Spectroscopic investigations of a filament reconnecting with coronal loops during a two-ribbon solar flare

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Table 1.

Fit parameters for the IRIS Si IV FUV spectrum. Individual components plotted in Fig. 8 are indicated.

Time	Line	I₀ [DN]	λ [Å]	v_D [km s⁻¹]	FWHM [Å]	FWHM [km s⁻¹]	Notes
	O IV	40.0 ± 1.5	1400.365 ± 0.012	−170.8 ± 2.7	0.706 ± 0.062	151.1 ± 13.3	Gaussian
00:30:20 UT	Si IV	361.6 ± 4.6	1401.797 ± 0.010	−207.9 ± 2.2	0.567 ± 0.023	121.2 ± 4.9	κ = 3.27 ± 0.50
	Si IV	79.4 ± 6.6	1402.423 ± 0.012	−74.2 ± 2.5	0.429 ± 0.227	91.6 ± 48.5	Gaussian
	Si IV	28.5 ± 15.3	1402.793 ± 0.016	+2.7 ± 3.6	0.220 ± 0.101	47.0 ± 21.6	Gaussian, weak

	O IV	22.2 ± 1.1	1400.788 ± 0.030	−80.3 ± 6.3	0.891 ± 0.122	190.6 ± 26.1	Gaussian, weak
00:32:54 UT	Si IV	64.8 ± 6.4	1401.922 ± 0.026	−181.3 ± 5.6	0.568 ± 0.123	121.4 ± 26.3	Gaussian
	Si IV	174.8 ± 3.5	1402.457 ± 0.014	−66.9 ± 3.0	0.681 ± 0.018	145.5 ± 3.8	Gaussian

	O IV	13.1 ± 1.3	1400.005 ± 0.033	−247.7 ± 7.1^a	0.721 ± 0.178	154.3 ± 38.1^a	Gaussian, weak
00:34:11 UT	?	97.2 ± 3.0	1401.443 ± 0.017	−283.1 ± 3.6^b	0.789 ± 0.080	168.6 ± 17.1^b	Gaussian
	Si IV	203.2 ± 2.7	1402.523 ± 0.008	−52.8 ± 1.8	0.820 ± 0.083	175.2 ± 17.7	Gaussian
	Si IV	239.7 ± 9.0	1403.182 ± 0.004	+88.1 ± 0.9	0.404 ± 0.016	86.4 ± 3.4	Gaussian

Notes.

^(a)

If interpreted as O IV.

^(b)

If interpreted as Si IV.

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