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Home All issues Volume 507 / No 3 (December I 2009) A&A, 507 3 (2009) 1485-1502 Full HTML
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Table 3:

Coordinates and flux densities of 2MASS & IRAC 3.6/4.5 $\mu $m PMS sources in NGC 2023/L 1630.

Source 		$\alpha_{2000}$ $\delta_{2000}$ J H $K_{\rm s}$ F3.6 F4.5 Named
L1630           mJy mJy  
NIR-1 5:40:46.70 -2:29:07.1 16.36 $\pm$ 0.09 15.75 $\pm$ 0.10 15.33 $\pm$ 0.16 0.40 $\pm$ 0.01 0.36 $\pm$ 0.00  
NIR-2 5:40:52.70 -2:26:25.8 16.69 $\pm$ 0.13 15.42 $\pm$ 0.08 15.15 $\pm$ 0.14 0.37 $\pm$ 0.01 0.29 $\pm$ 0.00  
NIR-3 5:40:54.87 -2:08:33.7 17.05 $\pm$ 0.18 15.66 $\pm$ 0.09 15.07 $\pm$ 0.13 0.49 $\pm$ 0.01 0.38 $\pm$ 0.01  
NIR-4 5:40:57.64 -2:07:13.2 17.68 $\pm$ 0.10 16.00 $\pm$ 0.10 14.93 $\pm$ 0.14 0.78 $\pm$ 0.01 0.66 $\pm$ 0.01  
NIR-5 5:40:58.36 -2:11:34.6 15.62 $\pm$ 0.06 14.38 $\pm$ 0.04 13.61 $\pm$ 0.05 2.09 $\pm$ 0.02 1.33 $\pm$ 0.01  
NIR-6 5:40:59.39 -2:21:24.8 14.82 $\pm$ 0.04 14.18 $\pm$ 0.03 13.59 $\pm$ 0.05 2.14 $\pm$ 0.02 1.78 $\pm$ 0.01  
NIR-7 5:41:05.54 -2:27:17.9 18.37 $\pm$ 0.01 16.04 $\pm$ 0.13 14.36 $\pm$ 0.07 1.64 $\pm$ 0.01 1.31 $\pm$ 0.01 B33-31
NIR-8 5:41:14.12 -2:29:01.6 17.01 $\pm$ 0.18 15.84 $\pm$ 0.12 15.68 $\pm$ 0.26 0.42 $\pm$ 0.01 0.234 $\pm$ 0.01 B33-33
NIR-9 5:41:15.61 -2:14:49.1 18.70 $\pm$ 0.10 16.21 $\pm$ 0.17 15.10 $\pm$ 0.15 0.44 $\pm$ 0.01 0.36 $\pm$ 0.01  
NIR-10 5:41:18.30 -2:17:13.6 16.83 $\pm$ 0.15 15.10 $\pm$ 0.06 14.38 $\pm$ 0.08 0.72 $\pm$ 0.01 0.57 $\pm$ 0.01  
NIR-11 5:41:19.79 -2:22:09.2 18.27 $\pm$ 0.10 16.01 $\pm$ 0.13 14.87 $\pm$ 0.13 0.50 $\pm$ 0.01 0.38 $\pm$ 0.01  
NIR-12 5:41:22.48 -2:09:15.0 16.93 $\pm$ 0.10 15.74 $\pm$ 0.13 14.60 $\pm$ 0.11 0.74 $\pm$ 0.01 0.69 $\pm$ 0.01  
NIR-13 5:41:22.49 -2:17:18.6 14.68 $\pm$ 0.04 12.95 $\pm$ 0.03 12.05 $\pm$ 0.02 8.05 $\pm$ 0.03 6.89 $\pm$ 0.03  
NIR-14 5:41:30.06 -2:14:47.7 17.67 $\pm$ 0.10 15.54 $\pm$ 0.10 14.42 $\pm$ 0.08 0.85 $\pm$ 0.01 0.76 $\pm$ 0.01  
NIR-15 5:41:31.93 -2:17:25.7 17.19 $\pm$ 0.10 16.03 $\pm$ 0.10 15.00 $\pm$ 0.17 0.64 $\pm$ 0.01 1.18 $\pm$ 0.01 HH 247
NIR-16 5:41:32.67 -2:10:51.9 16.93 $\pm$ 0.14 15.14 $\pm$ 0.06 14.46 $\pm$ 0.09 0.72 $\pm$ 0.01 0.56 $\pm$ 0.01  
