Near-infrared evolution of the equatorial ring of SN 1987A

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Table 6

Fluxes of relatively strong emission lines in the SINFONI spectra in units of 10⁻¹⁵ erg s⁻¹ cm⁻².

Day	[Fe II] 1.533 µm	[Fe II] 1.644 µm	He I 1.701 µm	Br 10 1.737 µm	[Fe II] 2.050 µm	He I 2.058 µm	He I 2.113 µm	Brγ 2.166 µm
6832	2.16±0.33	5.72±0.82	1.78±0.26	2.42±0.36	1.16±0.18	14.6±2.1	1.07+0.18	7.9+1.2
7612	3.19±0.48	7.54±1.08	2.54±0.37	2.74±0.40	1.67±0.24	17.8±2.6	1.31+0.20	9.2+1.4
8708	3.86±0.56	8.61±1.24	2.64±0.39	2.98±0.43	1.97±0.29	20.4±3.0	1.47+0.23	10.0+1.5
10111	3.41±0.49	8.01±1.15	1.82±0.28	2.39±0.36	2.23±0.32	17.9±2.6	1.30+0.20	8.5+1.3
11269	2.26±0.33	5.12±0.73	1.39±0.21	1.64±0.24	1.46±0.21	11.7±1.7	0.87+0.14	6.0+0.9

Notes. We include a systematic 10% error from flux calibration and another 10% from extraction in the uncertainties; this is the dominant error for the strong lines. The line fluxes have not been multiplied by a scaling factor.

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