Figure) are consistent with detections. The black crosses in the diagram are X-ray sources in the dashed rectangles in Figs. 20 and 21: also these sources do not appear to have particularly high or low X-ray/NIR flux ratios, and are therefore homogeneous with the rest of NAP X-ray sources.

We have estimated X-ray luminosities $L_{X}$ for our X-ray sources, using PIMMS to compute conversion factors between count-rate and flux. These are weakly dependent on the emitting plasma temperature if this is above 1 keV, as often found in active PMS stars, but vary considerably as a function of $N_{H}$ , across the range of inferred absorption values for our NAP sources. As above, we estimated $N_{H}$ for individual sources from their $J-H$ color, and using the above conversion between this and $A_{V}$ , and between $A_{V}$ and $N_{H}$ . Since we do not know individual distances for possible foreground stars, we might be overestimating $L_{X}$ for these latter. The derived $L_{X}$ distribution is shown in Figure 26, for both the total NAP X-ray sample and selected subsamples. The total sample and the X-ray emitting M dwarfs are X-ray selected samples, and therefore do not include upper limits. For independently-selected samples such as H58 stars and RGS11 YSOs we have instead computed individual $L_{X}$ upper limits using PW(X)Detect; these are used to compute maximum-likelihood X-ray luminosity functions, using the survival R software package333http://cran.r-project.org/web/packages/survival, shown in Fig. 26. With less than 20% of objects detected in X-rays, our sampling of the X-ray properties of flat-spectrum and Class I YSOs is rather poor, compared to the $>$ 60% X-ray detections among Class 0-I YSOs in the ONC by Prisinzano et al. (2008); nevertheless, the $L_{X}$ medians for the flat-spectrum and Class I YSOs from Fig. 26 fall very close to the $L_{X}$ median of Class 0-Ib objects in Prisinzano et al. (2008; note that YSO classification was made differently by these authors and RGS11). The X-ray luminosity function of RGS11 Class II YSOs (33% detection rate) also has a median $L_{X}\sim 29.75$ (erg/s), which compares well to the Preibisch and Feigelson (2005) results for the ONC M stars (median $L_{X}\sim 29.55$ erg/s), but is significantly lower than the median $L_{X}$ of more massive stars in the ONC (or NGC 2264, or Chamaeleon: median $L_{X}\sim 29.9-30.5$ erg/s). We have however found from our color-color diagrams that only a minor fraction of our X-ray sources are consistent with M-star colors. One possible solution to this contradiction is that we might be strongly underestimating absorption $N_{H}$ , and with it also $L_{X}$ , since we probably underestimated $E(J-H)$ as discussed above, if these stars’ masses are much above $\sim 0.5M_{\odot}$ . To test this, we have computed the maximum $E(J-H)$ (and corresponding $N_{H}$ ) for each star, assuming an intrinsic value $(J-H)_{0}=0.15$ , appropriate to $1.4M_{\odot}$ stars at 100 Myr (Fig. 15), but definitely not to $0.5M_{\odot}$ stars: the resulting X-ray luminosity function for Class II YSOs is shown (dashed) in Fig. 26: the resulting median $\log L_{X}\sim 30.1$ is closer to the ONC value, and even more to the values for NGC 2264 and Chamaeleon stars in Preibisch and Feigelson (2005) for the mass range $0.5-0.9M_{\odot}$ , but remains a factor $\sim 2$ below the median $L_{X}$ for stars in the mass range $0.9-1.2M_{\odot}$ in the same clusters, for which $E(J-H)_{0}=0.15$ would be most appropriate. Therefore, reddening underestimates may be only a partial explanation of the low X-ray luminosity function of Class II objects in the NAP.

The H58 stars, most of which are not M stars, and which are only lightly absorbed, as seen above, have higher $L_{X}$ than the Class II YSOs (solid magenta line in Fig. 26), well consistent with PMS stars in the mass range $M=0.5-0.9M_{\odot}$ from the different clusters shown by Preibisch and Feigelson (2005).