NIR-17 5:41:32.73 -2:13:17.5 17.29 $\pm$ 0.23 15.55 $\pm$ 0.10 14.47 $\pm$ 0.08 0.82 $\pm$ 0.01 0.79 $\pm$ 0.01  
NIR-18 5:41:32.75 -2:24:22.0 18.65 $\pm$ 0.10 16.20 $\pm$ 0.15 14.74 $\pm$ 0.10 1.01 $\pm$ 0.01 0.82 $\pm$ 0.01  
NIR-19 5:41:32.97 -2:22:14.1 17.32 $\pm$ 0.10 16.16 $\pm$ 0.17 15.17 $\pm$ 0.14 0.53 $\pm$ 0.01 0.42 $\pm$ 0.01  
NIR-20 5:41:35.74 -2:08:55.8 17.20 $\pm$ 0.10 15.61 $\pm$ 0.11 14.69 $\pm$ 0.10 0.59 $\pm$ 0.01 0.47 $\pm$ 0.01  
NIR-21 5:41:35.74 -2:26:35.6 18.73 $\pm$ 0.10 15.95 $\pm$ 0.12 14.67 $\pm$ 0.10 0.79 $\pm$ 0.01 0.64 $\pm$ 0.01  
NIR-22 5:41:35.95 -2:30:16.3 18.59 $\pm$ 0.10 16.17 $\pm$ 0.16 14.80 $\pm$ 0.11 0.93 $\pm$ 0.01 0.78 $\pm$ 0.01  
NIR-23a 5:41:41.51 -2:15:43.9 11.38 $\pm$ 0.11 11.63 $\pm$ 0.11 14.10 $\pm$ 0.04 7.86 $\pm$ 0.08b 4.00 $\pm$ 0.04 WB 59
NIR-24a 5:41:43.09 -2:17:39.8 13.03 $\pm$ 0.03 12.35 $\pm$ 0.02 12.11 $\pm$ 0.03 4.90 $\pm$ 0.03 3.21 $\pm$ 0.02 WB 57
NIR-25c 5:41:44.22 -2:16:07.5 13.38 $\pm$ 0.04 12.51 $\pm$ 0.05 11.93 $\pm$ 0.04 14.67 $\pm$ 0.08 15.03 $\pm$ 0.07 13/W218
NIR-26 5:41:45.48 -2:19:46.4 17.52 $\pm$ 0.10 16.28 $\pm$ 0.18 14.95 $\pm$ 0.14 0.85 $\pm$ 0.01 0.69 $\pm$ 0.01  
NIR-27 5:41:46.67 -2:28:38.1 16.72 $\pm$ 0.14 15.98 $\pm$ 0.12 15.24 $\pm$ 0.17 0.45 $\pm$ 0.01 0.39 $\pm$ 0.00  
NIR-28 5:41:46.70 -2:17:13.9 16.92 $\pm$ 0.16 16.20 $\pm$ 0.18 15.26 $\pm$ 0.18 0.43 $\pm$ 0.01 0.38 $\pm$ 0.01  
NIR-29 5:41:50.44 -2:17:39.6 18.20 $\pm$ 0.10 16.39 $\pm$ 0.20 14.56 $\pm$ 0.12 1.11 $\pm$ 0.01 1.01 $\pm$ 0.01  
NIR-30 5:41:52.31 -2:16:11.8 16.42 $\pm$ 0.10 14.25 $\pm$ 0.07 12.97 $\pm$ 0.04 3.46 $\pm$ 0.02 2.88 $\pm$ 0.01  
NIR-31 5:41:56.21 -2:16:45.9 16.86 $\pm$ 0.18 16.30 $\pm$ 0.20 15.15 $\pm$ 0.10 0.40 $\pm$ 0.01 0.39 $\pm$ 0.01  

a H$\alpha$ emission line star (Weaver & Babcock 2004); b 3.6 $\mu $m photometry is unreliable due to severe contamination from PAH emission; c completely hidden in the Airy pattern of the of the exceedingly bright star L1630MIR-72 at both 5.8 and 8.0 $\mu $m; d integers correspond to NIR sources detected by Depoy et al. (1990), WB stands for sources detected by Weaver & Babcock (2004), W are sources detected by Witt et al. (1984) and B33 are names from Bowler et al. (2009).


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