The unreddened M dwarfs have a $L_{X}$ distribution much lower than the bulk of NAP sources; if they are NAP members, the lower $L_{X}$ would not be surprising, since these stars are at the lower end of the mass spectrum (Fig. 19) and their $L_{X}$ distribution of Fig. 26 is close to that of similar-mass stars in the ONC (e.g. Preibisch and Feigelson 2005). However, we cannot rule out that these are M stars with ages similar to the Pleiades ( $\sim$ 100 Myr), 3-10 times nearer to us, so that their actual $L_{X}$ would be 10-100 times lower than shown in Fig. 26: also in this case their $L_{X}$ distribution would agree with the data presented in Preibisch and Feigelson (2005; fig.4).

5.8 X-ray sensitivity limits

It is important to recognize to what extent the results presented above may be affected by the uneven sensitivity of the available X-ray data. As discussed in detail e.g. by Broos et al. (2011), two distinct causes contribute to the effect that an astrophysical object with a given intrinsic X-ray flux (at the NAP distance) may be detected or not. The first cause is instrumental, the detection sensitivity being not uniform across the imaged FOV, because of both mirror vignetting and PSF off-axis degradation. The second cause is of astrophysical origin and resides in the uneven column density of absorbing matter along the line of sight to the source, which was seen above to span a wide range inside the surveyed region. Therefore, we try here to quantitatively examine both effects individually.

The instrument-related effects are relatively easy to model, once the background level of each individual X-ray observation is measured, and properties like vignetting and PSF shape are known. If the spatial distribution of X-ray sources is wide enough, this gives rise to what was termed the “egg-crate effect” by Broos et al. (2011), since the smaller PSF near the (ACIS-I) FOV center results in a larger spatial density of detections there, with respect to FOV borders. We have computed nominal minimum detectable fluxes $f_{x}$ (for point sources) for the entire NAP survey area using the capabilities of PW(X)Detect: the resulting map is shown in Figure 27, including both ACIS and EPIC pointings. In order to compare different detectors in the same map, we cannot use purely instrumental quantities (counts/sec), but physical ones, scaling counts to erg/cm2 with the adoption of the nominal instrument effective area at a representative energy of 1 keV. Since the two ACIS-I ObsIds 13647 and 15592 were analyzed together and the ACIS-S ObsId 14545 has higher sensitivity than ACIS-I datasets, all ACIS fields span approximately the same range of $f_{x}$ . Instead, the various XMM-Newton EPIC exposures are of unequal duration (see Table 1), and their $f_{x}$ is more sensitive to background than ACIS datasets: therefore, despite the more uniform PSF they collectively span a wider range of $f_{x}$ . This is more cleary seen in the $f_{x}$ histograms of Figure 28, separately for ACIS and EPIC data: most of the width of the EPIC histogram is related to ObsId-to-ObsId variations, while most of the width of the ACIS histogram is related to center-to-border effects, the various ACIS FOV having similar $f_{x}$ ranges.

The strong center-to-border $f_{x}$ variation in ACIS datasets is responsible for the egg-crate effect, when this is found. However, the distribution of X-ray detections in NAP ACIS-I FOVs (Figure 21) does not show such a centrally-symmetric shape, so we may conclude that any egg-crate effect is not primarily responsible for the observed spatial distribution of NAP X-ray sources. As far as other effects are concerned, it is interesting to observe from Figure 25 (including only ACIS-I data) that upper limits span a wide range of almost two orders of magnitude, because they are computed on the basis of the individual source absorption values. The fact that they are even more frequent in the upper part of the diagram emphasizes that absorption, more than uneven detector properties, is the most important factor against their detection. This emerges also clearly from a comparison between the range in the ordinates of Figure 25 of 2.5 orders of magnitude, and that spanned by the instrumental ACIS sensitivity (one order of magnitude) in the red histogram of Figure 28.

The distribution of absorption-based (from $J-H$ colors) X-ray count-rate-to-flux conversion factors is shown in Figure 29, separately for ACIS and EPIC detectors (and regardless of whether each detector actually imaged a given source), under the same assumptions about the intrinsic source spectrum as in the previous subsection. For both instruments, the bulk of stars span approximately 1.5 orders of magnitude, in agreement with conclusions given just above. While the total NAP cloud absorption shows definite spatial properties (Figure 17), the X-ray colors (Figures 4 to 6) and NIR colors (Figures 20 and 21) of X-ray sources are not generally correlated with the local total depth. This suggests that X-ray sources are located at various depths in the cloud, and the extrapolation of the undetected source density on the basis of the local density of detections is here at risk of being misleading. Such an approach was instead used by e.g. Kuhn et al. (2015) in their X-ray study of several massive SFRs, in which absorption is more uniform and source statistics (per FOV) is much higher than in the NAP, permitting a believable reconstruction of the undetected population. Contrarily to the data studied by Kuhn et al. (2015), in the NAP dataset the flux completeness limit (a flux above which we are confident to have detected near 100% of sources) is near the upper end of the detected source range, as can be understood from Figure 25 where upper limits are found up to the top of the count-rate scale; this also renders the approach adopted by those authors unapplicable here. The conclusion drawn from Figure 29 is that the intrinsic X-ray luminosities of undetected sources may range up to 1.5 orders of magnitude above their unabsorbed value, whose spatial distribution was shown in Figure 27. The peaks of the instrumental-sensitivity and conversion-factor histograms, taken together, correspond to an intrinsic X-ray luminosity $\log L_{x}\sim 29.9$ erg/s, detectable over most of the NAP fields. This $L_{x}$ value being typical of low-mass PMS stars, we conclude that our NAP detection list can be considered representative of the young star population in this SFR.

While a proper reconstruction of the space and flux distributions of undetected NAP sources is unfeasible, we may nevertheless mitigate the instrumental effects described above, by considering only detections above a uniform threshold for a given X-ray FOV. Figure 30 shows the detected X-ray sources in the “Gulf of Mexico” ACIS FOV, already shown in Fig. 21 (lower-left panel), but limited to sources with more than 15 counts, and therefore detectable across the whole FOV (thus free from egg-crate effects). Although the source statistics becomes smaller, the non-uniform spatial distribution of detections is still clear, especially near one of the Cambresy’s NIR clusters. Therefore, the main conclusions of the previous subsections are not dramatically affected by instrumental factors.

6 Discussion

The results reported in the above sections emphasize once again the known complexity of the NAP star formation region, made of several subgroups of young stars (Cambrésy et al. 2002, RGS11), with no obvious connection between them. Although it was very difficult to assess individual membership for our X-ray detected sources, above results show that many (or most) of them exhibit properties (X-ray/NIR flux ratios, X-ray variability and spectrum hardness) consistent with young PMS stars. The non-detection in the X-rays of most YSOs, even those of Class II whose X-ray properties are best known, remains puzzling, since optical/NIR color-color diagrams seem to rule out for most of them the low mass values ( $M<0.5M_{\odot}$ ) that their X-ray luminosity function would imply. A better characterization of these objects would be desirable.

Perhaps the spatial distribution of our X-ray sources is our most interesting result. Although the illuminating O5 star 2MASS J20555125+4352246 does not fall in any of our X-ray FOVs, we observed its immediate neighborhood, a few arcmin away from it: there is no sign of any concentration of X-ray sources around it, in agreement with the finding by its discoverers that it is remarkably isolated (Comerón and Pasquali 2005). This isolation refers therefore not only to comparably massive stars, but to stars down to solar-like masses, to which our survey is sensitive even at the extinction of the O5 star. This is very different from most star-forming regions, where the highest-mass stars are immediately surrounded by low-mass PMS stars. It would be interesting to investigate if this is a runaway star, with implications on the timescales on which it might have interacted with the molecular cloud; although no such information is available now, the Gaia data should provide it in a short time frame.

The two sub-regions with the highest YSO spatial density, the Gulf of Mexico and Pelican, are also those with the largest number of X-ray detections (although this might be somewhat biased by having used there the most sensitive ACIS detectors). In the Gulf of Mexico, closest to the O5 star, there is a clear spatial trend: YSOs are clustered near the border of the dark cloud which faces the O star (and not inside the cloud), and tens of X-ray sources follow the same pattern; moreover, several other tens X-ray sources are found between the YSO cluster(s) and the O star, forming an apparently distinct layer. It is interesting to remark that in Figure 20 of RGS11 the Class III stars fall in this same intermediate region. This is highly suggestive of a time sequence, with formation of stars proceeding southwards, under the strong influence of the massive O star nearby. The X-ray sources without a YSO counterpart, as well as the Class III stars, would thus be the oldest, with younger stars being currently formed in the outer layers of the dense dust cloud. Toujima et al. (2011) also suggested triggered star formation in NGC 7000, on the basis of molecular-line observations. The disk-free X-ray detected stars are not necessarily much older than the others (no such separation is found in our de-reddened CMD), since when exposed to strong UV irradiation disk lifetimes are likely to be significantly shortened (e.g. Guarcello et al. 2007, 2009). In other places in the NAP, a similar segregation between the YSO and X-ray source distributions is observed, as in the “Pelican hat”, but its origin is much less clear, since the triggerer of the possible time sequence is not obvious. Moreover, we recover at least three of the Cambrésy et al. (2002) NIR clusters in X-rays, confirming their existence.

The assessment of membership for the X-ray detected sources was difficult, as discussed above for each of the possible indicators. Only $\sim 29$ % of all X-ray sources have H $\alpha$ or NIR excesses (either from this work or from RGS11 and H58), and are therefore high-probability members individually. Most other X-ray sources have however X-ray properties, colors and extinction very similar to the former, and are probable members as well. The foreground extinction towards the NAP is very small, as we find from color-color diagrams and in agreement with Laugalys et al. (2006, 2007), and therefore foreground X-ray sources may only be found at near-zero reddening: we found only a few tens such sources above. Extinction rises rather abruptly in the NAP, although this may be position-dependent as we have examined above (in agreement with Cambrésy et al. 2002). Background X-ray sources, behind such large absorbing column, are unlikely to be coronal sources, but may be distant compact objects or even AGNs, both characterized by large X-ray-to-optical flux ratios. We tentatively identify these classes of sources with our unidentified X-ray sources (115 out of 721 total detections), which must have large X-ray-to-optical flux ratios if they are missed in both of the very deep IPHAS/UKIDSS catalogs. To summarize, most of the NAP X-ray sources with an optical/NIR counterpart, except perhaps a significant fraction of the unreddened ones, are good candidates as young NAP members.

7 Summary

We have performed the first extensive, wide-area X-ray survey of the North-America and Pelican star-forming region, using both Chandra/ACIS and XMM-Newton/EPIC detectors. More than 700 unique X-ray sources have been detected, of which $\sim 85$ % have a counterpart in at least one of the IPHAS/UKIDSS/2MASS catalogs. Only $\sim 29$ % of X-ray sources are identified with previously known YSOs or CTTS, or with newly found H $\alpha$ -emission or NIR-excess stars. We argued that most of the optically/NIR identified X-ray sources are probable members of the star-forming region. A few tens unreddened X-ray sources are probable active foreground low-mass stars.

In the Gulf-of-Mexico region, the respective spatial properties of dark obscuration, YSOs, and X-ray sources without YSO association are suggestive of a sequential star-formation scenario, with the O5 star illuminating the entire nebula as the probable triggerer. Unlike most star-forming regions, this most massive star appears isolated even in X-ray images. The large-scale spatial distribution of the X-ray detected member candidates follows qualitatively that of the known YSOs, with several sub-clusters, apparently physically unconnected.

Detailed follow-up (spectroscopic) observations will be needed to confirm individual membership of the X-ray sources found here.

Appendix A 2MASS - UKIDSS calibration

The UKIDSS $J,H,K$ photometric system is calibrated to the 2MASS system (Hodgkin et al. 2009); however, the calibration was made at low reddening, and we find that small adjustments are required to match the two catalogs at large reddening values, typical of the NGC 7000/IC 5070 region. The difference between 2MASS and UKIDSS $J$ magnitudes is shown in Figure 31: although small, this difference is often significant compared to the very small errors in the UKIDSS magnitudes. Only objects with errors $<0.07$ mag in both $J$ bands, and errors $<0.1$ mag in $(J-H)_{UKIDSS}$ , are shown. A least-square fit to the data (with fixed zero intercept) has the form:

[TABLE]

The $J-H$ colors differ between 2MASS and UKIDSS more appreciably, however, by almost 8% (Figure 32, where only objects with errors $<0.1$ mag in both $(J-H)_{UKIDSS}$ and $(J-H)_{2MASS}$ are shown). The best fit to the data (with zero intercept) has the form:

[TABLE]

Similarly, Figure 33 shows the comparison between the respective $H-K$ colors, with the best fit here given by:

[TABLE]

All UKIDSS magnitudes were therefore rescaled according to the $(J-H)_{UKIDSS}$ color, to match the 2MASS photometric system even at large reddening. At low reddening (low $J-H$ ), this recalibration is irrelevant, and does not interfere with the one presented by Hodgkin et al. (2009). After recalibration, we merged the 2MASS and UKIDSS catalogs into a single NIR source catalog, choosing the more precise UKIDSS magnitudes when available.

Appendix B IPHAS - VPHAS $+$ calibration

Although the IPHAS $r,i$ photometric system is similar to the Sloan Survey system, the formulae in Barentsen et al. (2014) indicate that significat differences exist between the two systems. Moreover, no recipe is given to convert the IPHAS $r,i$ magnitudes into Johnson/Cousin $VRI$ magnitudes. Such a recipe is instead given by Drew et al. (2014) for the VPHAS $+$ $ugriz$ magnitudes, which are closely related to the IPHAS filter system. The BHAC evolutionary tracks and isochrones, moreover, are currently available for the $UBVRI$ filters, but not for either the Sloan or the IPHAS/VPHAS $+$ filters, so we attempt here to recalibrate the IPHAS $r,i$ magnitudes in terms of the VPHAS $+$ $r,i$ , whose relation with $VRI$ is known from Drew et al. (2014). We consider an equatorial field where both IPHAS and VPHAS $+$ data are available, to study their photometric differences. The results of this experiment are shown in Figures 34 and 35, where only objects with errors $<0.05$ mag in all bands are shown. The best-fit relations shown in these Figures are:

[TABLE]

These relations (together with those given in Drew et al. 2014) were used to convert the BHAC tracks/isochrones in the Johnson/Cousin filters into the appropriate IPHAS $r,i$ magnitudes and colors.

Appendix C Reddening law

We study here the empirical reddening law for the NGC 7000/IC 5070 region, in the $r,i,J,H,K$ bands. With respect to previous studies, we benefit here from an extensive optical/NIR catalog, reaching down to faint magnitudes with small photometric errors. Thanks to these properties, we are able to discern in several color-color diagrams the giant-star locus from the dwarfs locus. Figure 36 shows the $(J-H,H-K)$ diagram of all sources in the studied region: the reddened red-giant sequence starts at $J-H\sim 0.8$ , whereas the dwarf sequence starts at $J-H\sim 0$ , but the giants being more luminous remain observable up to larger reddening values. We have therefore visually fitted the giant sequence with the red line in the Figure (with slope $E(J-H)/E(H-K)=1.9$ ). It should be remarked that at low reddening dwarfs dominate the distribution because of their higher spatial density, but at large reddening giants dominate being observable up to larger distances: it is therefore incorrect to derive the reddening vector slope by simply joining the low and high ends of the color distribution with a straight line, since this would mix together stars with different intrinsic NIR colors, and the resulting slope would be higher than the true one. The upper envelope of datapoints in the Figure also agrees with the slope we estimate from the giant sequence.

Figure 37 is a mixed optical/NIR $(r-i,J-H)$ diagram, where we can discern well the reddened giant sequence (the lowest one, including the highest-reddening stars) from the dwarf sequence. Protruding upwards, the M-dwarf sequence is also clearly seen (cf. Fig. 12). The reddening vector has a slope of $E(r-i)/E(J-H)=1.79$ .

In the $(r-i,i-J)$ diagram of Figure 38, instead, the dwarf and giant sequence are not distinct, but the M-dwarfs are. The reddening-vector slope is here $E(r-i)/E(i-J)=0.6$ .

In order to connect these reddening laws to the $V$ -band extinction, and to obtain the total-to-selective extinction ratio $A_{i}/E(r-i)$ for the IPHAS filters, we need two more equations. Assuming that the $J$ band is least affected by peculiar reddening laws, we therefore take from Rieke and Lebofsky (1985) the ratios $A_{J}/A_{V}=0.282$ and $E(J-H)/A_{V}=0.107$ . The set of relative extinctions $A_{\lambda}/A_{V}$ for the NAP thus becomes:

[TABLE]

where equations 10 and 11 are merely the Rieke and Lebofsky (1985) relations, included for convenience.

Acknowledgements.

We wish to thank an anonymous referee for his/her helpful suggestions. I.P. acknowledges support by Chandra fund 16617814 contract GO2-13021X. The scientific results reported in this article are based on observations made by the Chandra and XMM-Newton X-ray Observatories. This paper also makes use of data obtained as part of the INT Photometric H $\alpha$ Survey of the Northern Galactic Plane (IPHAS, www.iphas.org) carried out at the Isaac Newton Telescope (INT). The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge. The bandmerged DR2 catalogue was assembled at the Centre for Astrophysics Research, University of Hertfordshire, supported by STFC grant ST/J001333/1. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research makes use of the SIMBAD database, operated at CDS, Strasbourg, France. We also make heavy use of R: A language and environment for statistical computing. R Foundation for Statistical Computing, Vienna, Austria. (http://www.R-project.org/).

Bibliography55

The reference list from the paper itself. Each links out to its DOI / PubMed record.

1Armond et al. (2011) Armond, T., Reipurth, B., Bally, J., & Aspin, C. 2011, A&A, 528, A 125
2Aspin (2011) Aspin, C. 2011, AJ, 141, 196
3Bally & Reipurth (2003) Bally, J., & Reipurth, B. 2003, AJ, 126, 893
4Bally et al. (2014) Bally, J., Ginsburg, A., Probst, R., et al. 2014, AJ, 148, 120
5Baraffe et al. (2015) Baraffe, I., Homeier, D., Allard, F., & Chabrier, G. 2015, A&A, 577, A 42
6Barentsen et al. (2014) Barentsen, G., Farnhill, H. J., Drew, J. E., et al. 2014, MNRAS, 444, 3230
7Broos et al. (2011) Broos, P. S., Townsley, L. K., Feigelson, E. D., et al. 2011, Ap JS, 194, 2
8Cambrésy et al. (2002) Cambrésy, L., Beichman, C. A., Jarrett, T. H., & Cutri, R. M. 2002, AJ, 123, 2559

TL;DR

Contribution

Findings

Abstract

Peer Reviews

Videos

X-ray survey of the North-America and Pelican star-forming complex

Abstract

Key Words.:

1 Introduction

2 X-ray observations

3 X-ray data analysis

4 Auxiliary data: optical and near-IR

5 Results

5.1 Distance

5.2 Hα\alphaα-emission stars

5.3 Optical and near-IR color-color diagrams

5.4 Color-magnitude diagrams

5.5 Extinction and reddening

5.6 Spatial distributions

5.7 X-ray spectra, lightcurves and luminosities

5.8 X-ray sensitivity limits

6 Discussion

7 Summary

Appendix A 2MASS - UKIDSS calibration

Appendix B IPHAS - VPHAS+++ calibration

Appendix C Reddening law

Acknowledgements.

5.2 H $\alpha$ -emission stars

Appendix B IPHAS - VPHAS $+$ calibration